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J/ApJ/704/385        M31 integrated light abundances            (Colucci+, 2009)

M31 globular cluster abundances from high-resolution, integrated-light spectroscopy. Colucci J.E., Bernstein R.A., Cameron S., McWilliam A., Cohen J.G. <Astrophys. J., 704, 385-414 (2009)> =2009ApJ...704..385C
ADC_Keywords: Abundances ; Clusters, globular ; Equivalent widths ; Spectroscopy Keywords: galaxies: abundances - galaxies: individual (M31) - galaxies: star clusters - globular clusters: general Abstract: We report the first detailed chemical abundances for five globular clusters (GCs) in M31 from high-resolution (R∼25000) spectroscopy of their integrated light (IL). These GCs are the first in a larger set of clusters observed as part of an ongoing project to study the formation history of M31 and its GC population. The data presented here were obtained with the HIRES echelle spectrograph on the Keck I telescope and are analyzed using a new IL spectra analysis method that we have developed. In these clusters, we measure abundances for Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Fe, Co, Ni, Y, and Ba, ages ≥10Gyr, and a range in [Fe/H] of -0.9 to -2.2. As is typical of Milky Way GCs, we find these M31 GCs to be enhanced in the α-elements Ca, Si, and Ti relative to Fe. Description: For this work, we obtained high-resolution IL (integrated light) spectra of the M31 GCs using the HIRES spectrograph on the Keck I telescope over the dates 2006 September 10-14. We used the D3 decker, which provides a slit size of 1.7"x7.0" and spectral resolution of R=24000. The wavelength coverage of the HIRES spectra is approximately 3800-8300Å. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 83 5 M31 spectroscopically confirmed clusters ew.dat 38 1095 Line parameters and integrated light equivalent widths for M31 GCs (table 4 of the paper)
See also: J/MNRAS/402/803 : M31 globular cluster system (Peacock+, 2010) J/A+A/508/1285 : Metallicity estimates of M31 globular clusters (Galleti+, 2009) J/A+A/471/127 : New globular clusters in M31 (Galleti+, 2007) J/AJ/133/2764 : M31 globular clusters structural parameters (Barmby+, 2007) J/A+A/416/917 : Revised Bologna Catalog of M31 globular clusters (Galleti+, 2004) J/AJ/123/2490 : RV and [Fe/H] of M31 globular cluster system (Perrett+, 2002) J/AJ/122/2458 : M31 globular clusters from HST (Barmby+, 2001) J/AJ/119/727 : M31 globular clusters photometry (Barmby+, 2000) J/AcA/48/455 : Globular Clusters in M31 and M33 (Mochejska+, 1998) J/AJ/114/1488 : Globulars in M31 (Holland+ 1997) J/A+AS/116/447 : M31 globulars clusters ellipticities (Staneva+, 1996) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 9 A9 --- Cl Cluster identification (GNNN-BNNN) from Barmby et al. (2000, Cat. J/AJ/119/727, <[BHB2000] NNN-NNN> in Simbad; with B part before G) 11- 12 I2 h RAh Hour of right ascension (J2000) 14- 15 I2 min RAm Minute of right ascension (J2000) 17- 21 F5.2 s RAs Second of right ascension (J2000) 23 A1 --- DE- Sign of declination (J2000) 24- 25 I2 deg DEd Degree of declination (J2000) 27- 28 I2 arcmin DEm Arcminute of declination (J2000) 30- 33 F4.1 arcsec DEs Arcsecond of declination (J2000) 35- 39 F5.2 mag Vmag V-band magnitude 41- 44 F4.2 --- E(B-V) B-V color excess from Rich et al. (2005AJ....129.2670R ) 45 A1 --- r_E(B-V) [g] g: from Fan et al. (2008MNRAS.385.1973F) 47- 51 F5.2 mag VMtot V0, dereddened total absolute magnitude (1) 53- 57 F5.2 kpc Rgc Galactocentric radius from Perrett et al. (2002, Cat. J/AJ/123/2490) 59- 63 F5.2 [-] [Fe/H] Low-resolution spectroscopic metallicities of Huchra et al. (1991ApJ...370..495H) 65- 68 F4.2 [-] e_[Fe/H] Uncertainty in [Fe/H] 70- 73 F4.2 [-] [a/Fe] ? Low-resolution [α/Fe] of Puzia et al. 2005A&A...434..909P 75- 78 F4.2 [-] e_[a/Fe] ? Uncertainty in [a/Fe] 80- 83 F4.2 --- HBR ? Horizontal branch morphology ratios (HBRs) (2)
Note (1): Reddening corrected and using a distance modulus for M31 of (m-M)=24.47 (Holland 1998AJ....115.1916H) Note (2): HBRs defined as the "Mironov index"=B/B+R, where B and R correspond to the number of horizontal branch stars bluer or redder than V-I=0.5 in the observed CMD of Rich et al. (2005AJ....129.2670R)
Byte-by-byte Description of file: ew.dat
Bytes Format Units Label Explanations
1- 4 A4 --- Cl Cluster identification (GNNN) 6- 10 A5 --- Ion Species identification (1) 12- 19 F8.3 0.1nm lambda Wavelength in Angstroms λ 21- 25 F5.3 eV ExPot Excitation potential 27- 32 F6.3 [-] log(gf) Log of the oscillator strength 34- 38 F5.1 10-13m EW ? Equivalent width (in mÅ)
Note (1): Lines listed twice correspond to those measured in adjacent orders with overlapping wavelength coverage.
History: From electronic version of the journal References: McWilliam & Bernstein. Paper I. 2008ApJ...684..326M Colucci et al. Paper III. 2011ApJ...735...55C Cat. J/ApJ/735/55 Colucci et al. Paper IV. 2012ApJ...746...29C
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 04-Nov-2011
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