The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

Samuel W. Yee; Joshua N. Winn; Joel D. Hartman; Joseph E. Rodriguez; George Zhou; Samuel N. Quinn; David W. Latham; Allyson Bieryla; Karen A. Collins; Brett C. Addison; Isabel Angelo; Khalid Barkaoui; Paul Benni; Andrew W. Boyle; Rafael Brahm; R. Paul Butler; David R. Ciardi; Kevin I. Collins; Dennis M. Conti; Jeffrey D. Crane; Fei Dai; Courtney D. Dressing; Jason D. Eastman; Zahra Essack; Raquel Forés-Toribio; Elise Furlan; Tianjun Gan; Steven Giacalone; Holden Gill; Eric Girardin; Thomas Henning; Christopher E. Henze; Melissa J. Hobson; Jonathan Horner; Andrew W. Howard; Steve B. Howell; Chelsea X. Huang; Howard Isaacson; Jon M. Jenkins; Eric L.N. Jensen; Andrés Jordán; Stephen R. Kane; John F. Kielkopf; Slawomir Lasota; Alan M. Levine; Jack Lubin; Andrew W. Mann; Bob Massey; Kim K. McLeod; Matthew W. Mengel; Jose A. Muñoz; Felipe Murgas; Enric Palle; Peter Plavchan; Adam Popowicz; Don J. Radford; George R. Ricker; Pamela Rowden; Boris S. Safonov; Arjun B. Savel; Richard P. Schwarz; S. Seager; Ramotholo Sefako; Avi Shporer; Gregor Srdoc; Ivan S. Strakhov; Johanna K. Teske; C. G. Tinney; Dakotah Tyler; Robert A. Wittenmyer; Hui Zhang; Carl Ziegler

doi:10.3847/1538-3881/ac73ff

The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

Samuel W. Yee, Joshua N. Winn, Joel D. Hartman, Joseph E. Rodriguez, George Zhou, Samuel N. Quinn, David W. Latham, Allyson Bieryla, Karen A. Collins, Brett C. Addison, Isabel Angelo, Khalid Barkaoui, Paul Benni, Andrew W. Boyle, Rafael Brahm, R. Paul Butler, David R. Ciardi, Kevin I. Collins, Dennis M. Conti, Jeffrey D. CraneFei Dai, Courtney D. Dressing, Jason D. Eastman, Zahra Essack, Raquel Forés-Toribio, Elise Furlan, Tianjun Gan, Steven Giacalone, Holden Gill, Eric Girardin, Thomas Henning, Christopher E. Henze, Melissa J. Hobson, Jonathan Horner, Andrew W. Howard, Steve B. Howell, Chelsea X. Huang, Howard Isaacson, Jon M. Jenkins, Eric L.N. Jensen, Andrés Jordán, Stephen R. Kane, John F. Kielkopf, Slawomir Lasota, Alan M. Levine, Jack Lubin, Andrew W. Mann, Bob Massey, Kim K. McLeod, Matthew W. Mengel, Jose A. Muñoz, Felipe Murgas, Enric Palle, Peter Plavchan, Adam Popowicz, Don J. Radford, George R. Ricker, Pamela Rowden, Boris S. Safonov, Arjun B. Savel, Richard P. Schwarz, S. Seager, Ramotholo Sefako, Avi Shporer, Gregor Srdoc, Ivan S. Strakhov, Johanna K. Teske, C. G. Tinney, Dakotah Tyler, Robert A. Wittenmyer, Hui Zhang, Carl Ziegler

Astrophysical Sciences

Research output: Contribution to journal › Article › peer-review

8 Scopus citations

Abstract

Hot Jupiters - short-period giant planets - were the first extrasolar planets to be discovered, but many questions about their origin remain. NASA's Transiting Exoplanet Survey Satellite (TESS), an all-sky search for transiting planets, presents an opportunity to address these questions by constructing a uniform sample of hot Jupiters for demographic study through new detections and unifying the work of previous ground-based transit surveys. As the first results of an effort to build this large sample of planets, we report here the discovery of 10 new hot Jupiters (TOI-2193A b, TOI-2207b, TOI-2236b, TOI-2421b, TOI-2567b, TOI-2570b, TOI-3331b, TOI-3540A b, TOI-3693b, TOI-4137b). All of the planets were identified as planet candidates based on periodic flux dips observed by TESS, and were subsequently confirmed using ground-based time-series photometry, high-angular-resolution imaging, and high-resolution spectroscopy coordinated with the TESS Follow-up Observing Program. The 10 newly discovered planets orbit relatively bright F and G stars (G < 12.5, Teff between 4800 and 6200 K). The planets' orbital periods range from 2 to 10 days, and their masses range from 0.2 to 2.2 Jupiter masses. TOI-2421b is notable for being a Saturn-mass planet and TOI-2567b for being a "sub-Saturn,"with masses of 0.322 ± 0.073 and 0.195 ± 0.030 Jupiter masses, respectively. We also measured a detectably eccentric orbit (e = 0.17 ± 0.05) for TOI-2207b, a planet on an 8 day orbit, while placing an upper limit of e < 0.052 for TOI-3693b, which has a 9 day orbital period. The 10 planets described here represent an important step toward using TESS to create a large and statistically useful sample of hot Jupiters.

Original language	English (US)
Article number	70
Journal	Astronomical Journal
Volume	164
Issue number	2
DOIs	https://doi.org/10.3847/1538-3881/ac73ff
State	Published - Aug 1 2022

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Access to Document

10.3847/1538-3881/ac73ff

Cite this

Yee, S. W., Winn, J. N., Hartman, J. D., Rodriguez, J. E., Zhou, G., Quinn, S. N., Latham, D. W., Bieryla, A., Collins, K. A., Addison, B. C., Angelo, I., Barkaoui, K., Benni, P., Boyle, A. W., Brahm, R., Butler, R. P., Ciardi, D. R., Collins, K. I., Conti, D. M., ... Ziegler, C. (2022). The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets. Astronomical Journal, 164(2), Article 70. https://doi.org/10.3847/1538-3881/ac73ff

@article{f4999af69c884cc4a9be70bf39b6fd52,

title = "The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets",

abstract = "Hot Jupiters - short-period giant planets - were the first extrasolar planets to be discovered, but many questions about their origin remain. NASA's Transiting Exoplanet Survey Satellite (TESS), an all-sky search for transiting planets, presents an opportunity to address these questions by constructing a uniform sample of hot Jupiters for demographic study through new detections and unifying the work of previous ground-based transit surveys. As the first results of an effort to build this large sample of planets, we report here the discovery of 10 new hot Jupiters (TOI-2193A b, TOI-2207b, TOI-2236b, TOI-2421b, TOI-2567b, TOI-2570b, TOI-3331b, TOI-3540A b, TOI-3693b, TOI-4137b). All of the planets were identified as planet candidates based on periodic flux dips observed by TESS, and were subsequently confirmed using ground-based time-series photometry, high-angular-resolution imaging, and high-resolution spectroscopy coordinated with the TESS Follow-up Observing Program. The 10 newly discovered planets orbit relatively bright F and G stars (G < 12.5, Teff between 4800 and 6200 K). The planets' orbital periods range from 2 to 10 days, and their masses range from 0.2 to 2.2 Jupiter masses. TOI-2421b is notable for being a Saturn-mass planet and TOI-2567b for being a {"}sub-Saturn,{"}with masses of 0.322 ± 0.073 and 0.195 ± 0.030 Jupiter masses, respectively. We also measured a detectably eccentric orbit (e = 0.17 ± 0.05) for TOI-2207b, a planet on an 8 day orbit, while placing an upper limit of e < 0.052 for TOI-3693b, which has a 9 day orbital period. The 10 planets described here represent an important step toward using TESS to create a large and statistically useful sample of hot Jupiters.",

author = "Yee, {Samuel W.} and Winn, {Joshua N.} and Hartman, {Joel D.} and Rodriguez, {Joseph E.} and George Zhou and Quinn, {Samuel N.} and Latham, {David W.} and Allyson Bieryla and Collins, {Karen A.} and Addison, {Brett C.} and Isabel Angelo and Khalid Barkaoui and Paul Benni and Boyle, {Andrew W.} and Rafael Brahm and Butler, {R. Paul} and Ciardi, {David R.} and Collins, {Kevin I.} and Conti, {Dennis M.} and Crane, {Jeffrey D.} and Fei Dai and Dressing, {Courtney D.} and Eastman, {Jason D.} and Zahra Essack and Raquel For{\'e}s-Toribio and Elise Furlan and Tianjun Gan and Steven Giacalone and Holden Gill and Eric Girardin and Thomas Henning and Henze, {Christopher E.} and Hobson, {Melissa J.} and Jonathan Horner and Howard, {Andrew W.} and Howell, {Steve B.} and Huang, {Chelsea X.} and Howard Isaacson and Jenkins, {Jon M.} and Jensen, {Eric L.N.} and Andr{\'e}s Jord{\'a}n and Kane, {Stephen R.} and Kielkopf, {John F.} and Slawomir Lasota and Levine, {Alan M.} and Jack Lubin and Mann, {Andrew W.} and Bob Massey and McLeod, {Kim K.} and Mengel, {Matthew W.} and Mu{\~n}oz, {Jose A.} and Felipe Murgas and Enric Palle and Peter Plavchan and Adam Popowicz and Radford, {Don J.} and Ricker, {George R.} and Pamela Rowden and Safonov, {Boris S.} and Savel, {Arjun B.} and Schwarz, {Richard P.} and S. Seager and Ramotholo Sefako and Avi Shporer and Gregor Srdoc and Strakhov, {Ivan S.} and Teske, {Johanna K.} and Tinney, {C. G.} and Dakotah Tyler and Wittenmyer, {Robert A.} and Hui Zhang and Carl Ziegler",

note = "Funding Information: Some of the data presented herein were obtained at the M inerva –Australis facility from telescope time allocated under the NN-EXPLORE program with support from the National Aeronautics and Space Administration. M inerva –Australis is supported by Australian Research Council LIEF grant LE160100001, Discovery grants DP180100972 and DP220100365, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. We respectfully acknowledge the traditional custodians of all lands throughout Australia, and recognize their continued cultural and spiritual connection to the land, waterways, cosmos, and community. We pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Kambuwal nations, upon whose lands the M inerva –Australis facility at Mt. Kent is situated. Funding Information: This paper contains data taken with the NEID instrument, which was funded by the NASA-NSF Exoplanet Observational Research (NN-EXPLORE) partnership and built by Pennsylvania State University. NEID is installed on the WIYN telescope, which is operated by the National Optical Astronomy Observatory, and the NEID archive is operated by the NASA Exoplanet Science Institute at the California Institute of Technology. NN-EXPLORE is managed by the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. The data presented herein were obtained at the WIYN Observatory from telescope time allocated to NN-EXPLORE through the scientific partnership of the National Aeronautics and Space Administration, the National Science Foundation, and NOIRLab. This work was supported by a NASA WIYN PI Data Award, administered by the NASA Exoplanet Science Institute. The authors thank Sarah Logsdon and Heidi Schweiker for help with the NEID observations. The authors are honored to be permitted to conduct astronomical research on Iolkam Du'ag (Kitt Peak), a mountain with particular significance to the Tohono O'odham. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This research has used data from the CTIO/SMARTS 1.5m telescope, which is operated as part of the SMARTS Consortium by RECONS (www.recons.org) members Todd Henry, Hodari James, Wei-Chun Jao, and Leonardo Paredes. At the telescope, observations were carried out by Roberto Aviles and Rodrigo Hinojosa. The CHIRON data were obtained from telescope time allocated under the NN-EXPLORE program with support from the National Aeronautics and Space Administration. Some of the data presented herein were obtained at the MINERVA-Australis facility from telescope time allocated under the NN-EXPLORE program with support from the National Aeronautics and Space Administration. MINERVA- Australis is supported by Australian Research Council LIEF grant LE160100001, Discovery grants DP180100972 and DP220100365, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. We respectfully acknowledge the traditional custodians of all lands throughout Australia, and recognize their continued cultural and spiritual connection to the land, waterways, cosmos, and community. We pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Kambuwal nations, upon whose lands the MINERVA-Australis facility at Mt. Kent is situated. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This paper makes use of data from the MEarth Project, which is a collaboration between Harvard University and the Smithsonian Astrophysical Observatory. The MEarth Project acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering, the National Science Foundation under grants AST-0807690, AST-1109468, AST-1616624 and AST-1004488 (Alan T. Waterman Award), the National Aeronautics and Space Administration under grant No. 80NSSC18K0476 issued through the XRP Program, and the John Templeton Foundation. Adam Popowicz and Slawomir Lasota were responsible for data processing and automation of observations at SUTO observatories and were financed by grant BK-246/RAu-11/2022. A.J. acknowledges support from ANID - Millennium Science Initiative - ICN12_009 and FONDECYT project 1210718. J.H. acknowledges support from NASA grants 80NSSC 19K0386, 80NSSC19K1728, and 80NSSC21K0335. Facilities:TESS, MAST, Gaia, Keck: I (HIRES), WIYN (NEID), Magellan: Clay (PFS), CTIO: 1.5m (CHIRON), Max Planck: 2.2m (FEROS), FLWO: 1.5m (TRES), LCOGT, Gemini. Funding Information: This paper makes use of data from the MEarth Project, which is a collaboration between Harvard University and the Smithsonian Astrophysical Observatory. The MEarth Project acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering, the National Science Foundation under grants AST-0807690, AST-1109468, AST-1616624 and AST-1004488 (Alan T. Waterman Award), the National Aeronautics and Space Administration under grant No. 80NSSC18K0476 issued through the XRP Program, and the John Templeton Foundation. Funding Information: J.H. acknowledges support from NASA grants 80NSSC19K0386, 80NSSC19K1728, and 80NSSC21K0335. Funding Information: Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Keck telescope time was granted by NOIRLab (Prop. ID 2021B-0162, PI: Yee) through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Funding Information: Adam Popowicz and Slawomir Lasota were responsible for data processing and automation of observations at SUTO observatories and were financed by grant BK-246/RAu-11/2022. A.J. acknowledges support from ANID—Millennium Science Initiative—ICN12_009 and FONDECYT project 1210718. Funding Information: This paper contains data taken with the NEID instrument, which was funded by the NASA-NSF Exoplanet Observational Research (NN-EXPLORE) partnership and built by Pennsylvania State University. NEID is installed on the WIYN telescope, which is operated by the National Optical Astronomy Observatory, and the NEID archive is operated by the NASA Exoplanet Science Institute at the California Institute of Technology. NN-EXPLORE is managed by the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. The data presented herein were obtained at the WIYN Observatory from telescope time allocated to NN-EXPLORE through the scientific partnership of the National Aeronautics and Space Administration, the National Science Foundation, and NOIRLab. This work was supported by a NASA WIYN PI Data Award, administered by the NASA Exoplanet Science Institute. The authors thank Sarah Logsdon and Heidi Schweiker for help with the NEID observations. The authors are honored to be permitted to conduct astronomical research on Iolkam Du{\textquoteright}ag (Kitt Peak), a mountain with particular significance to the Tohono O{\textquoteright}odham. Funding Information: This paper includes data collected by the TESS mission that are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA{\textquoteright}s Science Mission Directorate. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. We also acknowledge the use of data from the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research made use of Lightkurve, a Python package for Kepler and TESS data analysis (Lightkurve Collaboration et al. ). Funding Information: This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. Publisher Copyright: {\textcopyright} 2022. The Author(s).",

year = "2022",

month = aug,

day = "1",

doi = "10.3847/1538-3881/ac73ff",

language = "English (US)",

volume = "164",

journal = "Astronomical Journal",

issn = "0004-6256",

publisher = "IOP Publishing Ltd.",

number = "2",

}

Yee, SW, Winn, JN, Hartman, JD, Rodriguez, JE, Zhou, G, Quinn, SN, Latham, DW, Bieryla, A, Collins, KA, Addison, BC, Angelo, I, Barkaoui, K, Benni, P, Boyle, AW, Brahm, R, Butler, RP, Ciardi, DR, Collins, KI, Conti, DM, Crane, JD, Dai, F, Dressing, CD, Eastman, JD, Essack, Z, Forés-Toribio, R, Furlan, E, Gan, T, Giacalone, S, Gill, H, Girardin, E, Henning, T, Henze, CE, Hobson, MJ, Horner, J, Howard, AW, Howell, SB, Huang, CX, Isaacson, H, Jenkins, JM, Jensen, ELN, Jordán, A, Kane, SR, Kielkopf, JF, Lasota, S, Levine, AM, Lubin, J, Mann, AW, Massey, B, McLeod, KK, Mengel, MW, Muñoz, JA, Murgas, F, Palle, E, Plavchan, P, Popowicz, A, Radford, DJ, Ricker, GR, Rowden, P, Safonov, BS, Savel, AB, Schwarz, RP, Seager, S, Sefako, R, Shporer, A, Srdoc, G, Strakhov, IS, Teske, JK, Tinney, CG, Tyler, D, Wittenmyer, RA, Zhang, H & Ziegler, C 2022, 'The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets', Astronomical Journal, vol. 164, no. 2, 70. https://doi.org/10.3847/1538-3881/ac73ff

TY - JOUR

T1 - The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

AU - Yee, Samuel W.

AU - Winn, Joshua N.

AU - Hartman, Joel D.

AU - Rodriguez, Joseph E.

AU - Zhou, George

AU - Quinn, Samuel N.

AU - Latham, David W.

AU - Bieryla, Allyson

AU - Collins, Karen A.

AU - Addison, Brett C.

AU - Angelo, Isabel

AU - Barkaoui, Khalid

AU - Benni, Paul

AU - Boyle, Andrew W.

AU - Brahm, Rafael

AU - Butler, R. Paul

AU - Ciardi, David R.

AU - Collins, Kevin I.

AU - Conti, Dennis M.

AU - Crane, Jeffrey D.

AU - Dai, Fei

AU - Dressing, Courtney D.

AU - Eastman, Jason D.

AU - Essack, Zahra

AU - Forés-Toribio, Raquel

AU - Furlan, Elise

AU - Gan, Tianjun

AU - Giacalone, Steven

AU - Gill, Holden

AU - Girardin, Eric

AU - Henning, Thomas

AU - Henze, Christopher E.

AU - Hobson, Melissa J.

AU - Horner, Jonathan

AU - Howard, Andrew W.

AU - Howell, Steve B.

AU - Huang, Chelsea X.

AU - Isaacson, Howard

AU - Jenkins, Jon M.

AU - Jensen, Eric L.N.

AU - Jordán, Andrés

AU - Kane, Stephen R.

AU - Kielkopf, John F.

AU - Lasota, Slawomir

AU - Levine, Alan M.

AU - Lubin, Jack

AU - Mann, Andrew W.

AU - Massey, Bob

AU - McLeod, Kim K.

AU - Mengel, Matthew W.

AU - Muñoz, Jose A.

AU - Murgas, Felipe

AU - Palle, Enric

AU - Plavchan, Peter

AU - Popowicz, Adam

AU - Radford, Don J.

AU - Ricker, George R.

AU - Rowden, Pamela

AU - Safonov, Boris S.

AU - Savel, Arjun B.

AU - Schwarz, Richard P.

AU - Seager, S.

AU - Sefako, Ramotholo

AU - Shporer, Avi

AU - Srdoc, Gregor

AU - Strakhov, Ivan S.

AU - Teske, Johanna K.

AU - Tinney, C. G.

AU - Tyler, Dakotah

AU - Wittenmyer, Robert A.

AU - Zhang, Hui

AU - Ziegler, Carl

N1 - Funding Information: Some of the data presented herein were obtained at the M inerva –Australis facility from telescope time allocated under the NN-EXPLORE program with support from the National Aeronautics and Space Administration. M inerva –Australis is supported by Australian Research Council LIEF grant LE160100001, Discovery grants DP180100972 and DP220100365, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. We respectfully acknowledge the traditional custodians of all lands throughout Australia, and recognize their continued cultural and spiritual connection to the land, waterways, cosmos, and community. We pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Kambuwal nations, upon whose lands the M inerva –Australis facility at Mt. Kent is situated. Funding Information: This paper contains data taken with the NEID instrument, which was funded by the NASA-NSF Exoplanet Observational Research (NN-EXPLORE) partnership and built by Pennsylvania State University. NEID is installed on the WIYN telescope, which is operated by the National Optical Astronomy Observatory, and the NEID archive is operated by the NASA Exoplanet Science Institute at the California Institute of Technology. NN-EXPLORE is managed by the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. The data presented herein were obtained at the WIYN Observatory from telescope time allocated to NN-EXPLORE through the scientific partnership of the National Aeronautics and Space Administration, the National Science Foundation, and NOIRLab. This work was supported by a NASA WIYN PI Data Award, administered by the NASA Exoplanet Science Institute. The authors thank Sarah Logsdon and Heidi Schweiker for help with the NEID observations. The authors are honored to be permitted to conduct astronomical research on Iolkam Du'ag (Kitt Peak), a mountain with particular significance to the Tohono O'odham. This paper includes data gathered with the 6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile. This research has used data from the CTIO/SMARTS 1.5m telescope, which is operated as part of the SMARTS Consortium by RECONS (www.recons.org) members Todd Henry, Hodari James, Wei-Chun Jao, and Leonardo Paredes. At the telescope, observations were carried out by Roberto Aviles and Rodrigo Hinojosa. The CHIRON data were obtained from telescope time allocated under the NN-EXPLORE program with support from the National Aeronautics and Space Administration. Some of the data presented herein were obtained at the MINERVA-Australis facility from telescope time allocated under the NN-EXPLORE program with support from the National Aeronautics and Space Administration. MINERVA- Australis is supported by Australian Research Council LIEF grant LE160100001, Discovery grants DP180100972 and DP220100365, Mount Cuba Astronomical Foundation, and institutional partners University of Southern Queensland, UNSW Sydney, MIT, Nanjing University, George Mason University, University of Louisville, University of California Riverside, University of Florida, and The University of Texas at Austin. We respectfully acknowledge the traditional custodians of all lands throughout Australia, and recognize their continued cultural and spiritual connection to the land, waterways, cosmos, and community. We pay our deepest respects to all Elders, ancestors and descendants of the Giabal, Jarowair, and Kambuwal nations, upon whose lands the MINERVA-Australis facility at Mt. Kent is situated. This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. This paper makes use of data from the MEarth Project, which is a collaboration between Harvard University and the Smithsonian Astrophysical Observatory. The MEarth Project acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering, the National Science Foundation under grants AST-0807690, AST-1109468, AST-1616624 and AST-1004488 (Alan T. Waterman Award), the National Aeronautics and Space Administration under grant No. 80NSSC18K0476 issued through the XRP Program, and the John Templeton Foundation. Adam Popowicz and Slawomir Lasota were responsible for data processing and automation of observations at SUTO observatories and were financed by grant BK-246/RAu-11/2022. A.J. acknowledges support from ANID - Millennium Science Initiative - ICN12_009 and FONDECYT project 1210718. J.H. acknowledges support from NASA grants 80NSSC 19K0386, 80NSSC19K1728, and 80NSSC21K0335. Facilities:TESS, MAST, Gaia, Keck: I (HIRES), WIYN (NEID), Magellan: Clay (PFS), CTIO: 1.5m (CHIRON), Max Planck: 2.2m (FEROS), FLWO: 1.5m (TRES), LCOGT, Gemini. Funding Information: This paper makes use of data from the MEarth Project, which is a collaboration between Harvard University and the Smithsonian Astrophysical Observatory. The MEarth Project acknowledges funding from the David and Lucile Packard Fellowship for Science and Engineering, the National Science Foundation under grants AST-0807690, AST-1109468, AST-1616624 and AST-1004488 (Alan T. Waterman Award), the National Aeronautics and Space Administration under grant No. 80NSSC18K0476 issued through the XRP Program, and the John Templeton Foundation. Funding Information: J.H. acknowledges support from NASA grants 80NSSC19K0386, 80NSSC19K1728, and 80NSSC21K0335. Funding Information: Some of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. Keck telescope time was granted by NOIRLab (Prop. ID 2021B-0162, PI: Yee) through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Funding Information: Adam Popowicz and Slawomir Lasota were responsible for data processing and automation of observations at SUTO observatories and were financed by grant BK-246/RAu-11/2022. A.J. acknowledges support from ANID—Millennium Science Initiative—ICN12_009 and FONDECYT project 1210718. Funding Information: This paper contains data taken with the NEID instrument, which was funded by the NASA-NSF Exoplanet Observational Research (NN-EXPLORE) partnership and built by Pennsylvania State University. NEID is installed on the WIYN telescope, which is operated by the National Optical Astronomy Observatory, and the NEID archive is operated by the NASA Exoplanet Science Institute at the California Institute of Technology. NN-EXPLORE is managed by the Jet Propulsion Laboratory, California Institute of Technology under contract with the National Aeronautics and Space Administration. The data presented herein were obtained at the WIYN Observatory from telescope time allocated to NN-EXPLORE through the scientific partnership of the National Aeronautics and Space Administration, the National Science Foundation, and NOIRLab. This work was supported by a NASA WIYN PI Data Award, administered by the NASA Exoplanet Science Institute. The authors thank Sarah Logsdon and Heidi Schweiker for help with the NEID observations. The authors are honored to be permitted to conduct astronomical research on Iolkam Du’ag (Kitt Peak), a mountain with particular significance to the Tohono O’odham. Funding Information: This paper includes data collected by the TESS mission that are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA’s Science Mission Directorate. We acknowledge the use of public TESS data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. Resources supporting this work were provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center for the production of the SPOC data products. We also acknowledge the use of data from the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This research made use of Lightkurve, a Python package for Kepler and TESS data analysis (Lightkurve Collaboration et al. ). Funding Information: This work makes use of observations from the LCOGT network. Part of the LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program (MSIP). MSIP is funded by NSF. Publisher Copyright: © 2022. The Author(s).

PY - 2022/8/1

Y1 - 2022/8/1

N2 - Hot Jupiters - short-period giant planets - were the first extrasolar planets to be discovered, but many questions about their origin remain. NASA's Transiting Exoplanet Survey Satellite (TESS), an all-sky search for transiting planets, presents an opportunity to address these questions by constructing a uniform sample of hot Jupiters for demographic study through new detections and unifying the work of previous ground-based transit surveys. As the first results of an effort to build this large sample of planets, we report here the discovery of 10 new hot Jupiters (TOI-2193A b, TOI-2207b, TOI-2236b, TOI-2421b, TOI-2567b, TOI-2570b, TOI-3331b, TOI-3540A b, TOI-3693b, TOI-4137b). All of the planets were identified as planet candidates based on periodic flux dips observed by TESS, and were subsequently confirmed using ground-based time-series photometry, high-angular-resolution imaging, and high-resolution spectroscopy coordinated with the TESS Follow-up Observing Program. The 10 newly discovered planets orbit relatively bright F and G stars (G < 12.5, Teff between 4800 and 6200 K). The planets' orbital periods range from 2 to 10 days, and their masses range from 0.2 to 2.2 Jupiter masses. TOI-2421b is notable for being a Saturn-mass planet and TOI-2567b for being a "sub-Saturn,"with masses of 0.322 ± 0.073 and 0.195 ± 0.030 Jupiter masses, respectively. We also measured a detectably eccentric orbit (e = 0.17 ± 0.05) for TOI-2207b, a planet on an 8 day orbit, while placing an upper limit of e < 0.052 for TOI-3693b, which has a 9 day orbital period. The 10 planets described here represent an important step toward using TESS to create a large and statistically useful sample of hot Jupiters.

AB - Hot Jupiters - short-period giant planets - were the first extrasolar planets to be discovered, but many questions about their origin remain. NASA's Transiting Exoplanet Survey Satellite (TESS), an all-sky search for transiting planets, presents an opportunity to address these questions by constructing a uniform sample of hot Jupiters for demographic study through new detections and unifying the work of previous ground-based transit surveys. As the first results of an effort to build this large sample of planets, we report here the discovery of 10 new hot Jupiters (TOI-2193A b, TOI-2207b, TOI-2236b, TOI-2421b, TOI-2567b, TOI-2570b, TOI-3331b, TOI-3540A b, TOI-3693b, TOI-4137b). All of the planets were identified as planet candidates based on periodic flux dips observed by TESS, and were subsequently confirmed using ground-based time-series photometry, high-angular-resolution imaging, and high-resolution spectroscopy coordinated with the TESS Follow-up Observing Program. The 10 newly discovered planets orbit relatively bright F and G stars (G < 12.5, Teff between 4800 and 6200 K). The planets' orbital periods range from 2 to 10 days, and their masses range from 0.2 to 2.2 Jupiter masses. TOI-2421b is notable for being a Saturn-mass planet and TOI-2567b for being a "sub-Saturn,"with masses of 0.322 ± 0.073 and 0.195 ± 0.030 Jupiter masses, respectively. We also measured a detectably eccentric orbit (e = 0.17 ± 0.05) for TOI-2207b, a planet on an 8 day orbit, while placing an upper limit of e < 0.052 for TOI-3693b, which has a 9 day orbital period. The 10 planets described here represent an important step toward using TESS to create a large and statistically useful sample of hot Jupiters.

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U2 - 10.3847/1538-3881/ac73ff

DO - 10.3847/1538-3881/ac73ff

M3 - Article

AN - SCOPUS:85135690911

SN - 0004-6256

VL - 164

JO - Astronomical Journal

JF - Astronomical Journal

IS - 2

M1 - 70

ER -

The TESS Grand Unified Hot Jupiter Survey. I. Ten TESS Planets

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