Chemical Composition of Comets C/2021 A1 (Leonard) and C/2022 E3 (ZTF) From Radio Spectroscopy and the Abundance of HCOOH and HNCO in Comets
We present the results of a molecular survey of long period comets C/2021 A1 (Leonard) and C/2022 E3 (ZTF). Comet C/2021 A1 was observed with the IRAM 30-m radio telescope in November-December 2021 before perihelion when it was closest to the Earth.
We observed C/2022 E3 in January-February 2023 with the Odin 1-m space telescope and IRAM 30-m, shortly after its perihelion, and when it was closest to the Earth. Snapshots were obtained during 12-16 November 2021 period for comet C/2021 A1. Spectral surveys were undertaken over the 8-13 December 2021 period for comet C/2021 A1 (8, 16, and 61 GHz bandwidth in the 3 mm, 2 mm, and 1 mm window) and over the 3-7 February 2023 period for comet C/2022 E3 (25 and 61 GHz at 2 and 1mm).
We report detections of 14 molecular species (HCN, HNC, CH3CN, HNCO, NH2CHO, CH3OH, H2CO, HCOOH, CH3CHO, H2S, CS, OCS, C2H5OH and aGg-(CH2OH)2 ) in both comets plus HC3N and CH2OHCHO marginally detected in C/2021 A1 and CO and H2O (with Odin detected in C/2022 E3. The spatial distribution of several species is investigated. Significant upper limits on the abundances of other molecules and isotopic ratios are also presented.
The activity of comet C/2021 A1 did not vary significantly between 13 November and 13 December 2021. Short-term variability in the outgassing of comet C/2022 E3 on the order of +-20% is present and possibly linked to its 8h rotation period. Both comets exhibit rather low abundances relative to water for volatiles species such as CO (< 2%) and H2S (0.15%). Methanol is also rather depleted in comet C/2021 A1 (0.9%).
Following their revised photo-destruction rates, HNCO and HCOOH abundances in comets have been reevaluated. Both molecules are relatively enriched in these two comets (0.2% relative to water). We cannot exclude that these species could be produced by the dissociation of ammonium salts.
N. Biver (1), D. Bockelee-Morvan (1), B. Handzlik (2), Aa. Sandqvist (3), J. Boissier (4), M. N. Drozdovskaya (5), R. Moreno (1), J. Crovisier (1), D. C. Lis (6), M. Cordiner (7, 8), S. Milam (7), N. X. Roth (7, 9), B. P. Bonev (9), N. Dello Russo (10), R. Vervack (10), C. Opitom (11), H. Kawakita (12) ((1) LESIA, Observatoire de Paris, PSL Research University, CNRS, Sorbonne Universite, Universite Paris-Cite, Meudon, France (2) Astronomical Observatory, Jagiellonian University, Krakow, Poland (3) Stockholm Observatory, Stockholm University, Sweden (4) IRAM, Saint Martin d Heres, France (5) Physikalish-Meteorologisches Observatorium Davos und Weltstrahlungszentrum (PMOD/WRC), Davos Dorf, Switzerland (6) Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA (7) Solar System Exploration Division, Astrochemistry Laboratory Code 691, NASA-GSFC, Greenbelt, MD, USA (8) Department of Physics, Catholic University of America, Washington, DC, USA (9) Department of Physics, American University, Washington, DC, USA (10) Johns Hopkins University Applied Physics Laboratory, MD, USA (11) Institute for Astronomy, University of Edinburgh, Royal Observatory, UK 12 Koyama Astronomical Observatory, Kyoto Sangyo University, Japan)
Comments: To be published in Astronomy & Astrophysics
Subjects: Earth and Planetary Astrophysics (astro-ph.EP)
Cite as: arXiv:2408.10759 [astro-ph.EP] (or arXiv:2408.10759v1 [astro-ph.EP] for this version)
https://doi.org/10.48550/arXiv.2408.10759
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Submission history
From: Nicolas Biver
[v1] Tue, 20 Aug 2024 11:49:03 UTC (2,418 KB)
https://arxiv.org/abs/2408.10759
Astrobiology, Astrochemistry,
