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GBM Accreting Pulsar Histories
For each source we plot the history of pulse frequency and pulsed
flux measured
using the Fermi Gamma-Ray Burst Monitor (GBM) NaI detectors.
For these measurements we use the CTIME data which normally has 0.256
s time bins,
and eight energy channels. Our analysis normally uses channels 1
(12-25 keV) and
2 (25-55 keV).
The integration intervals used varys from source to source, ranging
from one to
four days. For elipsing systems each egress to ingress interval is
divide into
an integral number of equal parts, with no measurement made during
the eclipse.
The measured frequencies are barycentered. For sources where the
binary orbit is known the
frequencies are corrected for the binary motion.
The R.M.S. pulsed flux is given in the energy band that the pulse
search was made. This
usually includes only the first and second harmonics.
These results are preliminary. Please contact
Mark Finger
for further information.
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