Mid‐Infrared Spectroscopy of Lensed Galaxies at 1 &lt;<i>z</i>&lt; 3: The Nature of Sources Near the MIPS Confusion Limit

Rigby, J. Keith; Marcillac, D.; Egami, Eiichi; Rieke, G. H.; Richard, Johan; Kneib, Jean-Paul; Fadda, D.; Willmer, Christopher N. A.; Borys, Colin; Werf, P. P. van der; Pérez‐González, Pablo G.; Knudsen, K. K.; Papovich, Casey

doi:10.1086/525273

Cited by 92 publications

(147 citation statements)

References 85 publications

(167 reference statements)

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“…This result is consistent with the earlier findings by various Spitzer observations (e.g., Papovich et al 2007;Rigby et al 2008). This also implies that these higher-redshift star-forming galaxies have a larger amount of colder dust compared to the local galaxies with similar infrared luminosities.…”

Section: Overview Of the Bullet Cluster Sdp Datasupporting

confidence: 94%

“…However, the validity of all these Spitzer-based results rests on the assumption that the total infrared luminosities of high-redshift infrared galaxies can be estimated accurately by sampling their rest-frame mid-infrared emission (e.g., the MIPS 24 μm band samples the rest-frame 8 μm emission at z = 2). Indeed, some Spitzer results have already questioned this assumption, suggesting that the use of local galaxy spectral energy distribution (SED) templates may lead to overestimating the total infrared luminosities of high-redshift galaxies (e.g., Papovich et al 2007;Rigby et al 2008). Herschel will allow us to measure the total infrared luminosities of a large number of high-redshift galaxies directly for the first time.…”

Section: Introductionmentioning

confidence: 99%

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TheHerschelLensing Survey (HLS): Overview

Egami¹,

Rex²,

Rawle³

et al. 2010

A&A

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The Herschel Lensing Survey (HLS) will conduct deep PACS and SPIRE imaging of ∼40 massive clusters of galaxies. The strong gravitational lensing power of these clusters will enable us to penetrate through the confusion noise, which sets the ultimate limit on our ability to probe the Universe with Herschel. Here we present an overview of our survey and a summary of the major results from our science demonstration phase (SDP) observations of the Bullet cluster (z = 0.297). The SDP data are rich and allow us to study not only the background high-redshift galaxies (e.g., strongly lensed and distorted galaxies at z = 2.8 and 3.2) but also the properties of cluster-member galaxies. Our preliminary analysis shows a great diversity of far-infrared/submillimeter spectral energy distributions (SEDs), indicating that we have much to learn with Herschel about the properties of galaxy SEDs. We have also detected the Sunyaev-Zel'dovich (SZ) effect increment with the SPIRE data. The success of this SDP program demonstrates the great potential of the Herschel Lensing Survey to produce exciting results in a variety of science areas.

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Section: Overview Of the Bullet Cluster Sdp Datasupporting

confidence: 94%

Section: Introductionmentioning

confidence: 99%

TheHerschelLensing Survey (HLS): Overview

Egami¹,

Rex²,

Rawle³

et al. 2010

A&A

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“…Rigby et al 2008;Farrah et al 2008). On the one hand, Engelbracht et al (2008) find that the differences between the SEDs of local and z ∼ 2 ULIRGs are qualitatively consistent with a difference in metallicity of a factor 1.5-2.…”

Section: Introductionmentioning

confidence: 82%

Integral field spectroscopy based Hαsizes of local luminous and ultraluminous infrared galaxies

Arribas

Colina

Alonso‐Herrero

et al. 2012

A&A

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Aims. We study the analogy between local luminous and ultraluminous infrared galaxies (U/LIRGs) and high-z massive star forming galaxies (SFGs) by comparing their basic Hα structural characteristics, such as size and luminosity surface density, in an homogeneous way (i.e. same tracer, size definition, and similar physical scales). Methods. We use integral field spectroscopy (IFS) based Hα emission maps for a representative sample of 54 local U/LIRGs (66 galaxies) observed with INTEGRAL/WHT and VIMOS/VLT. From this initial sample, we select 26 objects with similar Hα luminosities (L(Hα)) to those of massive (i.e. M ∼ 10 10 M or larger) SFGs at z ∼ 2, and observed on similar physical scales. We then directly compare the sizes, and luminosity (and SFR) surface densities of these local and high-z samples.Results. The size of the Hα emitting region in the local U/LIRGs that we study has a wide range of values, with r 1/2 (Hα) from 0.2 kpc to 7 kpc. However, about two-thirds of local U/LIRGs with L ir > 10 11.4 L have compact Hα emission (i.e. r 1/2 < 2 kpc). The comparison sample of local U/LIRGs also contains a larger fraction (59%) of objects with compact Hα emission than the high-z sample (25%). This gives further support to the idea that for this luminosity range the size of the star forming region is a distinctive factor when comparing local and distant galaxies of similar SFRs. However, when using Hα as a tracer for both local and high-z samples, the differences are smaller than those reported using a variety of other tracers. In the L(Hα) -L(Hα) surface density (Σ Hα ) plane, most of the local U/LIRGs and high-z SF galaxies follow the same trend (i.e. higher luminosity for higher surface density) and cover a similar range, except for about 20-40% of local U/LIRGs, which have a higher Σ Hα by a factor of about 10. This is considerably smaller than the factors of 1000 or more reported in similar planes (i.e. L(TIR) versus Σ TIR ). Despite of the higher fraction of galaxies with compact Hα emission, a sizable group (about one-third) of local U/LIRGs are large (i.e. r 1/2 > 2 kpc). These are systems that show evidence of pre-coalescence merger activity and are indistinguishable from the massive high-z SFGs galaxies in terms of their Hα sizes, and luminosity and SFR surface densities.

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“…They make use of observations of suppressed PAH emission in local LIRGs and ULIRGs (whereby heavy molecules are destroyed in the most dense star forming environments, e.g. Rigby et al, 2008;Díaz-Santos et al, 2010) to distinguish two modes of star formation where normal main sequence galaxies have IR8 values consistent with local LIRGs, whereby starbursts have elevated IR8 ratios, consistent with local ULIRGs. They find that ULIRGs at z ∼ 1−2 have IR8 ratios consistent with normal main sequence star forming galaxies and thus conclude that most Herschel-Pacs detected galaxies are not merger dominated.…”

Section: Mid-infrared Diagnosticsmentioning

confidence: 99%

“…The physical origins of DOGs mid-infrared emission could have been AGN-heating or bright PAH emission lines. Rigby et al (2008), Farrah et al (2008), Murphy (2009 and Takagi et al (2010) found the latter (note however that not all of these works explicitly use the DOG selection criterion, their samples overlap substantially). Indeed, the AGN fraction of DOGs (and similar z ∼ 2 BzKs) appears to be smaller than was originally anticipated ∼30% at S 24 < 1 mJy Alexander et al, 2011).…”

Section: Mid-infrared Spitzer-selected Populationsmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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Mid‐Infrared Spectroscopy of Lensed Galaxies at 1 <z< 3: The Nature of Sources Near the MIPS Confusion Limit

Cited by 92 publications

References 85 publications

TheHerschelLensing Survey (HLS): Overview

TheHerschelLensing Survey (HLS): Overview

Integral field spectroscopy based Hαsizes of local luminous and ultraluminous infrared galaxies

Dusty star-forming galaxies at high redshift

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