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J/A+A/445/79    Nearby early-type gal. with ionized gas. II.   (Annibali+, 2006)

Nearby early-type galaxies with ionized gas. II. Line-strength indices for 18 additional galaxies. Annibali F., Bressan A., Rampazzo R., Zeilinger W.W. <Astron. Astrophys., 445, 79-91 (2006)> =2006A&A...445...79A
ADC_Keywords: Galaxies, nearby ; Galaxies, spectra ; Equivalent widths Keywords: galaxies: elliptical and lenticular, cD - galaxies: fundamental parameters - galaxies: formation - galaxies: evolution Abstract: Rampazzo et al., 2005, Cat. J/A+A/433/497 (Paper I) presented a data-set of line-strength indices for 50 early-type galaxies in the nearby Universe. The galaxy sample is biased toward galaxies showing emission lines, located in environments corresponding to a broad range of local galaxy densities, although predominantly in low density environments. The present addendum enlarges the above data-set of line-strength indices by analyzing 18 additional early-type galaxies (three galaxies, NGC 3607, NGC 5077 and NGC 5898 were presented in the previous set). We measured 25 line-strength indices, defined by the Lick IDS "standard" system (Trager et al., 1998, Cat. J/ApJS/116/1; Worthey & Ottaviani, 1997, Cat. J/ApJS/111/377), for 7 luminosity weighted apertures and 4 gradients of each galaxy. This addendum presents the line-strength data-set and compares it with the available data in the literature. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 88 18 Overview of the observed sample table5.dat 31 119 Hβ corrections for apertures table6.dat 31 65 Hβ corrections for gradients table8.dat 361 454 *Aperture fully corrected line-strength indices table9.dat 361 257 *Gradients fully corrected line-strength indices
Note on table8.dat and table9.dat: these tables provide the final line-strength indices of the gradients and apertures for the whole sample of 65 galaxies (Papers I + II). In these tables the Hβ index has been corrected for emission using the Hα line.
See also: J/A+A/433/497 : Nearby early-type galaxies with ionized gas I (Rampazzo+ 2005) J/A+A/463/455 : Nearby early-type gal. with ionized gas III (Annibali+ 2007) J/A+A/519/A40 : Nearby early-type gal. with ionized gas. IV (Annibali+, 2010) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Galaxy Galaxy name 9- 10 I2 h RAh Right ascension (J2000) 12- 13 I2 min RAm Right ascension (J2000) 15- 18 F4.1 s RAs Right ascension (J2000) 20 A1 --- DE- Declination sign (J2000) 21- 22 I2 deg DEd Declination (J2000) 24- 25 I2 arcmin DEm Declination (J2000) 27- 28 I2 arcsec DEs Declination (J2000) 30- 40 A11 --- MType1 Spectral type from RSA (Sandage & Tamman, 1987, Cat. VII/51) 42- 48 A7 --- MType2 Spectral type from RC3 (de Vaucouleurs, Cat. VII/155) 50- 52 I3 deg PA Position angle of the isophotes along the major axis 54- 58 F5.2 mag B0mag Total corrected B magnitude (from RC3) 60- 63 F4.2 mag (B-V)0 ? Total corrected B-V colour index (from RC3) 65- 68 F4.2 mag (U-B)0 ? Total corrected U-B colour index (from RC3) 70- 73 I4 km/s HV Heliocentric systemic velocity (2) 75- 78 F4.1 arcsec re Effective radius (1) 80- 83 F4.2 Mpc-3 rhoxyz ? Measure of the richness of the environment, in galaxies/Mpc3 85- 88 F4.2 --- eps Average ellipticity of the galaxy (2)
Note (1): The value of re of NGC 4696, NGC 5090 and NGC 5266 have been derived from ESO-LV (Lauberts & Valentijn, 1989, Cat. VII/115) while the value for NGC 5044 is derived from Goudfrooij (1994, Cat. J/A+AS/104/179) Note (2): From HYPERCAT: http://www-obs.univ-lyon1.fr/hypercat
Byte-by-byte Description of file: table5.dat table6.dat
Bytes Format Units Label Explanations
1- 7 A7 --- Galaxy Galaxy designation 9 I1 --- iz [0/6] Indicates the aperture (table5) or the gradient (table6) code (G2) 12- 18 F7.3 0.1nm EWHb1 Equivalent width of Hβ as derived from [OIII] 23 I1 --- Qual Quality of the measure (G1) 25- 31 F7.3 0.1nm EWHb2 Equivalent width of Hβ as derived from Hα
Byte-by-byte Description of file: table8.dat table9.dat
Bytes Format Units Label Explanations
1- 7 A7 -- Galaxy Galaxy designation 9 I1 -- iz [0/6] Indicates the aperture (table8) or the gradient (table9) code (G2) 11- 15 F5.3 --- r1 Relative aperture radius (lower limit) 17- 21 F5.3 --- r2 Relative aperture radius (upper limit) 23- 27 F5.3 --- rwl Luminosity weighted radius 29- 32 F4.1 arcsec req Adopted equivalent radius 33- 34 A2 --- --- [00] 36- 41 F6.3 mag CN1 Line-strength index of CN1 43- 48 F6.3 mag CN2 Line-strength index of CN2 50- 55 F6.3 0.1nm Ca4227 Line-strength index of Ca4227 57- 62 F6.3 0.1nm G4300 Line-strength index of G4300 64- 69 F6.3 0.1nm Fe4383 Line-strength index of Fe4383 71- 76 F6.3 0.1nm Ca4455 Line-strength index of Ca4455 78- 83 F6.3 0.1nm Fe4531 Line-strength index of Fe4531 85- 90 F6.3 0.1nm Fe4668 Line-strength index of Fe4668 92- 97 F6.3 0.1nm Hbeta Line-strength index of Hbeta 99-105 F7.3 0.1nm Fe5015 Line-strength index of Fe5015 107-112 F6.3 mag Mg1 Line-strength index of Mg1 114-119 F6.3 mag Mg2 Line-strength index of Mg2 121-126 F6.3 0.1nm Mgb Line-strength index of Mgb 128-133 F6.3 0.1nm Fe5270 Line-strength index of Fe5270 135-140 F6.3 0.1nm Fe5335 Line-strength index of Fe5335 142-147 F6.3 0.1nm Fe5406 Line-strength index of Fe5406 149-154 F6.3 0.1nm Fe5709 Line-strength index of Fe5709 156-161 F6.3 0.1nm Fe5782 Line-strength index of Fe5782 163-168 F6.3 0.1nm NaD Line-strength index of NaD 170-175 F6.3 mag TiO1 Line-strength index of TiO1 177-182 F6.3 mag TiO2 Line-strength index of TiO2 184-189 F6.3 0.1nm HdeltaA Line-strength index of HdeltaA 191-197 F7.3 0.1nm HgammaA Line-strength index of HgammaA 199-204 F6.3 0.1nm HdeltaF Line-strength index of HdeltaF 206-211 F6.3 0.1nm HgammaF Line-strength index of HgammaF 213-217 F5.3 mag e_CN1 Error on Line-strength index of CN1 219-223 F5.3 mag e_CN2 Error on Line-strength index of CN2 225-229 F5.3 0.1nm e_Ca4227 Error on Line-strength index of Ca4227 231-235 F5.3 0.1nm e_G4300 Error on Line-strength index of G4300 237-241 F5.3 0.1nm e_Fe4383 Error on Line-strength index of Fe4383 243-247 F5.3 0.1nm e_Ca4455 Error on Line-strength index of Ca4455 249-253 F5.3 0.1nm e_Fe4531 Error on Line-strength index of Fe4531 255-259 F5.3 0.1nm e_Fe4668 Error on Line-strength index of Fe4668 261-265 F5.3 0.1nm e_Hbeta Error on Line-strength index of Hbeta 267-271 F5.3 0.1nm e_Fe5015 Error on Line-strength index of Fe5015 273-277 F5.3 mag e_Mg1 Error on Line-strength index of Mg1 279-283 F5.3 mag e_Mg2 Error on Line-strength index of Mg2 285-289 F5.3 0.1nm e_Mgb Error on Line-strength index of Mgb 291-295 F5.3 0.1nm e_Fe5270 Error on Line-strength index of Fe5270 297-301 F5.3 0.1nm e_Fe5335 Error on Line-strength index of Fe5335 303-307 F5.3 0.1nm e_Fe5406 Error on Line-strength index of Fe5406 309-313 F5.3 0.1nm e_Fe5709 Error on Line-strength index of Fe5709 315-319 F5.3 0.1nm e_Fe5782 Error on Line-strength index of Fe5782 321-325 F5.3 0.1nm e_NaD Error on Line-strength index of NaD 327-331 F5.3 mag e_TiO1 Error on Line-strength index of TiO1 333-337 F5.3 mag e_TiO2 Error on Line-strength index of TiO2 339-343 F5.3 0.1nm e_HdeltaA Error on Line-strength index of HdeltaA 345-349 F5.3 0.1nm e_HgammaA Error on Line-strength index of HgammaA 351-355 F5.3 0.1nm e_HdeltaF Error on Line-strength index of HdeltaF 357-361 F5.3 0.1nm e_HgammaF Error on Line-strength index of HgammaF
Global notes: Note (G1): When the emission is lower than the variance the quality is set to 0. When the emission is between 1 and 2sigma or larger than 2sigma the quality is set to 1 and 2 respectively. Note (G2): In tables 5 and 8, the aperture code is the following: 0 = r = 1.5" 1 = r = 2.5" 2 = r = 10" 3 = r = re/10 4 = r = re/8 5 = r = re/4 6 = r = re/2 In table 9 the gradient code is the following: 0 = 0 < r < re/16 1 = re/16 < r < re/8 2 = re/8 < r < re/4 3 = re/4 < r < re/2
Acknowledgements: Francesca Annibali, annibali(at)stsci.edu
(End) Patricia Vannier [CDS] 26-Jan-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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