Contributions to galaxy photometry. VIII - Reduction to the standard B[SUB]T[/SUB] system of the galaxy magnitudes in the Ames, Reiz, and Zwicky catalogs of the Virgo cluster area

1979 ◽  
Vol 39 ◽  
pp. 49 ◽  
Author(s):  
G. de Vaucouleurs ◽  
W. D. Pence
Keyword(s):  
Virgo Cluster ◽  
Cluster Area ◽  
The Galaxy

scholarly journals The Ursa Major Cluster Redefined as a ‘Supergroup’

2016 ◽  
Vol 33 ◽  
Author(s):  
K. Wolfinger ◽  
V. A. Kilborn ◽  
E. V. Ryan-Weber ◽  
B. S. Koribalski
Keyword(s):  
Real Data ◽  
Virgo Cluster ◽  
Sloan Digital Sky Survey ◽  
Galaxy Groups ◽  
The Third ◽  
Evolutionary State ◽  
Sky Survey ◽  
Major Cluster ◽  
The Galaxy ◽  
Major Region

AbstractWe identify gravitationally bound structures in the Ursa Major region using positions, velocities and photometry from the Sloan Digital Sky Survey (SDSS DR7) and the Third Reference Catalogue of Bright Galaxies (RC3). A friends-of-friends algorithm is extensively tested on mock galaxy lightcones and then implemented on the real data to determine galaxy groups whose members are likely to be physically and dynamically associated with one another. We find several galaxy groups within the region that are likely bound to one another and in the process of merging. We classify 6 galaxy groups as the Ursa Major ‘supergroup’, which are likely to merge and form a poor cluster with a mass of ~ 8 × 1013 M⊙. Furthermore, the Ursa Major supergroup as a whole is likely bound to the Virgo cluster, which will eventually form an even larger system in the context of hierarchical structure formation. We investigate the evolutionary state of the galaxy groups in the Ursa Major region and conclude that these groups are in an early evolutionary state and the properties of their member galaxies are similar to those in the field.

scholarly journals Structure and kinematics of the Bootes filament

2014 ◽  
Vol 11 (S308) ◽  
pp. 187-192
Author(s):  
O. Nasonova ◽  
I. Karachentsev ◽  
V. Karachentseva
Keyword(s):  
Dark Matter ◽  
Stellar Mass ◽  
Average Density ◽  
Virgo Cluster ◽  
Galaxy Groups ◽  
Peculiar Velocities ◽  
Galaxy Distribution ◽  
The Galaxy ◽  
Virial Mass ◽  
Individual Distance

AbstractBootes filament of galaxies is a dispersed chain of groups residing on sky between the Local Void and the Virgo cluster. We consider a sample of 361 galaxies inside the sky area of RA = 13h0...18h.5 and Dec = .5°... + 10° with radial velocities VLG < 2000 km/s to clarify its structure and kinematics. In this region, 161 galaxies have individual distance estimates. We use these data to draw the Hubble relation for galaxy groups, pairs as well as the field galaxies, and to examine the galaxy distribution on peculiar velocities. Our analysis exposes the known Virgo-centric infall at RA < 14h and some signs of outflow from the Local Void at RA > 17h. According to the galaxy grouping criterion, this complex contains the members of 13 groups, 11 pairs and 140 field galaxies. The most prominent group is dominated by NGC 5846. The Bootes filament contains the total stellar mass of 2.7 ×1012M⊙ and the total virial mass of 9.07×1013M⊙, having the average density of dark matter to be Ωm = 0.09, i.e. a factor three lower than the global cosmic value.

scholarly journals A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE)

2019 ◽  
Vol 623 ◽  
pp. A52 ◽  
Author(s):  
A. Boselli ◽  
M. Fossati ◽  
A. Longobardi ◽  
G. Consolandi ◽  
P. Amram ◽  
...  
Keyword(s):  
Galaxy Evolution ◽  
Narrow Band ◽  
Elliptical Galaxy ◽  
Virgo Cluster ◽  
Environmental Survey ◽  
Narrow Band Image ◽  
The North ◽  
Optical Images ◽  
The Galaxy ◽  
North Western

We observed the giant elliptical galaxy M 87 during the Virgo Environmental Survey Tracing Galaxy Evolution (VESTIGE), a blind narrow-band Hα+[NII] imaging survey of the Virgo cluster carried out with MegaCam at the Canada French Hawaii Telescope (CFHT). The deep narrow-band image confirmed the presence of a filament of ionised gas extending up to ≃3 kpc in the north-western direction and ≃8 kpc to the southeast, with a couple of plumes of ionised gas, the weakest of which, at ≃18 kpc from the nucleus, was previously unknown. The analysis of deep optical images taken from the NGVS survey confirms that this gas filament is associated with dust seen in absorption which is now detected up to ≃2.4 kpc from the nucleus. We also analysed the physical and kinematical properties of the ionised gas filament using deep IFU MUSE data covering the central 4.8 × 4.8 kpc2 of the galaxy. The spectroscopic data confirm a perturbed kinematics of the ionised gas, with differences in velocity of ≃700–800 km s−1 on scales of ≲1 kpc. The analysis of 2D diagnostic diagrams and the observed relationship between the shock-sensitive [OI]/Hα line ratio and the velocity dispersion of the gas suggest that the gas is shock-ionised.

scholarly journals Nuclear molecular gas in the Virgo Cluster S0 galaxy NGC 4710

1993 ◽  
Vol 153 ◽  
pp. 439-440
Author(s):  
J.M. Wrobel ◽  
J.D.P. Kenney
Keyword(s):  
Interstellar Medium ◽  
Emission Line ◽  
Optical Emission ◽  
Virgo Cluster ◽  
Gas Analysis ◽  
Molecular Gas ◽  
Star Forming ◽  
The Galaxy

The CO(J=1→0) emission from NGC 4710, a star–forming S0 galaxy in the Virgo Cluster, was synthesized with spatial and velocity resolutions of 7″ and 26 km s—1, respectively. The CO shows a compact morphology and co–rotates with the galaxy's stars and nuclear optical emission line gas. Analysis of the CO distribution and kinematics indicates that the nuclear molecular gas is probably gravitationally unstable, and this may explain why the galaxy is presently forming stars. Four possible origins for the nuclear molecular gas are considered. An origin via bulge star ejecta being deposited into a residual interstellar medium is favored.

scholarly journals HST WFPC-2 Imaging of Four Nearby LSB Galaxies

1999 ◽  
Vol 171 ◽  
pp. 210-213
Author(s):  
Karen O’Neil
Keyword(s):  
Elliptical Galaxies ◽  
Virgo Cluster ◽  
Small Scale ◽  
Giant Stars ◽  
Structural Peculiarities ◽  
The Galaxy ◽  
Dwarf Elliptical Galaxies ◽  
Giant Branch Stars ◽  
Lsb Galaxies ◽  
Spiral Arm

AbstractBetween May, 1996 and January, 1997 HST WFPC-2 images of four nearby LSB galaxies were taken through both the 8140Å and 3000Å filters. The first galaxy imaged, UGC 12695, is a nearby (z~0.021) LSB disk galaxy. UGC 12695 has an unusual morphology, consisting of a Y-shaped nucleus surrounded by a faint spiral arm. Additionally, numerous HI regions are spread throughout the galaxy. One of the surprising discoveries with the WFPC2 imaging was that a number of what were previously believed to be structural peculiarities in the galaxy are actually background galaxies. Once the effects of these galaxies are removed, the resultant U—I color of UGC 12695 is only −0.2, making it possibly the bluest galaxy in the local universe. When combined with the metallicity studies of McGaugh (1992), these colors indicate UGC 12695 to be a highly unevolved galaxy.The other three galaxies imaged - V1L4, V2L8, and V7L3 - are dwarf elliptical galaxies located in the Virgo cluster. The intent of their images was to determine the galaxies’ small scale structure and place limits on the density and type of giant branch stars within each galaxy. Placed at the distance of the Virgo cluster, luminosity fluctuations indicate the galaxies to contain only from 4 – 13 stars per pixel, coinciding with a K/M giant ratio ranging from 6 to ∞ (no M giant stars). Additionally, we found no evidence for stellar clumping in these galaxies although an extremely red, extremely small bulge was found at the core of V2L8.

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

scholarly journals The VIRGO PN population and the mass assembly in M87

2016 ◽  
Vol 12 (S323) ◽  
pp. 288-292
Author(s):  
Alessia Longobardi ◽  
Magda Arnaboldi ◽  
Ortwin Gerhard
Keyword(s):  
Galaxy Formation ◽  
Virgo Cluster ◽  
Galaxy Halos ◽  
Galaxy Formation And Evolution ◽  
Low Surface Brightness ◽  
The Galaxy ◽  
Galaxy Halo ◽  
Formation And Evolution ◽  
Mass Assembly ◽  
Intracluster Light

AbstractCosmological simulations allow us to study in detail the evolution of galaxy halos in cluster environments, but the extremely low surface brightness of such components makes it difficult to gather observational constraints. Planetary nebulas (PNs) offer a unique tool to investigate these environments owing to their strong [OIII] emission line. We study the light and kinematics of the Virgo cluster and its central galaxy, M87, prime targets to address the topic of galaxy formation and evolution in dense environments. We make use of a deep and extended PN sample (~300 objects) that extends out to 150 kpc in radius from M87’s centre. We show that at all distance the galaxy halo overlaps with the Virgo intracluster light (ICL). Halo and ICL are dynamically distinct components with different parent stellar populations, consistent with the halo of M87 being redder and more metal rich than the ICL. The synergy between PN kinematic information and deep V/B-band photometry made it possible to unravel an ongoing accretion process in the outskirt of M87. This accretion event represents a non-negligible perturbation of the halo light, showing that this galaxy is still growing by accretion of smaller systems.

Sign in / Sign up

Export Citation Format

Share Document