Ultraviolet-to-far infrared properties of Lyman break galaxies and luminous infrared galaxies at z ∼ 1

D. Burgarella, P. G. Pérez-González, K. D. Tyler, G. H. Rieke, V. Buat, T. T. Takeuchi, S. Lauger, S. Arnouts, O. Ilbert, T. A. Barlow, L. Bianchi, Y. W. Lee, B. F. Madore, R. F. Malina, A. S. Szalay, S. K. Yi

Research output: Contribution to journalArticle

36 Citations (Scopus)

Abstract

Aims. We present the first large, unbiased sample of Lyman Break Galaxies (LBGs) at z ∼ 1. Far ultraviolet-dropout (1530 Å) galaxies in the Chandra Deep Field South have been selected using GALEX data. This first large sample in the z ∼ 1 universe provides us with a high quality reference sample of LBGs. Methods. We analyzed the sample from the UV to the IR using GALEX, SPITZER, ES O and HS T data. Results. The morphology (obtained from GOODS data) of 75% of our LBGs is consistent with a disk. The vast majority of LBGs with an IR detection are also Luminous Infrared Galaxies (LIRGs). As a class, the galaxies not detected at 24 μm are an order of magnitude fainter relative to the UV compared with those detected individually, suggesting that there may be two types of behavior within the sample. For the IR-bright galaxies, there is an apparent upper limit for the UV dust attenuation and this upper limit is anti-correlated with the observed UV luminosity. Previous estimates of dust attenuations based on the ultraviolet slope are compared to new ones based on the FIR/UV ratio (for LBGs detected at 24 μm), which is usually a more reliable estimator. Depending on the calibration we use to estimate the total IR luminosity, β-based attenuations AFUV are larger by 0.2 to 0.6 mag. than the ones estimated from FIR/UV ratio. Finally, for IR-bright LBGs, median estimated β-based SFRs are 2-3 times larger than the total SFRs estimated as SFRTOT = SFRUV + SFRIR while IR-based SFRs provide values below SFRTOT by 15-20%. We use a stacking method to statistically constrain the 24 μm flux of LBGs non individually detected. The results suggest that these LBGs do not contain large amounts of dust.

Original languageEnglish
Pages (from-to)69-76
Number of pages8
JournalAstronomy and Astrophysics
Volume450
Issue number1
DOIs
Publication statusPublished - 2006 Apr 1

Fingerprint

galaxies
dust
reference sample
stacking
calibration
attenuation
luminosity
dropouts
method
estimates
estimators
universe
slopes
detection
goods

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Burgarella, D. ; Pérez-González, P. G. ; Tyler, K. D. ; Rieke, G. H. ; Buat, V. ; Takeuchi, T. T. ; Lauger, S. ; Arnouts, S. ; Ilbert, O. ; Barlow, T. A. ; Bianchi, L. ; Lee, Y. W. ; Madore, B. F. ; Malina, R. F. ; Szalay, A. S. ; Yi, S. K. / Ultraviolet-to-far infrared properties of Lyman break galaxies and luminous infrared galaxies at z ∼ 1. In: Astronomy and Astrophysics. 2006 ; Vol. 450, No. 1. pp. 69-76.
@article{f7b3ab54e1314971be7331c21ab35df2,
title = "Ultraviolet-to-far infrared properties of Lyman break galaxies and luminous infrared galaxies at z ∼ 1",
abstract = "Aims. We present the first large, unbiased sample of Lyman Break Galaxies (LBGs) at z ∼ 1. Far ultraviolet-dropout (1530 {\AA}) galaxies in the Chandra Deep Field South have been selected using GALEX data. This first large sample in the z ∼ 1 universe provides us with a high quality reference sample of LBGs. Methods. We analyzed the sample from the UV to the IR using GALEX, SPITZER, ES O and HS T data. Results. The morphology (obtained from GOODS data) of 75{\%} of our LBGs is consistent with a disk. The vast majority of LBGs with an IR detection are also Luminous Infrared Galaxies (LIRGs). As a class, the galaxies not detected at 24 μm are an order of magnitude fainter relative to the UV compared with those detected individually, suggesting that there may be two types of behavior within the sample. For the IR-bright galaxies, there is an apparent upper limit for the UV dust attenuation and this upper limit is anti-correlated with the observed UV luminosity. Previous estimates of dust attenuations based on the ultraviolet slope are compared to new ones based on the FIR/UV ratio (for LBGs detected at 24 μm), which is usually a more reliable estimator. Depending on the calibration we use to estimate the total IR luminosity, β-based attenuations AFUV are larger by 0.2 to 0.6 mag. than the ones estimated from FIR/UV ratio. Finally, for IR-bright LBGs, median estimated β-based SFRs are 2-3 times larger than the total SFRs estimated as SFRTOT = SFRUV + SFRIR while IR-based SFRs provide values below SFRTOT by 15-20{\%}. We use a stacking method to statistically constrain the 24 μm flux of LBGs non individually detected. The results suggest that these LBGs do not contain large amounts of dust.",
author = "D. Burgarella and P{\'e}rez-Gonz{\'a}lez, {P. G.} and Tyler, {K. D.} and Rieke, {G. H.} and V. Buat and Takeuchi, {T. T.} and S. Lauger and S. Arnouts and O. Ilbert and Barlow, {T. A.} and L. Bianchi and Lee, {Y. W.} and Madore, {B. F.} and Malina, {R. F.} and Szalay, {A. S.} and Yi, {S. K.}",
year = "2006",
month = "4",
day = "1",
doi = "10.1051/0004-6361:20054309",
language = "English",
volume = "450",
pages = "69--76",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",
number = "1",

}

Burgarella, D, Pérez-González, PG, Tyler, KD, Rieke, GH, Buat, V, Takeuchi, TT, Lauger, S, Arnouts, S, Ilbert, O, Barlow, TA, Bianchi, L, Lee, YW, Madore, BF, Malina, RF, Szalay, AS & Yi, SK 2006, 'Ultraviolet-to-far infrared properties of Lyman break galaxies and luminous infrared galaxies at z ∼ 1', Astronomy and Astrophysics, vol. 450, no. 1, pp. 69-76. https://doi.org/10.1051/0004-6361:20054309

Ultraviolet-to-far infrared properties of Lyman break galaxies and luminous infrared galaxies at z ∼ 1. / Burgarella, D.; Pérez-González, P. G.; Tyler, K. D.; Rieke, G. H.; Buat, V.; Takeuchi, T. T.; Lauger, S.; Arnouts, S.; Ilbert, O.; Barlow, T. A.; Bianchi, L.; Lee, Y. W.; Madore, B. F.; Malina, R. F.; Szalay, A. S.; Yi, S. K.

In: Astronomy and Astrophysics, Vol. 450, No. 1, 01.04.2006, p. 69-76.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Ultraviolet-to-far infrared properties of Lyman break galaxies and luminous infrared galaxies at z ∼ 1

AU - Burgarella, D.

AU - Pérez-González, P. G.

AU - Tyler, K. D.

AU - Rieke, G. H.

AU - Buat, V.

AU - Takeuchi, T. T.

AU - Lauger, S.

AU - Arnouts, S.

AU - Ilbert, O.

AU - Barlow, T. A.

AU - Bianchi, L.

AU - Lee, Y. W.

AU - Madore, B. F.

AU - Malina, R. F.

AU - Szalay, A. S.

AU - Yi, S. K.

PY - 2006/4/1

Y1 - 2006/4/1

N2 - Aims. We present the first large, unbiased sample of Lyman Break Galaxies (LBGs) at z ∼ 1. Far ultraviolet-dropout (1530 Å) galaxies in the Chandra Deep Field South have been selected using GALEX data. This first large sample in the z ∼ 1 universe provides us with a high quality reference sample of LBGs. Methods. We analyzed the sample from the UV to the IR using GALEX, SPITZER, ES O and HS T data. Results. The morphology (obtained from GOODS data) of 75% of our LBGs is consistent with a disk. The vast majority of LBGs with an IR detection are also Luminous Infrared Galaxies (LIRGs). As a class, the galaxies not detected at 24 μm are an order of magnitude fainter relative to the UV compared with those detected individually, suggesting that there may be two types of behavior within the sample. For the IR-bright galaxies, there is an apparent upper limit for the UV dust attenuation and this upper limit is anti-correlated with the observed UV luminosity. Previous estimates of dust attenuations based on the ultraviolet slope are compared to new ones based on the FIR/UV ratio (for LBGs detected at 24 μm), which is usually a more reliable estimator. Depending on the calibration we use to estimate the total IR luminosity, β-based attenuations AFUV are larger by 0.2 to 0.6 mag. than the ones estimated from FIR/UV ratio. Finally, for IR-bright LBGs, median estimated β-based SFRs are 2-3 times larger than the total SFRs estimated as SFRTOT = SFRUV + SFRIR while IR-based SFRs provide values below SFRTOT by 15-20%. We use a stacking method to statistically constrain the 24 μm flux of LBGs non individually detected. The results suggest that these LBGs do not contain large amounts of dust.

AB - Aims. We present the first large, unbiased sample of Lyman Break Galaxies (LBGs) at z ∼ 1. Far ultraviolet-dropout (1530 Å) galaxies in the Chandra Deep Field South have been selected using GALEX data. This first large sample in the z ∼ 1 universe provides us with a high quality reference sample of LBGs. Methods. We analyzed the sample from the UV to the IR using GALEX, SPITZER, ES O and HS T data. Results. The morphology (obtained from GOODS data) of 75% of our LBGs is consistent with a disk. The vast majority of LBGs with an IR detection are also Luminous Infrared Galaxies (LIRGs). As a class, the galaxies not detected at 24 μm are an order of magnitude fainter relative to the UV compared with those detected individually, suggesting that there may be two types of behavior within the sample. For the IR-bright galaxies, there is an apparent upper limit for the UV dust attenuation and this upper limit is anti-correlated with the observed UV luminosity. Previous estimates of dust attenuations based on the ultraviolet slope are compared to new ones based on the FIR/UV ratio (for LBGs detected at 24 μm), which is usually a more reliable estimator. Depending on the calibration we use to estimate the total IR luminosity, β-based attenuations AFUV are larger by 0.2 to 0.6 mag. than the ones estimated from FIR/UV ratio. Finally, for IR-bright LBGs, median estimated β-based SFRs are 2-3 times larger than the total SFRs estimated as SFRTOT = SFRUV + SFRIR while IR-based SFRs provide values below SFRTOT by 15-20%. We use a stacking method to statistically constrain the 24 μm flux of LBGs non individually detected. The results suggest that these LBGs do not contain large amounts of dust.

UR - http://www.scopus.com/inward/record.url?scp=33645822757&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=33645822757&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:20054309

DO - 10.1051/0004-6361:20054309

M3 - Article

AN - SCOPUS:33645822757

VL - 450

SP - 69

EP - 76

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

IS - 1

ER -