Kinematics , ages , and metallicities of star clusters in NGC 1316 : A 3 Gyr old merger remnant †

  title={Kinematics , ages , and metallicities of star clusters in NGC 1316 : A 3 Gyr old merger remnant †},
  author={Paul Goudfrooij and Jennifer Mack and Markus Kissler – Patig and Georges Meylan and Dante Minniti},
We report on multi-object spectroscopy in the red spectral region of 37 candidate star clusters in an ,8 8 arcmin field centred on the giant early-type radio galaxy NGC 1316 (Fornax A), the brightest galaxy in the Fornax cluster. Out of this sample, 24 targets are found to be genuine star clusters associated with NGC 1316, and 13 targets are Galactic foreground stars. For the star cluster sample, we measure a mean heliocentric velocity vhel ˆ 1698 ^ 46 km s and a velocity dispersion s ˆ 227… CONTINUE READING


Publications citing this paper.
Showing 1-3 of 3 extracted citations


Publications referenced by this paper.
Showing 1-10 of 14 references

Globular Cluster Systems

C W.Allen
Astrophysical Quantities. Athlone, London Arnaboldi M. et al., • 1973
View 5 Excerpts
Highly Influenced

age-sensitive) and the Ca ii triplet, the equivalent width (hereafter EW) of which is controlled by the stellar metallicity for stellar populations older than 1 Gyr (Bica

Ha being
Alloin • 1987
View 7 Excerpts
Highly Influenced

1999), all of which have cluster ages of order 300±500 Myr: The fate of these massive clusters has been an issue of some debate. From spectroscopy of luminous clusters in NGC

View 2 Excerpts
Highly Influenced

During that time, one would expect the X-ray luminosity to grow as the remaining atomic and molecular gas contents are shockheated or evaporated by electrons within the already existing hot plasma

Gyr Dupraz
View 2 Excerpts
Highly Influenced

studied the star cluster system of NGC

View 2 Excerpts

The line strengths were measured as described in Goudfrooij

Emsellem • 1998

studied the dynamics in the outer regions

View 1 Excerpt

the molecular gas is found to be already depleted in the central region, being concentrated in the dusty regions at , 30±50 arcsec from the centre instead (Sage

e.g, Knapp
Rupen • 1996

who used the first-generation Planetary Camera aboard HST (V, I imaging), and Goudfrooij et al. (in preparation, hereafter Paper II), who used ground-based

View 2 Excerpts

Interactions at Low & High Redshift

B C.Whitmore, W B.Sparks, R A.Lucas, F D.Macchetto, J A.Biretta

Similar Papers

Loading similar papers…