Vaccari, M. 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) The HerMES SPIRE submillimeter local luminosity function. Astronomy and Astrophysics, 518 . L20. ISSN 0004-6361. http://resolver.caltech.edu/CaltechAUTHORS:20101115-102412434
- Published Version
See Usage Policy.
Use this Persistent URL to link to this item: http://resolver.caltech.edu/CaltechAUTHORS:20101115-102412434
Local luminosity functions are fundamental benchmarks for high-redshift galaxy formation and evolution studies as well as for models describing these processes. Determining the local luminosity function in the submillimeter range can help to better constrain in particular the bolometric luminosity density in the local Universe, and Herschel offers the first opportunity to do so in an unbiased way by imaging large sky areas at several submillimeter wavelengths. We present the first Herschel measurement of the submillimeter 0 < z < 0.2 local luminosity function and infrared bolometric (8–1000 μm) local luminosity density based on SPIRE data from the HerMES Herschel key program over 14.7 deg^2. Flux measurements in the three SPIRE channels at 250, 350 and 500 μm are combined with Spitzer photometry and archival data. We fit the observed optical-to-submillimeter spectral energy distribution of SPIRE sources and use the 1/V_(max) estimator to provide the first constraints on the monochromatic 250, 350 and 500 μm as well as on the infrared bolometric (8–1000 μm) local luminosity function based on Herschel data. We compare our results with modeling predictions and find a slightly more abundant local submillimeter population than predicted by a number of models. Our measurement of the infrared bolometric (8–1000 μm) local luminosity function suggests a flat slope at low luminosity, and the inferred local luminosity density, 1.31_(-0.21)^(+0.24) × 10^8 L_☉ Mpc^(-3), is consistent with the range of values reported in recent literature.
|Additional Information:||© 2010 ESO. Received 1 April 2010; Accepted 27 April 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. M.V. acknowledges support from a University of Padova “Herschel & ALMA” Fellowship and ASI “Herschel Science” Contract I/005/07/0. Micol Bolzonella kindly provided advice on the use of hyperz and Mattia Negrello swiftly produced additional predictions based on his models. SPIRE has been developed by a consortium of institutes led by Cardiff University (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); and 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). The data presented in this paper will be released through the Herschel Database in Marseille (HeDaM, http://hedam.oamp.fr/HerMES).|
|Subject Keywords:||galaxies: luminosity function, mass functions; galaxies: evolution; galaxies: statistics; submillimeter: galaxies|
|Official Citation:||The HerMES SPIRE submillimeter local luminosity function M. Vaccari, L. Marchetti, A. Franceschini, B. Altieri, A. Amblard, V. Arumugam, R. Auld, H. Aussel, T. Babbedge, A. Blain, J. Bock, A. Boselli, 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, S. Eales, D. Elbaz, D. Farrah, M. Fox, W. Gear, J. Glenn, E. A. González Solares, M. Griffin, M. Halpern, E. Hatziminaoglou, J. Huang, E. Ibar, K. Isaak, R. J. Ivison, G. Lagache, L. Levenson, N. Lu, S. Madden, B. Maffei, G. Mainetti, A. M. J. Mortier, H. T. Nguyen, B. O'Halloran, S. J. Oliver, A. Omont, M. J. Page, P. Panuzzo, A. Papageorgiou, C. P. Pearson, I. Pérez-Fournon, M. Pohlen, J. I. Rawlings, G. Raymond, D. Rigopoulou, D. Rizzo, G. Rodighiero, I. G. Roseboom, M. Rowan-Robinson, M. Sánchez Portal, B. Schulz, D. Scott, N. Seymour, D. L. Shupe, A. J. Smith, J. A. Stevens, M. Symeonidis, M. Trichas, K. E. Tugwell, E. Valiante, I. Valtchanov, L. Vigroux, L. Wang, R. Ward, G. Wright, C. K. Xu and M. Zemcov A&A 518 L20 (2010) DOI: 10.1051/0004-6361/201014694|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Jason Perez|
|Deposited On:||15 Nov 2010 19:34|
|Last Modified:||07 Dec 2016 21:28|
Repository Staff Only: item control page