Transiting Exoplanet Monitoring Project (TEMP). I. Refined System Parameters and Transit Timing Variations of HAT-P-29b
We report the photometry of six transits of the hot Jupiter HAT-P-29b obtained from 2013 October to 2015 January. We analyze the new light curves, in combination with the published photometric, Doppler velocimetric, and spectroscopic measurements, finding an updated orbital ephemeris for the HAT-P-2...
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| Veröffentlicht in: | The Astronomical journal 2018-10, Vol.156 (4), p.181 |
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| creator | Wang, Songhu Wang, Xian-Yu Wang, Yong-Hao Liu, Hui-Gen Hinse, Tobias C. Eastman, Jason Bayliss, Daniel Hori, Yasunori Hu, Shao-Ming Li, Kai Liu, Jinzhong Narita, Norio Peng, Xiyan Wittenmyer, R. A. Wu, Zhen-Yu Zhang, Hui Zhang, Xiaojia Zhao, Haibin Zhou, Ji-Lin Zhou, George Zhou, Xu Laughlin, Gregory |
| description | We report the photometry of six transits of the hot Jupiter HAT-P-29b obtained from 2013 October to 2015 January. We analyze the new light curves, in combination with the published photometric, Doppler velocimetric, and spectroscopic measurements, finding an updated orbital ephemeris for the HAT-P-29 system, and P = 5.723390(13) days. This result is 17.63 s (4.0 ) longer than the previously published value, amounting to errors exceeding 2.5 hr at the time of writing (on UTC 2018 June 1). The measured transit mid-times for HAT-P-29b show no compelling evidence of timing anomalies from a linear model, which rules out the presence of perturbers with masses greater than 0.6, 0.7, 0.5, and 0.4 M⊕ near the 1:2, 2:3, 3:2, and 2:1 resonances with HAT-P-29b, respectively. |
| doi_str_mv | 10.3847/1538-3881/aadcfc |
| format | Article |
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I. Refined System Parameters and Transit Timing Variations of HAT-P-29b</title><source>IOP Publishing Free Content</source><creator>Wang, Songhu ; Wang, Xian-Yu ; Wang, Yong-Hao ; Liu, Hui-Gen ; Hinse, Tobias C. ; Eastman, Jason ; Bayliss, Daniel ; Hori, Yasunori ; Hu, Shao-Ming ; Li, Kai ; Liu, Jinzhong ; Narita, Norio ; Peng, Xiyan ; Wittenmyer, R. A. ; Wu, Zhen-Yu ; Zhang, Hui ; Zhang, Xiaojia ; Zhao, Haibin ; Zhou, Ji-Lin ; Zhou, George ; Zhou, Xu ; Laughlin, Gregory</creator><creatorcontrib>Wang, Songhu ; Wang, Xian-Yu ; Wang, Yong-Hao ; Liu, Hui-Gen ; Hinse, Tobias C. ; Eastman, Jason ; Bayliss, Daniel ; Hori, Yasunori ; Hu, Shao-Ming ; Li, Kai ; Liu, Jinzhong ; Narita, Norio ; Peng, Xiyan ; Wittenmyer, R. A. ; Wu, Zhen-Yu ; Zhang, Hui ; Zhang, Xiaojia ; Zhao, Haibin ; Zhou, Ji-Lin ; Zhou, George ; Zhou, Xu ; Laughlin, Gregory</creatorcontrib><description>We report the photometry of six transits of the hot Jupiter HAT-P-29b obtained from 2013 October to 2015 January. We analyze the new light curves, in combination with the published photometric, Doppler velocimetric, and spectroscopic measurements, finding an updated orbital ephemeris for the HAT-P-29 system, and P = 5.723390(13) days. This result is 17.63 s (4.0 ) longer than the previously published value, amounting to errors exceeding 2.5 hr at the time of writing (on UTC 2018 June 1). The measured transit mid-times for HAT-P-29b show no compelling evidence of timing anomalies from a linear model, which rules out the presence of perturbers with masses greater than 0.6, 0.7, 0.5, and 0.4 M⊕ near the 1:2, 2:3, 3:2, and 2:1 resonances with HAT-P-29b, respectively.</description><identifier>ISSN: 0004-6256</identifier><identifier>EISSN: 1538-3881</identifier><identifier>DOI: 10.3847/1538-3881/aadcfc</identifier><language>eng</language><publisher>Madison: The American Astronomical Society</publisher><subject>Anomalies ; Astronomy ; Extrasolar planets ; Gas giant planets ; Jupiter ; Light curve ; Photometry ; planetary systems ; planets and satellites: fundamental parameters ; planets and satellites: individual (HAT-P-29b) ; stars: fundamental parameters ; stars: individual (HAT-P-29) ; techniques: photometric ; Transit ; Universal time</subject><ispartof>The Astronomical journal, 2018-10, Vol.156 (4), p.181</ispartof><rights>2018. The American Astronomical Society. All rights reserved.</rights><rights>Copyright IOP Publishing Oct 2018</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c416t-68fa0f63f23b843f1ed97e8638328dabe5571cc2290c27e538757c9fe6f9fc373</citedby><cites>FETCH-LOGICAL-c416t-68fa0f63f23b843f1ed97e8638328dabe5571cc2290c27e538757c9fe6f9fc373</cites><orcidid>0000-0002-6612-5127 ; 0000-0003-0261-6362 ; 0000-0001-8870-3146 ; 0000-0002-3253-2621 ; 0000-0003-4676-0251 ; 0000-0001-8511-2981 ; 0000-0002-4891-3517 ; 0000-0003-1680-2940 ; 0000-0003-3491-6394 ; 0000-0001-5162-1753 ; 0000-0003-3773-5142 ; 0000-0003-3217-7794 ; 0000-0001-6023-1335</orcidid></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><linktopdf>$$Uhttps://iopscience.iop.org/article/10.3847/1538-3881/aadcfc/pdf$$EPDF$$P50$$Giop$$H</linktopdf><link.rule.ids>314,776,780,27903,27904,38847,38869,53819,53846</link.rule.ids><linktorsrc>$$Uhttps://iopscience.iop.org/article/10.3847/1538-3881/aadcfc$$EView_record_in_IOP_Publishing$$FView_record_in_$$GIOP_Publishing</linktorsrc></links><search><creatorcontrib>Wang, Songhu</creatorcontrib><creatorcontrib>Wang, Xian-Yu</creatorcontrib><creatorcontrib>Wang, Yong-Hao</creatorcontrib><creatorcontrib>Liu, Hui-Gen</creatorcontrib><creatorcontrib>Hinse, Tobias C.</creatorcontrib><creatorcontrib>Eastman, Jason</creatorcontrib><creatorcontrib>Bayliss, Daniel</creatorcontrib><creatorcontrib>Hori, Yasunori</creatorcontrib><creatorcontrib>Hu, Shao-Ming</creatorcontrib><creatorcontrib>Li, Kai</creatorcontrib><creatorcontrib>Liu, Jinzhong</creatorcontrib><creatorcontrib>Narita, Norio</creatorcontrib><creatorcontrib>Peng, Xiyan</creatorcontrib><creatorcontrib>Wittenmyer, R. A.</creatorcontrib><creatorcontrib>Wu, Zhen-Yu</creatorcontrib><creatorcontrib>Zhang, Hui</creatorcontrib><creatorcontrib>Zhang, Xiaojia</creatorcontrib><creatorcontrib>Zhao, Haibin</creatorcontrib><creatorcontrib>Zhou, Ji-Lin</creatorcontrib><creatorcontrib>Zhou, George</creatorcontrib><creatorcontrib>Zhou, Xu</creatorcontrib><creatorcontrib>Laughlin, Gregory</creatorcontrib><title>Transiting Exoplanet Monitoring Project (TEMP). I. Refined System Parameters and Transit Timing Variations of HAT-P-29b</title><title>The Astronomical journal</title><addtitle>AJ</addtitle><addtitle>Astron. J</addtitle><description>We report the photometry of six transits of the hot Jupiter HAT-P-29b obtained from 2013 October to 2015 January. We analyze the new light curves, in combination with the published photometric, Doppler velocimetric, and spectroscopic measurements, finding an updated orbital ephemeris for the HAT-P-29 system, and P = 5.723390(13) days. This result is 17.63 s (4.0 ) longer than the previously published value, amounting to errors exceeding 2.5 hr at the time of writing (on UTC 2018 June 1). The measured transit mid-times for HAT-P-29b show no compelling evidence of timing anomalies from a linear model, which rules out the presence of perturbers with masses greater than 0.6, 0.7, 0.5, and 0.4 M⊕ near the 1:2, 2:3, 3:2, and 2:1 resonances with HAT-P-29b, respectively.</description><subject>Anomalies</subject><subject>Astronomy</subject><subject>Extrasolar planets</subject><subject>Gas giant planets</subject><subject>Jupiter</subject><subject>Light curve</subject><subject>Photometry</subject><subject>planetary systems</subject><subject>planets and satellites: fundamental parameters</subject><subject>planets and satellites: individual (HAT-P-29b)</subject><subject>stars: fundamental parameters</subject><subject>stars: individual (HAT-P-29)</subject><subject>techniques: photometric</subject><subject>Transit</subject><subject>Universal time</subject><issn>0004-6256</issn><issn>1538-3881</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2018</creationdate><recordtype>article</recordtype><recordid>eNp1kM1LwzAYxoMoOKd3jwEvCnZLmjZNj2NMN3BYtHotWZpIxprUJEP339vSoSdPLzw8H7w_AK4xmhCWZFOcEhYRxvCU81oocQJGv9IpGCGEkojGKT0HF95vEcKYoWQEvkrHjddBmw-4-LbtjhsZ4NoaHazrxcLZrRQB3paLdXE3gasJfJFKG1nD14MPsoEFd7yRQToPuanhsRCWuunz79xpHrQ1HloFl7MyKqI431yCM8V3Xl4d7xi8PSzK-TJ6en5czWdPkUgwDRFliiNFiYrJhiVEYVnnmWSUMBKzmm9kmmZYiDjOkYgz2T2cpZnIlaQqV4JkZAxuht7W2c-99KHa2r0z3WQVE5rSDh0jnQsNLuGs906qqnW64e5QYVT1eKueZdWzrAa8XeR-iGjb_nX-a_8BmSN8JA</recordid><startdate>20181001</startdate><enddate>20181001</enddate><creator>Wang, Songhu</creator><creator>Wang, Xian-Yu</creator><creator>Wang, Yong-Hao</creator><creator>Liu, Hui-Gen</creator><creator>Hinse, Tobias C.</creator><creator>Eastman, Jason</creator><creator>Bayliss, Daniel</creator><creator>Hori, Yasunori</creator><creator>Hu, Shao-Ming</creator><creator>Li, Kai</creator><creator>Liu, Jinzhong</creator><creator>Narita, Norio</creator><creator>Peng, Xiyan</creator><creator>Wittenmyer, R. 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A.</au><au>Wu, Zhen-Yu</au><au>Zhang, Hui</au><au>Zhang, Xiaojia</au><au>Zhao, Haibin</au><au>Zhou, Ji-Lin</au><au>Zhou, George</au><au>Zhou, Xu</au><au>Laughlin, Gregory</au><format>journal</format><genre>article</genre><ristype>JOUR</ristype><atitle>Transiting Exoplanet Monitoring Project (TEMP). I. Refined System Parameters and Transit Timing Variations of HAT-P-29b</atitle><jtitle>The Astronomical journal</jtitle><stitle>AJ</stitle><addtitle>Astron. J</addtitle><date>2018-10-01</date><risdate>2018</risdate><volume>156</volume><issue>4</issue><spage>181</spage><pages>181-</pages><issn>0004-6256</issn><eissn>1538-3881</eissn><abstract>We report the photometry of six transits of the hot Jupiter HAT-P-29b obtained from 2013 October to 2015 January. We analyze the new light curves, in combination with the published photometric, Doppler velocimetric, and spectroscopic measurements, finding an updated orbital ephemeris for the HAT-P-29 system, and P = 5.723390(13) days. This result is 17.63 s (4.0 ) longer than the previously published value, amounting to errors exceeding 2.5 hr at the time of writing (on UTC 2018 June 1). The measured transit mid-times for HAT-P-29b show no compelling evidence of timing anomalies from a linear model, which rules out the presence of perturbers with masses greater than 0.6, 0.7, 0.5, and 0.4 M⊕ near the 1:2, 2:3, 3:2, and 2:1 resonances with HAT-P-29b, respectively.</abstract><cop>Madison</cop><pub>The American Astronomical Society</pub><doi>10.3847/1538-3881/aadcfc</doi><tpages>11</tpages><orcidid>https://orcid.org/0000-0002-6612-5127</orcidid><orcidid>https://orcid.org/0000-0003-0261-6362</orcidid><orcidid>https://orcid.org/0000-0001-8870-3146</orcidid><orcidid>https://orcid.org/0000-0002-3253-2621</orcidid><orcidid>https://orcid.org/0000-0003-4676-0251</orcidid><orcidid>https://orcid.org/0000-0001-8511-2981</orcidid><orcidid>https://orcid.org/0000-0002-4891-3517</orcidid><orcidid>https://orcid.org/0000-0003-1680-2940</orcidid><orcidid>https://orcid.org/0000-0003-3491-6394</orcidid><orcidid>https://orcid.org/0000-0001-5162-1753</orcidid><orcidid>https://orcid.org/0000-0003-3773-5142</orcidid><orcidid>https://orcid.org/0000-0003-3217-7794</orcidid><orcidid>https://orcid.org/0000-0001-6023-1335</orcidid><oa>free_for_read</oa></addata></record> |
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| subjects | Anomalies Astronomy Extrasolar planets Gas giant planets Jupiter Light curve Photometry planetary systems planets and satellites: fundamental parameters planets and satellites: individual (HAT-P-29b) stars: fundamental parameters stars: individual (HAT-P-29) techniques: photometric Transit Universal time |
| title | Transiting Exoplanet Monitoring Project (TEMP). I. Refined System Parameters and Transit Timing Variations of HAT-P-29b |
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