A Dynamical Study of Galaxies in the Hickson Compact Groups

Nishiura, S.; Shimada, Masashi; Ohyama, Youichi; Murayama, Takashi; Taniguchi, Yoshiaki

doi:10.1086/301561

Cited by 36 publications

(34 citation statements)

References 35 publications

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“…In conclusion, our FP data agree roughly with long slit-data (Rubin et al 1990;Nishiura et al 2000;Lopez-Sanchez et al 2004), as well as with FP data from Richer et al (2003) and HI data from Verdes-Montenegro et al (2005).…”

Section: Long Slit Through C (Pa = 41supporting

confidence: 91%

“…We present in Appendix A a detailed comparison between our results (FP, for Fabry-Perot data) and measurements available in the literature (LS for long-slit data) by Rubin et al (1990), Nishiura et al (2000), López-Sánchez et al (2004), as well as FP data from Richer et al (2003) and HI data from Verdes-Montenegro et al (2005). The spectral and spatial resolution for the various optical and HI data available in the literature for HCG 31 are summarized in Table 3.…”

Section: Comparison With Previous Workmentioning

confidence: 85%

“…We compare our data with those of Nishiura et al (2000) who presented RCs for A, B, and C from long-slit spectroscopy. We plot the two data sets using the same parameters and the center given by the continuum emission.…”

Section: A2 Comparison Between Our Fabry-perot Data and Nishiura Etmentioning

confidence: 93%

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HCG 31: a multiple merger in progress

Amram

Oliveira

Plana

et al. 2007

A&A

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Context. HCG 31 is one of the most intriguing compact groups in Hickson's catalogue. It contains a central pair of interacting dwarf galaxies and other small members that are highly peculiar. Aims. The main goal of this study is to investigate the evolutionary stage of the group and measure the internal kinematics of the individual galaxies and of the possible tidal dwarf galaxies. Methods. We obtained new Fabry-Perot data cubes, including Hα images, velocity fields, velocity dispersion maps, lambda maps, position-velocity plots and rotation curves. We have taken advantage of the high spatial (sampling of ∼0.4 arcsec) and spectral (velocity sampling of ∼3 km s −1 ) resolutions of our Fabry-Perot data. Results. Kinematic peculiarities and overlapping double velocity components are measurable throughout the velocity field of A+C, with no signature of either distinct rotating disks or a single rotating galaxy. The velocity dispersion map shows widespread lowvelocity values throughout the group (consistent with the turbulent velocity of the gas), except in a narrow interface between A and C, where the merging may be occurring. The velocity curves of four candidate tidal dwarf galaxies (regions E, F, A1, and A2) show flat velocity patterns in two cases (A1 and F) and gradients with amplitudes of A ∼ 30−40 km s −1 in two others (E and A2). Our measurements show good agreement with previous optical literature data, but our data set has a much improved velocity sampling and deeper coverage. Moreover, within the star-forming regions of the group, our data profit from the higher spatial resolution with respect to HI data. Conclusions. The dynamics of the A+C system, with two main velocity components of approximately the same intensities, indicate that it is in a pre-merger stage. The two disks, in a bound orbit and in the process of merging, have had at least one earlier passage. They rotate with almost parallel spin axes like a set of gear wheels. This prograde encounter and the high star-formation rates favor the formation of a new disk. Object F may turn into a tidal dwarf galaxy bound to the group.

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Section: Long Slit Through C (Pa = 41supporting

confidence: 91%

Section: Comparison With Previous Workmentioning

confidence: 85%

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HCG 31: a multiple merger in progress

Amram

Oliveira

Plana

et al. 2007

A&A

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“…We could derive kinematic information mainly for the late-type members. We also present a comparison of rotation curves (RCs) we derived, with previous studies using long-slit spectroscopy made by Rubin et al (1991) (hereafter referred to as RHF1991) and Nishiura et al (2000) (hereafter referred to as NSOMT2000).…”

Section: Introductionmentioning

confidence: 92%

Gas kinematics of a sample of five Hickson Compact Groups

Amram¹,

Plana²,

Oliveira³

et al. 2003

A&A

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Abstract. We present Fabry Perot observations of galaxies in five Hickson Compact Groups: HCG 10, HCG 19, HCG 87, HCG 91 and HCG 96. We observed a total of 15 galaxies and we have detected ionized gas for 13 of them. We were able to derive 2D velocity, monochromatic, continuum maps and rotation curves for the 13 objects. Almost all galaxies in this study are late-type systems; only HCG 19a is an elliptical galaxy. We can see a trend of kinematic evolution within a group and among different groups -from strongly interacting systems to galaxies with no signs of interaction -HCG 10 exhibits at least one galaxy strongly disturbed; HCG 19 seems to be quite evolved; HCG 87 does not show any sign of merging but a possible gas exchange between two galaxies; HCG 91 could be accreting a new intruder; HCG 96 exhibits past and present interactions.

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“…See also Bertola & Capaccioli (1977) and Emsellem & Arsenault (1997) for NGC 128. Nine galaxies have available ionized-gas rotation curves, all of them measured from H: IC 4767 (Rubin, Whitmore, & Ford 1988;Amram et al 1995), NGC 1886, NGC 2788A, IC 2531, ESO 443-G042, ESO 240-G011 (Mathewson, Ford, & Buchhorn 1992), NGC 4469, NGC 4710 (Rubin, Waterman, & Kenney 1999), and ESO 597-G036 (Nishiura et al 2000). We note that Bureau & Freeman (1999) did not extract rotation curves from their data, relying instead on the entire PVD diagrams.…”

Section: Comparison With Published Datamentioning

confidence: 99%

Stellar Kinematics of Boxy Bulges: Large-Scale Bars and Inner Disks

2004

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Long-slit stellar kinematic observations were obtained along the major axis of 30 edge-on spiral galaxies, 24 with a boxy or peanut-shaped (B/PS) bulge and six with other bulge types for comparison. Such B/ PS bulges are identified in at least 45% of highly inclined systems, and a growing body of theoretical and observational work suggests that they are the edge-on projection of thickened bars. Profiles of the mean stellar velocity V, the velocity dispersion , as well as the asymmetric (h 3 ) and symmetric (h 4 ) deviations from a pure Gaussian are presented for all objects. Comparing these profiles with stellar kinematic bar diagnostics developed from N-body simulations, we find bar signatures in 24 of our sample galaxies (80%). Galaxies with a B/ PS bulge typically show a double-humped rotation curve with an intermediate dip or plateau. They also frequently show a rather flat central velocity dispersion profile accompanied by a secondary peak or plateau, and numerous galaxies have a local central minimum (k40%). The h 3 profiles display up to three slope reversals. Most importantly, h 3 is normally correlated with V over the presumed bar length, contrary to expectations from axisymmetric disks. These characteristic bar signatures strengthen the case for a close relationship between B/ PS bulges and bars and leave little room for other explanations of the bulges' shape. We also find that h 3 is anticorrelated with V in the very center of most galaxies (k60%), indicating that these objects additionally harbor cold and dense decoupled (quasi-) axisymmetric central stellar disks, which may be related to the central light peaks. These central disks coincide with previously identified star-forming ionized-gas disks (nuclear spirals) in gas-rich systems, and we argue that they formed out of gas accumulated by the bar at its center through inflow. As suggested by N-body models, the asymmetry of the velocity profile (h 3 ) appears to be a reliable tracer of asymmetries in disks, allowing us to discriminate between axisymmetric and barred disks seen in projection. B/ PS bulges (and thus a large fraction of all bulges) appear to be made up mostly of disk material, which has acquired a large vertical extent through bar-driven vertical instabilities. Their formation is thus probably dominated by secular evolution processes rather than merging.

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A Dynamical Study of Galaxies in the Hickson Compact Groups

Cited by 36 publications

References 35 publications

HCG 31: a multiple merger in progress

HCG 31: a multiple merger in progress

Gas kinematics of a sample of five Hickson Compact Groups

Stellar Kinematics of Boxy Bulges: Large-Scale Bars and Inner Disks

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