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J/A+A/486/9 Galaxy populations in z 0.25 clusters (Verdugo+, 2008)
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table3.dat
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Beginning of ReadMe :J/A+A/486/9 Redshifts in z 0.25 clusters (Verdugo+, 2008)
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The galaxy populations from the centers to the infall regions in
z 0.25 clusters.
Verdugo M., Ziegler B.L., Gerken B.
<Astron. Astrophys. 486, 9 (2008)>
=2008A&A...486....9V
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ADC_Keywords: Clusters, galaxy ; Redshifts ; Galaxies, photometry ;
Equivalent widths
Keywords: galaxies: general - galaxies: evolution -
galaxies: fundamental parameters - galaxies: clusters: general
Abstract:
We investigate the relation between star-formation activity and
environment in six intermediate redshift clusters (z 0.25) out to
large clustercentric distances ( 4R_vir_). For that, we conducted a
panoramic spectroscopic campaign with MOSCA at the Calar Alto
observatory. We acquired spectra of more than 500 objects.
Approximately 150 of these spectra were of galaxies that are members
of the clusters. Other 150 are field galaxies or galaxies belonging to
groups, serendipitously found during the investigation. The rest of
the spectra did not met the quality criteria or were stars. The
wavelength range allows us to quantify the star formation activity by
using the [OII] and the Halpha lines. This activity is examined in
terms of the large-scale environment expressed by the clustercentric
distance of the galaxies as well as on local scales given by the
spatial galaxy densities. The suppression of the star-formation
activity is observed at large clustercentric distances and low
projected densities. Galaxies with current star-formation show similar
activity, regardless of the environment, Therefore, the decline of the
star-formation activity inside the investigated clusters is driven
mainly by the significant change in the fraction of active versus
passive populations. This suggests that the suppression of the
star-formation activity occurs on short timescales. We also detect a
significant population of red star-forming galaxies whose colors are
consistent with the red-sequence of passive galaxies. They appear to
be in an intermediate evolutionary stage between active and passive
types.
Description:
We present measurements for all objects for which we were able to
derive secure redshifts. This includes galaxies belonging to the six
aforementioned clusters, four serendipitously found groups and the
general field (see the paper and below). For each object, table3.dat
provides the identification code, membership, right ascension and
declination (J2000.0); redshift, I-band magnitude and V-I color from
Gilbank et al. (2004MNRAS.348..551G); B and R-band absolute magnitude
derived with k-correct (Blanton and Roweis, 2007AJ....133..734B);
stellar mass also derived using k-correct and the equivalent widths of
the [OII] and the Halpha emission lines and associated errors.
Objects are sorted by membership to facilitate any specific search.
The clusters studied are the following:
VMF194 or RX J1729.0+7440;
XDCS220, short for XDCS cmJ172333+744410;
VMF131 or RX J1309.9+3222;
VMF132 or RX J1313.2+3229;
VMF73 or RX J0943.5+1640;
VMF74 or RX J0943.7+1644;
Galaxies belonging to the groups candidates are tagged with a group
number which corresponds to one of the following identifications:
group1 is r220_1J 172604+742830;
group2 is r220_2J 172518+742844;
group3 is r220_3J 172958+744204;
group4 is r265_1J 131030+322840.
Galaxies without any identifiable membership are tagged as belonging
to the field.