The 3D structure of the Virgo cluster from H-band Fundamental Plane and Tully--Fisher distance determinations

Gavazzi, G.; Boselli, A.; Scodeggio, M.; Pierini, D.; Belsole, E.

doi:10.1046/j.1365-8711.1999.02350.x

Cited by 225 publications

(340 citation statements)

References 59 publications

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“…included in NED. The adopted threshold in redshift guarantees the inclusion of galaxies in the infalling regions and in the different substructures of Virgo that are mainly located at slightly higher distance than the main body of the cluster associated to M87, which is generally called cluster A (Gavazzi et al 1999). As defined, the analysed sample is optical and UV selected and can thus suffer from incompleteness in the two bands.…”

Section: The Samplementioning

confidence: 99%

“…Distances are determined assuming the mean distance of the different cluster substructures indicated in Table 3, as suggested by Gavazzi et al (1999). For galaxies at the periphery of the cluster, we assume the typical distance of the main body of the cluster (17 Mpc).…”

Section: The Derived Parametersmentioning

confidence: 99%

“…Virgo is thus an ideal laboratory for studying and comparing the effects induced by different kinds of perturbations. Furthermore, thanks to its proximity (∼16.5-17 Mpc; Gavazzi et al 1999;Mei et al 2007), observations of Virgo dwarf galaxies are possible at almost any frequency. This is important, since these are the most fragile objects easily perturbed in any kind of physical process.…”

Section: Introductionmentioning

confidence: 99%

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The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Voyer

Boissier

et al. 2014

A&A

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We study the role of the environment on galaxy evolution using a sample of 868 galaxies in the Virgo cluster and in its surrounding regions that are selected from the GALEX Ultraviolet Virgo Cluster Survey (GUViCS) with the purpose of understanding the origin of the red sequence in dense environments. The sample spans a wide range in morphological types (from dwarf ellipticals to Im and BCD) and stellar masses (10 7 M star 10 11.5 M ). We collected multifrequency data covering the whole electromagnetic spectrum for most of the galaxies, including UV, optical, mid-and far-infrared imaging data, as well as optical and HI spectroscopic data. We first identify the different dynamical substructures that compose the Virgo cluster, and we calculate the local density of galaxies using different methods. We then study the distribution of galaxies belonging to the red sequence, the green valley, and the blue cloud within the different cluster substructures or as a function of galaxy density. Our analysis indicates that all the most massive galaxies (M star 10 11 M ) are slow rotators and are the dominant galaxies of the different cluster substructures, which are generally associated with a diffuse X-ray emission. They are probably the result of major merging events that occurred at early epochs, as also indicated by their very old stellar populations. Slow rotators of lower stellar mass (10 8.5M star 10 11 M ) are also preferentially located within the different high-density substructures of the cluster. Their position in the velocity space indicates that they are virialised within the cluster; thus, they are Virgo members since its formation. They have been shaped by gravitational perturbations occurring within the infalling groups that later form the cluster (pre-processing). On the contrary, low-mass star-forming systems are extremely rare in the inner regions of the Virgo cluster A, where the density of the intergalactic medium is at its maximum. Our ram pressure stripping models consistently indicate that these star-forming systems can be rapidly deprived of their interstellar medium during their interaction with the intergalactic medium. The lack of gas quenches their star-formation activity transforming them into quiescent dwarf ellipticals. This mild transformation does not perturb the kinematic properties of these galaxies, which still have rotation curves typical of star-forming systems.

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Section: The Samplementioning

confidence: 99%

Section: The Derived Parametersmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Voyer

Boissier

et al. 2014

A&A

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153

254

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“…Studies of the substructure of the Virgo Cluster (including Tully & Shaya 1984 ;Pierce & Tully 1988 ;Binggeli et al 1987Binggeli et al , 1993Yasuda et al 1997 ;Gavazzi et al 1999 ;Schindler et al 1999) agree that the Virgo Cluster is made up of several associated clouds or groups of galaxies, with two main components : cluster A, associated with M87, and cluster B, associated with M49 (although Gavazzi et al 1999 place M49 closer than cluster B, based on Tully-Fisher distances). Within subcluster A is a smaller core of mostly spheroidal galaxies.…”

Section: Structure Of the V Irgo Clustermentioning

confidence: 99%

An Atlas of Hα and R Images and Radial Profiles of 63 Bright Virgo Cluster Spiral Galaxies

Koopmann

Kenney

Young

2001

ASTROPHYS J SUPPL S

123

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“…Both VCC 781 and VCC 951 reside in the central, densely crowded region of the Virgo cluster (cluster A), and also the HI detected galaxy VCC 209 is well surrounded by galaxies in the N cloud (at the same distance as cluster A, but blue-shifted with respect to Virgo, [6]), while several HI-detected dwarfs in the outskirts of Virgo have not been detected with Herschel (implying a dust content <10 4 Mˇ). One possible explanation for this could be that dust in dwarfs is more closely related to the molecular gas, which is more centrally peaked in a galaxy's potential well and therefore, not easily removed by any stripping mechanism [1,10,15].…”

Section: Discussionmentioning

confidence: 99%

Dust in Cluster Dwarf Elliptical Galaxies

Baes

Fritz

Verstappen

et al. 2011

Astrophysics and Space Science Proceedings

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Based on single cross-scan data of the Herschel Virgo Cluster Survey, we report the first detections of dust in cluster early-type dwarf galaxies: VCC 209, VCC 781 and VCC 951. All three galaxies have dust masses reside in densely crowded regions close to the center of the Virgo cluster, and several HI-detected dwarfs in the outskirts of Virgo were not detected by Herschel (implying a dust content <10 4 Mˇ), this might imply that dust in dwarfs is more closely related to the molecular gas, which is more centrally peaked in a galaxy's potential well and therefore, not easily removed by any stripping mechanism. We conclude that the removal of interstellar dust from these early-type dwarfs appears to be less efficient than the removal of the HI gas.

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The 3D structure of the Virgo cluster from H-band Fundamental Plane and Tully--Fisher distance determinations

Cited by 225 publications

References 59 publications

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

An Atlas of Hα and R Images and Radial Profiles of 63 Bright Virgo Cluster Spiral Galaxies

Dust in Cluster Dwarf Elliptical Galaxies

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