A5067537221- Astrophysics and Star Formation Studies
- Stellar, planetary, and galactic studies
- Atmospheric Ozone and Climate
- Astro and Planetary Science
- Molecular Spectroscopy and Structure
- Photocathodes and Microchannel Plates
- Astronomical Observations and Instrumentation
- Astronomy and Astrophysical Research
- Solar and Space Plasma Dynamics
- CCD and CMOS Imaging Sensors
- Spectroscopy and Chemometric Analyses
- Radioactive element chemistry and processing
- Crystallography and molecular interactions
- Galaxies: Formation, Evolution, Phenomena
- Spacecraft and Cryogenic Technologies
- Calibration and Measurement Techniques
- Chemical Synthesis and Characterization
- Advanced Chemical Physics Studies
- Planetary Science and Exploration
- Advanced Statistical Methods and Models
- Gamma-ray bursts and supernovae
- Geophysics and Gravity Measurements
- Maritime and Coastal Archaeology
- Space exploration and regulation
- Atomic and Molecular Physics
Universidad Complutense de Madrid
2016-2024
Spanish National Observatory
2022-2023
Context. Gas phase Elemental abundances in molecular CloudS (GEMS) is an IRAM 30-m Large Program aimed at determining the elemental of carbon (C), oxygen (O), nitrogen (N), and sulfur (S) a selected set prototypical star-forming filaments. In particular, abundance S remains uncertain by several orders magnitude, its determination one most challenging goals this program. Aims. This paper aims to constrain Taurus, Perseus, Orion A based on GEMS database. The regions are prototypes low-mass,...
Context. The Galaxy Evolution Explorer (GALEX) has produced the largest photometric catalogue of ultraviolet (UV) sources. As such, it defined new standard bands for UV photometry: near band (NUV) and far (FUV). However, due to brightness limits, GALEX mission avoided Galactic plane which is crucial astrophysical research future space missions.
Context. The first hydrostatic core (FHSC) phase is a brief stage in the protostellar evolution that difficult to detect. Its chemical composition determine of later evolutionary stages. Numerical simulations are tool choice study these objects. Aims. Our goal characterize gas and dust during formation FHSC. Moreover, we interested analyzing, for time with 3D magnetohydrodynamic (MHD) simulations, role grain growth its chemistry. Methods. We postprocessed 2 × 10 5 tracer particles from...
In the denser and colder regions of interstellar medium (ISM), gas-phase sulfur is depleted by 2 or 3 orders magnitude with respect to its cosmic abundance. Thus, which species are main carriers an open question. Recent studies have proposed S$_n$ as potential reservoirs. Among various allotropes, most stable one S$_8$ ring, detected in asteroid Ryugu Orgueil meteorite. Shorter species, namely S$_3$ S$_4$, been found comet 67P/C-G, but their presence ISM remains elusive. this study, we...
There is growing observational evidence of dust coagulation in the dense filaments within molecular clouds. Infrared observations show that grain size distribution becomes shallower and relative fraction small to large grains decreases as local density increases. Ultraviolet (UV) strength 2175-Å feature, so-called UV bump, also with cloud density. In this paper, we apply technique developed for a study Taurus Orion confirm bump over densest cores well heavily UV-irradiated λ Orionis shell....
Sulphur depletion in the interstellar medium (ISM) is a long-standing issue, as only 1% of its cosmic abundance detected dense molecular clouds (MCs), while it does not appear to be depleted other environments. In addition gas phase species, MCs also contain dust grains, which are irregular, micron-sized, solid aggregates carbonaceous materials and/or silicates. Grains provide surface where species can meet, accrete, and react. Although freeze-out sulphur onto grains could explain depletion,...
Abstract The path to understanding star formation processes begins with the study of molecular clouds. outskirts these clouds are characterized by low column densities that allow penetration ultraviolet radiation, resulting in a nonnegligible ionization fraction and charging small dust grains mixed gas; this diffuse phase is then coupled ambient magnetic field. Despite general assumption gas tightly correlated, several observational theoretical studies have reported variations dust-to-gas...
The first hydrostatic core (FHSC) phase is a brief stage in the protostellar evolution that difficult to detect. Our goal characterize chemical of gas and dust during formation FHSC. Moreover, we are interested analyzing, for time with 3D magnetohydrodynamic (MHD) simulations, role grain growth its chemistry. We postprocessed $2\times10^{5}$ tracer particles from $\texttt{RAMSES}$ non-ideal MHD simulation using codes $\texttt{NAUTILUS}$ $\texttt{SHARK}$ follow chemistry throughout...
(Abridged) We explore the chemistry of most abundant C, O, S, and N bearing species in molecular clouds, context IRAM 30 m Large Programme Gas phase Elemental abundances Molecular Clouds (GEMS). In this work, we aim to assess limitations introduced observational works when a uniform density is assumed along line sight for fitting observations, developing very simple numerical model turbulent box. perform MHD simulation order reproduce steady-state box with properties typical filament before...
Context. The observational detection of some metastable isomers in the interstellar medium with abundances comparable to those most stable isomer, or even when isomer is not detected, highlights importance non-equilibrium chemistry. This challenges our understanding chemistry and shows need study isomeric forms molecular species constrain chemical processes occurring medium. Aims. Our goal through sulphur pair HNCS HSCN, since HSCN has been observed regions where its HNCS/HSCN ratio seems...
The observational detection of some metastable isomers in the interstellar medium with abundances comparable to those most stable isomer, or even when isomer is not detected, highlights importance non-equilibrium chemistry. This challenges our understanding We present a chemical study through sulphur pair HNCS and HSCN, since HSCN has been observed regions where its HNCS/HSCN ratio seems significantly vary from cold warm regions. have used Nautilus code model formation destruction paths...
Abstract In the current era when access to space is becoming easier and at a lower cost thanks standardised cubesat technology, numerous missions are expected be launched observe, particularly, ultraviolet wavelengths. Given reduced dimensions of telescope that can carry, most these will focused on photometric surveys sample targets interest, therefore each mission define their own bands according scientific objectives orbital constraints. However, in order provide coherent view sky, data...
Context. Determining a complete census of young stars in any star forming region is challenge even for the nearest and best-observed molecular clouds, such as Taurus-Auriga (TAMC). Deep surveys at infrared (IR) X-ray wavelengths astrometric using Gaia DR2 DR3 have been carried out to detect sparse population constrain low-mass end initial mass function. These compilations resulted lists more than 500 sources, including reliable members association candidates. The information provided by...
Context. Carbon monosulphide (CS) is among the few sulphur-bearing species that have been widely observed in all environments, including most extreme, such as diffuse clouds. Moreover, CS has used a tracer of gas density interstellar medium our Galaxy and external galaxies. Therefore, complete understanding its chemistry environments paramount importance for study matter. Aims. Our group revising rates main formation destruction mechanisms CS. In particular, we focus on those involving...
There is a growing interest in Lunar exploration fed by the perception that Moon can be made accessible to low-cost missions next decade. The on-going projects set communications relay orbit and deep space Gateway, as well spreading of commercial-of-the shelf (COTS) technology for small platforms such cubesats contribute this perception. Small, cubesat size satellites orbiting offer ample opportunities study enjoy an advantage point monitor Solar System large scale interaction between Earth...
Variations in the grain size distribution are to be expected interstellar medium (ISM) due growth and destruction. In this work, we present a dust collision model implemented inside magnetohydrodynamical (MHD) code that takes into account shattering of charged grains given composition (silicate or graphite). We integrate MHD Athena, builds on previous implementation dynamics same code. To demonstrate performance coagulation model, study variations single-sized population with radius 0.05...
We revise the rates of reactions CH + S -> CS H and C_2 C, important formation routes in dark diffuse warm gas. performed ab initio calculations to characterize main features all electronic states correlating open shell reactants. For CH+S we have calculated full potential energy surfaces for lowest doublet reaction rate constant with a quasi-classical method. C_2+S, can only take place through three lower triplet states, which present deep insertion wells. A detailed study long-range...