Transiting Exoplanet Monitoring Project (TEMP). I. Refined System Parameters and Transit Timing Variations of HAT-P-29b

Wang, Y. H.; Wang, S.; Liu, Hui-Gen; Hinse, T. C.; Laughlin, Gregory; Wu, Dong-Hong; Zhang, X.; Zhou, Xu; Wu, Zhenyu; Zhou, Jie; Wittenmyer, R. A.; Eastman, Jason D.; Zhang, H.; Hori, Yasunori; Narita, Norio; Chen, Y.; Ma, Jun; Peng, Xiyan; Zhang, T. M.; Zou, Hu; Nie, Jun; Zhou, Zhiming

doi:10.3847/1538-3881/aadcfc

Cited by 15 publications

(2 citation statements)

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“…While the primary focus of MINERVA-Australis will be the radial velocity follow-up of transiting planet candidates found by TESS, five secondary photometric science goals include: photometric follow-up of TESS and other transit survey planets to ensure that the ephemerides are up-to-date and accurate for future followup observations (e.g., Hoyer et al 2016;Wang et al 2018b), ruling out potential false positives from nearby eclipsing binaries (Collins et al 2018;Ziegler et al 2018), searching for transit timing variations (Malavolta et al 2017;Saad-Olivera et al 2017) and longer-period planets (e.g., Otor et al 2016;Almenara et al 2018) and follow-up of planets found by radial velocity observations from the AAPS (e.g., Tinney et al 2011;Wittenmyer et al 2014). In addition, target-of-opportunity observations of high-priority solar system occultation events (e.g., Sicardy et al 2011a;Ortiz et al 2012Ortiz et al , 2017 are also planned using a very high-cadence camera that will be installed at a future date.…”

Section: First Science Results With Minerva-australismentioning

confidence: 99%

“…4. FIRST SCIENCE RESULTS WITH MINERVA-AUSTRALISWhile the primary focus of MINERVA-Australis will be the radial velocity follow-up of transiting planet candidates found by TESS, five secondary photometric science goals include: photometric follow-up of TESS and other transit survey planets to ensure that the ephemerides are up-to-date and accurate for future follow-up observations (e.g.,Hoyer et al 2016;Wang et al 2018b), ruling out potential false positives from…”

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Minerva-Australis. I. Design, Commissioning, and First Photometric Results

Addison

Wright

Wittenmyer

et al. 2019

PASP

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The MINERVA-Australis telescope array is a facility dedicated to the follow-up, confirmation, characterization, and mass measurement of planets orbiting bright stars discovered by the Transiting Exoplanet Survey Satellite (TESS) -a category in which it is almost unique in the Southern Hemisphere. It is located at the University of Southern Queensland's Mount Kent Observatory near Toowoomba, Australia. Its flexible design enables multiple 0.7 m robotic telescopes to be used both in combination, and independently, for high-resolution spectroscopy and precision photometry of TESS transit planet candidates.MINERVA-Australis also enables complementary studies of exoplanet spin-orbit alignments via Doppler observations of the Rossiter-McLaughlin effect, radial velocity searches for nontransiting planets, planet searches using transit timing variations, and ephemeris refinement for TESS planets. In this first paper, we describe the design, photometric instrumentation, software, and science goals of MINERVA-Australis, and note key differences from its Northern Hemisphere counterpart, the MINERVA array. We use recent transit observations of four PASP 3 planets, WASP-2b, WASP-44b, WASP-45b, and HD 189733b, to demonstrate the photometric capabilities of MINERVA-Australis.

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Section: First Science Results With Minerva-australismentioning

confidence: 99%

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Minerva-Australis. I. Design, Commissioning, and First Photometric Results

Addison

Wright

Wittenmyer

et al. 2019

PASP

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100

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Ephemeris refinement of 21 hot Jupiter exoplanets with high timing uncertainties

Mallonn

Essen

Herrero

et al. 2019

A&A

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Transit events of extrasolar planets offer a wealth of information for planetary characterization. However, for many known targets, the uncertainty of their predicted transit windows prohibits an accurate scheduling of follow-up observations. In this work, we refine the ephemerides of 21 hot Jupiter exoplanets with the largest timing uncertainties. We collected 120 professional and amateur transit light curves of the targets of interest, observed with a range of telescopes of 0.3m to 2.2m, and analyzed them along with the timing information of the planets discovery papers. In the case of WASP-117b, we measured a timing deviation compared to the known ephemeris of about 3.5 hours, and for HAT-P-29b and HAT-P-31b the deviation amounted to about 2 hours and more. For all targets, the new ephemeris predicts transit timings with uncertainties of less than 6 minutes in the year 2018 and less than 13 minutes until 2025. Thus, our results allow for an accurate scheduling of follow-up observations in the next decade.

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TraMoS

Cortés-Zuleta

Rojo

Wang

et al. 2020

A&A

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We present 22 new transit observations of the exoplanets WASP-18Ab, WASP-19b, and WASP-77Ab, from the Transit Monitoring in the South project. We simultaneously model our newly collected transit light curves with archival photometry and radial velocity data to obtain refined physical and orbital parameters. We include TESS light curves of the three exoplanets to perform an extended analysis of the variations in their transit mid-time (TTV) and to refine their planetary orbital ephemeris. We did not find significant TTVRMS variations larger than 47, 65, and 86 s for WASP-18Ab, WASP-19b, and WASP-77Ab, respectively. Dynamical simulations were carried out to constrain the masses of a possible perturber. The observed mean square (RMS) could be produced by a perturber body with an upper limit mass of 9, 2.5, 11 and 4 M⊕ in 1:2, 1:3, 2:1, and 3:1 resonances in the WASP-18Ab system. In the case of WASP-19b, companions with masses up to 0.26, 0.65, 1, and 2.8 M⊕, in 1:2, 2:1, 3:1, and 5:3 resonances respectively, produce the RMS. For the WASP-77Ab system, this RMS could be produced by a planet with mass in the range of 1.5−9 M⊕ in 1:2, 1:3, 2:1, 2:3, 3:1, 3:5, or 5:3 resonances. Comparing our results with RV variations, we discard massive companions with 350 M⊕ in 17:5 resonance for WASP-18Ab, 95 M⊕ in 4:1 resonance for WASP-19b, and 105 M⊕ in 5:2 resonance for WASP-77Ab. Finally, using a Lomb-Scargle period search we find no evidence of a periodic trend on our TTV data for the three exoplanets.

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Transiting Exoplanet Monitoring Project (TEMP). I. Refined System Parameters and Transit Timing Variations of HAT-P-29b

Cited by 15 publications

References 74 publications

Minerva-Australis. I. Design, Commissioning, and First Photometric Results

Minerva-Australis. I. Design, Commissioning, and First Photometric Results

Ephemeris refinement of 21 hot Jupiter exoplanets with high timing uncertainties

TraMoS

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