Issue |
A&A
Volume 494, Number 2, February I 2009
|
|
---|---|---|
Page(s) | 443 - 460 | |
Section | Cosmology (including clusters of galaxies) | |
DOI | https://doi.org/10.1051/0004-6361:200809617 | |
Published online | 20 November 2008 |
The great observatories origins deep survey
VLT/VIMOS spectroscopy in the GOODS-south field
P. Popesso1 - M. Dickinson4 - M. Nonino3 - E. Vanzella2,3 - E. Daddi8 - R. A. E. Fosbury5 - H. Kuntschner5 - V. Mainieri7 - S. Cristiani3 - C. Cesarsky7 - M. Giavalisco6 - A. Renzini2 - the GOODS Team
1 - Max-Planck-Institut fur extraterrestrische Physik,, Giessenbachstrasse 2, 85748 Garching, Germany
2 -
Dipartimento di Astronomia dell'Università di Padova,
Vicolo dell'Osservatorio 2,
35122 Padova, Italy
3 -
INAF - Osservatorio Astronomico di Trieste, Via G.B. Tiepolo 11,
40131 Trieste, Italy
4 -
National Optical Astronomy Obs., PO Box 26732, Tucson, AZ 85726, USA
5 -
ST-ECF, Karl-Schwarzschild Str. 2, 85748 Garching, Germany
6 -
Space Telescope Science Institute, 3700 San Martin Drive,
Baltimore, MD 21218, USA
7 -
European Southern Observatory, Karl-Schwarzschild-Strasse 2,
Garching, 85748, Germany
8 -
Université Paris-Sud 11, 15 rue Georges Clemenceau, 91405 Orsay, France
Received 20 February 2008 / Accepted 14 November 2008
Abstract
Aims. We present the first results from the VIsible Multiobject Spectrograph (VIMOS) ESO/GOODS program of spectroscopy for faint galaxies in the Chandra Deep Field South (CDF-S). This program complements the FORS2 ESO/GOODS campaign.
Methods. All 3312 spectra were obtained in service mode with VIMOS at the ESO/VLT UT3. The VIMOS LR-Blue and MR grisms were used to cover different redshift ranges. Galaxies at
1.8 < z < 3.5 were observed in the GOODS VIMOS-LR-Blue campaign. Galaxies at z < 1 and Lyman Break Galaxies at z > 3.5 were observed in the VIMOS MR survey.
Results. Here we report results for the first 12 masks (out of 20 total). We extracted 2344 from 6 LR-Blue masks and 968 from 6 MR masks. A large percentage, 33% of the LR-Blue and 18% of the MR spectra, are serendipitous observations. We obtained 1481 and 656 redshifts in the LR-Blue and MR campaign, respectively, for a total success rate of 70% and 75%, respectively, which decrease to 63% and 68% when also the serendipitous targets are considered. The typical redshift accuracy is
.
The reliability of the redshift estimate varies with the quality flag. The LR-Blue quality flag A redshifts are reliable at
95% confidence level, flag B redshifs at
70% and quality C et
40%. The MR redshift reliability is somewhat higher: 100% for quality flag A,
90% for quality flag B and
70% for flag C. By complementing our VIMOS spectroscopic catalog with all existing spectroscopic redshifts publicly available in the CDF-S, we created a redshift master catalog. By comparing this redshift compilation with different photometric redshift catalogs we estimate the completeness level of the CDF-S spectroscopic coverage in several redshift bins.
Conclusions. The completeness level is very high, >60%, at z < 3.5, and it is very uncertain at higher redshift. The master catalog was used also to estimate completeness and contamination levels of different galaxy photometric selection techniques. The BzK selection method leads to a 86% complete sample of z > 1.4 galaxies at
iAB < 25 mag and with a contamination
23% of lower redshift objects. The so-called ``sub''-U-dropout and the U-dropout methods lead to an 80% complete galaxy sample at z > 1.4 and
iAB < 25 mag, with
24% low redshift contaminants.
Key words: cosmology: observations - cosmology: large-scale structure of Universe - galaxies: evolution
1 Introduction
The Great Observatories Origins Deep Survey (GOODS) is a public, multi-facility project that aims at answering some of the most profound questions in cosmology: how did galaxies form and assemble their stellar mass? When was the morphological differentiation of galaxies established and how did the Hubble sequence form? How did AGN form and evolve, and what role do they play in galaxy evolution? How much do galaxies and AGN contribute to the extragalactic background light? A project of this scope requires large and coordinated efforts from many facilities, pushed to their limits, to collect a database with sufficient quality and size for the task at hand. It also requires that the data be readily available to the worldwide community for independent analysis, verification, and follow-up.
The program targets two carefully selected fields, the Hubble Deep Field North (HDF-N) and the Chandra Deep Field South (CDF-S), with three NASA Great Observatories (HST, Spitzer and Chandra), ESA's XMM-Newton, and a wide variety of ground-based facilities. The area common to all the observing programs is 320 arcmin2, equally divided between the North and South fields. For an overview of GOODS, see Dickinson et al. (2003), Renzini et al. (2003) and Giavalisco et al. (2004).
Spectroscopy is essential to reach the scientific goals of GOODS.
Reliable redshifts provide the time coordinate needed to delineate the
evolution of galaxy masses, morphologies, clustering, and star
formation. They calibrate the photometric redshifts that can be
derived from the imaging data at 0.36-8 m. Spectroscopy will
measure physical diagnostics for galaxies in the GOODS field (e.g.,
emission line strengths and ratios to trace star formation, AGN
activity, ionization, and chemical abundance; absorption lines and
break amplitudes that are related to the stellar population
ages). Precise redshifts are also indispensable to properly plan for
future follow-up at higher dispersion, e.g., to study galaxy
kinematics or detailed spectral-line properties.
The ESO/GOODS spectroscopic program is designed to observe all galaxies in the CDF-S field for which VLT optical spectroscopy is likely to yield useful data. The program is organized in two campaigns, carried out at VLT/FORS2 at UT1 and VLT/VIMOS at UT3. The program makes full use of the VLT instrument capabilities, matching targets to instrument and disperser combinations in order to maximize the effectiveness of the observations.
The FORS2 campaign is now completed (Vanzella et al. 2005, 2006,
2008). 1715 spectra of 1225 individual targets have been observed and
887 redshifts have determined as a result. Galaxies have been selected
adopting three different color criteria and using photometric
redshifts. The resulting redshift distribution typically spans two
redshift domains: from z=0.5 to 2 and z=3 to 6.5. The reduced
spectra and the derived redshifts have been released to the community
through the ESO web pages
http://archive.eso.org/cms/eso-data/data-packages. The typical
redshift uncertainty is estimated to be
.
We have carried out the VIMOS ESO/GOODS spectroscopic survey to complement
the observations done with the FORS2 instrument, in order to ensure optimal
completeness and sky coverage. The FORS2 campaign was designed to take
advantage of that instrument's very high throughput at red wavelengths.
This was particularly important for detecting rest-frame optical and
near-ultraviolet spectral features (such as the [OII]3727 Å emission
line) out to
,
and rest-frame UV emission and absorption
lines at z > 4. The GOODS VIMOS campaign, in turn, takes advantage of
that instrument's very large field of view and multiplexing capability,
and its good instrumental throughput at roughly 360-900 nm. This enables
us to measure large numbers of redshifts at z < 1.4 from the [OII]3727 Å
emission line and other optical and near-UV features, as well as redshifts
at
1.5 < z < 3.5 from Lyman
emission and rest-frame UV absorption
lines. The cumulative source counts on the CDF-S field taken from the deep
public FORS1 data (Szokoly et al. 2004), show that down to
VAB=25 mag
there are
6000 objects over the 160
of the GOODS field.
The high multiplexing capabilities of VIMOS at VLT make it possible to reach
the desired redshift completeness in a reasonable amount of observing time.
The GOODS VIMOS program used two different observational configurations,
with different object selection criteria for each. Observations with the
Medium Resolution (MR) orange grism target galaxies in the redshift ranges
0.5 < z < 1.3 (primarily from [OII]) and z > 3.5 (from Ly ).
Observations with the low resolution blue (LR-Blue) grism cover the
wavelengths of Ly
and UV rest-frame absorption lines at
1.8 < z < 3.5, a range not covered by the FORS2 spectroscopy.
On average,
330 objects at a time have been observed with the low
resolution (
)
blue grism and
140 with the medium resolution
(
orange grism. The overall goal of the GOODS spectroscopic
campaign was to reach signal-to-noise ratios adequate for measuring redshifts
for galaxies with AB magnitudes in the range
24-25, in the B-band
for objects observed with the VIMOS LR-Blue grism, in the R-band for objects
observed with the VIMOS MR grism, and in the z-band for objects
observed with FORS2.
In this paper we report on the first 60% of the VIMOS spectroscopic follow-up campaign in the Chandra Deep Field South (CDF-S), carried out with the VIMOS instrument at the VLT from ESO observing periods P74 through P78 (mid-2004 through early 2007). 10 masks have been observed in the LR-Blue grism and 10 with the MR grism. Here we report results for the first 6 masks that have been analyzed from each of the LR-Blue and MR grisms.
The paper is organized as follows: in Sect. 2 we describe the survey
strategy and in Sect. 3 the observations and the data reduction. The
details of the redshift determination is presented in Sect. 4. In
Sect. 5 we discuss the data and in Sect. 6 the reliability of the
photometric techniques used to identify the high redshift targets. In
Sect. 7 we present our the conclusions. Throughout this paper the
magnitudes are given in the AB system (
), and the ACS F435W,
F606W, F775W, and F850LP filters are denoted hereafter as B435,
V606, i775 and z850, respectively. We assume a
cosmology with
and H0 = 70 km s-1 Mpc-1.
2 The survey strategy
2.1 The VIMOS instrument
The VIsible MultiObject Spectrograph (VIMOS) is installed on the
ESO/VLT, at the Nasmyth focus of the VLT/UT3 ``Melipal'' (Le Fevre et al. 2003). VIMOS is a 4-channel imaging spectrograph, each channel (a
``quadrant'') covering
for a total
field of view (a ``pointing'') of
218
.
Each
channel is a complete spectrograph, using either broad band filters
for direct imaging, or
slit masks
at the entrance focal plane and grisms to disperse spectra onto
EEV CCDs.
The pixel scale is 0.205 arcsec/pixel, providing excellent sampling of
the Paranal mean image quality and Nyquist sampling for a slit width
of 0.5 arcsec. The spectra resolution ranges from 200 to
5000. Because of the large field of view of the instrument
(
)
and the lack of an atmospheric
dispersion compensator, observations are restricted to 1.1 airmasses
to minimize the loss of light due to atmospheric refractions.
In the MOS mode of observations, short ``pre-images'' are taken ahead of the observing run. Sources from a user-supplied catalog of targets are identified with objects in the pre-images in order to map the celestial coordinates of the observer's targets to the instrumental coordinate system. The slit masks are then prepared using the VMMPS tool, provided by ESO, with an automated optimization of slit number and position (see Bottini et al. 2005).
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Figure 1: Example of the VIMOS field coverage of the GOODS area in the CDF-S. Only three pointings from the VIMOS-MR campaign are shown for clarity. Each color indicates the position of one instrument quadrant in the three different pointings. |
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2.2 The field coverage: VIMOS pointing layout
The VIMOS geometry (
,
with a cross gap of
between the quadrants) is such that only 50% of its instantaneous field of view
can overlap with the
region that roughly defines
the GOODS-CDFS field. At least 3 VIMOS pointings are required to cover the
whole GOODS area (see Fig. 1), filling the gaps between the
spectrograph quadrants, and some fraction of the VIMOS coverage will fall
outside the nominal GOODS area. The VIMOS multiplex allows observations
to target an average of
360 objects per pointing in the case of
the Low Resolution (LR) grism and
150 objects in the case of the Medium
Resolution (MR) grism. Before the program began, we estimated that 10 Low Resolution
and 10 Medium Resolution masks (on average 3 LR and 3 MR masks per pointing)
would be needed to achieve
96% completeness in the spectroscopic coverage
of
6000 targets. With an average integration time of 4 h per mask and
30% overheads, the observations therefore required a total of 125 h.
2.3 Target selection
Several categories of object selection criteria were used to ensure a sufficiently high density of target candidates on the sky to efficiently fill out multi-slit masks. Different criteria were used for the low resolution ``LR-Blue'' grism and the medium resolution ``MR Orange'' grism, based on the wavelength coverage of each instrumental configuration and the redshift ranges expected for the targeted objects. In general, the target selection strategy was designed to take advantages of VIMOS' strengths (very large multiplex, and the comparative blue sensitivity of the LR-B grism) and to complement those of other instruments being used in the overall GOODS spectroscopic effort (e.g., the high red throughput of FORS2). The VIMOS selection criteria were adjusted over the course of the multi-year observing campaign to optimize the survey success rate. Target catalogs were updated as the available GOODS imaging and photometric data improved (e.g., as the HST/ACS campaign was completed, and as VLT/ISAAC imaging coverage expanded concurrent with the spectroscopic campaign). The target lists were also updated to take into account partial results of this and other spectroscopic surveys (e.g., GOODS/FORS2, VVDS).
For the portion of the VIMOS field of view that overlaps the GOODS-S area proper, targets were selected for observation mainly using photometry from the GOODS-S HST/ACS and VLT/ISAAC imaging, as well as CTIO 4 m/MOSAIC U-band imaging. Slits outside the ACS and ISAAC coverage were populated by targets (mainly U-dropout and ``sub-U-dropout'' Lyman break galaxies) selected using ground-based optical data, primarily BVRI imaging from the ESO 2.2 m WFI and U-band data from the CTIO 4 m. We summarize here the imaging data, source catalogs, and the main selection criteria used during the GOODS VIMOS survey in ESO observing periods P74-P78:
- CTIO 4 m MOSAIC U-band imaging and ESO 2.2 m WFI B- and R-band
imaging, covering the
``Extended'' CDF (ECDFS), with AB magnitude 5
depths 26, 26.2 and 25.8 mag, respectively (Giavalisco et al. 2004), used for Lyman break U-dropout and ``sub-U-dropout'' color selection, both inside and outside the nominal GOODS-S area. Source detection was done in the R-band image, and colors were measured through matched apertures in each band using data whose point spread functions were matched to achieve common angular resolution. The WFI R-band catalog also served as the primary astrometric reference catalog for mask design, and to define R-band magnitude limits for all samples targeted with VIMOS;
- HST-ACS B435 (B-band) and F850LP (z-band) imaging, covering the
GOODS-S field (approximately 165 arcmin2) with depth 27.8 and 27.4 mag
(Giavalisco et al. 2004), used for the BzK color-selection technique
within GOODS-S proper;
- VLT-ISAAC
-band imaging covering the GOODS-S field with depth 25.1 mag (Retzlaff et al. in preparation), for applying the BzK selection technique in GOODS-S field. Source detection was done in a mosaic of the ISAAC
images, and photometry colors were measured through matched apertures on binned mosaics of the HST/ACS images, degraded to match the PSF of the ISAAC data;
- Chandra Deep Field South X-ray catalog (Giacconi et al. 2002;
Lehmer et al. 2005), covering an area somewhat larger than GOODS-S,
with approximate sensitivity
(in detail, varying with distance from the Chandra aim point at the field center).


- U-dropouts: Lyman break color selection of galaxies using
the CTIO U and WFI B and R photometry. See Sect. 6 and
Lee et al. (2006) for a detailed description of the selection criteria.
This method was applied over the whole VIMOS area, both inside and
outside the GOODS-S region proper. These criteria are designed
to select blue, star-forming galaxies at
;
- so-called ``sub-U-dropouts'': UBR color-selected objects with
U-B colors somewhat bluer than those of the normal
U-dropout Lyman break selection criteria, similar to ``BX'' selection criterion of Adelberger et al. (2004); see Sect. 6 for the detailed description of the selection criteria. These criteria are designed to select star-forming galaxies at somewhat lower redshifts than those of the regular U-dropouts, nominally
to 2.5;
- BzK color-selection (Daddi et al. 2004). The BzK method
uses galaxies detected initially in the K-band, with color criteria
designed to select galaxies at
1.4 < z < 2.5, largely independent of
their stellar population or dust reddening properties. Late in the
VIMOS campaign, we also experimented with applying additional
Spitzer/IRAC color criteria to refine the BzK method, but this is
largely unimportant for the purposes of the present discussion;
- X-ray sources from the CDF-S and E-CDF-S X-ray catalogs
(Giacconi et al. 2002; Lehmer et al. 2005).
The wavelength range of the VIMOS MR grism is
4000-10 000 ,
similarly to that of FORS2. However, the fringing at red wavelength
(
)
is somewhat stronger than in FORS2, and
the VIMOS red throughput is lower. Hence, optical rest-frame spectral
features for galaxies at z > 1, and the ultraviolet rest-frame spectral
features of Lyman break galaxies (LBGs) at
,which would
appear at very red optical wavelengths, are harder to detect with VIMOS
than with FORS2. Therefore, our VIMOS target selection was limited to
brighter galaxies (mainly expected to be at z < 1.2), and to color-selected
LBGs in the redshift range
2.8 < z < 4.8. As for the LR-Blue campaign,
target selection used the available imaging data and photometry
catalogs according to the following criteria:
- 1.
- galaxies with R < 24.5, with no other color pre-selection,
excluding VIMOS LR-Blue targets and objects already observed in other
spectroscopic programs. In the later VIMOS campaigns, some preference
was given to galaxies detected at 24
m from the GOODS Spitzer MIPS data (Dickinson et al. in preparation; Chary et al. in preparation), meeting the same R < 24.5 mag limit. We do not consider the MIPS-detected sources as a separate category for the purposes of this paper;
- 2.
- relatively bright Lyman break galaxies at
i775 < 25, selected
as B435, V606 dropouts (nominally, redshifts
and 5, respectively), according to the same color criteria described in Vanzella et al. (2005, 2006, 2008).
3 Observations and data reduction
The VLT/VIMOS spectroscopic observations were carried out in service mode during ESO observing periods P74-P78.
3.1 Preparation of VIMOS observations
For each pointing a
short V-band image was taken with VIMOS in advance of the spectroscopic
observations. We used this pre-imaging, together with the GOODS WFI R band
image, to derive the transformation matrix from the (,
)
celestial reference frame of the target catalogs to the
(
,
)
VIMOS instrumental coordinate system. This
procedure was carried out using the routines geomap and
geoxytran in the IRAF environment. The rms of the residuals
from these transformations were
0.05 arcsec, ten times better
than the accuracy of the matching procedure implemented in the VIMOS mask
preparation software (VMMPS, Bottini et al. 2005). This is due to the
choice of a higher order polynomial of the fitting procedure, which is
not allowed in VMMPS.
Once the target catalog was expressed in the (
,
)
VIMOS instrumental coordinate system, the next steps in the slit mask
design were conducted with the VMMPS tool. After placing two reference
apertures on bright stars for each pointing quadrant, slits were assigned
to sources drawn from the target catalog. The automated SPOC (Slit Positioning
Optimization Code, Bottini et al. 2005) algorithm was run to maximize
the number of slits assigned, given the geometrical and optical constraints
of the VIMOS set-up. We designed masks with slit widths of one arcsec,
and required that a minimum of 1.8 arcsec of sky is left on
each side of a targeted object to allow for accurate sky background
fitting and removal during later spectroscopic data processing.
The spectral range of the VIMOS LR-Blue masks, projected onto the
VIMOS CCDs, is short enough that it is possible to have several ``layers''
of slits whose spectra do not overlap in the dispersion axis.
Because of this spectral multiplexing, each GOODS LR-Blue mask could
include up to 360 slits in the combined four quadrants. Masks for the
VIMOS MR grism were designed with no multiplexing in the dispersion
axis to avoid the superposition of zero and negative orders.
The combined four quadrants of a GOODS MR mask contained 150 slits
on average. The observations were dithered to move targets along the
axis of the slits in order to improve the sky subtraction and the removal
of CCD cosmetic defects. In the LR-Blue survey, the dithering pattern consisted
of three position separated by a step of 1.4 arcsec. In the MR survey,
the dithering pattern consisted of five position separated by a step of
1.5 arcsec, in order to provide enough independent pointings to construct
and apply a correction for fringing at red wavelengths (see Sect. 3.2).
In the LR-Blue campaign, we used the LR-Blue grism together with
the OS-Blue cutoff filter, which limits the bandpass and order
overlap. With 1 arcsec slits, the spectral resolution is 28
and the dispersion is 5.7
.
10 exposures of 24 min
each were taken for a total exposure time of 4 h per mask. In the MR campaign, the MR grism was used together with the GG475
filter. With 1 arcsec slits, the resolution is
13
and the
dispersion is 2.55
.
12 exposures of 20 min each
were taken for a total exposure time of 4 h per mask. We requested
nightly arc-lamp calibrations to measure the wavelength solution of
the spectra and reduce problems due to instrument flexure.
3.2 Data reduction
The pipeline processing of the VIMOS-GOODS
data is carried out using the VIMOS Interactive Pipeline Graphical
Interface (VIPGI, see Scodeggio et al. 2005, for a full description).
The data reduction is performed in several interactive steps:
locating the spectra in the individual spectroscopic frames,
wavelength calibration, sky subtraction and fringing correction,
combination of the 2D spectra of dithered observations, extraction of
the 1D spectra, and flux calibration. The location of the slits is
known from the mask design process, hence, knowing the grism zero
deviation wavelength and the dispersion curve, the approximate location
of each spectrum on the detectors is known a priori. However, small
shifts from the predicted
positions are possible. From the predicted position, the location of the
spectra are identified accurately on the 4 detectors and an extraction
window is defined for each slit. The wavelength calibration is
secured by the observation of nightly arc-lamps through each slit
mask. Wavelength calibration spectra are extracted at the same
location as the object spectra and calibration lines are identified to
derive the pixel to wavelength mapping for each slit. The wavelength
to detector pixel transformation is fit using a third order
polynomial, resulting in a median rms residual of 0.7
across the wavelength range in the LR-Blue masks and
0.36
in the MR masks. A low order polynomial (second order) is fit along
the slit, modeling the sky background contribution at each wavelength
position, and subtracted from the 2D spectrum. For the LR-Blue data,
fringing is not present, and all 10 exposures of a
sequence are directly combined by shifting the 2D spectra following
the offset pattern to register the object at the same position. The
individual frames are combined with a median, sigma-clipping algorithm
to produce the final summed, sky subtracted 2D spectrum. In the case
of the Medium Resolution spectra, the fringing is significant at
and needs to be removed. Therefore, a fringing
correction is applied before combining the dithered exposures. As the
object is moved to different positions along the slit following the
dithering pattern, the median of the 2D sky subtracted spectra produces a
frame from which the object is eliminated, but that includes all
residuals not corrected by sky subtraction, in particular the fringing
pattern varying with position across the slit and wavelength. This
sky/fringing residual image is then subtracted from each individual 2D sky subtracted frame. The fringing corrected frames are then shifted
and combined as in the case of the LR-Blue spectra.
The last step done automatically by VIPGI is to extract a 1D spectrum from the summed 2D spectrum, using an optimal extraction following the slit profile measured in each slit (Horne 1986). The 1D spectrum is flux calibrated using a transformation computed from observations of spectrophotometric standard stars.
Final, we checked each 1D calibrated spectra individually, and removed the most discrepant features manually, cleaning each spectrum of zero order contamination, strong sky lines residuals and negative unphysical features.
3.3 The VIMOS LR-Blue wiggles
Spurious wiggles with amplitude of about 3 to 8% are found in VIMOS MOS spectra taken with the combination of LR_Blue grism and OS_Blue Order Sorting (OS) filter. The position of the wiggles in the spectrum compares well with the wiggles in the response curve of the OS_Blue filter (see also the ESO VIMOS User Manual, Fig. A.3). This clearly indicates that the wiggles originate in the OS filter. The effect of the wiggles should therefore be multiplicative. In principle, spectroscopic screen flat-fields, even taken during the day, would be sufficient to correct the wiggles. However, several aspects make this correction very difficult. The position and amplitude of the wiggles are found to depend on the spectral resolution, which in turn depends on slit width and object size. The wiggle pattern and the overall shape of the flat field spectra depend significantly on the position of the slit in the field of view. In addition, the normalization of flat field spectra is made problematic by the possible overlap of 0th-order spectra from neighboring slits. For these reasons we prefer not to correct the wiggles observed in the LR-Blue spectra.
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Figure 2:
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3.4 Target coordinates
The rotation angle of the VIMOS
GOODS pointings (-20 deg) is different from the default values
accepted by VIPGI (0 and 90 deg). Therefore, VIPGI does not provide the
astrometry of the extracted spectra. The only information provided by
VIPGI are the coordinates in mm on the focal plane stored in the
VIPGI object table. To overcome this problem, we
transform the focal plane coordinates of each object into CCD
coordinates using the appropriate distortion solution recorded in the headers
of our VIMOS observations. Slits which contain only one object (only
one spectrum extracted) are used to calculate the transformation
matrix from VIMOS coordinates to the GOODS R-band WFI CCD coordinates through
the IRAF routines geomap and geoxytran. Finally, the
WFI
and
assigned to each extracted spectrum are
converted to
,
on the basis of the GOODS WFI R-band
astrometry. These ``reconstructed'' coordinates are, then, matched to
the original GOODS VIMOS target catalog to identify the primary
targets as well as any serendipitous objects extracted from our slits.
For objects that match, we assign the original coordinates of the target
GOODS catalog. Otherwise the ``reconstructed'' coordinates are used. The
coordinate conversion is done separately quadrant by quadrant. Figure 2 shows the distribution of the
and
in the cross-correlation of the reconstructed WFI coordinates and the
original targets coordinates. The very strong distortion of the VIMOS
CCD is not completely removed, as indicated by the trend in the
-
distribution shown in the main panel. This is due to
the fact the we can use few objects to calculate the transformation
matrix from VIMOS to the GOODS R-band WFI CCD coordinates. However,
the rms of the cross-correlation is smaller than 0.2 arcsec in both
coordinates, allowing for reliable identification of the targets
from the imaging catalogs.
It is worth noting that, due to a bug, VIPGI assigns incorrect focal
plane coordinates to a small number of objects in slits from which
more than two spectra were extracted. In the released catalog the
slit center coordinates are assigned to these objects, with an
uncertainty of 5 arcsec. These objects are, then, normally
processed in the data reduction procedure. We find 82 cases of this
from the LR-Blue campaign, of which 80% have no redshift
determination, and 34 in the MR campaign, of which 50% have no
redshift determination. The failures to measure redshifts are
simply due to the low S/N in these spectra. Those objects are
given focal plane coordinates
.
Moreover, on the
basis of the reconstructed WFI coordinates, these objects would be
located completely out of the slits where they should be. The complete
list of those objects is available at
http://archive.eso.org/cms/eso-data/data-packages.
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Figure 3:
Redshift differences between objects observed twice or more
in independent VIMOS LR-Blue ( left panel) and MR ( right panel)
observations. The distribution has a dispersion of
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4 Redshift determination
2344 spectra have been extracted from the 6 LR-Blue masks and 968 have been extracted from 6 MR masks. From these, we have been able to determine 1481 redshifts in the LR-Blue campaign and 656 in the MR campaign. 33% of the LR-Blue slits and 18% of the MR slits contain more than one spectrum. Most of the secondary spectra obtained provide additional observations of known targets. We have identified 2235 unique LR-Blue objects and 886 unique MR objects.
Redshift estimation has been performed by cross-correlating the individual observed spectra with templates of different spectral types. Templates for ordinary S0, Sa, Sb, Sc, and elliptical galaxies were used to measure redshifts of relatively low redshift galaxies. At higher redshifts, where the VIMOS observations mainly sample the ultraviolet rest frame, several different spectral templates for Lyman break galaxies, BzK-selected galaxies, and AGN were used. The cross-correlation is carried out using the rvsao package (xcsao routine, Kurtz & Ming 1998) in the IRAF environment. In particular, a trial-and-error approach is used for the z > 1.8 galaxies, whose redshift determination is made difficult by the low S/N ratio of the spectral absorption features and the wiggles in the LR-Blue spectrum.
In the large majority of the cases the redshift has been determined through the identification of prominent features of galaxy spectra:
- at low redshift the absorption features: the 4000 Å break, Ca H and
K, H
and H
in absorption, g-band, MgII 2798;
- and the emission features: [O II]3727, [O
III]4959,5007, H
, H
;
- at high redshift: Ly
, in emission and absorption, ultraviolet absorption features such as [Si II]1260, [O I]1302, [C II]1335, [Si IV]1393,1402, [S II]1526, [C IV]1548,1550, [Fe II]1608 and [Al III]1670 (see also Fig. B.1 of the appendix).
- flag A: high quality, values of the xcsao correlation
coefficient
; emission lines and strong absorption features are well identified;
- flag B: intermediate quality, values of the xcsao correlation
coefficient
; one emission line plus few absorption features are well identified;
- flag C: low quality, values of the xcsao correlation coefficient R < 3, features of the continuum not well identified.
- flag X: no redshift estimated, no features identified.




In
of the cases the redshift is based only on one emission
line, usually identified with [O II]3727 or Ly
.
In
these cases, the continuum shape, the presence of breaks, the absence
of other spectral features in the observed spectral range, and the
broad band photometry are considered in the redshift evaluation.
In general these solo-emission line redshifts are classified as
``likely'' (B) or ``tentative'' (C) if no other information is
provided by the continuum. In a few cases, the quality flag is set
to A if the photometry or the availability of photometric redshifts
help in distinguishing between high and low redshift sources (see
Kirby et al. 2007, for the DEEP2 survey).
The internal redshift accuracy can be estimated from a sample of
galaxies which have been observed twice in independent VIMOS mask
sets. We find 39 such cases in the LR-Blue masks and 40 in the
MR masks, with quality flag A or B.
of these objects have
been observed as serendipitous targets. The distribution of measured
redshift differences is presented in Fig. 3. The mean
of the
distributions is close to zero (
10-5)
for both the LR-Blue and MR observations. The redshift dispersion is
(
400
)
for the LR-Blue objects
and
(
200
)
for the MR redshifts.
This latter estimation is in very good agreement with the value obtained
in the GOODS-FORS2 survey (Vanzella et al. 2005), conducted on similar
objects using similar spectral resolution and spectral range as VIMOS
MR. We note that the mean values of the redshift estimation
uncertainty estimated in this way are
3 times larger than the
mean error (
in the LR-Blue survey and
in the MR survey) calculated by the IRAF routine
xcsao.
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Figure 4: Color-magnitude diagram of the LR-Blue and MR primary targets. The first panel shows the B-R vs. B diagram for A and B high quality LR-Blue redshifts. Low quality LR-Blue redshifts (C flag, dots) and failure (X flag, stars) are shown in the central panel. The bottom panel shows the i-z vs. z diagram for the MR primary targets. The black dots are the high quality (A and B flag) MR redshifts at z < 0.8, the empty circles are high quality (A and B flag) MR redshifts at z > 0.8. The stars represent the C and X cases. |
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4.1 The success rate
4.1.1 The VIMOS LR-Blue targets
We measured redshifts for 70% (63% including also the secondary
serendipitous objects) of the observed LR_Blue spectra. However, to
estimate the success rate of the surveys we use only the objects with
high quality flags, A and B. In the LR-Blue survey the success rate is
48% for the original target sample and 39% if we consider also the
secondary targets. The serendipitous sources, which account for 33% of the sample, are usually faint neighbors and lie often at the edge
of the 2D spectrum. Moreover, they are not subject to the color
pre-selection used for the primary LR-Blue targets, and it is likely that
they often lie at redshifts which are not accessible to the wavelength
range covered by the VIMOS LR-Blue grism (see Sect. 5.1 for details).
For these objects the success rate is very low, .
We have
investigated how the success rate depends on the target selection and
on the redshift windows. Figure 4 shows the color-magnitude
diagram of different targets and for different redshift quality. In
particular, the first and central panels show the B-R vs. B diagram of
the LR-Blue targets in case of successful redshift determination (top
panel) and in case of failure (C or X cases). The latter cases lie all
at very faint B magnitudes, indicating that the failures are mainly
due to the poor S/N of the spectra. As described in Sect. 2.2, the
LR-Blue targets can be divided in 4 families: U-dropouts, BzK objects,
sub-U-dropouts and X-ray sources. The BzK and sub-U-dropouts samples
have considerable overlap. In this discussion, we consider these two
families separately. Table 1 shows the fraction of targets observed
in the analyzed masks and the corresponding success rate for each
target family. The BzK objects have the lowest success rate. 64% of
those objects have flag C or no redshift (flag X).
All of the other target families have a success rate of
.
In addition we find a strong dependence of the success
rate on the redshift window. In particular:
- objects at low redshift (
) and in the range
have the highest fraction of A flags,
;
- very high redshift galaxies (
) have mainly quality flag B because the Ly
in emission is in the very red part of the spectrum, and other features are not well identified;
- objects at
show the highest fraction of insecure redshift determinations (percentage of the C flag determination
).






4.1.2 The MR targets
We measured redshifts for 75% (67% including also the secondary
serendipitous objects) of the observed MR spectra. In the VIMOS MR
campaign the overall success rate (A+B flag redshifts) is 60% and
reaches the 65% level if only the primary targets are considered. We
do not note any dependence on the target selection criteria or
redshift windows. The bottom panel of Fig. 4 shows the i-zvs. z diagram for the MR primary targets. The black dots are the high
quality (A and B flag) MR redshifts at z < 0.8, the empty circles are (A
and B flag) MR redshifts at z > 0.8. The stars represent the C and X
cases. The C and X cases are concentrated in the region populated by
objects at z > 0.8. This is due to the fact that above this redshift
the main spectral features enter the wavelength range where both the OH
sky emission lines and the CCD fringing are strong, at
Å, making line identification very difficult.
5 Discussion
5.1 Reliability of the redshifts - comparison with previous surveys
A practical way to assess the reliability of the redshifts is to compare the present results with independent measurements from other surveys. For this purpose we use the results of four other surveys conducted on the same field: the GOODS-FORS2 campaign (Vanzella et al. 2005, 2006, 2008), which mainly targeted faint galaxies whose red i-z colors imply redshifts z > 1, as well as z > 3.5 Lyman break galaxies; the K20 survey of K-band selected galaxies (Cimatti et al. 2002); the Szokoly et al. (2004) survey of (mainly) CDFS X-ray sources; and the VVDS survey (Le Fevre et al. 2005), which was limited by I-band apparent magnitude and the IMAGES survey (Ravikumar et al. 2007) limited to MJ < -20.3. To create a secure redshift reference sample, we have selected only the high quality redshift determinations of those surveys: GOODS FORS2 quality A and B, K20 quality 1, VVDS quality 3 and 4 and Szokoly et al. 2004 quality 3 and 2+ redshifts, which all nominally have a confidence level higher than 95%.
Among the LR-Blue redshift determinations, there are 113 VIMOS objects
in common with this high quality reference sample within an angular
matching tolerance of 0.5 arcsec. 58 of them have VIMOS quality flag A, 16 have flag B, 16 have flag C and 23 do not have a redshift
estimation (flag X). These 23 quality X objects have redshifts in the
other surveys that fall in the redshift range
0.8 < z < 1.7, which is
not readily accessible to the VIMOS LR_Blue observations given their
wavelength coverage. 27 cases of the A, B and C quality redshifts show
``catastrophic'' discrepancies
(
). These account for 5 of the
VIMOS flag A objects, 8 of the flag B sources, and 11 of the flag C sources.
After visual comparison of the VIMOS and FORS2/K20/CDF/VVDS spectra we find that 3 of the 5 VIMOS quality A spectra with ``catastrophic'' discrepancies are likely to be incorrect GOODS/VIMOS redshift determinations:
- -
- VIMOS GOODS_LRb_001_q2_1_1 versus FORS2
GDS_J033217.78-274823.8 (flag A): the [OIII] in emission is
identified in the FORS2 spectrum and it is hidden by a strong sky line
residual in the VIMOS spectrum. Thus, the [OII] in the VIMOS spectrum
is misclassified as Ly
due to the absence of
and [OIII] emissions.
- -
- VIMOS GOODS_LRb_001_1_q1_51_1 versus FORS2
GDS_J033226.67-274013.4 (flag A): the [OII] in the FORS2 spectrum is
identified at z=1.612, a redshift window not accessible to VIMOS
LR-Blue. No emission lines are visible in the VIMOS spectrum and the
low S/N UV absorption features are misclassified.
- -
- VIMOS GOODS_LRb_001_q2_35_1 versus VVDS
VVDS 32126 (flag 3, observed with the VIMOS LR-Red grism):
the strong UV absorption features identified in our VIMOS LR-Blue
spectrum provide a xcsao correlation coefficient similar to
that of the FeII and NeV absorption features identified in the VVDS LR-Red
spectrum. We have combined the two spectra and re-performed the cross
correlation. The highest correlation peak corresponds to the VVDS
redshift value
- -
- VIMOS GOODS_LRb_001_q3_71_2 versus VIMOS LR-Red VVDS
16975 (flag 24): the VIMOS LR-Blue source is an emission line galaxy
and the reference VVDS spectrum is clearly an early type galaxy
without any emission line. The two spectra can not refer to the same
object. Since 16975 is a secondary object and not a primary target,
we suspect that the coordinates provided by VIPGI (used to reduce
the VVDS data) could be wrong as explained in Sect. 3.4. Thus, we
consider our VIMOS redshift estimation correct, although the object
identification may be incorrect.
Table 1: Success rate of the GOODS VIMOS LR-Blue campaign. The first column lists the name of the target family, the second column lists the fraction of the target catalog due to the corresponding color selection (BzK and sub-dropout family overlap largely but they are considered as separated family in the table). The third column lists the success rate (fraction A+B flag objects) of each target family. The last four columns list the percentage of A, B, C and X flag redshift determinations, respectively.
- -
- VIMOS GOODS_LRb_002_q2_55_1 versus FORS2
GDS_J033221.94-274338.8 (flag A): the strong emission line in the VIMOS
spectrum is identified as a Ly
due to the absence of
and [OIII] emission and due to the photometry (the target was selected to be a U-dropout). The emission line could be classified as a [OII] at much lower redshift (z=0.166) with a much lower xcsao correlation coefficient. In either case, the FORS2 redshift is not in agreement. We have combined the two spectra and re-measured the redshift. The correlation gives a good result only with a Ly
emitter template at z=2.576. No match is found for the emission seen in the FORS2 spectrum, which has a very low S/N. We think that the line identified as [OII] in the FORS2 spectrum is instead due to a fringing residual since it is sitting on a sky line. Thus, we believe that the VIMOS redshift estimation is likely to be correct.


The comparison between the VIMOS MR redshift determinations and FORS2/K20/CDF/VVDS measurements is simplified by the fact that our MR observations cover a similar wavelength range to those observed in the other surveys. There are 94 VIMOS objects in common with the high quality reference sample within a positional tolerance of 0.5 arcsec. 69 of them have VIMOS quality flag A, 17 have quality flag B and 8 have quality flag C. We find 5 ``catastrophic'' discrepancies: 1 has flag A, 1 has flag B and 3 have flag C:
- -
- flag A case GOODS_MR_new_1_d_q3_22_1 versus FORS2 GDS_J033243.19-275034.9 (flag A): an accurate analysis is provided by Vanzella et al. (2006, see their Fig. 2). The continuum shows increasing bumps/bands in the red, very similar to typical cold stars. After visual inspection of the ACS color image Vanzella et al. (2006) concluded that GDS_J033243.19-275034.9 is a simultaneous spectrum of two very close sources: a star and a possible high-z galaxy;
- -
- B flag case VIMOS GOODS_MR_new_1_d_q2_21_2 versus FORS2
GDS_J033249.04-2705015.5 (flag A): the spectral features used to
identify the VIMOS redshift are all at
, where the fringing is very strong. The corresponding FORS2 spectra, which suffer less of fringing, show more convincing spectral features.
Thus, we obtain a confidence level of 98% for the quality A MR redshifts (1 mistake out of 69 redshifts), 94% for the quality B redshifts (1 mistakes out of 17 determinations) and 62% for the
quality C cases (3 mistakes out of 8 determinations). The overall
confidence level of the redshift determinations of the MR redshift
survey is 95%. For the 89 cases out of 94 which show good agreement,
we find a mean difference
.
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Figure 5:
Comparison of the GOODS-MUSIC and the GOODS photometric
redshift catalog. The small inset panel shows the distribution
of redshift differences,
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Figure 6:
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Figure 7:
Completeness level of the VIMOS survey (filled squares)
and of the GOODS-S master catalog (empty squares) as a function of the
I ( left panel) and |
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5.2 Reliability of the redshifts - comparison with photometric redshift
An alternative way to assess the reliability of the redshifts is to
compare the present results with accurate photometric
redshifts. Photometric redshift determinations are inevitably plagued
by a rather high incidence of catastrophic failures, and can exhibit
biases depending on the redshift determination procedure applied. Thus,
to partially mitigate these concerns, we simultaneously consider two different
photometric redshift catalogs: the GOODS-MUSIC catalog (Grazian et al. 2006) and a GOODS photometric redshift catalog (Daddi et al.,
private communication). The GOODS-MUSIC photometric redshifts are
based on a high quality multiwavelength (from 0.3 to 8.0 mm)
catalog, which includes accurate ``PSF-matched'' ACS, JHKs ESO VLT,
Spitzer IRAC and the first 3 h U-band VLT-VIMOS magnitudes. They were
trained on the high quality GOODS-FORS2 and VVDS spectroscopic
redshifts. The Daddi et al. (private communication) catalog is based
on most of the same GOODS imaging data used by Grazian et al., including
IRAC but not the VIMOS U-band, but the two catalogs use independent
photometric measurements (different software, apertures, etc.).
The Daddi photometric redshifts were trained using high quality
spectroscopic redshifts from GOODS-FORS2, K20, and GMASS (Kurk et al.,
in preparation). For our purposes, we have
cross-correlated the two photometric redshift catalogs and created a
high quality reference sample which includes only those objects with
concordant GOODS-MUSIC and GOODS redshift estimations. We have
calculated the standard deviation of the photometric redshift differences,
,
finding
,
We define the photometric redshift reference sample to be those objects
with
,
i.e.,
.
Figure 5 shows the comparison of the Grazian and Daddi
photometric redshifts. The filled circles lying within the
lines
(the solid lines in the figure) are those included in our photometric
redshift reference sample, and the empty circles are excluded from
it.
Next, we have compared this high quality reference
sample
with our VIMOS LR-Blue and MR spectroscopic redshift measurements.
Figure 6 shows the result of the comparison. We
define ``catastrophic'' discrepancies to be those measurements
with
.
For the LR-Blue survey:
- we find 150 common objects between the
reference sample and the LR-Blue spectroscopic catalog. 65 of them have flag A, 34 have flag B and 51 have flag C;
- there are 4 flag A ``catastrophic'' discrepancies: 1 is
a secure Lyman break galaxies with strong Ly
in emission and well identified ultraviolet features, and is not consistent with the
. In the remaining 3 spectra the emission line is identified as Ly
but it could be also an [OII] as suggested by the
. Thus 3
determinations out of 65 can be considered wrong, which confirms a confidence level of 95% in the low resolution flag A redshifts;
- we find 8 flag B discrepancies: 2 of them are secure low
redshift emission line galaxies ([OII], H
and [OIII] well identified). The remaining 6 spectra are solo-emission line ([OII] or Ly
) spectra with few other low S/N features identified. If the line is identified differently ([OII] instead of Ly
or vice-versa) the resulting
is consistent with
. Thus, we consider these measurements wrong. The resulting confidence level is 82%;
- there are 23 flag C
which are not confirmed by the
, which results in a confidence level about 55%.
- we find 177 common objects between the
reference sample and the MR spectroscopic catalog. 123 of them have flag A, 37 have flag B and 17 have flag C;
- there are 2 flag A ``catastrophic'' discrepancies. Both cases
are secure low redshift emission line galaxies ([OII], H
and [OIII] well identified). Thus the confidence level of the MR A flag redshifts, in this test, is 100%;
- we find 6 flag B discrepancies: 2 of them are secure low redshift emission line galaxies. In the remaining 4 spectra, the emission line is located in the fringing region and could be misclassified. The resulting confidence level is 89%;
- there are 4 flag C
which are not confirmed by the
, which results in a confidence level of 76%.
![]() |
Figure 8:
Completeness level of GOODS spectroscopy in the CDF-S in
several redshift bins. The left panel shows the coarse-grain redshift
distribution of the
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Figure 9: Fine-grain redshift distribution of the available spectroscopic catalogs: the VIMOS LR-Blue catalog in the top panel, the VIMOS MR catalog in the central panel, and the GOODS master catalog in the bottom panel. The smaller panels within the main frames show the distribution in redshift regions of particular interest. |
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Figure 10:
Galaxy density in velocity space. The solid line is the
background distribution obtained by smoothing the observed
distribution with a Gaussian with
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5.3 The survey completeness
The following analysis is restricted only to the GOODS-S area, which is the main region of interest of the overall GOODS-VIMOS spectroscopic survey. Therefore, we consider for this analysis only VIMOS LR-Blue and MR spectroscopic sources belonging to the GOODS-S region proper (i.e., the area covered by deep HST/ACS and Spitzer data), and we apply the same restriction to any other spectroscopic catalog used for creating the GOODS-S master catalog (see below for details).
5.3.1 Completeness as a function of magnitude
The main purpose of the two complementary GOODS-South redshift
surveys, the FORS2 and VIMOS campaigns, is to provide a highly
complete spectroscopic sample down to
i775=25 mag. Thus, it is
important to know which is the real level of completeness reached
so far after the completion of the whole FORS2 survey and 60% of the
VIMOS survey. For this purpose we have created a GOODS-S
spectroscopic ``master catalog''. This is namely the compilation of
all high quality spectroscopic redshifts available in the GOODS-S
region: GOODS FORS2 quality A and B, VIMOS LR-Blue and MR quality A
and B, K20 quality 1, VVDS quality 3 and 4, Szokoly et al. (2004)
quality 3 and 2+ and Ravikumar et al. (2007) quality 2
redshifts. We have cleaned the GOODS-S spectroscopic ``master catalog''
of duplicate observations. In case of double or multiple observations
we made a visual inspection of the different spectra and chose the most
convincing redshift estimate. Figure 7
shows the completeness level of the VIMOS survey (filled squares) and
of the GOODS-S ``master catalog'' (empty squares) as a function of the
I (left panel) and
(right panel) AB magnitudes. The final
completeness level achieved in the field by the GOODS-S
spectroscopic ``master catalog'' (empty squares in the figure) is on
average
down to
iAB=22.5 mag and
mag,
respectively. At fainter magnitudes the completeness level decreases
to
.
5.3.2 Completeness in different redshift bins
In principle, the selection function of a spectroscopic survey could
be estimated by comparison with appropriate simulations able to
reproduce the results of the applied target selection criteria. In the
case of the FORS2 and VIMOS campaigns this is complicated by the fact
that the selection criteria are not uniform throughout the survey. In
fact, they were tailored for each observing run in order to optimizing
the survey success rate in terms of redshift estimation on the basis
of partial results from previous observations. To overcome this problem we use
a different approach, comparing our spectroscopic redshift catalog with
a fairly complete photometric redshift catalog. As in the previous
section we use two
catalogs, the GOODS-MUSIC catalog of
Grazian et al. (2006) and the GOODS catalog of Daddi et al. (2007b),
to control possible biases. The largest fraction of the
GOODS-MUSIC sample is 90% complete at
and
mag (AB scale). In a similar way, the GOODS catalog of Daddi et al. (2007b) includes all the GOODS sources with
mag. Since
we are calculating the selection function of our spectroscopic catalog
in the ACS i band, we have checked that both
catalogs are
able to reproduce the observed i-band number counts band down to the
required magnitude limit (
i775=25).
As shown in the left panel of Fig. 8, both
catalogs are able to reproduce the same coarse-grain
redshift distribution within
(considering only
Poisson errors). The redshift bin is chosen to be
,
similar to the
uncertainty obtained in the comparison of the
two
catalogs. The same panel shows also the coarse-grain
redshift distribution of the VIMOS (LR-Blue+MR, the filled circles)
survey and of the GOODS-S ``master catalog''. The completeness level
in each redshift bin is calculated as the ratio
.
The central panel of Fig. 8 shows
the redshift-dependent completeness level of the whole GOODS-VIMOS
survey. The GOODS-VIMOS survey samples a small fraction (
)
of the total galaxy population at
iAB < 25 mag a z < 1.5.
This is expected because the LR-Blue targets, which account for 2/3 of
the whole GOODS-VIMOS spectroscopic sample, are selected to be at z>2.
Indeed, at
2 < z < 3.5 the GOODS-VIMOS survey samples
of the whole high redshift population at
iAB < 25 mag. We
adopt the same approach also for analyzing the ``selection function'' of
the GOODS-S spectroscopic ``master catalog''. The right panel shows
the redshift-dependent completeness level in this case. The
completeness level of the GOODS master catalog is
up to
.
This is reinforced by the fact that the two
catalogs provide consistent results within the error bars
up to this redshift. At higher redshift, the results obtained with the
two different
catalogs are too discrepant (more than
;
the error bars are not shown in the central and right
panels for clarity). This large discrepancy does not allow us to draw any
conclusion in this redshift range. It is worth noting that high
level of completeness in the
2 < z < 3.5 redshift bins is mainly due
to the GOODS-S VIMOS spectroscopic survey, which accounts for almost
65% of the whole spectroscopic redshifts available in the GOODS-S
region in that redshift range.
5.4 Redshift distribution and large scale structure
Figure 9 shows the fine-grain redshift distribution of the
VIMOS LR-Blue (top panel), the VIMOS MR (the central panel) and the
GOODS master spectroscopic catalog (the bottom panel). The smaller
panels within each main panel show redshift regions of particular
interest. Only the very high quality redshifts have been used for the
analysis (flag A and B VIMOS and FORS2 redshift, flag 1 K20, flag 3
and 4 VVDS redshifts and flag 2 and 3 of Szokoly et al. 2004; flag 2
Ravikumar et al. 2007). To assess the significance of the observed
large scale structures we follow a procedure suggested by Gilli et al. (2003) and similar to the one of Cohen et al. (1999). The sources
are distributed in
rather then in redshift, since dVcorresponds to local velocity variations relative to the Hubble
expansion. The observed distribution is then smoothed with a Gaussian
with
km s-1 (see Fig. 10) to obtain the
``signal'' distribution. Since there is no a priori knowledge of the
``background'' distribution, we heavily smoothed the observed
distribution with a Gaussian with
km s-1 and
considered this as the background distribution. We then searched for
possible redshift peaks in the signal distribution, computing for each
of them the signal to noise ratio defined as
S/N=(S-B)/B1/2,
where S is the number of sources in a velocity interval of fixed width
km s-1 around the center of each peak candidate
and B is the number of background sources in the same
interval. Adopting the threshold
we find 14 peaks. In
order to estimate the expected fraction of possibly ``spurious'' peaks
arising from the background fluctuations, we have simulated 105samples of the same size of the observed distribution and randomly
extracted from the smoothed background distribution and applied our
peak detection method to each simulated sample. With the adopted
threshold, the average number of spurious peaks due to background
fluctuations is 0.09. Of the simulated samples, 6.6
show one
spurious peak, 0.3
show two spurious peaks, and only two
simulation (out of 105) has three spurious peaks. None of the
simulated samples have four or more spurious peaks. The 14 peaks
detected in the procedure described above are listed in Table 2,
with the mean redshift of the peak, the number of object (N) within
1000 km s-1 from the peak, the S/N threshold, and a short
description of the kind of large scale structure defined by visual
inspection of the galaxy spatial distribution. We briefly compare our
findings those of previous studies:
- The three clusters at z = 0.53, 0.67 and 0.73, already seen in the
GOODS-FORS2 and K20 surveys are confirmed by the VIMOS redshifts. The
peak at z = 0.077 seen in Gilli et al. is not detected in the master
catalog. We confirm the sheet-like structures observed at z = 0.219 in
Gilli et al. (2003) and find a structure at redshift marginally
lower, z=0.339, than the one at z=0.367 found by Gilli et al. (2003). An additional scale structure is visible at
z = 0.1241.
A cluster-like structure is also visible at
z = 0.9766, as confirmed by
extended X-ray emission reported by Szokoly et al. (2004). We confirm
the detection of the concentrated structures at z=1.031, 1.224, and 1.616,
already seen in K20 by Cimatti et al. (2003), in the X-ray sample by
Gilli et al. (2003), and in the FORS2 sample by Vanzella et al. (2006). We observe additional significant peaks at z=1.0990 and
1.3060, also seen by Adami et al. (2005) and Vanzella et al. (2006);
- we note that other two peaks are been detected with
at z = 2.316 and 2.560. The latter peak has also been reported by Gilli et al. (2003). In both cases, the galaxy within 1000 km s-1 from the peak occupy the whole GOODS region in a sheet-like structure. The mean projected distance between galaxies and their nearest neighbors is about 4 Mpc in both cases. The probability to detect spurious peaks arising from the background distribution with a SN equal or greater than
is about 10-3;
- 124 galaxies are observed in the GOODS master sample in the redshift range 3 < z < 4. No over-densities are confirmed in the considered redshift range;
- 51 galaxies are observed in the GOODS master sample in the redshift range 4 < z < 5 and 46 at z > 5. No over-densities are confirmed in the considered redshift range.
Table 2:
Peaks detected in the master catalog redshift distributions,
sorted by increasing redshift. The signal and background distribution
are smoothed with
km s-1 and
km s-1,
respectively. The mean redshift of each peak, the number of sources N
within 1000 km s-1 from each peak, and the type of large scale structure are also indicated.
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Figure 11: BzK diagrams of the GOODS-S master catalog. The left panel shows all galaxies with redshifts 1.4 < z < 2.5. The central panel shows galaxies with z < 1.4 (open circles) and confirmed stars (star symbols), and the right panel shows galaxies at z > 2.5. The solid lines mark the BzK color selection regions at (z-K)-(B-z) > 0.2 and (z-K)-(B-z) < 0.2, B-z > 2.5 where the star-forming and passive BzK galaxies, respectively, are expected to lie. |
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6 Reliability of photometric techniques for the selection of galaxies at 1 < z < 3
Many photometric techniques have been proposed to select galaxies at
high redshift, particularly at z > 1.5. Several of these (BzK,
``sub''-U-dropouts, U-, B- and V-dropouts criteria) have been used to
select targets for the various GOODS-S spectroscopic surveys.
The master redshift catalog described in the previous section reaches
a completeness level >
at
1.5 < z < 3.5, and allows us to check the
completeness and reliability of different photometric selection techniques
by estimating their contamination due to foreground (and background)
interlopers outside of the expected redshift ranges for each color
selection method.
Figure 11 shows the BzK diagram of Daddi et al. (2004), which
aims to select galaxies at
1.4 < z < 2.5. Spectroscopically confirmed
galaxies at
1.4 < z < 2.5 (left panel), z < 1.4 (central panel) and
z > 2.5 (right panel) are shown in each diagram, along with lines that
define the BzK color selection criteria. The PSF-matched photometry of the
BzK catalog used in Daddi et al. (2007a,b) has been used to construct
these figures.
of galaxies at
1.4 < z < 2.5lie in the expected BzK region. 14% of galaxies with redshifts in this range
fall outside the BzK color selection window, although most are only
slightly outside the expected color ranges, consistent with very modest
uncertainties in the photometric measurements. As shown in the central panel,
92% of the galaxies with z < 1.4 fall outside the BzK selection region.
Again, of the 8% of low redshift galaxies within the BzK area, most are near
the color selection boundaries, again consistent with modest photometric errors.
The galaxies at z > 2.5 are not localized in a specific region of the diagram.
Only 27% of those higher redshift objects lie at
(z-K)-(B-z) > 0.2,
and the remaining 73% are located in the same color-color region as the low redshift
galaxies. This is expected because at z > 2.5 the Lyman forest starts to enter the
B band, producing a redder B-z color. To estimate the contamination due to low
redshift galaxies in the BzK selection, we examine the redshift distributions
of galaxies within and outside the BzK color selection regions.
For galaxies within the color selection region for star-forming BzK galaxies,
67% of the sample lie at
1.4 <z < 2.5, 10% at z > 2.5, and the contamination
of low redshift interlopers is 23% (see the left panel of Fig. 13).
In the BzK passive galaxy region there are only 4 galaxies. 2 of them are at
1.4 < z < 2.5, one is at z > 2.5 and one has z < 1.4. We note that
the B-band data used for the color measurements is not as deep as would
be required to robustly identify passive BzK galaxies, which have extremely
red B-z colors.
When the same analysis is carried out adopting a brighter magnitude limit,
23 < i < 23.5, the results are unchanged. Our estimate of the BzK foreground
contamination is higher than the 8% fraction found by
Daddi et al. (2007a).
The difference is largely due to the fact that the latter work excluded
from the analysis hard X-ray sources and blended galaxies. AGN contamination
of the stellar light from faint galaxies can make them appear redder, and
Daddi et al. have found that foreground X-ray sources frequently mimic
the redder BzK colors of ordinary galaxies at z > 1.4.
![]() |
Figure 12: U-B-B-R color-color diagrams of the GOODS-S master catalog. The left panel shows the galaxies at 1.4 < z < 3, the central panel shows the low redshift galaxies (z < 1.4), and the right panel shows the galaxies at z > 3. In the central panel, the empty circles refer to the low redshift galaxies and the stars refer to stars. The region comprised between the solid and the dashed lines is the sub-U-dropout locus. The U-dropouts lie above the dashed line. |
Open with DEXTER |
![]() |
Figure 13: Redshift distribution of the BzK-selected ( left panel) and sub-U-dropout ( right panel) galaxies. |
Open with DEXTER |


and not meeting the standard U-drop criterion. The U-dropout criteria are:
Figure 12 shows the U-B and B-R color color diagram for galaxies with measured redshifts 1.4 < z < 3 (left panel), z < 1.4 (central panel) and z > 3 (right panel), respectively. The sub-U-dropout color window is located below the U-dropout color limits (thus, the name ``sub''-U-dropouts). It is bounded by the solid and the dashed lines showed in the diagrams of Fig. 12. The U-dropouts lie in the area enclosed by the dashed line. As shown in the left panel of the figure, most (80%) of the galaxies at 1.4 < z< 3 lie in the the sub-U-dropout color selection region, with 8% in the U-drop color region. Most galaxies at z < 1.4 (92%) do not lie in the sub-U-dropouts and U-dropouts loci, as shown in the central panel. 58% of the galaxies at z > 3 lie in the U-dropout region and 16% in the sub-U-dropout region (left panel). We have estimated the contamination of the sub-U-drop criterion in a manner analogous to that which we used to test the BzK method. 72% of the sub-U-dropouts candidates at R > 23 turn out to be at 1.4 < z < 3, with a 24% contamination of low redshift objects (z < 1.4) and a remaining 4% of higher redshift objects (z > 3) (see also the right panel of Fig. 13). In particular, there is a peak of galaxies at





7 Conclusions
We have observed a large sample of galaxies in the Chandra Deep Field
South with the VIMOS spectrograph on the VLT, as part of a public
campaign of ESO spectroscopy for the Great Observatories Origins Deep
Survey southern field. A total of 3312 objects with
has been observed with the VIMOS LR-Blue and MR grisms, providing
2137 redshift measurements. From a variety of diagnostics the
measurement of the redshifts appears to be accurate (with a typical
)
and reliable. The reliability of the redshift
estimate varies with the quality flag. VIMOS LR-Blue quality flag A
redshifts are reliable at 93-95% confidence level, flag B redshidts
at 60-80% and quality C et 30-50%. In the MR case, quality flag A
redshifts are reliable at 100% confidence level, quality B at 80-95%
and quality C
at 60-75%. The confidence level ranges are
determined in all cases by comparing our redshift estimates with
estimates provided by different spectroscopic surveys and photometeric
redshift catalogs. The spectroscopic coverage of the CDF-S achieved
by combining the VIMOS spectroscopic sample with other redshifts
available from the literature is very high,
up to redshift
.
It is more uncertain at higher redshifts. A ``master
catalog'' combining the VIMOS redshifts presented in this paper and
other, large samples available in the literature have been used to
test the accuracy of the BzK, sub-U-dropout color selection
techniques. We show that any of these methods permits the selection of
high redshift galaxies with a contamination of
of low
redshift sources and a completeness level of 80%. We also identify
several large scale structures in the GOODS region.
The reduced spectra and the derived redshifts have been released to the community (http://archive.eso.org/cms/eso-data/data-packages). They constitute an essential contribution to achieve the scientific goals of GOODS, providing the time coordinate needed to delineate the evolution of galaxy properties, morphologies, and star formation and to underhand the galaxy mass assembly.
Acknowledgements
We are grateful to the ESO staff in Paranal and Garching who greatly helped in the development of this program. We would like to thank Martino Romaniello and Carlo Izzo for many stimulating discussions and for the help in reducing the VIMOS data. We would like to thank also Remco Slijkhuis and Joerg Retzlaff for their work on VIMOS/GOODS release.
Appendix A: Spectra quality flags
Figure A.1 shows examples of spectra with redshift estimates
of different quality. The left column of the figure illustrates 1D and
2D spectra observed with the VIMOS LR-Blue grism with redshift of
quality flag A, B, C and X. The right column shows the same examples
for the MR grism. Quality A spectra (first two panels) show clear
emission and absorption features. Quality B spectra (second row of the
Fig. A.1) show clear emission and absorption features but
with somewhat lower quality: Ly
absorption at the edge of the
spectrum in the LR-Blue spectrum (left panel), strong [OII] emission in
the fringing area in the MR spectrum (right panel). The C quality
spectra (third row of the Fig. A.1) show only marginally
significant features: only OI and CIV absorption in the LR-Blue
spectrum (left panel) and faint [OII] emission in the fringing region
of the MR spectrum (right panel). The quality X spectra (last row of
the Fig. A.1) do not show any emission or absorption
features.
![]() |
Figure A.1: Examples of spectra with redshift estimates of different quality. The left column of the figure illustrates 1D and 2D spectra observed with the VIMOS LR-Blue grism with redshift of quality flag A, B, C and X. The right column shows the same examples for the MR grism. |
Open with DEXTER |
Appendix B: Spectra templates
Figure B.1 shows several templates of the high redshift
galaxies observed during the GOODS-VIMOS spectroscopic campaign. The
templates have been obtained by stacking the 1D rest-frame
spectra. The first row of the figure show the Ly emission
(left panel) and absorption (right panel) galaxies at
obtained by stacking
150 LR-Blue spectra. The second row of the
figure shows Ly
emission (left panel) and absorption (right
panel) galaxies at
obtained by stacking in both cases 13 MR spectra. The last row shows a template of BzK spectrum at
.
All the emission and absorption features used to identify the
spectroscopic redshifts are outlined in the individual panels.
![]() |
Figure B.1:
Combined 1D spectra of high redshift galaxies in different
redshift bins. The top panels show LBGs with the Ly |
Open with DEXTER |
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Footnotes
- ... France
- Based on observations made at the European Southern Observatory, Paranal, Chile (ESO program 171.A-3045 The Great Observatories Origins Deep Survey: ESO Public Observations of the SIRTF Legacy/HST Treasury/Chandra Deep Field South.)
All Tables
Table 1: Success rate of the GOODS VIMOS LR-Blue campaign. The first column lists the name of the target family, the second column lists the fraction of the target catalog due to the corresponding color selection (BzK and sub-dropout family overlap largely but they are considered as separated family in the table). The third column lists the success rate (fraction A+B flag objects) of each target family. The last four columns list the percentage of A, B, C and X flag redshift determinations, respectively.
Table 2:
Peaks detected in the master catalog redshift distributions,
sorted by increasing redshift. The signal and background distribution
are smoothed with
km s-1 and
km s-1,
respectively. The mean redshift of each peak, the number of sources N
within 1000 km s-1 from each peak, and the type of large scale structure are also indicated.
All Figures
![]() |
Figure 1: Example of the VIMOS field coverage of the GOODS area in the CDF-S. Only three pointings from the VIMOS-MR campaign are shown for clarity. Each color indicates the position of one instrument quadrant in the three different pointings. |
Open with DEXTER | |
In the text |
![]() |
Figure 2:
|
Open with DEXTER | |
In the text |
![]() |
Figure 3:
Redshift differences between objects observed twice or more
in independent VIMOS LR-Blue ( left panel) and MR ( right panel)
observations. The distribution has a dispersion of
|
Open with DEXTER | |
In the text |
![]() |
Figure 4: Color-magnitude diagram of the LR-Blue and MR primary targets. The first panel shows the B-R vs. B diagram for A and B high quality LR-Blue redshifts. Low quality LR-Blue redshifts (C flag, dots) and failure (X flag, stars) are shown in the central panel. The bottom panel shows the i-z vs. z diagram for the MR primary targets. The black dots are the high quality (A and B flag) MR redshifts at z < 0.8, the empty circles are high quality (A and B flag) MR redshifts at z > 0.8. The stars represent the C and X cases. |
Open with DEXTER | |
In the text |
![]() |
Figure 5:
Comparison of the GOODS-MUSIC and the GOODS photometric
redshift catalog. The small inset panel shows the distribution
of redshift differences,
|
Open with DEXTER | |
In the text |
![]() |
Figure 6:
|
Open with DEXTER | |
In the text |
![]() |
Figure 7:
Completeness level of the VIMOS survey (filled squares)
and of the GOODS-S master catalog (empty squares) as a function of the
I ( left panel) and |
Open with DEXTER | |
In the text |
![]() |
Figure 8:
Completeness level of GOODS spectroscopy in the CDF-S in
several redshift bins. The left panel shows the coarse-grain redshift
distribution of the
|
Open with DEXTER | |
In the text |
![]() |
Figure 9: Fine-grain redshift distribution of the available spectroscopic catalogs: the VIMOS LR-Blue catalog in the top panel, the VIMOS MR catalog in the central panel, and the GOODS master catalog in the bottom panel. The smaller panels within the main frames show the distribution in redshift regions of particular interest. |
Open with DEXTER | |
In the text |
![]() |
Figure 10:
Galaxy density in velocity space. The solid line is the
background distribution obtained by smoothing the observed
distribution with a Gaussian with
|
Open with DEXTER | |
In the text |
![]() |
Figure 11: BzK diagrams of the GOODS-S master catalog. The left panel shows all galaxies with redshifts 1.4 < z < 2.5. The central panel shows galaxies with z < 1.4 (open circles) and confirmed stars (star symbols), and the right panel shows galaxies at z > 2.5. The solid lines mark the BzK color selection regions at (z-K)-(B-z) > 0.2 and (z-K)-(B-z) < 0.2, B-z > 2.5 where the star-forming and passive BzK galaxies, respectively, are expected to lie. |
Open with DEXTER | |
In the text |
![]() |
Figure 12: U-B-B-R color-color diagrams of the GOODS-S master catalog. The left panel shows the galaxies at 1.4 < z < 3, the central panel shows the low redshift galaxies (z < 1.4), and the right panel shows the galaxies at z > 3. In the central panel, the empty circles refer to the low redshift galaxies and the stars refer to stars. The region comprised between the solid and the dashed lines is the sub-U-dropout locus. The U-dropouts lie above the dashed line. |
Open with DEXTER | |
In the text |
![]() |
Figure 13: Redshift distribution of the BzK-selected ( left panel) and sub-U-dropout ( right panel) galaxies. |
Open with DEXTER | |
In the text |
![]() |
Figure A.1: Examples of spectra with redshift estimates of different quality. The left column of the figure illustrates 1D and 2D spectra observed with the VIMOS LR-Blue grism with redshift of quality flag A, B, C and X. The right column shows the same examples for the MR grism. |
Open with DEXTER | |
In the text |
![]() |
Figure B.1:
Combined 1D spectra of high redshift galaxies in different
redshift bins. The top panels show LBGs with the Ly |
Open with DEXTER | |
In the text |
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