2,088 research outputs found
Luminosities of Barred and Unbarred S0 Galaxies
Lenticular galaxies with M_B < -21.5 are almost exclusively unbarred, whereas
both barred and unbarred objects occur at fainter luminosity levels. This
effect is observed both for objects classified in blue light, and for those
that were classified in the infrared. This result suggests that the most
luminous (massive) S0 galaxies find it difficult to form bars. As a result the
mean luminosity of unbarred lenticular galaxies in both B and IR light is
observed to be ~0.4 mag brighter than than that of barred lenticulars. A small
contribution to the observed luminosity difference that is found between SA0
and SB0 galaxies may also be due to the fact that there is an asymmetry between
the effects of small classification errors on SA0 and SB0 galaxies. An E galaxy
might be misclassified as an S0, or an S0 as an E. However, an E will never be
misclassified an SB0, nor will an SB0 ever be called an E. This asymmetry is
important because elliptical (E) galaxies are typically twice as luminous as
lenticular (S0) galaxies. The present results suggest that the evolution of
luminous lenticular galaxies may be closely linked to that of elliptical
galaxies, whereas fainter lenticulars might be more closely associated with
ram-pressure stripped spiral galaxies. Finally it is pointed out that fine
details of the galaxy formation process might account for some of the
differences between the classifications of the same galaxy by individual
competent morphologists.Comment: Astrophysical Journal, in pres
Approaches to Automated Morphological Classification of Galaxies
There is an obvious need for automated classification of galaxies, as the
number of observed galaxies increases very fast. We examine several approaches
to this problem, utilising {\em Artificial Neural Networks} (ANNs). We quote
results from a recent study which show that ANNs can classsify galaxies
morphologically as well as humans can.Comment: 8 pages, uu-encoded compressed postscript file (containing 2 figures
Quantitative Morphology of Galaxies in the Hubble Deep Field
We measure quantitative structural parameters of galaxies in the Hubble Deep
Field (HDF) on the drizzled F814W images. Our structural parameters are based
on a two-component surface brightness made up of a S\'ersic profile and an
exponential profile. We compare our results to the visual classification of van
den Bergh et al. (1996) and the classification of Abraham et al. (1996a).
Our morphological analysis of the galaxies in the HDF indicates that the
spheroidal galaxies, defined here as galaxies with a dominant bulge profile,
make up for only a small fraction, namely 8% of the galaxy population down to
m = 26.0. We show that the larger fraction of early-type systems
in the van den Bergh sample is primarily due to the difference in
classification of 40% of small round galaxies with half-light radii <
0\arcsecpoint 31. Although these objects are visually classified as elliptical
galaxies, we find that they are disk-dominated with bulge fractions < 0.5.
Given the existing large dataset of HDF galaxies with measured spectroscopic
redshifts, we are able to determine that the majority of distant galaxies
() from this sample are disk-dominated. Our analysis reveals a subset of
HDF galaxies which have profiles flatter than a pure exponential profile.Comment: 35 pages, LaTeX, 18 Postscript Figures, Tables available at
http://astro.berkeley.edu/~marleau/. Accepted for Publication in The
Astrophysical Journa
Mid-Infrared Galaxy Morphology Along the Hubble Sequence
The mid-infrared emission from 18 nearby galaxies imaged with the IRAC
instrument on Spitzer Space Telescope samples the spatial distributions of the
reddening-free stellar photospheric emission and the warm dust in the ISM.
These two components provide a new framework for galaxy morphological
classification, in which the presence of spiral arms and their emission
strength relative to the starlight can be measured directly and with high
contrast. Four mid-infrared classification methods are explored, three of which
are based on quantitative global parameters (colors, bulge-to-disk ratio)
similar to those used in the past for optical studies; in this limited sample,
all correlate well with traditional B-band classification. We suggest reasons
why infrared classification may be superior to optical classification.Comment: ApJS (in press), Spitzer Space Telescope Special Issue; 13 pages,
LaTeX (or Latex, etc); Figure 1ab is large, color plate; full-resolution
plates in .pdf format available at
http://cfa-www.harvard.edu/irac/publications
Dependence of Spiral Galaxy Distribution on Viewing Angle in RC3
The normalized inclination distributions are presented for the spiral
galaxies in RC3. The results show that, except for the bin of
-, in which the apparent minor isophotal diameters that
are used to obtain the inclinations, are affected by the central bulges, the
distributions for Sa, Sab, Scd and Sd are well consistent with the Monte-Carlo
simulation of random inclinations within 3-, and Sb and Sbc almost, but
Sc is different. One reason for the difference between the real distribution
and the Monte-Carlo simulation of Sc may be that some quite inclined spirals,
the arms of which are inherently loosely wound on the galactic plane and should
be classified to Sc galaxies, have been incorrectly classified to the earlier
ones, because the tightness of spiral arms which is one of the criteria of the
Hubble classification in RC3 is different between on the galactic plane and on
the tangent plane of the celestial sphere. Our result also implies that there
might exist biases in the luminosity functions of individual Hubble types if
spiral galaxies are only classified visually.Comment: 5 pages + 8 figures, LaTe
What are S0 (0) Galaxies?
Among early-type galaxies with almost circular isophotes E0 and E1 galaxies
are, at 99.3% significance, more luminous than face-on objects classified as S0
(0) and S(0) (1). This result supports the view that rotation and "diskiness"
are more important in the outer regions of faint-early type galaxies than they
are for more luminous galaxies of very early morphological type.Comment: 7 pages. 0 figures. Astrophysical Jounral Letters in pres
Spiral Structure and Galaxy Environment
Among 330 normal spirals of types Sa-Sc the fraction of objects exhibiting
``ring'', ``intermediate'' and ``spiral'' arm varieties does not correlated
with environment. A similar conclusion appears to apply to the arm varieties of
123 barred spirals of types SBa-SBc. It is concluded that, among the northern
Shapley-Ames galaxies, the distinction between the spiral and ring varieties of
spiral arms is, within the accuracy of presently available data, independent of
galaxy environment. This result suggests that the detailed morphology of spiral
arms depends primarily on parent galaxy characteristics, rather than on the
galactic environment.Comment: 8 pages. no figures. To be published in the August 2202 issue of A
The CMB Dipole and Circular Galaxy Distribution
The validity of Hubble's law defies the determination of the center of the
big bang expansion, even if it exists. Every point in the expanding universe
looks like the center from which the rest of the universe flies away. In this
article, the author shows that the distribution of apparently circular galaxies
is not uniform in the sky and that there exists a special direction in the
universe in our neighborhood. The data is consistent with the assumption that
the tidal force due to the mass distribution around the universe center causes
the deformation of galactic shapes depending on its orientation and location
relative to the center and our galaxy. Moreover, the cmb dipole data can also
be associated with the center of the universe expansion, if the cmb dipole at
the center of our supercluster is assumed to be due to Hubble flow. The
location of the center is estimated from the cmb dipole data. The direction to
the center from both sets of data is consistent and the distance to the center
is computed from the cmb dipole data.Comment: 9 pages, 3 figures (10 figure captions), 1 tabl
Limitations of model fitting methods for lensing shear estimation
Gravitational lensing shear has the potential to be the most powerful tool
for constraining the nature of dark energy. However, accurate measurement of
galaxy shear is crucial and has been shown to be non-trivial by the Shear
TEsting Programme. Here we demonstrate a fundamental limit to the accuracy
achievable by model-fitting techniques, if oversimplistic models are used. We
show that even if galaxies have elliptical isophotes, model-fitting methods
which assume elliptical isophotes can have significant biases if they use the
wrong profile. We use noise-free simulations to show that on allowing
sufficient flexibility in the profile the biases can be made negligible. This
is no longer the case if elliptical isophote models are used to fit galaxies
made up of a bulge plus a disk, if these two components have different
ellipticities. The limiting accuracy is dependent on the galaxy shape but we
find the most significant biases for simple spiral-like galaxies. The
implications for a given cosmic shear survey will depend on the actual
distribution of galaxy morphologies in the universe, taking into account the
survey selection function and the point spread function. However our results
suggest that the impact on cosmic shear results from current and near future
surveys may be negligible. Meanwhile, these results should encourage the
development of existing approaches which are less sensitive to morphology, as
well as methods which use priors on galaxy shapes learnt from deep surveys.Comment: 10 pages, 8 figure
Constraints on the Massive Supernova Progenitors
Generally accepted scheme distinguishes two main classes of supernovae (SNe):
Ia resulting from the old stellar population (deflagration of a white dwarf in
close binary systems), and SNe of type II and Ib/c whose ancestors are young
massive stars (died in a core-collapse explosion). Concerning the latter, there
are suggestions that the SNe II are connected to early B stars, and SNe Ib/c to
isolated O or Wolf-Rayet (W-R) stars. However, little or no effort was made to
further separate SNe Ib from Ic. We have used assumed SN rates for different SN
types in spiral galaxies in an attempt to perform this task. If isolated
progenitor hypothesis is correct, our analysis indicates that SNe Ib result
from stars of main-sequence mass , while the progenitors of SNe Ic are more
massive stars with .
Alternatively, if the majority of SNe Ib/c appear in close binary systems
(CBs) then they would result from the same progenitor population as most of the
SNe II, i.e. early B stars with initial masses of order . Future observations of SNe at high-redshift () and
their rate will provide us with unique information on SN progenitors and
star-formation history of galaxies. At higher- (deeper in the cosmic past)
we expect to see the lack of type Ia events, i.e. the dominance of
core-collapse SNe. Better understanding of the stripped-envelope SNe (Ib/c),
and their potential use as distance indicators at high-, would therefore be
of great practical importance.Comment: 11 pages, 2 figures, accepted for publication in IJMP
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