WINGS-SPE  Spectroscopy in the WIde-field Nearby Galaxy-cluster Survey

Cava, A.; Bettoni, D.; Poggianti, Bianca M.; Couch, W.; Moles, M.; Varela, J.; Biviano, A.; D’Onofrio, M.; Dressler, Alan; Fasano, G.; Fritz, J.; Kjærgaard, P.; Ramella, M.; Valentinuzzi, T.

doi:10.1051/0004-6361:200810997

Cited by 150 publications

(234 citation statements)

References 65 publications

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“…This galaxy is listed as a member galaxy of Z8338 (Smith et al 2004; and a spectroscopic redshift of 0.0511 in Cava et al 2009, in agreement with the cluster redshift in P11). According to F11, this is the galaxy with the highest mass, by far the highest star formation (SF) rate in the past (5.5 M /yr, while no SF is detected in current age), and the highest age within Z8338.…”

Section: Counterparts In Other Wavelengthssupporting

confidence: 79%

The long X-ray tail in Zwicky 8338

Schellenberger

Reiprich

2015

A&A

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The interaction processes in galaxy clusters between the hot ionized gas (ICM) and the member galaxies are of crucial importance to understand the dynamics in galaxy clusters, the chemical enrichment processes, and the validity of their hydrostatic mass estimates. Recently, several X-ray tails associated with gas that was partly stripped of galaxies have been discovered. We report on the X-ray tail in the 3 keV galaxy cluster Zwicky 8338, which might be the longest galaxy-scale stripping process ever observed. We derive the properties of the galaxy cluster environment and give hints on the substructure present in this X-ray tail, which is very likely associated with the galaxy CGCG254-021. The X-ray tail is extraordinarily luminous (2 × 10 42 erg s −1 ), the thermal emission has a temperature of 0.8 keV, and the X-ray luminous gas might be stripped off completely from the galaxy. From assumptions about the 3D geometry, we estimate the gas mass fraction (<0.1%) and conclude that the gas has been compressed and/or heated.

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Section: Counterparts In Other Wavelengthssupporting

confidence: 79%

The long X-ray tail in Zwicky 8338

Schellenberger

Reiprich

2015

A&A

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“…Spectroscopic information for ∼ 6, 000 galaxies in the field of 48 WINGS clusters has been provided by a follow-up multi-fibre, medium-resolution survey (WINGS-SPE; Cava et al 2009). Detailed information about spectral features are available for a subset of these galaxies (Fritz et al 2007(Fritz et al , 2011(Fritz et al , 2014.…”

Section: Spectroscopic Data: the Extended (Wings+literature) Samplementioning

confidence: 99%

Structural and dynamical modeling of WINGS clusters

Cava

Biviano

Mamon

et al. 2017

A&A

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Context. We study the distribution of galaxies in nearby clusters to shed light on the evolutionary processes at work within clusters and prepare for a full dynamical analysis to be conducted in forthcoming papers of this series. Aims. We use the Wide-field Nearby Galaxy-clusters Survey (WINGS) database complemented with literature data. We assign galaxy membership to individual clusters, then select a sample of 67 clusters with at least 30 spectroscopic members each. 53 of these clusters do not show evidence of substructures in phase-space, as measured by the Dressler-Shectman test, while 14 do. We estimate the virial radii and circular velocities of the 67 clusters by a variety of proxies (velocity dispersion, X-ray temperature, and richness) and use these estimates to build stack samples from these 53 and 14 clusters, that we call 'Reg' and 'Irr' stacks, respectively. We show that our results are robust with regard to the choice of the virial radii and circular velocities used to scale galaxy radii and velocities in the stacking procedure. We determine the number-density and velocity-dispersion profiles of Elliptical (E), S0, and Spiral+Irregular (S) galaxies in the Reg and Irr samples, separately, and fit models to these profiles. Methods. The number density profiles of E, S0, and S galaxies are adequately described by either a Navarro, Frenk, & White (NFW) or a cored King model, both for the Reg and Irr samples, with a slight preference for the NFW model. The spatial distribution concentration increases from the S to the S0 and to the E populations, both in the Reg and the Irr stacks, reflecting the well-known morphology-radius relation. Reg clusters have a more concentrated spatial distribution of E and S0 galaxies than Irr clusters, while the spatial distributions of S galaxies in Reg and Irr clusters have a similar concentration. We propose a new phenomenological model that provides acceptable fits to the velocity dispersion profile of all our galaxy samples. The velocity dispersion profiles become steeper and with a higher normalization from E to S0 to S galaxies. The S0 velocity dispersion profile is close to that of E galaxies in Reg clusters, and intermediate between those of E and S galaxies in Irr clusters. Results. Our results suggest that S galaxies are a recently accreted cluster population, that take ≤ 3 Gyr to evolve into S0 galaxies after accretion, and in doing so modify their phase-space distribution, approaching that of cluster ellipticals. While in Reg clusters this evolutionary process is mostly completed, it is still ongoing in Irr clusters.

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“…7 together with the L X −σ v relation for the WINGS nearby cluster sample (Fasano et al 2006;Cava et al 2009). The two relations are in good agreement with one another.…”

Section: X −σ V Relationmentioning

confidence: 99%

Fossil group origins

Zarattini¹,

Barrena²,

Girardi³

et al. 2014

A&A

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Context. Virialized halos grow by the accretion of smaller ones in the cold dark matter scenario. The rate of accretion depends on the different properties of the host halo. Those halos for which this accretion rate was very fast and efficient resulted in systems dominated by a central galaxy surrounded by smaller galaxies that were at least two magnitudes fainter. These galaxy systems are called fossil systems, and they can be the fossil relics of ancient galaxy structures. Aims. We started an extensive observational program to characterize a sample of 34 fossil group candidates spanning a broad range of physical properties. Methods. Deep r-band images were obtained with the 2.5-m Isaac Newton Telescope and Nordic Optic Telescope. Optical spectroscopic observations were performed at the 3.5-m Telescopio Nazionale Galileo for ∼1200 galaxies. This new dataset was completed with Sloan Digital Sky Survey Data Release 7 archival data to obtain robust cluster membership and global properties of each fossil group candidate. For each system, we recomputed the magnitude gaps between the two brightest galaxies (Δm 12 ) and the first and fourth ranked galaxies (Δm 14 ) within 0.5 R 200 . We consider fossil systems to be those with Δm 12 ≥ 2 mag or Δm 14 ≥ 2.5 mag within the errors. Results. We find that 15 candidates turned out to be fossil systems. Their observational properties agree with those of non-fossil systems. Both follow the same correlations, but the fossil systems are always extreme cases. In particular, they host the brightest central galaxies, and the fraction of total galaxy light enclosed in the brightest group galaxy is larger in fossil than in non-fossil systems. Finally, we confirm the existence of genuine fossil clusters. Conclusions. Combining our results with others in the literature, we favor the merging scenario in which fossil systems formed from mergers of L * galaxies. The large magnitude gap is a consequence of the extreme merger ratio within fossil systems and therefore it is an evolutionary effect. Moreover, we suggest that at least one fossil group candidate in our sample could represent a transitional fossil stage. This system could have been a fossil in the past, but not now owing to the recent accretion of another group of galaxies.

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WINGS-SPE Spectroscopy in the WIde-field Nearby Galaxy-cluster Survey

Cited by 150 publications

References 65 publications

The long X-ray tail in Zwicky 8338

The long X-ray tail in Zwicky 8338

Structural and dynamical modeling of WINGS clusters

Fossil group origins

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