Amblard, Alexandre and Cooray, Asantha and Blain, A. and Bock, J. and Dowell, C. D. and Levenson, L. and Lu, N. and Nguyen, H. T. and Schulz, B. and Shupe, D. L. and Vieira, J. D. and Xu, C. K. and Zemcov, M. (2011) Submillimetre galaxies reside in dark matter haloes with masses greater than 3 × 10^(11) solar masses. Nature, 470 (7335). pp. 510-512. ISSN 0028-0836. http://resolver.caltech.edu/CaltechAUTHORS:20110314-094552984
Full text is not posted in this repository. Consult Related URLs below.
Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20110314-094552984
The extragalactic background light at far-infrared wavelengths comes from optically faint, dusty, star-forming galaxies in the Universe with star formation rates of a few hundred solar masses per year. These faint, submillimetre galaxies are challenging to study individually because of the relatively poor spatial resolution of far-infrared telescopes. Instead, their average properties can be studied using statistics such as the angular power spectrum of the background intensity variations. A previous attempt at measuring this power spectrum resulted in the suggestion that the clustering amplitude is below the level computed with a simple ansatz based on a halo model. Here we report excess clustering over the linear prediction at arcminute angular scales in the power spectrum of brightness fluctuations at 250, 350 and 500 µm. From this excess, we find that submillimetre galaxies are located in darkmatter haloes with a minimum mass, M_(min), such that log_(10)[M_(min)/M_⊙] = 11.5^(+0.7)_(-0.2) at 350 µm, where M_⊙ is the solar mass. This minimum dark matter halo mass corresponds to the most efficient mass scale for star formation in the Universe, and is lower than that predicted by semi-analytical models for galaxy formation.
|Additional Information:||© 2011 Macmillan Publishers Limited. Received 11 August; accepted 20 December 2010. Published online 16 February 2011. SPIRE has been developed by a consortium of institutes led by Cardiff University (UK) and including the University of Lethbridge (Canada); NAOC (China); CEA and LAM (France); IFSI and the University of Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC and the University of Sussex (UK); and Caltech/JPL, IPAC and the University of Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES and CNRS (France); ASI (Italy); MCINN (Spain); SNSB (Sweden); STFC (UK); and NASA (USA). We thank M. Viero for comments. A.A., A. Cooray, P.S., A.A.K., K.M.-W. and other US co-authors are supported by NASA funds for US participants in Herschel through an award from JPL. Author Contributions: This paper represents the combined work of the HerMES collaboration, the SPIRE Instrument Team’s Extragalactic Survey, and has been extensively internally reviewed. A. Cooray planned the study, supervised the research work of A.A. and P.S., and wrote the draft version of this paper. A.A. performed the power spectrum measurements and P.S. interpreted those measurements with the halo model. All other co-authors of this paper contributed extensively and equally by their varied contributions to the SPIRE instrument, Herschel mission, analysis of SPIRE and HerMES data, planning of HerMES observations and scientific support of HerMES, and by commenting on this manuscript as part of an internal review process.|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Tony Diaz|
|Deposited On:||16 Mar 2011 18:12|
|Last Modified:||23 Aug 2016 09:59|
Repository Staff Only: item control page