| Full text | |
| Author(s): Show less - |
Cortesi, Arianna
[1]
;
Chies-Santos, Ana L.
[1, 2, 3]
;
Pota, Vincenzo
[4]
;
Foster, Caroline
[5]
;
Coccato, Lodovico
[6]
;
de Oliveira, Claudia Mendes
[1]
;
Forbes, Duncan A.
[7]
;
Merrifield, Michael M.
[3]
;
Bamford, Steven P.
[3]
;
Romanowsky, Aaron J.
[4, 8]
;
Brodie, Jean P.
[4]
;
Kartha, Sreeja S.
[7]
;
Alabi, Adebusola B.
[7]
;
Proctor, Robert N.
[1]
;
Almeida, Andres
[9]
Total Authors: 15
|
| Affiliation: | [1] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Dept Astron, Cidade Univ, BR-05508900 Sao Paulo, SP - Brazil
[2] Univ Fed Rio Grande do Sul, Inst Fis, Dept Astron, BR-90040060 Porto Alegre, RS - Brazil
[3] Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD - England
[4] Univ Calif Observ, 1156 High St, Santa Cruz, CA 95064 - USA
[5] Australian Astron Observ, POB 915, N Ryde, NSW 1670 - Australia
[6] European So Observ, Karl Schwarzschild Strae 2, D-85748 Garching - Germany
[7] Swinburne Univ Technol, Ctr Astrophys & Supercomp, Hawthorn, Vic 3122 - Australia
[8] San Jose State Univ, Dept Phys & Astron, One Washington Sq, San Jose, CA 95192 - USA
[9] Univ La Serena, Dept Phys & Astron, La Serena 1200 - Chile
Total Affiliations: 9
|
| Document type: | Journal article |
| Source: | Monthly Notices of the Royal Astronomical Society; v. 456, n. 3, p. 2611-2621, MAR 1 2016. |
| Web of Science Citations: | 5 |
| Abstract | |
Globular clusters (GCs) can be considered discrete, long-lived, dynamical tracers that retain crucial information about the assembly history of their parent galaxy. In this paper, we present a new catalogue of GC velocities and colours for the lenticular galaxy NGC 1023, we study their kinematics and spatial distribution, in comparison with the underlying stellar kinematics and surface brightness profile, and we test a new method for studying GC properties. Specifically, we decompose the galaxy light into its spheroid (assumed to represent the bulge+halo components) and disc components and use it to assign to each GC a probability of belonging to one of the two components. Then we model the galaxy kinematics, assuming a disc and spheroidal component, using planetary nebulae and integrated stellar light. We use this kinematic model and the probability previously obtained from the photometry to recalculate for each GC its likelihood of being associated with the disc, the spheroid, or neither. We find that the reddest GCs are likely to be associated with the disc, as found for faint fuzzies in this same galaxy, suggesting that the disc of this S0 galaxy originated at z similar or equal to 2. The majority of blue GCs are found likely to be associated with the spheroidal (hot) component. The method also allows us to identify objects that are unlikely to be in equilibrium with the system. In NGC 1023 some of the rejected GCs form a substructure in phase space that is connected with NGC 1023 companion galaxy. (AU) | |
| FAPESP's process: | 13/04582-4 - Tracing the origin of lenticular galaxies using information from kinematics and stellar populations |
| Grantee: | Arianna Cortesi |
| Support Opportunities: | Scholarships in Brazil - Post-Doctoral |