Please note that eDoc will be permanently shut down in the first quarter of 2021!      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 Astrophysik     Collection: High Energy Astrophysics at MPA     Display Documents



  history
ID: 10467.0, MPI für Astrophysik / High Energy Astrophysics at MPA
The globular cluster system of NGC 1316
Authors:Gomez, M.; Richtler, T.; Infante, L.; Drenkhahn, G.
Language:English
Publisher:Astronomical Society of the Pacific
Place of Publication:San Francsisco, CA (US)
Date of Publication (YYYY-MM-DD):2002
Title of Proceedings:Extragalatic star clusters
Start Page:321
End Page:323
Title of Series:IAU Symposium
Name of Conference/Meeting:Extragalatic star clusters
Place of Conference/Meeting:Pucón, Chile
(Start) Date of Conference/Meeting
 (YYYY-MM-DD):
2001-03-12
End Date of Conference/Meeting 
 (YYYY-MM-DD):
2001-03-16
Review Status:not specified
Audience:Experts Only
Abstract / Description:We have studied the Globular Cluster System of the merger galaxy NGC 1316 in Fornax, using CCD BVI photometry. Dividing the sample into red (presumably metal-rich) and blue (metal- poor) subpopulations at B - I = 1.75, we find that they follow strikingly different angular distributions. The red clusters show a strong correlation with the galaxy elongation, but the blue ones are circularly distributed. An astonishingly low specific frequency for NGC 1316 of only S-N = 0.9+/-0.2 is derived, which confirms with a larger field a previous finding by Grillmair et al. (1999). Assuming a "normal" S-N of similar to 4 for early-type galaxies, we use stellar population synthesis models to estimate the merger age to about 2 Gyr, if an intermediate-age population were to explain the low SN we observe. By fitting t(5) functions to the Globular Cluster Luminosity Function (GCLF), we derive the following turnover magnitudes: M-B(T) = 24.69 +/- 0.15, m(V)(T) = 23.87 +/- 0.20 and M-I(T) = 22.72 +/- 0.14. They support that NGC 1316, in spite of its outlying location, is at the same distance as the core of the Fornax cluster.
External Publication Status:published
Document Type:Conference-Paper
Communicated by:N. N.
Affiliations:MPI für Astrophysik
Identifiers:ISI:000179397100065
ISSN:0074-1809
ISBN:1-58381-115-X
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.