@misc{9248475,
  abstract     = {{Combining high-contrast imaging (HCI) with high-resolution spectroscopy (HRS) is one of the leading strategies for the next generation of direct-imaging instruments on the Extremely Large Telescope (ELT). HCI suppresses the host star’s light spatially through adaptive optics and coronagraphy, while HRS suppresses it spectrally by exploiting the Doppler-shifted molecular lines in the planet’s atmosphere. In principle, the two methods multiply, and a joint contrast gain of several orders of magnitude beyond either alone has been predicted. This is the design baseline of the ELT instruments ANDES and PCS.
This thesis develops an end-to-end simulation pipeline to quantify that gain for selfluminous giant exoplanets observed with ANDES on the ELT. The pipeline generates stellar and planetary spectra from physical models, propagates them through a simplified on-axis/off-axis differential observation including coronagraphic suppression and detector noise, and retrieves the planetary signal via cross-correlation against a noiseless template.
The pipeline is applied to four self-luminous companions with Teff = 400 − 1600 K around a common early-F host star, across angular separations of 20−79 mas, lower and upper halves of the 0.95 − 1.80 μm wavelength window, and resolving powers R = 5 × 104 − 1.9 × 105. At the reference configuration the cross-correlation deepens the accessible contrast by roughly three orders of magnitude in contrast relative to the raw coronagraphic contrast. Detection distances up to ∼ 340 pc are found for the hottest companion, and up to ∼ 15 pc for the coolest. The lower half of the wavelength window drives most of the detection for the cooler companions, while the resolving-power dependence is weak.}},
  author       = {{Magnusson, Sebastian}},
  language     = {{eng}},
  note         = {{Student Paper}},
  title        = {{High-resolution spectroscopy for high-contrast imaging of exoplanets with ELT instruments}},
  year         = {{2026}},
}