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

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Table 1

Log of NuSTAR observations used in this work and some adopted parameters.

Source	ObsID	Start	Stop	Exposure	min S/N	Count rate^(a)	Flux	P_spin

		UT	UTC	ks		3–70 keV	10⁻⁹erg cm⁻² s⁻¹	s
4U 1626-67	30101029002	2015-05-04 12:26:07	2015-05-05 20:41:07	65.0	10	15.62	1.22	7.672951 ± 0.000016
Her X-1	30002006005	2012-09-22 04:26:07	2012-09-22 18:36:07	21.9	16	96.84	8.22	1.2377185 ± 0.0000010
Cen X-3	30101055002	2015-11-30 18:11:08	2015-12-01 05:01:08	21.4	16	63.24	4.35	4.802581 ± 0.000003^(b)
Cep X-4	80002016002	2014-06-18 22:01:07	2014-06-19 20:11:07	40.4	10	41.99	2.82	66.3357 ± 0.0017

Notes. The flux is the observed value in the 3–70 keV band. ^(a)The FPMA count rate in the 3–70 keV energy range. ^(b)The period derivative is ṗ = (3.71 ± 0.15) × 10⁻⁹ ss⁻¹.

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