Energy-resolved pulse profiles of accreting pulsars: Diagnostic tools for spectral features

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Table 5

Best-fit parameters of the Cep X-4 Obs ID 80002016002 pulse and amplitude models compared to spectral results (Fürst et al. 2015).

	PF	1^st	Spectral
	1.4/15	0.8/8	–
	1.5/35	1.3/39	–
	3	6	–
	3	3	–
E_split	13.35	11.18	–	keV
A_Fe	−0.0308 ± 0.0019	(−8 ± 2) ×10⁻³	(1.39 ± 0.16) × 10⁻³
E_Fe	6.444 ± 0.019	6.62 ± 0.04	6.47 ± 0.03	keV
σ_Fe	0.46 ± 0.02	0.33 ± 0.05	0.42 ± 0.05	keV
A_Cyc	−4.1 ± 0.7	−2.08 ± 0.12
E_Cyc	31.00± 0.18	30.32 ± 0.10		keV
σ_Cyc	5.3 ± 0.3	3.75 ± 0.12	5.8 ± 0.4	keV

Notes. and are the reduced χ² for the lower- and higher-energy sections, respectively, with and the corresponding polynomial orders. E_split is the energy at which we separate the two regions.

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