Globular clusters in NGC147, 185, and 205

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Journal titleTriggered Star Formation in a Turbulent ISM
Series titleProceedings of the International Astronomical Union; Volume 2
Pages473473; # of pages: 1
Subjectgalaxies: star clusters; galaxies: individual
AbstractStudying the chemical compositions and color-magnitude diagrams of globular clusters in the nearby low-mass galaxies is critical to compare properties of these long-living objects situated in galaxies of different type and mass, and to establish the role of dwarf galaxies as building blocks of massive early-type and spiral galaxies. We present measurements of ages, metallicities and [α/Fe] ratios for 16 globular clusters (GC) in NGC147, NGC185, and NGC205 and for the central regions of the diffuse galaxy light in NGC185, and NGC205, based on measurements of absorption line indices as defined by the Lick standard system in spectra obtained with the SCORPIO multi-slit spectrograph at the 6-m telescope of the Russian Academy of Sciences. We include in our analysis high-quality HST/WFPC2 photometry of individual stars in the GGs to investigate the influence of their horizontal branch (HB) morphology on the spectroscopic analysis. The HB morphologies for our sample GCs follow the same behavior with metallicity as younger halo Galactic globular clusters. We show that it is unlikely that they bias our spectroscopic age estimates based on Balmer absorption-line indices. Almost all our sample GCs appear to be old (T > 8 Gyr) and metal-poor ([Z/H]<−1.1). We find that most of the GCs in the studied galaxies are weakly or not α-enhanced, in contrast to the population of GCs in nearby early-type galaxies, and to the halo population of GCs in M31 and Milky Way.
Publication date
PublisherInternational Astronomical Union
AffiliationNRC Herzberg Institute of Astrophysics; National Research Council Canada
Peer reviewedYes
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This is a non-NRC publication

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NPARC number13053907
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Record identifier80854db1-71ed-4167-9906-5969350007d9
Record created2009-11-25
Record modified2017-06-02
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