Rotation Curves of 38 Galaxies in Clusters from Scanning Fabry-Perot observations

Amram, P.; Marcelin, M.; Balkowski, C.; Boulesteix, J.; Coarer, E. Le; Cayatte, V.; Sullivan, W. T.

doi:10.1017/s025292110002279x

Cited by 38 publications

(61 citation statements)

References 3 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…It shows more H i flux on the higher velocity side, in agreement with the optical rotation curve. The optical velocity map of Amram et al (1992) further confirms the observed asymmetry in the H distribution. The I-band image suggests an increase in flux in front of the nucleus (as does that of UGC 8096/IC 3949).…”

Section: Populationsupporting

confidence: 71%

M/L, Hα Rotation Curves, and HiGas Measurements for 329 Nearby Cluster and Field Spirals. II. Evidence for Galaxy Infall

et al. 2004

View full text Add to dashboard Cite

We have conducted a study of optical and H i properties of spiral galaxies (size, luminosity, H flux distribution, circular velocity, and H i gas mass) to explore the role of gas stripping as a driver of morphological evolution in clusters. We find a strong correlation between the spiral and S0 fractions within clusters, and the spiral fraction scales tightly with cluster X-ray gas luminosity. We explore young star formation and identify spirals that are (1) asymmetric, with truncated H emission and H i gas reservoirs on the leading edge of the disk, on a first pass through the dense intracluster medium in the cores of rich clusters; (2) strongly H i deficient and stripped, with star formation confined to the inner 5 h À1 kpc and 3 disk scale lengths; or (3) reddened, extremely H i deficient, and quenched, where star formation has been halted across the entire disk. We propose that these spirals are in successive stages of morphological transformation, between infalling field spirals and cluster S0's, and that the process that acts to remove the H i gas reservoir suppresses new star formation on a similarly fast timescale. These data suggest that gas stripping plays a significant role in morphological transformation and rapid truncation of star formation across the disk.

show abstract

Section: Populationsupporting

confidence: 71%

M/L, Hα Rotation Curves, and HiGas Measurements for 329 Nearby Cluster and Field Spirals. II. Evidence for Galaxy Infall

et al. 2004

View full text Add to dashboard Cite

show abstract

“…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

View full text Add to dashboard Cite

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.

show abstract

“…Velocity maps derived using 3D spectroscopy reproduce the complete velocity field, contrary to longslit spectra. Hα observations using FP instruments have been used for some 40 years now (Tully 1974;Deharveng & Pellet 1975;Dubout et al 1976or de Vaucouleurs & Pence 1980; and have been designed to derive velocity fields of nearby galaxies (e.g., Atherton et al 1982or Boulesteix et al 1984, and to create high signal-to-noise ratio (S/N) rotation curves for many spiral galaxies (e.g., Marcelin, Boulesteix & Georgelin 1985;Bonnarel et al 1988;Pence, Taylor & Atherton 1990;Corradi & Capaccioli 1991;Amram et al 1992;Cecil, Wilson & Tully 1992;Amram et al 1994;Sicotte, Carignan & Durand 1996;Ryder et al 1998;Jiménez-Vicente et al 1999;Knapen et al 2000 and many more). Chemin et al (2006) presented an Hα FP survey of Virgo cluster galaxies.…”

mentioning

confidence: 99%

Hα kinematics of S4G spiral galaxies – II. Data description and non-circular motions

Erroz-Ferrer¹,

Knapen²,

Leaman³

et al. 2015

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We present a kinematical study of 29 spiral galaxies included in the Spitzer Survey of Stellar Structure in Galaxies, using Hα Fabry-Perot data obtained with the Galaxy Hα Fabry-Perot System instrument at the William Herschel Telescope in La Palma, complemented with images in the R band and in Hα. The primary goal is to study the evolution and properties of the main structural components of galaxies through the kinematical analysis of the FP data, complemented with studies of morphology, star formation and mass distribution. In this paper we describe how the FP data have been obtained, processed and analysed. We present the resulting moment maps, rotation curves, velocity model maps and residual maps. Images are available in FITS format through the NASA/IPAC Extragalactic Database and the Centre de Données Stellaires. With these data products we study the non-circular motions, in particular those found along the bars and spiral arms. The data indicate that the amplitude of the non-circular motions created by the bar does not correlate with the bar strength indicators. The amplitude of those non-circular motions in the spiral arms does not correlate with either arm class or star formation rate along the spiral arms. This implies that the presence and the magnitude of the streaming motions in the arms is a local phenomenon.

show abstract

Rotation Curves of 38 Galaxies in Clusters from Scanning Fabry-Perot observations

Cited by 38 publications

References 3 publications

M/L, Hα Rotation Curves, and HiGas Measurements for 329 Nearby Cluster and Field Spirals. II. Evidence for Galaxy Infall

M/L, Hα Rotation Curves, and HiGas Measurements for 329 Nearby Cluster and Field Spirals. II. Evidence for Galaxy Infall

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

Hα kinematics of S4G spiral galaxies – II. Data description and non-circular motions

Contact Info

Product

Resources

About