The first planet detected in the WTS: an inflated hot Jupiter in a 3.35 d orbit around a late F star

Cappetta, M.; Saglia, R.; Birkby, Jayne; Koppenhoefer, J.; Pinfield, D. J.; Hodgkin, S. T.; Cruz, P.; Kovács, G.; Sipőcz, Brigitta; Barrado, D.; Nefs, B.; Pavlenko, Ya. V.; Fossati, L.; Burgo, C. del; Martín, E. L.; Snellen, I. A. G.; Barnes, John; Bayo, A.; Campbell, David A.; Catalán, S.; Gálvez-Ortiz, M. C.; Goulding, N.; Haswell, C. A.; Ivanyuk, O.; Jones, H. R. A.; Кузнецов, М. К.; Lodieu, N.; Marocco, F.; Mislis, D.; Murgas, F.; Napiwotzki, R.; Πάλλη, Ε.; Pollacco, D.; Sarro, L. M.; Solano, E.; Steele, P. R.; Stoev, H.; Tata, R.; Zendejas, J.

doi:10.1111/j.1365-2966.2012.21937.x

Cited by 44 publications

(11 citation statements)

References 80 publications

(100 reference statements)

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“…Radial velocities are derived by fitting each resulting cross-correlation function (CCF) with a Gaussian (Baranne et al 1996;Pepe et al 2002). For the HRS, the RVs were computed using a series of dedicated routines based on IRAF and cross-correlating the spectra with a G2 star template (Cappetta et al 2012). All the observations for each star were corrected to the zero point of HARPS, as explained in Pasquini et al (2012), and were analyzed together.…”

Section: Radial Velocities and Orbital Solutionsmentioning

confidence: 99%

Three planetary companions around M 67 stars

Brucalassi

Pasquini

Saglia

et al. 2014

A&A

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For the past six years we have carried out a search for massive planets around main sequence and evolved stars in the open cluster M 67, using radial velocity (RV) measurements obtained with HARPS at ESO (La Silla), SOPHIE at OHP and HRS at HET. Additional RV data come from CORALIE at the Euler Swiss Telescope. We aim to perform a long-term study on giant planet formation in open clusters and determine how it depends on stellar mass and chemical composition. We report the detection of three new extrasolar planets: two in orbit around the two G dwarfs YBP1194 and YBP1514, and one around the evolved star S364. The orbital solution for YBP1194 yields a period of 6.9 days, an eccentricity of 0.24, and a minimum mass of 0.34 M Jup . YBP1514 shows periodic RV variations of 5.1 days, a minimum mass of 0.40 M Jup , and an eccentricity of 0.39. The best Keplerian solution for S364 yields a period of 121.7 days, an eccentricity of 0.35 and a minimum mass of 1.54 M Jup . An analysis of Hα core flux measurements as well as of the line bisectors spans revealed no correlation with the RV periods, indicating that the RV variations are best explained by the presence of a planetary companion. Remarkably, YBP1194 is one of the best solar twins identified so far, and YBP1194b is the first planet found around a solar twin that belongs to a stellar cluster. In contrast with early reports and in agreement with recent findings, our results show that massive planets around stars of open clusters are as frequent as those around field stars.

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Section: Radial Velocities and Orbital Solutionsmentioning

confidence: 99%

Three planetary companions around M 67 stars

Brucalassi

Pasquini

Saglia

et al. 2014

A&A

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“…Spectroscopic follow-up includes medium resolution RV (with WHT/ISIS or CAHA/TWIN) and high resolution RV (HET/HDS or Gemini/GNIRS). In the 19 hr field we ruled out all but two planet candidates, they are published and named WTS-1b [6] and WTS-2b [7]. We did not find any planets around M dwarfs.…”

Section: Candidatesmentioning

confidence: 90%

WTS: A near-infrared transit survey

Sipőcz

Kovács

Hodgkin

et al. 2013

EPJ Web of Conferences

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Abstract. The WFCAM Transit Survey is a transiting planet survey running on the United Kingdom Infrared Telescope targeting M dwarf stars in the near infrared. The survey has been operating since 2007 and gathering photometric time series of about 15000 M dwarf stars brighter than J = 17 mag. We identified and followed-up planet candidates from the most complete field and found two hot Jupiters around non-M dwarf hosts (WTS-1b & WTS-2b) but found no planets around the M dwarfs. OBSERVATIONS AND DATA QUALITYThe WFCAM Transit Survey (WTS) is an ongoing campaign survey on the United Kingdom Infrared Telescope (UKIRT) operating in the near-infrared, in J-band since 2007. The WTS targets 4 superfields, two in the winter and two in the summer sky and each covering 1.6 square degrees in size. A field is made up of 8 pawprints with slightly overlapping regions at the edges. The WTS operates as a backup program of the large UKIRT surveys (such as the UKIDSS surveys and UHS). The WTS runs in queue mode using 1 or 0.5 hour long observing blocks resulting 4 or 2 epochs per block respectively. The exposure time is 90 s. Table 1 summarizes main properties of the fields and the current number of epochs. We expect to complete 1 2-3 fields before the closure of UKIRT in 2013.The main science goal to identify planets orbiting around M dwarfs or earlier stars. Other science topics includes but not limited to characterizing of low mass eclipsing binaries; studying M dwarf variability in the J band; identifying high proper motion sources e.g. cool white dwarfs, brown dwarfs, TNOs.Figure 1 summarizes our light curve noise properties in the 19 hr field. The saturation appears at J = 13 mag. We reach 3-4 mmag precision at the bright end and at J = 17 mag where the sky noise dominates we have a precision of 2%. Mainly because of follow-up possibilities, we limit our main science goal of finding planets to stellar sources brighter than J = 17 magnitude, but for other science topics we used fainter sources, too. For reference we show the signal depth for a few star-planet systems.In Figure 2 we present a basic sensitivity diagram, showing the effect of the irregular observing pattern and number of epochs in the different fields. We used a simple simulation of a Neptune sized planet transiting around an M0 star. The simulation provides us an unbiased sample of different transit lengths and timings derived from random geometry of inclination (we allow grazing systems, too). a e-mail: b.sipocz@herts.ac.uk 1 A field is considered complete when it get 1000 or more observed epochs. This is an Open Access article distributed under the terms of the Creative Commons Attribution License 2.0, which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.

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“…The phase values were computed from the epochs of the observations, expressed in Julian date, and using the extremely well determined P and t 0 values obtained from the fit of the J and i light curves. Further details on the analysis of the properties of the WTS1 system can be found in [1].…”

Section: The Wts1 Systemmentioning

confidence: 99%

“…Exoplanet searches often focus on the detection of small Earth-like exoplanets, but understanding the formation mechanism and evolution of the giant planets is a key question in astrophysics. We report on WTS1 b [1], the first planet discovery in the WFCAM Transit Survey (WTS, [3]), an infrared photometric monitoring program operating as back-up program at the UKIRT telescope at Mauna Kea, Hawaii. Since the WTS was primarily designed to find planets transiting M-dwarf stars, the observations are obtained in the J-band (∼1.25 m).…”

Section: Introductionmentioning

confidence: 99%

WTS1 b: The first planet detected in the WFCAM Transit Survey

Cappetta

Saglia

Birkby

et al. 2013

EPJ Web of Conferences

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Abstract. We report the discovery of WTS1 b, the first extrasolar planet found by the WFCAM Transit Survey. For one of the most promising transiting candidates, high-resolution spectra taken at the HobbyEberly Telescope (HET) allowed us to estimate the spectroscopic parameters of the host star, a late-F main sequence dwarf (V = 16.13), and to measure its radial velocity variations. The combined analysis of the light curves and spectroscopic data resulted in an orbital period of the companion of 3.35 days, a planetary mass of 4.01 ± 0.35 M J , and a planetary radius of 1.49 +0.16 −0.18 R J . WTS1 b has one of the largest radius anomalies among the known hot Jupiters in the mass range 3-5 M J .

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The first planet detected in the WTS: an inflated hot Jupiter in a 3.35 d orbit around a late F star

Cited by 44 publications

References 80 publications

Three planetary companions around M 67 stars

Three planetary companions around M 67 stars

WTS: A near-infrared transit survey

WTS1 b: The first planet detected in the WFCAM Transit Survey

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