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The Herschel Reference Survey

Boselli, A. and Eales, S. and Cortese, L. and Bendo, G. and Chanial, P. and Buat, V. and Davies, J. and Auld, R. and Rigby, E. and Baes, M. and Barlow, M. and Bock, J. and Bradford, M. and Castro-Rodríguez, N. and Charlot, S. and Clements, D. and Cormier, D. and Dwek, E. and Elbaz, D. and Galametz, M. and Galliano, F. and Gear, W. and Glenn, J. and Gomez, H. and Griffin, M. and Hony, S. and Isaak, K. and Levenson, L. and Lu, N. and Madden, S. and O'Halloran, B. and Okamura, K. and Oliver, S. and Page, M. and Panuzzo, P. and Papageorgiou, A. and Parkin, T. and Pérez-Fournon, I. and Pohlen, M. and Rangwala, N. and Roussel, H. and Rykala, A. and Sacchi, N. and Sauvage, M. and Schulz, B. and Schirm, M. and Smith, M. W. L. and Spinoglio, L. and Stevens, J. and Symeonidis, M. and Vaccari, M. and Vigroux, L. and Wilson, C. and Wozniak, H. and Wright, G. and Zeilinger, W. (2010) The Herschel Reference Survey. Publications of the Astronomical Society of the Pacific, 122 (889). pp. 261-287. ISSN 0004-6280. http://resolver.caltech.edu/CaltechAUTHORS:20100331-134059745

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Abstract

The Herschel Reference Survey is a Herschel guaranteed time key project and will be a benchmark study of dust in the nearby universe. The survey will complement a number of other Herschel key projects including large cosmological surveys that trace dust in the distant universe. We will use Herschel to produce images of a statistically-complete sample of 323 galaxies at 250, 350, and 500 μm. The sample is volume-limited, containing sources with distances between 15 and 25 Mpc and flux limits in the K band to minimize the selection effects associated with dust and with young high-mass stars and to introduce a selection in stellar mass. The sample spans the whole range of morphological types (ellipticals to late-type spirals) and environments (from the field to the center of the Virgo Cluster) and as such will be useful for other purposes than our own. We plan to use the survey to investigate (i) the dust content of galaxies as a function of Hubble type, stellar mass, and environment; (ii) the connection between the dust content and composition and the other phases of the interstellar medium; and (iii) the origin and evolution of dust in galaxies. In this article, we describe the goals of the survey, the details of the sample and some of the auxiliary observing programs that we have started to collect complementary data. We also use the available multifrequency data to carry out an analysis of the statistical properties of the sample.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1086/651535DOIArticle
http://www.journals.uchicago.edu/doi/abs/10.1086/651535PublisherArticle
ORCID:
AuthorORCID
Bock, J.0000-0002-5710-5212
Clements, D.0000-0002-9548-5033
Dwek, E.0000-0001-8033-1181
Galametz, M.0000-0002-0283-8689
Lu, N.0000-0002-8948-1044
Oliver, S.0000-0001-7862-1032
Page, M.0000-0002-6689-6271
Vaccari, M.0000-0002-6748-0577
Additional Information:© 2010. The Astronomical Society of the Pacific. Received 2008 August 17; accepted 2010 January 26; published 2010 February 26. We would like to thank the Herschel Project Scientist, G. Pilbratt; the SPIRE team; and all the people involved in the construction and the launch of Herschel. This research has made use of the NASA/IPAC Extragalactic Database (NED) which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration; and of the GOLD Mine database. A. B. wishes to thank S. Boissier for his help in the construction of the HRS database. We are grateful to the anonymous referee forinvaluable comments and suggestions which helped to improve the quality of the manuscript.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
NASA/JPL/CaltechUNSPECIFIED
GOLD Mine databaseUNSPECIFIED
Record Number:CaltechAUTHORS:20100331-134059745
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20100331-134059745
Official Citation:A. Boselli, S. Eales, L. Cortese, G. Bendo, P. Chanial, V. Buat, J. Davies, R. Auld, E. Rigby, M. Baes, M. Barlow, J. Bock, M. Bradford, N. Castro-Rodriguez, S. Charlot, D. Clements, D. Cormier, E. Dwek, D. Elbaz, M. Galametz, F. Galliano, W. Gear, J. Glenn, H. Gomez, M. Griffin, S. Hony, K. Isaak, L. Levenson, N. Lu, S. Madden, B. O’Halloran, K. Okamura, S. Oliver, M. Page, P. Panuzzo, A. Papageorgiou, T. Parkin, I. Perez-Fournon, M. Pohlen, N. Rangwala, H. Roussel, A. Rykala, N. Sacchi, M. Sauvage, B. Schulz, M. Schirm, M. W. L. Smith, L. Spinoglio, J. Stevens, M. Symeonidis, M. Vaccari, L. Vigroux, C. Wilson, H. Wozniak, G. Wright, and W. Zeilinger Publications of the Astronomical Society of the Pacific 2010 122:889, 261-287
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:17831
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:31 Mar 2010 21:23
Last Modified:09 Jul 2019 21:22

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