CaltechAUTHORS
  A Caltech Library Service

The suppression of star formation on the smallest scales: what role does environment play?

Rodriguez Wimberly, M. K. and Cooper, M. C. and Fillingham, S. P. and Boylan-Kolchin, M. and Bullock, J. S. and Garrison-Kimmel, S. (2019) The suppression of star formation on the smallest scales: what role does environment play? Monthly Notices of the Royal Astronomical Society, 483 (3). pp. 4031-4039. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20190417-112256207

[img] PDF - Published Version
See Usage Policy.

821Kb

Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20190417-112256207

Abstract

The predominantly ancient stellar populations observed in the lowest mass galaxies (i.e. ultra-faint dwarfs) suggest that their star formation was suppressed by reionization. Most of the well-studied ultra-faint dwarfs, however, are within the central half of the Milky Way dark matter halo, such that they are consistent with a population that was accreted at early times and thus potentially quenched via environmental processes. To study the potential role of environment in suppressing star formation on the smallest scales, we utilize the Exploring the Local Volume in Simulations suite of N-body simulations to constrain the distribution of infall times for low-mass subhaloes likely to host the ultra-faint population. For the ultra-faint satellites of the Milky Way with star formation histories inferred from Hubble Space Telescopeimaging, we find that environment is highly unlikely to play a dominant role in quenching their star formation. Even when including the potential effects of pre-processing, there is a ≲0.1 per cent probability that environmental processes quenched all of the known ultra-faint dwarfs early enough to explain their observed star formation histories. Instead, we argue for a mass floor in the effectiveness of satellite quenching at roughly M⋆∼10^5M⊙, below which star formation in surviving galaxies is globally suppressed by reionization. We predict a large population of quenched ultra-faint dwarfs in the Local Field (1 < R/R_(vir) < 2), with as many as ∼250 to be discovered by future wide-field imaging surveys.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/sty3357DOIArticle
ORCID:
AuthorORCID
Rodriguez Wimberly, M. K.0000-0003-1848-5571
Cooper, M. C.0000-0003-1371-6019
Fillingham, S. P.0000-0002-8425-0351
Boylan-Kolchin, M.0000-0002-9604-343X
Garrison-Kimmel, S.0000-0002-4655-8128
Additional Information:© 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2018 December 5. Received 2018 December 4; in original form 2018 June 19. Published: 11 December 2018. We thank Tyler Kelley, Dan Weisz, Josh Simon, Alex Riley, and Mary Jenkins for helpful discussions regarding this project. This work was supported in part by NSF grants AST-1518257, AST-1518291, AST-1517226, and AST-1815475. MBK also acknowledges support from NSF CAREER grant AST-1752913 and NASA grant NNX17AG29G. Additional support for this work was provided by NASA through grants GO-12914, AR-13888, AR-13896, GO-14191, AR-14282, AR-14289, AR-14554, and AR-15006 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. MKRW acknowledges support from the National Science Foundation Graduate Research Fellowship. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship Program under Grant No. DGE-1321846. This research made use of ASTROPY, a community-developed core PYTHON package for Astronomy (Astropy Collaboration et al. 2013). Additionally, the PYTHON packages NUMPY (Walt, Colbert & Varoquaux 2011), IPYTHON (Pérez & Granger 2007), SCIPY (Jones et al. 2001), and MATPLOTLIB (Hunter 2007) were utilized for the majority of our data analysis and presentation.
Group:TAPIR
Funders:
Funding AgencyGrant Number
NSFAST-1518257
NSFAST-1518291
NSFAST-1517226
NSFAST-1815475
NSFAST-1752913
NASANNX17AG29G
NASA Hubble FellowshipGO-12914
NASA Hubble FellowshipAR-13888
NASA Hubble FellowshipAR-13896
NASA Hubble FellowshipGO-14191
NASA Hubble FellowshipAR-14282
NASA Hubble FellowshipAR-14289
NASA Hubble FellowshipAR-14554
NASA Hubble FellowshipAR-15006
NASANAS 5-26555
NSF Graduate Research FellowshipDGE-1321846
Subject Keywords:galaxies: dwarf – galaxies: evolution – galaxies: formation – galaxies: general – Local Group – galaxies: star formation
Record Number:CaltechAUTHORS:20190417-112256207
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20190417-112256207
Official Citation:M K Rodriguez Wimberly, M C Cooper, S P Fillingham, M Boylan-Kolchin, J S Bullock, S Garrison-Kimmel, The suppression of star formation on the smallest scales: what role does environment play?, Monthly Notices of the Royal Astronomical Society, Volume 483, Issue 3, March 2019, Pages 4031–4039, https://doi.org/10.1093/mnras/sty3357
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:94747
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:17 Apr 2019 21:41
Last Modified:17 Apr 2019 21:41

Repository Staff Only: item control page