Abstract
In this research the interpretation of Suzaku spectral observation of Fe kα emission line from Sigma Gem system was carried out. Sigma Gem was observed using Suzaku satellite with observation ID 402033010 at an exposure time of 142. 82 ks. Spectral analysis of all observations was performed using XSPEC version 12.8. We used version 2.00 of the standard Suzaku pipeline products and the HEA Soft version 6.16 for our analysis of data. We adopted a 250′′ radius to extract all events for the XIS detector to produce the source spectra, but we adjusted the 250′′ radius slightly where it overlaps with the calibration sources at the corners, to avoid capturing source background light. Modeling the spectrum using either power law or bremsstrahlung model with three Gaussian line for the 6.4 keV, He–like 6.7 keV, H–like 7.0 keV, Fe Kα emission lines shows that the 6.4 keV, 7.0 keV lines and absorption in both full and partial covering matter could not be measured in all the sources. We were able to resolve the three-narrow iron kα emission lines with different ionization states, which constraints the Sigma Gem emission models. The iron K- line complex was clearly resolved into three individual peaks at 6.41 keV, 6.7 keV and 7.0 keV. The light curve shows that the Sigma Gem was at a quiescent state at the point of observation and The light curve shows a considerable quiescent behavior of the source of the point of observation showing the source is not flaring.
Highlights
Iron K-alpha (Fe Kα) emission lines result when an electron transits to the innermost “K” shell from a 2p orbital of the second or “L” shell of atom releasing 6.4 keV of energy as florescence emission line photon [1]
The Fe Kα emission line is a veritable tool used for the study of the geometry, physics and kinematics of astrophysical sites
We obtained our data from the High Energy Astrophysics data archive research Centre Japan
Summary
Iron K-alpha (Fe Kα) emission lines result when an electron transits to the innermost “K” shell (principal quantum number 1) from a 2p orbital of the second or “L” shell (with principal quantum number 2) of atom releasing 6.4 keV of energy as florescence emission line photon [1]. The cold iron can produce a fluorescent line at 6.41 keV. It was observed firstly using the CCD detectors on the ASCA satellite, which gave 120-eV resolution [4,5,6,7,8]. An example of K-alpha lines is those seen for iron as iron atoms radiating Xrays spirall into a black hole at the center of a galaxy. For such purpose the energy, E of the line is adequately calculated to 2-digit accuracy by the use of Moseley’s law:
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