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J/ApJ/499/112       HST CFRS and LDSS redshift surveys. I.   (Brinchmann+ 1998)

Hubble space telescope imaging of the CFRS and LDSS redshift surveys. I. Morphological properties. Brinchmann J., Abraham R., Schade D., Tresse L., Ellis R.S., Lilly S., Le Fevre O., Glazebrook K., Hammer F., Colless M., Crampton D., Broadhurst T. <Astrophys. J. 499, 112 (1998)> =1998ApJ...499..112B (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, photometry ; Redshifts ; Spectroscopy Mission_Name: HST Keywords: galaxies: fundamental parameters - galaxy: structure - surveys Abstract: We analyze Hubble Space Telescope images of a complete sample of 341 galaxies drawn from the Canada-France Redhsift Survey (CFRS) and Low-Dispersion Survey Spectrograph (LDSS) ground-based redshift surveys. In this, the first paper in the series, each galaxy has been morphologically classified according to a scheme similar to that developed for the Medium Deep Survey. We discuss the reproducibility of these classifications and quantify possible biases that may arise from various redshift-dependent effects. We then discuss automated classifications of the sample and conclude, from several tests, that we can expect an apparent migration with redshift to later Hubble types that corresponds to a misclassification in our adopted machine classification system of ∼24%±11 of the true "spirals" as "peculiars" at a redshift z~=0.9. After allowing for such biases, the redshift distribution for normal spirals, together with their luminosity function derived as a function of redshift, indicates approximately 1mag of luminosity evolution in BAB by z~=1. The elliptical sample is too small for precise evolutionary constraints. However, we find a substantial increase in the proportion of galaxies with irregular morphology at large redshift from 9%±3% for 0.3≤z≤0.5 to 32%±12% for 0.7≤z≤0.9. These galaxies also appear to be the dominant cause of the rapid rise with redshift in the blue luminosity density identified in the redshift surveys. Although galaxies with irregular morphology may well comprise a mixture of different physical systems and might not correspond to present-day irregulars, it is clear that the apparently declining abundance and luminosities of our distant "irregulars" holds an important key to understanding recent evolution in the star formation history of normal galaxies. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 80 341 Data for objects in the survey
See also: J/ApJ/455/60 : CFRS II: 0000-00 and 1000+25 fields (Le Fevre+ 1995) J/ApJ/455/75 : CFRS III: 1415+52 and 2215+00 fields (Lilly+ 1995) J/ApJ/455/88 : CFRS IV: 0300+00 field (Hammer+ 1995) J/ApJ/464/79 : CFRS XI: High-redshift field galaxies morphology (Schade+ 1996) J/ApJ/481/49 : CFRS XIV. Field galaxies up to z=1 (Hammer+ 1997) J/MNRAS/273/157 : A faint galaxy survey to B = 24. (Glazebrook+ 1995) Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 8 F8.5 --- ID Identification number 10- 14 F5.3 --- z ? Redshift 15 A1 --- n_z [g] Note on z (1) 17- 21 F5.2 mag F814W ? F814W magnitude 23- 28 F6.2 mag BMag ? Absolute BAB magnitude 29 A1 --- n_BMag [hi] Note on BMag (2) 31- 32 I2 --- Class Redhsift confidence class (3) 34- 35 I2 --- MClass Eyeball morphological classification for the object 37- 41 F5.3 --- A ? Uncorrected rotational asymmetry factor 43- 47 F5.3 --- C ? Uncorrected central concentration index 49- 50 I2 --- MClassAC AC morphological classification (4) 52- 54 I3 0.1nm EW[OII] ? [O II] equivalent width (5) 56- 57 I2 0.1nm e_EW[OII] ? rms uncertainty on EW[OII] 59- 65 A7 --- Origin Origin (6) 67- 80 A14 --- OldID Old identification (7)
Note (1): g: The object is clearly extended, but was given z=0 in in the CFRS survey Note (2): h: The HST photometry here is uncertain, and MAB is based on the original bJ photometry i: The absolute magnitude is the original Autofib absolute magnitude based on bJ transformed to AB Note (3): Each object identification was assigned a confidence class. The notation was set to classes 0-4, 8, 9, 12-14, 91-94 as follow: 0-4: 0: when no redshift could be assigned 1: probability of 50% that the measurement was correct 2: probability of more than 75% that the measurement was correct 3: measurement at least 95% secure 4: unquestionably correct identification 8-9: 8: object for which the algorithm indicates that the emission line is [O II]λ3727 9: object for which the redshift ambiguity still could not be resolved 12-14: QSO are identified with the same quality notation 1-4 as galaxies, but a 1 is placed in front, e.g., 14 is a very secure QSO. 91-94: Objects which do not belong to the main catalog, either because they have IAB=22.5 or IAB<17.5, because of instrumental problems but have a redshift determination, or whose photometry was adjusted fainter than IAB=22.5 after the spectroscopic observation, are kept in a supplemental catalog and are identified by a 9 in front of the confidence class, e.g., 93. The objects in this supplemental catalog may thus have biases that will not be present in the statistically complete sample. For the LDSS objects this has been transformed to the CFRS system by assigning note = 4 to confident redshifts, note = 2 to less secure redshifts, and 0 to failures. For the few LDSS objects for which there is no confidence class, we have assigned note = -1. For CFRS 03.1027, the original "39" value was modified in "9", as in table1 of Cat. J/ApJ/455/88 Note (4): AC classification for the object using the division lines in Fig. 8. Note (5): For the CFRS objects this is from Hammer et al. (1997, Cat. J/ApJ/481/49); for the LDSS objects it is from the Autofib survey (Ellis et al., 1996MNRAS.280..235E) Note (6): CFRS: Canada-France Redhsift Survey, Lilly et al., 1995ApJ...455...50L; Le Fevre et al. 1995, Cat. J/ApJ/455/60 GRTH: Groth et al., 1994BAAS..185.5309G LDSS-1: Low-Dispersion Survey Spectrograph (Colless et al., 1993MNRAS.261...19C) LDSS-2: Low-Dispersion Survey Spectrograph (Glazebrook et al., 1995) Cat. J/MNRAS/273/157) Autofib: Autofib Survey (Ellis et al., 1996MNRAS.280..235E) Note (7): The identification given in the original LDSS paper
History: From electronic ApJ version References: Lilly et al., Paper II. 1998ApJ...500...75L
(End) James Marcout, Patricia Bauer [CDS] 22-Sep-1998
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