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Title:
A 12 μm ISOCAM survey of the ESO-Sculptor field. Data reduction and analysis
Authors:
Seymour, N.; Rocca-Volmerange, B.; de Lapparent, V.
Affiliation:
AA(Institut d'Astrophysique de Paris, UMR7095 CNRS / Univ. Pierre & Marie Curie, 98 bis boulevard Arago, 75014 Paris, France ; Spitzer Science Center, California Institute of Technology, Mail Code 220-6, 1200 East California Boulevard, Pasadena, CA 91125, USA), AB( Institut d'Astrophysique de Paris, UMR7095 CNRS / Univ. Pierre & Marie Curie, 98 bis boulevard Arago, 75014 Paris, France; Université Paris-Sud, Bât. 121, 91405 Orsay Cedex, France), AC( Institut d'Astrophysique de Paris, UMR7095 CNRS / Univ. Pierre & Marie Curie, 98 bis boulevard Arago, 75014 Paris, France)
Publication:
Astronomy and Astrophysics, Volume 475, Issue 3, 2007, pp.791-799 (A&A Homepage)
Publication Date:
12/2007
Origin:
EDP Sciences
Keywords:
infrared: galaxies, Galaxy: evolution, methods: data analysis, catalogs, galaxies: photometry
DOI:
10.1051/0004-6361:20065218
Bibliographic Code:
2007A&A...475..791S

Abstract

We present a detailed reduction of a mid-infrared 12 μm (LW10 filter) ISOCAM open time observation performed on the ESO-Sculptor Survey field (Arnouts et al. 1997, A&AS, 124, 163). A complete catalogue of 142 sources (120 galaxies and 22 stars), detected with high significance (equivalent to 5σ), is presented above an integrated flux density of 0.24 {mJy}. Star/galaxy separation is performed by a detailed study of colour-colour diagrams. The catalogue is complete to 1 {mJy} and, below this flux density, the incompleteness is corrected using two independent methods. The first method uses stars and the second uses optical counterparts of the ISOCAM galaxies; these methods yield consistent results. We also apply an empirical flux density calibration using stars in the field. For each star, the 12 μm flux density is derived by fitting optical colours from a multi-band χ2 to stellar templates (BaSel-2.0) and using empirical optical-IR colour-colour relations. This article is a companion analysis to our 2007 paper (Rocca-Volmerange et al. 2007, A&A, 475, 801) where the 12 μ m faint galaxy counts are presented and analysed per galaxy type with the evolutionary code PÉGASE.3.

Based on observations collected at the European Southern Observatory (ESO), La Silla, Chile, and on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, the Netherlands, and the United Kingdom) and with the participation of ISAS and NASA. Full Table [see full textsee full textsee full textsee full textsee full textsee full text] is only available in electronic form at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/475/791

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