The FORS deep field:: Field selection, photometric observations and photometric catalog

被引：74

作者：

Heidt, J ^{[1
]}

Appenzeller, I

Gabasch, A

Jäger, K

Seitz, S

Bender, R

Böhm, A

Snigula, J

Fricke, KJ

Hopp, U

Kümmel, M

Möllenhoff, C

Szeifert, T

Ziegler, B

Drory, N

Mehlert, D

Moorwood, A

Nicklas, H

Noll, S

Saglia, RP

Seifert, W

Stahl, O

Sutorius, E

Wagner, SJ

机构：

[1] Landessternwarte Heidelberg, D-69117 Heidelberg, Germany

[2] Univ Sternwarte Munchen, D-81679 Munich, Germany

[3] Univ Sternwarte Gottingen, D-37083 Gottingen, Germany

[4] Max Planck Inst Astron, D-69117 Heidelberg, Germany

[5] European So Observ Santiago, Santiago 19, Chile

[6] Akad Wissensch, D-37079 Gottingen, Germany

[7] European So Observ, D-85738 Garching, Germany

[8] Royal Observ Edinburgh, Edinburgh EH9 3HJ, Midlothian, Scotland

来源：

ASTRONOMY & ASTROPHYSICS | 2003年 / 398卷 / 01期

关键词：

methods : data analysis; catalogs; galaxies : general; galaxies : fundamental parameters; galaxies : photometry;

D O I：

10.1051/0004-6361:20021620

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The FORS Deep Field project is a multi-colour, multi-object spectroscopic investigation of a similar to7' x 7' region near the south galactic pole based mostly on observations carried out with the FORS instruments attached to the VLT telescopes. It includes the QSO Q 0103-260 (z = 3.36). The goal of this study is to improve our understanding of the formation and evolution of galaxies in the young Universe. In this paper the field selection, the photometric observations, and the data reduction are described. The source detection and photometry of objects in the FORS Deep Field is discussed in detail. A combined B and 1 selected UBgRIJKs photometric catalog of 8753 objects in the FDF is presented and its properties are briefly discussed. The formal 50% completeness limits for point sources, derived from the co-added images, are 25.64, 27.69, 26.86, 26.68, 26.37, 23.60 and 21.57 in U, B, g, R, I, J and Ks (Vega-system), respectively. A comparison of the number counts in the FORS Deep Field to those derived in other deep field surveys shows very good agreement.

引用

页码：49 / 61

页数：13

共 44 条

[1]

APPENZELLER I, 2002, IN PRESS STUDIES GAL

[2]

Appenzeller I., 1998, The Messenger, V94, P1

[3]

Arnouts S, 1999, ASTRON ASTROPHYS, V341, P641

[4]

BENDER R, 2001, ESO ASTROPHYSICS S, V96

[5] Near-infrared galaxy counts to J and K∼24 as a function of image size [J].

Bershady, MA ;

Lowenthal, JD ;

Koo, DC .

ASTROPHYSICAL JOURNAL, 1998, 505 (01) :50-73

[6] SExtractor: Software for source extraction [J].

Bertin, E ;

Arnouts, S .

ASTRONOMY & ASTROPHYSICS SUPPLEMENT SERIES, 1996, 117 (02) :393-404

[7]

Bertin E, 1997, ASTRON ASTROPHYS, V317, P43

[8] REDDENINGS DERIVED FROM H-1 AND GALAXY COUNTS - ACCURACY AND MAPS [J].

BURSTEIN, D ;

HEILES, C .

ASTRONOMICAL JOURNAL, 1982, 87 (08) :1165-&

[9] THE RELATIONSHIP BETWEEN INFRARED, OPTICAL, AND ULTRAVIOLET EXTINCTION [J].

CARDELLI, JA ;

CLAYTON, GC ;

MATHIS, JS .

ASTROPHYSICAL JOURNAL, 1989, 345 (01) :245-256

[10]

COHEN JG, 1998, STSCI S SER, V11, P52

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