The Herschel★ PEP/HerMES luminosity function – I. Probing the evolution of PACS selected Galaxies to z ≃ 4

著者: C. Gruppioni, F. Pozzi, G. Rodighiero, I. Delvecchio, S. Berta, L. Pozzetti, G. Zamorani, P. Andreani, A. Cimatti, O. Ilbert, E. Le Floc’h, D. Lutz, B. Magnelli, L. Marchetti, Pierluigi Monaco, R. Nordon, S. Oliver, P. Popesso, L. Riguccini, I. G. Roseboom, D. J. Rosario, M. Sargent, M. Vaccari, B. Altieri, H. Aussel, Á. Bongiovanni, J. Cepa, E. Daddi, H. Domínguez-Sánchez, D. Elbaz, N. Förster Schreiber, R. Genzel, Álvaro Iribarrem, M. Magliocchetti, R. Maiolino, A. Poglitsch, A. M. Pérez García, M. Sánchez‐Portal, E. Sturm, L. J. Tacconi, I. Valtchanov, A. Amblard, V. Arumugam, M. Béthermin, J. Böck, A. Boselli, V. Buat, D. Burgarella, N. Castro-Rodríguez, A. Cava, P. Chanial, D. L. Clements, A. Conley, Asantha Cooray, C. D. Dowell, E. Dwek, S. Eales, A. Franceschini, J. Glenn, Matt Griffin, E. Hatziminaoglou, E. Ibar, K. G. Isaak, R. J. Ivison, G. Lagache, L. Levenson, N. Lu, S. C. Madden, B. Maffei, G Mainetti, H. T. Nguyen, B. O’Halloran, M. J. Page, P. Panuzzo, Ανδρέας Παπαγεωργίου, C. P. Pearson, I. Pérez-Fournon, M. Pohlen, D. Rigopoulou, M. Rowan-Robinson, B. Schulz, D. Scott, N. Seymour, D. L. Shupe, A. J. Smith, J. A. Stevens, M. Symeonidis, M. Trichas, K. E. Tugwell, L. Vigroux, L. Wang, Geraldine A. Wright, C. K. Xu, M. Zemcov, S. Bardelli, C. M. Carollo, T. Contini, O. Le Fèvre, S. J. Lilly, V. Mainieri, A. Renzini, M. Scodeggio, E. Zucca - Monthly Notices of the Royal Astronomical Society 2013 被引用: 449

Understanding the origin and growth of the galaxies we ob- serve today is one of the main problems of current cosmol- ogy. The luminosity function (LF) provides one of the fun- damental tools to probe the distribution of galaxies over cosmological time, since it allows us to assess the statisti- cal nature of galaxy formation and evolution. When com- puted at di erent redshifts, the LF constitutes the most di- rect method for exploring the evolution of a galaxy popula- tion, describing the relative number of sources of di erent luminosities counted in representative volumes of the Uni- verse. The LF computed for di erent samples of galaxies can provide a crucial comparison between the distribution of di erent galaxy types, i.e. galaxies at di erent redshifts, in di erent enviroments or selected at di erent wavelengths.