717 research outputs found
On the association of G343.1-2.3 and PSR 1706-44
The association of G343.1-2.3 and PSR 1706-44 has been controversial from its
first proposal. In this paper we address the difficulties, and argue that the
association is still likely. New evidence comes from images of G343.1-2.3
obtained using the Australia Telescope Compact Array (ATCA), and the pulsar
obtained using the CHANDRA X-ray observatory. Mosaicing was required to cover
the full extent of G343.1-2.3, and we present the polarisation images from this
experiment. Also an X-ray pulsar wind nebula has been found in the archived
CHANDRA observations, with the correct morphology to support the association.
The ATCA observations confirm the much larger extent of the SNR, which now
encompasses the pulsar. The X-ray morphology points back toward the centre of
the SNR, indicating the direction of the proper motion, and that the PSR and
SNR are associated.Comment: 11 pages, 5 figures, submitted to MNRA
Line Ratios Reveal N2H+ Emission Originates Above the Midplane in TW Hydrae
Line ratios for different transitions of the same molecule have long been
used as a probe of gas temperature. Here we use ALMA observations of the N2H+
J~=~1-0 and J~=~4-3 lines in the protoplanetary disk around TW Hya to derive
the temperature at which these lines emit. We find an averaged temperature of
39~K with a one sigma uncertainty of 2~K for the radial range 0.8-2'',
significantly warmer than the expected midplane temperature beyond 0.5'' in
this disk. We conclude that the N2H+ emission in TW Hya is not emitting from
near the midplane, but rather from higher in the disk, in a region likely
bounded by processes such as photodissociation or chemical reprocessing of CO
and N2 rather than freeze out.Comment: Accepted for publication in ApJ Letters, 5 pages, 1 figur
A recent accretion burst in the low-mass protostar IRAS 15398-3359: ALMA imaging of its related chemistry
Low-mass protostars have been suggested to show highly variable accretion
rates through-out their evolution. Such changes in accretion, and related
heating of their ambient envelopes, may trigger significant chemical variations
on different spatial scales and from source-to-source. We present images of
emission from C17O, H13CO+, CH3OH, C34S and C2H toward the low-mass protostar
IRAS 15398-3359 on 0.5" (75 AU diameter) scales with the Atacama Large
Millimeter/submillimeter Array (ALMA) at 340 GHz. The resolved images show that
the emission from H13CO+ is only present in a ring-like structure with a radius
of about 1-1.5" (150-200 AU) whereas the CO and other high dipole moment
molecules are centrally condensed toward the location of the central protostar.
We propose that HCO+ is destroyed by water vapor present on small scales. The
origin of this water vapor is likely an accretion burst during the last
100-1000 years increasing the luminosity of IRAS 15398-3359 by a factor of 100
above its current luminosity. Such a burst in luminosity can also explain the
centrally condensed CH3OH and extended warm carbon-chain chemistry observed in
this source and furthermore be reflected in the relative faintness of its
compact continuum emission compared to other protostars.Comment: Accepted for publication in ApJ Letters; 14 pages, 5 figure
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