Hα Survey of the Milky Way and Magellanic Clouds

Marcelin, M.; Amram, P.; Boulesteix, J.; Georgelin, Y. P.; Laval, A.; Coarer, E. Le; Rosado, M.; Goldès, G.

doi:10.1007/978-94-011-1146-1_106

Cited by 7 publications

(11 citation statements)

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“…These peculiar ‘hotspots’ in the nuclear region have been identified and described in different ways by various authors. Marcelin, Boulesteix & Georgelin (1983) found six ‘hotspots’ forming a linear structure that crosses the central region. A later study in infrared and radio by Wynn‐Williams & Becklin (1985) showed that bursts of SF were not confined to the visible hotspots.…”

Section: Results On Individual Galaxiesmentioning

confidence: 99%

Circumnuclear regions in barred spiral galaxies — I. Near-infrared imaging

Pérez-Ramírez

Knapen

Peletier

et al. 2000

Monthly Notices of the Royal Astronomical Society

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We present subarcsecond‐resolution, ground‐based, near‐infrared images of the central regions of a sample of 12 barred galaxies with circumnuclear star formation activity, which is organized in ring‐like regions typically 1 kpc in diameter. We also present Hubble Space Telescope near‐infrared images of 10 of our sample galaxies, and compare them with our ground‐based data. Although our sample galaxies were selected for the presence of circumnuclear star formation activity, our broad‐band near‐infrared images are heterogeneous, showing a substantial amount of small‐scale structure in some galaxies, and practically none in others. We argue that, where it exists, this structure is caused by young stars, which also cause the characteristic bumps or changes in slope in the radial profiles of ellipticity, major axis position angle, surface brightness and colour at the radius of the circumnuclear ring in most of our sample galaxies. In seven out of 10 HST images, star formation in the nuclear ring is clearly visible as a large number of small emitting regions, organized into spiral arm fragments, which are accompanied by dust lanes. Near‐infrared colour index maps show much more clearly the location of dust lanes and, in certain cases, regions of star formation than single broad‐band images. Circumnuclear spiral structure thus outlined appears to be common in barred spiral galaxies with circumnuclear star formation.

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Section: Results On Individual Galaxiesmentioning

confidence: 99%

Circumnuclear regions in barred spiral galaxies — I. Near-infrared imaging

Pérez-Ramírez

Knapen

Peletier

et al. 2000

Monthly Notices of the Royal Astronomical Society

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“…These are to our knowledge the deepest Hα observations of this galaxy. Other Hα studies include that of Marcelin et al (1985) and Hoopes et al (1996). The first obtained a rotation curve extending only to r = 10 arcmin, and the second reached EMs between 6 and 500 cm −6 pc.…”

Section: Discussionmentioning

confidence: 99%

“…For NGC 247, we seek to see if diffuse optical emission can also be seen on a scale similar to the H i disc, and even beyond. For NGC 300, the H i disc extends to r = 20 arcmin, but previous Hα studies have only been able to detect ionized gas up to r ∼ 10 arcmin (Marcelin, Boulesteix & Georgelin 1985) and down to emission measures (EMs) of 6 cm −6 pc (Hoopes, Walterbos & Greenwalt 1996). Although we will be limited by our field of view for this galaxy, we will be able to reach further distances ( r ∼ 14 arcmin) and at least an order of magnitude deeper in flux, allowing us to further study the Hα kinematics of the galaxy.…”

Section: Introductionmentioning

confidence: 99%

Deep Fabry-Perot Hα observations of two Sculptor group galaxies, NGC 247 and 300

Hlavacek-Larrondo

Marcelin

Épinat

et al. 2011

Monthly Notices of the Royal Astronomical Society

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It has been suggested that diffuse ionized gas can extend all the way to the end of the H i disc, and even beyond, such as in the case of the warped galaxy NGC 253 (Bland‐Hawthorn et al.). Detecting ionized gas at these radii could carry significant implications as to the distribution of dark matter in galaxies. With the aim of detecting this gas, we carried out a deep Hα kinematical analysis of two Sculptor group galaxies, NGC 247 and 300. The Fabry–Perot data were taken at the 36‐cm Marseille Telescope in La Silla, Chile, offering a large field of view. With almost 20 hours of observations for each galaxy, very faint diffuse emission is detected. Typical emission measures of 0.1 cm−6 pc are reached. For NGC 247, emission extending up to a radius comparable with that of the H i disc (r∼ 13 arcmin) is found, but no emission is seen beyond the H i disc. For NGC 300, we detect ionized gas on the entirety of our field of view (rmax∼ 14 arcmin), and find that the bright H ii regions are embedded in a diffuse background. Using the deep data, extended optical rotation curves are obtained, as well as mass models. These are the most extended optical rotation curves thus far for these galaxies. We find no evidence suggesting that NGC 247 has a warped disc, and to account for our non‐detection of Hα emission beyond its H i disc, as opposed to the warped galaxy NGC 253, our results favour the model in which, only through a warp, ionization by hot young stars in the central region of a galaxy can let photons escape and ionize the interstellar medium in the outer parts.

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“…Nevertheless, for a perturbed system, it is important to have kinematical information of larger portions of the disk using observational techniques such as extended-object Fabry-Perot scanning interferometry since extended kinematical information can help determine the effect the interacting process has had on each of the members of the interacting system and because axial symmetry is probably lost during the interaction (Marcelin et al 1987;Amram et al 1994Amram et al , 2002.…”

Section: Introductionmentioning

confidence: 99%

The isolated interacting galaxy pair NGC 5426/27 (Arp 271)

Fuentes-Carrera

Rosado

Amram

et al. 2004

A&A

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Abstract. We present Hα observations of the isolated interacting galaxy pair NGC 5426/27 using the scanning Fabry-Perot interferometer PUMA. The velocity field, various kinematical parameters and rotation curve for each galaxy were derived. The FWHM map and the residual velocities map were also computed to study the role of non-circular motions of the gas. Most of these motions can be associated with the presence of spiral arms and structure such as central bars. We found a small bar-like structure in NGC 5426, a distorted velocity field for NGC 5427 and a bridge-like feature between both galaxies which seems to be associated with NGC 5426. Using the observed rotation curves, a range of possible masses was computed for each galaxy. These were compared with the orbital mass of the pair derived from the relative motion of the participants. The rotation curve of each galaxy was also used to fit different mass distribution models considering the most common theoretical dark halo models. An analysis of the interaction process is presented and a possible 3D scenario for this encounter is also suggested.

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Hα Survey of the Milky Way and Magellanic Clouds

Cited by 7 publications

References 1 publication

Circumnuclear regions in barred spiral galaxies — I. Near-infrared imaging

Circumnuclear regions in barred spiral galaxies — I. Near-infrared imaging

Deep Fabry-Perot Hα observations of two Sculptor group galaxies, NGC 247 and 300

The isolated interacting galaxy pair NGC 5426/27 (Arp 271)

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