A deep H<i>α</i>survey of galaxies in the two nearby clusters Abell 1367 and Coma

Iglésias-Páramo, J.; Boselli, A.; Cortese, Luca; Vı́lchez, J. M.; Gavazzi, G.

doi:10.1051/0004-6361:20011830

Cited by 70 publications

(108 citation statements)

References 48 publications

(59 reference statements)

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“…2 red points) or from previous observations of 155 optically selected CGCG galaxies by Gavazzi et al (1999Gavazzi et al ( , 2002aGavazzi et al ( ,b, 2006, , Iglesias-Páramo et al (2002), and Cortese et al (2006) (see Fig. 2 blue points).…”

Section: Coma Superclustermentioning

confidence: 71%

Hα3: an Hαimaging survey of HI selected galaxies from ALFALFA

Fossati

Gavazzi

Savorgnan

et al. 2013

A&A

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Context. We present the analysis of the galaxy structural parameters from Hα3, an Hα narrow-band imaging follow-up survey of ∼800 galaxies selected from the HI Arecibo Legacy Fast ALFA Survey (ALFALFA) in the Local supercluster, including the Virgo cluster, and in the Coma supercluster. Aims. Taking advantage of Hα3, which provides the complete census of the recent star-forming, HI-rich galaxies in the local universe, we aim to investigate the structural parameters of the young (<10 Myr) and the old (>1 Gyr) stellar populations. By comparing the sizes of these stellar components, we investigated the spatial scale on which galaxies are growing at the present cosmological epoch and the role of the environment in quenching the star-formation activity. Methods. We computed the concentration, asymmetry, and clumpiness (CAS) structural parameters for recently born and old stars. To quantify the sizes we computed half-light radii and a new parameter dubbed EW/r based on the half-light radius of the Hα equivalent width map. To highlight the environmental perturbation, we adopt an updated calibration of the HI-deficiency parameter (De f HI ) that we use to divide the sample in unperturbed galaxies (De f HI ≤ 0.3) and perturbed galaxies (De f HI > 0.3). Results. The concentration index computed in the r band depends on the stellar mass and on the Hubble type these variables are related because most massive galaxies are bulge dominated therefore highly concentrated. Going toward later spirals and irregulars the concentration index and the mass decrease along with the bulge-to-disk ratio. Blue compact dwarfs (BCDs) are an exception because they have similar mass, but they are more concentrated than dwarf irregulars. The asymmetry and the clumpiness increase along the spiral sequence up to Sc-Sd, but they decrease going in the dwarf regime, where the light distribution is smooth and more symmetric. When measured on Hα images, the CAS parameters show no obvious correlations with Hubble type. Irrespective of whether we used the ratio between effective radii or the EW/r parameter, we found that the concentration index is the main parameter that describes the current growth of isolated galaxies but, for a fixed concentration, the stellar mass plays a second-order role. At the present epoch, massive galaxies are growing inside-out, conversely, the dwarfs are growing on the scale of their already assembled mass.

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Section: Coma Superclustermentioning

confidence: 71%

Hα3: an Hαimaging survey of HI selected galaxies from ALFALFA

Fossati

Gavazzi

Savorgnan

et al. 2013

A&A

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“…The Hα gas around a galaxy in a cluster suggests a recent or ongoing gas-loss event of the parent galaxy, since the gas is heated by the ambient hot plasma and will eventually get mixed with it. Such extended ionized gas (EIG) was reported in various nearby clusters; in Abell 1367 (e.g., Gavazzi et al 2001a;Iglesias-Páramo et al 2002;Sakai et al 2002;Gavazzi et al 2003a;Sakai et al 2012), in the Virgo cluster (e.g., Kenney & Koopmann 1999;Yoshida et al 2002;Kenney et al 2008;Arrigoni Battaia et al 2012;Kenney et al 2014), in the Coma cluster (e.g., Yagi et al 2007;Yoshida et al 2008;Yagi et al 2010;Yoshida et al 2012;Fossati et al 2012), in Abell 3627 (e.g., Sun et al 2007Sun et al , 2010, and in some distant clusters (e.g.. Abell 851 Yagi et al 2015a). Yagi et al (2010) found 14 EIGs in the central 1 Mpc of the Coma cluster, a nearby rich cluster.…”

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confidence: 83%

“…Gavazzi et al (2001a) discovered Hα cometary trails coinciding in length and direction with the radio continuum ones. Iglesias-Páramo et al (2002) gives the Hα emitter catalog of the Abell 1367 (including the Coma cluster) using four exposures of 0.5 degree 2 each obtained with the WFC camera attached to the 2.5m William Herschel Telescope (WHT), with a sensitivity of approximately 10 −15.5 erg s −1 cm −2 obtained with one hour exposures per field. The total number of galaxies with Hα in this sensitivity was 41.…”

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confidence: 99%

Extended Ionized Gas Clouds in the Abell 1367 Cluster^∗

Yagi

Yoshida

Gavazzi

et al. 2017

ApJ

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We surveyed a central 0.6 deg 2 region of Abell 1367 cluster for extended ionized gas clouds (EIGs) using the Subaru prime-focus camera (Suprime-Cam) with a narrow-band filter that covers Hα. We discovered six new EIGs in addition to five known EIGs. We also found that the Hα tail from the blue infalling group (BIG) is extended to about 330 kpc in projected distance, which is about twice longer than previously reported. Candidates of star-forming blobs in the tail are detected. The properties of the EIG parent galaxies in Abell 1367 basically resemble those in the Coma cluster. A noticeable difference is that the number of detached EIGs is significantly fewer in Abell 1367, while the fraction of blue member galaxies is higher. The results suggest a difference in the evolutionary stage of the clusters; Abell 1367 is at an earlier stage than the Coma cluster.

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“…We have observed 1 square degree of Coma cluster. The images were obtained using the Sloan-Gunn r filter of the WFC (see Iglesias-Páramo et al 2002). The B band magnitudes of the galaxies were obtained from the Godwin et al (1983) catalogue of Coma cluster galaxies.…”

Section: Structural Parameters and Color Distributionmentioning

confidence: 99%

Environmental effects in the structural parameters of Coma galaxies

Aguerri

Iglesias-Píaramo²,

Vı́lchez

et al. 2004

IAU

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Abstract.We have studied the quantitative morphology of the galaxies of the Coma cluster brighter than mr = 17. The surface brightness profiles of all galaxies were decomposed into the structural components: bulge and disc. We found a correlation between the scale length of the discs and the location in the cluster. Galaxies located at small projected distances show smaller discs than those located in the outermost regions of the cluster. We have also investigated the correlation betwenn the B−r color of the galaxies and their environment. For late-type galaxies there is a correlation between the color and the position in the cluster. The bluest galaxies are located in the outermost regions of the cluster and show the largest discs. These results can be explained in terms of galaxy harassment.

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A deep Hαsurvey of galaxies in the two nearby clusters Abell 1367 and Coma

Cited by 70 publications

References 48 publications

Hα3: an Hαimaging survey of HI selected galaxies from ALFALFA

Hα3: an Hαimaging survey of HI selected galaxies from ALFALFA

Extended Ionized Gas Clouds in the Abell 1367 Cluster^∗

Environmental effects in the structural parameters of Coma galaxies

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A deep Hαsurvey of galaxies in the two nearby clusters Abell 1367 and Coma

Cited by 70 publications

References 48 publications

Hα3: an Hαimaging survey of HI selected galaxies from ALFALFA

Hα3: an Hαimaging survey of HI selected galaxies from ALFALFA

Extended Ionized Gas Clouds in the Abell 1367 Cluster∗

Environmental effects in the structural parameters of Coma galaxies

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Product

Resources

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Extended Ionized Gas Clouds in the Abell 1367 Cluster^∗