From ssm@latte.msfc.nasa.gov Tue Mar 25 00:54:59 1997 Received: from space.mit.edu by wiwaxia AA06498; Tue, 25 Mar 97 00:54:58 EST Received: from head-cfa (head-cfa.harvard.edu) by space.mit.edu AA20425; Tue, 25 Mar 97 00:54:56 EST Received: from latte.msfc.nasa.gov by head-cfa (SMI-8.6/SMI-SVR4) id AAA29081; Tue, 25 Mar 1997 00:53:35 -0500 Received: from latte.msfc.nasa.gov (ssm@localhost [127.0.0.1]) by latte.msfc.nasa.gov (8.7.5/8.7.3) with ESMTP id FAA09565 for ; Tue, 25 Mar 1997 05:53:53 GMT Message-Id: <199703250553.FAA09565@latte.msfc.nasa.gov> To: head@head-cfa.harvard.edu Subject: HRC Status #4 Date: Tue, 25 Mar 1997 05:53:53 +0000 From: "Stephen S. Murray" Status: R Since the last status report HRC operations at XRCF have been fairly routine. We completed a series of effective area measurements with the central segment of the HRC-S and the detector is behaving rather well. We were able to determine the focval plane position for HRC-S using shutter tests to an accuracy of about 100 microns (two tests agree) and determine that the HRC-S is about 600 microns in front of HRC-I (we expected a bit less - 300 microns) but this is well within the tolerance buildup. The count rate linearity for the HRC-S is quite good. Up to about 10ct/sec in a focused beam we see good linearity with the input flux. There is no evidence of any depression in detection efficiency in the center of the image. Using the Ring Focus of the HRMA we were able to map out the location of the HESF flats on the HRC-S. THese are complex data to analyze fully. Jeremy Drake is working on the data with the HRC Team. We will know the relative position of the flats in time to carry out the reflectivity measurement planned over the rest of the calibration. It is good to note that the flats do not reflect very much at 2.5 keV were the ring focus tests were done! Our last "first light" was today when the HRC-S and LETG were finally operated together. We have some very beautiful and informative images that were taken spanning energies from 7 keV down to about 1.5 keV. The mutilple orders (at least to 9-th) there seen, and the supression of second order relative to third is quite dramatic. we could spend a lot of time fully analyzing these images. When these higher energy tests are completed we will change out the DCM for the C-Ka source and begin again with the HRC-I in place. Dr. Stephen S. Murray - Sr. Astrophysicist Associate Director - High Energy Astrophysics Division _______________________________________*_______________________________________ Smithsonian Astrophysical Observatory__| phone: (617) 495-7205 High Energy Astrophysics Division __| fax: (617) 495-7356 60 Garden Street, MS-2 __| email: ssm@head-cfa.harvard.edu Cambridge, MA 02138 __| http://hea-www.harvard.edu/~ssm/HomePage.html ___________________________|___________________________________________________