The Tully-Fisher Relation in Coma and Virgo Cluster S0 Galaxies

2003 ◽  
Vol 126 (6) ◽  
pp. 2622-2634 ◽  
Author(s):  
J. L. Hinz ◽  
G. H. Rieke ◽  
N. Caldwell
Keyword(s):  
Virgo Cluster ◽  
Fisher Relation ◽  
S0 Galaxies

scholarly journals Nuclear Stellar Disks in E/S0 Galaxies

1997 ◽  
Vol 163 ◽  
pp. 626-629
Author(s):  
Walter Jaffe ◽  
Frank van den Bosch
Keyword(s):  
Black Hole ◽  
Virgo Cluster ◽  
Lower Mass ◽  
Central Black Hole ◽  
Color Gradients ◽  
Different Color ◽  
S0 Galaxies ◽  
High Metallicity

AbstractNew HST images and spectra of the nuclear disks in two Virgo Cluster E/S0 galaxies reveal that they were probably formed together with their parent galaxies. The two galaxies show very different color gradients. This is most likely caused by the escape of high metallicity gas from early stars in the lower mass galaxy. One galaxy shows strong kinematic evidence for a massive central black hole.

scholarly journals The Galactic Neighbourhood

1978 ◽  
Vol 79 ◽  
pp. 71-91 ◽  
Author(s):  
G. A. Tammann ◽  
R. Kraan
Keyword(s):  
Luminosity Function ◽  
Velocity Dispersion ◽  
Radial Component ◽  
Virgo Cluster ◽  
Cluster Centre ◽  
Different Types ◽  
Peculiar Motion ◽  
The Mean ◽  
S0 Galaxies ◽  
Hubble Flow

Several properties of the 131 galaxies known within 9. 1 Mpc are investigated. 88 of these galaxies are concentrated into eight groups, leaving 33 percent of true field galaxies. There are E/S0 and S0 galaxies among the field galaxies; their types must be of cosmogonic origin. the groups have small velocity dispersion which limits the mean mass-to-light ratio for the different types of group galaxies to m/L < 20. Within the supergalactic plane the deviation from an ideal Hubble flow are small: the changes of ΔHO/<HO> with distance and direction are not larger than ten percent; the radial component of the peculiar motion of field galaxies is <25 km s−1. the differential luminosity function of S/Im galaxies is well approximated by a Gaussian with and . the luminosity function of E/S0 galaxies is much flatter with a possible minimum, separating true E's and dwarf ellipticals (Reaves, 1977). the sample galaxies are strongly concentrated toward the supergalactic plane; at a distance of 4 Mpc of the plane the luminosity density drops to half its value. There is also a pronounced luminosity density decrease with increasing distance from the Virgo cluster centre; at a distance of 30 Mpc the density has decreased by more than a factor of 104. the best estimate of the mean luminosity density within a sphere of 30 Mpc radius centered on the Virgo cluster is 1.5 · 108 L⊙ Mpc−3.

A Comparison of Coma Cluster S0 Galaxies with the Tully-Fisher Relation for Late-Type Spirals

2001 ◽  
Vol 121 (2) ◽  
pp. 683-691 ◽  
Author(s):  
Joannah L. Hinz ◽  
Hans-Walter Rix ◽  
Gary M. Bernstein
Keyword(s):  
Coma Cluster ◽  
Late Type ◽  
Fisher Relation ◽  
S0 Galaxies

scholarly journals Understanding the transformation of spirals to lenticulars

2014 ◽  
Vol 10 (S309) ◽  
pp. 225-226
Author(s):  
Evelyn J. Johnston ◽  
Alfonso Aragón-Salamanca ◽  
Michael R. Merrifield
Keyword(s):  
Star Formation ◽  
Virgo Cluster ◽  
Sequence Of Events ◽  
Star Formation Activity ◽  
Central Regions ◽  
Individual Star ◽  
Components Analysis ◽  
The Individual ◽  
Star Formation Histories ◽  
S0 Galaxies

AbstractBy studying the individual star-formation histories of the bulges and discs of lenticular (S0) galaxies, it is possible to build up a sequence of events that leads to the cessation of star formation and the consequent transformation from the progenitor spiral. In order to separate the bulge and disc stellar populations, we spectroscopically decomposed long-slit spectra of Virgo Cluster S0s into bulge and disc components. Analysis of the decomposed spectra shows that the most recent star formation activity in these galaxies occurred within the bulge regions, having been fuelled by residual gas from the disc. These results point towards a scenario where the star formation in the discs of spiral galaxies are quenched, followed by a final episode of star formation in the central regions from the gas that has been funnelled inwards through the disc.

scholarly journals Study of the Virgo Cluster Using the B ‐Band Tully‐Fisher Relation

1997 ◽  
Vol 108 (2) ◽  
pp. 417-448 ◽  
Author(s):  
Naoki Yasuda ◽  
Masataka Fukugita ◽  
Sadanori Okamura
Keyword(s):  
Virgo Cluster ◽  
Fisher Relation

scholarly journals Detailed Surface Photometry of Dwarf Elliptical and Dwarf S0 Galaxies in the Virgo Cluster

1999 ◽  
Vol 517 (2) ◽  
pp. 650-660 ◽  
Author(s):  
Barbara S. Ryden ◽  
Donald M. Terndrup ◽  
Richard W. Pogge ◽  
Tod R. Lauer
Keyword(s):  
Virgo Cluster ◽  
Surface Photometry ◽  
Detailed Surface ◽  
S0 Galaxies

scholarly journals A Tully-Fisher Relation for S0 Galaxies

1999 ◽  
Vol 117 (6) ◽  
pp. 2666-2675 ◽  
Author(s):  
Eyal Neistein ◽  
Dan Maoz ◽  
Hans-Walter Rix ◽  
John L. Tonry
Keyword(s):  
Fisher Relation ◽  
S0 Galaxies
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