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J/ApJ/684/1026      Photometric profiles from GOODS data    (Azzollini+, 2008)

Cosmic evolution of stellar disk truncations: from z∼1 to the Local Universe. Azzollini R., Trujillo I., Beckman J.E. <Astrophys. J., 684, 1026-1047 (2008)> =2008ApJ...684.1026A
ADC_Keywords: Galaxies, optical ; Morphology ; Redshifts Keywords: galaxies: evolution - galaxies: fundamental parameters - galaxies: high-redshift - galaxies: structure Abstract: We have conducted the largest systematic search so far for stellar disk truncations in disklike galaxies at intermediate redshift (z<1.1), using the Great Observatories Origins Deep Survey-South (GOODS-S) data from the Hubble Space Telescope ACS. Focusing on type II galaxies (i.e., downbending profiles), we explore whether the position of the break in the rest-frame B-band radial surface brightness profile (a direct estimator of the extent of the disk where most of the massive star formation is taking place) evolves with time. The number of galaxies under analysis (238 of a total of 505) is an order of magnitude larger than in previous studies. For the first time, we probe the evolution of the break radius for a given stellar mass (a parameter well suited to address evolutionary studies). We have explored the distribution of the scale lengths of the disks in the region inside the break and how this parameter relates to the break radius. We also present results of the statistical analysis of profiles of artificial galaxies, to assess the reliability of our results. Description: We have worked with objects present in imaging data from HST ACS observations of the GOODS-South field (Giavalisco et al., 2004, Cat. II/261), which subtends an area in the sky of roughly 170arcmin2. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 99 505 Results on the classification and characterization of surface brightness profiles
See also: II/253 : Chandra Deep Field South: multi-colour data (Wolf+, 2008) II/261 : GOODS initial results (Giavalisco+, 2004) J/MNRAS/400/1962 : Southern GEMS groups. II. (Kilborn+, 2009) J/ApJS/172/615 : GALFIT result for GEMS galaxies (Haussler+, 2007) J/A+A/449/951 : GOODS-MUSIC sample: multicolour catalog (Grazian+, 2006) J/A+A/434/53 : GOODS-South Field redshifts (Vanzella+, 2005) : GOODS home page Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [GEMS] 5- 23 A19 --- GEMS GEMS name ( (1) 25- 26 I2 h RAh Hour of Right Ascension (J2000) (2) 28- 29 I2 min RAm Minute of Right Ascension (J2000) (2) 31- 35 F5.2 s RAs Second of Right Ascension (J2000) (2) 37 A1 --- DE- Sign of the Declination (J2000)(2) 38- 39 I2 deg DEd Degree of Declination (J2000) (2) 41- 42 I2 arcmin DEm Arcminute of Declination (J2000) (2) 44- 48 F5.2 arcsec DEs Arcsecond of Declination (J2000) (2) 50- 53 F4.2 --- z COMBO-17 (photometric) redshift (3) 55- 60 A6 --- Type Galaxy profile type (I, II or III) (5) 62- 66 F5.2 kpc RB ? Break radius; measured in B-band 68- 71 F4.2 kpc e_RB ? Uncertainty in RB 73- 77 F5.2 mag/arcsec2 muB ? Surface density at Break; B-band 79- 82 F4.2 mag/arcsec2 e_muB ? Uncertainty in muB 84- 88 F5.2 kpc h1 ? Scale length of inner disk part (4) 90- 99 A10 --- Com Comment
Note (1): Designations from Rix et al. 2004ApJS..152..163R Note (2): Coordinates are those retrieved by our software on GOODS-HST/ACS images. Note (3): From COMBO17 (Wolf et al. 2001A&A...365..681W, 2003A&A...401...73W; see also Cat. II/253). Note (4): The median value of the Pearson's R parameter for the linear fit from where h1 is derived is r1=0.993. Note (5): Profiles are classified in types I = no break apparent (exponential profile fit) II = break or truncation (profile steeper at larger radii, h1>h) III = antitruncation (inner profile steeper, h1<h)
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 10-Dec-2010
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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