1. C/2014 UN271(Bernardinelli-Bernstein): The Nearly Spherical Cow of Comets
- Author
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David J. James, R. Cawthon, H. T. Diehl, Maria E. S. Pereira, Josh Frieman, Ramon Miquel, Y.-H. Zhang, David J. Brooks, D. L. Hollowood, S. Serrano, Enrique Gaztanaga, Benjamin T. Montet, Marcelle Soares-Santos, Robert Weryk, A. Carnero Rosell, G. Tarle, R. L. C. Ogando, E. Bertin, Juan Garcia-Bellido, I. Ferrero, M. Costanzi, J. Carretero, Chun-Hao To, E. J. Sanchez, A. Roodman, Richard J. Wainscoat, A. A. Plazas Malagón, J. Gschwend, Adriano Pieres, M. A. G. Maia, M. Rodriguez-Monroy, Salcedo Romero de Ávila, A. R. Walker, M. Carrasco Kind, B. Flaugher, Gary Bernstein, Samuel Hinton, Robert Morgan, S. Everett, M. N. K. Smith, F. Andrade-Oliveira, G. Gutierrez, J. De Vicente, A. K. Romer, Pedro H. Bernardinelli, K. Kuehn, Michael Troxel, E. Suchyta, Jennifer L. Marshall, J. Annis, Michael Schubnell, O. Lahav, D. L. Burke, S. Allam, Robert A. Gruendl, C. J. Conselice, Michel Aguena, I. Sevilla-Noarbe, N. Kuropatkin, T. N. Varga, L. N. da Costa, Felipe Menanteau, K. Honscheid, M. E. C. Swanson, F. Paz-Chinchón, Daniel Gruen, D. W. Gerdes, National Science Foundation (US), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Instituto Nacional de Ciência e Tecnologia (Brasil), UAM. Departamento de Física Teórica, University of Pennsylvania, University of New South Wales, University of Western Ontario, University of Hawaii, Laboratório Interinstitucional de E-Astronomia - LIneA, Fermi National Accelerator Laboratory, Universidade Estadual Paulista (UNESP), Universidad Autonoma de Madrid, Institut d'Astrophysique de Paris, University College London, Stanford University, SLAC National Accelerator Laboratory, National Center for Supercomputing Applications, University of Illinois at Urbana-Champaign, Barcelona Institute of Science and Technology, University of Wisconsin-Madison, University of Manchester, School of Physics and Astronomy, University of Trieste, INAF-Osservatorio Astronomico di Trieste, Institute for Fundamental Physics of the Universe, Observatório Nacional, University of Michigan, Universitat Hamburg, Medioambientales y Tecnológicas (CIEMAT), Santa Cruz Institute for Particle Physics, University of Oslo, University of Chicago, Institut d'Estudis Espacials de Catalunya (IEEC), Institute of Space Sciences (ICE CSIC), Ludwig-Maximilians-Universitat, University of Queensland, Ohio State University, Center for Astrophysics | Harvard and Smithsonian, Macquarie University, Lowell Observatory, Texas A and M University, Institució Catalana de Recerca i Estudis Avancats, University of Cambridge, Peyton Hall, University of Sussex, University of Southampton, Oak Ridge National Laboratory, 382 Via Pueblo Mall, Duke University, Max Planck Institute for Extraterrestrial Physics, Ludwig-Maximilians Universitat München, NSF's National Optical-Infrared Astronomy Research Laboratory, Bernardinelli, P. H., Bernstein, G. M., Montet, B. T., Weryk, R., Wainscoat, R., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Avila, S., Bertin, E., Brooks, D., Burke, D. L., Carnero Rosell, A., Kind, M. C., Carretero, J., Cawthon, R., Conselice, C., Costanzi, M., Da Costa, L. N., Pereira, M. E. S., De Vicente, J., Diehl, H. T., Everett, S., Ferrero, I., Flaugher, B., Frieman, J., Garcia-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Morgan, R., Ogando, R. L. C., Paz-Chinchon, F., Pieres, A., Malagon, A. A. P., Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sanchez, E., Schubnell, M., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Suchyta, E., Swanson, M. E. C., Tarle, G., To, C., Troxel, M. A., Varga, T. N., Walker, A. R., and Zhang, Y.
- Subjects
Rotation period ,Absolute magnitude ,Brightness ,Long period comets ,Small Solar System bodies ,Comet nuclei ,Comet dynamics ,Comet origins ,933 ,1469 ,2160 ,2213 ,2203 ,Astrophysics - Earth and Planetary Astrophysics ,Comet ,FOS: Physical sciences ,Astrophysics ,01 natural sciences ,Comet origin ,Long Period Comets (933) ,Geometric albedo ,0103 physical sciences ,Comet Nuclei (2160) ,Surface brightness ,010303 astronomy & astrophysics ,Earth and Planetary Astrophysics (astro-ph.EP) ,Physics ,Long period comet ,Small Solar System Bodies (1469) ,05 social sciences ,Uranus ,050301 education ,Física ,Astronomy and Astrophysics ,Comet dynamic ,Radiative equilibrium ,Small Solar System bodie ,Comet Dynamics (2213) ,Comet Origins (2203) ,Space and Planetary Science ,0503 education - Abstract
Comet C/2014 UN271 (Bernardinelli-Bernstein), incoming from the Oort cloud, is remarkable in having the brightest (and presumably largest) nucleus of any well-measured comet and having been discovered at the heliocentric distance r h ≈ 29 au, farther than any Oort cloud comet. In this work, we describe the discovery process and observations and the properties that can be inferred from images recorded until the first reports of activity in 2021 June. The orbit has i = 95°, with a perihelion of 10.97 au to be reached in 2031 and a previous aphelion at 40,400 ± 260 au. Backward integration of the orbit under a standard Galactic tidal model and known stellar encounters suggests a perihelion of q ≈ 18 au on its previous perihelion passage 3.5 Myr ago; hence, the current data could be the first ever obtained of a comet that has not been inside Uranus's orbit in 4 Gyr. The photometric data show an unresolved nucleus with absolute magnitude H r = 8.0, colors that are typical of comet nuclei or Damocloids, and no secular trend as it traversed the range 34-23 au. For the r-band geometric albedo p r , this implies a diameter of km. There is strong evidence of brightness fluctuations at the ±0.2 mag level, but no rotation period can be discerned. A coma, nominally consistent with a "stationary"1/ρ surface brightness distribution, grew in scattering cross section at an exponential rate from A f ρ ≈ 1 to ≈150 m as the comet approached from 28 to 20 au. The activity rate is consistent with a very simple model of sublimation of a surface species in radiative equilibrium with the Sun. The inferred enthalpy of sublimation matches those of CO2 and NH3. More volatile species, such as N2, CH4, and CO, must be far less abundant on the sublimating surfaces., The DES data management system is supported by the National Science Foundation under grant Nos. AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007–2013), including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).
- Published
- 2021