J/A+A/544/A104 Cl 1103.7-1245 at z=0.96: spectroscopic catalog (Vulcani+, 2012)
Cl 1103.7-1245 at z=0.96: the highest redshift galaxy cluster in the
EDisCS survey.
Vulcani B., Aragon-Salamanca A., Poggianti B.M., Milvang-Jensen B.,
von der Linden A., Fritz J., Jablonka P., Johnson O., Zaritsky D.
<Astron. Astrophys. 544, A104 (2012)>
=2012A&A...544A.104V 2012A&A...544A.104V
ADC_Keywords: Galaxy catalogs; Spectroscopy ; Redshifts
Keywords: galaxies: clusters: general - galaxies: evolution -
galaxies: distances and redshifts
Abstract:
We present new spectroscopic observations in a field containing the
highest redshift cluster of the ESO Distant Cluster Survey (EDisCS).
We measure galaxy redshifts and determine the velocity dispersions of
the galaxy structures located in this field. Together with the main
cluster Cl 1103.7-1245 (z=0.9580; σclus=522±111km/s) we find
a secondary structure at z=0.9830, Cl 1103.7-1245c. We then
characterize the galaxy properties in both systems. These new
spectroscopic observations for Cl 1103.7-1245 complement the
previous analysis of Milvang-Jensen et al. (2008, Cat. J/A+A/482/419),
whose observations targetted z=0.70.
Description:
The target selection strategy, mask design procedure and observations
are similar to those adopted for the EDisCS spectroscopy, described in
detail in Halliday et al. (2004, Cat. J/A+A/427/397) and
Milvang-Jensen et al. (2008, Cat. J/A+A/482/419). The target
selection was based on the available VLT/FORS2 optical photometry
(White et al., 2005, Cat. J/A+A/444/365) and the NTT/SOFI NIR
photometry (Aragon-Salamanca et al., in preparation). The optical data
cover 6.5'x6.5' and are well-matched to the FORS2 spectrograph
field-of-view. The NIR data cover a somewhat smaller region of
4.2'x5.4'.
Spectroscopic observations were completed using the FORS2 spectrograph
(cf. Appenzeller et al., 1998Msngr..94....1A 1998Msngr..94....1A) on the VLT, during one
observing run in March 2008, comprised of 3 half-nights. A
high-efficiency grism was used (grism 600RI+19,
λcentral=6780Å, resolution FWHM∼6Å). The exposure time
was 1800 seconds per frame, for a total of 8 frames per mask. A total
of 3 masks were observed, for a total of 94 slits (33 slits in mask 1
and 2 and 28 slits in mask 3). The reduction was performed using an
"improved sky subtraction", whose properties and advantages have been
largely described and discussed in Milvang-Jensen et al. (2008, Cat.
J/A+A/482/419).
Galaxy redshifts were measured from the reduced 1D spectra, using
emission lines where possible, as done in Poggianti et al.
(2006ApJ...642..188P 2006ApJ...642..188P).
In addition, when possible, we also measured the equivalent width of
[OII] and Hδ. Note that for star-forming galaxies the Hδ
absorption line may be affected by emission in-filling. We have not
attempted to correct for this effect.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 119 214 Main catalog
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See also:
J/ApJS/137/117 : Las Campanas Distant Cluster Survey (LCDCS) (Gonzalez+, 2001)
J/A+A/427/397 : Redshifts of 5 EDisCS galaxy clusters (Halliday+, 2004)
J/A+A/444/365 : ESO Distant Cluster Survey, EDisCS (White+, 2005)
J/A+A/482/419 : ESO Distant Cluster Survey, EDisCS. II (Milvang-Jensen+, 2008)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- --- EDCSN
6- 21 A16 --- EDCSN EDisCS name, JHHMMSSs+DDMMSSs,
in Simbad
23- 28 F6.3 mag Imag ?=99.99 I-band Magnitude for aperture radius 1"
30- 35 F6.4 --- z ?=9.9999 Spectroscopic redshift
(z=0.0000 corresponds to stars)
37 I1 --- q_z [0/3] redshift quality, 0=best (1)
39- 40 A2 --- Mmb Membership flag (2)
42- 48 F7.2 0.1nm WOII ?=- Rest-frame equivalent width of
the [OII](3727) line (3)
50- 55 F6.2 0.1nm WHd ?=- rest-frame equivalent width of the
Hδ line (3)
57- 62 F6.3 [Msun] log(M*) ?=- Mass estimates, converted to a
Kroupa (2001MNRAS.322..231K 2001MNRAS.322..231K) IMF
64- 68 F5.3 --- Weights Spectroscopic magnitude completeness weights
70- 72 I3 --- TType ?=- Morphological classification (4)
74-119 A46 --- Comm Some useful comments
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Note (1): The redshift quality is as follows:
0 = redshift measurement is robust
1 = secure redshifts but with larger uncertainties
2 = doubtful redshifts
3 = no redshift estimates
Note (2): Membership is defined as being within ±3σcl from zcl.
The membership flag is as follows:
1 = members of the main cluster
1c = members of secondary structures
1d = members of secondary structures
1e = members of secondary structures
0 = field galaxy or star and object without a determined redshift
Note (3): The rest-frame equivalent width is given adopting the convention
that EWs are negative when in emission.
--- indicates the measurement was not possible due to low S/N.
Note (4): The morphological classification is as follows:
-7 = star
-6 = nonstellar but too compact to see structure
-5 = ellipticals
2 = S0
1 = Sa
3 = Sb
5 = Sc
7 = Sd
9 = Sm
11 = Irr/Pec
111 = no HST data corresponding to ground-based object
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Acknowledgements:
Benedatta Vulcani, benedetta.vulcani(at)oapd.inaf.it
(End) Patricia Vannier [CDS] 06-Jul-2012