H I observations in the Virgo cluster area. III - All 'member' spirals

1989 ◽  
Vol 69 ◽  
pp. 65 ◽  
Author(s):  
G. Lyle Hoffman ◽  
B. M. Williams ◽  
B. M. Lewis ◽  
George Helou ◽  
E. E. Salpeter
Keyword(s):  
Virgo Cluster ◽  
Cluster Area

Effects of environment on neutral hydrogen distribution for disk galaxies in the Virgo Cluster area

1983 ◽  
Vol 267 ◽  
pp. 35 ◽  
Author(s):  
C. Giovanardi ◽  
G. Helou ◽  
E. E. Salpeter ◽  
N. Krumm
Keyword(s):  
Neutral Hydrogen ◽  
Virgo Cluster ◽  
Disk Galaxies ◽  
Hydrogen Distribution ◽  
Cluster Area

IRAS observations of galaxies in the Virgo cluster area

1988 ◽  
Vol 68 ◽  
pp. 151 ◽  
Author(s):  
George Helou ◽  
Iffat R. Khan ◽  
Ladan Malek ◽  
Lisa Boehmer
Keyword(s):  
Virgo Cluster ◽  
Cluster Area

H I detection survey of a complete magnitude-limited sample of dwarf irregular galaxies in the Virgo Cluster area

1987 ◽  
Vol 63 ◽  
pp. 247 ◽  
Author(s):  
G. Lyle Hoffman ◽  
John Glosson ◽  
George Helou ◽  
E. E. Salpeter ◽  
A. Sandage
Keyword(s):  
Virgo Cluster ◽  
Limited Sample ◽  
Cluster Area ◽  
Irregular Galaxies ◽  
Dwarf Irregular Galaxies

H I observations in the Virgo cluster area

1981 ◽  
Vol 46 ◽  
pp. 267 ◽  
Author(s):  
G. Helou ◽  
E. E. Salpeter ◽  
C. Giovanardi ◽  
N. Krumm
Keyword(s):  
Virgo Cluster ◽  
Cluster Area

Malmquist Bias and the Distance to the Virgo Cluster

1997 ◽  
Vol 485 (1) ◽  
pp. 80-86 ◽  
Author(s):  
Anthony H. Gonzalez ◽  
S. M. Faber
Keyword(s):  
Virgo Cluster

scholarly journals Refining the true parameters of the open cluster NGC 4852

2009 ◽  
Vol 5 (S266) ◽  
pp. 539-539
Author(s):  
Gladys Solivella ◽  
Edgard Giorg ◽  
Rubén Vázquez ◽  
Giovanni Carraro
Keyword(s):  
Emission Line ◽  
Open Cluster ◽  
Open Clusters ◽  
Occurrence Rate ◽  
Hot Stars ◽  
Cluster Area ◽  
Young Object ◽  
Cluster Distance ◽  
Be Star ◽  
Compact Cluster

AbstractNGC 4852 is a moderately compact cluster centered at α2000 = 13 : 00 : 09; δ = −59 : 36 : 48, located near the center of an Hα superring. This cluster forms part of an extended region including young stellar aggregates inside a circle with a radius of 3 degrees, where many show an abundance of emission line stars. In the field of this cluster, two stars of known type exist: Wray 15–1039 (emission-line object) and CD −58:4845 (emission-line star). We do not yet know whether the Be phase is transient or whether it is just what randomly happens in some hot stars. It appears that Be star may be found even in clusters as old as 70 Myr with a high occurrence rate in clusters of 25–27 Myr old. A recent photometric survey in NGC 4852 down to V = 22 – 23 mag established that NGC 4852 is about 200 – 250 Myr old, located at 1.1 kpc from the Sun and with a mean E(B − V) = 0.45 mag. Since the presence of potential Be-type stars in the cluster area suggests it may be a very young object instead of moderately old, we decided to carry out spectroscopy for 33 selected stars and CCD UBVI photometry for the bright objects in the cluster area. This way, we attempt to clarify their evolutionary state and include them in the framework of emission-line stars and open clusters. From our analysis, we agree with the cluster distance and reddening determined by earlier studies, but we derive that the age of NGC 4852 is younger than 40 Myr.

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