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26 April 2024 |
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Characterizing Earth-like Planets Using a Combination of High-Dispersion Spectroscopy and High-Contrast Instruments: Doppler-shifted Water and Oxygen Lines | | Hajime Kawahara
; | | Date: |
19 Sep 2014 | | Abstract: | Future radial velocity, astrometric and direct imaging surveys will find
nearby Earth-sized planets within the habitable zone (HZ) in the near future.
How can we search for water and oxygen in those non-transiting planets? We
propose a combination of high-dispersion spectroscopy and coronagraphic
techniques as a method to detect molecular lines in Earth-like planets (ELPs).
In this method, the planetary signals are spectroscopically separated from the
telluric absorption due to the Doppler shift. Assuming a long observing
campaign ($T_mathrm{exp}=$ 20 days) using the high-dispersion spectrometer ($R
= 50,000$) with the speckle suppression on a 30 m telescope, we simulate the
spectra from the ELPs around M dwarfs at 5 pc. Performing the cross-correlation
analysis with the binary template of the molecular lines, we find that the raw
contrasts of $10^{-4}$ (0.8-1.8 $mu$m) and $10^{-4.5}$ (use of J-band only) at
30 mas are required to detect the water vapor for a $sim 4 - 5 sigma$
detection. The raw contrast of $10^{-5}$ is required for a 4 $sigma$ detection
of the oxygen 1.27 $mu$m band. For the ELPs around solar-type stars, it is
necessary to assume a several hundred times better contrast than that for M
dwarfs in order to detect water vapor. This method does not require any
additional post-processings and is less sensitive to the terrestrial noise than
the low resolution spectroscopy. We conclude that a combination of
high-dispersion spectroscopy and high-contrast instruments can be a powerful
means to characterize the ELPs in the extremely large telescope era. | | Source: | arXiv, 1409.5740 | | Services: | Forum | Review | PDF | Favorites | |
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