Dust mass distribution around comet 67P/Churyumov–Gerasimenko determined via parallax measurements using Rosetta's OSIRIS cameras

Theresa Ott 1 Esther Drolshagen 2 Detlef Koschny 3, 4 Carsten Güttler 5 Cécilia Tubiana 5 Elisa Frattin 6, 7 Jessica Agarwal 5 Holger Sierks 5 Ivano Bertini 7 Cesare Barbieri 7 Philippe L. Lamy 8 Rafael Rodrigo 9, 10 Hans Rickman 11, 12 Michael F. A’hearn 5, 13, 14 Maria Antonella Barucci 15 Jean-Loup Bertaux 16 Steve Boudreault 5 Gabriele Cremonese 6 Vania Da Deppo 17 Björn Davidsson 14 Stefano Debei 18 Mariolino de Cecco 19 Jakob Deller 5 Clément Feller 15 Sonia Fornasier 15 Marco Fulle 20 Bernhard Geiger 21 Adeline Gicquel 5 Olivier Groussin 8 Pedro J. Gutiérrez 22 Marc Hofmann 5 Stubbe F. Hviid 23 Wing-Huen Ip 24, 25 Laurent Jorda 8 Horst Uwe Keller 26, 23 Jörg Knollenberg 23 Gabor Kovacs 5 J.-Rainer Kramm 5 Ekkehard Kührt 23 Michael Küppers 21 Luisa M. Lara 22 Monica Lazzarin 7 Zhong-Yi Lin 25 José J. López-Moreno 22 Francesco Marzari 7 Stefano Mottola 23 Giampiero Naletto 27, 17, 28 Nilda Oklay 23 Maurizio Pajola 29 X. Shi 5 Nicolas Thomas 30 Jean-Baptiste Vincent 23 Björn Poppe 2
Abstract : The OSIRIS (optical, spectroscopic and infrared remote imaging system) instrument on board the ESA Rosetta spacecraft collected data of 67P/Churyumov–Gerasimenko for over 2 yr. OSIRIS consists of two cameras, a Narrow Angle Camera and a Wide Angle Camera. For specific imaging sequences related to the observation of dust aggregates in 67P's coma, the two cameras were operating simultaneously. The two cameras are mounted 0.7 m apart from each other, as a result this baseline yields a parallax shift of the apparent particle trails on the analysed images directly proportional to their distance. Thanks to such shifts, the distance between observed dust aggregates and the spacecraft was determined. This method works for particles closer than 6000 m to the spacecraft and requires very few assumptions. We found over 250 particles in a suitable distance range with sizes of some centimetres, masses in the range of 10−6–102 kg and a mean velocity of about 2.4 m s−1 relative to the nucleus. Furthermore, the spectral slope was analysed showing a decrease in the median spectral slope of the particles with time. The further a particle is from the spacecraft the fainter is its signal. For this reason, this was counterbalanced by a debiasing. Moreover, the dust mass-loss rate of the nucleus could be computed as well as the Afρ of the comet around perihelion. The summed-up dust mass-loss rate for the mass bins 10−4–102 kg is almost 8300 kg s−1.
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Theresa Ott, Esther Drolshagen, Detlef Koschny, Carsten Güttler, Cécilia Tubiana, et al.. Dust mass distribution around comet 67P/Churyumov–Gerasimenko determined via parallax measurements using Rosetta's OSIRIS cameras. Monthly Notices of the Royal Astronomical Society, Oxford University Press (OUP): Policy P - Oxford Open Option A, 2017, 469 (Suppl_2), pp.S276 - S284. ⟨10.1093/mnras/stx1419⟩. ⟨insu-01574533⟩



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