Disc wind or disc line? The extraordinary Fe-K feature of Mrk 1513

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Table 1.

Log of the 2003 (ObsID 0150470701) and 2015 (ObsID 0744370201) XMM-Newton observations of Mrk 1513.

Date	Exposure ^(a) (s)			Counts ^(b) (5−10 keV)			Flux ^(c) (0.3−10 keV)
	pn	MOS1	MOS2	pn	MOS1	MOS2	(10⁻¹¹ erg s⁻¹ cm⁻²)
2003 May 16	24 267	29 764	36 920	2478 ± 52	685 ± 28	857 ± 30	0.656 ± 0.004
2015 May 1	25 599	31 236	31 220	688 ± 28	622 ± 25	657 ± 26	1.086 ± 0.007

Notes.

^(a)

Net exposure after dead-time correction and filtering of high-background periods.

^(b)

Net counts in the hard X-ray band; we note that the major shortcoming with the 2015 pn data.

^(c)

Observed flux (not corrected for Galactic absorption) computed through a phenomenological spectral model. The difference is mostly due to the intensity of the soft X-ray emission below ∼3 keV.

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