Welcome to the new version of CaltechAUTHORS. Login is currently restricted to library staff. If you notice any issues, please email coda@library.caltech.edu
Published November 2000 | Published + Accepted Version
Journal Article Open

Caltech Faint Galaxy Redshift Survey. XIV. Galaxy Morphology in the Hubble Deep Field (North) and Its Flanking Fields to z =  1.2


Morphological classifications are reported for Hubble Space Telescope images of 241 galaxies in the Hubble Deep Field and its flanking fields with measured redshifts in the interval 0.25 < z < 1.2, drawn from a magnitude-limited redshift survey to R = 24.0. The galaxies are divided into three groups with redshifts in the intervals 0.25–0.6, 0.6–0.8, and 0.8–1.2. R_(606) images from the first group and I_(814) images from the second and third groups are compared with B-band images of nearby galaxies. All classifications were therefore made at approximately the same rest wavelength. Selection biases are discussed. We corroborate and extend the results of earlier investigations by observing that 1. Most intermediate- and late-type galaxies with z ≳ 0.5 have morphologies that are dramatically different from those of local galaxies and cannot be shoehorned into the Hubble "tuning fork" classification scheme; 2. Grand-design spirals appear to be rare or absent for z ≳ 0.3; 3. Many Sa and Sb spirals with z ≳ 0.6 do not exhibit well-defined spiral arms, and the arms of distant Sc galaxies appear more chaotic than those of their nearby counterparts; 4. The fraction of all galaxies that are of types Sc and Scd drops from 23% at z ~ 0 to 5% for z > 0.6. 5. Barred spirals are extremely rare for z ≳ 0.5; 6. Roughly one in five galaxies with z ≳ 0.8 is a compact objects that resembles local E, S0, or Sa galaxies. 7. Peculiar galaxies are more common beyond z = 0.3, especially among late-type spirals, than they are at z ~ 0; 8. Merging galaxies, particularly those with three or more components, also become more common with increasing redshift. On the basis of these and similar observations, it is inferred that the development of pronounced spiral structure was delayed until ~5 Gyr and that most bulges are probably not formed by disintegrating bars. Major morphological changes were still taking place only ~5 Gyr ago, even though changes in the integrated light of most galaxies were then much slower than they were ~10 Gyr ago.

Additional Information

© 2000 The American Astronomical Society. Received 2000 June 27; accepted 2000 August 2. Based in part on observations obtained at the W. M. Keck Observatory, which is operated jointly by the California Institute of Technology and the University of California. It is a pleasure to thank Peter Stetson for his help with the rescaling of the present images, Simon Morris for cosmological consultations, and Jerry Sellwood for information on the formation of galactic bars. The extragalactic work of J. G. C., who is the principal investigator of the Caltech Faint Galaxy Redshift Survey, is not supported by any federal agency. R. B. acknowledges support under NSF grant AST 99-00866.

Attached Files

Published - van_den_Bergh_2000_AJ_120_2190.pdf

Accepted Version - 0008051.pdf


Files (471.6 kB)
Name Size Download all
268.0 kB Preview Download
203.6 kB Preview Download

Additional details

August 19, 2023
October 20, 2023