Characterizing the atmospheres of hot Jupiters is important in understanding the formation and migration of these exotic planets. Ho we ver, there are still many open questions about the chemical and physical properties of these atmospheres. Here, we confirm the detection of water vapour in thermal emission from the non-Transiting hot Jupiter Bo ötis Ab with the high-resolution NIR CARMENES spectrograph. Combining o v er 17 h of observations (560 spectra) and using a Bayesian cross-correlation to log-likelihood approach, we measure a systemic velocity of V sys =-11 . 51 + 0 . 59-0 . 60 km s-1 and a radial velocity semi-Amplitude of K P = 106 . 21 + 1 . 76-1 . 71 km s-1 for the planet, which results in an absolute mass of M P = 6 . 24 + 0 . 17-0 . 18 M J and an orbital inclination of 41 . 6 + 1 . 0-0 . 9 de grees. Our retriev ed V sys shows a significant shift ( + 5 km s-1 ) from the literature value, which could be caused by an inaccurate time of periastron. Within the explored model grid, we measure a preference for solar water abundance (VMR = 10-3 ) and find no evidence for additional minor species in the atmosphere. Given the e xtensiv e orbital co v erage of the data, we searched for a phase dependency in the water signal but found no strong evidence of variation with orbital phase. This detection is at odds with recent observations from SPIRou/CFHT and their tight upper limit on water abundance. We recommend further observations of the atmosphere Bo ötis Ab to try and resolve these discrepancies.
Water observed in the atmosphere of tau Bootis Ab with CARMENES/CAHA
Matteo Brogi;
2022-01-01
Abstract
Characterizing the atmospheres of hot Jupiters is important in understanding the formation and migration of these exotic planets. Ho we ver, there are still many open questions about the chemical and physical properties of these atmospheres. Here, we confirm the detection of water vapour in thermal emission from the non-Transiting hot Jupiter Bo ötis Ab with the high-resolution NIR CARMENES spectrograph. Combining o v er 17 h of observations (560 spectra) and using a Bayesian cross-correlation to log-likelihood approach, we measure a systemic velocity of V sys =-11 . 51 + 0 . 59-0 . 60 km s-1 and a radial velocity semi-Amplitude of K P = 106 . 21 + 1 . 76-1 . 71 km s-1 for the planet, which results in an absolute mass of M P = 6 . 24 + 0 . 17-0 . 18 M J and an orbital inclination of 41 . 6 + 1 . 0-0 . 9 de grees. Our retriev ed V sys shows a significant shift ( + 5 km s-1 ) from the literature value, which could be caused by an inaccurate time of periastron. Within the explored model grid, we measure a preference for solar water abundance (VMR = 10-3 ) and find no evidence for additional minor species in the atmosphere. Given the e xtensiv e orbital co v erage of the data, we searched for a phase dependency in the water signal but found no strong evidence of variation with orbital phase. This detection is at odds with recent observations from SPIRou/CFHT and their tight upper limit on water abundance. We recommend further observations of the atmosphere Bo ötis Ab to try and resolve these discrepancies.
I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
