---------- X-Sun-Data-Type: text X-Sun-Data-Description: text X-Sun-Data-Name: text X-Sun-Charset: us-ascii X-Sun-Content-Lines: 12 All: My name is Christopher Garasi and I am 3rd year grad student at NMSU. I have been consulting with the WSMR (White Sande Missle Range) engineers concerning the AMBER IR camera to be installed sometime this November. Below are two emails I have begun circulating concering the filters to be used with this detector. Please feel free to email me with any questions you might have. ---------- X-Sun-Data-Type: default X-Sun-Data-Name: message1 X-Sun-Charset: us-ascii X-Sun-Content-Lines: 35 All: I received word today from a White Sands engineer (John Corvo) asking about filters for the AMBER IR detector. Specifically, the filter wheel to be used in the dewer will have 5 slots (of which we will use 2). Below is a listing of what filters I requested (rest lambda and range) and what they can offer to get us (their expense). Please note if you think the filter ranges they have given us are unaccepatable and why. I already have had input from Tom Harrison about the K filter going too far into an atmospheric absorption band on the shortward side. ______________________________________________________________________ Name Rest lambda(microns) Range what WSMR can get ______________________________________________________________________ J 1.2 1.1 - 1.3 1.09 - 1.4 or 1.13 - 1.43 H 1.6 1.45 - 1.75 1.45 - 1.95 K 2.2 2.0 - 2.4 1.875 - 2.4 L' 3.8 3.5 - 4.2 3.45 - 4.14 M 4.9 4.55 - 5.25 4.66 - 5.2 Note, the L' filter is what the WSMR range people will be using for their tests. Lucky for us it winds up being L'! Mr.Corvo has asked me to look into these numbers and get back to him ASAP ( by this Wednesday 8/23). They are really trying to push the dewer manufacturer to supply these filters and get the instrument set up by November. Any input which you could give on this matter would be appreciated: Chris Garasi ---------- X-Sun-Data-Type: default X-Sun-Data-Name: message3 X-Sun-Charset: us-ascii X-Sun-Content-Lines: 51 AMBER detector (InSb- Indium Antimonide) Pixel Elements: 512x512 Pixel Size: 25x25 microns Operating Temp: 78 K (Liquid Nitrogen cooled) QE: 0.68 (Non AR coated); >80 with AR coating Dynamic Range: >10,000 Readout Noise: <250 electrons Nonlinearity: <1.5% Bandpass for chip: ~1 - 5.4 microns There are no focal reducers to be used with the AMBER camera, therefore the camera will work at F10. using the following relation: _____________________________________ arcsec/pix= pixsize/(F*D) * (180/Pi) * 3600 F=Focal ratio, D telescope primary Diameter (meters), pixel size (meters) _____________________________________ one can obtain the pixel sky coverage. ___________________________________________________ GRIM | AMBER | F/5 0.41 "/pix | - F/10 0.235 "/pix | 0.147 "/pix F/20 0.1178 "/pix | - ___________________________________________________ Note: The pixel size for GRIM is 40 microns as compared to 25 microns for AMBER. This is why the amount of sky covered per pixel is smaller. Comparisons of Field-of-Views is: ___________________________________________________ GRIM | AMBER | F/5 ~ 2 arcminutes | - F/10 ~ 1 arcminute | ~ 1.25 arcminutes F/20 ~ 30 arcseconds | - ___________________________________________________ Point to remember: We are not going to get much more sky coverage with AMBER even if the chip size is twice as large as GRIM simply because the pixel sizes are almost 1/2 of that for GRIM. APO APO APO APO APO Apache Point Observatory 3.5m APO APO APO APO APO This is message 1 in the apo35-amber archive. You can find APO the archive in /u/strauss/apo/mailer/apo35-amber on astro.princeton.edu APO To join/leave the list, send mail to apo35-request@astro.princeton.edu APO To post a message, mail it to apo35-amber@astro.princeton.edu APO APO APO APO APO APO APO APO APO APO APO APO APO APO APO APO APO