A long-period (P = 61.8 d) M5V dwarf eclipsing a Sun-like star from TESS and NGTS

Gill, Samuel; Cooke, Benjamin F.; Nielsen, L. D.; Lendl, M.; Wheatley, P. J.; Anderson, D. R.; Moyano, Maximiliano; Bryant, Edward M.; Acton, Jack S.; Belardi, Claudia; Bouchy, F.; Burleigh, M. R.; Casewell, Sarah L.; Chaushev, Alexander; Goad, M. R.; Jackman, James A. G.; Jenkins, James S.; McCormac, J.; Günther, Maximilian N.; Osborn, H.; Pollacco, D.; Raynard, Liam; Smith, A. M. S.; Tilbrook, Rossana H.; Turner, O. D.; Udry, S.; Vines, José I.; Watson, C. A.; West, R. G.

doi:10.1093/mnras/staa1248

Cited by 16 publications

(4 citation statements)

References 40 publications

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“…The component stars have masses 1.1 M and 0.23 M and radii 1.0 R and 0.18 R , so the secondary has a radius consistent with that of an inflated giant planet. A very similar result was found for TIC 231005575 by Gill et al [313]: it is a 61.8 d EB with a G-type primary (1.0 M and 1.0 R ) and a low-mass secondary (0.13 M , 0.15 R ) masquerading as a planet.…”

Section: The Connection Between Binaries and Planetssupporting

confidence: 86%

Space-Based Photometry of Binary Stars: From Voyager to TESS

Southworth

2021

Universe

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Binary stars are crucial laboratories for stellar physics, so have been photometric targets for space missions beginning with the very first orbiting telescope (OAO-2) launched in 1968. This review traces the binary stars observed and the scientific results obtained from the early days of ultraviolet missions (OAO-2, Voyager, ANS, IUE), through a period of diversification (Hipparcos, WIRE, MOST, BRITE), to the current era of large planetary transit surveys (CoRoT, Kepler, TESS). In this time observations have been obtained of detached, semi-detached and contact binaries containing dwarfs, sub-giants, giants, supergiants, white dwarfs, planets, neutron stars and accretion discs. Recent missions have found a huge variety of objects such as pulsating stars in eclipsing binaries, multi-eclipsers, heartbeat stars and binaries hosting transiting planets. Particular attention is paid to eclipsing binaries, because they are staggeringly useful, and to the NASA Transiting Exoplanet Survey Satellite (TESS) because its huge sky coverage enables a wide range of scientific investigations with unprecedented ease. These results are placed into context, future missions are discussed, and a list of important science goals is presented.

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Section: The Connection Between Binaries and Planetssupporting

confidence: 86%

Space-Based Photometry of Binary Stars: From Voyager to TESS

Southworth

2021

Universe

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“…Gandolfi et al 2018;Huang et al 2018;Vanderspek et al 2019;Gilbert et al 2020) as well as discoveries of systems for which we observe only a single transit (e.g. Gill et al 2019Gill et al , 2020bLendl et al 2020), including the first monotransiting planet from TESS (Gill et al 2020a). The detection of monotransits is a natural consequence of the limited temporal coverage of TESS when compared to other surveys such as the Wide Angle Search for Planets (WASP; Pollacco et al 2006) or Kepler/K2 (Borucki et al 2010;Howell et al 2014).…”

Section: Introductionmentioning

confidence: 60%

“…These monotransits have been explored via simulations (Cooke et al 2018;Villanueva, Dragomir & Gaudi 2019), which show we can expect a large number of monotransit candidates in the TESS primary mission data. These predictions have been verified by recent monotransit searches including Montalto et al (2020) who find 15 Southern hemisphere candidates and the NGTS monotransit team (see Gill et al 2020aGill et al , 2020b for a description of the pipeline used) who have identified over 50 candidates from the first few TESS sectors alone. Many of these candidates exhibit additional extended mission transit events as discussed later in this paper.…”

Section: Introductionmentioning

confidence: 64%

Resolving period aliases for TESS monotransits recovered during the extended mission

Cooke

Pollacco

Anderson

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We set out to explore how best to mitigate the number of period aliases for a transiting TESS system with two identified transits separated by a large time period on the order of years. We simulate a realistic population of doubly transiting planets based on the observing strategy of the TESS primary and extended missions. We next simulate additional observations using photometry (NGTS) and spectroscopy (HARPS and CORALIE) and assess its impact on the period aliases of systems with two TESS transits. We find that TESS will detect around 400 exoplanets that exhibit one transit in each of the primary and extended missions. Based on the temporal coverage, each of these systems will have an average of 38 period aliases. We find that, assuming a combination of NGTS and CORALIE over observing campaigns spanning 50 days, we can find the true alias, and thus solve the period, for up to 207 of these systems with even more being solved if the observing campaigns are extended or we upgrade to HARPS over CORALIE.

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“…JWST (Beichman et al 2014). Archival searches and carefully-planned photometric monitoring programs from the ground (Cooke et al 2018;Kovacs 2019;Dholakia et al 2020;Yao et al 2019Yao et al , 2021 and in space (Cooke et al 2019(Cooke et al , 2020 and groundbased radial-velocity (RV) work (e.g., Hébrard et al 2019;Gill et al 2020;Dalba et al 2020Dalba et al , 2021aDalba et al ,b, 2022Ulmer-Moll et al 2022) are typically the channels used for the purpose. However, space-based high-precision astrometry with the Gaia mission (Gaia Collaboration et al 2016Collaboration et al , 2022b) also bears the potential for important contributions to this task.…”

Section: Introductionmentioning

confidence: 99%

On the follow-up efforts of long-period transiting planet candidates detected with Gaia astrometry

Sozzetti¹,

P.²,

Lattanzi³

et al. 2023

Preprint

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The class of transiting cold Jupiters, orbiting at 0.5−1.0 au, is to-date underpopulated. Probing their atmospheric composition and physical characteristics is particularly valuable, as it allows for direct comparisons with the Solar System giant planets. We investigate some aspects of the synergy between Gaia astrometry and other ground-based and space-borne programs for detection and characterization of such companions. We carry out numerical simulations of Gaia observations of systems with one cold transiting gas giant, using Jovian planets around a sample of nearby low-mass stars as proxies. Using state-of-the-art orbit fitting tools, we gauge the potential of Gaia astrometry to predict the time of transit centre 𝑇 𝑐 for the purpose of follow-up observations to verify that the companions are indeed transiting. Typical uncertainties on 𝑇 𝑐 will be on the order of a few months, reduced to several weeks for high astrometric signal-to-noise ratios and periods shorter than ∼ 3 yr. We develop a framework for the combined analysis of Gaia astrometry and radial-velocity data from representative ground-based campaigns and show that combined orbital fits would allow to significantly reduce the transit windows to be searched for, down to about ±2 weeks (2 − 𝜎 level) in the most favourable cases. These results are achievable with a moderate investment of observing time (∼ 0.5 nights per candidate, ∼ 50 nights for the top 100 candidates), reinforcing the notion that Gaia astrometric detections of potentially transiting cold giant planets, starting with Data Release 4, will constitute a valuable sample worthy of synergistic follow-up efforts with a variety of techniques.

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A long-period (P = 61.8 d) M5V dwarf eclipsing a Sun-like star from TESS and NGTS

Cited by 16 publications

References 40 publications

Space-Based Photometry of Binary Stars: From Voyager to TESS

Space-Based Photometry of Binary Stars: From Voyager to TESS

Resolving period aliases for TESS monotransits recovered during the extended mission

On the follow-up efforts of long-period transiting planet candidates detected with Gaia astrometry

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