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10 results on '"Benneke, Björn"'

1. A sub-Neptune transiting the young field star HD 18599 at 40 pc

Author

de Leon, Jerome P., Livingston, John H., Jenkins, James S., Vines, Jose I., Wittenmyer, Robert A., Clark, Jake T., Winn, Joshua I. M., Addison, Brett, Ballard, Sarah, Bayliss, Daniel, Beichman, Charles, Benneke, Björn, Berardo, David Anthony, Bowler, Brendan P., Brown, Tim, Bryant, Edward M., Christiansen, Jessie, Ciardi, David, Collins, Karen A., Collins, Kevin I., Crossfield, Ian, Deming, Drake, Dragomir, Diana, Dressing, Courtney D., Fukui, Akihiko, Gan, Tianjun, Giacalone, Steven, Gill, Samuel, Alvarez, Erica Gonz\' alez, Hesse, Katharine, Horner, Jonathan, Howell, Steve B., Jenkins, Jon M., Kane, Stephen R., Kendall, Alicia, Kielkopf, John F., Kreidberg, Laura, Latham, David W., Liu, Huigen, Lund, Michael B., Matson, Rachel, Matthews, Elisabeth, Mengel, Matthew W., Morales, Farisa, Mori, Mayuko, Narita, Norio, Nishiumi, Taku, Okumura, Jack, Plavchan, Peter, Quinn, Sam, Rabus, Markus, Ricker, George, Rudat, Alexander, Schlieder, Joshua, Schwarz, Richard P., Seager, Sara, Shporer, Avi, Smith, Alexis M. S., Sphorer, Avi, Stassun, Keivan, Tamura, Motohide, Tan, Thiam Guan, Tinney, C. G., Vanderspek, Roland, Gorjian, Varoujan, Werner, Michael W., West, Richard G., Wright, Duncan, Zhang, Hui, and Zhou, George

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), planets and satellites: detection, Space and Planetary Science, techniques: radial velocities, stars: individual: TOI-179, FOS: Physical sciences, Astronomy and Astrophysics, techniques: spectroscopic, Astrophysics - Earth and Planetary Astrophysics
Abstract

Transiting exoplanets orbiting young nearby stars are ideal laboratories for testing theories of planet formation and evolution. However, to date only a handful of stars with age, submitted to MNRAS

Published
2023
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2. Vanadium oxide and a sharp onset of cold-trapping on a giant exoplanet

Author

Pelletier, Stefan, Benneke, Björn, Ali-Dib, Mohamad, Prinoth, Bibiana, Kasper, David, Seifahrt, Andreas, Bean, Jacob L., Debras, Florian, Klein, Baptiste, Bazinet, Luc, Hoeijmakers, H. Jens, Kesseli, Aurora Y., Lim, Olivia, Carmona, Andres, Pino, Lorenzo, Casasayas-Barris, Núria, Hood, Thea, and Stürmer, Julian

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

The abundance of refractory elements in giant planets can provide key insights into their formation histories. Due to the Solar System giants' low temperatures, refractory elements condense below the cloud deck limiting sensing capabilities to only highly volatile elements. Recently, ultra-hot giant exoplanets have allowed for some refractory elements to be measured showing abundances broadly consistent with the solar nebula with titanium likely condensed out of the photosphere. Here we report precise abundance constraints of 14 major refractory elements on the ultra-hot giant planet WASP-76b that show distinct deviations from proto-solar, and a sharp onset in condensation temperature. In particular, we find nickel to be enriched, a possible sign of the accretion of a differentiated object's core during the planet's evolution. Elements with condensation temperatures below 1,550 K otherwise closely match those of the Sun before sharply transitioning to being strongly depleted above 1,550 K, well explained by nightside cold-trapping. We further unambiguously detect vanadium oxide on WASP-76b, a molecule long hypothesized to drive atmospheric thermal inversions, and also observe a global east-west asymmetry in its absorption signals. Overall, our findings indicate that giant planets have a mostly stellar-like refractory elemental content and suggest that temperature sequences of hot Jupiter spectra can show abrupt transitions wherein a mineral species is either present, or completely absent if a cold-trap exists below its condensation temperature., Published online in Nature on June 14, 2023

Published
2023

3. A broadband thermal emission spectrum of the ultra-hot Jupiter WASP-18b

Author

Coulombe, Louis-Philippe, Benneke, Björn, Challener, Ryan, Piette, Anjali A. A., Wiser, Lindsey S., Mansfield, Megan, MacDonald, Ryan J., Beltz, Hayley, Feinstein, Adina D., Radica, Michael, Savel, Arjun B., Dos Santos, Leonardo A., Bean, Jacob L., Parmentier, Vivien, Wong, Ian, Rauscher, Emily, Komacek, Thaddeus D., Kempton, Eliza M.-R., Tan, Xianyu, Hammond, Mark, Lewis, Neil T., Line, Michael R., Lee, Elspeth K. H., Shivkumar, Hinna, Crossfield, Ian J. M., Nixon, Matthew C., Rackham, Benjamin V., Wakeford, Hannah R., Welbanks, Luis, Zhang, Xi, Batalha, Natalie M., Berta-Thompson, Zachory K., Changeat, Quentin, Désert, Jean-Michel, Espinoza, Néstor, Goyal, Jayesh M., Harrington, Joseph, Knutson, Heather A., Kreidberg, Laura, López-Morales, Mercedes, Shporer, Avi, Sing, David K., Stevenson, Kevin B., Aggarwal, Keshav, Ahrer, Eva-Maria, Alam, Munazza K., Bell, Taylor J., Blecic, Jasmina, Caceres, Claudio, Carter, Aarynn L., Casewell, Sarah L., Crouzet, Nicolas, Cubillos, Patricio E., Decin, Leen, Fortney, Jonathan J., Gibson, Neale P., Heng, Kevin, Henning, Thomas, Iro, Nicolas, Kendrew, Sarah, Lagage, Pierre-Olivier, Leconte, Jérémy, Lendl, Monika, Lothringer, Joshua D., Mancini, Luigi, Mikal-Evans, Thomas, Molaverdikhani, Karan, Nikolov, Nikolay K., Ohno, Kazumasa, Palle, Enric, Piaulet, Caroline, Redfield, Seth, Roy, Pierre-Alexis, Tsai, Shang-Min, Venot, Olivia, and Wheatley, Peter J.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Multidisciplinary, 520 Astronomy, FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), exoplanets hot Jupiter JWST, Astrophysics - Earth and Planetary Astrophysics
Abstract

Close-in giant exoplanets with temperatures greater than 2,000 K (''ultra-hot Jupiters'') have been the subject of extensive efforts to determine their atmospheric properties using thermal emission measurements from the Hubble and Spitzer Space Telescopes. However, previous studies have yielded inconsistent results because the small sizes of the spectral features and the limited information content of the data resulted in high sensitivity to the varying assumptions made in the treatment of instrument systematics and the atmospheric retrieval analysis. Here we present a dayside thermal emission spectrum of the ultra-hot Jupiter WASP-18b obtained with the NIRISS instrument on JWST. The data span 0.85 to 2.85 $\mu$m in wavelength at an average resolving power of 400 and exhibit minimal systematics. The spectrum shows three water emission features (at $>$6$\sigma$ confidence) and evidence for optical opacity, possibly due to H$^-$, TiO, and VO (combined significance of 3.8$\sigma$). Models that fit the data require a thermal inversion, molecular dissociation as predicted by chemical equilibrium, a solar heavy element abundance (''metallicity'', M/H = 1.03$_{-0.51}^{+1.11}$ $\times$ solar), and a carbon-to-oxygen (C/O) ratio less than unity. The data also yield a dayside brightness temperature map, which shows a peak in temperature near the sub-stellar point that decreases steeply and symmetrically with longitude toward the terminators., Comment: JWST ERS bright star observations. Uploaded to inform JWST Cycle 2 proposals. Manuscript under review. 50 pages, 14 figures, 2 tables

Published
2023
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4. Photochemically produced SO2 in the atmosphere of WASP-39b

Author

Tsai, Shang-Min, Lee, Elspeth K H, Powell, Diana, Gao, Peter, Zhang, Xi, Moses, Julianne, Hébrard, Eric, Venot, Olivia, Parmentier, Vivien, Jordan, Sean, Hu, Renyu, Alam, Munazza K, Alderson, Lili, Batalha, Natalie M, Bean, Jacob L, Benneke, Björn, Bierson, Carver J, Brady, Ryan P, Carone, Ludmila, Carter, Aarynn L, Chubb, Katy L, Inglis, Julie, Leconte, Jérémy, Line, Michael, López-Morales, Mercedes, Miguel, Yamila, Molaverdikhani, Karan, Rustamkulov, Zafar, Sing, David K, Stevenson, Kevin B, Wakeford, Hannah R, Yang, Jeehyun, Aggarwal, Keshav, Baeyens, Robin, Barat, Saugata, de Val-Borro, Miguel, Daylan, Tansu, Fortney, Jonathan J, France, Kevin, Goyal, Jayesh M, Grant, David, Kirk, James, Kreidberg, Laura, Louca, Amy, Moran, Sarah E, Mukherjee, Sagnick, Nasedkin, Evert, Ohno, Kazumasa, Rackham, Benjamin V, Redfield, Seth, Taylor, Jake, Tremblin, Pascal, Visscher, Channon, Wallack, Nicole L, Welbanks, Luis, Youngblood, Allison, Ahrer, Eva-Maria, Batalha, Natasha E, Behr, Patrick, Berta-Thompson, Zachory K, Blecic, Jasmina, Casewell, S L, Crossfield, Ian J M, Crouzet, Nicolas, Cubillos, Patricio E, Decin, Leen, Désert, Jean-Michel, Feinstein, Adina D, Gibson, Neale P, Harrington, Joseph, Heng, Kevin, Henning, Thomas, Kempton, Eliza M-R, Krick, Jessica, Lagage, Pierre-Olivier, Lendl, Monika, Lothringer, Joshua D, Mansfield, Megan, Mayne, N J, Mikal-Evans, Thomas, Palle, Enric, Schlawin, Everett, Shorttle, Oliver, Wheatley, Peter J, Yurchenko, Sergei N, Tsai, Shang-Min [0000-0002-8163-4608], Apollo - University of Cambridge Repository, and University of St Andrews. School of Physics and Astronomy

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), MCC, Multidisciplinary, 520 Astronomy, 520 Astronomie, FOS: Physical sciences, DAS, 5109 Space Sciences, Astrophysics - Solar and Stellar Astrophysics, QB Astronomy, 51 Physical Sciences, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics - Earth and Planetary Astrophysics, QB
Abstract

Photochemistry is a fundamental process of planetary atmospheres that regulates the atmospheric composition and stability. However, no unambiguous photochemical products have been detected in exoplanet atmospheres to date. Recent observations from the JWST Transiting Exoplanet Early Release Science Program found a spectral absorption feature at 4.05 $\mu$m arising from SO$_2$ in the atmosphere of WASP-39b. WASP-39b is a 1.27-Jupiter-radii, Saturn-mass (0.28 M$_J$) gas giant exoplanet orbiting a Sun-like star with an equilibrium temperature of $\sim$1100 K. The most plausible way of generating SO$_2$ in such an atmosphere is through photochemical processes. Here we show that the SO$_2$ distribution computed by a suite of photochemical models robustly explains the 4.05 $\mu$m spectral feature identified by JWST transmission observations with NIRSpec PRISM (2.7$\sigma$) and G395H (4.5$\sigma$). SO$_2$ is produced by successive oxidation of sulphur radicals freed when hydrogen sulphide (H$_2$S) is destroyed. The sensitivity of the SO$_2$ feature to the enrichment of the atmosphere by heavy elements (metallicity) suggests that it can be used as a tracer of atmospheric properties, with WASP-39b exhibiting an inferred metallicity of $\sim$10$\times$ solar. We further point out that SO$_2$ also shows observable features at ultraviolet and thermal infrared wavelengths not available from the existing observations., Comment: 39 pages, 14 figures, accepted to be published in Nature

Published
2023
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5. Identification of carbon dioxide in an exoplanet atmosphere

Author

The JWST Transiting Exoplanet Community Early Release Science Team, Ahrer, Eva-Maria, Alderson, Lili, Batalha, Natalie M., Batalha, Natasha E., Bean, Jacob L., Beatty, Thomas G., Bell, Taylor J., Benneke, Björn, Berta-Thompson, Zachory K., Carter, Aarynn L., Crossfield, Ian J. M., Espinoza, Néstor, Feinstein, Adina D., Fortney, Jonathan J., Gibson, Neale P., Goyal, Jayesh M., Kempton, Eliza M. -R., Kirk, James, Kreidberg, Laura, López-Morales, Mercedes, Line, Michael R., Lothringer, Joshua D., Moran, Sarah E., Mukherjee, Sagnick, Ohno, Kazumasa, Parmentier, Vivien, Piaulet, Caroline, Rustamkulov, Zafar, Schlawin, Everett, Sing, David K., Stevenson, Kevin B., Wakeford, Hannah R., Allen, Natalie H., Birkmann, Stephan M., Brande, Jonathan, Crouzet, Nicolas, Cubillos, Patricio E., Damiano, Mario, Désert, Jean-Michel, Gao, Peter, Harrington, Joseph, Hu, Renyu, Kendrew, Sarah, Knutson, Heather A., Lagage, Pierre-Olivier, Leconte, Jérémy, Lendl, Monika, MacDonald, Ryan J., May, E. M., Miguel, Yamila, Molaverdikhani, Karan, Moses, Julianne I., Murray, Catriona Anne, Nehring, Molly, Nikolov, Nikolay K., de la Roche, D. J. M. Petit dit, Radica, Michael, Roy, Pierre-Alexis, Stassun, Keivan G., Taylor, Jake, Waalkes, William C., Wachiraphan, Patcharapol, Welbanks, Luis, Wheatley, Peter J., Aggarwal, Keshav, Alam, Munazza K., Banerjee, Agnibha, Barstow, Joanna K., Blecic, Jasmina, Casewell, S. L., Changeat, Quentin, Chubb, K. L., Colón, Knicole D., Coulombe, Louis-Philippe, Daylan, Tansu, de Val-Borro, Miguel, Decin, Leen, Santos, Leonardo A. Dos, Flagg, Laura, France, Kevin, Fu, Guangwei, Muñoz, A. García, Gizis, John E., Glidden, Ana, Grant, David, Heng, Kevin, Henning, Thomas, Hong, Yu-Cian, Inglis, Julie, Iro, Nicolas, Kataria, Tiffany, Komacek, Thaddeus D., Krick, Jessica E., Lee, Elspeth K. H., Lewis, Nikole K., Lillo-Box, Jorge, Lustig-Yaeger, Jacob, Mancini, Luigi, Mandell, Avi M., Mansfield, Megan, Marley, Mark S., Mikal-Evans, Thomas, Morello, Giuseppe, Nixon, Matthew C., Ceballos, Kevin Ortiz, Piette, Anjali A. A., Powell, Diana, Rackham, Benjamin V., Ramos-Rosado, Lakeisha, Rauscher, Emily, Redfield, Seth, Rogers, Laura K., Roman, Michael T., Roudier, Gael M., Scarsdale, Nicholas, Shkolnik, Evgenya L., Southworth, John, Spake, Jessica J., Steinrueck, Maria E, Tan, Xianyu, Teske, Johanna K., Tremblin, Pascal, Tsai, Shang-Min, Tucker, Gregory S., Turner, Jake D., Valenti, Jeff A., Venot, Olivia, Waldmann, Ingo P., Wallack, Nicole L., Zhang, Xi, and Zieba, Sebastian

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Multidisciplinary, Settore FIS/05, 530 Physics, 520 Astronomy, FOS: Physical sciences, 500 Science, Q1, QB460, QA, QB600, Astrophysics - Earth and Planetary Astrophysics, QB, QB799
Abstract

Carbon dioxide (CO2) is a key chemical species that is found in a wide range of planetary atmospheres. In the context of exoplanets, CO2 is an indicator of the metal enrichment (i.e., elements heavier than helium, also called "metallicity"), and thus formation processes of the primary atmospheres of hot gas giants. It is also one of the most promising species to detect in the secondary atmospheres of terrestrial exoplanets. Previous photometric measurements of transiting planets with the Spitzer Space Telescope have given hints of the presence of CO2 but have not yielded definitive detections due to the lack of unambiguous spectroscopic identification. Here we present the detection of CO2 in the atmosphere of the gas giant exoplanet WASP-39b from transmission spectroscopy observations obtained with JWST as part of the Early Release Science Program (ERS). The data used in this study span 3.0 to 5.5 {\mu}m in wavelength and show a prominent CO2 absorption feature at 4.3 {\mu}m (26{\sigma} significance). The overall spectrum is well matched by one-dimensional, 10x solar metallicity models that assume radiative-convective-thermochemical equilibrium and have moderate cloud opacity. These models predict that the atmosphere should have water, carbon monoxide, and hydrogen sulfide in addition to CO2, but little methane. Furthermore, we also tentatively detect a small absorption feature near 4.0 {\mu}m that is not reproduced by these models., Comment: 27 pages, 6 figures, Accepted for publication in Nature, data and models available at https://doi.10.5281/zenodo.6959427

Published
2023
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6. The Hubble PanCET Program: A Featureless Transmission Spectrum for WASP-29b and Evidence of Enhanced Atmospheric Metallicity on WASP-80b

Author

Wong, Ian, Chachan, Yayaati, Knutson, Heather A., Henry, Gregory W., Adams, Danica, Kataria, Tiffany, Benneke, Björn, Gao, Peter, Deming, Drake, López-Morales, Mercedes, Sing, David K., Alam, Munazza K., Ballester, Gilda E., Barstow, Joanna K., Buchhave, Lars A., dos Santos, Leonardo A., Fu, Guangwei, Muñoz, Antonio García, MacDonald, Ryan J., Mikal-Evans, Thomas, Sanz-Forcada, Jorge, and Wakeford, Hannah R.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Exoplanet atmospheric composition, Space and Planetary Science, Transmission spectroscopy, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics, Exoplanet atmospheres, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present a uniform analysis of transit observations from the Hubble Space Telescope and Spitzer Space Telescope of two warm gas giants orbiting K-type stars - WASP-29b and WASP-80b. The transmission spectra, which span 0.4-5.0 $\mu$m, are interpreted using a suite of chemical equilibrium PLATON atmospheric retrievals. Both planets show evidence of significant aerosol opacity along the day-night terminator. The spectrum of WASP-29b is flat throughout the visible and near-infrared, suggesting the presence of condensate clouds extending to low pressures. The lack of spectral features hinders our ability to constrain the atmospheric metallicity and C/O ratio. In contrast, WASP-80b shows a discernible, albeit muted H$_2$O absorption feature at 1.4 $\mu$m, as well as a steep optical spectral slope that is caused by fine-particle aerosols and/or contamination from unocculted spots on the variable host star. WASP-80b joins the small number of gas-giant exoplanets that show evidence for enhanced atmospheric metallicity: the transmission spectrum is consistent with metallicities ranging from $\sim$30-100 times solar in the case of cloudy limbs to a few hundred times solar in the cloud-free scenario. In addition to the detection of water, we infer the presence of CO$_2$ in the atmosphere of WASP-80b based on the enhanced transit depth in the Spitzer 4.5 $\mu$m bandpass. From a complementary analysis of Spitzer secondary eclipses, we find that the dayside emission from WASP-29b and WASP-80b is consistent with brightness temperatures of $937 \pm 48$ and $851 \pm 14$ K, respectively, indicating relatively weak day-night heat transport and low Bond albedo., Comment: Published in AJ, 26 pages, 13 figures. Updated to reflect proof changes

Published
2022
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7. Evidence for the volatile-rich composition of a 1.5-$R_\oplus$ planet

Author

Piaulet, Caroline, Benneke, Björn, Almenara, Jose M., Dragomir, Diana, Knutson, Heather A., Thorngren, Daniel, Peterson, Merrin S., Crossfield, Ian J. M., Kempton, Eliza M. -R., Kubyshkina, Daria, Howard, Andrew W., Angus, Ruth, Isaacson, Howard, Weiss, Lauren M., Beichman, Charles A., Fortney, Jonathan J., Fossati, Luca, Lammer, Helmut, McCullough, P. R., Morley, Caroline V., and Wong, Ian

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

The population of planets smaller than approximately $1.7~R_\oplus$ is widely interpreted as consisting of rocky worlds, generally referred to as super-Earths. This picture is largely corroborated by radial-velocity (RV) mass measurements for close-in super-Earths but lacks constraints at lower insolations. Here we present the results of a detailed study of the Kepler-138 system using 13 Hubble and Spitzer transit observations of the warm-temperate $1.51\pm0.04~R_\oplus$ planet Kepler-138 d ($T_{\mathrm{eq, A_B=0.3}}$~350 K) combined with new Keck/HIRES RV measurements of its host star. We find evidence for a volatile-rich "water world" nature of Kepler-138 d, with a large fraction of its mass contained in a thick volatile layer. This finding is independently supported by transit timing variations, RV observations ($M_d=2.1_{-0.7}^{+0.6}~M_\oplus$), as well as the flat optical/IR transmission spectrum. Quantitatively, we infer a composition of $11_{-4}^{+3}$\% volatiles by mass or ~51% by volume, with a 2000 km deep water mantle and atmosphere on top of a core with an Earth-like silicates/iron ratio. Any hypothetical hydrogen layer consistent with the observations ($, Published in Nature Astronomy. 4 main figures, 10 extended data figures, 13 supplementary figures. 4 tables

Published
2022
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8. TOI 560 : Two Transiting Planets Orbiting a K Dwarf Validated with iSHELL, PFS and HIRES RVs

Author

Mufti, Mohammed El, Plavchan, Peter P., Isaacson, Howard, Cale, Bryson L., Feliz, Dax L., Reefe, Michael A., Hellier, Coel, Stassun, Keivan, Eastman, Jason, Polanski, Alex, Crossfield, Ian J. M., Gaidos, Eric, Kostov, Veselin, Villasenor, Joel, Schlieder, Joshua E., Bouma, Luke G., Collins, Kevin I., Wittrock, Justin M., Zohrabi, Farzaneh, Lee, Rena A., Sohani, Ahmad, Berberian, John, Vermilion, David, Newman, Patrick, Geneser, Claire, Tanner, Angelle, Batalha, Natalie M., Dressing, Courtney, Fulton, Benjamin, Howard, Andrew W., Huber, Daniel, Kane, Stephen R., Petigura, Erik A., Robertson, Paul, Roy, Arpita, Weiss, Lauren M., Behmard, Aida, Beard, Corey, Chontos, Ashley, Dai, Fei, Dalba, Paul A., Fetherolf, Tara, Giacalone, Steven, Hill, Michelle L., Hirsch, Lea A., Holcomb, Rae, Lubin, Jack, Mayo, Andrew, Movcnik, Teo, Murphy, Joseph M. Akana, Rosenthal, Lee J., Rubenzahl, Ryan A., Scarsdale, Nicholas, Stockdale, Christopher, Collins, Karen, Cloutier, Ryan, Relles, Howard, Tan, Thiam-Guan, Scott, Nicholas J, Hartman, Zach, Matthews, Elisabeth, Ciardi, David, Gonzales, Erica, Matson, Rachel A., Beichman, Charles, Furlan, E., Gnilka, Crystal L., Howell, Steve B., Ziegler, Carl, Briceno, Cesar, Law, Nicholas, Mann, Andrew W., Rabus, Markus, Johnson, Marshall C., Christiansen, Jessie, Kreidberg, Laura, Berardo, David Anthony, Deming, Drake, Gorjian, Varoujan, Morales, Farisa Y., Benneke, Björn, Dragomir, Diana, Wittenmyer, Robert A., Ballard, Sarah, Bowler, Brendan P., Horner, Jonathan, Kielkopf, John, Liu, Huigen, Shporer, Avi, Tinney, C. G., Zhang, Hui, Wright, Duncan J., Addison, Brett C., Mengel, Matthew W., and Okumura, Jack

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), FOS: Physical sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract

We validate the presence of a two-planet system orbiting the 0.15--1.4 Gyr K4 dwarf TOI 560 (HD 73583). The system consists of an inner moderately eccentric transiting mini-Neptune (TOI 560 b, $P = 6.3980661^{+0.0000095}_{-0.0000097}$ days, $e=0.294^{+0.13}_{-0.062}$, $M= 0.94^{+0.31}_{-0.23}M_{Nep}$) initially discovered in the Sector 8 \tess\ mission observations, and a transiting mini-Neptune (TOI 560 c, $P = 18.8805^{+0.0024}_{-0.0011}$ days, $M= 1.32^{+0.29}_{-0.32}M_{Nep}$) discovered in the Sector 34 observations, in a rare near-1:3 orbital resonance. We utilize photometric data from \tess\, \textit{Spitzer}, and ground-based follow-up observations to confirm the ephemerides and period of the transiting planets, vet false positive scenarios, and detect the photo-eccentric effect for TOI 560 b. We obtain follow-up spectroscopy and corresponding precise radial velocities (RVs) with the iSHELL spectrograph at the NASA Infrared Telescope Facility and the HIRES Spectrograph at Keck Observatory to validate the planetary nature of these signals, which we combine with published PFS RVs from Magellan Observatory. We detect the masses of both planets at $> 3-σ$ significance. We apply a Gaussian process (GP) model to the \tess\ light curves to place priors on a chromatic radial velocity GP model to constrain the stellar activity of the TOI 560 host star, and confirm a strong wavelength dependence for the stellar activity demonstrating the ability of NIR RVs in mitigating stellar activity for young K dwarfs. TOI 560 is a nearby moderately young multi-planet system with two planets suitable for atmospheric characterization with James Webb Space Telescope (JWST) and other upcoming missions. In particular, it will undergo six transit pairs separated by $, AAS Journals, Accepted for publication

Published
2021
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9. Bright Opportunities for Atmospheric Characterization of Small Planets: Masses and Radii of K2-3 b, c, and d and GJ3470 b from Radial Velocity Measurements and Spitzer Transits

Author

Kosiarek, Molly R., Crossfield, Ian J. M., Hardegree-Ullman, Kevin K., Livingston, John H., Benneke, Björn, Henry, Gregory W., Howard, Ward S., Berardo, David, Blunt, Sarah, Fulton, Benjamin J., Hirsch, Lea A., Howard, Andrew W., Isaacson, Howard, Petigura, Erik A., Sinukoff, Evan, Weiss, Lauren, Bonfils, X., Dressing, Courtney D., Knutson, Heather A., Schlieder, Joshua E., Werner, Michael, Gorjian, Varoujan, Krick, Jessica, Morales, Farisa Y., Astudillo-Defru, Nicola, Almenara, J.-M., Delfosse, X., Forveille, T., Lovis, C., Mayor, M., Murgas, F., Pepe, F., Santos, N. C., Udry, S., Corbett, H. T., Fors, Octavi, Law, Nicholas M., Ratzloff, Jeffrey K., del Ser, Daniel, Kosiarek, Molly, Crossfield, Ian, Hardegree-Ullman, Kevin, Livingston, John, Henry, Gregory, Howard, Ward, Fulton, Benjamin, Hirsch, Lea, Howard, Andrew, Petigura, Erik, Dressing, Courtney, Knutson, Heather, Schlieder, Joshua, Morales, Farisa, Law, Nicholas, Ratzloff, Jeffrey, Ser, Daniel del, Département de Physique [Montréal], Université de Montréal [Montréal], Department of Earth and Planetary Science [UC Berkeley] (EPS), University of California [Berkeley], University of California-University of California, Institute for Astronomy [Honolulu], University of Hawai‘i [Mānoa] (UHM), Université de Montréal - UdeM (CANADA), Université de Montréal (UdeM), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Division of Geological and Planetary Sciences [Pasadena], California Institute of Technology (CALTECH), Observatoire Astronomique de l'Université de Genève (ObsGE), Université de Genève (UNIGE), Universidad de Concepción [Chile], Centro de Astrofísica da Universidade do Porto (CAUP), Universidade do Porto [Porto], Department of Astronomy and Astrophysics [UCSC Santa Cruz], University of California [Santa Cruz] (UCSC), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology (MIT), SRI International [Menlo Park] (SRI), Infrared Processing and Analysis Center (IPAC), Caltech Department of Astronomy [Pasadena], Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, University of Leeds, Tennessee State University, Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), and Universidade do Porto

Subjects
010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Rotation, Ephemeris, 01 natural sciences, techniques: photometric, Planet, 0103 physical sciences, techniques: radial velocities, Transit (astronomy), 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Earth and Planetary Astrophysics (astro-ph.EP), Stellar rotation, planets and satellites: composition, Astronomy and Astrophysics, Radial velocity, Stars, Photometry (astronomy), 13. Climate action, Space and Planetary Science, [SDU]Sciences of the Universe [physics], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics
Abstract

We report improved masses, radii, and densities for four planets in two bright M-dwarf systems, K2-3 and GJ3470, derived from a combination of new radial velocity and transit observations. Supplementing K2 photometry with follow-up Spitzer transit observations refined the transit ephemerides of K2-3 b, c, and d by over a factor of 10. We analyze ground-based photometry from the Evryscope and Fairborn Observatory to determine the characteristic stellar activity timescales for our Gaussian Process fit, including the stellar rotation period and activity region decay timescale. The stellar rotation signals for both stars are evident in the radial velocity data and are included in our fit using a Gaussian process trained on the photometry. We find the masses of K2-3 b, K2-3 c and GJ3470 b to be 6.48$^{+0.99}_{-0.93}$, 2.14$^{+1.08}_{-1.04}$, and 12.58$^{+1.31}_{-1.28}$ M$_\oplus$ respectively. K2-3 d was not significantly detected and has a 3-$\sigma$ upper limit of 2.80 M$_\oplus$. These two systems are training cases for future TESS systems; due to the low planet densities ($\rho$ $, Comment: 21 pages, 11 figures, accepted to AJ

Published
2019
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10. An Improved Transit Measurement for a 2.4 R_{Earth} Planet Orbiting A Bright Mid-M Dwarf K2$-$28

Author

Chen, Ge, Knutson, Heather A., Dressing, Courtney D., Morley, Caroline V., Werner, Michael, Gorjian, Varoujan, Beichman, Charles, Benneke, Björn, Christiansen, Jessie, Ciardi, David, Crossfield, Ian, Howell, Steve B., Krick, Jessica E., Livingston, John, Morales, Farisa Y., and Schlieder, Joshua E.

Subjects
Earth and Planetary Astrophysics (astro-ph.EP), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present a new {\em Spitzer} transit observation of K2$-$28b, a sub-Neptune ($R_{\rm p} = 2.45\pm0.28 R_{Earth}$) orbiting a relatively bright ($V_{\rm mag} = 16.06$, $K_{\rm mag} = 10.75$) metal-rich M4 dwarf (EPIC 206318379). This star is one of only seven with masses less than 0.2 M_{Sun} known to host transiting planets, and the planet appears to be a slightly smaller analogue of GJ 1214b ($2.85\pm0.20 R_{Earth}$; \citealt{2013A&A...549A..10H}). Our new {\em Spitzer} observations were taken two years after the original K2 discovery data and have a significantly higher cadence, allowing us to derive improved estimates for this planet's radius, semi-major axis, and orbital period, which greatly reduce the uncertainty in the prediction of near future transit times for the {\em James Webb Space Telescope} ({\em JWST}) observations. We also evaluate the system's suitability for atmospheric characterization with {\em JWST} and find that it is currently the only small (< 3 R_{Earth}) and cool ($< 600$ K) planet aside from GJ 1214b with a potentially detectable secondary eclipse. We also note that this system is a favorable target for near-infrared radial velocity instruments on larger telescopes (e.g., the Habitable Planet Finder on the Hobby-Eberly Telescope), making it one of only a handful of small, cool planets accessible with this technique. Finally, we compare our results with the simulated catalog of the Transiting Exoplanet Survey Satellite ({\em TESS}) and find K2$-$28b to be representative of the kind of mid-M systems that should be detectible in the {\em TESS} sample., 9 pages, 6 figures, accepted by AJ

Published
2018
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