J/other/AstBu/73.124 Galaxies in the Local Supercluster band (Kashibadze+, 2018)
Surveying the Local Supercluster Plane.
Kashibadze O.G., Karachentsev I.D., Karachentseva V.E.
<Astrophys. Bull., 73, 124-141 (2018)>
=2018AstBu..73..124K 2018AstBu..73..124K (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; Redshifts
Keywords: galaxies: clusters: individual: Virgo -
galaxies: kinematics and dynamics -
galaxies: distances and redshifts - galaxies: groups
Abstract:
We investigate the distribution and velocity field of galaxies
situated in a band of 100x20 degrees centered on M87 and oriented
along the Local supercluster plane. Our sample amounts 2158 galaxies
with radial velocities less than 2000 km/s. Of them, 1119 galaxies
(52%) have distance and peculiar velocity estimates. About 3/4 of
early-type galaxies are concentrated within the Virgo cluster core,
most of the late-type galaxies in the band locate outside the virial
radius. Distribution of gas-rich dwarfs with MHI> M* looks to be
insensitive to the Virgo cluster presence. Among 50 galaxy groups in
the equatorial supercluster band 6 groups have peculiar velocities
about 500-1000km/s comparable with virial motions in rich clusters.
The most cryptic case is a flock of nearly 30 galaxies around NGC4278
(Coma I cloud), moving to us with the mean peculiar velocity of
-840km/s. This cloud (or filament?) resides at a distance of 16.1Mpc
from us and approximately 5Mpc away from the Virgo center. Galaxies
around Virgo cluster exhibit Virgocentric infall with an amplitude of
about 500 km/s. Assuming the spherically symmetric radial infall, we
estimate the radius of the zero-velocity surface to be
R0=(7.0±0.3)Mpc that yields the total mass of Virgo cluster to be
(7.4±0.9)x1014 solar masses, in tight agreement with its virial
mass estimates. We conclude that the Virgo outskirts does not contain
significant amounts of dark mater beyond its virial core.
Description:
The list of 2158 galaxies with supergalactic coordinates
SGL = [52.9, 152.9] degrees, SGB = [-12.4, +7.6] degrees and radial
velocities VLG<2000km/s. 1119 galaxies have distance measurements.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
lsci.dat 95 2158 Galaxies in the Local Supercluster band
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Byte-by-byte Description of file: lsci.dat
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Bytes Format Units Label Explanations
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1- 24 A24 --- Name Galaxy name
26- 27 I2 h RAh Right ascension (J2000.0)
28- 29 I2 min RAm Right ascension (J2000.0)
30- 33 F4.1 s RAs Right ascension (J2000.0)
34 A1 --- DE- Declination sign (J2000.0)
35- 36 I2 deg DEd Declination (J2000.0)
37- 38 I2 arcmin DEm Declination (J2000.0)
39- 40 I2 arcsec DEs Declination (J2000.0)
42- 47 F6.2 deg SGL Supergalactic longitude
49- 54 F6.2 deg SGB Supergalactic latitude
56- 59 I4 km/s VLG Radial velocity relative to the Local Group
centroid (1)
61- 63 A3 --- Type Morphological type (2)
65- 69 F5.2 mag BT Apparent B-magnitude (3) (4)
71- 73 I3 km/s W50 ? 21cm HI line width at half maximum (3)
74 A1 --- u_W50 Uncertainty flag on W50
75- 79 F5.2 mag m21 ? Apparent HI-magnitude (3)
81- 85 F5.2 mag m-M ? Distance modulus
87- 91 F5.2 Mpc D ? Galaxy distance
93- 95 A3 --- Meth Method applied to determine distance (5)
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Note (1): Apex parameters according to
Karachentsev & Makarov (1996AJ....111..794K 1996AJ....111..794K).
Note (2): We use de Vaucouleurs classification; in addition to the de
Vaucouleurs types we note also for compact objects: Ec (compact ellipticals)
and BCD (blue compact dwarfs); for dwarfs of low and very low surface
brightness we use the designations: Ed, Edn (elliptical shape), Sph, Sphn
(round); the symbol 'n' means a presence of a star-like nucleus; I, Ir
(diffuse objects having no blue knots).
Note (3): Data from HyperLEDA (http://leda.univ-lyon1.fr)
(Makarov et al. 2014A&A...570A..13M 2014A&A...570A..13M).
Note (4): Data from NASA Extragalactic Database = NED
(http://ned.ipac.caltech.edu).
Values without decimals indicate our visual estimates.
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, Cat. J/ApJ/533/744)
TFb = our estimates based on baryonic TF relation
(Karachentsev et al. 2017AJ....153....6K 2017AJ....153....6K, Cat. J/AJ/153/6)
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Acknowledgements:
Olga Kashibadze, phiruzi(at)gmail.com
References:
Karachentsev, Kaisina & Kashibadze, 2017AJ....153....6K 2017AJ....153....6K, Cat. J/AJ/153/6
The Local Tully-Fisher Relation for Dwarf Galaxies
Karachentsev & Makarov, 1996AJ....111..794K 1996AJ....111..794K
The Galaxy Motion Relative to Nearby Galaxies and the Local Velocity Field
Kashibadze, Karachentsev & Karachentseva, 2020, A&A, in prep.
Structure and kinematics of the Virgo cluster of galaxies
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) Patricia Vannier [CDS] 08-Mar-2020