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1. IGAPS: the merged IPHAS and UVEX optical surveys of theNorthern Galactic Plane

Author

Monguió, M., Greimel, R., Drew, J. E., Barentsen, G., Groot, P. J., Irwin, M. J., Casares, J., Gänsicke, B. T., Carter, P. J., Corral-Santana, J. M., Gentile-Fusillo, N. P., Greiss, S., van Haaften, L. M., Hollands, M., Jones, D., Kupfer, T., Manser, C. J., Murphy, D. N. A., McLeod, A. F., Oosting, T., Parker, Q. A., Pyrzas, S., Rodríguez-Gil, P., van Roestel, J., Scaringi, S., Schellart, P., Toloza, O., Vaduvescu, O., van Spaandonk, L., Verbeek, K., Wright, N. J., Eislöffel, J., Fabregat, J., Harris, A., Morris, R. A. H., Phillipps, S., Raddi, R., Sabin, L., Unruh, Y., Vink, J. S, Wesson, R., Cardwell, A., Cochrane, R. K., Doostmohammadi, S., Mocnik, T., Stoev, H., Suárez-Andrés, L., Tudor, V., Wilson, T. G., and Zegmott, T. J.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

The INT Galactic Plane Survey (IGAPS) is the merger of the optical photometric surveys, IPHAS and UVEX, based on data from the Isaac Newton Telescope (INT) obtained between 2003 and 2018. Here, we present the IGAPS point source catalogue. It contains 295.4 million rows providing photometry in the filters, i, r, narrow-band Halpha, g and U_RGO. The IGAPS footprint fills the Galactic coordinate range, |b| < 5deg and 30deg < l < 215deg. A uniform calibration, referred to the Pan-STARRS system, is applied to g, r and i, while the Halpha calibration is linked to r and then is reconciled via field overlaps. The astrometry in all 5 bands has been recalculated on the Gaia DR2 frame. Down to i ~ 20 mag (Vega system), most stars are also detected in g, r and Halpha. As exposures in the r band were obtained within the IPHAS and UVEX surveys a few years apart, typically, the catalogue includes two distinct r measures, r_I and r_U. The r 10sigma limiting magnitude is ~21, with median seeing 1.1 arcsec. Between ~13th and ~19th magnitudes in all bands, the photometry is internally reproducible to within 0.02 magnitudes. Stars brighter than r=19.5 have been tested for narrow-band Halpha excess signalling line emission, and for variation exceeding |r_I-r_U| = 0.2 mag. We find and flag 8292 candidate emission line stars and over 53000 variables (both at >5sigma confidence). The 174-column catalogue will be available via CDS Strasbourg., Comment: 28 pages, 22 figures

Published
2020
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2. The 2014-2017 outburst of the young star ASASSN-13db: A time-resolved picture of a very low-mass star between EXors and FUors

Author

Sicilia-Aguilar, A., Oprandi, A., Froebrich, D., Fang, M., Prieto, J. L., Stanek, K., Scholz, A., Kochanek, C. S., Henning, Th., Gredel, R., Holoien, T. W. -S., Rabus, M., Shappee, B. J., Billington, S. J., Campbell-White, J., and Zegmott, T. J.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

ASASSN-13db is a M5-type star with a protoplanetary disk, the lowest mass star known to experience accretion outbursts. Since its discovery in 2013, it has experienced two outbursts, the second of which started in November 2014 and lasted until February 2017. We use high- and low-resolution spectroscopy and time-resolved photometry from the ASAS-SN survey, the LCOGT and the Beacon Observatory to study the lightcurve and the dynamical and physical properties of the accretion flow. The 2014-2017 outburst lasted for nearly 800 days. A 4.15d period in the lightcurve likely corresponds to rotational modulation of a star with hot spot(s). The spectra show multiple emission lines with variable inverse P-Cygni profiles and a highly variable blueshifted absorption below the continuum. Line ratios from metallic emission lines (Fe I/Fe II, Ti I/Ti II) suggest temperatures of $\sim$5800-6000 K in the accretion flow. Photometrically and spectroscopically, the 2014-2017 event displays an intermediate behavior between EXors and FUors. The accretion rate (\.{M}=1-3$\times$10$^{-7}$M$_\odot$/yr), about 2 orders of magnitude higher than the accretion rate in quiescence, is not significantly different from the accretion rate observed in 2013. The absorption features in the spectra suggest that the system is viewed at a high angle and drives a powerful, non-axisymmetric wind, maybe related to magnetic reconnection. The properties of ASASSN-13db suggest that temperatures lower than those for solar-type stars are needed for modeling accretion in very low-mass systems. Finally, the rotational modulation during the outburst reveals that accretion-related structures settled after the begining of the outburst and can be relatively stable and long-lived. Our work also demonstrates the power of time-resolved photometry and spectroscopy to explore the properties of variable and outbursting stars. (Abridged)., Comment: A&A in press. 19 pages plus appendix. Revised version: corrected for typos

Published
2017
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3. The 67P/Churyumov-Gerasimenko observation campaign in support of the Rosetta mission

Author

Snodgrass, C., A'Hearn, M. F., Aceituno, F., Afanasiev, V., Bagnulo, S., Bauer, J., Bergond, G., Besse, S., Biver, N., Bodewits, D., Boehnhardt, H., Bonev, B. P., Borisov, G., Carry, B., Casanova, V., Cochran, A., Conn, B. C., Davidsson, B., Davies, J. K., de León, J., de Mooij, E., de Val-Borro, M., Delacruz, M., DiSanti, M. A., Drew, J. E., Duffard, R., Edberg, N. J. T., Faggi, S., Feaga, L., Fitzsimmons, A., Fujiwara, H., Gibb, E. L., Gillon, M., Green, S. F., Guijarro, A., Guilbert-Lepoutre, A., Gutiérrez, P. J., Hadamcik, E., Hainaut, O., Haque, S., Hedrosa, R., Hines, D., Hopp, U., Hoyo, F., Hutsemékers, D., Hyland, M., Ivanova, O., Jehin, E., Jones, G. H., Keane, J. V., Kelley, M. S. P., Kiselev, N., Kleyna, J., Kluge, M., Knight, M. M., Kokotanekova, R., Koschny, D., Kramer, E., López-Moreno, J. J., Lacerda, P., Lara, L. M., Lasue, J., Lehto, H. J., Levasseur-Regourd, A. C., Licandro, J., Lin, Z. Y., Lister, T., Lowry, S. C., Mainzer, A., Manfroid, J., Marchant, J., McKay, A. J., McNeill, A., Meech, K. J., Micheli, M., Mohammed, I., Monguió, M., Moreno, F., Muñoz, O., Mumma, M. J., Nikolov, P., Opitom, C., Ortiz, J. L., Paganini, L., Pajuelo, M., Pozuelos, F. J., Protopapa, S., Pursimo, T., Rajkumar, B., Ramanjooloo, Y., Ramos, E., Ries, C., Riffeser, A., Rosenbush, V., Rousselot, P., Ryan, E. L., Santos-Sanz, P., Schleicher, D. G., Schmidt, M., Schulz, R., Sen, A. K., Somero, A., Sota, A., Stinson, A., Sunshine, J., Thompson, A., Tozzi, G. P., Tubiana, C., Villanueva, G. L., Wang, X., Wooden, D. H., Yagi, M., Yang, B., Zaprudin, B., and Zegmott, T. J.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present a summary of the campaign of remote observations that supported the European Space Agency's Rosetta mission. Telescopes across the globe (and in space) followed comet 67P/Churyumov-Gerasimenko from before Rosetta's arrival until nearly the end of mission in September 2016. These provided essential data for mission planning, large-scale context information for the coma and tails beyond the spacecraft, and a way to directly compare 67P with other comets. The observations revealed 67P to be a relatively `well behaved' comet, typical of Jupiter family comets and with activity patterns that repeat from orbit-to-orbit. Comparison between this large collection of telescopic observations and the in situ results from Rosetta will allow us to better understand comet coma chemistry and structure. This work is just beginning as the mission ends -- in this paper we present a summary of the ground-based observations and early results, and point to many questions that will be addressed in future studies., Comment: Author prepared version; final published version available at journal. 22 pages

Published
2017
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4. IGAPS: The merged IPHAS and UVEX optical surveys of the northern Galactic plane

Author

Monguió-Tortajada, Marta, Casares, J., Corral-Santana, Jesús M., Jones, David, Rodriguez-Gil, Pablo, Vaduvescu, Ovidiu, Zegmott, T. J., Science and Technology Facilities Council (UK), Ministerio de Economía y Competitividad (España), Universidad de Barcelona, Netherlands Organization for Scientific Research, Ministerio de Ciencia, Innovación y Universidades (España), European Commission, and German Research Foundation

Subjects
general [Stars], evolution [Stars], Surveys, Catalogues, disk [Galaxy]
Abstract

The INT Galactic Plane Survey (IGAPS) is the merger of the optical photometric surveys, IPHAS and UVEX, based on data from the Isaac Newton Telescope (INT) obtained between 2003 and 2018. Here, we present the IGAPS point source catalogue. It contains 295.4 million rows providing photometry in the filters, i, r, narrow-band Hα, g, and URGO. The IGAPS footprint fills the Galactic coordinate range, |b| < 5° and 30°ℓ < < 215°. A uniform calibration, referred to as the Pan-STARRS system, is applied to g, r, and i, while the Hα calibration is linked to r and then is reconciled via field overlaps. The astrometry in all five bands has been recalculated in the reference frame of Gaia Data Release 2. Down to i ∼ 20 mag (Vega system), most stars are also detected in g, r, and Hα. As exposures in the r band were obtained in both the IPHAS and UVEX surveys, typically a few years apart, the catalogue includes two distinct r measures, rI and rU. The r 10σ limiting magnitude is approximately 21, with median seeing of 1.1 arcsec. Between approximately 13th and 19th mag in all bands, the photometry is internally reproducible to within 0.02 mag. Stars brighter than r = 19.5 mag are tested for narrow-band Hα excess signalling line emission, and for variation exceeding |rIℓ-ℓ rU| = 0.2 mag. We find and flag 8292 candidate emission line stars and over 53 000 variables (both at > 5σ confidence). MM, JED and GB acknowledge the support of research grants funded by the Science, Technology and Facilities Council of the UK (STFC, grants ST/M001008/1 and ST/J001333/1). MM was partially supported by the MINECO (Spanish Ministry of Economy) through grant ESP2016-80079-C2-1-R and RTI2018-095076-B-C21 (MINECO/FEDER, UE), and MDM-2014-0369 of ICCUB (Unidad de Excelencia “María de Maeztu”). RG benefitted from support via STFC grant ST/M001334/1 as a visitor to UCL. PJG acknowledges support from the Netherlands Organisation for Scientific Research (NWO), in contributing to the Isaac Newton Group of Telescopes and through grant 614.000.601. JC acknowldges support by the Spanish Ministry of Economy, Industry and Competitiveness (MINECO) under grant AYA2017-83216-P. DJ and PR-G acknowledge support from the State Research Agency (AEI) of the Spanish Ministry of Science, Innovation and Universities (MCIU) and the European Regional Development Fund (FEDER) under grant AYA2017-83383-P. RR acknowledges funding by the German Science foundation (DFG) through grants HE1356/71-1 and IR190/1-1. We thank Eugene Magnier for providing support on Pan-STARRS data. This research has made use of the University of Hertfordshire high-performance computing facility (https://uhhpc.herts.ac.uk/) located at the University of Hertfordshire (supported by STFC grants including ST/P000096/1). We thank Martin Hardcastle for his support and expertise in connection with our use of the facility. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www. cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Much of the analysis presented has been carried out via TopCat and stilts (Taylor et al. 2006). We thank the referee for comments on this paper that have improved its content.

Published
2020

5. IGAPS: the merged IPHAS and UVEX optical surveys of the northern Galactic plane

Author

Monguió, M., primary, Greimel, R., additional, Drew, J. E., additional, Barentsen, G., additional, Groot, P. J., additional, Irwin, M. J., additional, Casares, J., additional, Gänsicke, B. T., additional, Carter, P. J., additional, Corral-Santana, J. M., additional, Gentile-Fusillo, N. P., additional, Greiss, S., additional, van Haaften, L. M., additional, Hollands, M., additional, Jones, D., additional, Kupfer, T., additional, Manser, C. J., additional, Murphy, D. N. A., additional, McLeod, A. F., additional, Oosting, T., additional, Parker, Q. A., additional, Pyrzas, S., additional, Rodríguez-Gil, P., additional, van Roestel, J., additional, Scaringi, S., additional, Schellart, P., additional, Toloza, O., additional, Vaduvescu, O., additional, van Spaandonk, L., additional, Verbeek, K., additional, Wright, N. J., additional, Eislöffel, J., additional, Fabregat, J., additional, Harris, A., additional, Morris, R. A. H., additional, Phillipps, S., additional, Raddi, R., additional, Sabin, L., additional, Unruh, Y., additional, Vink, J. S., additional, Wesson, R., additional, Cardwell, A., additional, de Burgos, A., additional, Cochrane, R. K., additional, Doostmohammadi, S., additional, Mocnik, T., additional, Stoev, H., additional, Suárez-Andrés, L., additional, Tudor, V., additional, Wilson, T. G., additional, and Zegmott, T. J., additional

Published
2020
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6. Shape model and spin-state analysis of PHA contact binary (85990) 1999 JV6 from combined radar and optical observations

Author

Rożek, A., primary, Lowry, S. C., additional, Nolan, M. C., additional, Taylor, P. A., additional, Benner, L. A. M., additional, Fitzsimmons, A., additional, Zegmott, T. J., additional, Weissman, P. R., additional, Green, S. F., additional, Rozitis, B., additional, Snodgrass, C., additional, Smythe, W. D., additional, Hicks, M. D., additional, Howell, E. S., additional, Virkki, A. K., additional, Aponte-Hernandez, B., additional, Rivera-Valentín, E. G., additional, Rodriguez-Ford, L. A., additional, Zambrano-Marin, L. F., additional, Brozović, M., additional, Naidu, S. P., additional, Giorgini, J. D., additional, Snedeker, L. G., additional, Jao, J. S., additional, and Ghigo, F. D., additional

Published
2019
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7. The 2014–2017 outburst of the young star ASASSN-13db

Author

Sicilia-Aguilar, A., primary, Oprandi, A., additional, Froebrich, D., additional, Fang, M., additional, Prieto, J. L., additional, Stanek, K., additional, Scholz, A., additional, Kochanek, C. S., additional, Henning, Th., additional, Gredel, R., additional, Holoien, T. W.- S., additional, Rabus, M., additional, Shappee, B. J., additional, Billington, S. J., additional, Campbell-White, J., additional, and Zegmott, T. J., additional

Published
2017
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8. The 67P/Churyumov–Gerasimenko observation campaign in support of the Rosetta mission

Author

Snodgrass, C., primary, A'Hearn, M. F., additional, Aceituno, F., additional, Afanasiev, V., additional, Bagnulo, S., additional, Bauer, J., additional, Bergond, G., additional, Besse, S., additional, Biver, N., additional, Bodewits, D., additional, Boehnhardt, H., additional, Bonev, B. P., additional, Borisov, G., additional, Carry, B., additional, Casanova, V., additional, Cochran, A., additional, Conn, B. C., additional, Davidsson, B., additional, Davies, J. K., additional, de León, J., additional, de Mooij, E., additional, de Val-Borro, M., additional, Delacruz, M., additional, DiSanti, M. A., additional, Drew, J. E., additional, Duffard, R., additional, Edberg, N. J. T., additional, Faggi, S., additional, Feaga, L., additional, Fitzsimmons, A., additional, Fujiwara, H., additional, Gibb, E. L., additional, Gillon, M., additional, Green, S. F., additional, Guijarro, A., additional, Guilbert-Lepoutre, A., additional, Gutiérrez, P. J., additional, Hadamcik, E., additional, Hainaut, O., additional, Haque, S., additional, Hedrosa, R., additional, Hines, D., additional, Hopp, U., additional, Hoyo, F., additional, Hutsemékers, D., additional, Hyland, M., additional, Ivanova, O., additional, Jehin, E., additional, Jones, G. H., additional, Keane, J. V., additional, Kelley, M. S. P., additional, Kiselev, N., additional, Kleyna, J., additional, Kluge, M., additional, Knight, M. M., additional, Kokotanekova, R., additional, Koschny, D., additional, Kramer, E. A., additional, López-Moreno, J. J., additional, Lacerda, P., additional, Lara, L. M., additional, Lasue, J., additional, Lehto, H. J., additional, Levasseur-Regourd, A. C., additional, Licandro, J., additional, Lin, Z. Y., additional, Lister, T., additional, Lowry, S. C., additional, Mainzer, A., additional, Manfroid, J., additional, Marchant, J., additional, McKay, A. J., additional, McNeill, A., additional, Meech, K. J., additional, Micheli, M., additional, Mohammed, I., additional, Monguió, M., additional, Moreno, F., additional, Muñoz, O., additional, Mumma, M. J., additional, Nikolov, P., additional, Opitom, C., additional, Ortiz, J. L., additional, Paganini, L., additional, Pajuelo, M., additional, Pozuelos, F. J., additional, Protopapa, S., additional, Pursimo, T., additional, Rajkumar, B., additional, Ramanjooloo, Y., additional, Ramos, E., additional, Ries, C., additional, Riffeser, A., additional, Rosenbush, V., additional, Rousselot, P., additional, Ryan, E. L., additional, Santos-Sanz, P., additional, Schleicher, D. G., additional, Schmidt, M., additional, Schulz, R., additional, Sen, A. K., additional, Somero, A., additional, Sota, A., additional, Stinson, A., additional, Sunshine, J. M., additional, Thompson, A., additional, Tozzi, G. P., additional, Tubiana, C., additional, Villanueva, G. L., additional, Wang, X., additional, Wooden, D. H., additional, Yagi, M., additional, Yang, B., additional, Zaprudin, B., additional, and Zegmott, T. J., additional

Published
2017
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10. Shape model and spin-state analysis of PHA contact binary (85990) 1999 JV6 from combined radar and optical observations

Author

Rozek, A., Lowry, S. C., Nolan, M. C., Taylor, P. A., Benner, L. A. M., Fitzsimmons, A., Zegmott, T. J., Weissman, P. R., Green, Simon, Rozitis, Benjamin, Snodgrass, Colin, Smythe, W. D., Hicks, M. D., Howell, E. S., Virkki, A. K., Aponte-Hernandez, B., Rivera-Valentin, E. G., Rodriguez-Ford, L. A., Zambrano-Marin, L. F., Brozovic, M., Naidu, S. P., Giorgini, J. D., Snedeker, L. G., Jao, J. S., Ghigo, F. D., Rozek, A., Lowry, S. C., Nolan, M. C., Taylor, P. A., Benner, L. A. M., Fitzsimmons, A., Zegmott, T. J., Weissman, P. R., Green, Simon, Rozitis, Benjamin, Snodgrass, Colin, Smythe, W. D., Hicks, M. D., Howell, E. S., Virkki, A. K., Aponte-Hernandez, B., Rivera-Valentin, E. G., Rodriguez-Ford, L. A., Zambrano-Marin, L. F., Brozovic, M., Naidu, S. P., Giorgini, J. D., Snedeker, L. G., Jao, J. S., and Ghigo, F. D.

Abstract

Context. The potentially hazardous asteroid (85990)1999 JV6 has been a target of previously published thermal-infrared observations and optical photometry. It has been identified as a promising candidate for possible Yarkovsky-O’Keefe-Radzievskii-Paddack (YORP) effect detection. Aims. The YORP effect is a small thermal-radiation torque considered to be a key factor in spin-state evolution of small Solar System bodies. In order to detect YORP on 1999 JV6 we developed a detailed shape model and analysed the spin-state using both optical and radar observations. Methods. For 1999 JV6, we collected optical photometry between 2007 and 2016. Additionally, we obtained radar echo-power spectra and imaging observations with Arecibo and Goldstone planetary radar facilities in 2015, 2016, and 2017. We combined our data with published optical photometry to develop a robust physical model. Results. We determine that the rotation pole resides at negative latitudes in an area with a 5◦ radius close to the south ecliptic pole. The refined sidereal rotation period is 6.536787±0.000007 h. The radar images are best reproduced with a bilobed shape model. Both lobes of 1999 JV6 can be represented as oblate ellipsoids with a smaller, more spherical component resting at the end of a larger, more elongated component. While contact binaries appear to be abundant in the near-Earth population, there are only a few published shape models for asteroids in this particular configuration. By combining the radar-derived shape model with optical light curves we determine a constant-period solution that fits all available data well. Using light-curve data alone we determine an upper limit for YORP of 8.5×10−8 rad day−2. Conclusions. The bifurcated shape of 1999 JV6 might be a result of two ellipsoidal components gently merging with each other, or a deformation of a rubble pile with a weak-tensile-strength core due t

11. The 67P/Churyumov–Gerasimenko observation campaign in support of the Rosetta mission

Author

Snodgrass, C., A'Hearn, M. F., Aceituno, F., Afanasiev, V., Bagnulo, S., Bauer, J., Bergond, G., Besse, S., Biver, N., Bodewits, D., Boehnhardt, H., Bonev, B. P., Borisov, G., Carry, B., Casanova, V., Cochran, A., Conn, B. C., Davidsson, B., Davies, J. K., de León, J., de Mooij, E., de Val-Borro, M., Delacruz, M., DiSanti, M. A., Drew, J. E., Duffard, R., Edberg, N. J. T., Faggi, S., Feaga, L., Fitzsimmons, A., Fujiwara, H., Gibb, E. L., Gillon, M., Green, S. F., Guijarro, A., Guilbert-Lepoutre, A., Gutiérrez, P. J., Hadamcik, E., Hainaut, O., Haque, S., Hedrosa, R., Hines, D., Hopp, U., Hoyo, F., Hutsemékers, D., Hyland, M., Ivanova, O., Jehin, E., Jones, G. H., Keane, J. V., Kelley, M. S. P., Kiselev, N., Kleyna, J., Kluge, M., Knight, M. M., Kokotanekova, R., Koschny, D., Kramer, E. A., López-Moreno, J. J., Lacerda, P., Lara, L. M., Lasue, J., Lehto, H. J., Levasseur-Regourd, A. C., Licandro, J., Lin, Z. Y., Lister, T., Lowry, S. C., Mainzer, A., Manfroid, J., Marchant, J., McKay, A. J., McNeill, A., Meech, K. J., Micheli, M., Mohammed, I., Monguió, M., Moreno, F., Muñoz, O., Mumma, M. J., Nikolov, P., Opitom, C., Ortiz, J. L., Paganini, L., Pajuelo, M., Pozuelos, F. J., Protopapa, S., Pursimo, T., Rajkumar, B., Ramanjooloo, Y., Ramos, E., Ries, C., Riffeser, A., Rosenbush, V., Rousselot, P., Ryan, E. L., Santos-Sanz, P., Schleicher, D. G., Schmidt, M., Schulz, R., Sen, A. K., Somero, A., Sota, A., Stinson, A., Sunshine, J. M., Thompson, A., Tozzi, G. P., Tubiana, C., Villanueva, G. L., Wang, X., Wooden, D. H., Yagi, M., Yang, B., Zaprudin, B., Zegmott, T. J., Snodgrass, C., A'Hearn, M. F., Aceituno, F., Afanasiev, V., Bagnulo, S., Bauer, J., Bergond, G., Besse, S., Biver, N., Bodewits, D., Boehnhardt, H., Bonev, B. P., Borisov, G., Carry, B., Casanova, V., Cochran, A., Conn, B. C., Davidsson, B., Davies, J. K., de León, J., de Mooij, E., de Val-Borro, M., Delacruz, M., DiSanti, M. A., Drew, J. E., Duffard, R., Edberg, N. J. T., Faggi, S., Feaga, L., Fitzsimmons, A., Fujiwara, H., Gibb, E. L., Gillon, M., Green, S. F., Guijarro, A., Guilbert-Lepoutre, A., Gutiérrez, P. J., Hadamcik, E., Hainaut, O., Haque, S., Hedrosa, R., Hines, D., Hopp, U., Hoyo, F., Hutsemékers, D., Hyland, M., Ivanova, O., Jehin, E., Jones, G. H., Keane, J. V., Kelley, M. S. P., Kiselev, N., Kleyna, J., Kluge, M., Knight, M. M., Kokotanekova, R., Koschny, D., Kramer, E. A., López-Moreno, J. J., Lacerda, P., Lara, L. M., Lasue, J., Lehto, H. J., Levasseur-Regourd, A. C., Licandro, J., Lin, Z. Y., Lister, T., Lowry, S. C., Mainzer, A., Manfroid, J., Marchant, J., McKay, A. J., McNeill, A., Meech, K. J., Micheli, M., Mohammed, I., Monguió, M., Moreno, F., Muñoz, O., Mumma, M. J., Nikolov, P., Opitom, C., Ortiz, J. L., Paganini, L., Pajuelo, M., Pozuelos, F. J., Protopapa, S., Pursimo, T., Rajkumar, B., Ramanjooloo, Y., Ramos, E., Ries, C., Riffeser, A., Rosenbush, V., Rousselot, P., Ryan, E. L., Santos-Sanz, P., Schleicher, D. G., Schmidt, M., Schulz, R., Sen, A. K., Somero, A., Sota, A., Stinson, A., Sunshine, J. M., Thompson, A., Tozzi, G. P., Tubiana, C., Villanueva, G. L., Wang, X., Wooden, D. H., Yagi, M., Yang, B., Zaprudin, B., and Zegmott, T. J.

Abstract

We present a summary of the campaign of remote observations that supported the European Space Agency's Rosetta mission. Telescopes across the globe (and in space) followed comet 67P/Churyumov–Gerasimenko from before Rosetta's arrival until nearly the end of the mission in September 2016. These provided essential data for mission planning, large-scale context information for the coma and tails beyond the spacecraft and a way to directly compare 67P with other comets. The observations revealed 67P to be a relatively ‘well-behaved’ comet, typical of Jupiter family comets and with activity patterns that repeat from orbit to orbit. Comparison between this large collection of telescopic observations and the in situ results from Rosetta will allow us to better understand comet coma chemistry and structure. This work is just beginning as the mission ends—in this paper, we present a summary of the ground-based observations and early results, and point to many questions that will be addressed in future studies.

12. The 67P/Churyumov–Gerasimenko observation campaign in support of the Rosetta mission

Author

Snodgrass, C., A'Hearn, M. F., Aceituno, F., Afanasiev, V., Bagnulo, S., Bauer, J., Bergond, G., Besse, S., Biver, N., Bodewits, D., Boehnhardt, H., Bonev, B. P., Borisov, G., Carry, B., Casanova, V., Cochran, A., Conn, B. C., Davidsson, B., Davies, J. K., de León, J., de Mooij, E., de Val-Borro, M., Delacruz, M., DiSanti, M. A., Drew, J. E., Duffard, R., Edberg, N. J. T., Faggi, S., Feaga, L., Fitzsimmons, A., Fujiwara, H., Gibb, E. L., Gillon, M., Green, S. F., Guijarro, A., Guilbert-Lepoutre, A., Gutiérrez, P. J., Hadamcik, E., Hainaut, O., Haque, S., Hedrosa, R., Hines, D., Hopp, U., Hoyo, F., Hutsemékers, D., Hyland, M., Ivanova, O., Jehin, E., Jones, G. H., Keane, J. V., Kelley, M. S. P., Kiselev, N., Kleyna, J., Kluge, M., Knight, M. M., Kokotanekova, R., Koschny, D., Kramer, E. A., López-Moreno, J. J., Lacerda, P., Lara, L. M., Lasue, J., Lehto, H. J., Levasseur-Regourd, A. C., Licandro, J., Lin, Z. Y., Lister, T., Lowry, S. C., Mainzer, A., Manfroid, J., Marchant, J., McKay, A. J., McNeill, A., Meech, K. J., Micheli, M., Mohammed, I., Monguió, M., Moreno, F., Muñoz, O., Mumma, M. J., Nikolov, P., Opitom, C., Ortiz, J. L., Paganini, L., Pajuelo, M., Pozuelos, F. J., Protopapa, S., Pursimo, T., Rajkumar, B., Ramanjooloo, Y., Ramos, E., Ries, C., Riffeser, A., Rosenbush, V., Rousselot, P., Ryan, E. L., Santos-Sanz, P., Schleicher, D. G., Schmidt, M., Schulz, R., Sen, A. K., Somero, A., Sota, A., Stinson, A., Sunshine, J. M., Thompson, A., Tozzi, G. P., Tubiana, C., Villanueva, G. L., Wang, X., Wooden, D. H., Yagi, M., Yang, B., Zaprudin, B., Zegmott, T. J., Snodgrass, C., A'Hearn, M. F., Aceituno, F., Afanasiev, V., Bagnulo, S., Bauer, J., Bergond, G., Besse, S., Biver, N., Bodewits, D., Boehnhardt, H., Bonev, B. P., Borisov, G., Carry, B., Casanova, V., Cochran, A., Conn, B. C., Davidsson, B., Davies, J. K., de León, J., de Mooij, E., de Val-Borro, M., Delacruz, M., DiSanti, M. A., Drew, J. E., Duffard, R., Edberg, N. J. T., Faggi, S., Feaga, L., Fitzsimmons, A., Fujiwara, H., Gibb, E. L., Gillon, M., Green, S. F., Guijarro, A., Guilbert-Lepoutre, A., Gutiérrez, P. J., Hadamcik, E., Hainaut, O., Haque, S., Hedrosa, R., Hines, D., Hopp, U., Hoyo, F., Hutsemékers, D., Hyland, M., Ivanova, O., Jehin, E., Jones, G. H., Keane, J. V., Kelley, M. S. P., Kiselev, N., Kleyna, J., Kluge, M., Knight, M. M., Kokotanekova, R., Koschny, D., Kramer, E. A., López-Moreno, J. J., Lacerda, P., Lara, L. M., Lasue, J., Lehto, H. J., Levasseur-Regourd, A. C., Licandro, J., Lin, Z. Y., Lister, T., Lowry, S. C., Mainzer, A., Manfroid, J., Marchant, J., McKay, A. J., McNeill, A., Meech, K. J., Micheli, M., Mohammed, I., Monguió, M., Moreno, F., Muñoz, O., Mumma, M. J., Nikolov, P., Opitom, C., Ortiz, J. L., Paganini, L., Pajuelo, M., Pozuelos, F. J., Protopapa, S., Pursimo, T., Rajkumar, B., Ramanjooloo, Y., Ramos, E., Ries, C., Riffeser, A., Rosenbush, V., Rousselot, P., Ryan, E. L., Santos-Sanz, P., Schleicher, D. G., Schmidt, M., Schulz, R., Sen, A. K., Somero, A., Sota, A., Stinson, A., Sunshine, J. M., Thompson, A., Tozzi, G. P., Tubiana, C., Villanueva, G. L., Wang, X., Wooden, D. H., Yagi, M., Yang, B., Zaprudin, B., and Zegmott, T. J.

Abstract

We present a summary of the campaign of remote observations that supported the European Space Agency's Rosetta mission. Telescopes across the globe (and in space) followed comet 67P/Churyumov–Gerasimenko from before Rosetta's arrival until nearly the end of the mission in September 2016. These provided essential data for mission planning, large-scale context information for the coma and tails beyond the spacecraft and a way to directly compare 67P with other comets. The observations revealed 67P to be a relatively ‘well-behaved’ comet, typical of Jupiter family comets and with activity patterns that repeat from orbit to orbit. Comparison between this large collection of telescopic observations and the in situ results from Rosetta will allow us to better understand comet coma chemistry and structure. This work is just beginning as the mission ends—in this paper, we present a summary of the ground-based observations and early results, and point to many questions that will be addressed in future studies.

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