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1. The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems V: Do Self-Consistent Atmospheric Models Represent JWST Spectra? A Showcase With VHS 1256 b

Author

Petrus, Simon, Whiteford, Niall, Patapis, Polychronis, Biller, Beth A., Skemer, Andrew, Hinkley, Sasha, Suárez, Genaro, Lueber, Anna, Palma-Bifani, Paulina, Stone, Jordan M., Vos, Johanna M., Morley, Caroline V., Tremblin, Pascal, Charnay, Benjamin, Helling, Christiane, Miles, Brittany E., Carter, Aarynn L., Wang, Jason J., Janson, Markus, Gonzales, Eileen C., Sutlieff, Ben, Hoch, Kielan K. W., Bonnefoy, Mickaël, Chauvin, Gaël, Absil, Olivier, Balmer, William O., Boccaletti, Anthony, Bonavita, Mariangela, Booth, Mark, Bowler, Brendan P., Briesemeister, Zackery W., Bryan, Marta L., Calissendorff, Per, Cantalloube, Faustine, Chen, Christine H., Choquet, Elodie, Christiaens, Valentin, Cugno, Gabriele, Currie, Thayne, Danielski, Camilla, De Furio, Matthew, Dupuy, Trent J., Factor, Samuel M., Faherty, Jacqueline K., Fitzgerald, Michael P., Fortney, Jonathan J., Franson, Kyle, Girard, Julien H., Grady, Carol A., Henning, Thomas, Hines, Dean C., Hood, Callie E., Howe, Alex R., Kalas, Paul, Kammerer, Jens, Kennedy, Grant M., Kenworthy, Matthew A., Kervella, Pierre, Kim, Minjae, Kitzmann, Daniel, Kraus, Adam L., Kuzuhara, Masayuki, Lagage, Pierre-Olivier, Lagrange, Anne-Marie, Lawson, Kellen, Lazzoni, Cecilia, Leisenring, Jarron M., Lew, Ben W. P., Liu, Michael C., Liu, Pengyu, Llop-Sayson, Jorge, Lloyd, James P., Macintosh, Bruce, Mâlin, Mathilde, Manjavacas, Elena, Marino, Sebastián, Marley, Mark S., Marois, Christian, Martinez, Raquel A., Matthews, Elisabeth C., Matthews, Brenda C., Mawet, Dimitri, Mazoyer, Johan, McElwain, Michael W., Metchev, Stanimir, Meyer, Michael R., Millar-Blanchaer, Maxwell A., Mollière, Paul, Moran, Sarah E., Mukherjee, Sagnick, Pantin, Eric, Perrin, Marshall D., Pueyo, Laurent, Quanz, Sascha P., Quirrenbach, Andreas, Ray, Shrishmoy, Rebollido, Isabel, Redai, Jea Adams, Ren, Bin B., Rickman, Emily, Sallum, Steph, Samland, Matthias, Sargent, Benjamin, Schlieder, Joshua E., Stapelfeldt, Karl R., Tamura, Motohide, Tan, Xianyu, Theissen, Christopher A., Uyama, Taichi, Vasist, Malavika, Vigan, Arthur, Wagner, Kevin, Ward-Duong, Kimberly, Wolff, Schuyler G., Worthen, Kadin, Wyatt, Mark C., Ygouf, Marie, Zurlo, Alice, Zhang, Xi, Zhang, Keming, Zhan, Zhoujian, and Zhou, Yifan

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The unprecedented medium-resolution (R~1500-3500) near- and mid-infrared (1-18um) spectrum provided by JWST for the young (140+/-20Myr) low-mass (12-20MJup) L-T transition (L7) companion VHS1256b gives access to a catalogue of molecular absorptions. In this study, we present a comprehensive analysis of this dataset utilizing a forward modelling approach, applying our Bayesian framework, ForMoSA. We explore five distinct atmospheric models to assess their performance in estimating key atmospheric parameters: Teff, log(g), [M/H], C/O, gamma, fsed, and R. Our findings reveal that each parameter's estimate is significantly influenced by factors such as the wavelength range considered and the model chosen for the fit. This is attributed to systematic errors in the models and their challenges in accurately replicating the complex atmospheric structure of VHS1256b, notably the complexity of its clouds and dust distribution. To propagate the impact of these systematic uncertainties on our atmospheric property estimates, we introduce innovative fitting methodologies based on independent fits performed on different spectral windows. We finally derived a Teff consistent with the spectral type of the target, considering its young age, which is confirmed by our estimate of log(g). Despite the exceptional data quality, attaining robust estimates for chemical abundances [M/H] and C/O, often employed as indicators of formation history, remains challenging. Nevertheless, the pioneering case of JWST's data for VHS1256b has paved the way for future acquisitions of substellar spectra that will be systematically analyzed to directly compare the properties of these objects and correct the systematics in the models., Comment: 32 pages, 16 figures, 6 tables, 2 appendices

Published
2023

2. 15NH3 in the atmosphere of a cool brown dwarf

Author

Barrado, David, Mollière, Paul, Patapis, Polychronis, Min, Michiel, Tremblin, Pascal, Martinez, Francisco Ardevol, Whiteford, Niall, Vasist, Malavika, Argyriou, Ioannis, Samland, Matthias, Lagage, Pierre-Olivier, Decin, Leen, Waters, Rens, Henning, Thomas, Morales-Calderón, María, Guedel, Manuel, Vandenbussche, Bart, Absil, Olivier, Baudoz, Pierre, Boccaletti, Anthony, Bouwman, Jeroen, Cossou, Christophe, Coulais, Alain, Crouzet, Nicolas, Gastaud, René, Glasse, Alistair, Glauser, Adrian M., Kamp, Inga, Kendrew, Sarah, Krause, Oliver, Lahuis, Fred, Mueller, Michael, Olofsson, Göran, Pye, John, Rouan, Daniel, Royer, Pierre, Scheithauer, Silvia, Waldmann, Ingo, Colina, Luis, van Dishoeck, Ewine F., Ray, Tom, Östlin, Göran, and Wright, Gillian

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

Brown dwarfs serve as ideal laboratories for studying the atmospheres of giant exoplanets on wide orbits as the governing physical and chemical processes in them are nearly identical. Understanding the formation of gas giant planets is challenging, often involving the endeavour to link atmospheric abundance ratios, such as the carbon-to-oxygen (C/O) ratio, to formation scenarios. However, the complexity of planet formation requires additional tracers, as the unambiguous interpretation of the measured C/O ratio is fraught with complexity. Isotope ratios, such as deuterium-to-hydrogen and 14N/15N, offer a promising avenue to gain further insight into this formation process, mirroring their utility within the solar system. For exoplanets only a handful of constraints on 12C/13C exist, pointing to the accretion of 13C-rich ice from beyond the disks' CO iceline. Here we report on the mid-infrared detection of the 14NH3 and 15NH3 isotopologues in the atmosphere of a cool brown dwarf with an effective temperature of 380 K in a spectrum taken with the Mid-InfraRed Instrument of the James Webb Space Telescope. As expected, our results reveal a 14N/15N value consistent with star-like formation by gravitational collapse, demonstrating that this ratio can be accurately constrained. Since young stars and their planets should be more strongly enriched in the 15N isotope, we expect that 15NH3 will be detectable in a number of cold, wide-separation exoplanets., Comment: Accepted by Nature. 28 pages, 7 figures, uses nature3.cls

Published
2023
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3. The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems III: Aperture Masking Interferometric Observations of the star HIP 65426

Author

Ray, Shrishmoy, Sallum, Steph, Hinkley, Sasha, Sivamarakrishnan, Anand, Cooper, Rachel, Kammerer, Jens, Greebaum, Alexandra Z., Thatte, Deepashri, Lazzoni, Cecilia, Tokovinin, Andrei, de Furio, Matthew, Factor, Samuel, Meyer, Michael, Stone, Jordan M., Carter, Aarynn, Biller, Beth, Skemer, Andrew, Suarez, Genaro, Leisenring, Jarron M., Perrin, Marshall D., Kraus, Adam L., Absil, Olivier, Balmer, William O., Bonnefoy, Mickael, Bryan, Marta L., Betti, Sarah K., Boccaletti, Anthony, Bonavita, Mariangela, Booth, Mark, Bowler, Brendan P., Briesemeister, Zackery W., Cantalloube, Faustine, Chauvin, Gael, Christiaens, Valentin, Cugno, Gabriele, Currie, Thayne, Danielski, Camilla, Dupuy, Trent J., Faherty, Jacqueline K., Chen, Christine H., Calissendorff, Per, Choquet, Elodie, Fitzgerald, Michael P., Fortney, Jonathan J., Franson, Kyle, Girard, Julien H., Grady, Carol A., Gonzales, Eileen C., Henning, Thomas, Hines, Dean C., Hoch, Kielan K. W., Hood, Callie E., Howe, Alex R., Janson, Markus, Kalas, Paul, Kennedy, Grant M., Kenworthy, Matthew A., Kervella, Pierre, Kitzmann, Daniel, Kuzuhara, Masayuki, Lagrange, Anne-Marie, Lagage, Pierre-Olivier, Lawson, Kellen, Lew, Ben W. P., Liu, Michael C., Liu, Pengyu, Llop-Sayson, Jorge, Lloyd, James P., Lueber, Anna, Macintosh, Bruce, Manjavacas, Elena, Marino, Sebastian, Marley, Mark S., Marois, Christian, Martinez, Raquel A., Matthews, Brenda C., Matthews, Elisabeth C., Mawet, Dimitri, Mazoyer, Johan, McElwain, Michael W., Metchev, Stanimir, Miles, Brittany E., Millar-Blanchaer, Maxwell A., Molliere, Paul, Moran, Sarah E., Morley, Caroline V., Mukherjee, Sagnick, Palma-Bifani, Paulina, Pantin, Eric, Patapis, Polychronis, Petrus, Simon, Pueyo, Laurent, Quanz, Sascha P., Quirrenbach, Andreas, Rebollido, Isabel, Redai, Jea Adams, Ren, Bin B., Rickman, Emily, Samland, Matthias, Sargent, B. A., Schlieder, Joshua E., Schneider, Glenn, Stapelfeldt, Karl R., Sutlieff, Ben J., Tamura, Motohide, Tan, Xianyu, Theissen, Christopher A., Uyama, Taichi, Vigan, Arthur, Vasist, Malavika, Vos, Johanna M., Wagner, Kevin, Wang, Jason J., Ward-Duong, Kimberly, Whiteford, Niall, Wolff, Schuyler G., Worthen, Kadin, Wyatt, Mark C., Ygouf, Marie, Zhang, Xi, Zhang, Keming, Zhang, Zhoujian, and Zhou, Yifan

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present aperture masking interferometry (AMI) observations of the star HIP 65426 at $3.8\,\rm{\mu m}$ as a part of the JWST Direct Imaging Early Release Science (ERS) program obtained using the Near Infrared Imager and Slitless Spectrograph (NIRISS) instrument. This mode provides access to very small inner working angles (even separations slightly below the Michelson limit of $0.5\lambda/D$ for an interferometer), which are inaccessible with the classical inner working angles of the JWST coronagraphs. When combined with JWST's unprecedented infrared sensitivity, this mode has the potential to probe a new portion of parameter space across a wide array of astronomical observations. Using this mode, we are able to achieve a $5\sigma$ contrast of $\Delta m{\sim}7.62{\pm}0.13$ mag relative to the host star at separations ${\gtrsim}0.07{"}$, and the contrast deteriorates steeply at separations ${\lesssim}0.07{"}$. However, we detect no additional companions interior to the known companion HIP 65426 b (at separation ${\sim}0.82{"}$ or, $87^{+108}_{-31}\,\rm{au}$). Our observations thus rule out companions more massive than $10{-}12\,\rm{M_{Jup}}$ at separations ${\sim}10{-}20\,\rm{au}$ from HIP 65426, a region out of reach of ground or space-based coronagraphic imaging. These observations confirm that the AMI mode on JWST is sensitive to planetary mass companions at close-in separations (${\gtrsim}0.07{"}$), even for thousands of more distant stars at $\sim$100 pc, in addition to the stars in the nearby young moving groups as stated in previous works. This result will allow the planning and successful execution of future observations to probe the inner regions of nearby stellar systems, opening an essentially unexplored parameter space., Comment: 20 pages, 12 figures, submitted to ApJL

Published
2023

4. The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems IV: NIRISS Aperture Masking Interferometry Performance and Lessons Learned

Author

Sallum, Steph, Ray, Shrishmoy, Kammerer, Jens, Sivaramakrishnan, Anand, Cooper, Rachel, Greebaum, Alexandra Z., Thatte, Deepashri, de Furio, Matthew, Factor, Samuel, Meyer, Michael, Stone, Jordan M., Carter, Aarynn, Biller, Beth, Hinkley, Sasha, Skemer, Andrew, Suarez, Genaro, Leisenring, Jarron M., Perrin, Marshall D., Kraus, Adam L., Absil, Olivier, Balmer, William O., Bonnefoy, Mickael, Bryan, Marta L., Betti, Sarah K., Boccaletti, Anthony, Bonavita, Mariangela, Booth, Mark, Bowler, Brendan P., Briesemeister, Zackery W., Cantalloube, Faustine, Chauvin, Gael, Christiaens, Valentin, Cugno, Gabriele, Currie, Thayne, Danielski, Camilla, Dupuy, Trent J., Faherty, Jacqueline K., Chen, Christine H., Calissendorff, Per, Choquet, Elodie, Fitzgerald, Michael P., Fortney, Jonathan J., Franson, Kyle, Girard, Julien H., Grady, Carol A., Gonzales, Eileen C., Henning, Thomas, Hines, Dean C., Hoch, Kielan K. W., Hood, Callie E., Howe, Alex R., Janson, Markus, Kalas, Paul, Kennedy, Grant M., Kenworthy, Matthew A., Kervella, Pierre, Kitzmann, Daniel, Kuzuhara, Masayuki, Lagrange, Anne-Marie, Lagage, Pierre-Olivier, Lawson, Kellen, Lazzoni, Cecilia, Lew, Ben W. P., Liu, Michael C., Liu, Pengyu, Llop-Sayson, Jorge, Lloyd, James P., Lueber, Anna, Macintosh, Bruce, Manjavacas, Elena, Marino, Sebastian, Marley, Mark S., Marois, Christian, Martinez, Raquel A., Matthews, Brenda C., Matthews, Elisabeth C., Mawet, Dimitri, Mazoyer, Johan, McElwain, Michael W., Metchev, Stanimir, Miles, Brittany E., Millar-Blanchaer, Maxwell A., Molliere, Paul, Moran, Sarah E., Morley, Caroline V., Mukherjee, Sagnick, Palma-Bifani, Paulina, Pantin, Eric, Patapis, Polychronis, Petrus, Simon, Pueyo, Laurent, Quanz, Sascha P., Quirrenbach, Andreas, Rebollido, Isabel, Redai, Jea Adams, Ren, Bin B., Rickman, Emily, Samland, Matthias, Sargent, B. A., Schlieder, Joshua E., Schneider, Glenn, Stapelfeldt, Karl R., Sutlieff, Ben J., Tamura, Motohide, Tan, Xianyu, Theissen, Christopher A., Uyama, Taichi, Vigan, Arthur, Vasist, Malavika, Vos, Johanna M., Wagner, Kevin, Wang, Jason J., Ward-Duong, Kimberly, Whiteford, Niall, Wolff, Schuyler G., Worthen, Kadin, Wyatt, Mark C., Ygouf, Marie, Zhang, Xi, Zhang, Keming, Zhang, Zhoujian, Zhou, Yifan, and Zurlo, Alice

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present a performance analysis for the aperture masking interferometry (AMI) mode on board the James Webb Space Telescope Near Infrared Imager and Slitless Spectrograph (JWST/NIRISS). Thanks to self-calibrating observables, AMI accesses inner working angles down to and even within the classical diffraction limit. The scientific potential of this mode has recently been demonstrated by the Early Release Science (ERS) 1386 program with a deep search for close-in companions in the HIP 65426 exoplanetary system. As part of ERS 1386, we use the same data set to explore the random, static, and calibration errors of NIRISS AMI observables. We compare the observed noise properties and achievable contrast to theoretical predictions. We explore possible sources of calibration errors and show that differences in charge migration between the observations of HIP 65426 and point-spread function calibration stars can account for the achieved contrast curves. Lastly, we use self-calibration tests to demonstrate that with adequate calibration NIRISS F380M AMI can reach contrast levels of $\sim9-10$ mag at $\gtrsim \lambda/D$. These tests lead us to observation planning recommendations and strongly motivate future studies aimed at producing sophisticated calibration strategies taking these systematic effects into account. This will unlock the unprecedented capabilities of JWST/NIRISS AMI, with sensitivity to significantly colder, lower-mass exoplanets than lower-contrast ground-based AMI setups, at orbital separations inaccessible to JWST coronagraphy., Comment: 20 pages, 12 figures, accepted to Astrophysical Journal Letters

Published
2023

5. The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems: Best Practices for Data Collection in Cycle 2 and Beyond

Author

Hinkley, Sasha, Biller, Beth, Skemer, Andrew, Carter, Aarynn L., Girard, Julien, Hines, Dean, Kammerer, Jens, Leisenring, Jarron, Balmer, William, Choquet, Elodie, Millar-Blanchaer, Maxwell A., Perrin, Marshall, Pueyo, Laurent, Wang, Jason, Ward-Duong, Kimberly, Boccaletti, Anthony, Miles, Brittany, Patapis, Polychronis, Rebollido, Isabel, Rickman, Emily, Sargent, B., Worthen, Kadin, Hoch, Kielan, Chen, Christine, Sallum, Stephanie, Ray, Shrishmoy, Stapelfeldt, Karl, Zhou, Yifan, Meyer, Michael, Bonnefoy, Mickael, Currie, Thayne, Danielski, Camilla, Matthews, Elisabeth C., Sivaramakrishnan, Anand, Cooper, Rachel A., Thatte, Deepashri, Stone, Jordan, and Vasist, Malavika

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

We present a set of recommended best practices for JWST data collection for members of the community focussed on the direct imaging and spectroscopy of exoplanetary systems. These findings and recommendations are based on the early analysis of the JWST Early Release Science Program 1386, "High-Contrast Imaging of Exoplanets and Exoplanetary Systems with JWST." Our goal is for this information to be useful for observers in preparation of JWST proposals for Cycle 2 and beyond. In addition to compiling a set of best practices from our ERS program, in a few cases we also draw on the expertise gained within the instrument commissioning programs, as well as include a handful of data processing best practices. We anticipate that this document will be regularly updated and resubmitted to arXiv.org to ensure that we have distributed our knowledge of best-practices for data collection as widely and efficiently as possible., Comment: Not yet submitted for publication. Intended only to be a community resource for JWST Cycle 2 proposals

Published
2023

6. Neural posterior estimation for exoplanetary atmospheric retrieval

Author

Vasist, Malavika, Rozet, François, Absil, Olivier, Mollière, Paul, Nasedkin, Evert, and Louppe, Gilles

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Retrieving the physical parameters from spectroscopic observations of exoplanets is key to understanding their atmospheric properties. Exoplanetary atmospheric retrievals are usually based on approximate Bayesian inference and rely on sampling-based approaches to compute parameter posterior distributions. Accurate or repeated retrievals, however, can result in very long computation times due to the sequential nature of sampling-based algorithms. We aim to amortize exoplanetary atmospheric retrieval using neural posterior estimation (NPE), a simulation-based inference algorithm based on variational inference and normalizing flows. In this way, we aim (i) to strongly reduce inference time, (ii) to scale inference to complex simulation models with many nuisance parameters or intractable likelihood functions, and (iii) to enable the statistical validation of the inference results. We evaluate NPE on a radiative transfer model for exoplanet spectra petitRADTRANS, including the effects of scattering and clouds. We train a neural autoregressive flow to quickly estimate posteriors and compare against retrievals computed with MultiNest. NPE produces accurate posterior approximations while reducing inference time down to a few seconds. We demonstrate the computational faithfulness of our posterior approximations using inference diagnostics including posterior predictive checks and coverage, taking advantage of the quasi-instantaneous inference time of NPE. Our analysis confirms the reliability of the approximate posteriors produced by NPE. The accuracy and reliability of the inference results produced by NPE establishes it as a promising approach for atmospheric retrievals. Amortization of the posterior inference makes repeated inference on several observations computationally inexpensive since it does not require on-the-fly simulations, making the retrieval efficient, scalable, and testable., Comment: The paper has been submitted to AandA after a final revision

Published
2023
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7. The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems II: A 1 to 20 Micron Spectrum of the Planetary-Mass Companion VHS 1256-1257 b

Author

Miles, Brittany E., Biller, Beth A., Patapis, Polychronis, Worthen, Kadin, Rickman, Emily, Hoch, Kielan K. W., Skemer, Andrew, Perrin, Marshall D., Whiteford, Niall, Chen, Christine H., Sargent, B., Mukherjee, Sagnick, Morley, Caroline V., Moran, Sarah E., Bonnefoy, Mickael, Petrus, Simon, Carter, Aarynn L., Choquet, Elodie, Hinkley, Sasha, Ward-Duong, Kimberly, Leisenring, Jarron M., Millar-Blanchaer, Maxwell A., Pueyo, Laurent, Ray, Shrishmoy, Stapelfeldt, Karl R., Stone, Jordan M., Wang, Jason J., Absil, Olivier, Balmer, William O., Boccaletti, Anthony, Bonavita, Mariangela, Booth, Mark, Bowler, Brendan P., Chauvin, Gael, Christiaens, Valentin, Currie, Thayne, Danielski, Camilla, Fortney, Jonathan J., Girard, Julien H., Greenbaum, Alexandra Z., Henning, Thomas, Hines, Dean C., Janson, Markus, Kalas, Paul, Kammerer, Jens, Kenworthy, Matthew A., Kervella, Pierre, Lagage, Pierre-Olivier, Lew, Ben W. P., Liu, Michael C., Macintosh, Bruce, Marino, Sebastian, Marley, Mark S., Marois, Christian, Matthews, Elisabeth C., Matthews, Brenda C., Mawet, Dimitri, McElwain, Michael W., Metchev, Stanimir, Meyer, Michael R., Molliere, Paul, Pantin, Eric, Rebollido, Andreas Quirrenbachm Isabel, Ren, Bin B., Vasist, Malavika, Wyatt, Mark C., Zhou, Yifan, Briesemeister, Zackery W., Bryan, Marta L., Calissendorff, Per, Catalloube, Faustine, Cugno, Gabriele, De Furio, Matthew, Dupuy, Trent J., Factor, Samuel M., Faherty, Jacqueline K., Fitzgerald, Michael P., Franson, Kyle, Gonzales, Eileen C., Hood, Callie E., Howe, Alex R., Kraus, Adam L., Kuzuhara, Masayuki, Lawson, Kellen, Lazzoni, Cecilia, Liu, Pengyu, Llop-Sayson, Jorge, Lloyd, James P., Martinez, Raquel A., Mazoyer, Johan, Quanz, Sascha P., Redai, Jea Adams, Samland, Matthias, Schlieder, Joshua E., Tamura, Motohide, Tan, Xianyu, Uyama, Taichi, Vigan, Arthur, Vos, Johanna M., Wagner, Kevin, Wolff, Schuyler G., Ygouf, Marie, Zhang, Keming, and Zhang, Zhoujian

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

We present the highest fidelity spectrum to date of a planetary-mass object. VHS 1256 b is a $<$20 M$_\mathrm{Jup}$ widely separated ($\sim$8\arcsec, a = 150 au), young, planetary-mass companion that shares photometric colors and spectroscopic features with the directly imaged exoplanets HR 8799 c, d, and e. As an L-to-T transition object, VHS 1256 b exists along the region of the color-magnitude diagram where substellar atmospheres transition from cloudy to clear. We observed VHS 1256~b with \textit{JWST}'s NIRSpec IFU and MIRI MRS modes for coverage from 1 $\mu$m to 20 $\mu$m at resolutions of $\sim$1,000 - 3,700. Water, methane, carbon monoxide, carbon dioxide, sodium, and potassium are observed in several portions of the \textit{JWST} spectrum based on comparisons from template brown dwarf spectra, molecular opacities, and atmospheric models. The spectral shape of VHS 1256 b is influenced by disequilibrium chemistry and clouds. We directly detect silicate clouds, the first such detection reported for a planetary-mass companion., Comment: Accepted ApJL. Iterations of spectra reduced by the ERS team are hosted at this link: https://github.com/bemiles/JWST_VHS1256b_Reduction/tree/main/reduced_spectra

Published
2022
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8. The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems I: High Contrast Imaging of the Exoplanet HIP 65426 b from 2-16 $\mu$m

Author

Carter, Aarynn L., Hinkley, Sasha, Kammerer, Jens, Skemer, Andrew, Biller, Beth A., Leisenring, Jarron M., Millar-Blanchaer, Maxwell A., Petrus, Simon, Stone, Jordan M., Ward-Duong, Kimberly, Wang, Jason J., Girard, Julien H., Hines, Dean C., Perrin, Marshall D., Pueyo, Laurent, Balmer, William O., Bonavita, Mariangela, Bonnefoy, Mickael, Chauvin, Gael, Choquet, Elodie, Christiaens, Valentin, Danielski, Camilla, Kennedy, Grant M., Matthews, Elisabeth C., Miles, Brittany E., Patapis, Polychronis, Ray, Shrishmoy, Rickman, Emily, Sallum, Steph, Stapelfeldt, Karl R., Whiteford, Niall, Zhou, Yifan, Absil, Olivier, Boccaletti, Anthony, Booth, Mark, Bowler, Brendan P., Chen, Christine H., Currie, Thayne, Fortney, Jonathan J., Grady, Carol A., Greenbaum, Alexandra Z., Henning, Thomas, Hoch, Kielan K. W., Janson, Markus, Kalas, Paul, Kenworthy, Matthew A., Kervella, Pierre, Kraus, Adam L., Lagage, Pierre-Olivier, Liu, Michael C., Macintosh, Bruce, Marino, Sebastian, Marley, Mark S., Marois, Christian, Matthews, Brenda C., Mawet, Dimitri, McElwain, Michael W., Metchev, Stanimir, Meyer, Michael R., Molliere, Paul, Moran, Sarah E., Morley, Caroline V., Mukherjee, Sagnick, Pantin, Eric, Quirrenbach, Andreas, Rebollido, Isabel, Ren, Bin B., Schneider, Glenn, Vasist, Malavika, Worthen, Kadin, Wyatt, Mark C., Briesemeister, Zackery W., Bryan, Marta L., Calissendorff, Per, Cantalloube, Faustine, Cugno, Gabriele, De Furio, Matthew, Dupuy, Trent J., Factor, Samuel M., Faherty, Jacqueline K., Fitzgerald, Michael P., Franson, Kyle, Gonzales, Eileen C., Hood, Callie E., Howe, Alex R., Kuzuhara, Masayuki, Lagrange, Anne-Marie, Lawson, Kellen, Lazzoni, Cecilia, Lew, Ben W. P., Liu, Pengyu, Llop-Sayson, Jorge, Lloyd, James P., Martinez, Raquel A., Mazoyer, Johan, Palma-Bifani, Paulina, Quanz, Sascha P., Redai, Jea Adams, Samland, Matthias, Schlieder, Joshua E., Tamura, Motohide, Tan, Xianyu, Uyama, Taichi, Vigan, Arthur, Vos, Johanna M., Wagner, Kevin, Wolff, Schuyler G., Ygouf, Marie, Zhang, Xi, Zhang, Keming, and Zhang, Zhoujian

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

We present JWST Early Release Science (ERS) coronagraphic observations of the super-Jupiter exoplanet, HIP 65426 b, with the Near-Infrared Camera (NIRCam) from 2-5 $\mu$m, and with the Mid-Infrared Instrument (MIRI) from 11-16 $\mu$m. At a separation of $\sim$0.82" (86$^{+116}_{-31}$ au), HIP 65426 b is clearly detected in all seven of our observational filters, representing the first images of an exoplanet to be obtained by JWST, and the first ever direct detection of an exoplanet beyond 5 $\mu$m. These observations demonstrate that JWST is exceeding its nominal predicted performance by up to a factor of 10, depending on separation and subtraction method, with measured 5$\sigma$ contrast limits of $\sim$1$\times10^{-5}$ and $\sim$2$\times10^{-4}$ at 1" for NIRCam at 4.4 $\mu$m and MIRI at 11.3 $\mu$m, respectively. These contrast limits provide sensitivity to sub-Jupiter companions with masses as low as 0.3$M_\mathrm{Jup}$ beyond separations of $\sim$100 au. Together with existing ground-based near-infrared data, the JWST photometry are well fit by a BT-SETTL atmospheric model from 1-16 $\mu$m, and span $\sim$97% of HIP 65426 b's luminous range. Independent of the choice of model atmosphere we measure an empirical bolometric luminosity that is tightly constrained between $\mathrm{log}\!\left(L_\mathrm{bol}/L_{\odot}\right)$=-4.31 to $-$4.14, which in turn provides a robust mass constraint of 7.1$\pm$1.2 $M_\mathrm{Jup}$. In totality, these observations confirm that JWST presents a powerful and exciting opportunity to characterise the population of exoplanets amenable to high-contrast imaging in greater detail., Comment: 35 pages, 16 figures, 4 tables, 1 wonderful telescope; Submitted to AAS Journals

Published
2022
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9. The JWST Early Release Science Program for the Direct Imaging & 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 D., Pueyo, Laurent, Schneider, Glenn, Stapelfeldt, Karl, Wang, Jason, Ward-Duong, Kimberly, Bowler, Brendan P., Boccaletti, Anthony, Girard, Julien H., 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, De Furio, Matthew, Factor, Samuel M., Fortney, Jonathan J., Grady, Carol, Greenbaum, Alexandra, Henning, Thomas, 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, 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

Subjects
Astrophysics - Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Solar and Stellar Astrophysics
Abstract

The direct characterization 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$\mu$m, 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 maximise 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-hour Early Release Science Program that will utilize all four JWST instruments to extend the characterisation of planetary mass companions to $\sim$15$\mu$m 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 datasets that will enable a broad user base to effectively plan for general observing programs in future cycles., Comment: 21 pages, 7 figures. Accepted for Publication in PASP

Published
2022
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10. The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems. V. Do Self-consistent Atmospheric Models Represent JWST Spectra? A Showcase with VHS 1256–1257 b

Author

Petrus, Simon, primary, Whiteford, Niall, additional, Patapis, Polychronis, additional, Biller, Beth A., additional, Skemer, Andrew, additional, Hinkley, Sasha, additional, Suárez, Genaro, additional, Palma-Bifani, Paulina, additional, Morley, Caroline V., additional, Tremblin, Pascal, additional, Charnay, Benjamin, additional, Vos, Johanna M., additional, Wang, Jason J., additional, Stone, Jordan M., additional, Bonnefoy, Mickaël, additional, Chauvin, Gaël, additional, Miles, Brittany E., additional, Carter, Aarynn L., additional, Lueber, Anna, additional, Helling, Christiane, additional, Sutlieff, Ben J., additional, Janson, Markus, additional, Gonzales, Eileen C., additional, Hoch, Kielan K. W., additional, Absil, Olivier, additional, Balmer, William O., additional, Boccaletti, Anthony, additional, Bonavita, Mariangela, additional, Booth, Mark, additional, Bowler, Brendan P., additional, Briesemeister, Zackery W., additional, Bryan, Marta L., additional, Calissendorff, Per, additional, Cantalloube, Faustine, additional, Chen, Christine H., additional, Choquet, Elodie, additional, Christiaens, Valentin, additional, Cugno, Gabriele, additional, Currie, Thayne, additional, Danielski, Camilla, additional, De Furio, Matthew, additional, Dupuy, Trent J., additional, Factor, Samuel M., additional, Faherty, Jacqueline K., additional, Fitzgerald, Michael P., additional, Fortney, Jonathan J., additional, Franson, Kyle, additional, Girard, Julien H., additional, Grady, Carol A., additional, Henning, Thomas, additional, Hines, Dean C., additional, Hood, Callie E., additional, Howe, Alex R., additional, Kalas, Paul, additional, Kammerer, Jens, additional, Kennedy, Grant M., additional, Kenworthy, Matthew A., additional, Kervella, Pierre, additional, Kim, Minjae, additional, Kitzmann, Daniel, additional, Kraus, Adam L., additional, Kuzuhara, Masayuki, additional, Lagage, Pierre-Olivier, additional, Lagrange, Anne-Marie, additional, Lawson, Kellen, additional, Lazzoni, Cecilia, additional, Leisenring, Jarron M., additional, Lew, Ben W. P., additional, Liu, Michael C., additional, Liu, Pengyu, additional, Llop-Sayson, Jorge, additional, Lloyd, James P., additional, Macintosh, Bruce, additional, Mâlin, Mathilde, additional, Manjavacas, Elena, additional, Marino, Sebastián, additional, Marley, Mark S., additional, Marois, Christian, additional, Martinez, Raquel A., additional, Matthews, Elisabeth C., additional, Matthews, Brenda C., additional, Mawet, Dimitri, additional, Mazoyer, Johan, additional, McElwain, Michael W., additional, Metchev, Stanimir, additional, Meyer, Michael R., additional, Millar-Blanchaer, Maxwell A., additional, Mollière, Paul, additional, Moran, Sarah E., additional, Mukherjee, Sagnick, additional, Pantin, Eric, additional, Perrin, Marshall D., additional, Pueyo, Laurent, additional, Quanz, Sascha P., additional, Quirrenbach, Andreas, additional, Ray, Shrishmoy, additional, Rebollido, Isabel, additional, Adams Redai, Jea, additional, Ren, Bin B., additional, Rickman, Emily, additional, Sallum, Steph, additional, Samland, Matthias, additional, Sargent, Benjamin, additional, Schlieder, Joshua E., additional, Stapelfeldt, Karl R., additional, Tamura, Motohide, additional, Tan, Xianyu, additional, Theissen, Christopher A., additional, Uyama, Taichi, additional, Vasist, Malavika, additional, Vigan, Arthur, additional, Wagner, Kevin, additional, Ward-Duong, Kimberly, additional, Wolff, Schuyler G., additional, Worthen, Kadin, additional, Wyatt, Mark C., additional, Ygouf, Marie, additional, Zurlo, Alice, additional, Zhang, Xi, additional, Zhang, Keming, additional, Zhang, Zhoujian, additional, and Zhou, Yifan, additional

Published
2024
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11. 15NH3 in the atmosphere of a cool brown dwarf

Author

Barrado, David, primary, Mollière, Paul, additional, Patapis, Polychronis, additional, Min, Michiel, additional, Tremblin, Pascal, additional, Ardevol Martinez, Francisco, additional, Whiteford, Niall, additional, Vasist, Malavika, additional, Argyriou, Ioannis, additional, Samland, Matthias, additional, Lagage, Pierre-Olivier, additional, Decin, Leen, additional, Waters, Rens, additional, Henning, Thomas, additional, Morales-Calderón, María, additional, Guedel, Manuel, additional, Vandenbussche, Bart, additional, Absil, Olivier, additional, Baudoz, Pierre, additional, Boccaletti, Anthony, additional, Bouwman, Jeroen, additional, Cossou, Christophe, additional, Coulais, Alain, additional, Crouzet, Nicolas, additional, Gastaud, René, additional, Glasse, Alistair, additional, Glauser, Adrian M., additional, Kamp, Inga, additional, Kendrew, Sarah, additional, Krause, Oliver, additional, Lahuis, Fred, additional, Mueller, Michael, additional, Olofsson, Göran, additional, Pye, John, additional, Rouan, Daniel, additional, Royer, Pierre, additional, Scheithauer, Silvia, additional, Waldmann, Ingo, additional, Colina, Luis, additional, van Dishoeck, Ewine F., additional, Ray, Tom, additional, Östlin, Göran, additional, and Wright, Gillian, additional

Published
2023
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12. Workshop Summary: Exoplanet Orbits and Dynamics

Author

Maire, Anne-Lise, primary, Delrez, Laetitia, additional, Pozuelos, Francisco J., additional, Becker, Juliette, additional, Espinoza, Nestor, additional, Lillo-Box, Jorge, additional, Revol, Alexandre, additional, Absil, Olivier, additional, Agol, Eric, additional, Almenara, José M., additional, Anglada-Escudé, Guillem, additional, Beust, Hervé, additional, Blunt, Sarah, additional, Bolmont, Emeline, additional, Bonavita, Mariangela, additional, Brandner, Wolfgang, additional, Mirek Brandt, G., additional, Brandt, Timothy D., additional, Brown, Garett, additional, Cantero Mitjans, Carles, additional, Charalambous, Carolina, additional, Chauvin, Gaël, additional, Correia, Alexandre C. M., additional, Cranmer, Miles, additional, Defrère, Denis, additional, Deleuil, Magali, additional, Demory, Brice-Olivier, additional, De Rosa, Robert J., additional, Desidera, Silvano, additional, Dévora-Pajares, Martín, additional, Díaz, Rodrigo F., additional, Do Ó, Clarissa, additional, Ducrot, Elsa, additional, Dupuy, Trent J., additional, Ferrer-Chávez, Rodrigo, additional, Fontanive, Clémence, additional, Gillon, Michaël, additional, Giuppone, Cristian, additional, Gkouvelis, Leonardos, additional, de Oliveira Gomes, Gabriel, additional, Gomes, Sérgio R. A., additional, Günther, Maximilian N., additional, Hadden, Sam, additional, Han, Yinuo, additional, Hernandez, David M., additional, Jehin, Emmanuel, additional, Kane, Stephen R., additional, Kervella, Pierre, additional, Kiefer, Flavien, additional, Konopacky, Quinn M., additional, Langlois, Maud, additional, Lanssens, Benjamin, additional, Lazzoni, Cecilia, additional, Lendl, Monika, additional, Li, Yiting, additional, Libert, Anne-Sophie, additional, Lovos, Flavia, additional, Miculán, Romina G., additional, Murray, Zachary, additional, Pallé, Enric, additional, Rein, Hanno, additional, Rodet, Laetitia, additional, Roisin, Arnaud, additional, Sahlmann, Johannes, additional, Siverd, Robert, additional, Stalport, Manu, additional, Carlos Suárez, Juan, additional, Tamayo, Daniel, additional, Teyssandier, Jean, additional, Thuillier, Antoine, additional, Timmermans, Mathilde, additional, Triaud, Amaury H. M. J., additional, Trifonov, Trifon, additional, Valente, Ema F. S., additional, Van Grootel, Valérie, additional, Vasist, Malavika, additional, Wang, Jason J., additional, Wyatt, Mark C., additional, Xuan, Jerry, additional, Young, Steven, additional, and Zimmerman, Neil T., additional

Published
2023
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13. The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems I: High-contrast Imaging of the Exoplanet HIP 65426 b from 2 to 16 μm

Author

Carter, Aarynn L., primary, Hinkley, Sasha, additional, Kammerer, Jens, additional, Skemer, Andrew, additional, Biller, Beth A., additional, Leisenring, Jarron M., additional, Millar-Blanchaer, Maxwell A., additional, Petrus, Simon, additional, Stone, Jordan M., additional, Ward-Duong, Kimberly, additional, Wang, Jason J., additional, Girard, Julien H., additional, Hines, Dean C., additional, Perrin, Marshall D., additional, Pueyo, Laurent, additional, Balmer, William O., additional, Bonavita, Mariangela, additional, Bonnefoy, Mickael, additional, Chauvin, Gael, additional, Choquet, Elodie, additional, Christiaens, Valentin, additional, Danielski, Camilla, additional, Kennedy, Grant M., additional, Matthews, Elisabeth C., additional, Miles, Brittany E., additional, Patapis, Polychronis, additional, Ray, Shrishmoy, additional, Rickman, Emily, additional, Sallum, Steph, additional, Stapelfeldt, Karl R., additional, Whiteford, Niall, additional, Zhou, Yifan, additional, Absil, Olivier, additional, Boccaletti, Anthony, additional, Booth, Mark, additional, Bowler, Brendan P., additional, Chen, Christine H., additional, Currie, Thayne, additional, Fortney, Jonathan J., additional, Grady, Carol A., additional, Greebaum, Alexandra Z., additional, Henning, Thomas, additional, Hoch, Kielan K. W., additional, Janson, Markus, additional, Kalas, Paul, additional, Kenworthy, Matthew A., additional, Kervella, Pierre, additional, Kraus, Adam L., additional, Lagage, Pierre-Olivier, additional, Liu, Michael C., additional, Macintosh, Bruce, additional, Marino, Sebastian, additional, Marley, Mark S., additional, Marois, Christian, additional, Matthews, Brenda C., additional, Mawet, Dimitri, additional, McElwain, Michael W., additional, Metchev, Stanimir, additional, Meyer, Michael R., additional, Molliere, Paul, additional, Moran, Sarah E., additional, Morley, Caroline V., additional, Mukherjee, Sagnick, additional, Pantin, Eric, additional, Quirrenbach, Andreas, additional, Rebollido, Isabel, additional, Ren, Bin B., additional, Schneider, Glenn, additional, Vasist, Malavika, additional, Worthen, Kadin, additional, Wyatt, Mark C., additional, Briesemeister, Zackery W., additional, Bryan, Marta L., additional, Calissendorff, Per, additional, Cantalloube, Faustine, additional, Cugno, Gabriele, additional, De Furio, Matthew, additional, Dupuy, Trent J., additional, Factor, Samuel M., additional, Faherty, Jacqueline K., additional, Fitzgerald, Michael P., additional, Franson, Kyle, additional, Gonzales, Eileen C., additional, Hood, Callie E., additional, Howe, Alex R., additional, Kuzuhara, Masayuki, additional, Lagrange, Anne-Marie, additional, Lawson, Kellen, additional, Lazzoni, Cecilia, additional, Lew, Ben W. P., additional, Liu, Pengyu, additional, Llop-Sayson, Jorge, additional, Lloyd, James P., additional, Martinez, Raquel A., additional, Mazoyer, Johan, additional, Palma-Bifani, Paulina, additional, Quanz, Sascha P., additional, Redai, Jea Adams, additional, Samland, Matthias, additional, Schlieder, Joshua E., additional, Tamura, Motohide, additional, Tan, Xianyu, additional, Uyama, Taichi, additional, Vigan, Arthur, additional, Vos, Johanna M., additional, Wagner, Kevin, additional, Wolff, Schuyler G., additional, Ygouf, Marie, additional, Zhang, Xi, additional, Zhang, Keming, additional, and Zhang, Zhoujian, additional

Published
2023
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15. The \textit{JWST} Early Release Science Program for Direct Observations of Exoplanetary Systems III: Aperture Masking Interferometric Observations of the star HIP\,65426 at $\boldsymbol{3.8\,\rm{\mu m}}$

Author

Ray, Shrishmoy, Sallum, Steph, Hinkley, Sasha, Sivamarakrishnan, Anand, Cooper, Rachel, Kammerer, Jens, Greebaum, Alexandra Z., Thatte, Deepashri, Lazzoni, Cecilia, Tokovinin, Andrei, de Furio, Matthew, Factor, Samuel, Meyer, Michael, Stone, Jordan M., Carter, Aarynn, Biller, Beth, Skemer, Andrew, Suarez, Genaro, Leisenring, Jarron M., Perrin, Marshall D., Kraus, Adam L., Absil, Olivier, Balmer, William O., Bonnefoy, Mickael, Bryan, Marta L., Betti, Sarah K., Boccaletti, Anthony, Bonavita, Mariangela, Booth, Mark, Bowler, Brendan P., Briesemeister, Zackery W., Cantalloube, Faustine, Chauvin, Gael, Christiaens, Valentin, Cugno, Gabriele, Currie, Thayne, Danielski, Camilla, Dupuy, Trent J., Faherty, Jacqueline K., Chen, Christine H., Calissendorff, Per, Choquet, Elodie, Fitzgerald, Michael P., Fortney, Jonathan J., Franson, Kyle, Girard, Julien H., Grady, Carol A., Gonzales, Eileen C., Henning, Thomas, Hines, Dean C., Hoch, Kielan K. W., Hood, Callie E., Howe, Alex R., Janson, Markus, Kalas, Paul, Kennedy, Grant M., Kenworthy, Matthew A., Kervella, Pierre, Kitzmann, Daniel, Kuzuhara, Masayuki, Lagrange, Anne-Marie, Lagage, Pierre-Olivier, Lawson, Kellen, Lew, Ben W. P., Liu, Michael C., Liu, Pengyu, Llop-Sayson, Jorge, Lloyd, James P., Lueber, Anna, Macintosh, Bruce, Manjavacas, Elena, Marino, Sebastian, Marley, Mark S., Marois, Christian, Martinez, Raquel A., Matthews, Brenda C., Matthews, Elisabeth C., Mawet, Dimitri, Mazoyer, Johan, McElwain, Michael W., Metchev, Stanimir, Miles, Brittany E., Millar-Blanchaer, Maxwell A., Molliere, Paul, Moran, Sarah E., Morley, Caroline V., Mukherjee, Sagnick, Palma-Bifani, Paulina, Pantin, Eric, Patapis, Polychronis, Petrus, Simon, Pueyo, Laurent, Quanz, Sascha P., Quirrenbach, Andreas, Rebollido, Isabel, Redai, Jea Adams, Ren, Bin B., Rickman, Emily, Samland, Matthias, Sargent, B. A., Schlieder, Joshua E., Schneider, Glenn, Stapelfeldt, Karl R., Sutlieff, Ben J., Tamura, Motohide, Tan, Xianyu, Theissen, Christopher A., Uyama, Taichi, Vigan, Arthur, Vasist, Malavika, Vos, Johanna M., Wagner, Kevin, Wang, Jason J., Ward-Duong, Kimberly, Whiteford, Niall, Wolff, Schuyler G., Worthen, Kadin, Wyatt, Mark C., Ygouf, Marie, Zhang, Xi, Zhang, Keming, Zhang, Zhoujian, Zhou, Yifan, Ray, Shrishmoy, Sallum, Steph, Hinkley, Sasha, Sivamarakrishnan, Anand, Cooper, Rachel, Kammerer, Jens, Greebaum, Alexandra Z., Thatte, Deepashri, Lazzoni, Cecilia, Tokovinin, Andrei, de Furio, Matthew, Factor, Samuel, Meyer, Michael, Stone, Jordan M., Carter, Aarynn, Biller, Beth, Skemer, Andrew, Suarez, Genaro, Leisenring, Jarron M., Perrin, Marshall D., Kraus, Adam L., Absil, Olivier, Balmer, William O., Bonnefoy, Mickael, Bryan, Marta L., Betti, Sarah K., Boccaletti, Anthony, Bonavita, Mariangela, Booth, Mark, Bowler, Brendan P., Briesemeister, Zackery W., Cantalloube, Faustine, Chauvin, Gael, Christiaens, Valentin, Cugno, Gabriele, Currie, Thayne, Danielski, Camilla, Dupuy, Trent J., Faherty, Jacqueline K., Chen, Christine H., Calissendorff, Per, Choquet, Elodie, Fitzgerald, Michael P., Fortney, Jonathan J., Franson, Kyle, Girard, Julien H., Grady, Carol A., Gonzales, Eileen C., Henning, Thomas, Hines, Dean C., Hoch, Kielan K. W., Hood, Callie E., Howe, Alex R., Janson, Markus, Kalas, Paul, Kennedy, Grant M., Kenworthy, Matthew A., Kervella, Pierre, Kitzmann, Daniel, Kuzuhara, Masayuki, Lagrange, Anne-Marie, Lagage, Pierre-Olivier, Lawson, Kellen, Lew, Ben W. P., Liu, Michael C., Liu, Pengyu, Llop-Sayson, Jorge, Lloyd, James P., Lueber, Anna, Macintosh, Bruce, Manjavacas, Elena, Marino, Sebastian, Marley, Mark S., Marois, Christian, Martinez, Raquel A., Matthews, Brenda C., Matthews, Elisabeth C., Mawet, Dimitri, Mazoyer, Johan, McElwain, Michael W., Metchev, Stanimir, Miles, Brittany E., Millar-Blanchaer, Maxwell A., Molliere, Paul, Moran, Sarah E., Morley, Caroline V., Mukherjee, Sagnick, Palma-Bifani, Paulina, Pantin, Eric, Patapis, Polychronis, Petrus, Simon, Pueyo, Laurent, Quanz, Sascha P., Quirrenbach, Andreas, Rebollido, Isabel, Redai, Jea Adams, Ren, Bin B., Rickman, Emily, Samland, Matthias, Sargent, B. A., Schlieder, Joshua E., Schneider, Glenn, Stapelfeldt, Karl R., Sutlieff, Ben J., Tamura, Motohide, Tan, Xianyu, Theissen, Christopher A., Uyama, Taichi, Vigan, Arthur, Vasist, Malavika, Vos, Johanna M., Wagner, Kevin, Wang, Jason J., Ward-Duong, Kimberly, Whiteford, Niall, Wolff, Schuyler G., Worthen, Kadin, Wyatt, Mark C., Ygouf, Marie, Zhang, Xi, Zhang, Keming, Zhang, Zhoujian, and Zhou, Yifan

Abstract

We present aperture masking interferometry (AMI) observations of the star HIP 65426 at $3.8\,\rm{\mu m}$ as a part of the \textit{JWST} Direct Imaging Early Release Science (ERS) program obtained using the Near Infrared Imager and Slitless Spectrograph (NIRISS) instrument. This mode provides access to very small inner working angles (even separations slightly below the Michelson limit of ${}0.5\lambda/D$ for an interferometer), which are inaccessible with the classical inner working angles of the \textit{JWST} coronagraphs. When combined with \textit{JWST}'s unprecedented infrared sensitivity, this mode has the potential to probe a new portion of parameter space across a wide array of astronomical observations. Using this mode, we are able to achieve a contrast of $\Delta m_{F380M}{\sim }7.8$\,mag relative to the host star at a separation of ${\sim}0.07\arcsec$ but detect no additional companions interior to the known companion HIP\,65426\,b. Our observations thus rule out companions more massive than $10{-}12\,\rm{M\textsubscript{Jup}}$ at separations ${\sim}10{-}20\,\rm{au}$ from HIP\,65426, a region out of reach of ground or space-based coronagraphic imaging. These observations confirm that the AMI mode on \textit{JWST} is sensitive to planetary mass companions orbiting at the water frost line, even for more distant stars at $\sim$100\,pc. This result will allow the planning and successful execution of future observations to probe the inner regions of nearby stellar systems, opening essentially unexplored parameter space., Comment: 15 pages, 9 figures, submitted to ApJ Letters

Published
2023

16. 15NH3 in the atmosphere of a cool brown dwarf.

Author

Barrado, David, Mollière, Paul, Patapis, Polychronis, Min, Michiel, Tremblin, Pascal, Ardevol Martinez, Francisco, Whiteford, Niall, Vasist, Malavika, Argyriou, Ioannis, Samland, Matthias, Lagage, Pierre-Olivier, Decin, Leen, Waters, Rens, Henning, Thomas, Morales-Calderón, María, Guedel, Manuel, Vandenbussche, Bart, Absil, Olivier, Baudoz, Pierre, and Boccaletti, Anthony

Abstract

Brown dwarfs serve as ideal laboratories for studying the atmospheres of giant exoplanets on wide orbits, as the governing physical and chemical processes within them are nearly identical1,2. Understanding the formation of gas-giant planets is challenging, often involving the endeavour to link atmospheric abundance ratios, such as the carbon-to-oxygen (C/O) ratio, to formation scenarios3. However, the complexity of planet formation requires further tracers, as the unambiguous interpretation of the measured C/O ratio is fraught with complexity4. Isotope ratios, such as deuterium to hydrogen and 14N/15N, offer a promising avenue to gain further insight into this formation process, mirroring their use within the Solar System5–7. For exoplanets, only a handful of constraints on 12C/13C exist, pointing to the accretion of 13C-rich ice from beyond the CO iceline of the disks8,9. Here we report on the mid-infrared detection of the 14NH3 and 15NH3 isotopologues in the atmosphere of a cool brown dwarf with an effective temperature of 380 K in a spectrum taken with the Mid-Infrared Instrument (MIRI) of JWST. As expected, our results reveal a 14N/15N value consistent with star-like formation by gravitational collapse, demonstrating that this ratio can be accurately constrained. Because young stars and their planets should be more strongly enriched in the 15N isotope10, we expect that 15NH3 will be detectable in several cold, wide-separation exoplanets.Observations from the JWST MIRI showed the detection of 14NH3 and 15NH3 isotopologues in the atmosphere of a cool brown dwarf, along with a 14N/15N value consistent with star-like formation by gravitational collapse. [ABSTRACT FROM AUTHOR]

Published
2023
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17. The JWST Early-release Science Program for Direct Observations of Exoplanetary Systems II: A 1 to 20 μm Spectrum of the Planetary-mass Companion VHS 1256–1257 b

Author

Miles, Brittany E., primary, Biller, Beth A., additional, Patapis, Polychronis, additional, Worthen, Kadin, additional, Rickman, Emily, additional, Hoch, Kielan K. W., additional, Skemer, Andrew, additional, Perrin, Marshall D., additional, Whiteford, Niall, additional, Chen, Christine H., additional, Sargent, B., additional, Mukherjee, Sagnick, additional, Morley, Caroline V., additional, Moran, Sarah E., additional, Bonnefoy, Mickael, additional, Petrus, Simon, additional, Carter, Aarynn L., additional, Choquet, Elodie, additional, Hinkley, Sasha, additional, Ward-Duong, Kimberly, additional, Leisenring, Jarron M., additional, Millar-Blanchaer, Maxwell A., additional, Pueyo, Laurent, additional, Ray, Shrishmoy, additional, Sallum, Steph, additional, Stapelfeldt, Karl R., additional, Stone, Jordan M., additional, Wang, Jason J., additional, Absil, Olivier, additional, Balmer, William O., additional, Boccaletti, Anthony, additional, Bonavita, Mariangela, additional, Booth, Mark, additional, Bowler, Brendan P., additional, Chauvin, Gael, additional, Christiaens, Valentin, additional, Currie, Thayne, additional, Danielski, Camilla, additional, Fortney, Jonathan J., additional, Girard, Julien H., additional, Grady, Carol A., additional, Greenbaum, Alexandra Z., additional, Henning, Thomas, additional, Hines, Dean C., additional, Janson, Markus, additional, Kalas, Paul, additional, Kammerer, Jens, additional, Kennedy, Grant M., additional, Kenworthy, Matthew A., additional, Kervella, Pierre, additional, Lagage, Pierre-Olivier, additional, Lew, Ben W. P., additional, Liu, Michael C., additional, Macintosh, Bruce, additional, Marino, Sebastian, additional, Marley, Mark S., additional, Marois, Christian, additional, Matthews, Elisabeth C., additional, Matthews, Brenda C., additional, Mawet, Dimitri, additional, McElwain, Michael W., additional, Metchev, Stanimir, additional, Meyer, Michael R., additional, Molliere, Paul, additional, Pantin, Eric, additional, Quirrenbach, Andreas, additional, Rebollido, Isabel, additional, Ren, Bin B., additional, Schneider, Glenn, additional, Vasist, Malavika, additional, Wyatt, Mark C., additional, Zhou, Yifan, additional, Briesemeister, Zackery W., additional, Bryan, Marta L, additional, Calissendorff, Per, additional, Cantalloube, Faustine, additional, Cugno, Gabriele, additional, De Furio, Matthew, additional, Dupuy, Trent J., additional, Factor, Samuel M., additional, Faherty, Jacqueline K., additional, Fitzgerald, Michael P., additional, Franson, Kyle, additional, Gonzales, Eileen C., additional, Hood, Callie E., additional, Howe, Alex R., additional, Kraus, Adam L., additional, Kuzuhara, Masayuki, additional, Lagrange, Anne-Marie, additional, Lawson, Kellen, additional, Lazzoni, Cecilia, additional, Liu, Pengyu, additional, Llop-Sayson, Jorge, additional, Lloyd, James P., additional, Martinez, Raquel A., additional, Mazoyer, Johan, additional, Quanz, Sascha P., additional, Redai, Jea Adams, additional, Samland, Matthias, additional, Schlieder, Joshua E., additional, Tamura, Motohide, additional, Tan, Xianyu, additional, Uyama, Taichi, additional, Vigan, Arthur, additional, Vos, Johanna M., additional, Wagner, Kevin, additional, Wolff, Schuyler G., additional, Ygouf, Marie, additional, Zhang, Xi, additional, Zhang, Keming, additional, and Zhang, Zhoujian, additional

Published
2023
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18. The JWST Early Release Science Program for Direct Observations of Exoplanetary Systems I: High Contrast Imaging of the Exoplanet HIP 65426 b from 2−16 µm

Author

Carter, Aarynn L., Hinkley, Sasha, Kammerer, Jens, Skemer, Andrew, Biller, Beth A., Leisenring, Jarron M., Millar-Blanchaer, Maxwell A., Petrus, Simon, Stone, Jordan M., Ward-Duong, Kimberly, Wang, Jason J., Girard, Julien H., Hines, Dean C., Perrin, Marshall D., Pueyo, Laurent, Balmer, William O., Bonavita, Mariangela, Bonnefoy, Mickael, Chauvin, Gael, Choquet, Elodie, Christiaens, Valentin, Danielski, Camilla, Kennedy, Grant M., Matthews, Elisabeth C., Miles, Brittany E., Patapis, Polychronis, Ray, Shrishmoy, Rickman, Emily, Sallum, Steph, Stapelfeldt, Karl R., Whiteford, Niall, Zhou, Yifan, Absil, Olivier, Boccaletti, Anthony, Booth, Mark, Bowler, Brendan P., Chen, Christine H., Currie, Thayne, Fortney, Jonathan J., Grady, Carol A., Greenbaum, Alexandra Z., Henning, Thomas, Hoch, Kielan K. W., Janson, Markus, Kalas, Paul, Kenworthy, Matthew A., Kervella, Pierre, Kraus, Adam L., Lagage, Pierre-Olivier, Liu, Michael C., Macintosh, Bruce, Marino, Sebastian, Marley, Mark S., Marois, Christian, Matthews, Brenda C., Mawet, Dimitri, Mcelwain, Michael W., Metchev, Stanimir, Meyer, Michael R., Molliere, Paul, Moran, Sarah E., Morley, Caroline V., Mukherjee, Sagnick, Pantin, Eric, Quirrenbach, Andreas, Rebollido, Isabel, Ren, Bin B., Schneider, Glenn, Vasist, Malavika, Worthen, Kadin, Wyatt, Mark C., Briesemeister, Zackery W., Bryan, Marta L., Calissendorff, Per, Cantalloube, Faustine, Cugno, Gabriele, Furio, Matthew De, Dupuy, Trent J., Factor, Samuel M., Faherty, Jacqueline K., Fitzgerald, Michael P., Franson, Kyle, Gonzales, Eileen C., Hood, Callie E., Howe, Alex R., Kuzuhara, Masayuki, Lagrange, Anne-Marie, Lawson, Kellen, Lazzoni, Cecilia, Lew, Ben W. P., Liu, Pengyu, Llop-Sayson, Jorge, Lloyd, James P., Martinez, Raquel A., Mazoyer, Johan, Quanz, Sascha P., Redai, Jea Adams, Samland, Matthias, Schlieder, Joshua E., Tamura, Motohide, Tan, Xianyu, Uyama, Taichi, Vigan, Arthur, Vos, Johanna M., Wagner, Kevin, Wolff, Schuyler G., Ygouf, Marie, Zhang, Xi, Zhang, Keming, Zhang, Zhoujian, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'études spatiales et d'instrumentation en astrophysique = Laboratory of Space Studies and Instrumentation in Astrophysics (LESIA), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph]
Published
2022

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

Author

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

Published
2022
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20. 15NH3in the atmosphere of a cool brown dwarf

Author

Barrado, David, Mollière, Paul, Patapis, Polychronis, Min, Michiel, Tremblin, Pascal, Ardevol Martinez, Francisco, Whiteford, Niall, Vasist, Malavika, Argyriou, Ioannis, Samland, Matthias, Lagage, Pierre-Olivier, Decin, Leen, Waters, Rens, Henning, Thomas, Morales-Calderón, María, Guedel, Manuel, Vandenbussche, Bart, Absil, Olivier, Baudoz, Pierre, Boccaletti, Anthony, Bouwman, Jeroen, Cossou, Christophe, Coulais, Alain, Crouzet, Nicolas, Gastaud, René, Glasse, Alistair, Glauser, Adrian M., Kamp, Inga, Kendrew, Sarah, Krause, Oliver, Lahuis, Fred, Mueller, Michael, Olofsson, Göran, Pye, John, Rouan, Daniel, Royer, Pierre, Scheithauer, Silvia, Waldmann, Ingo, Colina, Luis, van Dishoeck, Ewine F., Ray, Tom, Östlin, Göran, and Wright, Gillian

Abstract

Brown dwarfs serve as ideal laboratories for studying the atmospheres of giant exoplanets on wide orbits, as the governing physical and chemical processes within them are nearly identical1,2. Understanding the formation of gas-giant planets is challenging, often involving the endeavour to link atmospheric abundance ratios, such as the carbon-to-oxygen (C/O) ratio, to formation scenarios3. However, the complexity of planet formation requires further tracers, as the unambiguous interpretation of the measured C/O ratio is fraught with complexity4. Isotope ratios, such as deuterium to hydrogen and 14N/15N, offer a promising avenue to gain further insight into this formation process, mirroring their use within the Solar System5–7. For exoplanets, only a handful of constraints on 12C/13C exist, pointing to the accretion of 13C-rich ice from beyond the CO iceline of the disks8,9. Here we report on the mid-infrared detection of the 14NH3and 15NH3isotopologues in the atmosphere of a cool brown dwarf with an effective temperature of 380 K in a spectrum taken with the Mid-Infrared Instrument (MIRI) of JWST. As expected, our results reveal a 14N/15N value consistent with star-like formation by gravitational collapse, demonstrating that this ratio can be accurately constrained. Because young stars and their planets should be more strongly enriched in the 15N isotope10, we expect that 15NH3will be detectable in several cold, wide-separation exoplanets.

Published
2023
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