Simulation Data Model Version 1.0

Lemson, Gerard; Wozniak, H.; Bourgès, Laurent; Cervino, Miguel; Gheller, C.; Gray, Norman; LePetit, Franck; Louys, Mireille; Ooghe, Benjamin; Wagner, Rick

doi:10.5479/ads/bib/2012ivoa.spec.0503l

Cited by 11 publications

(11 citation statements)

References 8 publications

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“…Analyzing synthetic data from simulations alongside galaxy surveys promises to be a valuable approach to constrain the physics of galaxy evolution. Powerful pipelines have been developed to convert theoretical models of galaxy formation into useful mock surveys, such as the Millennium Run Database and Observatory (Lemson 2006;Overzier et al 2013), the Theoretical Astrophysical Observatory (Bernyk et al 2014), and the simple semi-empirical approach by Taghizadeh-Popp et al (2015). Moreover, such models now include treatments motivated by high-resolution simulations for the morphological transformations that may be a key aspect of galaxy evolution (e.g., Porter et al 2014;Brennan et al 2015).…”

Section: Discussionmentioning

confidence: 99%

Galaxy morphology and star formation in the Illustris Simulation atz = 0

Snyder

Torrey

Lotz

et al. 2015

Mon. Not. R. Astron. Soc.

203

195

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We study how optical galaxy morphology depends on mass and star formation rate (SFR) in the Illustris Simulation. To do so, we measure automated galaxy structures in 10808 simulated galaxies at z = 0 with stellar masses 10 9.7 < M * /M < 10 12.3 . We add observational realism to idealized synthetic images and measure non-parametric statistics in rest-frame optical and near-IR images from four directions. We find that Illustris creates a morphologically diverse galaxy population, occupying the observed bulge strength locus and reproducing median morphology trends versus stellar mass, SFR, and compactness. Morphology correlates realistically with rotation, following classification schemes put forth by kinematic surveys. Type fractions as a function of environment agree roughly with data. These results imply that connections among mass, star formation, and galaxy structure arise naturally from models matching global star formation and halo occupation functions when simulated with accurate methods. This raises a question of how to construct experiments on galaxy surveys to better distinguish between models. We predict that at fixed halo mass near 10 12 M , discdominated galaxies have higher stellar mass than bulge-dominated ones, a possible consequence of the Illustris feedback model. While Illustris galaxies at M * ∼ 10 11 M have a reasonable size distribution, those at M * ∼ 10 10 M have half-light radii larger than observed by a factor of two. Furthermore, at M * ∼ 10 10.5 -10 11 M , a relevant fraction of Illustris galaxies have distinct "ring-like" features, such that the bright pixels have an unusually wide spatial extent.

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Section: Discussionmentioning

confidence: 99%

Galaxy morphology and star formation in the Illustris Simulation atz = 0

Snyder

Torrey

Lotz

et al. 2015

Mon. Not. R. Astron. Soc.

203

195

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“…In Fig. 8 we overlay the predictions of the Millennium Simulation (Lemson et al 2006), the largest numerical simulation to date based on CDM theory, with the semianalytic galaxy formation model of De Lucia & Blaizot (2007), scaled to fit to the local observations (by a factor of ∼0.4). The stellar mass of the Millennium model has been shifted by +0.25 dex in order to correct for the different IMFs adopted (the model adopts the Chabrier (2003) IMF).…”

Section: Discussionmentioning

confidence: 99%

Witnessing the active assembly phase of massive galaxies sincez= 1

Matsuoka

Kawara

2010

Monthly Notices of the Royal Astronomical Society

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We present an analysis of ∼60 000 massive (stellar mass M > 10 11 M ) galaxies out to z = 1 drawn from 55.2 deg 2 of the United Kingdom Infrared Telescope (UKIRT) Infrared Deep Sky Survey (UKIDSS) and the Sloan Digital Sky Survey (SDSS) II Supernova Survey. This is by far the largest survey of massive galaxies with robust mass estimates, based on infrared (K-band) photometry, reaching to the Universe at about half its present age. We find that the most massive (M > 10 11.5 M ) galaxies have experienced rapid growth in number since z = 1, while the number densities of the less massive systems show rather mild evolution. Such a hierarchical trend of evolution is consistent with the predictions of the current semi-analytic galaxy formation model based on CDM theory. While the majority of massive galaxies are red-sequence populations, we find that a considerable fraction of galaxies are blue star-forming galaxies. The blue fraction is smaller in more massive systems and decreases toward the local Universe, leaving the red, most massive galaxies at low redshifts, which would support the idea of active 'bottom-up' formation of these populations during 0 < z < 1.

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“…Detailed descriptions of the simulations and the semianalytic modelling have been covered extensively elsewhere, and we kindly refer the reader to those works for more information (e.g. Kauffmann et al 1999;De Lucia, Kauffmann & White 2004;Croton et al 2006;Lemson & Springel 2006;De Lucia & Blaizot 2007, and references therein).…”

Section: Simulation Descriptionmentioning

confidence: 99%

ΛCDM predictions for galaxy protoclusters - I. The relation between galaxies, protoclusters and quasars at

Overzier

Guo

Kauffmann

et al. 2009

Monthly Notices of the Royal Astronomical Society

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103

131

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Motivated by recent observational studies of the environment of z∼ 6 QSOs, we have used the Millennium Run (MR) simulations to construct a very large (∼4°× 4°) mock redshift survey of star‐forming galaxies at z∼ 6. We use this simulated survey to study the relation between density enhancements in the distribution of i775‐dropouts and Lyα emitters, and their relation to the most massive haloes and protocluster regions at z∼ 6. Our simulation predicts significant variations in surface density across the sky with some voids and filaments extending over scales of 1°, much larger than probed by current surveys. Approximately one‐third of all z∼ 6 haloes hosting i‐dropouts brighter than z= 26.5 mag (≈M*UV,z=6) become part of z= 0 galaxy clusters. i‐dropouts associated with protocluster regions are found in regions where the surface density is enhanced on scales ranging from a few to several tens of arcminutes on the sky. We analyse two structures of i‐dropouts and Lyα emitters observed with the Subaru Telescope and show that these structures must be the seeds of massive clusters in formation. In striking contrast, six z∼ 6 QSO fields observed with Hubble Space Telescope show no significant enhancements in their i775‐dropout number counts. With the present data, we cannot rule out the QSOs being hosted by the most massive haloes. However, neither can we confirm this widely used assumption. We conclude by giving detailed recommendations for the interpretation and planning of observations by current and future ground‐ and space‐based instruments that will shed new light on questions related to the large‐scale structure at z∼ 6.

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Simulation Data Model Version 1.0

Cited by 11 publications

References 8 publications

Galaxy morphology and star formation in the Illustris Simulation atz = 0

Galaxy morphology and star formation in the Illustris Simulation atz = 0

Witnessing the active assembly phase of massive galaxies sincez= 1

ΛCDM predictions for galaxy protoclusters - I. The relation between galaxies, protoclusters and quasars at

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