237 research outputs found
Possible Local Spiral Counterparts to Compact Blue Galaxies at Intermediate Redshift
We identify nearby disk galaxies with optical structural parameters similar
to those of intermediate-redshift compact blue galaxies. By comparing HI and
optical emission-line widths, we show that the optical widths substantially
underestimate the true kinematic widths of the local galaxies. By analogy,
optical emission-line widths may underrepresent the masses of intermediate-z
compact objects. For the nearby galaxies, the compact blue morphology is the
result of tidally-triggered central star formation: we argue that interactions
and minor mergers may cause apparently compact morphology at higher redshift.Comment: 5 pages, uses emulateapj5 and psfig. To appear in ApJ
Angular Sizes of Faint Field Disk Galaxies: Intrinsic Luminosity Evolution
In order to explain the small scale-lengths detected in the recent deep field
observations performed from large ground-based telescopes and from the Hubble
Space Telescope, we investigate the predictions at high redshifts for disk
galaxies that formed by infall. Changes with redshift in the observed
properties of field galaxies are directly related to the evolution of the disks
and of the stellar populations. We see that changes in the rest frame
luminosity of a galaxy induce smaller values of half-light radii than are
predicted assuming no evolution. Comparisons are presented with two observed
samples from Mutz et al. (1994) and Smail et al. (1995).Comment: plain tex file + 3 postscript figures. To be published in ApJ
CO-bandhead spectroscopy of IC 342: mass and age of the nuclear star cluster
We have used the NASA Infra-Red Telescope Facility (IRTF) to observe the
nuclear stellar cluster in the nearby, face-on, giant Scd spiral IC 342. From
high resolution (R = 21500) spectra at the 12CO (2-0) bandhead at 2.3 micron we
derive a line-of-sight stellar velocity dispersion sigma = (33 +- 3) km/s.
To interpret this observation we construct dynamical models based on the
Jeans equation for a spherical system. The light distribution of the cluster is
modeled using an isophotal analysis of an HST V-band image from the HST Data
Archive, combined with new ground-based K-band imaging. Under the assumption of
an isotropic velocity distribution, the observed kinematics imply a K-band
mass-to-light ratio M/L_K = 0.05, and a cluster mass M ~ 6 times 10^6 Msun. We
model the mass-to-light ratio with the `starburst99' stellar population
synthesis models of Leitherer and collaborators, and infer a best-fitting
cluster age in the range 63-630 Myears. Although this result depends somewhat
on a number of uncertainties in the modeling (e.g., the assumed extinction
along the line-of-sight towards the nucleus, the IMF of the stellar population
model, and the velocity dispersion anisotropy of the cluster), none of these
can be plausibly modified to yield a significantly larger age. We discuss the
implications of this result on possible scenarios for the frequency of nuclear
starbursts and their impact on secular evolution of spiral galaxy nuclei.
As a byproduct of our analysis, we infer that IC 342 cannot have any central
black hole more massive than 0.5 million solar masses. This is ~ 6 times less
massive than the black hole inferred to exist in our Galaxy, consistent with
the accumulating evidence that galaxies with less massive bulges harbor less
massive black holes.Comment: 27 pages, incl. 9 figures, submitted to The Astronomical Journa
Retrieving Bulge and Disk Parameters and Asymptotic Magnitudes from the Growth Curves of Galaxies
We show that the growth curves of galaxies can be used to determine their
bulge and disk parameters and bulge-to-total luminosity ratios, in addition to
their conventional asymptotic magnitudes, provided that the point spread
function is accurately known and signal-to-noise ratio is modest
(S/N). The growth curve is a fundamental quantity that most future
large galaxy imaging surveys will measure. Bulge and disk parameters retrieved
from the growth curve will enable us to perform statistical studies of
luminosity structure for a large number of galaxies.Comment: 28 pages including 13 PS figures; accepted for publication in PAS
Seismic Risk Assessment Tools Workshop
Held in the European Crisis Management Laboratory on 11-12 May 2017, the Workshop brought together on one side the developers of some of the most widely used modern seismic risk assessment tools and on the other a number of Civil Protection authorities from countries of the European Civil Protection Mechanism. The objective was to demonstrate the use and capabilities of the tools, explore the possible use in near-real-time impact assessment and promote their use in risk planning and disaster response.
The systems presented in the workshop demonstrated a very high sophistication and increased flexibility in accepting data from a large number of sources and formats. Systems that were initially developed on a national scale can now work on a global level with little effort and the use of global-scale exposure data is almost seamless. An urgent need for more accurate exposure data being openly available was identified, as well as the need of proper use of the fragility curves. Inter-system collaboration and interoperability in some cases to increase ease of use was greatly appreciated and encouraged. All systems participated in a real-time simulation exercise on previously unknown seismic data provided by the JRC; some additional automation might be in order, but in general all systems demostrated a capacity to produce results on a near-real-time basis. The demonstrations were unanimously welcomed as very useful by the participating Civil Protection Authorities, most of which are either using a locally-developed system of moving towards using one of those presented in the workshop.JRC.E.1-Disaster Risk Managemen
A near infrared photometric plane for ellipticals and bulges of spirals
We report the existence of a single plane in the space of global photometric
parameters describing elliptical galaxies and the bulges of early type spiral
galaxies. The three parameters which define the plane are obtained by fitting
the Sersic form to the brightness distribution obtained from near-infrared K
band images. We find, from the range covered by their shape parameters, that
the elliptical galaxies form a more homogeneous population than the bulges.
Known correlations like the Kormendy relation are projections of the
photometric plane. The existence of the plane has interesting implications for
bulge formation models.Comment: 12 pages, LaTeX including 5 figures. To appear in the Astrophysical
Journal Letter
Optical observations of a newly identified compact galaxy group near the Zone of Avoidance
We have identified a new group of galaxies, CG J0247+44.9, at low Galactic
latitude (l=143.64 deg, b=-13.29 deg), which satisfies Hickson's criteria
(Hickson 1997) for Compact Groups (CGs). Our group consists of six members, two
of which are in close interaction (IRAS 02443+4437). We present here optical
photometry (BVRI) and low resolution spectroscopy of the individual galaxies
and investigate the global properties of the group. Our morphological analysis
reveals that two out of the six objects are lenticular galaxies. The others are
spirals showing emission lines in their spectra through which we could classify
them as a starburst galaxy (the spiral member of the IRAS 02443+4437 close
pair), a Seyfert 2, a LINER and a weak H II galaxy. Since the S0/Sa is the
prevailing morphology for the galaxies of this group, which is also
characterized by a short crossing time and a relatively high velocity
dispersion, we suggest that CG J0247+44.9 is a dynamically old compact group.Comment: 17 pages, 5 figures out of which 4 are in jpg format. A postscript
version of the paper including all figures is available at:
http://astro.uibk.ac.at/~giovanna/preprints/Temporins.ps.gz Accepted for
publication in Astronomy and Astrophysic
Two dimensional bulge disk decomposition
We propose a two dimensional galaxy fitting algorithm to extract parameters
of the bulge, disk, and a central point source from broad band images of
galaxies. We use a set of realistic galaxy parameters to construct a large
number of model galaxy images which we then use as input to our galaxy fitting
program to test it. We find that our approach recovers all structural
parameters to a fair degree of accuracy. We elucidate our procedures by
extracting parameters for 3 real galaxies -- NGC 661, NGC 1381, and NGC 1427.Comment: 23 pages, LaTeX, AASTEX macros used, 7 Postscript figures, submitted
to Ap
The Galaxy Populations of X-Ray Detected, Poor Groups
(Abridged) We determine the quantitative morphology and star formation
properties of galaxies in six nearby X-ray detected, poor groups using
multi-object spectroscopy and wide-field R imaging. We measure structural
parameters for each galaxy by fitting a PSF-convolved, two component model to
their surface brightness profiles. To compare directly the samples, we fade,
smooth, and rebin each galaxy image so that we effectively observe each galaxy
at the same redshift (9000 km/s) and physical resolution (0.87h^(-1) kpc). We
compare results for the groups to a sample of field galaxies. We find that: 1)
Galaxies spanning a wide range in morphological type and luminosity are
well-fit by a de Vaucouleurs bulge with exponential disk profile. 2)
Morphologically classifying these nearby group galaxies by their bulge fraction
(B/T) is fairly robust on average, even when their redshift has increased by up
to a factor of four and the effective resolution of the images is degraded by
up to a factor of five. 3) The fraction of bulge-dominated systems in these
groups is higher than in the field (~50% vs. ~20%). 4) The fraction of
bulge-dominated systems in groups decreases with increasing radius, similar to
the morphology-radius (~density) relation observed in galaxy clusters. 5)
Current star formation in group galaxies is correlated with significant
morphological asymmetry for disk-dominated systems (B/T<0.4). 6) The group
galaxies that are most disk-dominated (B/T<0.2) are less star forming and
asymmetric on average than their counterparts in the field.Comment: Accepted for publication in the Astrophysical Journal (26 pages + 12
figures); Figs 1 & 2 also available at
http://www.ucolick.org/~vy/astronomy/groups_figs.tar.g
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