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Comparison of High-resolution 3-micron
Spectra of Jupiter, Saturn, and Titan
Sang Joon Kim, Chae Kyung Sim, Aeran Jung, and Mirim SohnSchool of Space Research,
Kyung Hee University
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High-resolution 1.45 – 2.45 m Planetary Spectra are NOT Available!!?
• IGRIN spectral coverage: H (1.45 - 1.90 m) and K (2.00-2.45 m) 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 m spectra of Jupiter, Saturn, and Titan become available in literature.
• We can predict that the future IGRIN investigation of the 1.45 – 2.45 m range of the outer planets and Titan will follow the pattern of the investigation and understanding of high-resolution 2.8 – 3.5 m spectra of these solar system objects.
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Spectral resolving power
Below, an example of “low” resolution spectroscopy
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An example of “mid” resolution spectroscopy
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An example of “High” resolution spectroscopy
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An example of “Super-High” resolution spectroscopy – Reserved for our children?
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(Ex) High Resolution vs Mid Resolution - Jupiter
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A high-resolution spectrometer is heavy and big
Then, why don’t we put a high-resolution spectrometer on a space observatory?
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Infrared Spectroscopy
vs
Infrared imaging
An Image of collisions between 22 fragments of comet S-L9 and Jupiter in 1994
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Different spectral shapes caused by different electron densities
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Detection of H3+ ions on the auroral zone of Jupiter
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Kim et al. (2000)Methane (CH4) Fluorescence
Cassini VIMS 2004 Image
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NIRSPEC/KeckII slit position on Titan at the time of Keck II observations on Nov. 21, 2001 (UT)Seo, et al. (Icarus,
2009)
Titan Resolving power : 25,000Slit size : 0.43” × 12”
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Best fitting model spectrum of Titan (solid line) for 2.87 – 2.92 m compared with observed spectrum (dotted line). Unidentified features are marked by arrows. All the major absorption features are reproduced using the 2 + 3 band lines of CH3D.
.
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Three model spectra (green, red, and blue lines) and the NIRSPEC spectrum (black line) for the 2.92 – 2.98 m range. The green line is the best fit.
.
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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.
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.
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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)
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Keck II/NIRSPEC observations of Saturn
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Conclusion
We predict that the future IGRIN investigation of the 1.45 – 2.45 m range of Jupiter, Saturn, and Titan will follow the pattern of the exciting investigation and understanding of high-resolution 2.8 – 3.5 m spectra of these solar system objects.