A kinematic study of planetary nebulae in the dwarf irregular galaxy IC10

Gonçalves, Denise R.; Teodorescu, A. M.; Alves-Brito, Alan; Méndez, R. H.; Magrini, L.

doi:10.1111/j.1365-2966.2012.21726.x

Cited by 11 publications

(11 citation statements)

References 41 publications

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“…7) consist exclusively of FSR 486 stars. The derived distance modulus to IC 10 in previous works is larger than 24 mag (Borissova et al 2000;Hunter 2001;Sanna et al 2008;Gonçalves et al 2012). However, we derive a distance modulus of ≈ 14 mag for FSR 486.…”

Section: Fsr 486 and The Dwarf Galaxy Ic 10mentioning

confidence: 62%

Towards a census of the Galactic anticentre star clusters – III. Tracing the spiral structure in the outer disc

Camargo¹,

Bica²,

Bonatto³

2013

Monthly Notices of the Royal Astronomical Society

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In this paper we investigate the nature of 27 star cluster candidates, most of them projected towards the Galactic anticentre. We derive fundamental parameters for 20 confirmed clusters, among these 7 are new identifications. Four of the remaining are uncertain cases that require deeper photometry to establish their nature, and 4 are probably field fluctuations. In addition, we provide a partial census of the open clusters towards the Galactic anticentre. We also include in this study some interesting objects outside the anticentre region, in the second and third Galactic quadrants, mainly in the Perseus and Outer arms. These clusters confirm the extension of the Outer arm along the third quadrant. We also point out that the embedded cluster FSR 486, at a distance of 7.2 ± 1.3 kpc from de Sun, is projected on the line of sight of the Local Group irregular dwarf galaxy IC 10. Thus, part of the unusual properties of IC 10 may be explained by a Galactic contamination. We point out the importance of embedded clusters in tracing the spiral structure.

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Section: Fsr 486 and The Dwarf Galaxy Ic 10mentioning

confidence: 62%

Towards a census of the Galactic anticentre star clusters – III. Tracing the spiral structure in the outer disc

Camargo¹,

Bica²,

Bonatto³

2013

Monthly Notices of the Royal Astronomical Society

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“…carried out by Gonçalves et al (2012), who reported that there is a kinematical connection between both populations in IC 10. Several authors have also used the PN population to analyze the kinematics of elliptical galaxies, for example, Mc Neil-Moylan et al (2012), Teodorescu et al (2011), and Coccato et al (2009) have analyzed PNe kinematics in ellipticals at about 20 Mpc, and Ventimiglia et al (2011) and Gerhard et al (2007) have studied ellipticals at 50-100 Mpc.…”

Section: Introductionmentioning

confidence: 98%

Kinematic study of planetary nebulae in NGC 6822

Flores-Durán

Peña

Hernández-Martínez

et al. 2014

A&A

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Context. The kinematics of planetary nebulae in external galaxies and in our own is a clue for understanding the behavior of the lowand intermediate-mass stars and their relation with other components of the galaxies.Aims. By measuring precise radial velocities of planetary nebulae (which belong to the intermediate-age population), H ii regions and A-type supergiant stars (which are members of the young population) in NGC 6822, we aim to determine whether both types of population share the kinematics of the disk of H i found in this galaxy.Methods. Spectroscopic data for six planetary nebulae were obtained with the high spectral-resolution spectrograph Magellan Inamori Kyocera Echelle (MIKE) on the Magellan telescope at Las Campanas Observatory. Data for another three PNe and one H ii region were obtained from the SPM Catalog of Extragalactic Planetary Nebulae, which employed the Manchester Echelle Spectrometer attached to the 2.1m telescope at the Observatorio Astronómico Nacional, México. An additional PN and one H ii region were observed with this same telescope-spectrograph in 2013. Thus, in total we have high-quality data for 10 of the 26 PNe detected in this galaxy. In the wavelength calibrated spectra, the heliocentric radial velocities were measured with a precision better than 5-6 km s −1 . Data for two additional H ii regions and two A-type supergiant stars were collected from the literature. The heliocentric radial velocities of the different objects were compared to the velocities of the H i disk at the same position.Results. From the analysis of radial velocities we found that H ii regions and A-type supergiants do share the kinematics of the H i disk at the same position, as expected for these young objects. In contrast, most planetary nebula velocities differ significantly (more than 12 km s −1 ) from that of the H i at the same position. The kinematics of planetary nebulae is different from the young population kinematics and is more similar to the behavior shown by carbon stars, which are intermediate-age members of the stellar spheroid existing in this galaxy. Our results confirm that there are at least two very different kinematical systems in NGC 6822.

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“…This indicates that IC 10 is forming massive stars at the same rate as a star-forming region in a spiral galaxy, such as M33, throughout its disk. Gonçlaves et al (2012) used the Subaru telescope to study the kinematics of 35 planetary nebulae in IC 10 that traced the stellar motions. They concluded that the planetary nebulae generally follow the same kinematic trends as the gas, as measured by Very Large Array 2 (VLA), including the kinematics of some of the outer, counterrotating gas.…”

Section: Introductionmentioning

confidence: 99%

THE H I CHRONICLES OF LITTLE THINGS BCDs II: THE ORIGIN OF IC 10's H I STRUCTURE

Ashley

Elmegreen²,

Johnson

et al. 2014

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In this paper we analyze Very Large Array (VLA) telescope and Green Bank Telescope (GBT) atomic hydrogen (H I) data for the LITTLE THINGS 1 blue compact dwarf galaxy IC 10. The VLA data allow us to study the detailed H I kinematics and morphology of IC 10 at high resolution while the GBT data allow us to search the surrounding area at high sensitivity for tenuous H I. IC 10's H I appears highly disturbed in both the VLA and GBT H I maps with a kinematically distinct northern H I extension, a kinematically distinct southern plume, and several spurs in the VLA data that do not follow the general kinematics of the main disk. We discuss three possible origins of its H I structure and kinematics in detail: a current interaction with a nearby companion, an advanced merger, and accretion of intergalactic medium. We find that IC 10 is most likely an advanced merger or a galaxy undergoing accretion.

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A kinematic study of planetary nebulae in the dwarf irregular galaxy IC10

Cited by 11 publications

References 41 publications

Towards a census of the Galactic anticentre star clusters – III. Tracing the spiral structure in the outer disc

Towards a census of the Galactic anticentre star clusters – III. Tracing the spiral structure in the outer disc

Kinematic study of planetary nebulae in NGC 6822

THE H I CHRONICLES OF LITTLE THINGS BCDs II: THE ORIGIN OF IC 10's H I STRUCTURE

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