J/AJ/154/251 Spectroscopy of galaxies in z=0.2-0.9 clusters (Jorgensen+, 2017)
Galaxy populations in massive z=0.2-0.9 clusters.
I. Analysis of spectroscopy.
Jorgensen I., Chiboucas K., Berkson E., Smith O., Takamiya M., Villaume A.
<Astron. J., 154, 251 (2017)>
=2017AJ....154..251J 2017AJ....154..251J (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Photometry, SDSS ; Redshifts ;
Velocity dispersion ; Populations, stellar ; Galaxies, spectra
Keywords: galaxies: clusters: individual (Abell 1689/RXJ1311.4-0120,
Abell 115/RXJ0056.2+2622, RXJ0027.6) - galaxies: evolution -
galaxies: stellar content
Abstract:
We present an analysis of stellar populations in passive galaxies in
seven massive X-ray clusters at z=0.19-0.89. Based on absorption-line
strengths measured from our high signal-to-noise spectra, the data
support primarily passive evolution of the galaxies. We use the
scaling relations between velocity dispersions and the absorption-line
strengths to determine representative mean line strengths for the
clusters. From the age determinations based on the line strengths (and
stellar population models), we find a formation redshift of
zform=1.96-0.19+0.24. Based on line strength measurements from
high signal-to-noise composite spectra of our data, we establish the
relations between velocity dispersions, ages, metallicities [M/H], and
abundance ratios [α/Fe] as a function of redshift. The
[M/H]-velocity dispersion and [α/Fe]-velocity dispersion
relations are steep and tight. The age-velocity dispersion relation is
flat, with zero-point changes reflecting passive evolution. The
scatter in all three parameters is within 0.08-0.15 dex at fixed
velocity dispersions, indicating a large degree of synchronization in
the evolution of the galaxies. We find an indication of cluster-to-cluster
differences in metallicities and abundance ratios. However, variations
in stellar populations with the cluster environment can only account
for a very small fraction of the intrinsic scatter in the scaling
relations. Thus, within these very massive clusters, the main driver
of the properties of the stellar populations in passive galaxies
appears to be the galaxy velocity dispersion.
Description:
Imaging of Abell 1689, RXJ0056.2+2622, and RXJ0027.6+2616 was obtained
with the Gemini Multi-Object Spectrograph on Gemini North (GMOS-N), while
RXJ1347.5-1145 was observed with the twin instrument GMOS-S on Gemini
South. For a full description of GMOS-N and its twin, see Hook et al.
(2004PASP..116..425H 2004PASP..116..425H). All four clusters were observed using the
g', r', and i' filters. The seeing for the observations varied between
∼0.5" and 1.1".
The spectroscopic observations were obtained in multi-object
spectroscopic mode with GMOS-N or GMOS-S. Two fields were observed in
Abell 1689, each with two masks. Two fields were observed in RXJ0056.2+2622
with one mask each. RXJ0027.6+2616 and RXJ1347.5-1145 each have one field
observed with two masks. The sample selection for the spectroscopic
observations was based on the photometry from the ground-based imaging.
Objects:
----------------------------------------------------------------------
RA (ICRS) DE Designation(s)
----------------------------------------------------------------------
13 11 26.48 -01 20 10.9 Abell 1689 = ACO 1689
00 27 45.90 +26 16 25.0 RXJ0027.6+2616 = 2MASX J00274579+2616264
00 55 59.5 +26 19 14 RXJ0056.2+2622 = ACO 115
13 47 33.5 -11 45 42 RXJ1347.5-1145 = ClG J1347-1145
----------------------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table8.dat 83 251 GMOS Photometric Data for the Spectroscopic
Samples
table13.dat 63 247 Results from Template Fitting
table14.dat 190 216 Line Indices for Cluster Members
--------------------------------------------------------------------------------
See also:
I/252 : The USNO-A2.0 Catalogue (Monet+ 1998)
J/A+A/382/60 : BVR photometry in Abell 1689 (Duc+, 2002)
J/MNRAS/335/10 : Hα survey of Abell 1689 (Balogh+, 2002)
J/A+A/469/861 : Radial velocities of A115 galaxies (Barrena+, 2007)
J/MNRAS/423/256 : Abell 1689 imaging and spectroscopy (Houghton+, 2012)
J/ApJ/837/88 : SPT-GMOS spectroscopy of gal. in massive clusters
(Bayliss+, 2017)
Byte-by-byte Description of file: table8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Cluster Galaxy cluster name
9- 12 I4 --- ID [1/1480] Galaxy identification number
14- 15 I2 h RAh Hour of Right Ascension (J2000) (1)
17- 18 I2 min RAm Minute of Right Ascension (J2000) (1)
20- 24 F5.2 s RAs Second of Right Ascension (J2000) (1)
26 A1 --- DE- Sign of the Declination (J2000) (1)
27- 28 I2 deg DEd Degree of Declination (J2000) (1)
30- 31 I2 arcmin DEm Arcminute of Declination (J2000) (1)
33- 36 F4.1 arcsec DEs Arcsecond of Declination (J2000) (1)
38- 42 F5.2 mag gpmag [17.45/24.48] SDSS g'-band total magnitude
(2)
44- 48 F5.2 mag rpmag [16.2/23.17] SDSS r'-band total magnitude (2)
50- 54 F5.2 mag ipmag [15.73/22.37] SDSS i'-band total magnitude
(2)
56- 60 F5.3 mag gp-rp(tot) [0.244/1.916] SDSS g'-r' color from total
magnitudes (2)
62- 66 F5.3 mag rp-ip(tot) [0.095/1.096] SDSS r'-i' color from total
magnitudes (2)
68- 72 F5.3 mag gp-rp(ap) [0.336/1.909] SDSS g'-r' color from aperture
magnitudes (2)
74- 78 F5.3 mag rp-ip(ap) [0.062/1.177] SDSS r'-i' color from aperture
magnitudes (2)
80- 83 F4.1 --- nSer [0.5/11.3]? Sersic index (3)
--------------------------------------------------------------------------------
Note (1): Positions are consistent with USNO (Monet et al., 1998, Cat. I/252)
with an rms scatter of ∼0.5".
Note (2): Not corrected for Galactic extinction.
Note (3): From Houghton et al. (2012, J/MNRAS/423/256) used for sample selection
(see text).
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Byte-by-byte Description of file: table13.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Cluster Galaxy cluster name
9- 12 I4 --- ID [1/1480] Galaxy identification number
14- 19 F6.4 --- z [0.0816/1.0244] Redshift
21 I1 --- Member [0/2]? Adopted membership (1)
23- 27 F5.3 [km/s] logsig [1.908/2.523]? Log of velocity dispersion (2)
29- 33 F5.3 [km/s] logsigc [1.813/2.533]? Log of corrected velocity
dispersion (3)
35- 39 F5.3 [km/s] e_logsig [0/0.072]? Uncertainty on logsig
41- 44 F4.2 --- B8V [0/0.81]? Fraction of the template star of
type B8V
46- 49 F4.2 --- G1V [0.02/0.86]? Fraction of the template star of
type G1V
51- 54 F4.2 --- K0III [0/0.86]? Fraction of the template star of
type K0III
56- 59 F4.1 --- chi2 [0.9/20.8]? The χ2 value
61- 63 I3 --- S/N [5/449] Signal-to-noise ratio (4)
--------------------------------------------------------------------------------
Note (1): Adopted membership as follows:
1 = Member of the cluster;
0 = Not a member.
2 = For RXJ0027, member of the poor foreground group.
Note (2): Raw measurement value.
Note (3): Corrected to a standard size aperture equivalent to a circular
aperture with a diameter of 3.4" at the distance of the Coma cluster.
Corrected for systematic effects see Appendix Eq. B2 and B3.
Note (4): Per Angstrom in the rest frame of the galaxy. For the clusters A1689
and RXJ0056.2+2622 the wavelength interval was 4100-5500Å.
For the cluster RXJ0027.6+2616 the wavelength interval was chosen based on
the redshift of the galaxy:
Redshift less than 0.4: 4100-5500Å;
Redshift larger than 0.4: 3750-4100Å.
For the cluster RXJ1347.5-1145 the wavelength interval was:
Redshift less than 0.6: 4100-5500Å;
Redshift larger than 0.6: 3750-4100Å.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table14.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Cluster Galaxy cluster name
9- 12 I4 --- ID [1/1480] Galaxy identification number
14- 18 F5.2 0.1nm HzetaA [-1.03/5.15]? The HζA line index (1)
20- 24 F5.3 mag CN3883 [0.032/0.438]? The CN3883 line index (1)
26- 30 F5.2 0.1nm CaHK [3.54/31.43]? The CaHK line index (1)
32- 36 F5.3 --- D4000 [1.226/3.137]? The D4000 line index (1)
38- 42 F5.2 0.1nm HdeltaA [-5.68/8.27]? The HδA line index (1)
44- 48 F5.3 mag CN1 [0.014/0.152]? The CN1 line index (1)
50- 54 F5.3 mag CN2 [0.02/0.178]? The CN2 line index (1)
56- 60 F5.2 0.1nm G4300 [-1.36/7.98]? The G4300 line index (1)
62- 66 F5.2 0.1nm HgammaA [-9.76/7.0]? The HγA line index (1)
68- 72 F5.2 0.1nm Fe4383 [-0.05/6.89]? The Fe4383 line index (1)
74- 77 F4.2 0.1nm C4668 [0.72/9.95]? The C4668 line index (1)
79- 84 F6.2 0.1nm Hbeta [-18.43/5.13]? The Hβ line index (1)
86- 91 F6.2 0.1nm HbetaG [-17.99/5.04]? The HβG line index (1)
93- 96 F4.2 0.1nm Mgb [0.61/9.31]? The Mgb line index (1)
98-101 F4.2 0.1nm Fe5270 [0.67/5.77]? The Fe5270 line index (1)
103-106 F4.2 0.1nm Fe5335 [0.49/4.58]? The Fe5335 line index (1)
108-111 F4.2 0.1nm e_HzetaA [0.03/1.0]? Uncertainty in HzetaA (2)
113-117 F5.3 mag e_CN3883 [0.001/0.039]? Uncertainty in CN3883 (2)
119-122 F4.2 0.1nm e_CaHK [0.07/1.55]? Uncertainty in CaHK (2)
124-128 F5.3 --- e_D4000 [0.001/0.031]? Uncertainty in D4000 (2)
130-133 F4.2 0.1nm e_HdeltaA [0.03/0.84]? Uncertainty in HdeltaA (2)
135-139 F5.3 mag e_CN1 [0.001/0.019]? Uncertainty in CN1 (2)
141-145 F5.3 mag e_CN2 [0.001/0.022]? Uncertainty in CN2 (2)
147-150 F4.2 0.1nm e_G4300 [0.02/0.64]? Uncertainty in G4300 (2)
152-155 F4.2 0.1nm e_HgammaA [0.02/0.74]? Uncertainty in HggammaA (2)
157-160 F4.2 0.1nm e_Fe4383 [0.03/0.82]? Uncertainty in Fe4383 (2)
162-165 F4.2 0.1nm e_C4668 [0.02/0.81]? Uncertainty in C4668 (2)
167-170 F4.2 0.1nm e_Hbeta [0.01/0.43]? Uncertainty in Hbeta (2)
172-175 F4.2 0.1nm e_HbetaG [0.01/0.38]? Uncertainty in HbetaG (2)
177-180 F4.2 0.1nm e_Mgb [0.01/0.44]? Uncertainty in Mgb (2)
182-185 F4.2 0.1nm e_Fe5270 [0.01/0.46]? Uncertainty in Fe5270 (2)
187-190 F4.2 0.1nm e_Fe5335 [0.01/0.43]? Uncertainty in Fe5335 (2)
--------------------------------------------------------------------------------
Note (1): The indices have been corrected for galaxy velocity dispersion and
aperture corrected.
Note (2): Determined from the local S/N.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 24-Aug-2018