Diverse structural evolution at z > 1 in cosmologically simulated galaxies
Entity
UAM. Departamento de Física TeóricaPublisher
Oxford University Press on behalf of the Royal Astronomical SocietyDate
2015-06-30Citation
10.1093/mnras/stv1231
Monthly Notices of Royal Astronomical Society 451.4 (2015): 4290-4310
ISSN
0035-8711 (print); 1365-2966 (online)DOI
10.1093/mnras/stv1231Funded by
This work was partially supported by MINECO-AYA2012-31101. DC is a Juan de la Cierva fellow. This research has been partly supported by ISF grant 24/12, by NSF grant AST-1010033, and by the I-CORE Program of the PBC and the ISF grant 1829/12. GS and JL appreciate support from the HST grants program, number HST-AR-12856:01-A. Support for program #12856 (PI J. Lotz) was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555Project
Gobierno de España. AYA2012- 31101Editor's Version
http://dx.doi.org/10.1093/mnras/stv1231Subjects
Galaxies formation; Galaxies structure; Methods numerical; FísicaNote
This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2015 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reservedRights
© 2015 The Authors: Published by Oxford University Press on behalf of the Royal Astronomical SocietyAbstract
From mock Hubble Space Telescope images, we quantify non-parametric statistics of galaxy morphology, thereby predicting the emergence of relationships among stellar mass, star formation, and observed rest-frame optical structure at 1 < z < 3. We measure automated diagnostics of galaxy morphology in cosmological simulations of the formation of 22 central galaxies with 9.3 < log10 M_*/M_sun < 10.7. These high-spatial-resolution zoom-in calculations enable accurate modeling of the rest-frame UV and optical morphology. Even with small numbers of galaxies, we find that structural evolution is neither universal nor monotonic: galaxy interactions can trigger either bulge or disc formation, and optically bulge-dominated galaxies at this mass may not remain so forever. Simulated galaxies with M_* > 10^10 M_sun contain relatively more disc-dominated light profiles than those with lower mass, reflecting significant disc brightening in some haloes at 1 < z < 2. By this epoch, simulated galaxies with specific star formation rates below 10^-9.7 yr^-1 are more likely than normal star-formers to have a broader mix of structural types, especially at M_* > 10^10 M_sun. We analyze a cosmological major merger at z ~ 1.5 and find that the newly proposed MID morphology diagnostics trace later merger stages while G-M20 trace earlier ones. MID is sensitive also to clumpy star-forming discs. The observability time of typical MID-enhanced events in our simulation sample is less than 100 Myr. A larger sample of cosmological assembly histories may be required to calibrate such diagnostics in the face of their sensitivity to viewing angle, segmentation algorithm, and various phenomena such as clumpy star formation and minor mergers
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Google Scholar:Snyder, Gregory F.
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Lotz, Jennifer
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Moody, Christopher
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Peth, Michael
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Freeman, Peter
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Ceverino Rodríguez, Daniel
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Primack, Joel
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Dekel, Avishai
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