Synchronous Rotation in the (136199) Eris-Dysnomia System

Gary M. Bernstein; Bryan J. Holler; Rosario Navarro-Escamilla; Pedro H. Bernardinelli; T. M.C. Abbott; M. Aguena; S. Allam; O. Alves; F. Andrade-Oliveira; J. Annis; D. Bacon; D. Brooks; D. L. Burke; A. Carnero Rosell; J. Carretero; L. N. da Costa; M. E.S. Pereira; J. De Vicente; S. Desai; P. Doel; A. Drlica-Wagner; S. Everett; I. Ferrero; J. Frieman; J. García-Bellido; D. W. Gerdes; D. Gruen; G. Gutierrez; K. Herner; S. R. Hinton; D. L. Hollowood; K. Honscheid; D. J. James; K. Kuehn; N. Kuropatkin; J. L. Marshall; J. Mena-Fernández; R. Miquel; R. L.C. Ogando; A. Pieres; A. A.Plazas Malagón; M. Raveri; K. Reil; E. Sanchez; I. Sevilla-Noarbe; M. Smith; M. Soares-Santos; E. Suchyta; M. E.C. Swanson; P. Wiseman

doi:10.3847/PSJ/acdd5f

Synchronous Rotation in the (136199) Eris-Dysnomia System

Gary M. Bernstein, Bryan J. Holler, Rosario Navarro-Escamilla, Pedro H. Bernardinelli, T. M.C. Abbott, M. Aguena, S. Allam, O. Alves, F. Andrade-Oliveira, J. Annis, D. Bacon, D. Brooks, D. L. Burke, A. Carnero Rosell, J. Carretero, L. N. da Costa, M. E.S. Pereira, J. De Vicente, S. Desai, P. DoelA. Drlica-Wagner, S. Everett, I. Ferrero, J. Frieman, J. García-Bellido, D. W. Gerdes, D. Gruen, G. Gutierrez, K. Herner, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, N. Kuropatkin, J. L. Marshall, J. Mena-Fernández, R. Miquel, R. L.C. Ogando, A. Pieres, A. A.Plazas Malagón, M. Raveri, K. Reil, E. Sanchez, I. Sevilla-Noarbe, M. Smith, M. Soares-Santos, E. Suchyta, M. E.C. Swanson, P. Wiseman

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Abstract

We combine photometry of Eris from a 6 month campaign on the Palomar 60 inch telescope in 2015, a 1 month Hubble Space Telescope WFC3 campaign in 2018, and Dark Energy Survey data spanning 2013-2018 to determine a light curve of definitive period 15.771 ± 0.008 days (1σ formal uncertainties), with nearly sinusoidal shape and peak-to-peak flux variation of 3%. This is consistent at part-per-thousand precision with the P = 15.785 90 ± 0.00005 day sidereal period of Dysnomia’s orbit around Eris, strengthening the recent detection of synchronous rotation of Eris by Szakáts et al. with independent data. Photometry from Gaia are consistent with the same light curve. We detect a slope of 0.05 ± 0.01 mag per degree of Eris’s brightness with respect to illumination phase averaged across g, V, and r bands, intermediate between Pluto’s and Charon’s values. Variations of 0.3 mag are detected in Dysnomia’s brightness, plausibly consistent with a double-peaked light curve at the synchronous period. The synchronous rotation of Eris is consistent with simple tidal models initiated with a giant-impact origin of the binary, but is difficult to reconcile with gravitational capture of Dysnomia by Eris. The high albedo contrast between Eris and Dysnomia remains unexplained in the giant-impact scenario.

Original language	English
Article number	115
Journal	Planetary Science Journal
Volume	4
Issue number	6
DOIs	https://doi.org/10.3847/PSJ/acdd5f
State	Published - Jun 1 2023

Funding

Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Funda\u00E7\u00E3o Carlos Chagas Filho de Amparo \u00E0 Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cient\u00EDfico e Tecnol\u00F3gico and the Minist\u00E9rio da Ci\u00EAncia, Tecnologia e Inova\u00E7\u00E3o, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. 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\u2019s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ci\u00EAncia e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics, and has gone through internal reviews by the DES collaboration. We thank the anonymous referees for their assistance in improving the paper. The authors would also like to thank Richard Walters, Associate Research Engineer at the Palomar Observatory, for his help and patience in scheduling the imaging observations at the 60 inch telescope. The authors appreciate the work of Crystal Mannfolk, Linda Dressel, and Kailash Sahu of STScI in helping to optimize the HST observations prior to execution. Darin Ragozzine, Anne Verbiscer, Leslie Young, Michael Mommert, James Bauer, and Susan Benecchi provided helpful advice throughout this investigation. This work is based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. Support for this work was provided by NASA through grant No. GO-15171.001 from STScI. Work by G.M.B., P.H.B., and R.N.E. was supported by National Science Foundation grants AST-2009210 and AST-2205808. P.H.B. acknowledges support from the DIRAC Institute in the Department of Astronomy at the University of Washington. The DIRAC Institute is supported through generous gifts from the Charles and Lisa Simonyi Fund for Arts and Sciences, and the Washington Research Foundation.

Funders	Funder number
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
Brazilian Instituto Nacional de Ciência e Tecnologia
High Energy Physics
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Entomological Society of America
Ohio State University
University of Chicago
Engineering Research Centers
Generalitat de Catalunya
Higher Education Funding Council for England
Financiadora de Estudos e Projetos
Space Telescope Science Institute
Ministry of Education and Science of Ukraine
Deutsche Forschungsgemeinschaft
European Commission
Instituto Nacional de Ciência e Tecnologia para Excitotoxicidade e Neuroproteção
U.S. Department of Energy
Institute for Data Intensive Research in Astrophysics and Cosmology, University of Washington
Science and Technology Facilities Council of the United Kingdom
Ministério da Ciência, Tecnologia e Inovação
Office of Science
National Centre for Supercomputing Applications
University of Washington
European Research Council
European Regional Development Fund
Washington Research Foundation
Charles and Lisa Simonyi Fund for Arts and Sciences
Collaborating Institutions in the Dark Energy Survey
National Science Foundation	AST-2205808, AST-1138766, AST-2009210, AST-1536171
Fermi Research Alliance, LLC	DE-AC02-07CH11359
Ministerio de Ciencia e Innovación	SEV-2016-0588, SEV-2016-0597, MDM-2015-0509, PGC2018-094773, PGC2018-102021, ESP2017-89838
Conselho Nacional de Desenvolvimento Científico e Tecnológico	465376/2014-2
Seventh Framework Programme	2009210, AST-1138766, 240672, 306478, 291329
National Aeronautics and Space Administration	NAS 5-26555, GO-15171.001

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Bernstein, G. M., Holler, B. J., Navarro-Escamilla, R., Bernardinelli, P. H., Abbott, T. M. C., Aguena, M., Allam, S., Alves, O., Andrade-Oliveira, F., Annis, J., Bacon, D., Brooks, D., Burke, D. L., Carnero Rosell, A., Carretero, J., da Costa, L. N., Pereira, M. E. S., De Vicente, J., Desai, S., ... Wiseman, P. (2023). Synchronous Rotation in the (136199) Eris-Dysnomia System. Planetary Science Journal, 4(6), Article 115. https://doi.org/10.3847/PSJ/acdd5f

@article{49098038b871406dba2ac9f4a7ff5e3d,

title = "Synchronous Rotation in the (136199) Eris-Dysnomia System",

abstract = "We combine photometry of Eris from a 6 month campaign on the Palomar 60 inch telescope in 2015, a 1 month Hubble Space Telescope WFC3 campaign in 2018, and Dark Energy Survey data spanning 2013-2018 to determine a light curve of definitive period 15.771 ± 0.008 days (1σ formal uncertainties), with nearly sinusoidal shape and peak-to-peak flux variation of 3%. This is consistent at part-per-thousand precision with the P = 15.785 90 ± 0.00005 day sidereal period of Dysnomia{\textquoteright}s orbit around Eris, strengthening the recent detection of synchronous rotation of Eris by Szak{\'a}ts et al. with independent data. Photometry from Gaia are consistent with the same light curve. We detect a slope of 0.05 ± 0.01 mag per degree of Eris{\textquoteright}s brightness with respect to illumination phase averaged across g, V, and r bands, intermediate between Pluto{\textquoteright}s and Charon{\textquoteright}s values. Variations of 0.3 mag are detected in Dysnomia{\textquoteright}s brightness, plausibly consistent with a double-peaked light curve at the synchronous period. The synchronous rotation of Eris is consistent with simple tidal models initiated with a giant-impact origin of the binary, but is difficult to reconcile with gravitational capture of Dysnomia by Eris. The high albedo contrast between Eris and Dysnomia remains unexplained in the giant-impact scenario.",

author = "Bernstein, {Gary M.} and Holler, {Bryan J.} and Rosario Navarro-Escamilla and Bernardinelli, {Pedro H.} and Abbott, {T. M.C.} and M. Aguena and S. Allam and O. Alves and F. Andrade-Oliveira and J. Annis and D. Bacon and D. Brooks and Burke, {D. L.} and {Carnero Rosell}, A. and J. Carretero and {da Costa}, {L. N.} and Pereira, {M. E.S.} and {De Vicente}, J. and S. Desai and P. Doel and A. Drlica-Wagner and S. Everett and I. Ferrero and J. Frieman and J. Garc{\'i}a-Bellido and Gerdes, {D. W.} and D. Gruen and G. Gutierrez and K. Herner and Hinton, {S. R.} and Hollowood, {D. L.} and K. Honscheid and James, {D. J.} and K. Kuehn and N. Kuropatkin and Marshall, {J. L.} and J. Mena-Fern{\'a}ndez and R. Miquel and Ogando, {R. L.C.} and A. Pieres and Malag{\'o}n, {A. A.Plazas} and M. Raveri and K. Reil and E. Sanchez and I. Sevilla-Noarbe and M. Smith and M. Soares-Santos and E. Suchyta and Swanson, {M. E.C.} and P. Wiseman",

note = "Publisher Copyright: {\textcopyright} 2023. The Author(s). Published by the American Astronomical Society.",

year = "2023",

month = jun,

day = "1",

doi = "10.3847/PSJ/acdd5f",

language = "English",

volume = "4",

journal = "Planetary Science Journal",

issn = "2632-3338",

publisher = "IOP Publishing",

number = "6",

}

Bernstein, GM, Holler, BJ, Navarro-Escamilla, R, Bernardinelli, PH, Abbott, TMC, Aguena, M, Allam, S, Alves, O, Andrade-Oliveira, F, Annis, J, Bacon, D, Brooks, D, Burke, DL, Carnero Rosell, A, Carretero, J, da Costa, LN, Pereira, MES, De Vicente, J, Desai, S, Doel, P, Drlica-Wagner, A, Everett, S, Ferrero, I, Frieman, J, García-Bellido, J, Gerdes, DW, Gruen, D, Gutierrez, G, Herner, K, Hinton, SR, Hollowood, DL, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Marshall, JL, Mena-Fernández, J, Miquel, R, Ogando, RLC, Pieres, A, Malagón, AAP, Raveri, M, Reil, K, Sanchez, E, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Suchyta, E, Swanson, MEC & Wiseman, P 2023, 'Synchronous Rotation in the (136199) Eris-Dysnomia System', Planetary Science Journal, vol. 4, no. 6, 115. https://doi.org/10.3847/PSJ/acdd5f

TY - JOUR

T1 - Synchronous Rotation in the (136199) Eris-Dysnomia System

AU - Bernstein, Gary M.

AU - Holler, Bryan J.

AU - Navarro-Escamilla, Rosario

AU - Bernardinelli, Pedro H.

AU - Abbott, T. M.C.

AU - Aguena, M.

AU - Allam, S.

AU - Alves, O.

AU - Andrade-Oliveira, F.

AU - Annis, J.

AU - Bacon, D.

AU - Brooks, D.

AU - Burke, D. L.

AU - Carnero Rosell, A.

AU - Carretero, J.

AU - da Costa, L. N.

AU - Pereira, M. E.S.

AU - De Vicente, J.

AU - Desai, S.

AU - Doel, P.

AU - Drlica-Wagner, A.

AU - Everett, S.

AU - Ferrero, I.

AU - Frieman, J.

AU - García-Bellido, J.

AU - Gerdes, D. W.

AU - Gruen, D.

AU - Gutierrez, G.

AU - Herner, K.

AU - Hinton, S. R.

AU - Hollowood, D. L.

AU - Honscheid, K.

AU - James, D. J.

AU - Kuehn, K.

AU - Kuropatkin, N.

AU - Marshall, J. L.

AU - Mena-Fernández, J.

AU - Miquel, R.

AU - Ogando, R. L.C.

AU - Pieres, A.

AU - Malagón, A. A.Plazas

AU - Raveri, M.

AU - Reil, K.

AU - Sanchez, E.

AU - Sevilla-Noarbe, I.

AU - Smith, M.

AU - Soares-Santos, M.

AU - Suchyta, E.

AU - Swanson, M. E.C.

AU - Wiseman, P.

PY - 2023/6/1

Y1 - 2023/6/1

N2 - We combine photometry of Eris from a 6 month campaign on the Palomar 60 inch telescope in 2015, a 1 month Hubble Space Telescope WFC3 campaign in 2018, and Dark Energy Survey data spanning 2013-2018 to determine a light curve of definitive period 15.771 ± 0.008 days (1σ formal uncertainties), with nearly sinusoidal shape and peak-to-peak flux variation of 3%. This is consistent at part-per-thousand precision with the P = 15.785 90 ± 0.00005 day sidereal period of Dysnomia’s orbit around Eris, strengthening the recent detection of synchronous rotation of Eris by Szakáts et al. with independent data. Photometry from Gaia are consistent with the same light curve. We detect a slope of 0.05 ± 0.01 mag per degree of Eris’s brightness with respect to illumination phase averaged across g, V, and r bands, intermediate between Pluto’s and Charon’s values. Variations of 0.3 mag are detected in Dysnomia’s brightness, plausibly consistent with a double-peaked light curve at the synchronous period. The synchronous rotation of Eris is consistent with simple tidal models initiated with a giant-impact origin of the binary, but is difficult to reconcile with gravitational capture of Dysnomia by Eris. The high albedo contrast between Eris and Dysnomia remains unexplained in the giant-impact scenario.

AB - We combine photometry of Eris from a 6 month campaign on the Palomar 60 inch telescope in 2015, a 1 month Hubble Space Telescope WFC3 campaign in 2018, and Dark Energy Survey data spanning 2013-2018 to determine a light curve of definitive period 15.771 ± 0.008 days (1σ formal uncertainties), with nearly sinusoidal shape and peak-to-peak flux variation of 3%. This is consistent at part-per-thousand precision with the P = 15.785 90 ± 0.00005 day sidereal period of Dysnomia’s orbit around Eris, strengthening the recent detection of synchronous rotation of Eris by Szakáts et al. with independent data. Photometry from Gaia are consistent with the same light curve. We detect a slope of 0.05 ± 0.01 mag per degree of Eris’s brightness with respect to illumination phase averaged across g, V, and r bands, intermediate between Pluto’s and Charon’s values. Variations of 0.3 mag are detected in Dysnomia’s brightness, plausibly consistent with a double-peaked light curve at the synchronous period. The synchronous rotation of Eris is consistent with simple tidal models initiated with a giant-impact origin of the binary, but is difficult to reconcile with gravitational capture of Dysnomia by Eris. The high albedo contrast between Eris and Dysnomia remains unexplained in the giant-impact scenario.

UR - http://www.scopus.com/inward/record.url?scp=85177221537&partnerID=8YFLogxK

U2 - 10.3847/PSJ/acdd5f

DO - 10.3847/PSJ/acdd5f

M3 - Article

AN - SCOPUS:85177221537

SN - 2632-3338

VL - 4

JO - Planetary Science Journal

JF - Planetary Science Journal

IS - 6

M1 - 115

ER -

Synchronous Rotation in the (136199) Eris-Dysnomia System

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