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HI and Hα Mapping of M31 & M33

Published online by Cambridge University Press:  05 December 2011

Z. S. Kam ,
C. Carignan ,
L. Chemin ,
O. Hernandez ,
M. de Denus-Baillargeon  and
Y. Djabo
Z. S. Kam
Affiliation:
Laboratoire d'Astrophysique Expérimentale (LAE), Département de physique, Université de Montréal, C.P. 6128, Succ. Centre-ville, Montréal, Qc, CanadaH3C 3J7
C. Carignan
Affiliation:
Laboratoire d'Astrophysique Expérimentale (LAE), Département de physique, Université de Montréal, C.P. 6128, Succ. Centre-ville, Montréal, Qc, CanadaH3C 3J7 Observatoire d'Astrophysique de l'Université de Ouagadougou (ODAUO), UFR/SEA, B.P. 7021, Ouagadougou 03, Burkina Faso Department of Astronomy, University of Cape Town, Private Bag X3, Rondebosh 7701, South Africa email: kam@ASTRO.UMontreal.CA
L. Chemin
Affiliation:
Laboratoire d'Astrophysique de Bordeaux 2, rue de l'Observatoire, BP 89, 33271 Floirac CedexFrance.
O. Hernandez
Affiliation:
Laboratoire d'Astrophysique Expérimentale (LAE), Département de physique, Université de Montréal, C.P. 6128, Succ. Centre-ville, Montréal, Qc, CanadaH3C 3J7
M. de Denus-Baillargeon
Affiliation:
Laboratoire d'Astrophysique Expérimentale (LAE), Département de physique, Université de Montréal, C.P. 6128, Succ. Centre-ville, Montréal, Qc, CanadaH3C 3J7
Y. Djabo
Affiliation:
Laboratoire d'Astrophysique Expérimentale (LAE), Département de physique, Université de Montréal, C.P. 6128, Succ. Centre-ville, Montréal, Qc, CanadaH3C 3J7
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Résumé

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We performed a deep Hi and Hα mapping of M31 and M33 in order to get accurate kinematical data of those two galaxies and also to make a comparison between the Hi and Hα kinematics. The Hi data were obtained with the DRAO interferometer and the Hα data with the Fabry-Perot system of the Observatoire du mont Mégantic using an EMCCD as a detector. These data will give us the best possible datasets to derive accurate rotation curves and mass models for those two Local Group spirals and provide some new data for the Hii regions studies of these galaxies. While the Hi observations are of low resolution (~1 arcmin), the high resolution of the Hα data (~1 arcsec) should allow us to get much more details in the central regions, allowing at the same time a much better determination of the kinematical parameters. Hence, the inner part of the rotation curve, so inportant to constraint properly the mass models, will be determined more accurately.

Keywords

Galaxy: individual: M31M33Galaxy: kinematicsISM: lines: HiHα
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S277: Tracing the Ancestry of Galaxies (on the land of our ancestors) , December 2010 , pp. 116 - 120
Copyright
Copyright © International Astronomical Union 2011

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