34 research outputs found
Molecular absorption lines toward star-forming regions : a comparative study of HCO+, HNC, HCN, and CN
Aims. The comparative study of several molecular species at the origin of the
gas phase chemistry in the diffuse interstellar medium (ISM) is a key input in
unraveling the coupled chemical and dynamical evolution of the ISM. Methods.
The lowest rotational lines of HCO+, HCN, HNC, and CN were observed at the
IRAM-30m telescope in absorption against the \lambda 3 mm and \lambda 1.3 mm
continuum emission of massive star-forming regions in the Galactic plane. The
absorption lines probe the gas over kiloparsecs along these lines of sight. The
excitation temperatures of HCO+ are inferred from the comparison of the
absorptions in the two lowest transitions. The spectra of all molecular species
on the same line of sight are decomposed into Gaussian velocity components.
Most appear in all the spectra of a given line of sight. For each component, we
derived the central opacity, the velocity dispersion, and computed the
molecular column density. We compared our results to the predictions of
UV-dominated chemical models of photodissociation regions (PDR models) and to
those of non-equilibrium models in which the chemistry is driven by the
dissipation of turbulent energy (TDR models). Results. The molecular column
densities of all the velocity components span up to two orders of magnitude.
Those of CN, HCN, and HNC are linearly correlated with each other with mean
ratios N(HCN)/N(HNC) = 4.8 1.3 and N(CN)/N(HNC) = 34 12, and more
loosely correlated with those of HCO+, N(HNC)/N(HCO+) = 0.5 0.3,
N(HCN)/N(HCO+) = 1.9 0.9, and N(CN)/N(HCO+) = 18 9. These ratios
are similar to those inferred from observations of high Galactic latitude lines
of sight, suggesting that the gas sampled by absorption lines in the Galactic
plane has the same chemical properties as that in the Solar neighbourhood. The
FWHM of the Gaussian velocity components span the range 0.3 to 3 km s-1 and
those of the HCO+ lines are found to be 30% broader than those of CN-bearing
molecules. The PDR models fail to reproduce simultaneously the observed
abundances of the CN-bearing species and HCO+, even for high-density material
(100 cm-3 < nH < 104 cm-3). The TDR models, in turn, are able to reproduce the
observed abundances and abundance ratios of all the analysed molecules for the
moderate gas densities (30 cm-3 < nH < 200 cm-3) and the turbulent energy
observed in the diffuse interstellar medium. Conclusions. Intermittent
turbulent dissipation appears to be a promising driver of the gas phase
chemistry of the diffuse and translucent gas throughout the Galaxy. The details
of the dissipation mechanisms still need to be investigated
A cyclic bipolar wind in the interacting binary V393 Scorpii
V393 Scorpii is a Double Periodic Variable characterized by a relatively
stable non-orbital photometric cycle of 253 days. Mennickent et al. argue for
the presence of a massive optically thick disc around the more massive B-type
component and describe the evolutionary stage of the system. In this paper we
analyze the behavior of the main spectroscopic optical lines during the long
non-orbital photometric cycle. We study the radial velocity of the donor
determining their orbital elements and find a small but significant orbital
eccentricity (e = 0.04). The donor spectral features are modeled and removed
from the spectrum at every observing epoch using the light-curve model given by
Mennickent et al. We find that the line emission is larger during eclipses and
mostly comes from a bipolar wind. We find that the long cycle is explained in
terms of a modulation of the wind strength; the wind has a larger line and
continuum emissivity on the high state. We report the discovery of highly
variable chromospheric emission in the donor, as revealed by Doppler maps of
the emission lines MgII 4481 and CI 6588. We discuss notable and some novel
spectroscopic features like discrete absorption components, especially visible
at blue-depressed OI 7773 absorption wings during the second half-cycle, Balmer
double emission with V/R-curves showing "Z-type" and "S-type" excursions around
secondary and main eclipse, respectively, and H_beta emission wings extending
up to +- 2000 km/s. We discuss possible causes for these phenomena and for
their modulations with the long cycle.Comment: 19 pages, 22 figures, accepted for publication in MNRA
Nitrogen hydrides in interstellar gas: Herschel/HIFI observations towards G10.6-0.4 (W31C)
The HIFI instrument on board the Herschel Space Observatory has been used to
observe interstellar nitrogen hydrides along the sight-line towards G10.6-0.4
in order to improve our understanding of the interstellar chemistry of
nitrogen. We report observations of absorption in NH N=1-0, J=2-1 and ortho-NH2
1_1,1-0_0,0. We also observed ortho-NH3 1_0-0_0, and 2_0-1_0, para-NH3 2_1-1_1,
and searched unsuccessfully for NH+. All detections show emission and
absorption associated directly with the hot-core source itself as well as
absorption by foreground material over a wide range of velocities. All spectra
show similar, non-saturated, absorption features, which we attribute to diffuse
molecular gas. Total column densities over the velocity range 11-54 km/s are
estimated. The similar profiles suggest fairly uniform abundances relative to
hydrogen, approximately 6*10^-9, 3*10^-9, and 3*10^-9 for NH, NH2, and NH3,
respectively. These abundances are discussed with reference to models of
gas-phase and surface chemistry.Comment: 5 pages, 3 figures, 2 online pages with 2 figures. Accepted for
publication in A&A July 6 (Herschel/HIFI special issue
Comparative study of CH+ and SH+ absorption lines observed towards distant star-forming regions
Aims. The HIFI instrument onboard Herschel has allowed high spectral
resolution and sensitive observations of ground-state transi- tions of three
molecular ions: the methylidyne cation CH+, its isotopologue 13CH+, and
sulfanylium SH+. Because of their unique chemical properties, a comparative
analysis of these cations provides essential clues to the link between the
chemistry and dynamics of the diffuse interstellar medium. Methods. The CH+,
13CH+, and SH+ lines are observed in absorption towards the distant high-mass
star-forming regions (SFRs) DR21(OH), G34.3+0.1, W31C, W33A, W49N, and W51, and
towards two sources close to the Galactic centre, SgrB2(N) and SgrA*+50. All
sight lines sample the diffuse interstellar matter along pathlengths of several
kiloparsecs across the Galactic Plane. In order to compare the velocity
structure of each species, the observed line profiles were deconvolved from the
hyperfine structure of the SH+ transition and the CH+, 13CH+, and SH+ spectra
were independently decomposed into Gaussian velocity components. To analyse the
chemical composition of the foreground gas, all spectra were divided, in a
second step, into velocity intervals over which the CH+, 13CH+, and SH+ column
densities and abundances were derived. Results. SH+ is detected along all
observed lines of sight, with a velocity structure close to that of CH+ and
13CH+. The linewidth distributions of the CH+, SH+, and 13CH+ Gaussian
components are found to be similar. These distributions have the same mean
( ~ 4.2 km s-1) and standard deviation
(\sigma(\delta\u{psion}) ~ 1.5 km s-1). This mean value is also close to that
of the linewidth distribution of the CH+ visible transitions detected in the
solar neighbourhood. We show that the lack of absorption components narrower
than 2 km s-1 is not an artefact caused by noise: the CH+, 13CH+, and SH+ line
profiles are therefore statistically broader than those of most species
detected in absorption in diffuse interstellar gas (e. g. HCO+, CH, or CN). The
SH+/CH+ column density ratio observed in the components located away from the
Galactic centre spans two orders of magnitude and correlates with the CH+
abundance. Conversely, the ratio observed in the components close to the
Galactic centre varies over less than one order of magnitude with no apparent
correlation with the CH+ abundance. The observed dynamical and chemical
properties of SH+ and CH+ are proposed to trace the ubiquitous process of
turbulent dissipation, in shocks or shears, in the diffuse ISM and the specific
environment of the Galactic centre regions
Nitrogen hydrides in interstellar gas II. Analysis of Herschel/HIFI observations towards W49N and G10.6-0.4 (W31C)
We have used the Herschel-HIFI instrument to observe interstellar nitrogen
hydrides along the sight-lines towards W49N and G10.6-0.4 in order to elucidate
the production pathways leading to nitrogen-bearing species in diffuse gas. All
detections show absorption by foreground material over a wide range of
velocities, as well as absorption associated directly with the hot-core source
itself. As in the previously published observations towards G10.6-0.4, the NH,
NH2 and NH3 spectra towards W49N show strikingly similar and non-saturated
absorption features. We decompose the absorption of the foreground material
towards W49N into different velocity components in order to investigate whether
the relative abundances vary among the velocity components, and, in addition,
we re-analyse the absorption lines towards G10.6-0.4 in the same manner.
Abundances, with respect to molecular hydrogen, in each velocity component are
estimated using CH. The analysis points to a co-existence of the nitrogen
hydrides in diffuse or translucent interstellar gas with a high molecular
fraction. Towards both sources, we find that NH is always at least as abundant
as both o-NH2 and o-NH3, in sharp contrast to previous results for dark clouds.
We find relatively constant N(NH)/N(o-NH3) and N(o-NH2)/N(o-NH3) ratios with
mean values of 3.2 and 1.9 towards W49N, and 5.4 and 2.2 towards G10.6-0.4,
respectively. The mean abundance of o-NH3 is ~2x10^-9 towards both sources. The
nitrogen hydrides also show linear correlations with CN and HNC towards both
sources, and looser correlations with CH. The upper limits on the NH+ abundance
indicate column densities < 2 - 14 % of N(NH). Surprisingly low values of the
ammonia ortho-to-para ratio are found in both sources, ~0.5 - 0.7 +- 0.1. This
result cannot be explained by current models as we had expected to find a value
of unity or higher.Comment: 35 pages, 74 figure
A search for diffuse bands in the circumstellar envelopes of post-AGB stars
In this work we present the results of a systematic search for diffuse bands
(DBs, hereafter) in the circumstellar envelopes of a carefully selected sample
of post-AGB stars. We concentrated on the analysis of 9 of the DBs most
commonly found in the interstellar medium. The strength of these features is
determined using high resolution optical spectroscopy and the results obtained
are compared with literature data on field stars affected only by interstellar
reddening. Based on the weak features observed in the subsample of post-AGB
stars dominated by circumstellar reddening we conclude that the carrier(s) of
these DBs must not be present in the circumstellar environment of these
sources, or at least not under the excitation conditions in which DBs are
formed. The conclusion is applicable to all the post-AGB stars studied,
irrespective of the dominant chemistry or the spectral type of the star
considered. A detailed radial velocity analysis of the features observed in
individual sources confirms this result, as the Doppler shifts measured are
found to be consistent with an interstellar origin.Comment: Accepted for A&
CH abundance gradient in TMC-1
We observed the 9-cm Lambda-doubling lines of CH along the dense filament of
TMC-1. The CH column densities were compared with the total H2 column densities
derived using the 2MASS NIR data and previously published SCUBA maps and with
OH column densities derived using previous observations with Effelsberg. We
also modelled the chemical evolution of TMC-1 adopting physical conditions
typical of dark clouds using the UMIST Database for Astrochemistry gas-phase
reaction network to aid the interpretation of the observed OH/CH abundance
ratios. The CH column density has a clear peak in the vicinity of the
cyanopolyyne maximum of TMC-1. The fractional CH abundance relative to H2
increases steadily from the northwestern end of the filament where it lies
around 1.0e-8, to the southeast where it reaches a value of 2.0e-8. The OH and
CH column densities are well correlated, and we obtained OH/CH abundance ratios
of ~ 16 - 20. These values are clearly larger than what has been measured
recently in diffuse interstellar gas and is likely to be related to C to CO
conversion at higher densities. The good correlation between CH and OH can be
explained by similar production and destruction pathways. We suggest that the
observed CH and OH abundance gradients are mainly due to enhanced abundances in
a low-density envelope which becomes more prominent in the southeastern part
and seems to continue beyond the dense filament. An extensive envelope probably
signifies an early stage of dynamical evolution, and conforms with the
detection of a large CH abundance in the southeastern part of the cloud. The
implied presence of other simple forms of carbon in the gas phase provides a
natural explanation for the observation of "early-type" molecules in this
region.Comment: 12 pages, 16 figure
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Landscapes of cellular phenotypic diversity in breast cancer xenografts and their impact on drug response
Funder: Cancer Research UK (CRUK); doi: https://doi.org/10.13039/501100000289Funder: AstraZeneca; doi: https://doi.org/10.13039/100004325Abstract: The heterogeneity of breast cancer plays a major role in drug response and resistance and has been extensively characterized at the genomic level. Here, a single-cell breast cancer mass cytometry (BCMC) panel is optimized to identify cell phenotypes and their oncogenic signalling states in a biobank of patient-derived tumour xenograft (PDTX) models representing the diversity of human breast cancer. The BCMC panel identifies 13 cellular phenotypes (11 human and 2 murine), associated with both breast cancer subtypes and specific genomic features. Pre-treatment cellular phenotypic composition is a determinant of response to anticancer therapies. Single-cell profiling also reveals drug-induced cellular phenotypic dynamics, unravelling previously unnoticed intra-tumour response diversity. The comprehensive view of the landscapes of cellular phenotypic heterogeneity in PDTXs uncovered by the BCMC panel, which is mirrored in primary human tumours, has profound implications for understanding and predicting therapy response and resistance