1,845 research outputs found
Identification of SH ro-vibrational lines in R And
We report the identification of SH ro-vibrational lines in the
published high-resolution infrared spectrum of the S-type star, R And. This is
the first astronomical detection of this molecule. The lines show inverse
P-Cygni profiles, indicating infall motion of the molecular layer due to
stellar pulsation. A simple spherical shell model with a constant infall
velocity is adopted to determine the condition of the layer. It is found that a
single excitation temperature of 2200 K reproduces the observed line
intensities satisfactory. SH is located in a layer from 1.0 to ~1.1 stellar
radii, which is moving inward with a velocity of 9 km s-1. These results are
consistent with the previous measurements of CO transitions. The
estimated molecular abundance SH/H is 1x10^-7, consistent with a thermal
equilibrium calculation.Comment: 10 pages, 2 figures. Accepted for publication in ApJ Letter
Carbon stars in the IRTS survey
We have identified 139 cool carbon stars in the near-infrared
spectro-photometric survey of the InfraRed Telescope in Space (IRTS) from the
conspicuous presence of molecular absorption bands at 1.8, 3.1 and 3.8 microns.
Among them 14 are new, bright (K ~ 4.0-7.0), carbon stars. We find a trend
relating the 3.1 microns band strength to the K-L' color index, which is known
to correlate with mass-loss rate. This could be an effect of a relation between
the depth of the 3.1 microns feature and the degree of development of the
extended stellar atmosphere where dust starts to form.Comment: accepted by the PASP; December 7, 200
An AKARI Search for Intracluster Dust of Globular Clusters
We report the observations of 12 globular clusters with the AKARI/FIS. Our
goal is to search for emission from the cold dust within clusters. We detect
diffuse emissions toward NGC 6402 and 2808, but the IRAS 100-micron maps show
the presence of strong background radiation. They are likely emitted from the
galactic cirrus, while we cannot rule out the possible association of a bump of
emission with the cluster in the case of NGC 6402. We also detect 28 point-like
sources mainly in the WIDE-S images (90 micron). At least several of them are
not associated with the clusters but background galaxies based on some external
catalogs. We present the SEDs by combining the near-and-mid infrared data
obtained with the IRC if possible. The SEDs suggest that most of the point
sources are background galaxies. We find one candidate of the intracluster dust
which has no mid-infrared counterpart unlike the other point-like sources,
although some features such as its point-like appearance should be explained
before we conclude its intracluster origin. For most of the other clusters, we
have confirmed the lack of the intracluster dust. We evaluate upper limits of
the intracluster dust mass to be between 1.0E-05 and 1.0E-03 solar mass
depending on the dust temperature. The lifetime of the intracluster dust
inferred from the upper limits is shorter than 5 Myr (T=70K) or 50 Myr (35K).
Such short lifetime indicates some mechanism(s) are at work to remove the
intracluster dust. We also discuss its impact on the chemical evolution of
globular clusters.Comment: Accepted for publication in PASJ AKARI special issue. 14 pages, 11
figure
AKARI Near- to Mid-Infrared Imaging and Spectroscopic Observations of the Small Magellanic Cloud. I. Bright Point Source List
We carried out a near- to mid-infrared imaging and spectroscopic observations
of the patchy areas in the Small Magellanic Cloud using the Infrared Camera on
board AKARI. Two 100 arcmin2 areas were imaged in 3.2, 4.1, 7, 11, 15, and 24
um and also spectroscopically observed in the wavelength range continuously
from 2.5 to 13.4 um. The spectral resolving power (lambda/Delta lambda) is
about 20, 50, and 50 at 3.5, 6.6 and 10.6 um, respectively. Other than the two
100 arcmin2 areas, some patchy areas were imaged and/or spectroscopically
observed as well. In this paper, we overview the observations and present a
list of near- to mid-infrared photometric results, which lists ~ 12,000
near-infrared and ~ 1,800 mid-infrared bright point sources detected in the
observed areas. The 10 sigma limits are 16.50, 16.12, 13.28, 11.26, 9.62, and
8.76 in Vega magnitudes at 3.2, 4.1, 7, 11, 15, and 24 um bands, respectively.Comment: 16 pages, 7 figures, accepted for publication in PASJ. Full
resolution version is available at
http://www-irc.mtk.nao.ac.jp/%7Eyita/smc20100112.pd
AKARI Detections of Hot Dust in Luminous Infrared Galaxies
We present a new sample of active galactic nuclei (AGNs) identified using the
catalog of the AKARI Mid-infrared(MIR) All-Sky Survey. Our MIR search has an
advantage in detecting AGNs that are obscured at optical wavelengths due to
extinction. We first selected AKARI 9micron excess sources with
F(9micron)/F(K_S)>2 where K_S magnitudes were taken from the Two Micron All Sky
Survey. We then obtained follow-up near-infrared spectroscopy with the
AKARI/IRC, to confirm that the excess is caused by hot dust. We also obtained
optical spectroscopy with the Kast Double Spectrograph on the Shane 3-m
telescope at Lick Observatory. On the basis of on these observations, we
detected hot dust with a characteristic temperature of ~500K in two luminous
infrared galaxies. The hot dust is suspected to be associated with AGNs that
exhibit their nonstellar activity not in the optical, but in the near- and
mid-infrared bands, i.e., they harbor buried AGNs. The host galaxy stellar
masses of 4-6 x 10^9 M_sun are small compared with the hosts in
optically-selected AGN populations. These objects were missed by previous
surveys, demonstrating the power of the AKARI MIR All-Sky Survey to widen AGN
searches to include more heavily obscured objects. The existence of multiple
dusty star clusters with massive stars cannot be completely ruled out with our
current data.Comment: 15 pages, 4 figures, to be published in Astronomy & Astrophysic
Cholinergic Muscarinic Receptor: Biochemical and Light Autoradiographic Localization in the Brain
The muscanmc cholinergic antagonist 3-quinudidinyl benzilate
(QNB) binds avidly but reversibly to the muscarinic cholinergic
receptor of mammalian brain and peripheral tissues. [3H]-QNB
binding provides a simple, sensitive and specific assay for the muscarinic
cholinergic receptor binding. Inhibition of [3H]-QNB binding
to homogenates of brain and guinea pig ileum by muscarinic
drugs correlates with their pharmacologic potencies, while nicotinic
agents and noncholinergic drugs have negligible affinity. The
regional distribution of [3H]-QNB binding throughout rat and monkey
brain parallels to a major extent other cholinergic markers,
suggesting that the majority of cholinergic synapses in the brain
are muscarinic. [3H]-QNB accumulation in various brain regions
after intravenous injection provides a means of labelling the muscarinic
receptor in vivo. By labelling the receptor in vivo, autoradiographic
studies under the light microscope have been performed
to visualize the muscarinic receptor
The time variation in infrared water-vapour bands in Mira variables
The time variation in the water-vapour bands in oxygen-rich Mira variables
has been investigated using multi-epoch ISO/SWS spectra of four Mira variables
in the 2.5-4.0 micron region. All four stars show H2O bands in absorption
around minimum in the visual light curve. At maximum, H2O emission features
appear in the ~3.5-4.0 micronm region, while the features at shorter
wavelengths remain in absorption. These H2O bands in the 2.5-4.0 micron region
originate from the extended atmosphere.
The analysis has been carried out with a disk shape, slab geometry model. The
observed H2O bands are reproduced by two layers; a `hot' layer with an
excitation temperature of 2000 K and a `cool' layer with an excitation
temperature of 1000-1400 K. The radii of the `hot' layer (R_hot) are ~1 R_* at
visual minimum and 2 R_* at maximum, where R_* is a radius of background source
of the model. The time variation of R_hot/R_* from 1 to 2 is attributed to the
actual variation in the radius of the H2O layer. A high H2O density shell
occurs near the surface of the star around minimum, and moves out with the
stellar pulsation. This shell gradually fades away after maximum, and a new
high H2O density shell is formed in the inner region again at the next minimum.
Due to large optical depth of H2O, the near-infrared variability is dominated
by the H2O layer, and the L'-band flux correlates with the area of the H2O
shell. The infrared molecular bands trace the structure of the extended
atmosphere and impose appreciable effects on near-infrared light curve of Mira
variables.Comment: 15 pages, 16 figures, accepted by A&
Quantum deformation of the Dirac bracket
The quantum deformation of the Poisson bracket is the Moyal bracket. We
construct quantum deformation of the Dirac bracket for systems which admit
global symplectic basis for constraint functions. Equivalently, it can be
considered as an extension of the Moyal bracket to second-class constraints
systems and to gauge-invariant systems which become second class when
gauge-fixing conditions are imposed.Comment: 18 pages, REVTe
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