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Not so lumpy after all: modelling the depletion of dark matter subhaloes by Milky Way-like galaxies

Garrison-Kimmel, Shea and Wetzel, Andrew and Bullock, James S. and Hopkins, Philip F. and Boylan-Kolchin, Michael and Faucher-Giguère, Claude-André and Kereš, Dušan and Quataert, Eliot and Sanderson, Robyn E. and Graus, Andrew S. and Kelley, Tyler (2017) Not so lumpy after all: modelling the depletion of dark matter subhaloes by Milky Way-like galaxies. Monthly Notices of the Royal Astronomical Society, 471 (2). pp. 1709-1727. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20170921-133516143

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Abstract

Among the most important goals in cosmology is detecting and quantifying small (M_(halo)≃10^(6−9) M⊙) dark matter (DM) subhaloes. Current probes around the Milky Way (MW) are most sensitive to such substructure within ∼20 kpc of the halo centre, where the galaxy contributes significantly to the potential. We explore the effects of baryons on subhalo populations in ΛCDM using cosmological zoom-in baryonic simulations of MW-mass haloes from the Latte simulation suite, part of the Feedback In Realistic Environments (FIRE) project. Specifically, we compare simulations of the same two haloes run using (1) DM-only (DMO), (2) full baryonic physics and (3) DM with an embedded disc potential grown to match the FIRE simulation. Relative to baryonic simulations, DMO simulations contain ∼2 × as many subhaloes within 100 kpc of the halo centre; this excess is ≳5 × within 25 kpc. At z = 0, the baryonic simulations are completely devoid of subhaloes down to 3×10^6M⊙ within 15 kpc of the MW-mass galaxy, and fewer than 20 surviving subhaloes have orbital pericentres <20 kpc. Despite the complexities of baryonic physics, the simple addition of an embedded central disc potential to DMO simulations reproduces this subhalo depletion, including trends with radius, remarkably well. Thus, the additional tidal field from the central galaxy is the primary cause of subhalo depletion. Subhaloes on radial orbits that pass close to the central galaxy are preferentially destroyed, causing the surviving population to have tangentially biased orbits compared to DMO predictions. Our method of embedding a potential in DMO simulations provides a fast and accurate alternative to full baryonic simulations, thus enabling suites of cosmological simulations that can provide accurate and statistical predictions of substructure populations.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stx1710DOIArticle
https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stx1710PublisherArticle
ORCID:
AuthorORCID
Wetzel, Andrew0000-0003-0603-8942
Hopkins, Philip F.0000-0003-3729-1684
Boylan-Kolchin, Michael0000-0002-9604-343X
Kereš, Dušan0000-0002-1666-7067
Quataert, Eliot0000-0001-9185-5044
Additional Information:© 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2017 July 5. Received 2017 July 5; in original form 2017 January 17. Published: 08 July 2017. Support for SGK was provided by NASA through Einstein Postdoctoral Fellowship grant number PF5-160136 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under contract NAS8-03060. AW was supported by a Caltech-Carnegie Fellowship, in part through the Moore Center for Theoretical Cosmology and Physics at Caltech, and by NASA through grant HST-GO-14734 from STScI. JSB and TK were supported by NSF grant AST-1518291 and by NASA through HST theory grants (programs AR-13921, AR-13888, and AR-14282.001) awarded by the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy (AURA), Inc., under NASA contract NAS5-26555. 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. MBK acknowledges support from the National Science Foundation (grant AST-1517226) and from NASA through HST theory grants (programs AR-12836, AR-13888, AR-13896 and AR-14282) awarded by STScI. CAFG was supported by NSF through grants AST-1412836 and AST-1517491, and by NASA through grant NNX15AB22G. DK acknowledges support from NSF grant AST-1412153 and the Cottrell Scholar Award from the Research Corporation for Science Advancement. 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 ASG was provided by NSF grant AST-1009973. Numerical calculations were run on the Caltech compute cluster ‘Zwicky’ (NSF MRI award #PHY-0960291) and allocation TG-AST130039 granted by the Extreme Science and Engineering Discovery Environment (XSEDE) supported by the NSF. Resources supporting this work were also provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center. This work also made use of ASTROPY, a community-developed core Python package for Astronomy (Astropy Collaboration et al. 2013), MATPLOTLIB (Hunter 2007), NUMPY (van der Walt, Colbert & Varoquaux 2011), SCIPY (Jones et al. 2001), IPYTHON (Perez & Granger 2007), MAYAVI (Ramachandran & Varoquaux 2011), and NASA’s Astrophysics Data System.
Group:TAPIR, Moore Center for Theoretical Cosmology and Physics
Funders:
Funding AgencyGrant Number
NASA Einstein FellowshipPF5-160136
NASANAS8-03060
Caltech Moore Center for Theoretical Cosmology and PhysicsUNSPECIFIED
NASAHST-GO-14734
NSFAST-1518291
NASA Hubble FellowshipAR-13921
NASA Hubble FellowshipAR-13888
NASA Hubble FellowshipAR-14282.001
NASANAS5-26555
Alfred P. Sloan FoundationUNSPECIFIED
NASANNX14AH35G
NSFAST-1411920
NSFAST-1455342
NSFAST-1517226
NASA Hubble FellowshipAR-12836
NASA Hubble FellowshipAR-13896
NASA Hubble FellowshipAR-14282
NSFAST-1412836
NSFAST-1517491
NASANNX15AB22G
NSFAST-1412153
Research CorporationUNSPECIFIED
NASA12-APT12-0183
Simons FoundationUNSPECIFIED
David and Lucile Packard FoundationUNSPECIFIED
NSFAST-1009973
NSFPHY-0960291
NSFTG-AST130039
Subject Keywords:galaxies: haloes – Local Group – dark matter – cosmology: theory
Record Number:CaltechAUTHORS:20170921-133516143
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20170921-133516143
Official Citation:Shea Garrison-Kimmel, Andrew Wetzel, James S. Bullock, Philip F. Hopkins, Michael Boylan-Kolchin, Claude-André Faucher-Giguère, Dušan Kereš, Eliot Quataert, Robyn E. Sanderson, Andrew S. Graus, Tyler Kelley; Not so lumpy after all: modelling the depletion of dark matter subhaloes by Milky Way-like galaxies , Monthly Notices of the Royal Astronomical Society, Volume 471, Issue 2, 21 October 2017, Pages 1709–1727, https://doi.org/10.1093/mnras/stx1710
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:81691
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:21 Sep 2017 21:11
Last Modified:21 Sep 2017 21:11

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