141 research outputs found
The detection of Class I methanol masers towards regions of low-mass star formation
Six young bipolar outflows in regions of low-to-intermediate-mass star
formation were observed in the 7_0-6_1A+, 8_0-7_1A+, and 5_{-1}-4_0E methanol
lines at 44, 95, and 84 GHz, respectively. Narrow features were detected
towards NGC 1333IRAS4A, HH 25MMS, and L1157 B1. Flux densities of the detected
lines are no higher than 11 Jy, which is much lower than the flux densities of
strong maser lines in regions of high-mass star formation. Analysis shows that
most likely the narrow features are masers.Comment: 12 pages, 6 figures, to be published in Astronomy Report
Dense gas in nearby galaxies XVI. The nuclear starburst environment in NGC4945
A multi-line millimeter-wave study of the nearby starburst galaxy NGC 4945
has been carried out using the Swedish-ESO Submillimeter Telescope (SEST). The
study covers the frequency range from 82 GHz to 354 GHz and includes 80
transitions of 19 molecules. 1.3 mm continuum data of the nuclear source are
also presented. A large number of molecular species indicate the presence of a
prominent high density interstellar gas component characterized by cm. Abundances of molecular species are calculated and
compared with abundances observed toward the starburst galaxies NGC 253 and M
82 and galactic sources. Apparent is an `overabundance' of HNC in the nuclear
environment of NGC 4945. While the HNC/HCN =1--0 line intensity ratio is
0.5, the HNC/HCN abundance ratio is 1. While HCN is subthermally
excited (8 K), CN is even less excited (3--4
K), indicating that it arises from a less dense gas component and that its
=2--1 line can be optically thin even though its =1--0 emission is
moderately optically thick. Overall, fractional abundances of NGC 4945 suggest
that the starburst has reached a stage of evolution that is intermediate
between those observed in NGC 253 and M 82. Carbon, nitrogen, oxygen and sulfur
isotope ratios are also determined. Within the limits of uncertainty, carbon
and oxygen isotope ratios appear to be the same in the nuclear regions of NGC
4945 and NGC 253. High O/O, low O/O and
N/N and perhaps also low S/S ratios appear to be
characteristic properties of a starburst environment in which massive stars
have had sufficient time to affect the isotopic composition of the surrounding
interstellar medium.Comment: 26 pages, 16 figures, accepted bt A&
An atomic and molecular database for analysis of submillimetre line observations
Atomic and molecular data for the transitions of a number of astrophysically
interesting species are summarized, including energy levels, statistical
weights, Einstein A-coefficients and collisional rate coefficients. Available
collisional data from quantum chemical calculations and experiments are
extrapolated to higher energies. These data, which are made publically
available through the WWW at http://www.strw.leidenuniv.nl/~moldata, are
essential input for non-LTE line radiative transfer programs. An online version
of a computer program for performing statistical equilibrium calculations is
also made available as part of the database. Comparisons of calculated emission
lines using different sets of collisional rate coefficients are presented. This
database should form an important tool in analyzing observations from current
and future (sub)millimetre and infrared telescopes.Comment: Accepted for publication in A&A, 14 pages, 5 figure
Methanol maps of low-mass protostellar systems: the Serpens Molecular Core
Observations of Serpens have been performed at the JCMT using Harp-B. Maps
over a 4.5'x5.4' region were made in a frequency window around 338 GHz,
covering the 7-6 transitions of methanol. Emission is extended over each
source, following the column density of H2 but showing up also particularly
strongly around outflows. The rotational temperature is low, 15-20 K, and does
not vary with position within each source. The abundance is typically 10^-9 -
10^-8 with respect to H2 in the outer envelope, whereas "jumps" by factors of
up to 10^2 -10^3 inside the region where the dust temperature exceeds 100 K are
not excluded. A factor of up to ~ 10^3 enhancement is seen in outflow gas. In
one object, SMM4, the ice abundance has been measured to be ~ 3x10^-5 with
respect to H2 in the outer envelope, i.e., a factor of 10^3 larger than the
gas-phase abundance. Comparison with C18O J=3-2 emission shows that strong CO
depletion leads to a high gas-phase abundance of CH3OH not just for the Serpens
sources, but for a larger sample of protostars. The observations illustrate the
large-scale, low-level desorption of CH3OH from dust grains, extending out to
and beyond 7500 AU from each source, a scenario which is consistent with
non-thermal (photo-)desorption from the ice. The observations also illustrate
the usefulness of CH3OH as a tracer of energetic input in the form of outflows,
where methanol is sputtered from the grain surfaces. Finally, the observations
provide further evidence of CH3OH formation through CO hydrogenation proceeding
on grain surfaces in low-mass envelopes.Comment: Accepted for publication in A&A
Molecular excitation in the Interstellar Medium: recent advances in collisional, radiative and chemical processes
We review the different excitation processes in the interstellar mediumComment: Accepted in Chem. Re
Multi-stakeholder consensus on a target product profile for an HIV cure
Developing a cure for HIV is a global priority. Target product profiles are a tool commonly used throughout the drug development process to align interested parties around a clear set of goals or requirements for a potential product. Three distinct therapeutic modalities (combination therapies, ex-vivo gene therapy, and in-vivo gene therapy) for a target product profile for an HIV cure were identified. Using a process of expert face-to-face consultation and an online Delphi consultation, we found a high degree of agreement regarding the criteria for the optimum target product profile. Although the minimum attributes for a cure were debated, the broad consensus was that an acceptable cure need not be as safe and effective as optimally delivered antiretroviral therapy. An intervention that successfully cured a reasonable fraction of adults would be sufficient to advance to the clinic. These target product profiles will require further discussion and ongoing revisions as the field matures
The case for an HIV cure and how to get there
In light of the increasing global burden of new HIV infections, growing financial requirements, and shifting funding landscape, the global health community must accelerate the development and delivery of an HIV cure to complement existing prevention modalities. An effective curative intervention could prevent new infections, overcome the limitations of antiretroviral treatment, combat stigma and discrimination, and provide a sustainable financial solution for pandemic control. We propose steps to plan for an HIV cure now, including defining a target product profile and establishing the HIV Cure Africa Acceleration Partnership (HCAAP), a multidisciplinary public-private partnership that will catalyse and promote HIV cure research through diverse stakeholder engagement. HCAAP will convene stakeholders, including people living with HIV, at an early stage to accelerate the design, social acceptability, and rapid adoption of HIV-cure products
H2CO and CH3OH abundances in the envelopes around low-mass protostars
This paper presents the third in a series of single-dish studies of molecular
abundances in the envelopes around a large sample of 18 low-mass pre- and
protostellar objects. It focuses on typical grain mantle products and organic
molecules, including H2CO, CH3OH and CH3CN. With a few exceptions, all H2CO
lines can be fit by constant abundances of 7e(-11)-8e(-9) throughout the
envelopes if ortho- and para lines are considered independently. The current
observational dataset does not require a large H2CO abundance enhancement in
the inner warm regions, but this can also not be ruled out. Through comparison
of the H2CO abundances of the entire sample, the H2CO ortho-para ratio is
constrained to be 1.6+/-0.3 consistent with thermalization on grains at
temperatures of 10-15 K. The H2CO abundances can be related to the empirical
chemical network established on the basis of our previously reported survey of
other species and is found to be closely correlated with that of the
nitrogen-bearing molecules. These correlations reflect the freeze-out of
molecules at low temperatures and high densities. An improved fit to the data
is obtained with a `drop' abundance structure in which the abundance decrease
when the temperature is lower than the evaporation temperature and the density
high enough so that the timescale for depletion is less than the lifetime of
the core. The derived abundance structures for CH3OH are consistent with a
scenario where CH3OH probes the action of compact outflows on the envelopes,
which is further supported by comparison to high frequency, high excitation CS
J=10-9 and HDO line profiles. The extent to which the outflow dominates the
abundance enhancements compared with the passively heated inner envelope
depends on the filling factors of the two components in the observing beam.Comment: Accepted for publication in A&A. Abstract abridge
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