diff --git "a/B9E0T4oBgHgl3EQfQABU/content/tmp_files/load_file.txt" "b/B9E0T4oBgHgl3EQfQABU/content/tmp_files/load_file.txt" new file mode 100644--- /dev/null +++ "b/B9E0T4oBgHgl3EQfQABU/content/tmp_files/load_file.txt" @@ -0,0 +1,1327 @@ +filepath=/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf,len=1326 +page_content='MNRAS 000, 1–16 (0000) Preprint 6 January 2023 Compiled using MNRAS LATEX style file v3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 Inferring the impact of feedback on the matter distribution using the Sunyaev Zel’dovich effect: Insights from CAMELS simulations and ACT+DES data Shivam Pandey,1,2 Kai Lehman,3,4 Eric J.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Baxter,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 Yueying Ni,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 Daniel Angl´es-Alc´azar,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='6,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='7 Shy Genel,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='7,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 Francisco Villaescusa-Navarro,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='7 Ana Maria Delgado,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 Tiziana di Matteo9 1Department of Physics,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Columbia University,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' New York,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' NY,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' USA 10027 2Department of Physics and Astronomy,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' University of Pennsylvania,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Philadelphia,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' PA 19104,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' USA 3Institute for Astronomy,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' University of Hawai‘i,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2680 Woodlawn Drive,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Honolulu,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' HI 96822,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' USA 4Universit¨ats-Sternwarte M¨unchen,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Fakult¨at f¨ur Physik,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Ludwig-Maximilians-Universit¨at,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Scheinerstr.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 1,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 81679 M¨unchen,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Germany 5Center for Astrophysics | Harvard & Smithsonian,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Cambridge,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' MA 02138,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' US 6Department of Physics,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' University of Connecticut,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 196 Auditorium Road,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' U-3046,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Storrs,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' CT,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 06269,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' USA 7Center for Computational Astrophysics,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Flatiron Institute,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 162 5th Avenue,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' New York,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' NY,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 10010,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' USA 9McWilliams Center for Cosmology,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Department of Physics,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Carnegie Mellon University,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Pittsburgh,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' PA 15213 6 January 2023 ABSTRACT Feedback from active galactic nuclei and stellar processes changes the matter distri- bution on small scales,' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' leading to significant systematic uncertainty in weak lensing constraints on cosmology.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We investigate how the observable properties of group-scale halos can constrain feedback’s impact on the matter distribution using Cosmology and Astrophysics with MachinE Learning Simulations (CAMELS).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Extending the results of previous work to smaller halo masses and higher wavenumber, k, we find that the baryon fraction in halos contains significant information about the impact of feed- back on the matter power spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We explore how the thermal Sunyaev Zel’dovich (tSZ) signal from group-scale halos contains similar information.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Using recent Dark Energy Survey (DES) weak lensing and Atacama Cosmology Telescope (ACT) tSZ cross-correlation measurements and models trained on CAMELS, we obtain 10% con- straints on feedback effects on the power spectrum at k ∼ 5 h/Mpc.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We show that with future surveys, it will be possible to constrain baryonic effects on the power spec- trum to O(< 1%) at k = 1 h/Mpc and O(3%) at k = 5 h/Mpc using the methods that we introduce here.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Finally, we investigate the impact of feedback on the matter bispectrum, finding that tSZ observables are highly informative in this case.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Key words: large-scale structure of Universe – methods: statistical 1 INTRODUCTION The statistics of the matter distribution on scales k ≳ 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 hMpc−1 are tightly constrained by current weak lensing surveys (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Asgari et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2021;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Abbott et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' How- ever, modeling the matter distribution on these scales to ex- tract cosmological information is complicated by the effects of baryonic feedback (Rudd et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2008).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Energetic output from active galactic nuclei (AGN) and stellar processes (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' winds and supernovae) directly impacts the distribution of gas on small scales, thereby changing the total matter dis- tribution (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Chisari et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2019).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 The coupling between these processes and the large-scale gas distribution is chal- lenging to model theoretically and in simulations because of the large dynamic range involved, from the scales of individ- ual stars to the scales of galaxy clusters.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' While it is generally agreed that feedback leads to a suppression of the matter power spectrum on scales 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 hMpc−1 ≲ k ≲ 20 hMpc−1, the amplitude of this suppression remains uncertain by tens of percent (van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2020;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Villaescusa-Navarro et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 1 Changes to the gas distribution can also gravitationally influ- ence the dark matter distribution, further modifying the total matter distribution.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' © 0000 The Authors arXiv:2301.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='02186v1 [astro-ph.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='CO] 5 Jan 2023 2 Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2021) (see also Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 1).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This systematic uncertainty limits constraints on cosmological parameters from current weak lensing surveys (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Abbott et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Asgari et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For future surveys, such as the Vera Rubin Observatory LSST (The LSST Dark Energy Science Collaboration et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2018) and Euclid (Euclid Collaboration et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2020), the problem will become even more severe given expected in- creases in statistical precision.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In order to reduce the sys- tematic uncertainties associated with feedback, we would like to identify observable quantities that carry information about the impact of feedback on the matter distribution and develop approaches to extract this information (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Nicola et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Recently, van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020) showed that the halo baryon fraction, fb, in halos with M ∼ 1014 M⊙ carries sig- nificant information about suppression of the matter power spectrum caused by baryonic feedback.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' They found that the relation between fb and matter power suppression was ro- bust to at least some changes in the subgrid prescriptions for feedback physics.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that fb as defined by van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020) counts baryons in both the intracluster medium as well as those in stars.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The connection between fb and feed- back is expected, since one of the main drivers of feedback’s impact on the matter distribution is the ejection of gas from halos by AGN.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Therefore, when feedback is strong, halos will be depleted of baryons and fb will be lower.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The conversion of baryons into stars — which will not significantly impact the matter power spectrum on large scales — does not im- pact fb, since fb includes baryons in stars as well as the ICM.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020) specifically consider the measure- ment of fb in halos with 6 × 1013M⊙ ≲ M500c ≲ 1014 M⊙.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In much more massive halos, the energy output of AGN is small compared to the binding energy of the halo, preventing gas from being expelled.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In smaller halos, van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020) found that the correlation between power spectrum suppression and fb is less clear.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Although fb carries information about feedback, it is somewhat unclear how one would measure fb in practice.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Observables such as the kinematic Sunyaev Zel’dovich (kSZ) effect can be used to constrain the gas density;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' combined with some estimate of stellar mass, fb could then be in- ferred.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' However, measuring the kSZ is challenging, and cur- rent measurements have low signal-to-noise (Hand et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2012;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Hill et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2016;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Soergel et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2016).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Moreover, van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020) consider a relatively limited range of feedback prescriptions.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' It is unclear whether a broader range of feedback models could lead to a greater spread in the relationship between fb and baryonic effects on the power spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In any case, it is worthwhile to consider other potential observational probes of feedback.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Another potentially powerful probe of baryonic feed- back is the thermal SZ (tSZ) effect.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The tSZ effect is caused by inverse Compton scattering of CMB photons with a pop- ulation of electrons at high temperature.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This scattering pro- cess leads to a spectral distortion in the CMB that can be reconstructed from multi-frequency CMB observations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The amplitude of this distortion is sensitive to the line-of-sight integral of the electron pressure.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Since feedback changes the distribution and thermodynamics of the gas, it stands to rea- son that it could impact the tSZ signal.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Indeed, several works using both data (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2019, 2022;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Gatti et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022a) and simulations (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Scannapieco et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2008;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Bhat- tacharya et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2008;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Moser et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Wadekar et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022) have shown that the tSZ signal from low-mass (group scale) halos is sensitive to feedback.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Excitingly, the sensitivity of tSZ measurements is expected to increase dramatically in the near future due to high-sensitivity CMB measurements from e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' SPT-3G (Benson et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2014), Advanced ACTPol (Henderson et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2016), Simons Observatory (Ade et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2019), and CMB Stage 4 (Abazajian et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2016).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The goal of this work is to investigate what informa- tion the tSZ signals from low-mass halos contain about the impact of feedback on the small-scale matter distribution.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The tSZ signal, which we denote with the Compton y pa- rameter, carries different information from fb.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For one, y is sensitive only to the gas and not to stellar mass.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Moreover, y carries sensitivity to both the gas density and tempera- ture, unlike fb which depends only on the gas density.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The y signal is also easier to measure than fb, since it can be estimated simply by cross-correlating halos with a tSZ map.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The signal-to-noise of such cross-correlation measurements is already high with current data, on the order of 10s of σ (Vikram et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2017;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2019, 2022;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' S´anchez et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In this paper, we investigate the information content of the tSZ signal from group-scale halos using the Cosmol- ogy and Astrophysics with MachinE Learning Simulations (CAMELS) simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' As we describe in more detail in §2, CAMELS is a suite of many hydrodynamical simula- tions run across a range of different feedback prescriptions and different cosmological parameters.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The relatively small volume of the CAMELS simulations ((25/h)3 Mpc3) means that we are somewhat limited in the halo masses and scales that we can probe.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We therefore view our analysis as an ex- ploratory work that investigates the information content of low-mass halos for constraining feedback and how to extract this information;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' more accurate results over a wider range of halo mass and k may be obtained in the future using the same methods applied to larger volume simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' By training statistical models on the CAMELS sim- ulations, we explore what information about feedback ex- ists in tSZ observables, and how robust this information is to changes in subgrid feedback prescriptions.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We consider three very different prescriptions for feedback based on the SIMBA (Dav´e et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2019), Illustris-TNG (Pillepich et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2018, henceforth TNG) and Astrid (Bird et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Ni et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022) models across a wide range of possible parameter val- ues, including variations in cosmology.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The flexibility of the statistical models we employ means that it is possible to uncover more complex relationships between e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' fb, y, and the baryonic suppression of the power spectrum than consid- ered in van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The work presented here is complementary to Delgado et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2023) which explores the information content in the baryon fraction of halos en- compassing broader mass range (M > 1010M⊙/h), finding a broad correlation with the matter power suppression.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Finally, we apply our trained statistical models to recent measurements of the y signal from low-mass halos by Gatti et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022a) and Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' These analyses in- ferred the halo-integrated y signal from the cross-correlation of galaxy lensing and the tSZ effect using lensing data from the Dark Energy Survey (DES) (Amon et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Secco et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022) and tSZ measurements from the Atacama Cos- mology Telescope (ACT) (Madhavacheril et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2020).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In MNRAS 000, 1–16 (0000) Probing feedback with the SZ 3 addition to providing interesting constraints on the impact of feedback, these results highlight the potential of future similar analyses with e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Dark Energy Spectroscopic Ex- periment (DESI;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' DESI Collaboration et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2016), Simons Observatory (Ade et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2019), and CMB Stage 4 (Abaza- jian et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2016).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Two recent works — Moser et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022) and Wadekar et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022) — have used the CAMELS simulations to ex- plore the information content of the tSZ signal for constrain- ing feedback.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' These works focus on the ability of tSZ ob- servations to constrain the parameters of subgrid feedback models in hydrodynamical simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Here, in contrast, we attempt to connect the observable quantities directly to the impact of feedback on the matter power spectrum and bis- pectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Additionally, unlike some of the results presented in Moser et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022) and Wadekar et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022), we consider the full parameter space explored by the CAMELS simula- tions rather than the small variations around a fiducial point that are relevant to calculation of the Fisher matrix.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Finally, we only focus on the intra-halo gas profile of the halos in the mass range captured by the CAMELS simulations (c.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='f.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Moser et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We do not expect the inter-halo gas pres- sure to be captured by the small boxes used here as it may be sensitive to higher halo masses (Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2020).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Nonlinear evolution of the matter distribution induces non-Gaussianity, and hence there is additional information to be recovered beyond the power spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Recent mea- surements detect higher-order matter correlations at cos- mological scales at O(10σ)(Secco et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Gatti et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022b), and the significance of these measurements is ex- pected to rapidly increase with up-coming surveys (Pyne & Joachimi 2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Jointly analyzing two-point and three- point correlations of the matter field can help with self- calibration of systematic parameters and improve cosmolog- ical constraints.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' As described in Foreman et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020), the matter bispectrum is expected to be impacted by baryonic physics at O(10%) over the scales of interest.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' With these considerations in mind, we also investigate whether the SZ observations carry information about the impact of baryonic feedback on the matter bispectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The plan of the paper is as follows.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In §2 we discuss the CAMELS simulation and the data products that we use in this work.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In §3, we present the results of our explorations with the CAMELS simulations, focusing on the information content of the tSZ signal for inferring the impact of feedback on the matter distribution.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In §4, we apply our analysis to the DES and ACT measurements.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We summarize our results and conclude in §5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2 CAMELS SIMULATIONS AND OBSERVABLES 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 Overview of CAMELS simulations We investigate the use of SZ signals for constraining the impact of feedback on the matter distribution using approx- imately 3000 cosmological simulations run by the CAMELS collaboration (Villaescusa-Navarro et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' One half of these are gravity-only N-body simulations and the other half are hydrodynamical simulations with matching initial con- ditions.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The simulations are run using three different hy- drodynamical sub-grid codes, TNG (Pillepich et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2018), SIMBA (Dav´e et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2019) and Astrid (Bird et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Ni et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' As detailed in Villaescusa-Navarro et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2021), for each sub-grid implementation six parameters are varied: two cosmological parameters (Ωm and σ8) and four param- eters dealing with baryonic astrophysics.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Of these, two deal with supernovae feedback (ASN1 and ASN2) and two deal with AGN feedback (AAGN1 and AAGN2).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The meanings of the feedback parameters for each subgrid model are summa- rized in Table 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that the astrophysical parameters have somewhat different physical meanings for the different subgrid pre- scriptions, and there is usually a complex interplay between the parameters and their impact on the properties of galax- ies and gas.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For example, the parameter ASN1 approximately corresponds to the pre-factor for the overall energy output in galactic wind feedback per-unit star-formation in both the TNG (Pillepich et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2018) and Astrid (Bird et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022) sim- ulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' However, in the SIMBA simulations it corresponds to the to the wind-driven mass outflow rate per unit star- formation calibrated from the Feedback In Realistic Envi- ronments (FIRE) zoom-in simulations (Angl´es-Alc´azar et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2017b).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Similarly, the AAGN2 parameter controls the bursti- ness and the temperature of the heated gas during the AGN bursts in the TNG simulations (Weinberger et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2017).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In the SIMBA suite, it corresponds to the speed of the kinetic AGN jets with constant momentum flux (Angl´es-Alc´azar et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2017a;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Dav´e et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2019).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' However, in the Astrid suite, it corresponds to the efficiency of thermal mode of AGN feedback.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' As we describe in § 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2, this can result in counter- intuitive impact on the matter power spectrum in the Astrid simulation, relative to TNG and SIMBA.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For each of the sub-grid physics prescriptions, three va- rieties of simulations are provided.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' These include 27 sims for which the parameters are fixed and initial conditions are varied (cosmic variance, or CV, set), 66 simulations varying only one parameter at a time (1P set) and 1000 sims varying parameters in a six dimensional latin hyper-cube (LH set).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We use the CV simulations to estimate the variance expected in the matter power suppression due to stochasticity (see Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 1).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We use the 1P sims to understand how the matter suppression responds to variation in each parameter individ- ually.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Finally we use the full LH set to effectively marginalize over the full parameter space varying all six parameters.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We use publicly available power spectrum and bispectrum mea- surements for these simulation boxes (Villaescusa-Navarro et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 Where unavailable, we calculate the power spectrum and bispectrum, using the publicly available code Pylians.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 Baryonic effects on the power spectrum and bispectrum The left panel of Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 1 shows the measurement of the power spectrum suppression caused by baryonic effects in the TNG, SIMBA, and Astrid simulations for their fiducial feedback settings.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The right two panels of the figure show the impact of baryonic effects on the bispectrum for two different 2 See also https://www.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='camel-simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='org/data.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3 https://github.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='com/franciscovillaescusa/Pylians3 MNRAS 000, 1–16 (0000) 4 Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='Simulation ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='Type/Code ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='Astrophysical parameters varied ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='& its meaning ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='TNG ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='Magneto-hydrodynamic/ ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='AREPO ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='ASN1: (Energy of Galactic winds)/SFR ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='ASN2: Speed of galactic winds ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='AAGN1: Energy/(BH accretion rate) ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='AAGN2: Jet ejection speed or burstiness ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='SIMBA ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='Hydrodynamic/GIZMO ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='ASN1 : Mass loading of galactic winds ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='ASN2 : Speed of galactic winds ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='AAGN1 : Momentum flux in QSO and jet mode of feedback ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='AAGN2 : Jet speed in kinetic mode of feedback ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='Astrid ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='Hydrodynamic/pSPH ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='ASN1: (Energy of Galactic winds)/SFR ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='ASN2: Speed of galactic winds ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='AAGN1: Energy/(BH accretion rate) ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='AAGN2: Thermal feedback efficiency ' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='Table 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Summary of the three feedback models used in this analysis.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For each model, four feedback parameters are varied: AAGN1, AAGN2, ASN1, and ASN2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The meanings of these parameters are different for each model, and are summarized in the rightmost column.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In addition to these four astrophysical parameters, the cosmological parameters Ωm and σ8 were also varied.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 100 101 k (h/Mpc) −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='6 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 ∆P/PDMO Illustris-TNG Illustris-TNG (LH suite) SIMBA Astrid 100 101 keq (h/Mpc) −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='6 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 ∆Beq/Beq;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='DMO 100 101 ksq (h/Mpc) −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='6 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 ∆Bsq/Bsq;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='DMO Figure 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Far left: Baryonic suppression of the matter power spectrum, ∆P/PDMO, in the CAMELS simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The dark-blue, red and orange shaded regions correspond to the 1σ range of the cosmic variance (CV) suite of TNG, SIMBA and Astrid simulations, respectively.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The light-blue region corresponds to the 1σ range associated with the latin hypercube (LH) suite of TNG, illustrating the range of feedback models explored across all parameter values.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Middle and right panels: the impact of baryonic feedback on the matter bispectrum for equilateral and squeezed triangle configurations, respectively.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' tringle configurations (equilateral and squeezed).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' To com- pute these quantitites, we use the matter power spectra and bispectra of the hydrodynamical simulations (hydro) and the dark-matter only (DMO) simulations generated at varying initial conditions (ICs).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For each of the 27 unique IC runs, we calculate the ratios ∆P/PDMO = (Phydro−PDMO)/PDMO and ∆B/BDMO = (Bhydro − BDMO)/BDMO.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' As the hydro- dynamical and the N-body simulations are run with same initial conditions, the ratios ∆P/PDMO and ∆B/BDMO are roughly independent of sample variance.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' It is clear that the amplitude of suppression of the small-scale matter power spectrum can be significant: sup- pression on the order of tens of percent is reached for all three simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' It is also clear that the impact is sig- nificantly different between the three simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Even for the simulations in closest agreement (TNG and Astrid), the measurements of ∆P/PDMO disagree by more than a fac- tor of two at k = 5 h/Mpc.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The width of the curves in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 1 represents the standard deviation measured across the cosmic variance simulations, which all have the same parameter values but different initial conditions.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For the bis- pectrum, we show both the equilateral and squeezed trian- gle configurations with cosine of angle between long sides fixed to µ = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='9.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Interestingly, the spread in ∆P/PDMO and ∆B/BDMO increases with increasing k over the range 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 h/Mpc ≲ k ≲ 10 h/Mpc.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This increase is driven by stochasticity arising from baryonic feedback.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The middle and right panels show the impact of feedback on the bis- pectrum for the equilateral and squeezed triangle configura- tions, respectively.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Throughout this work, we will focus on the regime 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 h/Mpc < k < 10 h/Mpc.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Larger scales modes are not present in the (25Mpc/h)3 CAMELS simulations, and in any case, the impact of feedback on large scales is typically small.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Much smaller scales, on the other hand, are difficult to model even in the absence of baryonic feedback (Schneider et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2016).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In Appendix A we show how the matter power suppression changes when varying the resolution and volume of the simulation boxes.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' When comparing with the original TNG boxes, we find that while the box sizes do not change MNRAS 000, 1–16 (0000) Probing feedback with the SZ 5 the measured power suppression significantly, the resolution of the boxes has a non-negligible impact.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This is expected since the physical effect of feedback mechanisms depend on the resolution of the simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that the errorbars presented in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 1 will also depend on the default choice of feedback values assumed.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 Measuring gas profiles around halos We use 3D grids of various fields (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' gas density and pres- sure) made available by the CAMELS team to extract the profiles of these fields around dark matter halos.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The grids are generated with resolution of 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='05 Mpc/h.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Following van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020), we define fb as (Mgas + Mstars)/Mtotal, where Mgas, Mstars and Mtotal are the mass in gas, stars and all the components, respectively.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The gas mass is computed by integrating the gas number density profile around each halo.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We typically measure fb within the spherical overden- sity radius r500c.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 The SZ effect is sensitive to the electron pressure.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We compute the electron pressure profiles, Pe, using Pe = 2(XH + 1)/(5XH + 3)Pth, where Pth is the total thermal pressure, and XH = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='76 is the primordial hydrogen frac- tion.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Given the electron pressure profile, we measure the integrated SZ signal within r500c as: Y500c = σT mec2 � r500c 0 4πr2 Pe(r) dr, (1) where, σT is the Thomson scattering cross-section, me is the electron mass and c is the speed of light.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We normalize the SZ observables by the self-similar ex- pectation (Battaglia et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2012b),5 Y SS = 131.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='7h−1 70 � M500c 1015h−1 70 M⊙ �5/3 Ωb 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='043 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='25 Ωm kpc2, (2) where, M200c is mass inside r200c and h70 = h/0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This cal- culation, which scales as M 5/3, assumes hydrostatic equilib- rium and that the baryon fraction is equal to cosmic bary- onic fraction.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Hence deviations from this self-similar scaling provide a probe of the effects of baryonic feedback.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Our final SZ observable is defined as Y500c/Y SS.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' On the other hand, the amplitude of the pressure profile approximately scales as M 2/3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Therefore, when considering the pressure profile as the observable, we factor out a M 2/3 scaling.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3 RESULTS I: SIMULATIONS 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 Inferring feedback parameters from fb and y We first consider how the halo Y signal can be used to con- strain the parameters describing the subgrid physics mod- els.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This question has been previously investigated using the CAMELS simulations by Moser et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022) and Wadekar 4 We define spherical overdensity radius (r∆c, where ∆ = 200, 500) and overdensity mass (M∆c) such that the mean density within r∆ is ∆ times the critical density ρcrit, M∆ = ∆ 4 3 πr3 ∆ρcrit.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 5 Note that we use spherical overdensity mass corresponding to ∆ = 500 and hence adjust the coefficients accordingly, while keep- ing other approximations used in their derivations as the same.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The rest of our analysis will focus on constrain- ing changes to the power spectrum and bispectrum, and our intention here is mainly to provide a basis of comparison for those results.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Similar to Wadekar et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022), we treat the mean log(Y500c/M 5/3) value of all the halos in two mass bins (1012 < M(M⊙/h) < 5 × 1012 and 5 × 1012 < M(M⊙/h) < 1014) as our observable;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' we refer to this observable as ⃗d.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In this section, we restrict our analysis to only the TNG simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Here and throughout our investigations with CAMELS we ignore the contributions of measurement un- certainty since our intention is mainly to assess the infor- mation content of the SZ signals.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We therefore use the CV simulations to determine the covariance, C, of the ⃗d.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that the level of cosmic variance will depend on the volume probed, and can be quite large for the CAMELS simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Given this covariance, we use the Fisher matrix formalism to forecast the precision with which the feedback and cos- mological parameters can be constrained.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The Fisher matrix, Fij, is given by Fij = ∂ ⃗dT ∂θi C−1 ∂ ⃗d ∂θi , (3) where θi refers to the ith parameter value.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Calculation of the derivatives ∂ ⃗d/∂θi is complicated by the large amount of stochasticity between the CAMELS simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' To per- form the derivative calculation, we use a radial basis function interpolation method based on Moser et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022);' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Cromer et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We show an example of the derivative calcu- lation in Appendix B.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We additionally assume a Gaussian prior on parameter p with σ(ln p) = 1 for the feedback pa- rameters and σ(p) = 1 for the cosmological parameters.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The forecast parameter covariance matrix, Cp, is then related to the Fisher matrix by Cp = F−1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The parameter constraints corresponding to our calcu- lated Fisher matrix are shown in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We show results only for Ωm, ASN1 and AAGN2, but additionally marginalize over σ8, ASN2 and AAGN1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The degeneracy directions seen in our results are consistent with those in Wadekar et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We we find a weaker constraint on AAGN2, likely owing to the large sample variance contribution to our calculation.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' It is clear from Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2 that the marginalized constraints on the feedback parameters are weak.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' If information about Ωm is not used, we effectively have no information about the feedback parameters.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Even when Ωm is fixed, the con- straints on the feedback parameters are not very precise.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This finding is consistent with Wadekar et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022), for which measurement uncertainty was the main source of vari- ance rather than sample variance.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Part of the reason for the poor constraints is the degeneracy between the AGN and SN parameters.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' As we show below, the impacts of SN and AGN feedback can have opposite impacts on the Y signal;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' more- over, even AAGN1 and AAGN2 can have opposite impacts on Y .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' These degeneracies, as well as degeneracies with cosmo- logical parameters like Ωm, make it difficult to extract tight constraints on the feedback parameters from measurements of Y .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' However, for the purposes of cosmology, we are ul- timately most interested in the impact of feedback on the matter distribution, and not the values of the feedback pa- rameters themselves.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' These considerations motivate us to instead explore direct inference of changes to the statistics MNRAS 000, 1–16 (0000) 6 Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 0 1 Ωm −2 0 2 log(AAGN2) −2 0 2 log(ASN1) −2 0 2 log(ASN1) −2 0 2 log(AAGN2) Free Ωm and σ8 Fixed Ωm and σ8 Figure 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Forecast constraints on the feedback parameters when log Y500c/Y SS in two halo mass bins is treated as the observable.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Even when the cosmological model is fixed (red contours), the AGN parameters (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' AAGN2) remain effectively unconstrained (note that we impose a Gaussian prior with σ(ln p) = 1 on all feed- back parameters, p).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' When the cosmological model is free (blue contours), all feedback parameters are unconstrained.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We assume that the only contribution to the variance of the observable is sample variance coming from the finite volume of the CAMELS simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' of the matter distribution from the Y observables.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This will be the focus of the rest of the paper.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 fb and y as probes of baryonic effects on the matter power spectrum As discussed above, van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020) observed a tight correlation between suppression of the matter power spec- trum and the baryon fraction, fb, in halos with 6×1013M⊙ ≲ M500c ≲ 1014 M⊙.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' That relation was found to hold regard- less of the details of the feedback implementation, suggest- ing that by measuring fb, one could robustly infer the im- pact of baryonic feedback on the power spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We be- gin by investigating the connection between matter power spectrum suppression and integrated tSZ parameter in low- mass, M ∼ 1013 M⊙, halos to test if similar correlation ex- ists (c.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='f.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Delgado et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2023) for a similar figure between fb and ∆P/PDMO).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We also consider a wider range of feedback models than van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020), including the SIMBA and Astrid models.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3 shows the impact of cosmological and feed- back parameters on the relationship between the power spectrum suppression (∆P/PDMO) and the ratio Y500c/Y SS for the SIMBA simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Each point corresponds to a single simulation, taking the average over all halos with 1013 < M(M⊙/h) < 1014 when computing Y500c/Y SS.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that since the halo mass function rapidly declines at high masses, the average will be dominated by the low mass ha- los.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We observe that the largest suppression (i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' more nega- tive ∆P/PDMO) occurs when AAGN2 is large.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This is caused by powerful AGN jet-mode feedback ejecting gas from halos, −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 ∆P/PDMO −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 ∆P/PDMO −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 ∆P/PDMO −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 ∆P/PDMO −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 ∆P/PDMO 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='6 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='8 Y500c/YSS −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 ∆P/PDMO 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 Ωm 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='7 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='8 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='9 σ8 1 2 3 ASN1 1 2 3 AAGN1 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='75 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='00 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='25 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='50 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='75 ASN2 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='75 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='00 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='25 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='50 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='75 AAGN2 Figure 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We show the relation between matter power suppres- sion at k = 2h/Mpc and the integrated tSZ signal, Y500c/Y SS, of halos in the mass range 1013 < M (M⊙/h) < 1014 in the SIMBA simulation suite.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In each of six panels, the points are col- ored corresponding to the parameter value given in the associated colorbar.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' MNRAS 000, 1–16 (0000) Probing feedback with the SZ 7 leading to a significant reduction in the matter power spec- trum, as described by e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020);' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Borrow et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020);' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Gebhardt et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2023).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For SIMBA, the pa- rameter AAGN2 controls the velocity of the ejected gas, with higher velocities (i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' higher AAGN2) leading to gas ejected to larger distances.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' On the other hand, when ASN2 is large, ∆P/PDMO is small.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This is because efficient supernovae feed- back prevents the formation of massive galaxies which host AGN and hences reduces the strength of the AGN feedback.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The parameter AAGN1, on the other hand, controls the radia- tive quasar mode of feedback, which has slower gas outflows and thus a smaller impact on the matter distribution.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' It is also clear from Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3 that increasing Ωm reduces |∆P/PDMO|, relatively independently of the other parame- ters.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' By increasing Ωm, the ratio Ωb/Ωm decreases, meaning that halos of a given mass have fewer baryons, and the im- pact of feedback is therefore reduced.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We propose a very simple toy model for this effect in §3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The impact of σ8 in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3 is less clear.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For halos in the mass range shown, we find that increasing σ8 leads to a roughly monotonic decrease in Y500c (and fb), presumably because higher σ8 means that there are more halos amongst which the same amount of baryons must be distributed.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This effect would not occur for cluster-scale halos because these are rare and large enough to gravitationally dominate their local environments, giving them fb ∼ Ωb/Ωm, regardless of σ8.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In any case, no clear trend with σ8 is seen in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3 because σ8 does not correlate strongly with ∆P/PDMO.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 4 shows the relationship between ∆P/PDMO at k = 2 h/Mpc and fb or Y500c in different halo mass bins and for different amounts of feedback, colored by the value of AAGN2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' As in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3, each point represents an average over all halos in the indicated mass range for a particular CAMELS simulation (i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' at fixed values of cosmological and feedback parameters).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that the meaning of AAGN2 is not exactly the same across the different feedback models, as noted in §2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For TNG and SIMBA we expect increasing AAGN2 to lead to stronger AGN feedback driving more gas out of the halos, leading to more power suppression with- out strongly regulating the growth of black holes.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' However, for Astrid, increasing AAGN2 parameter would more strongly regulate and suppress the black hole growth in the box since controls the efficiency of thermal mode of AGN feedback (Ni et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This drastically reduces the number of high mass black holes and hence effectively reducing the amount of feedback that can push the gas out of the halos, leading to less matter power suppression.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We see this difference re- flected in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 4 where for the Astrid simulations the points corresponding to high AAGN2, result in ∆P/PDMO ∼ 0, in contrast to TNG and SIMBA suite of simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For the highest mass bin (1013 < M(M⊙/h) < 1014, rightmost column of Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 4) our results are in agreement with van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020): we find that there is a robust corre- lation between between fb/(Ωb/Ωm) and the matter power suppression (also see Delgado et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2023)).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This relation is roughly consistent across different feedback subgrid models, although the different models appear to populate different parts of this relation.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Moreover, varying AAGN2 appears to move points along this relation, rather than broadening the relation.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This is in contrast to Ωm, which as shown in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3, tends to move simulations in the direction orthogonal to the narrow Y500c-∆P/PDMO locus.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For this reason, and given current constraints on Ωm, we restrict Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 4 to simulations with 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 < Ωm < 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The dashed curves shown in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 4 correspond to the toy model discussed in §3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' At low halo mass, the relation between fb/(Ωb/Ωm) and ∆P/PDMO appears similar to that for the high-mass bin, although it is somewhat flatter at high fb, and some- what steeper at low fb.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Again the results are fairly consistent across the different feedback prescriptions, although points with high fb/(Ωb/Ωm) are largely absent for SIMBA.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This is because the feedback mechanisms are highly efficient in SIMBA, driving the gas out of their parent halos.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The relationships between Y and ∆P/PDMO appear quite similar to those between ∆P/PDMO and fb/(Ωb/Ωm).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This is not too surprising because Y is sensitive to the gas density, which dominates fb/(Ωb/Ωm).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' However, Y is also sensitive to the gas temperature.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Our results suggest that variations in gas temperature are not significantly impact- ing the Y500c-∆P/PDMO relation.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The possibility of using the tSZ signal to infer the impact of feedback on the matter distribution rather than fb/(Ωb/Ωm) is therefore appealing.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This will be the focus of the remainder of the paper.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 5 shows the same quantities as Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 4, but now for a fixed halo mass range (1013 < M/(M⊙/h) < 1014), fixed subgrid prescription (TNG), and varying values of k.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We find roughly similar results when using the different sub- grid physics prescriptions.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' At low k, we find that there is a regime at high fb/(Ωb/Ωm) for which ∆P/PDMO changes negligibly.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' It is only when fb/(Ωb/Ωm) becomes very low that ∆P/PDMO begins to change.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' On the other hand, at high k, there is a near-linear relation between fb/(Ωb/Ωm) and ∆P/PDMO.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 A toy model for power suppression We now describe a simple model for the effects of feedback on the relation between fb or Y and ∆P/PDMO that ex- plains some of the features seen in Figs.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3, 4 and 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We assume in this model that it is removal of gas from halos by AGN feedback that is responsible for changes to the matter power spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' SN feedback, on the other hand, can pre- vent gas from accreting onto the SMBH and therefore reduce the impact of AGN feedback (Angl´es-Alc´azar et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2017c;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Habouzit et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2017).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This scenario is consistent with the fact that at high SN feedback, we see that ∆P/PDMO goes to zero (second panel from the bottom in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Stellar feedback can also prevent gas from accreting onto low-mass halos (Pandya et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2020, 2021).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In some sense, the dis- tinction between gas that is ejected by AGN and gas that is prevented from accreting onto halos by stellar feedback does not matter for our simple model.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Rather, all that matters is that some amount of gas that would otherwise be in the halo is instead outside of the halo as a result of feedback effects, and it is this gas which is responsible for changes to the matter power spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We identify three relevant scales: (1) the halo radius, Rh, (2) the distance to which gas is ejected by the AGN, Rej, and (3) the scale at which the power spectrum is mea- sured, 2π/k.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' If Rej ≪ 2π/k, then there will be no impact on ∆P at k: this corresponds to a rearrangement of the matter distribution on scales well below where we measure the power spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' If, on the other hand, Rej ≪ Rh, then there will be no impact on fb or Y , since the gas is not MNRAS 000, 1–16 (0000) 8 Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 ∆P/PDMO Illustris-TNG 5 × 1012 < M(M⊙/h) < 1013 Illustris-TNG 5 × 1012 < M(M⊙/h) < 1013 Illustris-TNG 1013 < M(M⊙/h) < 1014 Illustris-TNG 1013 < M(M⊙/h) < 1014 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 ∆P/PDMO SIMBA 5 × 1012 < M(M⊙/h) < 1013 SIMBA 5 × 1012 < M(M⊙/h) < 1013 SIMBA 1013 < M(M⊙/h) < 1014 SIMBA 1013 < M(M⊙/h) < 1014 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='00 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='25 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='50 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='75 Y500c/YSS −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 ∆P/PDMO Astrid 5 × 1012 < M(M⊙/h) < 1013 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 fb/(Ωb/Ωm) Astrid 5 × 1012 < M(M⊙/h) < 1013 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 Y500c/YSS Astrid 1013 < M(M⊙/h) < 1014 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 fb/(Ωb/Ωm) Astrid 1013 < M(M⊙/h) < 1014 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 AAGN2 Figure 4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Impact of baryonic physics on the matter power spectrum at k = 2h/Mpc for the TNG, SIMBA and Astrid simulations (top, middle, and bottom rows).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Each point corresponds to an average across halos in the indicated mass ranges in a different CAMELS simulation.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We restrict the figure to simulations that have 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 < Ωm < 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The dashed curves illustrate the behavior of the model described in §3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 when the gas ejection distance is large compared to the halo radius and 2π/k.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 fb/(Ωb/Ωm) −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 ∆P/PDMO k = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='6 h/Mpc 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 fb/(Ωb/Ωm) k = 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 h/Mpc 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 fb/(Ωb/Ωm) k = 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 h/Mpc 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 fb/(Ωb/Ωm) k = 10.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 h/Mpc 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='6 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='8 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='6 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='8 AAGN2 Figure 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Similar to Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 4, but for different values of k.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For simplicity, we show only the TNG simulations for halos in the mass range 1013 < M(M⊙/h) < 1014.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The dashed curves illustrate the behavior of the model described in §3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 in the regime that the radius to which gas is ejected by AGN is larger than the halo radius, and larger than 2π/k.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' As expected, this model performs best in the limit of high k and large halo mass.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' ejected out of the halo.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We therefore consider four regimes defined by the relative amplitudes of Rh, Rej, and 2π/k, as described below.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that there is not a one-to-one corre- spondence between physical scale in configuration space and 2π/k;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' therefore, the inequalities below should be considered as approximate.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The four regimes are: Regime 1: Rej < Rh and Rej < 2π/k.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In this regime, changes to the feedback parameters have no impact on fb or ∆P.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Regime 2: Rej > Rh and Rej < 2π/k.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In this regime, changes to the feedback parameters result in movement along the fb or Y axis without changing ∆P.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Gas is be- ing removed from the halo, but the resultant changes to the matter distribution are below the scale at which we measure the power spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that Regime 2 cannot occur when Rh > 2π/k (i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' high-mass halos at large k).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' MNRAS 000, 1–16 (0000) Probing feedback with the SZ 9 Regime 3: Rej > Rh and Rej > 2π/k.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In this regime, chang- ing the feedback amplitude directly changes the amount of gas ejected from halos as well as ∆P/PDMO.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Regime 4: Rej < Rh and Rej > 2π/k.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In this regime, gas is not ejected out of the halo, so fb and Y should not change.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In principle, the redistribution of gas within the halo could lead to changes in ∆P/PDMO.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' However, as we discuss below, this does not seem to happen in practice.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Let us now consider the behavior of ∆P/PDMO and fb or Y as the feedback parameters are varied in Regime 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' A halo of mass M is associated with an overdensity δm in the absence of feedback, which is changed to δ′ m due to ejec- tion of baryons as a result of feedback.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In Regime 3, some amount of gas, Mej, is completely removed from the halo.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This changes the size of the overdensity associated with the halo to δ′ m δm = 1 − Mej M .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (4) The change to the power spectrum is then ∆P PDMO ∼ �δ′ m δm �2 − 1 ≈ −2Mej M , (5) where we have assumed that Mej is small compared to M.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We have ignored the k dependence here, but in Regime 3, the ejection radius is larger than the scale of interest, so the calculated ∆P/PDMO should apply across a range of k in this regime.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The ejected gas mass can be related to the gas mass in the absence of feedback.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We write the gas mass in the absence of feedback as fc(Ωb/Ωm)M, where fc encapsulates non-feedback processes that result in the halo having less than the cosmic baryon fraction.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We then have Mej = fc(Ωb/Ωm)M − fbM − M0, (6) where M0 is the mass that has been removed from the gaseous halo, but that does not change the power spectrum, e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' the conversion of gas to stars.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Substituting into Eq.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 5, we have ∆P PDMO = −2fcΩb Ωm � 1 − fbΩm fcΩb − ΩmM0 fcΩbM � .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (7) In other words, for Regime 3, we find a linear relation be- tween ∆P/PDMO and fbΩm/Ωb.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For high mass halos, we should have fc ≈ 1 and M0/M ≈ 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In this limit, the rela- tionship between fb and ∆P/PDMO becomes ∆P PDMO = −2 Ωb Ωm � 1 − fbΩm Ωb � , (8) which is linear between endpoints at (∆P/PDMO, fbΩm/Ωb) = (−2Ωb/Ωm, 0) and (∆P/PDMO, fbΩm/Ωb) = (0, 1).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We show this relation as the dashed line in the fb columns of Figs.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 4 and Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We can repeat the above argument for Y .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Unlike the case with fb, processes other than the removal of gas may reduce Y ;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' these include, e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=', changes to the gas temperature in the absence of AGN feedback, or nonthermal pressure sup- port.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We account for these with a term Y0, defined such that when Mej = M0 = 0, we have Y + Y0 = fc(Ωb/Ωm)MT/α, where we have assumed constant gas temperature, T, and α is a dimensionful constant of proportionality.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We ignore detailed modeling of variation in the temperature of the gas due to feedback and departures from hydro-static equilib- rium (Ostriker et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2005).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We then have α(Y + Y0) T = fc(Ωb/Ωm)M − Mej − M0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (9) Substituting the above equation into Eq.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 5 we have ∆P PDMO = −2fcΩb Ωm � 1 − α(Y + Y0)Ωm fcTMΩb − ΩmM0 fcΩbM � .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (10) Following Eq.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2, we define the self-similar value of Y , Y SS, via αY SS/T = (Ωb/Ωm)M, (11) leading to ∆P PDMO = −2fcΩb Ωm � 1 − (Y + Y0) fcY SS − ΩmM0 fcΩbM � .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (12) Again taking the limit that fc ≈ 1 and M0/M ≈ 0, we have ∆P PDMO = −2 Ωb Ωm � 1 − (Y + Y0) Y SS � .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (13) Thus, we see that in Regime 3, the relation between Y/Y SS and ∆P/PDMO is linear.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The Y/Y SS columns of Figs.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 4 show this relationship, assuming Y0 = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In summary, we interpret the results of Figs.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 4 and 5 in the following way.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Starting at low feedback amplitude, we are initially in Regime 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In this regime, the simulations clus- ter around fbfcΩm/Ωb ≈ 1 (or Y ≈ Y0) and ∆P/PDMO ≈ 0 since changing the feedback parameters in this regime does not impact fb or ∆P/PDMO.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For high mass halos, we have fc ≈ 1 and Y0 ≈ 0 (although SIMBA appears to have Y0 > 0, even at high mass);' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' for low mass halos, fc < 1 and Y0 > 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' As we increase the AGN feedback amplitude, the behavior is different depending on halo mass and k: For low halo masses or low k, increasing the AGN feed- back amplitude leads the simulations into Regime 2.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Increas- ing the feedback amplitude in this regime moves points to lower Y/Y SS (or fbΩm/Ωb) without significantly impacting ∆P/PDMO.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Eventually, when the feedback amplitude is suf- ficiently strong, these halos enter Regime 3, and we see a roughly linear decline in ∆P/PDMO with decreasing Y/Y SS (or fbΩm/Ωb), as discussed above.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' For high mass halos and high k, we never enter Regime 2 since it is not possible to have Rej > Rh and Rej < 2π/k when Rh is very large.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In this case, we eventually enter Regime 3, leading to a linear trend of decreasing ∆P/PDMO with decreasing Y/Y SS or fbΩm/Ωb, as predicted by the above discussion.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This behavior is especially clear in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 5: at high k, the trend closely follows the predicted linear rela- tion.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' At low k, on the other hand, we see a more prominent Regime 2 region.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The transition between these two regimes is expected to occur when k ∼ 2π/Rh, which is roughly 5 h−1Mpc for the halo mass regime shown in the figure.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This expectation is roughly confirmed in the figure.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Interestingly, we never see Regime 4 behavior: when the halo mass is large and k is large, we do not see rapid changes in ∆P/PDMO with little change to fb and Y .' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This could be because this regime corresponds to movement of the gas entirely within the halo.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' If the gas has time to re-equilibrate, it makes sense that we would see little change to ∆P/PDMO in this regime.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' MNRAS 000, 1–16 (0000) 10 Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 Predicting the power spectrum suppression from the halo observables While the toy model described above roughly captures the trends between Y (or fb) and ∆P/PDMO, it of course does not capture all of the physics associated with feedback.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' It is also clear that there is significant scatter in the relation- ships between observable quantities and ∆P.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' It is possible that this scatter is reduced in some higher dimensional space that includes more observables.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' To address both of these issues, we now train statistical models to learn the rela- tionships between observable quantities and ∆P/PDMO.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We will focus on results obtained with random forest regression (Breiman 2001).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We have also tried using neural networks to infer these relationships, but have not found any significant improvement with respect to the random forest results, pre- sumably because the space is low-dimensional (i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' we con- sider at most about five observable quantities at a time).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We leave a detailed comparison with other decision tree based approaches, such as gradient boosted trees (Friedman 2001) to a future study.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We train a random forest model to go from observable quantities (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' fb/(Ωb/Ωm) and Y500c/Y SS) to a prediction for ∆P/PDMO at multiple k values.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The random forest model uses 100 trees with a maxdepth = 10.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='6 In this section we an- alyze the halos in the mass bin 5 × 1012 < Mhalo(M⊙/h) < 1014 but we also show the results for halos with lower masses in Appendix D.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We also consider supplying the values of Ωm as input to the random forest, since it can be constrained precisely through other observations (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' primary CMB ob- servations), and as we showed in §3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2, the cosmological pa- rameters can impact the observables.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='7 Ultimately, we are interested in making predictions for ∆P/PDMO using observable quantities.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' However, the sam- ple variance in the CAMELS simulations limits the precision with which we can measure ∆P/PDMO.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' It is not possible to predict ∆P/PDMO to better than this precision.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We will therefore normalize the uncertainties in the RF predictions by the cosmic variance error.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In order to obtain the un- certainty in the predictions, we randomly split the data into 70% training and 30% test set.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' After training the RF regres- sor using the training set and a given observable, we make compute the 16th and 84th percentile of the distribution of prediction errors evaluated on the test set.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This constitutes our assessment of prediction uncertainty.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 6 shows the accuracy of the RF predictions for ∆P/PDMO when trained on stacked fb (for halos in 5 × 1012 < Mhalo(M⊙/h) < 1014) and Ωm, normalized to the sample variance error in ∆P/PDMO.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' As we will show later in this section, this combination of inputs results in pre- 6 We use a publicly available code: https://scikit-learn.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' org/stable/modules/generated/sklearn.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='ensemble.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' RandomForestRegressor.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='html.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We also verified that our conclusions are robust to changing the settings of the random forest.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 7 One might worry that using cosmological information to con- strain ∆P/PDMO defeats the whole purpose of constraining ∆P/PDMO in order to improve cosmological constraints.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' How- ever, observations, such as those of CMB primary anisotropies, already provide precise constraints on the matter density with- out using information in the small-scale matter distribution.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' cise constraints on the matter power suppression.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Specifi- cally to obtain the constraints, after training the RF regres- sor on the train simulations, we predict the ∆P/PDMO on test simulation boxes at four scales.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Thereafter, we create a histogram of the difference between truth and predicted ∆P/PDMO, normalized by the variance obtained from the CV set of simulations, for each respective suite of simula- tions (see Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 1).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 6, each errorbar corresponds to the 16th and 84th percentile from this histogram and the marker corresponds to its peak.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We show the results of training and testing on a single simulation suite, and also the results of training/testing across different simulation suites.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' It is clear that when training and testing on the same simulation suite, the RF learns a model that comes close to the best possi- ble uncertainty on ∆P/PDMO (i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' cosmic variance).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' When training on one or two simulation suites and testing another, however, the predictions show bias at low k.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This suggests that the model learned from one simulation does not gen- eralize very well to another in this regime.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This result is somewhat different from the findings of van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020), where it was found that the relationship between fb and ∆P/PDMO did generalize to different simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This difference may result from the fact that we are considering a wider range of feedback prescriptions than in van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020), as well as considering significant variations in cosmological parameters.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 6 also shows the results of testing and training on all three simulations (black points with errorbars).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Encour- agingly, we find that in this case, the predictions are of comparable accuracy to those obtained from training and predicting on the same simulation suite.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This suggests that there is a general relationship across all feedback models that can be learned to go from Ωm and fb to ∆P/PDMO.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Henceforth, we will show results trained on all simulation suites and tested on all simulations suites.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Of course, this result does not imply that our results will generalize to some completely different feedback prescription.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 7 we show the results of training the random forest on different combinations of fb, Y500c and Ωm.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Con- sistent with the findings of van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020), we find that fb/(Ωb/Ωm) results in robust constraints on the matter power suppression (blue points with errors).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' These constraints come close to the cosmic variance limit across a wide range of k.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We additionally find that providing fb and Ωm as sepa- rate inputs to the RF improves the precision of the predic- tions for ∆P/PDMO relative to using just the combination fb/(Ωb/Ωm), with the largest improvement coming at small scales.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This is not surprising given the predictions of our simple model, for which it is clear that ∆P/PDMO can be impacted by both Ωm and fb/(Ωb/Ωb) independently.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Sim- ilarly, it is clear from Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3 that changing Ωm changes the relationship between ∆P/PDMO and the halo gas-derived quantities (like Y and fb).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We next consider a model trained on Y500c/Y SS (orange points in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 7).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This model yields reasonable predictions for ∆P/PDMO, although not quite as good as the model trained on fb/(Ωb/Ωm).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The Y/Y SS model yields somewhat larger errorbars, and the distribution of ∆P/PDMO predic- tions is highly asymmetric.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' When we train the RF model jointly on Y500c/Y SS and Ωm (green points), we find that the predictions improve considerably, particularly at high k.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' MNRAS 000, 1–16 (0000) Probing feedback with the SZ 11 100 101 k (h/Mpc) −4 −3 −2 −1 0 1 2 3 4 Error ∆P/PDMO prediction relative to CV (σ) CV Train:TNG, Test:TNG Train:SIMBA, Test:SIMBA Train:Astrid, Test:Astrid Train: TNG, SIMBA Test: Astrid Train: TNG, Astrid Test: SIMBA Train: SIMBA, Astrid Test: TNG Train: TNG, SIMBA, Astrid Test: TNG, SIMBA, Astrid Figure 6.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We show the results of the random forest regressor predictions for the baryonic power suppression, represented by ∆P/PDMO, across the LH suite of simulations at four different scales k using the subgrid physics models for TNG, SIMBA, and Astrid.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The model was trained using the average fb of halos with masses between 5 × 1012 < M(M⊙/h) < 1014 and the cosmological parameter Ωm.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The errorbars indicate the uncertainty in the predictions normalized by the uncertainity in the CV suite at each scale, showing the 16-84 percentile error on the test set.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The gray band represents the expected 1σ error from the CV suite.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The model performs well when the training and test simulations are the same.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' When tested on an independent simulation, it remains robust at high k but becomes biased at low k.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The results presented in the remainder of the paper are based on training the model on all three simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The data points at each scale are staggered for clarity.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 100 101 k (h/Mpc) −4 −3 −2 −1 0 1 2 3 4 Error ∆P/PDMO prediction relative to CV (σ) CV fb/(Ωb/Ωm) fb, Ωm Y500c/YSS Y500c/YSS, Ωm fb, Y500c/YSS, Ωm Figure 7.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Similar to Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 6, but showing results when training the RF model on different observables from all three simulations (TNG, SIMBA and Astrid) to predict ∆P/PDMO of a random subset of the the three simulations not used in training.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We find that jointly training on the deviation of the integrated SZ profile from the self-similar expectation, Y500c/Y SS and Ωm results in inference of power suppression that is comparable to cosmic variance errors, with small improvements when additionally adding the baryon fraction (fb) of halos in the above mass range.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In this case, the predictions are typically symmetric around the true ∆P/PDMO, have smaller uncertainty compared to the model trained on fb/(Ωb/Ωm), and comparable uncer- tainty to the model trained on {fb/(Ωb/Ωm),Ωm}.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We thus conclude that when combined with matter density informa- tion, Y/Y SS provides a powerful probe of baryonic effects on the matter power spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Above we have considered the integrated tSZ signal from halos, Y500c.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Measurements in data, however, can po- tentially probe the tSZ profiles rather than only the inte- grated tSZ signal (although the instrumental resolution may limit the extent to which this is possible).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 8 we con- sider RF models trained on the stacking the full electron density and pressure profiles in the halo mass range instead of just the integrated quantities.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The electron pressure and number density profiles are measured in eight logarithmi- MNRAS 000, 1–16 (0000) 12 Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 100 101 k (h/Mpc) −4 −3 −2 −1 0 1 2 3 4 Error ∆P/PDMO prediction relative to CV (σ) CV Pe(r)/PSS e Pe(r)/PSS e , Ωm Pe(r)/PSS e , ne(r), Ωm Pe(r)/PSS e , Ωm Low+High mass bins Figure 8.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Same as Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 7 but showing results from using the full pressure profile, Pe(r), and electron number density profiles, ne(r), instead of the integrated quantities.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We again find that with pressure profile and Ωm information we can recover robust and precise constraints on the matter power suppression.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' cally spaced bins between 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 < r/r200c < 1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We find that while the ratio Pe(r)/P SS results in robust predictions for ∆P/PDMO, simultaneously providing Ωm makes the predic- tions more precise.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Similar to the integrated profile case, we find that additionally providing the electron density profile information only marginally improves the constraints.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We also show the results when jointly using the measured pres- sure profiles for both the low and high mass halos to infer the matter power suppression.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We find that this leads to only a marginal improvements in the constraints.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that we have input the 3D pressure and electron density profiles in this case.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Even though observed SZ maps are projected quantities, we can infer the 3D pressure profiles from the model used to analyze the projected correlations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 Predicting baryonic effects on the bispectrum with fb and the electron pressure In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 9, we repeat our analysis from above to make predictions for baryonic effects on the matter bispectrum, ∆B(k)/B(k).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Similar to the matter power spectrum, we train and test our model on a combination of the three simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We train and test on equilateral triangle bis- pectrum configurations with different scales k.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We again see that information about the electron pressure and Ωm results in precise and unbiased constraints on the impact of bary- onic physics on the bispectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The constraints improve as we go to the small scales.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In Appendix E we show similar methodology applied to squeezed bispectrum configurations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' However, there are several important caveats to these results.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The bispectrum is sensitive to high-mass (M > 5 × 1013M⊙/h) halos (Foreman et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2020) which are miss- ing from the CAMELS simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Consequently, our mea- surements of baryonic effects on the bispectrum can be bi- ased when using CAMELS.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The simulation resolution can also impact the bispectrum significantly.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' A future analysis with larger volume sims at high resolution could use the methodology introduced here to obtain more robust results.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Finally, there would is likely to be covariance between the power spectrum suppression and baryonic effects on the bis- pectrum, as they both stem from same underlying physics.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We defer a complete exploration of these effects to future work.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 4 RESULTS II: ACTXDES MEASUREMENTS AND FORECAST Our analysis above has resulted in a statistical model (i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' a random forest regressor) that predicts the matter power suppression ∆P/PDMO given values of Y500c for low-mass halos.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This model is robust to significant variations in the feedback prescription, at least across the SIMBA, TNG and Astrid models.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We now apply this model to constraints on Y500c coming from the cross-correlation of galaxy lensing shear with tSZ maps measured using Dark Energy Survey (DES) and Atacama Cosmology Telescope (ACT) data.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Gatti et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022a) and Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022) measured the cross-correlations of DES galaxy lensing with Compton y maps from a combination of Advanced ACT (Madhavacheril et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2020) and Planck data (Planck Collaboration et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2016) over an area of 400 sq.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' deg.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' They analyze these cross- correlations using a halo model framework, where the pres- sure profile in halos was parameterized using a generalized Navarro-Frenk-White profile (Navarro et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 1996;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Battaglia et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2012a).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This pressure profile is described using four free parameters, allowing for scaling with mass, redshift and distance from halo center.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The constraints on the parame- terized pressure profiles can be translated directly into con- straints on Y500c for halos in the mass range relevant to our random forest models.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We use the parameter constraints from Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022) to generate 400 samples of the inferred 3D profiles of halos at z = 0 (i.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' the redshift at which the RF models are trained) in ten logarithmically-spaced mass bins in range 12.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='7 < log10(M/h−1M⊙) < 14.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We then perform the volume MNRAS 000, 1–16 (0000) Probing feedback with the SZ 13 100 101 keq (h/Mpc) −4 −3 −2 −1 0 1 2 3 4 Error ∆Beq/Beq;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='DMO prediction relative to CV (σ) CV Y500c/YSS, Ωm Pe(r)/PSS e Pe(r)/PSS e , Ωm Pe(r)/PSS e , ne(r), Ωm Figure 9.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Same as Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 7, but for the impact of feedback on the bispectrum in equilateral triangle configurations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We find that the inclusion of pressure profile information results in unbiased constraints on feedback effects on the bispectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 100 k (h/Mpc) −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='40 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='35 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='30 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='25 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='20 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='15 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='10 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='05 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='00 ∆P/PDMO Chen et al 2022 w/ cosmology prior Schneider et al 2022 OWLS BAHAMAS BAHAMAS highAGN TNG-300 DESxACT;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Data DESIxS4;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Forecast Figure 10.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Constraints on the impact of feedback on the matter power spectrum obtained using our trained random forest model applied to measurements of Y500c/Y SS from the DESxACT analysis of Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022) (black points with errorbars).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We also show the expected improvements from future halo-y correlations from DESIxSO using the constraints in Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We compare these to the inferred constraints obtained using cosmic shear (Chen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2023) and additionally including X-ray and kSZ data (Schneider et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2022).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We also compare with the results from larger simulations: OWLS (Schaye et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2010), BAHAMAS (McCarthy et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2017) and TNG-300 (Springel et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2018).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' integral of these profiles to infer the Y500c(M, z) (see Eq.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 1).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Next, we generate a halo-averaged value of Y500c/Y SS for the jth sample by integrating over the halo mass distribution in CAMELS: �Y500c Y SS �j = 1 ¯nj � dM � dn dM �j CAMELS Y j 500c(M) Y SS (14) where ¯nj = � dM(dn/dM)j CAMELS and (dn/dM)j CAMELS are a randomly chosen halo mass function from the CV set of boxes of TNG, SIMBA or Astrid.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This procedure allows us to incorporate the impact and uncertainties of the CAMELS box size on the halo mass function.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that due to the small box size of CAMELS, there is a deficit of high mass halos and hence the functional form of the mass function MNRAS 000, 1–16 (0000) 14 Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' differs somewhat from other fitting functions in literature, e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Tinker et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2008).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 10 shows the results feeding the Y500c/Y SS values calculated above into our trained RF model to infer the im- pact of baryonic feedback on the matter power spectrum (black points with errorbars).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The RF model used is that trained on the TNG, SIMBA and Astrid simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The errorbars represent the 16th and 84th percentile of the recov- ered ∆P/PDMO distribution using the 400 samples described above.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that in this inference we fix the matter density parameter, Ωm = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3, same value as used by the CAMELS CV simulations as we use these to estimate the halo mass function.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In the same figure, we also show the constraints from Chen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2023) and Schneider et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022) obtained using the analysis of complementary datasets.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Chen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2023) analyze the small scale cosmic shear measurements from DES Year-3 data release using a baryon correction model.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that in this analysis, they only use a limited range of cosmologies, particularly restricting to high σ8 due to the requirements of emulator calibration.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Moreover they also impose cosmology constraints from the large scale analy- sis of the DES data.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that unlike the procedure pre- sented here, their modeling and constraints are sensitive to the priors on σ8.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Schneider et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022) analyze the X-ray data (as presented in Giri & Schneider 2021) and kSZ data from ACT and SDSS (Schaan et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2021) and the cosmic shear measurement from KiDS (Asgari et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2021), using another version of baryon correction model.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' A joint analysis from these complementary dataset leads to crucial degen- eracy breaking in the parameters.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' It would be interesting to include the tSZ observations presented here in the same framework as it can potentially make the constraints more precise.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Several caveats about our analysis with data are in or- der.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' First, the lensing-SZ correlation is most sensitive to halos in the mass range of Mhalo ≥ 1013M⊙/h.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' However, our RF model operates on halos with mass in the range of 5 × 1012 ≥ Mhalo ≤ 1014M⊙/h, with the limited vol- ume of the simulations restricting the number of halos above 1013M⊙/h.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We have attempted to account for this selection effect by using the halo mass function from the CV sims of the CAMELS simulations when calculating the stacked pro- file.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' However, using a larger volume simulation suite would be a better alternative (also see discussion in Appendix A).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Moreover, the CAMELS simulation suite also fix the value of Ωb.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' There may be a non-trivial impact on the inference of ∆P/PDMO when varying that parameter.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note, though, that Ωb is tightly constrained by other cosmological obser- vations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Lastly, the sensitivity of the lensing-SZ correlations using DES galaxies is between 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 < z < 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='6.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' However, in this study we extrapolate those constraints to z = 0 using the pressure profile model of Battaglia et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2012a).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We note that inference obtained at the peak sensitivity redshift would be a better alternative but we do not expect this to have a significant impact on the conclusions here.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In order to shift the sensitivity of the data correlations to lower halo masses, it would be preferable to analyze the galaxy-SZ and halo-SZ correlations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020) we forecast the constraints on the inferred 3D pressure pro- file from the future halo-SZ correlations using DESI and CMB-S4 SZ maps for a wide range of halo masses.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 10 we also show the expected constraints on the matter power suppression using the halo-SZ correlations from halos in the range M500c > 5 × 1012M⊙/h.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We again follow the same methodology as described above to create a stacked normal- ized integrated pressure (see Eq.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 14).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Moreover, we also fix Ω = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 to predict the matter power suppression.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that we shift the mean value of ∆P/PDMO to the recovered value from BAHAMAS high-AGN simulations (McCarthy et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2017).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' As we can see in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 10, we can expect to obtain significantly more precise constraints from these future ob- servations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 5 CONCLUSIONS We have shown that the tSZ signals from low-mass halos contain significant information about the impacts of bary- onic feedback on the small-scale matter distribution.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Using models trained on hydrodynamical simulations with a wide range of feedback implementations, we demonstrate that in- formation about baryonic effects on the power spectrum and bispectrum can be robustly extracted.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' By applying these same models to measurements with ACT and DES, we have shown that current tSZ measurements already constrain the impact of feedback on the matter distribution.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Our results suggest that using simulations to learn the relationship be- tween halo gas observables and baryonic effects on the mat- ter distribution is a promising way forward for constraining these effects with data.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Our main findings from our explorations with the CAMELS simulations are the following: In agreement with van Daalen et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2020), we find that baryon fraction in halos correlates with the power spectrum suppression.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We find that the correlation is especially robust at small scales.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We find (in agreement with Delgado et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2023) that there can be significant scatter in the relationship between baryon fraction and power spectrum suppression at low halo mass, and that the relationship varies to some degree with feed- back implementation.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' However, the bulk trends appear to be consistent regardless of feedback implementation.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We propose a simple model that qualitatively (and in some cases quantitatively) captures the broad features in the re- lationships between the impact of feedback on the power spectrum, ∆P/PDMO, at different values of k, and halo gas- related observables like fb and Y500c at different halo masses.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Despite significant scatter in the relations between Y500c and ∆P/PDMO at low halo mass, we find that simple ran- dom forest models yield tight and robust constraints on ∆P/PDMO given information about Y500c in low-mass ha- los and Ωm.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Using the pressure profile instead of just the inte- grated Y500c signal provides additional information about ∆P/PDMO, leading to 20-50% improvements when not us- ing any cosmological information.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' When additionally pro- viding the Ωm information, the improvements in constraints on baryonic changes to the power spectrum or bispectrum are modest when using the full pressure profile relative to integrated quantities like Y500c.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The pressure profiles and baryon fractions also carry infor- mation about baryonic effects on the bispectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' MNRAS 000, 1–16 (0000) Probing feedback with the SZ 15 Our main results from our analysis of constraints from the DESxACT shear-y correlation analysis are We have used the DES-ACT measurement of the shear- tSZ correlation from Gatti et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022a) and Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2022) to infer Y500c for halos in the mass range relevant to our random forest models.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Feeding the measured Y500c into these models, we have inferred the impact of baryonic effects on the power spectrum, as shown in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 10.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We show that constraints on baryonic effects on the power spectrum will improve significantly in the future, particu- larly using halo catalogs from DESI and tSZ maps from CMB-S4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' With data from future galaxy and CMB surveys, we expect constraints on the tSZ signal from halos across a wide mass and redshift range to improve significantly.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' These improvements will come from both the galaxy side (e.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='g.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' halos detected over larger areas of the sky, down to lower halo masses, and out to higher redshifts) and the CMB side (more sensitive tSZ maps over larger areas of the sky).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Our forecast for DESI and CMB Stage 4 in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 10 suggests that very tight constraints can be obtained on the impact of baryonic feedback on the matter power spectrum.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We expect that these constraints on the impact of baryonic feedback will enable the extraction of more cosmological information from the small-scale matter distribution.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 6 ACKNOWLEDGEMENTS DAA acknowledges support by NSF grants AST-2009687 and AST-2108944, CXO grant TM2-23006X, and Simons Foundation award CCA-1018464.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 7 DATA AVAILABILITY The TNG and SIMBA simulations used in this work are part of the CAMELS public data release (Villaescusa- Navarro et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2021) and are available at https://camels.' metadata={'source': 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'/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='02075 Weinberger R.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=', et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=', 2017, MNRAS, 465, 3291 van Daalen M.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' P.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=', McCarthy I.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' G.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=', Schaye J.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=', 2020, MNRAS, 491, 2424 APPENDIX A: IMPACT OF LIMITED VOLUME OF CAMELS SIMULATIONS In order to analyze the impact of varying box sizes and res- olution on the matter power suppression, we use the TNG simulations as presented in Springel et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' (2018).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Partic- ularly we use their boxes with side lengths of 210 Mpc/h, 75 Mpc/h and 35 Mpc/h (which they refer to as TNG-300, TNG-100 and TNG-50 as it corresponds to side length in the units of Mpc).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We then make the comparison to 25 Mpc/h TNG boxes run from CAMELS.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We use the CV set of simulations and use them to infer the expected variance due to stochasticity induced by changing initial conditions.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Note that the hydrodynamical model is identical between CAMELS CV runs and the bigger TNG boxes.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' A1, we show the power suppression for these boxes, including the runs at varying resolution.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We find that while changing box sizes gives relatively robust values of power suppression, changing resolution can have non-negligible impact.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' How- ever, all the TNG boxes are consistent at 2-3σ level relative to the CAMELS boxes.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' APPENDIX B: EXAMPLE OF EMULATION We present an example of the constructed emulator from §3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 for the AAGN1 parameter in Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' B1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This shows how we estimate the derivative of the observable (Y500c/M 5/3) in a way that is robust to stochasticity.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' APPENDIX C: ROBUSTNESS OF RESULTS TO DIFFERENT TRAIN SIMULATIONS In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' C1, we test the impact of changing the simulations used to train the random forest regressor.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We then use these different trained models to infer the constraints on the mat- ter power suppression from the same stacked ⟨Y500c/Y SS⟩ as described in § 4.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We see that our inferred constraints remain consistent when changing the simulations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' APPENDIX D: TEST WITH LOWER HALO MASSES In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' D1, we show the constraints on the power suppres- sion obtained by analyzing the observables obtained from halos with lower masses, 1 × 1012 < M(M⊙/h) < 5 × 1012.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We see that remarkably, even these lower halo masses pro- vide unbiased constraints on the matter power suppression with robust inference especially at smaller scales.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' However, when compared to the results descibed in § 3.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2, we obtain less precise constraints.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This is expected as lower halos with −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 ∆P/PDMO TNG-210 NDM = 25003 TNG-70 NDM = 9103 TNG-35 NDM = 5403 TNG-25 NDM = 2563 100 101 k (h/Mpc) −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 ∆P/PDMO TNG70 NDM = 18203 TNG 70 NDM = 4553 Figure A1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Comparison of the suppression of matter power in the CAMELS TNG simulation and simulations using the same sub-grid prescription but larger box sizes (Springel et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 2018).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We also show 1σ and 2σ uncertainty due to cosmic variance.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In the top panel we change the TNG box sizes, while preserving the resolution, where as in the bottom panel we preserve the TNG box size while changing the resolution.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' lower masses are more susceptible to environmental effects which induces a larger scatter in the relation between their observables (such as fb or Y500c) and their halo masses gov- erning feedback processes.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' APPENDIX E: TEST WITH OTHER BISPECTRUM CONFIGURATIONS In Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' E1, we show the constraints obtained on the sup- pression of the squeezed bispectrum configurations.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We fix the the angle between the long sides of the triangle to corre- spond to µ = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='9.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We again find robust inference of baryonic effects on the bispectrum when using either the integrated pressure profile or full radial pressure profile.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' This paper has been typeset from a TEX/LATEX file prepared by the author.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' MNRAS 000, 1–16 (0000) Probing feedback with the SZ 17 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='6 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='6 log(AAGN1) −5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='5 −5.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 log(Y500c/M 5/3) Resulting Emulator Resulting Derivative Figure B1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' The constructed emulator and resulting derivative for the AAGN1 parameter in the mass bin 1012 < M(M⊙/h) < 5 × 1012.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 100 101 k −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='4 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='3 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='2 −0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='1 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='0 ∆P/PDMO Train TNG+SIMBA+Astrid Train TNG+SIMBA Train SIMBA+Astrid Train TNG+Astrid Figure C1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' In this figure we change the simulations used to train the RF when inferring the power suppression from the data measurements.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' MNRAS 000, 1–16 (0000) 18 Pandey et al.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 100 101 k (h/Mpc) −4 −3 −2 −1 0 1 2 3 4 Error ∆P/PDMO prediction relative to CV (σ) CV Y500c/YSS, Ωm Pe(r)/PSS e Pe(r)/PSS e , Ωm Pe(r)/PSS e , ne(r), Ωm Figure D1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Same as Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 7 and Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 8, but obtained on lower halo masses, 1 × 1012 < M(M⊙/h) < 5 × 1012.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' We find that having pressure profile information results in unbiased constraints here as well, albeit with a larger errorbars 100 101 ksq (h/Mpc) −4 −3 −2 −1 0 1 2 3 4 Error ∆Bsq/Bsq;' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='DMO prediction relative to CV (σ) CV Y500c/YSS, Ωm Pe(r)/PSS e Pe(r)/PSS e , Ωm Pe(r)/PSS e , ne(r), Ωm Figure E1.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' Same as Fig.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' 9, but for squeezed triangle configurations (µ = 0.' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content='9).' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'} +page_content=' MNRAS 000, 1–16 (0000)' metadata={'source': '/home/zjlab/wf/langchain-ChatGLM/knowledge_base/B9E0T4oBgHgl3EQfQABU/content/2301.02186v1.pdf'}