Lyman break galaxies and the Lγα forest

Juna A. Kollmeier, David H. Weinberg, Romeel S Dave, Neal Katz

Research output: Contribution to journalArticle

37 Citations (Scopus)

Abstract

We use hydrodynamic cosmological simulations to predict correlations between Lγα forest absorption and the galaxy distribution at redshift z ≈ 3. The probability distribution function (PDF) of Lγα flux decrements shifts systematically toward higher values in the vicinity of galaxies, reflecting the overdense environments in which these galaxies reside. The predicted signal remains strong in spectra smoothed over 50-200 km s-1, allowing tests with moderate-resolution quasar spectra. The strong bias of high-redshift galaxies toward high-density regions imprints a clear signature on the flux PDF, but the predictions are not sensitive to galaxy baryon mass or star formation rate, and they are similar for galaxies and dark matter halos. The dependence of the flux PDF on galaxy proximity is sensitive to redshift determination errors, with rms errors of 150-300 km s-1 substantially weakening the predicted trends. On larger scales, the mean galaxy overdensity in a cube of 5 or 10 h-1 Mpc (comoving) is strongly correlated with the mean Lγα flux decrement on a line of sight through the cube center. The slope of the correlation is ∼3 times steeper for galaxies than for dark matter as a result of galaxy bias. The predicted large-scale correlation is in qualitative agreement with recently reported observational results. However, observations also show a drop in the average absorption in the immediate vicinity of galaxies, which our models do not predict even if we allow the galaxies or active galactic nuclei within them to be ionizing sources. This decreased absorption could be a signature of galaxy feedback on the surrounding intergalactic medium, perhaps via galactic winds. We find that a simplified "wind" model that eliminates neutral hydrogen in spheres around the galaxies can marginally explain the data. However, because peculiar velocities allow gas at large distances to produce saturated absorption at the galaxy redshift, these winds (or any other feedback mechanism) must extend to comoving radii of ∼ 1.5 h-1 Mpc to reproduce the observations. We also discuss the possibility that extended Lγα emission from the target galaxies "fills in" the expected Lγα forest absorption at small angular separations.

Original languageEnglish (US)
Pages (from-to)75-96
Number of pages22
JournalAstrophysical Journal
Volume594
Issue number1 I
DOIs
StatePublished - Sep 1 2003

Fingerprint

galaxies
feedback mechanism
probability distribution functions
hydrodynamics
hydrogen
distribution
dark matter
prediction
gas
signatures
simulation
galactic winds
intergalactic media
star formation rate
active galactic nuclei
quasars
line of sight
proximity
baryons
halos

Keywords

  • Galaxies: high-redshift
  • Quasars: absorption lines

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Kollmeier, J. A., Weinberg, D. H., Dave, R. S., & Katz, N. (2003). Lyman break galaxies and the Lγα forest. Astrophysical Journal, 594(1 I), 75-96. https://doi.org/10.1086/376789

Lyman break galaxies and the Lγα forest. / Kollmeier, Juna A.; Weinberg, David H.; Dave, Romeel S; Katz, Neal.

In: Astrophysical Journal, Vol. 594, No. 1 I, 01.09.2003, p. 75-96.

Research output: Contribution to journalArticle

Kollmeier, JA, Weinberg, DH, Dave, RS & Katz, N 2003, 'Lyman break galaxies and the Lγα forest', Astrophysical Journal, vol. 594, no. 1 I, pp. 75-96. https://doi.org/10.1086/376789
Kollmeier, Juna A. ; Weinberg, David H. ; Dave, Romeel S ; Katz, Neal. / Lyman break galaxies and the Lγα forest. In: Astrophysical Journal. 2003 ; Vol. 594, No. 1 I. pp. 75-96.
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AB - We use hydrodynamic cosmological simulations to predict correlations between Lγα forest absorption and the galaxy distribution at redshift z ≈ 3. The probability distribution function (PDF) of Lγα flux decrements shifts systematically toward higher values in the vicinity of galaxies, reflecting the overdense environments in which these galaxies reside. The predicted signal remains strong in spectra smoothed over 50-200 km s-1, allowing tests with moderate-resolution quasar spectra. The strong bias of high-redshift galaxies toward high-density regions imprints a clear signature on the flux PDF, but the predictions are not sensitive to galaxy baryon mass or star formation rate, and they are similar for galaxies and dark matter halos. The dependence of the flux PDF on galaxy proximity is sensitive to redshift determination errors, with rms errors of 150-300 km s-1 substantially weakening the predicted trends. On larger scales, the mean galaxy overdensity in a cube of 5 or 10 h-1 Mpc (comoving) is strongly correlated with the mean Lγα flux decrement on a line of sight through the cube center. The slope of the correlation is ∼3 times steeper for galaxies than for dark matter as a result of galaxy bias. The predicted large-scale correlation is in qualitative agreement with recently reported observational results. However, observations also show a drop in the average absorption in the immediate vicinity of galaxies, which our models do not predict even if we allow the galaxies or active galactic nuclei within them to be ionizing sources. This decreased absorption could be a signature of galaxy feedback on the surrounding intergalactic medium, perhaps via galactic winds. We find that a simplified "wind" model that eliminates neutral hydrogen in spheres around the galaxies can marginally explain the data. However, because peculiar velocities allow gas at large distances to produce saturated absorption at the galaxy redshift, these winds (or any other feedback mechanism) must extend to comoving radii of ∼ 1.5 h-1 Mpc to reproduce the observations. We also discuss the possibility that extended Lγα emission from the target galaxies "fills in" the expected Lγα forest absorption at small angular separations.

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