21,914 research outputs found
Discovery of Crystallized Water Ice in a Silhouette Disk in the M43 Region
We present the 1.9--4.2um spectra of the five bright (L<11.2) young stars
associated with silhouette disks with moderate to high inclination angle of
39--80deg in the M42 and M43 regions. The water ice absorption is seen toward
d121-1925 and d216-0939, while the spectra of d182-316, d183-405, and d218-354
show no water ice feature around 3.1um within the detection limits. By
comparing the water ice features toward nearby stars, we find that the water
ice absorption toward d121-1925 and d216-0939 most likely originates from the
foreground material and the surrounding disk, respectively. The angle of the
disk inclination is found to be mainly responsible for the difference of the
optical depth of the water ice among the five young stars. Our results suggest
that there is a critical inclination angle between 65deg and 75deg for the
circumstellar disk where the water ice absorption becomes strong. The average
density at the disk surface of d216-0939 was found to be 6.38x10^(-18) g
cm^(-3). The water ice absorption band in the d216-0939 disk is remarkable in
that the maximum optical depth of the water ice band is at a longer wavelength
than detected before. It indicates that the primary carrier of the feature is
purely crystallized water ice at the surface of the d216-0939 disk with
characteristic size of ~0.8um, which suggests grain growth. This is the first
direct detection of purely crystallized water ice in a silhouette disk.Comment: 28 pages, 8 figures, Accepted by Ap
The MUSE-Wide Survey: A first catalogue of 831 emission line galaxies
We present a first instalment of the MUSE-Wide survey, covering an area of
22.2 arcmin (corresponding to 20% of the final survey) in the
CANDELS/Deep area of the Chandra Deep Field South. We use the MUSE integral
field spectrograph at the ESO VLT to conduct a full-area spectroscopic mapping
at a depth of 1h exposure time per 1 arcmin pointing. We searched for
compact emission line objects using our newly developed LSDCat software based
on a 3-D matched filtering approach, followed by interactive classification and
redshift measurement of the sources. Our catalogue contains 831 distinct
emission line galaxies with redshifts ranging from 0.04 to 6. Roughly one third
(237) of the emission line sources are Lyman emitting galaxies with , only four of which had previously measured spectroscopic redshifts.
At lower redshifts 351 galaxies are detected primarily by their [OII] emission
line (), 189 by their [OIII] line (), and 46 by their H line (). Comparing our spectroscopic redshifts to photometric redshift estimates
from the literature, we find excellent agreement for with a median
of only and an outlier rate of 6%, however a
significant systematic offset of and an outlier rate of 23%
for Ly emitters at . Together with the catalogue we also release
1D PSF-weighted extracted spectra and small 3D datacubes centred on each of the
831 sources.Comment: 24 pages, 14 figures, accepted for publication in A&A, data products
are available for download from http://muse-vlt.eu/science/muse-wide-survey/
and later via the CD
Bayesian nonparametric models for peak identification in MALDI-TOF mass spectroscopy
We present a novel nonparametric Bayesian approach based on L\'{e}vy Adaptive
Regression Kernels (LARK) to model spectral data arising from MALDI-TOF (Matrix
Assisted Laser Desorption Ionization Time-of-Flight) mass spectrometry. This
model-based approach provides identification and quantification of proteins
through model parameters that are directly interpretable as the number of
proteins, mass and abundance of proteins and peak resolution, while having the
ability to adapt to unknown smoothness as in wavelet based methods. Informative
prior distributions on resolution are key to distinguishing true peaks from
background noise and resolving broad peaks into individual peaks for multiple
protein species. Posterior distributions are obtained using a reversible jump
Markov chain Monte Carlo algorithm and provide inference about the number of
peaks (proteins), their masses and abundance. We show through simulation
studies that the procedure has desirable true-positive and false-discovery
rates. Finally, we illustrate the method on five example spectra: a blank
spectrum, a spectrum with only the matrix of a low-molecular-weight substance
used to embed target proteins, a spectrum with known proteins, and a single
spectrum and average of ten spectra from an individual lung cancer patient.Comment: Published in at http://dx.doi.org/10.1214/10-AOAS450 the Annals of
Applied Statistics (http://www.imstat.org/aoas/) by the Institute of
Mathematical Statistics (http://www.imstat.org
Kinematic classifications of local interacting galaxies: implications for the merger/disk classifications at high-z
The classification of galaxy mergers and isolated disks is key for
understanding the relative importance of galaxy interactions and secular
evolution during the assembly of galaxies. The kinematic properties of galaxies
as traced by emission lines have been used to suggest the existence of a
significant population of high-z star-forming galaxies consistent with isolated
rotating disks. However, recent studies have cautioned that post-coalescence
mergers may also display disk-like kinematics. To further investigate the
robustness of merger/disk classifications based on kinematic properties, we
carry out a systematic classification of 24 local (U)LIRGs spanning a range of
galaxy morphologies: from isolated spiral galaxies, ongoing interacting
systems, to fully merged remnants. We artificially redshift the WiFeS
observations of these local (U)LIRGs to z=1.5 to make a realistic comparison
with observations at high-z, and also to ensure that all galaxies have the same
spatial sampling of ~900 pc. Using both kinemetry-based and visual
classifications, we find that the reliability of kinematic classification shows
a strong trend with the interaction stage of galaxies. Mergers with two nuclei
and tidal tails have the most distinct kinematic properties compared to
isolated disks, whereas a significant population of the interacting disks and
merger remnants are indistinguishable from isolated disks. The high fraction of
late-stage mergers showing disk-like kinematics reflects the complexity of the
dynamics during galaxy interactions. However, the exact fractions of
misidentified disks and mergers depend on the definition of kinematic
asymmetries and the classification threshold when using kinemetry-based
classifications. Our results suggest that additional indicators such as
morphologies traced by stars or molecular gas are required to further constrain
the merger/disk classifications at high-z.Comment: 16 pages, 5 figures, ApJ accepte
Blazar Flaring Patterns (B-FlaP): Classifying Blazar Candidates of Uncertain type in the third Fermi-LAT catalog by Artificial Neural Networks
The Fermi Large Area Telescope (LAT) is currently the most important facility
for investigating the GeV -ray sky. With Fermi LAT more than three
thousand -ray sources have been discovered so far. 1144 () of
the sources are active galaxies of the blazar class, and 573 () are
listed as Blazar Candidate of Uncertain type (BCU), or sources without a
conclusive classification. We use the Empirical Cumulative Distribution
Functions (ECDF) and the Artificial Neural Networks (ANN) for a fast method of
screening and classification for BCUs based on data collected at -ray
energies only, when rigorous multiwavelength analysis is not available. Based
on our method, we classify 342 BCUs as BL Lacs and 154 as FSRQs, while 77
objects remain uncertain. Moreover, radio analysis and direct observations in
ground-based optical observatories are used as counterparts to the statistical
classifications to validate the method. This approach is of interest because of
the increasing number of unclassified sources in Fermi catalogs and because
blazars and in particular their subclass High Synchrotron Peak (HSP) objects
are the main targets of atmospheric Cherenkov telescopes.Comment: 18 pages, 17 figures, accepted for publication on MNRA
An information adaptive system study report and development plan
The purpose of the information adaptive system (IAS) study was to determine how some selected Earth resource applications may be processed onboard a spacecraft and to provide a detailed preliminary IAS design for these applications. Detailed investigations of a number of applications were conducted with regard to IAS and three were selected for further analysis. Areas of future research and development include algorithmic specifications, system design specifications, and IAS recommended time lines
The complex galaxy cluster Abell 514: New results obtained with the XMM - Newton satellite
We study the X-ray morphology and dynamics of the galaxy cluster Abell 514.
Also, the relation between the X-ray properties and Faraday Rotation measures
of this cluster are investigated in order to study the connection of magnetic
fields and the intra-cluster medium. We use two combined XMM - Newton pointings
that are split into three distinct observations. The data allow us to evaluate
the overall cluster properties like temperature and metallicity with high
accuracy. Additionally, a temperature map and the metallicity distribution are
computed, which are used to study the dynamical state of the cluster in detail.
Abell 514 represents an interesting merger cluster with many substructures
visible in the X-ray image and in the temperature and abundance distributions.
The new XMM - Newton data of Abell 514 confirm the relation between the X-ray
brightness and the sigma of the Rotation Measure (S_X - sigma_RM relation)
proposed by Dolag et al. (2001).Comment: 9 pages, 13 figures, accepted for publication in A&
Signal estimation in cognitive satellite networks for satellite-based industrial internet of things
Satellite industrial Internet of Things (IIoT) plays an important role in industrial manufactures without requiring the support of terrestrial infrastructures. However, due to the scarcity of spectrum resources, existing satellite frequency bands cannot satisfy the demand of IIoT, which have to explore other available spectrum resources. Cognitive satellite networks are promising technologies and have the potential to alleviate the shortage of spectrum resources and enhance spectrum efficiency by sharing both spectral and spatial degrees of freedom. For effective signal estimations, multiple features of wireless signals are needed at receivers, the transmissions of which may cause considerable overhead. To mitigate the overhead, part of parameters, such as modulation order, constellation type, and signal to noise ratio (SNR), could be obtained at receivers through signal estimation rather than transmissions from transmitters to receivers. In this article, a grid method is utilized to process the constellation map to obtain its equivalent probability density function. Then, binary feature matrix of the probability density function is employed to construct a cost function to estimate the modulation order and constellation type for multiple quadrature amplitude modulation (MQAM) signal. Finally, an improved M 2 M ∞ method is adopted to realize the SNR estimation of MQAM. Simulation results show that the proposed method is able to accurately estimate the modulation order, constellation type, and SNR of MQAM signal, and these features are extremely useful in satellite-based IIoT
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