PPT-UVIS

Auroral Movies As of June 2008 Wayne Pryor Central Arizona CollegeSpace Environment Technologies 8 UVIS Polar Movies in Hand 2007 day 96 April 6 only 1 with disturbed solar wind conditions. . C. luster . L. ensing . A. nd . S. upernova survey with . H. ubble. ACS Parallels. WFC3 Parallels. 6 arcmin. = 2.2 Mpc @ z=0.5. Footprints of HST Cameras: . ACS FOV in yellow, . WFC3/IR FOV in red, . Kozhurina-Platais. Ω. Cen observed with the . WFC3/UVIS and IR . F606W & F160W filters. Wide . Range PA_V3 . and Large . POSTARG ±40. ”. Observations. L_Flat. and Distortion Cal Programs:. Outline. 1.) Step 1 – TV3 Calibration. 2.) Step 2 – SMOV4 (+ Cycle 17 Calibration). 3.) Step 3 – Final Calibration (present analysis). - More data. - New flat fields. - Astrodrizzle. - Precise calibration. s Report on . PSFs and . Pixels. Jay Anderson, Elena . Sabbi. , . Kailash. . Sahu. , and Matthew Bourque. TIPS Feb 19, 2015. Lots of Inter-related Issues. Why do we need a good PSF? (Or . do. we?). -Contributed to . Kurth. et al., Saturn chapter on “auroral processes”. -Mitchell et al. 2009 paper compared UVIS auroras to INCA ring current data. -. Gustin. et al., 2009 FUSE/UVIS auroral spectroscopy . Greg Holsclaw, Bill McClintock. June 18, 2012. Braunschweig. , Germany. Extended source . vs. point source. An extended source appears to exhibit flat field effects. The total signal from a point source, as a function of position on the detector, does not. Greg Holsclaw. Jan 8, 2014. 1. Outline. Calibrations since the last . meeting. Future calibrations. Calibration update. Status . of new calibration . routine. Website updates. A restructured calibration routine. JOSEPH AJELLO. JPL. MICHAEL STEVENS. NRL. JACQUES GUSTIN. LPAP. GREG HOLSCLAW. CU. TODD BRADLEY. UCF. team meeting: . january. 2010. T. b. LIMB MODEL, RECENT LAB ANALYSIS & UVIS OBSERVATIONS . SUBMITTED FUV LIMB PAPER (T. 1/5/12. 1. UVIS Team Meeting. Problem description. No match between the FUV data and the minimum ray high from geometer.. several seconds discrepancy.. Good match of the HSP data with geometer.. We were expecting 379 integrations and only 371 could be found in DAPS.. JOSEPH AJELLO. JPL. MICHAEL STEVENS. NRL. ROBERT WEST. JPL. JACQUES GUSTIN. LPAP. GREG HOLSCLAW. CU. TODD BRADLEY. UCF. agu. : . dEC. 2011. TITAN PROTON PLASMA (0.1 keV-4 . MeV. ) & SOLAR XUV GENERATES . JOSEPH AJELLO. JPL. MICHAEL STEVENS. NRL. ROBERT WEST. JPL. JACQUES GUSTIN. LPAP. GREG HOLSCLAW. CU. TODD BRADLEY. UCF. Team meeting: Jan20112. TITAN PROTON PLASMA (0.1 keV-4 . MeV. ) & SOLAR XUV GENERATES . Enceladus. ’ Plume – Results from Cassini’s Ultraviolet Imaging Spectrograph (UVIS) . C. J. Hansen, L. W. Esposito,. A. Hendrix, A. . Portyankina. , J. . . Colwell . August 2018. Introduction . Atmospheres node. Kickoff . Telecon. : Motivation (3/16/18) . • Cassini migration given a high priority by NASA HQ. • Need to have an understanding of what we all proposed to do (either through regular CAN activities or through recent augmentation process).