88 research outputs found
A Strong Dichotomy in S0 Disk Profiles Between the Virgo Cluster and the Field
We report evidence for a striking difference between S0 galaxies in the local
field and in the Virgo Cluster. While field S0 galaxies have disks whose
surface-brightness profiles are roughly equally divided between the three main
types (Types I, II, and III: single-exponential, truncated, and antitruncated),
Virgo S0s appear to be entirely lacking in disk truncations. More specifically,
the fraction of truncations in S0 galaxies with M_B < -17 is 28% +7/-6% for the
field, versus 0% +4/-0% for the Virgo Cluster galaxies; the difference is
significant at the 99.7% level. The discrepancy is made up almost entirely by
Type I profiles, which are almost twice as frequent in the Virgo Cluster as
they are in the field.
This suggests that S0 formation may be driven by different processes in
cluster and field environments, and that outer-disk effects can be useful tests
of S0 formation models.Comment: pdflatex, 6 pages, 3 PDF figures (emulateapj format). To appear in
The Astrophysical Journal Letter
Surface photometry and structure of high redshift disk galaxies in the HDF-S NICMOS field
A photometric study of 22 disk galaxies at redshifs z=0.5-2.6 is conducted,
using deep NICMOS J and H band and STIS open mode observations of the HDF-S
NICMOS parallel field. Rest-frame B-profiles and (U-V) color profiles are
constructed. A number of disks show steeper decrease of luminosity than
exponential, referring to disk truncation. Shape of the luminosity profiles
does not vary with redshift, but galactic sizes decrease significantly. (U-V)
colors and color gradients suggest more intense and centrally concentrated star
formation at earlier epochs. On the basis of (U-V) color and chemical evolution
models, the disks at z~2.5 have formed between z=3.5-7. The studied parameters
are idependent of absolute B luminosity within the sample.Comment: 13 pages, 8 figures, Astron. Astrophys. accepte
HST observations of nuclear stellar disks
We present observations of four nearby early-type galaxies with previously
known nuclear stellar disks using two instruments on-board the Hubble Space
Telescope. We observed NGC4128, NGC4612, and NGC5308 with the Wide Field
Planetary Camera 2, and the same three galaxies, plus NGC4570, with the Space
Telescope Imaging Spectrograph. We have detected a red nucleus in NGC4128, a
blue nucleus in NGC4621, and a blue disk in NGC5308. Additionally, we have
discovered a blue disk-like feature with position angle ~15 degrees from the
major axis in NGC4621. In NGC5308 there is evidence for a blue region along the
minor axis. We discovered a blue transient on the images of NGC4128 at position
0.14" west and 0.32" north from the nucleus. The extracted kinematic profiles
belong to two groups: fast (NGC4570 and NGC5308) and kinematically disturbed
rotators (NGC4128 and NGC4621). We report the discovery of a kinematically
decoupled core in NGC4128. Galaxies have mostly old (10-14 Gyr) stellar
populations with large spread in metallicities (sub- to super-solar). We
discuss the possible formation scenarios, including bar-driven secular
evolution and the influence of mergers, which can explain the observed color
and kinematic features.Comment: 22 pages, 14 figures, A&A in pres
Frequency and properties of bars in cluster and field galaxies at intermediate redshifts
We present a study of large-scale bars in field and cluster environments out
to redshifts of ~0.8 using a final sample of 945 moderately inclined disk
galaxies drawn from the EDisCS project. We characterize bars and their host
galaxies and look for relations between the presence of a bar and the
properties of the underlying disk. We investigate whether the fraction and
properties of bars in clusters are different from their counterparts in the
field. The total optical bar fraction in the redshift range z=0.4-0.8 (median
z=0.60), averaged over the entire sample, is 25% (20% for strong bars). For the
cluster and field subsamples, we measure bar fractions of 24% and 29%,
respectively. We find that bars in clusters are on average longer than in the
field and preferentially found close to the cluster center, where the bar
fraction is somewhat higher (~31%) than at larger distances (~18%). These
findings however rely on a relatively small subsample and might be affected by
small number statistics. In agreement with local studies, we find that
disk-dominated galaxies have a higher optical bar fraction (~45%) than
bulge-dominated galaxies (~15%). This result is based on Hubble types and
effective radii and does not change with redshift. The latter finding implies
that bar formation or dissolution is strongly connected to the emergence of the
morphological structure of a disk and is typically accompanied by a transition
in the Hubble type. (abridged)Comment: 17 pages, accepted for publication in A&
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