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class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.03464">arXiv:2303.03464</a> <span> [<a href="https://arxiv.org/pdf/2303.03464">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41586-023-05878-z">10.1038/s41586-023-05878-z <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Momentum Transfer from the DART Mission Kinetic Impact on Asteroid Dimorphos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Cheng%2C+A+F">Andrew F. Cheng</a>, <a href="/search/?searchtype=author&query=Agrusa%2C+H+F">Harrison F. Agrusa</a>, <a href="/search/?searchtype=author&query=Barbee%2C+B+W">Brent W. Barbee</a>, <a href="/search/?searchtype=author&query=Meyer%2C+A+J">Alex J. Meyer</a>, <a href="/search/?searchtype=author&query=Farnham%2C+T+L">Tony L. Farnham</a>, <a href="/search/?searchtype=author&query=Raducan%2C+S+D">Sabina D. Raducan</a>, <a href="/search/?searchtype=author&query=Richardson%2C+D+C">Derek C. Richardson</a>, <a href="/search/?searchtype=author&query=Dotto%2C+E">Elisabetta Dotto</a>, <a href="/search/?searchtype=author&query=Zinzi%2C+A">Angelo Zinzi</a>, <a href="/search/?searchtype=author&query=Della+Corte%2C+V">Vincenzo Della Corte</a>, <a href="/search/?searchtype=author&query=Statler%2C+T+S">Thomas S. Statler</a>, <a href="/search/?searchtype=author&query=Chesley%2C+S">Steven Chesley</a>, <a href="/search/?searchtype=author&query=Naidu%2C+S+P">Shantanu P. Naidu</a>, <a href="/search/?searchtype=author&query=Hirabayashi%2C+M">Masatoshi Hirabayashi</a>, <a href="/search/?searchtype=author&query=Li%2C+J">Jian-Yang Li</a>, <a href="/search/?searchtype=author&query=Eggl%2C+S">Siegfried Eggl</a>, <a href="/search/?searchtype=author&query=Barnouin%2C+O+S">Olivier S. Barnouin</a>, <a href="/search/?searchtype=author&query=Chabot%2C+N+L">Nancy L. Chabot</a>, <a href="/search/?searchtype=author&query=Chocron%2C+S">Sidney Chocron</a>, <a href="/search/?searchtype=author&query=Collins%2C+G+S">Gareth S. Collins</a>, <a href="/search/?searchtype=author&query=Daly%2C+R+T">R. Terik Daly</a>, <a href="/search/?searchtype=author&query=Davison%2C+T+M">Thomas M. Davison</a>, <a href="/search/?searchtype=author&query=DeCoster%2C+M+E">Mallory E. DeCoster</a>, <a href="/search/?searchtype=author&query=Ernst%2C+C+M">Carolyn M. Ernst</a>, <a href="/search/?searchtype=author&query=Ferrari%2C+F">Fabio Ferrari</a> , et al. (44 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.03464v1-abstract-short" style="display: inline;"> The NASA Double Asteroid Redirection Test (DART) mission performed a kinetic impact on asteroid Dimorphos, the satellite of the binary asteroid (65803) Didymos, at 23:14 UTC on September 26, 2022 as a planetary defense test. DART was the first hypervelocity impact experiment on an asteroid at size and velocity scales relevant to planetary defense, intended to validate kinetic impact as a means of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.03464v1-abstract-full').style.display = 'inline'; document.getElementById('2303.03464v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.03464v1-abstract-full" style="display: none;"> The NASA Double Asteroid Redirection Test (DART) mission performed a kinetic impact on asteroid Dimorphos, the satellite of the binary asteroid (65803) Didymos, at 23:14 UTC on September 26, 2022 as a planetary defense test. DART was the first hypervelocity impact experiment on an asteroid at size and velocity scales relevant to planetary defense, intended to validate kinetic impact as a means of asteroid deflection. Here we report the first determination of the momentum transferred to an asteroid by kinetic impact. Based on the change in the binary orbit period, we find an instantaneous reduction in Dimorphos's along-track orbital velocity component of 2.70 +/- 0.10 mm/s, indicating enhanced momentum transfer due to recoil from ejecta streams produced by the impact. For a Dimorphos bulk density range of 1,500 to 3,300 kg/m$^3$, we find that the expected value of the momentum enhancement factor, $尾$, ranges between 2.2 and 4.9, depending on the mass of Dimorphos. If Dimorphos and Didymos are assumed to have equal densities of 2,400 kg/m$^3$, $尾$= 3.61 +0.19/-0.25 (1 $蟽$). These $尾$ values indicate that significantly more momentum was transferred to Dimorphos from the escaping impact ejecta than was incident with DART. Therefore, the DART kinetic impact was highly effective in deflecting the asteroid Dimorphos. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.03464v1-abstract-full').style.display = 'none'; document.getElementById('2303.03464v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted by Nature</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.01700">arXiv:2303.01700</a> <span> [<a href="https://arxiv.org/pdf/2303.01700">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41586-023-05811-4">10.1038/s41586-023-05811-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ejecta from the DART-produced active asteroid Dimorphos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Li%2C+J">Jian-Yang Li</a>, <a href="/search/?searchtype=author&query=Hirabayashi%2C+M">Masatoshi Hirabayashi</a>, <a href="/search/?searchtype=author&query=Farnham%2C+T+L">Tony L. Farnham</a>, <a href="/search/?searchtype=author&query=Sunshine%2C+J+M">Jessica M. Sunshine</a>, <a href="/search/?searchtype=author&query=Knight%2C+M+M">Matthew M. Knight</a>, <a href="/search/?searchtype=author&query=Tancredi%2C+G">Gonzalo Tancredi</a>, <a href="/search/?searchtype=author&query=Moreno%2C+F">Fernando Moreno</a>, <a href="/search/?searchtype=author&query=Murphy%2C+B">Brian Murphy</a>, <a href="/search/?searchtype=author&query=Opitom%2C+C">Cyrielle Opitom</a>, <a href="/search/?searchtype=author&query=Chesley%2C+S">Steve Chesley</a>, <a href="/search/?searchtype=author&query=Scheeres%2C+D+J">Daniel J. Scheeres</a>, <a href="/search/?searchtype=author&query=Thomas%2C+C+A">Cristina A. Thomas</a>, <a href="/search/?searchtype=author&query=Fahnestock%2C+E+G">Eugene G. Fahnestock</a>, <a href="/search/?searchtype=author&query=Cheng%2C+A+F">Andrew F. Cheng</a>, <a href="/search/?searchtype=author&query=Dressel%2C+L">Linda Dressel</a>, <a href="/search/?searchtype=author&query=Ernst%2C+C+M">Carolyn M. Ernst</a>, <a href="/search/?searchtype=author&query=Ferrari%2C+F">Fabio Ferrari</a>, <a href="/search/?searchtype=author&query=Fitzsimmons%2C+A">Alan Fitzsimmons</a>, <a href="/search/?searchtype=author&query=Ieva%2C+S">Simone Ieva</a>, <a href="/search/?searchtype=author&query=Ivanovski%2C+S+L">Stavro L. Ivanovski</a>, <a href="/search/?searchtype=author&query=Kareta%2C+T">Teddy Kareta</a>, <a href="/search/?searchtype=author&query=Kolokolova%2C+L">Ludmilla Kolokolova</a>, <a href="/search/?searchtype=author&query=Lister%2C+T">Tim Lister</a>, <a href="/search/?searchtype=author&query=Raducan%2C+S+D">Sabina D. Raducan</a>, <a href="/search/?searchtype=author&query=Rivkin%2C+A+S">Andrew S. Rivkin</a> , et al. (39 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.01700v1-abstract-short" style="display: inline;"> Some active asteroids have been proposed to be the result of impact events. Because active asteroids are generally discovered serendipitously only after their tail formation, the process of the impact ejecta evolving into a tail has never been directly observed. NASA's Double Asteroid Redirection Test (DART) mission, apart from having successfully changed the orbital period of Dimorphos, demonstra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.01700v1-abstract-full').style.display = 'inline'; document.getElementById('2303.01700v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.01700v1-abstract-full" style="display: none;"> Some active asteroids have been proposed to be the result of impact events. Because active asteroids are generally discovered serendipitously only after their tail formation, the process of the impact ejecta evolving into a tail has never been directly observed. NASA's Double Asteroid Redirection Test (DART) mission, apart from having successfully changed the orbital period of Dimorphos, demonstrated the activation process of an asteroid from an impact under precisely known impact conditions. Here we report the observations of the DART impact ejecta with the Hubble Space Telescope (HST) from impact time T+15 minutes to T+18.5 days at spatial resolutions of ~2.1 km per pixel. Our observations reveal a complex evolution of ejecta, which is first dominated by the gravitational interaction between the Didymos binary system and the ejected dust and later by solar radiation pressure. The lowest-speed ejecta dispersed via a sustained tail that displayed a consistent morphology with previously observed asteroid tails thought to be produced by impact. The ejecta evolution following DART's controlled impact experiment thus provides a framework for understanding the fundamental mechanisms acting on asteroids disrupted by natural impact. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.01700v1-abstract-full').style.display = 'none'; document.getElementById('2303.01700v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted by Nature</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.12791">arXiv:2212.12791</a> <span> [<a href="https://arxiv.org/pdf/2212.12791">pdf</a>, <a href="https://arxiv.org/format/2212.12791">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> CUBES: a UV spectrograph for the future </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/?searchtype=author&query=Alcala%27%2C+J+M">J. M. Alcala'</a>, <a href="/search/?searchtype=author&query=Alencar%2C+S+H+P">S. H. P. Alencar</a>, <a href="/search/?searchtype=author&query=Balashev%2C+S+A">S. A. Balashev</a>, <a href="/search/?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/?searchtype=author&query=Bastian%2C+N">N. Bastian</a>, <a href="/search/?searchtype=author&query=Battino%2C+U">U. Battino</a>, <a href="/search/?searchtype=author&query=Bissell%2C+L">L. Bissell</a>, <a href="/search/?searchtype=author&query=Bristow%2C+P">P. Bristow</a>, <a href="/search/?searchtype=author&query=Calcines%2C+A">A. Calcines</a>, <a href="/search/?searchtype=author&query=Calderone%2C+G">G. Calderone</a>, <a href="/search/?searchtype=author&query=Cambianica%2C+P">P. Cambianica</a>, <a href="/search/?searchtype=author&query=Carini%2C+R">R. Carini</a>, <a href="/search/?searchtype=author&query=Carter%2C+B">B. Carter</a>, <a href="/search/?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/?searchtype=author&query=Castilho%2C+B+V">B. V. Castilho</a>, <a href="/search/?searchtype=author&query=Cescutti%2C+G">G. Cescutti</a>, <a href="/search/?searchtype=author&query=Christlieb%2C+N">N. Christlieb</a>, <a href="/search/?searchtype=author&query=Cirami%2C+R">R. Cirami</a>, <a href="/search/?searchtype=author&query=Conzelmann%2C+R">R. Conzelmann</a>, <a href="/search/?searchtype=author&query=Coretti%2C+I">I. Coretti</a>, <a href="/search/?searchtype=author&query=Cooke%2C+R">R. Cooke</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Cunha%2C+K">K. Cunha</a> , et al. (64 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.12791v1-abstract-short" style="display: inline;"> In spite of the advent of extremely large telescopes in the UV/optical/NIR range, the current generation of 8-10m facilities is likely to remain competitive at ground-UV wavelengths for the foreseeable future. The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high-efficiency (>40%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.12791v1-abstract-full').style.display = 'inline'; document.getElementById('2212.12791v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.12791v1-abstract-full" style="display: none;"> In spite of the advent of extremely large telescopes in the UV/optical/NIR range, the current generation of 8-10m facilities is likely to remain competitive at ground-UV wavelengths for the foreseeable future. The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high-efficiency (>40%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R>20,000, although a lower-resolution, sky-limited mode of R ~ 7,000 is also planned. CUBES will offer new possibilities in many fields of astrophysics, providing access to key lines of stellar spectra: a tremendous diversity of iron-peak and heavy elements, lighter elements (in particular Beryllium) and light-element molecules (CO, CN, OH), as well as Balmer lines and the Balmer jump (particularly important for young stellar objects). The UV range is also critical in extragalactic studies: the circumgalactic medium of distant galaxies, the contribution of different types of sources to the cosmic UV background, the measurement of H2 and primordial Deuterium in a regime of relatively transparent intergalactic medium, and follow-up of explosive transients. The CUBES project completed a Phase A conceptual design in June 2021 and has now entered the Phase B dedicated to detailed design and construction. First science operations are planned for 2028. In this paper, we briefly describe the CUBES project development and goals, the main science cases, the instrument design and the project organization and management. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.12791v1-abstract-full').style.display = 'none'; document.getElementById('2212.12791v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Proceedings for the HACK100 conference, Trieste, June 2022. arXiv admin note: substantial text overlap with arXiv:2208.01672</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.10150">arXiv:2211.10150</a> <span> [<a href="https://arxiv.org/pdf/2211.10150">pdf</a>, <a href="https://arxiv.org/format/2211.10150">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2629936">10.1117/12.2629936 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Transmission curves of narrow-band filters in large-FoV and fast astronomical instruments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Battaini%2C+F">Federico Battaini</a>, <a href="/search/?searchtype=author&query=Ragazzoni%2C+R">Roberto Ragazzoni</a>, <a href="/search/?searchtype=author&query=Milone%2C+A+P">Antonino P. Milone</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">Gabriele Cremonese</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.10150v1-abstract-short" style="display: inline;"> Narrow-band filters are often used to constrain the chemical composition of astronomical objects through photometry. A challenge to derive accurate photometry is that narrow-band filters are based on interference of multiple reflections and refractions between thin layers of transparent dielectric material. When the light rays reach the surface of a filter not perpendicular to it, they cross the l… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.10150v1-abstract-full').style.display = 'inline'; document.getElementById('2211.10150v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.10150v1-abstract-full" style="display: none;"> Narrow-band filters are often used to constrain the chemical composition of astronomical objects through photometry. A challenge to derive accurate photometry is that narrow-band filters are based on interference of multiple reflections and refractions between thin layers of transparent dielectric material. When the light rays reach the surface of a filter not perpendicular to it, they cross the layers obliquely travelling a path longer than the thickness of the layers and different for each inclination. This results in a blue-shift of the central wavelength and a distortion of the transmission curve. Hence, particular care should be taken when narrow band filters are used in presence of small f-numbers and large non-telecentric angles, as frequent in the large field of view (FoV) instruments. Sometimes, the broadening and central wavelength shift of the transmission curve are considered and compensated in the design of filters for instruments with a small f-number. Here we consider the combined effect of small f-number, non-telecentricity and large FoV. Where single spectral lines are considered, a shift in central wavelength or a change in the shape of the transmission curve may introduce an instrumental dispersion in luminosity and in the linked color indices. We found that transmission curves of narrow band filters can be significantly different in shape than the nominal ones. The bottom limits for filters' effective FWHM for each f-number; the monotonic behavior of the blue-shift with distance from the center of FoV; the monotonic quality decrease of the transmission curves and the photometric dispersion introduced by the filters are computationally estimated. This work could represent a useful tool to evaluate the fitness of a particular filter at a particular facility. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.10150v1-abstract-full').style.display = 'none'; document.getElementById('2211.10150v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 14 figures, SPIE Astronomical Telescopes + Instrumentation, 2022, Montr茅al, Qu茅bec, Canada</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proc. SPIE 12188, Advances in Optical and Mechanical Technologies for Telescopes and Instrumentation V, 1218821 (29 August 2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.04316">arXiv:2210.04316</a> <span> [<a href="https://arxiv.org/pdf/2210.04316">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.pss.2022.105580">10.1016/j.pss.2022.105580 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> In-flight radiometric calibration of the ExoMars TGO Colour and Stereo Surface Imaging System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pommerol%2C+A">Antoine Pommerol</a>, <a href="/search/?searchtype=author&query=Thomas%2C+N">Nicolas Thomas</a>, <a href="/search/?searchtype=author&query=Almeida%2C+M">Miguel Almeida</a>, <a href="/search/?searchtype=author&query=Read%2C+M">Mattew Read</a>, <a href="/search/?searchtype=author&query=Becerra%2C+P">Patricio Becerra</a>, <a href="/search/?searchtype=author&query=Cesar%2C+C">Camila Cesar</a>, <a href="/search/?searchtype=author&query=Valantinas%2C+A">Adomas Valantinas</a>, <a href="/search/?searchtype=author&query=Simioni%2C+E">Emanuele Simioni</a>, <a href="/search/?searchtype=author&query=McEwen%2C+A+S">Alfred S. McEwen</a>, <a href="/search/?searchtype=author&query=Perry%2C+J">Jason Perry</a>, <a href="/search/?searchtype=author&query=Marriner%2C+C">Charlotte Marriner</a>, <a href="/search/?searchtype=author&query=Munaretto%2C+G">Giovanni Munaretto</a>, <a href="/search/?searchtype=author&query=Pajola%2C+M">Maurizio Pajola</a>, <a href="/search/?searchtype=author&query=Tornabene%2C+L+L">Livio L. Tornabene</a>, <a href="/search/?searchtype=author&query=M%C3%A8ge%2C+D">Daniel M猫ge</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">Vania Da Deppo</a>, <a href="/search/?searchtype=author&query=Re%2C+C">Cristina Re</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">Gabriele Cremonese</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.04316v1-abstract-short" style="display: inline;"> The Colour and Stereo Surface Science Imaging System (CaSSIS) of the ExoMars Trace Gas Orbiter returns on average twenty images per day of the Martian surface, most of them in 3 or 4 colours and some of them in stereo. CaSSIS uses a push-frame approach to acquire colour images, with four bandpass filters deposited directly above the sensor and an imaging cadence synchronized with the ground track… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.04316v1-abstract-full').style.display = 'inline'; document.getElementById('2210.04316v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.04316v1-abstract-full" style="display: none;"> The Colour and Stereo Surface Science Imaging System (CaSSIS) of the ExoMars Trace Gas Orbiter returns on average twenty images per day of the Martian surface, most of them in 3 or 4 colours and some of them in stereo. CaSSIS uses a push-frame approach to acquire colour images, with four bandpass filters deposited directly above the sensor and an imaging cadence synchronized with the ground track velocity to cover the imaged area with tens of small, partially overlapping images. These "framelets" are later map-projected and mosaicked to build the final image. This approach offers both advantages and challenges in terms of radiometric calibration. While the collection of dark and flatfield frames is considerably enhanced by the frequent and fast acquisition of tens of successive images, mosaics assembled from the adjacent framelets highlight the straylight and changes in the bias of the detector. Both issues have been identified on CaSSIS images, with low intensities overall (up to a few percents), but sufficient to generate prominent artefacts on the final assembled colour images. We have therefore developed methods to correct these artefacts that are now included into the radiometric calibration pipeline. We detail here the different steps of the calibration procedure and the generation of the products used for calibration, and discuss the efficacy of the corrections. The relative uncertainties on the bias and flatfield frames are low, of the order of 0.2 and 0.1 percents, respectively. The uncertainty on the absolute radiometric calibration is of 3 percents, which is quite low for such an instrument. The straylight adds an estimated about 1 percent error to the absolute calibration. The residuals after corrections of the straylight and bias offsets are of the order of a few DNs to tens of DNs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.04316v1-abstract-full').style.display = 'none'; document.getElementById('2210.04316v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.01677">arXiv:2208.01677</a> <span> [<a href="https://arxiv.org/pdf/2208.01677">pdf</a>, <a href="https://arxiv.org/format/2208.01677">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s10686-022-09864-7">10.1007/s10686-022-09864-7 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The CUBES Science Case </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Evans%2C+C">Chris Evans</a>, <a href="/search/?searchtype=author&query=Cristiani%2C+S">Stefano Cristiani</a>, <a href="/search/?searchtype=author&query=Opitom%2C+C">Cyrielle Opitom</a>, <a href="/search/?searchtype=author&query=Cescutti%2C+G">Gabriele Cescutti</a>, <a href="/search/?searchtype=author&query=D%27Odorico%2C+V">Valentina D'Odorico</a>, <a href="/search/?searchtype=author&query=Alcal%C3%A1%2C+J+M">Juan Manuel Alcal谩</a>, <a href="/search/?searchtype=author&query=Alencar%2C+S+H+P">Silvia H. P. Alencar</a>, <a href="/search/?searchtype=author&query=Balashev%2C+S">Sergei Balashev</a>, <a href="/search/?searchtype=author&query=Barbuy%2C+B">Beatriz Barbuy</a>, <a href="/search/?searchtype=author&query=Bastian%2C+N">Nate Bastian</a>, <a href="/search/?searchtype=author&query=Battino%2C+U">Umberto Battino</a>, <a href="/search/?searchtype=author&query=Cambianica%2C+P">Pamela Cambianica</a>, <a href="/search/?searchtype=author&query=Carini%2C+R">Roberta Carini</a>, <a href="/search/?searchtype=author&query=Carter%2C+B">Brad Carter</a>, <a href="/search/?searchtype=author&query=Cassisi%2C+S">Santi Cassisi</a>, <a href="/search/?searchtype=author&query=Castilho%2C+B+V">Bruno Vaz Castilho</a>, <a href="/search/?searchtype=author&query=Christlieb%2C+N">Norbert Christlieb</a>, <a href="/search/?searchtype=author&query=Cooke%2C+R">Ryan Cooke</a>, <a href="/search/?searchtype=author&query=Covino%2C+S">Stefano Covino</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">Gabriele Cremonese</a>, <a href="/search/?searchtype=author&query=Cunha%2C+K">Katia Cunha</a>, <a href="/search/?searchtype=author&query=da+Silva%2C+A+R">Andr茅 R. da Silva</a>, <a href="/search/?searchtype=author&query=D%27Elia%2C+V">Valerio D'Elia</a>, <a href="/search/?searchtype=author&query=De+Cia%2C+A">Annalisa De Cia</a>, <a href="/search/?searchtype=author&query=De+Silva%2C+G">Gayandhi De Silva</a> , et al. (29 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.01677v2-abstract-short" style="display: inline;"> We introduce the scientific motivations for the development of the Cassegrain U-Band Efficient Spectrograph (CUBES) that is now in construction for the Very Large Telescope. The assembled cases span a broad range of contemporary topics across Solar System, Galactic and extragalactic astronomy, where observations are limited by the performance of current ground-based spectrographs shortwards of 400… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.01677v2-abstract-full').style.display = 'inline'; document.getElementById('2208.01677v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.01677v2-abstract-full" style="display: none;"> We introduce the scientific motivations for the development of the Cassegrain U-Band Efficient Spectrograph (CUBES) that is now in construction for the Very Large Telescope. The assembled cases span a broad range of contemporary topics across Solar System, Galactic and extragalactic astronomy, where observations are limited by the performance of current ground-based spectrographs shortwards of 400nm. A brief background to each case is presented and specific technical requirements on the instrument design that flow-down from each case are identified. These were used as inputs to the CUBES design, that will provide a factor of ten gain in efficiency for astronomical spectroscopy over 300-405nm, at resolving powers of R~24,000 and ~7,000. We include performance estimates that demonstrate the ability of CUBES to observe sources that are up to three magnitudes fainter than currently possible at ground-ultraviolet wavelengths, and we place its predicted performance in the context of existing facillities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.01677v2-abstract-full').style.display = 'none'; document.getElementById('2208.01677v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Experimental Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.01672">arXiv:2208.01672</a> <span> [<a href="https://arxiv.org/pdf/2208.01672">pdf</a>, <a href="https://arxiv.org/format/2208.01672">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> CUBES, the Cassegrain U-Band Efficient Spectrograph </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Cristiani%2C+S">S. Cristiani</a>, <a href="/search/?searchtype=author&query=Alcal%C3%A1%2C+J+M">J. M. Alcal谩</a>, <a href="/search/?searchtype=author&query=Alencar%2C+S+H+P">S. H. P. Alencar</a>, <a href="/search/?searchtype=author&query=Balashev%2C+S+A">S. A. Balashev</a>, <a href="/search/?searchtype=author&query=Bastian%2C+N">N. Bastian</a>, <a href="/search/?searchtype=author&query=Barbuy%2C+B">B. Barbuy</a>, <a href="/search/?searchtype=author&query=Battino%2C+U">U. Battino</a>, <a href="/search/?searchtype=author&query=Calcines%2C+A">A. Calcines</a>, <a href="/search/?searchtype=author&query=Calderone%2C+G">G. Calderone</a>, <a href="/search/?searchtype=author&query=Cambianica%2C+P">P. Cambianica</a>, <a href="/search/?searchtype=author&query=Carini%2C+R">R. Carini</a>, <a href="/search/?searchtype=author&query=Carter%2C+B">B. Carter</a>, <a href="/search/?searchtype=author&query=Cassisi%2C+S">S. Cassisi</a>, <a href="/search/?searchtype=author&query=Castilho%2C+B+V">B. V. Castilho</a>, <a href="/search/?searchtype=author&query=Cescutti%2C+G">G. Cescutti</a>, <a href="/search/?searchtype=author&query=Christlieb%2C+N">N. Christlieb</a>, <a href="/search/?searchtype=author&query=Cirami%2C+R">R. Cirami</a>, <a href="/search/?searchtype=author&query=Coretti%2C+I">I. Coretti</a>, <a href="/search/?searchtype=author&query=Cooke%2C+R">R. Cooke</a>, <a href="/search/?searchtype=author&query=Covino%2C+S">S. Covino</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Cunha%2C+K">K. Cunha</a>, <a href="/search/?searchtype=author&query=Cupani%2C+G">G. Cupani</a>, <a href="/search/?searchtype=author&query=da+Silva%2C+A+R">A. R. da Silva</a>, <a href="/search/?searchtype=author&query=De+Caprio%2C+V">V. De Caprio</a> , et al. (52 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.01672v1-abstract-short" style="display: inline;"> In the era of Extremely Large Telescopes, the current generation of 8-10m facilities are likely to remain competitive at ground-UV wavelengths for the foreseeable future. The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high-efficiency (>40%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R>20,000 (with a lowe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.01672v1-abstract-full').style.display = 'inline'; document.getElementById('2208.01672v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.01672v1-abstract-full" style="display: none;"> In the era of Extremely Large Telescopes, the current generation of 8-10m facilities are likely to remain competitive at ground-UV wavelengths for the foreseeable future. The Cassegrain U-Band Efficient Spectrograph (CUBES) has been designed to provide high-efficiency (>40%) observations in the near UV (305-400 nm requirement, 300-420 nm goal) at a spectral resolving power of R>20,000 (with a lower-resolution, sky-limited mode of R ~ 7,000). With the design focusing on maximizing the instrument throughput (ensuring a Signal to Noise Ratio (SNR) ~20 per high-resolution element at 313 nm for U ~18.5 mag objects in 1h of observations), it will offer new possibilities in many fields of astrophysics, providing access to key lines of stellar spectra: a tremendous diversity of iron-peak and heavy elements, lighter elements (in particular Beryllium) and light-element molecules (CO, CN, OH), as well as Balmer lines and the Balmer jump (particularly important for young stellar objects). The UV range is also critical in extragalactic studies: the circumgalactic medium of distant galaxies, the contribution of different types of sources to the cosmic UV background, the measurement of H2 and primordial Deuterium in a regime of relatively transparent intergalactic medium, and follow-up of explosive transients. The CUBES project completed a Phase A conceptual design in June 2021 and has now entered the detailed design and construction phase. First science operations are planned for 2028. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.01672v1-abstract-full').style.display = 'none'; document.getElementById('2208.01672v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">SPIE proceedings, SPIE Astronomical Telescopes + Instrumentation 2022, Montr茅al, Canada; 20 pages, 13 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.15579">arXiv:2203.15579</a> <span> [<a href="https://arxiv.org/pdf/2203.15579">pdf</a>, <a href="https://arxiv.org/format/2203.15579">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s10686-022-09853-w">10.1007/s10686-022-09853-w <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cometary science with CUBES </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Opitom%2C+C">Cyrielle Opitom</a>, <a href="/search/?searchtype=author&query=Snodgrass%2C+C">Colin Snodgrass</a>, <a href="/search/?searchtype=author&query=La+Forgia%2C+F">Fiorangela La Forgia</a>, <a href="/search/?searchtype=author&query=Evans%2C+C">Chris Evans</a>, <a href="/search/?searchtype=author&query=Cambianica%2C+P">Pamela Cambianica</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">Gabriele Cremonese</a>, <a href="/search/?searchtype=author&query=Fitzsimmons%2C+A">Alan Fitzsimmons</a>, <a href="/search/?searchtype=author&query=Lazzarin%2C+M">Monica Lazzarin</a>, <a href="/search/?searchtype=author&query=Migliorini%2C+A">Alessandra Migliorini</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.15579v1-abstract-short" style="display: inline;"> The proposed CUBES spectrograph for ESO's Very Large Telescope will be an exceptionally powerful instrument for the study of comets. The gas coma of a comet contains a large number of emission features in the near-UV range covered by CUBES (305-400 nm), which are diagnostic of the composition of the ices in its nucleus and the chemistry in the coma. Production rates and relative ratios between dif… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.15579v1-abstract-full').style.display = 'inline'; document.getElementById('2203.15579v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.15579v1-abstract-full" style="display: none;"> The proposed CUBES spectrograph for ESO's Very Large Telescope will be an exceptionally powerful instrument for the study of comets. The gas coma of a comet contains a large number of emission features in the near-UV range covered by CUBES (305-400 nm), which are diagnostic of the composition of the ices in its nucleus and the chemistry in the coma. Production rates and relative ratios between different species reveal how much ice is present and inform models of the conditions in the early solar system. In particular, CUBES will lead to advances in detection of water from very faint comets, revealing how much ice may be hidden in the main asteroid belt, and in measuring isotopic and molecular composition ratios in a much wider range of comets than currently possible, provide constraints on their formation temperatures. CUBES will also be sensitive to emissions from gaseous metals (e.g., FeI and NiI), which have recently been identified in comets and offer an entirely new area of investigation to understand these enigmatic objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.15579v1-abstract-full').style.display = 'none'; document.getElementById('2203.15579v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Experimental Astronomy</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.10950">arXiv:2104.10950</a> <span> [<a href="https://arxiv.org/pdf/2104.10950">pdf</a>, <a href="https://arxiv.org/format/2104.10950">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stab1152">10.1093/mnras/stab1152 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observational constraints to the dynamics of dust particles in the coma of comet 67P/Churyumov-Gerasimenko </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Frattin%2C+E">Elisa Frattin</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Ivanovski%2C+S+L">S. L. Ivanovski</a>, <a href="/search/?searchtype=author&query=Marzari%2C+F">F. Marzari</a>, <a href="/search/?searchtype=author&query=Fulle%2C+M">M. Fulle</a>, <a href="/search/?searchtype=author&query=Zakharov%2C+V+V">V. V. Zakharov</a>, <a href="/search/?searchtype=author&query=Moreno%2C+F">F. Moreno</a>, <a href="/search/?searchtype=author&query=Naletto%2C+G">G. Naletto</a>, <a href="/search/?searchtype=author&query=Lazzarin%2C+M">M. Lazzarin</a>, <a href="/search/?searchtype=author&query=Cambianica%2C+P">P. Cambianica</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Ferrari%2C+S">S. Ferrari</a>, <a href="/search/?searchtype=author&query=Ferri%2C+F">F. Ferri</a>, <a href="/search/?searchtype=author&query=Guettler%2C+C">C. Guettler</a>, <a href="/search/?searchtype=author&query=La+Forgia%2C+F">F. La Forgia</a>, <a href="/search/?searchtype=author&query=Lucchetti%2C+A">A. Lucchetti</a>, <a href="/search/?searchtype=author&query=Pajola%2C+M">M. Pajola</a>, <a href="/search/?searchtype=author&query=Penasa%2C+L">L. Penasa</a>, <a href="/search/?searchtype=author&query=Rotundi%2C+A">A. Rotundi</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Tubiana%2C+C">C. Tubiana</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2104.10950v1-abstract-short" style="display: inline;"> In this work we aim to characterise the dust motion in the inner coma of comet 67P/Churyumov- Gerasimenko to provide constraints for theoretical 3D coma models. The OSIRIS camera onboard the Rosetta mission was able for the first time to acquire images of single dust particles from inside the cometary coma, very close to the nucleus. We analyse a large number of particles, performing a significant… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.10950v1-abstract-full').style.display = 'inline'; document.getElementById('2104.10950v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.10950v1-abstract-full" style="display: none;"> In this work we aim to characterise the dust motion in the inner coma of comet 67P/Churyumov- Gerasimenko to provide constraints for theoretical 3D coma models. The OSIRIS camera onboard the Rosetta mission was able for the first time to acquire images of single dust particles from inside the cometary coma, very close to the nucleus. We analyse a large number of particles, performing a significant statistic of their behaviour during the post perihelion period, when the spacecraft covered distances from the nucleus ranging between 80 and 400 km. We describe the particle trajectories, investigating their orientation and finding highly radial motion with respect to the nucleus. Then, from the particle brightness profiles, we derive a particle rotational frequency of v < 3.6 Hz, revealing that they are slow rotators and do not undergo fragmentation. We use scattering models to compare the observed spectral radiance of the particles with the simulated ones in order to estimate their size, finding values that range from millimetres up to centimetres. The statistics performed in this paper provide useful parameters to constrain the cometary coma dynamical models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.10950v1-abstract-full').style.display = 'none'; document.getElementById('2104.10950v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.06248">arXiv:2003.06248</a> <span> [<a href="https://arxiv.org/pdf/2003.06248">pdf</a>, <a href="https://arxiv.org/format/2003.06248">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Software Engineering">cs.SE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.13140/RG.2.2.10451.73762">10.13140/RG.2.2.10451.73762 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High Quality Software for Planetary Science from Space </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lazzarotto%2C+F">Francesco Lazzarotto</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">Gabriele Cremonese</a>, <a href="/search/?searchtype=author&query=Lucchetti%2C+A">Alice Lucchetti</a>, <a href="/search/?searchtype=author&query=Re%2C+C">Cristina Re</a>, <a href="/search/?searchtype=author&query=Simioni%2C+E">Emanuele Simioni</a>, <a href="/search/?searchtype=author&query=Pajola%2C+M">Maurizio Pajola</a>, <a href="/search/?searchtype=author&query=Cambianica%2C+P">Pamela Cambianica</a>, <a href="/search/?searchtype=author&query=Munaretto%2C+G">Giovanni Munaretto</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2003.06248v2-abstract-short" style="display: inline;"> Planetary science space missions need high quality software ed efficient algorithms in order to extract innovative scientific results from flight data. Reliable and efficient software technologies are increasingly vital to improve and prolong the exploiting of the results of a mission, to allow the application of established algorithms and technologies also to future space missions and for the sci… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.06248v2-abstract-full').style.display = 'inline'; document.getElementById('2003.06248v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.06248v2-abstract-full" style="display: none;"> Planetary science space missions need high quality software ed efficient algorithms in order to extract innovative scientific results from flight data. Reliable and efficient software technologies are increasingly vital to improve and prolong the exploiting of the results of a mission, to allow the application of established algorithms and technologies also to future space missions and for the scientific analysis of archived data. Here after will be given an in-depth analysis study accompanied by implementation examples on ESA and ASI missions and some remarkable results fruit of decades of important experience reached by space agencies and research institutes in the field. Space applications software quality analysis is not different from other application contexts, among the hi-tech and hi-reliability fields. We describe here a Software Quality study in general, then we will focus on the quality of space mission software (s/w) with details on some notable cases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.06248v2-abstract-full').style.display = 'none'; document.getElementById('2003.06248v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">presentation at XVI Congresso Nazionale di Scienze Planetarie (National Conference on Planetary Sciences) held at Centro Culturale San Gaetano, via Altinate, 71, Padova, Italy on 3-7 February, 2020 Affiliation: University of Padova, 6 pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 85-04 (Primary); 85-05; 85-06 (Secondary) <span class="has-text-black-bis has-text-weight-semibold">ACM Class:</span> D.2.2; B.8.2 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1908.07731">arXiv:1908.07731</a> <span> [<a href="https://arxiv.org/pdf/1908.07731">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> GAUSS -- A Sample Return Mission to Ceres </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Shi%2C+X">Xian Shi</a>, <a href="/search/?searchtype=author&query=Castillo-Rogez%2C+J">Julie Castillo-Rogez</a>, <a href="/search/?searchtype=author&query=Hsieh%2C+H">Henry Hsieh</a>, <a href="/search/?searchtype=author&query=Hui%2C+H">Hejiu Hui</a>, <a href="/search/?searchtype=author&query=Ip%2C+W">Wing-Huen Ip</a>, <a href="/search/?searchtype=author&query=Lei%2C+H">Hanlun Lei</a>, <a href="/search/?searchtype=author&query=Li%2C+J">Jian-Yang Li</a>, <a href="/search/?searchtype=author&query=Tosi%2C+F">Federico Tosi</a>, <a href="/search/?searchtype=author&query=Zhou%2C+L">Liyong Zhou</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">Jessica Agarwal</a>, <a href="/search/?searchtype=author&query=Barucci%2C+A">Antonella Barucci</a>, <a href="/search/?searchtype=author&query=Beck%2C+P">Pierre Beck</a>, <a href="/search/?searchtype=author&query=Bagatin%2C+A+C">Adriano Campo Bagatin</a>, <a href="/search/?searchtype=author&query=Capaccioni%2C+F">Fabrizio Capaccioni</a>, <a href="/search/?searchtype=author&query=Coates%2C+A">Andrew Coates</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">Gabriele Cremonese</a>, <a href="/search/?searchtype=author&query=Duffard%2C+R">Rene Duffard</a>, <a href="/search/?searchtype=author&query=Jaumann%2C+R">Ralf Jaumann</a>, <a href="/search/?searchtype=author&query=Jones%2C+G">Geraint Jones</a>, <a href="/search/?searchtype=author&query=Grande%2C+M">Manuel Grande</a>, <a href="/search/?searchtype=author&query=Kallio%2C+E">Esa Kallio</a>, <a href="/search/?searchtype=author&query=Lin%2C+Y">Yangting Lin</a>, <a href="/search/?searchtype=author&query=Mousis%2C+O">Olivier Mousis</a>, <a href="/search/?searchtype=author&query=Nathues%2C+A">Andreas Nathues</a>, <a href="/search/?searchtype=author&query=Oberst%2C+J">J眉rgen Oberst</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1908.07731v2-abstract-short" style="display: inline;"> The goal of Project GAUSS is to return samples from the dwarf planet Ceres. Ceres is the most accessible ocean world candidate and the largest reservoir of water in the inner solar system. It shows active cryovolcanism and hydrothermal activities in recent history that resulted in minerals not found in any other planets to date except for Earth's upper crust. The possible occurrence of recent subs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.07731v2-abstract-full').style.display = 'inline'; document.getElementById('1908.07731v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1908.07731v2-abstract-full" style="display: none;"> The goal of Project GAUSS is to return samples from the dwarf planet Ceres. Ceres is the most accessible ocean world candidate and the largest reservoir of water in the inner solar system. It shows active cryovolcanism and hydrothermal activities in recent history that resulted in minerals not found in any other planets to date except for Earth's upper crust. The possible occurrence of recent subsurface ocean on Ceres and the complex geochemistry suggest possible past habitability and even the potential for ongoing habitability. Aiming to answer a broad spectrum of questions about the origin and evolution of Ceres and its potential habitability, GAUSS will return samples from this possible ocean world for the first time. The project will address the following top-level scientific questions: 1) What is the origin of Ceres and the origin and transfer of water and other volatiles in the inner solar system? 2) What are the physical properties and internal structure of Ceres? What do they tell us about the evolutionary and aqueous alteration history of icy dwarf planets? 3) What are the astrobiological implications of Ceres? Was it habitable in the past and is it still today? 4) What are the mineralogical connections between Ceres and our current collections of primitive meteorites? GAUSS will first perform a high-resolution global remote sensing investigation, characterizing the geophysical and geochemical properties of Ceres. Candidate sampling sites will then be identified, and observation campaigns will be run for an in-depth assessment of the candidate sites. Once the sampling site is selected, a lander will be deployed on the surface to collect samples and return them to Earth in cryogenic conditions that preserves the volatile and organic composition as well as the original physical status as much as possible. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1908.07731v2-abstract-full').style.display = 'none'; document.getElementById('1908.07731v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 August, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Section 3.4 revised; List of team members updated; Typos corrected</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1905.03022">arXiv:1905.03022</a> <span> [<a href="https://arxiv.org/pdf/1905.03022">pdf</a>, <a href="https://arxiv.org/format/1905.03022">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201834869">10.1051/0004-6361/201834869 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Diurnal variation of dust and gas production in comet 67P/Churyumov-Gerasimenko at the inbound equinox as seen by OSIRIS and VIRTIS-M on board Rosetta </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Tubiana%2C+C">C. Tubiana</a>, <a href="/search/?searchtype=author&query=Rinaldi%2C+G">G. Rinaldi</a>, <a href="/search/?searchtype=author&query=G%C3%BCttler%2C+C">C. G眉ttler</a>, <a href="/search/?searchtype=author&query=Snodgrass%2C+C">C. Snodgrass</a>, <a href="/search/?searchtype=author&query=Shi%2C+X">X. Shi</a>, <a href="/search/?searchtype=author&query=Hu%2C+X">X. Hu</a>, <a href="/search/?searchtype=author&query=Marschall%2C+R">R. Marschall</a>, <a href="/search/?searchtype=author&query=Fulle%2C+M">M. Fulle</a>, <a href="/search/?searchtype=author&query=Bockel%C3%A9e-Morvan%2C+D">D. Bockel茅e-Morvan</a>, <a href="/search/?searchtype=author&query=Naletto%2C+G">G. Naletto</a>, <a href="/search/?searchtype=author&query=Capaccioni%2C+F">F. Capaccioni</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Arnold%2C+G">G. Arnold</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Bodewits%2C+D">D. Bodewits</a>, <a href="/search/?searchtype=author&query=Capria%2C+M+T">M. T. Capria</a>, <a href="/search/?searchtype=author&query=Ciarniello%2C+M">M. Ciarniello</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Crovisier%2C+J">J. Crovisier</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Debei%2C+S">S. Debei</a>, <a href="/search/?searchtype=author&query=De+Cecco%2C+M">M. De Cecco</a>, <a href="/search/?searchtype=author&query=Deller%2C+J">J. Deller</a> , et al. (31 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1905.03022v1-abstract-short" style="display: inline;"> On 27 Apr 2015, when 67P/C-G was at 1.76 au from the Sun and moving towards perihelion, the OSIRIS and VIRTIS-M instruments on Rosetta observed the evolving dust and gas coma during a complete rotation of the comet. We aim to characterize the dust, H2O and CO2 gas spatial distribution in the inner coma. To do this we performed a quantitative analysis of the release of dust and gas and compared the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.03022v1-abstract-full').style.display = 'inline'; document.getElementById('1905.03022v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1905.03022v1-abstract-full" style="display: none;"> On 27 Apr 2015, when 67P/C-G was at 1.76 au from the Sun and moving towards perihelion, the OSIRIS and VIRTIS-M instruments on Rosetta observed the evolving dust and gas coma during a complete rotation of the comet. We aim to characterize the dust, H2O and CO2 gas spatial distribution in the inner coma. To do this we performed a quantitative analysis of the release of dust and gas and compared the observed H2O production rate with the one calculated using a thermo-physical model. For this study we selected OSIRIS WAC images at 612 nm (dust) and VIRTIS-M image cubes at 612 nm, 2700 nm (H2O) and 4200 nm (CO2). We measured the average signal in a circular annulus, to study spatial variation around the comet, and in a sector of the annulus, to study temporal variation in the sunward direction with comet rotation, both at a fixed distance of 3.1 km from the comet centre. The spatial correlation between dust and water, both coming from the sun-lit side of the comet, shows that water is the main driver of dust activity in this time period. The spatial distribution of CO2 is not correlated with water and dust. There is no strong temporal correlation between the dust brightness and water production rate as the comet rotates. The dust brightness shows a peak at 0deg sub-solar longitude, which is not pronounced in the water production. At the same epoch, there is also a maximum in CO2 production. An excess of measured water production, with respect to the value calculated using a simple thermo-physical model, is observed when the head lobe and regions of the Southern hemisphere with strong seasonal variations are illuminated. A drastic decrease in dust production, when the water production (both measured and from the model) displays a maximum, happens when typical Northern consolidated regions are illuminated and the Southern hemisphere regions with strong seasonal variations are instead in shadow. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1905.03022v1-abstract-full').style.display = 'none'; document.getElementById('1905.03022v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.09017">arXiv:1903.09017</a> <span> [<a href="https://arxiv.org/pdf/1903.09017">pdf</a>, <a href="https://arxiv.org/format/1903.09017">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201834824">10.1051/0004-6361/201834824 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Surface evolution of the Anhur region on comet 67P from high-resolution OSIRIS images </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fornasier%2C+S">S. Fornasier</a>, <a href="/search/?searchtype=author&query=Feller%2C+C">C. Feller</a>, <a href="/search/?searchtype=author&query=Hasselmann%2C+P+H">P. H. Hasselmann</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Sunshine%2C+J">J. Sunshine</a>, <a href="/search/?searchtype=author&query=Vincent%2C+J+-">J. -B. Vincent</a>, <a href="/search/?searchtype=author&query=Shi%2C+X">X. Shi</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Naletto%2C+G">G. Naletto</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+L">P. L. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Bodewits%2C+D">D. Bodewits</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Debei%2C+S">S. Debei</a>, <a href="/search/?searchtype=author&query=De+Cecco%2C+M">M. De Cecco</a>, <a href="/search/?searchtype=author&query=Deller%2C+J">J. Deller</a>, <a href="/search/?searchtype=author&query=Ferrari%2C+S">S. Ferrari</a>, <a href="/search/?searchtype=author&query=Fulle%2C+M">M. Fulle</a>, <a href="/search/?searchtype=author&query=Gutierrez%2C+P+J">P. J. Gutierrez</a>, <a href="/search/?searchtype=author&query=G%C3%BCttler%2C+C">C. G眉ttler</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1903.09017v1-abstract-short" style="display: inline;"> The southern hemisphere of comet 67P/Churyumov-Gerasimenko (67P) became observable by the Rosetta mission in March 2015, a few months before cometary southern vernal equinox. The Anhur region in the southern part of the comet's larger lobe was found to be highly eroded, enriched in volatiles, and highly active. We analyze high-resolution images of the Anhur region pre- and post-perihelion acquired… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.09017v1-abstract-full').style.display = 'inline'; document.getElementById('1903.09017v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.09017v1-abstract-full" style="display: none;"> The southern hemisphere of comet 67P/Churyumov-Gerasimenko (67P) became observable by the Rosetta mission in March 2015, a few months before cometary southern vernal equinox. The Anhur region in the southern part of the comet's larger lobe was found to be highly eroded, enriched in volatiles, and highly active. We analyze high-resolution images of the Anhur region pre- and post-perihelion acquired by the OSIRIS imaging system on board the Rosetta mission. The Narrow Angle Camera is particularly useful for studying the evolution in Anhur in terms of morphological changes and color variations.}{Radiance factor images processed by the OSIRIS pipeline were coregistered, reprojected onto the 3D shape model of the comet, and corrected for the illumination conditions. We find a number of morphological changes in the Anhur region that are related to formation of new scarps; removal of dust coatings; localized resurfacing in some areas, including boulders displacements; and vanishing structures, which implies localized mass loss that we estimate to be higher than 50 million kg. The strongest changes took place in and nearby the Anhur canyon-like structure, where significant dust cover was removed, an entire structure vanished, and many boulders were rearranged. All such changes are potentially associated with one of the most intense outbursts registered by Rosetta during its observations, which occurred one day before perihelion passage. Moreover, in the niche at the foot of a new observed scarp, we also see evidence of water ice exposure that persisted for at least six months. The abundance of water ice, evaluated from a linear mixing model, is relatively high (> 20%). Our results confirm that the Anhur region is volatile-rich and probably is the area on 67P with the most pristine exposures near perihelion. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.09017v1-abstract-full').style.display = 'none'; document.getElementById('1903.09017v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 16 figures; accepted for publication in Astronomy and Astrophysics for the Rosetta 2 special number</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 630, A13 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.05975">arXiv:1901.05975</a> <span> [<a href="https://arxiv.org/pdf/1901.05975">pdf</a>, <a href="https://arxiv.org/format/1901.05975">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stz129">10.1093/mnras/stz129 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Experimental phase function and degree of linear polarization of cometary dust analogs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Frattin%2C+E">Elisa Frattin</a>, <a href="/search/?searchtype=author&query=Mu%C3%B1oz%2C+O">Olga Mu帽oz</a>, <a href="/search/?searchtype=author&query=Moreno%2C+F">Fernando Moreno</a>, <a href="/search/?searchtype=author&query=Nava%2C+J">Jacopo Nava</a>, <a href="/search/?searchtype=author&query=Escobar-Cerezo%2C+J">Jes煤s Escobar-Cerezo</a>, <a href="/search/?searchtype=author&query=Martin%2C+J+C+G">Juan Carlos Gomez Martin</a>, <a href="/search/?searchtype=author&query=Guirado%2C+D">Daniel Guirado</a>, <a href="/search/?searchtype=author&query=Cellino%2C+A">Alberto Cellino</a>, <a href="/search/?searchtype=author&query=Coll%2C+P">Patrice Coll</a>, <a href="/search/?searchtype=author&query=Raulin%2C+F">Francois Raulin</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">Ivano Bertini</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">Gabriele Cremonese</a>, <a href="/search/?searchtype=author&query=Lazzarin%2C+M">Monica Lazzarin</a>, <a href="/search/?searchtype=author&query=Naletto%2C+G">Giampiero Naletto</a>, <a href="/search/?searchtype=author&query=La+Forgia%2C+F">Fiorangela La Forgia</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1901.05975v2-abstract-short" style="display: inline;"> We present experimental phase function and degree of linear polarization curves for seven samples of cometary dust analogues namely: ground pieces of Allende, DaG521, FRO95002 and FRO99040 meteorites, Mg-rich olivine and pyroxene, and a sample of organic tholins. The experimental curves have been obtained at the IAA Cosmic Dust Laboratory at a wavelength of 520 nm covering a phase angle range from… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.05975v2-abstract-full').style.display = 'inline'; document.getElementById('1901.05975v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.05975v2-abstract-full" style="display: none;"> We present experimental phase function and degree of linear polarization curves for seven samples of cometary dust analogues namely: ground pieces of Allende, DaG521, FRO95002 and FRO99040 meteorites, Mg-rich olivine and pyroxene, and a sample of organic tholins. The experimental curves have been obtained at the IAA Cosmic Dust Laboratory at a wavelength of 520 nm covering a phase angle range from 3掳 to 175掳. We also provide values of the backscattering enhancement (BCE) for our cometary analogue samples. The final goal of this work is to compare our experimental curves with observational data of comets and asteroids to better constrain the nature of cometary and asteroidal dust grains. All measured phase functions present the typical behavior for 渭m-sized cosmic dust grains. Direct comparison with data provided by the OSIRIS/Rosetta camera for comet 67P Churyumov-Gerasimenko reveals significant differences and supports the idea of a coma dominated by big chunks, larger than one micrometer. The polarization curves are qualitatively similar to ground-based observations of comets and asteroids. The position of the inversion polarization angle seems to be dependent on the composition of the grains.We find opposite dependence of the maximum of the polarization curve for grains sizes in the Rayleigh-resonance and geometric optics domains, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.05975v2-abstract-full').style.display = 'none'; document.getElementById('1901.05975v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.03166">arXiv:1901.03166</a> <span> [<a href="https://arxiv.org/pdf/1901.03166">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.icarus.2018.12.023">10.1016/j.icarus.2018.12.023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fluids mobilization in Arabia Terra, Mars: depth of pressurized reservoir from mounds self-similar clustering </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pozzobon%2C+R">Riccardo Pozzobon</a>, <a href="/search/?searchtype=author&query=Mazzarini%2C+F">Francesco Mazzarini</a>, <a href="/search/?searchtype=author&query=Massironi%2C+M">Matteo Massironi</a>, <a href="/search/?searchtype=author&query=Rossi%2C+A+P">Angelo Pio Rossi</a>, <a href="/search/?searchtype=author&query=Pondrelli%2C+M">Monica Pondrelli</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">Gabriele Cremonese</a>, <a href="/search/?searchtype=author&query=Marinangeli%2C+L">Lucia Marinangeli</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1901.03166v1-abstract-short" style="display: inline;"> Arabia Terra is a region of Mars where signs of past-water occurrence are recorded in several landforms. Broad and local scale geomorphological, compositional and hydrological analyses point towards pervasive fluid circulation through time. In this work we focus on mound fields located in the interior of three casters larger than 40 km (Firsoff, Kotido and unnamed crater 20 km to the east) and sho… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.03166v1-abstract-full').style.display = 'inline'; document.getElementById('1901.03166v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.03166v1-abstract-full" style="display: none;"> Arabia Terra is a region of Mars where signs of past-water occurrence are recorded in several landforms. Broad and local scale geomorphological, compositional and hydrological analyses point towards pervasive fluid circulation through time. In this work we focus on mound fields located in the interior of three casters larger than 40 km (Firsoff, Kotido and unnamed crater 20 km to the east) and showing strong morphological and textural resemblance to terrestrial mud volcanoes and spring-related features. We infer that these landforms likely testify the presence of a pressurized fluid reservoir at depth and past fluid upwelling. We have performed morphometric analyses to characterize the mound morphologies and consequently retrieve an accurate automated mapping of the mounds within the craters for spatial distribution and fractal clustering analysis. The outcome of the fractal clustering yields information about the possible extent of the percolating fracture network at depth below the craters. We have been able to constrain the depth of the pressurized fluid reservoir between ~2.5 and 3.2 km of depth and hence, we propose that mounds and mounds alignments are most likely associated to the presence of fissure ridges and fluid outflow. Their process of formation is genetically linked to the formation of large intra-crater bulges previously interpreted as large scale spring deposits. The overburden removal caused by the impact crater formation is the inferred triggering mechanism for fluid pressurization and upwelling, that through time led to the formation of the intra-crater bulges and, after compaction and sealing, to the widespread mound fields in their surroundings. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.03166v1-abstract-full').style.display = 'none'; document.getElementById('1901.03166v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.09415">arXiv:1812.09415</a> <span> [<a href="https://arxiv.org/pdf/1812.09415">pdf</a>, <a href="https://arxiv.org/format/1812.09415">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201833807">10.1051/0004-6361/201833807 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> ROSETTA/OSIRIS observations of the 67P nucleus during the April 2016 flyby: high-resolution spectrophotometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Feller%2C+C">C. Feller</a>, <a href="/search/?searchtype=author&query=Fornasier%2C+S">S. Fornasier</a>, <a href="/search/?searchtype=author&query=Ferrari%2C+S">S. Ferrari</a>, <a href="/search/?searchtype=author&query=Hasselmann%2C+P+H">P. H. Hasselmann</a>, <a href="/search/?searchtype=author&query=Barucci%2C+A">A. Barucci</a>, <a href="/search/?searchtype=author&query=Massironi%2C+M">M. Massironi</a>, <a href="/search/?searchtype=author&query=Deshapriya%2C+J+D+P">J. D. P Deshapriya</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Naletto%2C+G">G. Naletto</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+L">P. L. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B+J+R">B. J. R. Davidsson</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Bodewits%2C+D">D. Bodewits</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Debei%2C+S">S. Debei</a>, <a href="/search/?searchtype=author&query=De+Cecco%2C+M">M. De Cecco</a>, <a href="/search/?searchtype=author&query=Fulle%2C+M">M. Fulle</a>, <a href="/search/?searchtype=author&query=Guti%C3%A9rrez%2C+P+J">P. J. Guti茅rrez</a>, <a href="/search/?searchtype=author&query=G%C3%BCttler%2C+C">C. G眉ttler</a>, <a href="/search/?searchtype=author&query=Ip%2C+W+-">W. -H. Ip</a>, <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a> , et al. (13 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1812.09415v1-abstract-short" style="display: inline;"> In April 2016, the Rosetta spacecraft performed a low-altitude low-phase-angle flyby over the Imhotep-Khepry transition of 67P/Churyumov-Gerasimenko's nucleus. The OSIRIS/Narrow-Angle-Camera (NAC) acquired 112 images with mainly 3 broadband filters in the visible at a resolution of up to 0.53 m/px and for phase angles between 0.095掳 and 62掳. Using those images, we have investigated the morphologic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.09415v1-abstract-full').style.display = 'inline'; document.getElementById('1812.09415v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.09415v1-abstract-full" style="display: none;"> In April 2016, the Rosetta spacecraft performed a low-altitude low-phase-angle flyby over the Imhotep-Khepry transition of 67P/Churyumov-Gerasimenko's nucleus. The OSIRIS/Narrow-Angle-Camera (NAC) acquired 112 images with mainly 3 broadband filters in the visible at a resolution of up to 0.53 m/px and for phase angles between 0.095掳 and 62掳. Using those images, we have investigated the morphological and spectrophotometrical properties of this area. We assembled the images into coregistered color cubes. Using a 3D shape model, we produced the illumination conditions and georeference for each image. We projected the observations on a map to investigate its geomorphology. Observations were photometrically corrected using the Lommel-Seeliger disk law. Spectrophotometric analyses were performed on the coregistered color cubes. These data were used to estimate the local phase reddening. This region of the nucleus hosts numerous and varied types of terrains and features. We observe an association between a feature's nature, its reflectance, and its spectral slope. Fine material deposits exhibit an average reflectance and spectral slope, while terrains with diamictons, consolidated material, degraded outcrops, or features such as somber boulders, present a lower-than-average reflectance and higher-than-average spectral slope. Bright surfaces present here a spectral behavior consistent with terrains enriched in water-ice. We find a phase-reddening slope of 0.064{\pm}0.001{\%}/100nm/掳 at 2.7 au outbound, similarly to the one obtained at 2.3 au inbound during the February 2015 flyby. Identified as the source region of multiple jets and a host of water-ice material, the Imhotep-Khepry transition appeared in April 2016, close to the frost line, to further harbor several potential locations with exposed water-ice material among its numerous different morphological terrain units. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.09415v1-abstract-full').style.display = 'none'; document.getElementById('1812.09415v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 14 figures, 5 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1812.00590">arXiv:1812.00590</a> <span> [<a href="https://arxiv.org/pdf/1812.00590">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Abundance and size-frequency distributions of boulders in Linne crater's ejecta (Moon) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pajola%2C+M">Maurizio Pajola</a>, <a href="/search/?searchtype=author&query=Pozzobon%2C+R">Riccardo Pozzobon</a>, <a href="/search/?searchtype=author&query=Lucchetti%2C+A">Alice Lucchetti</a>, <a href="/search/?searchtype=author&query=Rossato%2C+S">Sandro Rossato</a>, <a href="/search/?searchtype=author&query=Baratti%2C+E">Emanuele Baratti</a>, <a href="/search/?searchtype=author&query=Galluzzi%2C+V">Valentina Galluzzi</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">Gabriele Cremonese</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1812.00590v1-abstract-short" style="display: inline;"> This paper presents the abundances and the size-frequency distributions (SFD) of the ejected boulders surrounding the Linne crater, located on the Moon's Mare Serenitatis basin. By means of Lunar Reconnaissance Orbiter Camera high-resolution images we prepare a context geological map of the Linne crater as well as we identify 12000 boulders > 4.4 m, with a maximum measured size of 30.8 m. The cumu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.00590v1-abstract-full').style.display = 'inline'; document.getElementById('1812.00590v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1812.00590v1-abstract-full" style="display: none;"> This paper presents the abundances and the size-frequency distributions (SFD) of the ejected boulders surrounding the Linne crater, located on the Moon's Mare Serenitatis basin. By means of Lunar Reconnaissance Orbiter Camera high-resolution images we prepare a context geological map of the Linne crater as well as we identify 12000 boulders > 4.4 m, with a maximum measured size of 30.8 m. The cumulative number of boulders per km2 is fitted with a power-law curve with index -4.03 +0.09/-0.10. By studying the radial ejecta abundances, we find that the largest ones are located within the first 2 km from the crater's centre, while few tens of boulders with sizes < 8 m are detectable above 5 km from the crater's rim. We find that the Linne proximal ejecta blanket is slightly asymmetrical, as indicated in the geological map too, showing a density increase in the NE-SW direction. This may be the result of an oblique impact emplacement of the original impactor, or it may be explained with a perpendicular impact in the Mare Serenitatis location, but on a surface with lunar basalts with different local mechanical properties. By exploiting our boulders size density as a function of the distance from the crater's centre, we derive a possible regolith thickness at the Linne impact of 4.75 m, supporting similar values based on Earth-based radar and optical data in the Mare Serenitatis basin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1812.00590v1-abstract-full').style.display = 'none'; document.getElementById('1812.00590v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Paper accepted by Planetary and Space Science Journal on 27 Nov 2018</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1809.10424">arXiv:1809.10424</a> <span> [<a href="https://arxiv.org/pdf/1809.10424">pdf</a>, <a href="https://arxiv.org/format/1809.10424">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/aae526">10.3847/1538-3881/aae526 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Models of Rosetta/OSIRIS 67P dust coma phase function </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Moreno%2C+F">Fernando Moreno</a>, <a href="/search/?searchtype=author&query=Guirado%2C+D">Daniel Guirado</a>, <a href="/search/?searchtype=author&query=Mu%C3%B1oz%2C+O">Olga Mu帽oz</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">Ivano Bertini</a>, <a href="/search/?searchtype=author&query=Tubiana%2C+C">Cecilia Tubiana</a>, <a href="/search/?searchtype=author&query=Guttler%2C+C">Carsten Guttler</a>, <a href="/search/?searchtype=author&query=Fulle%2C+M">Marco Fulle</a>, <a href="/search/?searchtype=author&query=Rotundi%2C+A">Alessandra Rotundi</a>, <a href="/search/?searchtype=author&query=Della+Corte%2C+V">Vincenzo Della Corte</a>, <a href="/search/?searchtype=author&query=Ivanovski%2C+S">Stavro Ivanovski</a>, <a href="/search/?searchtype=author&query=Rinaldi%2C+G">Giovanna Rinaldi</a>, <a href="/search/?searchtype=author&query=Bockelee-Morvan%2C+D">Dominique Bockelee-Morvan</a>, <a href="/search/?searchtype=author&query=Zakharov%2C+V">Vladimir Zakharov</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">Jessica Agarwal</a>, <a href="/search/?searchtype=author&query=Mottola%2C+S">Stefano Mottola</a>, <a href="/search/?searchtype=author&query=Toth%2C+I">Imre Toth</a>, <a href="/search/?searchtype=author&query=Frattin%2C+E">Elisa Frattin</a>, <a href="/search/?searchtype=author&query=Lara%2C+L">Luisa Lara</a>, <a href="/search/?searchtype=author&query=Gutierrez%2C+P">Pedro Gutierrez</a>, <a href="/search/?searchtype=author&query=Lin%2C+Z+Y">Zhong Yi Lin</a>, <a href="/search/?searchtype=author&query=Kolokolova%2C+L">Ludmilla Kolokolova</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">Holger Sierks</a>, <a href="/search/?searchtype=author&query=Naletto%2C+G">Giampiero Naletto</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P">Philippe Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">Rafael Rodrigo</a> , et al. (17 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1809.10424v1-abstract-short" style="display: inline;"> The phase function of the dust coma of comet 67P has been determined from Rosetta/OSIRIS images \citep{Bertini17}. This function show a deep minimum at phase angles near 100$^\circ$, and a strong backscattering enhancement. These two properties cannot be reproduced by regular models of cometary dust, most of them based on wavelength-sized and randomly-oriented aggregate particles. We show, however… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.10424v1-abstract-full').style.display = 'inline'; document.getElementById('1809.10424v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1809.10424v1-abstract-full" style="display: none;"> The phase function of the dust coma of comet 67P has been determined from Rosetta/OSIRIS images \citep{Bertini17}. This function show a deep minimum at phase angles near 100$^\circ$, and a strong backscattering enhancement. These two properties cannot be reproduced by regular models of cometary dust, most of them based on wavelength-sized and randomly-oriented aggregate particles. We show, however, that an ensamble of oriented elongated particles of a wide variety of aspect ratios, with radii $r \gtrsim$10 $渭$m, and whose long axes are perpendicular to the direction of the solar radiation, are capable of reproducing the observed phase function. These particles must be absorbing, with an imaginary part of the refractive index of about 0.1 to match the expected geometric albedo, and with porosity in the 60-70\% range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.10424v1-abstract-full').style.display = 'none'; document.getElementById('1809.10424v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by Astronomical Journal, September 26th, 2018. 21 pages, 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1809.03997">arXiv:1809.03997</a> <span> [<a href="https://arxiv.org/pdf/1809.03997">pdf</a>, <a href="https://arxiv.org/format/1809.03997">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201833803">10.1051/0004-6361/201833803 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Linking surface morphology, composition, and activity on the nucleus of 67P/Churyumov-Gerasimenko </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fornasier%2C+S">S. Fornasier</a>, <a href="/search/?searchtype=author&query=Hoang%2C+V+H">V. H. Hoang</a>, <a href="/search/?searchtype=author&query=Hasselmann%2C+P+H">P. H. Hasselmann</a>, <a href="/search/?searchtype=author&query=Feller%2C+C">C. Feller</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Deshapriya%2C+J+D+P">J. D. P. Deshapriya</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Naletto%2C+G">G. Naletto</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+L">P. L. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Bodewits%2C+D">D. Bodewits</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Debei%2C+S">S. Debei</a>, <a href="/search/?searchtype=author&query=De+Cecco%2C+M">M. De Cecco</a>, <a href="/search/?searchtype=author&query=Deller%2C+J">J. Deller</a>, <a href="/search/?searchtype=author&query=Ferrari%2C+S">S. Ferrari</a>, <a href="/search/?searchtype=author&query=Fulle%2C+M">M. Fulle</a>, <a href="/search/?searchtype=author&query=Gutierrez%2C+P+J">P. J. Gutierrez</a> , et al. (15 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1809.03997v1-abstract-short" style="display: inline;"> The Rosetta space probe accompanied comet 67P/Churyumov-Gerasimenko for more than two years, obtaining an unprecedented amount of unique data of the comet nucleus and inner coma. This work focuses identifying the source regions of faint jets and outbursts and on studying the spectrophotometric properties of some outbursts. We use observations acquired with the OSIRIS/NAC camera during July-October… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.03997v1-abstract-full').style.display = 'inline'; document.getElementById('1809.03997v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1809.03997v1-abstract-full" style="display: none;"> The Rosetta space probe accompanied comet 67P/Churyumov-Gerasimenko for more than two years, obtaining an unprecedented amount of unique data of the comet nucleus and inner coma. This work focuses identifying the source regions of faint jets and outbursts and on studying the spectrophotometric properties of some outbursts. We use observations acquired with the OSIRIS/NAC camera during July-October 2015, that is, close to perihelion. More than 200 jets of different intensities were identified directly on the nucleus. Some of the more intense outbursts appear spectrally bluer than the comet dark terrain in the vivible-to-near-infrared region. We attribute this spectral behavior to icy grains mixed with the ejected dust. Some of the jets have an extremely short lifetime. They appear on the cometary surface during the color sequence observations, and vanish in less than some few minutes after reaching their peak. We also report a resolved dust plume observed in May 2016 at a resolution of 55 cm/pixel, which allowed us to estimate an optical depth of $\sim$0.65 and an ejected mass of $\sim$ 2200 kg. We present the results on the location, duration, and colors of active sources on the nucleus of 67P from the medium-resolution (i.e., 6-10 m/pixel) images acquired close to perihelion passage. The observed jets are mainly located close to boundaries between different morphological regions. Jets depart not only from cliffs, but also from smooth and dust-covered areas, from fractures, pits, or cavities that cast shadows and favor the recondensation of volatiles. This study shows that faint jets or outbursts continuously contribute to the cometary activity close to perihelion passage, and that these events are triggered by illumination conditions. Faint jets or outbursts are not associated with a particular terrain type or morphology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.03997v1-abstract-full').style.display = 'none'; document.getElementById('1809.03997v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication on Astronomy and Astrophysics on 27 August 2018. 27 pages, 18 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 630, A7 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1712.07508">arXiv:1712.07508</a> <span> [<a href="https://arxiv.org/pdf/1712.07508">pdf</a>, <a href="https://arxiv.org/format/1712.07508">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201732155">10.1051/0004-6361/201732155 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Tensile Strength of 67P/Churyumov-Gerasimenko Nucleus Material from Overhangs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Attree%2C+N">N. Attree</a>, <a href="/search/?searchtype=author&query=Groussin%2C+O">O. Groussin</a>, <a href="/search/?searchtype=author&query=Jorda%2C+L">L. Jorda</a>, <a href="/search/?searchtype=author&query=N%C3%A9bouy%2C+D">D. N茅bouy</a>, <a href="/search/?searchtype=author&query=Thomas%2C+N">N. Thomas</a>, <a href="/search/?searchtype=author&query=Brouet%2C+Y">Y. Brouet</a>, <a href="/search/?searchtype=author&query=K%C3%BChrt%2C+E">E. K眉hrt</a>, <a href="/search/?searchtype=author&query=Preusker%2C+F">F. Preusker</a>, <a href="/search/?searchtype=author&query=Scholten%2C+F">F. Scholten</a>, <a href="/search/?searchtype=author&query=Knollenberg%2C+J">J. Knollenberg</a>, <a href="/search/?searchtype=author&query=Hartogh%2C+P">P. Hartogh</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P">P. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M+F">M. F. A'Hearn</a>, <a href="/search/?searchtype=author&query=Auger%2C+A+-">A. -T. Auger</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Bodewits%2C+D">D. Bodewits</a>, <a href="/search/?searchtype=author&query=Boudreault%2C+S">S. Boudreault</a> , et al. (30 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1712.07508v1-abstract-short" style="display: inline;"> We directly measure twenty overhanging cliffs on the surface of comet 67P/Churyumov-Gerasimenko extracted from the latest shape model and estimate the minimum tensile strengths needed to support them against collapse under the comet's gravity. We find extremely low strengths of around one Pa or less (one to five Pa, when scaled to a metre length). The presence of eroded material at the base of mos… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.07508v1-abstract-full').style.display = 'inline'; document.getElementById('1712.07508v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1712.07508v1-abstract-full" style="display: none;"> We directly measure twenty overhanging cliffs on the surface of comet 67P/Churyumov-Gerasimenko extracted from the latest shape model and estimate the minimum tensile strengths needed to support them against collapse under the comet's gravity. We find extremely low strengths of around one Pa or less (one to five Pa, when scaled to a metre length). The presence of eroded material at the base of most overhangs, as well as the observed collapse of two features and implied previous collapse of another, suggests that they are prone to failure and that true material strengths are close to these lower limits (although we only consider static stresses and not dynamic stress from, for example, cometary activity). Thus, a tensile strength of a few pascals is a good approximation for the tensile strength of 67P's nucleus material, which is in agreement with previous work. We find no particular trends in overhang properties with size, over the $\sim10-100$ m range studied here, or location on the nucleus. There are no obvious differences, in terms of strength, height or evidence of collapse, between the populations of overhangs on the two cometary lobes, suggesting that 67P is relatively homogenous in terms of tensile strength. Low material strengths are supportive of cometary formation as a primordial rubble pile or by collisional fragmentation of a small (tens of km) body. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1712.07508v1-abstract-full').style.display = 'none'; document.getElementById('1712.07508v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 December, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 11 figures. Accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 611, A33 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1710.10235">arXiv:1710.10235</a> <span> [<a href="https://arxiv.org/pdf/1710.10235">pdf</a>, <a href="https://arxiv.org/format/1710.10235">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stx2386">10.1093/mnras/stx2386 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence of sub-surface energy storage in comet 67P from the outburst of 2016 July 3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=Della+Corte%2C+V">V. Della Corte</a>, <a href="/search/?searchtype=author&query=Feldman%2C+P+D">P. D. Feldman</a>, <a href="/search/?searchtype=author&query=Geiger%2C+B">B. Geiger</a>, <a href="/search/?searchtype=author&query=Merouane%2C+S">S. Merouane</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Bodewits%2C+D">D. Bodewits</a>, <a href="/search/?searchtype=author&query=Fornasier%2C+S">S. Fornasier</a>, <a href="/search/?searchtype=author&query=Gruen%2C+E">E. Gruen</a>, <a href="/search/?searchtype=author&query=Hasselmann%2C+P">P. Hasselmann</a>, <a href="/search/?searchtype=author&query=Hilchenbach%2C+M">M. Hilchenbach</a>, <a href="/search/?searchtype=author&query=Hoefner%2C+S">S. Hoefner</a>, <a href="/search/?searchtype=author&query=Ivanovski%2C+S">S. Ivanovski</a>, <a href="/search/?searchtype=author&query=Kolokolova%2C+L">L. Kolokolova</a>, <a href="/search/?searchtype=author&query=Pajola%2C+M">M. Pajola</a>, <a href="/search/?searchtype=author&query=Rotundi%2C+A">A. Rotundi</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Steffl%2C+A+J">A. J. Steffl</a>, <a href="/search/?searchtype=author&query=Thomas%2C+N">N. Thomas</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M+F">M. F. A'Hearn</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Boudreault%2C+S">S. Boudreault</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a> , et al. (45 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1710.10235v1-abstract-short" style="display: inline;"> On 3 July 2016, several instruments on board ESA's Rosetta spacecraft detected signs of an outburst event on comet 67P, at a heliocentric distance of 3.32 AU from the sun, outbound from perihelion. We here report on the inferred properties of the ejected dust and the surface change at the site of the outburst. The activity coincided with the local sunrise and continued over a time interval of 14 -… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.10235v1-abstract-full').style.display = 'inline'; document.getElementById('1710.10235v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.10235v1-abstract-full" style="display: none;"> On 3 July 2016, several instruments on board ESA's Rosetta spacecraft detected signs of an outburst event on comet 67P, at a heliocentric distance of 3.32 AU from the sun, outbound from perihelion. We here report on the inferred properties of the ejected dust and the surface change at the site of the outburst. The activity coincided with the local sunrise and continued over a time interval of 14 - 68 minutes. It left a 10m-sized icy patch on the surface. The ejected material comprised refractory grains of several hundred microns in size, and sub-micron-sized water ice grains. The high dust mass production rate is incompatible with the free sublimation of crystalline water ice under solar illumination as the only acceleration process. Additional energy stored near the surface must have increased the gas density. We suggest a pressurized sub-surface gas reservoir, or the crystallization of amorphous water ice as possible causes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.10235v1-abstract-full').style.display = 'none'; document.getElementById('1710.10235v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 19 figures, 5 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> MNRAS 469, S606-S625, 2017 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.06812">arXiv:1707.06812</a> <span> [<a href="https://arxiv.org/pdf/1707.06812">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stx1726">10.1093/mnras/stx1726 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Seasonal Mass Transfer on the Nucleus of Comet 67P/Chuyumov-Gerasimenko </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a>, <a href="/search/?searchtype=author&query=Mottola%2C+S">S. Mottola</a>, <a href="/search/?searchtype=author&query=Hviid%2C+S+F">S. F. Hviid</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=K%C3%BChrt%2C+E">E. K眉hrt</a>, <a href="/search/?searchtype=author&query=Skorov%2C+Y">Y. Skorov</a>, <a href="/search/?searchtype=author&query=Otto%2C+K">K. Otto</a>, <a href="/search/?searchtype=author&query=Vincent%2C+J+-">J. -B. Vincent</a>, <a href="/search/?searchtype=author&query=Oklay%2C+N">N. Oklay</a>, <a href="/search/?searchtype=author&query=Schr%C3%B6der%2C+S+E">S. E. Schr枚der</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a>, <a href="/search/?searchtype=author&query=Pajola%2C+M">M. Pajola</a>, <a href="/search/?searchtype=author&query=Shi%2C+X">X. Shi</a>, <a href="/search/?searchtype=author&query=Bodewits%2C+D">D. Bodewits</a>, <a href="/search/?searchtype=author&query=Toth%2C+I">I. Toth</a>, <a href="/search/?searchtype=author&query=Preusker%2C+F">F. Preusker</a>, <a href="/search/?searchtype=author&query=Scholten%2C+F">F. Scholten</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P">P. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M+F">M. F. A'Hearn</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a> , et al. (25 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1707.06812v1-abstract-short" style="display: inline;"> We collect observational evidence that supports the scheme of mass transfer on the nucleus of comet 67P/Churyumov-Gerasimenko. The obliquity of the rotation axis of 67P causes strong seasonal variations. During perihelion the southern hemisphere is four times more active than the north. Northern territories are widely covered by granular material that indicates back fall originating from the activ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.06812v1-abstract-full').style.display = 'inline'; document.getElementById('1707.06812v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.06812v1-abstract-full" style="display: none;"> We collect observational evidence that supports the scheme of mass transfer on the nucleus of comet 67P/Churyumov-Gerasimenko. The obliquity of the rotation axis of 67P causes strong seasonal variations. During perihelion the southern hemisphere is four times more active than the north. Northern territories are widely covered by granular material that indicates back fall originating from the active south. Decimetre sized chunks contain water ice and their trajectories are influenced by an anti-solar force instigated by sublimation. OSIRIS observations suggest that up to 20 % of the particles directly return to the nucleus surface taking several hours of travel time. The back fall covered northern areas are active if illuminated but produce mainly water vapour. The decimetre chunks from the nucleus surface are too small to contain more volatile compounds such as CO 2 or CO. This causes a north-south dichotomy of the composition measurements in the coma. Active particles are trapped in the gravitational minimum of Hapi during northern winter. They are "shock frozen" and only reactivated when the comet approaches the sun after its aphelion passage. The insolation of the big cavity is enhanced by self-heating, i. e. reflection and IR radiation from the walls. This, together with the pristinity of the active back fall, explains the early observed activity of the Hapi region. Sobek may be a role model for the consolidated bottom of Hapi. Mass transfer in the case of 67P strongly influences the evolution of the nucleus and the interpretation of coma measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.06812v1-abstract-full').style.display = 'none'; document.getElementById('1707.06812v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 20 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Monthly Notices of the Royal Astronomical Society stx1726, 13 July 2017 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.02945">arXiv:1707.02945</a> <span> [<a href="https://arxiv.org/pdf/1707.02945">pdf</a>, <a href="https://arxiv.org/format/1707.02945">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stx1275">10.1093/mnras/stx1275 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The highly active Anhur-Bes regions in the 67P/Churyumov - Gerasimenko comet: results from OSIRIS/ROSETTA observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fornasier%2C+S">S. Fornasier</a>, <a href="/search/?searchtype=author&query=Feller%2C+C">C. Feller</a>, <a href="/search/?searchtype=author&query=Lee%2C+J+C">J. C. Lee</a>, <a href="/search/?searchtype=author&query=Ferrari%2C+S">S. Ferrari</a>, <a href="/search/?searchtype=author&query=Massironi%2C+M">M. Massironi</a>, <a href="/search/?searchtype=author&query=Hasselmann%2C+P+H">P. H. Hasselmann</a>, <a href="/search/?searchtype=author&query=Deshapriya%2C+J+D+P">J. D. P Deshapriya</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=El-Maarry%2C+M+R">M. R. El-Maarry</a>, <a href="/search/?searchtype=author&query=Giacomini%2C+L">L. Giacomini</a>, <a href="/search/?searchtype=author&query=Mottola%2C+S">S. Mottola</a>, <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a>, <a href="/search/?searchtype=author&query=Ip%2C+W+H">W. H. Ip</a>, <a href="/search/?searchtype=author&query=Lin%2C+Z+Y">Z. Y. Lin</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+L">P. L. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M">M. A'Hearn</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a> , et al. (29 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1707.02945v1-abstract-short" style="display: inline;"> The Southern hemisphere of the 67P/Churyumov-Gerasimenko comet has become visible from Rosetta only since March 2015. It was illuminated during the perihelion passage and therefore it contains the regions that experienced the strongest heating and erosion rate, thus exposing the subsurface most pristine material. In this work we investigate, thanks to the OSIRIS images, the geomorphology, the spec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.02945v1-abstract-full').style.display = 'inline'; document.getElementById('1707.02945v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.02945v1-abstract-full" style="display: none;"> The Southern hemisphere of the 67P/Churyumov-Gerasimenko comet has become visible from Rosetta only since March 2015. It was illuminated during the perihelion passage and therefore it contains the regions that experienced the strongest heating and erosion rate, thus exposing the subsurface most pristine material. In this work we investigate, thanks to the OSIRIS images, the geomorphology, the spectrophotometry and some transient events of two Southern hemisphere regions: Anhur and part of Bes. Bes is dominated by outcropping consolidated terrain covered with fine particle deposits, while Anhur appears strongly eroded with elongated canyon-like structures, scarp retreats, different kinds of deposits, and degraded sequences of strata indicating a pervasive layering. We discovered a new 140 m long and 10 m high scarp formed in the Anhur/Bes boundary during/after the perihelion passage, close to the area where exposed CO$_2$ and H$_2$O ices were previously detected. Several jets have been observed originating from these regions, including the strong perihelion outburst, an active pit, and a faint optically thick dust plume. We identify several areas with a relatively bluer slope (i.e. a lower spectral slope value) than their surroundings, indicating a surface composition enriched with some water ice. These spectrally bluer areas are observed especially in talus and gravitational accumulation deposits where freshly exposed material had fallen from nearby scarps and cliffs. The investigated regions become spectrally redder beyond 2 au outbound when the dust mantle became thicker, masking the underlying ice-rich layers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.02945v1-abstract-full').style.display = 'none'; document.getElementById('1707.02945v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 15 figures, published online on 24 May 2017 on Mon. Not. R. Astron. Soc. stx1275, https://doi.org/10.1093/mnras/stx1275</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.00734">arXiv:1707.00734</a> <span> [<a href="https://arxiv.org/pdf/1707.00734">pdf</a>, <a href="https://arxiv.org/format/1707.00734">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stx1691">10.1093/mnras/stx1691 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on cometary surface evolution derived from a statistical analysis of 67P's topography </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Vincent%2C+J+-">J. -B. Vincent</a>, <a href="/search/?searchtype=author&query=Hviid%2C+S+F">S. F. Hviid</a>, <a href="/search/?searchtype=author&query=Mottola%2C+S">S. Mottola</a>, <a href="/search/?searchtype=author&query=Kuehrt%2C+E">E. Kuehrt</a>, <a href="/search/?searchtype=author&query=Preusker%2C+F">F. Preusker</a>, <a href="/search/?searchtype=author&query=Scholten%2C+F">F. Scholten</a>, <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a>, <a href="/search/?searchtype=author&query=Oklay%2C+N">N. Oklay</a>, <a href="/search/?searchtype=author&query=de+Niem%2C+D">D. de Niem</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a>, <a href="/search/?searchtype=author&query=Fulle%2C+M">M. Fulle</a>, <a href="/search/?searchtype=author&query=Pajola%2C+M">M. Pajola</a>, <a href="/search/?searchtype=author&query=Hofmann%2C+M">M. Hofmann</a>, <a href="/search/?searchtype=author&query=Hu%2C+X">X. Hu</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=Lin%2C+Z+-">Z. -Y. Lin</a>, <a href="/search/?searchtype=author&query=Feller%2C+C">C. Feller</a>, <a href="/search/?searchtype=author&query=Gicquel%2C+A">A. Gicquel</a>, <a href="/search/?searchtype=author&query=Boudreault%2C+S">S. Boudreault</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+L">P. L. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M+F">M. F. A'Hearn</a> , et al. (29 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1707.00734v2-abstract-short" style="display: inline;"> We present a statistical analysis of the distribution of large scale topographic features on comet 67P/Churyumov-Gerasimenko. We observe that the cumulative cliff height distribution across the surface follows a power law with a slope equal to -1.69 +- 0.02. When this distribution is studied independently for each region, we find a good correlation between the slope of the power law and the orbita… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.00734v2-abstract-full').style.display = 'inline'; document.getElementById('1707.00734v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.00734v2-abstract-full" style="display: none;"> We present a statistical analysis of the distribution of large scale topographic features on comet 67P/Churyumov-Gerasimenko. We observe that the cumulative cliff height distribution across the surface follows a power law with a slope equal to -1.69 +- 0.02. When this distribution is studied independently for each region, we find a good correlation between the slope of the power law and the orbital erosion rate of the surface. For instance, the northern hemisphere topography is dominated by structures on the 100~m scale while the southern hemisphere topography, illuminated at perihelion, is dominated by 10~m scale terrain features. Our study suggest that the current size of a cliff is controlled not only by material cohesion but by the dominant erosional process in each region. This observation can be generalized to other comets, where we argue that primitive nuclei are characterized by the presence of large cliffs with a cumulative height power index equal to or above -1.5, while older, eroded cometary surfaces have a power index equal to or below -2.3. In effect, our model shows that a measure of the topography provides a quantitative assessment of a comet's erosional history, i.e. its evolutionary age. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.00734v2-abstract-full').style.display = 'none'; document.getElementById('1707.00734v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.00606">arXiv:1707.00606</a> <span> [<a href="https://arxiv.org/pdf/1707.00606">pdf</a>, <a href="https://arxiv.org/format/1707.00606">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computer Vision and Pattern Recognition">cs.CV</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.asr.2017.10.025">10.1016/j.asr.2017.10.025 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Geometric calibration of Colour and Stereo Surface Imaging System of ESA's Trace Gas Orbiter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Tulyakov%2C+S">Stepan Tulyakov</a>, <a href="/search/?searchtype=author&query=Ivanov%2C+A">Anton Ivanov</a>, <a href="/search/?searchtype=author&query=Thomas%2C+N">Nicolas Thomas</a>, <a href="/search/?searchtype=author&query=Roloff%2C+V">Victoria Roloff</a>, <a href="/search/?searchtype=author&query=Pommerol%2C+A">Antoine Pommerol</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">Gabriele Cremonese</a>, <a href="/search/?searchtype=author&query=Weigel%2C+T">Thomas Weigel</a>, <a href="/search/?searchtype=author&query=Fleuret%2C+F">Francois Fleuret</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1707.00606v1-abstract-short" style="display: inline;"> There are many geometric calibration methods for "standard" cameras. These methods, however, cannot be used for the calibration of telescopes with large focal lengths and complex off-axis optics. Moreover, specialized calibration methods for the telescopes are scarce in literature. We describe the calibration method that we developed for the Colour and Stereo Surface Imaging System (CaSSIS) telesc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.00606v1-abstract-full').style.display = 'inline'; document.getElementById('1707.00606v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.00606v1-abstract-full" style="display: none;"> There are many geometric calibration methods for "standard" cameras. These methods, however, cannot be used for the calibration of telescopes with large focal lengths and complex off-axis optics. Moreover, specialized calibration methods for the telescopes are scarce in literature. We describe the calibration method that we developed for the Colour and Stereo Surface Imaging System (CaSSIS) telescope, on board of the ExoMars Trace Gas Orbiter (TGO). Although our method is described in the context of CaSSIS, with camera-specific experiments, it is general and can be applied to other telescopes. We further encourage re-use of the proposed method by making our calibration code and data available on-line. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.00606v1-abstract-full').style.display = 'none'; document.getElementById('1707.00606v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to Advances in Space Research</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1706.02729">arXiv:1706.02729</a> <span> [<a href="https://arxiv.org/pdf/1706.02729">pdf</a>, <a href="https://arxiv.org/ps/1706.02729">ps</a>, <a href="https://arxiv.org/format/1706.02729">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stx1441">10.1093/mnras/stx1441 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Modeling of the outburst on July 29th, 2015 observed with OSIRIS cameras in the southern hemisphere of comet 67P/Churyumov-Gerasimenko </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gicquel%2C+A">A. Gicquel</a>, <a href="/search/?searchtype=author&query=Rose%2C+M">M. Rose</a>, <a href="/search/?searchtype=author&query=Vincent%2C+J+-">J. -B. Vincent</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a>, <a href="/search/?searchtype=author&query=Bodewits%2C+D">D. Bodewits</a>, <a href="/search/?searchtype=author&query=Hearn%2C+M+F+A">M. F. A Hearn</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=Fougere%2C+N">N. Fougere</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Lin%2C+Z+-">Z. -Y. Lin</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+L">P. L. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Besse%2C+S">S. Besse</a>, <a href="/search/?searchtype=author&query=Boudreault%2C+S">S. Boudreault</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Debei%2C+S">S. Debei</a>, <a href="/search/?searchtype=author&query=Deller%2C+J">J. Deller</a> , et al. (38 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1706.02729v1-abstract-short" style="display: inline;"> Images of the nucleus and the coma (gas and dust) of comet 67P/Churyumov- Gerasimenko have been acquired by the OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System) cameras since March 2014 using both the Wide Angle Camera (WAC) and the Narrow Angle Camera (NAC). We use images from the NAC camera to study a bright outburst observed in the southern hemisphere on July 29, 2015. The hi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.02729v1-abstract-full').style.display = 'inline'; document.getElementById('1706.02729v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1706.02729v1-abstract-full" style="display: none;"> Images of the nucleus and the coma (gas and dust) of comet 67P/Churyumov- Gerasimenko have been acquired by the OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System) cameras since March 2014 using both the Wide Angle Camera (WAC) and the Narrow Angle Camera (NAC). We use images from the NAC camera to study a bright outburst observed in the southern hemisphere on July 29, 2015. The high spatial resolution of the NAC is needed to localize the source point of the outburst on the surface of the nucleus. The heliocentric distance is 1.25 au and the spacecraft-comet distance is 186 km. Aiming to better understand the physics that led to the outgassing, we used the Direct Simulation Monte Carlo (DSMC) method to study the gas flow close to the nucleus and the dust trajectories. The goal is to understand the mechanisms producing the outburst. We reproduce the opening angle of the outburst in the model and constrain the outgassing ratio between the outburst source and the local region. The outburst is in fact a combination of both gas and dust, in which the active surface is approximately 10 times more active than the average rate found in the surrounding areas. We need a number of dust particles 7.83 $\times$ 10$^{11}$ - 6.90 $\times$ 10$^{15}$ (radius 1.97 - 185 渭m), which corresponds to a mass of dust 220 - 21 $\times$ 10$^{3}$kg. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1706.02729v1-abstract-full').style.display = 'none'; document.getElementById('1706.02729v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> MN-17-1040-MJ.R1 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1705.03740">arXiv:1705.03740</a> <span> [<a href="https://arxiv.org/pdf/1705.03740">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.pss.2017.04.018">10.1016/j.pss.2017.04.018 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Distance determination method of dust particles using Rosetta OSIRIS NAC and WAC data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Drolshagen%2C+E">E. Drolshagen</a>, <a href="/search/?searchtype=author&query=Ott%2C+T">T. Ott</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=G%C3%BCttler%2C+C">C. G眉ttler</a>, <a href="/search/?searchtype=author&query=Tubiana%2C+C">C. Tubiana</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+I">P. I. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M+F">M. F. A'Hearn</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a>, <a href="/search/?searchtype=author&query=Debei%2C+S">S. Debei</a>, <a href="/search/?searchtype=author&query=De+Cecco%2C+M">M. De Cecco</a>, <a href="/search/?searchtype=author&query=Deller%2C+J">J. Deller</a>, <a href="/search/?searchtype=author&query=Feller%2C+C">C. Feller</a>, <a href="/search/?searchtype=author&query=Fornasier%2C+S">S. Fornasier</a>, <a href="/search/?searchtype=author&query=Fulle%2C+M">M. Fulle</a>, <a href="/search/?searchtype=author&query=Gicquel%2C+A">A. Gicquel</a> , et al. (20 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1705.03740v1-abstract-short" style="display: inline;"> The ESA Rosetta spacecraft has been tracking its target, the Jupiter-family comet 67P/Churyumov-Gerasimenko, in close vicinity for over two years. It hosts the OSIRIS instruments: the Optical, Spectroscopic, and Infrared Remote Imaging System composed of two cameras, see e.g. Keller et al. (2007). In some imaging sequences dedicated to observe dust particles in the comet's coma, the two cameras to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.03740v1-abstract-full').style.display = 'inline'; document.getElementById('1705.03740v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1705.03740v1-abstract-full" style="display: none;"> The ESA Rosetta spacecraft has been tracking its target, the Jupiter-family comet 67P/Churyumov-Gerasimenko, in close vicinity for over two years. It hosts the OSIRIS instruments: the Optical, Spectroscopic, and Infrared Remote Imaging System composed of two cameras, see e.g. Keller et al. (2007). In some imaging sequences dedicated to observe dust particles in the comet's coma, the two cameras took images at the same time. The aim of this work is to use these simultaneous double camera observations to calculate the dust particles' distance to the spacecraft. As the two cameras are mounted on the spacecraft with an offset of 70 cm, the distance of particles observed by both cameras can be determined by a shift of the particles' apparent trails on the images. This paper presents first results of the ongoing work, introducing the distance determination method for the OSIRIS instrument and the analysis of an example particle. We note that this method works for particles in the range of about 500 m - 6000 m from the spacecraft. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.03740v1-abstract-full').style.display = 'none'; document.getElementById('1705.03740v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2017. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.00012">arXiv:1611.00012</a> <span> [<a href="https://arxiv.org/pdf/1611.00012">pdf</a>, <a href="https://arxiv.org/format/1611.00012">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stw2511">10.1093/mnras/stw2511 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Decimetre-scaled spectrophotometric properties of the nucleus of comet 67P/Churyumov-Gerasimenko from OSIRIS observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Feller%2C+C">C. Feller</a>, <a href="/search/?searchtype=author&query=Fornasier%2C+S">S. Fornasier</a>, <a href="/search/?searchtype=author&query=Hasselmann%2C+P+H">P. H. Hasselmann</a>, <a href="/search/?searchtype=author&query=Barucci%2C+A">A. Barucci</a>, <a href="/search/?searchtype=author&query=Preusker%2C+F">F. Preusker</a>, <a href="/search/?searchtype=author&query=Scholten%2C+F">F. Scholten</a>, <a href="/search/?searchtype=author&query=Jorda%2C+L">L. Jorda</a>, <a href="/search/?searchtype=author&query=Pommerol%2C+A">A. Pommerol</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M">M. A'Hearn</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Boudreault%2C+S">S. Boudreault</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B+J+R">B. J. R. Davidsson</a>, <a href="/search/?searchtype=author&query=Debei%2C+S">S. Debei</a>, <a href="/search/?searchtype=author&query=De+Cecco%2C+M">M. De Cecco</a>, <a href="/search/?searchtype=author&query=Deller%2C+J">J. Deller</a>, <a href="/search/?searchtype=author&query=Fulle%2C+M">M. Fulle</a>, <a href="/search/?searchtype=author&query=Giquel%2C+A">A. Giquel</a>, <a href="/search/?searchtype=author&query=Groussin%2C+O">O. Groussin</a>, <a href="/search/?searchtype=author&query=Gutierrez%2C+P+J">P. J. Gutierrez</a>, <a href="/search/?searchtype=author&query=G%C3%BCttler%2C+C">C. G眉ttler</a> , et al. (21 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1611.00012v1-abstract-short" style="display: inline;"> We present the results of the photometric and spectrophotometric properties of the 67P/Churyumov-Gerasimenko nucleus derived with the OSIRIS instrument during the closest fly-by over the comet, which took place on 14 th February 2015 at a distance of {\~} 6 km from the surface. Several images covering the 0掳-33掳 phase angle range were acquired, and the spatial resolution achieved was 11 cm/pxl. Th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.00012v1-abstract-full').style.display = 'inline'; document.getElementById('1611.00012v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.00012v1-abstract-full" style="display: none;"> We present the results of the photometric and spectrophotometric properties of the 67P/Churyumov-Gerasimenko nucleus derived with the OSIRIS instrument during the closest fly-by over the comet, which took place on 14 th February 2015 at a distance of {\~} 6 km from the surface. Several images covering the 0掳-33掳 phase angle range were acquired, and the spatial resolution achieved was 11 cm/pxl. The flown-by region is located on the big lobe of the comet, near the borders of the Ash, Apis and Imhotep regions. Our analysis shows that this region features local heterogeneities at the decimetre scale. We observed difference of reflectance up to 40{\%} between bright spots and sombre regions, and spectral slope variations up to 50{\%}. The spectral reddening effect observed globally on the comet surface by Fornasier et al. (2015) is also observed locally on this region, but with a less steep behaviour. We note that numerous metre-sized boulders, which exhibit a smaller opposition effect, also appear spectrally redder than their surroundings. In this region, we found no evidence linking observed bright spots to exposed water-ice-rich material. We fitted our dataset using the Hapke 2008 photometric model. The region overflown is globally as dark as the whole nucleus (geometric albedo of 6.8{\%}) and it has a high porosity value in the uppermost-layers (86{\%}). These results of the photometric analysis at a decimetre scale indicate that the photometric properties of the flown-by region are similar to those previously found for the whole nucleus. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.00012v1-abstract-full').style.display = 'none'; document.getElementById('1611.00012v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 16 figures, 5 tables, (also presented at DPS48/ESPC11: http://cdsads.u-strasbg.fr/abs/2016DPS....4830004F)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.07743">arXiv:1609.07743</a> <span> [<a href="https://arxiv.org/pdf/1609.07743">pdf</a>, <a href="https://arxiv.org/format/1609.07743">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stw2409">10.1093/mnras/stw2409 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Summer fireworks on comet 67P </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Vincent%2C+J+-">J. -B. Vincent</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M+F">M. F. A'Hearn</a>, <a href="/search/?searchtype=author&query=Lin%2C+Z+-">Z. -Y. Lin</a>, <a href="/search/?searchtype=author&query=El-Maarry%2C+M+R">M. R. El-Maarry</a>, <a href="/search/?searchtype=author&query=Pajola%2C+M">M. Pajola</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+L">P. L. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Besse%2C+S">S. Besse</a>, <a href="/search/?searchtype=author&query=Bodewits%2C+D">D. Bodewits</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a>, <a href="/search/?searchtype=author&query=Debei%2C+S">S. Debei</a>, <a href="/search/?searchtype=author&query=De+Cecco%2C+M">M. De Cecco</a>, <a href="/search/?searchtype=author&query=Deller%2C+J">J. Deller</a>, <a href="/search/?searchtype=author&query=Fornasier%2C+S">S. Fornasier</a> , et al. (30 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1609.07743v1-abstract-short" style="display: inline;"> During its two years mission around comet 67P/Churyumov-Gerasimenko, ESA's Rosetta spacecraft had the unique opportunity to follow closely a comet in the most active part of its orbit. Many studies have presented the typical features associated to the activity of the nucleus, such as localized dust and gas jets. Here we report on series of more energetic transient events observed during the three… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.07743v1-abstract-full').style.display = 'inline'; document.getElementById('1609.07743v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.07743v1-abstract-full" style="display: none;"> During its two years mission around comet 67P/Churyumov-Gerasimenko, ESA's Rosetta spacecraft had the unique opportunity to follow closely a comet in the most active part of its orbit. Many studies have presented the typical features associated to the activity of the nucleus, such as localized dust and gas jets. Here we report on series of more energetic transient events observed during the three months surrounding the comet's perihelion passage in August 2015. We detected and characterized 34 outbursts with the Rosetta cameras, one every 2.4 nucleus rotation. We identified 3 main dust plume morphologies associated to these events: a narrow jet, a broad fan, and more complex plumes featuring both previous types together. These plumes are comparable in scale and temporal variation to what has been observed on other comets. We present a map of the outbursts source locations, and discuss the associated topography. We find that the spatial distribution sources on the nucleus correlates well with morphological region boundaries, especially in areas marked by steep scarps or cliffs. Outbursts occur either in the early morning or shortly after the local noon, indicating two potential processes: Morning outbursts may be triggered by thermal stresses linked to the rapid change of temperature, afternoon events are most likely related to the diurnal or seasonal heat wave reaching volatiles buried under the first surface layer. In addition, we propose that some events can be the result of a completely different mechanism, in which most of the dust is released upon the collapse of a cliff. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.07743v1-abstract-full').style.display = 'none'; document.getElementById('1609.07743v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">MNRAS (2016)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.00551">arXiv:1609.00551</a> <span> [<a href="https://arxiv.org/pdf/1609.00551">pdf</a>, <a href="https://arxiv.org/format/1609.00551">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201628764">10.1051/0004-6361/201628764 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of exposed H$_2$O ice on the nucleus of comet 67P/Churyumov-Gerasimenko </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Filacchione%2C+G">G. Filacchione</a>, <a href="/search/?searchtype=author&query=Fornasier%2C+S">S. Fornasier</a>, <a href="/search/?searchtype=author&query=Raponi%2C+A">A. Raponi</a>, <a href="/search/?searchtype=author&query=Deshapriya%2C+J+D+P">J. D. P. Deshapriya</a>, <a href="/search/?searchtype=author&query=Tosi%2C+F">F. Tosi</a>, <a href="/search/?searchtype=author&query=Feller%2C+C">C. Feller</a>, <a href="/search/?searchtype=author&query=Ciarniello%2C+M">M. Ciarniello</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Capaccioni%2C+F">F. Capaccioni</a>, <a href="/search/?searchtype=author&query=Pommerol%2C+A">A. Pommerol</a>, <a href="/search/?searchtype=author&query=Massironi%2C+M">M. Massironi</a>, <a href="/search/?searchtype=author&query=Oklay%2C+N">N. Oklay</a>, <a href="/search/?searchtype=author&query=Merlin%2C+F">F. Merlin</a>, <a href="/search/?searchtype=author&query=Vincent%2C+J+-">J. -B. Vincent</a>, <a href="/search/?searchtype=author&query=Fulchignoni%2C+M">M. Fulchignoni</a>, <a href="/search/?searchtype=author&query=Guilbert-Lepoutre%2C+A">A. Guilbert-Lepoutre</a>, <a href="/search/?searchtype=author&query=Perna%2C+D">D. Perna</a>, <a href="/search/?searchtype=author&query=Capria%2C+M+T">M. T. Capria</a>, <a href="/search/?searchtype=author&query=Hasselmann%2C+P+H">P. H. Hasselmann</a>, <a href="/search/?searchtype=author&query=Rousseau%2C+B">B. Rousseau</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Bockelee-Morvan%2C+D">D. Bockelee-Morvan</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+L">P. L. Lamy</a>, <a href="/search/?searchtype=author&query=De+Sanctis%2C+C">C. De Sanctis</a> , et al. (20 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1609.00551v1-abstract-short" style="display: inline;"> Since the orbital insertion of the Rosetta spacecraft, comet 67P/Churyumov-Gerasimenko (67P/C-G) has been mapped by OSIRIS camera and VIRTIS spectro-imager, producing a huge quantity of images and spectra of the comet's nucleus. The aim of this work is to search for the presence of H$_2$O on the nucleus which, in general, appears very dark and rich in dehydrated organic material. After selecting i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.00551v1-abstract-full').style.display = 'inline'; document.getElementById('1609.00551v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.00551v1-abstract-full" style="display: none;"> Since the orbital insertion of the Rosetta spacecraft, comet 67P/Churyumov-Gerasimenko (67P/C-G) has been mapped by OSIRIS camera and VIRTIS spectro-imager, producing a huge quantity of images and spectra of the comet's nucleus. The aim of this work is to search for the presence of H$_2$O on the nucleus which, in general, appears very dark and rich in dehydrated organic material. After selecting images of the bright spots which could be good candidates to search for H$_2$O ice, taken at high resolution by OSIRIS, we check for spectral cubes of the selected coordinates to identify these spots observed by VIRTIS. The selected OSIRIS images were processed with the OSIRIS standard pipeline and corrected for the illumination conditions for each pixel using the Lommel-Seeliger disk law. The spots with higher I/F were selected and then analysed spectrophotometrically and compared with the surrounding area. We selected 13 spots as good targets to be analysed by VIRTIS to search for the 2 micron absorption band of water ice in the VIRTIS spectral cubes. Out of the 13 selected bright spots, eight of them present positive H$_2$O ice detection on the VIRTIS data. A spectral analysis was performed and the approximate temperature of each spot was computed. The H$_2$O ice content was confirmed by modeling the spectra with mixing (areal and intimate) of H$_2$O ice and dark terrain, using Hapke's radiative transfer modeling. We also present a detailed analysis of the detected spots. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.00551v1-abstract-full').style.display = 'none'; document.getElementById('1609.00551v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">paper in press in A&A, 13 pages, 6 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 595, A102 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1608.08774">arXiv:1608.08774</a> <span> [<a href="https://arxiv.org/pdf/1608.08774">pdf</a>, <a href="https://arxiv.org/ps/1608.08774">ps</a>, <a href="https://arxiv.org/format/1608.08774">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stw2117">10.1093/mnras/stw2117 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sublimation of icy aggregates in the coma of comet 67P/Churyumov-Gerasimenko detected with the OSIRIS cameras onboard Rosetta </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gicquel%2C+A">A. Gicquel</a>, <a href="/search/?searchtype=author&query=Vincent%2C+J+-">J. -B. Vincent</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M+F">M. F. A'Hearn</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Bodewits%2C+D">D. Bodewits</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Lin%2C+Z+-">Z. -Y. Lin</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+L">P. L. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Besse%2C+S">S. Besse</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a>, <a href="/search/?searchtype=author&query=Debei%2C+S">S. Debei</a>, <a href="/search/?searchtype=author&query=Deller%2C+J">J. Deller</a>, <a href="/search/?searchtype=author&query=De+Cecco%2C+M">M. De Cecco</a>, <a href="/search/?searchtype=author&query=Frattin%2C+E">E. Frattin</a>, <a href="/search/?searchtype=author&query=El-Maarry%2C+M+R">M. R. El-Maarry</a> , et al. (36 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1608.08774v1-abstract-short" style="display: inline;"> Beginning in March 2014, the OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System) cameras began capturing images of the nucleus and coma (gas and dust) of comet 67P/Churyumov-Gerasimenko using both the wide angle camera (WAC) and the narrow angle camera (NAC). The many observations taken since July of 2014 have been used to study the morphology, location, and temporal variation of t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.08774v1-abstract-full').style.display = 'inline'; document.getElementById('1608.08774v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1608.08774v1-abstract-full" style="display: none;"> Beginning in March 2014, the OSIRIS (Optical, Spectroscopic, and Infrared Remote Imaging System) cameras began capturing images of the nucleus and coma (gas and dust) of comet 67P/Churyumov-Gerasimenko using both the wide angle camera (WAC) and the narrow angle camera (NAC). The many observations taken since July of 2014 have been used to study the morphology, location, and temporal variation of the comet's dust jets. We analyzed the dust monitoring observations shortly after the southern vernal equinox on May 30 and 31, 2015 with the WAC at the heliocentric distance Rh = 1.53 AU, where it is possible to observe that the jet rotates with the nucleus. We found that the decline of brightness as a function of the distance of the jet is much steeper than the background coma, which is a first indication of sublimation. We adapted a model of sublimation of icy aggregates and studied the effect as a function of the physical properties of the aggregates (composition and size). The major finding of this article was that through the sublimation of the aggregates of dirty grains (radius a between 5 microm and 50 microm) we were able to completely reproduce the radial brightness profile of a jet beyond 4 km from the nucleus. To reproduce the data we needed to inject a number of aggregates between 8.5 x $10^{13}$ and 8.5 x $10^{10}$ for a = 5 microm and 50 microm respectively, or an initial mass of $H_2O$ ice around 22kg. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.08774v1-abstract-full').style.display = 'none'; document.getElementById('1608.08774v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 August, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures, 3 tables, special issue "The ESLAB 50 Symposium - spacecraft at comets from 1P/Halley to 67P/Churyumov-Gerasimenko" in the Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1608.07933">arXiv:1608.07933</a> <span> [<a href="https://arxiv.org/pdf/1608.07933">pdf</a>, <a href="https://arxiv.org/format/1608.07933">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stw2179">10.1093/mnras/stw2179 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Acceleration of Individual, Decimetre-sized Aggregates in the Lower Coma of Comet 67P/Churyumov-Gerasimenko </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M+F">M. F. A'Hearn</a>, <a href="/search/?searchtype=author&query=Vincent%2C+J+-">J. -B. Vincent</a>, <a href="/search/?searchtype=author&query=Guettler%2C+C">C. Guettler</a>, <a href="/search/?searchtype=author&query=Hoefner%2C+S">S. Hoefner</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Tubiana%2C+C">C. Tubiana</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+L">P. L. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Boudreault%2C+S">S. Boudreault</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a>, <a href="/search/?searchtype=author&query=Debei%2C+S">S. Debei</a>, <a href="/search/?searchtype=author&query=De+Cecco%2C+M">M. De Cecco</a>, <a href="/search/?searchtype=author&query=Deller%2C+J">J. Deller</a>, <a href="/search/?searchtype=author&query=Fornasier%2C+S">S. Fornasier</a>, <a href="/search/?searchtype=author&query=Fulle%2C+M">M. Fulle</a>, <a href="/search/?searchtype=author&query=Gicquel%2C+A">A. Gicquel</a> , et al. (19 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1608.07933v1-abstract-short" style="display: inline;"> We present OSIRIS/NAC observations of decimetre-sized, likely ice-containing aggregates ejected from a confined region on the surface of comet 67P/Churyumov-Gerasimenko. The images were obtained in January 2016 when the comet was at 2 AU from the Sun out-bound from perihelion. We measure the acceleration of individual aggregates through a two-hour image series. Approximately 50% of the aggregates… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.07933v1-abstract-full').style.display = 'inline'; document.getElementById('1608.07933v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1608.07933v1-abstract-full" style="display: none;"> We present OSIRIS/NAC observations of decimetre-sized, likely ice-containing aggregates ejected from a confined region on the surface of comet 67P/Churyumov-Gerasimenko. The images were obtained in January 2016 when the comet was at 2 AU from the Sun out-bound from perihelion. We measure the acceleration of individual aggregates through a two-hour image series. Approximately 50% of the aggregates are accelerated away from the nucleus, and 50% towards it, and likewise towards either horizontal direction. The accelerations are up to one order of magnitude stronger than local gravity, and are most simply explained by the combined effect of gas drag accelerating all aggregates upwards, and the recoil force from asymmetric outgassing, either from rotating aggregates with randomly oriented spin axes and sufficient thermal inertia to shift the temperature maximum away from an aggregate's subsolar region, or from aggregates with variable ice content. At least 10% of the aggregates will escape the gravity field of the nucleus and feed the comet's debris trail, while others may fall back to the surface and contribute to the deposits covering parts of the northern hemisphere. The rocket force plays a crucial role in pushing these aggregates back towards the surface. Our observations show the future back fall material in the process of ejection, and provide the first direct measurement of the acceleration of aggregates in the innermost coma (<2km) of a comet, where gas drag is still significant. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.07933v1-abstract-full').style.display = 'none'; document.getElementById('1608.07933v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 August, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 14 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1607.05632">arXiv:1607.05632</a> <span> [<a href="https://arxiv.org/pdf/1607.05632">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/0004-6256/152/5/130">10.3847/0004-6256/152/5/130 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Changes in the physical environment of the inner coma of 67P/Churyumov-Gerasimenko with decreasing heliocentric distance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bodewits%2C+D">D. Bodewits</a>, <a href="/search/?searchtype=author&query=Lara%2C+L+M">L. M. Lara</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M+F">M. F. A'Hearn</a>, <a href="/search/?searchtype=author&query=La+Forgia%2C+F">F. La Forgia</a>, <a href="/search/?searchtype=author&query=Giquel%2C+A">A. Giquel</a>, <a href="/search/?searchtype=author&query=Kovacs%2C+G">G. Kovacs</a>, <a href="/search/?searchtype=author&query=Knollenberg%2C+J">J. Knollenberg</a>, <a href="/search/?searchtype=author&query=Lazzarin%2C+M">M. Lazzarin</a>, <a href="/search/?searchtype=author&query=Lin%2C+Z+-">Z. -Y. Lin</a>, <a href="/search/?searchtype=author&query=Shi%2C+X">X. Shi</a>, <a href="/search/?searchtype=author&query=Snodgrass%2C+C">C. Snodgrass</a>, <a href="/search/?searchtype=author&query=Tubiana%2C+C">C. Tubiana</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+M">P. M. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Boudreault%2C+S">S. Boudreault</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=DaDeppo%2C+V">V. DaDeppo</a> , et al. (21 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1607.05632v1-abstract-short" style="display: inline;"> The Wide Angle Camera of the OSIRIS instrument on board the Rosetta spacecraft is equipped with several narrowband filters that are centered on the emission lines and bands of various fragment species. These are used to determine the evolution of the production and spatial distribution of the gas in the inner coma of comet 67P with time and heliocentric distance, here between 2.6 - 1.3 AU pre-peri… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.05632v1-abstract-full').style.display = 'inline'; document.getElementById('1607.05632v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.05632v1-abstract-full" style="display: none;"> The Wide Angle Camera of the OSIRIS instrument on board the Rosetta spacecraft is equipped with several narrowband filters that are centered on the emission lines and bands of various fragment species. These are used to determine the evolution of the production and spatial distribution of the gas in the inner coma of comet 67P with time and heliocentric distance, here between 2.6 - 1.3 AU pre-perihelion. Our observations indicate that the emission observed in the OH, OI, CN, NH, and NH2 filters is mostly produced by dissociative electron impact excitation of different parent species. We conclude that CO2 rather than H2O is a significant source of the [OI] 630 nm emission. A strong plume-like feature observed in the in CN and [OI] filters is present throughout our observations. This plume is not present in OH emission and indicates a local enhancement of the CO2/H2O ratio by as much as a factor of 3. We observed a sudden decrease in intensity levels after March 2015, which we attribute to decreased electron temperatures in the first kilometers above the nucleus surface. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.05632v1-abstract-full').style.display = 'none'; document.getElementById('1607.05632v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 figures, 6 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1605.02095">arXiv:1605.02095</a> <span> [<a href="https://arxiv.org/pdf/1605.02095">pdf</a>, <a href="https://arxiv.org/ps/1605.02095">ps</a>, <a href="https://arxiv.org/format/1605.02095">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201527784">10.1051/0004-6361/201527784 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observations and analysis of a curved jet in the coma of comet 67P/Churyumov-Gerasimenko </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lin%2C+Z">Zhong-Yi Lin</a>, <a href="/search/?searchtype=author&query=Lai%2C+I+-">I. -L. Lai</a>, <a href="/search/?searchtype=author&query=Su%2C+C+-">C. -C. Su</a>, <a href="/search/?searchtype=author&query=Ip%2C+W+-">W. -H. Ip</a>, <a href="/search/?searchtype=author&query=Lee%2C+J+-">J. -C. Lee</a>, <a href="/search/?searchtype=author&query=Wu%2C+J+-">J. -S. Wu</a>, <a href="/search/?searchtype=author&query=Vincent%2C+J+-">J. -B. Vincent</a>, <a href="/search/?searchtype=author&query=La+Forgia%2C+F">F. La Forgia</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+L">P. L. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M+F">M. F. A'Hearn</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Bodewits%2C+D">D. Bodewits</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a>, <a href="/search/?searchtype=author&query=Debet%2C+S">S. Debet</a> , et al. (26 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1605.02095v1-abstract-short" style="display: inline;"> We analyze the physical properties and dynamical origin of a curved jet of comet 67P/Churyumov-Gerasimenko that was observed repeatedly in several nucleus rotations starting on May 30 and persisting until early August, 2015. We simulated the motion of dust grains ejected from the nucleus surface under the influence of the gravity and viscous drag effect of the expanding gas flow from the rotating… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.02095v1-abstract-full').style.display = 'inline'; document.getElementById('1605.02095v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.02095v1-abstract-full" style="display: none;"> We analyze the physical properties and dynamical origin of a curved jet of comet 67P/Churyumov-Gerasimenko that was observed repeatedly in several nucleus rotations starting on May 30 and persisting until early August, 2015. We simulated the motion of dust grains ejected from the nucleus surface under the influence of the gravity and viscous drag effect of the expanding gas flow from the rotating nucleus. The formation of the curved jet is a combination of the size of the dust particles (~0.1-1 mm) and the location of the source region near the nucleus equator. This enhances the spiral feature of the collimated dust stream after the dust is accelerated to a terminal speed on the order of m/s. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.02095v1-abstract-full').style.display = 'none'; document.getElementById('1605.02095v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5pages, 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1602.01965">arXiv:1602.01965</a> <span> [<a href="https://arxiv.org/pdf/1602.01965">pdf</a>, <a href="https://arxiv.org/ps/1602.01965">ps</a>, <a href="https://arxiv.org/format/1602.01965">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201527564">10.1051/0004-6361/201527564 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The dust environment of comet 67P/Churyumov-Gerasimenko from Rosetta OSIRIS and VLT observations in the 4.5 to 2.9 au heliocentric distance range inbound </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Moreno%2C+F">F. Moreno</a>, <a href="/search/?searchtype=author&query=Snodgrass%2C+C">C. Snodgrass</a>, <a href="/search/?searchtype=author&query=Hainaut%2C+O">O. Hainaut</a>, <a href="/search/?searchtype=author&query=Tubiana%2C+C">C. Tubiana</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+L">P. L. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=AHearn%2C+M+F">M. F. AHearn</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+L">J. L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Besse%2C+S">S. Besse</a>, <a href="/search/?searchtype=author&query=Bodewits%2C+D">D. Bodewits</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a>, <a href="/search/?searchtype=author&query=Debei%2C+S">S. Debei</a>, <a href="/search/?searchtype=author&query=De+Cecco%2C+M">M. De Cecco</a>, <a href="/search/?searchtype=author&query=Ferri%2C+F">F. Ferri</a>, <a href="/search/?searchtype=author&query=Fornasier%2C+S">S. Fornasier</a> , et al. (29 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1602.01965v1-abstract-short" style="display: inline;"> The ESA Rosetta spacecraft, currently orbiting around comet 67P, has already provided in situ measurements of the dust grain properties from several instruments, particularly OSIRIS and GIADA. We propose adding value to those measurements by combining them with ground-based observations of the dust tail to monitor the overall, time-dependent dust-production rate and size distribution. To constrain… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.01965v1-abstract-full').style.display = 'inline'; document.getElementById('1602.01965v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1602.01965v1-abstract-full" style="display: none;"> The ESA Rosetta spacecraft, currently orbiting around comet 67P, has already provided in situ measurements of the dust grain properties from several instruments, particularly OSIRIS and GIADA. We propose adding value to those measurements by combining them with ground-based observations of the dust tail to monitor the overall, time-dependent dust-production rate and size distribution. To constrain the dust grain properties, we take Rosetta OSIRIS and GIADA results into account, and combine OSIRIS data during the approach phase (from late April to early June 2014) with a large data set of ground-based images that were acquired with the ESO Very Large Telescope (VLT) from February to November 2014. A Monte Carlo dust tail code has been applied to retrieve the dust parameters. Key properties of the grains (density, velocity, and size distribution) were obtained from Rosetta observations: these parameters were used as input of the code to considerably reduce the number of free parameters. In this way, the overall dust mass-loss rate and its dependence on the heliocentric distance could be obtained accurately. The dust parameters derived from the inner coma measurements by OSIRIS and GIADA and from distant imaging using VLT data are consistent, except for the power index of the size-distribution function, which is $伪$=--3, instead of $伪$=--2, for grains smaller than 1 mm. This is possibly linked to the presence of fluffy aggregates in the coma. The onset of cometary activity occurs at approximately 4.3 au, with a dust production rate of 0.5 kg/s, increasing up to 15 kg/s at 2.9 au. This implies a dust-to-gas mass ratio varying between 3.8 and 6.5 for the best-fit model when combined with water-production rates from the MIRO experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.01965v1-abstract-full').style.display = 'none'; document.getElementById('1602.01965v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by Astronomy and Astrophysics (January 17th, 2016)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1512.03193">arXiv:1512.03193</a> <span> [<a href="https://arxiv.org/pdf/1512.03193">pdf</a>, <a href="https://arxiv.org/format/1512.03193">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201527159">10.1051/0004-6361/201527159 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Are fractured cliffs the source of cometary dust jets ? Insights from OSIRIS/Rosetta at 67P </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Vincent%2C+J+-">J. -B. Vincent</a>, <a href="/search/?searchtype=author&query=Oklay%2C+N">N. Oklay</a>, <a href="/search/?searchtype=author&query=Pajola%2C+M">M. Pajola</a>, <a href="/search/?searchtype=author&query=H%C3%B6fner%2C+S">S. H枚fner</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Hu%2C+X">X. Hu</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+L">P. L. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M+F">M. F. A'Hearn</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Besse%2C+S">S. Besse</a>, <a href="/search/?searchtype=author&query=Bodewits%2C+D">D. Bodewits</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a>, <a href="/search/?searchtype=author&query=Debei%2C+S">S. Debei</a>, <a href="/search/?searchtype=author&query=De+Cecco%2C+M">M. De Cecco</a>, <a href="/search/?searchtype=author&query=El-Maarry%2C+M+R">M. R. El-Maarry</a>, <a href="/search/?searchtype=author&query=Fornasier%2C+S">S. Fornasier</a> , et al. (30 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1512.03193v2-abstract-short" style="display: inline;"> Dust jets, i.e. fuzzy collimated streams of cometary material arising from the nucleus, have been observed in-situ on all comets since the Giotto mission flew by comet 1P/Halley in 1986. Yet their formation mechanism remains unknown. Several solutions have been proposed, from localized physical mechanisms on the surface/sub-surface (see review in Belton (2010)) to purely dynamical processes involv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.03193v2-abstract-full').style.display = 'inline'; document.getElementById('1512.03193v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.03193v2-abstract-full" style="display: none;"> Dust jets, i.e. fuzzy collimated streams of cometary material arising from the nucleus, have been observed in-situ on all comets since the Giotto mission flew by comet 1P/Halley in 1986. Yet their formation mechanism remains unknown. Several solutions have been proposed, from localized physical mechanisms on the surface/sub-surface (see review in Belton (2010)) to purely dynamical processes involving the focusing of gas flows by the local topography (Crifo et al. 2002). While the latter seems to be responsible for the larger features, high resolution imagery has shown that broad streams are composed of many smaller features (a few meters wide) that connect directly to the nucleus surface. We monitored these jets at high resolution and over several months to understand what are the physical processes driving their formation, and how this affects the surface. Using many images of the same areas with different viewing angles, we performed a 3-dimensional reconstruction of collimated jets, and linked them precisely to their sources on the nucleus. Results.We show here observational evidence that the Northern hemisphere jets of comet 67P arise from areas with sharp topographic changes and describe the physical processes involved. We propose a model in which active cliffs are the main source of jet-like features, and therefore the regions eroding the fastest on comets. We suggest that this is a common mechanism taking place on all comets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.03193v2-abstract-full').style.display = 'none'; document.getElementById('1512.03193v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by Astronomy & Astrophysics on 4 December 2015</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 587, A14 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.02794">arXiv:1509.02794</a> <span> [<a href="https://arxiv.org/pdf/1509.02794">pdf</a>, <a href="https://arxiv.org/format/1509.02794">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201527020">10.1051/0004-6361/201527020 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Temporal morphological changes in the Imhotep region of comet 67P/Churyumov-Gerasimenko </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Groussin%2C+O">O. Groussin</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P">P. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a>, <a href="/search/?searchtype=author&query=Hearn%2C+M+F+A">M. F. A Hearn</a>, <a href="/search/?searchtype=author&query=Auger%2C+A+-">A. -T. Auger</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Besse%2C+S">S. Besse</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a>, <a href="/search/?searchtype=author&query=Debei%2C+S">S. Debei</a>, <a href="/search/?searchtype=author&query=De+Cecco%2C+M">M. De Cecco</a>, <a href="/search/?searchtype=author&query=El-Maarry%2C+M+R">M. R. El-Maarry</a>, <a href="/search/?searchtype=author&query=Fornasier%2C+S">S. Fornasier</a>, <a href="/search/?searchtype=author&query=Fulle%2C+M">M. Fulle</a>, <a href="/search/?searchtype=author&query=Guti%C3%A9rrez%2C+P+J">P. J. Guti茅rrez</a>, <a href="/search/?searchtype=author&query=G%C3%BCttler%2C+C">C. G眉ttler</a>, <a href="/search/?searchtype=author&query=Hviid%2C+S">S. Hviid</a> , et al. (23 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1509.02794v1-abstract-short" style="display: inline;"> We report on the first major temporal morphological changes observed on the surface of the nucleus of comet 67P/Churyumov-Gerasimenko, in the smooth terrains of the Imhotep region. We use images of the OSIRIS cameras onboard Rosetta to follow the temporal changes from 24 May 2015 to 11 July 2015. The morphological changes observed on the surface are visible in the form of roundish features, which… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.02794v1-abstract-full').style.display = 'inline'; document.getElementById('1509.02794v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.02794v1-abstract-full" style="display: none;"> We report on the first major temporal morphological changes observed on the surface of the nucleus of comet 67P/Churyumov-Gerasimenko, in the smooth terrains of the Imhotep region. We use images of the OSIRIS cameras onboard Rosetta to follow the temporal changes from 24 May 2015 to 11 July 2015. The morphological changes observed on the surface are visible in the form of roundish features, which are growing in size from a given location in a preferential direction, at a rate of 5.6 - 8.1$\times$10$^{-5}$ m s$^{-1}$ during the observational period. The location where changes started and the contours of the expanding features are bluer than the surroundings, suggesting the presence of ices (H$_2$O and/or CO$_2$) exposed on the surface. However, sublimation of ices alone is not sufficient to explain the observed expanding features. No significant variations in the dust activity pattern are observed during the period of changes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.02794v1-abstract-full').style.display = 'none'; document.getElementById('1509.02794v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 3 figures; Letter for Astronomy and Astrophysics: accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 583, A36 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.02707">arXiv:1509.02707</a> <span> [<a href="https://arxiv.org/pdf/1509.02707">pdf</a>, <a href="https://arxiv.org/format/1509.02707">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201526379">10.1051/0004-6361/201526379 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gravitational slopes, geomorphology, and material strengths of the nucleus of comet 67P/Churyumov-Gerasimenko from OSIRIS observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Groussin%2C+O">O. Groussin</a>, <a href="/search/?searchtype=author&query=Jorda%2C+L">L. Jorda</a>, <a href="/search/?searchtype=author&query=Auger%2C+A+-">A. -T. Auger</a>, <a href="/search/?searchtype=author&query=K%C3%BChrt%2C+E">E. K眉hrt</a>, <a href="/search/?searchtype=author&query=Gaskell%2C+R">R. Gaskell</a>, <a href="/search/?searchtype=author&query=Capanna%2C+C">C. Capanna</a>, <a href="/search/?searchtype=author&query=Scholten%2C+F">F. Scholten</a>, <a href="/search/?searchtype=author&query=Preusker%2C+F">F. Preusker</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P">P. Lamy</a>, <a href="/search/?searchtype=author&query=Hviid%2C+S">S. Hviid</a>, <a href="/search/?searchtype=author&query=Knollenberg%2C+J">J. Knollenberg</a>, <a href="/search/?searchtype=author&query=Keller%2C+U">U. Keller</a>, <a href="/search/?searchtype=author&query=Huettig%2C+C">C. Huettig</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=Hearn%2C+M+F+A">M. F. A Hearn</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Boudreault%2C+S">S. Boudreault</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a> , et al. (27 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1509.02707v1-abstract-short" style="display: inline;"> We study the link between gravitational slopes and the surface morphology on the nucleus of comet 67P/Churyumov-Gerasimenko and provide constraints on the mechanical properties of the cometary material. We computed the gravitational slopes for five regions on the nucleus that are representative of the different morphologies observed on the surface, using two shape models computed from OSIRIS image… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.02707v1-abstract-full').style.display = 'inline'; document.getElementById('1509.02707v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.02707v1-abstract-full" style="display: none;"> We study the link between gravitational slopes and the surface morphology on the nucleus of comet 67P/Churyumov-Gerasimenko and provide constraints on the mechanical properties of the cometary material. We computed the gravitational slopes for five regions on the nucleus that are representative of the different morphologies observed on the surface, using two shape models computed from OSIRIS images by the stereo-photoclinometry (SPC) and stereo-photogrammetry (SPG) techniques. We estimated the tensile, shear, and compressive strengths using different surface morphologies and mechanical considerations. The different regions show a similar general pattern in terms of the relation between gravitational slopes and terrain morphology: i) low-slope terrains (0-20 deg) are covered by a fine material and contain a few large ($>$10 m) and isolated boulders, ii) intermediate-slope terrains (20-45 deg) are mainly fallen consolidated materials and debris fields, with numerous intermediate-size boulders from $<$1 m to 10 m for the majority of them, and iii) high-slope terrains (45-90 deg) are cliffs that expose a consolidated material and do not show boulders or fine materials. The best range for the tensile strength of overhangs is 3-15 Pa (upper limit of 150 Pa), 4-30 Pa for the shear strength of fine surface materials and boulders, and 30-150 Pa for the compressive strength of overhangs (upper limit of 1500 Pa). The strength-to-gravity ratio is similar for 67P and weak rocks on Earth. As a result of the low compressive strength, the interior of the nucleus may have been compressed sufficiently to initiate diagenesis, which could have contributed to the formation of layers. Our value for the tensile strength is comparable to that of dust aggregates formed by gravitational instability and tends to favor a formation of comets by the accrection of pebbles at low velocities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.02707v1-abstract-full').style.display = 'none'; document.getElementById('1509.02707v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 15 figures, 1 table; Astronomy and Astrophysics, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1505.06888">arXiv:1505.06888</a> <span> [<a href="https://arxiv.org/pdf/1505.06888">pdf</a>, <a href="https://arxiv.org/ps/1505.06888">ps</a>, <a href="https://arxiv.org/format/1505.06888">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201525901">10.1051/0004-6361/201525901 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectrophotometric properties of the nucleus of comet 67P/Churyumov-Gerasimenko from the OSIRIS instrument onboard the ROSETTA spacecraft </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fornasier%2C+S">S. Fornasier</a>, <a href="/search/?searchtype=author&query=Hasselmann%2C+P+H">P. H. Hasselmann</a>, <a href="/search/?searchtype=author&query=Barucci%2C+M+A">M. A. Barucci</a>, <a href="/search/?searchtype=author&query=Feller%2C+C">C. Feller</a>, <a href="/search/?searchtype=author&query=Besse%2C+S">S. Besse</a>, <a href="/search/?searchtype=author&query=Leyrat%2C+C">C. Leyrat</a>, <a href="/search/?searchtype=author&query=Lara%2C+L">L. Lara</a>, <a href="/search/?searchtype=author&query=Gutierrez%2C+P+J">P. J. Gutierrez</a>, <a href="/search/?searchtype=author&query=Oklay%2C+N">N. Oklay</a>, <a href="/search/?searchtype=author&query=Tubiana%2C+C">C. Tubiana</a>, <a href="/search/?searchtype=author&query=Scholten%2C+F">F. Scholten</a>, <a href="/search/?searchtype=author&query=Sierks%2C+H">H. Sierks</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P+L">P. L. Lamy</a>, <a href="/search/?searchtype=author&query=Rodrigo%2C+R">R. Rodrigo</a>, <a href="/search/?searchtype=author&query=Koschny%2C+D">D. Koschny</a>, <a href="/search/?searchtype=author&query=Rickman%2C+H">H. Rickman</a>, <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=A%27Hearn%2C+M+F">M. F. A'Hearn</a>, <a href="/search/?searchtype=author&query=Bertaux%2C+J+-">J. -L. Bertaux</a>, <a href="/search/?searchtype=author&query=Bertini%2C+I">I. Bertini</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Da+Deppo%2C+V">V. Da Deppo</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a> , et al. (29 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1505.06888v1-abstract-short" style="display: inline;"> The Rosetta mission of the European Space Agency has been orbiting the comet 67P/Churyumov-Gerasimenko (67P) since August 2014 and is now in its escort phase. A large complement of scientific experiments designed to complete the most detailed study of a comet ever attempted are onboard Rosetta. We present results for the photometric and spectrophotometric properties of the nucleus of 67P derived f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.06888v1-abstract-full').style.display = 'inline'; document.getElementById('1505.06888v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1505.06888v1-abstract-full" style="display: none;"> The Rosetta mission of the European Space Agency has been orbiting the comet 67P/Churyumov-Gerasimenko (67P) since August 2014 and is now in its escort phase. A large complement of scientific experiments designed to complete the most detailed study of a comet ever attempted are onboard Rosetta. We present results for the photometric and spectrophotometric properties of the nucleus of 67P derived from the OSIRIS imaging system, which consists of a Wide Angle Camera (WAC) and a Narrow Angle Camera (NAC). The disk-averaged phase function of the nucleus of 67P shows a strong opposition surge with a G parameter value of -0.13$\pm$0.01 in the HG system formalism and an absolute magnitude $H_v(1,1,0)$ = 15.74$\pm$0.02 mag. The integrated spectrophotometry in 20 filters covering the 250-1000 nm wavelength range shows a red spectral behavior, without clear absorption bands except for a potential absorption centered at $\sim$ 290 nm that is possibly due to SO$_2$ ice. The nucleus shows strong phase reddening, with disk-averaged spectral slopes increasing from 11\%/(100 nm) to 16\%/(100 nm) in the 1.3$^{\circ}$--54$^{\circ}$ phase angle range. The geometric albedo of the comet is 6.5$\pm$0.2\% at 649 nm, with local variations of up to $\sim$ 16\% in the Hapi region. From the disk-resolved images we computed the spectral slope together with local spectrophotometry and identified three distinct groups of regions (blue, moderately red, and red). The Hapi region is the brightest, the bluest in term of spectral slope, and the most active surface on the comet. Local spectrophotometry shows an enhancement of the flux in the 700-750 nm that is associated with coma emissions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.06888v1-abstract-full').style.display = 'none'; document.getElementById('1505.06888v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 May, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18, pages, 14 figures, Astronomy and Astrophysics, in press</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 583, A30 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1211.7284">arXiv:1211.7284</a> <span> [<a href="https://arxiv.org/pdf/1211.7284">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> MarcoPolo-R narrow angle camera: a three-mirror anastigmat design proposal with a smart finite conjugates refocusing optical system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Antichi%2C+J">Jacopo Antichi</a>, <a href="/search/?searchtype=author&query=Tordi%2C+M">Massimiliano Tordi</a>, <a href="/search/?searchtype=author&query=Magrin%2C+D">Demetrio Magrin</a>, <a href="/search/?searchtype=author&query=Ragazzoni%2C+R">Roberto Ragazzoni</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">Gabriele Cremonese</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1211.7284v1-abstract-short" style="display: inline;"> MarcoPolo-R is a medium-class space mission proposed for the 2015-2025 ESA Cosmic Vision Program with primary goal to return to Earth an unaltered sample from a primitive near-Earth asteroid (NEA). Among the proposed instruments on board, its narrow-angle camera (NAC) should be able to image the candidate object with spatial resolution of 3 mm per pixel at 200 m from its surface. The camera should… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.7284v1-abstract-full').style.display = 'inline'; document.getElementById('1211.7284v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1211.7284v1-abstract-full" style="display: none;"> MarcoPolo-R is a medium-class space mission proposed for the 2015-2025 ESA Cosmic Vision Program with primary goal to return to Earth an unaltered sample from a primitive near-Earth asteroid (NEA). Among the proposed instruments on board, its narrow-angle camera (NAC) should be able to image the candidate object with spatial resolution of 3 mm per pixel at 200 m from its surface. The camera should also be able to support the lander descent operations by imaging the target from several distances in order to locate a suitable place for the landing. Hence a refocusing system is requested to accomplish this task, extending its imaging capabilities. Here we present a three-mirror anastigmat (TMA) common-axis optical design, providing high-quality imaging performances by selecting as entrance pupil the system aperture stop and exploiting the motion of a single mirror inside the instrument to allow the wide image refocusing requested, from infinity up to 200 m above the NEA surface. Such proposal matches with the NAC technical specifications and can be easily implemented with present day technology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.7284v1-abstract-full').style.display = 'none'; document.getElementById('1211.7284v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 November, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 26 figures, SPIE 2012 Optical Systems Design</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1105.5272">arXiv:1105.5272</a> <span> [<a href="https://arxiv.org/pdf/1105.5272">pdf</a>, <a href="https://arxiv.org/ps/1105.5272">ps</a>, <a href="https://arxiv.org/format/1105.5272">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.pss.2011.06.007">10.1016/j.pss.2011.06.007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The effects of the target material properties and layering on the crater chronology: the case of Raditladi and Rachmaninoff basins on Mercury </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Marchi%2C+S">S. Marchi</a>, <a href="/search/?searchtype=author&query=Massironi%2C+M">M. Massironi</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Martellato%2C+E">E. Martellato</a>, <a href="/search/?searchtype=author&query=Giacomini%2C+L">L. Giacomini</a>, <a href="/search/?searchtype=author&query=Prockter%2C+L">L. Prockter</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1105.5272v1-abstract-short" style="display: inline;"> In this paper we present a crater age determination of several terrains associated with the Raditladi and Rachmaninoff basins. These basins were discovered during the first and third MESSENGER flybys of Mercury, respectively. One of the most interesting features of both basins is their relatively fresh appearance. The young age of both basins is confirmed by our analysis on the basis of age determ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1105.5272v1-abstract-full').style.display = 'inline'; document.getElementById('1105.5272v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1105.5272v1-abstract-full" style="display: none;"> In this paper we present a crater age determination of several terrains associated with the Raditladi and Rachmaninoff basins. These basins were discovered during the first and third MESSENGER flybys of Mercury, respectively. One of the most interesting features of both basins is their relatively fresh appearance. The young age of both basins is confirmed by our analysis on the basis of age determination via crater chronology. The derived Rachmaninoff and Raditladi basin model ages are about 3.6 Ga and 1.1 Ga, respectively. Moreover, we also constrain the age of the smooth plains within the basins' floors. This analysis shows that Mercury had volcanic activity until recent time, possibly to about 1 Ga or less. We find that some of the crater size-frequency distributions investigated suggest the presence of a layered target. Therefore, within this work we address the importance of considering terrain parameters, as geo-mechanical properties and layering, into the process of age determination. We also comment on the likelihood of the availability of impactors able to form basins with the sizes of Rachmaninoff and Raditladi in relatively recent times. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1105.5272v1-abstract-full').style.display = 'none'; document.getElementById('1105.5272v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 May, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by PSS, to appear on MESSENGER Flybys special issue</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1003.5655">arXiv:1003.5655</a> <span> [<a href="https://arxiv.org/pdf/1003.5655">pdf</a>, <a href="https://arxiv.org/ps/1003.5655">ps</a>, <a href="https://arxiv.org/format/1003.5655">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.pss.2010.03.017">10.1016/j.pss.2010.03.017 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Cratering History of Asteroid (2867) Steins </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Marchi%2C+S">S. Marchi</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Kueppers%2C+M">M. Kueppers</a>, <a href="/search/?searchtype=author&query=Marzari%2C+F">F. Marzari</a>, <a href="/search/?searchtype=author&query=Davidsson%2C+B">B. Davidsson</a>, <a href="/search/?searchtype=author&query=Keller%2C+H+U">H. U. Keller</a>, <a href="/search/?searchtype=author&query=Besse%2C+S">S. Besse</a>, <a href="/search/?searchtype=author&query=Lamy%2C+P">P. Lamy</a>, <a href="/search/?searchtype=author&query=Mottola%2C+S">S. Mottola</a>, <a href="/search/?searchtype=author&query=Massironi%2C+M">M. Massironi</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1003.5655v1-abstract-short" style="display: inline;"> The cratering history of main belt asteroid (2867) Steins has been investigated using OSIRIS imagery acquired during the Rosetta flyby that took place on the 5th of September 2008. For this purpose, we applied current models describing the formation and evolution of main belt asteroids, that provide the rate and velocity distributions of impactors. These models coupled with appropr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1003.5655v1-abstract-full').style.display = 'inline'; document.getElementById('1003.5655v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1003.5655v1-abstract-full" style="display: none;"> The cratering history of main belt asteroid (2867) Steins has been investigated using OSIRIS imagery acquired during the Rosetta flyby that took place on the 5th of September 2008. For this purpose, we applied current models describing the formation and evolution of main belt asteroids, that provide the rate and velocity distributions of impactors. These models coupled with appropriate crater scaling laws, allow the cratering history to be estimated. Hence, we derive Steins' cratering retention age, namely the time lapsed since its formation or global surface reset. We also investigate the influence of various factors -like bulk structure and crater erasing- on the estimated age, which spans from a few hundred Myrs to more than 1Gyr, depending on the adopted scaling law and asteroid physical parameters. Moreover, a marked lack of craters smaller than about 0.6km has been found and interpreted as a result of a peculiar evolution of Steins cratering record, possibly related either to the formation of the 2.1km wide impact crater near the south pole or to YORP reshaping. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1003.5655v1-abstract-full').style.display = 'none'; document.getElementById('1003.5655v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 March, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by Planetary and Space Science</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0910.1399">arXiv:0910.1399</a> <span> [<a href="https://arxiv.org/pdf/0910.1399">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1029/2009GL040353">10.1029/2009GL040353 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mercury's geochronology revised by applying Model Production Functions to Mariner 10 data: geological implications </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Massironi%2C+M">M. Massironi</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Marchi%2C+S">S. Marchi</a>, <a href="/search/?searchtype=author&query=Martellato%2C+M">M. Martellato</a>, <a href="/search/?searchtype=author&query=Mottola%2C+M">M. Mottola</a>, <a href="/search/?searchtype=author&query=Wagner%2C+R+J">R. J. Wagner</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0910.1399v1-abstract-short" style="display: inline;"> Model Production Function chronology uses dynamic models of the Main Belt Asteroids (MBAs) and Near Earth Objects (NEOs) to derive the impactor flux to a target body. This is converted into the crater size-frequency-distribution for a specific planetary surface, and calibrated using the radiometric ages of different regions of the Moon's surface. This new approach has been applied to the crater… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0910.1399v1-abstract-full').style.display = 'inline'; document.getElementById('0910.1399v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0910.1399v1-abstract-full" style="display: none;"> Model Production Function chronology uses dynamic models of the Main Belt Asteroids (MBAs) and Near Earth Objects (NEOs) to derive the impactor flux to a target body. This is converted into the crater size-frequency-distribution for a specific planetary surface, and calibrated using the radiometric ages of different regions of the Moon's surface. This new approach has been applied to the crater counts on Mariner 10 images of the highlands and of several large impact basins on Mercury. MPF estimates for the plains show younger ages than those of previous chronologies. Assuming a variable uppermost layering of the Hermean crust, the age of the Caloris interior plains may be as young as 3.59 Ga, in agreement with MESSENGER results that imply that long-term volcanism overcame contractional tectonics. The MPF chronology also suggests a variable projectile flux through time, coherent with the MBAs for ancient periods and then gradually comparable also to the NEOs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0910.1399v1-abstract-full').style.display = 'none'; document.getElementById('0910.1399v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 October, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by Journal Geophysical Research Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0903.5137">arXiv:0903.5137</a> <span> [<a href="https://arxiv.org/pdf/0903.5137">pdf</a>, <a href="https://arxiv.org/ps/0903.5137">ps</a>, <a href="https://arxiv.org/format/0903.5137">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0004-6256/137/6/4936">10.1088/0004-6256/137/6/4936 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new chronology for the Moon and Mercury </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Marchi%2C+S">S. Marchi</a>, <a href="/search/?searchtype=author&query=Mottola%2C+S">S. Mottola</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Massironi%2C+M">M. Massironi</a>, <a href="/search/?searchtype=author&query=Martellato%2C+E">E. Martellato</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0903.5137v1-abstract-short" style="display: inline;"> In this paper we present a new method for dating the surface of the Moon, obtained by modeling the incoming flux of impactors and converting it into a size distribution of resulting craters. We compare the results from this model with the standard chronology for the Moon showing their similarities and discrepancies. In particular, we find indications of a non-constant impactor flux in the last 5… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0903.5137v1-abstract-full').style.display = 'inline'; document.getElementById('0903.5137v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0903.5137v1-abstract-full" style="display: none;"> In this paper we present a new method for dating the surface of the Moon, obtained by modeling the incoming flux of impactors and converting it into a size distribution of resulting craters. We compare the results from this model with the standard chronology for the Moon showing their similarities and discrepancies. In particular, we find indications of a non-constant impactor flux in the last 500 Myr and also discuss the implications of our findings for the Late Heavy Bombardment hypothesis. We also show the potential of our model for accurate dating of other inner Solar System bodies, by applying it to Mercury. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0903.5137v1-abstract-full').style.display = 'none'; document.getElementById('0903.5137v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 March, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 13 figures, 1 table; accepted by AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0209373">arXiv:astro-ph/0209373</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0209373">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0209373">ps</a>, <a href="https://arxiv.org/format/astro-ph/0209373">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/S1384-1076(02)00176-8">10.1016/S1384-1076(02)00176-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Asteroid detection at millimetric wavelengths with the Planck survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Marzari%2C+F">F. Marzari</a>, <a href="/search/?searchtype=author&query=Burigana%2C+C">C. Burigana</a>, <a href="/search/?searchtype=author&query=Maris%2C+M">M. Maris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0209373v1-abstract-short" style="display: inline;"> The Planck mission, originally devised for cosmological studies, offers the opportunity to observe Solar System objects at millimetric and submillimetric wavelengths. We concentrate in this paper on the asteroids of the Main Belt. We intend to estimate the number of asteroids that can can be detected during the mission and to evaluate the strength of their signal. We have rescaled the instrument… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0209373v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0209373v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0209373v1-abstract-full" style="display: none;"> The Planck mission, originally devised for cosmological studies, offers the opportunity to observe Solar System objects at millimetric and submillimetric wavelengths. We concentrate in this paper on the asteroids of the Main Belt. We intend to estimate the number of asteroids that can can be detected during the mission and to evaluate the strength of their signal. We have rescaled the instrument sensitivities, calculated by the LFI and HFI teams for sources fixed in the sky, introducing some degradation factors to properly account for moving objects. In this way a detection threshold is derived for asteroidal detection that is related to the diameter of the asteroid and its geocentric distance. We have developed a numerical code that models the detection of asteroids in the LFI and HFI channels during the mission. This code perfoprms a detailed integration of the orbits of the asteroids in the timespan of the mission and identifies those bodies that fall in the beams of Planck and their signal stenght. According to our simulations, a total of 397 objects will be observed by Planck and an asteroidal body will be detected in some beam in 30% of the total sky scan--circles. A significant fraction (in the range from ~50 to 100 objects) of the 397 asteroids will be observed with a high S/N ratio. Flux measurements of a large sample of asteroids in the submillimeter and millimeter range are relevant since they allow to analyze the thermal emission and its relation to the surface and regolith properties. Furthermore, it will be possible to check on a wider base the two standard thermal models, based on a nonrotating or rapidly rotating sphere. Our method can also be used to separate Solar System sources from cosmological sources in the survey. This work is based on Planck LFI activities. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0209373v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0209373v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 September, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2002. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Contact person cremonese@pd.astro.it. Accepted for pubblication in New Astronomy (2002). 1 figure in .eps format. Needs elsart.cls style + harvard.sty</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> New Astron. 7 (2002) 483-494 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0106447">arXiv:astro-ph/0106447</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0106447">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0106447">ps</a>, <a href="https://arxiv.org/format/astro-ph/0106447">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1046/j.1365-8711.2001.04748.x">10.1046/j.1365-8711.2001.04748.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 1999 Quadrantids and the lunar Na atmosphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Verani%2C+S">S. Verani</a>, <a href="/search/?searchtype=author&query=Barbieri%2C+C">C. Barbieri</a>, <a href="/search/?searchtype=author&query=Benn%2C+C+R">C. R. Benn</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Mendillo%2C+M">M. Mendillo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0106447v1-abstract-short" style="display: inline;"> Enhancements of the Na emission and temperature from the lunar atmosphere were reported during the Leonids meteor showers of 1995, 1997 and 1998. Here we report a search for similar enhancement during the 1999 Quadrantids, which have the highest mass flux of any of the major streams. No enhancements were detected. We suggest that different chemical-physical properties of the Leonid and Quadranti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0106447v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0106447v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0106447v1-abstract-full" style="display: none;"> Enhancements of the Na emission and temperature from the lunar atmosphere were reported during the Leonids meteor showers of 1995, 1997 and 1998. Here we report a search for similar enhancement during the 1999 Quadrantids, which have the highest mass flux of any of the major streams. No enhancements were detected. We suggest that different chemical-physical properties of the Leonid and Quadrantid streams may be responsible for the difference. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0106447v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0106447v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 June, 2001; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2001. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 1 figure, accepted for publication in MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mon.Not.Roy.Astron.Soc. 327 (2001) 244 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0101493">arXiv:astro-ph/0101493</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0101493">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0101493">ps</a>, <a href="https://arxiv.org/format/astro-ph/0101493">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/320378">10.1086/320378 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multicolor Photometry of the Uranus Irregular Satellites Sycorax and Caliban </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Maris%2C+M">Michele Maris</a>, <a href="/search/?searchtype=author&query=Carraro%2C+G">Giovanni Carraro</a>, <a href="/search/?searchtype=author&query=Cremonese%2C+G">Gabriele Cremonese</a>, <a href="/search/?searchtype=author&query=Fulle%2C+M">Marco Fulle</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/0101493v1-abstract-short" style="display: inline;"> We report on accurate BVRI photometry for the two Uranus irregular satellites Sycorax and Caliban. We derive colours, showing that Sycorax is bluer than Caliban. Our data allows us to detect a significant variability in the Caliban's light-curve, which suggests an estimated period of about 3 hours. Despite it is the brighter of the two bodies, Sycorax does not display a strong statistically sig… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0101493v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0101493v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0101493v1-abstract-full" style="display: none;"> We report on accurate BVRI photometry for the two Uranus irregular satellites Sycorax and Caliban. We derive colours, showing that Sycorax is bluer than Caliban. Our data allows us to detect a significant variability in the Caliban's light-curve, which suggests an estimated period of about 3 hours. Despite it is the brighter of the two bodies, Sycorax does not display a strong statistically significant variability. However our data seem to suggest a period of about 4 hours <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0101493v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0101493v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 January, 2001; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2001. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 2 eps figures, in press in Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9710022">arXiv:astro-ph/9710022</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9710022">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9710022">ps</a>, <a href="https://arxiv.org/format/astro-ph/9710022">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1086/311040">10.1086/311040 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutral sodium from comet Hale-Bopp: a third type of tail </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Cremonese%2C+G">G. Cremonese</a>, <a href="/search/?searchtype=author&query=Boehnhardt%2C+H">H. Boehnhardt</a>, <a href="/search/?searchtype=author&query=Crovisier%2C+J">J. Crovisier</a>, <a href="/search/?searchtype=author&query=Fitzsimmons%2C+A">A. Fitzsimmons</a>, <a href="/search/?searchtype=author&query=Fulle%2C+M">M. Fulle</a>, <a href="/search/?searchtype=author&query=Licandro%2C+J">J. Licandro</a>, <a href="/search/?searchtype=author&query=Pollacco%2C+D">D. Pollacco</a>, <a href="/search/?searchtype=author&query=Rauer%2C+H">H. Rauer</a>, <a href="/search/?searchtype=author&query=Tozzi%2C+G+P">G. P. Tozzi</a>, <a href="/search/?searchtype=author&query=West%2C+R+M">R. M. West</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="astro-ph/9710022v1-abstract-short" style="display: inline;"> We report on the discovery and analysis of a striking neutral sodium gas tail associated with comet C/1995 O1 Hale-Bopp. Sodium D-line emission has been observed at heliocentric distance r<1.4 AU in some long-period comets and the presence of neutral sodium in the tailward direction of a few bright comets has been noted, but the extent, and in particular the source, has never been clear. Here we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9710022v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9710022v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9710022v1-abstract-full" style="display: none;"> We report on the discovery and analysis of a striking neutral sodium gas tail associated with comet C/1995 O1 Hale-Bopp. Sodium D-line emission has been observed at heliocentric distance r<1.4 AU in some long-period comets and the presence of neutral sodium in the tailward direction of a few bright comets has been noted, but the extent, and in particular the source, has never been clear. Here we describe the first observations and analysis of a neutral sodium gas tail in comet Hale-Bopp, entirely different from the previously known ion and dust tails. We show that the observed characteristics of this third type of tail are consistent with itbeing produced by radiation pressure due to resonance fluorescence of sodium atoms and that the lifetime for photoionization is consistent with recent theoretical calculation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9710022v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9710022v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 October, 1997; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 1997. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 3 figures, it will pubblished on A.P.J. Letter</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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