Infrared galaxies in the IRAS minisurvey

Soifer, B. T.; Rowan-Robinson, M.; Houck, J. R.; Jong, T. de; Neugebauer, G.; Aumann, Hartmut H.; Beichman, Charles; Boggess, N. W.; Clegg, P. E.; Emerson, J. P.; Gillett, F. C.; Habing, H. J.; Hauser, M. G.; Low, F. J.; Miley, G. K.; Young, E. T.

doi:10.1086/184226

Cited by 189 publications

(138 citation statements)

References 3 publications

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“…The majority of local IRAS-selected and ISO-selected galaxies were infrared galaxies with infrared luminosities within 10 11 < L IR < 10 12 L , though a small subset (∼12 galaxies) were ultraluminous infrared galaxies, or ULIRGs, with 10 12 < L IR < 10 13 L . Careful analysis of these galaxies, from studying their morphological structure in the optical, near-infrared, molecular gas and dust emission, indicated that the majority of systems above ∼10 11.5 L −or above star formation rates ∼50 M yr −1 −were major mergers of two or more equalmass galaxies Soifer et al 1984;Lonsdale et al 1984;Joseph & Wright 1985;Veilleux et al 2002, for a review, see Sanders & Mirabel, 1996).…”

Section: Local Infrared-luminous Galaxiesmentioning

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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Section: Local Infrared-luminous Galaxiesmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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“…The importance of gas dynamics and triggered star formation in mergers is reinforced by observations of ultraluminous infrared galaxies (ULIRGs; e.g., Soifer et al 1984aSoifer et al , 1984b, which are invariably associated with mergers in the local universe (Joseph & Wright 1985;Sanders & Mirabel 1996). The infrared emission from ULIRGs is thought to be powered by intense starbursts in their nuclei, originating in central concentrations of gas (e.g., Scoville et al 1986;Sargent et al 1987Sargent et al , 1989, which will leave dense stellar remnants ( Kormendy & Sanders 1992;Hibbard & Yun 1999;Rothberg & Joseph 2004), as predicted theoretically (Mihos & Hernquist 1994c).…”

Section: Introductionmentioning

confidence: 99%

Dissipation and the Fundamental Plane: Observational Tests

Hopkins

Cox

Hernquist

2008

Astrophysical Journal

128

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We develop observational tests of the idea that dissipation in gas-rich mergers produces the fundamental plane (FP) and related correlations obeyed by ellipticals. The FP ''tilt'' implies that lower mass ellipticals have a higher ratio of stellar to dark matter within their stellar effective radii. Models argue that mergers between more gas-rich (typically lower mass) disks yield larger mass fractions formed in compact starbursts, giving a smaller stellar R e and higher M Ã /M tot within that R e . Such starbursts leave a characteristic imprint in the surface brightness profile: a central excess above an outer profile established by the dissipationless violent relaxation of disk stars. In previous work, we developed empirical methods to decompose the observed profiles of ellipticals and robustly estimate the amount of dissipation in the original spheroid-forming merger(s). Applying this to a large sample of observed ellipticals, we test whether or not their location on the FP and its tilt are driven by dissipation. At fixed mass, ellipticals formed in more dissipational events are smaller and have higher M Ã /M tot . At fixed degree of dissipation, there is no tilt in the FP. We show that the dynamical mass estimator R e 2 /G is a good estimator of the true mass: the observed FP tilt cannot primarily owe to other forms of nonhomology. Removing the effects of dissipation, observed ellipticals obey the same FP correlations as disks: unusual progenitors are not required to make typical ellipticals. Dissipation appears to be both necessary and sufficient to explain the FP tilt.

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“…The significance of galaxies with an infrared excess was highlighted early by Low & Kleinmann (1968) and Rieke & Low (1972), and lately recognized by observations of the IRAS satellite (Soifer et al 1984). Among the sources that emit the bulk of their energy in the infrared, the Ultra-Luminous Infrared Galaxies (ULIRGs, 10 12 L ≤ L bol ∼ L IR [8-1000 μm] ≤ 10 13 L ), are amongst the brightest objects in the local Universe (see reviews in Lonsdale et al 2006;Sanders & Mirabel 1996).…”

Section: Introductionmentioning

confidence: 99%

Integral field optical spectroscopy of a representative sample of ULIRGs

García-Marín

Colina²,

Arribas³

2009

A&A

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Context. Ultraluminous infrared galaxies are merging systems characterized for containing large amounts of dust and emitting the bulk of their energy in the infrared. Dust affects several of the observed properties derived from optical and near-IR rest-frame data, such as the stellar morphology and the ionized gas distribution. Systematic analysis of the dust distribution in representative samples of ULIRGs are needed to investigate its two-dimensional structure, and to establish its impact in the derivation of fundamental properties such as star formation rates, effective radii, and dynamical masses. Aims. We investigate the two-dimensional kpc-scale structure of the extinction in a representative sample of local ULIRGs using the Hα/Hβ line ratio. Methods. We use optical integral field spectroscopy obtained with the INTEGRAL instrument at the William Herschel Telescope. Complementary optical and near-IR high angular resolution HST images have also been used. Compared to classical optical long-slit analysis, our data provides information about the entire system, and not only in pre-selected orientations. Results. The extinction exhibits a very complex and patchy structure in ULIRGs on kpc scales, from basically transparent regions to others deeply embedded in dust (A V 0.0 to A V 8.0 mag). Nuclear extinction covers a broad range in A V from 0.4 to 7.7 mag , 69% of the nuclei having A V ≥ 2.0 mag. Extinction in the external regions is substantially lower than in the nuclei with 60% of the ULIRGs in the sample having median A V of less than 2 mag for the entire galaxy. While post-coalescence nuclei tend to cluster around A V values of 2 to 3 mag, pre-coalescence nuclei appear more homogeneously distributed over the entire 0.4 mag ≤A V ≤ 7.7 mag range. For the average extinction (A V 2.0) derived for the ULIRGs of the sample, the ratio of the de-reddened to observed SFR values is 6. The extinction-corrected, Hα-based SFR ranges from 10 to 300 M yr −1 . For only 27% of the cases the de-reddened SFR is <20 M yr −1 , whereas for the observed SFR this percentage increases to 87%. The IR-based SFR is always higher than the opticalbased one, with differences ranging from about 2 to up to 30. The nuclear observed SFR has an average contribution to the total one of 16% for the entire sample. Once corrected for extinction, the average value becomes 31%. Because of mostly extinction effects, the optical (I-band) half-light radius in the sample galaxies is on average a factor 2.3 larger than the corresponding near-IR (H-band) value.

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Infrared galaxies in the IRAS minisurvey

Cited by 189 publications

References 3 publications

Dusty star-forming galaxies at high redshift

Dusty star-forming galaxies at high redshift

Dissipation and the Fundamental Plane: Observational Tests

Integral field optical spectroscopy of a representative sample of ULIRGs

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