Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Quick Search
My eDoc
Session History
Support Wiki
Direct access to
document ID:

          Institute: MPI für Astronomie     Collection: Publikationen_mpia     Display Documents

ID: 607589.0, MPI für Astronomie / Publikationen_mpia
The evolution of stellar structures in dwarf galaxies
Authors:Bastian, N.; Weisz, D. R.; Skillman, E. D.; McQuinn, K. B. W.; Dolphin, A. E.; Gutermuth, R. A.; Cannon, J. M.; Ercolano, B.; Gieles, M.; Kennicutt, R. C.; Walter, F.
Date of Publication (YYYY-MM-DD):2011
Journal Abbrev.:Monthly Notices of the Royal Astronomical Society
Issue / Number:3
Start Page:1539
End Page:1551
Audience:Not Specified
Abstract / Description:We present a study of the variation of spatial structure of stellar populations within dwarf galaxies as a function of the population age. We use deep Hubble Space Telescope/Advanced Camera for Surveys imaging of nearby dwarf galaxies in order to resolve individual stars and create composite colour-magnitude diagrams (CMDs) for each galaxy. Using the obtained CMDs, we select blue helium burning stars, which can be unambiguously age-dated by comparing the absolute magnitude of individual stars with stellar isochrones. Additionally, we select a very young (≲10 Myr) population of OB stars for a subset of the galaxies based on the tip of the young main sequence. By selecting stars in different age ranges, we can then study how the spatial distribution of these stars evolves with time. We find, in agreement with previous studies, that stars are born within galaxies with a high degree of substructure which is made up of a continuous distribution of clusters, groups and associations from parsec to hundreds of parsec scales. These structures disperse on time-scales of tens to hundreds of Myr, which we quantify using the two-point correlation function and the Q-parameter developed by Cartwright & Whitworth. On galactic scales, we can place lower limits on the time it takes to remove the original structure (i.e. structure survives for at least this long), tevo, which varies between Ëœ100 Myr (NGC 2366) and Ëœ350 Myr (DDO 165). This is similar to what we have found previously for the Small Magellanic Cloud (Ëœ80 Myr) and the Large Magellanic Cloud (Ëœ175 Myr). We do not find any strong correlations between tevo and the luminosity of the host galaxy.
Free Keywords:galaxies: dwarf; galaxies: individual: DDO 165; galaxies: individual: Holmberg II; galaxies: individual: IC 2574; galaxies: individual: NGC 784; galaxies: individual: NGC 2366
External Publication Status:published
Document Type:Article
Communicated by:N. N.
Affiliations:MPI für Astronomie
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.