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Comparison of High-resolution 3-micron Spectra of Jupiter, Saturn, and Titan

Comparison of High-resolution 3-micron Spectra of Jupiter, Saturn, and Titan. Sang Joon Kim, Chae Kyung Sim, Aeran Jung, and Mirim Sohn School of Space Research, Kyung Hee University. High-resolution 1.45 – 2.45 m m Planetary Spectra are NOT Available!!?.

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Comparison of High-resolution 3-micron Spectra of Jupiter, Saturn, and Titan

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  1. Comparison of High-resolution 3-micron Spectra of Jupiter, Saturn, and Titan Sang Joon Kim, Chae Kyung Sim, Aeran Jung, and Mirim Sohn School of Space Research, Kyung Hee University

  2. High-resolution 1.45 – 2.45 mm Planetary Spectra are NOT Available!!? • IGRIN spectral coverage: H (1.45 - 1.90 mm) and K (2.00-2.45 mm) bands. • Some high-resolution (R > 20,000) H and K spectra are available for inner planets (Earth, Venus, and Mars) • High-resolution (R > 20,000) H and K spectra for outer planets (Jupiter, Saturn, Uranus, Neptune) and Titan are not seen in literature. • Only after 2005, high-resolution 2.8 – 3.5 mm spectra of Jupiter, Saturn, and Titan become available in literature. • We can predict that the future IGRIN investigation of the 1.45 – 2.45 mm range of the outer planets and Titan will follow the pattern of the investigation and understanding of high-resolution 2.8 – 3.5 mm spectra of these solar system objects.

  3. Spectral resolving powerBelow, an example of “low” resolution spectroscopy

  4. An example of “mid” resolution spectroscopy

  5. An example of “High” resolution spectroscopy

  6. An example of “Super-High” resolution spectroscopy – Reserved for our children?

  7. (Ex) High Resolution vs Mid Resolution - Jupiter

  8. Then, why don’t we put a high-resolution spectrometer on a space observatory? A high-resolution spectrometer is heavy and big

  9. Infrared Spectroscopy vs Infrared imaging An Image of collisions between 22 fragments of comet S-L9 and Jupiter in 1994

  10. Different spectral shapes caused by different electron densities

  11. Detection of H3+ ions on the auroral zone of Jupiter

  12. Kim et al. (2000) Methane (CH4) Fluorescence Cassini VIMS 2004 Image

  13. Titan Resolving power : 25,000 Slit size : 0.43” × 12” NIRSPEC/KeckII slit position on Titan at the time of Keck II observations on Nov. 21, 2001 (UT) Seo, et al. (Icarus, 2009)

  14. . Best fitting model spectrum of Titan (solid line) for 2.87 – 2.92 mm compared with observed spectrum (dotted line). Unidentified features are marked by arrows. All the major absorption features are reproduced using the n2 + n3 band lines of CH3D.

  15. . Three model spectra (green, red, and blue lines) and the NIRSPEC spectrum (black line) for the 2.92 – 2.98 mm range. The green line is the best fit.

  16. Fig.1 Gemini/NIFS Spectro-Imagery Deconvolved observational images with E-W/N-S scan averaged in the wavelength range of 2.05-2.07, 2.09-2.11, and 2.17-2.19 microns.

  17. 3-Micron Features in High-resolution Spectra of Jupiter (Kim, Sang Joon, 2009) • Observation • Date: 18 April, 2006 ~ 22 August 2006(UT) (20 hours) • Observatory: UKIRT (CGS4 – Echelle) • Resolving power: 37,000 • Slit size: 0.41 arcsec X 90 arcsec • Slit position angle : 17.5 degree CCW • Slit position : Along the CML • (Extracted Region : NP, EZ, SP) • Standard Star: HD130841(A3IV) • HD125337(A1V)

  18. Keck II/NIRSPEC observations of Saturn

  19. Conclusion We predict that the future IGRIN investigation of the 1.45 – 2.45 mm range of Jupiter, Saturn, and Titan will follow the pattern of the exciting investigation and understanding of high-resolution 2.8 – 3.5 mm spectra of these solar system objects.

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