Scott, K. S. and Bock, J. and Bradford, C. M. and Carpenter, J. M. and Cooray, A. and Dowell, C. D. and Murphy, E. J. and Nguyen, H. T. and Riechers, D. and Vieira, J. D. and Zmuidzinas, J. (2011) Redshift Determination and CO Line Excitation Modeling for the Multiply Lensed Galaxy HLSW-01. Astrophysical Journal, 733 (1). Art. No. 29. ISSN 0004-637X. http://resolver.caltech.edu/CaltechAUTHORS:20110531-132533695
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We report on the redshift measurement and CO line excitation of HERMES J105751.1+573027 (HLSW-01), a strongly lensed submillimeter galaxy discovered in Herschel/SPIRE observations as part of the Herschel Multi-tiered Extragalactic Survey (HerMES). HLSW-01 is an ultra-luminous galaxy with an intrinsic far-infrared luminosity of L _(FIR) = 1.4 × 10^(13) L _⊙, and is lensed by a massive group of galaxies into at least four images with a total magnification of μ = 10.9 ± 0.7. With the 100 GHz instantaneous bandwidth of the Z-Spec instrument on the Caltech Submillimeter Observatory, we robustly identify a redshift of z = 2.958 ± 0.007 for this source, using the simultaneous detection of four CO emission lines (J = 7 → 6, J = 8 → 7, J = 9 → 8, and J = 10 → 9). Combining the measured line fluxes for these high-J transitions with the J = 1 → 0, J = 3 → 2, and J = 5 → 4 line fluxes measured with the Green Bank Telescope, the Combined Array for Research in Millimeter Astronomy, and the Plateau de Bure Interferometer, respectively, we model the physical properties of the molecular gas in this galaxy. We find that the full CO spectral line energy distribution is described well by warm, moderate-density gas with T _(kin) = 86-235 K and n_H_2 = (1.1-3.5)x10^3 cm^(–3). However, it is possible that the highest-J transitions are tracing a small fraction of very dense gas in molecular cloud cores, and two-component models that include a warm/dense molecular gas phase with T _(kin) ~ 200 K, n_H_2 ~ 10^5 cm^(–3) are also consistent with these data. Higher signal-to-noise measurements of the J _(up) ≥ 7 transitions with high spectral resolution, combined with high spatial resolution CO maps, are needed to improve our understanding of the gas excitation, morphology, and dynamics of this interesting high-redshift galaxy.
|Additional Information:||© 2011 The American Astronomical Society. Received 2011 February 14; accepted 2011 March 14; published 2011 April 29. We thank the anonymous referees for their suggestions, which improved the presentation of these results. We also thank the staff at CSO for support of the Z-Spec observations, and we appreciate the help of Robert Hanni and Jon Rodriguez with observing. J.E.A. acknowledges support by NSF grant AST-0807990 and by the CSO NSF Cooperative Agreement AST-0838261. J.K. acknowledges funding through an NSF graduate research fellowship. A.J.B. acknowledges support from NSF grant AST-0708653. Z-spec was constructed under NASA SARA grants NAGS-11911 and NAGS-12788 and an NSF Career grant (AST-0239270) and a Research Corporation Award (RI0928) to J.G., in collaboration with the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. We acknowledge Peter Ade and his group for their filters and Lionel Duband for the 3He/4He refrigerator in Z-Spec, and are grateful for their help in the early integration of the instrument. Facilities: CSO (Z-Spec), GBT (Zpectrometer), IRAM: Interferometer (PdBI), CARMA, SMA, Herschel (SPIRE)|
|Subject Keywords:||galaxies: high-redshift; galaxies: individual (HERMES J105751.1+573027); galaxies: starburst; submillimeter: galaxies|
|Classification Code:||PACS: 98.54.Ep; 98.62.Py; 98.58.Db; 98.58.Bz; 95.85.Fm|
|Official Citation:||Redshift Determination and CO Line Excitation Modeling for the Multiply Lensed Galaxy HLSW-01 K. S. Scott, R. E. Lupu, J. E. Aguirre, R. Auld, H. Aussel, A. J. Baker, A. Beelen, J. Bock, C. M. Bradford, D. Brisbin, D. Burgarella, J. M. Carpenter, P. Chanial, S. C. Chapman, D. L. Clements, A. Conley, A. Cooray, P. Cox, C. D. Dowell, S. Eales, D. Farrah, A. Franceschini, D. T. Frayer, R. Gavazzi, J. Glenn, M. Griffin, A. I. Harris, E. Ibar, R. J. Ivison, J. Kamenetzky, S. Kim, M. Krips, P. R. Maloney, H. Matsuhara, A. M. J. Mortier, E. J. Murphy, B. J. Naylor, R. Neri, H. T. Nguyen, S. J. Oliver, A. Omont, M. J. Page, A. Papageorgiou, C. P. Pearson, I. Pérez-Fournon, M. Pohlen, J. I. Rawlings, G. Raymond, D. Riechers, G. Rodighiero, I. G. Roseboom, M. Rowan-Robinson, D. Scott, N. Seymour, A. J. Smith, M. Symeonidis, K. E. Tugwell, M. Vaccari, J. D. Vieira, L. Vigroux, L. Wang, G. Wright and J. Zmuidzinas doi: 10.1088/0004-637X/733/1/29|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Ruth Sustaita|
|Deposited On:||31 May 2011 21:29|
|Last Modified:||07 Jan 2017 01:27|
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