25 research outputs found
On the use of scaling relations for the Tolman test
The use of relations between structural parameters of early type galaxies to
perform the Tolman test is reconsidered. Scaling relations such as the FP or
the Kormendy relation, require the transformation from angular to metric sizes,
to compare the relation at different z values. This transformation depends on
the assumed world model: galaxies of a given angular size, at a given z, are
larger (in kpc) in a non-expanding universe than in an expanding one.
Furthermore, the luminosities of galaxies are expected to evolve with z in an
expanding model. These effects are shown to conspire to reduce the difference
between the predicted SB change with redshift in the expanding and non
expanding cases. We find that the predictions for the visible photometric bands
of the expanding models with passive luminosity evolution are very similar to
those of the static model till z about 1, and therefore, the test cannot
distinguish between the two world models. Recent good quality data are
consistent with the predictions from both models. In the K-band, where the
expected (model) luminosity evolutionary corrections are smaller, the
differences between the xpanding and static models amount to about 0.4 (0.8)
magnitudes at z = 0.4 (1). It is shown that, due to that small difference
between the predictions in the covered z-range, and to the paucity and
uncertainties of the relevant SB photometry, the existing K-band data is not
adequate to distinguish between the different world metrics, and cannot be yet
used to discard the static case. It is pointed out that the scaling relations
could still be used to rule out the non-evolving case if it could be shown that
the coefficients change with the redshift.Comment: Latex, 15 pages with 2 figures. To be published in ApJ Letter
Multiwavelength Energy Distributions and Bolometric Luminosities of the 12--Micron Galaxy Sample
Aperture photometry from our own observations and the literature is presented
for the 12\um\ Galaxies in the near infrared J, H and K bands and, in some
cases, in the L band. These data are corrected to ``total'' near--infrared
magnitudes, (with a typical uncertainty of 0.3 magnitudes) for a direct
comparison with our IRAS fluxes which apply to the entire galaxy. The corrected
data are used to derive integrated total NIR and FIR luminosities. We then
combine these with blue photometry and an estimate of the flux contribution
from cold dust at wavelengths longward of 100\um\ to derive the first {\it
bolometric\/} luminosities for a large sample of galaxies. We use
multiwavelength correlations to identify several combinations of infrared
colors which discriminate between Seyfert~1 and~2 galaxies, LINERs, and
ultraluminous starbursts. We find that bolometric luminosity is more closely
proportional to 12-micron luminosity than to 60-micron, 25-micron or optical
luminosity.Comment: AASTeX, 18 pages. Text only. Figures (28) and tables (3) available at
ftp://eggneb.astro.ucla.edu/pub/rush/, named Spinoglio95-Table*.dat (ASCII)
and Spinoglio95-figs.ps (PostScript; 7 pages, by 4 per page). Scheduled for
the 1995 November 10 issue of Ap
Near-Infrared Imaging of Early-Type Galaxies III. The Near-Infrared Fundamental Plane
Near-infrared imaging data on 251 early-type galaxies in clusters and groups
are used to construct the near-infrared Fundamental Plane (FP) r_eff ~
sigma_0^1.53 _eff^-0.79. The slope of the FP therefore departs from
the virial expectation of r_eff ~ sigma_0^2 _eff^-1 at all optical and
near-infrared wavelengths, which could be a result of the variation of M/L
along the elliptical galaxy sequence, or a systematic breakdown of homology
among the family of elliptical galaxies. The slope of the near-infrared FP
excludes metallicity variations as the sole cause of the slope of the FP. Age
effects, dynamical deviations from a homology, or any combination of these
(with or without metallicity), however, are not excluded. The scatter of both
the near-infrared and optical FP are nearly identical and substantially larger
than the observational uncertainties, demonstrating small but significant
intrinsic cosmological scatter for the FP at all wavelengths. The lack of a
correlation of the residuals of the near-infrared FP and the residuals from the
Mg_2-sigma relation indicates that the thickness of these relations cannot be
ascribed only to age or metallicity effects. Due to this metallicity
independence, the small scatter of the near-infrared FP excludes a model in
which age and metallicity effects ``conspire'' to keep the optical FP thin. All
of these results suggest that the possible physical origins of the FP relations
are complicated due to combined effects of variations of stellar populations
and structural parameters among elliptical galaxies.Comment: to appear in The Astronomical Journal; 35 pages, including 13
Postscript figures and 1 table; uses AAS LaTeX style file
Clues on the Physical Origin of the Fundamental Plane from Self-consistent Hydrodynamical Simulations
We report on a study of the parameters characterizing the mass and velocity
distributions of two samples of relaxed elliptical-like objects (ELOs)
identified, at z=0, in a set of self-consistent hydrodynamical simulations
operating in the context of a concordance cosmological model. Star formation
(SF) has been phenomenologically implemented in the simulations in the
framework of the turbulent sequential scenario through a threshold gas density
and an efficiency parameter. Each ELO sample is characterized by the values
these parameters take. We have found that the (logarithms of the) ELO stellar
masses, projected stellar half-mass radii, and stellar central line-of-sight
(LOS) velocity dispersions define dynamical fundamental planes (FPs). Zero
points depend on the particular values that the SF parameters take, while
slopes do not change. The ELO samples have been found to show systematic trends
with the mass scale in both the relative content and the relative distributions
of the baryonic and the dark mass ELO components. The physical origin of these
trends lies in the systematic decrease, with increasing ELO mass, of the
relative dissipation experienced by the baryonic mass component along ELO mass
assembly, resulting in a tilt of the dynamical FP relative to the virial plane.
The dynamical FPs shown by the two ELO samples are consistent with that shown
by the SDSS elliptical sample in the same variables, with no further need for
any relevant contribution from stellar population effects to explain the
observed tilt. These effects could, however, have contributed to the scatter of
the observed FP, as the dynamical FPs have been found to be thinner than the
observed one. The results we report on hint, for the first time, at a possible
way to understand the tilt of the observed FP in a cosmological context.Comment: 12 pages, 1 figure. Accepted to Astrophysical Journal Letter
The Near-Infrared Fundamental Plane of Elliptical Galaxies
We present results from a near-infrared -band imaging survey of 59
elliptical galaxies in five nearby clusters. We measure photometric parameters
for each galaxy using surface photometry and draw velocity dispersions from the
literature. Three observables define a near-infrared Fundamental Plane (FP) of
elliptical galaxies with . The scatter in the near-infrared relation is small at
\% in distance, which is equivalent to, or less than, the scatter of the
optical FP. We suggest that the small deviation of the near-infrared FP
relation from the optical FP is due to the reduction of metallicity effects in
the near-infrared bandpass. While the small scatter of the optical FP could be
consistent with compensating effects of age and metallicity, the similarly
small scatter of the near-infrared FP is nearly independent of metallicity and
hence places a strong constraint on possible age spreads among elliptical
galaxies at every point along the FP. We suggest that the departure of the
near-infrared FP from the pure virial form , and the corresponding observed relation , may be explained by slight systematic departures of
the structure and dynamics of elliptical galaxies from a homology.Comment: to appear in The Astrophysical Journal (Letters); 12 pages, including
2 Postscript figures and 1 table; uuencoded, compressed format; the paper is
also available in various formats from
http://astro.caltech.edu/~map/map.bibliography.refereed.htm
Unresolved H-Alpha Enhancements at High Galactic Latitude in the WHAM Sky Survey Maps
We have identified 85 regions of enhanced H-Alpha emission at |b| > 10
degrees subtending approximately 1 degree or less on the Wisconsin H-Alpha
Mapper (WHAM) sky survey. These high latitude ``WHAM point sources'' have
H-Alpha fluxes of 10^{-11} to 10^{-9} erg cm^-2 s^-1, radial velocities within
about 70 km/s of the LSR, and line widths that range from less than 20 km/s to
about 80 km/s (FWHM). Twenty nine of these enhancements are not identified with
either cataloged nebulae or hot stars and appear to have kinematic properties
that differ from those observed for planetary nebulae. Another 14 enhancements
are near hot evolved low mass stars that had no previously reported detections
of associated nebulosity. The remainder of the enhancements are cataloged
planetary nebulae and small, high latitude H II regions surrounding massive O
and early B stars.Comment: 22 pages, 8 figures, 2 tables, to appear in Feb. 2005 A
Effect of the Milky Way on Magellanic Cloud structure
A combination of analytic models and n-body simulations implies that the
structural evolution of the Large Magellanic Cloud (LMC) is dominated by its
dynamical interaction with the Milky Way. Although expected at some level, the
scope of the involvement has significant observational consequences. First, LMC
disk orbits are torqued out of the disk plane, thickening the disk and
populating a spheroid. The torque results from direct forcing by the Milky Way
tide and, indirectly, from the drag between the LMC disk and its halo resulting
from the induced precession of the LMC disk. The latter is a newly reported
mechanism that can affect all satellite interations. However, the overall
torque can not isotropize the stellar orbits and their kinematics remains
disk-like. Such a kinematic signature is observed for nearly all LMC
populations. The extended disk distribution is predicted to increase the
microlensing toward the LMC. Second, the disk's binding energy slowly decreases
during this process, puffing up and priming the outer regions for subsequent
tidal stripping. Because the tidally stripped debris will be spatially
extended, the distribution of stripped stars is much more extended than the HI
Magellanic Stream. This is consistent with upper limits to stellar densities in
the gas stream and suggests a different strategy for detecting the stripped
stars. And, finally, the mass loss over several LMC orbits is predicted by
n-body simulation and the debris extends to tens of kiloparsecs from the tidal
boundary. Although the overall space density of the stripped stars is low,
possible existence of such intervening populations have been recently reported
and may be detectable using 2MASS.Comment: 15 pages, color Postscript figures, uses emulateapj.sty. Also
available from http://www-astro.phast.umass.edu/~weinberg/weinberg-pubs.htm
Vasorelaxant activity of Euphorbia furcillata Kunth mainly by activation of NO/cGMP pathway and calcium channel blockade
The aim of current study was to determinate ex vivo and chromatographic fingerprint by HPLC of four extracts of Euphorbia furcillata K. Ethyl acetate extract of Euphorbia furcillata (EaEEf) was the most effective and potent extract (Emax=98.69±1.24%) and its effect was partially endothelium-dependent. Functional vasorelaxant mechanism of action of EaEEf was determinate, EaEEf showed efficient relaxation of KCl [80 mM]-induced contraction and norepinephrine and CaCl2 contraction curves showed diminution of maximal contraction in the presence of EAEEf and EaEEf-relaxation curve was shifted to the right in the presence of L-NAME (nitric oxide synthase inhibitor) and ODQ (guanylate cyclase inhibitor). Chromatographic fingerprints analysis suggests presence of diterpenoid such as abietane, tigliane, and ingenane skeletons. Our experiments suggest the EaEEf vasorelaxant activity could be attributed to diterpenoid molecules whose mechanism involves nitric oxide production and calcium channel blockade
Stellar streams around the Magellanic Clouds
Using Blue Horizontal Branch stars identified in the Dark Energy Survey Year
1 data, we report the detection of an extended and lumpy stellar debris
distribution around the Magellanic Clouds. At the heliocentric distance of the
Clouds, overdensities of BHBs are seen to reach at least to ~30 degrees, and
perhaps as far as ~50 degrees from the LMC. In 3D, the stellar halo is
traceable to between 25 and 50 kpc from the LMC. We catalogue the most
significant of the stellar sub-structures revealed, and announce the discovery
of a number of narrow streams and diffuse debris clouds. Two narrow streams
appear approximately aligned with the Magellanic Clouds' proper motion.
Moreover, one of these overlaps with the gaseous Magellanic Stream on the sky.
Curiously, two diffuse BHB agglomerations seem coincident with several of the
recently discovered DES satellites. Given the enormous size and the conspicuous
lumpiness of the LMC's stellar halo, we speculate that the dwarf could easily
have been more massive than previously had been assumed.Comment: 15 pages, 11 figures. Figures improved. Accepted to MNRA
N-body simulations of the Magellanic Stream
A suite of high-resolution N-body simulations of the Magellanic Clouds --
Milky Way system are presented and compared directly with newly available data
from the HI Parkes All-Sky Survey (HIPASS). We show that the interaction
between Small and Large Magellanic Clouds results in both a spatial and
kinematical bifurcation of both the Stream and the Leading Arm. The spatial
bifurcation of the Stream is readily apparent in the HIPASS data, and the
kinematical bifurcation is also tentatively identified. This bifurcation
provides strong support for the tidal disruption origin for the Magellanic
Stream. A fiducial model for the Magellanic Clouds is presented upon completion
of an extensive parameter survey of the potential orbital configurations of the
Magellanic Clouds and the viable initial boundary conditions for the disc of
the Small Magellanic Cloud. The impact of the choice of these critical
parameters upon the final configurations of the Stream and Leading Arm is
detailed.Comment: Accepted by MNRAS, 07 Jun 2006. 14 pages, 14 figures, 3 tables. LaTeX
(mn2e.sty). File with decent resolution images (strongly recommended)
available at http://astronomy.swin.edu.au/~tconnors/publications/ .
References added; distance and HI-LOres difference figures added; clearer
figures; discussion added to, but conclusions unchange