GHASP : An Halpha kinematic survey of spiral and irregular galaxies - VI. New Halpha data cubes for 108 galaxies B. Epinat, P. Amram, M. Marcelin, C. Balkowski, O. Daigle, O. Hernandez, L. Chemin, C. Carignan, J. -L. Gach, P. Balard
To cite this version:
B. Epinat, P. Amram, M. Marcelin, C. Balkowski, O. Daigle, et al.. GHASP : An Halpha kinematic survey of spiral and irregular galaxies - VI. New Halpha data cubes for 108 galaxies. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2008, 388, pp.500. hal-00325102
HAL Id: hal-00325102 https://hal.archives-ouvertes.fr/hal-00325102 Submitted on 30 Apr 2021
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GHASP:anHα kinematic survey of spiral and irregular galaxies – VI. New Hα data cubes for 108 galaxies
B. Epinat,1 P. Amram,1 M. Marcelin,1 C. Balkowski,2 O. Daigle,1,3 O. Hernandez,1,3 L. Chemin,2 C. Carignan,3 J.-L. Gach1 and P. Balard1 1Laboratoire d’Astrophysique de Marseille, OAMP, Universite´ de Provence & CNRS, 38 rue F. Joliot - Curie, 13388 Marseille, Cedex 13, France 2GEPI, Observatoire de Paris-Meudon, Universite´ Paris VII, 5 Place Jules Janssen, 92195 Meudon, France 3LAE et Observatoire du mont Megantic,´ Universite´ de Montreal,´ C. P. 6128 succ. centre ville, Montreal,´ Quebec,´ Canada H3C 3J7 Downloaded from https://academic.oup.com/mnras/article/388/2/500/976912 by guest on 30 April 2021 Accepted 2008 May 7. Received 2008 May 4; in original form 2008 January 15
ABSTRACT We present the Fabry–Perot observations obtained for a new set of 108 galaxies in the frame of the Gassendi Hα survey of SPirals (GHASP). The GHASP survey consists of 3D Hα 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 Hα data cubes from which are computed Hα 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. Key words: galaxies: dwarf – galaxies: irregular – galaxies: kinematics and dynamics – galaxies: spiral.
(GHASP). The GHASP survey consists of a sample of 203 spiral 1 INTRODUCTION and irregular galaxies, mostly located in nearby low density envi- As it is nowadays largely admitted, 2D velocity fields allow the ronments, observed with a scanning Fabry–Perot for studying their computation of 1D rotation curves in a more robust way than long- kinematical and dynamical properties through the ionized hydrogen slit spectrography. Indeed, first of all, the spatial coverage is larger component. and moreover, the kinematical parameters are determined a posteri- Studying the links between parameters reflecting the dynamical ori instead of a priori in long-slit spectrography. In that context, we state of a galaxy will help us to have a better understanding of the have undertaken the kinematical 3D Gassendi Hα survey of SPirals evolution of galaxies. This sample has been constituted in order: (i) to compute the local Tully–Fisher relation; (ii) to compare the kinematics of galaxies in different envi- E-mail: [email protected] ronments (field, pairs, compact groups, galaxies in cluster) for