Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents



ID: 709872.0, MPI für Astronomie / Publikationen_mpia
The Panchromatic Hubble Andromeda Treasury. V. Ages and masses of the year 1 stellar clusters
Authors:Fouesneau, M.; Johnson, L. C.; Weisz, D. R.; Dalcanton, J. J.; Bell, E. F.; Bianchi, L.; Caldwell, N.; Gouliermis, D. A.; Guhathakurta, P.; Kalirai, J.; Larsen, S. S.; Rix, H.-W.; Seth, A. C.; Skillman, E. D.; Williams, B. F.
Date of Publication (YYYY-MM-DD):2014
Title of Journal:The Astrophysical Journal
Volume:786
Start Page:id. 117 (17 pp)
Audience:Not Specified
Abstract / Description:We present ages and masses for 601 star clusters in M31 from the analysis of the six filter integrated light measurements from near-ultraviolet to near-infrared wavelengths, made as part of the Panchromatic Hubble Andromeda Treasury (PHAT). We derive the ages and masses using a probabilistic technique, which accounts for the effects of stochastic sampling of the stellar initial mass function. Tests on synthetic data show that this method, in conjunction with the exquisite sensitivity of the PHAT observations and their broad wavelength baseline, provides robust age and mass recovery for clusters ranging from ~102 to 2 × 106 M &sun;. We find that the cluster age distribution is consistent with being uniform over the past 100 Myr, which suggests a weak effect of cluster disruption within M31. The age distribution of older (>100 Myr) clusters falls toward old ages, consistent with a power-law decline of index -1, likely from a combination of fading and disruption of the clusters. We find that the mass distribution of the whole sample can be well described by a single power law with a spectral index of -1.9 ± 0.1 over the range of 103-3 × 105 M &sun;. However, if we subdivide the sample by galactocentric radius, we find that the age distributions remain unchanged. However, the mass spectral index varies significantly, showing best-fit values between -2.2 and -1.8, with the shallower slope in the highest star formation intensity regions. We explore the robustness of our study to potential systematics and conclude that the cluster mass function may vary with respect to environment. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555.
Free Keywords:galaxies: individual: M31; galaxies: star clusters: general; methods: data analysis; techniques: photometric
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:ISSN:0004-637X
URL:http://cdsads.u-strasbg.fr/abs/2014ApJ...786..117F
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.