SG256RP Data (doi:10.7910/DVN/87R91P)

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SG256RP Data

doi:10.7910/DVN/87R91P

Harvard Dataverse

2013-06-14

1

Wise, John; Turk, Matthew; Abel, Tom; Smith, Britton, 2013, "SG256RP Data", https://doi.org/10.7910/DVN/87R91P, Harvard Dataverse, V1

SG256RP Data

Replication Data for "The Birth of a Galaxy. II. The Role of Radiation Pressure"

doi:10.7910/DVN/87R91P

Wise, John (Georgia Tech, School of Physics, Center for Relativistic Astrophysics)

Turk, Matthew (Columbia University)

Abel, Tom (Stanford University)

Smith, Britton (Michigan State University)

2013

2.0

2.5

1.8

1.6.1

1.1.0

1211626

Harvard Dataverse

Lizzy Rolando

2013-06-14

2013

https://doi.org/10.7910/DVN/87R91P

Cosmology, Galaxies, Galaxies Formation, Stars Formation, Radiative Transfer, Hydrodynamics

These files contain analyzed data from a cosmological simulation of early galaxy formation from approximately 50 different timesteps that span from 200 to 750 million years after the Big Bang. This simulation included the effects of radiation pressure, which may aid in regulating star formation in dwarf galaxies. The paper reporting on the analysis of these data can be found in the publication field of this record. <br></br> Related Publication Abstract: Massive stars provide feedback that shapes the interstellar medium of galaxies at all redshifts and their resulting stellar populations. Here we present three adaptive mesh refinement radiation hydrodynamics simulations that illustrate the impact of momentum transfer from ionising radiation to the absorbing gas on star formation in high-redshift dwarf galaxies. Momentum transfer is calculated by solving the radiative transfer equation with a ray tracing algorithm that is adaptive in spatial and angular coordinates. We find that momentum input partially affects star formation by increasing the turbulent support to a three-dimensional rms velocity equal to the circular velocity of early haloes. Compared to a calculation that neglects radiation pressure, the star formation rate is decreased by a factor of five to 1.8 x 10^{-2} solar masses per year in a dwarf galaxy with a dark matter and stellar mass of 2.0 x 10^8 solar masses and 4.5 x 10^5 solar masses, respectively,when radiation pressure is included. Its mean metallicity of 10^{-2.1} solar is consistent with the observed dwarf galaxy luminosity-metallicity relation. However, what one may naively expect from the calculation without radiation pressure, the central region of the galaxy overcools and produces a compact, metal-rich stellar population with an average metallicity of 0.3 solar, indicative of an incorrect physical recipe. In addition to photo-heating in HII regions, radiation pressure further drives dense gas from star forming regions, so supernovae feedback occurs in a warmer and more diffuse medium, launching metal-rich outflows. Capturing this aspect and a temporal separation between the start of radiative and supernova feedback are numerically important in the modeling of galaxies to avoid the "overcooling problem''. We estimate that dust in early low-mass galaxies is unlikely to aid in momentum transfer from radiation to the gas.

2011-04-17-2011-06-02

This simulation was run at the NASA machine, pleaides, on 512 cores.

Please contact John Wise if you plan to use these data.

John Wise, 404-894-5208, jwise@physics.gatech.edu

This dataset is made available with limited information on how it can be used. You may wish to communicate with the Contact(s) specified before use.

Wise, J. H., Abel, T., Turk, M. J., Norman, M. L., & Smith, B. D. 2012, “The Birth of a Galaxy. II. The Role of Radiation Pressure”, Monthly Notices of the Royal Astronomical Society, 427, 311-326. doi:10.1111/j.1365-2966.2012.21809.x.

1206.1043

Wise, J. H., Abel, T., Turk, M. J., Norman, M. L., & Smith, B. D. 2012, “The Birth of a Galaxy. II. The Role of Radiation Pressure”, Monthly Notices of the Royal Astronomical Society, 427, 311-326. doi:10.1111/j.1365-2966.2012.21809.x.

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