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Author (up) McGruder, C.D.; Lopez-Morales, M.; Kirk, J.; Rackham, B.V.; May, E.; Ahrer, E.M.; King, G.W.; Alam, M.K.; Allen, N.H.; Ceballos, K.O.; Espinoza, N.; Gardner, T.; Jordan, A.; Meyer, K.; Monnier, J.D.; Osip, D.J.; Wheatley, P.J. doi  openurl
  Title ACCESS, LRG-BEASTS, and MOPSS: Featureless Optical Transmission Spectra of WASP-25b and WASP-124b Type
  Year 2023 Publication Astronomical Journal Abbreviated Journal Astron. J.  
  Volume 166 Issue 3 Pages 120  
  Keywords ACTIVITY-ROTATION RELATIONSHIP; HST PANCET PROGRAM; VLT FORS2; TRANSIT SPECTROSCOPY; RAYLEIGH-SCATTERING; BAYESIAN-INFERENCE; RETRIEVAL ANALYSIS; CLEAR ATMOSPHERE; MODEL SELECTION; HD 189733B  
  Abstract We present new optical transmission spectra for two hot Jupiters: WASP-25b (M = 0.56 M ( J ); R = 1.23 R ( J ); P = 3.76 days) and WASP-124b (M = 0.58 M ( J ); R = 1.34 R ( J ); P = 3.37 days), with wavelength coverages of 4200-9100 & ANGS; and 4570-9940 & ANGS;, respectively. These spectra are from the ESO Faint Object Spectrograph and Camera (v.2) mounted on the New Technology Telescope and Inamori-Magellan Areal Camera & Spectrograph on Magellan Baade. No strong spectral features were found in either spectra, with the data probing 4 and 6 scale heights, respectively. Exoretrievals and PLATON retrievals favor stellar activity for WASP-25b, while the data for WASP-124b did not favor one model over another. For both planets the retrievals found a wide range in the depths where the atmosphere could be optically thick (& SIM;0.4 & mu;-0.2 bars for WASP-25b and 1.6 & mu;-32 bars for WASP-124b) and recovered a temperature that is consistent with the planets' equilibrium temperatures, but with wide uncertainties (up to & PLUSMN;430 K). For WASP-25b, the models also favor stellar spots that are & SIM;500-3000 K cooler than the surrounding photosphere. The fairly weak constraints on parameters are owing to the relatively low precision of the data, with an average precision of 840 and 1240 ppm per bin for WASP-25b and WASP-124b, respectively. However, some contribution might still be due to an inherent absence of absorption or scattering in the planets' upper atmospheres, possibly because of aerosols. We attempt to fit the strength of the sodium signals to the aerosol-metallicity trend proposed by McGruder et al., and find WASP-25b and WASP-124b are consistent with the prediction, though their uncertainties are too large to confidently confirm the trend.  
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  ISSN 0004-6256 ISBN Medium  
  Area Expedition Conference  
  Notes WOS:001051670600001 Approved  
  Call Number UAI @ alexi.delcanto @ Serial 1871  
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