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Astron. Astrophys. 341, 641-652 (1999)


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The NTT SUSI deep field *

S. Arnouts 1,2, S. D'Odorico 2, S. Cristiani 1, S. Zaggia 2,4, A. Fontana 3 and E. Giallongo 3

1 Dipartimento di Astronomia, Università di Padova, vicolo dell'Osservatorio 5, I-35122, Padova, Italy
2 European Southern Observatory, Karl-Schwarzschild-Strasse 2, D-85748 Garching, Germany
3 Osservatorio Astronomico di Roma, via dell'Osservatorio, I-00040 Monteporzio, Italy
4 Osservatorio Astronomico di Capodimonte, via Moiariello 15, I-80131 Napoli, Italy

Received 16 June 1998 / Accepted 4 November 1998

Abstract

We present a deep BVrI multicolor catalog 1 of galaxies in a 5.62 sq.arcmin field 80 arcsec south of the high redshift ([FORMULA]) quasar BR 1202-0725, derived from observations with the direct CCD camera SUSI at the ESO NTT. The formal 5[FORMULA] magnitude limits (in [FORMULA] FWHM apertures) are 26.9, 26.5, 25.9 and 25.3 in B, V, r and I respectively. Counts, colors for the star and galaxy samples are discussed and a comparison with a deep HST image in the I band is presented. The percentage of merged or blended galaxies in the SUSI data to this magnitude limit is estimated to be not higher than 1%.

At the same galactic latitude of the HDF but pointing toward the galactic center, the star density in this field is found to be [FORMULA] times higher, with [FORMULA] of the objects with V-I[FORMULA]3.0. Reliable colors have been measured for galaxies selected down to [FORMULA]. The choice of the optical filters has been optimized to define a robust multicolor selection of galaxies at [FORMULA]. Within this interval the surface density of galaxy candidates with [FORMULA] in this field is [FORMULA] arcmin-2 corresponding to a comoving density of Star Formation Rate at [FORMULA] of [FORMULA].

Key words: galaxy: stellar content – galaxies: evolution – cosmology: observations – cosmology: large-scale structure of Universe

* Based on observations collected at the NTT 3.5m of ESO, Chile

Send offprint requests to: S. Arnouts

© European Southern Observatory (ESO) 1999

Online publication: December 16, 1998

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