The formation of ultra-compact and ultra-diffuse galaxies in clusters
Diffuse intergalactic magnetic fields and constraints for observations by CTA and ...
Studying the Be star content of the young open cluster NGC 1850
| Full text | |
| Author(s): |
Torres-Flores, S.
[1, 2, 3, 4]
;
Mendes de Oliveira, C.
[2]
;
de Mello, D. F.
[5, 6]
;
Scarano, Jr., S.
[2]
;
Urrutia-Viscarra, F.
[2]
Total Authors: 5
|
| Affiliation: | [1] Univ La Serena, Dept Fis, La Serena - Chile
[2] Univ Sao Paulo, Dept Astron, Inst Astron Geofis & Ciencias Atmosfer, BR-05508090 Sao Paulo - Brazil
[3] Univ Aix Marseille 1, OAMP, Lab Astrophys Marseille, F-13388 Marseille 13 - France
[4] CNRS, F-13388 Marseille 13 - France
[5] Catholic Univ Amer, Washington, DC 20064 - USA
[6] NASA, Goddard Space Flight Ctr, Observat Cosmol Lab, Greenbelt, MD 20771 - USA
Total Affiliations: 6
|
| Document type: | Journal article |
| Source: | Monthly Notices of the Royal Astronomical Society; v. 421, n. 4, p. 3612-3621, APR 2012. |
| Web of Science Citations: | 15 |
| Abstract | |
We have searched for young star-forming regions around the merger remnant NGC 2782. By using Galaxy Evolution Explorer far-ultraviolet and near-ultraviolet imaging and H i data we found seven ultraviolet sources, located at distances greater than 26 kpc from the centre of NGC 2782, and coinciding with its western H i tidal tail. These regions were resolved in several smaller systems when Gemini/Gemini multi-object spectrograph (GMOS) r-band images were used. We compared the observed colours to stellar population synthesis models and found that these objects have ages of similar to 1 to 11 Myr and masses ranging from 103.9 to 104.6 M circle dot. By using Gemini/GMOS spectroscopic data we confirm memberships and derive high metallicities for three of the young regions in the tail (12+log(O/H) = 8.74 +/- 0.20, 8.81 +/- 0.20 and 8.78 +/- 0.20). These metallicities are similar to the value presented by the nuclear region of NGC 2782 and also similar to the value presented for an object located close to the main body of NGC 2782. The high metallicities measured for the star-forming regions in the gaseous tidal tail of NGC 2782 could be explained if they were formed out of highly enriched gas which was once expelled from the centre of the merging galaxies when the system collided. An additional possibility is that the tail has been a nursery of a few generations of young stellar systems which ultimately polluted this medium with metals, further enriching the already pre-enriched gas ejected to the tail when the galaxies collided. (AU) | |
| FAPESP's process: | 09/05181-8 - Determination of the Spatial Orientation of Galaxies Using Spiral Arms and Velocity Fields |
| Grantee: | Sergio Scarano Junior |
| Support Opportunities: | Scholarships in Brazil - Post-Doctoral |
| FAPESP's process: | 06/56213-9 - New physics from space: formation and evolution of structures in the universe |
| Grantee: | Claudia Lucia Mendes de Oliveira |
| Support Opportunities: | Research Projects - Thematic Grants |
| FAPESP's process: | 07/07973-3 - The internal kinematics of galaxies in Hickson compact groups |
| Grantee: | Sergio Patricio Torres Flores |
| Support Opportunities: | Scholarships in Brazil - Doctorate (Direct) |
| FAPESP's process: | 07/06436-4 - Mapping of extragalactic star forming regions in interacting systems |
| Grantee: | Paula Maria Fernanda Urrutia Viscarra |
| Support Opportunities: | Scholarships in Brazil - Master |