Multiple water band detections in the CARMENES near-infrared transmission spectrum of HD 189733 b. (arXiv:1811.08901v1 [astro-ph.EP])
<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:+Sanchez_Lopez_A/0/1/0/all/0/1">A. Sánchez-López</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:+Lopez_Puertas_M/0/1/0/all/0/1">M. López-Puertas</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:+Amado_P/0/1/0/all/0/1">P. J. Amado</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:+Caballero_J/0/1/0/all/0/1">J. A. Caballero</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:+Nortmann_L/0/1/0/all/0/1">L. Nortmann</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:+Salz_M/0/1/0/all/0/1">M. Salz</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:+Ribas_I/0/1/0/all/0/1">I. Ribas</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:+Aceituno_J/0/1/0/all/0/1">J. Aceituno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Anglada_Escude_G/0/1/0/all/0/1">G. Anglada-Escudé</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:+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:+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:+Lampon_M/0/1/0/all/0/1">M. Lampón</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:+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:+Tal_Or_L/0/1/0/all/0/1">L. Tal-Or</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:+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>
Aims: We explore the capabilities of CARMENES for characterizing hot-Jupiter
atmospheres by targeting multiple water bands, in particular, those at 1.15 and
1.4 $mu$m. Hubble Space Telescope observations suggest that this wavelength
region is relevant for distinguishing between hazy/cloudy and clear
atmospheres.
Methods: We observed one transit of the hot Jupiter HD 189733 b with
CARMENES. Telluric and stellar absorption lines were removed using Sysrem,
which performs a principal component analysis including proper error
propagation. The residual spectra were analysed for water absorption with
cross-correlation techniques using synthetic atmospheric absorption models.
Results: We report a cross-correlation peak at a signal-to-noise ratio (SNR)
of 6.6, revealing the presence of water in the transmission spectrum of HD
189733 b. The absorption signal appeared slightly blueshifted at -3.9 $pm$ 1.3
kms$^{-1}$. We measured the individual cross-correlation signals of the water
bands at 1.15 and 1.4 $mu$m, finding cross-correlation peaks at SNRs of 4.9
and 4.4, respectively. The 1.4 $mu$m feature is consistent with that observed
with the Hubble Space Telescope.
Conclusions: The water bands studied in this work have been mainly observed
in a handful of planets from space. The ability of also detecting them
individually from the ground at higher spectral resolution can provide
insightful information to constrain the properties of exoplanet atmospheres.
Although the current multiband detections can not yet constrain atmospheric
haze models for HD 189733 b, future observations at higher signal-to-noise
ratio could provide an alternative way to achieve this aim.
Aims: We explore the capabilities of CARMENES for characterizing hot-Jupiter
atmospheres by targeting multiple water bands, in particular, those at 1.15 and
1.4 $mu$m. Hubble Space Telescope observations suggest that this wavelength
region is relevant for distinguishing between hazy/cloudy and clear
atmospheres.
Methods: We observed one transit of the hot Jupiter HD 189733 b with
CARMENES. Telluric and stellar absorption lines were removed using Sysrem,
which performs a principal component analysis including proper error
propagation. The residual spectra were analysed for water absorption with
cross-correlation techniques using synthetic atmospheric absorption models.
Results: We report a cross-correlation peak at a signal-to-noise ratio (SNR)
of 6.6, revealing the presence of water in the transmission spectrum of HD
189733 b. The absorption signal appeared slightly blueshifted at -3.9 $pm$ 1.3
kms$^{-1}$. We measured the individual cross-correlation signals of the water
bands at 1.15 and 1.4 $mu$m, finding cross-correlation peaks at SNRs of 4.9
and 4.4, respectively. The 1.4 $mu$m feature is consistent with that observed
with the Hubble Space Telescope.
Conclusions: The water bands studied in this work have been mainly observed
in a handful of planets from space. The ability of also detecting them
individually from the ground at higher spectral resolution can provide
insightful information to constrain the properties of exoplanet atmospheres.
Although the current multiband detections can not yet constrain atmospheric
haze models for HD 189733 b, future observations at higher signal-to-noise
ratio could provide an alternative way to achieve this aim.
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