Morphology and size differences between local and high-redshift luminous infrared galaxies

Wiphu Rujopakarn, George H. Rieke, Daniel J. Eisenstein, St́ephanie Juneau

Research output: Contribution to journalArticle

33 Citations (Scopus)

Abstract

We show that the star-forming regions in high-redshift luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs) and submillimeter galaxies (SMGs) have similar physical scales to those in local normal star-forming galaxies. To first order, their higher infrared (IR) luminosities result from higher luminosity surface density. We also find a good correlation between the IR luminosity and IR luminosity surface density in starburst galaxies across over five orders of magnitude of IR luminosity from local normal galaxies to z ∼ 2 SMGs. The intensely star-forming regions of local ULIRGs are significantly smaller than those in their high-redshift counterparts and hence diverge significantly from this correlation, indicating that the ULIRGs found locally are a different population from the high-redshift ULIRGs and SMGs. Based on this relationship, we suggest that luminosity surface density should serve as a more accurate indicator for the IR emitting environment, and hence the observable properties, of star-forming galaxies than their IR luminosity. We demonstrate this approach by showing that ULIRGs at z ∼ 1 and a lensed galaxy at z ∼ 2.5 exhibit aromatic features agreeing with local LIRGs that are an order of magnitude less luminous, but have similar IR luminosity surface density. A consequence of this relationship is that the aromatic emission strength in star-forming galaxies will appear to increase at z > 1 for a given IR luminosity compared to their local counterparts.

Original languageEnglish (US)
JournalAstrophysical Journal
Volume726
Issue number2
DOIs
StatePublished - Jan 10 2011

Fingerprint

luminosity
galaxies
stars
starburst galaxies

Keywords

  • Galaxies: evolution
  • Galaxies: high-redshift
  • Galaxies: starburst
  • Galaxies: structure
  • Infrared: galaxies

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Morphology and size differences between local and high-redshift luminous infrared galaxies. / Rujopakarn, Wiphu; Rieke, George H.; Eisenstein, Daniel J.; Juneau, St́ephanie.

In: Astrophysical Journal, Vol. 726, No. 2, 10.01.2011.

Research output: Contribution to journalArticle

Rujopakarn, Wiphu ; Rieke, George H. ; Eisenstein, Daniel J. ; Juneau, St́ephanie. / Morphology and size differences between local and high-redshift luminous infrared galaxies. In: Astrophysical Journal. 2011 ; Vol. 726, No. 2.
@article{b97218e382684bf8a0f5e795da098d41,
title = "Morphology and size differences between local and high-redshift luminous infrared galaxies",
abstract = "We show that the star-forming regions in high-redshift luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs) and submillimeter galaxies (SMGs) have similar physical scales to those in local normal star-forming galaxies. To first order, their higher infrared (IR) luminosities result from higher luminosity surface density. We also find a good correlation between the IR luminosity and IR luminosity surface density in starburst galaxies across over five orders of magnitude of IR luminosity from local normal galaxies to z ∼ 2 SMGs. The intensely star-forming regions of local ULIRGs are significantly smaller than those in their high-redshift counterparts and hence diverge significantly from this correlation, indicating that the ULIRGs found locally are a different population from the high-redshift ULIRGs and SMGs. Based on this relationship, we suggest that luminosity surface density should serve as a more accurate indicator for the IR emitting environment, and hence the observable properties, of star-forming galaxies than their IR luminosity. We demonstrate this approach by showing that ULIRGs at z ∼ 1 and a lensed galaxy at z ∼ 2.5 exhibit aromatic features agreeing with local LIRGs that are an order of magnitude less luminous, but have similar IR luminosity surface density. A consequence of this relationship is that the aromatic emission strength in star-forming galaxies will appear to increase at z > 1 for a given IR luminosity compared to their local counterparts.",
keywords = "Galaxies: evolution, Galaxies: high-redshift, Galaxies: starburst, Galaxies: structure, Infrared: galaxies",
author = "Wiphu Rujopakarn and Rieke, {George H.} and Eisenstein, {Daniel J.} and St́ephanie Juneau",
year = "2011",
month = "1",
day = "10",
doi = "10.1088/0004-637X/726/2/93",
language = "English (US)",
volume = "726",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2",

}

TY - JOUR

T1 - Morphology and size differences between local and high-redshift luminous infrared galaxies

AU - Rujopakarn, Wiphu

AU - Rieke, George H.

AU - Eisenstein, Daniel J.

AU - Juneau, St́ephanie

PY - 2011/1/10

Y1 - 2011/1/10

N2 - We show that the star-forming regions in high-redshift luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs) and submillimeter galaxies (SMGs) have similar physical scales to those in local normal star-forming galaxies. To first order, their higher infrared (IR) luminosities result from higher luminosity surface density. We also find a good correlation between the IR luminosity and IR luminosity surface density in starburst galaxies across over five orders of magnitude of IR luminosity from local normal galaxies to z ∼ 2 SMGs. The intensely star-forming regions of local ULIRGs are significantly smaller than those in their high-redshift counterparts and hence diverge significantly from this correlation, indicating that the ULIRGs found locally are a different population from the high-redshift ULIRGs and SMGs. Based on this relationship, we suggest that luminosity surface density should serve as a more accurate indicator for the IR emitting environment, and hence the observable properties, of star-forming galaxies than their IR luminosity. We demonstrate this approach by showing that ULIRGs at z ∼ 1 and a lensed galaxy at z ∼ 2.5 exhibit aromatic features agreeing with local LIRGs that are an order of magnitude less luminous, but have similar IR luminosity surface density. A consequence of this relationship is that the aromatic emission strength in star-forming galaxies will appear to increase at z > 1 for a given IR luminosity compared to their local counterparts.

AB - We show that the star-forming regions in high-redshift luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs) and submillimeter galaxies (SMGs) have similar physical scales to those in local normal star-forming galaxies. To first order, their higher infrared (IR) luminosities result from higher luminosity surface density. We also find a good correlation between the IR luminosity and IR luminosity surface density in starburst galaxies across over five orders of magnitude of IR luminosity from local normal galaxies to z ∼ 2 SMGs. The intensely star-forming regions of local ULIRGs are significantly smaller than those in their high-redshift counterparts and hence diverge significantly from this correlation, indicating that the ULIRGs found locally are a different population from the high-redshift ULIRGs and SMGs. Based on this relationship, we suggest that luminosity surface density should serve as a more accurate indicator for the IR emitting environment, and hence the observable properties, of star-forming galaxies than their IR luminosity. We demonstrate this approach by showing that ULIRGs at z ∼ 1 and a lensed galaxy at z ∼ 2.5 exhibit aromatic features agreeing with local LIRGs that are an order of magnitude less luminous, but have similar IR luminosity surface density. A consequence of this relationship is that the aromatic emission strength in star-forming galaxies will appear to increase at z > 1 for a given IR luminosity compared to their local counterparts.

KW - Galaxies: evolution

KW - Galaxies: high-redshift

KW - Galaxies: starburst

KW - Galaxies: structure

KW - Infrared: galaxies

UR - http://www.scopus.com/inward/record.url?scp=84891172383&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84891172383&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/726/2/93

DO - 10.1088/0004-637X/726/2/93

M3 - Article

AN - SCOPUS:84891172383

VL - 726

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2

ER -