NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-08-22 T19:14:06 PDT
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For refcode 2002A&A...391..453P:
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Copyright by European Southern Observatory (ESO). Reproduced by permission
2002A&A...391..453P Extragalactic globular clusters in the near-infrared II. The globular clusters systems of NGC 3115 and NGC 4365 T. H. Puzia, S. E. Zepf, M. Kissler-Patig, M. Hilker, D. Minniti and P. Goudfrooij Sternwarte der Ludwig-Maximilians-Universitat, Scheinerstr. 1, 81679 Munchen, Germany; e-mail: puzia@usm.uni-muenchen.de Department of Astronomy, Yale University, PO Box 208101, New Haven, CT 06520-8101, USA Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824, USA; e-mail: zepf@pa.msu.edu European Southern Observatory, 85749 Garching bei Munchen, Germany e-mail: mkissler@eso.org Sternwarte der Universitat Bonn, Auf dem Hugel 71, 53121 Bonn, Germany e-mail: mhilker@astro.uni-bonn.de Departamento de Astronomia y Astrofisica, P. Universidad Catolica, Casilla 104, Santiago 22, Chile; e-mail: dante@astro.puc.cl Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA; e-mail: goudfroo@stsci.edu Received 18 February 2002/Accepted 15 May 2002 Abstract. We combine near-infrared photometry obtained with the VLT/ISAAC instrument and archival HST/WFPC2 optical images to determine VIK magnitudes and colours of globular clusters in two early-type galaxies, NGC 3115 and NGC 4365. The combination of near-IR and optical photometry provides a way to lift the age-metallicity degeneracy. For NGC 3115, the globular cluster colours reveal two major sub-populations, consistent with previous studies. By comparing the V-I, V-K colours of the NGC 3115 globular clusters with stellar populations models, we find that the colour difference between the two >~10 Gyr old major sub-populations is primarily due to a difference in metallicity. We find {DELTA}[ Fe/H ] = 1.0 +/- 0.3 dex and the blue (metal-poor) and red (metal-rich) globular cluster sub-populations being coeval within 3 Gyr. In contrast to the NGC 3115 globular clusters, the globular cluster system in NGC 4365 exhibits a more complex age and metallicity structure. We find a significant population of intermediate-age very metal-rich globular clusters along with an old population of both metal-rich and metal-poor clusters. Specifically, we observe a large population of globular clusters with red V-K colours but intermediate V-I colours, for which all current stellar population models give ages and metallicities in the range ~2-8 Gyr and ~0.5 Z_sun_-3 Z_sun_, respectively. After 10 Gyr of passive evolution, the intermediate-age globular clusters in NGC 4365 will have colours which are consistent with the very metal-rich population of globular clusters in giant elliptical galaxies, such as M 87. Our results for both globular cluster systems are consistent with previous age and metallicity studies of the diffuse galactic light. In addition to the major globular cluster populations in NGC 3115 and NGC 4365 we report on the detection of objects with extremely red colours (V-K >~ 3.8 mag), whose nature could not ultimately be revealed with the present data. Key words: galaxies: formation - galaxies: star clusters - galaxies: individual: NGC 3115, NGC 4365
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