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The correction for telluric sodium emission as applied to one HAT-P-12b observation. The top panel shows the data before the correction, with emission features present in both lines of the sodium doublet, while the bottom panel shows the same observation after the features have been removed.
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We present high-resolution optical transmission spectroscopy of two sub-Saturn mass transiting exoplanets, HAT-P-12b and WASP-69b. With relatively low densities and high atmospheric scale heights, these planets are particularly well-suited to characterization through transit spectroscopy, and serve as ideal candidates for extending previously-teste...
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... with the sum of a Gaussian and polynomial function, and subtract off the Gaussian in order to preserve the noise in the data. We found that a first-order polynomial was sufficient in characterizing the shape of the emission features, as they were present only in a very small region of the sodium doublet that could be approximated as linear (see Fig. 1). The emission features are removed in this way from both lines of the sodium doublet for every spectrum of both the HAT-P-12b and WASP-69b observations. Fig. 1 shows a comparison of one frame of our HAT-P-12b observations before and after the telluric sodium emission has been corrected for. Similar features, though with varying ...
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... was sufficient in characterizing the shape of the emission features, as they were present only in a very small region of the sodium doublet that could be approximated as linear (see Fig. 1). The emission features are removed in this way from both lines of the sodium doublet for every spectrum of both the HAT-P-12b and WASP-69b observations. Fig. 1 shows a comparison of one frame of our HAT-P-12b observations before and after the telluric sodium emission has been corrected for. Similar features, though with varying strengths, were observed throughout both sets of ...
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... the thousands of water lines across each spectrum of our WASP-69b observations with models at Doppler shifts of -100 km/s to +100 km/s. The colour represents the correlation strength. The top panels show the analysis process for our data, and the bottom panels show the same process repeated on the data with a water model injected (see Fig. 11). The signal from water is visible in the bottom-left panel as a diagonal line across the in-transit portion of the map, corresponding to roughly -0.01 to + 0.01 orbital phase. Likewise, the signal is visible at the Keplerian velocity of the exoplanet in the bottom-right panel, at the expected Vsys and Kp of the planet: 0 km/s and ∼ ...
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... full data reduction process as applied to the WASP-69b observations. Explanations for each panel of the figure are provided in the caption of Fig. 8 Na absorption absorption K Figure 10. The model spectra used in our analysis. ...
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... to the WASP-69b observations. Explanations for each panel of the figure are provided in the caption of Fig. 8 Na absorption absorption K Figure 10. The model spectra used in our analysis. The top panel shows the spectrum calculated for HAT-P-12b, and the bottom panel shows the spectrum calculated for WASP-69b. Water bands can be identified from Fig. 11, but the locations of other important species are marked. Figure 11. The model spectra used in our analysis. The top panel shows the spectrum calculated for HAT-P-12b, and the bottom panel shows the spectrum calculated for WASP-69b. These models only include lines from ...
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... with the sum of a Gaussian and polynomial function, and subtract off the Gaussian in order to preserve the noise in the data. We found that a first-order polynomial was sufficient in characterizing the shape of the emission features, as they were present only in a very small region of the sodium doublet that could be approximated as linear (see Fig. 1). The emission features are removed in this way from both lines of the sodium doublet for every spectrum of both the HAT-P-12b and WASP-69b observations. Fig. 1 shows a comparison of one frame of our HAT-P-12b observations before and after the telluric sodium emission has been corrected for. Similar fea- tures, though with varying ...
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... was sufficient in characterizing the shape of the emission features, as they were present only in a very small region of the sodium doublet that could be approximated as linear (see Fig. 1). The emission features are removed in this way from both lines of the sodium doublet for every spectrum of both the HAT-P-12b and WASP-69b observations. Fig. 1 shows a comparison of one frame of our HAT-P-12b observations before and after the telluric sodium emission has been corrected for. Similar fea- tures, though with varying strengths, were observed throughout both sets of ...
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... the thousands of water lines across each spectrum of our WASP-69b observations with models at Doppler shifts of -100 km/s to +100 km/s. The colour represents the correlation strength. The top panels show the analysis process for our data, and the bottom panels show the same process repeated on the data with a water model injected (see Fig. 11). The signal from water is visible in the bottom-left panel as a diagonal line across the in-transit portion of the map, corresponding to roughly -0.01 to + 0.01 orbital phase. Likewise, the signal is visible at the Keplerian velocity of the exoplanet in the bottom-right panel, at the expected Vsys and Kp of the planet: 0 km/s and ∼ ...
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... full data reduction process as applied to the WASP-69b observations. Explanations for each panel of the figure are provided in the caption of Fig. 8 Na absorption absorption K Figure 10. The model spectra used in our analysis. ...
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... to the WASP-69b observations. Explanations for each panel of the figure are provided in the caption of Fig. 8 Na absorption absorption K Figure 10. The model spectra used in our analysis. The top panel shows the spectrum calculated for HAT-P-12b, and the bottom panel shows the spectrum calculated for WASP-69b. Water bands can be identified from Fig. 11, but the locations of other important species are marked. Figure 11. The model spectra used in our analysis. The top panel shows the spectrum calculated for HAT-P-12b, and the bottom panel shows the spectrum calculated for WASP-69b. These models only include lines from ...
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