GHASP: an Hα kinematic survey of spiral and irregular galaxies - VI. New Hα data cubes for 108 galaxies

By B. Epinat, P. Amram, Michael W. Marcelin, C. Balkowski, O. Daigle, O. Hernández, L. Chemin, C. Carignan, J. Gach, P. Balard. 2008

137 citations recorded by the source corpus.

We present the Fabry-Perot observations obtained for a new set of 108 galaxies in the frame of the Gassendi Ha survey of SPirals (GHASP). The GHASP survey consists of 3D Ha data cubes for 203 spiral and irregular galaxies, covering a large range in morphological types and absolute magnitudes, for kinematics analysis. The new set of data presented here completes the survey. The GHASP sample is by now the largest sample of Fabry-Perot data ever published. The analysis of the whole GHASP sample will be done in forthcoming papers. Using adaptive binning techniques based on Voronoi tessellations, we have derived Ha data cubes from which are computed Ha maps, radial velocity fields as well as residual velocity fields, position-velocity diagrams, rotation curves and the kinematical parameters for almost all galaxies. Original improvements in the determination of the kinematical parameters, rotation curves and their uncertainties have been implemented in the reduction procedure. This new method is based on the whole 2D velocity field and on the power spectrum of the residual velocity field rather than the classical method using successive crowns in the velocity field. Among the results, we point out that morphological position angles have systematically higher uncertainties than kinematical ones, especially for galaxies with low inclination. The morphological inclination of galaxies having no robust determination of their morphological position angle cannot be constrained correctly. Galaxies with high inclination show a better agreement between their kinematical inclination and their morphological inclination computed assuming a thin disc. The consistency of the velocity amplitude of our rotation curves has been checked using the Tully-Fisher relationship. Our data are in good agreement with previous determinations found in the literature. Nevertheless, galaxies with low inclination have statistically higher velocities than expected and fast rotators are less luminous than expected.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/08458ef16f74477bfc10b5f5b90dd94d77542255

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THE EPOCH OF DISK SETTLING: z ∼ 1 TO NOW (2012, unknown): “Although GHASP spans a larger range in stellar mass than our mass-limited sample: 9.0 < logM∗(M ) < 11.7 for a ‘diet’ Salpeter IMF (Epinat et al. 2008) (which is roughly 0.15 dex higher than the Chabrier 2003 IMF used in this paper), the sample medians are consistent with extrapolations of our…”
Evidence for strong dynamical evolution in disc galaxies through the last 11 Gyr. GHASP VIII – a local reference sample of rotating disc galaxies for high‐redshift studies (2009, methodology): “In Figure 12, we compare the maximum rotation velocity determined by Epinat et al. (2008b) with those determined from these two methods.”
THE 2MASS REDSHIFT SURVEY—DESCRIPTION AND DATA RELEASE (2011, unknown): “…Cortese et al. (2008) 2008MNRAS.385.1297B Brookes et al. (2008) 2008MNRAS.386..715T Trager et al. (2008) 2008MNRAS.386.2311S Smith Castelli et al. (2008) 2008MNRAS.388..500E Epinat et al. (2008) 2008MNRAS.389..749M Mendel et al. (2008) 2008MNRAS.389.1593K Krabbe et al. (2008) 20096dF...”
Integral field spectroscopy with SINFONI of VVDS galaxies I. Galaxy dynamics and mass assembly at 1.2 < z < 1.6 (2009, background): “At low redshifts, the knowledge of 2D velocity fields has proved to be a powerful kinematical tool to investigate the properties of nearby galaxies (Östlin et al. 2001; Veilleux et al. 2001; Swinbank et al. 2003; Mendes de Oliveira et al. 2003; Garrido et al. 2004; Epinat et al. 2008a,b).”
Core formation in dwarf haloes with self-interacting dark matter: no fine-tuning necessary (2014, methodology): “…for the purely dispersion galaxies are calculated using the Wolf et al. (2010) formula, where measurements for stellar velocity dispersion, σ?, are taken from Hoffman et al. (1996), Simon & Geha (2007), Epinat et al. (2008), Fraternali et al. (2009), Collins et al. (2013), and Kirby et al. (2014).”