SHARC-2 350 μm Observations of Distant Submillimeter-selected Galaxies

By A. Kovács, S. Chapman, C. Dowell, A. Blain, R. Ivison, I. Smail, T. Phillips. Astrophysical Journal, 2006

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We present 350 μm observations of 15 Chapman et al. submillimeter galaxies (SMGs) with radio counterparts and optical redshifts. We detect 12 and obtain sensitive upper limits for three, providing direct, precise measurements of their far-infrared luminosities and characteristic dust temperatures. With these, we verify the linear radio-far-infrared correlation at redshifts of z ~ 1-3 and luminosities of 1011-1013 L☉, with a power-law index of 1.02 ± 0.12 and rms scatter of 0.12 dex. However, either the correlation constant q or the dust emissivity index β is lower than measured locally. The best-fitting q ≃ 2.14 is consistent with SMGs being predominantly starbust galaxies, without significant AGN contribution, at far-infrared wavelengths. Gas-to-dust mass ratios are estimated at 54 , depending on the absoption efficiency κν, with intrinsic dispersion ≃40% around the mean value. Dust temperatures consistent with 34.6 ± 3 K (1.5/β)0.71, at z ~ 1.5-3.5, suggest that far-infrared photometric redshifts may be viable, and perhaps accurate to 10% ≲ dz/(1 + z), for up to 80% of the SMG population in this range, if the above temperature characterizes the full range of SMGs. However, observed temperature evolution of Td ∝ (1 + z) is also plausible and could result from selection effects. From the observed luminosity-temperature (L-T) relation, L ∝ T, we derive scaling relations for dust mass versus dust temperature, and we identify expressions to interrelate the observed quantities. These suggest that measurements at a single wavelength, in the far-infrared, submillimeter, or radio wave bands, might constrain dust temperatures and far-infrared luminosities for most SMGs with redshifts at z ~ 0.5-4.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

• Scuba-2: On-sky calibration using submillimetre standard sources (2013, methodology): “SHARC-II, the 350µm bolometer camera at Caltech Submillimeter Observatory, reports a calibration uncertainty of 15 per cent (Kovács et al. 2006), and as it shares the same site as SCUBA-2 it provides a point of comparison for the SCUBA-2 450µm accuracy, as the 350µm and 450µm atmospheric windows…”
• Energetic galaxy-wide outflows in high-redshift ultraluminous infrared galaxies hosting AGN activity (2012, background): “For the source RG J0302+0010 we estimated the infrared luminosity uing the radio-infrared relationship for star-forming galaxies (e.g., Helou et al. 1985) withq= 2.1, which is a typical value for highredshift ULIRGs (Kovács et al. 2006).”
• VERY HIGH GAS FRACTIONS AND EXTENDED GAS RESERVOIRS IN z = 1.5 DISK GALAXIES (2009, methodology): “…not to adopt the IR luminosities for SMGs estimated by Greve et al. (2005) but use a lower conversion factor between 850µm flux and IR luminosity to account for the evidence that their SEDs are colder than previously thought (e.g., Pope et al. 2006; 2008; Kovacs et al. 2006; Daddi et al. 2009).”
• Submillimetre galaxies in a hierarchical universe: number counts, redshift distribution, and implications for the IMF (2012, background): “…address: Space Exploration Technologies, 1 Rocket Road, Hawthorne, CA 90250, USA. and star formation rates (SFRs) of the order of ∼102–103 M yr−1 (e.g. Kovács et al. 2006; Coppin et al. 2008; Chapman et al. 2010; Magnelli et al. 2010, 2012; Michałowski, Hjorth & Watson 2010; Michałowski et al.…”
• Testing the evolutionary link between submillimetre galaxies and quasars: CO observations of QSOs at z∼ 2 (2008, background): “These systems have ULIRG-like bolometric luminosities, LIR ≥ 10 12 L⊙ (Kovács et al. 2006; Coppin et al. 2008), and they have many of the properties expected for gas-rich mergers (Swinbank et al. 2004, 2006; Tacconi et al. 2006).”
• THE SCUBA-2 COSMOLOGY LEGACY SURVEY: ALMA RESOLVES THE REST-FRAME FAR-INFRARED EMISSION OF SUB-MILLIMETER GALAXIES (2014, methodology): “We adopt a dust–to–gas ratio of fdg = 1/90 (Magnelli et al. 2012; Swinbank et al. 2014), but note that fdg = 1/50 has also been suggested for star-forming galaxies (Kovács et al. 2006).”
• The Herschel census of infrared SEDs through cosmic time (2013, background): “Moreover, the exploitation of long-wavelength data from ISO (Rowan-Robinson et al. 2005) and Spitzer (Symeonidis et al. 2008) enabled the discovery of IR-luminous galaxies at z < 1, with a spectrum of properties which overlapped with both the local population and the SCUBA-detected, z > 2, sources, ”
• Mid-Infrared Spectral Diagnosis of Submillimeter Galaxies (2007, background): “This is consistent with previous estimates of dust temperatures in SMGs (Chapman et al. 2005; Kovács et al. 2006; Pope et al. 2006).”
• MID-INFRARED SPECTROSCOPY OF SUBMILLIMETER GALAXIES: EXTENDED STAR FORMATION IN MASSIVE HIGH-REDSHIFT GALAXIES (2009, methodology): “To assess the contribution of the AGN to the energetics of the SMGs we first estimate the far-IR luminosities of the SMGs using the observed radio–far-IR correlation for SMGs (Kovács et al. 2006), yielding an average far-IR luminosity of Lfar−IR ∼ 5 × 10 45 erg s−1.”
• Deep multi-frequency radio imaging in the Lockman Hole using the GMRT and VLA (2009, background): “Kovács et al. (2006) employed 350-µm observations of 15 radio-detected SMGs with known redshifts to constrain their characteristic temperatures.”
• An ALMA survey of sub-millimetre Galaxies in the Extended Chandra Deep Field South: the far-infrared properties of SMGs (2013, background): “…/mid-infrared detected subset of the population gave a median redshift of z ∼ 2.5 (Chapman et al. 2005), confirming their ULIRG-like luminosities (Kovács et al. 2006; Coppin et al. 2008a; Magnelli et al. 2012a) and demonstrated that ULIRGs undergo a 1000-fold increase in space density from…”
• A Herschel view of the far-infrared properties of submillimetre galaxies (2012, methodology): “Using 350µm SHARC-2 observations, Kovács et al. (2006, 2010) provided more robust estimates of the infrared luminosity of a handful of SMGs.”
• Characterization of Scuba-2 450 μm and 850 μm selected galaxies in the COSMOS field (2013, background): “The combination of a greybody and mid-infrared powerlaw accounts for both galaxy-wide cold dust emission and smaller-scale warm dust emission (Blain et al. 2003; Kovács et al. 2006).”
• WHAT DOES A SUBMILLIMETER GALAXY SELECTION ACTUALLY SELECT? THE DEPENDENCE OF SUBMILLIMETER FLUX DENSITY ON STAR FORMATION RATE AND DUST MASS (2010, background): “…Hughes et al. 1998; Eales et al. 1999; see Blain et al. 2002 for a review) are extremely luminous (bolometric luminosity Lbol ∼ 1012–1013 L ; e.g., Kovács et al. 2006), high-redshift (Chapman et al. 2005) galaxies powered primarily by star formation rather than active galactic nuclei (AGNs;…”
• THE STELLAR MASS CONTENT OF SUBMILLIMETER-SELECTED GALAXIES (2010, background): “The far-IR luminosities (> 1012L⊙; e.g., Chapman et al. 2005; Kovács et al. 2006; Magnelli et al. 2010; Chapman et al. 2010) of these dusty, gas-rich galaxies (e.g., Frayer et al. 1998; Greve et al. 2005) imply star formation rates in excess of 103 M⊙ yr−1, sufficient to form the stellar mass of…”
• EXTRAGALACTIC MILLIMETER-WAVE SOURCES IN SOUTH POLE TELESCOPE SURVEY DATA: SOURCE COUNTS, CATALOG, AND STATISTICS FOR AN 87 SQUARE-DEGREE FIELD (2009, background): “…they have dynamical masses of ∼1011 M and total far-infrared luminosities of ∼1013 L (Swinbank et al. 2004; Greve et al. 2005; Chapman et al. 2005; Kovács et al. 2006; Pope et al. 2006); (2) they are forming stars prodigiously at ∼1000 M yr−1 (Chapman et al. 2005; Tacconi et al. 2006); (3)…”
• An ALMA survey of submillimetre galaxies in the Extended Chandra Deep Field South: high-resolution 870 μm source counts (2012, background): “…of studies (e.g., Ibar et al. 2008; Sargent et al. 2010; Ivison et al. 2010; Bourne et al. 2011) have attempted to trace the evolution of this relation over a range of redshifts, of which several focussed on submillimetre-bright sources (e.g., Kovács et al. 2006; Murphy et al. 2009; Murphy 2009).”
• MOLECULAR GAS IN z ∼ 6 QUASAR HOST GALAXIES (2010, methodology): “Data reduction was performed with the CRUSH data reduction package version 1.63 (Kovács et al. 2006a) and the rms noise values in the final maps are < 5 mJy beam−1 for all targets.”
• DETERMINING STAR FORMATION RATES FOR INFRARED GALAXIES (2008, methodology): “In addition, the figure shows the 1.4GHz and submm measurements of luminous infrared galaxies at z ∼ 2 by Kovács et al. (2006) (including only cases with z ≥ 1.4 and excluding numbers 2, 3, 9, and 10 in their Table 1, since three of them appear to be significantly contaminated by AGN and one was…”