Line Spread Function of CHANDRA HETG: application

Details Line Spread Function of CHANDRA HETG: application Line Spread Function of CHANDRA HETG: application

Mar 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003head....7.2211i&link_type=abstract

American Astronomical Society, HEAD meeting #7, #22.11; Bulletin of the American Astronomical Society, Vol. 35, p.641

Astronomy and Astrophysics

Astronomy

Scientific paper

Instrumental spectral line profile of CHANDRA HETG instrument is known to be skewed. Hence a simple Gaussian function as a fitting kernel is not an appropriate action for line profile analysis. In the worst case, it may mislead observers to think that observed spectral lines are naturally skewed. In order to minimize such blunders, CHANDRA HETG users are recommended to make their own response matrix functions (RMFs) based on a set of parameterized line spread functions (LSFPARMS) provided with CHANDRA CALDB (version 2.17 or higher), and then to use their RMFs to define a line fitting kernel in their favorite fitting tools.
This presentation will provide descriptions on the current state of calibration for LSFPARMS of CHANDRA HETG instrument. And this work will also illustrate the use of the LSFPARMS (or RMF) products by analyzing real spectral lines of stellar X-ray sources.

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