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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. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 539 32 For each of our sample galaxy, the 33 measured gradients and their attached errors are presented
See also: J/A+A/474/1081 : Stellar population gradients in bulges. I (Gorgas+, 2007) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 11 A11 --- Name Galaxy name 13- 19 F7.4 --- Hdelta'A ?=99 Measured radial gradient of Hdelta'_A_ (1) 21- 27 F7.4 --- Hdelta'F ?=99 Measured radial gradient of Hdelta'_F_ (1) 29- 35 F7.4 --- CN1 ?=99 Measured radial gradient of CN1 (1) 37- 43 F7.4 --- CN2 ?=99 Measured radial gradient of CN2 (1) 45- 51 F7.4 --- Ca4227' ?=99 Measured radial gradient of Ca4227' (1) 53- 59 F7.4 --- G-band ?=99 Measured radial gradient of G-band (1) 61- 67 F7.4 --- Hgamma'A ?=99 Measured radial gradient of Hgamma'_A_ (1) 69- 75 F7.4 --- Hgamma'F ?=99 Measured radial gradient of Hgamma'_F_ (1) 77- 83 F7.4 --- Fe4383' ?=99 Measured radial gradient of Fe4383' (1) 85- 91 F7.4 --- Ca4455' ?=99 Measured radial gradient of Ca4455' (1) 93- 99 F7.4 --- Fe4531' ?=99 Measured radial gradient of Fe4531' (1) 101-107 F7.4 --- e_Hdelta'A ?=99 rms uncertainty on Hdelta'A 109-115 F7.4 --- e_Hdelta'F ?=99 rms uncertainty on Hdelta'F 117-123 F7.4 --- e_CN1 ?=99 rms uncertainty on CN1 125-131 F7.4 --- e_CN2 ?=99 rms uncertainty on CN2 133-139 F7.4 --- e_Ca4227' ?=99 rms uncertainty on Ca4227' 141-147 F7.4 --- e_G-band ?=99 rms uncertainty on G-band 149-155 F7.4 --- e_Hgamma'A ?=99 rms uncertainty on Hgamma'A 157-163 F7.4 --- e_Hgamma'F ?=99 rms uncertainty on Hgamma'F 165-171 F7.4 --- e_Fe4383' ?=99 rms uncertainty on Fe4383' 173-179 F7.4 --- e_Ca4455' ?=99 rms uncertainty on Ca4455' 181-187 F7.4 --- e_Fe4531' ?=99 rms uncertainty on Fe4531' 189-195 F7.4 --- C4668' ?=99 Measured radial gradient of C4668' (1) 197-203 F7.4 --- Hbeta' ?=99 Measured radial gradient of Hbeta' (1) 205-211 F7.4 --- Fe5015' ?=99 Measured radial gradient of Fe5015' (1) 213-219 F7.4 --- Mg1 ?=99 Measured radial gradient of Mg1 (1) 221-227 F7.4 --- Mg2 ?=99 Measured radial gradient of Mg2 (1) 229-235 F7.4 --- Mgb ?=99 Measured radial gradient of Mgb (1) 237-243 F7.4 --- Fe5270' ?=99 Measured radial gradient of Fe5270' (1) 245-251 F7.4 --- Fe5335' ?=99 Measured radial gradient of Fe5335' (1) 253-259 F7.4 --- Fe5406' ?=99 Measured radial gradient of Fe5406' (1) 261-267 F7.4 --- Fe5709' ?=99 Measured radial gradient of Fe5709' (1) 269-275 F7.4 --- Fe5782' ?=99 Measured radial gradient of Fe5782' (1) 277-283 F7.4 --- e_C4668' ?=99 rms uncertainty on C4668' 285-291 F7.4 --- e_Hbeta' ?=99 rms uncertainty on Hbeta' 293-299 F7.4 --- e_Fe5015' ?=99 rms uncertainty on Fe5015' 301-307 F7.4 --- e_Mg1 ?=99 rms uncertainty on Mg1 309-315 F7.4 --- e_Mg2 ?=99 rms uncertainty on Mg2 317-323 F7.4 --- e_Mgb ?=99 rms uncertainty on Mgb 325-331 F7.4 --- e_Fe5270' ?=99 rms uncertainty on Fe5270' 333-339 F7.4 --- e_Fe5335' ?=99 rms uncertainty on Fe5335' 341-347 F7.4 --- e_Fe5406' ?=99 rms uncertainty on Fe5406' 349-355 F7.4 --- e_Fe5709' ?=99 rms uncertainty on Fe5709' 357-363 F7.4 --- e_Fe5782' ?=99 rms uncertainty on Fe5782' 365-371 F7.4 --- Na5895' ?=99 Measured radial gradient of Na5895' (1) 373-379 F7.4 --- TiO1 ?=99 Measured radial gradient of TiO1 (1) 381-387 F7.4 --- TiO2 ?=99 Measured radial gradient of TiO2 (1) 389-395 F7.4 --- <Fe>' ?=99 Measured radial gradient of <Fe>' (1) 397-403 F7.4 --- Fe3' ?=99 Measured radial gradient of Fe3' (1) 405-411 F7.4 --- Fe4' ?=99 Measured radial gradient of Fe4' (1) 413-419 F7.4 --- Fe5' ?=99 Measured radial gradient of Fe5' (1) 421-427 F7.4 --- Fe6' ?=99 Measured radial gradient of Fe6' (1) 429-435 F7.4 --- HA' ?=99 Measured radial gradient of H_A_' (1) 437-443 F7.4 --- HF' ?=99 Measured radial gradient of H_F_' (1) 445-451 F7.4 --- Balmer ?=99 Measured radial gradient of Balmer (1) 453-459 F7.4 --- e_Na5895' ?=99 rms uncertainty on Na5895' 461-467 F7.4 --- e_TiO1 ?=99 rms uncertainty on TiO1 469-475 F7.4 --- e_TiO2 ?=99 rms uncertainty on TiO2 477-483 F7.4 --- e_<Fe>' ?=99 rms uncertainty on <Fe>' 485-491 F7.4 --- e_Fe3' ?=99 rms uncertainty on Fe3' 493-499 F7.4 --- e_Fe4' ?=99 rms uncertainty on Fe4' 501-507 F7.4 --- e_Fe5' ?=99 rms uncertainty on Fe5' 509-515 F7.4 --- e_Fe6' ?=99 rms uncertainty on Fe6' 517-523 F7.4 --- e_HA' ?=99 rms uncertainty on HA' 525-531 F7.4 --- e_HF' ?=99 rms uncertainty on HF' 533-539 F7.4 --- e_Balmer ?=99 rms uncertainty on Balmer
Note (1): the gradient is the coefficient A in the relation I' = A log(r/reff) + B where is the r is the distance from the bulge center, and reff the bulge effective radius, I' being the line strength expressed in magnitudes (see paper)
History: From electronic version of the journal References: Gorgas et al., Paper I 2007A&A...474.1081G
(End) Patricia Vannier [CDS] 30-Nov-2007
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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