The Atacama Cosmology Telescope: Modelling the Gas Thermodynamics in BOSS CMASS galaxies from Kinematic and Thermal Sunyaev-Zel’dovich Measurements. (arXiv:2009.05558v1 [astro-ph.CO])

The Atacama Cosmology Telescope: Modelling the Gas Thermodynamics in BOSS CMASS galaxies from Kinematic and Thermal Sunyaev-Zel’dovich Measurements. (arXiv:2009.05558v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Amodeo_S/0/1/0/all/0/1">Stefania Amodeo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Battaglia_N/0/1/0/all/0/1">Nicholas Battaglia</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schaan_E/0/1/0/all/0/1">Emmanuel Schaan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ferraro_S/0/1/0/all/0/1">Simone Ferraro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moser_E/0/1/0/all/0/1">Emily Moser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Aiola_S/0/1/0/all/0/1">Simone Aiola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Austermann_J/0/1/0/all/0/1">Jason E. Austermann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beall_J/0/1/0/all/0/1">James A. Beall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bean_R/0/1/0/all/0/1">Rachel Bean</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Becker_D/0/1/0/all/0/1">Daniel T. Becker</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bond_R/0/1/0/all/0/1">Richard J. Bond</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calabrese_E/0/1/0/all/0/1">Erminia Calabrese</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calafut_V/0/1/0/all/0/1">Victoria Calafut</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_S/0/1/0/all/0/1">Steve K. Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Denison_E/0/1/0/all/0/1">Edward V. Denison</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Devlin_M/0/1/0/all/0/1">Mark Devlin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duff_S/0/1/0/all/0/1">Shannon M. Duff</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Duivenvoorden_A/0/1/0/all/0/1">Adriaan J. Duivenvoorden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunkley_J/0/1/0/all/0/1">Jo Dunkley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dunner_R/0/1/0/all/0/1">Rolando Dünner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gallardo_P/0/1/0/all/0/1">Patricio A. Gallardo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hall_K/0/1/0/all/0/1">Kirsten R. Hall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Han_D/0/1/0/all/0/1">Dongwon Han</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hill_J/0/1/0/all/0/1">J. Colin Hill</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hilton_G/0/1/0/all/0/1">Gene C. Hilton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hilton_M/0/1/0/all/0/1">Matt Hilton</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hlozek_R/0/1/0/all/0/1">Renée Hložek</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hubmayr_J/0/1/0/all/0/1">Johannes Hubmayr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huffenberger_K/0/1/0/all/0/1">Kevin M. Huffenberger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hughes_J/0/1/0/all/0/1">John P. Hughes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koopman_B/0/1/0/all/0/1">Brian J. Koopman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+MacInnis_A/0/1/0/all/0/1">Amanda MacInnis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McMahon_J/0/1/0/all/0/1">Jeff McMahon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Madhavacheril_M/0/1/0/all/0/1">Mathew S. Madhavacheril</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moodley_K/0/1/0/all/0/1">Kavilan Moodley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mroczkowski_T/0/1/0/all/0/1">Tony Mroczkowski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Naess_S/0/1/0/all/0/1">Sigurd Naess</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nati_F/0/1/0/all/0/1">Federico Nati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Newburgh_L/0/1/0/all/0/1">Laura B. Newburgh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Niemack_M/0/1/0/all/0/1">Michael D. Niemack</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Page_L/0/1/0/all/0/1">Lyman A. Page</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Partridge_B/0/1/0/all/0/1">Bruce Partridge</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schillaci_A/0/1/0/all/0/1">Alessandro Schillaci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sehgal_N/0/1/0/all/0/1">Neelima Sehgal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sifon_C/0/1/0/all/0/1">Cristóbal Sifón</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spergel_D/0/1/0/all/0/1">David N. Spergel</a>, et al. (9 additional authors not shown)

The thermal and kinematic Sunyaev-Zel’dovich effects (tSZ, kSZ) probe the
thermodynamic properties of the circumgalactic and intracluster medium (CGM and
ICM) of galaxies, groups, and clusters, since they are proportional,
respectively, to the integrated electron pressure and momentum along the
line-of-sight. We present constraints on the gas thermodynamics of CMASS
galaxies in the Baryon Oscillation Spectroscopic Survey (BOSS) using new
measurements of the kSZ and tSZ signals obtained in a companion paper.
Combining kSZ and tSZ measurements, we measure within our model the amplitude
of energy injection $epsilon M_star c^2$, where $M_star$ is the stellar
mass, to be $epsilon=(33^{+2}_{-5})times10^{-6}$, and the amplitude of the
non-thermal pressure profile to be $alpha_{rm Nth}=0.30^{+0.06}_{-0.07}$,
indicating that 30% of the total pressure within the virial radius is due to a
non-thermal component. We estimate the effects of including baryons in the
modeling of weak-lensing galaxy cross-correlation measurements using the best
fit density profile from the kSZ measurement. Our estimate reduces the
difference between the original theoretical model and the weak-lensing galaxy
cross-correlation measurements in arXiv:1611.08606 by half (50% at most), but
does not fully reconcile it. Comparing the kSZ and tSZ measurements to
cosmological simulations, we find that they under predict the CGM pressure and
to a lesser extent the CGM density at larger radii. This suggests that the
energy injected via feedback models in the simulations that we compared against
does not sufficiently heat the gas at these radii. We do not find significant
disagreement at smaller radii. These measurements provide novel tests of
current and future simulations. This work demonstrates the power of joint, high
signal-to-noise kSZ and tSZ observations, upon which future cross-correlation
studies will improve.

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