Wednesday 19th Sept 2012


A new HST/Herschel deep field at the North Ecliptic Pole: preparing the way for JWST, SPICA and Euclid

Stephen Serjeant, Veronique Buat, Denis Burgarella, Dave Clements, Gianfranco De Zotti, Tomo Goto, Bunyo Hatsukade, Rosalind Hopwood, Narae Hwang, Hanae Inami, Woong-Seob Jeong, Seong Jin Kim, Mirko Krumpe, Myung Gyoon Lee, Matt Malkan, Hideo Matsuhara, Takamitsu Miyaji, Shinki Oyabu, Chris Pearson, Tsutomu Takeuchi, Mattia Vaccari, Ivan Valtchanov, Paul van der Werf, Takehiko Wada, Glenn White

We propose a co-ordinated multi-observatory survey at the North Ecliptic Pole. This field is the natural extragalactic deep field location for most space observatories (e.g. containing the deepest Planck, WISE and eROSITA data), is in the continuous viewing zones for e.g. Herschel, HST, JWST, and is a natural high-visibility field for the L2 halo orbit of SPICA with deep and wide-field legacy surveys already planned. The field is also a likely deep survey location for the forthcoming Euclid mission. It is already a multi-wavelength legacy field in its own right (e.g. AKARI, LOFAR, SCUBA-2): the outstanding and unparalleled continuous mid-IR photometric coverage in this field and nowhere else enables a wide range of galaxy evolution diagnostics unachievable in any other survey field, by spanning the wavelengths of redshifted PAH and silicate features and the peak energy output of AGN hot dust. We argue from the science needs of Euclid and JWST, and from the comparative multiwavelength depths, that the logical approach is (1) a deep (H-UDF) UV/optical tile in the NEP over ~10 square arcminutes, and (2) an overlapping wide-field UV/optical HST survey tier covering >100 square arcminutes, with co-ordinated submm SPIRE mapping up to or beyond the submm point source confusion limit over a wider area and PACS data over the shallower HST tier.


The Spitzer Extragalactic Representative Volume Survey (SERVS): survey definition and goals

J.-C. Mauduit, M. Lacy, D. Farrah, J. A. Surace, M. Jarvis, S. Oliver, C. Maraston, M. Vaccari, L. Marchetti, G. Zeimann, E. A. Gonzalez-Solares, J. Pforr, A. O. Petric, B. Henriques, P. A. Thomas, J. Afonso, A. Rettura, G. Wilson, J. T. Falder, J. E. Geach, M. Huynh, R. P. Norris, N. Seymour, G. T. Richards, S. A. Stanford, D. M. Alexander, R. H. Becker, P. N. Best, L. Bizzocchi, D. Bonfield, N. Castro, A. Cava, S. Chapman, N. Christopher, D. L. Clements, G. Covone, N. Dubois, J. S. Dunlop, E. Dyke, A. Edge, H. C. Ferguson, S. Foucaud, A. Franceschini, R. R. Gal, J. K. Grant, M. Grossi, E. Hatziminaoglou, S. Hickey, J. A. Hodge, J.-S. Huang, R. J. Ivison, M. Kim, O. LeFevre, M. Lehnert, C. J. Lonsdale, L. M. Lubin, R. J. McLure, H. Messias, A. Martinez-Sansigre, A. M. J. Mortier, D. M. Nielsen, et al. (23 additional authors not shown)

We present the Spitzer Extragalactic Representative Volume Survey (SERVS), an 18 deg2 mediumdeep survey at 3.6 and 4:5 m with the post-cryogenic Spitzer Space Telescope to 2 Jy (AB = 23:1) depth of ve highly observed astronomical elds (ELAIS-N1, ELAIS-S1, Lockman Hole, Chandra Deep Field South and XMM-LSS). SERVS is designed to enable the study of galaxy evolution as a function of environment from z 5 to the present day, and is the rst extragalactic survey that is both large enough and deep enough to put rare objects such as luminous quasars and galaxy clusters at z >1 into their cosmological context. SERVS is designed to overlap with several key surveys at optical, near- through far-infrared, submillimeter and radio wavelengths to provide an unprecedented view of the formation and evolution of massive galaxies. In this article, we discuss the SERVS survey design, the data processing flow from image reduction and mosaicking to catalogs, and coverage of ancillary data from other surveys in the SERVS elds. We also highlight a variety of early science results from the survey

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