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13 results on '"Carter, Aarynn L."'

1. Sulfur dioxide in the mid-infrared transmission spectrum of WASP-39b

Author

Powell, Diana, Feinstein, Adina D., Lee, Elspeth K. H., Zhang, Michael, Tsai, Shang-Min, Taylor, Jake, Kirk, James, Bell, Taylor, Barstow, Joanna K., Gao, Peter, Bean, Jacob L., Blecic, Jasmina, Chubb, Katy L., Crossfield, Ian J. M., Jordan, Sean, Kitzmann, Daniel, Moran, Sarah E., Morello, Giuseppe, Moses, Julianne I., Welbanks, Luis, Yang, Jeehyun, Zhang, Xi, Ahrer, Eva-Maria, Bello-Arufe, Aaron, Brande, Jonathan, Casewell, S. L., Crouzet, Nicolas, Cubillos, Patricio E., Demory, Brice-Olivier, Dyrek, Achrène, Flagg, Laura, Hu, Renyu, Inglis, Julie, Jones, Kathryn D., Kreidberg, Laura, López-Morales, Mercedes, Lagage, Pierre-Olivier, Meier Valdés, Erik A., Miguel, Yamila, Parmentier, Vivien, Piette, Anjali A. A., Rackham, Benjamin V., Radica, Michael, Redfield, Seth, Stevenson, Kevin B., Wakeford, Hannah R., Aggarwal, Keshav, Alam, Munazza K., Batalha, Natalie M., Batalha, Natasha E., Benneke, Björn, Berta-Thompson, Zach K., Brady, Ryan P., Caceres, Claudio, Carter, Aarynn L., Désert, Jean-Michel, Harrington, Joseph, Iro, Nicolas, Line, Michael R., Lothringer, Joshua D., MacDonald, Ryan J., Mancini, Luigi, Molaverdikhani, Karan, Mukherjee, Sagnick, Nixon, Matthew C., Oza, Apurva V., Palle, Enric, Rustamkulov, Zafar, Sing, David K., Steinrueck, Maria E., Venot, Olivia, Wheatley, Peter J., and Yurchenko, Sergei N.

Abstract

The recent inference of sulfur dioxide (SO2) in the atmosphere of the hot (approximately 1,100 K), Saturn-mass exoplanet WASP-39b from near-infrared JWST observations1–3suggests that photochemistry is a key process in high-temperature exoplanet atmospheres4. This is because of the low (<1 ppb) abundance of SO2under thermochemical equilibrium compared with that produced from the photochemistry of H2O and H2S (1–10 ppm)4–9. However, the SO2inference was made from a single, small molecular feature in the transmission spectrum of WASP-39b at 4.05 μm and, therefore, the detection of other SO2absorption bands at different wavelengths is needed to better constrain the SO2abundance. Here we report the detection of SO2spectral features at 7.7 and 8.5 μm in the 5–12-μm transmission spectrum of WASP-39b measured by the JWST Mid-Infrared Instrument (MIRI) Low Resolution Spectrometer (LRS)10. Our observations suggest an abundance of SO2of 0.5–25 ppm (1σrange), consistent with previous findings4. As well as SO2, we find broad water-vapour absorption features, as well as an unexplained decrease in the transit depth at wavelengths longer than 10 μm. Fitting the spectrum with a grid of atmospheric forward models, we derive an atmospheric heavy-element content (metallicity) for WASP-39b of approximately 7.1–8.0 times solar and demonstrate that photochemistry shapes the spectra of WASP-39b across a broad wavelength range.

Published
2024
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2. Inhomogeneous terminators on the exoplanet WASP-39 b

Author

Espinoza, Néstor, Steinrueck, Maria E., Kirk, James, MacDonald, Ryan J., Savel, Arjun B., Arnold, Kenneth, Kempton, Eliza M.-R., Murphy, Matthew M., Carone, Ludmila, Zamyatina, Maria, Lewis, David A., Samra, Dominic, Kiefer, Sven, Rauscher, Emily, Christie, Duncan, Mayne, Nathan, Helling, Christiane, Rustamkulov, Zafar, Parmentier, Vivien, May, Erin M., Carter, Aarynn L., Zhang, Xi, López-Morales, Mercedes, Allen, Natalie, Blecic, Jasmina, Decin, Leen, Mancini, Luigi, Molaverdikhani, Karan, Rackham, Benjamin V., Palle, Enric, Tsai, Shang-Min, Ahrer, Eva-Maria, Bean, Jacob L., Crossfield, Ian J. M., Haegele, David, Hébrard, Eric, Kreidberg, Laura, Powell, Diana, Schneider, Aaron D., Welbanks, Luis, Wheatley, Peter, Brahm, Rafael, and Crouzet, Nicolas

Abstract

Transmission spectroscopy has been a workhorse technique used over the past two decades to constrain the physical and chemical properties of exoplanet atmospheres1–5. One of its classical key assumptions is that the portion of the atmosphere it probes—the terminator region—is homogeneous. Several works from the past decade, however, have put this into question for highly irradiated, hot (Teq≳ 1,000 K) gas giant exoplanets, both empirically6–10and through three-dimensional modelling11–17. While models have predicted clear differences between the evening (day-to-night) and morning (night-to-day) terminators, direct morning and evening transmission spectra in a wide wavelength range have not been reported for an exoplanet so far. Under the assumption of precise and accurate orbital parameters for the exoplanet WASP-39 b, here we report the detection of inhomogeneous terminators on WASP-39 b, which has allowed us to retrieve its morning and evening transmission spectra in the near-infrared (2–5 μm) using the James Webb Space Telescope. We have observed larger transit depths in the evening, which are, on average, 405 ± 88 ppm larger than the morning ones, and also have qualitatively larger features than the morning spectrum. The spectra are best explained by models in which the evening terminator is hotter than the morning terminator by 177−57+65K, with both terminators having C/O ratios consistent with solar. General circulation models predict temperature differences broadly consistent with the above value and point towards a cloudy morning terminator and a clearer evening terminator.

Published
2024
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3. Photochemically produced SO2in 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., and Yurchenko, Sergei N.

Abstract

Photochemistry is a fundamental process of planetary atmospheres that regulates the atmospheric composition and stability1. However, no unambiguous photochemical products have been detected in exoplanet atmospheres so far. Recent observations from the JWST Transiting Exoplanet Community Early Release Science Program2,3found a spectral absorption feature at 4.05 μm arising from sulfur dioxide (SO2) in the atmosphere of WASP-39b. WASP-39b is a 1.27-Jupiter-radii, Saturn-mass (0.28 MJ) gas giant exoplanet orbiting a Sun-like star with an equilibrium temperature of around 1,100 K (ref. 4). The most plausible way of generating SO2in such an atmosphere is through photochemical processes5,6. Here we show that the SO2distribution computed by a suite of photochemical models robustly explains the 4.05-μm spectral feature identified by JWST transmission observations7with NIRSpec PRISM (2.7σ)8and G395H (4.5σ)9. SO2is produced by successive oxidation of sulfur radicals freed when hydrogen sulfide (H2S) is destroyed. The sensitivity of the SO2feature 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 about 10× solar. We further point out that SO2also shows observable features at ultraviolet and thermal infrared wavelengths not available from the existing observations.

Published
2023
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4. 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.

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 Space Telescope (HST) and Spitzer Space Telescope1–3. 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 analysis3–12. Here we present a dayside thermal emission spectrum of the ultra-hot Jupiter WASP-18b obtained with the NIRISS13instrument on the JWST. The data span 0.85 to 2.85 μm in wavelength at an average resolving power of 400 and exhibit minimal systematics. The spectrum shows three water emission features (at >6σconfidence) and evidence for optical opacity, possibly attributable to H−, TiO and VO (combined significance of 3.8σ). 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+1.11times 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 substellar point that decreases steeply and symmetrically with longitude towards the terminators.

Published
2023
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5. Early Release Science of the exoplanet WASP-39b with JWST NIRISS

Author

Feinstein, Adina D., Radica, Michael, Welbanks, Luis, Murray, Catriona Anne, Ohno, Kazumasa, Coulombe, Louis-Philippe, Espinoza, Néstor, Bean, Jacob L., Teske, Johanna K., Benneke, Björn, Line, Michael R., Rustamkulov, Zafar, Saba, Arianna, Tsiaras, Angelos, Barstow, Joanna K., Fortney, Jonathan J., Gao, Peter, Knutson, Heather A., MacDonald, Ryan J., Mikal-Evans, Thomas, Rackham, Benjamin V., Taylor, Jake, Parmentier, Vivien, Batalha, Natalie M., Berta-Thompson, Zachory K., Carter, Aarynn L., Changeat, Quentin, dos Santos, Leonardo A., Gibson, Neale P., Goyal, Jayesh M., Kreidberg, Laura, López-Morales, Mercedes, Lothringer, Joshua D., Miguel, Yamila, Molaverdikhani, Karan, Moran, Sarah E., Morello, Giuseppe, Mukherjee, Sagnick, Sing, David K., Stevenson, Kevin B., Wakeford, Hannah R., Ahrer, Eva-Maria, Alam, Munazza K., Alderson, Lili, Allen, Natalie H., Batalha, Natasha E., Bell, Taylor J., Blecic, Jasmina, Brande, Jonathan, Caceres, Claudio, Casewell, S. L., Chubb, Katy L., Crossfield, Ian J. M., Crouzet, Nicolas, Cubillos, Patricio E., Decin, Leen, Désert, Jean-Michel, Harrington, Joseph, Heng, Kevin, Henning, Thomas, Iro, Nicolas, Kempton, Eliza M.-R., Kendrew, Sarah, Kirk, James, Krick, Jessica, Lagage, Pierre-Olivier, Lendl, Monika, Mancini, Luigi, Mansfield, Megan, May, E. M., Mayne, N. J., Nikolov, Nikolay K., Palle, Enric, Petit dit de la Roche, Dominique J. M., Piaulet, Caroline, Powell, Diana, Redfield, Seth, Rogers, Laura K., Roman, Michael T., Roy, Pierre-Alexis, Nixon, Matthew C., Schlawin, Everett, Tan, Xianyu, Tremblin, P., Turner, Jake D., Venot, Olivia, Waalkes, William C., Wheatley, Peter J., and Zhang, Xi

Abstract

The Saturn-mass exoplanet WASP-39b has been the subject of extensive efforts to determine its atmospheric properties using transmission spectroscopy1–4. However, these efforts have been hampered by modelling degeneracies between composition and cloud properties that are caused by limited data quality5–9. Here we present the transmission spectrum of WASP-39b obtained using the Single-Object Slitless Spectroscopy (SOSS) mode of the Near Infrared Imager and Slitless Spectrograph (NIRISS) instrument on the JWST. This spectrum spans 0.6–2.8 μm in wavelength and shows several water-absorption bands, the potassium resonance doublet and signatures of clouds. The precision and broad wavelength coverage of NIRISS/SOSS allows us to break model degeneracies between cloud properties and the atmospheric composition of WASP-39b, favouring a heavy-element enhancement (‘metallicity’) of about 10–30 times the solar value, a sub-solar carbon-to-oxygen (C/O) ratio and a solar-to-super-solar potassium-to-oxygen (K/O) ratio. The observations are also best explained by wavelength-dependent, non-grey clouds with inhomogeneous coverageof the planet’s terminator.

Published
2023
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6. Early Release Science of the exoplanet WASP-39b with JWST NIRCam

Author

Ahrer, Eva-Maria, Stevenson, Kevin B., Mansfield, Megan, Moran, Sarah E., Brande, Jonathan, Morello, Giuseppe, Murray, Catriona A., Nikolov, Nikolay K., Petit dit de la Roche, Dominique J. M., Schlawin, Everett, Wheatley, Peter J., Zieba, Sebastian, Batalha, Natasha E., Damiano, Mario, Goyal, Jayesh M., Lendl, Monika, Lothringer, Joshua D., Mukherjee, Sagnick, Ohno, Kazumasa, Batalha, Natalie M., Battley, Matthew P., Bean, Jacob L., Beatty, Thomas G., Benneke, Björn, Berta-Thompson, Zachory K., Carter, Aarynn L., Cubillos, Patricio E., Daylan, Tansu, Espinoza, Néstor, Gao, Peter, Gibson, Neale P., Gill, Samuel, Harrington, Joseph, Hu, Renyu, Kreidberg, Laura, Lewis, Nikole K., Line, Michael R., López-Morales, Mercedes, Parmentier, Vivien, Powell, Diana K., Sing, David K., Tsai, Shang-Min, Wakeford, Hannah R., Welbanks, Luis, Alam, Munazza K., Alderson, Lili, Allen, Natalie H., Anderson, David R., Barstow, Joanna K., Bayliss, Daniel, Bell, Taylor J., Blecic, Jasmina, Bryant, Edward M., Burleigh, Matthew R., Carone, Ludmila, Casewell, S. L., Changeat, Quentin, Chubb, Katy L., Crossfield, Ian J. M., Crouzet, Nicolas, Decin, Leen, Désert, Jean-Michel, Feinstein, Adina D., Flagg, Laura, Fortney, Jonathan J., Gizis, John E., Heng, Kevin, Iro, Nicolas, Kempton, Eliza M.-R., Kendrew, Sarah, Kirk, James, Knutson, Heather A., Komacek, Thaddeus D., Lagage, Pierre-Olivier, Leconte, Jérémy, Lustig-Yaeger, Jacob, MacDonald, Ryan J., Mancini, Luigi, May, E. M., Mayne, N. J., Miguel, Yamila, Mikal-Evans, Thomas, Molaverdikhani, Karan, Palle, Enric, Piaulet, Caroline, Rackham, Benjamin V., Redfield, Seth, Rogers, Laura K., Roy, Pierre-Alexis, Rustamkulov, Zafar, Shkolnik, Evgenya L., Sotzen, Kristin S., Taylor, Jake, Tremblin, P., Tucker, Gregory S., Turner, Jake D., de Val-Borro, Miguel, Venot, Olivia, and Zhang, Xi

Abstract

Measuring the metallicity and carbon-to-oxygen (C/O) ratio in exoplanet atmospheres is a fundamental step towards constraining the dominant chemical processes at work and, if in equilibrium, revealing planet formation histories. Transmission spectroscopy (for example, refs. 1,2) provides the necessary means by constraining the abundances of oxygen- and carbon-bearing species; however, this requires broad wavelength coverage, moderate spectral resolution and high precision, which, together, are not achievable with previous observatories. Now that JWST has commenced science operations, we are able to observe exoplanets at previously uncharted wavelengths and spectral resolutions. Here we report time-series observations of the transiting exoplanet WASP-39b using JWST’s Near InfraRed Camera (NIRCam). The long-wavelength spectroscopic and short-wavelength photometric light curves span 2.0–4.0 micrometres, exhibit minimal systematics and reveal well defined molecular absorption features in the planet’s spectrum. Specifically, we detect gaseous water in the atmosphere and place an upper limit on the abundance of methane. The otherwise prominent carbon dioxide feature at 2.8 micrometres is largely masked by water. The best-fit chemical equilibrium models favour an atmospheric metallicity of 1–100-times solar (that is, an enrichment of elements heavier than helium relative to the Sun) and a substellar C/O ratio. The inferred high metallicity and low C/O ratio may indicate significant accretion of solid materials during planet formation (for example, refs. 3,4,) or disequilibrium processes in the upper atmosphere (for example, refs. 5,6).

Published
2023
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7. Early Release Science of the exoplanet WASP-39b with JWST NIRSpec G395H

Author

Alderson, Lili, Wakeford, Hannah R., Alam, Munazza K., Batalha, Natasha E., Lothringer, Joshua D., Adams Redai, Jea, Barat, Saugata, Brande, Jonathan, Damiano, Mario, Daylan, Tansu, Espinoza, Néstor, Flagg, Laura, Goyal, Jayesh M., Grant, David, Hu, Renyu, Inglis, Julie, Lee, Elspeth K. H., Mikal-Evans, Thomas, Ramos-Rosado, Lakeisha, Roy, Pierre-Alexis, Wallack, Nicole L., Batalha, Natalie M., Bean, Jacob L., Benneke, Björn, Berta-Thompson, Zachory K., Carter, Aarynn L., Changeat, Quentin, Colón, Knicole D., Crossfield, Ian J. M., Désert, Jean-Michel, Foreman-Mackey, Daniel, Gibson, Neale P., Kreidberg, Laura, Line, Michael R., López-Morales, Mercedes, Molaverdikhani, Karan, Moran, Sarah E., Morello, Giuseppe, Moses, Julianne I., Mukherjee, Sagnick, Schlawin, Everett, Sing, David K., Stevenson, Kevin B., Taylor, Jake, Aggarwal, Keshav, Ahrer, Eva-Maria, Allen, Natalie H., Barstow, Joanna K., Bell, Taylor J., Blecic, Jasmina, Casewell, Sarah L., Chubb, Katy L., Crouzet, Nicolas, Cubillos, Patricio E., Decin, Leen, Feinstein, Adina D., Fortney, Joanthan J., Harrington, Joseph, Heng, Kevin, Iro, Nicolas, Kempton, Eliza M.-R., Kirk, James, Knutson, Heather A., Krick, Jessica, Leconte, Jérémy, Lendl, Monika, MacDonald, Ryan J., Mancini, Luigi, Mansfield, Megan, May, Erin M., Mayne, Nathan J., Miguel, Yamila, Nikolov, Nikolay K., Ohno, Kazumasa, Palle, Enric, Parmentier, Vivien, Petit dit de la Roche, Dominique J. M., Piaulet, Caroline, Powell, Diana, Rackham, Benjamin V., Redfield, Seth, Rogers, Laura K., Rustamkulov, Zafar, Tan, Xianyu, Tremblin, P., Tsai, Shang-Min, Turner, Jake D., de Val-Borro, Miguel, Venot, Olivia, Welbanks, Luis, Wheatley, Peter J., and Zhang, Xi

Abstract

Measuring the abundances of carbon and oxygen in exoplanet atmospheres is considered a crucial avenue for unlocking the formation and evolution of exoplanetary systems1,2. Access to the chemical inventory of an exoplanet requires high-precision observations, often inferred from individual molecular detections with low-resolution space-based3–5and high-resolution ground-based6–8facilities. Here we report the medium-resolution (R≈ 600) transmission spectrum of an exoplanet atmosphere between 3 and 5 μm covering several absorption features for the Saturn-mass exoplanet WASP-39b (ref. 9), obtained with the Near Infrared Spectrograph (NIRSpec) G395H grating of JWST. Our observations achieve 1.46 times photon precision, providing an average transit depth uncertainty of 221 ppm per spectroscopic bin, and present minimal impacts from systematic effects. We detect significant absorption from CO2(28.5σ) and H2O (21.5σ), and identify SO2as the source of absorption at 4.1 μm (4.8σ). Best-fit atmospheric models range between 3 and 10 times solar metallicity, with sub-solar to solar C/O ratios. These results, including the detection of SO2, underscore the importance of characterizing the chemistry in exoplanet atmospheres and showcase NIRSpec G395H as an excellent mode for time-series observations over this critical wavelength range10.

Published
2023
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9. Direct imaging and spectroscopy of exoplanetary systems with the JWST early release science program

Author

Coyle, Laura E., Matsuura, Shuji, Perrin, Marshall D., Hinkley, Sasha, Carter, Aarynn L., Ray, Shrishmoy, Biller, Beth, Skemer, Andrew, Choquet, Elodie, Millar-Blanchaer, Maxwell A., Sallum, Stephanie, Miles, Brittany, Whiteford, Niall, Patapis, Polychronis, Perrin, Marshall, Pueyo, Laurent, Stapelfeldt, Karl, Wang, Jason, Ward-Duong, Kimberly, Girard, Julien H., Hines, Dean, Kammerer, Jens, Leisenring, Jarron, Zhou, Yifan, Meyer, Michael, Liu, Michael C., Bonnefoy, Mickael, Petrus, Simon, Bonavita, Mariangela, Chauvin, Gael, Chen, Christine, Currie, Thayne, Hoch, Kielan K. H., Lazzoni, Cecilia, Matthews, Elisabeth C., McElwain, Michael, Rebollido, Isabel, Rickman, Emily, Schneider, Glenn, Sivaramakrishnan, Anand, and Stone, Jordan M.

Published
2022
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11. Simulating JWST high contrast observations with PanCAKE

Author

Shaklan, Stuart B., Ruane, Garreth J., Carter, Aarynn L., Skemer, Andrew J. I., Danielski, Camilla, Leisenring, Jarron, Wang, Jason J., Van Gorkom, Kyle, York, Brian, Adams, Jea, Biller, Beth, Girard, Julien H., Hinkley, Sasha, Nickson, Bryony, Perrin, Marshall, and Pueyo, Laurent

Published
2021
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12. The JWST Early Release Science Program for the Direct Imaging and Spectroscopy of Exoplanetary Systems

Author

Hinkley, Sasha, Carter, Aarynn L., Ray, Shrishmoy, Skemer, Andrew, Biller, Beth, Choquet, Elodie, Millar-Blanchaer, Maxwell A., Sallum, Stephanie, Miles, Brittany, Whiteford, Niall, Patapis, Polychronis, Perrin, Marshall, Pueyo, Laurent, Schneider, Glenn, Stapelfeldt, Karl, Wang, Jason, Ward-Duong, Kimberly, Bowler, Brendan P., Boccaletti, Anthony, H. Girard, Julien, Hines, Dean, Kalas, Paul, Kammerer, Jens, Kervella, Pierre, Leisenring, Jarron, Pantin, Eric, Zhou, Yifan, Meyer, Michael, Liu, Michael C., Bonnefoy, Mickael, Currie, Thayne, McElwain, Michael, Metchev, Stanimir, Wyatt, Mark, Absil, Olivier, Adams, Jea, Barman, Travis, Baraffe, Isabelle, Bonavita, Mariangela, Booth, Mark, Bryan, Marta, Chauvin, Gael, Chen, Christine, Danielski, Camilla, Furio, Matthew De, Factor, Samuel M., Fitzgerald, Michael P., Fortney, Jonathan J., Grady, Carol, Greenbaum, Alexandra, Henning, Thomas, Hoch, Kielan K. W., Janson, Markus, Kennedy, Grant, Kenworthy, Matthew, Kraus, Adam, Kuzuhara, Masayuki, Lagage, Pierre-Olivier, Lagrange, Anne-Marie, Launhardt, Ralf, Lazzoni, Cecilia, Lloyd, James, Marino, Sebastian, Marley, Mark, Martinez, Raquel, Marois, Christian, Matthews, Brenda, Matthews, Elisabeth C., Mawet, Dimitri, Mazoyer, Johan, Phillips, Mark, Petrus, Simon, Quanz, Sascha P., Quirrenbach, Andreas, Rameau, Julien, Rebollido, Isabel, Rickman, Emily, Samland, Matthias, Sargent, B., Schlieder, Joshua E., Sivaramakrishnan, Anand, Stone, Jordan M., Tamura, Motohide, Tremblin, Pascal, Uyama, Taichi, Vasist, Malavika, Vigan, Arthur, Wagner, Kevin, and Ygouf, Marie

Abstract

The directcharacterization of exoplanetary systems with high-contrast imaging is among the highest priorities for the broader exoplanet community. As large space missions will be necessary for detecting and characterizing exo-Earth twins, developing the techniques and technology for direct imaging of exoplanets is a driving focus for the community. For the first time, JWST will directly observe extrasolar planets at mid-infrared wavelengths beyond 5 μm, deliver detailed spectroscopy revealing much more precise chemical abundances and atmospheric conditions, and provide sensitivity to analogs of our solar system ice-giant planets at wide orbital separations, an entirely new class of exoplanet. However, in order to maximize the scientific output over the lifetime of the mission, an exquisite understanding of the instrumental performance of JWST is needed as early in the mission as possible. In this paper, we describe our 55 hr Early Release Science Program that will utilize all four JWST instruments to extend the characterization of planetary-mass companions to ∼15 μm as well as image a circumstellar disk in the mid-infrared with unprecedented sensitivity. Our program will also assess the performance of the observatory in the key modes expected to be commonly used for exoplanet direct imaging and spectroscopy, optimize data calibration and processing, and generate representative data sets that will enable a broad user base to effectively plan for general observing programs in future Cycles.

Published
2022
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13. The Transiting Exoplanet Community Early Release Science Program for JWST

Author

Bean, Jacob L., Stevenson, Kevin B., Batalha, Natalie M., Berta-Thompson, Zachory, Kreidberg, Laura, Crouzet, Nicolas, Benneke, Björn, Line, Michael R., Sing, David K., Wakeford, Hannah R., Knutson, Heather A., Kempton, Eliza M.-R., Désert, Jean-Michel, Crossfield, Ian, Batalha, Natasha E., Wit, Julien de, Parmentier, Vivien, Harrington, Joseph, Moses, Julianne I., Lopez-Morales, Mercedes, Alam, Munazza K., Blecic, Jasmina, Bruno, Giovanni, Carter, Aarynn L., Chapman, John W., Decin, Leen, Dragomir, Diana, Evans, Thomas M., Fortney, Jonathan J., Fraine, Jonathan D., Gao, Peter, Muñoz, Antonio García, Gibson, Neale P., Goyal, Jayesh M., Heng, Kevin, Hu, Renyu, Kendrew, Sarah, Kilpatrick, Brian M., Krick, Jessica, Lagage, Pierre-Olivier, Lendl, Monika, Louden, Tom, Madhusudhan, Nikku, Mandell, Avi M., Mansfield, Megan, May, Erin M., Morello, Giuseppe, Morley, Caroline V., Nikolov, Nikolay, Redfield, Seth, Roberts, Jessica E., Schlawin, Everett, Spake, Jessica J., Todorov, Kamen O., Tsiaras, Angelos, Venot, Olivia, Waalkes, William C., Wheatley, Peter J., Zellem, Robert T., Angerhausen, Daniel, Barrado, David, Carone, Ludmila, Casewell, Sarah L., Cubillos, Patricio E., Damiano, Mario, Val-Borro, Miguel de, Drummond, Benjamin, Edwards, Billy, Endl, Michael, Espinoza, Nestor, France, Kevin, Gizis, John E., Greene, Thomas P., Henning, Thomas K., Hong, Yucian, Ingalls, James G., Iro, Nicolas, Irwin, Patrick G. J., Kataria, Tiffany, Lahuis, Fred, Leconte, Jérémy, Lillo-Box, Jorge, Lines, Stefan, Lothringer, Joshua D., Mancini, Luigi, Marchis, Franck, Mayne, Nathan, Palle, Enric, Rauscher, Emily, Roudier, Gaël, Shkolnik, Evgenya L., Southworth, John, Swain, Mark R., Taylor, Jake, Teske, Johanna, Tinetti, Giovanna, Tremblin, Pascal, Tucker, Gregory S., Boekel, Roy van, Waldmann, Ingo P., Weaver, Ian C., and Zingales, Tiziano

Abstract

The James Webb Space Telescope(JWST) presents the opportunity to transform our understanding of planets and the origins of life by revealing the atmospheric compositions, structures, and dynamics of transiting exoplanets in unprecedented detail. However, the high-precision, timeseries observations required for such investigations have unique technical challenges, and prior experience with Hubble, Spitzer, and other facilities indicates that there will be a steep learning curve when JWSTbecomes operational. In this paper, we describe the science objectives and detailed plans of the Transiting Exoplanet Community Early Release Science (ERS) Program, which is a recently approved program for JWSTobservations early in Cycle 1. We also describe the simulations used to establish the program. The goal of this project, for which the obtained data will have no exclusive access period, is to accelerate the acquisition and diffusion of technical expertise for transiting exoplanet observations with JWST, while also providing a compelling set of representative data sets that will enable immediate scientific breakthroughs. The Transiting Exoplanet Community ERS Program will exercise the timeseries modes of all four JWSTinstruments that have been identified as the consensus highest priorities, observe the full suite of transiting planet characterization geometries (transits, eclipses, and phase curves), and target planets with host stars that span an illustrative range of brightnesses. The observations in this program were defined through an inclusive and transparent process that had participation from JWSTinstrument experts and international leaders in transiting exoplanet studies. The targets have been vetted with previous measurements, will be observable early in the mission, and have exceptional scientific merit. Community engagement in the project will be centered on a two-phase Data Challenge that culminates with the delivery of planetary spectra, timeseries instrument performance reports, and open-source data analysis toolkits in time to inform the agenda for Cycle 2 of the JWSTmission.

Published
2018
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