WASP-127 Archives

The detections of H2O, CO, and total atmospheric signal in the atmosphere of WASP-127 b. The CC maps shown here are generated by cross-correlating the residual data with solar composition RCTE models with opacity from H2O alone, CO alone, and all absorbers respectively. The tellurics have been masked and the out-of-transit frames have been cropped in the residual data. The white dashed lines in these maps denote the literature reported values of Vsys0 and Kp0 for the WASP-127 b system. The red cross indicates the peak value of the SNR within each map. Similar to the trail, the peak signal in these maps can be seen blue shifted. The bottom red curves under each panel shows the row/cross-section of the CC SNRs at the peak Kp. -- astro-ph.EP

Astronomy & Telescopes, Atmospheres, Climate, Weather, Exoplanets, -moons, -comets, Imaging & Spectroscopy, Status Report

IGRINS Observations of WASP-127 b: H2O, CO, and Super-Solar Atmospheric Metallicity in the Inflated sub-Saturn

by Keith CowingJune 21, 2024June 21, 2024

High resolution spectroscopy of exoplanet atmospheres provides insights into their composition and dynamics from the resolved line shape and depth of thousands of spectral lines. WASP-127 b is an extremely […]

Different scenarios of super-rotating atmospheric material. Panels a, b and c show the scenario of a homogeneously rotating planet. The purple solid line shows the velocity kernel of the material at rotation consistent with tidally locked rotation (panel b) and the resulting shape of the cross-correlation function (panel c). The turquoise dashed line shows the effect of the planet rotating approximately six times faster. Panels d, e and f show two cases of a super-rotating equatorial jet, with the poles rotating at tidally locked velocities. The difference between the two cases is the opening angle of the equatorial region (35◦ orange dashed, and 65◦ solid green). Panels g, h and i explore the case of the velocity kernel of a super-rotating equatorial jet (blue and red solid lines in panel h) with the polar region represented by the velocity kernel of super-rotating velocity (grey dash-dotted line) or tidally locked velocity (grey dotted line) but not contributing to the transmission spectrum due to muted atmospheric features, leading in both cases to only two peaks in the CCF (panel i). -- astro-ph.EP

Astronomy & Telescopes, Atmospheres, Climate, Weather, Biogeochemical Cycles & Geobiology, Exoplanets, -moons, -comets, Gas Giants, Imaging & Spectroscopy, Press Release

CRIRES+ Transmission Spectroscopy of WASP-127b. Detection Of The Resolved Signatures Of A Supersonic Equatorial Jet And Cool Poles In A Hot Planet

by Keith CowingApril 20, 2024April 20, 2024

General circulation models of gas giant exoplanets predict equatorial jets that drive inhomogeneities across the planetary atmosphere. We studied the transmission spectrum of the hot Jupiter WASP-127b during one transit […]

WASP-127

IGRINS Observations of WASP-127 b: H2O, CO, and Super-Solar Atmospheric Metallicity in the Inflated sub-Saturn

CRIRES+ Transmission Spectroscopy of WASP-127b. Detection Of The Resolved Signatures Of A Supersonic Equatorial Jet And Cool Poles In A Hot Planet

Tricorder Tech: New Handheld Device Maps Chemical Composition Using Infrared Light

No Statistically Significant Evidence For A Correlation Between Stellar And planetary Composition

Water Planet Recon: How Accurately Can We Measure Earth Ocean’s Deepest Point?

Webb Reveals A Stunning Panorama Of Star Formation

Deep Learning of SHERLOC Raman Spectra For Facilitating Mars Astromaterial Identification