Author: "Fausnaugh, Michael" - Searchworks@Jio Institute Digital Library Search Results

Your search keyword '"Fausnaugh, Michael"' showing total 315 results

Start Over Author "Fausnaugh, Michael"

315 results on '"Fausnaugh, Michael"'

101. Big surprises from small supermassive black holes

Author: Fausnaugh, Michael
Published: 2019
Full Text: View/download PDF

102. TESS Data Release Notes: Sector 1, DR1

Author: Fausnaugh, Michael M, Caldwell, Douglas A, Jenkins, Jon M, Smith, Jeffrey C, Vanderspek, Roland, Doty, John P, Li, Jie, Ting, Eric B, and Villasenor, Joel S
Subjects: Astronomy
Abstract: This release note discusses the science data products produced by the Science Processing Operations Center at Ames Research Center from Sector 1 observations made with the TESS spacecraft and cameras as a means to document instrument performance and data characteristics.
Published: 2018

103. Complex Modulation of Rapidly Rotating Young M Dwarfs:Adding Pieces to the Puzzle

Author: Günther, Maximilian N., Berardo, David A., Ducrot, Elsa, Murray, Catriona A., Stassun, Keivan G., Olah, Katalin, Bouma, L. G., Rappaport, Saul, Winn, Joshua N., Feinstein, Adina D., Matthews, Elisabeth C., Sebastian, Daniel, Rackham, Benjamin V., Seli, Bálint, Amaury, Amaury H.M., Gillen, Edward, Levine, Alan M., Demory, Brice Olivier, Gillon, Michaël, Queloz, Didier, Ricker, George R., Vanderspek, Roland K., Seager, Sara, Latham, David W., Jenkins, Jon M., Brasseur, C. E., Colón, Knicole D., Daylan, Tansu, Delrez, Laetitia, Fausnaugh, Michael, Garcia, Lionel J., Jayaraman, Rahul, Jehin, Emmanuel, Kristiansen, Martti H., Kruijssen, J. M.Diederik, Pedersen, Peter Pihlmann, Pozuelos, Francisco J., Rodriguez, Joseph E., Wohler, Bill, Zhan, Zhuchang, Günther, Maximilian N., Berardo, David A., Ducrot, Elsa, Murray, Catriona A., Stassun, Keivan G., Olah, Katalin, Bouma, L. G., Rappaport, Saul, Winn, Joshua N., Feinstein, Adina D., Matthews, Elisabeth C., Sebastian, Daniel, Rackham, Benjamin V., Seli, Bálint, Amaury, Amaury H.M., Gillen, Edward, Levine, Alan M., Demory, Brice Olivier, Gillon, Michaël, Queloz, Didier, Ricker, George R., Vanderspek, Roland K., Seager, Sara, Latham, David W., Jenkins, Jon M., Brasseur, C. E., Colón, Knicole D., Daylan, Tansu, Delrez, Laetitia, Fausnaugh, Michael, Garcia, Lionel J., Jayaraman, Rahul, Jehin, Emmanuel, Kristiansen, Martti H., Kruijssen, J. M.Diederik, Pedersen, Peter Pihlmann, Pozuelos, Francisco J., Rodriguez, Joseph E., Wohler, Bill, and Zhan, Zhuchang
Abstract: New sets of young M dwarfs with complex, sharp-peaked, and strictly periodic photometric modulations have recently been discovered with Kepler/K2 (scallop shells) and TESS (complex rotators). All are part of star-forming associations, are distinct from other variable stars, and likely belong to a unified class. Suggested hypotheses include starspots, accreting dust disks, corotating clouds of material, magnetically constrained material, spots and misaligned disks, and pulsations. Here, we provide a comprehensive overview and add new observational constraints with TESS and SPECULOOS Southern Observatory photometry. We scrutinize all hypotheses from three new angles: (1) We investigate each scenario's occurrence rates via young star catalogs, (2) we study the feature's longevity using over one year of combined data, and (3) we probe the expected color dependency with multicolor photometry. In this process, we also revisit the stellar parameters accounting for activity effects, study stellar flares as activity indicators over year-long timescales, and develop toy models to simulate typical morphologies. We rule out most hypotheses, and only (i) corotating material clouds and (ii) spots and misaligned disks remain feasible-with caveats. For (i), corotating dust might not be stable enough, while corotating gas alone likely cannot cause percentage-scale features and (ii) would require misaligned disks around most young M dwarfs. We thus suggest a unified hypothesis, a superposition of large-amplitude spot modulations and sharp transits of corotating gas clouds. While the complex rotators' mystery remains, these new observations add valuable pieces to the puzzle going forward.
Published: 2022

104. A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of p Men c

Author: National Aeronautics and Space Administration (US), National Science Foundation (US), Australian Research Council, Danish National Research Foundation, Fundação para a Ciência e a Tecnologia (Portugal), European Commission, Research Council of Lithuania, Alexander von Humboldt Foundation, Ministerio de Ciencia e Innovación (España), Chinese Academy of Sciences, Kavli Foundation, Huber, Daniel, White, Timothy R., Metcalfe, T.S., Chontos, Ashley, Fausnaugh, Michael, Ho, Cynthia S. K., Eylen, Vicent van, Ball, Warrick H., Basu, Sarbani, Bedding, Timothy R., Benomar, Othman, Bossini, Diego, Breton, Sylvain N., Buzasi, Derek, Campante, Tiago L., Chaplin, William J., Christensen-Dalsgaard, Jørgen, Cunha, Margarida S., Deal, Morgan, García, Raquel A., García Muñoz, Josep Lluís, Gehan, Charlotte, González-Cuesta, L., Jiang, Chen, Kayhan, Cenk, Kjeldsen, Hans, Lundkvist, Mia S., Mathis, Stéphane, Mathur, Savita, Monteiro, Mario J.P.F.G., Nsamba, Benard, Ong, Jia Mian Joel, Pakštienė, Erika, Serenelli, Aldo, Silva Aguirre, Víctor, Stassun, Keivan G., Stello, Dennis, Stilling, Sissel Norgaard, Winther, Mark L., Wu, Tao, Barclay, Thomas, Daylan, Tansu, Günther, Maximilian N., Hermes, James J., Jenkins, Jon M., Latham, David W., Levine, Alan M., Ricker, George R., Seager, Sara, Shporer, A., Twicken, Joseph D., Vanderspek, R.K., Winn, Joshua N., National Aeronautics and Space Administration (US), National Science Foundation (US), Australian Research Council, Danish National Research Foundation, Fundação para a Ciência e a Tecnologia (Portugal), European Commission, Research Council of Lithuania, Alexander von Humboldt Foundation, Ministerio de Ciencia e Innovación (España), Chinese Academy of Sciences, Kavli Foundation, Huber, Daniel, White, Timothy R., Metcalfe, T.S., Chontos, Ashley, Fausnaugh, Michael, Ho, Cynthia S. K., Eylen, Vicent van, Ball, Warrick H., Basu, Sarbani, Bedding, Timothy R., Benomar, Othman, Bossini, Diego, Breton, Sylvain N., Buzasi, Derek, Campante, Tiago L., Chaplin, William J., Christensen-Dalsgaard, Jørgen, Cunha, Margarida S., Deal, Morgan, García, Raquel A., García Muñoz, Josep Lluís, Gehan, Charlotte, González-Cuesta, L., Jiang, Chen, Kayhan, Cenk, Kjeldsen, Hans, Lundkvist, Mia S., Mathis, Stéphane, Mathur, Savita, Monteiro, Mario J.P.F.G., Nsamba, Benard, Ong, Jia Mian Joel, Pakštienė, Erika, Serenelli, Aldo, Silva Aguirre, Víctor, Stassun, Keivan G., Stello, Dennis, Stilling, Sissel Norgaard, Winther, Mark L., Wu, Tao, Barclay, Thomas, Daylan, Tansu, Günther, Maximilian N., Hermes, James J., Jenkins, Jon M., Latham, David W., Levine, Alan M., Ricker, George R., Seager, Sara, Shporer, A., Twicken, Joseph D., Vanderspek, R.K., and Winn, Joshua N.
Abstract: We present an analysis of the first 20 second cadence light curves obtained by the TESS space telescope during its extended mission. We find improved precision of 20 second data compared to 2 minute data for bright stars when binned to the same cadence (˜10%-25% better for T ? 8 mag, reaching equal precision at T ˜ 13 mag), consistent with pre-flight expectations based on differences in cosmic-ray mitigation algorithms. We present two results enabled by this improvement. First, we use 20 second data to detect oscillations in three solar analogs (? Pav, ? Tuc, and p Men) and use asteroseismology to measure their radii, masses, densities, and ages to ˜1%, ˜3%, ˜1%, and ˜20% respectively, including systematic errors. Combining our asteroseismic ages with chromospheric activity measurements, we find evidence that the spread in the activity-age relation is linked to stellar mass and thus the depth of the convection zone. Second, we combine 20 second data and published radial velocities to recharacterize p Men c, which is now the closest transiting exoplanet for which detailed asteroseismology of the host star is possible. We show that p Men c is located at the upper edge of the planet radius valley for its orbital period, confirming that it has likely retained a volatile atmosphere and that the "asteroseismic radius valley"remains devoid of planets. Our analysis favors a low eccentricity for p Men c (<0.1 at 68% confidence), suggesting efficient tidal dissipation (Q/k 2,1 ? 2400) if it formed via high-eccentricity migration. Combined, these early results demonstrate the strong potential of TESS 20 second cadence data for stellar astrophysics and exoplanet science.
Published: 2022

105. A nearby transiting rocky exoplanet that is suitable for atmospheric investigation

Author: Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Fausnaugh, Michael, Ricker, George R, Seager, Sara, Shporer, Abraham-Avi, Tenenbaum, Peter, Vanderspek, Roland K, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Fausnaugh, Michael, Ricker, George R, Seager, Sara, Shporer, Abraham-Avi, Tenenbaum, Peter, and Vanderspek, Roland K
Abstract: Spectroscopy of transiting exoplanets can be used to investigate their atmospheric properties and habitability. Combining radial velocity (RV) and transit data provides additional information on exoplanet physical properties. We detect a transiting rocky planet with an orbital period of 1.467 days around the nearby red dwarf star Gliese 486. The planet Gliese 486 b is 2.81 Earth masses and 1.31 Earth radii, with uncertainties of 5%, as determined from RV data and photometric light curves. The host star is at a distance of ~8.1 parsecs, has a J-band magnitude of ~7.2, and is observable from both hemispheres of Earth. On the basis of these properties and the planet's short orbital period and high equilibrium temperature, we show that this terrestrial planet is suitable for emission and transit spectroscopy.
Published: 2022

106. HD 219134 Revisited: Planet d Transit Upper Limit and Planet f Transit Nondetection with ASTERIA and TESS

Author: Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Haystack Observatory, Seager, Sara, Knapp, Mary E., Krishnamurthy, Akshata, Huang, Chelsea X., Badenas, Mariona, Shporer, Abraham-Avi, Ricker, George R, Vanderspek, Roland K, Fausnaugh, Michael, Glidden, Ana, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Haystack Observatory, Seager, Sara, Knapp, Mary E., Krishnamurthy, Akshata, Huang, Chelsea X., Badenas, Mariona, Shporer, Abraham-Avi, Ricker, George R, Vanderspek, Roland K, Fausnaugh, Michael, and Glidden, Ana
Abstract: HD 219134 is a K3V dwarf star with six reported radial-velocity discovered planets. The two innermost planets b and c show transits, raising the possibility of this system to be the nearest (6.53 pc), brightest (V = 5.57) example of a star with a compact multiple transiting planet system. Ground-based searches for transits of planets beyond b and c are not feasible because of the infrequent transits, long transit duration (~5 hr), shallow transit depths (<1%), and large transit time uncertainty (~half a day). We use the space-based telescopes the Arcsecond Space Telescope Enabling Research in Astrophysics (ASTERIA) and the Transiting Exoplanet Survey Satellite (TESS) to search for transits of planets f (P = 22.717 days and M sin i = 7.3 ± 0.04M ) and d (P?=?46.859 days and M sin i = 16.7 ± 0.64MÅ). ASTERIA was a technology demonstration CubeSat with an opportunity for science in an extended program. ASTERIA observations of HD 219134 were designed to cover the 3s transit windows for planets f and d via repeated visits over many months. While TESS has much higher sensitivity and more continuous time coverage than ASTERIA, only the HD 219134 f transit window fell within the TESS survey's observations. Our TESS photometric results definitively rule out planetary transits for HD 219134 f. We do not detect the Neptune-mass HD 219134 d transits and our ASTERIA data are sensitive to planets as small as 3.6 R . We provide TESS updated transit times and periods for HD 219134 b and c, which are designated TOI 1469.01 and 1469.02 respectively. ⊙ ⊙
Published: 2022

107. The TESS Faint-star Search: 1617 TOIs from the TESS Primary Mission

Author: Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Kunimoto, Michelle, Daylan, Tansu, Guerrero, Natalia, Fong, William, Bryson, Steve, Ricker, George R, Fausnaugh, Michael, Huang, Chelsea X, Sha, Lizhou, Shporer, Avi, Vanderburg, Andrew, Vanderspek, Roland K, Yu, Liang, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Kunimoto, Michelle, Daylan, Tansu, Guerrero, Natalia, Fong, William, Bryson, Steve, Ricker, George R, Fausnaugh, Michael, Huang, Chelsea X, Sha, Lizhou, Shporer, Avi, Vanderburg, Andrew, Vanderspek, Roland K, and Yu, Liang
Abstract: Abstract We present the detection of 1617 new transiting-planet candidates, identified in the Transiting Exoplanet Survey Satellite (TESS) full-frame images observed during the Primary Mission (Sectors 1–26). These candidates were initially detected by the Quick-Look Pipeline (QLP), which extracts full-frame image lightcurves for, and searches all stars brighter than, TESS magnitude T = 13.5 mag in each sector. However, QLP heavily relies on manual inspection for the identification of planet candidates, limiting vetting efforts to planet-hosting stars brighter than T = 10.5 mag and leaving millions of potential transit signals unvetted. We describe an independent vetting pipeline applied to QLP transit search results, incorporating both automated vetting tests and manual inspection to identify promising planet candidates around these fainter stars. The new candidates discovered by this ongoing project will allow TESS to significantly improve the statistical power of demographic studies of giant, close-in exoplanets.
Published: 2022

108. HD 191939: Three Sub-Neptunes Transiting a Sun-like Star Only 54 pc Away

Author: Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Badenas, Mariona, Günther, Maximilian N., Daylan, Tansu, Mikal-Evans, Thomas, Huang, Chelsea X., Matthews, Elisabeth C, Rackham, Benjamin V, Shporer, Abraham-Avi, Seager, Sara, Ricker, George R, Vanderspek, Roland K, Niraula, Prajwal, Crossfield, Ian Jm, Fausnaugh, Michael, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Badenas, Mariona, Günther, Maximilian N., Daylan, Tansu, Mikal-Evans, Thomas, Huang, Chelsea X., Matthews, Elisabeth C, Rackham, Benjamin V, Shporer, Abraham-Avi, Seager, Sara, Ricker, George R, Vanderspek, Roland K, Niraula, Prajwal, Crossfield, Ian Jm, and Fausnaugh, Michael
Abstract: © 2020. The American Astronomical Society. All rights reserved. We present the discovery of three sub-Neptune-sized planets transiting the nearby and bright Sun-like star HD 191939 (TIC 269701147, TOI 1339), a K s = 7.18 mag G8 V dwarf at a distance of only 54 pc. We validate the planetary nature of the transit signals by combining 5 months of data from the Transiting Exoplanet Survey Satellite with follow-up ground-based photometry, archival optical images, radial velocities, and high angular resolution observations. The three sub-Neptunes have similar radii (Rb=3.42-0.11+0.11, Rc=3.23-0.11+0.11, and Rd=3.16-0.11+0.11,R⊕), and their orbits are consistent with a stable, circular, and coplanar architecture near mean-motion resonances of 1:3 and 3:4 (P b = 8.88, P c = 28.58, and P d = 38.35 days). The HD 191939 system is an excellent candidate for precise mass determinations of the planets with high-resolution spectroscopy due to the host star's brightness and low chromospheric activity. Moreover, the system's compact and near-resonant nature can provide an independent way to measure planetary masses via transit timing variations while also enabling dynamical and evolutionary studies. Finally, as a promising target for multiwavelength transmission spectroscopy of all three planets' atmospheres, HD 191939 can offer valuable insight into multiple sub-Neptunes born from a protoplanetary disk that may have resembled that of the early Sun.
Published: 2022

109. A remnant planetary core in the hot-Neptune desert

Author: Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Huang, Chelsea X., Matthews, Elisabeth C, Crossfield, Ian Jm, Fausnaugh, Michael, Günther, Maximilian N., Ricker, George R, Seager, Sara, Sha, Lizhou, Vanderspek, Roland K, Villasenor, Jesus Noel Samonte, Zhan, Zhuchang, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Huang, Chelsea X., Matthews, Elisabeth C, Crossfield, Ian Jm, Fausnaugh, Michael, Günther, Maximilian N., Ricker, George R, Seager, Sara, Sha, Lizhou, Vanderspek, Roland K, Villasenor, Jesus Noel Samonte, and Zhan, Zhuchang
Abstract: © 2020, The Author(s), under exclusive licence to Springer Nature Limited. The interiors of giant planets remain poorly understood. Even for the planets in the Solar System, difficulties in observation lead to large uncertainties in the properties of planetary cores. Exoplanets that have undergone rare evolutionary processes provide a route to understanding planetary interiors. Planets found in and near the typically barren hot-Neptune ‘desert’1,2 (a region in mass–radius space that contains few planets) have proved to be particularly valuable in this regard. These planets include HD149026b3, which is thought to have an unusually massive core, and recent discoveries such as LTT9779b4 and NGTS-4b5, on which photoevaporation has removed a substantial part of their outer atmospheres. Here we report observations of the planet TOI-849b, which has a radius smaller than Neptune’s but an anomalously large mass of 39.1−2.6+2.7 Earth masses and a density of 5.2−0.8+0.7 grams per cubic centimetre, similar to Earth’s. Interior-structure models suggest that any gaseous envelope of pure hydrogen and helium consists of no more than 3.9−0.9+0.8 per cent of the total planetary mass. The planet could have been a gas giant before undergoing extreme mass loss via thermal self-disruption or giant planet collisions, or it could have avoided substantial gas accretion, perhaps through gap opening or late formation6. Although photoevaporation rates cannot account for the mass loss required to reduce a Jupiter-like gas giant, they can remove a small (a few Earth masses) hydrogen and helium envelope on timescales of several billion years, implying that any remaining atmosphere on TOI-849b is likely to be enriched by water or other volatiles from the planetary interior. We conclude that TOI-849b is the remnant core of a giant planet.
Published: 2022

110. A super-Earth and two sub-Neptunes transiting the nearby and quiet M dwarf TOI-270

Author: Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Günther, Maximilian N., Dragomir, Diana, Daylan, Tansu, Huang, Chelsea X., Burt, Jennifer A, Matthews, Elisabeth C, Ricker, George R, Vanderspek, Roland K, Seager, Sara, Crossfield, Ian Jm, Fausnaugh, Michael, Furesz, Gabor, Guerrero, Natalia M., Relles, Howard M., Shporer, Abraham-Avi, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Günther, Maximilian N., Dragomir, Diana, Daylan, Tansu, Huang, Chelsea X., Burt, Jennifer A, Matthews, Elisabeth C, Ricker, George R, Vanderspek, Roland K, Seager, Sara, Crossfield, Ian Jm, Fausnaugh, Michael, Furesz, Gabor, Guerrero, Natalia M., Relles, Howard M., and Shporer, Abraham-Avi
Abstract: © 2019, The Author(s), under exclusive licence to Springer Nature Limited. One of the primary goals of exoplanetary science is to detect small, temperate planets passing (transiting) in front of bright and quiet host stars. This enables the characterization of planetary sizes, orbits, bulk compositions, atmospheres and formation histories. These studies are facilitated by small and cool M dwarf host stars. Here we report the Transiting Exoplanet Survey Satellite (TESS)1 discovery of three small planets transiting one of the nearest and brightest M dwarf hosts observed to date, TOI-270 (TIC 259377017, with K-magnitude 8.3, and 22.5 parsecs away from Earth). The M3V-type star is transited by the super-Earth-sized planet TOI-270 b (1.247−0.083+0.089R⊕) and the sub-Neptune-sized planets TOI-270 c (2.42 ± 0.13 R⊕) and TOI-270 d (2.13 ± 0.12 R⊕). The planets orbit close to a mean-motion resonant chain, with periods (3.36 days, 5.66 days and 11.38 days, respectively) near ratios of small integers (5:3 and 2:1). TOI-270 is a prime target for future studies because (1) its near-resonance allows the detection of transit timing variations, enabling precise mass measurements and dynamical studies; (2) its brightness enables independent radial-velocity mass measurements; (3) the outer planets are ideal for atmospheric characterization via transmission spectroscopy; and (4) the quietness of the star enables future searches for habitable zone planets. Altogether, very few systems with small, temperate exoplanets are as suitable for such complementary and detailed characterization as TOI-270.
Published: 2022

111. The TESS Objects of Interest Catalog from the TESS Prime Mission

Author: Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Massachusetts Institute of Technology. Department of Electrical Engineering and Computer Science, Guerrero, Natalia M., Seager, Sara, Huang, Chelsea X., Mireles, Ismael, Hesse, Katharine, Fong, William, Glidden, Ana, Shporer, Abraham-Avi, Crossfield, Ian Jm, Vanderspek, Roland K, Fausnaugh, Michael, Burke, Christopher J., Ricker, George R, Daylan, Tansu, Essack, Zahra, Günther, Maximilian N., Osborn, Hugh P, Sha, Lizhou, Villanueva Jr, Steven, Yu, Liang, Berardo, David Anthony, Dittmann, Jason A, Mikal-Evans, Thomas, Jayaraman, Rahul, Krishnamurthy, Akshata, Mehrle, Nicholas, Rackham, Benjamin V, Sousa-Silva, Clara, Wong, Ian, Zhan, Zhuchang, Zivanovic, Goran, Pál, András, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Massachusetts Institute of Technology. Department of Electrical Engineering and Computer Science, Guerrero, Natalia M., Seager, Sara, Huang, Chelsea X., Mireles, Ismael, Hesse, Katharine, Fong, William, Glidden, Ana, Shporer, Abraham-Avi, Crossfield, Ian Jm, Vanderspek, Roland K, Fausnaugh, Michael, Burke, Christopher J., Ricker, George R, Daylan, Tansu, Essack, Zahra, Günther, Maximilian N., Osborn, Hugh P, Sha, Lizhou, Villanueva Jr, Steven, Yu, Liang, Berardo, David Anthony, Dittmann, Jason A, Mikal-Evans, Thomas, Jayaraman, Rahul, Krishnamurthy, Akshata, Mehrle, Nicholas, Rackham, Benjamin V, Sousa-Silva, Clara, Wong, Ian, Zhan, Zhuchang, Zivanovic, Goran, and Pál, András
Abstract: We present 2,241 exoplanet candidates identified with data from the Transiting Exoplanet Survey Satellite (TESS) during its two-year prime mission. We list these candidates in the TESS Objects of Interest (TOI) Catalog, which includes both new planet candidates found by TESS and previously-known planets recovered by TESS observations. We describe the process used to identify TOIs and investigate the characteristics of the new planet candidates, and discuss some notable TESS planet discoveries. The TOI Catalog includes an unprecedented number of small planet candidates around nearby bright stars, which are well-suited for detailed follow-up observations. The TESS data products for the Prime Mission (Sectors 1-26), including the TOI Catalog, light curves, full-frame images, and target pixel files, are publicly available on the Mikulski Archive for Space Telescopes.
Published: 2022

112. TOI-132 b: A short-period planet in the Neptune desert transiting a V = 11.3 G-type star★

Author: MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Fausnaugh, Michael, Glidden, Ana, Mireles, Ismael, Seager, Sara, Vanderspek, Roland K, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Fausnaugh, Michael, Glidden, Ana, Mireles, Ismael, Seager, Sara, and Vanderspek, Roland K
Abstract: © 2020 The Author(s). The Neptune desert is a feature seen in the radius-period plane, whereby a notable dearth of short period, Neptune-like planets is found. Here, we report the Transiting Exoplanet Survey Satellite (TESS) discovery of a new short-period planet in the Neptune desert, orbiting the G-type dwarf TYC8003-1117-1 (TOI-132). TESS photometry shows transit-like dips at the level of ∼1400 ppm occurring every ∼2.11 d. High-precision radial velocity follow-up with High Accuracy Radial Velocity Planet Searcher confirmed the planetary nature of the transit signal and provided a semi-amplitude radial velocity variation of 11.38+0.84-0.85 ms-1, which, when combined with the stellar mass of 0.97 ± 0.06 M⊙, provides a planetary mass of 22.40+1.90-1.92 M⊕. Modelling the TESS light curve returns a planet radius of 3.42+0.13-0.14 R⊕, and therefore the planet bulk density is found to be 3.08+0.44-0.46 g cm-3. Planet structure models suggest that the bulk of the planet mass is in the form of a rocky core, with an atmospheric mass fraction of 4.3+1.2-2.3 per cent. TOI-132 b is a TESS Level 1 Science Requirement candidate, and therefore priority follow-up will allow the search for additional planets in the system, whilst helping to constrain low-mass planet formation and evolution models, particularly valuable for better understanding of the Neptune desert.
Published: 2022

113. A Mini-Neptune from TESS and CHEOPS Around the 120 Myr Old AB Dor Member HIP 94235

Author: Zhou, George, primary, Wirth, Christopher P., additional, Huang, Chelsea X., additional, Venner, Alexander, additional, Franson, Kyle, additional, Quinn, Samuel N., additional, Bouma, L. G., additional, Kraus, Adam L., additional, Mann, Andrew W., additional, Newton, Elisabeth. R., additional, Dragomir, Diana, additional, Heitzmann, Alexis, additional, Lowson, Nataliea, additional, Douglas, Stephanie T., additional, Battley, Matthew, additional, Gillen, Edward, additional, Triaud, Amaury, additional, Latham, David W., additional, Howell, Steve B., additional, Hartman, J. D., additional, Tofflemire, Benjamin M., additional, Wittenmyer, Robert A., additional, Bowler, Brendan P., additional, Horner, Jonathan, additional, Kane, Stephen R., additional, Kielkopf, John, additional, Plavchan, Peter, additional, Wright, Duncan J., additional, Addison, Brett C., additional, Mengel, Matthew W., additional, Okumura, Jack, additional, Ricker, George, additional, Vanderspek, Roland, additional, Seager, Sara, additional, Jenkins, Jon M., additional, Winn, Joshua N., additional, Daylan, Tansu, additional, Fausnaugh, Michael, additional, and Kunimoto, Michelle, additional
Published: 2022
Full Text: View/download PDF

114. A low-eccentricity migration pathway for a 13-h-period Earth analogue in a four-planet system

Author: Serrano, Luisa Maria, primary, Gandolfi, Davide, additional, Mustill, Alexander J., additional, Barragán, Oscar, additional, Korth, Judith, additional, Dai, Fei, additional, Redfield, Seth, additional, Fridlund, Malcolm, additional, Lam, Kristine W. F., additional, Díaz, Matías R., additional, Grziwa, Sascha, additional, Collins, Karen A., additional, Livingston, John H., additional, Cochran, William D., additional, Hellier, Coel, additional, Bellomo, Salvatore E., additional, Trifonov, Trifon, additional, Rodler, Florian, additional, Alarcon, Javier, additional, Jenkins, Jon M., additional, Latham, David W., additional, Ricker, George, additional, Seager, Sara, additional, Vanderspeck, Roland, additional, Winn, Joshua N., additional, Albrecht, Simon, additional, Collins, Kevin I., additional, Csizmadia, Szilárd, additional, Daylan, Tansu, additional, Deeg, Hans J., additional, Esposito, Massimiliano, additional, Fausnaugh, Michael, additional, Georgieva, Iskra, additional, Goffo, Elisa, additional, Guenther, Eike, additional, Hatzes, Artie P., additional, Howell, Steve B., additional, Jensen, Eric L. N., additional, Luque, Rafael, additional, Mann, Andrew W., additional, Murgas, Felipe, additional, Osborne, Hannah L. M., additional, Palle, Enric, additional, Persson, Carina M., additional, Rowden, Pam, additional, Rudat, Alexander, additional, Smith, Alexis M. S., additional, Twicken, Joseph D., additional, Van Eylen, Vincent, additional, and Ziegler, Carl, additional
Published: 2022
Full Text: View/download PDF

115. The Curious Case of ASASSN-20hx: A Slowly Evolving, UV- and X-Ray-Luminous, Ambiguous Nuclear Transient

Author: Hinkle, Jason T., primary, Holoien, Thomas W.-S., additional, Shappee, Benjamin. J., additional, Neustadt, Jack M. M., additional, Auchettl, Katie, additional, Vallely, Patrick J., additional, Shahbandeh, Melissa, additional, Kluge, Matthias, additional, Kochanek, Christopher S., additional, Stanek, K. Z., additional, Huber, Mark E., additional, Post, Richard S., additional, Bersier, David, additional, Ashall, Christopher, additional, Tucker, Michael A., additional, Williams, Jonathan P., additional, de Jaeger, Thomas, additional, Do, Aaron, additional, Fausnaugh, Michael, additional, Gruen, Daniel, additional, Hopp, Ulrich, additional, Myles, Justin, additional, Obermeier, Christian, additional, Payne, Anna V., additional, and Thompson, Todd A., additional
Published: 2022
Full Text: View/download PDF

116. The TESS Faint-star Search: 1617 TOIs from the TESS Primary Mission

Author: Kunimoto, Michelle, primary, Daylan, Tansu, additional, Guerrero, Natalia, additional, Fong, William, additional, Bryson, Steve, additional, Ricker, George R., additional, Fausnaugh, Michael, additional, Huang, Chelsea X., additional, Sha, Lizhou, additional, Shporer, Avi, additional, Vanderburg, Andrew, additional, Vanderspek, Roland K., additional, and Yu, Liang, additional
Published: 2022
Full Text: View/download PDF

117. Complex Modulation of Rapidly Rotating Young M Dwarfs: Adding Pieces to the Puzzle

Author: Günther, Maximilian N., primary, Berardo, David A., additional, Ducrot, Elsa, additional, Murray, Catriona A., additional, Stassun, Keivan G., additional, Olah, Katalin, additional, Bouma, L. G., additional, Rappaport, Saul, additional, Winn, Joshua N., additional, Feinstein, Adina D., additional, Matthews, Elisabeth C., additional, Sebastian, Daniel, additional, Rackham, Benjamin V., additional, Seli, Bálint, additional, J. Triaud, Amaury H. M., additional, Gillen, Edward, additional, Levine, Alan M., additional, Demory, Brice-Olivier, additional, Gillon, Michaël, additional, Queloz, Didier, additional, Ricker, George R., additional, Vanderspek, Roland K., additional, Seager, Sara, additional, Latham, David W., additional, Jenkins, Jon M., additional, Brasseur, C. E., additional, Colón, Knicole D., additional, Daylan, Tansu, additional, Delrez, Laetitia, additional, Fausnaugh, Michael, additional, Garcia, Lionel J., additional, Jayaraman, Rahul, additional, Jehin, Emmanuel, additional, Kristiansen, Martti H., additional, Kruijssen, J. M. Diederik, additional, Pedersen, Peter Pihlmann, additional, Pozuelos, Francisco J., additional, Rodriguez, Joseph E., additional, Wohler, Bill, additional, and Zhan, Zhuchang, additional
Published: 2022
Full Text: View/download PDF

118. A 20 Second Cadence View of Solar-type Stars and Their Planets with TESS: Asteroseismology of Solar Analogs and a Recharacterization of π Men c

Author: Huber, Daniel, primary, White, Timothy R., additional, Metcalfe, Travis S., additional, Chontos, Ashley, additional, Fausnaugh, Michael M., additional, Ho, Cynthia S. K., additional, Van Eylen, Vincent, additional, Ball, Warrick H., additional, Basu, Sarbani, additional, Bedding, Timothy R., additional, Benomar, Othman, additional, Bossini, Diego, additional, Breton, Sylvain, additional, Buzasi, Derek L., additional, Campante, Tiago L., additional, Chaplin, William J., additional, Christensen-Dalsgaard, Jørgen, additional, Cunha, Margarida S., additional, Deal, Morgan, additional, García, Rafael A., additional, García Muñoz, Antonio, additional, Gehan, Charlotte, additional, González-Cuesta, Lucía, additional, Jiang, Chen, additional, Kayhan, Cenk, additional, Kjeldsen, Hans, additional, Lundkvist, Mia S., additional, Mathis, Stéphane, additional, Mathur, Savita, additional, Monteiro, Mário J. P. F. G., additional, Nsamba, Benard, additional, Ong, Jia Mian Joel, additional, Pakštienė, Erika, additional, Serenelli, Aldo M., additional, Silva Aguirre, Victor, additional, Stassun, Keivan G., additional, Stello, Dennis, additional, Norgaard Stilling, Sissel, additional, Lykke Winther, Mark, additional, Wu, Tao, additional, Barclay, Thomas, additional, Daylan, Tansu, additional, Günther, Maximilian N., additional, Hermes, J. J., additional, Jenkins, Jon M., additional, Latham, David W., additional, Levine, Alan M., additional, Ricker, George R., additional, Seager, Sara, additional, Shporer, Avi, additional, Twicken, Joseph D., additional, Vanderspek, Roland K., additional, and Winn, Joshua N., additional
Published: 2022
Full Text: View/download PDF

119. TESS Science Processing Operations Center Pipeline Status and Updates

Author: Jenkins, Jon M., Twicken, Joseph D., Caldwell, Douglas A., Ting, Eric B., Tenenbaum, Peter, Smith, Jeffrey C., Wohler, Bill, Rose, Mark, Henze, Christopher E., Fausnaugh, Michael, Burke, Christopher J., Vanderspek, Roland, and Hounsell, Rebekah
Subjects: exoplanets, TESS Mission, science pipelines, transit photometry
Abstract: The past eighteen months have seen a number of important changes for the TESS Science Processing Operations Center (SPOC) and our archival data products as TESS embarked upon its first extended mission. First, the SPOC developed and deployed a new 20-sec cadence pipeline, promising to unveil exciting new astrophysics at these short timescales for up to 1000 targets per observing sector. We also developed an FFI light curve pipeline that creates light curves and associated data products for up to 160,000 targets in each sector and archive these as High-Level Science Products (HLSP) at the Mikulski Archive for Space Telescopes (MAST). Soon we plan to perform transiting planet searches on these light curves and to release Data Validation reports and associated data products to the MAST. We also present results from the first multi-year transiting planet search of sectors 1 through 36. Finally, we discuss major changes to the SPOC pipeline that motivated the reprocessing of the first year of data, including the application of target- and cadence-specific scattered light flags, and an update to the sky background correction algorithm to mitigate bias in the original algorithm for dim and/or severely crowded stars. The TESS Mission is funded by NASA’s Science Mission Directorate.
Published: 2021
Full Text: View/download PDF

120. Uncovering Dwarf AGN With TESS

Author: Treiber, Helena P., Hinkle, Jason T., Fausnaugh, Michael M., Shappee, Benjamin J., Vallely, Patrick J., and ASAS-SN-TESS Team
Subjects: Accretion, Astrophysics::High Energy Astrophysical Phenomena, Extragalactic Astrophysics, Active Galactic Nuclei, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Supermassive Black Holes, Astrophysics::Galaxy Astrophysics
Abstract: We present the results of a systematic search for AGN in TESS light curves of dwarf galaxies. Evidence of short-term flux changes in dwarf galaxies can reveal an AGN even when emission line ratios fail to do so. Studies of dwarf AGN are essential for a general understanding of the relationship between black hole and galaxy evolution. The timescale from the commonly-used damped random walk model has been shown to correlate with black hole mass, but further studies are required to understand the physical processes driving this empirical model’s effectiveness. Partially because of this timescale relation, TESS is a unique tool for the identification of dwarf AGN; a light curve from a single sector can reveal adequate variability. We demonstrate a successful methodology that accounts for TESS systematics and contamination by variable stars. The newly-identified AGN help populate scaling relations at the low-mass end and demonstrate the crucial role of TESS in studies of dwarf AGN and AGN in general., {"references":["Baldassare et al. (2020). A Search for Optical AGN Variability in 35,000 Low-mass Galaxies with the Palomar Transient Factory","Burke et al. (2020). Optical Variability of the Dwarf AGN NGC 4395 from the Transiting Exoplanet Survey Satellite","Fausnaugh et al. (2021). Early-time Light Curves of Type Ia Supernovae Observed with TESS","Tonry et al. (2018). The ATLAS All-Sky Stellar Reference Catalog","Heinze et al. (2018). A First Catalog of Variable Stars Measured by the Asteroid Terrestrial-impact Last Alert System (ATLAS)","Jayasinghe et al. (2021). The ASAS-SN catalogue of variable stars IX: The spectroscopic properties of Galactic variable stars","Baldwin et al. (1981). Classification parameters for the emission-line spectra of extragalactic objects.","Fernandes et al. (2011). A comprehensive classification of galaxies in the Sloan Digital Sky Survey: how to tell true from fake AGN?"]}
Published: 2021
Full Text: View/download PDF

121. The Stellar and Observational Properties of the TESS Prime Mission 2-min Targets

Author: Pepper, Joshua, Barclay, Thomas, Bouma, Luke G., Burke, Christopher J., Fausnaugh, Michael, Gaudi, B. Scott, Oelkers, Ryan J., Stassun, Keivan G., Winn, Joshua N., and Adams, Elizabeth R
Subjects: TESS, Exoplanets
Abstract: TESS is not a statistical mission, but the data present a valuable opportunity for studies of exoplanet populations. In order to conduct such studies, it is essential to understand the properties of the target sample - why were specific stars selected, others excluded, using what criteria. The TESS prime mission produced light curves for the 2-min target stars, and is producing a larger light curve catalog from a subset of the stars observed at the 30-min cadence. Both sets were assembled using information from the TIC, with the bulk of the 2-min targets drawn from the ranked CTL. Here we describe the global properties of both the 2-min and 30-min sets, including their physical parameters and their observational and variability characteristics from TESS related to transit detection. We review the "K dwarf desert", the trends of photometric precision with stellar type, and the implications of the difference between the CTL population and the actual 2-min cadence population., {"references":["Stassun, Keivan et al. (2018). The TESS Input Catalog and Candidate Target List, AJ, 156, 102","Stassun, Keivan et al. (2019) The Revised TESS Input Catalog and Candidate Target List, AJ, 158, 138"]}
Published: 2021
Full Text: View/download PDF

122. Transit timings variations in the three-planet system: TOI-270

Author: Kaye, Laurel, primary, Vissapragada, Shreyas, additional, Günther, Maximilian N, additional, Aigrain, Suzanne, additional, Mikal-Evans, Thomas, additional, Jensen, Eric L N, additional, Parviainen, Hannu, additional, Pozuelos, Francisco J, additional, Abe, Lyu, additional, Acton, Jack S, additional, Agabi, Abdelkrim, additional, Alves, Douglas R, additional, Anderson, David R, additional, Armstrong, David J, additional, Barkaoui, Khalid, additional, Barragán, Oscar, additional, Benneke, Björn, additional, Boyd, Patricia T, additional, Brahm, Rafael, additional, Bruni, Ivan, additional, Bryant, Edward M, additional, Burleigh, Matthew R, additional, Casewell, Sarah L, additional, Ciardi, David, additional, Cloutier, Ryan, additional, Collins, Karen A, additional, Collins, Kevin I, additional, Conti, Dennis M, additional, Crossfield, Ian J M, additional, Crouzet, Nicolas, additional, Daylan, Tansu, additional, Dragomir, Diana, additional, Dransfield, Georgina, additional, Fabrycky, Daniel, additional, Fausnaugh, Michael, additional, Fuűrész, Gábor, additional, Gan, Tianjun, additional, Gill, Samuel, additional, Gillon, Michaël, additional, Goad, Michael R, additional, Gorjian, Varoujan, additional, Greklek-McKeon, Michael, additional, Guerrero, Natalia, additional, Guillot, Tristan, additional, Jehin, Emmanuël, additional, Jenkins, J S, additional, Lendl, Monika, additional, Kamler, Jacob, additional, Kane, Stephen R, additional, Kielkopf, John F, additional, Kunimoto, Michelle, additional, Marie-Sainte, Wenceslas, additional, McCormac, James, additional, Mékarnia, Djamel, additional, Morales, Farisa Y, additional, Moyano, Maximiliano, additional, Palle, Enric, additional, Parmentier, Vivien, additional, Relles, Howard M, additional, Schmider, François-Xavier, additional, Schwarz, Richard P, additional, Seager, S, additional, Smith, Alexis M S, additional, Tan, Thiam-Guan, additional, Taylor, Jake, additional, Triaud, Amaury H M J, additional, Twicken, Joseph D, additional, Udry, Stephane, additional, Vines, J I, additional, Wang, Gavin, additional, Wheatley, Peter J, additional, and Winn, Joshua N, additional
Published: 2021
Full Text: View/download PDF

123. The TESS–Keck Survey. VI. Two Eccentric Sub-Neptunes Orbiting HIP-97166

Author: MacDougall, Mason G., primary, Petigura, Erik A., additional, Angelo, Isabel, additional, Lubin, Jack, additional, Batalha, Natalie M., additional, Beard, Corey, additional, Behmard, Aida, additional, Blunt, Sarah, additional, Brinkman, Casey, additional, Chontos, Ashley, additional, Crossfield, Ian J. M., additional, Dai, Fei, additional, Dalba, Paul A., additional, Dressing, Courtney, additional, Fulton, Benjamin, additional, Giacalone, Steven, additional, Hill, Michelle L., additional, Howard, Andrew W., additional, Huber, Daniel, additional, Isaacson, Howard, additional, Kane, Stephen R., additional, Mayo, Andrew, additional, Močnik, Teo, additional, Akana Murphy, Joseph M., additional, Polanski, Alex, additional, Rice, Malena, additional, Robertson, Paul, additional, Rosenthal, Lee J., additional, Roy, Arpita, additional, Rubenzahl, Ryan A., additional, Scarsdale, Nicholas, additional, Turtelboom, Emma, additional, Zandt, Judah Van, additional, Weiss, Lauren M., additional, Matthews, Elisabeth, additional, Jenkins, Jon M., additional, Latham, David W., additional, Ricker, George R., additional, Seager, S., additional, Vanderspek, Roland K., additional, Winn, Joshua N., additional, Brasseur, C. E., additional, Doty, John, additional, Fausnaugh, Michael, additional, Guerrero, Natalia, additional, Henze, Chris, additional, Lund, Michael B., additional, and Shporer, Avi, additional
Published: 2021
Full Text: View/download PDF

124. A Uniform Search for Nearby Planetary Companions to Hot Jupiters in TESS Data Reveals Hot Jupiters Are Still Lonely

Author: Hord, Benjamin J., primary, Colón, Knicole D., additional, Kostov, Veselin, additional, Galgano, Brianna, additional, Ricker, George R., additional, Vanderspek, Roland, additional, Seager, S., additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Barclay, Thomas, additional, Caldwell, Douglas A., additional, Essack, Zahra, additional, Fausnaugh, Michael, additional, Guerrero, Natalia M., additional, and Wohler, Bill, additional
Published: 2021
Full Text: View/download PDF

125. Quick-look Pipeline Lightcurves for 9.1 Million Stars Observed over the First Year of the TESS Extended Mission

Author: Kunimoto, Michelle, primary, Huang, Chelsea, additional, Tey, Evan, additional, Fong, Willie, additional, Hesse, Katharine, additional, Shporer, Avi, additional, Guerrero, Natalia, additional, Fausnaugh, Michael, additional, Vanderspek, Roland, additional, and Ricker, George, additional
Published: 2021
Full Text: View/download PDF

126. TESS Data for Asteroseismology: Photometry

Author: Handberg, Rasmus, primary, Lund, Mikkel N., additional, White, Timothy R., additional, Hall, Oliver J., additional, Buzasi, Derek L., additional, Pope, Benjamin J. S., additional, Hansen, Jonas S., additional, von Essen, Carolina, additional, Carboneau, Lindsey, additional, Huber, Daniel, additional, Vanderspek, Roland K., additional, Fausnaugh, Michael M., additional, Tenenbaum, Peter, additional, and Jenkins, Jon M., additional
Published: 2021
Full Text: View/download PDF

127. TOI–1278 B: SPIRou Unveils a Rare Brown Dwarf Companion in Close-in Orbit around an M Dwarf

Author: Artigau, Étienne, primary, Hébrard, Guillaume, additional, Cadieux, Charles, additional, Vandal, Thomas, additional, Cook, Neil J., additional, Doyon, René, additional, Gagné, Jonathan, additional, Moutou, Claire, additional, Martioli, Eder, additional, Frasca, Antonio, additional, Jahandar, Farbod, additional, Lafrenière, David, additional, Malo, Lison, additional, Donati, Jean-François, additional, Cortés-Zuleta, Pía, additional, Boisse, Isabelle, additional, Delfosse, Xavier, additional, Carmona, Andres, additional, Fouqué, Pascal, additional, Morin, Julien, additional, Rowe, Jason, additional, Marino, Giuseppe, additional, Papini, Riccardo, additional, Ciardi, David R., additional, Lund, Michael B., additional, Martins, Jorge H. C., additional, Pelletier, Stefan, additional, Arnold, Luc, additional, Bouchy, François, additional, Forveille, Thierry, additional, Santos, Nuno C., additional, Bonfils, Xavier, additional, Figueira, Pedro, additional, Fausnaugh, Michael, additional, Ricker, George, additional, Latham, David W., additional, Seager, Sara, additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Ting, Eric B., additional, Torres, Guillermo, additional, and da Silva, João Gomes, additional
Published: 2021
Full Text: View/download PDF

128. The TESS Mission Target Selection Procedure

Author: Fausnaugh, Michael, primary, Morgan, Ed, additional, Vanderspek, Roland, additional, Pepper, Joshua, additional, Burke, Christopher J., additional, Levine, Alan M., additional, Rudat, Alexander, additional, Villaseñor, Jesus Noel S., additional, Vezie, Michael, additional, Goeke, Robert F., additional, Ricker, George R., additional, Latham, David W., additional, Seager, S., additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Bakos, G. Á., additional, Barclay, Thomas, additional, Berta-Thompson, Zachory K., additional, Bouma, Luke G., additional, Boyd, Patricia T., additional, Brasseur, C. E., additional, Burt, Jennifer, additional, Caldwell, Douglas A., additional, Charbonneau, David, additional, Christensen-Dalsgaard, J., additional, Clampin, Mark, additional, Collins, Karen A., additional, Colón, Knicole D., additional, De Lee, Nathan, additional, Dunham, Edward, additional, Fleming, Scott W., additional, Fong, William, additional, Garcia Soto, Aylin, additional, Scott Gaudi, B., additional, Guerrero, Natalia M., additional, Hesse, Katharine, additional, Holman, Matthew J., additional, Huang, Chelsea X., additional, Kaltenegger, Lisa, additional, Lissauer, Jack J., additional, McDermott, Scott, additional, McLean, Brian, additional, Mireles, Ismael, additional, Mullally, Susan E., additional, Oelkers, Ryan J., additional, Paegert, Martin, additional, Pál, András, additional, Quintana, Elisa V., additional, Rinehart, S. A., additional, Rodriguez, David R., additional, Rose, Mark, additional, Sasselov, Dimitar D., additional, Schlieder, Joshua E., additional, Sha, Lizhou, additional, Shporer, Avi, additional, Smith, Jeffrey C., additional, Stassun, Keivan G., additional, Tenenbaum, Peter, additional, Ting, Eric B., additional, Torres, Guillermo, additional, Twicken, Joseph D., additional, Vanderburg, Andrew, additional, Wohler, Bill, additional, and Yu, Liang, additional
Published: 2021
Full Text: View/download PDF

129. ASASSN-14ko is a Periodic Nuclear Transient in ESO 253-G003

Author: Payne, Anna V., Shappee, Benjamin J., Hinkle, Jason T., Vallely, Patrick J., Kochanek, Christopher S., Holoien, Thomas W. -S., Auchettl, Katie, Stanek, K. Z., Thompson, Todd A., Neustadt, Jack M. M., Tucker, Michael A., Armstrong, James D., Brimacombe, Joseph, Cacella, Paulo, Cornect, Robert, Denneau, Larry, Fausnaugh, Michael M., Flewelling, Heather, Grupe, Dirk, Heinze, A. N., Lopez, Laura A., Monard, Berto, Prieto, Jose L., Schneider, Adam C., Sheppard, Scott S., Tonry, John L., Weiland, Henry, Payne, Anna V., Shappee, Benjamin J., Hinkle, Jason T., Vallely, Patrick J., Kochanek, Christopher S., Holoien, Thomas W. -S., Auchettl, Katie, Stanek, K. Z., Thompson, Todd A., Neustadt, Jack M. M., Tucker, Michael A., Armstrong, James D., Brimacombe, Joseph, Cacella, Paulo, Cornect, Robert, Denneau, Larry, Fausnaugh, Michael M., Flewelling, Heather, Grupe, Dirk, Heinze, A. N., Lopez, Laura A., Monard, Berto, Prieto, Jose L., Schneider, Adam C., Sheppard, Scott S., Tonry, John L., and Weiland, Henry
Abstract: We present the discovery that ASASSN-14ko is a periodically flaring active galactic nucleus at the center of the galaxy ESO 253-G003. At the time of its discovery by the All-Sky Automated Survey for Supernovae (ASAS-SN), it was classified as a supernova close to the nucleus. The subsequent 6 yr of V- and g-band ASAS-SN observations revealed that ASASSN-14ko has nuclear flares occurring at regular intervals. The 17 observed outbursts show evidence of a decreasing period over time, with a mean period of P-0 = 114.2 0.4 days and a period derivative of P = -0.0017 +/- 0.003 . The most recent outburst in 2020 May, which took place as predicted, exhibited spectroscopic changes during the rise and had a UV bright, blackbody spectral energy distribution similar to tidal disruption events (TDEs). The X-ray flux decreased by a factor of 4 at the beginning of the outburst and then returned to its quiescent flux after similar to 8 days. The Transiting Exoplanet Survey Satellite observed an outburst during Sectors 4-6, revealing a rise time of 5.60 0.05 days in the optical and a decline that is best fit with an exponential model. We discuss several possible scenarios to explain ASASSN-14ko's periodic outbursts, but currently favor a repeated partial TDE. The next outbursts should peak in the optical on UT 2020 September 7.41.1 and UT 2020 December 26.51.4.
Published: 2021

130. GRB 191016A: A long gamma-ray burst detected by TESS

Author: National Aeronautics and Space Administration (US), Ministerio de Ciencia, Innovación y Universidades (España), Federal Government of the United States, Ministerio de Economía y Competitividad (España), European Commission, Smith, Krista Lynne, Ridden-Harper, Ryan, Fausnaugh, Michael, Daylan, Tansu, Omodei, Nicola, Racusin, Judith L., Weaver, Zachary, Barclay, Thomas, Veres, Péter, Kann, D.A., Arimoto, Makoto, National Aeronautics and Space Administration (US), Ministerio de Ciencia, Innovación y Universidades (España), Federal Government of the United States, Ministerio de Economía y Competitividad (España), European Commission, Smith, Krista Lynne, Ridden-Harper, Ryan, Fausnaugh, Michael, Daylan, Tansu, Omodei, Nicola, Racusin, Judith L., Weaver, Zachary, Barclay, Thomas, Veres, Péter, Kann, D.A., and Arimoto, Makoto
Abstract: The Transiting Exoplanet Survey Satellite (TESS) exoplanet-hunting mission detected the rising and decaying optical afterglow of GRB 191016A, a long gamma-ray burst (GRB) detected by Swift-BAT but without prompt XRT or UVOT follow-up due to proximity to the Moon. The afterglow has a late peak at least 1000 s after the BAT trigger, with a brightest-detected TESS data point at 2589.7 s post-Trigger. The burst was not detected by Fermi-LAT, but was detected by Fermi-GBM without triggering, possibly due to the gradual nature of the rising light curve. Using ground-based photometry, we estimate a photometric redshift of zphot = 3.29 ± 0.40. Combined with the high-energy emission and optical peak time derived from TESS, estimates of the bulk Lorentz factor ?BL range from 90 to 133. The burst is relatively bright, with a peak optical magnitude in ground-based follow-up of R = 15.1 mag. Using published distributions of GRB afterglows and considering the TESS sensitivity and sampling, we estimate that TESS is likely to detect ∼1 GRB afterglow per year above its magnitude limit. © 2021 Institute of Physics Publishing. All rights reserved.
Published: 2021

131. Stellar Flares from the First TESS Data Release: Exploring a New Sample of M Dwarfs

Author: Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Günther, Maximilian N, Zhan, Zhuchang, Seager, Sara, Rimmer, Paul B, Ranjan, Sukrit, Stassun, Keivan G, Oelkers, Ryan J, Daylan, Tansu, Newton, Elisabeth, Kristiansen, Martti H, Olah, Katalin, Gillen, Edward, Rappaport, Saul, Ricker, George R, Vanderspek, Roland K, Latham, David W, Winn, Joshua N, Jenkins, Jon M, Glidden, Ana, Fausnaugh, Michael, Levine, Alan M, Dittmann, Jason A, Quinn, Samuel N, Krishnamurthy, Akshata, Ting, Eric B, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, Günther, Maximilian N, Zhan, Zhuchang, Seager, Sara, Rimmer, Paul B, Ranjan, Sukrit, Stassun, Keivan G, Oelkers, Ryan J, Daylan, Tansu, Newton, Elisabeth, Kristiansen, Martti H, Olah, Katalin, Gillen, Edward, Rappaport, Saul, Ricker, George R, Vanderspek, Roland K, Latham, David W, Winn, Joshua N, Jenkins, Jon M, Glidden, Ana, Fausnaugh, Michael, Levine, Alan M, Dittmann, Jason A, Quinn, Samuel N, Krishnamurthy, Akshata, and Ting, Eric B
Abstract: © 2020. The American Astronomical Society. All rights reserved.. We perform a study of stellar flares for the 24,809 stars observed with 2 minute cadence during the first two months of the TESS mission. Flares may erode exoplanets' atmospheres and impact their habitability, but might also trigger the genesis of life around small stars. TESS provides a new sample of bright dwarf stars in our galactic neighborhood, collecting data for thousands of M dwarfs that might host habitable exoplanets. Here, we use an automated search for flares accompanied by visual inspection. Then, our public allesfitter code robustly selects the appropriate model for potentially complex flares via Bayesian evidence. We identify 1228 flaring stars, 673 of which are M dwarfs. Among 8695 flares in total, the largest superflare increased the stellar brightness by a factor of 16.1. Bolometric flare energies range from 1031.0 to 1036.9 erg, with a median of 1033.1 erg. Furthermore, we study the flare rate and energy as a function of stellar type and rotation period. We solidify past findings that fast rotating M dwarfs are the most likely to flare and that their flare amplitude is independent of the rotation period. Finally, we link our results to criteria for prebiotic chemistry, atmospheric loss through coronal mass ejections, and ozone sterilization. Four of our flaring M dwarfs host exoplanet candidates alerted on by TESS, for which we discuss how these effects can impact life. With upcoming TESS data releases, our flare analysis can be expanded to almost all bright small stars, aiding in defining criteria for exoplanet habitability.
Published: 2021

132. The TESS Objects of Interest Catalog from the TESS Prime Mission

Author: Guerrero, Natalia M., primary, Seager, S., additional, Huang, Chelsea X., additional, Vanderburg, Andrew, additional, Soto, Aylin Garcia, additional, Mireles, Ismael, additional, Hesse, Katharine, additional, Fong, William, additional, Glidden, Ana, additional, Shporer, Avi, additional, Latham, David W., additional, Collins, Karen A., additional, Quinn, Samuel N., additional, Burt, Jennifer, additional, Dragomir, Diana, additional, Crossfield, Ian, additional, Vanderspek, Roland, additional, Fausnaugh, Michael, additional, Burke, Christopher J., additional, Ricker, George, additional, Daylan, Tansu, additional, Essack, Zahra, additional, Günther, Maximilian N., additional, Osborn, Hugh P., additional, Pepper, Joshua, additional, Rowden, Pamela, additional, Sha, Lizhou, additional, Villanueva Jr., Steven, additional, Yahalomi, Daniel A., additional, Yu, Liang, additional, Ballard, Sarah, additional, Batalha, Natalie M., additional, Berardo, David, additional, Chontos, Ashley, additional, Dittmann, Jason A., additional, Esquerdo, Gilbert A., additional, Mikal-Evans, Thomas, additional, Jayaraman, Rahul, additional, Krishnamurthy, Akshata, additional, Louie, Dana R., additional, Mehrle, Nicholas, additional, Niraula, Prajwal, additional, Rackham, Benjamin V., additional, Rodriguez, Joseph E., additional, Rowden, Stephen J. L., additional, Sousa-Silva, Clara, additional, Watanabe, David, additional, Wong, Ian, additional, Zhan, Zhuchang, additional, Zivanovic, Goran, additional, Christiansen, Jessie L., additional, Ciardi, David R., additional, Swain, Melanie A., additional, Lund, Michael B., additional, Mullally, Susan E., additional, Fleming, Scott W., additional, Rodriguez, David R., additional, Boyd, Patricia T., additional, Quintana, Elisa V., additional, Barclay, Thomas, additional, Colón, Knicole D., additional, Rinehart, S. A., additional, Schlieder, Joshua E., additional, Clampin, Mark, additional, Jenkins, Jon M., additional, Twicken, Joseph D., additional, Caldwell, Douglas A., additional, Coughlin, Jeffrey L., additional, Henze, Chris, additional, Lissauer, Jack J., additional, Morris, Robert L., additional, Rose, Mark E., additional, Smith, Jeffrey C., additional, Tenenbaum, Peter, additional, Ting, Eric B., additional, Wohler, Bill, additional, Bakos, G. Á., additional, Bean, Jacob L., additional, Berta-Thompson, Zachory K., additional, Bieryla, Allyson, additional, Bouma, Luke G., additional, Buchhave, Lars A., additional, Butler, Nathaniel, additional, Charbonneau, David, additional, Doty, John P., additional, Ge, Jian, additional, Holman, Matthew J., additional, Howard, Andrew W., additional, Kaltenegger, Lisa, additional, Kane, Stephen R., additional, Kjeldsen, Hans, additional, Kreidberg, Laura, additional, Lin, Douglas N. C., additional, Minsky, Charlotte, additional, Narita, Norio, additional, Paegert, Martin, additional, Pál, András, additional, Palle, Enric, additional, Sasselov, Dimitar D., additional, Spencer, Alton, additional, Sozzetti, Alessandro, additional, Stassun, Keivan G., additional, Torres, Guillermo, additional, Udry, Stephane, additional, and Winn, Joshua N., additional
Published: 2021
Full Text: View/download PDF

133. ASASSN-14ko is a Periodic Nuclear Transient in ESO 253-G003

Author: Payne, Anna V., primary, Shappee, Benjamin J., additional, Hinkle, Jason T., additional, Vallely, Patrick J., additional, Kochanek, Christopher S., additional, Holoien, Thomas W.-S., additional, Auchettl, Katie, additional, Stanek, K. Z., additional, Thompson, Todd A., additional, Neustadt, Jack M. M., additional, Tucker, Michael A., additional, Armstrong, James D., additional, Brimacombe, Joseph, additional, Cacella, Paulo, additional, Cornect, Robert, additional, Denneau, Larry, additional, Fausnaugh, Michael M., additional, Flewelling, Heather, additional, Grupe, Dirk, additional, Heinze, A. N., additional, Lopez, Laura A., additional, Monard, Berto, additional, Prieto, Jose L., additional, Schneider, Adam C., additional, Sheppard, Scott S., additional, Tonry, John L., additional, and Weiland, Henry, additional
Published: 2021
Full Text: View/download PDF

134. GRB 191016A: A Long Gamma-Ray Burst Detected by TESS

Author: Smith, Krista Lynne, primary, Ridden-Harper, Ryan, additional, Fausnaugh, Michael, additional, Daylan, Tansu, additional, Omodei, Nicola, additional, Racusin, Judith, additional, Weaver, Zachary, additional, Barclay, Thomas, additional, Veres, Péter, additional, Kann, D. Alexander, additional, and Arimoto, Makoto, additional
Published: 2021
Full Text: View/download PDF

135. The Multiplanet System TOI-421*

Author: Carleo, Ilaria, Gandolfi, Davide, Barragan, Oscar, Livingston, John H., Persson, Carina M., Lam, Kristine W. F., Vidotto, Aline, Lund, Michael B., D'Angelo, Carolina Villarreal, Collins, Karen A., Fossati, Luca, Howard, Andrew W., Kubyshkina, Daria, Brahm, Rafael, Oklopcic, Antonija, Molliere, Paul, Redfield, Seth, Serrano, Luisa Maria, Dai, Fei, Fridlund, Malcolm, Borsa, Francesco, Korth, Judith, Esposito, Massimiliano, Diaz, Matias R., Nielsen, Louise Dyregaard, Hellier, Coel, Mathur, Savita, Deeg, Hans J., Hatzes, Artie P., Benatti, Serena, Rodler, Florian, Alarcon, Javier, Spina, Lorenzo, Santos, Angela R. G., Georgieva, Iskra, Garcia, Rafael A., Gonzalez-Cuesta, Lucia, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Albrecht, Simon, Batalha, Natalie M., Beard, Corey, Boyd, Patricia T., Bouchy, Francois, Burt, Jennifer A., Butler, R. Paul, Cabrera, Juan, Chontos, Ashley, Ciardi, David R., Cochran, William D., Collins, Kevin, I, Crane, Jeffrey D., Crossfield, Ian, Csizmadia, Szilard, Dragomir, Diana, Dressing, Courtney, Eigmueller, Philipp, Endl, Michael, Erikson, Anders, Espinoza, Nestor, Fausnaugh, Michael, Feng, Fabo, Flowers, Erin, Fulton, Benjamin, Gonzales, Erica J., Grieves, Nolan, Grziwa, Sascha, Guenther, Eike W., Guerrero, Natalia M., Henning, Thomas, Hidalgo, Diego, Hirano, Teruyuki, Hjorth, Maria, Huber, Daniel, Isaacson, Howard, Jones, Matias, Jordan, Andres, Kabath, Petr, Kane, Stephen R., Knudstrup, Emil, Lubin, Jack, Luque, Rafael, Mireles, Ismael, Narita, Norio, Nespral, David, Niraula, Prajwal, Nowak, Grzegorz, Palle, Enric, Paetzold, Martin, Petigura, Erik A., Prieto-Arranz, Jorge, Rauer, Heike, Robertson, Paul, Rose, Mark E., Roy, Arpita, Sarkis, Paula, Schlieder, Joshua E., Segransan, Damien, Shectman, Stephen, Skarka, Marek, Smith, Alexis M. S., Smith, Jeffrey C., Stassun, Keivan, Teske, Johanna, Twicken, Joseph D., Van Eylen, Vincent, Wang, Sharon, Weiss, Lauren M., Wyttenbach, Aurelien, Carleo, Ilaria, Gandolfi, Davide, Barragan, Oscar, Livingston, John H., Persson, Carina M., Lam, Kristine W. F., Vidotto, Aline, Lund, Michael B., D'Angelo, Carolina Villarreal, Collins, Karen A., Fossati, Luca, Howard, Andrew W., Kubyshkina, Daria, Brahm, Rafael, Oklopcic, Antonija, Molliere, Paul, Redfield, Seth, Serrano, Luisa Maria, Dai, Fei, Fridlund, Malcolm, Borsa, Francesco, Korth, Judith, Esposito, Massimiliano, Diaz, Matias R., Nielsen, Louise Dyregaard, Hellier, Coel, Mathur, Savita, Deeg, Hans J., Hatzes, Artie P., Benatti, Serena, Rodler, Florian, Alarcon, Javier, Spina, Lorenzo, Santos, Angela R. G., Georgieva, Iskra, Garcia, Rafael A., Gonzalez-Cuesta, Lucia, Ricker, George R., Vanderspek, Roland, Latham, David W., Seager, Sara, Winn, Joshua N., Jenkins, Jon M., Albrecht, Simon, Batalha, Natalie M., Beard, Corey, Boyd, Patricia T., Bouchy, Francois, Burt, Jennifer A., Butler, R. Paul, Cabrera, Juan, Chontos, Ashley, Ciardi, David R., Cochran, William D., Collins, Kevin, I, Crane, Jeffrey D., Crossfield, Ian, Csizmadia, Szilard, Dragomir, Diana, Dressing, Courtney, Eigmueller, Philipp, Endl, Michael, Erikson, Anders, Espinoza, Nestor, Fausnaugh, Michael, Feng, Fabo, Flowers, Erin, Fulton, Benjamin, Gonzales, Erica J., Grieves, Nolan, Grziwa, Sascha, Guenther, Eike W., Guerrero, Natalia M., Henning, Thomas, Hidalgo, Diego, Hirano, Teruyuki, Hjorth, Maria, Huber, Daniel, Isaacson, Howard, Jones, Matias, Jordan, Andres, Kabath, Petr, Kane, Stephen R., Knudstrup, Emil, Lubin, Jack, Luque, Rafael, Mireles, Ismael, Narita, Norio, Nespral, David, Niraula, Prajwal, Nowak, Grzegorz, Palle, Enric, Paetzold, Martin, Petigura, Erik A., Prieto-Arranz, Jorge, Rauer, Heike, Robertson, Paul, Rose, Mark E., Roy, Arpita, Sarkis, Paula, Schlieder, Joshua E., Segransan, Damien, Shectman, Stephen, Skarka, Marek, Smith, Alexis M. S., Smith, Jeffrey C., Stassun, Keivan, Teske, Johanna, Twicken, Joseph D., Van Eylen, Vincent, Wang, Sharon, Weiss, Lauren M., and Wyttenbach, Aurelien
Abstract: We report the discovery of a warm Neptune and a hot sub-Neptune transiting TOI-421 (BD-14 1137, TIC 94986319), a bright (V = 9.9) G9 dwarf star in a visual binary system observed by the Transiting Exoplanet Survey Satellite (TESS) space mission in Sectors 5 and 6. We performed ground-based follow-up observations-comprised of Las Cumbres Observatory Global Telescope transit photometry, NIRC2 adaptive optics imaging, and FIbre-fed Echelle Spectrograph, CORALIE, High Accuracy Radial velocity Planet Searcher, High Resolution echelle Spectrometer, and Planet Finder Spectrograph high-precision Doppler measurements-and confirmed the planetary nature of the 16 day transiting candidate announced by the TESS team. We discovered an additional radial velocity signal with a period of five days induced by the presence of a second planet in the system, which we also found to transit its host star. We found that the inner mini-Neptune, TOI-421 b, has an orbital period of P-b = 5.19672 +/- 0.00049 days, a mass of M-b = 7.17 +/- 0.66 M-circle plus, and a radius of R-b = R-circle plus, whereas the outer warm Neptune, TOI-421 c, has a period of P-c = 16.06819 +/- 0.00035 days, a mass of M-c = 16.42(-1.04)(+1.06)M(circle plus), a radius of R-c = 5.09(-0.15)(+0.16)R(circle plus), and a density of rho(c) = 0.685(-0.072)(+0.080) cm(-3). With its characteristics, the outer planet (rho(c) = 0.685(-0.0072)(+0.080) cm(-3)) is placed in the intriguing class of the super-puffy mini-Neptunes. TOI-421 b and TOI-421 c are found to be well-suited for atmospheric characterization. Our atmospheric simulations predict significant Ly alpha transit absorption, due to strong hydrogen escape in both planets, as well as the presence of detectable CH4 in the atmosphere of TOI-421 c if equilibrium chemistry is assumed.
Published: 2020

136. Stellar Flares from the First TESS Data Release: Exploring a New Sample of M Dwarfs

Author: Günther, Maximilian N., Zhan, Zhuchang, Seager, Sara, Rimmer, Paul B., Ranjan, Sukrit, Stassun, Keivan G., Oelkers, Ryan J., Daylan, Tansu, Newton, Elisabeth, Kristiansen, Martti H., Olah, Katalin, Gillen, Edward, Rappaport, Saul, Ricker, George R., Vanderspek, Roland K., Latham, David W., Winn, Joshua N., Jenkins, Jon M., Glidden, Ana, Fausnaugh, Michael, Levine, Alan M., Dittmann, Jason A., Quinn, Samuel N., Krishnamurthy, Akshata, Ting, Eric B., Günther, Maximilian N., Zhan, Zhuchang, Seager, Sara, Rimmer, Paul B., Ranjan, Sukrit, Stassun, Keivan G., Oelkers, Ryan J., Daylan, Tansu, Newton, Elisabeth, Kristiansen, Martti H., Olah, Katalin, Gillen, Edward, Rappaport, Saul, Ricker, George R., Vanderspek, Roland K., Latham, David W., Winn, Joshua N., Jenkins, Jon M., Glidden, Ana, Fausnaugh, Michael, Levine, Alan M., Dittmann, Jason A., Quinn, Samuel N., Krishnamurthy, Akshata, and Ting, Eric B.
Abstract: We perform a study of stellar flares for the 24,809 stars observed with 2 minute cadence during the first two months of the TESS mission. Flares may erode exoplanets’ atmospheres and impact their habitability, but might also trigger the genesis of life around small stars. TESS provides a new sample of bright dwarf stars in our galactic neighborhood, collecting data for thousands of M dwarfs that might host habitable exoplanets. Here, we use an automated search for flares accompanied by visual inspection. Then, our public allesfitter code robustly selects the appropriate model for potentially complex flares via Bayesian evidence. We identify 1228 flaring stars, 673 of which are M dwarfs. Among 8695 flares in total, the largest superflare increased the stellar brightness by a factor of 16.1. Bolometric flare energies range from 1031.0 to 1036.9 erg, with a median of 1033.1 erg. Furthermore, we study the flare rate and energy as a function of stellar type and rotation period. We solidify past findings that fast rotating M dwarfs are the most likely to flare and that their flare amplitude is independent of the rotation period. Finally, we link our results to criteria for prebiotic chemistry, atmospheric loss through coronal mass ejections, and ozone sterilization. Four of our flaring M dwarfs host exoplanet candidates alerted on by TESS, for which we discuss how these effects can impact life. With upcoming TESS data releases, our flare analysis can be expanded to almost all bright small stars, aiding in defining criteria for exoplanet habitability.
Published: 2020

137. TESS Hunt for Young and Maturing Exoplanets (THYME): a planet in the 45 Myr Tucana–Horologium association

Author: Massachusetts Institute of Technology. Department of Physics, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, MIT Kavli Institute for Astrophysics and Space Research, Newton, Elisabeth R., Ricker, George R., Vanderspek, Roland K., Seager, Sara, Burke, Christopher J., Fausnaugh, Michael, Villasenor, Jesus Noel Samonte, Villeneuva, Steven, Massachusetts Institute of Technology. Department of Physics, Massachusetts Institute of Technology. Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology. Department of Aeronautics and Astronautics, MIT Kavli Institute for Astrophysics and Space Research, Newton, Elisabeth R., Ricker, George R., Vanderspek, Roland K., Seager, Sara, Burke, Christopher J., Fausnaugh, Michael, Villasenor, Jesus Noel Samonte, and Villeneuva, Steven
Abstract: Young exoplanets are snapshots of the planetary evolution process. Planets that orbit stars in young associations are particularly important because the age of the planetary system is well constrained. We present the discovery of a transiting planet larger than Neptune but smaller than Saturn in the 45 Myr Tucana-Horologium young moving group. The host star is a visual binary, and our follow-up observations demonstrate that the planet orbits the G6V primary component, DS Tuc A (HD 222259A, TIC 410214986). We first identified transits using photometry from the Transiting Exoplanet Survey Satellite (TESS; alerted as TOI 200.01). We validated the planet and improved the stellar parameters using a suite of new and archival data, including spectra from Southern Astrophysical Research/Goodman, South African Extremely Large Telescope/High Resolution Spectrograph and Las Cumbres Observatories/Network of Robotic Echelle Spectrographs; transit photometry from Spitzer; and deep adaptive optics imaging from Gemini/Gemini Planet Imager. No additional stellar or planetary signals are seen in the data. We measured the planetary parameters by simultaneously modeling the photometry with a transit model and a Gaussian process to account for stellar variability. We determined that the planetary radius is 5.70 ± 0.17 R ⊕ and that the orbital period is 8.1 days. The inclination angles of the host star's spin axis, the planet's orbital axis, and the visual binary's orbital axis are aligned within 15° to within the uncertainties of the relevant data. DS Tuc Ab is bright enough (V = 8.5) for detailed characterization using radial velocities and transmission spectroscopy. ©2019
Published: 2020

138. HD 219134 Revisited: Planet d Transit Upper Limit and Planet f Transit Nondetection with ASTERIA and TESS

Author: Seager, Sara, primary, Knapp, Mary, additional, Demory, Brice-Olivier, additional, Krishnamurthy, Akshata, additional, Huang, Chelsea X., additional, Agusti, Mariona Badenas, additional, Shporer, Avi, additional, Weisserman, Drew, additional, Becker, Juliette, additional, Vanderburg, Andrew, additional, Smith, Matthew, additional, Pong, Christopher M., additional, Bailey, Vanessa P., additional, Donner, Amanda, additional, Pasquale, Peter Di, additional, Campuzano, Brian, additional, Smith, Colin, additional, Luu, Jason, additional, Babuscia, Alessandra, additional, Bocchino, Robert L., additional, Loveland, Jessica, additional, Colley, Cody, additional, Gedenk, Tobias, additional, Kulkarni, Tejas, additional, Hughes, Kyle, additional, White, Mary, additional, Krajewski, Joel, additional, Fesq, Lorraine, additional, Ricker, George, additional, Vanderspek, Roland, additional, Latham, David W., additional, Jenkins, Jon M., additional, Winn, Joshua N., additional, Caldwell, Douglas A., additional, Collins, Karen A., additional, Dragomir, Diana, additional, Fausnaugh, Michael, additional, Glidden, Ana, additional, Schlieder, Joshua E., additional, Twicken, Joseph D., additional, and Wohler, Bill, additional
Published: 2021
Full Text: View/download PDF

139. TOI-811b and TOI-852b: New Transiting Brown Dwarfs with Similar Masses and Very Different Radii and Ages from the TESS Mission

Author: Carmichael, Theron W., primary, Quinn, Samuel N., additional, Zhou, George, additional, Grieves, Nolan, additional, Irwin, Jonathan M., additional, Stassun, Keivan G., additional, Vanderburg, Andrew M., additional, Winn, Joshua N., additional, Bouchy, Francois, additional, Brasseur, Clara E., additional, Briceño, César, additional, Caldwell, Douglas A., additional, Charbonneau, David, additional, Collins, Karen A., additional, Colon, Knicole D., additional, Eastman, Jason D., additional, Fausnaugh, Michael, additional, Fong, William, additional, Fűrész, Gábor, additional, Huang, Chelsea, additional, Jenkins, Jon M., additional, Kielkopf, John F., additional, Latham, David W., additional, Law, Nicholas, additional, Lund, Michael B., additional, Mann, Andrew W., additional, Ricker, George R., additional, Rodriguez, Joseph E., additional, Schwarz, Richard P., additional, Shporer, Avi, additional, Tenenbaum, Peter, additional, Wood, Mackenna L., additional, and Ziegler, Carl, additional
Published: 2021
Full Text: View/download PDF

140. Calibrated Full-frame Images for the TESS Quick Look Pipeline

Author: Fausnaugh, Michael M., primary, Burke, Christopher J., additional, Ricker, George R., additional, and Vanderspek, Roland, additional
Published: 2020
Full Text: View/download PDF

141. Photometry of 10 Million Stars from the First Two Years of TESS Full Frame Images: Part II

Author: Huang, Chelsea X., primary, Vanderburg, Andrew, additional, Pál, Andras, additional, Sha, Lizhou, additional, Yu, Liang, additional, Fong, Willie, additional, Fausnaugh, Michael, additional, Shporer, Avi, additional, Guerrero, Natalia, additional, Vanderspek, Roland, additional, and Ricker, George, additional
Published: 2020
Full Text: View/download PDF

142. TESS Science Processing Operations Center FFI Target List Products

Author: Caldwell, Douglas A., primary, Tenenbaum, Peter, additional, Twicken, Joseph D., additional, Jenkins, Jon M., additional, Ting, Eric, additional, Smith, Jeffrey C., additional, Hedges, Christina, additional, Fausnaugh, Michael M., additional, Rose, Mark, additional, and Burke, Christopher, additional
Published: 2020
Full Text: View/download PDF

143. KELT-25 b and KELT-26 b: A Hot Jupiter and a Substellar Companion Transiting Young A Stars Observed by TESS*

Author: Martínez, Romy Rodríguez, primary, Gaudi, B. Scott, additional, Rodriguez, Joseph E., additional, Zhou, George, additional, Labadie-Bartz, Jonathan, additional, Quinn, Samuel N., additional, Penev, Kaloyan, additional, Tan, Thiam-Guan, additional, Latham, David W., additional, Paredes, Leonardo A., additional, Kielkopf, John F., additional, Addison, Brett, additional, Wright, Duncan J., additional, Teske, Johanna, additional, Howell, Steve B., additional, Ciardi, David, additional, Ziegler, Carl, additional, Stassun, Keivan G., additional, Johnson, Marshall C., additional, Eastman, Jason D., additional, Siverd, Robert J., additional, Beatty, Thomas G., additional, Bouma, Luke, additional, Bedding, Timothy, additional, Pepper, Joshua, additional, Winn, Joshua, additional, Lund, Michael B., additional, Villanueva, Steven, additional, Stevens, Daniel J., additional, Jensen, Eric L. N., additional, Kilby, Coleman, additional, Crane, Jeffrey D., additional, Tokovinin, Andrei, additional, Everett, Mark E., additional, Tinney, C. G., additional, Fausnaugh, Michael, additional, Cohen, David H., additional, Bayliss, Daniel, additional, Bieryla, Allyson, additional, Cargile, Phillip A., additional, Collins, Karen A., additional, Conti, Dennis M., additional, Colón, Knicole D., additional, Curtis, Ivan A., additional, Depoy, D. L., additional, Evans, Phil, additional, Feliz, Dax L., additional, Gregorio, Joao, additional, Rothenberg, Jason, additional, James, David J., additional, Joner, Michael D., additional, Kuhn, Rudolf B., additional, Manner, Mark, additional, Khakpash, Somayeh, additional, Marshall, Jennifer L., additional, McLeod, Kim K., additional, Penny, Matthew T., additional, Reed, Phillip A., additional, Relles, Howard M., additional, Stephens, Denise C., additional, Stockdale, Chris, additional, Trueblood, Mark, additional, Trueblood, Pat, additional, Yao, Xinyu, additional, Zambelli, Roberto, additional, Vanderspek, Roland, additional, Seager, Sara, additional, Jenkins, Jon M., additional, Henry, Todd J., additional, James, Hodari-Sadiki, additional, Jao, Wei-Chun, additional, Wang, Sharon Xuesong, additional, Butler, Paul, additional, Thompson, Ian, additional, Shectman, Stephen, additional, Wittenmyer, Robert, additional, Bowler, Brendan P., additional, Horner, Jonathan, additional, Kane, Stephen R., additional, Mengel, Matthew W., additional, Morton, Timothy D., additional, Okumura, Jack, additional, Plavchan, Peter, additional, Zhang, Hui, additional, Scott, Nicholas J., additional, Matson, Rachel A., additional, Mann, Andrew W., additional, Dragomir, Diana, additional, Günther, Max, additional, Ting, Eric B., additional, Glidden, Ana, additional, and Quintana, Elisa V., additional
Published: 2020
Full Text: View/download PDF

144. The Multiplanet System TOI-421

Author: Carleo, Ilaria, primary, Gandolfi, Davide, additional, Barragán, Oscar, additional, Livingston, John H., additional, Persson, Carina M., additional, Lam, Kristine W. F., additional, Vidotto, Aline, additional, Lund, Michael B., additional, D’Angelo, Carolina Villarreal, additional, Collins, Karen A., additional, Fossati, Luca, additional, Howard, Andrew W., additional, Kubyshkina, Daria, additional, Brahm, Rafael, additional, Oklopčić, Antonija, additional, Mollière, Paul, additional, Redfield, Seth, additional, Serrano, Luisa Maria, additional, Dai, Fei, additional, Fridlund, Malcolm, additional, Borsa, Francesco, additional, Korth, Judith, additional, Esposito, Massimiliano, additional, Díaz, Matías R., additional, Nielsen, Louise Dyregaard, additional, Hellier, Coel, additional, Mathur, Savita, additional, Deeg, Hans J., additional, Hatzes, Artie P., additional, Benatti, Serena, additional, Rodler, Florian, additional, Alarcon, Javier, additional, Spina, Lorenzo, additional, Santos, Ângela R. G., additional, Georgieva, Iskra, additional, García, Rafael A., additional, González-Cuesta, Lucía, additional, Ricker, George R., additional, Vanderspek, Roland, additional, Latham, David W., additional, Seager, Sara, additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Albrecht, Simon, additional, Batalha, Natalie M., additional, Beard, Corey, additional, Boyd, Patricia T., additional, Bouchy, François, additional, Burt, Jennifer A., additional, Butler, R. Paul, additional, Cabrera, Juan, additional, Chontos, Ashley, additional, Ciardi, David R., additional, Cochran, William D., additional, Collins, Kevin I., additional, Crane, Jeffrey D., additional, Crossfield, Ian, additional, Csizmadia, Szilard, additional, Dragomir, Diana, additional, Dressing, Courtney, additional, Eigmüller, Philipp, additional, Endl, Michael, additional, Erikson, Anders, additional, Espinoza, Nestor, additional, Fausnaugh, Michael, additional, Feng, Fabo, additional, Flowers, Erin, additional, Fulton, Benjamin, additional, Gonzales, Erica J., additional, Grieves, Nolan, additional, Grziwa, Sascha, additional, Guenther, Eike W., additional, Guerrero, Natalia M., additional, Henning, Thomas, additional, Hidalgo, Diego, additional, Hirano, Teruyuki, additional, Hjorth, Maria, additional, Huber, Daniel, additional, Isaacson, Howard, additional, Jones, Matias, additional, Jordán, Andrés, additional, Kabáth, Petr, additional, Kane, Stephen R., additional, Knudstrup, Emil, additional, Lubin, Jack, additional, Luque, Rafael, additional, Mireles, Ismael, additional, Narita, Norio, additional, Nespral, David, additional, Niraula, Prajwal, additional, Nowak, Grzegorz, additional, Palle, Enric, additional, Pätzold, Martin, additional, Petigura, Erik A, additional, Prieto-Arranz, Jorge, additional, Rauer, Heike, additional, Robertson, Paul, additional, Rose, Mark E., additional, Roy, Arpita, additional, Sarkis, Paula, additional, Schlieder, Joshua E., additional, Ségransan, Damien, additional, Shectman, Stephen, additional, Skarka, Marek, additional, Smith, Alexis M. S., additional, Smith, Jeffrey C., additional, Stassun, Keivan, additional, Teske, Johanna, additional, Twicken, Joseph D., additional, Eylen, Vincent Van, additional, Wang, Sharon, additional, Weiss, Lauren M., additional, and Wyttenbach, Aurélien, additional
Published: 2020
Full Text: View/download PDF

145. HD 191939: Three Sub-Neptunes Transiting a Sun-like Star Only 54 pc Away

Author: Badenas-Agusti, Mariona, primary, Günther, Maximilian N., additional, Daylan, Tansu, additional, Mikal-Evans, Thomas, additional, Vanderburg, Andrew, additional, Huang, Chelsea X., additional, Matthews, Elisabeth, additional, Rackham, Benjamin V., additional, Bieryla, Allyson, additional, Stassun, Keivan G., additional, Kane, Stephen R., additional, Shporer, Avi, additional, Fulton, Benjamin J., additional, Hill, Michelle L., additional, Nowak, Grzegorz, additional, Ribas, Ignasi, additional, Pallé, Enric, additional, Jenkins, Jon M., additional, Latham, David W., additional, Seager, Sara, additional, Ricker, George R., additional, Vanderspek, Roland K., additional, Winn, Joshua N., additional, Abril-Pla, Oriol, additional, Collins, Karen A., additional, Serra, Pere Guerra, additional, Niraula, Prajwal, additional, Rustamkulov, Zafar, additional, Barclay, Thomas, additional, Crossfield, Ian J. M., additional, Howell, Steve B., additional, Ciardi, David R., additional, Gonzales, Erica J., additional, Schlieder, Joshua E., additional, Caldwell, Douglas A., additional, Fausnaugh, Michael, additional, McDermott, Scott, additional, Paegert, Martin, additional, Pepper, Joshua, additional, Rose, Mark E., additional, and Twicken, Joseph D., additional
Published: 2020
Full Text: View/download PDF

146. A remnant planetary core in the hot-Neptune desert

Author: Armstrong, David J., primary, Lopez, Théo A., additional, Adibekyan, Vardan, additional, Booth, Richard A., additional, Bryant, Edward M., additional, Collins, Karen A., additional, Deleuil, Magali, additional, Emsenhuber, Alexandre, additional, Huang, Chelsea X., additional, King, George W., additional, Lillo-Box, Jorge, additional, Lissauer, Jack J., additional, Matthews, Elisabeth, additional, Mousis, Olivier, additional, Nielsen, Louise D., additional, Osborn, Hugh, additional, Otegi, Jon, additional, Santos, Nuno C., additional, Sousa, Sérgio G., additional, Stassun, Keivan G., additional, Veras, Dimitri, additional, Ziegler, Carl, additional, Acton, Jack S., additional, Almenara, Jose M., additional, Anderson, David R., additional, Barrado, David, additional, Barros, Susana C. C., additional, Bayliss, Daniel, additional, Belardi, Claudia, additional, Bouchy, Francois, additional, Briceño, César, additional, Brogi, Matteo, additional, Brown, David J. A., additional, Burleigh, Matthew R., additional, Casewell, Sarah L., additional, Chaushev, Alexander, additional, Ciardi, David R., additional, Collins, Kevin I., additional, Colón, Knicole D., additional, Cooke, Benjamin F., additional, Crossfield, Ian J. M., additional, Díaz, Rodrigo F., additional, Mena, Elisa Delgado, additional, Demangeon, Olivier D. S., additional, Dorn, Caroline, additional, Dumusque, Xavier, additional, Eigmüller, Philipp, additional, Fausnaugh, Michael, additional, Figueira, Pedro, additional, Gan, Tianjun, additional, Gandhi, Siddharth, additional, Gill, Samuel, additional, Gonzales, Erica J., additional, Goad, Michael R., additional, Günther, Maximilian N., additional, Helled, Ravit, additional, Hojjatpanah, Saeed, additional, Howell, Steve B., additional, Jackman, James, additional, Jenkins, James S., additional, Jenkins, Jon M., additional, Jensen, Eric L. N., additional, Kennedy, Grant M., additional, Latham, David W., additional, Law, Nicholas, additional, Lendl, Monika, additional, Lozovsky, Michael, additional, Mann, Andrew W., additional, Moyano, Maximiliano, additional, McCormac, James, additional, Meru, Farzana, additional, Mordasini, Christoph, additional, Osborn, Ares, additional, Pollacco, Don, additional, Queloz, Didier, additional, Raynard, Liam, additional, Ricker, George R., additional, Rowden, Pamela, additional, Santerne, Alexandre, additional, Schlieder, Joshua E., additional, Seager, Sara, additional, Sha, Lizhou, additional, Tan, Thiam-Guan, additional, Tilbrook, Rosanna H., additional, Ting, Eric, additional, Udry, Stéphane, additional, Vanderspek, Roland, additional, Watson, Christopher A., additional, West, Richard G., additional, Wilson, Paul A., additional, Winn, Joshua N., additional, Wheatley, Peter, additional, Villasenor, Jesus Noel, additional, Vines, Jose I., additional, and Zhan, Zhuchang, additional
Published: 2020
Full Text: View/download PDF

147. TESS Data for Asteroseismology: Timing Verification

Author: Essen, Carolina von, primary, Lund, Mikkel N., additional, Handberg, Rasmus, additional, Sosa, Marina S., additional, Gadeberg, Julie Thiim, additional, Kjeldsen, Hans, additional, Vanderspek, Roland K., additional, Mortensen, Dina S., additional, Mallonn, M., additional, Mammana, L., additional, Morgan, Edward H., additional, S. Villaseñor, Jesus Noel, additional, Fausnaugh, Michael M., additional, and Ricker, George R., additional
Published: 2020
Full Text: View/download PDF

148. TOI-132 b: A short-period planet in the Neptune desert transiting a V = 11.3 G-type star★

Author: Díaz, Matías R, primary, Jenkins, James S, additional, Gandolfi, Davide, additional, Lopez, Eric D, additional, Soto, Maritza G, additional, Cortés-Zuleta, Pía, additional, Berdiñas, Zaira M, additional, Stassun, Keivan G, additional, Collins, Karen A, additional, Vines, José I, additional, Ziegler, Carl, additional, Fridlund, Malcom, additional, Jensen, Eric L N, additional, Murgas, Felipe, additional, Santerne, Alexandre, additional, Wilson, Paul A, additional, Esposito, Massimiliano, additional, Hatzes, Artie P, additional, Johnson, Marshall C, additional, Lam, Kristine W F, additional, Livingston, John H, additional, Van Eylen, Vincent, additional, Narita, Norio, additional, Briceño, Cesar, additional, Collins, Kevin I, additional, Csizmadia, Szilárd, additional, Fausnaugh, Michael, additional, Gan, Tianjun, additional, García, Rafael A, additional, Georgieva, Iska, additional, Glidden, Ana, additional, González-Cuesta, Lucía, additional, Jenkins, Jon M, additional, Latham, David W, additional, Law, Nicholas M, additional, Mann, Andrew W, additional, Mathur, Savita, additional, Mireles, Ismael, additional, Morris, Robert, additional, Pallé, Enric, additional, Persson, Carina M, additional, Ricker, George, additional, Rinehart, Stephen, additional, Rose, Mark E, additional, Seager, Sara, additional, Smith, Jeffrey C, additional, Tan, Thiam-Guan, additional, Tokovinin, Andrei, additional, Vanderburg, Andrew, additional, Vanderspek, Roland, additional, Winn, Joshua N, additional, and Yahalomi, Daniel A, additional
Published: 2020
Full Text: View/download PDF

149. Stellar Flares from the FirstTESSData Release: Exploring a New Sample of M Dwarfs

Author: Günther, Maximilian N., primary, Zhan, Zhuchang, additional, Seager, Sara, additional, Rimmer, Paul B., additional, Ranjan, Sukrit, additional, Stassun, Keivan G., additional, Oelkers, Ryan J., additional, Daylan, Tansu, additional, Newton, Elisabeth, additional, Kristiansen, Martti H., additional, Olah, Katalin, additional, Gillen, Edward, additional, Rappaport, Saul, additional, Ricker, George R., additional, Vanderspek, Roland K., additional, Latham, David W., additional, Winn, Joshua N., additional, Jenkins, Jon M., additional, Glidden, Ana, additional, Fausnaugh, Michael, additional, Levine, Alan M., additional, Dittmann, Jason A., additional, Quinn, Samuel N., additional, Krishnamurthy, Akshata, additional, and Ting, Eric B., additional
Published: 2020
Full Text: View/download PDF

150. The New EXor Outburst of ESO-H alpha 99 Observed by Gaia ATLAS and TESS

Author: Hodapp, Klaus W., Reipurth, Bo, Pettersson, Bertil, Tonry, John, Denneau, Larry, Vallely, Patrick J., Shappee, Benjamin J., Armstrong, James D., Connelley, Michael S., Kochanek, C. S., Fausnaugh, Michael, Chini, Rolf, Haas, Martin, Figaredo, Catalina Sobrino, Hodapp, Klaus W., Reipurth, Bo, Pettersson, Bertil, Tonry, John, Denneau, Larry, Vallely, Patrick J., Shappee, Benjamin J., Armstrong, James D., Connelley, Michael S., Kochanek, C. S., Fausnaugh, Michael, Chini, Rolf, Haas, Martin, and Figaredo, Catalina Sobrino
Abstract: We report photometry and spectroscopy of the outburst of the young stellar object ESO-H?99. The outburst was first noticed in Gaia alert Gaia18dvc and later by the Asteroid Terrestrial-impact Last Alert System (ATLAS). We have established the outburst light curve with archival ATLAS orange filter photometry, Gaia data, new V-band photometry, and J, H, and K-s photometry from the Infrared Imaging System (IRIS) and the United Kingdom Infrared Telescope (UKIRT). The brightness has fluctuated several times near the light curve maximum. The Transiting Exoplanet Survey Satellite (TESS) satellite observed ESO-H99 with high cadence during one of these minor minima and found brightness fluctuations on timescales of days and hours. Imaging with UKIRT shows the outline of an outflow cavity, and we find one knot of emission, now named MHO 1520, on the symmetry axis of this nebula, indicating recent collimated outflow activity from ESO-H99. Its pre-outburst SED shows a flat far-infrared spectrum, confirming its early evolutionary state and its similarity to other deeply embedded objects in the broader EXor class. The pre-outburst luminosity is 34 L, a much higher luminosity than typical EXors, indicating that ESO-H alpha 99 may be a star of intermediate mass. Infrared and optical spectroscopy show a rich emission-line spectrum, including H i lines, strong red Ca ii emission, as well as infrared CO bandhead emission, all characteristic EXors in the broadest sense. Comparison of the present spectra with an optical spectrum obtained in 1993, presumably in the quiescent state of the object, shows that during the present outburst the continuum component of the spectrum has increased notably more than the emission lines. The H alpha equivalent width during the outburst is down to one-half of its 1993 level, and shock-excited emission lines are much less prominent.
Published: 2019
Full Text: View/download PDF

Catalog

Books, media, physical & digital resources

See catalog results

Searchworks

Select search scope, currently: Articles Catalog books, media & more in Jio Institute collections Articles journal articles & other e-resources

Search

Search Constraints

Refine your results

Search Limiters

Topic

Publication Year Range

Language

Publication Type

Journal

Database

Publisher

315 results on '"Fausnaugh, Michael"'

Search Results

Catalog

Select search scope, currently: Articles

Catalog

books, media & more in Jio Institute collections

Articles

journal articles & other e-resources