TESS Discovery of an Ultra-short-period Planet around the Nearby M Dwarf LHS 3844

Vanderspek, R.; Huang, Chelsea X.; Vanderburg, Andrew; Ricker, G.; Latham, David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Burt, Jennifer; Dittmann, Jason; Newton, Elisabeth R.; Quinn, Samuel N.; Shporer, Avi; Charbonneau, David; Irwin, Jonathan; Ment, Kristo; Winters, Jennifer G.; Collins, Karen A.; Evans, P.; Gan, Tianjun; Hart, Rhodes; Jensen, Eric L. N.; Kielkopf, John F.; Mao, Shude; Waalkes, William; Bouchy, F.; Marmier, M.; Nielsen, L. D.; Ottoni, G.; Pepe, F.; Ségransan, D.; Udry, S.; Henry, Todd J.; Paredes, Leonardo A.; James, Hodari-Sadiki; Hinojosa, R.; Silverstein, Michele L.; Πάλλη, Ε.; Berta-Thompson, Zachory K.; Crossfield, Ian J. M.; Davies, Misty; Dragomir, Diana; Fausnaugh, Michael; Glidden, Ana; Pepper, Joshua; Morgan, E.; Rose, Mark; Twicken, Joseph D.; Villaseñor, J.; Yu, Li; Bakos, G. Á.; Bean, Jacob L.; Buchhave, Lars A.; Christensen‐Dalsgaard, J.; Christiansen, Jessie L.; Ciardi, David R.; Clampin, Mark; Lee, Nathan De; Deming, Drake; Doty, J.; Jernigan, J. G.; Kaltenegger, Lisa; Lissauer, Jack J.; McCullough, P. R.; Narita, Norio; Paegert, Martin; Pál, András; Rinehart, Stephen A.; Sasselov, Dimitar; Sato, Bun’ei; Sozzetti, A.; Stassun, Keivan G.; Torres, Guillermo

doi:10.3847/2041-8213/aafb7a

Cited by 138 publications

(112 citation statements)

References 74 publications

(57 reference statements)

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“…Grey lines connect planets in the same system for a few select M-dwarf systems. Plot inspired by Figure 4 in Vanderspek et al (2019). than GJ 1214 (J=9.8) in J band with a J magnitude of J=10.1. Due to its relatively large transit depth and the brightness of its host star at NIR wavelengths, G 9-40b is amenable for transmission spectroscopic observations that could provide insight into the planet's bulk composition and formation history through measuring the elemental composition of its atmosphere and overall metal enrichment.…”

Section: Upper Bound On Mass Estimate Using the Hpf Rvsmentioning

confidence: 99%

A Sub-Neptune-sized Planet Transiting the M2.5 Dwarf G 9-40: Validation with the Habitable-zone Planet Finder

et al. 2020

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We validate the discovery of a 2 Earth radii sub-Neptune-size planet around the nearby high proper motion M2.5-dwarf G 9-40 (EPIC 212048748), using high-precision near-infrared (NIR) radial velocity (RV) observations with the Habitable-zone Planet Finder (HPF), precision diffuser-assisted ground-based photometry with a custom narrow-band photometric filter, and adaptive optics imaging. At a distance of d = 27.9 pc, G 9-40b is the second closest transiting planet discovered by K2 to date. The planet's large transit depth (∼3500ppm), combined with the proximity and brightness of the host star at NIR wavelengths (J=10, K=9.2) makes G 9-40b one of the most favorable sub-Neptune-sized planet orbiting an M-dwarf for transmission spectroscopy with JWST, ARIEL, and the upcoming Extremely Large Telescopes. The star is relatively inactive with a rotation period of ∼29 days determined from the K2 photometry. To estimate spectroscopic stellar parameters, we describe our implementation of an empirical spectral matching algorithm using the high-resolution NIR HPF spectra. Using this algorithm, we obtain an effective temperature of T eff = 3404 ± 73K, and metallicity of [Fe/H] = −0.08 ± 0.13. Our RVs, when coupled with the orbital parameters derived from the transit photometry, exclude planet masses above 11.7M ⊕ with 99.7% confidence assuming a circular orbit. From its radius, we predict a mass of M = 5.0 +3.8 −1.9 M ⊕ and an RV semi-amplitude of K = 4.1 +3.1 −1.6 m s −1 , making its mass measurable with current RV facilities. We urge further RV follow-up observations to precisely measure its mass, to enable precise transmission spectroscopic measurements in the future.

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Section: Upper Bound On Mass Estimate Using the Hpf Rvsmentioning

confidence: 99%

A Sub-Neptune-sized Planet Transiting the M2.5 Dwarf G 9-40: Validation with the Habitable-zone Planet Finder

et al. 2020

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“…Data acquired throughout each onemonth "sector" are downlinked at spacecraft perigee through the Deep Space Network. Descriptions of the spacecraft's design and operations are given by Ricker et al (2015) and Vanderspek et al (2018).…”

Section: Observationsmentioning

confidence: 99%

“…After subtracting the background, we mask out saturated pixels using a fixed saturation level of 8 × 10 4 analog-todigital units (ADU). This value was chosen based on the onset of bleeding charge trails in the images, and is a factor of two greater than the saturation level of 2 × 10 5 electrons, or about 4 × 10 4 ADU, reported by Vanderspek et al (2018). As a consequence, we do not analyze stars brighter than T ≈ 6.5, even though the TESS CCID-80 CCDs conserve charge across bloom trails up to at least T ≈ 4 Vanderspek et al (2018).…”

Section: Image Preparation and Background Removalmentioning

confidence: 99%

Cluster Difference Imaging Photometric Survey. I. Light Curves of Stars in Open Clusters from TESS Sectors 6 and 7

Bouma

Hartman

Bhatti

et al. 2019

ApJS

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The Transiting Exoplanet Survey Satellite (TESS) is providing precise time-series photometry for most star clusters in the solar neighborhood. Using the TESS images, we have begun a Cluster Difference Imaging Photometric Survey (CDIPS), in which we are focusing both on stars that are candidate cluster members, and on stars that show indications of youth. Our aims are to discover giant transiting planets with known ages, and to provide light curves suitable for studies in stellar astrophysics. For this work, we made 159,343 light curves of candidate young stars, across 596 distinct clusters. Each light curve represents between 20 and 25 days of observations of a star brighter than G Rp = 16, with 30-minute sampling. We describe the image subtraction and time-series analysis techniques we used to create the light curves, which have noise properties that agree with theoretical expectations. We also comment on the possible utility of the light curve sample for studies of stellar rotation evolution, and binary eccentricity damping. The light curves a) , which cover about one sixth of the galactic plane, are available as a High Level Science Product at MAST:

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“…It will now move its observations to the north, continuing its full-sky survey. At the time of writing TESS has already successfully discovered and confirmed 29 new transiting planets (NASA Exoplanet Archive 1 , Akeson et al 2013) including π Mensae c Gandolfi et al 2018), HD 202772A b, (Wang et al 2019), LHS 3844 b (Vanderspek et al 2019) and HD 219666 b, (Esposito et al 2019).…”

Section: Introductionmentioning

confidence: 99%

An examination of the effect of the TESS extended mission on southern hemisphere monotransits

Cooke

Pollacco

2019

A&A

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Context. NASA recently announced an extended mission for TESS. As a result it is expected that the southern ecliptic hemisphere will be re-observed approximately two years after the initial survey. Aims. We aim to explore how TESS re-observing the southern ecliptic hemisphere will impact the number and distribution of monotransits discovered during the first year of observations. This simulation will be able to be scaled to any future TESS re-observations. Methods. We carry out an updated simulation of TESS detections in the southern ecliptic hemisphere. This simulation includes realistic Sector window-functions based on the first 11 sectors of SPOC 2 min SAP lightcurves. We then extend this simulation to cover the expected Year 4 of the mission when TESS will re-observe the southern ecliptic fields. For recovered monotransits we also look at the possibility of predicting the period based on the coverage in the TESS data. Results. We find an updated prediction of 339 monotransits from the TESS Year 1 southern ecliptic hemisphere, and that approximately 80% of these systems (266/339) will transit again in the Year 4 observations. The Year 4 observations will also contribute new monotransits not seen in Year 1, resulting in a total of 149 monotransits from the combined Year 1 and Year 4 data sets. We find that 75% (189/266) of recovered Year 1 monotransits will only transit once in the Year 4 data set. For these systems we will be able to constrain possible periods, but period aliasing due to the large time gap between Year 1 and Year 4 observations means that the true period will remain unknown without further spectroscopic or photometric follow-up.

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TESS Discovery of an Ultra-short-period Planet around the Nearby M Dwarf LHS 3844

Cited by 138 publications

References 74 publications

A Sub-Neptune-sized Planet Transiting the M2.5 Dwarf G 9-40: Validation with the Habitable-zone Planet Finder

A Sub-Neptune-sized Planet Transiting the M2.5 Dwarf G 9-40: Validation with the Habitable-zone Planet Finder

Cluster Difference Imaging Photometric Survey. I. Light Curves of Stars in Open Clusters from TESS Sectors 6 and 7

An examination of the effect of the TESS extended mission on southern hemisphere monotransits

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