21 research outputs found
VTSCat - the VERITAS data catalogue
No full textVTSCat is the catalog of high-level data products from all publications of the [VERITAS collaboration](https://veritas.sao.arizona.edu/).
The VTSCat data collection contains:
- high-level data like spectral flux points, light curves, spectral fits in human- and machine-readable yaml and ecsv file format
- tabled data like upper limits tables from dark matter searches or results on the extragalactic background in ecsv file format
- sky maps (wherever available) in FITS file format
This is a pre-release for testing and early publications.
A forthcoming research note will provide more details on the catalog. Please check the README file and all documentation linked to the README.
VTSCat supplements the HEASARC catalogue of VERITAS results (to be published). VTSCat is inspired and derived from [gamma-cat](https://github.com/gammapy/gamma-cat).
If you are a previous VERITAS author and would like to be associated with this repository, please send an email to G. Maier.
Access:
- GitHub: https://github.com/VERITAS-Observatory/VERITAS-VTSCat
References:
- VERITAS: https://veritas.sao.arizona.edu/
- VER Dictionary of Nomenclature: https://cds.u-strasbg.fr/cgi-bin/Dic-Simbad?/17350620
- ICRC 2021 proceedings: https://arxiv.org/abs/2108.06424
New in version v0.8.0:
- 2021/2022 publications
- consistency fixesIf you use this software, please cite it using these metadata
VTSCat: The VERITAS Catalog of Gamma-Ray Observations
No full textVTSCat is the catalog of high-level data products from all publications of the [VERITAS collaboration(https://veritas.sao.arizona.edu/).
The VTSCat data collection contains:
- high-level data like spectral flux points, light curves, spectral fits in human
- and machine-readable yaml and ecsv file format - tabled data like upper limits tables from dark matter searches or results on the extragalactic background in ecsv file format
- sky maps (wherever available) in FITS file format
This is a pre-release for testing and early publications.
A forthcoming research note will provide more details on the catalog.
Please check the README file and all documentation linked to the README. VTSCat supplements the HEASARC catalogue of VERITAS results (to be published). VTSCat is inspired and derived from [gamma-cat](https://github.com/gammapy/gamma-cat). If you are a previous
VERITAS author and would like to be associated with this repository, please send an email to G. Maier.
Access:
- GitHub: https://github.com/VERITAS-Observatory/VERITAS-VTSCat
References:
- VERITAS: https://veritas.sao.arizona.edu/
- VER Dictionary of Nomenclature: https://cds.u-strasbg.fr/cgi-bin/Dic-Simbad?/17350620
- ICRC 2021 proceedings: https://arxiv.org/abs/2108.06424If you use this software, please cite it using these metadata
VTSCat: The VERITAS Catalog of Gamma-Ray Observations
No full text<p>VTSCat is the catalog of high-level data products from all publications of the <a href="https://veritas.sao.arizona.edu/">VERITAS collaboration</a>.</p><p>The VTSCat data collection contains:</p> <ul> <li>high-level data like spectral flux points, light curves, spectral fits in human</li> <li>and machine-readable yaml and ecsv file format</li> <li>tabled data like upper limits tables from dark matter searches or results on the extragalactic background in ecsv file format</li> <li>sky maps (wherever available) in FITS file format</li> </ul> <p>This is a pre-release for testing and early publications.</p> <p>A forthcoming research note will provide more details on the catalog.</p> <p>Please check the README file and all documentation linked to the README. VTSCat supplements the HEASARC catalogue of VERITAS results (to be published).</p> <p>VTSCat is inspired and derived from <a href="https://github.com/gammapy/gamma-cat">gamma-cat</a>.</p> <p>If you are a previous VERITAS author and would like to be associated with this repository, please send an email to G. Maier.</p> <p>Access:</p> <ul> <li>GitHub: <a class="autolink" href="https://github.com/VERITAS-Observatory/VERITAS-VTSCat">https://github.com/VERITAS-Observatory/VERITAS-VTSCat</a></li> </ul> <p>References:</p> <ul> <li> <a class="autolink" href="https://veritas.sao.arizona.edu/">https://veritas.sao.arizona.edu/</a></li> <li>VER Dictionary of Nomenclature: <a class="autolink" href="https://cds.u-strasbg.fr/cgi-bin/Dic-Simbad?/17350620">https://cds.u-strasbg.fr/cgi-bin/Dic-Simbad?/17350620</a></li> <li>ICRC 2021 proceedings: <a class="autolink" href="https://arxiv.org/abs/2108.06424">https://arxiv.org/abs/2108.06424</a></li> </ul>
VERITAS follow-up observation of the BL Lac blazar B2 1811+31 2020 Flare
No full textFull Author List VERITAS Collaboration :- A. Acharyya, C. B. Adams, A. Archer, P. Bangale, J. T. Bartkoske, P. Batista, W. Benbow, J. L. Christiansen, A. J. Chromey, A. Duerr, M. Errando, Q. Feng, G. M. Foote, L. Fortson, A. Furniss, C. Hahn, W. Hanlon, O. Hervet, C. E. Hinrichs, J. Hoang, J. Holder, Z. Hughes, T. B. Humensky, W. Jin, M. N. Johnson, M. Kertzman, M. Kherlakian, D. Kieda, T. K. Kleiner, N. Korzoun, S. Kumar, M. J. Lang, M. Lundy, G. Maier, C. E McGrath, E. T. Meyer, M. J. Millard, C. L. Mooney, P. Moriarty, R. Mukherjee, S. O’Brien, R. A. Ong, N. Park, C. Poggemann, M. Pohl, E. Pueschel, J. Quinn, P. L. Rabinowitz, K. Ragan, P. T. Reynolds, D. Ribeiro, E. Roache, J. L. Ryan, I. Sadeh, A. C. Sadun, L. Saha, M. Santander, G. H. Sembroski, R. Shang, M. Splettstoesser, A. K. Talluri, J. V. Tucci, V. V. Vassiliev, A. Weinstein, D. A. Williams, S. L. Wong, and J. Woo38th International Cosmic Ray Conference (ICRC2023), 26 July - 3 August, 2023, Nagoya, JapanVERITAS is an imaging atmospheric Cherenkov telescope (IACT) array most sensitive to gamma rays in the very-high-energy (VHE) energy band (85 GeV - 50 TeV). As a part of its active galactic nuclei (AGN) program, VERITAS focuses on the identification and follow-up of AGN flares reported by other multiwavelength observatories. Between October 15th and October 19th, 2020, VERITAS followed up on the Fermi-LAT and MAGIC detections of a flare of the intermediate-frequency-peaked BL Lacertae (IBL) object, B2 1811+31, located at a redshift of z=0.117. In this work, we present preliminary scientific results from the analysis of B2 1811+31’s 2020 flare, including the corresponding Fermi-LAT light curve and VERITAS detection analysis.This research is supported by grants from the U.S. Department of Energy Office of Science, the
U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, and by
the Helmholtz Association in Germany. This research used resources provided by the Open Science
Grid, which is supported by the National Science Foundation and the U.S. Department of Energy’s
Office of Science, and resources of the National Energy Research Scientific Computing Center
(NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract
No. DE-AC02-05CH11231. We acknowledge the excellent work of the technical support staff at
the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction
and operation of the instrument.https://pos.sissa.it/444/701
VERITAS Discovery of Very High Energy Gamma-Ray Emission from S3 1227+25 and Multiwavelength Observations
No full textFunding Information: This study was partly based on observations conducted using the 1.8 m Perkins Telescope Observatory (PTO) in Arizona (USA), which is owned and operated by Boston University. The BU group was supported in part by NASA Fermi Guest Investigator grant 80NSSC22K1571. Funding Information: A.A. and M.S. acknowledge support through NASA grants 80NSSC22K1515, 80NSSC22K0950, 80NSSC20K1587, and 80NSSC20K1494 and NSF grant PHY-1914579. Funding Information: This work has made use of data from the Asteroid Terrestrial-impact Last Alert System (ATLAS) project. The ATLAS project is primarily funded to search for near-Earth asteroids through NASA grants NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575; by-products of the NEO search include images and catalogs from the survey area. This work was partially funded by Kepler/K2 grants J1944/80NSSC19K0112 and HST GO-15889 and STFC grants ST/T000198/1 and ST/S006109/1. The ATLAS science products have been made possible through the contributions of the University of Hawaii Institute for Astronomy, the Queens University Belfast, the Space Telescope Science Institute, the South African Astronomical Observatory, and the Millennium Institute of Astrophysics (MAS), Chile. Funding Information: This research has made use of data from the OVRO 40 m monitoring program (Richards et al. ), supported by private funding from the California Institute of Technology and the Max Planck Institute for Radio Astronomy, and by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G and NSF grants AST-0808050 and AST-1109911. Funding Information: This work has made use of data from the Steward Observatory, supported by NASA Fermi Guest Investigator grant NNX12AO93G. Funding Information: S.K. acknowledges support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program under grant agreement No. 771282. Funding Information: This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, and the Smithsonian Institution; by NSERC in Canada; and by the Helmholtz Association in Germany. This research used resources provided by the Open Science Grid, which is supported by the National Science Foundation and the U.S. Department of Energy’s Office of Science, and resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under contract No. DE-AC02-05CH11231. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. Publisher Copyright: © 2023. The Author(s). Published by the American Astronomical Society.We report the detection of very high energy gamma-ray emission from the blazar S3 1227+25 (VER J1230+253) with the Very Energetic Radiation Imaging Telescope Array System (VERITAS). VERITAS observations of the source were triggered by the detection of a hard-spectrum GeV flare on 2015 May 15 with the Fermi-Large Area Telescope (LAT). A combined 5 hr VERITAS exposure on May 16 and 18 resulted in a strong 13? detection with a differential photon spectral index, "= 3.8 ± 0.4, and a flux level at 9% of the Crab Nebula above 120 GeV. This also triggered target-of-opportunity observations with Swift, optical photometry, polarimetry, and radio measurements, also presented in this work, in addition to the VERITAS and Fermi-LAT data. A temporal analysis of the gamma-ray flux during this period finds evidence of a shortest variability timescale of ? obs = 6.2 ± 0.9 hr, indicating emission from compact regions within the jet, and the combined gamma-ray spectrum shows no strong evidence of a spectral cutoff. An investigation into correlations between the multiwavelength observations found evidence of optical and gamma-ray correlations, suggesting a single-zone model of emission. Finally, the multiwavelength spectral energy distribution is well described by a simple one-zone leptonic synchrotron self-Compton radiation model.Peer reviewe
VTSCat: The VERITAS Catalog of Gamma-Ray Observations
No full textVTSCat is the catalog of high-level data products from all publications of the VERITAS collaboration . This is release version v2.0.3 adding publications from end of 2022 to mid of 2023. The VTSCat data collection contains: high-level data like spectral flux points, light curves, spectral fits in human- and machine-readable yaml and ecsv file format tabled data like upper limits tables from dark matter searches or results on the extragalactic background in ecsv file format sky maps (wherever available) in FITS file format A detailed description of VTSCat can be found in A. Acharyya et al 2023 Res. Notes AAS 7 6 . Please check also the README file and all documentation linked to the README. VTSCat supplements the HEASARC catalogue of VERITAS results, accessible through this link . VTSCat is inspired and derived from gamma-cat . If you are a previous VERITAS author and would like to be associated with this repository, please send an email to G. Maier. Access: GitHub: https://github.com/VERITAS-Observatory/VERITAS-VTSCat HEASARC: HEASARC: https://heasarc.gsfc.nasa.gov/W3Browse/all/verimaster.html References: VERITAS: https://veritas.sao.arizona.edu/ VER Dictionary of Nomenclature: https://cds.u-strasbg.fr/cgi-bin/Dic-Simbad?/17350620 ZENODO: https://doi.org/10.5281/zenodo.4723219 HEASARC: https://heasarc.gsfc.nasa.gov/W3Browse/all/verimaster.html Research note A. Acharyya et al 2023 Res. Notes AAS 7 6 ; see also arXiv:2301.04498 ICRC 2021 proceedings: https://arxiv.org/abs/2108.06424 Changes in relation with v2.0.1: fix in CITATION.cf
VTSCat: The VERITAS Catalog of Gamma-Ray Observations
No full textVTSCat is the catalog of high-level data products from all publications of the VERITAS collaboration.
Most recent versions of VTSCat are available through https://doi.org/10.5281/zenodo.6988967
The VTSCat data collection contains:
high-level data like spectral flux points, light curves, spectral fits in human- and machine-readable yaml and ecsv file format
tabled data like upper limits tables from dark matter searches or results on the extragalactic background in ecsv file format
sky maps (wherever available) in FITS file format
The data collection contains results from gamma-ray measurements only. This is a pre-release for testing and early publications.
A forthcoming research note will provide more details on the catalog. Please check the README file and all documentation linked to the README.
VTSCat supplements the HEASARC catalogue of VERITAS results (to be published). VTSCat is inspired and derived from gamma-cat.
If you are a previous VERITAS author and would like to be associated with this repository, please send an email to G. Maier.
Access:
GitHub: https://github.com/VERITAS-Observatory/VERITAS-VTSCat
References:
VERITAS: https://veritas.sao.arizona.edu/
VER Dictionary of Nomenclature: https://cds.u-strasbg.fr/cgi-bin/Dic-Simbad?/1735062
Intravenous Thrombolysis Prior to Endovascular Treatment in Basilar Artery Occlusions: A Patient Pooled Analysis of Four Randomized Controlled Trials
No full textThis study assessed intravenous thrombolysis (IVT) prior to endovascular treatment (EVT) versus EVT alone in patients with basilar artery occlusions (BAO).
This patient-level pooled analysis included data from four randomized controlled trials within the VERITAS collaboration (BEST, BASICS, ATTENTION, and BAOCHE). Patients were stratified into IVT plus EVT and EVT alone. Primary outcome was favorable functional outcome, defined as modified Rankin Scale (mRS) score of 0-3 at 3 months. Secondary outcomes included good functional outcome (mRS 0-2), mortality, and symptomatic intracranial hemorrhage (sICH) rates. Regression analyses were adjusted for covariates identified from baseline differences and univariable analyses. Inverse probability of treatment weighting (IPTW) and propensity score matching (PSM) to balance baseline differences and subgroup analyses were also conducted.
Out of total 988 included patients, 556 patients were allocated for EVT and analyzed. No significant differences were observed between patients treated with or without IVT prior to EVT in terms of mRS 0-3 at 3 months (47 vs 44%, adjusted odds ratio [aOR]:0.88, 95%CI 0.57-1.36), mRS 0-2 (39 vs 32%, aOR:1.22, 95%CI 0.78-1.91), mortality (33 vs 38%, aOR:0.93, 95%CI 0.59-1.44), and sICH rates (6.3 vs 4.9%, aOR:1.87, 95%CI 0.77-4.57). IPTW and PSM analyses yielded consistent results. Subgroup analyses did not reveal any differential treatment effect including time from symptom onset to imaging.
Findings from this patient-level pooled analysis of four randomized controlled trials suggest that bridging IVT over EVT alone was safe but not associated with significant improved outcomes. LEVEL OF EVIDENCE 2B: Level 2b, cohort study of a patient-level meta-analysis of 4 RCT's.
© 2025. The Author(s)
A Multiwavelength Study to Decipher the 2017 Flare of the Blazar OJ 287
No full textAcharyya, A. et al.--Full list of authors: Acharyya, A.; Adams, C. B.; Archer, A.; Bangale, P.; Bartkoske, J. T.; Batista, P.; Benbow, W.; Brill, A.; Caldwell, J. P.; Carini, M.; Christiansen, J. L.; Chromey, A. J.; Errando, M.; Falcone, A.; Feng, Q.; Finley, J. P.; Foote, J.; Fortson, L.; Furniss, A.; Gallagher, G.; Hanlon, W.; Hanna, D.; Hervet, O.; Hinrichs, C. E.; Hoang, J.; Holder, J.; Humensky, T. B.; Jin, W.; Johnson, M. N.; Kaaret, P.; Kertzman, M.; Kherlakian, M.; Kieda, D.; Kleiner, T. K.; Korzoun, N.; Krennrich, F.; Kumar, S.; Lang, M. J.; Lundy, M.; Maier, G.; McGrath, C. E.; Millard, M. J.; Millis, J.; Mooney, C. L.; Moriarty, P.; Mukherjee, R.; O'Brien, S.; Ong, R. A.; Pohl, M.; Pueschel, E.; Quinn, J.; Rabinowitz, P. L.; Ragan, K.; Reynolds, P. T.; Ribeiro, D.; Roache, E.; Ryan, J. L.; Sadeh, I.; Sadun, A. C.; Saha, L.; Santander, M.; Sembroski, G. H.; Shahinyan, K.; Shang, R.; Splettstoesser, M.; Tak, D.; Talluri, A. K.; Tucci, J. V.; Williams, D. A.; Wong, S. L.; VERITAS Collaboration; Jorstad, S. G.; Lico, R.; Lusen, P.; Marscher, A. P.In 2017 February, the blazar OJ 287 underwent a period of intense multiwavelength activity. It reached a new historic peak in the soft X-ray (0.3–10 keV) band, as measured by the Swift X-ray Telescope. This event coincides with a very-high-energy (VHE) γ-ray outburst that led VERITAS to detect emission above 100 GeV, with a detection significance of 10σ (from 2016 December 9 to 2017 March 31). The time-averaged VHE γ-ray spectrum was consistent with a soft power law (Γ = −3.81 ± 0.26) and an integral flux corresponding to ∼2.4% that of the Crab Nebula above the same energy. Contemporaneous data from multiple instruments across the electromagnetic spectrum reveal a complex flaring behavior, primarily in the soft X-ray and VHE bands. To investigate the possible origin of such an event, our study focuses on three distinct activity states: before, during, and after the 2017 February peak. The spectral energy distributions during these periods suggest the presence of at least two nonthermal emission zones, with the more compact one responsible for the observed flare. Broadband modeling results and observations of a new radio knot in the jet of OJ 287 in 2017 are consistent with a flare originating from a strong recollimation shock outside the radio core. © 2024. The Author(s). Published by the American Astronomical Society.VERITAS is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, and by NSERC in Canada. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. O.H. thanks NSF for support under grant PHY-2011420. The authors acknowledge support from the Centre de recherche en astrophysique du Québec, un regroupement stratégique du FRQNT.Peer reviewe
Gamma-ray observations of MAXI J1820+070 during the 2018 outburst
No full textVERITAS Collaboration: H. Abe et al.MAXI J1820+070 is a low-mass X-ray binary with a black hole (BH) as a compact object. This binary underwent an exceptionally bright X-ray outburst from 2018 March to October, showing evidence of a non-thermal particle population through its radio emission during this whole period. The combined results of 59.5 h of observations of the MAXI J1820+070 outburst with the H.E.S.S., MAGIC and VERITAS experiments at energies above 200 GeV are presented, together with Fermi-LAT data between 0.1 and 500 GeV, and multiwavelength observations from radio to X-rays. Gamma-ray emission is not detected from MAXI J1820+070, but the obtained upper limits and the multiwavelength data allow us to put meaningful constraints on the source properties under reasonable assumptions regarding the non-thermal particle population and the jet synchrotron spectrum. In particular, it is possible to show that, if a high-energy (HE) gamma-ray emitting region is present during the hard state of the source, its predicted flux should be at most a factor of 20 below the obtained Fermi-LAT upper limits, and closer to them for magnetic fields significantly below equipartition. During the state transitions, under the plausible assumption that electrons are accelerated up to ∼500 GeV, the multiwavelength data and the gamma-ray upper limits lead consistently to the conclusion that a potential HE and very-HE gamma-ray emitting region should be located at a distance from the BH ranging between 1011 and 1013 cm. Similar outbursts from low-mass X-ray binaries might be detectable in the near future with upcoming instruments such as CTA. © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.MAGIC acknowledgements: MAGIC would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF, MPG, and HGF; the Italian INFN and INAF; the Swiss National Fund SNF; the grants PID2019-104114RB-C31, PID2019-104114RB-C32, PID2019-104114RB-C33, PID2019-105510GB-C31, PID2019-107847RB-C41, PID2019-107847RB-C42, PID2019-107847RB-C44, PID2019-107988GB-C22 funded by MCIN/AEI/ 10.13039/501100011033; the Indian Department of Atomic Energy; the Japanese ICRR, the University of Tokyo, JSPS, and MEXT; the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-400/18.12.2020 and the Academy of Finland grant nr. 320045 is gratefully acknowledged. This work was also been supported by Centros de Excelencia ‘Severo Ochoa’ y Unidades ‘María de Maeztu’ program of the MCIN/AEI/ 10.13039/501100011033 (SEV-2016-0588, SEV-2017-0709, CEX2019-000920-S, CEX2019-000918-M, MDM-2015-0509-18-2) and by the CERCA institution of the Generalitat de Catalunya; by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project uniri-prirod-18-48; by the DFG Collaborative Research Centers SFB1491 and SFB876/C3; the Polish Ministry Of Education and Science grant No. 2021/WK/08; and by the Brazilian MCTIC, CNPq and FAPERJ. H.E.S.S. acknowledgements: the support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the Helmholtz Association, the Alexander von Humboldt Foundation, the French Ministry of Higher Education, Research and Innovation, the Centre National de la Recherche Scientifique (CNRS/IN2P3 and CNRS/INSU), the Commissariat à l’énergie atomique et aux énergies alternatives (CEA), the U.K. Science and Technology Facilities Council (STFC), the Irish Research Council (IRC) and the Science Foundation Ireland (SFI), the Knut and Alice Wallenberg Foundation, the Polish Ministry of Education and Science, agreement no. 2021/WK/06, the South African Department of Science and Technology and National Research Foundation, the University of Namibia, the National Commission on Research, Science & Technology of Namibia (NCRST), the Austrian Federal Ministry of Education, Science and Research and the Austrian Science Fund (FWF), the Australian Research Council (ARC), the Japan Society for the Promotion of Science, the University of Amsterdam and the Science Committee of Armenia grant 21AG-1C085. We appreciate the excellent work of the technical support staff in Berlin, Zeuthen, Heidelberg, Palaiseau, Paris, Saclay, Tübingen and in Namibia in the construction and operation of the equipment. This work benefited from services provided by the H.E.S.S. Virtual Organisation, supported by the national resource providers of the EGI Federation. VERITAS acknowledgements: VERITAS is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, and by the Helmholtz Association in Germany. This research used resources provided by the Open Science Grid, which is supported by the National Science Foundation and the U.S. Department of Energy’s Office of Science, and resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DE-AC02-05CH11231. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. E. Molina acknowledges support from MCIN through grant BES-2016-076342. V. Bosch-Ramon acknowledges financial support from the State Agency for Research of the Spanish Ministry of Science and Innovation under grant PID2019-105510GB-C31 and through the ‘Unit of Excellence María de Maeztu 2020-2023 award to the Institute of Cosmos Sciences (CEX2019-000918-M). V. Bosch-Ramon is Correspondent Researcher of CONICET, Argentina, at the IAR. M. Linares has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No. 101002352). G. Sala acknowledges support from the Spanish MINECO grant PID2020-117252GB-I00.Peer reviewe
