J/MNRAS/521/1292 Omega/WINGS clusters/fields galaxies (Perez-Millan+, 2023)
The relation between morphology, star formation history, and environment in
local Universe galaxies.
Perez-Millan D., Fritz J., Gonzalez-Lopezlira R.A., Moretti A.,
Cervantes Sodi B., Vulcani B., Gullieuszik M., Bruzual G., Charlot S.,
Bettoni D.
<Mon. Not. R. Astron. Soc. 521, 1292-1315 (2023)>
=2023MNRAS.521.1292P 2023MNRAS.521.1292P (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies ; Galaxies, group ; Clusters, galaxy ; Positional data ;
Redshifts ; Star Forming Region ; Stars, masses ; Extinction ;
Stars, ages ; Magnitudes, absolute ; Photometry ; Spectroscopy ;
Optical ; Infrared ; X-ray sources ; Velocity dispersion ;
Morphology
Keywords: galaxies: clusters: general - galaxies: evolution -
galaxies: fundamental parameters - galaxies: interactions -
galaxies: star formation - galaxies: stellar content
Abstract:
The observed properties of galaxies are strongly dependent on both
their total stellar mass and their morphology. Furthermore, the
environment is known to play a strong role in shaping them. The galaxy
population in the local Universe that is located in virialized
clusters is found to be red, poorly star-forming, and mostly composed
of early morphological types. Towards a holistic understanding of the
mechanisms that drive galaxy evolution, we exploit the
spectrophotometric data from the WINGS and OmegaWINGS local galaxy
cluster surveys, and study the role of both the local and the
large-scale environments. We attempt to disentangle their effects from
the intrinsic characteristics of the galaxies, in shaping the star
formation activity at fixed morphological type and stellar mass. Using
a sample of field galaxies from the same surveys for comparison, we
analyse the effects of the environment, embodied by the local density,
clustercentric distance, and close neighbours, respectively, on the
star formation histories of cluster galaxies. We find that local
effects have a more relevant impact on galaxy stellar properties than
the large-scale environment, and that morphology needs to be taken
into account to pinpoint the mechanisms that are driving the influence
of clusters in galaxy evolution.
Description:
Observations in the local Universe have shown that galaxies in
clusters are significantly different from their field counterparts, in
terms of both stellar content and morphology. These differences point
to a quite rapid evolution of cluster galaxies, compared to field
ones, and to the well-known morphology-density (MD) relation.
Leveraging current facilities, in this work we exploit one of the
largest, most complete, and most homogeneous data bases of cluster
galaxies in the local Universe WINGS and OmegaWINGS (0.04 < z < 0.07,
having both photometry images and optical spectra). The ultimate goal
of this paper is to establish causal connections between the galactic
stellar population properties and the characteristics of the
environment in which they are found, and possibly disentangle their
importance. We try to perform an analysis of the stellar population
properties of galaxies in clusters and their environments. As this
work heavily relies on the spectrophotometric code SINOPSIS. More we
make a distinction between 'local' and 'large-scale' environment,
local by the space immediately surrounding the galaxies quantified by
galaxy number density and large-scale by structure to which a galaxy
belongs, such as a cluster, a group, or the field, (i.e. see more in
section Introduction).
As discussed in section 2, photometry for the central parts (∼30
arcmin) of 77 clusters was obtained by WINGS, using the 2.5 m Isaac
Newton Telescope (INT/WFC) for the northern clusters, and the
MPG/ESO-2.2 m telescope for the southern clusters. The spectroscopic
follow-up of 46 of them (Cava et al. 2009A&A...495..707C 2009A&A...495..707C,
Cat. J/A+A/495/707) was taken through the AF2/WYFFOS multifiber
spectrograph, mounted on the 4.2 m William Herschel Telescope (WHT)
for the northern clusters, while the southern clusters were observed
with the 2dF multifiber spectrograph on the 3.9 m Anglo Australian
Telescope (AAT). OmegaWINGS represents the extension to a wider field
(∼1°, up to about 2.5 virial radii) for 46 clusters, randomly
selected from the 57 clusters that can be observed with the VLT to
span a wide range in X-ray luminosity and hence probe a complete range
in halo masses. OmegaWINGS was spectroscopically followed up as well;
33 of the 46 clusters were observed with the VST fibre spectrograph.
WINGS spectra cover a range of ∼3800-7000 Å, with an intermediate
resolution of 6-9 Å, and a fibre aperture of 1.6 arcsec for
northern clusters and 2 arcsec for southern clusters. OmegaWINGS
spectra cover ∼3800-9000 Å, with a resolution of 3.5-6 Å, and a
fibre diameter of 2.16 arcsec.
Next to select galaxies, we computed stellar masses (and further
galaxies such as colour, SFR, and internal structure informations,
morphologies) also as explained in section 3 with sinopsis which
reproduce an observed spectrum uses theoretical spectra of simple
stellar populations with 12 different ages. Also we used
parametrizations of the cluster environment as projected distance to
the cluster centre, the projected local density (LD), and the
projected distance to the nearest galaxy. Properties results from high
quality of spectrum fits (best chi2) are available in cluster.dat and
field.dat for respectively galaxy members of our 43 clusters sample
tablec1.dat and field galaxies, (i.e see section 3 and 4 for more
details).
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablec1.dat 38 76 *Basic properties of the WINGS/OmegaWINGS
clusters sample
cluster.dat 356 9278 Astrometrics and physical properties as ages,
masses and SFRs of WINGS cluster galaxies
field.dat 305 1572 Astrometrics and physical properties as ages,
masses and SFRs of WINGS field galaxies
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Note on tablec1.dat: In this work, we have used 3097 individual galaxy spectra
from WINGS and all 17985 spectra from OmegaWINGS, in a total of 43 clusters.
From these, 2711 WINGS and 7627 OmegaWINGS objects are cluster member galaxies.
The final sample from WINGS and OmegaWINGS, taking into account the criteria
defined in section 2, contains 4598 members (8845 after weighting)
in 43 clusters.
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See also:
J/MNRAS/432/3141 : Morphological classification of PM2GC galaxies (Calvi+,2013)
J/MNRAS/420/926 : Morphology of galaxies in WINGS clusters (Fasano+, 2012)
J/MNRAS/416/727 : Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)
J/MNRAS/318/333 : Extended ROSAT Bright Cluster Sample (Ebeling+ 2000)
J/MNRAS/301/881 : The ROSAT brightest cluster sample - I. (Ebeling+, 1998)
J/MNRAS/281/799 : XBACs, the sample (Ebeling+, 1996)
J/A+A/607/A81 : Properties of the sample of clusters (Biviano+, 2017)
J/A+A/599/A81 : OmegaWINGS local clusters of galaxies redshifts
(Moretti+, 2017)
J/A+A/599/A83 : ELG and AGN in WINGS clusters (Marziani+, 2017)
J/A+A/581/A41 : OmegaWINGS BV photometry of galaxy clusters
(Gullieuszik+, 2015)
J/A+A/566/A32 : Equivalent widths of WINGS galaxies (Fritz+, 2014)
J/A+A/497/667 : WINGS: Deep optical phot. of 77 nearby clusters
(Varela+, 2009)
J/A+A/495/707 : WINGS spectroscopy of 48 galaxy clusters (Cava+, 2009)
J/ApJ/949/73 : Galaxy morphologies and local densities from WINGS
(Vulcani+, 2023)
J/ApJ/927/91 : Stripping & unwinding galaxies from WINGS surveys
(Vulcani+, 2022)
J/ApJS/219/8 : SFR for WISE + SDSS spectroscopic galaxies (Chang+, 2015)
J/AJ/151/78 : Jellyfish galaxy candidates in galaxy clusters
(Poggianti+, 2016)
Byte-by-byte Description of file: tablec1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- Cluster Cluster field name
9- 15 F7.5 --- z The mean redshift
17- 20 I4 km/s sigma ? The velocity dispersion from data Biviano
et al. (2017A&A...607A..81B 2017A&A...607A..81B,
Cat. J/A+A/607/A81) and Gullieuszik et al.
(2020ApJ...899...13G 2020ApJ...899...13G, Cat. J/ApJ/899/13)
22- 26 F5.3 Mpc R200 ? The virial radius
28- 32 F5.2 [10-7W] logLX ? The X-ray luminosity taken from the ROSAT
All-Sky Survey
34 A1 --- Wings Flag to indicates if the cluster was
observed in spectroscopy with WINGS
36 A1 --- OWings Flag to indicates if the cluster was
observed in spectroscopy with Omega Wings
38 A1 --- Sinopsis Flag to whether WINGS/OmegaWINGS spectra
have sufficient signal-to-noise ratio to
run the sinopsis code
--------------------------------------------------------------------------------
Byte-by-byte Description of file: cluster.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 24 A24 --- WINGS WINGS identifier designation as
WINGSJHHMMSS.ss+DDMMSS.s (WINGS_ID)
26- 35 F10.6 deg RAdeg Right ascension (J2000) (RAJ2000)
37- 46 F10.6 deg DEdeg Declination (J2000) (DECJ2000)
48- 54 A7 --- Cluster Cluster designation as ANNNN (Cluster)
56- 66 F11.9 --- zgal Redshift of the galaxies (z_gal)
68- 73 F6.2 Mpc DL Distance luminosity (Lum_dist)
75- 82 F8.4 --- rChi Reduced chi squared of the SINOPSIS model
spectral profile fit (redchi)
84- 89 F6.4 mag AVy Extinction of the youngest stellar
populations as age ≤2*10^7 yr (Av_y)
91- 96 F6.4 mag Av Average extinction value for all the
stellar populations (Av)
98-104 F7.4 Msun/yr SFR1 SFR in first age-bin 0-19.95 Myr as
described in section 3 were selected based
on the presence and intensity of stellar
population features (SFR1) (G1)
106-111 F6.4 Msun/yr SFR2 SFR in second age-bin 19.95-571.5 Myr as
described in section 3 were selected based
on the presence and intensity of stellar
population features (SFR2) (G1)
113-118 F6.4 Msun/yr SFR3 SFR in third age-bin from 0.5715-5.754 Gyr
as described in section 3 were selected
based on the presence and intensity of
stellar population features (SFR3) (G1)
120-126 F7.4 Msun/yr SFR4 SFR in fourth age-bin from 5.754-tu Gyr
as described in sect. 3 were selected based
on the presence and intensity of stellar
population features (SFR4) (G1)
128-137 E10.5 Msun M*a3 Stellar mass, calculated according to
definition n.3 of the SFR3, normalized to
aperture magnitude or spectrum (AMass3)
139-148 E10.5 Msun TotM*3 Total stellar mass calculated according to
definition n.3 of the SFR3 (TotMass3)
150-159 E10.5 Msun M*a2 Stellar mass, calculated according to
definition n.2 of the SFR2, normalized to
aperture magnitude or spectrum (AMass2)
161-170 E10.5 Msun TotM*2 Total stellar mass calculated according to
definition n.2 of the SFR2 (TotMass2)
172-181 E10.5 Msun M*a1 Stellar mass, calculated according to
definition n.1 of the SFR1, normalized to
aperture magnitude or spectrum (AMass1)
183-192 E10.5 Msun TotM*1 Total stellar mass calculated according to
definition n.1 of the SFR1 (TotMass1)
194-200 F7.4 [yr] logAgelwV Logarithm of the luminosity-weighted age
in V-band (lVwage)
202-208 F7.4 [yr] logAgemw Logarithm of the mass-weighted age (mwage)
210-216 F7.2 0.1nm Hb The HΒ index (Hb)
218-224 F7.2 0.1nm Ha The Hα index (Ha)
226-232 F7.3 --- D4000 The D4000 4000Å break index (D4000)
234-240 F7.3 --- Dn4000 The Dn4000 spectral indicator (Dn4000)
242-246 F5.2 --- SNR Signal to noise ratio (SNR)
248-254 F7.3 mag BfibMag Absolute magnitude with fiber aperture in
B-band (ABSBfib)
256-262 F7.3 mag VfibMag Absolute magnitude with fiber aperture in
V-band (ABSVfib)
264-269 F6.3 mag Vmag Apparent magnitude with automatic aperture
in V-band (Vauto)
271-276 F6.3 mag Vfibmag Apparent magnitude with fiber aperture in
V-band (V_fib)
278-283 F6.3 mag Bmag Apparent magnitude with automatic aperture
in B-band (Bauto)
285-290 F6.3 mag Bfibmag Apparent magnitude with fiber aperture in
B-band (B_fib)
292-298 F7.3 mag VtotMag Total absolute magnitude in V-band
(ABSVtot)
300-306 F7.3 mag BtotMag Total absolute magnitude in B-band
(ABSBtot)
308-314 F7.5 --- zcl Redshift of the cluster (z_cl)
316-321 F6.1 km/s sigma The cluster velocity dispersion
σcl (sigma_cl)
323-326 F4.2 Mpc R200 The viral radius as defined by equation 1
of the section 2.3 (r200) (1)
328-331 F4.1 [10-7W] logLX The X-ray luminosity mostly taken from
ROSAT all-sky surveys (logLX)
333-342 F10.8 Mpc RXproj The clustercentric distance radius is
calculated in projection to the centre of
the cluster in the X-ray emission (RXproj)
344-348 A5 --- Morph Flag for cluster morphology of neighbour
galaxies as early and late types
(neigh_morph)
350-356 F7.4 --- RRv The cluster RRv quantity (RRv)
--------------------------------------------------------------------------------
Note (1): The distance to the closest neighbour galaxy is the projected
distance, normalized by the virial radius of the neighbour
(Rvir,neigh), calculated as the radius of a sphere whose density
of baryonic matter (approximated by the stellar mass obtained through
sinopsis) is equal to 200 times the critical density of the Universe
at that redshift.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: field.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 24 A24 --- WINGS WINGS identifier desingation as
WINGSJHHMMSS.ss+DDMMSS.s (WINGS_ID)
26- 35 F10.6 deg RAdeg Right ascension (J2000) (RAJ2000)
37- 46 F10.6 deg DEdeg Declination (J2000) (DECJ2000)
48- 54 A7 --- Cluster Cluster designation as ANNNN (Cluster)
56- 66 F11.9 --- zgal Redshift of the galaxies (z_gal)
68- 74 F7.2 Mpc DL Distance luminosity (Lum_dist)
76- 83 F8.4 --- rChi Reduced chi squared of the SINOPSIS model
spectral profile fit (redchi)
85- 90 F6.4 mag AVy Extinction of the youngest stellar
populations as age ≤2*10^7 yr (Av_y)
92- 97 F6.4 mag Av Average extinction value for all the
stellar populations (Av)
99-105 F7.4 Msun/yr SFR1 SFR in first age-bin from 0 to 19.95 Myr
as described in section 3 were selected
based on the presence and intensity of
stellar population features (SFR1) (G1)
107-112 F6.4 Msun/yr SFR2 SFR in second age-bin from 19.95 to
571.5 Myr as described in sect. 3 were
selected based on presence and intensity
of stellar population features (SFR2) (G1)
114-119 F6.4 Msun/yr SFR3 SFR in third age-bin from 0.5715-5.754 Gyr
as described in section 3 were selected
based on the presence and intensity of
stellar population features (SFR3) (G1)
121-127 F7.4 Msun/yr SFR4 SFR in fourth age-bin from 5.754-tu Gyr
as described in section 3 were selected
based on the presence and intensity of
stellar population features (SFR4) (G1)
129-138 E10.5 Msun M*a3 Stellar mass, calculated according to
definition n.3 of the SFR3, normalized to
aperture magnitude or spectrum (AMass3)
140-149 E10.5 Msun TotM*3 Total stellar mass calculated according to
definition n.3 of the SFR3 (TotMass3)
151-160 E10.5 Msun M*a2 Stellar mass, calculated according to
definition n.2 of the SFR2, normalized to
aperture magnitude or spectrum (AMass2)
162-171 E10.5 Msun TotM*2 Total stellar mass calculated according to
definition n.2 of the SFR2 (TotMass2)
173-182 E10.5 Msun M*a1 Stellar mass, calculated according to
definition n.1 of the SFR1, normalized to
aperture magnitude or spectrum (AMass1)
184-193 E10.5 Msun TotM*1 Total stellar mass calculated according to
definition n.1 of the SFR1 (TotMass1)
195-201 F7.4 [yr] logAgelwV Logarithm of the luminosity-weighted age
in V-band (lVwage)
203-209 F7.4 [yr] logAgemw Logarithm of the mass-weighted age (mwage)
211-217 F7.2 0.1nm Hb The HΒ index (Hb)
219-225 F7.2 0.1nm Ha The Hα index (Ha)
227-232 F6.3 --- D4000 The D4000 4000Å break index (D4000)
234-239 F6.3 --- Dn4000 The Dn4000 spectral indicator (Dn4000)
241-245 F5.2 --- SNR Signal to noise ratio (SNR)
247-253 F7.3 mag BfibMag Absolute magnitude with fiber aperture in
B-band (ABSBfib)
255-261 F7.3 mag VfibMag Absolute magnitude with fiber aperture in
V-band (ABSVfib)
263-268 F6.3 mag Vmag Apparent magnitude with automatic aperture
in V-band (Vauto)
270-275 F6.3 mag Vfibmag Apparent magnitude with fiber aperture in
V-band (V_fib)
277-282 F6.3 mag Bmag Apparent magnitude with automatic aperture
in B-band (Bauto)
284-289 F6.3 mag Bfibmag Apparent magnitude with fiber aperture in
B-band (B_fib)
291-297 F7.3 mag VtotMag Total absolute magnitude in V-band
(ABSVtot)
299-305 F7.3 mag BtotMag Total absolute magnitude in B-band
(ABSBtot)
--------------------------------------------------------------------------------
Global notes:
Note (G1): As described in section 3, based the stellar population properties
derived with the spectrophotometric code sinopsis, the best fit is
obtained, the solution is far from unique. Thus, a further binning
in age is implemented, such that the final resolution is lowered
to four age bins. The derived SFRs for these four ages constitute
the final SFH. The ages were selected based on the presence and
intensity of stellar population features (SFR1, SFR2, SFR3, SFR4).
SFR1 : characterized by emission lines and the strongest ultraviolet
emission,
SFR2 : by hydrogen lines from the Balmer series reach their
maximum intensity in absorption, while the Ca K,H UV lines still
have low equivalent width.
SFR3 : by the intensities of Balmer absorption lines decrease as
stellar ages increase, while the Ca absorption lines reach their
maximum intensity.
SFR4 : by stellar populations in this age bin are reddest, and
display the highest 4000 Å Break (D4000) values. Other spectral
characteristics reach an asymptotic behaviour at these ages.
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History:
From electronic version of the journal
License: CC-BY-4.0
(End) Luc Trabelsi [CDS] 26-May-2026