2009MNRAS.400.2135F


C.D.S. - SIMBAD4 rel 1.7 - 2020.12.02CET14:42:57

2009MNRAS.400.2135F - Mon. Not. R. Astron. Soc., 400, 2135-2146 (2009/December-3)

Metallicity gradients at large galactocentric radii using the near-infrared calcium triplet.

FOSTER C., PROCTOR R.N., FORBES D.A., SPOLAOR M., HOPKINS P.F. and BRODIE J.P.

Abstract (from CDS):

We describe a new spectroscopic technique for measuring radial metallicity gradients out to large galactocentric radii. We use the DEep Imaging Multi-Object Spectrograph (DEIMOS) on the Keck telescope and the galaxy spectrum extraction technique of Proctor et al. We also make use of the metallicity sensitive near-infrared Calciumii triplet (CaT) features together with single stellar population models to obtain metallicities. Our technique is applied as a pilot study to a sample of three relatively nearby (≤30 Mpc) intermediate-mass to massive early-type galaxies.
Result. are compared with previous literature inner region values and generally show good agreement. We also include a comparison with profiles from dissipational disc-disc major merger simulations. Based on our new extended metallicity gradients combined with other observational evidence and theoretical predictions, we discuss possible formation scenarios for the galaxies in our sample. The limitations of our new technique are also discussed.

Abstract Copyright: © 2009 The Authors. Journal compilation © 2009 RAS

Journal keyword(s): techniques: spectroscopic - Galaxies: abundances - galaxies: haloes - galaxies: individual (NGC 1407, NGC 2768, NGC 4494)

Simbad objects: 4

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Number of rows : 4

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NGC 1407 GiG 03 40 11.904 -18 34 49.36   10.64 9.67 9.13   ~ 532 1
2 NGC 2768 SyG 09 11 37.504 +60 02 13.95 11.30 10.84 9.87     ~ 469 2
3 NAME Coma I Group GrG 12 22 19.4 +29 53 47           ~ 100 0
4 NGC 4494 GiP 12 31 24.034 +25 46 29.93   10.55 9.74     ~ 452 0

    Equat.    Gal    SGal    Ecl

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2020.12.02-14:42:57

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