Red-skewed Kα iron lines in GX 13+1 | Astronomy & Astrophysics (A&A)

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Table 2.

Comparison of the best-fit parameters of the iron emission line with the previous analysis performed by Díaz Trigo et al. (2012).

		Obs. 1 ^(a)			Obs. 2 ^(b)
		Emission line parameters			Emission line parameters

Line model	Total model	E (keV)	σ (keV)	EW (eV)	E (keV)	σ (keV)	EW (eV)	Reference
Gaussian	Model 1 ^(c)							(Díaz Trigo et al. 2012, Table 3)
Gaussian	Model 2 ^(d)		^(h)			^(h)		(Díaz Trigo et al. 2012, Table 4)
Gaussian	Model 1 ^(c)							The present paper
Gaussian	Model 3 ^(e)							The present paper
Diskline	Model 4 ^(f)		−			−		The present paper
Windline	Model 5 ^(g)	[6.6]	−		[6.6]	−		The present paper

Notes. Spectral uncertainties are given at at 90% (Δχ² = 2.71) confidence level for one derived parameter. Fixed parameters are shown in brackets.

^(a)

XMM-Newton/PN Obs. 1 (Obs. ID 0505480101), which corresponds to Obs. 4 in Díaz Trigo et al. (2012).

^(b)

XMM-Newton/PN Obs. 2 (Obs. ID 0505480201), which corresponds to Obs. 6 in Díaz Trigo et al. (2012).

^(c)

XSPEC Model: TBABS*EDGE₁ *EDGE₂ *(DISKBB+BBODYRAD+GAU₁ +GAU₂ +GAU₃ +GAU₄ +GAU₅ ); where GAU₁ corresponds to a gaussian model, and GAU_{(2, …, 5)} correspond to negative gaussians.

^(d)

XSPEC Model: TBABS*CABS*WARMABS*(DISKBB+BBRAD+GAU₁ ).

^(e)

XSPEC Model: TBABS*(BBODYRAD+COMPTT+GAUSSIAN)*lgabs₁*lgabs₂*lgabs₃.

^(f)

XSPEC Model: TBABS*(BBODYRAD+COMPTT+DISKLINE)*lgabs₁*lgabs₂*lgabs₃.

^(g)

XSPEC Model: TBABS*(BBODYRAD+COMPTT+WINDLINE)*lgabs₁*lgabs₂*lgabs₃.

^(h)

Parameter is pegged.

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