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Date and Time of the Query: 2019-06-19 T12:46:15 PDT
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For refcode 2012A&A...543A..35J:
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Copyright by European Southern Observatory (ESO). Reproduced by permission
2012A&A...543A..35J Near-infrared properties of asymptotic giant branch stars in nearby dwarf elliptical galaxy NGC 205 Jung, M. Y.; Ko, J.; Kim, J.-W.; Chun, S.-H.; Kim, H.-I.; Sohn, Y.-J. Abstract. Aims: We investigated the distribution of resolved asymptotic giant branch (AGB) stars over a much larger area than covered by previous near-infrared studies in the nearby dwarf elliptical galaxy NGC 205. Methods: Using data obtained with the WIRCam near-infrared imager of the CFHT, we selected the AGB stars in the JHK_s_ color - magnitude diagrams, and separated the C stars from M-giant stars in the JHK_s_ color - color diagram. Results: We identified 1,550 C stars in NGC 205 with a mean absolute magnitude of < M_K_s_ > = -7.49 +/- 0.54, and colors of < (J - K_s_)_0_ > = 1.81 +/- 0.41 and < (H - K_s_)_0_ > = 0.76 +/- 0.24. The ratio of C stars to M-giant stars was estimated to be 0.15 +/- 0.01 in NGC 205, and the local C/M ratios for the southern region are somewhat lower than those for the northern region. The (J - K_s_) color distributions of AGB stars contain the main peak of the M-giant stars and the red tail of the C stars. A comparison of the theoretical isochrone models with the observed color distribution indicates that most of the bright M-giant stars in NGC 205 were formed at log (t_yr_) ~ 9.0-9.7. The logarithmic slope of the M_K_s_ luminosity function for M-giant stars was estimated to be 0.84 +/- 0.01, which is comparable with dwarf elliptical galaxies NGC 147 and NGC 185. Furthermore, we found that the logarithmic slopes of the M_K_s_ luminosity function for C and M-giant stars are different to places, implying a different star formation history within NGC 205. The bolometric luminosity function for M-giant stars extends to M_bol_ = -6.0 mag, and that for C stars spans -5.6 < M_bol_ < -3.0. The bolometric luminosity function of C stars is unlikely to be a Gaussian distribution and the mean bolometric magnitude of C stars is estimated to be M_bol_ = -4.24 +/- 0.55, which is consistent with our results for dwarf elliptical galaxies NGC 147 and NGC 185. Based on observations carried out at the Canada-France-Hawaii Telescope, operated by the National Research Council of Canada, the Centre National de la Recherche Scientifique de France, and the University of Hawaii.Calibrated photometry is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/543/A35 Key words: galaxies: individual: NGC 205, galaxies: stellar content, stars: AGB and post-AGB
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