On the Distance and Reddening of the Starburst Galaxy IC 10

The Astrophysical Journal (Impact Factor: 6.73). 12/2008; 688(2):L69. DOI: 10.1086/595551
Source: arXiv

ABSTRACT We present deep and accurate optical photometry of the Local Group starburst galaxy IC 10. The photometry is based on two sets of images collected with the Advanced Camera for Surveys and with the Wide Field Planetary Camera 2 on board the Hubble Space Telescope. We provide new estimates of the tip of the red giant branch (TRGB) magnitude, = 21.90 ± 0.03, and of the reddening, E(B − V) = 0.78 ± 0.06, using field stars in the Small Magellanic Cloud (SMC) as a reference. Adopting the SMC and two globulars, ω Cen and 47 Tuc, as references we estimate the distance modulus to IC 10: independent calibrations give weighted average distances of μ = 24.51 ± 0.08 (TRGB) and μ = 24.56 ± 0.08 (RR Lyrae). We also provide a new theoretical calibration for the TRGB luminosity, and using these predictions we find a very similar distance to IC 10 (μ ≈ 24.60 ± 0.15). These results suggest that IC 10 is a likely member of the M31 subgroup.

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    ABSTRACT: We have used observations of the galaxy IC 10 at the 6-m telescope of the Special Astrophysical Observatory with the SCORPIO focal reducer in the Fabry-Perot interferometer mode and with the MPFS spectrograph to study the structure and kinematics of ionized gas in the central region of current intense star formation. Archive VLA 21-cm observations are used to analyze the structure and kinematics of neutral gas in this region. High-velocity wings of the H-alpha and [SII] emission lines were revealed in the inner cavity of the nebula HL 111 and in other parts of the complex of violent star formation. We have discovered local expanding neutral-gas shells around the nebulae HL 111 and HL 106. Comment: 22 pages, 10 figures; accepted in Astronomy Reports
    Astronomy Reports 03/2010; · 0.76 Impact Factor
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    ABSTRACT: We estimate the reddening and distance of the nearest starburst galaxy IC 10 using deep near-infrared JHK S photometry obtained with the Multi-Object InfraRed Camera and Spectrograph (MOIRCS) on the Subaru telescope. We estimate the foreground reddening toward IC 10 using the UBV photometry of IC 10 from the Local Group Survey, obtaining E(B – V) = 0.52 ± 0.04 mag. We derive the total reddening including the internal reddening, E(B – V) = 0.98 ± 0.06 mag, using the UBV photometry of early-type stars in IC 10 and comparing the JHK S photometry of red giant branch stars in IC 10 and the Small Magellanic Cloud. Using the Two Micron All Sky Survey point-source catalog of 20 Galactic globular clusters, we derive a relation between the metallicity [Fe/H]CG97 and the slope of the red giant branch in the K S – (J – K S) color-magnitude diagram. The mean metallicity of the red giant branch stars in IC 10 is estimated to be [Fe/H]CG97 = –1.08 ± 0.28. The magnitude of the tip of the red giant branch (TRGB) of IC 10 in the K S band is measured to be K S,TRGB = 18.28 ± 0.01. Based on the TRGB method, we estimate the distance modulus of IC 10 to be (m – M)0 = 24.27 ± 0.03(random) ± 0.18(systematic), corresponding to the distance of d = 715 ± 10 ± 60 kpc. This confirms that IC 10 is a member of the Local Group.
    The Astrophysical Journal 09/2009; 703(1):816. · 6.73 Impact Factor
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    ABSTRACT: We present results from integral field spectroscopy with the Potsdam Multi-Aperture Spectrograph at the 3.5-m telescope at Calar Alto Observatory of the intense star-forming region [HL90] 111 at the centre of the starburst galaxy IC 10. We have obtained maps with a spatial sampling of 1 × 1 arcsec2= 3.9× 3.9 pc2 of different emission lines and analysed the extinction, physical conditions, nature of the ionization and chemical abundances of the ionized gas, as well determined locally the age of the most recent star formation event. By defining several apertures, we study the main integrated properties of some regions within [HL90] 111. Two contiguous spaxels show an unambiguous detection of the broad He iiλ4686 emission line, this feature seems to be produced by a single late-type WN star. We also report a probable N and He enrichment in the precise spaxels where the Wolf–Rayet (WR) features are detected. The enrichment pattern is roughly consistent with that expected for the pollution of the ejecta of a single or a very small number of WR stars. Furthermore, this chemical pollution is very localized (∼2 arcsec ∼7.8 pc) and it should be difficult to detect in star-forming galaxies beyond the Local Volume. We also discuss the use of the most common empirical calibrations to estimate the oxygen abundances of the ionized gas in nearby galaxies from 2D spectroscopic data. The ionization degree of the gas plays an important role when applying these empirical methods, as they tend to give lower oxygen abundances with increasing ionization degree.
    Monthly Notices of the Royal Astronomical Society 12/2010; 411(3):2076 - 2092. · 5.52 Impact Factor

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