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

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

doi:10.1088/1538-3873/ac77bd

Cited by 35 publications

(28 citation statements)

References 230 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Future missions such as the JWST and Ariel (Tinetti et al 2018) will provide higher sensitivity and/or wider spectral coverage than HST/WFC3. This will have a huge impact on the detection of atmospheric features on small exoplanets, even with the presence of clouds at high altitudes (Constantinou & Madhusudhan 2022;Hinkley et al 2022;Whittaker et al 2022). If there is a significant amount of HCN in the atmosphere of L 98-59 b, we should be able to detect a very strong absorption feature near 2.5 μm, which is covered by the wavelength ranges of instruments from both of JWST and Ariel.…”

Section: Future Missionsmentioning

confidence: 99%

Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere

Zhou

Wang

et al. 2022

View full text Add to dashboard Cite

We are using archived data from HST of transiting exoplanet L 98-59 b to place constraints on its potentially hot atmosphere. We analyze the data from five transit visits and extract the final combined transmission spectrum using Iraclis. Then we use the inverse atmospheric retrieval code TauREx to analyze the combined transmission spectrum. There is a weak absorption feature near 1.40 μm and 1.55 μm in the transmission spectrum, which can be modeled by a cloudy atmosphere with abundant hydrogen cyanide (HCN). However, the unrealistically high abundance of HCN derived cannot be explained by any equilibrium chemical model with reasonable assumptions. Thus, the likeliest scenario is that L 98-59 b has a flat, featureless transmission spectrum in the WFC3/G141 bandpass due to a thin atmosphere with high mean molecular weight, an atmosphere with an opaque aerosol layer, or no atmosphere, and it is very unlikely for L 98-59 b to have a clear hydrogen-dominated primary atmosphere. Due to the narrow wavelength coverage and low spectral resolution of HST/WFC3 G141 grism observation, we cannot tell these different scenarios apart. Our simulation shows future higher precision measurements over wider wavelengths from the James Webb Space Telescope can be used to better characterize the planetary atmosphere of L 98-59 b.

show abstract

Section: Future Missionsmentioning

confidence: 99%

Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere

Zhou

Wang

et al. 2022

View full text Add to dashboard Cite

show abstract

“…By comparing the luminosity of VHS 1256 b with evolutionary tracks, Dupuy et al (2022) found the companion's mass to be 11.8 ± 0.2M Jup or 16 ± 1M Jup , depending on the model choices. It is also among the first targets to be observed by JWST as part of an Early Release Science program (Hinkley et al 2022). In time-resolved observations, VHS 1256 b has exhibited high amplitude brightness and spectral variability (e.g., Bowler et al 2020;Zhou et al 2020).…”

Section: Introductionmentioning

confidence: 99%

Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere

Zhou

Bowler

Apai

et al. 2022

Self Cite

View full text Add to dashboard Cite

The photometric and spectral variability of brown dwarfs probes heterogeneous temperature and cloud distributions and traces the atmospheric circulation patterns. We present a new 42 hr Hubble Space Telescope (HST) Wide Field Camera 3 G141 spectral time series of VHS 1256-1257 b, a late L-type planetary-mass companion that has been shown to have one of the highest variability amplitudes among substellar objects. The light curve is rapidly evolving and best fit by a combination of three sine waves with different periods and a linear trend. The amplitudes of the sine waves and the linear slope vary with the wavelength, and the corresponding spectral variability patterns match the predictions by models invoking either heterogeneous clouds or thermal profile anomalies. Combining these observations with previous HST monitoring data, we find that the peak-to-valley flux difference is 33% ± 2% with an even higher amplitude reaching 38% in the J band, the highest amplitude ever observed in a substellar object. The observed light curve can be explained by maps that are composed of zonal waves, spots, or a mixture of the two. Distinguishing the origin of rapid light curve evolution requires additional long-term monitoring. Our findings underscore the essential role of atmospheric dynamics in shaping brown-dwarf atmospheres and highlight VHS 1256-1257 b as one of the most favorable targets for studying the atmospheres, clouds, and atmospheric circulation of planets and brown dwarfs.

show abstract

“…Using the on-sky JWST/NIRCam F444W contrast curve from Carter et al (2022) in the JWST ERS-1386 program (Hinkley et al 2022), we calculate the expected on-sky contrast for Vega with NIRCam F440W in Fig. 2 for JWST GTO-1193 observations as follows.…”

Section: Implications For Jwst Observationsmentioning

confidence: 99%

Planet Search with the Keck/NIRC2 Vortex Coronagraph in Ms-band for Vega

Ren¹,

Wallack²,

Hurt³

et al. 2023

Preprint

View full text Add to dashboard Cite

Context. Gaps in circumstellar disks can signal the existence of planetary perturbers, making such systems preferred targets for direct imaging observations of exoplanets. Aims. Being one of the brightest and closest stars to the Sun, the photometric standard star Vega hosts a two-belt debris disk structure. Together with the fact that its planetary system is being viewed nearly face-on, Vega has been one of the prime targets for planet imaging efforts. Methods. Using the vector vortex coronagraph on Keck/NIRC2 in M s -band at 4.67 µm, we report the planet detection limits from 1 au to 22 au for Vega with an on-target time of 1.8 h. Results. We reach a 3 M Jupiter limit exterior to 12 au, which is nearly an order of magnitude deeper than existing studies. Combining with existing radial velocity studies, we can confidently rule out the existence of companions more than ∼8 M Jupiter from 22 au down to 0.1 au for Vega. Interior and exterior to ∼4 au, this combined approach reaches planet detection limits down to ∼2-3 M Jupiter using radial velocity and direct imaging, respectively. Conclusions. By reaching multi-Jupiter mass detection limits, our results are expected to be complemented by the planet imaging of Vega in the upcoming observations using the James Webb Space Telescope to obtain a more holistic understanding of the planetary system configuration around Vega.

show abstract

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

Cited by 35 publications

References 230 publications

Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere

Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere

Roaring Storms in the Planetary-mass Companion VHS 1256-1257 b: Hubble Space Telescope Multiepoch Monitoring Reveals Vigorous Evolution in an Ultracool Atmosphere

Planet Search with the Keck/NIRC2 Vortex Coronagraph in Ms-band for Vega

Contact Info

Product

Resources

About