Astrophys. J., Suppl. Ser., 200, 10 (2012/May-0)
Quest for COSMOS submillimeter galaxy counterparts using CARMA and VLA: identifying three high-redshift starburst galaxies.
SMOLCIC V., NAVARRETE F., ARAVENA M., ILBERT O., YUN M.S., SHETH K., SALVATO M., McCRACKEN H.J., DIENER C., ARETXAGA I., RIECHERS D.A., FINOGUENOV A., BERTOLDI F., CAPAK P., HUGHES D., KARIM A., SCHINNERER E., SCOVILLE N.Z. and WILSON G.
Abstract (from CDS):
We report on interferometric observations at 1.3 mm at 2''-3'' resolution using the Combined Array for Research in Millimeter-wave Astronomy. We identify multi-wavelength counterparts of three submillimeter galaxies (SMGs; F_1 mm_> 5.5 mJy) in the COSMOS field, initially detected with MAMBO and AzTEC bolometers at low, ∼10''-30'', resolution. All three sources–AzTEC/C1, Cosbo-3, and Cosbo-8–are identified to coincide with positions of 20 cm radio sources. Cosbo-3, however, is not associated with the most likely radio counterpart, closest to the MAMBO source position, but with that farther away from it. This illustrates the need for intermediate-resolution (∼2'') mm-observations to identify the correct counterparts of single-dish-detected SMGs. All of our three sources become prominent only at NIR wavelengths, and their mm-to-radio flux based redshifts suggest that they lie at redshifts z ≳ 2. As a proof of concept, we show that photometric redshifts can be well determined for SMGs, and we find photometric redshifts of 5.6±1.2, 1.9+0.9_- 0.5_, and ∼4 for AzTEC/C1, Cosbo-3, and Cosbo-8, respectively. Using these we infer that these galaxies have radio-based star formation rates of ≳ 1000 M ☉/yr and IR luminosities of ∼1013 L☉ consistent with properties of high-redshift SMGs. In summary, our sources reflect a variety of SMG properties in terms of redshift and clustering, consistent with the framework that SMGs are progenitors of z ∼ 2 and today's passive galaxies.
galaxies: active - galaxies: distances and redshifts - galaxies: high-redshift - galaxies: starburst - submillimeter: galaxies
Paragr. 3.2.2 : IRAS 22491 may be IRAS 22491-1808
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