J/A+A/635/A135 Galaxies around M87 (Kashibadze+, 2020)
Structure and kinematics of the Virgo cluster of galaxies.
Kashibadze O.G., Karachentsev I.D, Karachentseva V.E
<Astron. Astrophys. 635, A135 (2020)>
=2020A&A...635A.135K 2020A&A...635A.135K (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Galaxies, photometry ; Photometry, CCD
Keywords: galaxies: clusters: individual: Virgo
Abstract:
This work considers the Virgo cluster of galaxies, focusing on its
structure, kinematics, and morphological landscape. Our principal aim is to
estimate the virial mass of the cluster. For this purpose, we present a
sample of 1537 galaxies with radial velocities VLG<2600km/s situated
within a region of 30x20 degrees around M87. About half of the galaxies
have distance estimates.
We selected 398 galaxies with distances in the (17±5)Mpc range.
Based on their 1D and 2D number-density profiles and their radial
velocity dispersions, we made an estimate for the virial mass of the
Virgo cluster. Results. We identify the infall of galaxies towards the
Virgo cluster core along the Virgo Southern Extention filament. From a
1D profile of the cluster, we obtain the virial mass estimate of
(6.3±0.9)x1014 solar masses, which is in tight agreement with its
mass estimate via the external infall pattern of galaxies.
We conclude that the Virgo cluster outskirts between the virial radius
and the zero-velocity radius do not contain significant amounts of
dark matter beyond the virial radius.
Description:
Galaxies around M87 with supergalactic coordinates
SGL=[87.9, 117.9] degrees, SGB=[-12.4, +7.6] degrees and radial
velocities VLG<2600km/s. The table contains 1537 galaxies, among
them, 738 galaxies have distance estimates: 358 from public databases
and 380 distances estimated for the first time in this paper
(indicated in the last column as TF or TFb).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
lscii.dat 107 1537 Galaxies around M87 (table 1)
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See also:
J/PAZh/27/403 : Surveying the Local Supercluster Plane (Kashibadze+, 2018)
Byte-by-byte Description of file: lscii.dat
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Bytes Format Units Label Explanations
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1- 23 A23 --- Name Galaxy name
25- 26 I2 h RAh Right ascension (J2000.0)
27- 28 I2 min RAm Right ascension (J2000.0)
29- 32 F4.1 s RAs Right ascension (J2000.0)
33 A1 --- DE- Declination sign (J2000.0)
34- 35 I2 deg DEd Declination (J2000.0)
36- 37 I2 arcmin DEm Declination (J2000.0)
38- 39 I2 arcsec DEs Declination (J2000.0)
41- 46 F6.2 deg SGL Supergalactic longitude
48- 53 F6.2 deg SGB Supergalactic latitude
55- 59 F5.2 deg Rp0 Projected distance of a galaxy from M87
61- 64 I4 km/s VLG Radial velocity relative to the
Local Group centroid
66- 69 A4 --- Type Morphological type (1)
71- 75 F5.2 mag BTmag ? Apparent B-magnitude (2), (3)
77- 81 F5.2 mag Kmag ? Apparent K-magnitude (4)
83- 85 I3 km/s W50 ? 21 cm HI line width at half maximum (2)
87- 91 F5.2 mag m21 ? Apparent $HI$-magnitude (2)
93- 97 F5.2 mag m-M ? Distance modulus
99-103 F5.2 Mpc D ? Galaxy distance
105-107 A3 --- Meth Method applied to determine distance (5)
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Note (1): We determined morphological types of the galaxies based on images from
Sloan Digital Sky Survey (SDSS, Abazajian et al., 2009ApJS..182..543A 2009ApJS..182..543A) and
Panoramic Survey Telescope and Rapid Response System (PanSTARRS,
Chambers et al., 2016arXiv161205560C 2016arXiv161205560C).
Note (2): Data from HyperLEDA (http://leda.univ-lyon1.fr)
(Makarov et al. 2014A&A...570A..13M 2014A&A...570A..13M).
Note (3): Data from NASA Extragalactic Database = NED
(http://ned.ipac.caltech.edu).
Note (4): K-magnitude is calculated from B-magnitude adjusted for the
morphological type of the galaxy according to Jarrett et al.
(2003AJ....125..525J 2003AJ....125..525J).
Note (5): Method applied to determine distance as follows:
cep = from Cepheids luminosity
SN = from supernovae luminosity
sbf = from surface brightness fluctuation
rgb = from the tip of the red giant branch
bs = from the brightest stars luminosity
FP = from the fundamental plane
gc = from luminosity function of globular clusters
tf = from Tully-Fisher (TF) relation; distance estimates from NED
TF = our estimates based on classical TF relation
(Tully & Pierce 2000ApJ...533..744T 2000ApJ...533..744T)
TFb = our estimates based on baryonic TF relation
(Karachentsev et al. 2017AJ....153....6K 2017AJ....153....6K)
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Acknowledgements:
Olga Kashibadze, phiruzi(at)gmail.com
References:
bazajian et al., 2009ApJS..182..543A 2009ApJS..182..543A
The Seventh Data Release of the Sloan Digital Sky Survey
Chambers et al., 2016arXiv161205560C 2016arXiv161205560C
The Pan-STARRS1 Surveys
Jarrett, Chester, Cutri et al., 2003AJ....125..525J 2003AJ....125..525J
The 2MASS Large Galaxy Atlas
Karachentsev, Kaisina & Kashibadze, 2017AJ....153....6K 2017AJ....153....6K, Cat. J/AJ/153/6
The Local Tully-Fisher Relation for Dwarf Galaxies
Kashibadze, Karachentsev & Karachentseva, 2018AstBu..73..124K 2018AstBu..73..124K
Surveying the Local Supercluster Plane
Makarov, Prugniel, Terekhova et al., 2014A&A...570A..13M 2014A&A...570A..13M
HyperLEDA. III. The catalogue of extragalactic distances
Tully & Pierce, 2000ApJ...533..744T 2000ApJ...533..744T, Cat. J/ApJ/533/744
Distances to Galaxies from the Correlation between Luminosities and Lin
Widths. III. Cluster Template and Global Measurement of H0
(End) Olga Kashibadze [SAO, Russia], Patricia Vannier [CDS] 26-Feb-2020