J/ApJ/949/73 Galaxy morphologies and local densities from WINGS (Vulcani+, 2023)
Clustercentric distance or local density? It depends on galaxy morphology.
Vulcani B., Poggianti B.M., Gullieuszik M., Moretti A., Fritz J.,
Bettoni D., Facciolli B., Fasano G., Omizzolo A.
<Astrophys. J., 949, 73 (2023)>
=2023ApJ...949...73V 2023ApJ...949...73V
ADC_Keywords: Clusters, galaxy; Galaxies, photometry; Galaxies, spectra;
Morphology; Surveys; Optical
Keywords: Galaxies ; Late-type galaxies ; Elliptical galaxies ;
Lenticular galaxies ; Spiral galaxies ; Early-type galaxies ;
Galaxy evolution
Abstract:
Determining which between projected local density and distance from
the cluster center plays a major role in regulating morphological
fractions in clusters is a longstanding debate. Reaching a definitive
answer will shed light on the main physical mechanisms at play in the
most extreme environments. Here we make use of the data from the
OmegaWINGS survey, currently the largest survey of clusters in the
local universe extending beyond 2 virial radii from the cluster cores,
to extend the previous analysis outside the virial radius. Local
density and clustercentric distance seems to play different roles for
galaxies of different morphology: the fraction of elliptical galaxies
mainly depends on local density, suggesting that their formation was
linked to the primordial densities, which now correspond to the
cluster cores. Only the fraction of low-mass ellipticals shows an
anticorrelation with clustercentric distance, suggesting a different
origin for these objects. Excluding elliptical galaxies, the relative
fraction of S0s and spirals instead depends on local density only far
from the cluster cores, while within the virial radius their
proportion is regulated by distance, suggesting that cluster-specific
processes halt the star formation and transform Sp galaxies into S0s.
This interpretation is supported by literature results on the
kinematical analysis of early- and late-type galaxies, according to
which fast and slow rotators have distinct dependencies on halo mass
and local density.
Description:
We base our analysis on the WIde-field Nearby Galaxy-cluster Survey
(WINGS; Fasano+ 2006A&A...445..805F 2006A&A...445..805F; Moretti+ 2014A&A...564A.138M 2014A&A...564A.138M),
a multiwavelength survey of 76 clusters of galaxies with 0.04<z<0.07
X-ray selected from ROSAT All Sky Survey data (see IX/30), and on its
extension, OmegaWINGS, which includes additional observations for 46
of these clusters (Gullieuszik+ 2015, J/A+A/581/A41;
Moretti+ 2017, J/A+A/599/A81).
Briefly, the WINGS survey is mainly based on optical B, V imaging that
covers a field of view (Varela+ 2009, J/A+A/497/667). A spectroscopic
survey for a subsample of 48 clusters was obtained with the
spectrographs WYFFOS at the William Herschel Telescope (WHT) and 2dF
at the Anglo-Australian Telescope (AAT) (Cava+ 2009, J/A+A/495/707).
See Section 2.
With this paper, we release both the local density estimation and the
morphologies for the full WINGS+OmegaWINGS sample (see Appendix A).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table6.dat 56 52322 The projected local densities catalog
table7.dat 53 68635 The galaxy morphologies catalog
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See also:
IX/30 : Second ROSAT PSPC Catalog (ROSAT, 2000)
J/MNRAS/281/799 : XBACs, the sample (Ebeling+, 1996)
J/A+AS/122/399 : K and evolutionary corrections (Poggianti, 1997)
J/MNRAS/301/881 : The ROSAT brightest cluster sample - I. (Ebeling+, 1998)
J/MNRAS/318/333 : Extended ROSAT Bright Cluster Sample (Ebeling+ 2000)
J/ApJ/542/673 : Morphological types of galaxies in clusters (Fasano+, 2000)
J/ApJ/549/172 : X-ray-detected, poor groups galaxy populations (Tran+, 2001)
J/ApJS/147/1 : Classification of nearby galaxies (Conselice+, 2003)
J/ApJ/591/53 : I photometry of Cl 0024+16 (Treu+, 2003)
J/A+A/451/881 : ESIS BVR catalog, ELAIS-S1 (Berta+, 2006)
J/A+A/495/707 : WINGS spectroscopy of 48 galaxy clusters (Cava+, 2009)
J/A+A/497/667 : WINGS: Deep opt. phot. of 77 nearby clusters (Varela+, 2009)
J/MNRAS/404/1490 : Shapes of BCGs in nearby clusters shapes (Fasano+, 2010)
J/MNRAS/416/727 : Padova-Millennium Galaxy and Group Catalogue (Calvi+, 2011)
J/MNRAS/413/813 : ATLAS3D project. I. (Cappellari+, 2011)
J/MNRAS/414/888 : ATLAS3D project. III. (Emsellem+, 2011)
J/MNRAS/420/926 : Morphology of galaxies in WINGS clusters (Fasano+, 2012)
J/A+A/581/A41 : OmegaWINGS BV phot. of galaxy clusters (Gullieuszik+, 2015)
J/A+A/607/A81 : Properties of the sample of clusters (Biviano+, 2017)
J/A+A/599/A81 : OmegaWINGS local clusters of gal. redshifts (Moretti+, 2017)
J/MNRAS/471/1428 : MASSIVE Survey. VII. (Veale+, 2017)
J/A+A/637/A54 : WINGS cluster survey 2nd u-band extension (D'Onofrio+, 2020)
J/ApJ/927/91 : Stripping & unwinding gal. from WINGS (Vulcani+, 2022)
Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- --- [WINGS]
6- 24 A19 --- WINGS Galaxy identifier (JHHMMSS.ss+DDMMSS.s) (1)
26- 36 F11.7 deg RAdeg Right Ascension (J2000) (1)
38- 48 F11.7 deg DEdeg [-62/22.4] Declination (J2000) (1)
50- 56 F7.4 [Mpc-2] logSigma [-0.4/2.8] log local density;
galaxies/Mpc2 (2)
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Note (1): Galaxy identifiers and coordinates (taken from
Fasano+ 2006A&A...445..805F 2006A&A...445..805F and Gullieuszik+ 2015, J/A+A/581/A41).
Note (2): Local density estimations, expressed in a logarithmic unit:
logΣ=log[10/(π*(R10[Mpc])2)],
with R radius of the area containing 10 neighbors, expressed in Mpc.
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- --- [WINGS]
6- 24 A19 --- WINGS Galaxy identifier (JHHMMSS.ss+DDMMSS.s) (1)
26- 36 F11.7 deg RAdeg Right Ascension (J2000) (1)
38- 48 F11.7 deg DEdeg [-62/79] Declination (J2000) (1)
50- 53 F4.1 --- TType [-9/10] Broad morphological class
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Note (1): Galaxy identifiers and coordinates (taken
from Fasano+ 2012, J/MNRAS/420/926; Gullieuszik+ 2015, J/A+A/581/A41)
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 11-Jul-2025