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Start Over Author "Naylor, D. A." Topic astrophysics
8 results on '"Naylor, D. A."'

1. The James Clerk Maxwell Telescope Legacy Survey of Nearby Star-forming Regions in the Gould Belt

Author

Ward-Thompson, D., Di Francesco, J., Hatchell, J., Hogerheijde, M. R., Bastien, P., Basu, S., Bonnell, I., Bowey, J., Brunt, C., Buckle, J., Butner, H., Cavanagh, B., Chrysostomou, A., Curtis, E., Davis, C. J., Dent, W. R. F., van Dishoeck, E., Edmunds, M. G., Fich, M., Fiege, J., Fissel, L., Friberg, P., Friesen, R., Frieswijk, W., Fuller, G. A., Gosling, A., Graves, S., Greaves, J. S., Helmich, F., Hills, R. E., Holland, W. S., Houde, M., Jayawardhana, R., Johnstone, D., Joncas, G., Kirk, H., Kirk, J. M., Knee, L. B. G., Matthews, B., Matthews, H., Matzner, C., Moriarty-Schieven, G. H., Naylor, D., Nutter, D., Padman, R., Plume, R., Rawlings, J. M. C., Redman, R. O., Reid, M., Richer, J. S., Shipman, R., Simpson, R. J., Spaans, M., Stamatellos, D., Tsanis, Y., Viti, S., Weferling, B., White, G. J., Whitworth, A. P., Wouterloot, J., Yates, J., and Zhu, M.

Subjects
Astrophysics
Abstract

This paper describes a James Clerk Maxwell Telescope (JCMT) legacy survey that has been awarded roughly 500 hrs of observing time to be carried out from 2007 to 2009. In this survey we will map with SCUBA-2 (Submillimetre Common User Bolometer Array 2) almost all of the well-known low-mass and intermediate-mass star-forming regions within 0.5 kpc that are accessible from the JCMT. Most of these locations are associated with the Gould Belt. From these observations we will produce a flux-limited snapshot of star formation near the Sun, providing a legacy of images, as well as point-source and extended-source catalogues, over almost 700 square degrees of sky. The resulting images will yield the first catalogue of prestellar and protostellar sources selected by submillimetre continuum emission, and should increase the number of known sources by more than an order of magnitude. We will also obtain CO maps with the array receiver HARP (Heterodyne Array Receiver Programme), in three CO isotopologues, of a large typical sample of prestellar and protostellar sources. We will then map the brightest hundred sources with the SCUBA-2 polarimeter (POL-2), producing the first statistically significant set of polarization maps in the submillimetre. The images and source catalogues will be a powerful reference set for astronomers, providing a detailed legacy archive for future telescopes, including ALMA, Herschel and JWST., Comment: 60 page manuscript, inc. 18 figures. Accepted by PASP

Published
2007
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2. First ground-based 200-um observing with THUMPER on JCMT - sky characterisation and planet maps

Author

Ward-Thompson, D., Ade, P. A. R., Araujo, H., Coulson, I., Cox, J., Davis, G. R., Evans, Rh., Griffin, M. J., Gear, W. K., Hargrave, P., Hargreaves, P., Hayton, D., Kiernan, B. J., Leeks, S. J., Mauskopf, P., Naylor, D., Potter, N., Rinehart, S. A., Sudiwala, R., Tucker, C. R., Walker, R. J., and Watkin, S. L.

Subjects
Astrophysics
Abstract

We present observations that were carried out with the Two HUndred Micron PhotometER (THUMPER) mounted on the James Clerk Maxwell Telescope (JCMT) in Hawaii, at a wavelength of 200 um (frequency 1.5 THz). The observations utilise a small atmospheric window that opens up at this wavelength under very dry conditions at high-altitude observing sites. The atmosphere was calibrated using the sky-dipping method and a relation was established between the optical depth, tau, at 1.5 THz and that at 225 GHz: tau_1.5THz = (95 +/- 10)*tau_225GHz. Mars and Jupiter were mapped from the ground at this wavelength for the first time, and the system characteristics measured. A noise equivalent flux density (NEFD) of ~65 +/- 10 Jy (1 sigma 1 second) was measured for the THUMPER-JCMT combination, consistent with predictions based upon our laboratory measurements. The main-beam resolution of 14 arcsec was confirmed and an extended error-beam detected at roughly two-thirds of the magnitude of the main beam. Measurements of the Sun allow us to estimate that the fraction of the power in the main beam is ~15%, consistent with predictions based on modelling the dish surface accuracy. It is therefore shown that the sky over Mauna Kea is suitable for astronomy at this wavelength under the best conditions. However, higher or drier sites should have a larger number of useable nights per year., Comment: 7 pages, 8 figures, accepted by MNRAS

Published
2005
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3. Fourier Transform Spectroscopy of the submillimetre continuum emission from hot molecular cores

Author

Friesen, R. K., Johnstone, D., Naylor, D. A., and Davis, G. R.

Subjects
Astrophysics
Abstract

We have used a Fourier Transform Spectrometer on the James Clerk Maxwell Telescope to study the submillimetre continuum emission from dust in three hot molecular cores (HMC). The spectral index beta of the dust emission for these sources has been determined solely within the 30 GHz wide 350 GHz (850 micron) passband to an accuracy comparable to those determined through multi-wavelength observations. We find an average beta = 1.6, in agreement with spectral indices determined from previous submillimetre observations of these sources and with those determined for HMC in general. The largest single source of uncertainty in these results is the variability of the atmosphere at 350 GHz, and with better sky subtraction techniques we show that the dust spectral index can clearly be determined within one passband to high accuracy with a submillimetre FTS. Using an imaging FTS on SCUBA-2, the next generation wide-field submillimetre camera currently under development to replace SCUBA at the JCMT in 2006, we calculate that at 350 GHz it will be possible to determine beta to +/- 0.1 for sources as faint as 400 mJy/beam and to +/- 0.3 for sources as faint as 140 mJy/beam., Comment: 11 pages, 5 figures, accepted for publication in MNRAS

Published
2005
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4. A Long-Term Vision for Space-Based Interferometry

Author

Rinehart, S. A, Arenberg, J, Baines, E, Chen, C. H, Cleeves, L. IIsedore, Creech-Eakman, M. J, Dale, D, Danchi, W, Farrah, D, Juanola-Parramon, R, Kraus, S, Knight, J. S, Lipscy, S, Leisawitz, D. T, MacGregor, M. A, Mennesson, B, Monnier, J, Naylor, D. A, O'Connor, R, Roberge, A, Savini, G, Schmitt, H, Sewilo, M, ten Brummelaar, T. A, van Belle, G, and Yorke, H. W

Subjects
Astrophysics
Abstract

The processes leading to the formation of planets; the extreme physics occurring near the event horizon of black holes; detailed studies of exoplanets through spectral-spatial mapping: new and unique insights into the physical processes involved across nearly the whole gamut of astrophysics await discovery at small angular scales. The fine spatial resolution needed to explore these processes, however, lies beyond the capabilities of current astronomical facilities and nearly all proposed future facilities. Interferometers can crack this angular resolution problem, and space-based interferometry missions promise to explore entirely new regions of scientific phase space, providing unique new insights into the physical processes lurking at small angular scales.

Published
2019

5. First results of Herschel/PACS observations of Neptune

Author

Lellouch, E., Hartogh, P., Feuchtgruber, H., Vandenbussche, B., de Graauw, Th., Moreno, R., Jarchow, C., Cavalie, T., Orton, G., Banaszkiewicz, M., Blecka, M. I., Bockelee-Morvan, D., Crovisier, J., Encrenaz, T., Fulton, T., Kueppers, M., Lara, L. M., Lis, D. C., Medvedev, A. S., Rengel, M., Sagawa, H., Swinyard, B., Szutowicz, S., Bensch, F., Bergin, E., Billebaud, F., Biver, N., Blake, G. A., Blommaert, J. A. D. L., Cernicharo, J., Courtin, R., Davis, G. R., Decin, L., Encrenaz, P., Gonzalez, A., Jehin, E., Kidger, M., Naylor, D., Portyankina, G., Schieder, R., Sidher, S., Thomas, N., de Val-Borro, M., Verdugo, E., Waelkens, C., Aarts, H., Comito, C., Kawamura, J. H., Maestrini, A., Peacocke, T., Teipen, R., Tils, T., Wildeman, K., Walker, H., Blake, G.A., Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max Planck Institute for Solar System Research (MPS), Max-Planck-Gesellschaft, Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1, Jet Propulsion Laboratory (JPL), NASA-California Institute of Technology (CALTECH), Space Research Centre of Polish Academy of Sciences (CBK), Polska Akademia Nauk = Polish Academy of Sciences (PAN), California Institute of Technology (CALTECH), Center for Mathematics and Physics, University of Aizu, Laboratoire Optimisation de la Conception et Ingénierie de l'Environnement (LOCIE), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Instituut voor Sterrenkunde [Leuven], Catholic University of Leuven - Katholieke Universiteit Leuven (KU Leuven), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Departamento de Biologia Celular, Facultad de Biologia, Universidad Complutense de Madrid = Complutense University of Madrid [Madrid] (UCM), European Southern Observatory (ESO), Centre Alexis Vautrin (CAV), Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Sonnensystemforschung = Max Planck Institute for Solar System Research (MPS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Nice Sophia Antipolis (1965 - 2019) (UNS), and Astronomy

Subjects
010504 meteorology & atmospheric sciences, [PHYS.ASTR.EP]Physics [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], [SDU.ASTR.EP]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Earth and Planetary Astrophysics [astro-ph.EP], Flux, FOS: Physical sciences, Astrophysics, 01 natural sciences, Troposphere, Neptune, 0103 physical sciences, Mixing ratio, 010303 astronomy & astrophysics, Stratosphere, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: atmospheres, planets and satellites: composition, Astronomy and Astrophysics, planets and satellites: individual: Neptune, Deuterium, GIANT PLANETS, 13. Climate action, Space and Planetary Science, URANUS, Polar, Millimeter, ABUNDANCE, Earth and Planetary Astrophysics, ATMOSPHERES, techniques: spectroscopic, Astrophysics - Earth and Planetary Astrophysics
Abstract

We report on the initial analysis of a Herschel/PACS full range spectrum of Neptune, covering the 51-220 micrometer range with a mean resolving power of ~ 3000, and complemented by a dedicated observation of CH4 at 120 micrometers. Numerous spectral features due to HD (R(0) and R(1)), H2O, CH4, and CO are present, but so far no new species have been found. Our results indicate that (i) Neptune's mean thermal profile is warmer by ~ 3 K than inferred from the Voyager radio-occultation; (ii) the D/H mixing ratio is (4.5+/-1) X 10**-5, confirming the enrichment of Neptune in deuterium over the protosolar value (~ 2.1 X 10**-5); (iii) the CH4 mixing ratio in the mid stratosphere is (1.5+/-0.2) X 10**-3, and CH4 appears to decrease in the lower stratosphere at a rate consistent with local saturation, in agreement with the scenario of CH4 stratospheric injection from Neptune's warm south polar region; (iv) the H2O stratospheric column is (2.1+/-0.5) X 10**14 cm-2 but its vertical distribution is still to be determined, so the H2O external flux remains uncertain by over an order of magnitude; and (v) the CO stratospheric abundance is about twice the tropospheric value, confirming the dual origin of CO suspected from ground-based millimeter/submillimeter observations., Accepted for publication in Astronomy & Astrophysics (special issue on Herschel first results)

Published
2010

6. Spatial variation of the cooling lines in the Orion Bar from Herschel/PACS.

Author

Bernard-Salas, J., Habart, E., Arab, H., Abergel, A., Dartois, E., Martin, P., Bontemps, S., Joblin, C., White, G. J., Bernard, J.-P., and Naylor, D.

Subjects
HEAT radiation & absorption, ORION (Constellation), CONSTELLATIONS, PHOTOELECTRIC photometry, ASTROPHYSICS
Abstract

Context. The energetics in photo-dissociation regions (PDRs) are mainly regulated by the balance between the heating from the photo-electric effect acting on dust grains, and the cooling via the copious emission of photons in far-infrared lines. The Orion Bar is a luminous and nearby PDR, which presents to the observer an ideal edge-on orientation in which to study this energy balance. Spatially resolved studies of such a nearby system are essential as they enable us to characterise the physical processes that control the energetics of the regions and can serve as templates for distant systems where these processes cannot be disentangled. Aims. We characterise the emission of the far-infrared fine-structure lines of [C II] (158 μm), [OI] (63 and 145 μm), and [N II] (122 μm) that trace the gas local conditions, via spatially resolved observations of the Orion Bar. The observed distribution and variation of the lines are discussed in relation to the underlying geometry and linked to the energetics associated with the Trapezium stars. Methods. Herschel/PACS observations are used to map the spatial distribution of these fine-structure lines across the Bar, with a spatial resolution between 4" and 11" and covering a total square area of about 120" × 105" . The spatial profile of the emission lines are modelled using the radiative transfer code Cloudy. Results. The Herschel observations reveal in unprecedented detail the morphology of the Bar. The spatial distribution of the [CII] line coincides with that of the [OI] lines. The [N II] line peaks closer to the ionising star than the other three lines, but with a small region of overlap. We can distinguish several knots of enhanced emission within the Bar indicating the presence of an inhomogenous and structured medium. The emission profiles cannot be reproduced by a single PDR, clearly indicating that, besides the Bar, there is a significant contribution from additional PDR(s) over the area studied. The combination of both the [NII] and [OI] 145 μm lines can be used to estimate the [C II] emission and distinguish between its ionised or neutral origin.We have calculated how much [CII] emission comes from the neutral and ionised region, and find that at least ∼82% originates from the photo-dissocciation region. Together, the [C II] 158 μm and [OI] 63 and 145 μm lines account for ∼90% of the power emitted by the main cooling lines in the Bar (including CO, H2, etc.), with [O I] 63 μm alone accounting for 72% of the total. [ABSTRACT FROM AUTHOR]

Published
2012
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7. First ground-based 200-μm observing with THUMPER on JCMT – sky characterization and planet maps.

Author

Ward-Thompson, D., Ade, P. A. R., Araujo, H., Coulson, I., Cox, J., Davis, G. R., Evans, Rh., Griffin, M. J., Gear, W. K., Hargrave, P., Hargreaves, P., Hayton, D., Kiernan, B. J., Leeks, S. J., Mauskopf, P., Naylor, D., Potter, N., Rinehart, S. A., Sudiwala, R., and Tucker, C. R.

Subjects
ASTRONOMICAL photometry, ASTROPHYSICS, SPACE sciences, TELESCOPES, PLANETS, SOLAR system
Abstract

We present observations that were carried out with the Two HUndred Micron PhotometER (THUMPER) mounted on the James Clerk Maxwell Telescope (JCMT) in Hawaii, at a wavelength of 200 μm (frequency 1.5 THz). The observations utilize a small atmospheric window that opens up at this wavelength under very dry conditions at high-altitude observing sites. The atmosphere was calibrated using the sky-dipping method and a relation was established between the optical depth, τ, at 1.5 THz and that at 225 GHz: . Mars and Jupiter were mapped from the ground at this wavelength for the first time, and the system characteristics measured. A noise-equivalent flux density (NEFD) of ∼ 65 ± 10 Jy (1σ 1s) was measured for the THUMPER–JCMT combination, consistent with predictions based upon our laboratory measurements. The main beam resolution of 14 arcsec was confirmed and an extended error beam detected at roughly two-thirds of the magnitude of the main beam. Measurements of the Sun allow us to estimate that the fraction of the power in the main beam is ∼15 per cent, consistent with predictions based on modelling the dish surface accuracy. It is therefore shown that the sky over Mauna Kea is suitable for astronomy at this wavelength under the best conditions. However, higher or drier sites should have a larger number of useable nights per year. [ABSTRACT FROM AUTHOR]

Published
2005
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8. Mid-IR cosmological spectrophotometric surveys from space: Measuring AGN and star formation at the cosmic noon with a SPICA-like mission

Author

Eiichi Egami, Sabrina Mordini, Evanthia Hatziminaoglou, Francesco Calura, Cristian Vignali, A. Labiano, Giulia Rodighiero, J. A. Fernández-Ontiveros, L. Bisigello, Luigi Spinoglio, Toru Yamada, David Elbaz, Kotaro Kohno, Lingyu Wang, Hideo Matsuhara, David A. Naylor, Eduardo Gonzalez Alfonso, Helmut Dannerbauer, Almudena Alonso-Herrero, Stephen Serjeant, Lee Armus, Miguel Pereira-Santaella, Asantha Cooray, L. Graziani, Tohru Nagao, Georgios E. Magdis, Matthew A. Malkan, Hidehiro Kaneda, Francesca Pozzi, Carlotta Gruppioni, Peter Roelfsema, Roberto Decarli, Francisco J. Carrera, Alberto Franceschini, Astronomy, Unidad de Excelencia Científica María de Maeztu Instituto de Astrofísica de Cantabria, MDM-2017-0765, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Spignoglio, L. [0000-0001-8840-1551], Fernández Ontiveros, J. A. [0000-0001-9490-899X], Gruppioni, C. [0000-0002-5836-4056], Graziani, L. [0000-0002-9231-1505], Agenzia Spaziale Italiana (ASI), Agencia Estatal de Investigación (AEI), Comunidad de Madrid, Agenzia Spaziale Italiana, Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), European Commission, Ministerio de Economía y Competitividad (España), European Research Council, Spinoglio L., Mordini S., Fernandez-Ontiveros J.A., Alonso-Herrero A., Armus L., Bisigello L., Calura F., Carrera F.J., Cooray A., Dannerbauer H., Decarli R., Egami E., Elbaz D., Franceschini A., Gonzalez Alfonso E., Graziani L., Gruppioni C., Hatziminaoglou E., Kaneda H., Kohno K., Labiano A., Magdis G., Malkan M.A., Matsuhara H., Nagao T., Naylor D., Pereira-Santaella M., Pozzi F., Rodighiero G., Roelfsema P., Serjeant S., Vignali C., Wang L., and Yamada T.

Subjects
active [Galaxies], astro-ph.GA, Extinction (astronomy), galaxies: active, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, 01 natural sciences, Keywords, star formation [Galaxies], Luminosity, spectroscopic [Techniques], infrared: galaxies, galaxies [Infrared], 0103 physical sciences, Galaxy formation and evolution, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), Physics, Luminous infrared galaxy, 010308 nuclear & particles physics, Star formation, infrared: galaxie, Astronomy and Astrophysics, telescopes, evolution [Galaxies], Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, galaxies: evolution, galaxies: star formation, techniques: spectroscopic, Other Physical Sciences, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics, Astronomical and Space Sciences, Telescopes
Abstract

arXiv:2103.03584v1, We use the SPace Infrared telescope for Cosmology and Astrophysics (SPICA) project as a template to demonstrate how deep spectrophotometric surveys covering large cosmological volumes over extended fields (1–15 deg2) with a mid-IR imaging spectrometer (17–36 µm) in conjunction with deep photometry with a far-IR camera, at wavelengths which are not affected by dust extinction can answer the most crucial questions in current galaxy evolution studies. A SPICA-like mission will be able for the first time to provide an unobscured three-dimensional (3D, i.e. x, y, and redshift z) view of galaxy evolution back to an age of the universe of less than ∼ 2 Gyrs, in the mid-IR rest frame. This survey strategy will produce a full census of the Star Formation Rate (SFR) in the universe, using polycyclic aromatic hydrocarbons (PAH) bands and fine-structure ionic lines, reaching the characteristic knee of the galaxy luminosity function, where the bulk of the population is distributed, at any redshift up to z ∼ 3.5. Deep follow-up pointed spectroscopic observations with grating spectrometers onboard the satellite, across the full IR spectral range (17–210 µm), would simultaneously measure Black Hole Accretion Rate (BHAR), from high-ionisation fine-structure lines, and SFR, from PAH and low- to mid-ionisation lines in thousands of galaxies from solar to low metallicities, down to the knee of their luminosity functions. The analysis of the resulting atlas of IR spectra will reveal the physical processes at play in evolving galaxies across cosmic time, especially its heavily dust-embedded phase during the activity peak at the cosmic noon (z ∼ 1–3), through IR emission lines and features that are insensitive to the dust obscuration., LS and JAFO acknowledge financial support by the Agenzia Spaziale Italiana (ASI) under the research contract 2018-31-HH.0. AAH acknowledges support from grants PGC2018-094671-B-I00 (MCIU/AEI/FEDER,UE) and No. MDM-2017-0737 at Unidad de Excelencia María de Maeztu-Centro de Astrobiología (INTACSIC). FJC acknowledges financial support from the Spanish Ministry MCIU under project RTI2018-096686-B-C21 (MCIU/AEI/FEDER/UE), cofunded by FEDER funds and from the Agencia Estatal de Investigación, Unidad de Excelencia María de Maeztu, ref. MDM-2017-0765. HD acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under the 2014 Ramón y Cajal program RYC-2014-15686 and AYA2017-84061-P, the later one co-financed by FEDER (European Regional Development Funds). AL acknowledges the support from Comunidad de Madrid through the Atracción de Talento grant 2017-T1/TIC-5213. MPS acknowledges support from the Comunidad de Madrid, Spain, through Atracción de Talento Investigador Grant 2018-T1/TIC-11035.

Published
2021

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