6 research outputs found
An ultra-short-period transiting super-Earth orbiting the M3 dwarf TOI-1685
Funding: We acknowledge financial support from the Agencia Estatal de InvestigaciĂłn of the Ministerio de Ciencia, InnovaciĂłn y Universidades and the ERDF through projects PID2019-109522GB-C5[1:4]/AEI/10.13039/501100011033, PGC2018-098153-B-C33, and the Centre of Excellence âSevero Ochoaâ and âMarĂa deMaeztuâ awards to the Instituto de AstrofĂsica de Canarias (SEV-2015-0548), Instituto de AstrofĂsica de AndalucĂa (SEV-2017-0709), and Centro de Astro-biologĂa (MDM-2017-0737), the Generalitat de Catalunya/CERCA programme,âla Caixaâ Foundation (100010434), European Unionâs Horizon 2020 research and innovation programme under the Marie SkĆodowska-Curie grant agreement No. 847648 (LCF/BQ/PI20/11760023), a University Research Support Grant from the National Astronomical Observatory of Japan, JSPS KAKENHI (JP15H02063, JP18H01265, JP18H05439, JP18H05442, and JP22000005), JSTPRESTO (JPMJPR1775), UK Science and Technology Facilities Council (ST/R000824/1), and NASA (NNX17AG24G).Dynamical histories of planetary systems, as well as the atmospheric evolution of highly irradiated planets, can be studied by characterizing the ultra-short-period planet population, which the TESS mission is particularly well suited to discover. Here, we report on the follow-up of a transit signal detected in the TESS sector 19 photometric time series of the M3.0 V star TOI-1685 (2MASS J04342248+4302148). We confirm the planetary nature of the transit signal, which has a period of Pb = 0.6691403â0.0000021+0.0000023 d, using precise radial velocity measurements taken with the CARMENES spectrograph. From the joint photometry and radial velocity analysis, we estimate the following parameters for TOI-1685 b: a mass of Mb = 3.78â0.63+0.63 Mâ, a radius of Rb = 1.70â0.07+0.07 Râ, which together result in a bulk density of Ïb = 4.21â0.82+0.95 g cmâ3, and an equilibrium temperature of Teq = 1069â16+16 K. TOI-1685 b is the least dense ultra-short-period planet around an M dwarf known to date. TOI-1685 b is also one of the hottest transiting super-Earth planets with accurate dynamical mass measurements, which makes it a particularly attractive target for thermal emission spectroscopy. Additionally, we report with moderate evidence an additional non-transiting planet candidate in the system, TOI-1685 [c], which has an orbital period of Pc = 9.02â0.12+0.10 d.Publisher PDFPeer reviewe
An ultra-short-period transiting super-Earth orbiting the M3 dwarf TOI-1685
Dynamical histories of planetary systems, as well as the atmospheric evolution of highly irradiated planets, can be studied by characterizing the ultra-short-period planet population, which the TESS mission is particularly well suited to discover. Here, we report on the follow-up of a transit signal detected in the TESS sector 19 photometric time series of the M3.0 V star TOI-1685 (2MASS J04342248+4302148). We confirm the planetary nature of the transit signal, which has a period of P_(b) = 0.6691403^(+0.0000023)_(â0.0000021) d, using precise radial velocity measurements taken with the CARMENES spectrograph. From the joint photometry and radial velocity analysis, we estimate the following parameters for TOI-1685 b: a mass of M_(b) = 3.78^(+0.63)_(â0.63) Mê©, a radius of R_(b) = 1.70^(+0.07)_(â0.07) Rê©, which together result in a bulk density of Ï_(b) = 4.21^(+0.95)_(â0.82) g cm^(â3) , and an equilibrium temperature of T_(eq) = 1069^(+16)_(â16) K. TOI-1685 b is the least dense ultra-short-period planet around an M dwarf known to date. TOI-1685 b is also one of the hottest transiting super-Earth planets with accurate dynamical mass measurements, which makes it a particularly attractive target for thermal emission spectroscopy. Additionally, we report with moderate evidence an additional non-transiting planet candidate in the system, TOI-1685 [c], which has an orbital period of P_(c) = 9.02^(+0.10)_(â0.12) d
An ultra-short-period transiting super-Earth orbiting the M3 dwarf TOI-1685
Dynamical histories of planetary systems, as well as the atmospheric evolution of highly irradiated planets, can be studied by characterizing the ultra-short-period planet population, which the TESS mission is particularly well suited to discover. Here, we report on the follow-up of a transit signal detected in the TESS sector 19 photometric time series of the M3.0 V star TOI-1685 (2MASS J04342248+4302148). We confirm the planetary nature of the transit signal, which has a period of Pb = 0.6691403â0.0000021+0.0000023 d, using precise radial velocity measurements taken with the CARMENES spectrograph. From the joint photometry and radial velocity analysis, we estimate the following parameters for TOI-1685 b: a mass of Mb = 3.78â0.63+0.63 Mâ, a radius of Rb = 1.70â0.07+0.07 Râ, which together result in a bulk density of Ïb = 4.21â0.82+0.95 g cmâ3, and an equilibrium temperature of Teq = 1069â16+16 K. TOI-1685 b is the least dense ultra-short-period planet around an M dwarf known to date. TOI-1685 b is also one of the hottest transiting super-Earth planets with accurate dynamical mass measurements, which makes it a particularly attractive target for thermal emission spectroscopy. Additionally, we report with moderate evidence an additional non-transiting planet candidate in the system, TOI-1685 [c], which has an orbital period of Pc = 9.02â0.12+0.10 d.</jats:p
An ultra-short-period transiting super-Earth orbiting the M3 dwarf TOI-1685
Full list of authors: Bluhm, P.; PallĂ©, E.; Molaverdikhani, K.; Kemmer, J.; Hatzes, A. P.; Kossakowski, D.; Stock, S.; Caballero, J. A.; Lillo-Box, J.; BĂ©jar, V. J. S.; Soto, M. G.; Amado, P. J.; Brown, P.; Cadieux, C.; Cloutier, R.; Collins, K. A.; Collins, K. I.; CortĂ©s-Contreras, M.; Doyon, R.; Dreizler, S.; Espinoza, N.; Fukui, A.; GonzĂĄlez-Ălvarez, E.; Henning, Th.; Horne, K.; Jeffers, S. V.; Jenkins, J. M.; Jensen, E. L. N.; Kaminski, A.; Kielkopf, J. F.; Kusakabe, N.; KĂŒrster, M.; LafreniĂšre, D.; Luque, R.; Murgas, F.; Montes, D.; Morales, J. C.; Narita, N.; Passegger, V. M.; Quirrenbach, A.; Schöfer, P.; Reffert, S.; Reiners, A.; Ribas, I.; Ricker, G. R.; Seager, S.; Schweitzer, A.; Schwarz, R. P.; Tamura, M.; Trifonov, T.; Vanderspek, R.; Winn, J.; Zechmeister, M.; Zapatero Osorio, M. R.Dynamical histories of planetary systems, as well as the atmospheric evolution of highly irradiated planets, can be studied by characterizing the ultra-short-period planet population, which the TESS mission is particularly well suited to discover. Here, we report on the follow-up of a transit signal detected in the TESS sector 19 photometric time series of the M3.0 V star TOI-1685 (2MASS J04342248+4302148). We confirm the planetary nature of the transit signal, which has a period of Pb = 0.6691403-0.0000021+0.0000023 d, using precise radial velocity measurements taken with the CARMENES spectrograph. From the joint photometry and radial velocity analysis, we estimate the following parameters for TOI-1685 b: a mass of Mb = 3.78-0.63+0.63 M? , a radius of Rb = 1.70-0.07+0.07 R? , which together result in a bulk density of Ïb = 4.21-0.82+0.95 g cm-3, and an equilibrium temperature of Teq = 1069-16+16 K. TOI-1685 b is the least dense ultra-short-period planet around an M dwarf known to date. TOI-1685 b is also one of the hottest transiting super-Earth planets with accurate dynamical mass measurements, which makes it a particularly attractive target for thermal emission spectroscopy. Additionally, we report with moderate evidence an additional non-transiting planet candidate in the system, TOI-1685 [c], which has an orbital period of Pc = 9.02-0.12+0.10 d. © ESO 2021.CARMENES is an instrument at the Centro AstronĂłmico Hispano-AlemĂĄn (CAHA) at Calar Alto (AlmerĂa, Spain), operated jointly by the Junta de AndalucĂa and the Instituto de AstrofĂsica de AndalucĂa (CSIC). CARMENES was funded by the Max-Planck-Gesellschaft (MPG), the Consejo Superior de Investigaciones CientĂficas (CSIC), the Ministerio de EconomĂa y Competitividad (MINECO) and the European Regional Development Fund (ERDF) through projects FICTS-2011-02, ICTS-2017-07-CAHA-4,
and CAHA16-CE-3978, and the members of the CARMENES Consortium (Max-Planck-Institut fĂŒr Astronomie, Instituto de AstrofĂsica de AndalucĂa, Landessternwarte Königstuhl, Institut de CiĂšncies de lâEspai, Institut fĂŒr Astrophysik Göttingen, Universidad Complutense de Madrid, ThĂŒringer Landessternwarte Tautenburg, Instituto de AstrofĂsica de Canarias, Hamburger Sternwarte, Cen tro de AstrobiologĂa and Centro AstronĂłmico Hispano-AlemĂĄn), with additional contributions by the MINECO, the Deutsche Forschungsgemeinschaft through the Major Research Instrumentation Programme and Research Unit FOR2544 âBlue Planets around Red Starsâ, the Klaus Tschira Stiftung, the states of Baden-WĂŒrttemberg and Niedersachsen, and by the Junta de AndalucĂa. We acknowledge financial support from the Agencia Estatal de InvestigaciĂłn of the Ministerio de Ciencia, InnovaciĂłn y Universidades and the ERDF through projects PID2019-109522GB- C5[1:4]/AEI/10.13039/501100011033, PGC2018-098153-B-C33, and the Centre of Excellence âSevero Ochoaâ and âMarĂa de Maeztuâ awards to the Instituto de AstrofĂsica de Canarias (SEV-2015-0548), Instituto de AstrofĂsica de AndalucĂa (SEV-2017-0709), and Centro de Astro biologĂa (MDM-2017-0737), the Generalitat de Catalunya/CERCA programme,âla Caixaâ Foundation (100010434), European Unionâs Horizon 2020 research and innovation programme under the Marie SkĆodowska-Curie grant agree ment No. 847 648 (LCF/BQ/PI20/11760023), a University Research Support Grant from the National Astronomical Observatory of Japan, JSPS KAKENHI
(JP15H02063, JP18H01265, JP18H05439, JP18H05442, and JP22000005), JST
PRESTO (JPMJPR1775), UK Science and Technology Facilities Council (ST/R000824/1), and NASA (NNX17AG24G) This article is based on obser vations made with the MuSCAT2 instrument, developed by ABC, at Telescopio Carlos SĂĄnchez operated on the island of Tenerife by the IAC in the Spanish Observatorio del Teide, with the Observatoire du Mont-MĂ©gantic, financed by UniversitĂ© de MontrĂ©al, UniversitĂ© Laval, the National Sciences and Engineer ing Council of Canada, the Fonds quĂ©bĂ©cois de la recherche sur la Nature et les technologies, and the Canada Economic Development program, and with the LCOGT network. LCOGT telescope time was granted by NOIRLab through the Mid-Scale Innovations Program , which is funded by NSF. Funding for the TESS mission is provided by NASAâs 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. This research has made use of the Exoplanet Follow-up Observation Program website, which is operated by the California Institute of Technology, under contract with the National Aeronau tics and Space Administration under the Exoplanet Exploration Program. This
research also made use of AstroImageJ, and TAPIR, and the SIMBAD database,
operated at CDS, Strasbourg, France.Peer reviewe
An ultra-short-period transiting super-Earth orbiting the M3 dwarf TOI-1685
Dynamical histories of planetary systems, as well as the atmospheric evolution of highly irradiated planets, can be studied by characterizing the ultra-short-period planet population, which the TESS mission is particularly well suited to discover. Here, we report on the follow-up of a transit signal detected in the TESS sector 19 photometric time series of the M3.0 V star TOI-1685 (2MASS J04342248+4302148). We confirm the planetary nature of the transit signal, which has a period of Pb = 0.6691403â0.0000021+0.0000023 d, using precise radial velocity measurements taken with the CARMENES spectrograph. From the joint photometry and radial velocity analysis, we estimate the following parameters for TOI-1685 b: a mass of Mb = 3.78â0.63+0.63 Mâ, a radius of Rb = 1.70â0.07+0.07 Râ, which together result in a bulk density of Ïb = 4.21â0.82+0.95 g cmâ3, and an equilibrium temperature of Teq = 1069â16+16 K. TOI-1685 b is the least dense ultra-short-period planet around an M dwarf known to date. TOI-1685 b is also one of the hottest transiting super-Earth planets with accurate dynamical mass measurements, which makes it a particularly attractive target for thermal emission spectroscopy. Additionally, we report with moderate evidence an additional non-transiting planet candidate in the system, TOI-1685 [c], which has an orbital period of Pc = 9.02â0.12+0.10 d.</jats:p