scholarly journals Titan airglow spectra from Cassini Ultraviolet Imaging Spectrograph (UVIS): EUV analysis

2007 ◽  
Vol 34 (24) ◽  
Author(s):  
Joseph M. Ajello ◽  
Michael H. Stevens ◽  
Ian Stewart ◽  
Kristopher Larsen ◽  
Larry Esposito ◽  
...  
Keyword(s):  
Imaging Spectrograph

scholarly journals The Infrared Imaging Spectrograph (IRIS) for TMT: instrument overview

2014 ◽  
Author(s):  
Anna M. Moore ◽  
James E. Larkin ◽  
Shelley A. Wright ◽  
Brian Bauman ◽  
Jennifer Dunn ◽  
...  
Keyword(s):  
Infrared Imaging ◽  
Imaging Spectrograph

A slitless x-ray imaging spectrograph concept for solar-pointed CubeSats (Conference Presentation)

2016 ◽  
Author(s):  
Amir Caspi ◽  
Albert Y. Shih ◽  
Harry P. Warren ◽  
Marek Steslicki ◽  
Janusz Sylwester ◽  
...  
Keyword(s):  
X Ray ◽  
X Ray Imaging ◽  
Imaging Spectrograph

The Ultraviolet Micromirror Imaging Spectrograph: a multi-object spectrograph for far UV astronomy

2021 ◽  
Author(s):  
Ambily Suresh ◽  
Brian T. Fleming ◽  
Natalie K. Anderson ◽  
Dmitry Vorobiev ◽  
Jack Williams ◽  
...  
Keyword(s):  
Uv Astronomy ◽  
Imaging Spectrograph

The Stellar Content of Henize 2‐10 from Space Telescope Imaging Spectrograph Ultraviolet Spectroscopy

2003 ◽  
Vol 586 (2) ◽  
pp. 939-958 ◽  
Author(s):  
Rupali Chandar ◽  
Claus Leitherer ◽  
Christy Tremonti ◽  
Daniela Calzetti
Keyword(s):  
Ultraviolet Spectroscopy ◽  
Stellar Content ◽  
Space Telescope ◽  
Imaging Spectrograph

scholarly journals COMPONENT-BASED DEVELOPMENT OF OBSERVATIONAL SOFTWARE FOR KASI SOLAR IMAGING SPECTROGRAPH

2005 ◽  
Vol 38 (4) ◽  
pp. 463-470
Author(s):  
Seong-Hwan Choi ◽  
Yeon-Han Kim ◽  
Yong-Jae Moon ◽  
Kyung-Seok Choi ◽  
Young-Deuk Park ◽  
...  
Keyword(s):  
Component Based Development ◽  
Imaging Spectrograph

Development of an integral field unit for a near-infrared multi-object imaging spectrograph SWIMS

2012 ◽  
Author(s):  
Shinobu Ozaki ◽  
Yutaro Kitagawa ◽  
Kentaro Motohara ◽  
Masahiro Konishi ◽  
Hidenori Takahashi ◽  
...  
Keyword(s):  
Near Infrared ◽  
Field Unit ◽  
Imaging Spectrograph ◽  
Integral Field ◽  
Object Imaging

The On-Orbit Performance of the Space Telescope Imaging Spectrograph

1998 ◽  
Vol 492 (2) ◽  
pp. L83-L93 ◽  
Author(s):  
R. A. Kimble ◽  
B. E. Woodgate ◽  
C. W. Bowers ◽  
S. B. Kraemer ◽  
M. E. Kaiser ◽  
...  
Keyword(s):  
Space Telescope ◽  
Imaging Spectrograph

All that is known about Mars discrete aurorae so far

2021 ◽  
Author(s):  
Lauriane Soret ◽  
Zachariah Milby ◽  
Jean-Claude Gérard ◽  
Nick Schneider ◽  
Sonal Jain ◽  
...  
Keyword(s):  
Magnetic Field ◽  
Emission Layer ◽  
Atmospheric Effect ◽  
Average Electron Energy ◽  
Mars Express ◽  
Spatially Correlated ◽  
Auroral Emissions ◽  
Average Electron ◽  
First Time ◽  
Imaging Spectrograph

<p>The discrete aurorae on Mars were discovered with the SPICAM spectrograph on board Mars Express. Now, they have been analyzed in detail using the much more sensitive MAVEN/IUVS imaging spectrograph.</p><p>This presentation gives a summary of the very latest results obtained by Schneider et al. and Soret et al. on this topic.</p><p>The main conclusions are the following:</p><ul><li>the number of auroral event detections has considerably increased since the Mars Express observations;</li> <li>many detections have been made outside of the Southern crustal magnetic field structures;</li> <li>the MUV spectrum shows the same emissions as those observed in the dayglow, with similar intensity ratios;</li> <li>the Vegard-Kaplan bands of N<sub>2</sub> have been observed for the first time in the Martian aurora;</li> <li>the CO Cameron and the CO<sub>2</sub><sup>+</sup> UVD emissions occur at the same altitude;</li> <li>the OI emission at 297.2 nm has been analyzed;</li> <li>the CO Cameron/CO<sub>2</sub><sup>+</sup> UVD ratio is quasi-constant;</li> <li>intensities are higher in B-field regions;</li> <li>auroral emissions are more frequent in the pre-midnight sector;</li> <li>the altitude of the emission layer is independent of local time and presence or absence of a crustal magnetic field;</li> <li>the altitude of the emission layer varies moderately with season (atmospheric effect);</li> <li>the events are spatially correlated with an increase in the flux of energetic electrons simultaneously measured by the MAVEN/SWEA (Solar Wind Electron Analyzer) detectors;</li> <li>the peak altitude of the emission is in good agreement with that expected from the average electron energy.</li> </ul>

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