M. Salz, S. Czesla, P. C. Schneider, E. Nagel, J. H. M. M. Schmitt, L. Nortmann, F. J. Alonso-Floriano, M. López-Puertas, M. Lampón, F. F. Bauer, I. A. G. Snellen, E. Pallé, J. A. Caballero, F. Yan, G. Chen, J. Sanz-Forcada, P. J. Amado, A. Quirrenbach, I. Ribas, A. Reiners, V. J. S. Béjar, N. Casasayas-Barris, M. Cortés-Contreras, S. Dreizler, E. W. Guenther, T. Hennin, S. V. Jeffers, A. Kaminski, M. Kürster, M. Lafarga, L. M. Lara, K. Molaverdikhani, D. Montes, J. C. Morales, A. Sánchez-López, W. Seifert, M. R. Zapatero Osorio and M. Zechmeister. 2018. Detection of He I lambda 10830 angstrom absorption on HD 189733 b with CARMENES high-resolution transmission spectroscopy. Astronomy and Astrophysics 620, DOI: 10.1051/0004-6361/201833694
We present three transit observations of HD 189733 b obtained with the high-resolution spectrograph CARMENES at Calar Alto. A strong absorption signal is detected in the near-infrared He I triplet at 10830 angstrom in all three transits. During mid-transit, the mean absorption level is 0.88 +/- 0.04% measured in a +/- 10 km s(-1) range at a net blueshift of -3.5 +/- 0.4 km s(-1) (10829.84-10830.57 angstrom). The absorption signal exhibits radial velocities of +6.5 +/- 3.1 km s(-1) and -12.6 +/- 1.0 km s(-1) during ingress and egress, respectively; all radial velocities are measured in the planetary rest frame. We show that stellar activity related pseudo-signals interfere with the planetary atmospheric absorption signal. They could contribute as much as 80% of the observed signal and might also affect the observed radial velocity signature, but pseudo-signals are very unlikely to explain the entire signal. The observed line ratio between the two unresolved and the third line of the He i triplet is 2.8 +/- 0.2, which strongly deviates from the value expected for an optically thin atmospheres. When interpreted in terms of absorption in the planetary atmosphere, this favors a compact helium atmosphere with an extent of only 0.2 planetary radii and a substantial column density on the order of 4 x 10(12) cm(2). The observed radial velocities can be understood either in terms of atmospheric circulation with equatorial superrotation or as a sign of an asymmetric atmospheric component of evaporating material. We detect no clear signature of ongoing evaporation, like pre- or post-transit absorption, which could indicate material beyond the planetary Roche lobe, or radial velocities in excess of the escape velocity. These findings do not contradict planetary evaporation, but only show that the detected helium absorption in HD 189733 b does not trace the atmospheric layers that show pronounced escape signatures.
