Eales, S. A. and Blain, A. and Bock, J. and Cooray, A. and Dowell, C. D. and Levenson, L. and Lu, N. and Nguyen, H. T. and Schulz, B. and Shupe, D. L. and Xu, C. K. and Zemcov, M. (2010) First results from HerMES on the evolution of the submillimetre luminosity function. Astronomy and Astrophysics, 518 . Art. No. L23. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20101201-111403706
- Published Version
See Usage Policy.
Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20101201-111403706
We have carried out two extremely deep surveys with SPIRE, one of the two cameras on Herschel, at 250 μm, close to the peak of the far-infrared background. We have used the results to investigate the evolution of the rest-frame 250-μm luminosity function out to z = 2. We find evidence for strong evolution out to z ≃ 1 but evidence for at most weak evolution beyond this redshift. Our results suggest that a significant part of the stars and metals in the universe today were formed at z ≤ 1.4 in spiral galaxies.
|Additional Information:||© 2010 ESO. Received 31 March 2010, Accepted 5 May 2010, Published online 16 July 2010. Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA. SPIRE has been developed by a consortium of institutes led by Cardiff Univ. (UK) and including Univ. Lethbridge (Canada); NAOC (China); CEA, LAM (France); IFSI, Univ. Padua (Italy); IAC (Spain); Stockholm Observatory (Sweden); Imperial College London, RAL, UCL-MSSL, UKATC, Univ. Sussex (UK); Caltech, JPL, NHSC, Univ. Colorado (USA). This development has been supported by national funding agencies: CSA (Canada); NAOC (China); CEA, CNES, CNRS (France); ASI (Italy); MCINN (Spain); Stockholm Observatory (Sweden); STFC (UK); and NASA (USA).|
|Subject Keywords:||galaxies: evoluton, galaxies: formation, galaxies: high-redshift, submillimeter: galaxies|
|Official Citation:||First results from HerMES on the evolution of the submillimetre luminosity function S. A. Eales, G. Raymond, I. G. Roseboom, B. Altieri, A. Amblard, V. Arumugam, R. Auld, H. Aussel, T. Babbedge, A. Blain, J. Bock, A. Boselli, D. Brisbin, V. Buat, D. Burgarella, N. Castro-Rodríguez, A. Cava, P. Chanial, D. L. Clements, A. Conley, L. Conversi, A. Cooray, C. D. Dowell, E. Dwek, S. Dye, D. Elbaz, D. Farrah, M. Fox, A. Franceschini, W. Gear, J. Glenn, E. A. González Solares, M. Griffin, M. Harwit, E. Hatziminaoglou, J. Huang, E. Ibar, K. Isaak, R. J. Ivison, G. Lagache, L. Levenson, C. J. Lonsdale, N. Lu, S. Madden, B. Maffei, G. Mainetti, L. Marchetti, G. E. Morrison, A. M. J. Mortier, H. T. Nguyen, B. O'Halloran, S. J. Oliver, A. Omont, F. N. Owen, M. J. Page, M. Pannella, P. Panuzzo, A. Papageorgiou, C. P. Pearson, I. Pérez-Fournon, M. Pohlen, J. I. Rawlings, D. Rigopoulou, D. Rizzo, M. Rowan-Robinson, M. Sánchez Portal, B. Schulz, D. Scott, N. Seymour, D. L. Shupe, A. J. Smith, J. A. Stevens, V. Strazzullo, M. Symeonidis, M. Trichas, K. E. Tugwell, M. Vaccari, I. Valtchanov, L. Vigroux, L. Wang, R. Ward, G. Wright, C. K. Xu and M. Zemcov A&A 518 L23 (2010) DOI: 10.1051/0004-6361/201014675|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Benjamin Perez|
|Deposited On:||01 Dec 2010 19:34|
|Last Modified:||07 Jan 2017 01:39|
Repository Staff Only: item control page