Äîêóìåíò âçÿò èç êýøà ïîèñêîâîé ìàøèíû. Àäðåñ îðèãèíàëüíîãî äîêóìåíòà : http://hea-www.harvard.edu/ChandraSNR/G011.2-00.3/fit_detail.cgi
Äàòà èçìåíåíèÿ: Unknown
Äàòà èíäåêñèðîâàíèÿ: Tue Oct 2 03:51:26 2012
Êîäèðîâêà:
Ïîèñêîâûå ñëîâà: magnitude

Chandra Images for G011.2-00.3

Chandra SNR

True Color Image Gallery: Galactic SNR | Magellanic Cloud SNR

Fit Detail for G011.2-00.3

Total:

Two thermal plasma model and power law
Elemental abundace of O, Ne, Mg, Fe were thawed.
Derived nH is much higher than Vasisht et al.(1996) (1.38, 2.19).
Fitting the central source with power law gives nH=1.7, see below.

source=(xswabs * ((xsvapec + xsvapec) + powlaw1d))
reduce chi^2 =
nh = 3.1445 10^22/cm^2
PARAMETERS

DataSet 1: 384 data points -- 373 degrees of freedom.

Statistic value = 2083.66
Probability [Q-value] = 0
Reduced statistic = 5.58621

--end--

Central Source:

central source was fitted with power law.
Flux was NOT derived from this fit result!

source=(xswabs * powlaw1d)
reduce chi^2 =
nh = 1.6675 10^22/cm^2
PARAMETERS

DataSet 2: 55 data points -- 52 degrees of freedom.

Statistic value = 45.7392
Probability [Q-value] = 0.717133
Reduced statistic = 0.879599

--end--

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