IC 10: More evidence that it is a blue compact dwarf

Richer, M. G.; Bullejos, A.; Borissova, J.; McCall, Marshall L.; Lee, H.; Kurtev, R.; Георгиев, Л.; Kingsburgh, R. L.; Ross, R. W.; Rosado, M.

doi:10.1051/0004-6361:20010206

Cited by 67 publications

(90 citation statements)

References 39 publications

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“…However, independent estimates of the total reddening (i.e., internal plus foreground) in IC10 by other authors suggest the value is nearer 0.7 -0.8 (e.g. 0.77 ± 0.07, Richer et al 2001;0.78 ± 0.06, Sanna et al 2008; but also 0.98 ± 0.06, Kim et al 2009). Given these uncertainties, adopting a spatially varying value on a star by star basis is not warranted, and we adopt a constant reddening value of E(B-V)= 0.77 ± 0.07 (Richer et al 2001).…”

Section: Data Acquisition Processing and Characterizationmentioning

confidence: 91%

“…Its high Hα luminosity (e.g., Kennicutt et al 2008) and an extremely high surface density of Wolf-Rayet stars that is approximately a factor of 20 times larger than the LMC (Massey & Armandroff 1995;Massey & Holmes 2002) lead it to be classified as a starburst galaxy. Richer et al 2001 argue that it also meets the criteria to be classified as a blue compact dwarf (BCD). Whatever its classification, IC10's star formation rate in comparison to our other nearby neighbours is unusually high.…”

Section: Introductionmentioning

confidence: 99%

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The red extended structure of IC 10, the nearest blue compact galaxy

Gerbrandt

McConnachie

Irwin

2015

Mon. Not. R. Astron. Soc.

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The Local Group starburst galaxy IC10 is the closest example of a blue compact galaxy. Here, we use optical gi imaging from CFHT/MegaCam and near infra-red JHK imaging from UKIRT/WFCAM to conduct a comprehensive survey of the structure of IC10. We examine the spatial distribution of its resolved young, intermediate and old stellar populations to large radius and low effective surface brightness levels. Akin to other dwarfs with multiple populations of different ages, stellar populations of decreasing average age are increasingly concentrated in this galaxy. We find that the young, star-bursting population, and the AGB population, are both offset from the geometric center of the older RGB population by a few hundred parsecs, implying that the younger star formation occurred significantly away from the center of the galaxy. The RGB population traces an extended structure that is typical of blue compact galaxies, with an effective radius of ∼ 5.75 arcmins (∼ 1.25 kpc). These measurements show that IC10 is much more extended than has previously been realized, and this blue compact galaxy is one of the most extended dwarf galaxies in the Local Group. The outermost isophotes of this galaxy are very regular in shape and essentially circular in morphology. Based on this analysis, we do not find any evidence to suggest that IC10 has undergone a recent, significant, interaction with an unknown companion.

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Section: Data Acquisition Processing and Characterizationmentioning

confidence: 91%

Section: Introductionmentioning

confidence: 99%

The red extended structure of IC 10, the nearest blue compact galaxy

Gerbrandt

McConnachie

Irwin

2015

Mon. Not. R. Astron. Soc.

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“…Its size and mass are comparable to the SMC while its metallicity of 12 + log(O/H) ≈ 8. 26 (1/2.7 Z assuming the solar abundance from Asplund et al 2009) lies between that of the Small and Large Magellanic Cloud (Garnett 1990;Lequeux et al 1979;Richer et al 2001;Skillman et al 1989). The starburst nature of IC 10 was first revealed by the discovery of a large number of WR stars by Massey et al (1992).…”

Section: Introductionmentioning

confidence: 99%

Oxygen-rich dust production in IC 10

Lebouteiller¹,

Sloan²,

Groenewegen³

et al. 2012

A&A

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Context. We report the detection of oxygen-rich circumstellar envelopes in stars of the nearby (700 kpc) starburst galaxy IC 10. The star-formation history and the chemical environment of this galaxy make it an ideal target to observe dust production by massive stars in a metal-poor environment. Aims. The goal of this study is to identify oxygen-rich stars in IC 10 and to constrain their nature between asymptotic giant branch stars (AGBs), red supergiants (RSGs), and other bright infrared sources. We examine the mass-loss rates of the stars and compare to results obtained for the Magellanic Clouds. Our objectives are to (1) assess whether RSGs can be significant dust producers in IC 10, and (2), solve the discrepancy between the star-formation history of IC 10 and the relatively low number of RSGs detected in the optical. Methods. We search for silicate dust in emission by using the spectral map observed with the Infrared Spectrograph on board the Spitzer Space Telescope. The optical (UBVRI) and infrared (JHK, Spitzer/IRAC and Spitzer/MIPS) photometry are used to assert the membership of the stars to IC 10 and distinguish between AGBs and RSGs. Radiative models are used to infer mass-loss rates and stellar luminosities. Results. The luminosity and colors of at least 9 silicate emission sources are consistent with stars within IC 10. Furthermore, the photometry of 2 of these sources is consistent with RSGs. We derive dust mass-loss rates similar to the values found in the Magellanic Clouds. Accounting for the sample completeness, RSGs are not important contributors to the dust mass budget in IC 10.

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“…The progenitor stars Chemical abundances of H ii regions in IC 10 have been obtained by several authors, starting with Lequeux et al (1979), then recomputed by Skillman et al (1989), by Garnett et al (1990) with updated atomic data and ionization correction factors relative to those used by Lequeux et al (1979), and by the spectroscopic observations of Richer et al (2001). The observations by MG09 enlarged the number of studied H ii regions in whose spectra the electron temperature can be measured, and complemented them with PN observations.…”

Section: Chemical Abundancesmentioning

confidence: 99%

“…1. Hodge & Lee 1990;Richer et al 2001). The scale-length of metallicity inhomogeneities is of 0.2−0.3 kpc, some clumps The left column shows the evolution of He, O, N, S abundances, and the right column shows the evolution of the total SFR, total gas mass, total stellar mass, total baryonic mass, and gas fraction.…”

Section: Models Without Galactic Windsmentioning

confidence: 99%

The chemical evolution of IC 10

Yin¹,

Magrini²,

Matteuccí

et al. 2010

A&A

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Context. Dwarf irregular galaxies are relatively simple unevolved objects where it is easy to test models of galactic chemical evolution. Aims. We attempt to determine the star formation and gas accretion history of IC 10, a local dwarf irregular for which abundance, gas, and mass determinations are available. Methods. We apply detailed chemical evolution models to predict the evolution of several chemical elements (He, O, N, S) and compared our predictions with the observational data. We consider additional constraints such as the present-time gas fraction, the star formation rate (SFR), and the total estimated mass of IC 10. We assume a dark matter halo for this galaxy and study the development of a galactic wind. We consider different star formation regimes: bursting and continuous. We explore different wind situations: i) normal wind, where all the gas is lost at the same rate and ii) metal-enhanced wind, where metals produced by supernovae are preferentially lost. We study a case without wind. We vary the star formation efficiency (SFE), the wind efficiency, and the time scale of the gas infall, which are the most important parameters in our models. Results. We find that only models with metal-enhanced galactic winds can reproduce the properties of IC 10. The star formation must have proceeded in bursts rather than continuously and the bursts must have been less numerous than ∼10 over the whole galactic lifetime. Finally, IC 10 must have formed by a slow process of gas accretion with a timescale of the order of 8 Gyr.

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IC 10: More evidence that it is a blue compact dwarf

Cited by 67 publications

References 39 publications

The red extended structure of IC 10, the nearest blue compact galaxy

The red extended structure of IC 10, the nearest blue compact galaxy

Oxygen-rich dust production in IC 10

The chemical evolution of IC 10

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