1 / 14

Kyoto 3DII (3DII) + AO188

Kyoto 3DII (3DII) + AO188. 2010 Apr 26 H ST What is 3DII? Purposes of 3DII + AO188 What is needed for this? Present status Cass or Nasmyth in future? Proposed schedule [I am sorry but some parts are written in Japanese. ]. http://optik2.mtk.nao.ac.jp/~minoways/AO_session/

ida
Download Presentation

Kyoto 3DII (3DII) + AO188

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Kyoto 3DII (3DII) + AO188 2010 Apr 26HST • What is 3DII? • Purposes of 3DII + AO188 • What is needed for this? • Present status • Cass or Nasmyth in future? • Proposed schedule [I am sorry but some parts are written in Japanese.] http://optik2.mtk.nao.ac.jp/~minoways/AO_session/ tutorial/index.htmlより

  2. What is 3DII? • Multi-mode spectrograph --- includes Integral field spectrograph (IFS) mode, Fabry-Perot mode, etc. • Optical wavelength (360-900nm) • Now used at Subaru Cassegrain Focus “The Kyoto Tridimensional Spectrograph II on Subaru and the University of Hawaii 88-inch Telescopes”, Sugai et al., 2010, PASP, 122, 103 Present members in Kyoto Univ.: Sugai(PI), Matsubayashi, Nakajima, Yoshimura cf. Shimono, Akita, Hattori

  3. In the case of Cassegrain At UH88: June 2002 At Subaru: August 2002

  4. Purposes of 3DII + AO188 • First optical instrument used with AO at 8-10m class telescopes ~0”.1 spatial sampling of 3DII • Providing evaluation of AO188 in optical wavelengths

  5. Expected improvements with AO (IFS mode) （下農他 2005, すばるUMポスターより） 0”.5 seeing 0”.7 seeing

  6. An example of present 3DII results IFS of gravitationally lensed Quasar (Z=0.658) Hb(broad line) [OIII](narrow line) 白い棒線が0”.5 = 2.2kpc at zlens=0.295。　最も暗い像Dは視野外。 "Integral Field Spectroscopy of the QuadruplyLensed Quasar 1RXS J1131-1231: New Light on Lens Substructures”, Sugai, Kawai, Shimono, Hattori, Kosugi, Kashikawa, Inoue, Chiba, 2007, ApJ, 660, 1016

  7. What is needed for this? • Mechanical interface Nasmyth Mount Four fixed points • Optical interface dichroic mirror

  8. now in Hawaii

  9. Optical interface (dichroic mirror: measured) cf. Laser guide star 589nm. AO low-order wave-front sensor 450-1000nm.

  10. Present status • Mechanical interface Nasmyth Mount Four fixed points • Optical interface dichroic mirror test done setting done to be installed on 2010 Apr 29, with Minowa-san

  11. Cass or Nasmyth in future? • Both desired Nasmyth for longer wavelengths (>650nm) Cass for shorter wavelengths (<650nm) We would try to minimize our changes of foci.

  12. Proposed schedule This must not damage AO188, IRCS, Hi-CIAO schedules. This must not damage Hawaii observatory schedules, including daycrews’ ones.

  13. Proposed schedule 2010/2011 Optical alignment between 3DII & AO188 (by using 3DII CCD & AO188 worked) Software integration with AO188 through Gen2 (SOSS compatible)? Test observations

More Related