Search for Transiting Exoplanets with HATNet

Bakos, G. Á.; Noyes, R. W.; Kovács, G.; Latham, David W.; Torres, Guillermo; Sasselov, Dimitar; Pál, András; Sipőcz, Brigitta; Kovács, G.

doi:10.1017/s1743921308026197

Cited by 6 publications

(5 citation statements)

References 19 publications

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“…The major observational disadvantage of the system is its period, very close to 4 d, which makes the eclipses not always possible to observe from one place during a single season. Further work on this system requires continuous photometry from a global network of telescopes, such as WET (Nather et al 1990), Solaris (Konacki et al 2012) or HAT-S (Bakos et al 2009), in order to derive some of the crucial parameters, like the radii or temperatures, even more accurately.…”

Section: Discussionmentioning

confidence: 99%

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue

Hełminiak

Brahm

Ratajczak

et al. 2014

A&A

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Aims. We present the results of the combined photometric and spectroscopic analysis of a bright (V = 9.14), close (d = 31 pc), late-type detached eclipsing binary, AK Fornacis. This P = 3.981 d system has not been previously recognised as a double-lined spectroscopic binary, and this is the first full physical model of this unique target. Methods. With the FEROS, CORALIE, and HARPS spectrographs, we collected a number of high-resolution spectra to calculate radial velocities of both components of the binary. Measurements were done with our own disentangling procedure and the TODCOR technique, and were later combined with the photometry from the ASAS and SuperWASP archives. We also performed an atmospheric analysis of the component spectra with the Spectroscopy Made Easy package. Results. Our analysis shows that AK For consists of two active, cool dwarfs having masses of M 1 = 0.6958 ± 0.0010 and M 2 = 0.6355 ± 0.0007 M and radii of R 1 = 0.687 ± 0.020 and R 2 = 0.609 ± 0.016 R , respectively, which are slightly less metal-abundant than the Sun. Parameters of both components are well reproduced by the models. Conclusions. AK For is the brightest system among the known eclipsing binaries with K-or M-type stars. Its orbital period is one of the longest, and its rotational velocities is one of the lowest, which allows us to obtain very precise radial velocity measurements. The precision in physical parameters that we obtained places AK For among the binaries with the best mass measurements in the literature. It also fills the gap in our knowledge of stars in the range of 0.5-0.8 M and between short and long-period systems. All this makes AK For a unique benchmark for understanding the properties of low-mass stars.

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Section: Discussionmentioning

confidence: 99%

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue

Hełminiak

Brahm

Ratajczak

et al. 2014

A&A

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“…The most productive asteroid and NEO search programs are currently the Catalina Sky Survey 4 (Larson et al 2003) Bakos et al 2009) are examples of surveys searching for planetary occultations. Such surveys must work at very high S/N at fast cadence, again at the expense of limiting magnitude, but their science does not lack for stars of suitable brightness.…”

Section: Ongoing and Planned Surveysmentioning

confidence: 99%

An Early Warning System for Asteroid Impact

Tonry

2011

Publications of the Astronomical Society of the Pacific

159

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Earth is bombarded by meteors, occasionally by one large enough to cause a significant explosion and possible loss of life. Although the odds of a deadly asteroid strike in the next century are low, the most likely impact is by a relatively small asteroid, and we suggest that the best mitigation strategy in the near term is simply to move people out of the way. We describe an "early warning" system that could provide a week's notice of most sizable asteroids or comets on track to hit the Earth. This system, dubbed "Asteroid Terrestrial-impact Last Alert System" (ATLAS), comprises two observatories separated by about 100km that simultaneously scan the visible sky twice a night, and can be implemented immediately for relatively low cost. The sensitivity of ATLAS permits detection of 140m asteroids (100 Mton impact energy) three weeks before impact, and 50m asteroids a week before arrival. An ATLAS alarm, augmented by other observations, should result in a determination of impact location and time that is accurate to a few kilometers and a few seconds. In addition to detecting and warning of approaching asteroids, ATLAS will continuously monitor the changing universe around us: most of the variable stars in our galaxy, many micro-lensing events from stellar alignments, luminous stars and novae in nearby galaxies, thousands of supernovae, nearly a million quasars and active galactic nuclei, tens of millions of galaxies, and a billion stars. With two views per day ATLAS will make the variable universe as familiar to us as the sunrise and sunset.Comment: 33 pages, 7 figures, accepted for publication in PASP, Jan 201

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“…To get true masses of the exoplanets via RV measurements (Mayor & Queloz 1995) we need planets transiting in front of bright stars. Interesting, but not surprising is the fact that the vast majority of these systems in the Kepler era was discovered not by the above mentioned Kepler and K2 missions, but by ground-based transit surveys, like HATNet (Bakos et al 2009), SuperWASP (Street et al 2003), or XO (McCullough et al 2005. For our follow-up observations, we selected the transiting exoplanet XO-6b, discovered recently by Crouzet et al (2017) within the framework of the XO project, which started in 2005.…”

Section: Introductionmentioning

confidence: 99%

Periodic transit timing variations and refined system parameters of the exoplanet XO-6b

Garai

Pribulla

Komžík

et al. 2019

Monthly Notices of the Royal Astronomical Society

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Only a few exoplanets are known to orbit around fast rotating stars. One of them is XO-6b, which orbits an F5V-type star. Shortly after the discovery, we started multicolor photometric and radial-velocity follow-up observations of XO-6b, using the telescopes of Astronomical Institute of the Slovak Academy of Sciences. Our main scientific goals were to better characterize the planetary system and to search for transit timing variations. We refined several planetary and orbital parameters. Based on our measurements, the planet XO-6b seems to be about 10% larger, which is, however, only about 2σ difference, but its orbit inclination angle, with respect to the plane of the sky, seems to be significantly smaller, than it was determined originally by the discoverers. In this case we found about 9.5σ difference. Moreover, we observed periodic transit timing variations of XO-6b with a semi-amplitude of about 14 min and with a period of about 450 days. There are two plausible explanations of such transit timing variations: (1) a third object in the system XO-6 causing light-time effect, or (2) resonant perturbations between the transiting planet XO-6b and another unknown low-mass planet in this system. From the O-C diagram we derived that the assumed third object in the system should have a stellar mass, therefore significant variations are expected in the radial-velocity measurements of XO-6. Since this is not the case, and since all attempts to fit radial velocities and O-C data simultaneously failed to provide a consistent solution, more realistic is the second explanation.

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Search for Transiting Exoplanets with HATNet

Cited by 6 publications

References 19 publications

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue

Orbital and physical parameters of eclipsing binaries from the All-Sky Automated Survey catalogue

An Early Warning System for Asteroid Impact

Periodic transit timing variations and refined system parameters of the exoplanet XO-6b

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