Catalogue of HII regions measured on 6 m telescope plates at Observatoire de Marseille

Abstract

Abstract. Several galaxies were studied at Observatoire de Marseille using the films obtained at the 6 m telescope with the Great Focal Reducer installed at the prime focus of the russian telescope.We thought that before we retire, it should be of some interest for the astronomical community to find in a single catalogue all the data we published to facilitate the research. (see hereunder the references).We give in this catalogue the data of the following galaxies: M 33, M 51, M 81, NGC 2403, NGC 4258 and NGC 7331. NGC 4258 was not studied with the 6 m telescope, but we added its results because it was published by the same team using the same softwares. For NGC 7331 (see Petit 1998).The flux values are followed by*; that means that they are not absolute fluxes like in the other publications.In order to make the catalogue easier to consult, we homogeneised the data. So, one can find some slight differences between the original data and the catalogue ones. The details of these modifications are precised in the Readme file associated to the catalogue in the data base. Send offprint requests to: H. PetitThe catalogue is available at the CDS via anonymous ftp 130.79.128.5 or http://cdsweb.u-strasbg.fr/Abstract.htmlWe did not keep the remarks so it is necessary to look at the original publication to find the full information.We give the whole references hereunder to facilitate the research of the original articles.

A New Catalog of H Ii Regions in M31

“…The characteristics of HII regions have been studied in many extragalactic Hα surveys [e.g. Knapen (1998) and references therein; Petit et al (1998); Thilker et al (2002); Kennicutt et al (2008)]. The studies by Kennicutt (1988) and Kennicutt et al (1989, KEH89 hereafter) of the population of HII regions in nearby galaxies confirmed that HII region population properties are strongly dependent on the host galaxy Hubble type.…”

Variation in the flare activity of the star UV Ceti

“…At least 50 of them are in binary and multiple systems, and it is still difficult to tell which of the remaining 43 is isolated. Of the 491 variable stars closer than 22 pc from the sun, 111 are UV Ceti flare stars, of which 55 are members of binary or multiple systems [8]. Thus, it is natural to assume that membership in a binary of multiple system is a characteristic feature of flare stars in the sun's neighborhood and may play an important role in the active physical processes observed in these stars.…”

On the rotation period of Capella

“…His light curve was rather erratic and undersampled and has never been verified so that we believe that it was spurious. Unfortunately, it made its way through the literature and was cited in the catalogs by Kukarkin et al (1982), Petit (1990), and Strassmeier et al (1993). The most recent photometry that we are aware of is that by Krisciunas & Guinan (1990), who observed the star independently between 1981 and 1990.…”