Understanding the Nature of Optically Faint Radio Sources and Their Connection to the Submillimeter Population

Chapman, Scott; Lewis, Geraint F.; Scott, Douglas; Borys, Colin; Richards, E. A.

doi:10.1086/339498

Cited by 52 publications

(75 citation statements)

References 45 publications

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“…If we propose that this local population of IR-luminous objects undergoes a strong luminosity evolution of the form ð1 þ zÞ 4 out to z ¼ 1:5, we can determine the relative numbers of cold and warm objects isolated by our selection function. This form of evolution has been shown to match the observe space density of high-z ULIRGs to the local population (see, e.g., Blain et al 1999;Chapman et al 2002a).…”

Section: Comparison With Higher Redshift Scuba Populationsmentioning

confidence: 73%

Optically Faint Counterparts to theInfrared Space ObservatoryFIRBACK 170 Micron Population: Discovery of Cold, Luminous Galaxies at High Redshift

Chapman

Smail

Ivison

et al. 2002

ApJ

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We present Keck spectroscopy and UKIRT near-IR imaging observations of two 170 lm-selected sources from the Infrared Space Observatory (ISO) FIRBACK survey that have faint counterparts in the optical and rÀK $ 5. Both sources were expected to lie at z > 1, based on their far-infrared, submillimeter, and radio fluxes, assuming a spectral energy distribution similar to that of the local ultraluminous infrared galaxy (ULIRG) Arp 220. However, our spectroscopy indicates that the redshifts of these galaxies are less than 1: z ¼ 0:91 for FIRBACK FN1-64, and z ¼ 0:45 for FIRBACK FN1-40. While the bolometric luminosities of both galaxies are similar to that of Arp 220, it appears that the dust emission in these systems has a characteristic temperature of $30 K, much cooler than the $50 K seen in Arp 220. Neither optical spectrum shows evidence of active galactic nucleus activity. If these galaxies are characteristic of the optically faint FIRBACK population, then evolutionary models of the far-infrared background must include a substantial population of cold, luminous galaxies. These galaxies provide an important intermediate comparison between the local luminous IR galaxies and the high-redshift, submillimeter-selected galaxies, for which there is very little information available.

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Section: Comparison With Higher Redshift Scuba Populationsmentioning

confidence: 73%

Optically Faint Counterparts to theInfrared Space ObservatoryFIRBACK 170 Micron Population: Discovery of Cold, Luminous Galaxies at High Redshift

Chapman

Smail

Ivison

et al. 2002

ApJ

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“…Figure 12 illustrates both 850-870µm number counts (from Scuba, Laboca, Scuba-2, and ALMA Blain et al, 1999;Scott et al, 2002;Chapman et al, 2002;Cowie et al, 2002;Borys et al, 2003;Webb et al, 2003;Barnard et al, 2004;Coppin et al, 2006;Scott et al, 2006;Knudsen et al, 2008;Beelen et al, 2008;Weiß et al, 2009a;Karim et al, 2013;Casey et al, 2013;Chen et al, 2013a) and 450-500µm (from Scuba, Herschel and Scuba-2 Smail et al, 2002;Oliver et al, 2010;Clements et al, 2010;Béthermin et al, 2012b;Geach et al, 2013;Casey et al, 2013;Chen et al, 2013a). Figure 13 illustrates other infrared and submillimeter number counts in the literature in direct units, from 70µm Béthermin et al, 2010a;Berta et al, 2011), 100µm (Héraudeau et al, 2004;Rodighiero & Franceschini, 2004;Kawara et al, 2004;Berta et al, 2011;Magnelli et al, 2013b), 160µm Kawara et al, 2004;Béthermin et al, 2010a;Berta et al, 2011;Magnelli et al, 2013b), 250µm and 350µm Chen+13 (850) Casey+13 (850 Figure 12: Differential submillimeter number counts at 850µm/870µm (left) and 450-500 µm (right).…”

Section: Number Countsmentioning

confidence: 99%

“…Figure 13 illustrates other infrared and submillimeter number counts in the literature in direct units, from 70µm Béthermin et al, 2010a;Berta et al, 2011), 100µm (Héraudeau et al, 2004;Rodighiero & Franceschini, 2004;Kawara et al, 2004;Berta et al, 2011;Magnelli et al, 2013b), 160µm Kawara et al, 2004;Béthermin et al, 2010a;Berta et al, 2011;Magnelli et al, 2013b), 250µm and 350µm Chen+13 (850) Casey+13 (850 Figure 12: Differential submillimeter number counts at 850µm/870µm (left) and 450-500 µm (right). The 850µm and 870µm number counts come the initial Scuba surveys Scott et al, 2002;Chapman et al, 2002;Cowie et al, 2002;Borys et al, 2003;Webb et al, 2003;Barnard et al, 2004;Coppin et al, 2006;Scott et al, 2006;Knudsen et al, 2008, , shown in brown, dark red, red, dark orange, orange, dark gold yellow, light green, green, dark teal, and teal respectively). Data from Beelen et al (2008), Weiß et al (2009a), and Karim et al (2013) are taken at 870µm rather than 850µm, the two former from Laboca and the latter from interferometric ALMA data.…”

Section: Number Countsmentioning

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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“…A galaxy thus selected from this model universe is then assigned a template spectral energy distribution from the catalog of Dale et al (2001) and Dale & Helou (2002), parameterized by the 60=100 m color and normalized to the FIR luminosity. This model scenario does not incorporate the intrinsic scatter in the FIR /radio correlation (0.2 dex), as was done in Chapman et al (2002;hereafter C02). Rather, this study concentrates on the properties of the intrinsic dust temperature distribution, which locally shows a larger scatter (0.3 dex) than the FIR /radio correlation and should be expected to dominate the high-redshift radio and submillimeter properties.…”

Section: Fittinggthe Multiwavv Elengg Th Counts and Backgg Roundsmentioning

confidence: 99%

Modeling the Evolution of Infrared Luminous Galaxies: The Influence of the Luminosity‐Temperature Distribution

Lewis

Chapman

Hélou

2005

ApJ

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The evolution of the luminous infrared galaxy population is explored using a pure luminosity evolution model that incorporates the locally observed luminosity-temperature distribution for IRAS galaxies. Pure luminosity evolution models in a fixed ÃCDM cosmology are fitted to submillimeter and infrared counts and backgrounds. We find that the differences between the locally determined bivariate model and the single-variable luminosity function ( LF) do not manifest themselves in the observed counts but rather are primarily apparent in the dust temperatures of sources in flux-limited surveys. Statistically significant differences in the redshift distributions are also observed. The bivariate model is used to predict the counts, redshifts, and temperature distributions of galaxies detectable by the Spitzer Space Telescope. The best-fitting model is compared to the high-redshift submillimeter galaxy population, revealing a median redshift for the total submillimeter population of z ¼ 1:8 þ0:9 À0:4 , in good agreement with recent spectroscopic studies of submillimeter galaxies. The temperature distribution for the submillimeter galaxies is modeled to predict the radio/submillimeter indices of the submillimeter galaxies, revealing that submillimeter galaxies exhibit a broader spread in spectral energy distributions than seen in the local IRAS galaxies.

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Understanding the Nature of Optically Faint Radio Sources and Their Connection to the Submillimeter Population

Cited by 52 publications

References 45 publications

Optically Faint Counterparts to theInfrared Space ObservatoryFIRBACK 170 Micron Population: Discovery of Cold, Luminous Galaxies at High Redshift

Optically Faint Counterparts to theInfrared Space ObservatoryFIRBACK 170 Micron Population: Discovery of Cold, Luminous Galaxies at High Redshift

Dusty star-forming galaxies at high redshift

Modeling the Evolution of Infrared Luminous Galaxies: The Influence of the Luminosity‐Temperature Distribution

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