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Forward and backward galaxy evolution in comoving cumulative number density space

Torrey, Paul and Wellons, Sarah and Ma, Chung-Pei and Hopkins, Philip F. and Vogelsberger, Mark (2017) Forward and backward galaxy evolution in comoving cumulative number density space. Monthly Notices of the Royal Astronomical Society, 467 (4). pp. 4872-4885. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20170428-153015888

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Abstract

Galaxy cumulative comoving number density is commonly used to forge progenitor/descendant links between observed galaxy populations at different epochs. However, this method breaks down in the presence of galaxy mergers, or when galaxies experience stochastic growth rates. We present a simple analytic framework to treat the physical processes that drive the evolution and diffusion of galaxies within comoving number density space. The evolution in mass rank order of a galaxy population with time is influenced by (1) the non-conservative nature of total galaxy number density driven by galaxies combining in mergers (which we tabulate as a galaxy ‘coagulation’ rate) and (2) galaxy ‘mass rank scatter’ driven by stochasticity in stellar-mass growth rates from in situ star formation and mergers. We quantify the relative contribution of these two effects to the total mass rank order evolution using the Illustris simulation. We show that galaxy coagulation is dominant at lower redshifts and stellar masses, while scattered growth rates dominate the mass rank evolution at higher redshifts and stellar masses. For a galaxy population at 10^(10) M⊙, coagulation has been the dominant effect since z = 2.2, but a galaxy population at 10^(11) M⊙ was dominated by mass rank scatter until z = 0.6. We show that although the forward and backward median cumulative number density evolution tracks are asymmetric, the backward median cumulative number density evolution can be obtained by convolving the descendant distribution function with progenitor relative abundances. We tabulate fits for the median cumulative number density evolution and scatter that can be applied to improve the way galaxy populations are linked in multi-epoch observational data sets.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1093/mnras/stx370DOIArticle
https://academic.oup.com/mnras/article-lookup/doi/10.1093/mnras/stx370PublisherArticle
https://arxiv.org/abs/1606.07271arXivDiscussion Paper
ORCID:
AuthorORCID
Torrey, Paul0000-0002-5653-0786
Hopkins, Philip F.0000-0003-3729-1684
Additional Information:© 2017 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2017 February 9. Received 2017 February 8; in original form 2016 June 23. Published: 16 February 2017. We thank the referee, Bart Clauwens, for the many thoughtful comments that have strengthened this work. PT is supported through Hubble Fellowship grant #HST-HF2-51384.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. Support for PFH was provided by an Alfred P. Sloan Research Fellowship, NASA ATP Grant NNX14AH35G, NSF Collaborative Research Grant #1411920 and CAREER Grant #1455342. MV acknowledges support through an MIT RSC award. The Illustris simulation was run on the CURIE supercomputer at CEA/France as part of PRACE project RA0844, and the SuperMUC computer at the Leibniz Computing Centre, Germany, as part of project pr85je. Further simulations were run on the Harvard Odyssey and CfA/ITC clusters, the Ranger and Stampede supercomputers at the Texas Advanced Computing Center through XSEDE and the Kraken supercomputer at Oak Ridge National Laboratory through XSEDE. The analysis reported in this paper was performed on the Caltech compute cluster ‘Zwicky’ (NSF MRI award #PHY-0960291), the joint partition of the MIT-Harvard computing cluster ‘Odyssey’ supported by MKI and FAS, and allocation TG-AST150059 granted by the Extreme Science and Engineering Discovery Environment (XSEDE) supported by the NSF.
Group:TAPIR
Funders:
Funding AgencyGrant Number
NASA Hubble FellowshipHST-HF2-51384.001-A
NASANAS5-26555
Alfred P. Sloan FoundationUNSPECIFIED
NASANNX14AH35G
NSFAST-1411920
NSFAST-1455342
Massachusetts Institute of Technology (MIT)UNSPECIFIED
NSFPHY-0960291
Harvard UniversityUNSPECIFIED
NSFTG-AST150059
Subject Keywords:galaxies: abundances, galaxies: evolution, galaxies: formation, galaxies: statistics
Record Number:CaltechAUTHORS:20170428-153015888
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20170428-153015888
Official Citation:Paul Torrey, Sarah Wellons, Chung-Pei Ma, Philip F. Hopkins, Mark Vogelsberger; Forward and backward galaxy evolution in comoving cumulative number density space. Mon Not R Astron Soc 2017; 467 (4): 4872-4885. doi: 10.1093/mnras/stx370
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:77069
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:28 Apr 2017 23:39
Last Modified:17 Aug 2017 19:05

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