J/A+A/579/A4 MCS J1206.2-0847 galaxies spectral classification (Girardi+, 2015)
CLASH-VLT: Substructure in the galaxy cluster MACS J1206.2-0847 from
kinematics of galaxy populations.
Girardi M., Mercurio A., Balestra I., Nonino M., Biviano A., Grillo C.,
Rosati P., Annunziatella M., Demarco R., Fritz A., Gobat R., Lemze D.,
Presotto V., Scodeggio M., Tozzi P., Bartosch Caminha G., Brescia M.,
Coe D., Kelson D., Koekemoer A., Lombardi M., Medezinski E., Postman M.,
Sartoris B., Umetsu K., Zitrin A., Boschin W., Czoske O., De Lucia G.,
Kuchner U., Maier C., Meneghetti M., Monaco P., Monna A., Munari E.,
Seitz S., Verdugo M., Ziegler B.
<Astron. Astrophys. 579, A4 (2015)>
=2015A&A...579A...4G 2015A&A...579A...4G
ADC_Keywords: Clusters, galaxy ; Galaxies, photometry ; Redshifts ; Spectroscopy
Keywords: galaxies: clusters: individual: MACS J1206.2-0847 -
galaxies: clusters: general - galaxies: kinematics and dynamics -
galaxies: evolution - cosmology: observations
Abstract:
In the effort to understand the link between the structure of galaxy
clusters and their galaxy populations, we focus on MACS J1206.2-0847
at z∼0.44 and probe its substructure in the projected phase space
through the spectrophotometric properties of a large number of
galaxies from the CLASH-VLT survey. Our analysis is mainly based on an
extensive spectroscopic dataset of 445 member galaxies, mostly
acquired with VIMOS@VLT as part of our ESO Large Programme, sampling
the cluster out to a radius ∼2R200 (4Mpc). We classify 412 galaxies
as passive, with strong Hdelta absorption (red and blue galaxies), and
with emission lines from weak to very strong. A number of tests for
substructure detection are applied to analyze the galaxy distribution
in the velocity space, in 2D space, and in 3D projected phase-space.
The observational scenario agrees with MACS J1206.2-0847 having
WNW-ESE as the direction of the main cluster accretion, traced by
passive galaxies and red strong Hδ galaxies. The red strong
Hδ galaxies, interpreted as poststarburst galaxies, date a
likely important event 1-2Gyr before the epoch of observation. The
emission line galaxies trace a secondary, ongoing infall where groups
are accreted along several directions.
Description:
The table contains the spectral classification of 412 galaxies
analysed in the paper. The objects are part of the spectroscopic
dataset collected within the ESO Large Programme 186.A-0798 "Dark
Matter Mass Distributions of Hubble Treasury Clusters and the
Foundations of LambdaCDM Structure Formation Models" (P.I.: P.
Rosati). This program aims at obtaining spectra for at least 500
cluster members for each of the 14 southern CLASH clusters with
0.2<z<0.6, using the VIsible Multi-Object Spectrograph (VIMOS) at VLT
(CLASH-VLT survey).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 78 412 Spectral classification of 412 member galaxies
of MACS 1206.2-0847
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See also:
J/ApJ/749/97 : Multiple lensed images in MCS J1206.2-0847 (Zitrin+, 2012)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/412] Running ID for galaxies
5- 6 I2 h RAh Right ascension (J2000.0)
8- 9 I2 min RAm Right ascension (J2000.0)
11- 15 F5.2 s RAs Right ascension (J2000.0)
17 A1 --- DE- Declination sign (J2000.0)
18- 19 I2 deg DEd Declination (J2000.0)
21- 22 I2 arcmin DEm Declination (J2000.0)
24- 27 F4.1 arcsec DEs Declination (J2000.0)
29- 34 F6.4 --- z [0.427/0.453] Spectroscopic redshift
36- 39 F4.2 mag B-Rc [0.27/2.49] Johnson-Cousins B-R color index
41- 44 F4.2 mag e_B-Rc [0.01/0.3] rms uncertainty on B-Rc
46- 51 F6.2 0.1nm EW([OII]) [-99/-1.5]?=0 Equivalent width of [OII] (1)
53- 57 F5.2 0.1nm e_EW([OII]) [0/88] rms uncertainty on EW([OII])
59- 64 F6.2 0.1nm EW(Hd) [-31/15.2] Equivalent width of Hδ
66- 70 F5.2 0.1nm e_EW(Hd) [0.2/21] rms uncertainty on EW(Hd)
72- 76 A5 --- Class Spectral classification (3)
78 A1 --- Note [a] Note (2)
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Note (1): We list '0.00' for EW[OII] when no emission is observed.
Note (2): Label 'a' indicates the few galaxies for which the spectrum does not
cover the [OII] region. In this cases, the Equivalent width of [OIII]
line is reported instead of [OII].
Note (3): the classes are as follows:
PAS = passive galaxy ([OIII] absent, Hδ absent)
HDSr = strong Hδ absorption, and red color
(no [OIII], EW(Hδ) > 3Å
HDSb = strong Hδ absorption, and blue color
(no [OIII], EW(Hδ) > 5Å
wELG = weak emission lines (EW([OIII]) > -7Å)
mELG = medium emission lines (-15Å ≤ EW([OIII]) ←7Å)
sELG = strong emission lines (-40Å ≤ EW([OIII])←15Å)
vsELG = very strong emission lines (=EW([OIII]) ≤ -40Å)
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Acknowledgements:
Amata Mercurio, mercurio(at)na.astro.it
(End) Patricia Vannier [CDS] 17-Apr-2015