Stellar population of the irregular galaxy IC 10

Тихонов, Н. А.; Galazutdinova, O. A.

doi:10.1134/s1063773709110036

Cited by 21 publications

(21 citation statements)

References 35 publications

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“…They detected several samples of old red giant stars (well fitted with isochrones of 13 Gyr) up to radial distances of 18–23 arcmin from the galactic centre, and an old star excess at least up to 34–42 arcmin from the centre. Similar results were also obtained by Tikhonov & Galazutdinova (), who detect an old stellar population coincident with the H i envelope. Thus, we can suppose that the external PNe are associated with the old and intermediate‐age stellar populations, since no young population is detected in the outskirts.…”

Section: Discussionsupporting

confidence: 90%

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

Gonçalves

Teodorescu

Alves-Brito

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present positions, kinematics and the planetary nebula luminosity function (PNLF) for 35 planetary nebulae (PNe) in the nearest starburst galaxy IC10 extending out to 3 kpc from the galaxy's centre. We take advantage of the deep imaging and spectroscopic capabilities provided by the Faint Object Camera and Spectrograph on the 8.2 m Subaru Telescope. The PN velocities were measured through the slitless‐spectroscopy technique, which allows us to explore the kinematics of IC10 with high precision. Using these velocities, we conclude that there is a kinematic connection between the H i envelope located around IC10 and the galaxy's PN population. By assuming that the PNe in the central regions and in the outskirts have similar ages, our results put strong observational constraints on the past tidal interactions in the Local Group. This is so because by dating the PN central stars, we, therefore, infer the epoch of a major episode of star formation likely linked to the first encounter of the H i extended envelope with the galaxy. Our deep [O iii] images also allow us to use the PNLF to estimate a distance modulus of 24.1 ± 0.25, which is in agreement with recent results in the literature based on other techniques.

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Section: Discussionsupporting

confidence: 90%

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

Gonçalves

Teodorescu

Alves-Brito

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…This means that the stellar halo and the hydrogen cloud have, within the errors, similar radial extents and resolve this peculiar feature of IC10 (Tikhonov & Galazutdinova 2009). Moreover, this evidence further supports the hypothesis that the hydrogen cloud is associated with the galaxy (stellar mass loss, pristine gas ;Huchtmeier 1979;Cohen 1979;Wilcots & Miller 1998).…”

Section: Resultsmentioning

confidence: 53%

“…Pointing δ includes 24 F 555W -band and 24 F 814W -band images of 500 s each. This pointing is located ∼3 NE of the galaxy center; it is outside the disk identified by Jarrett et al (2003; see the red ellipse in Figure 1) and inside the thick disk identified by Tikhonov & Galazutdinova (2009). The ground-based data were collected with the prime focus camera (Suprime-Cam, pointing ) on the Subaru telescope and with Mega-Cam on the Canada-France-Hawaii Telescope (CFHT, pointing ζ ).…”

Section: Photometric Datamentioning

confidence: 99%

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On the Radial Extent of the Dwarf Irregular Galaxy Ic10

Bono

Stetson²,

Ferraro

et al. 2010

ApJ

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We present new deep and accurate space (Advanced Camera for Surveys-Wide Field Planetary Camera 2 on board the Hubble Space Telescope) and ground-based (Suprime-Cam at Subaru Telescope, Mega-Cam at Canada-France-Hawaii Telescope) photometric and astrometric data for the Local Group dwarf irregular IC10. We confirm the significant decrease of the young stellar population when moving from the center toward the outermost regions. We find that the tidal radius of IC10 is significantly larger than previous estimates of r t 10 . By using the I, V -I color-magnitude diagram based on the Suprime-Cam data, we detect sizable samples of red giant (RG) stars up to radial distances of 18 -23 from the galactic center. The ratio between observed star counts (Mega-Cam data) across the tip of the RG branch and star counts predicted by Galactic models indicates a star count excess at least at a 3σ level up to 34 -42 from the center. This finding supports the hypothesis that the huge H i cloud covering more than 1• across the galaxy is associated with IC10. We also provide new estimates of the total luminosity (L V ∼ 9 × 10 7 L , M V ∼ −15.1 mag) that agree with similar estimates available in the literature. If we restrict our study to the regions where rotational velocity measurements are available (r ≈ 13 ), we find a mass-to-light ratio (∼10 M /L ) that is at least one order of magnitude larger than previous estimates. The new estimate should be cautiously treated, since it is based on a minimal fraction of the body of the galaxy.

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“…Uncertain data due to inhomogeneous background in crowded stellar fields are given without error bars and are marked by a colon. In the first column, we also indicate the objects from the paper of Hunter (2001) (HX-X), and those which we consider to be common with the list of Tikhonov & Galazutdinova (2009…”

Section: A P P E N D I X a : P H Oto M E T Ry O F C L U S T E R S I Nmentioning

confidence: 99%

SAO RAS 6-m telescope spectroscopic observations of globular clusters in nearby galaxies

Шарина

Chandar

Puzia

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We present the results of medium‐resolution spectroscopy of 28 globular clusters (GCs) in six nearby galaxies of different luminosities and morphological types, situated in M33 (15 objects), M31 (three), IC10 (four), UGCA86 (four), Holmberg IX (one) and DDO71 (one) obtained at the Special Astrophysical Observatory 6‐m telescope. Measurements of Lick absorption line indices and comparison with Simple Stellar Population models enabled us to obtain their spectroscopic ages, metallicities and α‐element to Fe abundance ratios. We found that all old‐ and intermediate‐age GCs in our sample have low metallicities [Z/H]≲ ‐0. 8 dex. Metal‐rich clusters are young and are preferentially found in galaxies more massive than ∼ 109 M⊙. The least massive dwarfs of our sample, DDO71 and Holmberg IX, host one massive intermediate‐age and one massive young metal‐poor GC, respectively. [α/Fe] abundance ratios tend to be enhanced but closer to solar values for dwarf galaxies compared to GCs in more massive galaxies. We analyse the age–metallicity relation for GCs in our sample and others from the literature, and find that (1) there is a general trend for GCs in low surface brightness dwarf galaxies to be more metal‐poor at a given age than GCs in more massive galaxies; (2) the GC metallicity spread is wider for more massive galaxies and (3) intermediate‐age GCs in early‐type dwarf galaxies are more metal‐rich at any given age than those in irregular galaxies of similar luminosity.

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Stellar population of the irregular galaxy IC 10

Cited by 21 publications

References 35 publications

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

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

On the Radial Extent of the Dwarf Irregular Galaxy Ic10

SAO RAS 6-m telescope spectroscopic observations of globular clusters in nearby galaxies

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