High Energy In Flight Calibration sources: Properties and Bibliography

This version is obviously just a beginning. Address suggestions for inclusions, deletions, re-organizations, etc. to keith_at_milkyway.gsfc.nasa.gov

White Dwarves

HZ 43, Sirius B
Notes. Soft (< 0.2 keV) non variable point sources

Isolated Neutron Stars
Notes. Faint, Non variable point sources. Emission below 1 keV

Crab Like Super Nova Remnants

Crab Pulsar and Nebula
Notes. Bright continuum source. 33 ms pulsar. Believed constant on longer time scales. Useful for absolute timing (0.1 msec level) when radio ephemeris is available

PSR 1821-24
Notes 3 millisecond pulsar with a sharp peak. This is probably the narrowest known X-ray peak, and thus potentially the most precise for timing cross calibrations.

PSR 1509-58

Thermal Super Nova Remnants
Notes provide line rich targets. Pointing and field of view are important considerations
Notes. Non variable line rich source. ~1 arc minute in extent



Keenan et al., "Soft X-Ray Emission Lines of Fe XV in Solar Flare Observations and the Chandra Spectrum of Capella", 2006, ApJ, 645, 597. Calculations comapred to "co-added spectrum of Capella obtained with the Chandra satellite, which is probably the highest signal-to-noise ratio observation achieved for a stellar source in the ~25-175 soft X-ray region."

AR Lac
Huenemoerder et al., "The Coronae of AR Lacertae", 2003, ApJ, 595, 1131

HR 1099
Osten et al., "A Multiwavelength Perspective of Flares on HR 1099: 4 Years of Coordinated Campaigns", 2004, ApJS, 153, 317

Brinkman et al., " First light measurements with the XMM-Newton reflection grating spectrometers: Evidence for an inverse first ionisation potential effect and anomalous Ne abundance in the Coronae of HR 1099", 2001, A&A, 365, 324


Notes. Point like continuum sources. Variable. Possible absorption features from IGM

PKS 2155-309
3C 273
Mkn 421

Clusters of Galaxies
Perseus Cluster

Abell 2199

Ophiucus Cluster

Cygnus Loop
Notes. Large, line rich source, potentially useful for monitoring contamination or setting energy scale. Size or remnant, and variation across remnant, imply that using this remnant requires attention to imaging and pointing capabilities

Miyata et al., "Detection of Highly-Ionized Carbon and Nitrogen Emission Lines from the Cygnus Loop Supernova Remnant with the Suzaku Observatory", 2007, PASJ, 59, 163

Leahy, "X-ray spectrum variations in the south-west Cygnus Loop", 2004, MNRAS, 351, 385 ( Chandra ACIS)