2018A&A...617A.119L


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST18:15:55

2018A&A...617A.119L - Astronomy and Astrophysics, volume 617A, 119-119 (2018/9-1)

Modelling of integrated-light spectra from the optical to the near-infrared: the globular cluster G280 in M31.

LARSEN S.S., PUGLIESE G. and BRODIE J.P.

Abstract (from CDS):


Context. In previous papers, we introduced our method for measuring chemical abundances from integrated-light spectra of globular clusters and applied it to a variety of extragalactic star clusters. Our work so far, however, has concentrated primarily on the optical range 4200Å-6200Å.
Aims. Here we extend our analysis technique to the infrared and test it on an H-band spectrum of the massive globular cluster G280 in M 31.
Methods. We simultaneously analyse an optical spectrum of G280, obtained with the HIRES spectrograph on the Keck I telescope, and an H-band spectrum obtained with NIRSPEC on Keck II. We discuss the sensitivity of our results to various modifications of the input assumptions, such as different line lists and isochrones and the possible presence of a metallicity spread in G280.
Results. When using the most recent version of the Kurucz line list, we measure iron abundances of [Fe/H]=-0.68±0.02 from the optical spectrum and [Fe/H]=-0.60±0.07 from the infrared spectrum. These values agree well with previous spectroscopic determinations of the metallicity of G280. While the small difference between the optical and infrared measurements is insignificant given the uncertainties, it is also consistent with a metallicity spread similar to that observed in massive GCs such as ω Cen and G1, and also hinted at by the colour-magnitude diagram of G280. The optical and infrared spectra both indicate an α-enhancement of about 0.3-0.4dex relative to solar-scaled abundances, as typically also observed in Milky Way GCs.
Conclusions. From this analysis, it appears that our integrated-light analysis technique also performs well in the H-band. However, complications due to the presence of molecular bands and telluric contamination are more severe in the infrared, and accurate modelling of the coolest giants is more critical.

Abstract Copyright: © ESO 2018

Journal keyword(s): galaxies: star clusters: individual: G280 - galaxies: star clusters: general - galaxies: individual: M31 - galaxies: abundances - techniques: spectroscopic

Simbad objects: 10

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Number of rows : 10

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NGC 104 GlC 00 24 05.359 -72 04 53.20   5.78 4.09     ~ 3548 0
2 NAME Mayall II GlC 00 32 46.53 +39 34 40.5   14.564 13.807 13.208 12.684 ~ 370 1
3 M 31 G 00 42 44.330 +41 16 07.50 4.86 4.36 3.44     ~ 10905 1
4 2E 166 GlC 00 44 29.5614604627 +41 21 35.695495111 15.50 15.000 14.220 13.679 13.02 ~ 124 0
5 NAME Fornax Dwarf Spheroidal G 02 39 59.3 -34 26 57   9.02 7.4     ~ 1473 1
6 * o Per * 03 42 22.6455526 +33 57 54.089323 4.13 4.912 4.972     B0.5V 280 0
7 NGC 1705 SBG 04 54 13.500 -53 21 39.82 12.32 12.96 12.56 12.58 12.9 ~ 596 1
8 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14832 1
9 NGC 5927 GlC 15 28 00.69 -50 40 22.9   10.13 8.86     ~ 404 0
10 NGC 6388 GlC 17 36 17.461 -44 44 08.34   7.40       ~ 805 1

    Equat.    Gal    SGal    Ecl

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2020.07.14-18:15:55

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