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THE REDSHIFT and NATURE of Aztec/COSMOS 1

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THE REDSHIFT and NATURE of Aztec/COSMOS 1 University of Massachusetts Amherst ScholarWorks@UMass Amherst Astronomy Department Faculty Publication Series Astronomy 2011 THE REDSHIFT AND NATURE OF AzTEC/ COSMOS 1: A STARBURST GALAXY AT z = 4.6* V Smolcic P Capak O Ilbert AW Blain M Salvato See next page for additional authors Follow this and additional works at: https://scholarworks.umass.edu/astro_faculty_pubs Part of the Astrophysics and Astronomy Commons Recommended Citation Smolcic, V; Capak, P; Ilbert, O; Blain, AW; Salvato, M; Aretxaga, I; Schinnerer, E; Masters, D; Moric, I; Riechers, DA; Sheth, K; Aravena, M; Aussel, H; Aguirre, J; Berta, S; Carilli, CL; Civano, F; Fazio, G; Huang, J; Hughes, D; Kartaltepe, J; Koekemoer, AM; Kneib, J-P; LeFloc'h, E; Lutz, D; McCracken, H; Mobasher, B; Murphy, E; Pozzi, F; Riguccini, L; Sanders, DB; Sargent, M; Scott, KS; Scoville, NZ; Taniguchi, Y; Thompson, D; Willot, C; Wilson, G; and Yun, Min, "THE REDSHIFT AND NATURE OF AzTEC/ COSMOS 1: A STARBURST GALAXY AT z = 4.6*" (2011). The Astrophysical Journal Letters. 1114. 10.1088/2041-8205/731/2/L27 This Article is brought to you for free and open access by the Astronomy at ScholarWorks@UMass Amherst. It has been accepted for inclusion in Astronomy Department Faculty Publication Series by an authorized administrator of ScholarWorks@UMass Amherst. For more information, please contact [email protected]. Authors V Smolcic, P Capak, O Ilbert, AW Blain, M Salvato, I Aretxaga, E Schinnerer, D Masters, I Moric, DA Riechers, K Sheth, M Aravena, H Aussel, J Aguirre, S Berta, CL Carilli, F Civano, G Fazio, J Huang, D Hughes, J Kartaltepe, AM Koekemoer, J-P Kneib, E LeFloc'h, D Lutz, H McCracken, B Mobasher, E Murphy, F Pozzi, L Riguccini, DB Sanders, M Sargent, KS Scott, NZ Scoville, Y Taniguchi, D Thompson, C Willot, G Wilson, and Min Yun This article is available at ScholarWorks@UMass Amherst: https://scholarworks.umass.edu/astro_faculty_pubs/1114 A Preprint typeset using LTEX style emulateapj v. 11/10/09 THE REDSHIFT AND NATURE OF AZTEC/COSMOS 1: A STARBURST GALAXY AT Z =4.6 V. Smolciˇ c´1,2, P. Capak3,4, O. Ilbert5, A.W. Blain3, M. Salvato3,9, I. Aretxaga14, E. Schinnerer23, D. Masters3,6, I. Moric´3,7, D. A. Riechers3,8, K. Sheth4, M. Aravena10, H. Aussel11, J. Aguirre12,13, S. Berta15, C. L. Carilli16, F. Civano17, G. Fazio17, J. Huang17, D. Hughes14, J. Kartaltepe18, A. M. Koekemoer19, J.-P. Kneib5, E. LeFloc’h18,20, D. Lutz15, H. McCracken5, B. Mobasher 6, E. Murphy4, F. Pozzi21, L. Riguccini22, D. B. Sanders18, M. Sargent23, K. S. Scott24, N.Z. Scoville3, Y. Taniguchi25, D. Thompson26, C. Willott27, G. Wilson28, M. Yun28 ABSTRACT Based on broad/narrow-band photometry and Keck DEIMOS spectroscopy we report a redshift of +0.06 z = 4.64−0.08 for AzTEC/COSMOS 1, the brightest sub-mm galaxy in the AzTEC/COSMOS field. In addition to the COSMOS-survey X-ray to radio data, we report observations of the source with Herschel/PACS (100, 160 µm), CSO/SHARC II (350 µm), CARMA and PdBI (3 mm). We do not detect CO(5 → 4) line emission in the covered redshift ranges, 4.56-4.76 (PdBI/CARMA) and 4.94- 5.02 (CARMA). If the line is within this bandwidth, this sets 3σ upper limits on the gas mass to 9 10 . 8 × 10 M⊙ and . 5 × 10 M⊙, respectively (assuming similar conditions as observed in z ∼ 2 SMGs). This could be explained by a low CO-excitation in the source. Our analysis of the UV-IR spectral energy distribution of AzTEC 1 shows that it is an extremely young (. 50 Myr), massive 11 −1 (M∗ ∼ 10 M⊙), but compact (. 2 kpc) galaxy forming stars at a rate of ∼ 1300 M⊙ yr . Our results imply that AzTEC 1 is forming stars in a ’gravitationally bound’ regime in which gravity prohibits the formation of a superwind, leading to matter accumulation within the galaxy and further generations of star formation. Subject headings: galaxies: distances and redshifts – galaxies: high-redshift – galaxies: active – galax- ies: starburst – galaxies: fundamental parameters 1 ESO ALMA COFUND Fellow, European Southern Ob- servatory, Karl-Schwarzschild-Strasse 2, 85748 Garching b. Muenchen, Germany 2 Argelander Institut for Astronomy, Auf dem H¨ugel 71, Bonn, 53121, Germany 3 California Institute of Technology, MC 249-17, 1200 East California Boulevard, Pasadena, CA 91125 4 Spitzer Science Center, 314-6 Caltech, 1201 E. California Blvd. Pasadena, CA, 91125 5 Laboratoire d’Astrophysique de Marseille, Universit´e de Provence, CNRS, BP 8, Traverse du Siphon, 13376 Marseille Cedex 12, France 6 Department of Physics and Astronomy, University of Cali- fornia, Riverside, CA, 92521, USA 7 University of Zagreb, Physics Department, Bijeniˇcka cesta 32, 10000 Zagreb, Croatia 8 Hubble Fellow 33, 00040 Monte Porzio Catone, Italy 9 Max-Planck-Institut fr Plasmaphysik, Boltzmanstrasse 2, 22 Laboratoire AIM-Paris-Saclay, CEA/DSM/Irfu CNRS Garching 85748, Germany Universite Paris Diderot, CE-Saclay, pt courrier 131, F-91191 10 National Radio Astronomy Observatory, 520 Edgemont Gif-sur-Yvette, France arXiv:1102.4329v1 [astro-ph.CO] 21 Feb 2011 Road, Charlottesville, VA 22903, USA 23 Max Planck Institut f¨ur Astronomie, K¨onigstuhl 17, Hei- 11 UMR AIM (CEA-UP7-CNRS), CEA-Saclay, Orme des delberg, D-69117, Germany Merisiers, bt. 709, F-91191 Gif-sur-Yvette Cedex, France 24 Department of Physics and Astronomy, University of Penn- 12 Jansky Fellow, National Radio Astronomy Observatory sylvania,Philadelphia PA, 19104 13 University of Pennsylvania, Department of Physics and As- 25 Research Center for Space and Cosmic Evolution, Ehime tronomy, 209 South 33rd Street, Philadelphia, PA 19104 University, Bunkyo-cho 2-5, Matsuyama 790-8577, Japan 14 Instituto Nacional de Astrof´ısica, Optica´ y Electr´onica 26 Large Binocular Telescope Observatory, University of Ari- (INAOE), Aptdo. Postal 51 y 216, 72000 Puebla, Pue., Mex- zona, 933 N. Cherry Ave., Tucson, AZ, 85721, USA 27 ico Herzberg Institute of Astrophysics, National Research 15 Max-Planck-Institut f¨ur extraterrestrische Physik, Postfach Council, 5071 West Saanich Rd., Victoria, BC V9E 2E7, Canada 28 1312, 85741 Garching, Germany Department of Astronomy, University of Massachusetts, 16 National Radio Astronomy Observatory, P.O. Box 0, So- Amherst, MA 01003, USA corro, NM 87801-0387 ⋆ Based on observations with: the W.M. Keck Observatory, 17 Harvard-Smithsonian Centre for Astrophysics, 60 Garden the Canada-France-Hawaii Telescope; the United Kingdom In- Street, Cambridge, MA 02138, USA frared Telescope; the Subaru Telescope; the NASA/ESA Hubble 18 Institute for Astronomy, University of Hawaii, 2680 Wood- Space Telescope; the NASA Spitzer Telescope; the Caltech Sub- lawn Drive, Honolulu, HI, 96822, USA mm Observatory; the Smithsonian Millimeter Array; and the Na- 19 Space Telescope Science Institute, 3700 San Martin Drive, tional Radio Astronomy Observatory. Herschel is an ESA space Baltimore, MD 21218 observatory with science instruments provided by European-led 20 Spitzer Fellow Principal Investigator consortia and with im- portant participa- 21 INAF Osservatorio Astronomico di Roma, via di Franscati tion from NASA. 2 V. Smolˇci´cet al. 1. INTRODUCTION E-array configuration in July/2009. The target was ob- served for 8.5 hrs on-source. The 3 mm receivers were Submillimeter galaxies (SMGs; S850µm > 5 mJy) are ultra-luminous, dusty starbursting systems with ex- tuned to 98.95 GHz (3.03 mm), with lower (upper) side- −1 bands centered at 96.43 (101.46) GHz, respectively. Each treme star formation rates (SFR ∼ 100 − 1000 M⊙ yr ; e.g. Blain et al. 2002). The bulk of this population has sideband was observed with 45 31.25 MHz wide channels, been shown to lie at 2 <z < 3 (e.g. Chapman et al. leading to a total bandwidth of 2.56 GHz. The data re- duction was performed with the MIRIAD package. No 2005). However, only recently have blank-field sub-mm → surveys started to discover the high-redshift (z > 4) tail line emission (the CO(5 4) transition is expected at of the SMG distribution. To date seven z > 4 SMGs have the source’s redshift) was detected across the observed been spectroscopically confirmed (and published: three bands covering 4.64 <z< 4.72 and 4.94 <z< 5.02. in GOODS-N, Daddi et al. 2009a,b; two in COSMOS, The uv-data were imaged merging both sidebands to- Capak et al. 2008; Schinnerer et al. 2008; Riechers et al. gether and using natural weighting. We infer an rms of 2010; Capak et al. 2010, one in ECDFS, Coppin et al. 0.36 mJy/beam in the continuum map, but no detection 2009, 2010; and one in Abell 2218, Knudsen et al. of the source. Using the new WideX correlator on PdBI, AzTEC-1 2010). These high-redshift SMGs, presenting a chal- ∼ lenge to cosmological models of structure growth (see was observed with 6 antennas in Apr/May/2010 for e.g. Coppin et al. 2009), may alter our understanding of 5.5 hrs on-source. The WideX correlator covered 3.6 GHz the role of SMGs in galaxy evolution. bandwidth using polarizations centered at 101.866394 Galaxies are thought to evolve in time from an ini- GHz. 1005+066 and 3C273 were used as phase and gain tial stage with irregular/spiral morphology towards pas- calibrators, respectively. The flux calibration error is es- 11 timated to be < 10%. The naturally weighted beam sive, very massive elliptical systems (M∗ > 10 M⊙; is 6.38”×5.01” (PA 32o). The 3 mm continuum emis- Faber et al. e.g. 2007). The morphology and spec- sion, shown in Fig. 1, is detected at 7.5σ with S = tral properties of passive galaxies indicate that they 3mm 0.3 ± 0.04 mJy and unresolved.
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