HATS-4b: A DENSE HOT JUPITER TRANSITING A SUPER METAL-RICH G STAR

Jordán, Andrés; Brahm, R.; Bakos, G. Á.; Bayliss, Daniel; Penev, K.; Hartman, J. D.; Zhou, G.; Mancini, L.; Mohler-Fischer, M.; Ciceri, S.; Sato, Bun’ei; Csubry, Z.; Rabus, M.; Suc, V.; Espinoza, N.; Bhatti, W.; Val-Borro, M. de; Buchhave, Lars A.; Csák, B.; Henning, Th.; Schmidt, B. P.; Tan, T. G.; Noyes, R. W.; Béky, B.; Butler, R. Paul; Shectman, Stephen; Crane, Jeffrey D.; Thompson, I. B.; Williams, A.; Martín, Roland; Contreras, Carlos; Lázár, J.; Papp, I.; Sári, P.

doi:10.1088/0004-6256/148/2/29

Cited by 93 publications

(61 citation statements)

References 48 publications

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“…The radial velocities were computed from the optical echelle spectra using the cross-correlation technique against a binary mask representative of a G2-type star. The uncertainties in radial velocity were computed using scaling relations (for more detail see Jordán et al 2014) with the signal-to-noise ratio and width of the cross-correlation peak, which were calibrated with Monte Carlo simulations. The observing dates and the obtained radial velocities are shown in Table 1.…”

Section: The Radial Velocity Curve Of Tyc 7218mentioning

confidence: 99%

The White Dwarf Binary Pathways Survey −III. Contamination from hierarchical triples containing a white dwarf

Lagos

Schreiber

Parsons

et al. 2020

Monthly Notices of the Royal Astronomical Society

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The White Dwarf Binary Pathways Survey aims at increasing the number of known detached A, F, G and K main sequence stars in close orbits with white dwarf companions (WD+AFGK binaries) to refine our understanding about compact binary evolution and the nature of Supernova Ia progenitors. These close WD+AFGK binary stars are expected to form through common envelope evolution, in which tidal forces tend to circularize the orbit. However, some of the identified WD+AFGK binary candidates show eccentric orbits, indicating that these systems are either formed through a different mechanism or perhaps they are not close WD+AFGK binaries. We observed one of these eccentric WD+AFGK binaries with SPHERE and find that the system TYC 7218-934-1 is in fact a triple system where the WD is a distant companion. The inner binary likely consists of the G-type star plus an unseen low mass companion in an eccentric orbit. Based on this finding, we estimate the fraction of triple systems that could contaminate the WD+AFGK sample. We find that less than 15 per cent of our targets with orbital periods shorter than 100 days might be hierarchical triples.

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Section: The Radial Velocity Curve Of Tyc 7218mentioning

confidence: 99%

The White Dwarf Binary Pathways Survey −III. Contamination from hierarchical triples containing a white dwarf

Lagos

Schreiber

Parsons

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…) that is capable of processing data in a homogeneous and optimal way coming from different echelle spectrographs. A description of a similar pipeline developed for the Coralie spectrograph can be found in Jordán et al (2014). This FEROS pipeline is able to achieve a long-term RV precision of 5 m/s in the high S/N limit.…”

Section: New Observationsmentioning

confidence: 99%

Search for associations containing young stars (SACY)

Elliott

Bayo

Melo

et al. 2016

A&A

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Context. The young associations offer us one of the best opportunities to study the properties of young stellar and substellar objects and to directly image planets thanks to their proximity (<200 pc) and age (≈5−150 Myr). However, many previous works have been limited to identifying the brighter, more active members (≈1 M ) owing to photometric survey sensitivities limiting the detections of lower mass objects. Aims. We search the field of view of 542 previously identified members of the young associations to identify wide or extremely wide (1000−100 000 au in physical separation) companions. Methods. We combined 2MASS near-infrared photometry (J, H, K) with proper motion values (from UCAC4, PPMXL, NOMAD) to identify companions in the field of view of known members. We collated further photometry and spectroscopy from the literature and conducted our own high-resolution spectroscopic observations for a subsample of candidate members. This complementary information allowed us to assess the efficiency of our method. Results. We identified 84 targets (45: 0.2−1.3 M , 17: 0.08−0.2 M , 22: <0.08 M ) in our analysis, ten of which have been identified from spectroscopic analysis in previous young association works. For 33 of these 84, we were able to further assess their membership using a variety of properties (X-ray emission, UV excess, H α , lithium and K I equivalent widths, radial velocities, and CaH indices). We derive a success rate of 76-88% for this technique based on the consistency of these properties. Conclusions. Once confirmed, the targets identified in this work would significantly improve our knowledge of the lower mass end of the young associations. Additionally, these targets would make an ideal new sample for the identification and study of planets around nearby young stars. Given the predicted substellar mass of the majority of these new candidate members and their proximity, high-contrast imaging techniques would facilitate the search for new low-mass planets.

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“…This is due to the overlap between the pointing of the cameras on a single mount and between the different pointing positions we use to tile the sky into target fields. As a matter of fact, some stars have multiple light curves from different cameras and pointing positions (e.g., HATS-4: Jordán et al 2014). Based on these observations, we have so far identified 1883 candidate transiting planets of which 1120 have undergone follow-up observations.…”

Section: The Hatsouth Surveymentioning

confidence: 99%

HATS-50b through HATS-53b: Four Transiting Hot Jupiters Orbiting G-type Stars Discovered by the HATSouth Survey*

Henning

Mancini

Sarkis

et al. 2018

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We report the discovery of four close-in transiting exoplanets (HATS-50b through HATS-53b), discovered using the HATSouth three-continent network of homogeneous and automated telescopes. These new exoplanets belong to the class of hot Jupiters and orbit G-type dwarf stars, with brightness in the range V=12.5-14.0 mag. While HATS-53 has many physical characteristics similar to the Sun, the other three stars appear to be metal-rich  0.595 0.089 M J ,  1.340 0.056 R J ) and similar orbital periods (3.8297 days, 3.3489 days, 3.8538 days, respectively). Instead, HATS-52b is more dense (mass  2.24 0.15 M J and radius  1.382 0.086 R J ) and has a shorter orbital period (1.3667 days). It also receives an intensive radiation from its parent star and, consequently, presents a high equilibrium temperature ( =  T 1834 73 eq K). HATS-50 shows a marginal additional transit feature consistent with an ultra-short-period hot super Neptune (upper mass limit 0.16 M J ), which will be able to be confirmed with TESS photometry.

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HATS-4b: A DENSE HOT JUPITER TRANSITING A SUPER METAL-RICH G STAR

Cited by 93 publications

References 48 publications

The White Dwarf Binary Pathways Survey −III. Contamination from hierarchical triples containing a white dwarf

The White Dwarf Binary Pathways Survey −III. Contamination from hierarchical triples containing a white dwarf

Search for associations containing young stars (SACY)

HATS-50b through HATS-53b: Four Transiting Hot Jupiters Orbiting G-type Stars Discovered by the HATSouth Survey*

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