2,673 research outputs found
A Supersymmetry Model of Leptons
If supersymmetry (SUSY) is not for stabilizing the electroweak energy scale,
what is it used for in particle physics? We propose that it is for flavor
problems. A cyclic family symmetry is introduced. Under the family symmetry,
only the -lepton is massive due to the vacuum expectation value (VEV) of
the Higgs field. This symmetry is broken by a sneutrino VEV which results in
the muon mass. The comparatively large sneutrino VEV does not result in a large
neutrino mass due to requiring heavy gauginos. SUSY breaks at a high scale
GeV. The electroweak energy scale is unnaturally small. No
additional global symmetry, like the R-parity, is imposed. Other aspects of the
model are discussed.Comment: 10 pages, no figure, revtex
Energetic radiation and the sulfur chemistry of protostellar envelopes: Submillimeter interferometry of AFGL 2591
CONTEXT: The chemistry in the inner few thousand AU of accreting envelopes
around young stellar objects is predicted to vary greatly with far-UV and X-ray
irradiation by the central star. Aim We search for molecular tracers of
high-energy irradiation by the protostar in the hot inner envelope. METHODS:
The Submillimeter Array (SMA) has observed the high-mass star forming region
AFGL 2591 in lines of CS, SO, HCN, HCN(v2=1), and HC15N with 0.6" resolution at
350 GHz probing radial scales of 600-3500 AU for an assumed distance of 1 kpc.
The SMA observations are compared with the predictions of a chemical model
fitted to previous single-dish observations. RESULTS: The CS and SO main peaks
are extended in space at the FWHM level, as predicted in the model assuming
protostellar X-rays. However, the main peak sizes are found smaller than
modeled by nearly a factor of 2. On the other hand, the lines of CS, HCN, and
HC15N, but not SO and HCN(v2=1), show pedestal emissions at radii of about 3500
AU that are not predicted. All lines except SO show a secondary peak within the
approaching outflow cone. A dip or null in the visibilities caused by a sharp
decrease in abundance with increasing radius is not observed in CS and only
tentatively in SO. CONCLUSIONS: The emission of protostellar X-rays is
supported by the good fit of the modeled SO and CS amplitude visibilities
including an extended main peak in CS. The broad pedestals can be interpreted
by far-UV irradiation in a spherically non-symmetric geometry, possibly
comprising outflow walls on scales of 3500 -- 7000 AU. The extended CS and SO
main peaks suggest sulfur evaporation near the 100 K temperature radius.Comment: Astronomy and Astrophysics, in pres
A non-equilibrium ortho-to-para ratio of water in the Orion PDR
The ortho-to-para ratio (OPR) of HO is thought to be sensitive to the
temperature of water formation. The OPR of HO is thus useful to study the
formation mechanism of water. We investigate the OPR of water in the Orion PDR
(Photon-dominated region), at the Orion Bar and Orion S positions, using data
from {\it Herschel}/HIFI. We detect the ground-state lines of ortho- and
para-HO in the Orion Bar and Orion S and we estimate the column
densities using LTE and non-LTE methods. Based on our calculations, the
ortho-to-para ratio (OPR) in the Orion Bar is 0.1 0.5, which is
unexpectedly low given the gas temperature of 85 K, and also lower than
the values measured for other interstellar clouds and protoplanetary disks.
Toward Orion S, our OPR estimate is below 2. This low OPR at 2 positions in the
Orion PDR is inconsistent with gas phase formation and with thermal evaporation
from dust grains, but it may be explained by photodesorption
Deep Learning for Galaxy Mergers in the Galaxy Main Sequence
Starburst galaxies are often found to be the result of galaxy mergers. As a
result, galaxy mergers are often believed to lie above the galaxy main
sequence: the tight correlation between stellar mass and star formation rate.
Here, we aim to test this claim. Deep learning techniques are applied to images
from the Sloan Digital Sky Survey to provide visual-like classifications for
over 340 000 objects between redshifts of 0.005 and 0.1. The aim of this
classification is to split the galaxy population into merger and non-merger
systems and we are currently achieving an accuracy of 91.5%. Stellar masses and
star formation rates are also estimated using panchromatic data for the entire
galaxy population. With these preliminary data, the mergers are placed onto the
full galaxy main sequence, where we find that merging systems lie across the
entire star formation rate - stellar mass plane.Comment: 4 pages, 1 figure. For Proceedings IAU Symposium No. 34
CH observations toward the Orion Bar
CH is one of the first radicals to be detected in the interstellar
medium. Its higher rotational transitions have recently become available with
the Herschel Space Observatory. We aim to constrain the physical parameters of
the CH emitting gas toward the Orion Bar. We analyse the CH line
intensities measured toward the Orion Bar CO Peak and Herschel/HIFI maps of
CH, CH, and HCO, and a NANTEN map of [CI]. We interpret the observed
CH emission using radiative transfer and PDR models. Five rotational
transitions of CH have been detected in the HIFI frequency range toward the
CO peak. A single component rotational diagram gives a rotation temperature
of ~64 K and a beam-averaged CH column density of 410
cm. The measured transitions cannot be explained by any single parameter
model. According to a non-LTE model, most of the CH column density produces
the lower- CH transitions and traces a warm ( ~ 100-150 K)
and dense ((H)~10-10 cm) gas. A small fraction of the
CH column density is required to reproduce the intensity of the highest-
transitions (=9-8 and N=10-9) originating from a high density
((H)~510 cm) hot ( ~ 400 K) gas. The
total beam-averaged CH column density in the model is 10 cm.
Both the non-LTE radiative transfer model and a simple PDR model representing
the Orion Bar with a plane-parallel slab of gas and dust suggest, that CH
cannot be described by a single pressure component, unlike the reactive ion
CH, which was previously analysed toward the Orion Bar CO peak. The
physical parameters traced by the higher rotational transitions
(=6-5,...,10-9) of CH may be consistent with the edges of dense clumps
exposed to UV radiation near the ionization front of the Orion Bar.Comment: Proposed for acceptance in A&A, abstract abridge
Identifying Galaxy Mergers in Observations and Simulations with Deep Learning
Mergers are an important aspect of galaxy formation and evolution. We aim to
test whether deep learning techniques can be used to reproduce visual
classification of observations, physical classification of simulations and
highlight any differences between these two classifications. With one of the
main difficulties of merger studies being the lack of a truth sample, we can
use our method to test biases in visually identified merger catalogues. A
convolutional neural network architecture was developed and trained in two
ways: one with observations from SDSS and one with simulated galaxies from
EAGLE, processed to mimic the SDSS observations. The SDSS images were also
classified by the simulation trained network and the EAGLE images classified by
the observation trained network. The observationally trained network achieves
an accuracy of 91.5% while the simulation trained network achieves 65.2% on the
visually classified SDSS and physically classified EAGLE images respectively.
Classifying the SDSS images with the simulation trained network was less
successful, only achieving an accuracy of 64.6%, while classifying the EAGLE
images with the observation network was very poor, achieving an accuracy of
only 53.0% with preferential assignment to the non-merger classification. This
suggests that most of the simulated mergers do not have conspicuous merger
features and visually identified merger catalogues from observations are
incomplete and biased towards certain merger types. The networks trained and
tested with the same data perform the best, with observations performing better
than simulations, a result of the observational sample being biased towards
conspicuous mergers. Classifying SDSS observations with the simulation trained
network has proven to work, providing tantalizing prospects for using
simulation trained networks for galaxy identification in large surveys.Comment: Submitted to A&A, revised after first referee report. 20 pages, 22
figures, 14 tables, 1 appendi
Temperatures of dust and gas in S~140
In dense parts of interstellar clouds (> 10^5 cm^-3), dust & gas are expected
to be in thermal equilibrium, being coupled via collisions. However, previous
studies have shown that the temperatures of the dust & gas may remain decoupled
even at higher densities. We study in detail the temperatures of dust & gas in
the photon-dominated region S 140, especially around the deeply embedded
infrared sources IRS 1-3 and at the ionization front. We derive the dust
temperature and column density by combining Herschel PACS continuum
observations with SOFIA observations at 37 m and SCUBA at 450 m. We
model these observations using greybody fits and the DUSTY radiative transfer
code. For the gas part we use RADEX to model the CO 1-0, CO 2-1, 13CO 1-0 and
C18O 1-0 emission lines mapped with the IRAM-30m over a 4' field. Around IRS
1-3, we use HIFI observations of single-points and cuts in CO 9-8, 13CO 10-9
and C18O 9-8 to constrain the amount of warm gas, using the best fitting dust
model derived with DUSTY as input to the non-local radiative transfer model
RATRAN. We find that the gas temperature around the infrared sources varies
between 35 and 55K and that the gas is systematically warmer than the dust by
~5-15K despite the high gas density. In addition we observe an increase of the
gas temperature from 30-35K in the surrounding up to 40-45K towards the
ionization front, most likely due to the UV radiation from the external star.
Furthermore, detailed models of the temperature structure close to IRS 1 show
that the gas is warmer and/or denser than what we model. Finally, modelling of
the dust emission from the sub-mm peak SMM 1 constrains its luminosity to a few
~10^2 Lo. We conclude that the gas heating in the S 140 region is very
efficient even at high densities, most likely due to the deep UV penetration
from the embedded sources in a clumpy medium and/or oblique shocks.Comment: 15 pages, 23 figures, 4 tables, accepted for publication in A&
Електронний путівник і координатор (Завдання та функції інформаційного ресурсу Науково-видавничої ради НАН України «Наукові публікації і видавнича діяльність»)
Purpose: Physical activity (PA) is an important behavior when it comes to preventing or slowing down disablement caused by aging and chronic diseases. It remains unclear whether PA can directly prevent or reduce disability in activities of daily living (ADL). This article presents a meta-analysis of the association between PA and the incidence and progression of basic ADL disability (BADL). Methods: Electronic literature search and cross-referencing of prospective longitudinal studies of PA and BADL in community dwelling older adults (50+) with baseline and follow-up measurements, multivariate analysis and reporting a point estimate for the association. Results: Compared with a low PA, a medium/high PA level reduced the risk of incident BADL disability by 0.51 (95% CI: 0.38, 0.68; p < 001), based on nine longitudinal studies involving 17,000 participants followed up for 3–10 years. This result was independent of age, length of follow-up, study quality, and differences in demographics, health status, functional limitations, and lifestyle. The risk of progression of BADL disability in older adults with a medium/high PA level compared with those with a low PA level was 0.55 (95% CI: 0.42, 0.71; p < 001), based on four studies involving 8500 participants. Discussion: This is the first meta-analysis to show that being physically active prevents and slows down he disablement process in aging or diseased populations, positioning PA as the most effective preventive trategy in preventing and reducing disability, independence and health care cost in aging societies
Observation-assisted optimal control of quantum dynamics
This paper explores the utility of instantaneous and continuous observations
in the optimal control of quantum dynamics. Simulations of the processes are
performed on several multilevel quantum systems with the goal of population
transfer. Optimal control fields are shown to be capable of cooperating or
fighting with observations to achieve a good yield, and the nature of the
observations may be optimized to more effectively control the quantum dynamics.
Quantum observations also can break dynamical symmetries to increase the
controllability of a quantum system. The quantum Zeno and anti-Zeno effects
induced by observations are the key operating principles in these processes.
The results indicate that quantum observations can be effective tools in the
control of quantum dynamics
Detection of interstellar H_2D^+ emission
We report the detection of the 1_{10}-1_{11} ground state transition of
ortho-H_2D^+ at 372.421 GHz in emission from the young stellar object NGC 1333
IRAS 4A. Detailed excitation models with a power-law temperature and density
structure yield a beam-averaged H_2D^+ abundance of 3 x 10^{-12} with an
uncertainty of a factor of two. The line was not detected toward W 33A, GL
2591, and NGC 2264 IRS, in the latter source at a level which is 3-8 times
lower than previous observations. The H_2D^+ data provide direct evidence in
support of low-temperature chemical models in which H_2D^+ is enhanced by the
reaction of H_3^+ and HD. The H_2D^+ enhancement toward NGC 1333 IRAS 4A is
also reflected in the high DCO^+/HCO^+ abundance ratio. Simultaneous
observations of the N_2H^+ 4-3 line show that its abundance is about 50-100
times lower in NGC 1333 IRAS 4A than in the other sources, suggesting
significant depletion of N_2. The N_2H^+ data provide independent lower limits
on the H_3^+ abundance which are consistent with the abundances derived from
H_2D^+. The corresponding limits on the H_3^+$ column density agree with recent
near-infrared absorption measurements of H_3^+ toward W 33A and GL 2591.Comment: Standard AAS LaTeX format (15 pages + 2 figures
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