Please use this identifier to cite or link to this item: http://hdl.handle.net/10995/101561
Title: ALMA and ROSINA detections of phosphorus-bearing molecules: The interstellar thread between star-forming regions and comets
Authors: Rivilla, V. M.
Drozdovskaya, M. N.
Altwegg, K.
Caselli, P.
Beltrán, M. T.
Fontani, F.
Van, Der, Tak, F. F. S.
Cesaroni, R.
Vasyunin, A.
Rubin, M.
Lique, F.
Marinakis, S.
Testi, L.
Balsiger, H.
Berthelier, J. J.
De Keyser, J.
Fiethe, B.
Fuselier, S. A.
Gasc, S.
Gombosi, T. I.
Sémon, T.
Tzou, C. -Y.
Issue Date: 2020
Publisher: Oxford University Press
Citation: ALMA and ROSINA detections of phosphorus-bearing molecules: The interstellar thread between star-forming regions and comets / V. M. Rivilla, M. N. Drozdovskaya, K. Altwegg, et al. — DOI 10.1093/mnras/stz3336 // Monthly Notices of the Royal Astronomical Society. — 2020. — Vol. 492. — Iss. 1. — P. 1180-1198.
Abstract: To understand how phosphorus (P)-bearing molecules are formed in star-forming regions, we have analysed the Atacama Large Millimeter/Submillimeter Array (ALMA) observations of PN and PO towards the massive star-forming region AFGL 5142, combined with a new analysis of the data of the comet 67P/Churyumov-Gerasimenko taken with the Rosetta Orbiter Spectrometer for Ion and NeutralAnalysis (ROSINA) instrument onboard Rosetta. TheALMA maps show that the emission of PN and PO arises from several spots associated with lowvelocity gas with narrow linewidths in the cavity walls of a bipolar outflow. PO is more abundant than PN in most of the spots, with the PO/PN ratio increasing as a function of the distance to the protostar. Our data favour a formation scenario in which shocks sputter phosphorus from the surface of dust grains, and gas-phase photochemistry induced by UV photons from the protostar allows efficient formation of the two species in the cavity walls. Our analysis of the ROSINA data has revealed that PO is the main carrier of P in the comet, with PO/PN > 10. Since comets may have delivered a significant amount of prebiotic material to the early Earth, this finding suggests that PO could contribute significantly to the phosphorus reservoir during the dawn of our planet. There is evidence that PO was already in the cometary ices prior to the birth of the Sun, so the chemical budget of the comet might be inherited from the natal environment of the Solar system, which is thought to be a stellar cluster including also massive stars. © 2019 The Author(s).
Keywords: ASTROCHEMISTRY
COMETS: GENERAL
ISM: MOLECULES
MOLECULAR DATA
STARS: FORMATION
URI: http://hdl.handle.net/10995/101561
Access: info:eu-repo/semantics/openAccess
SCOPUS ID: 85079445566
PURE ID: 12246018
524123cf-f856-4457-a1f6-1d618f929702
ISSN: 358711
DOI: 10.1093/mnras/stz3336
metadata.dc.description.sponsorship: We thank the anonymous referee for her/his instructive comments and suggestions. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.01071.S ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSC and ASIAA (Taiwan), and KASI (Republic of Korea), in co-operation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. Data from ROSINA, an instrument part of Rosettamission, were used in this work. Rosetta is a European Space Agency (ESA) mission with contributions from its member states and NASA. We acknowledge herewith the work of the entire ESA Rosetta team over the last 20 yr. This research utilized Queen Mary’s MidPlus computational facilities, supported by QMUL ResearchIT, http://doi.org/10.5281/zenodo.438045. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 664931. MND acknowledges the financial support of the SNSF Ambizione grant 180079, the Center for Space and Habitability (CSH) Fellowship, and the IAU Gruber Foundation Fellowship. The work by AV is supported by the Latvian Council of Science via the project lzp-2018/1-0170. MR acknowledges the support of the State of Bern, the Swiss National Science Foundation (SNSF; 200021–165869 and 200020–182418), the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract number 16.0008-2, and the PRODEX Programme of the European Space Agency.
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