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J/A+A/424/79  Photometry and Metallicity in ABCG 209 galaxies (Mercurio+, 2004)

Transformations of galaxies in the environments of the cluster ABCG 209 at z∼0.2 Mercurio A., Busarello G., Merluzzi P., La Barbera F., Girardi M., Haines C. <Astron. Astrophys. 424, 79 (2004)> =2004A&A...424...79M
ADC_Keywords: Clusters, galaxy ; Galaxies, photometry ; Galaxies, spectra ; Redshifts Keywords: Galaxy: evolution - Galaxy: fundamental parameters - galaxies: stellar content - galaxies: clusters: individual: ABCG 209 Abstract: We analyse the properties of galaxy populations in the rich Abell cluster ABCG 209 at redshift z∼0.21, on the basis of spectral classification of 102 member galaxies. We take advantage of available structural parameters to study separately the properties of bulge-dominated and disk-dominated galaxies. The star formation histories of the cluster galaxy populations are investigated by using line strengths and the 4000Å break, through a comparison to stellar population synthesis models. The dynamical properties of different spectral classes are examined in order to infer the past merging history of ABCG 209. The cluster is characterized by the presence of two components: an old galaxy population, formed very early (z_f≳3.5), and a younger (z_f≳1.2) population of infalling galaxies. We find evidence of a merger with an infalling group of galaxies occurred 3.5-4.5Gyr ago. The correlation between the position of the young H_delta-strong galaxies and the X-ray flux shows that the hot intracluster medium triggered a starburst in this galaxy population ∼3Gyr ago. Description: Photometric data (table1.dat) were collected on November 1999 using the CFH12K mosaic camera and spectroscopic data (table2.dat) have been obtained in the multi-object spectroscopy (MOS) mode of ESO Multi Mode Instrument at the ESO New Technology Telescoe (NTT) for 102 galaxies belonging to the cluster ABCG 209. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 85 102 Photometric parameters for 102 galaxies table4.dat 172 102 *Spectral indices for 102 galaxies
Note on table4.dat: The equivalent width is defined by: EW={Sum, i=1 to N}[(FCi-Fi)/FCi)*Δλ] where F_i is the flux in the pixel i, N is the number of pixels in the integration range, Δλ is the dispersion in Å/pixel and FCi is the straight line fitted to the blue and the red pseudo-continuum intervals, evaluated in the pixel i (pixels with values more than 3σ away from the continuum level were rejected). An index measured in magnitudes is: Mag=-2.5log[1-EW/(λ1-λ2)] where λ1 and λ2 are the wavelength limits of the feature bandpass. The errors of the equivalent width measurement are estimated from the relation of Czoske et al. (2001A&A...372..391C, Cat. J/A+A/372/391).
See also: J/A+A/397/431 : Redshifts of ABCG209 galaxies (Mercurio+, 2003) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Running number 6- 7 I2 h RAh Right ascension (J2000.0) 10- 11 I2 min RAm Right ascension (J2000.0) 14- 18 F5.2 s RAs Right ascension (J2000.0) 22 A1 --- DE- Declination sign (J2000.0) 23- 24 I2 deg DEd Declination (J2000.0) 27- 28 I2 arcmin DEm Declination (J2000.0) 31- 34 F4.1 arcsec DEs Declination (J2000.0) 38- 42 F5.2 mag Rmag R-band Kron magnitude corrected for Galactic extinction (1) 46- 49 F4.2 mag e_Rmag rms uncertainty on the R-band Kron magnitude determination (2) 52- 55 F4.2 mag B-R B-R colour index 59- 62 F4.2 mag e_B-R rms uncertainty on the color determination (2) 65- 70 F6.4 --- z heliocentric corrected redshift 74- 79 F6.4 --- e_z rms uncertainty on the redshift 82- 84 F3.1 --- n Sersic index
Note (1): Correction for foreground Galactic extinction according to Schlegel et al. (1998ApJ...500..525S) corresponds to the centre of cluster Note (2): Uncertainties in magnitudes and colours are rounded to the second decimal place.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq Running number 5- 8 F4.2 --- D4000 ? Strength of the 4000Å break 10- 13 F4.2 --- e_D4000 ? rms uncertainty on the 4000Å break measurement 15- 19 F5.1 0.1nm EW[OII] ? [OII] equivalent width (1) 21- 23 F3.1 0.1nm e_EW[OII] ? rms uncertainty on OII equivalent width 26- 29 F4.1 0.1nm EWHdA Hδ,A equivalent width 31- 33 F3.1 0.1nm e_EWHdA rms uncertainty on Hδ,A equivalent width 35- 39 F5.1 0.1nm EWHgA Hγ,A equivalent width 41- 43 F3.1 0.1nm e_EWHgA rms uncertainty on Hγ,A equivalent width 46- 49 F4.1 0.1nm EWFe4531 Fe4531 equivalent width 51- 53 F3.1 0.1nm e_EWFe4531 rms uncertainty on Fe4531 equivalent width 55- 59 F5.1 0.1nm EWHb Hβ equivalent width 61- 63 F3.1 0.1nm e_EWHb rms uncertainty on H_beta equivalent width 65- 69 F5.1 0.1nm EW[OIII] Equivalent width of [OIII] 71- 73 F3.1 0.1nm e_EW[OIII] rms uncertainty on [OIII] equivalent width 75- 79 F5.1 0.1nm EWFe5015 Fe5015 equivalent width 81- 83 F3.1 0.1nm e_EWFe5015 rms uncertainty on Fe5015 equivalent width 87- 90 F4.2 mag Mg1 Mg1 index 92- 95 F4.2 mag e_Mg1 rms uncertainty on Mg1 index 98-101 F4.2 mag Mg2 Mg2 index 103-106 F4.2 mag e_Mg2 rms uncertainty on Mg2 index 109-112 F4.1 0.1nm Mgb Mgb index 114-116 F3.1 0.1nm e_Mgb rms uncertainty on Mgb index 118-122 F5.1 0.1nm EWFe5270 Hβ equivalent width 124-126 F3.1 0.1nm e_EWFe5270 rms uncertainty on Fe5270 equivalent width 129-132 F4.1 0.1nm EWFe5335 Fe5335 equivalent width 134-136 F3.1 0.1nm e_EWFe5335 rms uncertainty on Fe5335 equivalent width 138-143 F6.1 0.1nm EWHa ? Halpha equivalent width (1) 145-147 F3.1 0.1nm e_EWHa ? rms uncertainty on H_alpha equivalent width 150-158 A9 --- Class Spectral classification (2)
Note (1): A value of '0.0' for the equivalent width for an emission-line indicates that no emission is observed, whereas '---' indicates that the equivalent width could not be measured as the line does not lie within the available wavelength range. Note (2): Spectral classification: ELG: emission line galaxies; HDS_blue: Hδ strong galaxies with blue colour; HDS_red: Hδ strong galaxies with red colour; P: passive evolving galaxies; Ab-spirals: passive evolving disk-dominated galaxies (nSersic≤2). Galaxy 62 presents very strong [OII], [OIII] and Hα emission, that could suggest the presence of an AGN. However, our data do not allow a reliable classification, leading us to exclude this object from the analysis..
Acknowledgements: Armata Mercurio
(End) Patricia Vannier [CDS] 04-Jun-2004
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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