J/A+A/632/A69 CaII transmission spectrum of WASP-33b and KELT-9b (Yan+, 2019)
Ionized calcium in the atmospheres of two ultra-hot exoplanets
WASP-33b and KELT-9b.
Yan F., Casasayas-Barris N., Molaverdikhani K., Alonso-Floriano F.J.,
Reiners A., Palle E., Henning T., Molliere P., Chen G., Nortmann L.,
Snellen I.A.G., Ribas I., Quirrenbach A., Caballero J.A., Amado P.J.,
Azzaro M., Bauer F.F., Cortes Contreras M., Czesla S., Khalafinejad S.,
Lara L.M., Lopez-Puertas M., Montes D., Nagel E., Oshagh M.,
Sanchez-Lopez A., Stangret M., Zechmeister M.
<Astron. Astrophys. 632, A69 (2019)>
=2019A&A...632A..69Y 2019A&A...632A..69Y
ADC_Keywords: Stars, double and multiple ; Exoplanets ; Spectroscopy
Keywords: planets and satellites: atmospheres - techniques: spectroscopic -
planets and satellites: individual: WASP-33b -
planets and satellites: individual: KELT-9b
Abstract:
Ultra-hot Jupiters are emerging as a new class of exoplanets. Studying
their chemical compositions and temperature structures will improve
the understanding of their mass loss rate as well as their formation
and evolution. We present the detection of ionized calcium in the two
hottest giant exoplanets - KELT-9b and WASP-33b. By utilizing
transit datasets from CARMENES and HARPS-N observations, we achieved
high confidence level detections of CaII using the cross-correlation
method. We further obtain the transmission spectra around the
individual lines of the CaII H&K doublet and the near-infrared
triplet, and measure their line profiles. The CaII H&K lines have an
average line depth of 2.02±0.17% (effective radius of 1.56Rp) for
WASP-33b and an average line depth of 0.78±0.04% (effective radius
of 1.47Rp) for KELT-9b, which indicates that the absorptions are from
very high upper atmosphere layers close to the planetary Roche lobes.
The observed CaII lines are significantly deeper than the predicted
values from the hydrostatic models. Such a discrepancy is probably a
result of hydrodynamic outflow that transports a significant amount of
CaII into the upper atmosphere. The prominent CaII detection with the
lack of significant CaI detection implies that calcium is mostly
ionized in the upper atmospheres of the two planets.
Description:
These are transmission spectra of Ca II H&K lines from HARPS-N
observation and CaII infra-red triplet lines from CARMENES
observation of WASP-33b and KLET-9b. These are all un-binned spectra.
Objects:
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RA (2000) DE Designation(s)
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02 26 51.06 +37 33 01.7 WASP-33b = HD 15082b
20 31 26.35 +39 56 19.8 KELT-9b = HD 195689b
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
f6w33hk.dat 32 6999 WASP-33b CaII H&K lines transmission spectrum
from HARPS-N observation
f6w33irt.dat 32 5868 WASP-33b CaII infra-red triplet lines
transmission spectrum from CARMENES observation
f7k9hk.dat 32 6998 KELT-9b CaII H&K lines transmission spectrum
from HARPS-N observation
f7k9irt.dat 32 5868 KELT-9b CaII infra-red triplet lines
transmission spectrum from CARMENES observation
f8w33hk.dat 32 600 WASP-33b CaII H&K lines transmission spectrum
from HARPS-N observation
f8w33irt.dat 32 560 WASP-33b CaII infra-red triplet lines
transmission spectrum from CARMENES observation
f8k9hk.dat 32 599 KELT-9b CaII H&K lines transmission spectrum
from HARPS-N observation
f8k9irt.dat 32 559 KELT-9b CaII infra-red triplet lines
transmission spectrum from CARMENES observation
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See also:
J/A+A/526/L10 : Transits of WASP-33 (Herrero+, 2011)
J/AcA/68/371 : WASP and KELT planet transits (Maciejewski+, 2018)
J/A+A/627/A165 : KELT-9b atmos. model transmission spectra (Hoeijmakers+, 2019)
Byte-by-byte Description of file: f6w33*.dat f7k9*.dat
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Bytes Format Units Label Explanations
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8- 16 F9.4 0.1nm lambda Wavelength
23- 32 F10.8 --- Flux Relative flux
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Byte-by-byte Description of file: f8w33*.dat f8k9*.dat
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Bytes Format Units Label Explanations
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7- 20 F14.9 km/s Vel Velocity
23- 32 F10.8 --- Flux Relative flux
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Acknowledgements:
Fei Yan, fei.yan(at)uni-goettingen.de
(End) Fei Yan [IAG, Germany], Patricia Vannier [CDS] 31-Oct-2019