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J/A+A/543/A35       Near-IR photometry of C stars in NGC 205       (Jung+, 2012)

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. <Astron. Astrophys. 543, A35 (2012)> =2012A&A...543A..35J
ADC_Keywords: Galaxies, nearby ; Stars, giant ; Stars, carbon ; Photometry, infrared Keywords: galaxies: individual: NGC205 - galaxies: stellar content - stars: AGB and post-AGB Abstract: 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. Using data obtained with the WIRCam near-infrared imager of the CFHT, we selected the AGB stars in the JHKs color - magnitude diagrams, and separated the C stars from M-giant stars in the JHKs color - color diagram. We identified 1,550 C stars in NGC 205 with a mean absolute magnitude of <M_Ks≥-7.49±0.54, and colors of <(J-K)_0≥1.81±0.41 and <(H-Ks)_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) 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(tyr)∼9.0-9.7. The logarithmic slope of the MKs 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 MKs 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 Mbol=-6.0mag, and that for C stars spans -5.6<Mbol←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 Mbol=-4.24±0.55, which is consistent with our results for dwarf elliptical galaxies NGC 147 and NGC 185. Description: Table 1 lists the equatorial coordinates, near-infrared photometric properties of 1,550 C stars, and color indices in RI bands of cross-identified C stars with Demers et al. (2003, Cat. J/AJ/125/3037). File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 113 1550 Coordinates and photometric properties for 1550 C stars in NGC 205
See also: J/AJ/125/3037 : RI photometry of NGC 205 carbon stars (Demers+, 2003) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 4 I4 --- ID ID number of C star 7 I1 h RAh Right Ascension J2000 (hours) 9- 10 I2 min RAm Right Ascension J2000 (minutes) 12- 16 F5.2 s RAs Right Ascension J2000 (seconds) 18 A1 --- DE- Declination J2000 (sign) 19- 20 I2 deg DEd Declination J2000 (degrees) 22- 23 I2 arcmin DEm Declination J2000 (minutes) 25- 28 F4.1 arcsec DEs Declination J2000 (seconds) 31- 36 F6.3 mag Ksmag Ks band magnitude of C star 38- 42 F5.3 mag e_Ksmag Error of Ks magnitude 45- 49 F5.3 mag J-Ks J-Ks color index 51- 55 F5.3 mag e_J-Ks Error of J-Ks color index 58- 62 F5.3 mag H-Ks H-Ks color index 64- 68 F5.3 mag e_H-Ks Error of H-Ks color index 71- 76 F6.3 mag Imag ? I band magnitude of C star (1) 78- 82 F5.3 mag e_Imag ? Error of I magnitude (1) 85- 89 F5.3 mag R-I ? R-I color index (1) 91- 95 F5.3 mag e_R-I ? Error of R-I color index (1) 98-102 F5.3 mag CN-TiO ? CN-TiO color index (1) 104-108 F5.3 mag e_CN-TiO ? Error of CN-TiO color index (1) 111-113 I3 --- [DBL2003] ? ID number of Demers et al., 2003, Cat. J/AJ/125/3037
Note (1): From Demers et al., 2003, Cat. J/AJ/125/3037
Acknowledgements: MiYoung Jung, myjung(at)galaxy.yonsei.ac.kr
(End) Patricia Vannier [CDS] 25-Jul-2012
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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