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



  history
ID: 421467.0, MPI für Astronomie / Publikationen_mpia
Building up mass in the centers of late type galaxies
Authors:Schinnerer, E.; Böker, T.; Emsellem, E.; Lisenfeld, U.; Downes, D.
Language:English
Publisher:Cambridge Univ. Press
Place of Publication:Cambridge
Date of Publication (YYYY-MM-DD):2008
Title of Proceedings:Formation and Evolution of Galaxy Bulges
Start Page:169
End Page:172
Title of Series:IAU Symposium
Volume (in Series):245
Name of Conference/Meeting:IAU Symposium
Review Status:not specified
Audience:Experts Only
Abstract / Description:We present highest angular resolution (~ 1" and 0.35") mm-interferometric observations of the HCN(1-0), 12CO(1-0) and 12CO(2-1) line emission in the central 300 pc of the late-type spiral galaxy NGC 6946. The data, obtained with the IRAM Plateau de Bure Interferometer (PdBI) shows for the first time a molecular gas spiral in the inner ~ 10" (270 pc) with a large concentration of molecular gas (MH_2 Ëœ 1.6×10^7 Mo) within the inner 60 pc, The gas distribution in the central 50 pc has been resolved and is consistent with a gas ring or spiral driven by a bar. Both the distribution of the molecular gas as well as its kinematics can be well explained by the influence of an inner stellar bar of about 400 pc length as tested via a qualitative model for the gas flow. NGC 6946 is a prime example of molecular gas kinematics being driven by a small-scale, secondary stellar bar. For the first time, it is possible to directly compare the location of (dense) giant molecular clouds with that of (optically) visible HII regions in space-based images. We use the 3 mm continuum and the HCN emission to estimate in the central 50 pc the star formation rates in young clusters that are still embedded in their parent clouds and hence are missed in optical and near-IR surveys of star formation. The amount of embedded star formation is about 1.6 times as high as that measured from HII regions alone, and appears roughly evenly split between ongoing dust-obscured star formation and very young giant molecular cloud cores that are just beginning to form stars. The build-up of central mass seems to have continued over the past >= 10 Myrs, to have occurred in an extended (albeit small) volume around the nucleus, and to be closely related to the presence of an inner bar.
Free Keywords:galaxies: ISM; galaxies: kinematics and dynamics; galaxies: nuclei; galaxies: individual (NGC 6946)
Comment of the Author/Creator:Date: 2008, n/a 1, 2008
External Publication Status:published
Document Type:Conference-Paper
Communicated by:N. N.
Affiliations:MPI für Astronomie
Identifiers:URL:http://adsabs.harvard.edu/abs/2008IAUS..245..169S [ID No:1]
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.