Planck intermediate results. XXXIX. The Planck list of high-redshift source candidates
Abstract
The Planck mission, thanks to its large frequency range and all-sky coverage, has a unique potential for systematically detecting the brightest, and rarest, submillimetre sources on the sky, including distant objects in the high-redshift Universe traced by their dust emission. A novel method, based on a component-separation procedure using a combination of Planck and IRAS data, has been applied to select the most luminous cold submm sources with spectral energy distributions peaking between 353 and 857GHz at 5' resolution. A total of 2151 Planck high-z source candidates (the PHZ) have been detected in the cleanest 26% of the sky, with flux density at 545GHz above 500mJy. Embedded in the cosmic infrared background close to the confusion limit, these high-z candidates exhibit colder colours than their surroundings, consistent with redshifts z>2, assuming a dust temperature of 35K and a spectral index of 1.5. First follow-up observations obtained from optical to submm have confirmed that this list consists of two distinct populations. A small fraction (around 3%) of the sources have been identified as strongly gravitationally lensed star-forming galaxies, which are amongst the brightest submm lensed objects (with flux density at 545GHz ranging from 350mJy up to 1Jy) at redshift 2 to 4. However, the vast majority of the PHZ sources appear as overdensities of dusty star-forming galaxies, having colours consistent with z>2, and may be considered as proto-cluster candidates. The PHZ provides an original sample, complementary to the Planck Sunyaev-Zeldovich Catalogue; by extending the population of the virialized massive galaxy clusters to a population of sources at z>1.5, the PHZ may contain the progenitors of today's clusters. Hence the PHZ opens a new window on the study of the early ages of structure formation, and the understanding of the intensively star-forming phase at high-z.
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Cite
@article{arxiv.1508.04171,
title = {Planck intermediate results. XXXIX. The Planck list of high-redshift source candidates},
author = {Planck Collaboration and P. A. R. Ade and N. Aghanim and M. Arnaud and J. Aumont and C. Baccigalupi and A. J. Banday and R. B. Barreiro and N. Bartolo and E. Battaner and K. Benabed and A. Benoit-Lévy and J. -P. Bernard and M. Bersanelli and P. Bielewicz and A. Bonaldi and L. Bonavera and J. R. Bond and J. Borrill and F. R. Bouchet and F. Boulanger and C. Burigana and R. C. Butler and E. Calabrese and A. Catalano and H. C. Chiang and P. R. Christensen and D. L. Clements and L. P. L. Colombo and F. Couchot and A. Coulais and B. P. Crill and A. Curto and F. Cuttaia and L. Danese and R. D. Davies and R. J. Davis and P. de Bernardis and A. de Rosa and G. de Zotti and J. Delabrouille and C. Dickinson and J. M. Diego and H. Dole and O. Doré and M. Douspis and A. Ducout and X. Dupac and F. Elsner and T. A. Enßlin and H. K. Eriksen and E. Falgarone and F. Finelli and I. Flores-Cacho and M. Frailis and A. A. Fraisse and E. Franceschi and S. Galeotta and S. Galli and K. Ganga and M. Giard and Y. Giraud-Héraud and E. Gjerløw and J. González-Nuevo and K. M. Górski and A. Gregorio and A. Gruppuso and J. E. Gudmundsson and F. K. Hansen and D. L. Harrison and G. Helou and C. Hernández-Monteagudo and D. Herranz and S. R. Hildebrandt and E. Hivon and M. Hobson and A. Hornstrup and W. Hovest and K. M. Huffenberger and G. Hurier and A. H. Jaffe and T. R. Jaffe and E. Keihänen and R. Keskitalo and T. S. Kisner and J. Knoche and M. Kunz and H. Kurki-Suonio and G. Lagache and J. -M. Lamarre and A. Lasenby and M. Lattanzi and C. R. Lawrence and R. Leonardi and F. Levrier and P. B. Lilje and M. Linden-Vørnle and M. López-Caniego and P. M. Lubin and J. F. Macías-Pérez and B. Maffei and G. Maggio and D. Maino and N. Mandolesi and A. Mangilli and M. Maris and P. G. Martin and E. Martínez-González and S. Masi and S. Matarrese and A. Melchiorri and A. Mennella and M. Migliaccio and S. Mitra and M. -A. Miville-Deschênes and A. Moneti and L. Montier and G. Morgante and D. Mortlock and D. Munshi and J. A. Murphy and F. Nati and P. Natoli and N. P. H. Nesvadba and F. Noviello and D. Novikov and I. Novikov and C. A. Oxborrow and L. Pagano and F. Pajot and D. Paoletti and B. Partridge and F. Pasian and T. J. Pearson and O. Perdereau and L. Perotto and V. Pettorino and F. Piacentini and M. Piat and S. Plaszczynski and E. Pointecouteau and G. Polenta and G. W. Pratt and S. Prunet and J. -L. Puget and J. P. Rachen and M. Reinecke and M. Remazeilles and C. Renault and A. Renzi and I. Ristorcelli and G. Rocha and C. Rosset and M. Rossetti and G. Roudier and J. A. Rubiño-Martín and B. Rusholme and M. Sandri and D. Santos and M. Savelainen and G. Savini and D. Scott and L. D. Spencer and V. Stolyarov and R. Stompor and R. Sudiwala and R. Sunyaev and A. -S. Suur-Uski and J. -F. Sygnet and J. A. Tauber and L. Terenzi and L. Toffolatti and M. Tomasi and M. Tristram and M. Tucci and M. Türler and G. Umana and L. Valenziano and J. Valiviita and B. Van Tent and P. Vielva and F. Villa and L. A. Wade and B. D. Wandelt and I. K. Wehus and N. Welikala and D. Yvon and A. Zacchei and A. Zonca},
journal= {arXiv preprint arXiv:1508.04171},
year = {2016}
}