The Great Observatories Origins Deep Survey - VLT/VIMOS spectroscopy in the GOODS-south field: Part II

Home

All issues

Volume 512 (March-April 2010)

A&A, 512 (2010) A12

Online Material

Free Access

Issue		A&A Volume 512, March-April 2010


Article Number		A12
Number of page(s)		22
Section		Cosmology (including clusters of galaxies)
DOI		https://doi.org/10.1051/0004-6361/200913626
Published online		23 March 2010

Online Material

Appendix A: Corrections to previous release

We revised some of the redshifts from the first release of the GOODS/VIMOS survey for objects that were observed more than once in the GOODS/VIMOS survey or in other surveys. After comparing their spectra, 7 redshift determinations were modified as follows:

GOODS_LRb_001_1_q1_51_1 at z=2.2077 (flag A) in the previous release, was observed also with FORS2 (GDS J033226.67-274013.4). The low-S/N UV absorption lines were misclassified in the VIMOS spectrum. Instead, thanks to the comparison with the FORS2 spectrum, CIII] in emission could be identified. The new redshift obtained, z=1.6045, with quality flag B, is in agreement with the FORS2 measurement (z=1.612, flag A);
GOODS_LRb_003_new_q1_61_1 at z=0.067 (flag A) in the previous release. A possibly broad CIII] emission line was previously identified as [OII]. This object was also observed by Silverman et al. (in preparation), where the measured redshift is z=1.089. Our new estimate of the redshift based on CIII] and FeII lines is in agreement with the more recent measurement. We find z=1.0890 with quality flag B;
GOODS_LRb_003_new_q3_11_1 at z=2.6114 (flag B) in the previous release. This object was also observed in another mask (GOODS_LRb_003_new_2_q3_30_1, z=2.5831, flag B). Both estimates are based on the detection of a Ly- $\alpha$ in emission. However, we noticed that the former measurement required a slight adjustment (i.e. the Ly- $\alpha$ was correctly identified, but slightly misaligned). The new resulting redshift, z=2.5882, with quality flag B, is in better agreement with the second VIMOS measurement;
GOODS_LRb_003_new_1_q3_68_1 at z=0.7297, flag C based on the identification of [OII]. The redshift is correct and it is confermed by a second observation in a MR mask (GOODS_MR_new_1_d_q2_32_1 at z=0.7308, flag A). We simply upgraded the quality flag from C to B in this case;
GOODS_LRb_003_new_2_q1_42_1 at z=2.1084 (flag B) in the previous release. The broad MgII emission line was misclassified as Ly- $\alpha$ . This object was also observed in one of the new reduced masks (GOODS_LRb_dec06_3_q1_46_2, z=0.7358, flag A). Two spectral features are clearly identified: a broad emission line from MgII and [OII]. Therefore, the new redshift assigned is z=0.7357 with quality flag A;
GOODS_MR_new_1_d_q3_2_1 at z=0.5107 (flag B) in the previous release. Two spectral features were misclassified: [OIII] and H $\beta$ . Thanks to the comparison with a second observation of this object (GOODS_MR_001_q4_3_1 z=1.0338, flag A), we identified [OII] and MgII instead. The new redshift estimate is z=1.0349 with quality flag B.

The following redshifts were also revised:

GOODS_LRb_001_1_q2_66_1 at z=0.240 (flag B) in the previous release. The broad MgII emission line was misclassified as [OII]. After revising the spectrum we could identify some typical AGN features (e.g. a broad MgII emission line and broad Fe bump at $\sim$ 2960 $\AA$ ) plus [OII] and Ca H and K. The new redshift obtained is z=0.6632 (flag A);
GOODS_LRb_001_1_q3_5_3 at z=0.076 (flag B) in the previous release. The spectrum shows only one visible emission line at $\sim$ 4000 $\AA$ , which was previously interpreted as [OII]. For this object we find more likely the identification as Ly- $\alpha$ in emission, which gives a new tentative redshift of z=2.2980 (flag C);
GOODS_LRb_001_q4_44_1 and GOODS_LRb_003_new_ q4_28_1 at z=1.6285 (flag B) in the previous release. We reviewed the redshifts of the two spectra for this object, which were based on the identification of two very broad emission lines (i.e. CIV and CIII]). In addition, we identified several absorption lines (e.g. FeII, AlIII) that helped further calibrating the redshifts. The new measurements are z=1.609 (flag A) and z=1.608 (flag A) for GOODS_LRb_001_q4_44_1 and GOODS_LRb_003_new_q4_28_1, respectively;
GOODS_LRb_003_new_1_q2_46_2 is the same object as GOODS_LRb_001_1_q2_66_1 (see above). The new redshift measurement is z=0.6649 (flag A);
GOODS_LRb_003_new_1_q4_63_2 at z=0.585 (flag C) in the previous release. The spectrum is red, but quite noisy and may resemble that of an elliptical galaxy. However, after the inspection of the WFI R-image and the ACS z-image of this object, we found that a more likely explanation might be given in terms of a star. Therefore, we assign z=0.000 and flag B to this object;
GOODS_MR_new_2_b_q4_15_1 at z=5.2936 (flag C) in the previous release. We could identify Ca H and K, Fe I and possibly [OII]. The new redshift assigned to this object is z=0.9250 with quality flag B.

Appendix B: Large scale structure

Table B.1: List of observed peaks in the redshift distribution of the reference master catalog.

Table B.1 and Figs. B.1-B.3 show the results of the analysis of the spatial distribution of the 14 confirmed density peaks, plus three additional tentative structures at $z\simeq2.8$ , $z\simeq3.5$ , and $z\simeq3.7$ , observed in the master catalog of redshifts of the CDFS, described in Sect. 5.1.

$\begin{figure} \par\includegraphics[width=3.02 cm, angle=0]{peakv0124.eps}\inclu... ...\includegraphics[width=6.02 cm, angle=0]{peak0736.eps} \vspace{4cm} \end{figure}$

Figure B.1:

Histograms of the velocity distribution, $V=c\ln(1+z)$ , and spatial distribution of galaxies belonging to each of the density peak listed in Table B.1. For each structure, we display ``secure'' redshifts (>99% c.l.) in blue and ``likely'' redshifts ( $\sim$ 70-90% c.l.) in red. The histograms show the Gaussian fit to the peak of the velocity distribution (black dashed curve) and the $2\sigma$ -intervals around the peak selected for the spatial analysis (vertical green dashed lines). All the histograms are binned to $\Delta V=500$ km s^-1. The green diamonds show the position of the extended X-ray sources (i.e. XID 645 at $z\sim 0.67$ ; XID 566 and XID 594 at $z\sim 0.73$ ; XID 249 at $z\sim 0.97$ ). The black contours indicate the GOODS area and the field coverage of the 2 Ms Chandra exposure.

Open with DEXTER

$\begin{figure} \par\mbox{\includegraphics[width=3.0 cm, angle=0]{peakv097.eps}\i... ...includegraphics[width=6.0 cm, angle=0]{peak161.eps} }\vspace{6cm} \end{figure}$

Figure B.2:

Histograms of the velocity distribution, $V=c\ln(1+z)$ , and spatial distribution of galaxies belonging to each of the density peak listed in Table B.1. For each structure, we display ``secure'' redshifts (>99% c.l.) in blue and ``likely'' redshifts ( $\sim$ 70-90% c.l.) in red. The histograms show the Gaussian fit to the peak of the velocity distribution (black dashed curve) and the $2\sigma$ -intervals around the peak selected for the spatial analysis (vertical green dashed lines). All the histograms are binned to $\Delta V=500$ km s^-1. The black contours indicate the GOODS area and the field coverage of the 2 Ms Chandra exposure.

Open with DEXTER

$\begin{figure} \par\mbox{\includegraphics[width=3.0 cm, angle=0]{peakv231.eps}\i... ...eakv370.eps}\includegraphics[width=6.0 cm, angle=0]{peak370.eps} }\end{figure}$

Figure B.3:

Histograms of the velocity distribution, $V=c\ln(1+z)$ , and spatial distribution of galaxies belonging to each of the density peak listed in Table B.1. For each structure, we display ``secure'' redshifts (>99% c.l.) in blue and ``likely'' redshifts ( $\sim$ 70-90% c.l.) in red. The histograms show the Gaussian fit to the peak of the velocity distribution (black dashed curve) and the $2\sigma$ -intervals around the peak selected for the spatial analysis (vertical green dashed lines). All the histograms are binned to $\Delta V=500$ km s^-1. The black contours indicate the GOODS area and the field coverage of the 2 Ms Chandra exposure.

Open with DEXTER

Appendix C: Spectra of X-ray sources with new redshift determinations

In Figs. C.1, C.2, and C.3 we show 12 VIMOS spectra of X-ray sources with new redshift determinations (i.e. either unknown before or improving previous estimates), obtained fromthe last 8 VIMOS masks released in this paper. Together with each spectrum we provide a finding chart with the position of the corresponding X-ray sources. These sources also appear in the new catalog of X-ray sources detected in the ECDFS, which includes the identification of optical and near-IR counterparts (Silverman et al., in preparation).

$\begin{figure} \par\mbox{\includegraphics[width=8.0 cm, angle=0]{GOODS_LRb_002_1... ...ps}\includegraphics[width=5.0 cm, angle=0]{LRb_002_1_q1_6_1.eps} }\end{figure}$

Figure C.1:

New VIMOS spectra of X-ray sources with WFI R-band $20''\times 20''$ cutout centered on the position of the matching WFI source. Red crosses indicate the reconstructed VIMOS coordinates. The blue circles show the position of the WFI-matched objects. The yellow and green circles display the position of X-ray sources from the 2 Ms CDFS or from the ECDFS catalog, respectively. Labels with corresponding colors indicate source identification numbers.

Open with DEXTER

$\begin{figure} \par\mbox{\includegraphics[width=8 cm, angle=0]{GOODS_LRb_002_1_q... ...ps}\includegraphics[width=5 cm, angle=0]{LRb_dec06_3_q1_2_1.eps} }\end{figure}$

Figure C.2:

Open with DEXTER

$\begin{figure} \par\mbox{\includegraphics[width=8 cm, angle=0]{GOODS_LRb_002_1_q... ...s}\includegraphics[width=5 cm, angle=0]{LRb_dec06_1_q4_79_2.eps} }\end{figure}$

Figure C.3:

Open with DEXTER

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.