This text treats our knowledge of the solar system from an astrophysical point of view. Part 1 deals with the formation of the solar system and its interaction with the interplanetary medium. Part 2 presents its various objects: planets and satellites, asteroids, comets and interplanetary dust. The final sections on comparative planetology, open questions and future space exploration round off an introduction to a field which has grown dramatically following the space missions of the last fifteen years. In this second corrected and revised edition students and lecturers in astronomy and planetary science as well as planet observers will find a mine of up-to-date information.

The Solar System

We report the first demonstration of a mid-IR reflection-based flat lens with high efficiency and near diffraction-limited focusing. Focusing efficiency as high as 80%, in good agreement with simulations (83%), has been achieved at 45° incidence angle at λ = 4.6 μm. The off-axis geometry considerably simplifies the optical arrangement compared to the common geometry of normal incidence in reflection mode which requires beam splitters. Simulations show that the effects of incidence angle are small compared to parabolic mirrors with the same NA. The use of single-step photolithography allows large scale fabrication. Such a device is important in the development of compact telescopes, microscopes, and spectroscopic designs.

/pdf/high-efficiency-near-diffraction-limited-mid-infrared-flat-22sy92rjcj.pdf

High efficiency near diffraction-limited mid-infrared flat lenses based on metasurface reflectarrays

We provide new measurements of wavenumbers and line identifications of 10, 100 U I and U II near-infrared (NIR) emission lines between 2500 cm–1 and 12, 000 cm–1 (4000-850 nm) using archival Fourier transform spectrometer spectra from the National Solar Observatory. This line list includes isolated uranium lines in the Y, J, H, K, and L bands (0.9-1.1 μm, 1.2-1.35 μm, 1.5-1.65 μm, 2.0-2.4 μm, and 3.0-4.0 μm, respectively), and provides six times as many calibration lines as thorium in the NIR spectral range. The line lists we provide enable inexpensive, commercially available uranium hollow cathode lamps to be used for high-precision wavelength calibration of existing and future high-resolution NIR spectrographs.

https://iopscience.iop.org/article/10.1088/0067-0049/195/2/24/pdf

The Infrared Spectrum of Uranium Hollow Cathode Lamps from 850 nm to 4000 nm: Wavenumbers and Line Identifications from Fourier Transform Spectra

A limiting factor in the development of mid-infrared optics is the lack of abundant materials that are transparent, low cost, lightweight, and easy to machine. In this paper, we demonstrate a metasurface device that circumvents these limitations. A flat lens based on antenna reflectarrays was designed to achieve near diffraction-limited focusing with a high efficiency (experiment: 80%, simulation: 83%) at 45(o) incidence angle at {\lambda} = 4.6 {\mu}m. This geometry considerably simplifies the experimental arrangement compared to the common geometry of normal incidence which requires beam splitters. Simulations show that the effect of comatic aberrations is small compared to parabolic mirrors. The use of single-step photolithography allows large scale fabrication.

We provide new measurements of wavenumbers and line identifications of 10 100 UI and UII near-infrared (NIR) emission lines between 2500 cm-1 and 12 000 cm-1 (4000 nm to 850 nm) using archival FTS spectra from the National Solar Observatory (NSO). This line list includes isolated uranium lines in the Y, J, H, K, and L bands (0.9 {\mu}m to 1.1 {\mu}m, 1.2 {\mu}m to 1.35 {\mu}m, 1.5 {\mu}m to 1.65 {\mu}m, 2.0 {\mu}m to 2.4 {\mu}m, and 3.0 {\mu}m to 4.0 {\mu}m, respectively), and provides six times as many calibration lines as thorium in the NIR spectral range. The line lists we provide enable inexpensive, commercially-available uranium hollow-cathode lamps to be used for high-precision wavelength calibration of existing and future high-resolution NIR spectrographs.

/pdf/the-infrared-spectrum-of-uranium-hollow-cathode-lamps-from-gnw8zur0x8.pdf

A feasibility design study was undertaken to assess the requirements of a mid-infrared echelle spectrograph (MIRES) 
with a resolving power of 120,000 and its associated mid-infrared adaptive optics (MIRAO) system on the Thirty-Meter 
Telescope. Our baseline design incorporates a 2K×2K Si:As array or array mosaic for the spectrograph and a 1K×1K 
Si:As array for the slit viewer. Various tradeoffs were studied to minimize risk and to optimize the sensitivity of the 
instrument. Major challenges are to integrate the spectrograph to the MIRAO system and, later, to an adaptive 
secondary, the procurement of a suitable window and large KRS-5 lenses, and the acquisition of large format mid-IR 
detector arrays suitable for the range of background conditions. We conclude that the overall risk is relatively low and 
there is no technical reason that should prevent this instrument from being ready for use at first light on the Thirty-
Meter Telescope.

Design tradeoffs for a high spectral resolution mid-infrared echelle spectrograph on the Thirty-Meter Telescope

We present a discussion of the science drivers and design approach for a high-resolution, mid-infrared spectrograph for the Thirty-Meter Telescope. The instrument will be integrated with an adaptive optics system optimized for the midinfrared; as a consequence it is not significantly larger or more complex than similar instruments designed for use on smaller telescopes. The high spatial and spectral resolution possible with such a design provides a unique scientific capability. The design provides spectral resolution of up to 120,000 for the 4.5-25 �� m region in a cross-dispersed format that provides continuous spectral coverage of up to 2% to 14 �� m. The basic concept is derived from the successful TEXES mid-infrared spectrograph. To facilitate operation, there are separate imaging channels for the near-infrared and the mid-infrared; both can be used for acquisition and the mid-infrared imaging mode can be used for science imaging and for guiding. Because the spectrograph is matched to the diffraction limit of a 30-m telescope, gains in sensitivity are roughly proportional to the square of the telescope diameter, opening up a volume within the Galaxy a thousand times greater than existing instruments.

Design of the TMT Mid-Infrared Echelle: Science Drivers and Design Overview

We present a preliminary optical design for a mid-infrared, high-resolution spectrograph (MIRES), together with an 
integrated adaptive optics system optimized for the mid-infrared, intended for use on a 30-meter telescope. The design 
includes laser guide star wavefront sensors, a near-infrared natural guide star wavefront sensor with a patrol field of 60 
arcseconds, and near-infrared and mid-infrared imaging channels, in addition to the cross-dispersed spectrograph itself. 
The spectrograph provides resolution of up to 120,000 and continuous spectral coverage over multiple cross-dispersed 
orders, with high efficiency between 4.5 and 25 microns.

Preliminary optical design for the TMT mid-infrared adaptive optics system and echelle spectrograph

We present a conceptual design for an innovative infrared cross-dispersed spectrograph for the NASA Infrared
Telescope Facility (IRTF) at Mauna Kea. This facility-class instrument will provide a resolving power of up to 80,000 at
1.2-2.5 μm and 67,000 at 3-5 μm with a minimum slit width of 0.25". The instrument employs a silicon immersion
grating in order to reduce the size of the instrument. The design incorporates a 2048×2048 infrared array for the
spectrograph and an infrared slit viewer. The optical design is optimized for the thermal infrared (2.8-5.5 μm).

Silicon immersion grating spectrograph design for the NASA Infrared Telescope Facility

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Design tradeoffs for a high spectral resolution mid-infrared echelle spectrograph on the Thirty-Meter Telescope

Design of the TMT Mid-Infrared Echelle: Science Drivers and Design Overview

Preliminary optical design for the TMT mid-infrared adaptive optics system and echelle spectrograph

Silicon immersion grating spectrograph design for the NASA Infrared Telescope Facility