The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli, A.; Boissier, S.; Heinis, S.; Cortese, Luca; Ilbert, O.; Hughes, T. M.; Cucciati, O.; Davies, Jonathan Ivor; Ferrarese, Laura; Giovanelli, Riccardo; Haynes, Martha P.; Baes, M.; Balkowski, C.; Brosch, Noah; Chapman, Scott; Charmandaris, V.; Clemens, M.; Dariush, Aliakbar; Looze, I. De; Alighieri, S. di Serego; Duc, P. A.; Durrell, P. R.; Emsellem, Éric; Erben, T.; Fritz, J.; Garcia‐Appadoo, D. A.; Gavazzi, G.; Grossi, M.; Jordán, Andrés; Hess, Kelley M.; Huertas-Company, M.; Hunt, L. K.; Kent, Brian R.; Lambas, D. García; Lançon, A.; MacArthur, Lauren A.; Madden, S.; Magrini, L.; Mei, S.; Momjian, Emmanuel; Olowin, R. P.; Papastergis, Emmanouil; Smith, M.; Solanes, J. M.; Spector, O.; Spekkens, Kristine; Taylor, James E.; Valotto, C.; Driel, W. van; Verstappen, J.; Vlahakis, C.; Vollmer, B.; Xilouris, E. M.

doi:10.1051/0004-6361/201016389

Cited by 93 publications

(38 citation statements)

References 83 publications

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“…Cluster A represents low-mass cluster population. Hence, we use the ICM of the Virgo cluster as reference as it is a well studied in the context of ram-pressure stripping (e.g Vollmer et al 2001;Chung et al 2009;Boselli et al 2011;Ferrarese et al 2012;Yoon et al 2017), and widely referenced in galaxy evolution studies. Cluster B instead represents high mass clusters.…”

Section: Cluster Modelsmentioning

confidence: 99%

GASP. IX. Jellyfish galaxies in phase-space: an orbital study of intense ram-pressure stripping in clusters

Jaffé

Poggianti

Moretti

et al. 2018

Monthly Notices of the Royal Astronomical Society

168

190

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It is well known that galaxies falling into clusters can experience gas stripping due to ram-pressure by the intra-cluster medium (ICM). The most spectacular examples are galaxies with extended tails of optically-bright stripped material known as "jellyfish". We use the first large homogeneous compilation of jellyfish galaxies in clusters from the WINGS and OmegaWINGS surveys, and follow-up MUSE observations from the GASP MUSE programme to investigate the orbital histories of jellyfish galaxies in clusters and reconstruct their stripping history through position vs. velocity phasespace diagrams. We construct analytic models to define the regions in phase-space where ram-pressure stripping is at play. We then study the distribution of cluster galaxies in phase-space and find that jellyfish galaxies have on average higher peculiar velocities (and higher cluster velocity dispersion) than the overall population of cluster galaxies at all clustercentric radii, which is indicative of recent infall into the cluster and radial orbits. In particular, the jellyfish galaxies with the longest gas tails reside very near the cluster cores (in projection) and are moving at very high speeds, which coincides with the conditions of the most intense ram-pressure. We conclude that many of the jellyfish galaxies seen in clusters likely formed via fast (∼ 1 − 2 Gyr), incremental, outside-in ram-pressure stripping during first infall into the cluster in highly radial orbits.

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Section: Cluster Modelsmentioning

confidence: 99%

GASP. IX. Jellyfish galaxies in phase-space: an orbital study of intense ram-pressure stripping in clusters

Jaffé

Poggianti

Moretti

et al. 2018

Monthly Notices of the Royal Astronomical Society

168

190

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“…where M FUV is the (linear) average M FUV of the sample, EW(Lyα) is measured in the coadded spectra, and the constant of proportionality comes from a combination of that given in Lemaux et al (2009), 4πd 2 L , where d L is 10 pc in cm, c is cm s −1 , and the λ e f f of the FUV filter (1539 × 10 −8 cm, Boselli et al 2011). We then define the escape fraction of Lyα as:…”

Section: Spectral Propertiesmentioning

confidence: 99%

The VIMOS Ultra-Deep Survey: Emerging from the dark, a massive proto-cluster at z ~ 4.57

Lemaux

Fèvre

Cucciati

et al. 2018

A&A

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113

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Using spectroscopic observations taken for the Visible Multi-Object Spectrograph (VIMOS) Ultra-Deep Survey (VUDS) we report here on the discovery of PCl J1001+0220, a massive proto-cluster of galaxies located at z spec ∼ 4.57 in the COSMOS field. With nine spectroscopic members, the proto-cluster was initially detected as a ∼ 12σ spectroscopic overdensity of typical star-forming galaxies in the blind spectroscopic survey of the early universe (2 < z ∼ < 6) performed by VUDS. It was further mapped using a new technique developed which statistically combines spectroscopic and photometric redshifts, the latter derived from a recent compilation of incredibly deep multi-band imaging performed on the COSMOS field. Through various methods, the descendant mass of PCl J1001+0220 is estimated to be log(M h /M ⊙ ) z=0 ∼ 14.5−15 with a large amount of mass apparently already in place at z ∼ 4.57. An exhaustive comparison was made between the properties of various spectroscopic and photometric member samples and matched samples of galaxies inhabiting less dense environments at the same redshifts. Tentative evidence is found for a fractional excess of older galaxies more massive in their stellar content amongst the member samples relative to the coeval field, an observation which suggests the pervasive early onset of vigorous star formation for proto-cluster galaxies. No evidence is found for the differences in the star formation rates (SFRs) of member and coeval field galaxies either through estimating by means of the rest-frame ultraviolet or through separately stacking extremely deep Very Large Array 3 GHz imaging for both samples. Additionally, no evidence for pervasive strong active galactic nuclei (AGN) activity is observed in either environment. Analysis of Hubble Space Telescope images of both sets of galaxies as well as their immediate surroundings provides weak evidence for an elevated incidence of galaxy-galaxy interaction within the bounds of the proto-cluster. The stacked and individual spectral properties of the two samples are compared, with a definite suppression of Lyα seen in the average member galaxy relative to the coeval field ( f esc, Lyα = 1.8 +0.3 −1.7 % and 4.0 +1.0 −0.8 %, respectively). This observation along with other lines of evidence leads us to infer the possible presence of a large, cool, diffuse medium within the proto-cluster environment evocative of a nascent intracluster medium forming in the early universe.

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“…The selection criteria are fully described in Boselli et al (2010a). The multiwavelength data used in this work have been taken from Boselli et al (2011), Boselli et al (2013), Boselli et al (2015), Ciesla et al (2012), Cortese et al (2012a), Cortese et al (2014. Morphological types and distances are taken from Cortese et al (2012a).…”

Section: The Datamentioning

confidence: 99%

The bivariate luminosity and mass functions of the local HRS galaxy sample

Andreani

Boselli

Ciesla

et al. 2018

A&A

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Aims. We discuss the results of the relationships between the K-band and stellar mass, far-infrared luminosities, star formation rate, dust and gas masses of nearby galaxies computing the bivariate K-band-Luminosity Function (BLF) and bivariate K-band-Mass Function (BMF) of the Herschel Reference Survey (HRS), a volume-limited sample with full wavelength coverage. Methods. We derive the BLFs and BMFs from the K-band and stellar mass, far-infrared luminosities, star formation rate, dust and gas masses cumulative distributions using a copula method which is outlined in detail. The use of the bivariate computed taking into account the upper limits allows us to derive on a more solid statistical ground the relationship between the observed physical quantities.Results. The analysis shows that the behaviour of the morphological (optically selected) subsamples is quite different. A statistically meaningful result can be obtained over the whole HRS sample only from the relationship between the K-band and the stellar mass, while for the remaining physical quantities (dust and gas masses, far-IR luminosity and star formation rate), the analysis is distinct for late-type (LT) and early-type galaxies (ETG). However, the number of ETGs is small to perform a robust statistical analysis, and in most of the case results are discussed only for the LTG subsample. The Luminosity and Mass Functions (LFs, MFs) of LTGs are generally dependent on the K-band and the various dependencies are discussed in detail. We are able to derive the corresponding LFs and MFs and compare them with those computed with other samples. Our statistical analysis allows us to characterise the HRS, that, although non homogeneously selected and partially biased towards low IR luminosities, may be considered as representative of the local LT galaxy population.

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The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Cited by 93 publications

References 83 publications

GASP. IX. Jellyfish galaxies in phase-space: an orbital study of intense ram-pressure stripping in clusters

GASP. IX. Jellyfish galaxies in phase-space: an orbital study of intense ram-pressure stripping in clusters

The VIMOS Ultra-Deep Survey: Emerging from the dark, a massive proto-cluster at z ~ 4.57

The bivariate luminosity and mass functions of the local HRS galaxy sample

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