KIC 7177553: A QUADRUPLE SYSTEM OF TWO CLOSE BINARIES
KIC 7177553 was observed by the Kepler satellite to be an eclipsing eccentric binary star system with an 18-day orbital period. Recently, an eclipse timing study of the Kepler binaries has revealed eclipse timing variations (ETVs) in this object with an amplitude of ~100 s and an outer period of 529...
| Main Authors: | , , , , , , |
|---|---|
| Other Authors: | |
| Format: | Article |
| Language: | en_US |
| Published: |
IOP Publishing
2016
|
| Online Access: | http://hdl.handle.net/1721.1/102651 https://orcid.org/0000-0003-3182-5569 |
| _version_ | 1811085250257747968 |
|---|---|
| author | Lehmann, H. Borkovits, T. Ngo, H. Mawet, D. Csizmadia, Sz. Rappaport, Saul A. Forgacs-Dajka, E. |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics Lehmann, H. Borkovits, T. Ngo, H. Mawet, D. Csizmadia, Sz. Rappaport, Saul A. Forgacs-Dajka, E. |
| author_sort | Lehmann, H. |
| collection | MIT |
| description | KIC 7177553 was observed by the Kepler satellite to be an eclipsing eccentric binary star system with an 18-day orbital period. Recently, an eclipse timing study of the Kepler binaries has revealed eclipse timing variations (ETVs) in this object with an amplitude of ~100 s and an outer period of 529 days. The implied mass of the third body is that of a super-Jupiter, but below the mass of a brown dwarf. We therefore embarked on a radial velocity (RV) study of this binary to determine its system configuration and to check the hypothesis that it hosts a giant planet. From the RV measurements, it became immediately obvious that the same Kepler target contains another eccentric binary, this one with a 16.5-day orbital period. Direct imaging using adaptive optics reveals that the two binaries are separated by 0[" over .]4 (~167 AU) and have nearly the same magnitude (to within 2%). The close angular proximity of the two binaries and very similar γ velocities strongly suggest that KIC 7177553 is one of the rare SB4 systems consisting of two eccentric binaries where at least one system is eclipsing. Both systems consist of slowly rotating, nonevolved, solar-like stars of comparable masses. From the orbital separation and the small difference in γ velocity, we infer that the period of the outer orbit most likely lies in the range of 1000–3000 yr. New images taken over the next few years, as well as the high-precision astrometry of the Gaia satellite mission, will allow us to set much narrower constraints on the system geometry. Finally, we note that the observed ETVs in the Kepler data cannot be produced by the second binary. Further spectroscopic observations on a longer timescale will be required to prove the existence of the massive planet. |
| first_indexed | 2024-09-23T13:05:58Z |
| format | Article |
| id | mit-1721.1/102651 |
| institution | Massachusetts Institute of Technology |
| language | en_US |
| last_indexed | 2024-09-23T13:05:58Z |
| publishDate | 2016 |
| publisher | IOP Publishing |
| record_format | dspace |
| spelling | mit-1721.1/1026512022-10-01T13:01:43Z KIC 7177553: A QUADRUPLE SYSTEM OF TWO CLOSE BINARIES Lehmann, H. Borkovits, T. Ngo, H. Mawet, D. Csizmadia, Sz. Rappaport, Saul A. Forgacs-Dajka, E. Massachusetts Institute of Technology. Department of Physics Rappaport, Saul A. KIC 7177553 was observed by the Kepler satellite to be an eclipsing eccentric binary star system with an 18-day orbital period. Recently, an eclipse timing study of the Kepler binaries has revealed eclipse timing variations (ETVs) in this object with an amplitude of ~100 s and an outer period of 529 days. The implied mass of the third body is that of a super-Jupiter, but below the mass of a brown dwarf. We therefore embarked on a radial velocity (RV) study of this binary to determine its system configuration and to check the hypothesis that it hosts a giant planet. From the RV measurements, it became immediately obvious that the same Kepler target contains another eccentric binary, this one with a 16.5-day orbital period. Direct imaging using adaptive optics reveals that the two binaries are separated by 0[" over .]4 (~167 AU) and have nearly the same magnitude (to within 2%). The close angular proximity of the two binaries and very similar γ velocities strongly suggest that KIC 7177553 is one of the rare SB4 systems consisting of two eccentric binaries where at least one system is eclipsing. Both systems consist of slowly rotating, nonevolved, solar-like stars of comparable masses. From the orbital separation and the small difference in γ velocity, we infer that the period of the outer orbit most likely lies in the range of 1000–3000 yr. New images taken over the next few years, as well as the high-precision astrometry of the Gaia satellite mission, will allow us to set much narrower constraints on the system geometry. Finally, we note that the observed ETVs in the Kepler data cannot be produced by the second binary. Further spectroscopic observations on a longer timescale will be required to prove the existence of the massive planet. 2016-05-24T13:13:31Z 2016-05-24T13:13:31Z 2016-02 2015-11 Article http://purl.org/eprint/type/JournalArticle 1538-4357 0004-637X http://hdl.handle.net/1721.1/102651 Lehmann, H., T. Borkovits, S. A. Rappaport, H. Ngo, D. Mawet, Sz. Csizmadia, and E. Forgacs-Dajka. “KIC 7177553: A QUADRUPLE SYSTEM OF TWO CLOSE BINARIES.” The Astrophysical Journal 819, no. 1 (February 25, 2016): 33. © 2016 The American Astronomical Society https://orcid.org/0000-0003-3182-5569 en_US http://dx.doi.org/10.3847/0004-637x/819/1/33 The Astrophysical Journal Article is made available in accordance with the publisher's policy and may be subject to US copyright law. Please refer to the publisher's site for terms of use. application/pdf IOP Publishing IOP Publishing |
| spellingShingle | Lehmann, H. Borkovits, T. Ngo, H. Mawet, D. Csizmadia, Sz. Rappaport, Saul A. Forgacs-Dajka, E. KIC 7177553: A QUADRUPLE SYSTEM OF TWO CLOSE BINARIES |
| title | KIC 7177553: A QUADRUPLE SYSTEM OF TWO CLOSE BINARIES |
| title_full | KIC 7177553: A QUADRUPLE SYSTEM OF TWO CLOSE BINARIES |
| title_fullStr | KIC 7177553: A QUADRUPLE SYSTEM OF TWO CLOSE BINARIES |
| title_full_unstemmed | KIC 7177553: A QUADRUPLE SYSTEM OF TWO CLOSE BINARIES |
| title_short | KIC 7177553: A QUADRUPLE SYSTEM OF TWO CLOSE BINARIES |
| title_sort | kic 7177553 a quadruple system of two close binaries |
| url | http://hdl.handle.net/1721.1/102651 https://orcid.org/0000-0003-3182-5569 |
| work_keys_str_mv | AT lehmannh kic7177553aquadruplesystemoftwoclosebinaries AT borkovitst kic7177553aquadruplesystemoftwoclosebinaries AT ngoh kic7177553aquadruplesystemoftwoclosebinaries AT mawetd kic7177553aquadruplesystemoftwoclosebinaries AT csizmadiasz kic7177553aquadruplesystemoftwoclosebinaries AT rappaportsaula kic7177553aquadruplesystemoftwoclosebinaries AT forgacsdajkae kic7177553aquadruplesystemoftwoclosebinaries |