METIS: the mid-infrared E-ELT imager and spectrograph

Brandl, Bernhard R.; Feldt, M.; Glasse, Alistair; Guêdel, M.; Heikamp, S.; Kenworthy, Matthew A.; Lenzen, R.; Meyer, Michael; Molster, Frank; Paalvast, S.L.; Pantin, É.; Quanz, Sascha P.; Schmalzl, Eva; Stuik, Remko; Venema, Lars; Waelkens, Christoffel

doi:10.1117/12.2056468

Cited by 38 publications

(24 citation statements)

References 25 publications

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“…Eventually, high-resolution spectra of exoplanets with broad spectral coverage will allow collating an inventory of the atmospheric chemical composition, will help explore aeronomic properties such as pressure-temperature profiles, and will lead to a better understanding of the formation and evolution of exoplanets. This is also a motivation for building a high-resolution spectrograph on the European Extremely-LargeTelescope such as HiReS and METIS (Udry et al 2014;Brandl et al 2014;Snellen et al 2015). In the meantime, extensive studies have to be made with existing facilities and data especially in the optical domain (e.g., Hoeijmakers et al 2015) to help observers make the best use of future facilities.…”

Section: Discussionmentioning

confidence: 99%

Spectrally resolved detection of sodium in the atmosphere of HD 189733b with the HARPS spectrograph

Wyttenbach

Ehrenreich

Lovis

et al. 2015

A&A

297

487

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Context. Atmospheric properties of exoplanets can be constrained with transit spectroscopy. At low spectral resolution, this technique is limited by the presence of clouds. The signature of atomic sodium (Na ), known to be present above the clouds, is a powerful probe of the upper atmosphere, where it can be best detected and characterized at high spectral resolution. Aims. Our goal is to obtain a high-resolution transit spectrum of HD 189733b in the region around the resonance doublet of Na  at 589 nm, to characterize the absorption signature that was previously detected from space at low resolution.Methods. We analyzed archival transit data of HD 189733b obtained with the HARPS spectrograph (R = 115 000) at the ESO 3.6-m telescope. We performed differential spectroscopy to retrieve the transit spectrum and light curve of the planet, implementing corrections for telluric contamination and planetary orbital motion. We compared our results to synthetic transit spectra calculated from isothermal models of the planetary atmosphere.Results. We spectrally resolve the Na  D doublet and measure line contrasts of 0.64 ± 0.07% (D2) and 0.40 ± 0.07% (D1) and FWHMs of 0.52 ± 0.08 Å. This corresponds to a detection at the 10σ level of excess of absorption of 0.32 ± 0.03% in a passband of 2 × 0.75 Å centered on each line. We derive temperatures of 2600 ± 600 K and 3270 ± 330 K at altitudes of 9800 ± 2800 and 12 700 ± 2600 km in the Na  D1 and D2 line cores, respectively. We measure a temperature gradient of ∼0.2 K km −1 in the region where the sodium absorption dominates the haze absorption from a comparison with theoretical models. We also detect a blueshift of 0.16 ± 0.04 Å (4σ) in the line positions. This blueshift may be the result of winds blowing at 8 ± 2 km s −1 in the upper layers of the atmosphere. Conclusions. We demonstrate the relevance of studying exoplanet atmospheres with high-resolution spectrographs mounted on 4-m-class telescopes. Our results pave the way for an in-depth characterization of physical conditions in the atmospheres of many exoplanetary systems with future spectrographs such as ESPRESSO on the VLT or HiReS and METIS on the E-ELT.

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Section: Discussionmentioning

confidence: 99%

Spectrally resolved detection of sodium in the atmosphere of HD 189733b with the HARPS spectrograph

Wyttenbach

Ehrenreich

Lovis

et al. 2015

A&A

297

487

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“…MIRI 5 at James Webb Space Telescope however, does not provide for spectroscopy in this regime. Hence, an instrument such as METIS 6 on the E-ELT will be of great value (Brandl et al 2014). As presented right now, METIS Echelle spectroscopy is implemented as a single order integral field mode.…”

Section: Prospects For Future Observationsmentioning

confidence: 99%

A CRIRES-search for H₃⁺emission from the hot Jupiter atmosphere of HD 209458 b

Lenz

Reiners

Seifahrt

et al. 2016

A&A

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Close-in extrasolar giant planets are expected to cool their thermospheres by producing H + 3 emission in the near-infrared (NIR), but simulations predict H + 3 emission intensities that differ in the resulting intensity by several orders of magnitude. We want to test the observability of H + 3 emission with CRIRES at the Very Large Telescope (VLT), providing adequate spectral resolution for planetary atmospheric lines in NIR spectra. We search for signatures of planetary H + 3 emission in the L band, using spectra of HD 209458 obtained during and after secondary eclipse of its transiting planet HD 209458 b. We searched for H + 3 emission signatures in spectra containing the combined light of the star and, possibly, the planet. With the information on the ephemeris of the transiting planet, we derive the radial velocities at the time of observation and search for the emission at the expected line positions. We also apply a cross-correlation test to search for planetary signals and use a shift and add technique combining all observed spectra taken after secondary eclipse to calculate an upper emission limit. We do not find signatures of atmospheric H + 3 emission in the spectra containing the combined light of HD 209458 and its orbiting planet. We calculate the emission limit for the H + 3 line at 3953.0 nm [Q(1, 0)] to be 8.32 × 10 18 W and a limit of 5.34 × 10 18 W for the line at 3985.5 nm [Q(3, 0)]. Comparing our emission limits to the theoretical predictions suggests that we lack 1 to 3 magnitudes of sensitivity to measure H + 3 emission in our target object. We show that under more favorable weather conditions the data quality can be improved significantly, reaching 5 × 10 16 W for star-planet systems that are close to Earth. We estimate that pushing the detection limit down to 10 15 W will be possible with ground-based observations with future instrumentation, for example, the European Extremly Large Telescope.

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“…This work includes a study of extending METIS to the Q band in the high spectral resolution mode. An update of this instrument is presented in these proceedings by Brandl et al 10 .…”

Section: Elt-mir/metismentioning

confidence: 96%

The E-ELT instrument roadmap: a status report

Ramsay¹,

Casali²,

González³

et al. 2014

SPIE Proceedings

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We present the status of the instrumentation programme for the European Extremely Large Telescope. The instrumentation planning is governed by the E-ELT Instrument Roadmap, which synthesises the scientific, technical and managerial influences on the instrument programme into a staged development plan. Preparations for the start of the design and build phases of the first light instruments and their adaptive optics systems are well underway and are summarised here. In parallel, the process for development of the next three instruments has begun. Recent work on the instrument interface to the telescope is described.

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METIS: the mid-infrared E-ELT imager and spectrograph

Cited by 38 publications

References 25 publications

Spectrally resolved detection of sodium in the atmosphere of HD 189733b with the HARPS spectrograph

Spectrally resolved detection of sodium in the atmosphere of HD 189733b with the HARPS spectrograph

A CRIRES-search for H₃⁺emission from the hot Jupiter atmosphere of HD 209458 b

The E-ELT instrument roadmap: a status report

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METIS: the mid-infrared E-ELT imager and spectrograph

Cited by 38 publications

References 25 publications

Spectrally resolved detection of sodium in the atmosphere of HD 189733b with the HARPS spectrograph

Spectrally resolved detection of sodium in the atmosphere of HD 189733b with the HARPS spectrograph

A CRIRES-search for H3+emission from the hot Jupiter atmosphere of HD 209458 b

The E-ELT instrument roadmap: a status report

Contact Info

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Resources

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A CRIRES-search for H₃⁺emission from the hot Jupiter atmosphere of HD 209458 b