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The impact of stellar feedback on hot gas in galaxy haloes: the Sunyaev–Zel'dovich effect and soft X-ray emission

van de Voort, Freeke and Quataert, Eliot and Hopkins, Philip F. and Faucher-Giguère, Claude-André and Feldmann, Robert and Kereš, Dušan and Chan, T. K. and Hafen, Zachary (2016) The impact of stellar feedback on hot gas in galaxy haloes: the Sunyaev–Zel'dovich effect and soft X-ray emission. Monthly Notices of the Royal Astronomical Society, 463 (4). pp. 4533-4544. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20170310-124122492

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Abstract

The thermal Sunyaev–Zel'dovich (SZ) effect and soft X-ray emission are routinely observed around massive galaxies and in galaxy groups and clusters. We study these observational diagnostics of galaxy haloes for a suite of cosmological ‘zoom-in’ simulations from the ‘Feedback In Realistic Environments’ project, which spans a large range in halo mass (10^(10–13) M_⊙). We explore the effect of stellar feedback on the hot gas observables. The properties of our simulated groups, such as baryon fractions, SZ flux, and X-ray luminosities (LX), are broadly consistent with existing observations, even though feedback from active galactic nuclei is not included. We make predictions for future observations of lower mass objects for both SZ and diffuse X-ray measurements, finding that they are not just scaled-down versions of massive galaxies, but more strongly affected by galactic winds driven by star formation. Low-mass haloes (≲ 10^(11) M_⊙) retain a low fraction of their baryons, which results in a strong suppression of the SZ signal. Our simulations therefore predict a scaling with halo mass that is steeper than self-similar for haloes less massive than 10^(13) M_⊙. For halo masses ≲ 10^(12) M_⊙, LX is time variable and correlated primarily with the star formation rate (SFR). For these objects, the diffuse X-ray emission is powered mostly by galactic winds and the gas dominating the X-ray emission is flowing out with radial velocities close to the halo's circular velocity. For halo masses ≳ 10^(13) M_⊙, on the other hand, LX is much less variable and not correlated with the SFR, because the emission originates from the quasi-hydrostatic, virialized halo gas.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stw2322DOIArticle
https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stw2322PublisherArticle
ORCID:
AuthorORCID
van de Voort, Freeke0000-0002-6301-638X
Quataert, Eliot0000-0001-9185-5044
Hopkins, Philip F.0000-0003-3729-1684
Feldmann, Robert0000-0002-1109-1919
Kereš, Dušan0000-0002-1666-7067
Additional Information:© 2016 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2016 September 13. Received 2016 August 16; in original form 2016 April 5. Published: 14 September 2016. We would like to thank the referee for constructive comments, the Simons Foundation and participants of the Simons Symposium ‘Galactic Superwinds: Beyond Phenomenology’ for inspiration for this work, and Tim Davis for helpful comments on an earlier version of the manuscript. FvdV also thanks Rob Crain and Ian McCarthy for useful discussions. EQ was supported by NASA ATP grant 12-APT12-0183, a Simons Investigator award from the Simons Foundation, and the David and Lucile Packard Foundation. Support for PFH was provided by an Alfred P. Sloan Research Fellowship, NASA ATP Grant NNX14AH35G, and NSF Collaborative Research Grant #1411920 and CAREER grant #1455342. CAFG and ZHH were supported by NSF through grants AST-1412836 and AST-1517491, by NASA through grant NNX15AB22G, and by STScI through grants HST-AR-14293.001-A and HST-GO-14268.022-A. DK was supported by NSF grant AST-1412153. The simulations presented here used computational resources granted by the Extreme Science and Engineering Discovery Environment (XSEDE), which is supported by NSF grant number OCI-1053575, specifically allocations TG-AST120025 (PI: Kereš), TG-AST130039 (PI: Hopkins), TG-AST1140023 (PI: Faucher-Giguère) as well as the Caltech computer cluster ‘Zwicky’ (NSF MRI award #PHY-0960291) and the Northwestern computer cluster Quest. Some simulations were run with resources provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center, proposal SMD-14-5492.
Group:TAPIR
Funders:
Funding AgencyGrant Number
NASA12-APT12-0183
Simons FoundationUNSPECIFIED
David and Lucile Packard FoundationUNSPECIFIED
Alfred P. Sloan FoundationUNSPECIFIED
NASANNX14AH35G
NSFAST-1411920
NSFAST-1455342
NSFAST-1412836
NSFAST-1517491
NASANNX15AB22G
NASAHST-AR-14293.001-A
NASAHST-GO-14268.022-A
NSFAST-1412153
NSFOCI-1053575
NSFTG-AST120025
NSFTG-AST130039
NSFTG-AST1140023
NSFPHY-0960291
NASASMD-14-5492
Subject Keywords:methods: numerical, galaxies: evolution, galaxies: formation, galaxies: haloes, intergalactic medium, X-rays: galaxies
Record Number:CaltechAUTHORS:20170310-124122492
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20170310-124122492
Official Citation:Freeke van de Voort, Eliot Quataert, Philip F. Hopkins, Claude-André Faucher-Giguère, Robert Feldmann, Dušan Kereš, T. K. Chan, Zachary Hafen; The impact of stellar feedback on hot gas in galaxy haloes: the Sunyaev–Zel'dovich effect and soft X-ray emission. Mon Not R Astron Soc 2016; 463 (4): 4533-4544. doi: 10.1093/mnras/stw2322
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:75030
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:10 Mar 2017 20:59
Last Modified:01 Nov 2017 16:52

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