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View article: First Detection of CH3OD in Prestellar Cores
First Detection of CH3OD in Prestellar Cores Open
The isotopic ratios of deuterated methanol derived around protostars are commonly used to infer the physical conditions under which they formed in the earlier prestellar stage. However, there is a discrepancy in the ratio of the singly deu…
View article: A Quest for Sulfur-bearing Refractory Species: Identification of CaS in the Interstellar Medium
A Quest for Sulfur-bearing Refractory Species: Identification of CaS in the Interstellar Medium Open
The recent detection of refractory molecules in massive star-forming regions provides a means of probing the innermost regions of disks around massive stars. These detections also make it possible to explore the chemical composition of ref…
View article: Gas phase Elemental abundances in Molecular cloudS (GEMS)
Gas phase Elemental abundances in Molecular cloudS (GEMS) Open
Context . Isotopic ratios have been used as chemical diagnostics to investigate the origin of the material in the Solar System. These isotopic ratios depend on the physical conditions at formation but can be altered during the star formati…
View article: Photodesorption of SO2 and SO from UV-irradiated SO2 ices
Photodesorption of SO2 and SO from UV-irradiated SO2 ices Open
The detection of high gas-phase abundances of Sulfur dioxide (SO$_2$) and sulfur monoxide (SO) in the cold envelope of an intermediate mass protostar suggests that these molecules might form on icy dust grains and subsequently desorb to th…
View article: Photodesorption of SO2 and SO from UV-irradiated SO2 ices
Photodesorption of SO2 and SO from UV-irradiated SO2 ices Open
The detection of high gas-phase abundances of SO2 and SO in the cold envelope of an intermediate mass protostar suggests that these molecules might form on icy dust grains and subsequently desorb to the gas phase by non-thermal desorption …
View article: PDRs4All
PDRs4All Open
Most protoplanetary disks experience a phase in which they are subjected to strong ultraviolet radiation from nearby massive stars. This UV radiation can substantially alter their chemistry by producing numerous radicals and molecular ions…
View article: PRODIGE – envelope to disk with NOEMA
PRODIGE – envelope to disk with NOEMA Open
Context . The 12 C/ 13 C isotope ratio has been derived towards numerous cold clouds (~20-50 K) and a couple of protoplanetary disks and exoplanet atmospheres. However, direct measurements of this ratio in the warm gas (>100 K) around youn…
View article: The Sulfur Plume in the Horsehead Nebula: New Detections of S<sub>2</sub>H, SH<sup>+</sup>, and CO<sup>+</sup>
The Sulfur Plume in the Horsehead Nebula: New Detections of S<sub>2</sub>H, SH<sup>+</sup>, and CO<sup>+</sup> Open
Sulfur is essential for life, but its abundance and distribution in the interstellar medium remain uncertain, with over 90% of sulfur undetected in cold molecular clouds. Sulfur allotropes (S n ) have been proposed as possible reservoirs, …
View article: Decoding the molecular torus of NGC 1068
Decoding the molecular torus of NGC 1068 Open
Context. Previous kinematic analysis of the pc-scale molecular torus in NGC 1068 have revealed a very complex and inhomogeneous system involving several physical components, such as non-circular motions, turbulence, high-velocity outflows,…
View article: Solar C/O ratio in planet-forming gas at 1 au in a highly irradiated disk
Solar C/O ratio in planet-forming gas at 1 au in a highly irradiated disk Open
The chemical composition of exoplanets is thought to be influenced by the composition of the disks in which they form. JWST observations have unveiled a variety of species in numerous nearby disks, showing significant variations in the C/O…
View article: PDRs4All
PDRs4All Open
The infrared emission from polycyclic aromatic hydrocarbons (PAHs), along with emission from atomic carbon and simple hydrocarbons, is a robust tracer of the interaction between stellar far-UV (FUV) radiation and molecular clouds. We prese…
View article: Predicting the detectability of sulphur-bearing molecules in the solid phase with simulated spectra of JWST instruments
Predicting the detectability of sulphur-bearing molecules in the solid phase with simulated spectra of JWST instruments Open
To date, gas phase observations of sulphur in dense interstellar environments have only constrained the molecular carriers of 1% of its predicted cosmic abundance. An additional 5% is known to be locked up in molecular solids in dense clou…
View article: Predicting the detectability of sulphur-bearing molecules in the solid phase with simulated spectra of JWST instruments
Predicting the detectability of sulphur-bearing molecules in the solid phase with simulated spectra of JWST instruments Open
To date, gas phase observations of sulphur in dense interstellar environments have only constrained the molecular carriers of ~1% of its predicted cosmic abundance. An additional ~5% is known to be locked up in molecular solids in dense cl…
View article: Ice origins of OCS and chemistry of CS2-bearing ice mantles
Ice origins of OCS and chemistry of CS2-bearing ice mantles Open
Understanding the formation of carbonyl sulfide (OCS) in interstellar ices is key to constrain the sulfur chemistry in the interstellar medium (ISM), since it is the only ice S-bearing molecule securely detected thus far. Two general pathw…
View article: Ice origins of OCS and chemistry of CS2-bearing ice mantles
Ice origins of OCS and chemistry of CS2-bearing ice mantles Open
Understanding the formation of carbonyl sulfide (OCS) in interstellar ices is key to constrain the sulfur chemistry in the interstellar medium (ISM), since it is the only ice S-bearing molecule securely detected thus far. Two general pathw…
View article: Sulfur monoxide (SO) as a shock tracer in protoplanetary disks: Case of AB Aurigae
Sulfur monoxide (SO) as a shock tracer in protoplanetary disks: Case of AB Aurigae Open
Context. Sulfur monoxide (SO) is known to be a good shock tracer in molecular clouds and protostar environments, but its abundance is difficult to reproduce, even with state-of-the-art astrochemical models. Aims. We investigate the propert…
View article: Binding Energies and Vibrational Spectral Features of S<sub> n </sub> Species on Amorphous Water-ice Mantles: A Quantum Mechanical Study
Binding Energies and Vibrational Spectral Features of S<sub> n </sub> Species on Amorphous Water-ice Mantles: A Quantum Mechanical Study Open
In the denser and colder regions of the interstellar medium (ISM), gas-phase sulfur is depleted by 2 or 3 orders of magnitude with respect to its cosmic abundance. Thus, which species are the main carriers of sulfur is an open question. Re…
View article: Formation and desorption of sulphur chains (H2S<i>x</i> and S<i>x</i>) in cometary ice: effects of ice composition and temperature
Formation and desorption of sulphur chains (H2S<i>x</i> and S<i>x</i>) in cometary ice: effects of ice composition and temperature Open
The reservoir of sulphur accounting for sulphur depletion in the gas of dense clouds and circumstellar regions is still unclear. One possibility is the formation of sulphur chains, which would be difficult to detect by spectroscopic techni…
View article: Gas phase Elemental abundances in Molecular cloudS (GEMS)
Gas phase Elemental abundances in Molecular cloudS (GEMS) Open
Context . We explore the chemistry of the most abundant C-, O-, S-, and N-bearing species in molecular clouds, in the context of the IRAM 30 m Large Programme Gas phase Elemental abundances in Molecular Clouds (GEMS). Thus far, we have stu…
View article: A fast neural emulator for interstellar chemistry
A fast neural emulator for interstellar chemistry Open
Astrochemical models are important tools to interpret observations of molecular and atomic species in different environments. However, these models are time-consuming, precluding a thorough exploration of the parameter space, leading to un…
View article: A fast neural emulator for interstellar chemistry
A fast neural emulator for interstellar chemistry Open
Astrochemical models are important tools to interpret observations of molecular and atomic species in different environments. However, these models are time-consuming, precluding a thorough exploration of the parameter space, leading to un…
View article: PDRs4All
PDRs4All Open
Context. Mid-infrared emission features are important probes of the properties of ionized gas and hot or warm molecular gas, which are difficult to probe at other wavelengths. The Orion Bar photodissociation region (PDR) is a bright, nearb…
View article: PDRs4All
PDRs4All Open
Context. One of the main problems in astrochemistry is determining the amount of sulfur in volatiles and refractories in the interstellar medium. The detection of the main sulfur reservoirs (icy H 2 S and atomic gas) has been challenging, …
View article: PRODIGE – envelope to disk with NOEMA
PRODIGE – envelope to disk with NOEMA Open
Context. Complex organic molecules (COMs) have been found toward low-mass protostars, but the origins of the COM emission are still unclear. It can be associated with, for example, hot corinos, outflows, and/or accretion shock and disk atm…
View article: PDRs4All IX. Sulfur elemental abundance in the Orion Bar
PDRs4All IX. Sulfur elemental abundance in the Orion Bar Open
One of the main problems in astrochemistry is determining the amount of sulfur in volatiles and refractories in the interstellar medium. The detection of the main sulfur reservoirs (icy H$_2$S and atomic gas) has been challenging, and esti…
View article: PDRs4All VIII: Mid-IR emission line inventory of the Orion Bar
PDRs4All VIII: Mid-IR emission line inventory of the Orion Bar Open
Mid-infrared emission features probe the properties of ionized gas, and hot or warm molecular gas. The Orion Bar is a frequently studied photodissociation region (PDR) containing large amounts of gas under these conditions, and was observe…
View article: PDRs4All
PDRs4All Open
Context . JWST has taken the sharpest and most sensitive infrared (IR) spectral imaging observations ever of the Orion Bar photodis-sociation region (PDR), which is part of the nearest massive star-forming region the Orion Nebula, and ofte…
View article: Grain growth and its chemical impact in the first hydrostatic core phase
Grain growth and its chemical impact in the first hydrostatic core phase Open
Context. The first hydrostatic core (FHSC) phase is a brief stage in the protostellar evolution that is difficult to detect. Its chemical composition determine that of later evolutionary stages. Numerical simulations are the tool of choice…
View article: Grain growth and its chemical impact in the first hydrostatic core phase
Grain growth and its chemical impact in the first hydrostatic core phase Open
The first hydrostatic core (FHSC) phase is a brief stage in the protostellar evolution that is difficult to detect. Our goal is to characterize the chemical evolution of gas and dust during the formation of the FHSC. Moreover, we are inter…
View article: A far-ultraviolet-driven photoevaporation flow observed in a protoplanetary disk
A far-ultraviolet-driven photoevaporation flow observed in a protoplanetary disk Open
Most low-mass stars form in stellar clusters that also contain massive stars, which are sources of far-ultraviolet (FUV) radiation. Theoretical models predict that this FUV radiation produces photo-dissociation regions (PDRs) on the surfac…