المؤلفون: Jake T. Clark, Brett C. Addison, Jack Okumura, Sydney Vach, Adriana Errico, Alexis Heitzmann, Joseph E. Rodriguez, Duncan J. Wright, Mathieu Clerté, Carolyn J. Brown, Tara Fetherolf, Robert A. Wittenmyer, Peter Plavchan, Stephen R. Kane, Jonathan Horner, John F. Kielkopf, Avi Shporer, C. G. Tinney, Liu Hui-Gen, Sarah Ballard, Brendan P. Bowler, Matthew W. Mengel, George Zhou, Annette S. Lee, Avelyn David, Jessica Heim, Michele E. Lee, Verónica Sevilla, Naqsh E. Zafar, Natalie R. Hinkel, Bridgette E. Allen, Daniel Bayliss, Arthur Berberyan, Perry Berlind, Allyson Bieryla, François Bouchy, Rafael Brahm, Edward M. Bryant, Jessie L. Christiansen, David R. Ciardi, Krys N. Ciardi, Karen A. Collins, Jules Dallant, Allen B. Davis, Matías R. Díaz, Courtney D. Dressing, Gilbert A. Esquerdo, Jan-Vincent Harre, Steve B. Howell, Jon M. Jenkins, Eric L. N. Jensen, Matías I. Jones, Andrés Jordán, David W. Latham, Michael B. Lund, James McCormac, Louise D. Nielsen, Jon Otegi, Samuel N. Quinn, Don J. Radford, George R. Ricker, Richard P. Schwarz, Sara Seager, Alexis M. S. Smith, Chris Stockdale, Thiam-Guan Tan, Stéphane Udry, Roland Vanderspek, Maximilian N. Günther, Songhu Wang, Geof Wingham, Joshua N. Winn

المصدر: The Astronomical Journal, Vol 165, Iss 5, p 207 (2023)

مصطلحات موضوعية: Exoplanets, Radial velocity, Transit photometry, Dynamical evolution, Astronomy, QB1-991

الوصف: NASA’s Transiting Exoplanet Survey Satellite (TESS) mission has been uncovering a growing number of exoplanets orbiting nearby, bright stars. Most exoplanets that have been discovered by TESS orbit narrow-line, slow-rotating stars, facilitating the confirmation and mass determination of these worlds. We present the discovery of a hot Jupiter orbiting a rapidly rotating ( $v\sin \,(i)=35.1\pm 1.0$ km s ^−1 ) early F3V-dwarf, HD 115447 (TOI-778). The transit signal taken from Sectors 10 and 37 of TESS's initial detection of the exoplanet is combined with follow-up ground-based photometry and velocity measurements taken from Minerva -Australis, TRES, CORALIE, and CHIRON to confirm and characterize TOI-778 b. A joint analysis of the light curves and the radial velocity measurements yields a mass, a radius, and an orbital period for TOI-778 b of ${2.76}_{-0.23}^{+0.24}$ M _J , 1.370 ± 0.043 R _J , and ∼4.63 days, respectively. The planet orbits a bright ( V = 9.1 mag) F3-dwarf with M = 1.40 ± 0.05 M _⊙ , R = 1.70 ± 0.05 R _⊙ , and $\mathrm{log}g=4.05\pm 0.17$ . We observed a spectroscopic transit of TOI-778 b, which allowed us to derive a sky-projected spin–orbit angle of 18° ± 11°, consistent with an aligned planetary system. This discovery demonstrates the capability of smaller-aperture telescopes such as Minerva -Australis to detect the radial velocity signals produced by planets orbiting broad-line, rapidly rotating stars.

وصف الملف: electronic resource

Relation: https://doaj.org/toc/1538-3881

URL الوصول: https://doaj.org/article/c91dc3ac8b394e20b5248750c3b9aa17

المؤلفون: Brett C. Addison, Duncan J. Wright, Belinda A. Nicholson, Bryson Cale, Teo Mocnik, Daniel Huber, Peter Plavchan, Robert A. Wittenmyer, Andrew Vanderburg, William J. Chaplin, Ashley Chontos, Jake T. Clark, Jason D. Eastman, Carl Ziegler, Rafael Brahm, Bradley D. Carter, Mathieu Clerte, Nestor Espinoza, Jonathan Horner, John Bentley, Andres Jordan, Stephen R. Kane, John F. Kielkopf, Emilie Laychock, Matthew W. Mengel, Jack Okumura, Keivan G. Stassun, Timothy R. Bedding, Brendan P. Bowler, Andrius Burnelis, Sergi Blanco-Cuaresma, Michaela Collins, Ian Crossfield, Allen B. Davis, Dag Evensberget, Alexis Heitzmann, Steve B. Howell, Nicholas Law, Andrew W. Mann, Stephen C. Marsden, Rachel A. Matson, James H. O’Connor, Avi Shporer, Catherine Stevens, C. G. Tinney, Christopher Tylor, Songhu Wang, Hui Zhang, Thomas Henning, Diana Kossakowski, George Ricker, Paula Sarkis, Martin Schlecker, Pascal Torres, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Ismael Mireles, Pam Rowden, Joshua Pepper, Tansu Daylan, Joshua E. Schlieder, Karen A. Collins, Kevin I. Collins, Thiam-Guan Tan, Warrick H. Ball, Sarbani Basu, Derek L. Buzasi, Tiago L. Campante, Enrico Corsaro, L. Gonz´alez-Cuesta, Guy R. Davies, Leandro de Almeida, Jose-Dias do Nascimento Jr, Rafael A. Garcpıa, Zhao Guo, Rasmus Handberg, Saskia Hekker, Daniel R. Hey, Thomas Kallinger, Steven D. Kawaler, Cenk Kayhan, James S. Kuszlewicz, Mikkel N. Lund, Alexander Lyttle, Savita Mathur, Andrea Miglio, Benoit Mosser, Martin B. Nielsen, Aldo M. Serenelli, Victor Silva Aguirre, Nathalie Themeßl

المصدر: Monthly Notices of the Royal Astronomical Society. 502(3)

مصطلحات موضوعية: Astrophysics

الوصف: We report the discovery of a warm sub-Saturn, TOI-257b (HD 19916b), based on data from NASA’s Transiting Exoplanet Survey Satellite (TESS). The transit signal was detected by TESS and confirmed to be of planetary origin based on radial velocity observations. An analysis of the TESS photometry, the MINERVA-Australis, FEROS, and HARPS radial velocities, and the asteroseismic data of the stellar oscillations reveals that TOI-257b has a mass of M(P) = 0.138 ± 0.023 M(J) (43.9 ± 7.3 Mꚛ), a radius of R(P) = 0.639 ± 0.013 R(J) (7.16 ± 0.15 Rꚛ⁠), bulk density of 0.65 (+0.12,−0.11) (cgs), and period 18.38818 (+0.00085,−0.00084) days⁠. TOI-257b orbits a bright (V = 7.612 mag) somewhat evolved late F-type star with M⁎ = 1.390 ± 0.046 M(sun)⁠, R⁎ = 1.888 ± 0.033 R(sun)⁠, T(eff) = 6075 ± 90 K⁠, and 𝜈sin 𝑖 = 11.3 ± 0.5 km/s. Additionally, we find hints for a second non-transiting sub-Saturn mass planet on a ∼71 day orbit using the radial velocity data. This system joins the ranks of a small number of exoplanet host stars (∼100) that have been characterized with asteroseismology. Warm sub-Saturns are rare in the known sample of exoplanets, and thus the discovery of TOI-257b is important in the context of future work studying the formation and migration history of similar planetary systems.

URL الوصول: https://ntrs.nasa.gov/citations/20210015041

المؤلفون: Allen B. Davis, Songhu Wang, Matias Jones, Jason D. Eastman, Maximilian N. Günther, Keivan G. Stassun, Brett C. Addison, Karen A. Collins, Samuel N. Quinn, David W. Latham, Trifon Trifonov, Sahar Shahaf, Tsevi Mazeh, Stephen R. Kane, Norio Narita, Xian-Yu Wang, Thiam-Guan Tan, David R Ciardi, Andrei Tokovinin, Carl Ziegler, René Tronsgaard, Sarah Millholland, Bryndis Cruz, Perry Berlind, Michael L. Calkins, Gilbert A. Esquerdo, Kevin I. Collins, Dennis M. Conti, Felipe Murgas, Phil Evans, Pablo Lewin, Don J. Radford, Leonardo A. Paredes, Todd J. Henry, James Hodari-Sadiki, Michael B. Lund20, Jessie L. Christiansen20, Nicholas M. Law, Andrew W. Mann, César Briceño, Hannu Parviainen, Enric Pallé, Noriharu Watanabe, George R Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M Jenkins, Akshata Krishnamurthy, Natalie M. Batalha, Jennifer Burt, Knicole Colon, Scott Dynes, Douglas A Caldwell, Robert Morris, Christopher E. Henze, Debra A Fischer

المصدر: Astronomical Journal. 160(5)

مصطلحات موضوعية: Astronomy

الوصف: We report the discovery and confirmation of two new hot Jupiters discovered by the Transiting Exoplanet Survey Satellite(TESS): TOI 564 b and TOI 905 b. The transits of these two planets were initially observed by TESS with orbital periods of 1.651 and 3.739 days, respectively. We conducted follow-up observations of each system from the ground, including photometry in multiple filters, speckle interferometry, and radial velocity measurements. For TOI 564 b, our global fitting revealed a classical hot Jupiter with a mass of-+1.4630.0960.10MJand a radius of-+1.020.290.71RJ. Also a classical hot Jupiter, TOI 905 b has a mass of-+0.6670.0410.042MJand radius of-+1.1710.0510.053RJ. Both planets orbit Sun-like, moderately bright, mid-G dwarf stars with V11. While TOI 905 b fully transits its star, we found that TOI 564 b has a very high transit impact parameter of-+0.9940.0490.083, making it one of only∼20 known systems to exhibit a grazing transit and one of the brightest host stars among them. Therefore, TOI 564 b is one of the most attractive systems to search for additional nontransiting, smaller planets by exploiting the sensitivity of grazing transits to small changes in inclination and transit duration over a timescale of several years.

URL الوصول: https://ntrs.nasa.gov/citations/20210011940

المؤلفون: Rafael Brahm, Louise D. Nielsen, Robert A. Wittenmyer, Songhu Wang, Joseph E. Rodriguez, Néstor Espinoza Perez, Matías I. Jones, Andrés Jordán, Thomas Henning, Melissa J. Hobson, Diana Kossakowski, Felipe Rojas, Paula Sarkis, Martin Schlecker, Trifon Trifonov, Sahar Shahaf, George R Ricker, Roland Vanderspek, David W. Latham, Sara Seager, Joshua N. Winn, Jon M. Jenkins, Brett C. Addison, Gáspár Á. Bakos, Waqas Bhatti, Daniel Bayliss, Perry Berlind, Allyson Bieryla, Francois Bouchy, Brendan P. Bowler, César Briceño, Timothy M. Brown, Edward M. Bryant, Douglas A. Caldwell, David Charbonneau, Karen A. Collins, Allen B. Davis, Gilbert A. Esquerdo, Benjamin J. Fulton, Natalia M. Guerrero, Christopher E. Henze, Aleisha Hogan, Jonathan Horner, Chelsea X. Huang, Jonathan Irwin, Stephen R. Kane, John Kielkopf, Andrew W. Mann, Tsevi Mazeh, James McCormac, Curtis McCully, Matthew W. Mengel, Ismael Mireles, Jack Okumura, Peter Plavchan, Samuel N. Quinn, Markus Rabus, Sophie Saesen, Joshua E. Schlieder, Damien Segransan, Bernie Shiao, Avi Shporer, Robert J. Siverd, Keivan G. Stassun, Vincent Suc, Thiam-Guan Tan, Pascal Torres, Chris G. Tinney, Stephane Udry, Leonardo Vanzi, Michael Vezie, Jose I. Vines, Maja Vuckovic, Duncan J. Wright, Daniel Yahalomi, Abner Zapata, Hui Zhang, Carl Ziegler

المصدر: The Astronomical Journal. 160(5)

مصطلحات موضوعية: Astronomy, Astrophysics

الوصف: We present the discovery of two new 10 day period giant planets from the Transiting Exoplanet Survey Satellite mission, whose masses were precisely determined using a wide diversity of ground-based facilities. TOI-481 b and TOI-892 b have similar radii (0.99 ± 0.01 R(J) and 1.07 ± 0.02 R(J), respectively), and orbital periods (10.3311 days and 10.6266 days, respectively), but significantly different masses (1.53 ± 0.03 M(J) versus 0.95 ± 0.07 M(J), respectively). Both planets orbit metal-rich stars ([Fe/HG] = +0.26 ± 0.05 dex and [Fe/H] = +0.24 ± 0.05 for TOI-481 and TOI-892, respectively) but at different evolutionary stages. TOI-481 is a M(*) = 1.14 ± 0.02 Mꙩ, R(*) = 1.66 ± 0.02 Rꙩ G-type star (T(eff) = 5735 ± 72 K), that with an age of 6.7 Gyr, is in the turn-off point of the main sequence. TOI-892 on the other hand, is a F-type dwarf star (T(eff) = 6261 ± 80 K), which has a mass of M(*) = 1.28 ± 0.03 Mꙩ and a radius of R(*) = 1.39 ± 0.02 Rꙩ. TOI-481 b and TOI-892 b join the scarcely populated region of transiting gas giants with orbital periods longer than 10 days, which is important to constrain theories of the formation and structure of hot Jupiters.

URL الوصول: https://ntrs.nasa.gov/citations/20210012866

المؤلفون: Jake T. Clark, Brett C. Addison, Jack Okumura, Sydney Vach, Adriana Errico, Alexis Heitzmann, Joseph E. Rodriguez, Duncan J. Wright, Mathieu Clerté, Carolyn J. Brown, Tara Fetherolf, Robert A. Wittenmyer, Peter Plavchan, Stephen R. Kane, Jonathan Horner, John F. Kielkopf, Avi Shporer, C. G. Tinney, Liu Hui-Gen, Sarah Ballard, Brendan P. Bowler, Matthew W. Mengel, George Zhou, Annette S. Lee, Avelyn David, Jessica Heim, Michele E. Lee, Verónica Sevilla, Naqsh E. Zafar, Natalie R. Hinkel, Bridgette E. Allen, Daniel Bayliss, Arthur Berberyan, Perry Berlind, Allyson Bieryla, François Bouchy, Rafael Brahm, Edward M. Bryant, Jessie L. Christiansen, David R. Ciardi, Krys N. Ciardi, Karen A. Collins, Jules Dallant, Allen B. Davis, Matías R. Díaz, Courtney D. Dressing, Gilbert A. Esquerdo, Jan-Vincent Harre, Steve B. Howell, Jon M. Jenkins, Eric L. N. Jensen, Matías I. Jones, Andrés Jordán, David W. Latham, Michael B. Lund, James McCormac, Louise D. Nielsen, Jon Otegi, Samuel N. Quinn, Don J. Radford, George R. Ricker, Richard P. Schwarz, Sara Seager, Alexis M. S. Smith, Chris Stockdale, Thiam-Guan Tan, Stéphane Udry, Roland Vanderspek, Maximilian N. Günther, Songhu Wang, Geof Wingham, Joshua N. Winn

مصطلحات موضوعية: Earth and Planetary Astrophysics (astro-ph.EP), Radial velocity, Space and Planetary Science, Exoplanets, FOS: Physical sciences, Astronomy and Astrophysics, Transit photometry, Dynamical evolution, Astrophysics - Earth and Planetary Astrophysics

الوصف: NASA's Transiting Exoplanet Survey Satellite (TESS) mission, has been uncovering a growing number of exoplanets orbiting nearby, bright stars. Most exoplanets that have been discovered by TESS orbit narrow-line, slow-rotating stars, facilitating the confirmation and mass determination of these worlds. We present the discovery of a hot Jupiter orbiting a rapidly rotating ($v\sin{(i)}= 35.1\pm1.0$km/s) early F3V-dwarf, HD115447 (TOI-778). The transit signal taken from Sectors 10 and 37 of TESS's initial detection of the exoplanet is combined with follow-up ground-based photometry and velocity measurements taken from Minerva-Australis, TRES, CORALIE and CHIRON to confirm and characterise TOI-778b. A joint analysis of the light curves and the radial velocity measurements yield a mass, radius, and orbital period for TOI-778b of $2.76^{+0.24}_{-0.23}$Mjup, $1.370\pm0.043$Rjup and $\sim4.63$ days, respectively. The planet orbits a bright ($V = 9.1$mag) F3-dwarf with $M=1.40\pm0.05$Msun, $R=1.70\pm0.05$Rsun, and $\log g=4.05\pm0.17$. We observed a spectroscopic transit of TOI-778b, which allowed us to derive a sky-projected spin-orbit angle of $18^{\circ}\pm11^{\circ}$, consistent with an aligned planetary system. This discovery demonstrates the capability of smaller aperture telescopes such as Minerva-Australis to detect the radial velocity signals produced by planets orbiting broad-line, rapidly rotating stars.
18 pages, 9 figures, and 4 tables. Submitted to the Astronomical Journal

URL الوصول: https://explore.openaire.eu/search/publication?articleId=doi_dedup___::087d4524033c01735eb412127d4eedad
http://arxiv.org/abs/2212.08242

المؤلفون: Songhu Wang, Matias Jones, Avi Shporer, Benjamin J Fulton, Leonardo A. Paredes, Trifon Trifonov, Diana Kossakowski, Jason Eastman, Seth Redfield, Maximilian N. Günther, Laura Kreidberg, Chelsea X. Huang, Sarah Millholland, Darryl Seligman, Debra A Fischer, Rafael Brahm, Xian-Yu Wang, Bryndis Cruz, Todd Henry, Hodari-Sadiki James, Brett Addison, En-Si Liang, Allen B. Davis, René Tronsgaard, Keduse Worku, John M. Brewer, Martin Kürster, Hui Zhang, Charles A. Beichman, Allyson Bieryla, Timothy M. Brown, Jessie L. Christiansen, David R. Ciardi, Karen A. Collins, Gilbert A. Esquerdo, Andrew W. Howard, Howard Isaacson, David W. Latham, Tsevi Mazeh, Erik A. Petigura, Samuel N. Quinn, Sahar Shahaf, Robert J. Siverd, Florian Rodle, Sabine Reffert, Olga Zakhozhay, George R Ricker, Roland K. Vanderspek, Sara Seager, Joshua N. Winn, Jon M Jenkins, Patricia T Boyd, Gábor Fűrész, Christopher Henze, Alen M. Levine, Robert Morris, Martin Paegert, Keivan G. Stassun, Eric Bi-wen Ting, Michael L Vezie, Gregory Laughlin

المصدر: The Astronomical Journal. 157(2)

مصطلحات موضوعية: Astronomy

الوصف: We report the first confirmation of a hot Jupiter discovered by the Transiting Exoplanet Survey Satellite (TESS) mission: HD 202772A b. The transit signal was detected in the data from TESS Sector 1, and was confirmed to be of planetary origin through radial velocity (RV) measurements. HD 202772A b is orbiting a mildly evolved star with a period of 3.3 days. With an apparent magnitude of V = 8.3, the star is among the brightest and most massive known to host a hot Jupiter. Based on the 27 days of TESS photometry and RV data from the CHIRON, HARPS, and Tillinghast Reflector Echelle Spectrograph, the planet has a mass of 1.017(Sup +0.070, sub 0.068) M(J) and radius of 1.545(sup +0.052, sub -0.060) R(J), making it an inflated gas giant. HD 202772A b is a rare example of a transiting hot Jupiter around a quickly evolving star. It is also one of the most strongly irradiated hot Jupiters currently known.

URL الوصول: https://ntrs.nasa.gov/citations/20205001898

المؤلفون: Christopher Leet, Samuel H. C. Cabot, Andrew Szymkowiak, Ryan R. Petersburg, Joe Llama, Lily Zhao, Allen B. Davis, Gregory Laughlin, Debra A. Fischer, John M. Brewer, J. M. Joel Ong, Ryan T. Blackman, Gregory W. Henry

مصطلحات موضوعية: 010504 meteorology & atmospheric sciences, media_common.quotation_subject, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Planet, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Eccentricity (behavior), 010303 astronomy & astrophysics, Spectrograph, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Astronomy, Astronomy and Astrophysics, Orbital period, Radial velocity, Stars, Orbit, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Terrestrial planet, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics

الوصف: The next generation of exoplanet-hunting spectrographs should deliver up to an order of magnitude improvement in radial velocity precision over the standard 1 m/s state of the art. This advance is critical for enabling the detection of Earth-mass planets around Sun-like stars. New calibration techniques such as laser frequency combs and stabilized etalons ensure that the instrumental stability is well characterized. However, additional sources of error include stellar noise, undetected short-period planets, and telluric contamination. To understand and ultimately mitigate error sources, the contributing terms in the error budget must be isolated to the greatest extent possible. Here, we introduce a new high cadence radial velocity program, the EXPRES 100 Earths program, which aims to identify rocky planets around bright, nearby G and K dwarfs. We also present a benchmark case: the 62-d orbit of a Saturn-mass planet orbiting the chromospherically quiet star, HD 3651. The combination of high eccentricity (0.6) and a moderately long orbital period, ensures significant dynamical clearing of any inner planets. Our Keplerian model for this planetary orbit has a residual RMS of 58 cm/s over a $\sim 6$ month time baseline. By eliminating significant contributors to the radial velocity error budget, HD 3651 serves as a standard for evaluating the long term precision of extreme precision radial velocity (EPRV) programs.
Comment: 11 pages, 6 figures, accepted for publication in Astronomical Journal

URL الوصول: https://explore.openaire.eu/search/publication?articleId=doi_dedup___::064b58c0b269b9928631082af556cb9e

المؤلفون: René Tronsgaard, David Ehrenreich, Lily Zhao, Samuel H. C. Cabot, Daniel Kitzmann, Debra A. Fischer, Allen B. Davis, Heather M. Cegla, Kevin Heng, Lars A. Buchhave, Vincent Bourrier, Christophe Lovis, H. Jens Hoeijmakers, Simon L. Grimm

المصدر: Jens Hoeijmakers, H, Cabot, S H C, Zhao, L, Buchhave, L A, Tronsgaard, R, Davis, A B, Kitzmann, D, Grimm, S L, Cegla, H M, Bourrier, V, Ehrenreich, D, Heng, K, Lovis, C & Fischer, D A 2020, ' High-resolution transmission spectroscopy of MASCARA-2 b with EXPRES ', Astronomy and Astrophysics, vol. 641, A120 . https://doi.org/10.1051/0004-6361/202037437
Astronomy & Astrophysics

مصطلحات موضوعية: High resolution, FOS: Physical sciences, Astrophysics, Mascara, 01 natural sciences, spectroscopic [Techniques], Transmission spectroscopy, Optics, 0103 physical sciences, spectrographs [Instrumentation], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, business.industry, Astronomy and Astrophysics, 3. Good health, gaseous planets [Planets and satellites], 13. Climate action, Space and Planetary Science, atmospheres [Planets and satellites], Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics

الوصف: We report detections of atomic species in the atmosphere of MASCARA-2 b, using the first transit observations obtained with the newly commissioned EXPRES spectrograph. EXPRES is a highly stabilised optical echelle spectrograph, designed to detect stellar reflex motions with amplitudes down to 30 cm/s, and was recently deployed at the Lowell Discovery Telescope. By analysing the transmission spectrum of the ultra-hot Jupiter MASCARA-2 b using the cross-correlation method, we confirm previous detections of Fe I, Fe II and Na I, which likely originate in the upper regions of the inflated atmosphere. In addition, we report significant detections of Mg I and Cr II. The absorption strengths change slightly with time, possibly indicating different temperatures and chemistry in the day-side and night-side terminators. Using the effective stellar line-shape variation induced by the transiting planet, we constrain the projected spin-orbit misalignment of the system to $1.6\pm3.1$ degrees, consistent with an aligned orbit. We demonstrate that EXPRES joins a suite of instruments capable of phase-resolved spectroscopy of exoplanet atmospheres.
Accepted for publication in A&A, 20 pages, 22 figures

وصف الملف: application/pdf

URL الوصول: https://explore.openaire.eu/search/publication?articleId=doi_dedup___::93d35b218336ad87068533221ec42a86
https://orbit.dtu.dk/en/publications/5dce1623-3d81-44d1-ab03-24b05759fc16

المؤلفون: Andrés Jordán, Derek Buzasi, K. I. Collins, Joshua Pepper, Jon M. Jenkins, Alexander Lyttle, Martin Schlecker, Ismael Mireles, Sara Seager, Brett C. Addison, Andrea Miglio, Jack Okumura, Savita Mathur, Christopher Tylor, Daniel R. Hey, Victor Silva Aguirre, Zhao Guo, Tansu Daylan, Paula Sarkis, Mikkel N. Lund, J. S. Bentley, Martin Bo Nielsen, Joshua E. Schlieder, Keivan G. Stassun, Aldo Serenelli, Jonathan Horner, Stephen R. Kane, Tiago L. Campante, B. D. Carter, Joshua N. Winn, Hui Zhang, Diana Kossakowski, Thomas Henning, Brendan P. Bowler, Rasmus Handberg, Jake T. Clark, Warrick H. Ball, Matthew W. Mengel, Pamela Rowden, L. González-Cuesta, Karen A. Collins, Andrew W. Mann, Nicholas M. Law, John F. Kielkopf, B. Mosser, Daniel Huber, Ian J. M. Crossfield, Mathieu Clerte, Michaela Collins, Ashley Chontos, Songhu Wang, Belinda A. Nicholson, Pascal Torres, Thomas Kallinger, Robert A. Wittenmyer, Stephen C. Marsden, Andrew Vanderburg, Dag Evensberget, N. Themeßl, Rachel A. Matson, José Dias do Nascimento, David W. Latham, Cenk Kayhan, Timothy R. Bedding, Allen B. Davis, Emilie Laychock, J. O'Connor, Néstor Espinoza, B. Cale, Andrius Burnelis, S. Hekker, Steven D. Kawaler, Avi Shporer, Duncan J. Wright, Sarbani Basu, Peter Plavchan, James S. Kuszlewicz, Guy R. Davies, Teo Mocnik, Leandro de Almeida, Jason D. Eastman, Carl Ziegler, Rafael Brahm, Enrico Corsaro, William J. Chaplin, C. G. Tinney, Catherine Stevens, Rafael A. García, Sergi Blanco-Cuaresma, Steve B. Howell, Alexis Heitzmann, Roland Vanderspek, Thiam-Guan Tan, George R. Ricker

المساهمون: Addison, Brett C, Wright, Duncan J, Nicholson, Belinda A, Cale, Bryson, Mocnik, Teo, Huber, Daniel, Plavchan, Peter, Wittenmyer, Robert A, Vanderburg, Andrew, Chaplin, William J, Chontos, Ashley, Clark, Jake T, Eastman, Jason D, Ziegler, Carl, Brahm, Rafael, Carter, Bradley D, Clerte, Mathieu, Espinoza, Néstor, Horner, Jonathan, Bentley, John, Jordán, André, Kane, Stephen R, Kielkopf, John F, Laychock, Emilie, Mengel, Matthew W, Okumura, Jack, Stassun, Keivan G, Bedding, Timothy R, Bowler, Brendan P, Burnelis, Andriu, Blanco-Cuaresma, Sergi, Collins, Michaela, Crossfield, Ian, Davis, Allen B, Evensberget, Dag, Heitzmann, Alexi, Howell, Steve B, Law, Nichola, Mann, Andrew W, Marsden, Stephen C, Matson, Rachel A, O’Connor, James H, Shporer, Avi, Stevens, Catherine, Tinney, C G, Tylor, Christopher, Wang, Songhu, Zhang, Hui, Henning, Thoma, Kossakowski, Diana, Ricker, George, Sarkis, Paula, Schlecker, Martin, Torres, Pascal, Vanderspek, Roland, Latham, David W, Seager, Sara, Winn, Joshua N, Jenkins, Jon M, Mireles, Ismael, Rowden, Pam, Pepper, Joshua, Daylan, Tansu, Schlieder, Joshua E, Collins, Karen A, Collins, Kevin I, Tan, Thiam-Guan, Ball, Warrick H, Basu, Sarbani, Buzasi, Derek L, Campante, Tiago L, Corsaro, Enrico, González-Cuesta, L, Davies, Guy R, de Almeida, Leandro, do Nascimento, Jose-Dia, García, Rafael A, Guo, Zhao, Handberg, Rasmu, Hekker, Saskia, Hey, Daniel R, Kallinger, Thoma, Kawaler, Steven D, Kayhan, Cenk, S. Kuszlewicz, Jame, Lund, Mikkel N, Lyttle, Alexander, Mathur, Savita, Miglio, Andrea, Mosser, Benoit, Nielsen, Martin B, Serenelli, Aldo M, Aguirre, Victor Silva, Themeßl, Nathalie, National Aeronautics and Space Administration (US), National Science Foundation (US), Danish National Research Foundation, National Natural Science Foundation of China, Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, European Commission, Centre National D'Etudes Spatiales (France), Ministerio de Economía y Competitividad (España), Kavli Institute for Theoretical Physics, Independent Research Fund Denmark, Carlsberg Foundation, Addison, Brett C., Wright, Duncan J., Nicholson, Belinda A., Wittenmyer, Robert A., Chaplin, William J., Clark, Jake T., Eastman, Jason D., Carter, Bradley D., Kane, Stephen R., Kielkopf, John F., Mengel, Matthew W., Stassun, Keivan G., Bedding, Timothy R., Bowler, Brendan P., Davis, Allen B., Howell, Steve B., Mann, Andrew W., Marsden, Stephen C., Matson, Rachel A., O'Connor, Jame, Tinney, C. G., Latham, David W., Winn, Joshua N., Jenkins, Jon M., Schlieder, Joshua E., Collins, Karen A., Collins, Kevin I., Ball, Warrick H., Buzasi, Derek L., Campante, Tiago L., González-Cuesta, Lucía, Davies, Guy R., do Nascimento, Jose-Dias, Jr., García, Rafael A., Hey, Daniel R., Kawaler, Steven D., Kuszlewicz, James S., Lund, Mikkel N., Nielsen, Martin B., Serenelli, Aldo M., Silva Aguirre, Victor

المصدر: Digital.CSIC. Repositorio Institucional del CSIC
instname
Addison, B C, Wright, D J, Nicholson, B A, Cale, B, Mocnik, T, Huber, D, Plavchan, P, Wittenmyer, R A, Vanderburg, A, Chaplin, W J, Chontos, A, Clark, J T, Eastman, J D, Ziegler, C, Brahm, R, Carter, B D, Clerte, M, Espinoza, N, Horner, J, Bentley, J, Kane, S R, Kielkopf, J F, Laychock, E, Mengel, M W, Okumura, J, Stassun, K G, Bedding, T R, Bowler, B P, Burnelis, A, Collins, M, Crossfield, I, Davis, A B, Evensberget, D, Heitzmann, A, Howell, S B, Law, N, Mann, A W, Marsden, S, O'Connor, J, Shporer, A, Stevens, C, Tinney, C G, Tylor, C, Wang, S, Zhang, H, Henning, T, Kossakowski, D, Ricker, G, Sarkis, P, Vanderspek, R, Latham, D W, Seager, S, Winn, J N, Jenkins, J M, Mireles, I, Rowden, P, Pepper, J, Daylan, T, Schlieder, J E, Collins, K A, Collins, K I, Tan, T-G, Ball, W H, Basu, S, Buzasi, D L, Campante, T L, Corsaro, E, González-Cuesta, L, Davies, G R, a, R A G, Guo, Z, Handberg, R, Hekker, S, Hey, D R, Kallinger, T, Kawaler, S D, Kayhan, C, Kuszlewicz, J S, Lund, M N, Lyttle, A, Mathur, S, Miglio, A, Mosser, B, Nielsen, M B, Serenelli, A M, Aguirre, V S & Themessl, N 2021, ' TOI-257b (HD 19916b) : a warm sub-saturn orbiting an evolved F-type star ', Monthly Notices of the Royal Astronomical Society, vol. 502, no. 3, pp. 3704-3722 . https://doi.org/10.1093/mnras/staa3960
arXiv

مصطلحات موضوعية: astro-ph.SR, Star (game theory), FOS: Physical sciences, Context (language use), Astrophysics, asteroseismology, Type (model theory), 01 natural sciences, Asteroseismology, spectroscopic [Techniques], techniques: photometric, stars: individual (TIC 200723869/TOI-257), 0103 physical sciences, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, Earth and Planetary Astrophysics (astro-ph.EP), individual (TIC 200723869/TOI-257) [Stars], radial velocities [Techniques], 010308 nuclear & particles physics, photometric [Techniques], techniques: radial velocitie, Astronomy and Astrophysics, Planetary system, planetary system, Exoplanet, Radial velocity, Stars, Planetary systems, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Techniques: radial velocities, astro-ph.EP, techniques: spectroscopic, Astrophysics - Earth and Planetary Astrophysics

الوصف: We report the discovery of a warm sub-Saturn, TOI-257b (HD 19916b), based on data from NASA's Transiting Exoplanet Survey Satellite (TESS). The transit signal was detected by TESS and confirmed to be of planetary origin based on radial velocity observations. An analysis of the TESS photometry, the Minerva-Australis, FEROS, and HARPS radial velocities, and the asteroseismic data of the stellar oscillations reveals that TOI-257b has a mass of MP = 0.138 ± 0.023 M J (43.9 ± 7.3, M⊕), a radius of RP = 0.639 ± 0.013 R J (7.16 ± 0.15, R ⊕), bulk density of 0.65+0.12-0.11 (cgs), and period 18.38818 +0.00085 -0.00084 days. TOI-257b orbits a bright (V = 7.612 mag) somewhat evolved late F-type star with M∗ = 1.390 ± 0.046 rm M sun, R∗ = 1.888 ± 0.033 Rsun, Teff = 6075 ± 90 rm K, and vsin i = 11.3 ± 0.5 km s-1. Additionally, we find hints for a second non-transiting sub-Saturn mass planet on a ∼71 day orbit using the radial velocity data. This system joins the ranks of a small number of exoplanet host stars (∼100) that have been characterized with asteroseismology. Warm sub-Saturns are rare in the known sample of exoplanets, and thus the discovery of TOI-257b is important in the context of future work studying the formation and migration history of similar planetary systems.
Daniel Huber acknowledges support by the National Aeronautics and Space Administration through the TESS Guest Investigator Program (80NSSC18K1585) and by the National Science Foundation (AST-1717000). Ashley Chontos acknowledges support from the National Science Foundation through the Graduate Research Fellowship Program (DGE 1842402). William J. Chaplin, Warrick H. Ball, Martin B. Nielsen, and Andrea Miglio. acknowledge support from the Science and Technology Facilities Council and UK Space Agency. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant DNRF106). Rafael Brahm acknowledges support from National Fund for Scientific and Technological Development Post-doctoral Fellowship Project 3180246, and from the Millennium Institute of Astrophysics (MAS). H.Z. Hui Zhang is supported by the Natural Science Foundation of China (NSFC grants 11673011, 11933001). Andres Jordan acknowledges support from FONDECYT project 1171208 and by the Ministry for the Economy, Development, and Tourism’s Programa Iniciativa Científica Milenio through grant IC 120009, awarded to the Millennium Institute of Astrophysics (MAS). Aldo M. Serenelli is partially supported by grants ESP2017-82674-R (Spanish Government) and 2017-SGR-1131 (Generalitat de Catalunya). Andrea Miglio acknowledges support from the European Research Council Consolidator Grant funding scheme (project ASTEROCHRONOMETRY, G.A. number 772293). Rafael A. Garcia acknowledges the support of the PLAnetary Transits and Oscillations of stars grant from the Centre National d'Études Spatiales. Savita Mathur acknowledges support from the Spanish Ministry with the Ramon y Cajal fellowship number RYC-2015-17697. Tiago L. Campante acknowledges support from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 792848 (PULSATION). This work was supported by Foundation of Science and Technology/Ministry of Science, Technology and Higher Education through national funds (UID/FIS/04434/2019). Enrico Corsaro is funded by the European Union’s Horizon 2020 research and innovation program under the Marie Sklodowska-Curie grant agreement No. 664931. L. González-Cuesta thanks the support from grant FPI-SO from the Spanish Ministry of Economy and Competitiveness (MINECO) (research project SEV-2015-0548-17-2 and predoctoral contract BES-2017-082610). Sarbani Basu acknowledges NASA grant NNX16AI09G and NSF grant AST-1514676. Ian J. M. Crossfield acknowledges support from the NSF through grant AST-1824644, and from NASA through Caltech/JPL grant RSA-1610091. Tansu Daylan acknowledges support from MIT’s Kavli Institute as a Kavli postdoctoral fellow. Derek L. Buzasi acknowledges support from NASA through the TESS Guest Investigator program (80NSSC19K0385). Cenk Kayhan acknowledges support by Erciyes University Scientific Research Projects Coordination Unit under grant number MAP-2020-9749. Emilie Laychock and Michaela Collins acknowledge support by the National Science Foundation under grant 1559487. Victor Silva Aguirre acknowledges support from the Independent Research Fund Denmark (Research grant 7027-00096B) and the Carlsberg Foundation (grant agreement CF19-0649).

وصف الملف: ELETTRONICO; application/pdf

URL الوصول: https://explore.openaire.eu/search/publication?articleId=doi_dedup___::3985bdf47299b8cd8d7592356769807c

المؤلفون: Tyler M. McCracken, Christopher Leet, Allen B. Davis, Samuel H. C. Cabot, René Tronsgaard, Debra A. Fischer, J. M. Joel Ong, Andrew Szymkowiak, Ryan T. Blackman, Ryan R. Petersburg, John M. Brewer, Colby A. Jurgenson, Mikhail Sharov, Lily Zhao, Lars A. Buchhave, David Sawyer

المصدر: Petersburg, R R, Joel Ong, J M, Zhao, L L, Blackman, R T, Brewer, J M, Buchhave, L A, Cabot, S H C, Davis, A B, Jurgenson, C A, Leet, C, McCracken, T M, Sawyer, D, Sharov, M, Tronsgaard, R, Szymkowiak, A E & Fischer, D A 2020, ' An Extreme-precision Radial-velocity Pipeline: First Radial Velocities from EXPRES ', Astrophysical Journal, vol. 159, no. 5, 187 . https://doi.org/10.3847/1538-3881/ab7e31

مصطلحات موضوعية: 010504 meteorology & atmospheric sciences, Pipeline (computing), FOS: Physical sciences, Residual, 01 natural sciences, law.invention, Telescope, Optics, law, 0103 physical sciences, Calibration, Chromatic scale, 010303 astronomy & astrophysics, Spectrograph, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), business.industry, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Exoplanet, Radial velocity, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics

الوصف: The EXtreme PREcision Spectrograph (EXPRES) is an environmentally stabilized, fiber-fed, $R=137,500$, optical spectrograph. It was recently commissioned at the 4.3-m Lowell Discovery Telescope (LDT) near Flagstaff, Arizona. The spectrograph was designed with a target radial-velocity (RV) precision of 30$\mathrm{~cm~s^{-1}}$. In addition to instrumental innovations, the EXPRES pipeline, presented here, is the first for an on-sky, optical, fiber-fed spectrograph to employ many novel techniques---including an "extended flat" fiber used for wavelength-dependent quantum efficiency characterization of the CCD, a flat-relative optimal extraction algorithm, chromatic barycentric corrections, chromatic calibration offsets, and an ultra-precise laser frequency comb for wavelength calibration. We describe the reduction, calibration, and radial-velocity analysis pipeline used for EXPRES and present an example of our current sub-meter-per-second RV measurement precision, which reaches a formal, single-measurement error of 0.3$\mathrm{~m~s^{-1}}$ for an observation with a per-pixel signal-to-noise ratio of 250. These velocities yield an orbital solution on the known exoplanet host 51 Peg that matches literature values with a residual RMS of 0.895$\mathrm{~m~s^{-1}}$.

وصف الملف: application/pdf

URL الوصول: https://explore.openaire.eu/search/publication?articleId=doi_dedup___::d4c706dab0ecc4366b00bd167ad5462f
https://orbit.dtu.dk/en/publications/35fdd74a-f535-4ab4-beda-0b5fa9689468