Detection of He I $lambda10830$ AA{} absorption on HD 189733 b with CARMENES high-resolution transmission spectroscopy. (arXiv:1812.02453v1 [astro-ph.EP])

Detection of He I $lambda10830$ AA{} absorption on HD 189733 b with CARMENES high-resolution transmission spectroscopy. (arXiv:1812.02453v1 [astro-ph.EP])
<a href="http://arxiv.org/find/astro-ph/1/au:+Salz_M/0/1/0/all/0/1">M. Salz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Czesla_S/0/1/0/all/0/1">S. Czesla</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schneider_P/0/1/0/all/0/1">P. C. Schneider</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nagel_E/0/1/0/all/0/1">E. Nagel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schmitt_J/0/1/0/all/0/1">J. H. M. M. Schmitt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nortmann_L/0/1/0/all/0/1">L. Nortmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alonso_Floriano_F/0/1/0/all/0/1">F. J. Alonso-Floriano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_Puertas_M/0/1/0/all/0/1">M. López-Puertas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lampon_M/0/1/0/all/0/1">M. Lampón</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bauer_F/0/1/0/all/0/1">F. F. Bauer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Snellen_I/0/1/0/all/0/1">I. A. G. Snellen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Palle_E/0/1/0/all/0/1">E. Pallé</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caballero_J/0/1/0/all/0/1">J. A. Caballero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yan_F/0/1/0/all/0/1">F. Yan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_G/0/1/0/all/0/1">G. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanz_Forcada_J/0/1/0/all/0/1">J. Sanz-Forcada</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Amado_P/0/1/0/all/0/1">P. J. Amado</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quirrenbach_A/0/1/0/all/0/1">A. Quirrenbach</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ribas_I/0/1/0/all/0/1">I. Ribas</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reiners_A/0/1/0/all/0/1">A. Reiners</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bejar_V/0/1/0/all/0/1">V. J. S. Béjar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Casasayas_Barris_N/0/1/0/all/0/1">N. Casasayas-Barris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cortes_Contreras_M/0/1/0/all/0/1">M. Cortés-Contreras</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dreizler_S/0/1/0/all/0/1">S. Dreizler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Guenther_E/0/1/0/all/0/1">E. W. Guenther</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Henning_T/0/1/0/all/0/1">T. Henning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jeffers_S/0/1/0/all/0/1">S. V. Jeffers</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kaminski_A/0/1/0/all/0/1">A. Kaminski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kurster_M/0/1/0/all/0/1">M. Kürster</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lafarga_M/0/1/0/all/0/1">M. Lafarga</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lara_L/0/1/0/all/0/1">L. M. Lara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Molaverdikhani_K/0/1/0/all/0/1">K. Molaverdikhani</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Montes_D/0/1/0/all/0/1">D. Montes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morales_J/0/1/0/all/0/1">J. C. Morales</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sanchez_Lopez_A/0/1/0/all/0/1">A. Sánchez-López</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Seifert_W/0/1/0/all/0/1">W. Seifert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Osorio_M/0/1/0/all/0/1">M. R. Zapatero Osorio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zechmeister_M/0/1/0/all/0/1">M. Zechmeister</a>

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 AA{} in all three
transits. During mid-transit, the mean absorption level is $0.88pm0.04$ %
measured in a $pm$10 km s$^{-1}$ range at a net blueshift of $-3.5pm0.4$ km
s$^{-1}$ (10829.84–10830.57 AA{}). The absorption signal exhibits radial
velocities of $+6.5pm3.1$ km s$^{-1}$ and $-12.6pm1.0$ km s$^{-1}$ during
ingress and egress, respectively; 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 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
$2.8pm0.2$, 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 $4times
10^{12}$ 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.

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