Transiting Exoplanet Survey Satellite (TESS)

Ricker, G.; Winn, Joshua N.; Vanderspek, R.; Latham, David W.; Bakos, G. Á.; Bean, Jacob L.; Berta-Thompson, Zachory K.; Brown, Timothy M.; Buchhave, Lars A.; Butler, Nathaniel R.; Butler, R. Paul; Chaplin, W. J.; Charbonneau, David; Christensen‐Dalsgaard, J.; Clampin, Mark; Deming, Drake; Doty, J.; Lee, Nathan De; Dressing, Courtney D.; Dunham, E. W.; Endl, Michael; Fressin, François; Ge, Jian; Henning, Thomas; Holman, Matthew J.; Howard, Andrew W.; Ida, Shigeru; Jenkins, J. S.; Jernigan, G.; Johnson, John Asher; Kaltenegger, Lisa; Kawai, N.; Kjeldsen, H.; Laughlin, Gregory; Levine, Alan M.; Lin, D. N. C.; Lissauer, Jack J.; MacQueen, Phillip J.; Marcy, Geoffrey W.; McCullough, P. R.; Morton, Timothy; Narita, Norio; Paegert, Martin; Πάλλη, Ε.; Pepe, F.; Pepper, Joshua; Quirrenbach, A.; Rinehart, Stephen A.; Sasselov, Dimitar; Sato, Bun’ei; Seager, Sara; Sozzetti, A.; Stassun, Keivan G.; Sullivan, Peter; Szentgyorgyi, Andrew; Torres, Guillermo; Udry, S.; Villaseñor, J.

doi:10.1117/12.2063489

Cited by 727 publications

(285 citation statements)

References 12 publications

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“…asteroseismology of 18 Sco and α Cen A; Li et al, 2012;Bazot, Bourguignon, and Christensen-Dalsgaard, 2012). This situation will soon improve, after the Transiting Exoplanet Survey Satellite (TESS; Ricker et al, 2014) yields asteroseismic data for bright stars across the sky during a two year mission (2018)(2019)(2020). Although the time-series photometry will span only 27 days for most TESS targets, this was sufficient to detect solar-like oscillations in hundreds of Kepler stars down to V∼12 (Chaplin et al, 2011).…”

Section: Discussion and Future Outlookmentioning

confidence: 99%

Magnetic Evolution and the Disappearance of Sun-Like Activity Cycles

Metcalfe

Saders

2017

Sol Phys

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After decades of effort, the solar activity cycle is exceptionally well characterized but it remains poorly understood. Pioneering work at the Mount Wilson Observatory demonstrated that other sun-like stars also show regular activity cycles, and suggested two possible relationships between the rotation rate and the length of the cycle. Neither of these relationships correctly describe the properties of the Sun, a peculiarity that demands explanation. Recent discoveries have started to shed light on this issue, suggesting that the Sun's rotation rate and magnetic field are currently in a transitional phase that occurs in all middleaged stars. Motivated by these developments, we identify the manifestation of this magnetic transition in the best available data on stellar cycles. We propose a reinterpretation of previously published observations to suggest that the solar cycle may be growing longer on stellar evolutionary timescales, and that the cycle might disappear sometime in the next 0.8-2.4 Gyr. Future tests of this hypothesis will come from ground-based activity monitoring of Kepler targets that span the magnetic transition, and from asteroseismology with the TESS mission to determine precise masses and ages for bright stars with known cycles.

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Section: Discussion and Future Outlookmentioning

confidence: 99%

Magnetic Evolution and the Disappearance of Sun-Like Activity Cycles

Metcalfe

Saders

2017

Sol Phys

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“…TESS is scheduled for launch in 2017, and is the next transit photometry planet detection mission in NASA's pipeline. 24 Transit photometry observations of potential planet signatures generally require follow-up confirmation, with RV being the most common. Currently, there is a dearth of high-precision RV facilities in the northern hemisphere, and HARPS-N is heavily committed to Kepler planet candidate followup.…”

Section: Transiting Exoplanet Survey Satellite Precovery Surveymentioning

confidence: 99%

Capabilities and performance of the Automated Planet Finder telescope with the implementation of a dynamic scheduler

Burt

Holden

Hanson

et al. 2015

J. Astron. Telesc. Instrum. Syst

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Abstract. We report initial performance results emerging from 600 h of observations with the Automated Planet Finder (APF) telescope and Levy spectrometer located at UCO/Lick Observatory. We have obtained multiple spectra of 80 G, K, and M-type stars, which comprise 4954 individual Doppler radial velocity (RV) measurements with a median internal uncertainty of 1.35 ms −1 . We find a strong, expected correlation between the number of photons accumulated in the 5000 to 6200 Å iodine region of the spectrum and the resulting internal uncertainty estimates. Additionally, we find an offset between the population of G and K stars and the M stars within the dataset when comparing these parameters. As a consequence of their increased spectral line densities, M-type stars permit the same level of internal uncertainty with 2× fewer photons than G-type and K-type stars. When observing M stars, we show that the APF/Levy has essentially the same speed-on-sky as Keck/high resolution echelle spectrometer (HIRES) for precision RVs. In the interest of using the APF for long-duration RV surveys, we have designed and implemented a dynamic scheduling algorithm. We discuss the operation of the scheduler, which monitors ambient conditions and combines on-sky information with a database of survey targets to make intelligent, real-time targeting decisions.

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“…The European Space Agency GAIA mission is expected to deliver several thousands new planets via the astrometric technique (Casertano et al 2008;Sozzetti 2010). The NASA TESS mission (Ricker et al 2010) is predicted to discover thousands transiting exoplanet candidates which are Earth-sized or larger. Are those numbers large enough to provide a meaningful classification of planets as we do with stars?…”

Section: Overviewmentioning

confidence: 99%

Spectroscopy of planetary atmospheres in our Galaxy

Tinetti

Encrenaz

Coustenis

2013

Astron Astrophys Rev

124

110

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About 20 years after the discovery of the first extrasolar planet, the number of planets known has grown by three orders of magnitude, and continues to increase at neck breaking pace. For most of these planets we have little information, except for the fact that they exist and possess an address in our Galaxy. For about one third of them, we know how much they weigh, their size and their orbital parameters. For less than 20, we start to have some clues about their atmospheric temperature and composition. How do we make progress from here?We are still far from the completion of a hypothetical Hertzsprung-Russell diagram for planets comparable to what we have for stars, and today we do not even know whether such classification will ever be possible or even meaningful for planetary objects. But one thing is clear: planetary parameters such as mass, radius and temperature alone do not explain the diversity revealed by current observations. The chemical composition of these planets is needed to trace back their formation history and evolution, as happened for the planets in our Solar System. As in situ measurements are and will remain off-limits for exoplanets, to study their chemical composition we will have to rely on remote sensing spectroscopic observations of their gaseous envelopes.

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Transiting Exoplanet Survey Satellite (TESS)

Cited by 727 publications

References 12 publications

Magnetic Evolution and the Disappearance of Sun-Like Activity Cycles

Magnetic Evolution and the Disappearance of Sun-Like Activity Cycles

Capabilities and performance of the Automated Planet Finder telescope with the implementation of a dynamic scheduler

Spectroscopy of planetary atmospheres in our Galaxy

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