The SCUBA HAlf Degree Extragalactic Survey (SHADES) – VII. Optical/IR photometry and stellar masses of submillimetre galaxies

Dye, S.; Eales, Stephen Anthony; Aretxaga, I.; Serjeant, S.; Dunlop, James; Babbedge, T.; Chapman, Scott; Cirasuolo, M.; Clements, D. L.; Coppin, K. E. K.; Dunne, L.; Egami, Eiichi; Farrah, D.; Ivison, R. J.; Kampen, E. van; Pope, Alexandra; Priddey, R.; Rieke, G. H.; Schael, A. M.; Scott, D.; Simpson, Chris; Takagi, Toshinobu; Takata, Tadafumi; Vaccari, M.

doi:10.1111/j.1365-2966.2008.13113.x

Cited by 89 publications

(130 citation statements)

References 64 publications

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“…In order to build up the stellar mass of one SMG, five such galaxies would need to form stars continuously at a rate of 20 M yr −1 , a value more likely to be sustainable over several Gyr. The latter scenario is consistent with the results of Dye et al (2008) based on observed optical to mid-IR data of 51 SMGs with photometric redshifts. They found that approximately half the stellar mass in SMGs has been formed over a long (∼1-2 Gyr) period of approximately constant star formation activity.…”

Section: Star Formation Ratessupporting

confidence: 81%

“…Due to the coarse resolution of SCUBA, localizations derived from high-resolution radio maps had to be used to measure their spectroscopic redshifts . Lots of studies have addressed the issue of characterizing the nature of SMGs (Egami et al 2004;Greve et al 2004Greve et al , 2005Smail et al 2004;Swinbank et al 2004Swinbank et al , 2006Swinbank et al , 2008Takagi et al 2004;Alexander et al 2005;Borys et al 2005;Kovács et al 2006;Laurent et al 2006;Pope et al 2006;Tacconi et al 2006Tacconi et al , 2008Takata et al 2006;Younger et al 2007Younger et al , 2008Younger et al , 2009aClements et al 2008;Coppin et al 2008;Dye et al 2008Dye et al , 2009Hainline et al 2009;Perera et al 2008;Scott et al 2008;Austermann et al 2009;Devlin et al 2009;Eales et al 2009;Murphy et al 2009;Murphy 2009;Tamura et al 2009;Weiß et al 2009b;Aravena et al 2010, some of these works were based on surveys with sensitivity worse than 3 mJy quoted above). However they were usually based on limited samples ( 20 sources), limited wavelength coverage or photometric redshifts.…”

Section: Introductionmentioning

confidence: 99%

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Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly

Michalowski

Hjorth

Watson

2010

A&A

235

278

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The nature of galaxies selected at submillimeter wavelengths (SMGs, S 850 3 mJy), some of the bolometrically most luminous objects at high redshifts, is still elusive. In particular their star formation histories and source of emission are not accurately constrained. In this paper we introduce a new approach to analyse the SMG data. Namely, we present the first self-consistent UV-to-radio spectral energy distribution fits of 76 SMGs with spectroscopic redshifts using all photometric datapoints from ultraviolet to radio simultaneously. We find that they are highly star-forming (median star formation rate 713 M yr −1 for SMGs at z > 0.5), moderately dust-obscured (median A V ∼ 2 mag), hosting significant stellar populations (median stellar mass 3.7 × 10 11 M ) of which only a minor part has been formed in the ongoing starburst episode. This implies that in the past, SMGs experienced either another starburst episode or merger with several galaxies. The properties of SMGs suggest that they are progenitors of present-day elliptical galaxies. We find that these bright SMGs contribute significantly to the cosmic star formation rate density (∼20%) and stellar mass density (∼30-50%) at redshifts 2-4. Using number counts at low fluxes we find that as much as 80% of the cosmic star formation at these redshifts took place in SMGs brighter than 0.1 mJy. We find evidence that a linear infrared-radio correlation holds for SMGs in an unchanged form up to redshift of 3.6, though its normalization is offset from the local relation by a factor of ∼2.1 towards higher radio luminosities. We present a compilation of photometry data of SMGs and determinations of cosmic SFR and stellar mass densities.

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Section: Star Formation Ratessupporting

confidence: 81%

Section: Introductionmentioning

confidence: 99%

Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly

Michalowski

Hjorth

Watson

2010

A&A

235

278

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“…This has primarily been done with Spitzer MIPS 24µm maps, as they cover large areas of sky to sufficient depths (e.g. Pope et al, 2006;Dye et al, 2008). While mid-infrared emission does roughly correlate with far-infrared emission, a few aspects of mid-infrared emission complicate the relation.…”

Section: Radio Counterpartsmentioning

confidence: 99%

“…Because this study was aimed at investigating X-ray detected SMGs (to compare stellar masses to black hole masses), contamination of the stellar masses by AGN is a potential issue, particularly because rest-frame K-band luminosities were used in the derivation. Dye et al (2008) determine the stellar masses for galaxies in the SHADES survey with only 8 bands of photometry utilizing the synthetic spectra of Bruzual & Charlot (2003); while they find comparable stellar masses to the work of Borys et al (2005), the margin of uncertainty from lack of observational constraints dominate.…”

Section: Stellar Massesmentioning

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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“…They represent a major phase of star formation at early epochs and are also characterized by high stellar masses (e.g., Borys et al 2005). They are thus ideal candidates to be the precursors of local massive elliptical galaxies (e.g., Blain et al 2002;Dye et al 2008;Lonsdale et al 2009, hereafter Lo09, and references therein). Nearly all of the enormous UV energy produced by their massive young stars is absorbed by interstellar dust and re-emitted at far-infrared wavelengths, with their far-infrared luminosity (L FIR ) able to reach 10 13 L .…”

Section: Introductionmentioning

confidence: 99%

Multi-wavelength properties ofSpitzerselected starbursts atz ~ 2

Fiolet

Omont

Polletta

et al. 2009

A&A

Self Cite

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Context. Wide-field Spitzer surveys allow identification of thousands of potentially high-z submillimeter galaxies (SMGs) through their bright 24 μm emission and their mid-IR colors. Aims. We want to determine the average properties of such z ∼ 2 Spitzer-selected SMGs by combining millimeter, radio, and infrared photometry for a representative IR-flux (λ rest ∼ 8 μm) limited sample of SMG candidates. Methods. A complete sample of 33 sources believed to be starbursts ("5.8 μm-peakers") was selected in the (0.5 deg 2 ) J1046+56 field with selection criteria F 24 μm > 400 μJy, the presence of a redshifted stellar emission peak at 5.8 μm, and r Vega > 23. The field, part of the SWIRE Lockman Hole field, benefits from very deep VLA/GMRT 20 cm, 50 cm, and 90 cm radio data (all 33 sources are detected at 50 cm), and deep 160 μm and 70 μm Spitzer data. The 33 sources, with photometric redshifts ∼1.5−2.5, were observed at 1.2 mm with IRAM-30m/MAMBO to an rms ∼0.7-0.8 mJy in most cases. Their millimeter, radio, 7-band Spitzer, and near-IR properties were jointly analyzed.Results. The entire sample of 33 sources has an average 1.2 mm flux density of 1.56 ± 0.22 mJy and a median of 1.61 mJy, so the majority of the sources can be considered SMGs. Four sources have confirmed 4σ detections, and nine were tentatively detected at the 3σ level. Because of its 24 μm selection, our sample shows systematically lower F 1.2 mm /F 24 μm flux ratios than classical SMGs, probably because of enhanced PAH emission. A median FIR SED was built by stacking images at the positions of 21 sources in the region of deepest Spitzer coverage. Its parameters are T dust = 37 ± 8 K, L FIR = 2.5 × 10 12 L , and SFR = 450 M yr −1 . The FIR-radio correlation provides another estimate of L FIR for each source, with an average value of 4.1 × 10 12 L ; however, this value may be overestimated because of some AGN contribution. Most of our targets are also luminous star-forming BzK galaxies which constitute a significant fraction of weak SMGs at 1.7 z 2.3. Conclusions. Spitzer 24 μm-selected starbursts and AGN-dominated ULIRGs can be reliably distinguished using IRAC-24 μm SEDs. Such "5.8 μm-peakers" with F 24 μm > 400 μJy have L FIR 10 12 L . They are thus z ∼ 2 ULIRGs, and the majority may be considered SMGs. However, they have systematically lower 1.2 mm/24 μm flux density ratios than classical SMGs, warmer dust, comparable or lower IR/mm luminosities, and higher stellar masses. About 2000−3000 "5.8 μm-peakers" may be easily identifiable within SWIRE catalogues over 49 deg 2 .

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The SCUBA HAlf Degree Extragalactic Survey (SHADES) – VII. Optical/IR photometry and stellar masses of submillimetre galaxies

Cited by 89 publications

References 64 publications

Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly

Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly

Dusty star-forming galaxies at high redshift

Multi-wavelength properties ofSpitzerselected starbursts atz ~ 2

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