1,048 research outputs found
Detection of a new methanol maser line with ALMA
Aims. We aimed at investigating the structure and kinematics of the gaseous
disk and outflows around the massive YSO S255 NIRS3 in the S255IR-SMA1 dense
clump. Methods. Observations of the S255IR region were carried out with ALMA at
two epochs in the compact and extended configurations. Results. We
serendipitously detected a new, never predicted, bright maser line at about
349.1 GHz, which most probably represents the CHOH A transition. The emission covers most of the 6.7 GHz methanol maser emission
area of almost 1 in size and shows a velocity gradient in the
same sense as the disk rotation. No variability was found on the time interval
of several months. It is classified as Class II maser and probably originates
in a ring at a distance of several hundreds AU from the central star.Comment: 4 pages, 4 figures, accepted by Astronomy and Astrophysic
RadioAstron probes the ultra-fine spatial structure in the HO maser emission in the star forming region W49N
HO maser emission associated with the massive star formation region W49N
were observed with the Space-VLBI mission RadioAstron. The procedure for
processing of the maser spectral line data obtained in the RadioAstron
observations is described. Ultra-fine spatial structures in the maser emission
were detected on space-ground baselines of up to 9.6 Earth diameters. The
correlated flux densities of these features range from 0.1% to 0.6% of the
total flux density. These low values of correlated flux density are probably
due to turbulence either in the maser itself or in the interstellar medium.Comment: Accepted for publication in Advances in Space Researc
The disk-outflow system in the S255IR area of high mass star formation
We report the results of our observations of the S255IR area with the SMA at
1.3 mm in the very extended configuration and at 0.8 mm in the compact
configuration as well as with the IRAM-30m at 0.8 mm. The best achieved angular
resolution is about 0.4 arcsec. The dust continuum emission and several tens of
molecular spectral lines are observed. The majority of the lines is detected
only towards the S255IR-SMA1 clump, which represents a rotating structure
(probably disk) around the young massive star. The achieved angular resolution
is still insufficient for conclusions about Keplerian or non-Keplerian
character of the rotation. The temperature of the molecular gas reaches 130-180
K. The size of the clump is about 500 AU. The clump is strongly fragmented as
follows from the low beam filling factor. The mass of the hot gas is
significantly lower than the mass of the central star. A strong DCN emission
near the center of the hot core most probably indicates a presence of a
relatively cold ( K) and rather massive clump there. High velocity
emission is observed in the CO line as well as in lines of high density tracers
HCN, HCO+, CS and other molecules. The outflow morphology obtained from
combination of the SMA and IRAM-30m data is significantly different from that
derived from the SMA data alone. The CO emission detected with the SMA traces
only one boundary of the outflow. The outflow is most probably driven by jet
bow shocks created by episodic ejections from the center. We detected a dense
high velocity clump associated apparently with one of the bow shocks. The
outflow strongly affects the chemical composition of the surrounding medium.Comment: 19 pages, 23 figures, accepted by The Astrophysical Journa
Asymptotic expansion of the integrated density of states of a two-dimensional periodic Schrodinger operator
We prove the complete asymptotic expansion of the integrated density of
states of a two-dimensional Schrodinger operator with a smooth periodic
potentialComment: 46 pages, 4 figure
Molecular hydrogen in the cosmic recombination epoch
The advent of precise measurements of the cosmic microwave background (CMB)
anisotropies has motivated correspondingly precise calculations of the cosmic
recombination history. Cosmic recombination proceeds far out of equilibrium
because of a "bottleneck" at the level of hydrogen: atoms can only reach
the ground state via slow processes: two-photon decay or Lyman-
resonance escape. However, even a small primordial abundance of molecules could
have a large effect on the interline opacity in the recombination epoch and
lead to an additional route for hydrogen recombination. Therefore, this paper
computes the abundance of the H molecule during the cosmic recombination
epoch. Hydrogen molecules in the ground electronic levels X can
either form from the excited H electronic levels B and
C or through the charged particles H, HeH and H. We
follow the transitions among all of these species, resolving the rotational and
vibrational sub-levels. Since the energies of the
X--B (Lyman band) and X-C
(Werner band) transitions are near the Lyman- energy, the distortion of
the CMB spectrum caused by escaped H Lyman-line photons accelerates both the
formation and the destruction of H due to this channel relative to the
thermal rates. This causes the populations of H molecules in
X energy levels to deviate from their thermal equilibrium
abundances. We find that the resulting H abundance is at
and at , which is too small to have any significant
influence on the recombination history.Comment: 13 pages, 10 figures, to be submitted to PR
Hour-glass magnetic excitations induced by nanoscopic phase separation in cobalt oxides LaSrCoO
The magnetic excitations in the cuprate superconductors might be essential
for an understanding of high-temperature superconductivity. In these cuprate
superconductors the magnetic excitation spectrum resembles an hour-glass and
certain resonant magnetic excitations within are believed to be connected to
the pairing mechanism which is corroborated by the observation of a universal
linear scaling of superconducting gap and magnetic resonance energy. So far,
charge stripes are widely believed to be involved in the physics of hour-glass
spectra. Here we study an isostructural cobaltate that also exhibits an
hour-glass magnetic spectrum. Instead of the expected charge stripe order we
observe nano phase separation and unravel a microscopically split origin of
hour-glass spectra on the nano scale pointing to a connection between the
magnetic resonance peak and the spin gap originating in islands of the
antiferromagnetic parent insulator. Our findings open new ways to theories of
magnetic excitations and superconductivity in cuprate superconductors.Comment: Nature Communications 5, 5731 (2014
Incommensurate spin correlations in highly oxidized cobaltates LaSrCoO
We observe quasi-static incommensurate magnetic peaks in neutron scattering
experiments on layered cobalt oxides La2-xSrxCoO4 with high Co oxidation states
that have been reported to be paramagnetic. This enables us to measure the
magnetic excitations in this highly hole-doped incommensurate regime and
compare our results with those found in the low-doped incommensurate regime
that exhibit hourglass magnetic spectra. The hourglass shape of magnetic
excitations completely disappears given a high Sr doping. Moreover, broad
low-energy excitations are found, which are not centered at the incommensurate
magnetic peak positions but around the quarter-integer values that are
typically exhibited by excitations in the checkerboard charge ordered phase.
Our findings suggest that the strong inter-site exchange interactions in the
undoped islands are critical for the emergence of hourglass spectra in the
incommensurate magnetic phases of La2-xSrxCoO4.Comment: http://www.nature.com/articles/srep25117
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