Gas kinematics of a sample of five Hickson Compact Groups

Amram, P.; Plana, H.; Oliveira, C. Mendes de; Balkowski, C.; Boulesteix, J.

doi:10.1051/0004-6361:20030034

Cited by 46 publications

(89 citation statements)

References 36 publications

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“…This is confirmed by a number of studies that have shown distorted kinematics and morphologies of compact group galaxies (e.g. Presotto et al 2010;Amram et al 2007;Coziol & Plauchu-Frayn 2007;Amram et al 2003;Plana et al 2003Plana et al , 1998, also by studies of groups containing HI tidal debris (Verdes-Montenegro et al 2001) and newly formed stars forming systems outside the luminous member galaxies (e.g. de Mello et al 2008), as well as studies of diffuse light presumably originated from stripped material from the outskirts of galaxies in compact groups (e.g.…”

Section: Outliers From the Tf Relationmentioning

confidence: 60%

“…The present study complements the sample of compact group galaxies with measured velocity maps presented by Plana et al (1998Plana et al ( , 2000Plana et al ( , 2003, Mendes de Oliveira et al (1998), Amram et al (2003Amram et al ( , 2004Amram et al ( , 2007, and Torres-Flores et al (2009). We present for the first time velocity maps for galaxies in nine Hickson compact groups (HCGs 37,40,47,49,54,56,68,79,and 93.…”

Section: Introductionmentioning

confidence: 71%

“…The observations were carried out using a Fabry-Perot instrument mounted either on the Canada France Hawaii telescope (MOSFP, Amram et al 2003) or on the European Southern Observatory 3.6 m telescope (CIGALE, Amram et al 1991), using a CCD or a photon counting system respectively. The observed compact groups, exposure times, and scanning wavelengths are listed in Table 1.…”

Section: Observationsmentioning

confidence: 99%

“…The output of this package consists of monochromatic, continuum, dispersion, and radial velocity maps. This procedure includes several improvements with respect to the data reduction and analysis performed to the data presented in Plana et al (2003) and Amram et al (2003), listed in the following. First, the present procedure uses an adaptive spatial binning to the data based on the 2D Voronoi tessellation method (see Cappellari & Copin 2003) applied to the 3D data cubes, optimizing the determination of the spatial resolution.…”

Section: Data Reductionmentioning

confidence: 99%

“…Mendes de , Amram et al (2003), have devised a scheme to classify galaxies as interacting or not, based on analysis of 2D velocity fields and other indicators. Using this same scheme, Torres-Flores et al (2009) classified HCG 2, HCG 7, HCG 22, and NGC 92 in different evolutionary stages.…”

Section: Interaction Indicatorsmentioning

confidence: 99%

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Kinematics of galaxies in compact groups

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We obtained new Fabry-Perot data cubes and derived velocity fields, monochromatic, and velocity dispersion maps for 28 galaxies in the Hickson compact groups 37, 40, 47, 49, 54, 56, 68, 79, and 93. We also derived rotation curves for 9 of the studied galaxies, 6 of which are strongly asymmetric. Combining these new data with previously published 2D kinematic maps of compact group galaxies, we investigated the differences between the kinematic and morphological position angles for a sample of 46 galaxies. We find that one third of the unbarred compact group galaxies have position angle misalignments between the stellar and gaseous components. This and the asymmetric rotation curves are clear signatures of kinematic perturbations, probably because of interactions among compact group galaxies. A comparison between the B-band Tully-Fisher relation for compact group galaxies and for the GHASP field-galaxy sample shows that, despite the high fraction of compact group galaxies with asymmetric rotation curves, these lay on the TF relation defined by galaxies in less dense environments, although with more scatter. This agrees with previous results, but now confirmed for a larger sample of 41 galaxies. We confirm the tendency for compact group galaxies at the low-mass end of the Tully-Fisher relation (HCG 49b, 89d, 96c, 96d, and 100c) to have either a magnitude that is too bright for its mass (suggesting brightening by star formation) and/or a low maximum rotational velocity for its luminosity (suggesting tidal stripping). These galaxies are outside the Tully Fisher relation at the 1σ level, even when the minimum acceptable values of inclinations are used to compute their maximum velocities. Including such galaxies with v < 100 km s −1 in the determination of the zero point and slope of the compact group B-band Tully-Fisher relation would strongly change the fit, making it different from the relation for field galaxies, which has to be kept in mind when studying scaling relations of interacting galaxies, especially at high redshifts.

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