==========================================================================
J/A+A/474/763 Stellar population gradients in bulges. II. (Jablonka+, 2007)
The following files can be converted to FITS (extension .fit .fgz or .fiZ)
table1.dat
==========================================================================
Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/A+A/474/763
==========================================================================
drwxr-xr-x 16 cats archive 277 Feb 7 2018 [Up]
drwxr-xr-x 2 cats archive 241 Jan 13 2023 [TAR file]
-rw-r--r-- 1 cats archive 471 Dec 19 2022 .message
-r--r--r-- 1 cats archive 8076 Mar 28 2008 ReadMe
-rw-r--r-- 1 cats archive 325 Apr 28 2008 +footg5.gif
-rw-r--r-- 1 cats archive 2569 Apr 28 2008 +footg8.gif
-r--r--r-- 1 cats archive 17280 Dec 1 2007 table1.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe :J/A+A/474/763 Stellar population gradients in bulges. II. (Jablonka+, 2007)
================================================================================
Stellar population gradients in bulges along the Hubble sequence.
II. Relations with galaxy properties.
Jablonka P., Gorgas J., Goudfrooij P.
<Astron. Astrophys., 474, 763-776 (2007)>
=2007A&A...474..763J
================================================================================
ADC_Keywords: Galaxies, nearby ; Abundances
Keywords: galaxies: abundances - galaxies: bulges - galaxies: formation -
galaxies: evolution - galaxies: stellar content - galaxies: spiral
Abstract:
We present the analysis of the radial gradients of stellar absorption
lines in a sample of 32 bulges of edge-on spiral galaxies, spanning
nearly the full Hubble sequence (from S0 to Sc types), and a large
range of velocity dispersion (from about 60 to 300km/s). Different
diagnostics such as index-index, gradient-gradient diagrams, and
simple stellar population models are used to tackle the origin of the
variation of the bulge stellar population. We find that the vast
majority of bulges show older age, lower metallicity and higher
[alpha/Fe] in their outer regions than in their central parts. The
radial gradients in [Fe/H] are 2 to 3 times larger than in Log(age).
The relation between gradient and bulge velocity dispersion is
interpreted as a gradual build up of the gradient mean values and
their dispersions from high to low velocity dispersion, rather than a
pure correlation. The bulge effective radii and the Hubble type of the
parent galaxies seem to play a more minor role in causing the observed
spatial distributions. At a given velocity dispersion, bulges and
ellipticals share common properties.