Infrared luminosity functions from the chandra deep field-south: The Spitzer view on the history of dusty star formation at 0 ≲ z ≲ 1 1

Emeric Le Floc'h, Casey Papovich, Hervé Dole, Eric F. Bell, Guilaine Lagache, George H. Rieke, Eiichi Egami, Pablo G. Pérez-González, Almudena Alonso-Herrero, Marcia J Rieke, Myra Blaylock, Charles W. Engelbracht, Karl D. Gordon, Dean C. Hines, Karl A. Misselt, Jane E. Morrison, Jeremy Mould

Research output: Contribution to journalArticle

610 Citations (Scopus)

Abstract

We analyze a sample of ∼2600 Spitzer MIPS 24 μm sources brighter than ∼80μJy and located in the Chandra Deep Field-South to characterize the evolution of the comoving infrared (IR) energy density of the universe up to z ∼ 1. Using published ancillary optical data, we first obtain a nearly complete redshift determination for the 24 μm objects associated with R ≲ 24 mag counterparts at z ≲ 1. These sources represent ∼55%-60% of the total MIPS 24 μm population with f24 μm ≳ 80 μJy, the rest of the sample likely lying at higher redshifts. We then determine an estimate of their total IR luminosities using various libraries of IR spectral energy distributions. We find that the 24μm population at 0.5 ≲ z ≲ 1 is dominated by "luminous infrared galaxies" (i.e., 1011 L ≤ LIR ≤ 1012 L), the counterparts of which appear to be also luminous at optical wavelengths and tend to be more massive than the majority of optically selected galaxies. A significant number of fainter sources (5 × 10 10 L ≤ LIR ≤ 1012 L ) are also detected at similar distances. We finally derive 15 μm and total IR luminosity functions (LFs) up to z ∼ 1. In agreement with the previous results from the Infrared Space Observatory (ISO) and SCUBA and as expected from the MIPS source number counts, we find very strong evolution of the contribution of the IR-selected population with look-back time. Pure evolution in density is firmly excluded by the data, but we find considerable degeneracy between strict evolution in luminosity and a combination of increases in both density and luminosity [ZLIR* ∝ (1 + z) 3.2_0.7 -0.2, φIR*IR ∝ (1 + z)0.7 +0.2 -0.6]. A significant steepening of the faint-end slope of the IR luminosity function is also unlikely, as it would overproduce the faint 24 μm source number counts. Our results imply that the comoving IR energy density of the universe evolves as (1 + z)3.9±0.4 up to z ∼ 1 and that galaxies luminous in the infrared (i.e., LIR ≥ 1011 L) are responsible for 70% ± 15% of this energy density at z ∼ 1. Taking into account the contribution of the UV luminosity evolving as (1 + z)∼2.5, we infer that these IR-luminous sources dominate the star-forming activity beyond z ∼ 0.7. The uncertainties affecting these conclusions are largely dominated by the errors in the k-corrections used to convert 24 μm fluxes into luminosities.

Original languageEnglish (US)
Pages (from-to)169-190
Number of pages22
JournalAstrophysical Journal
Volume632
Issue number1 I
DOIs
StatePublished - Oct 10 2005

Fingerprint

star formation
luminosity
histories
history
flux density
galaxies
energy
universe
Infrared Space Observatory (ISO)
spectral energy distribution
observatory
slopes
wavelength
stars
estimates
wavelengths

Keywords

  • Cosmology: observations
  • Galaxies: evolution
  • Galaxies: high-redshift infrared: galaxies

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Infrared luminosity functions from the chandra deep field-south : The Spitzer view on the history of dusty star formation at 0 ≲ z ≲ 1 1. / Le Floc'h, Emeric; Papovich, Casey; Dole, Hervé; Bell, Eric F.; Lagache, Guilaine; Rieke, George H.; Egami, Eiichi; Pérez-González, Pablo G.; Alonso-Herrero, Almudena; Rieke, Marcia J; Blaylock, Myra; Engelbracht, Charles W.; Gordon, Karl D.; Hines, Dean C.; Misselt, Karl A.; Morrison, Jane E.; Mould, Jeremy.

In: Astrophysical Journal, Vol. 632, No. 1 I, 10.10.2005, p. 169-190.

Research output: Contribution to journalArticle

Le Floc'h, E, Papovich, C, Dole, H, Bell, EF, Lagache, G, Rieke, GH, Egami, E, Pérez-González, PG, Alonso-Herrero, A, Rieke, MJ, Blaylock, M, Engelbracht, CW, Gordon, KD, Hines, DC, Misselt, KA, Morrison, JE & Mould, J 2005, 'Infrared luminosity functions from the chandra deep field-south: The Spitzer view on the history of dusty star formation at 0 ≲ z ≲ 1 1', Astrophysical Journal, vol. 632, no. 1 I, pp. 169-190. https://doi.org/10.1086/432789
Le Floc'h, Emeric ; Papovich, Casey ; Dole, Hervé ; Bell, Eric F. ; Lagache, Guilaine ; Rieke, George H. ; Egami, Eiichi ; Pérez-González, Pablo G. ; Alonso-Herrero, Almudena ; Rieke, Marcia J ; Blaylock, Myra ; Engelbracht, Charles W. ; Gordon, Karl D. ; Hines, Dean C. ; Misselt, Karl A. ; Morrison, Jane E. ; Mould, Jeremy. / Infrared luminosity functions from the chandra deep field-south : The Spitzer view on the history of dusty star formation at 0 ≲ z ≲ 1 1. In: Astrophysical Journal. 2005 ; Vol. 632, No. 1 I. pp. 169-190.
@article{043132eb677543fcac29a8b7a173d4cf,
title = "Infrared luminosity functions from the chandra deep field-south: The Spitzer view on the history of dusty star formation at 0 ≲ z ≲ 1 1",
abstract = "We analyze a sample of ∼2600 Spitzer MIPS 24 μm sources brighter than ∼80μJy and located in the Chandra Deep Field-South to characterize the evolution of the comoving infrared (IR) energy density of the universe up to z ∼ 1. Using published ancillary optical data, we first obtain a nearly complete redshift determination for the 24 μm objects associated with R ≲ 24 mag counterparts at z ≲ 1. These sources represent ∼55{\%}-60{\%} of the total MIPS 24 μm population with f24 μm ≳ 80 μJy, the rest of the sample likely lying at higher redshifts. We then determine an estimate of their total IR luminosities using various libraries of IR spectral energy distributions. We find that the 24μm population at 0.5 ≲ z ≲ 1 is dominated by {"}luminous infrared galaxies{"} (i.e., 1011 L⊙ ≤ LIR ≤ 1012 L⊙), the counterparts of which appear to be also luminous at optical wavelengths and tend to be more massive than the majority of optically selected galaxies. A significant number of fainter sources (5 × 10 10 L⊙ ≤ LIR ≤ 1012 L ⊙) are also detected at similar distances. We finally derive 15 μm and total IR luminosity functions (LFs) up to z ∼ 1. In agreement with the previous results from the Infrared Space Observatory (ISO) and SCUBA and as expected from the MIPS source number counts, we find very strong evolution of the contribution of the IR-selected population with look-back time. Pure evolution in density is firmly excluded by the data, but we find considerable degeneracy between strict evolution in luminosity and a combination of increases in both density and luminosity [ZLIR* ∝ (1 + z) 3.2_0.7 -0.2, φIR*IR ∝ (1 + z)0.7 +0.2 -0.6]. A significant steepening of the faint-end slope of the IR luminosity function is also unlikely, as it would overproduce the faint 24 μm source number counts. Our results imply that the comoving IR energy density of the universe evolves as (1 + z)3.9±0.4 up to z ∼ 1 and that galaxies luminous in the infrared (i.e., LIR ≥ 1011 L⊙) are responsible for 70{\%} ± 15{\%} of this energy density at z ∼ 1. Taking into account the contribution of the UV luminosity evolving as (1 + z)∼2.5, we infer that these IR-luminous sources dominate the star-forming activity beyond z ∼ 0.7. The uncertainties affecting these conclusions are largely dominated by the errors in the k-corrections used to convert 24 μm fluxes into luminosities.",
keywords = "Cosmology: observations, Galaxies: evolution, Galaxies: high-redshift infrared: galaxies",
author = "{Le Floc'h}, Emeric and Casey Papovich and Herv{\'e} Dole and Bell, {Eric F.} and Guilaine Lagache and Rieke, {George H.} and Eiichi Egami and P{\'e}rez-Gonz{\'a}lez, {Pablo G.} and Almudena Alonso-Herrero and Rieke, {Marcia J} and Myra Blaylock and Engelbracht, {Charles W.} and Gordon, {Karl D.} and Hines, {Dean C.} and Misselt, {Karl A.} and Morrison, {Jane E.} and Jeremy Mould",
year = "2005",
month = "10",
day = "10",
doi = "10.1086/432789",
language = "English (US)",
volume = "632",
pages = "169--190",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "1 I",

}

TY - JOUR

T1 - Infrared luminosity functions from the chandra deep field-south

T2 - The Spitzer view on the history of dusty star formation at 0 ≲ z ≲ 1 1

AU - Le Floc'h, Emeric

AU - Papovich, Casey

AU - Dole, Hervé

AU - Bell, Eric F.

AU - Lagache, Guilaine

AU - Rieke, George H.

AU - Egami, Eiichi

AU - Pérez-González, Pablo G.

AU - Alonso-Herrero, Almudena

AU - Rieke, Marcia J

AU - Blaylock, Myra

AU - Engelbracht, Charles W.

AU - Gordon, Karl D.

AU - Hines, Dean C.

AU - Misselt, Karl A.

AU - Morrison, Jane E.

AU - Mould, Jeremy

PY - 2005/10/10

Y1 - 2005/10/10

N2 - We analyze a sample of ∼2600 Spitzer MIPS 24 μm sources brighter than ∼80μJy and located in the Chandra Deep Field-South to characterize the evolution of the comoving infrared (IR) energy density of the universe up to z ∼ 1. Using published ancillary optical data, we first obtain a nearly complete redshift determination for the 24 μm objects associated with R ≲ 24 mag counterparts at z ≲ 1. These sources represent ∼55%-60% of the total MIPS 24 μm population with f24 μm ≳ 80 μJy, the rest of the sample likely lying at higher redshifts. We then determine an estimate of their total IR luminosities using various libraries of IR spectral energy distributions. We find that the 24μm population at 0.5 ≲ z ≲ 1 is dominated by "luminous infrared galaxies" (i.e., 1011 L⊙ ≤ LIR ≤ 1012 L⊙), the counterparts of which appear to be also luminous at optical wavelengths and tend to be more massive than the majority of optically selected galaxies. A significant number of fainter sources (5 × 10 10 L⊙ ≤ LIR ≤ 1012 L ⊙) are also detected at similar distances. We finally derive 15 μm and total IR luminosity functions (LFs) up to z ∼ 1. In agreement with the previous results from the Infrared Space Observatory (ISO) and SCUBA and as expected from the MIPS source number counts, we find very strong evolution of the contribution of the IR-selected population with look-back time. Pure evolution in density is firmly excluded by the data, but we find considerable degeneracy between strict evolution in luminosity and a combination of increases in both density and luminosity [ZLIR* ∝ (1 + z) 3.2_0.7 -0.2, φIR*IR ∝ (1 + z)0.7 +0.2 -0.6]. A significant steepening of the faint-end slope of the IR luminosity function is also unlikely, as it would overproduce the faint 24 μm source number counts. Our results imply that the comoving IR energy density of the universe evolves as (1 + z)3.9±0.4 up to z ∼ 1 and that galaxies luminous in the infrared (i.e., LIR ≥ 1011 L⊙) are responsible for 70% ± 15% of this energy density at z ∼ 1. Taking into account the contribution of the UV luminosity evolving as (1 + z)∼2.5, we infer that these IR-luminous sources dominate the star-forming activity beyond z ∼ 0.7. The uncertainties affecting these conclusions are largely dominated by the errors in the k-corrections used to convert 24 μm fluxes into luminosities.

AB - We analyze a sample of ∼2600 Spitzer MIPS 24 μm sources brighter than ∼80μJy and located in the Chandra Deep Field-South to characterize the evolution of the comoving infrared (IR) energy density of the universe up to z ∼ 1. Using published ancillary optical data, we first obtain a nearly complete redshift determination for the 24 μm objects associated with R ≲ 24 mag counterparts at z ≲ 1. These sources represent ∼55%-60% of the total MIPS 24 μm population with f24 μm ≳ 80 μJy, the rest of the sample likely lying at higher redshifts. We then determine an estimate of their total IR luminosities using various libraries of IR spectral energy distributions. We find that the 24μm population at 0.5 ≲ z ≲ 1 is dominated by "luminous infrared galaxies" (i.e., 1011 L⊙ ≤ LIR ≤ 1012 L⊙), the counterparts of which appear to be also luminous at optical wavelengths and tend to be more massive than the majority of optically selected galaxies. A significant number of fainter sources (5 × 10 10 L⊙ ≤ LIR ≤ 1012 L ⊙) are also detected at similar distances. We finally derive 15 μm and total IR luminosity functions (LFs) up to z ∼ 1. In agreement with the previous results from the Infrared Space Observatory (ISO) and SCUBA and as expected from the MIPS source number counts, we find very strong evolution of the contribution of the IR-selected population with look-back time. Pure evolution in density is firmly excluded by the data, but we find considerable degeneracy between strict evolution in luminosity and a combination of increases in both density and luminosity [ZLIR* ∝ (1 + z) 3.2_0.7 -0.2, φIR*IR ∝ (1 + z)0.7 +0.2 -0.6]. A significant steepening of the faint-end slope of the IR luminosity function is also unlikely, as it would overproduce the faint 24 μm source number counts. Our results imply that the comoving IR energy density of the universe evolves as (1 + z)3.9±0.4 up to z ∼ 1 and that galaxies luminous in the infrared (i.e., LIR ≥ 1011 L⊙) are responsible for 70% ± 15% of this energy density at z ∼ 1. Taking into account the contribution of the UV luminosity evolving as (1 + z)∼2.5, we infer that these IR-luminous sources dominate the star-forming activity beyond z ∼ 0.7. The uncertainties affecting these conclusions are largely dominated by the errors in the k-corrections used to convert 24 μm fluxes into luminosities.

KW - Cosmology: observations

KW - Galaxies: evolution

KW - Galaxies: high-redshift infrared: galaxies

UR - http://www.scopus.com/inward/record.url?scp=28044460090&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=28044460090&partnerID=8YFLogxK

U2 - 10.1086/432789

DO - 10.1086/432789

M3 - Article

AN - SCOPUS:28044460090

VL - 632

SP - 169

EP - 190

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1 I

ER -