The Environmental Impact of Lyman Break Galaxies

Tasker, Elizabeth J.; Bryan, Greg L.

doi:10.1086/504469

Cited by 10 publications

(11 citation statements)

References 25 publications

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“…Tasker & Bryan (2006) run a set of simulations similar to Li, Mac Low & Klessen (2005b) except that they include SN feedback and the gas is simulated on a grid. Even though their feedback implementation simply pours the feedback energy into the ISM, it proves effective at limiting star formation.…”

Section: Discussionmentioning

confidence: 99%

Star formation and feedback in smoothed particle hydrodynamic simulations – I. Isolated galaxies

Stinson¹,

Seth²,

Katz³

et al. 2006

Monthly Notices of the Royal Astronomical Society

773

1,072

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We present an analysis of star formation and feedback recipes appropriate for galactic smoothed particle hydrodynamics simulations. Using an isolated Milky Way-like galaxy, we constrain these recipes based on well-established observational results. Our star formation recipe is based on that of Katz with the additional inclusion of physically motivated supernova feedback recipes. We propose a new feedback recipe in which Type II supernovae are modelled using an analytical treatment of blastwaves. With this feedback mechanism and a tuning of other star formation parameters, the star formation in our isolated Milky Way-like galaxy follows the slope and normalization of the observed Schmidt law. In addition, we reproduce the lowdensity cut-off and filamentary structure of star formation observed in disc galaxies. Our final recipe will enable better comparison of N-body simulations with observations.

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Section: Discussionmentioning

confidence: 99%

Star formation and feedback in smoothed particle hydrodynamic simulations – I. Isolated galaxies

Stinson¹,

Seth²,

Katz³

et al. 2006

Monthly Notices of the Royal Astronomical Society

773

1,072

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“…At high redshifts, LBGs studies show that active star formation traced by the UV light resides preferentially in overdense regions Blaizot et al 2004;Giavalisco 2002;Steidel et al 1998;Tasker & Bryan 2006). At low redshift, Abbas & Sheth (2005) showed that the slope of the fitted power law is steeper in underdense regions, and that the correlation length is smaller.…”

Section: Discussionmentioning

confidence: 99%

Clustering Properties of Rest‐Frame UV‐Selected Galaxies. II. Migration of Star Formation Sites with Cosmic Time fromGALEXand CFHTLS

Heinis¹,

Milliard²,

Arnouts³

et al. 2007

ASTROPHYS J SUPPL S

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We analyze the clustering properties of ultraviolet-selected galaxies by using GALEX-SDSS data at z < 0:6 and CFHTLS deep u 0 imaging at z $ 1. These data sets provide a unique basis at z 1 which can be directly compared with high-redshift samples built with similar selection criteria. We discuss the dependence of the correlation function parameters (r 0 and ) on the ultraviolet luminosity, as well as the linear bias evolution. We find that the bias parameter shows a gradual decline from high (b 8 k 2) to low redshift (b 8 ' 0:79 þ0:1 À0:08 ). When accounting for the fraction of the star formation activity enclosed in the different samples, our results suggest that the bulk of star formation migrated from high-mass dark matter halos at z > 2 (10 12 M M min 10 13 M , located in high-density regions) to less massive halos at low redshift (M min 10 12 M , located in low-density regions). This result extends the ''downsizing'' picture (shift of the star formation activity from high stellar mass systems at high z to low stellar mass at low z) to the dark matter distribution.

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“…Currently, limitations in computer power as well as in the efficiency of available algorithms, make it possible to resolve at best scales of 100 pc in cosmological simulations (very recent simulations have been able to achieve a resolution of less than 50 pc, but they can only cover the first few billion years of evolution 43 ). Simulations with resolution adequate to follow directly molecular clouds, interstellar turbulence and star formation do exist, but are restricted to studying an isolated galaxy 64,65 or a small region of a single galaxy 66 . Detailed numerical models of the effects of supernovae explosions also exist, but again they are restricted to a small volume of the ISM 67,68 .…”

Section: Modeling Issuesmentioning

confidence: 99%

Formation of Disk Galaxies in Computer Simulations

Mayer¹,

Governato²,

Kaufmann³

2008

adv sci lett

125

145

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The formation of disk galaxies is one of the most outstanding problems in modern astrophysics and cosmology. We review the progress made by numerical simulations carried out on large parallel supercomputers. These simulations model the formation of disk galaxies within the current structure formation paradigm in which the Universe is dominated by a cold dark matter component and a cosmological constant. We discuss how computer simulations have been an essential tool in advancing the field further over the last decade or so. Recent progress stems from a combination of increased resolution and improved treatment of the astrophysical processes modeled in the simulations, such as the phenomenological description of the interstellar medium and of the process of star formation. We argue that high mass and spatial resolution is a necessary condition in order to obtain large disks comparable with observed spiral galaxies avoiding spurious dissipation of angular momentum. A realistic model of the star formation history. gas-to-stars ratio and the morphology of the stellar and gaseous component is instead controlled by the phenomenological description of the non-gravitational energy budget in the galaxy. This includes the energy injection by supernovae explosions as well as by accreting supermassive black holes at scales below the resolution. We continue by showing that simulations of gas collapse within cold dark matter halos including a phenomenological description of supernovae blast-waves allow to obtain stellar disks with nearly exponential surface density profiles as those observed in real disk galaxies, counteracting the tendency of gas collapsing in such halos to form cuspy baryonic profiles. However, the ab-initio formation of a realistic rotationally supported disk galaxy with a pure exponential disk in a fully cosmological simulation is still an open problem. We argue that the suppression of bulge formation is related to the physics of galaxy formation during the merger of the most massive protogalactic lumps at high redshift, where the reionization of the Universe likely plays a key role. A sufficiently high resolution during this early phase of galaxy formation is also crucial to avoid artificial angular momentum loss and spurious bulge formation. Finally, we discuss the role of mergers in disk formation, adiabatic halo contraction during the assembly of the disk, cold flows, thermal instability and other aspects of galaxy formation, focusing on their relevance to the puzzling origin of bulgeless galaxies.keywords:astrophysics, cosmology, computer science, fluid dynamics 1 Galaxy formation in a hierarchical UniverseGalaxies occupy a special place in our quest for understanding the Universe. They are large islands in a nearly empty space and contain most of the ordinary baryonic matter, stars and interstellar gas, that emits radiation and can thus be detected by astronomers 1 . Galaxies come essentially in two broad categories 2 , those in which the luminous mass is arranged in a rotating disk of stars...

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The Environmental Impact of Lyman Break Galaxies

Cited by 10 publications

References 25 publications

Star formation and feedback in smoothed particle hydrodynamic simulations – I. Isolated galaxies

Star formation and feedback in smoothed particle hydrodynamic simulations – I. Isolated galaxies

Clustering Properties of Rest‐Frame UV‐Selected Galaxies. II. Migration of Star Formation Sites with Cosmic Time fromGALEXand CFHTLS

Formation of Disk Galaxies in Computer Simulations

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