Hiccup accretion in the swinging pulsar IGR J18245–2452

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Volume 567 (July 2014)

A&A, 567 (2014) A77

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Table 5

Parameters of the best-fit models to the HR-resolved spectra of the magenta using the nthComp plus black-body.

Hardness^a

<0.25

0.25–0.33

0.33–0.43

0.43–0.70

>0.70^b

>0.70^c

N _H

23 ± 7

20 ± 7

16 ± 4

11 ± 8

× 10²⁰ cm^-2

k T _BB

0.40 ± 0.02

0.46

0.43

0.75

0.010

–

keV

R _BB

2.5 ± 0.3

2.4

2.8

0.86

–

N _H,pc

–

1.6

× 10²² cm^-2

F _pc

–

0.64 ± 0.08

1.71 ± 0.12

1.40 ± 0.05

1.35 ± 0.04

1.12

1.13

0.90 ± 0.04

k T _nthComp

0.19

0.22 ± 0.14

0.4

<0.1

0.90 ± 0.08

–

keV

N _nthComp,PL ^d

2.7 ± 0.8

5.8

6.8

7.1

1.40

4.0

× 10^-3

C2_P ^e

0.98 ± 0.02

0.949 ± 0.015

0.902 ± 0.009

0.64 ± 0.01

1.26 ± 0.03

C1_R ^e

0.87 ± 0.07

0.94 ± 0.07

0.858 ± 0.035

0.84 ± 0.07

0.88 ± 0.12

0.90 ± 0.13

C2_R ^e

0.83 ± 0.04

0.81 ± 0.03

0.58 ± 0.04

1.05 ± 0.12

1.07 ± 0.12

Flux^f

2.06 ± 0.04

6.26 ± 0.07

9.75 ± 0.10

7.10 ± 0.10

8.62 ± 0.14

8.67 ± 0.14

× 10^-11 erg s^-1 cm^-2

/d.o.f.

1.053/386

1.100/494

1.034/589

1.042/390

1.161/333

1.167/334

Notes. We also show the results obtained by adopting a partially covering power-law model for the spectrum extracted at HR > 0.7.

^(a)

HR values as computed in Fig. 1.

^(b)

The additional model is the disk black-body. Temperature and radius of the black-body are relative to its inner boundary. The radius is expressed modulo , where i is the inclination of the system with respect to the line of sight.

^(c)

Partial covering power-law model.

^(d)

Normalization of the nthComp or power-law component for HR < 0.7 or HR > 0.7.

^(e)

Cross-calibration constants: C1 and C2 refer to obs1 and obs2. P and R indicate the EPIC-pn and RGS.

^(f)

The absorbed flux is computed from the EPIC-pn spectrum in the 0.5–11 keV range of obs2. Uncertainties are only statistical.

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