10 research outputs found
Periodic Virtual Cell Manufacturing (P-VCM) - Concept, Design and Operation
No full textThis paper presents and discusses the concept of Periodic Virtual Cell Manufacturing (P-VCM). After giving an illustrative example of the operation and design complexity of a P-VCM system, we present an industrial case to study the applicability of the concept. The illustrative example and the industrial case indicate the context for which P-VCM is appropriate
Periodic Virtual Cell Manufacturing (P-VCM) - Concept, Design and Operation
No full textThis paper presents and discusses the concept of Periodic Virtual Cell Manufacturing (P-VCM). After giving an illustrative example of the operation and design complexity of a P-VCM system, we present an industrial case to study the applicability of the concept. The illustrative example and the industrial case indicate the context for which P-VCM is appropriate.</p
TOI-1259Ab - A Gas Giant Planet with 2.7 Per Cent Deep Transits and a Bound white Dwarf Companion
No full textWe present TOI-1259Ab, a 1.0RJup gas giant planet transiting a 0.71R⊙ K-dwarf on a 3.48 d orbit. The system also contains a bound white dwarf companion TOI-1259B with a projected distance of ∼1600 au from the planet host. Transits are observed in nine TESS sectors and are 2.7 per cent deep - among the deepest known - making TOI-1259Ab a promising target for atmospheric characterization. Our follow-up radial velocity measurements indicate a variability of semiamplitude , implying a planet mass of 0.44MJup. By fitting the spectral energy distribution of the white dwarf, we derive a total age of Gyr for the system. The K dwarf's light curve reveals rotational variability with a period of 28 d, which implies a gyrochronology age broadly consistent with the white dwarf's total age. © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.Fellow of the Swiss National Science Foundation
A Possible Alignment Between the Orbits of Planetary Systems and their Visual Binary Companions
No full textFull list of authors: Christian, Sam; Vanderburg, Andrew; Becker, Juliette; Yahalomi, Daniel A.; Pearce, Logan; Zhou, George ; Collins, Karen A.; Kraus, Adam L.; Stassun, Keivan G.; de Beurs, Zoe; Ricker, George R.; Vanderspek, Roland K.; Latham, David W.; Winn, Joshua N.; Seager, S.; Jenkins, Jon M.; Abe, Lyu; Agabi, Karim; Amado, Pedro J.; Baker, David; Barkaoui, Khalid; Benkhaldoun, Zouhair; Benni, Paul; Berberian, John; Berlind, Perry; Bieryla, Allyson; Esparza-Borges, Emma; Bowen, Michael; Brown, Peyton; Buchhave, Lars A.; Burke, Christopher J.; Buttu, Marco; Cadieux, Charles; Caldwell, Douglas A.; Charbonneau, David; Chazov, Nikita; Chimaladinne, Sudhish; Collins, Kevin I.; Combs, Deven; Conti, Dennis M.; Crouzet, Nicolas; de Leon, Jerome P.; Deljookorani, Shila; Diamond, Brendan; Doyon, René; Dragomir, Diana; Dransfield, Georgina; Essack, Zahra; Evans, Phil; Fukui, Akihiko; Gan, Tianjun; Esquerdo, Gilbert A.; Gillon, Michaël; Girardin, Eric; Guerra, Pere; Guillot, Tristan; K. Habich, Eleanor Kate; Henriksen, Andreea; Hoch, Nora; Isogai, Keisuke I.; Jehin, Emmanuël; Jensen, Eric L. N.; Johnson, Marshall C.; Livingston, John H.; Kielkopf, John F.; Kim, Kingsley; Kawauchi, Kiyoe; Krushinsky, Vadim; Kunzle, Veronica; Laloum, Didier; Leger, Dominic; Lewin, Pablo; Mallia, Franco; Massey, Bob; Mori, Mayuko; McLeod, Kim K.; Mékarnia, Djamel; Mireles, Ismael; Mishevskiy, Nikolay; Tamura, Motohide; Murgas, Felipe; Narita, Norio; Naves, Ramon; Nelson, Peter; Osborn, Hugh P.; Palle, Enric; Parviainen, Hannu; Plavchan, Peter; Pozuelos, Francisco J.; Rabus, Markus; Relles, Howard M.; Rodríguez López, Cristina; Quinn, Samuel N.; Schmider, Francois-Xavier; Schlieder, Joshua E.; Schwarz, Richard P.; Shporer, Avi; Sibbald, Laurie; Srdoc, Gregor; Stibbards, Caitlin; Stickler, Hannah; Suarez, Olga; Stockdale, Chris; Tan, Thiam-Guan; Terada, Yuka; Triaud, Amaury; Tronsgaard, Rene; Waalkes, William C.; Wang, Gavin; Watanabe, Noriharu; Wenceslas, Marie-Sainte; Wingham, Geof; Wittrock, Justin; Ziegler, Carl.--This is an Open Access article distributed under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted reuse, distribution, and reproduction in any medium, provided the original work is properly cited.Astronomers do not have a complete picture of the effects of wide-binary companions (semimajor axes greater than 100 au) on the formation and evolution of exoplanets. We investigate these effects using new data from Gaia Early Data Release 3 and the Transiting Exoplanet Survey Satellite mission to characterize wide-binary systems with transiting exoplanets. We identify a sample of 67 systems of transiting exoplanet candidates (with well-determined, edge-on orbital inclinations) that reside in wide visual binary systems. We derive limits on orbital parameters for the wide-binary systems and measure the minimum difference in orbital inclination between the binary and planet orbits. We determine that there is statistically significant difference in the inclination distribution of wide-binary systems with transiting planets compared to a control sample, with the probability that the two distributions are the same being 0.0037. This implies that there is an overabundance of planets in binary systems whose orbits are aligned with those of the binary. The overabundance of aligned systems appears to primarily have semimajor axes less than 700 au. We investigate some effects that could cause the alignment and conclude that a torque caused by a misaligned binary companion on the protoplanetary disk is the most promising explanation. © 2022. The Author(s). Published by the American Astronomical Society.The IRSF project is a collaboration between Nagoya University and the South African Astronomical Observatory (SAAO) supported by the Grants-in-Aid for Scientific Research on Priority Areas (A) (grant Nos. 10147207 and 10147214) and Optical & Near-Infrared Astronomy Inter-University Cooperation Program, from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan and the National Research Foundation (NRF) of South Africa. This work is partly supported by JSPS KAKENHI grant No. JP18H05439, and JST PRESTO grant No. JPMJPR1775, and a University Research Support Grant from the National Astronomical Observatory of Japan (NAOJ). This work is partly supported by Grant-in-Aid for JSPS Fellows, grant No. JP20J21872. This work is partly supported by JSPS KAKENHI grant No. JP17H04574.
This work is partly supported by JSPS KAKENHI grant No. JP20K14518, and by Astrobiology Center SATELLITE Research project AB022006. M.T. is supported by MEXT/JSPS KAKENHI grant Nos. 18H05442, 15H02063, and 22000005. This work is partly supported by JSPS KAKENHI grant No. JP21K13955. This work is partly supported by JSPS KAKENHI grant No. 20K14521. C.R.-L. acknowledges financial support from the State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709). M.R. acknowledges support from the Universidad Católica de lo Santísima Concepción grant DI-FIAI 03/2021. P.J.A. acknowledges support from grant AYA2016-79425-C3-3-P of the Spanish Ministry of Economy and Competitiveness (MINECO) and the Centre of Excellence "Severo Ochoa" award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709). This paper is based on observations made with the T150 telescope at the Sierra Nevada Observatory (Granada, Spain), operated by the Instituto de Astrofísica de Andalucía (IAA—CSIC). The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant FRFC 2.5.594.09.F. TRAPPIST-North is a project funded by the University of Liège (Belgium), in collaboration with Cadi Ayyad University of Marrakech (Morocco). D.D. acknowledges support from the TESS Guest Investigator Program grant No. 80NSSC19K1727 and NASA Exoplanet Research Program grant No. 18-2XRP18_2-0136. M.G. and E.J. are F.R.S.-FNRS Senior Research Associates. K.K.M. acknowledges support from the New York Community Trust's Fund for Astrophysical Research. This work has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation.Peer reviewe
Radial Distribution of the Dust Comae of Comets 45P/Honda–Mrkos–Pajdusáková and 46P/Wirtanen
No full textThere was an unprecedented opportunity to study the inner dust coma environments, where the dust and gas are not entirely decoupled, of comets 45P/Honda–Mrkos–Pajdusáková (45P/HMP) from 2016 December 26 to 2017 March 15, and 46P/Wirtanen from 2018 November 10 to 2019 February 13, both in visible wavelengths. The radial profile slopes of these comets were measured in the R and HB-BC filters most representative of dust, and deviations from a radially expanding coma were identified as significant. The azimuthally averaged radial profile slope of comet 45P/HMP gradually changes from −1.81 ± 0.20 at 5.24 days preperihelion to −0.35 ± 0.16 at 74.41 days postperihelion. Contrastingly, the radial profile slope of 46P/Wirtanen stays fairly constant over the observed time period at −1.05 ± 0.05. Additionally, we find that the radial profile of 46P/Wirtanen is azimuthally dependent on the sky-plane-projected solar position angle, while that of 45P/HMP is not. These results suggest that comets 45P/HMP and 46P/Wirtanen have vastly different coma dust environments and that their dust expansion properties are distinct. As evident from these two comets, well-resolved inner comae are vital for detailed characterization of dust environments. © 2022. The Author(s). Published by the American Astronomical Society.We would like to thank everyone who participated in the data-gathering process. This includes all students from the Lunar and Planetary Laboratory course PTYS 495B/595B (Fall 2018). We would also like to thank the additional organizers of the 4*P Campaign: Matthew Knight (United States Naval Academy) and Tony Farnham (University of Maryland). We would like the thank the Steward Observatory technical staff for the amount of time they dedicated to this project. Finally, we would like to thank the SSO grant No. NNX16A670G (Walt Harris) and the NESSF grant No. 80NSSC18K1241 (Cassandra Lejoly; P.I.: Walt Harris) for allowing this work to be completed. We would also like to thank the Slovak Academy of Sciences grant No. VEGA 2/ 0023/18 (Oleksandra Ivanova) and the Slovak Research and Development Agency under the Contract no. APVV-19-0072 (Oleksandra Ivanova)
Identification of the Top TESS Objects of Interest for Atmospheric Characterization of Transiting Exoplanets with JWST
No full textHord, Benjamin J. et al.--Full list of authors: Hord, Benjamin J.; Kempton, Eliza M-R; Evans-Soma, Thomas M.; Latham, David W.; Ciardi, David R.; Dragomir, Diana; Colon, Knicole D.; Ross, Gabrielle; Vanderburg, Andrew; De Beurs, Zoe L.; Collins, Karen A.; Watkins, Cristilyn N.; Bean, Jacob; Cowan, Nicolas B.; Daylan, Tansu; Ih, Jegug; Morley, Caroline V.; Barkaoui, Khalid; Baker, David; Behmard, Aida; Batalha, Natalie M.; Benkhaldoun, Zouhair; Belinski, Alexander; Bernacki, Krzysztof; Benni, Paul; Binnenfeld, Avraham; Bieryla, Allyson; Bouchy, Franccois; Bosch-Cabot, Pau; Brahm, Rafael; Bozza, Valerio; Chontos, Ashley; Clark, Catherine A.; Buchhave, Lars A.; Calkins, Michael; Collins, Kevin I.; Conti, Dennis M.; Cloutier, Ryan; Cointepas, Marion; de Leon, Jerome P.; Dransfield, Georgina; Crossfield, Ian J. M.; Dai, Fei; Esquerdo, Gilbert; Evans, Phil; Dressing, Courtney; Dustor, Adam; Frasca, Antonio; Fores-Toribio, Raquel; Fiolka, Jerzy; Fajardo-Acosta, Sergio B.; Gan, Tianjun; Furlan, Elise; Fulton, Benjamin; Fukui, Akihiko; Gilbert, Emily A.; Giacalone, Steven; Ghachoui, Mourad; Gandolfi, Davide; Horta, Ferran Grau; Gonzales, Erica; Girardin, Eric; Gillon, Michael; Hellier, Coel; Helm, Ian; Helminiak, Krzysztof G.; Henning, Thomas; Gregorio, Joao; Greklek-McKeon, Michael; Guerra, Pere; Hartman, J. D.; Huber, Daniel; Isopi, Giovanni; Jehin, Emmanuel; Jenkins, Jon M.; Hill, Michelle L.; Horne, Keith; Howard, Andrew W.; Howell, Steve B.; Krushinsky, Vadim; Kielkopf, John F.; Lee, Elena; Lasota, Slawomir; Johnson, Marshall C.; Jensen, Eric L. N.; Kane, Stephen R.; Jordan, Andres; Mann, Christopher R.; Mallia, Franco; Maslennikova, Nataliia; Marino, Giuseppi; Livingston, John H.; Lewin, Pablo; Lund, Michael B.; Lubin, Jack; Michaels, Edward J.; Mocnik, Teo; Mazeh, Tsevi; McLeod, Kim K.; Matthews, Elisabeth; Mayo, Andrew W.; Massey, Bob; Matson, Rachel; Osborn, Hugh; Palle, Enric; Natarajan, Krupa; Nielsen, Louise Dyregaard; Munoz, Jose A.; Narita, Norio; Mori, Mayuko; Mraz, Georgia; Radford, Don J.; Quinn, Samuel N.; Pozuelos, Francisco J.; Popowicz, Adam; Polanski, Alex S.; Plavchan, Peter; Papini, Riccardo; Panahi, Aviad; Schanche, Nicole; Rubenzahl, Ryan A.; Rosenthal, Lee J.; Rodriguez, Joseph E.; Robertson, Paul; Rice, Malena; Relles, Howard M.; Reed, Phillip A.; Timmermans, Mathilde; Tan, Thiam-Guan; Van Zandt, Judah; Ting, Eric B.; Waite, Ian; Vignes, J. P.; Weiss, Lauren M.; Watanabe, Noriharu; Schwarz, Richard P.; Schlieder, Joshua; Shporer, Avi; Sefako, Ramotholo; Srdoc, Gregor; Sozzetti, Alessandro; Tarasenkov, Alexander; Stockdale, Chris; Wittrock, Justin; Zhou, George; Ziegler, Carl; Zucker, ShayJWST has ushered in an era of unprecedented ability to characterize exoplanetary atmospheres. While there are over 5000 confirmed planets, more than 4000 Transiting Exoplanet Survey Satellite (TESS) planet candidates are still unconfirmed and many of the best planets for atmospheric characterization may remain to be identified. We present a sample of TESS planets and planet candidates that we identify as "best-in-class" for transmission and emission spectroscopy with JWST. These targets are sorted into bins across equilibrium temperature Teq and planetary radius Rp and are ranked by a transmission and an emission spectroscopy metric (TSM and ESM, respectively) within each bin. We perform cuts for expected signal size and stellar brightness to remove suboptimal targets for JWST. Of the 194 targets in the resulting sample, 103 are unconfirmed TESS planet candidates, also known as TESS Objects of Interest (TOIs). We perform vetting and statistical validation analyses on these 103 targets to determine which are likely planets and which are likely false positives, incorporating ground-based follow-up from the TESS Follow-up Observation Program to aid the vetting and validation process. We statistically validate 18 TOIs, marginally validate 31 TOIs to varying levels of confidence, deem 29 TOIs likely false positives, and leave the dispositions for four TOIs as inconclusive. Twenty-one of the 103 TOIs were confirmed independently over the course of our analysis. We intend for this work to serve as a community resource and motivate formal confirmation and mass measurements of each validated planet. We encourage more detailed analysis of individual targets by the community. © 2024. The Author(s). Published by the American Astronomical Society.Funding for the TESS mission is provided by NASA's Science Mission Directorate. This research has made use of the Exoplanet Follow-up Observation Program (ExoFOP) website (NExScI 2022), which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST) and produced by the Science Processing Operations Center (SPOC) at NASA Ames Research Center. This research effort made use of systematic error-corrected (PDCSAP) photometry. Funding for the TESS mission is provided by NASA's Science Mission directorate. 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. Some/all of the data presented in this paper were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via 10.17909/rd5r-m387. 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 is based on observations made with the MuSCAT3 instrument, developed by the Astrobiology Center and under financial support by JSPS KAKENHI (grant No. JP18H05439) and JST PRESTO (grant No. JPMJPR1775), at Faulkes Telescope North on Maui, HI, operated by the Las Cumbres Observatory. This paper makes use of observations made with the MuSCAT2 instrument, developed by the Astrobiology Center, at TCS operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. 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 grant Nos. 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. C.M. would like to gratefully acknowledge the entire Dragonfly Telephoto Array team, and Bob Abraham in particular, for allowing their telescope bright time to be put to use observing exoplanets. B.J.H. acknowledges support from the Future Investigators in NASA Earth and Space Science and Technology (FINESST) program (grant No. 80NSSC20K1551) and support by NASA under grant No. 80GSFC21M0002. K.A.C. and C.N.W. acknowledge support from the TESS mission via subaward s3449 from MIT. This research made use of Lightkurve, a Python package for Kepler and TESS data analysis (Lightkurve Collaboration et al. 2018). 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. 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. D.R.C. and C.A.C. acknowledge support from NASA through the XRP grant No. 18-2XRP18_2-0007. C.A.C. acknowledges that this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). This research was carried out in part at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration (80NM0018D0004). S.Z. and A.B. acknowledge support from the Israel Ministry of Science and Technology (grant No. 3-18143). The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant No. PDR T.0120.21. TRAPPIST-North is a project funded by the University of Liege (Belgium), in collaboration with Cadi Ayyad University of Marrakech (Morocco). M.G. is F.R.S.-FNRS Research Director and E.J. is F.R.S.-FNRS Senior Research Associate. The postdoctoral fellowship of K.B. is funded by F.R.S.-FNRS grant No. T.0109.20 and by the Francqui Foundation. H.P.O.'s contribution has been carried out within the framework of the NCCR PlanetS supported by the Swiss National Science Foundation under grant Nos. 51NF40_182901 and 51NF40_205606. F.J.P. acknowledges financial support from the grant No. CEX2021-001131-S funded by MCIN/AEI/ 10.13039/501100011033. A.J. acknowledges support from ANID—Millennium Science Initiative—ICN12_009 and from FONDECYT project 1210718. Z.L.D. acknowledges the MIT Presidential Fellowship and that this material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. 1745302. P.R. acknowledges support from the National Science Foundation grant No. 1952545. Some of the observations in this paper made use of the High-Resolution Imaging instruments 'Alopeke and Zorro, and were obtained under Gemini LLP Proposal Number GN/S-2021A-LP-105. 'Alopeke/Zorro were funded by the NASA Exoplanet Exploration Program and built at the NASA Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. Alopeke/Zorro was mounted on the Gemini North/South 8 m telescopes of the international Gemini Observatory, a program of NSF's NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation, on behalf of the Gemini partnership: the National Science Foundation (United States), National Research Council (Canada), Agencia Nacional de Investigación y Desarrollo (Chile), Ministerio de Ciencia, Tecnología e Innovación (Argentina), Ministério da Ciência, Tecnologia, Inovações e Comunicações (Brazil), and Korea Astronomy and Space Science Institute (Republic of Korea). This work is partly supported by JSPS KAKENHI grant Nos. JP17H04574, JP18H05439, JP21K20376; JST CREST grant No. JPMJCR1761; and Astrobiology Center SATELLITE Research project AB022006. This article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sánchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. This paper is based on observations made with the MuSCAT3 instrument, developed by the Astrobiology Center and under financial supports by JSPS KAKENHI (grant No. JP18H05439) and JST PRESTO (grant No. JPMJPR1775), at Faulkes Telescope North on Maui, HI, operated by the Las Cumbres Observatory. This publication benefits from the support of the French Community of Belgium in the context of the FRIA Doctoral Grant awarded to M.T. D.D. acknowledges support from TESS Guest Investigator Program grant Nos. 80NSSC22K1353, 80NSSC22K0185, and 80NSSC23K0769. A.B. acknowledges the support of M.V. Lomonosov Moscow State University Program of Development. T.D. was supported in part by the McDonnell Center for the Space Sciences. V.K. acknowledges support from the youth scientific laboratory project, topic FEUZ-2020-0038.With funding from the Spanish government through the "Severo Ochoa Centre of Excellence" accreditation (CEX2021-001131-S).Peer reviewe
A Possible Alignment between the Orbits of Planetary Systems and their Visual Binary Companions
No full textAstronomers do not have a complete picture of the effects of wide-binary companions (semimajor axes greater than 100 au) on the formation and evolution of exoplanets. We investigate these effects using new data from Gaia Early Data Release 3 and the Transiting Exoplanet Survey Satellite mission to characterize wide-binary systems with transiting exoplanets. We identify a sample of 67 systems of transiting exoplanet candidates (with well-determined, edge-on orbital inclinations) that reside in wide visual binary systems. We derive limits on orbital parameters for the wide-binary systems and measure the minimum difference in orbital inclination between the binary and planet orbits. We determine that there is statistically significant difference in the inclination distribution of wide-binary systems with transiting planets compared to a control sample, with the probability that the two distributions are the same being 0.0037. This implies that there is an overabundance of planets in binary systems whose orbits are aligned with those of the binary. The overabundance of aligned systems appears to primarily have semimajor axes less than 700 au. We investigate some effects that could cause the alignment and conclude that a torque caused by a misaligned binary companion on the protoplanetary disk is the most promising explanation. © 2022. The Author(s). Published by the American Astronomical Society.AB022006; ANR-15-IDEX-01; 80NSSC19K1727; National Science Foundation, NSF; National Aeronautics and Space Administration, NASA: 18-2XRP18_2-0136; New York Community Trust, NYCT; Australian Research Council, ARC; National Research Foundation, NRF; Japan Society for the Promotion of Science, KAKEN: 15H02063, 18H05442, 20K14521, 22000005, JP17H04574, JP18H05439, JP20J21872, JP20K14518, JP21K13955; Ministry of Education, Culture, Sports, Science and Technology, MEXT; Schweizerischer Nationalfonds zur Förderung der Wissenschaftlichen Forschung, SNF; Fonds De La Recherche Scientifique - FNRS, FNRS: FRFC 2.5.594.09; Ministry of Science, ICT and Future Planning, MSIP; Nagoya University, NU: 10147207, 10147214; Université de Liège, ULg; Universidad Católica de la Santísima Concepción, UCSC: DI-FIAI 03/2021; National Astronomical Observatory of Japan, NAOJ; Precursory Research for Embryonic Science and Technology, PRESTO: JPMJPR1775; Instituto de Astrofísica de Andalucía, IAA: SEV-2017-0709This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). Funding for the TESS mission is provided by NASA’s Science Mission directorate.K.K.M. acknowledges support from the New York Community Trust's Fund for Astrophysical Research.The research leading to these results has received funding from the ARC grant for Concerted Research Actions, financed by the Wallonia-Brussels Federation. TRAPPIST is funded by the Belgian Fund for Scientific Research (Fond National de la Recherche Scientifique, FNRS) under the grant FRFC 2.5.594.09.F. TRAPPIST-North is a project funded by the University of Liège (Belgium), in collaboration with Cadi Ayyad University of Marrakech (Morocco).This work is partly supported by JSPS KAKENHI grant No. JP20K14518, and by Astrobiology Center SATELLITE Research project AB022006.This work is partly supported by JSPS KAKENHI grant No. JP21K13955.This work is partly supported by JSPS KAKENHI grant No. 20K14521.This paper is based on observations made with the MuSCAT3 instrument, developed by the Astrobiology Center and under financial supports by JSPS KAKENHI (JP18H05439) and JST PRESTO (JPMJPR1775), at Faulkes Telescope North on Maui, HI, operated by the Las Cumbres Observatory.The IRSF project is a collaboration between Nagoya University and the South African Astronomical Observatory (SAAO) supported by the Grants-in-Aid for Scientific Research on Priority Areas (A) (grant Nos. 10147207 and 10147214) and Optical & Near-Infrared Astronomy Inter-University Cooperation Program, from the Ministry of Education, Culture, Sports, Science and Technology (MEXT) of Japan and the National Research Foundation (NRF) of South Africa.C.R.-L. acknowledges financial support from the State Agency for Research of the Spanish MCIU through the Center of Excellence Severo Ochoa award for the Instituto de Astrofísica de Andalucía (SEV-2017-0709).M.T. is supported by MEXT/JSPS KAKENHI grant Nos. 18H05442, 15H02063, and 22000005.This work is partly supported by JSPS KAKENHI grant No. JP18H05439, and JST PRESTO grant No. JPMJPR1775, and a University Research Support Grant from the National Astronomical Observatory of Japan (NAOJ).P.J.A. acknowledges support from grant AYA2016-79425-C3-3-P of the Spanish Ministry of Economy and Competitiveness (MINECO) and the Centre of Excellence “Severo Ochoa” award to the Instituto de Astrofísica de Andalucía (SEV-2017-0709)
Another shipment of six short-period giant planets from TESS
No full textWe present the discovery and characterization of six short-period, transiting giant planets from NASA’s Transiting Exoplanet Survey Satellite (TESS) – TOI-1811 (TIC 376524552), TOI-2025 (TIC 394050135), TOI-2145 (TIC 88992642), TOI-2152 (TIC 395393265), TOI-2154 (TIC 428787891), and TOI-2497 (TIC 97568467). All six planets orbit bright host stars (8.9 <G < 11.8, 7.7 <K < 10.1). Using a combination of time-series photometric and spectroscopic follow-up observations from the TESS Follow-up Observing Program Working Group, we have determined that the planets are Jovian-sized (RP = 0.99–1.45 RJ), have masses ranging from 0.92 to 5.26 MJ, and orbit F, G, and K stars (4766 ≤ Teff ≤ 7360 K). We detect a significant orbital eccentricity for the three longest-period systems in our sample: TOI-2025 b (P = 8.872 d, 0.394+0.035-0.038), TOI-2145 b (P = 10.261 d, e = 0.208+0.034-0.047), and TOI-2497 b (P = 10.656 d, e = 0.195+0.043-0.040). TOI-2145 b and TOI-2497 b both orbit subgiant host stars (3.8 < log g <4.0), but these planets show no sign of inflation despite very high levels of irradiation. The lack of inflation may be explained by the high mass of the planets; 5.26+0.38-0.37 MJ (TOI-2145 b) and 4.82 ± 0.41 MJ (TOI-2497 b). These six new discoveries contribute to the larger community effort to use TESS to create a magnitude-complete, self-consistent sample of giant planets with well-determined parameters for future detailed studies. © 2023 The Author(s).80NSSC20K0250; LE140100050; FEUZ-2020-0038, PGC2018-098153-B-C31; National Science Foundation, NSF: 1516242, 1608203, 2007811, AST-1751874, AST-1907790; David and Lucile Packard Foundation, DLPF; National Aeronautics and Space Administration, NASA: GN-2018B-LP-101, NNX13AM97A, XRP 80NSSC22K0233; W. M. Keck Foundation, WMKF; New York Community Trust, NYCT; Research Corporation for Science Advancement, RCSA; Pennsylvania Space Grant Consortium, PSGC; Ames Research Center, ARC; George Mason University, GMU; University of North Carolina, UNC; Massachusetts Institute of Technology, MIT; University of Pennsylvania; Ohio State University, OSU; California Institute of Technology, CIT; University of Florida, UF; Michigan State University, MSU; University of North Carolina at Chapel Hill, UNC-CH; Pennsylvania State University, PSU; University of Montana, UM; University of Texas at Austin, UT; Smithsonian Astrophysical Observatory, SAO; Horizon 2020 Framework Programme, H2020: 1952545, 724427; Mt. Cuba Astronomical Foundation; Accelerated Bridge Construction University Transportation Center, ABC-UTC; National Centres of Competence in Research SwissMAP; Diabetes Patient Advocacy Coalition, DPAC; European Research Council, ERC; European Space Agency, ESA; Australian Research Council, ARC: DP180100972, DP210103119, DP220100365, FL220100117, LE160100001; Deutsche Forschungsgemeinschaft, DFG: HA 3279/12-1, SPP1992; Japan Society for the Promotion of Science, KAKEN: JP18H05439; University of New South Wales, UNSW; University of Southern Queensland, USQ; Fondo Nacional de Desarrollo Científico y Tecnológico, FONDECYT: 11200751, 1210718, 14ENI2-26865, IC120009; Core Research for Evolutional Science and Technology, CREST: JPMJCR1761; Ministry of Education and Science of the Russian Federation, Minobrnauka: 075-15-2020-780, N13.1902.21.0039; Ministério da Ciência, Tecnologia e Inovação, MCTI; University of Toronto, U of T; Université de Genève, UNIGE; Ministry of Economy; Nanjing University, NJU; Instituto de Astrofísica de Canarias, IAC; NCCR Catalysis, NCCRThe authors thank the CHIRON team members, including Todd Henry, Leonardo Paredes, Hodari James, Azmain Nisak, Rodrigo Hinojosa, Roberto Aviles, Wei-Chun Jao, and CTIO staffs, for their work in acquiring RVs with CHIRON at CTIO. This research has made use of SAO/NASA’s Astrophysics Data System Bibliographic Services. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This work has made use of data from the European Space Agency (ESA) mission Gaia ( https://www.cosmos.esa.int/gaia ), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium ). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work makes use of observations from the LCO network. Based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia e Inovações (MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU).Funding for the TESS mission is provided by NASA’s Science Mission directorate. The authors acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the NASA Exoplanet Archive and the Exoplanet Follow-up Observation Program website, which are operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). This paper includes observations obtained under Gemini program GN-2018B-LP-101. 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. This publication makes use of The Data and Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planets data visualisation, exchange and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the Swiss expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch .LC, KS, EA, JR, JER, JAR, PW, and EZ are grateful for support from NSF grants AST-1751874 and AST-1907790, along with a Cottrell Fellowship from the Research Corporation. CZ is supported by a Dunlap Fellowship at the Dunlap Institute for Astronomy & Astrophysics, funded through an endowment established by the Dunlap family and the University of Toronto. T.H. acknowledges support from the European Research Council under the Horizon 2020 Framework Program via the ERC Advanced Grant Origins 83 24 28. JVS acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project Four Aces; grant agreement No. 724427). PR acknowledges support from NSF grant No. 1952545. RB and AJ acknowledges support from FONDECYT Projects 11200751 and 1210718 and from the CORFO project N◦14ENI2-26865. AJ, RB and MH acknowledge support from project IC120009 ‘Millennium Institute of Astrophysics (MAS)’ of the Millenium Science Initiative, Chilean Ministry of Economy. The Pennsylvania State University Eberly College of Science. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. KKM gratefully acknowledges support from the New York Community Trust’s Fund for Astrophysical Research. LG and AG are supported by NASA Massachusetts Space Grant Fellowships. EWG, ME, and PC acknowledge support by Deutsche Forschungsgemeinschaft (DFG) grant HA 3279/12-1 within the DFG Schwerpunkt SPP1992, Exploring the Diversity of Extrasolar Planets. BSG was partially supported by the Thomas Jefferson Chair for Space Exploration at the Ohio State University. CD acknowledges support from the Hellman Fellows Fund and NASA XRP via grant 80NSSC20K0250. BSS, MVG, and AAB acknowledge the support of Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780 (N13.1902.21.0039). BA is supported by Australian Research Council Discovery Grant DP180100972. TRB acknowledges support from the Australian Research Council (DP210103119). TRB acknowledges support from the Australian Research Council (DP210103119 and FL220100117). The authors thank the CHIRON team members, including Todd Henry, Leonardo Paredes, Hodari James, Azmain Nisak, Rodrigo Hinojosa, Roberto Aviles, Wei-Chun Jao, and CTIO staffs, for their work in acquiring RVs with CHIRON at CTIO. This research has made use of SAO/NASA’s Astrophysics Data System Bibliographic Services. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work makes use of observations from the LCO network. Based in part on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia e Inovações (MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). Funding for the TESS mission is provided by NASA’s Science Mission directorate. The authors acknowledge the use of public TESS Alert data from pipelines at the TESS Science Office and at the TESS Science Processing Operations Center. This research has made use of the NASA Exoplanet Archive and the Exoplanet Follow-up Observation Program website, which are operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program. This paper includes data collected by the TESS mission, which are publicly available from the Mikulski Archive for Space Telescopes (MAST). This paper includes observations obtained under Gemini program GN-2018B-LP-101. 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. This publication makes use of The Data and Analysis Center for Exoplanets (DACE), which is a facility based at the University of Geneva (CH) dedicated to extrasolar planets data visualisation, exchange and analysis. DACE is a platform of the Swiss National Centre of Competence in Research (NCCR) PlanetS, federating the Swiss expertise in Exoplanet research. The DACE platform is available at https://dace.unige.ch. MINERVA-Australis is supported by Australian Research Council LIEF Grant LE160100001 (Discovery Grant 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. The authors 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. The authors 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. MINERVA-North is a collaboration among the Harvard-Smithsonian Center for Astrophysics, The Pennsylvania State University, the University of Montana, the University of Southern Queensland, University of Pennsylvania, and George Mason University. It is made possible by generous contributions from its collaborating institutions and Mt. Cuba Astronomical Foundation, The David & Lucile Packard Foundation, National Aeronautics and Space Administration (EPSCOR grant NNX13AM97A, XRP 80NSSC22K0233), the Australian Research Council (LIEF grant LE140100050), and the National Science Foundation (grants 1516242, 1608203, and 2007811). This article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sánchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. This work is partly financed by the Spanish Ministry of Economics and Competitiveness through grants PGC2018-098153-B-C31.The work of VK was supported by the Ministry of science and higher education of the Russian Federation, topic FEUZ-2020-0038. This work is partly supported by JSPS KAKENHI Grant Number JP18H05439, JST CREST Grant Number JPMJCR1761. This article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sánchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide.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. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.This article is based on observations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos Sánchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide. This work is partly financed by the Spanish Ministry of Economics and Competitiveness through grants PGC2018-098153-B-C31.The work of VK was supported by the Ministry of science and higher education of the Russian Federation, topic FEUZ-2020-0038.LC, KS, EA, JR, JER, JAR, PW, and EZ are grateful for support from NSF grants AST-1751874 and AST-1907790, along with a Cottrell Fellowship from the Research Corporation. CZ is supported by a Dunlap Fellowship at the Dunlap Institute for Astronomy & Astrophysics, funded through an endowment established by the Dunlap family and the University of Toronto. T.H. acknowledges support from the European Research Council under the Horizon 2020 Framework Program via the ERC Advanced Grant Origins 83 24 28. JVS acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (project Four Aces; grant agreement No. 724427). PR acknowledges support from NSF grant No. 1952545. RB and AJ acknowledges support from FONDECYT Projects 11200751 and 1210718 and from the CORFO project N°14ENI2-26865. AJ, RB and MH acknowledge support from project IC120009 ‘Millennium Institute of Astrophysics (MAS)’ of the Millenium Science Initiative, Chilean Ministry of Economy. The Pennsylvania State University Eberly College of Science. The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium. KKM gratefully acknowledges support from the New York Community Trust’s Fund for Astrophysical Research. LG and AG are supported by NASA Massachusetts Space Grant Fellowships. EWG, ME, and PC acknowledge support by Deutsche Forschungsgemeinschaft (DFG) grant HA 3279/12-1 within the DFG Schwerpunkt SPP1992, Exploring the Diversity of Extrasolar Planets. BSG was partially supported by the Thomas Jefferson Chair for Space Exploration at the Ohio State University. CD acknowledges support from the Hellman Fellows Fund and NASA XRP via grant 80NSSC20K0250. BSS, MVG, and AAB acknowledge the support of Ministry of Science and Higher Education of the Russian Federation under the grant 075-15-2020-780 (N13.1902.21.0039). BA is supported by Australian Research Council Discovery Grant DP180100972. TRB acknowledges support from the Australian Research Council (DP210103119). TRB acknowledges support from the Australian Research Council (DP210103119 and FL220100117).Minerva -Australis is supported by Australian Research Council LIEF Grant LE160100001 (Discovery Grant 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. The authors 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. The authors 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.MINERVA-North is a collaboration among the Harvard-Smithsonian Center for Astrophysics, The Pennsylvania State University, the University of Montana, the University of Southern Queensland, University of Pennsylvania, and George Mason University. It is made possible by generous contributions from its collaborating institutions and Mt. Cuba Astronomical Foundation, The David & Lucile Packard Foundation, National Aeronautics and Space Administration (EPSCOR grant NNX13AM97A, XRP 80NSSC22K0233), the Australian Research Council (LIEF grant LE140100050), and the National Science Foundation (grants 1516242, 1608203, and 2007811)
