III/250 The VIMOS VLT deep survey (VVDS-DEEP) (Le Fevre+ 2005)
The VIMOS VLT deep survey.
Le Fevre O. et al.
<Astron. Astrophys. 439, 845 (2005) >
=2005A&A...439..845L 2005A&A...439..845L
ADC_Keywords: Photometry, UBVRI ; Photometry, infrared; Galaxies, spectra ;
Atlases
Keywords: cosmology: observations - galaxies: high-redshift -
galaxies: distances and redshift - surveys - galaxies: evolution -
cosmology: large scale structure of Universe
Decsription:
This catalog contains the "First Epoch" sample from the VIMOS VLT Deep
Survey (VVDS). The VVDS goals, observations, data reduction with the
VIPGI pipeline and redshift measurement scheme are discussed in the
paper. Data have been obtained with the VIsible Multi Object
Spectrograph (VIMOS) on the ESO-VLT UT3, allowing to observe ≃600
slits simultaneously at a spectral resolution R≃230. A total of 11564
objects have been observed in the VVDS-02h and VVDS-CDFS "Deep" fields
over a total area of 0.61deg2, selected solely on the basis of
apparent magnitude 17.5≤I(AB)≤24. The VVDS efficiently covers the
redshift range 0<z≤5, successfully going through the "redshift
desert" 1.5<z<2.2, while the range 2.2<z<2.7 remains of difficult
access because of the VVDS wavelength coverage.
A total of 9677 galaxies have a redshift measurement, 836 objects are
stars, 90 objects are AGN, and a redshift could not be measured for
961 objects. There are 1065 galaxies with a measured redshift z≥1.4.
When considering only the primary spectroscopic targets, the survey
reaches a redshift measurement completeness of 78% overall (93%
including less reliable objects), with a spatial sampling of the
population of galaxies of ∼25% and ∼30% in the VVDS-02h and VVDS-CDFS
respectively. The redshift accuracy measured from repeated
observations with VIMOS and comparison to other surveys is ∼276km/s.
From this sample we are able to present for the first time the
redshift distribution of a magnitude-limited spectroscopic sample down
to I(AB)=24.
The following papers to be cited for the usage of this catalog are:
-- Le Fevre et al. (2005A&A...439..845L 2005A&A...439..845L) for the spectroscopic survey
description and baseline properties
-- Le Brun et al. (2007 in preparation) for the information system
-- Le Fevre et al. (2004A&A...417..839L 2004A&A...417..839L) and McCracken et al.
(2003A&A...410...17M 2003A&A...410...17M) for the photometry
-- Iovino et al. (2005A&A...442..423I 2005A&A...442..423I) for the near-IR photometry
-- Radovich et al. (2004A&A...417...51R 2004A&A...417...51R) for the U-band photometry
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
vvds_dp.dat 307 8981 *The VVDS-DEEP Survey
--------------------------------------------------------------------------------
Note on vvds_dp.dat: the names of the columns in the original catalog
are given in parentheses in the "Byte-by-byte Description" below.
--------------------------------------------------------------------------------
See also:
J/A+A/428/1043 : Redshifts from VIMOS VLT Deep Survey (Le Fevre+, 2004)
J/A+A/439/413 : XMDS/VVDS 4σ catalogue (Chiappetti+, 2005)
J/A+A/463/519 : VVDS-VLA Deep Field: 610MHz catalog (Bondi+, 2007)
http://cencosw.oamp.fr/EN/index.en.html : the CENCOS home page
presenting the Vimos VLT Deep Survey
Byte-by-byte Description of file: vvds_dp.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 I09 --- ID Observation identification (NUM)
12- 16 A5 --- --- [VVDS-]
17- 35 A19 --- Jname Name based on J2000 position (ID_IAU)
40- 49 F10.6 deg RAdeg Right ascension (J2000) (ALPHA_J2000)
54- 63 F10.6 deg DEdeg Declination (J2000) (DELTA_J2000)
68- 72 F5.3 --- z Redshift (Z)
77- 79 I3 --- q_z [1,219] Redshift quality (ZFLAGS) (1)
89 I1 --- phf [0,1] Photometry is
0=questionable, 1=OK (PHOT_FLAG)
97-103 F7.3 mag UEmag ?=-99 AB magnitude in ESO U/360 filter
(MAGAUTOUESO) (2)
109-120 E12.5 mag e_UEmag ?=-99 Mean error on UEmag (MAGERRAUTOUESO)
131-137 F7.3 mag ULmag ?=-99 AB magnitude in Loiano U filter
(MAGAUTOULOIANO) (2)
146-157 E12.5 mag e_ULmag ?=-99 Mean error on ULmag (MAGERRAUTOULOIANO)
163-168 F6.3 mag Bmag ?=-99 AB magnitude in B filter (MAGAUTOB)
171-182 E12.5 mag e_Bmag ?=-99 Mean error on Bmag (MAGERRAUTOB)
188-193 F6.3 mag Vmag ?=-99 AB magnitude in V filter (MAGAUTOV)
196-207 E12.5 mag e_Vmag ?=-99 Mean error on Vmag (MAGERRAUTOV)
213-218 F6.3 mag Rmag ?=-99 AB magnitude in R filter (MAGAUTOR)
221-232 E12.5 mag e_Rmag ?=-99 Mean error on Rmag (MAGERRAUTOR)
238-243 F6.3 mag Imag ?=-99 AB magnitude in I filter (MAGAUTOI)
246-257 E12.5 mag e_Imag ?=-99 Mean error on Imag (MAGERRAUTOI)
262-268 F7.3 mag Jmag ?=-99 AB magnitude in J filter (MAGAUTOJ)
270-282 E13.5 mag e_Jmag ?=-99 Mean error on Jmag (MAGERRAUTOJ)
287-293 F7.3 mag Kmag ?=-99 AB magnitude in K filter (MAGAUTOK)
296-307 E12.5 mag e_Kmag ?=-99 Mean error on Kmag (MAGERRAUTOK)
--------------------------------------------------------------------------------
Note (1):
The last (rightmost) digit characterises the quality of the redshift:
0 = No redshift could be assigned to the 1D spectrum.
1 = 50% confidence in the redshift.
2 = 75% confidence in the redshift.
3 = 95% confidence.
4 = 100% confidence.
9 = Single isolated emission line spectra
A value less than 10 indicates the quality of primary targets, i.e.
objects which have been targeted in the VIMOS spectral slit.
To this quality value, the following number may be added:
+10 = a primary QSO target
+20 = a secondary identified target, i.e. an object which is present
by chance in the spectral slit in addition of the primary target;
thus the secondary object is not ensured to be fully centered
within the slit.
+210 = secondary QSO identified target
Note (2): the two U filters differ slightly:
-- the ESO U filter has a central wavelength of 340nm and a
FWHM of 73nm, has his highest wavelength close to 400nm.
-- the Loiano U filter has a central wavelength of 362nm and a
FWHM of 53nm; it also presents a red leak around 720nm
--------------------------------------------------------------------------------
Acknowledgements:
Chrystel Moreau (chrystel.moreau(at)oamp(fr))
Olivier Le Fevre (Olivier.LeFevre(at)oamp(fr))
(End) Francois Ochsenbein [CDS] 30-Mar-2007