113 research outputs found
Book Review
Review of Carl. E. Wasmuth, Law and the Surgical Team, Williams and Wilkins Co., 196
Book Review
Review of Carl. E. Wasmuth, Law and the Surgical Team, Williams and Wilkins Co., 196
Pharmacy, Law, and the U.C.C., and Patent Medicines
The primary legal concern of the pharmacist has been and continues to be in the field of negligence. With the increasing legal awareness of society, however, it becomes imperative to examine what liabilities may arise under the U.C.C. The main objective of this paper is to explore the possible areas of liability that may arise under the Code in the sale of patent medicines by the pharmacist
Pharmacy, Law, and the U.C.C., and Patent Medicines
The primary legal concern of the pharmacist has been and continues to be in the field of negligence. With the increasing legal awareness of society, however, it becomes imperative to examine what liabilities may arise under the U.C.C. The main objective of this paper is to explore the possible areas of liability that may arise under the Code in the sale of patent medicines by the pharmacist
Discovery of a Boxy Peanut Shaped Bulge in the Near Infrared
We report on the discovery of a boxy/peanut shaped bulge in the highly
inclined barred Seyfert 2 galaxy NGC~7582. The peanut shape is clearly evident
in near infrared images but obscured by extinction from dust in visible
images. This suggests that near infrared imaging surveys will discover a
larger number of boxy/peanut morphologies than visible surveys, particularly in
galaxies with heavy extinction such as NGC~7582. The bulge in NGC~7582 exhibits
strong boxiness compared to other boxy/peanut shaped bulges. If the starburst
was mediated by the bar, then it is likely that the bar formed in less than a
few bar rotation periods or a few years ago. If the bar also
caused the peanut, then the peanut would have formed quickly; on a timescale of
a few bar rotation periods.Comment: AAS Latex and Postcript Figures, accepted for publication in Ap
Radial distribution of stars, gas and dust in SINGS galaxies. I. Surface photometry and morphology
We present ultraviolet through far-infrared surface brightness profiles for
the 75 galaxies in the Spitzer Infrared Nearby Galaxies Survey (SINGS). The
imagery used to measure the profiles includes GALEX UV data, optical images
from KPNO, CTIO and SDSS, near-IR data from 2MASS, and mid- and far-infrared
images from Spitzer. Along with the radial profiles, we also provide
multi-wavelength asymptotic magnitudes and several non-parametric indicators of
galaxy morphology: the concentration index (C_42), the asymmetry (A), the Gini
coefficient (G) and the normalized second-order moment of the brightest 20% of
the galaxy's flux (M_20). Our radial profiles show a wide range of morphologies
and multiple components (bulges, exponential disks, inner and outer disk
truncations, etc.) that vary not only from galaxy to galaxy but also with
wavelength for a given object. In the optical and near-IR, the SINGS galaxies
occupy the same regions in the C_42-A-G-M_20 parameter space as other normal
galaxies in previous studies. However, they appear much less centrally
concentrated, more asymmetric and with larger values of G when viewed in the UV
(due to star-forming clumps scattered across the disk) and in the mid-IR (due
to the emission of Polycyclic Aromatic Hydrocarbons at 8.0 microns and very hot
dust at 24 microns).Comment: 66 pages in preprint format, 14 figures, published in ApJ. The
definitive publisher authenticated version is available online at
http://dx.doi.org/10.1088/0004-637X/703/2/156
The Frequency of Barred Spiral Galaxies in the Near-IR
We have determined the fraction of barred galaxies in the H-band for a
statistically well-defined sample of 186 spirals drawn from the Ohio State
University Bright Spiral Galaxy survey. We find 56% of our sample to be
strongly barred at H, while another 16% is weakly barred. Only 27% of our
sample is unbarred in the near-infrared. The RC3 and the Carnegie Atlas of
Galaxies both classify only about 30% of our sample as strongly barred. Thus
strong bars are nearly twice as prevalent in the near-infrared as in the
optical. The frequency of genuine optically hidden bars is significant, but
lower than many claims in the literature: 40% of the galaxies in our sample
that are classified as unbarred in the RC3 show evidence for a bar in the
H-band, while for the Carnegie Atlas this fraction is 66%. Our data reveal no
significant trend in bar fraction as a function of morphology in either the
optical or H-band. Optical surveys of high redshift galaxies may be strongly
biased against finding bars, as bars are increasingly difficult to detect at
bluer rest wavelengths.Comment: LaTeX with AASTeX style file, 23 pages with 6 figures. Accepted for
publication in The Astronomical Journal (Feb. 2000
Comparing Galaxy Morphology at Ultraviolet and Optical Wavelengths
We have undertaken an imaging survey of 34 nearby galaxies in far-ultraviolet
(FUV, ~1500A) and optical (UBVRI) passbands to characterize galaxy morphology
as a function of wavelength. This sample, which includes a range of classical
Hubble types from elliptical to irregular with emphasis on spirals at low
inclination angle, provides a valuable database for comparison with images of
high-z galaxies whose FUV light is redshifted into the optical and near-
infrared bands. Ultraviolet data are from the UIT Astro-2 mission. We present
images and surface brightness profiles for each galaxy, and we discuss the
wavelength-dependence of morphology for different Hubble types in the context
of understanding high-z objects. In general, the dominance of young stars in
the FUV produces the patchy appearance of a morphological type later than that
inferred from optical images. Prominent rings and circumnuclear star formation
regions are clearly evident in FUV images of spirals, while bulges, bars, and
old, red stellar disks are faint to invisible at these short wavelengths.
However, the magnitude of the change in apparent morphology ranges from
dramatic in early--type spirals with prominent optical bulges to slight in
late-type spirals and irregulars, in which young stars dominate both the UV and
optical emission. Starburst galaxies with centrally concentrated, symmetric
bursts display an apparent ``E/S0'' structure in the FUV, while starbursts
associated with rings or mergers produce a peculiar morphology. We briefly
discuss the inadequacy of the optically-defined Hubble sequence to describe FUV
galaxy images and estimate morphological k-corrections, and we suggest some
directions for future research with this dataset.Comment: Accepted for publication in the ApJS. 15 pages, 17 JPEG figures, 10
GIF figures. Paper and full resolution figures available at
http://nedwww.ipac.caltech.edu/level5/Kuchinski/frames.htm
Near-Infrared Properties of Metal-poor Globular Clusters in the Galactic Bulge Direction
Aims. J, H, and K' images obtained from the near-infrared imager CFHTIR on
the Canada-France-Hawaii Telescope are used to derive the morphological
parameters of the red giant branch (RGB) in the near-infrared color-magnitude
diagrams for 12 metal-poor globular clusters in the Galactic bulge direction.
Using the compiled data set of the RGB parameters for the observed 12 clusters,
in addition to the previously studied 5 clusters, we discuss the properties of
the RGB morphology for the clusters and compare them with the calibration
relations for the metal-rich bulge clusters and the metal-poor halo clusters.
Methods. The photometric RGB shape indices such as colors at fixed magnitudes
of MK = MH = (-5.5, -5, -4, and -3), magnitudes at fixed colors of (J - K)o =
(J - H)o = 0.7, and the RGB slope are measured from the fiducial normal points
defined in the near- infrared color-magnitude diagrams for each cluster. The
magnitudes of RGB bump and tip are also estimated from the differential and
cumulative luminosity functions of the selected RGB stars. The derived RGB
parameters have been used to examine the overall behaviors of the RGB
morphology as a function of cluster metallicity. Results. The correlations
between the near-infrared photometric RGB shape indices and the cluster
metallicity for the programme clusters compare favorably with the previous
observational calibration relations for metal-rich clusters in the Galactic
bulge and the metal-poor halo clusters. The observed near-infrared magnitudes
of the RGB bump and tip for the investigated clusters are also in accordance
with the previous calibration relations for the Galactic bulge clusters.Comment: 12 pages, 9 figures, accepted for publication in Astronomy &
Astrophysic
A New Non-Parametric Approach to Galaxy Morphological Classification
We present two new non-parametric methods for quantifying galaxy morphology:
the relative distribution of the galaxy pixel flux values (the Gini coefficient
or G) and the second-order moment of the brightest 20% of the galaxy's flux
(M20). We test the robustness of G and M20 to decreasing signal-to-noise and
spatial resolution, and find that both measures are reliable to within 10% at
average signal-to-noise per pixel greater than 3 and resolutions better than
1000 pc and 500 pc, respectively. We have measured G and M20, as well as
concentration (C), asymmetry (A), and clumpiness (S) in the rest-frame
near-ultraviolet/optical wavelengths for 150 bright local "normal" Hubble type
galaxies (E-Sd) galaxies and 104 0.05 < z < 0.25 ultra-luminous infrared
galaxies (ULIRGs).We find that most local galaxies follow a tight sequence in
G-M20-C, where early-types have high G and C and low M20 and late-type spirals
have lower G and C and higher M20. The majority of ULIRGs lie above the normal
galaxy G-M20 sequence, due to their high G and M20 values. Their high Gini
coefficients arise from very bright nuclei, while the high second-order moments
are produced by multiple nuclei and bright tidal tails. All of these features
are signatures of recent and on-going mergers and interactions. We also find
that in combination with A and S, G is more effective than C at distinguishing
ULIRGs from the "normal" Hubble-types. Finally, we measure the morphologies of
45 1.7 < z < 3.8 galaxies from HST NICMOS observations of the Hubble Deep Field
North. We find that many of the z 2 galaxies possess G and A higher than
expected from degraded images of local elliptical and spiral galaxies, and have
morphologies more like low-redshift single nucleus ULIRGs.Comment: 48 pages, 9 tables and 17 figures, accepted to the Astronomical
Journal with minor revision
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