Tidal generation of active spirals and S0 galaxies by rich clusters

Byrd, G. G.; Valtonen, Mauri

doi:10.1086/168362

Cited by 417 publications

(467 citation statements)

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“…In group environments with relatively low velocity dispersion, it has been known that interactions between member galaxies are more frequent (Toomre & Toomre 1972;Lavery & Henry 1988;Byrd & Valtonen 1990;Mamon 1990). This is supported by HI surveys of galaxies in the Ursa Major cluster in which a large fraction of galaxies show evidence of tidal interactions (see Verheijen & Sancisi 2001;Verheijen & Zwaan 2001;Verheijen 2004;Wolfinger et al 2013).…”

Section: Environmental Effects In a Lower Density Clustermentioning

confidence: 99%

The properties of early-type galaxies in the Ursa Major cluster

Pak¹,

Rey²,

Lisker³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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Using SDSS-DR7 and NASA/IPAC Extragalactic Database spectroscopic data, we identify 166 galaxies as members of the Ursa Major cluster with M r < −13.5 mag. We morphological classify all galaxies by means of carefully inspecting g−, r−, i−band colour and monochromatic images. We show that the Ursa Major cluster is dominated by late-type galaxies, but also contains a significant number of earlytype galaxies, particularly in the dwarf regime. We present further evidence for the existence of several subgroups in the cluster, consistent with previous findings. The early-type fraction is found to correlate with the mass of the subgroup. We also investigate environmental effects by comparing the properties of the Ursa Major early-type dwarf galaxies to those of the Virgo cluster. In contrast to the Virgo, the red sequence of the Ursa Major cluster is only sparsely populated in the optical and ultraviolet colour-magnitude relations. It also shows a statistically significant gap between −18 < M r < −17 mag, i.e. the Ursa Major cluster lacks early-type dwarf galaxies at the bright end of their luminosity function. We discover that the majority of early-type dwarf galaxies in the Ursa Major cluster have blue cores with hints of recent or ongoing star formation. We suggest that gravitational tidal interactions can trigger central blue star forming regions in early-type dwarfs. After that, star formation would only fade completely when the galaxies experience ram pressure stripping or harassment, both of which are nearly absent in the Ursa Major cluster.

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Section: Environmental Effects In a Lower Density Clustermentioning

confidence: 99%

The properties of early-type galaxies in the Ursa Major cluster

Pak¹,

Rey²,

Lisker³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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“…However, for the atomic hydrogen in the central regions of the disks of HI-deficient galaxies, the surface mass density appears somewhat higher than that of slightly HI-deficient galaxies. This effect could be understood as ram-pressure-induced compression of the gas in the inner region of the disk (Tonnesen & Bryan 2009) that increases locally the gas density (Byrd & Valtonen 1990). Alternatively, the differences in surface mass density can be simply due to uncertainties in the inclination corrections for two of the HI-deficient galaxies, NGC 4388 and NGC 4402, which are nearly edge-on.…”

Section: Radial Profilesmentioning

confidence: 99%

TheHerschelVirgo Cluster Survey

Pappalardo

Bianchi

Corbelli

et al. 2012

A&A

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Aims. We investigate the dust-to-gas mass ratio and the environmental effects on the various components of the interstellar medium for a spatially resolved sample of Virgo spirals. Methods. We have used the IRAM-30 m telescope to map over their full extent NGC 4189, NGC 4298, NGC 4388, and NGC 4299 in the 12 CO(1-0) and the 12 CO(2-1) lines. We observed the same lines in selected regions of NGC 4351, NGC 4294, and NGC 4424. The CO observations are combined with Herschel maps in 5 bands between 100-500 μm from the HeViCS survey, and with HI data from the VIVA survey, to obtain spatially resolved dust and gas distributions. We studied the environmental dependencies by adding to our sample eight galaxies with 12 CO(1-0) maps from the literature. Results. We estimate the integrated mass of molecular hydrogen for the galaxies observed in the CO lines. We find molecular-to-total gas mass fractions between 0.04 ≤ f mol ≤ 0.65, with the lowest values for the dimmest galaxy in the B-band. The integrated dust-togas ratio ranges between 0.011 and 0.004. For the 12 mapped galaxies we derive the radial distributions of the atomic gas, molecular gas, and dust. We also study the effect of different CO-to-H 2 conversion factors. Both the molecular gas and the dust distributions show steeper radial profiles for HI-deficient galaxies and the average dust-to-gas ratio for these galaxies increases or stays radially constant. On scales of ∼3 kpc, we find a strong correlation between the molecular gas and the 250 μm surface brightness that is tighter than average for non-deficient galaxies. The correlation becomes linear if we consider the total gas surface mass density. However, the inclusion of atomic hydrogen does not improve the statistical significance of the correlation. Conclusions. The environment can modify the distributions of molecules and dust within a galaxy, although these components are more tightly bound than the atomic gas.

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“…In a dense environment several mechanisms affect galaxies. This might happen through interactions with the intergalactic medium (IGM), such as ram-pressure stripping (Boselli et al 2008a,b), galaxy-galaxy interactions (e.g., Byrd & Valtonen 1990), and galaxy harassment (e.g., Moore et al 1998;Mastropietro et al 2005). It has been shown that all these interactions are able to reproduce some of the observational properties of local dEs in clusters, such as their structural parameters (Lisker et al 2006b(Lisker et al , 2007 or their stellar populations (Geha et al 2002(Geha et al , 2003van Zee et al 2004b;Michielsen et al 2008;Paudel et al 2010), but none of them have been tested against the kinematic properties.…”

Section: Introductionmentioning

confidence: 99%

Formation and evolution of dwarf early-type galaxies in the Virgo cluster

Toloba

Boselli

Cenarro

et al. 2011

A&A

130

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We present new medium resolution kinematic data for a sample of 21 dwarf early-type galaxies (dEs) mainly in the Virgo cluster, obtained with the WHT and INT telescopes at the Roque de los Muchachos Observatory (La Palma, Spain). These data are used to study the origin of the dwarf elliptical galaxy population inhabiting clusters. We confirm that dEs are not dark matter dominated galaxies, at least not up to the half-light radius. We also find that the observed galaxies in the outer parts of the cluster are mostly rotationally supported systems with disky morphological shapes. Rotationally supported dEs have rotation curves similar to those of star-forming galaxies of similar luminosity and follow the Tully-Fisher relation. This is expected if dE galaxies are the descendants of low-luminosity star-forming systems that have recently entered the cluster environment and lost their gas due to a ram-pressure stripping event, quenching their star formation activity and transforming into quiescent systems, but conserving their angular momentum.

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Tidal generation of active spirals and S0 galaxies by rich clusters

Cited by 417 publications

References 0 publications

The properties of early-type galaxies in the Ursa Major cluster

The properties of early-type galaxies in the Ursa Major cluster

TheHerschelVirgo Cluster Survey

Formation and evolution of dwarf early-type galaxies in the Virgo cluster

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