The TESS science processing operations center

Jenkins, Jon M.; Twicken, Joseph D.; McCauliff, Sean; Campbell, Jennifer R.; Sanderfer, Dwight T.; Lung, David Christopher; Mansouri-Samani, Masoud; Girouard, Forrest R.; Tenenbaum, Peter; Klaus, Todd C.; Smith, Jeffrey C.; Caldwell, Douglas A.; Chacon, A. D.; Henze, Christopher E.; Heiges, Cory; Latham, David W.; Morgan, E.; Swade, Daryl A.; Rinehart, Stephen A.; Vanderspek, R.

doi:10.1117/12.2233418

Cited by 706 publications

(289 citation statements)

References 4 publications

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“…2-minute) data is provided. We use the 2-minute Presearch Data Conditioning (PDC; Smith et al 2012;Stumpe et al 2012) light curve from the Science Processing Operations Center (SPOC) pipeline (Jenkins et al 2016;Jenkins 2017), which was originally developed for the Kepler mission (Jenkins et al 2010). These light curves are corrected for systematics by the SPOC pipeline.…”

Section: Tessmentioning

confidence: 99%

An unusually large gaseous transit in a debris disc

Iglesias

Olofsson

Bayo

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present the detection of an unusually large transient gas absorption in several ionized species in the debris disc star HD 37306 using high-resolution optical spectra. We have been analysing a large sample of debris discs searching for circumstellar gas absorptions aiming to determine the frequency of gas in debris discs. HD 37306 stood out showing remarkably broad absorptions superimposed onto several photospheric Ca ii, Fe ii and Ti ii lines. The observed absorptions, unlike typical exocometary transits, lasted for at least eight days. Here we analyse simultaneous spectroscopic and photometric data of the event and evaluate different scenarios that might explain the observed features. We conclude that the most likely scenario might be an exocometary break-up releasing a significant amount of gas close to the star, producing an occulting "ring"/"torus" shape.

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Section: Tessmentioning

confidence: 99%

An unusually large gaseous transit in a debris disc

Iglesias

Olofsson

Bayo

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…We found there to be 4 stars within this radius with magnitudes brighter than V=16, as shown in Figure 4). As we do not see a centroid shift during the time of the transit events, we can rule these out as the cause for the dips in light curve of TOI 813.Furthermore, the SPOC pipeline (Jenkins et al 2016) accounts for the contamination of the aperture by the neighbouring stars, so that we do not need to correct the measured transit depth for the effect of this light.…”

Section: Light Curve Based Vetting Checksmentioning

confidence: 93%

“…While most volunteers simply mark transit-like events, a significant proportion go much further, downloading and analysing TESS light curves at their own initiative. Jenkins et al 2016). These light curves have been corrected for both known pixel-level instrumental effects and systematics common to many light curves.…”

Section: The Citizen Science Approachmentioning

confidence: 99%

Planet Hunters TESS I: TOI 813, a subgiant hosting a transiting Saturn-sized planet on an 84-day orbit

Eisner

Barragán

Aigrain

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We report on the discovery and validation of TOI 813 b (TIC 55525572 b), a transiting exoplanet identified by citizen scientists in data from NASA's Transiting Exoplanet Survey Satellite (TESS ) and the first planet discovered by the Planet Hunters TESS project. The host star is a bright (V = 10.3 mag) subgiant (R = 1.94 R , M = 1.32 M ). It was observed almost continuously by TESS during its first year of operations, during which time four individual transit events were detected. The candidate passed all the standard light curve-based vetting checks, and ground-based follow-up spectroscopy and speckle imaging enabled us to statistically validate the planetary nature of the companion. Detailed modelling of the transits yields a period of 83.8911 +0.0027 −0.0031 days, a planet radius of 6.71 ± 0.38 R ⊕ and a semi major axis of 0.423 +0.031 −0.037 AU. The planet's orbital period combined with the evolved nature of the host star places this object in a relatively under-explored region of parameter space. We estimate that TOI 813 b induces a reflex motion in its host star with a semiamplitude of ∼ 6 m s −1 , making this system a promising target to measure the mass of a relatively long-period transiting planet. cated at low ecliptic latitudes (around 63 per cent of the sky) will be monitored for ≈27.4 continuous days, while a total of ∼2 per cent of the sky at the ecliptic poles will be observed continuously for ∼356 days. This observational strategy means that TESS will provide us with a plethora of short period planets ( 20 d) around bright (V 11 mag), nearby stars, which will allow for detailed characterization (e.g., Barclay et al. 2018;Gandolfi et al. 2018;Huang et al. 2018;Esposito et al. 2019).Longer-period planets will, however, be significantly

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“…Although no contamination ratio is available for this star in the TIC, it is the brightest star by about 2.5 mag in the TESS bandpass within a radius of 3.5 ′ (or about 10 pixels); therefore, the variations seen in the TESS light curve are likely intrinsic to HD 62658. The observations for this star were downloaded from the Mikulski Archive for Space Telescopes (MAST) 3 and we used the PDCSAP flux column from the light curve files generated by the TESS Science Processing Operations Center (Jenkins et al 2016).…”

Section: Tessmentioning

confidence: 99%

MOBSTER – III. HD 62658: a magnetic Bp star in an eclipsing binary with a non-magnetic ‘identical twin’

Shultz

Johnston

Labadie-Bartz

et al. 2019

Monthly Notices of the Royal Astronomical Society

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HD 62658 (B9p V) is a little-studied chemically peculiar star. Light curves obtained by the Kilodegree Extremely Little Telescope (KELT) and Transiting Exoplanet Survey Satellite (TESS) show clear eclipses with a period of about 4.75 d, as well as out-of-eclipse brightness modulation with the same 4.75 d period, consistent with synchronized rotational modulation of surface chemical spots. High-resolution ESPaDOnS circular spectropolarimetry shows a clear Zeeman signature in the line profile of the primary; there is no indication of a magnetic field in the secondary. PHOEBE modelling of the light curve and radial velocities indicates that the two components have almost identical masses of about 3 M ⊙ . The primary's longitudinal magnetic field B z varies between about +100 and −250 G, suggesting a surface magnetic dipole strength B d = 850 G. Bayesian analysis of the Stokes V profiles indicates B d = 650 G for the primary and B d < 110 G for the secondary. The primary's line profiles are highly variable, consistent with the hypothesis that the out-of-eclipse brightness modulation is a consequence of rotational modulation of that star's chemical spots. We also detect a residual signal in the light curve after removal of the orbital and rotational modulations, which might be pulsational in origin; this could be consistent with the weak line profile variability of the secondary. This system represents an excellent opportunity to examine the consequences of magnetic fields for stellar structure via comparison of two stars that are essentially identical with the exception that one is magnetic. The existence of such a system furthermore suggests that purely environmental explanations for the origin of fossil magnetic fields are incomplete.

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The TESS science processing operations center

Cited by 706 publications

References 4 publications

An unusually large gaseous transit in a debris disc

An unusually large gaseous transit in a debris disc

Planet Hunters TESS I: TOI 813, a subgiant hosting a transiting Saturn-sized planet on an 84-day orbit

MOBSTER – III. HD 62658: a magnetic Bp star in an eclipsing binary with a non-magnetic ‘identical twin’

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