TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties
A precise transit ephemeris serves as the premise for follow-up exoplanet observations. We compare TESS Object of Interest (TOI) transit timings of 262 hot Jupiters with the archival ephemeris and find 31 of them having TOI timing offsets, among which WASP-161b shows the most significant offset of −...
| Main Authors: | , , , , , , , , , , |
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| Format: | Article |
| Language: | English |
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IOP Publishing
2023-01-01
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| Series: | The Astrophysical Journal Supplement Series |
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| Online Access: | https://doi.org/10.3847/1538-4365/aca65f |
| _version_ | 1797697223903936512 |
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| author | Su-Su Shan Fan Yang You-Jun Lu Xing Wei Wen-Wu Tian Hai-Yan Zhang Rui Guo Xiao-Hong Cui Ai-Yuan Yang Bo Zhang Ji-Feng Liu |
| author_facet | Su-Su Shan Fan Yang You-Jun Lu Xing Wei Wen-Wu Tian Hai-Yan Zhang Rui Guo Xiao-Hong Cui Ai-Yuan Yang Bo Zhang Ji-Feng Liu |
| author_sort | Su-Su Shan |
| collection | DOAJ |
| description | A precise transit ephemeris serves as the premise for follow-up exoplanet observations. We compare TESS Object of Interest (TOI) transit timings of 262 hot Jupiters with the archival ephemeris and find 31 of them having TOI timing offsets, among which WASP-161b shows the most significant offset of −203.7 ± 4.1 minutes. The median value of these offsets is 17.8 minutes, equivalent to 3.6 σ . We generate TESS timings in each sector for these 31 hot Jupiters, using a self-generated pipeline. The pipeline performs photometric measurements to TESS images and produces transit timings by fitting the light curves. We refine and update the previous ephemeris, based on these TESS timings (uncertainty ∼1 minute) and a long timing baseline (∼10 yr). Our refined ephemeris gives the transit timing at a median precision of 0.82 minutes until 2025 and 1.21 minutes until 2030. We regard the timing offsets to mainly originate from the underestimated ephemeris uncertainty. All the targets with timing offset larger than 10 σ present earlier timings than the prediction, which cannot be due to underestimated ephemeris uncertainty, apsidal precision, or Rømer effect as those effects should be unsigned. For some particular targets, timing offsets are likely due to tidal dissipation. Our sample leads to the detection of period-decaying candidates of WASP-161b and XO-3b reported previously. |
| first_indexed | 2024-03-12T03:37:13Z |
| format | Article |
| id | doaj.art-f33457f3dc584598895aa9d701f18f07 |
| institution | Directory Open Access Journal |
| issn | 0067-0049 |
| language | English |
| last_indexed | 2024-03-12T03:37:13Z |
| publishDate | 2023-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal Supplement Series |
| spelling | doaj.art-f33457f3dc584598895aa9d701f18f072023-09-03T13:08:46ZengIOP PublishingThe Astrophysical Journal Supplement Series0067-00492023-01-0126423710.3847/1538-4365/aca65fTESS Timings of 31 Hot Jupiters with Ephemeris UncertaintiesSu-Su Shan0https://orcid.org/0000-0002-5744-2016Fan Yang1https://orcid.org/0000-0002-6039-8212You-Jun Lu2https://orcid.org/0000-0002-1310-4664Xing Wei3https://orcid.org/0000-0002-8033-2974Wen-Wu Tian4https://orcid.org/0000-0002-9079-7556Hai-Yan Zhang5Rui Guo6Xiao-Hong Cui7https://orcid.org/0000-0002-6322-7582Ai-Yuan Yang8Bo Zhang9https://orcid.org/0000-0002-6434-7201Ji-Feng Liu10https://orcid.org/0000-0002-2874-2706National Astronomical Observatories, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China sailoryf@nao.cas.cn, sailoryf1222@gmail.com, jfliu@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China sailoryf@nao.cas.cn, sailoryf1222@gmail.com, jfliu@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of China; Department of Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China sailoryf@nao.cas.cn, sailoryf1222@gmail.com, jfliu@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaDepartment of Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China sailoryf@nao.cas.cn, sailoryf1222@gmail.com, jfliu@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China sailoryf@nao.cas.cn, sailoryf1222@gmail.com, jfliu@nao.cas.cnDepartment of Astronomy, School of Physics and Astronomy, Shanghai Jiao Tong University , 800 Dongchuan Road, Shanghai 200240, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China sailoryf@nao.cas.cn, sailoryf1222@gmail.com, jfliu@nao.cas.cnMax Planck Institute for Radio Astronomy , Auf dem Hügel 69, D-53121 Bonn, GermanyNational Astronomical Observatories, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China sailoryf@nao.cas.cn, sailoryf1222@gmail.com, jfliu@nao.cas.cn; Department of Astronomy, Beijing Normal University , Beijing 100875, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , 20A Datun Road, Chaoyang District, Beijing 100101, People’s Republic of China sailoryf@nao.cas.cn, sailoryf1222@gmail.com, jfliu@nao.cas.cn; School of Astronomy and Space Science, University of Chinese Academy of Sciences , Beijing 100049, People’s Republic of China; WHU-NAOC Joint Center for Astronomy, Wuhan University , Wuhan, People’s Republic of ChinaA precise transit ephemeris serves as the premise for follow-up exoplanet observations. We compare TESS Object of Interest (TOI) transit timings of 262 hot Jupiters with the archival ephemeris and find 31 of them having TOI timing offsets, among which WASP-161b shows the most significant offset of −203.7 ± 4.1 minutes. The median value of these offsets is 17.8 minutes, equivalent to 3.6 σ . We generate TESS timings in each sector for these 31 hot Jupiters, using a self-generated pipeline. The pipeline performs photometric measurements to TESS images and produces transit timings by fitting the light curves. We refine and update the previous ephemeris, based on these TESS timings (uncertainty ∼1 minute) and a long timing baseline (∼10 yr). Our refined ephemeris gives the transit timing at a median precision of 0.82 minutes until 2025 and 1.21 minutes until 2030. We regard the timing offsets to mainly originate from the underestimated ephemeris uncertainty. All the targets with timing offset larger than 10 σ present earlier timings than the prediction, which cannot be due to underestimated ephemeris uncertainty, apsidal precision, or Rømer effect as those effects should be unsigned. For some particular targets, timing offsets are likely due to tidal dissipation. Our sample leads to the detection of period-decaying candidates of WASP-161b and XO-3b reported previously.https://doi.org/10.3847/1538-4365/aca65fExoplanet astronomyExoplanet systemsTransit photometryTransit timing variation method |
| spellingShingle | Su-Su Shan Fan Yang You-Jun Lu Xing Wei Wen-Wu Tian Hai-Yan Zhang Rui Guo Xiao-Hong Cui Ai-Yuan Yang Bo Zhang Ji-Feng Liu TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties The Astrophysical Journal Supplement Series Exoplanet astronomy Exoplanet systems Transit photometry Transit timing variation method |
| title | TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties |
| title_full | TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties |
| title_fullStr | TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties |
| title_full_unstemmed | TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties |
| title_short | TESS Timings of 31 Hot Jupiters with Ephemeris Uncertainties |
| title_sort | tess timings of 31 hot jupiters with ephemeris uncertainties |
| topic | Exoplanet astronomy Exoplanet systems Transit photometry Transit timing variation method |
| url | https://doi.org/10.3847/1538-4365/aca65f |
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