Probing the photoionised outflow in the NLS1 Arakelian 564: An XMM-Newton view

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Table B.1

Best fit for individual spectra from 2000−2011 as discussed in Sect. 4.2.

Param

# 01

# 02

# 03

# 04

# 05

# 06

# 07

# 08

# 09

# 10

# 11

# 12

# 13

Log ξ^a (Phase 1)

−0.23 ± 0.13

−0.16 ± 0.10

−0.24 ± 0.20

−0.13

−0.25 ± 0.07

−0.16 ± 0.10

−0.10 ± 0.09

−0.18 ± 0.09

−0.26 ± 0.08

−0.35 ± 0.09

−0.50 ± 0.15

−0.34 ± 0.12

−0.25 ± 0.10

Log ξ^a (Phase 2)

1.56 ± 0.10

1.73 ± 0.13

1.71 ± 0.65

0.55 ± 0.29

1.25 ± 0.07

1.21 ± 0.09

1.41 ± 0.10

1.36 ± 0.09

1.34 ± 0.07

1.24 ± 0.10

1.07 ± 0.13

0.95 ± 0.12

1.50 ± 0.10

Log ξ^a (Phase 3)

2.07 ± 0.12

2.41 ± 0.20

1.99 ± 0.20

2.36 ± 0.15

2.41 ± 0.08

2.43 ± 0.08

2.12 ± 0.07

2.29 ± 0.08

2.22 ± 0.11

1.95 ± 0.06

1.85 ± 0.05

2.60 ± 0.10

2.35 ± 0.10

O VII (f)^b

0.3

2.4 ± 0.6

1.1 ± 0.9

0.8 ± 0.6

0.9 ± 0.3

0.6 ± 0.4

1.3 ± 0.4

0.4 ± 0.3

7.7 ± 0.3

1.0 ± 0.4

1.0 ± 0.3

1.1 ± 0.4

0.9 ± 0.4

Ne IX (f)^b

0.8 ± 0.3

0.3 ± 0.2

0.8 ± 0.4

0.6 ± 0.2

0.3 ± 0.1

0.4 ± 0.2

0.5 ± 0.1

0.2 ± 0.1

0.3 ± 0.1

0.4 ± 0.1

0.3 ± 0.2

0.2 ± 0.2

N VII Lyα^b

0.3

1.6 ± 1.1

3.6 ± 1.7

2.8 ± 1.4

2.4 ± 0.4

2.6 ± 0.6

2.3 ± 0.5

2.4 ± 0.5

2.8 ± 0.5

2.2 ± 0.5

2.9 ± 0.7

2.9 ± 7.4

3.5 ± 0.9

N VI (i)^b

0.2

2.6 ± 0.8

1.7 ± 1.1

1.5 ± 0.8

1.3 ± 0.4

1.2 ± 0.6

1.1 ± 0.5

1.4 ± 0.5

1.2 ± 0.5

0.8 ± 0.5

0.9 ± 0.4

0.9 ± 0.5

1.3 ± 0.6

O VIII Lyα^b

1.8 ± 0.7

2.8 ± 0.7

1.7 ± 1.0

2.7 ± 0.7

1.4 ± 0.3

1.3 ± 0.4

1.7 ± 0.3

1.8 ± 0.3

2.1 ± 0.3

2.0 ± 0.3

1.5 ± 0.3

1.3 ± 0.4

2.1 ± 0.4

C VI Lyα^b

2.2 ± 1.7

0^+1.3

0^+1.5

2.2 ± 2.2

0.4

0.1^+1.0

2.7 ± 1.1

1.9 ± 1.1

43.0

1.3 ± 1.1

1.2 ± 1.2

1.1 ± 1.1

3.1 ± 1.5

O laor^c

12 ± 5

10 ± 4

20 ± 6

2 ⁺³

3 ± 2

2 ⁺³

8 ± 2

7 ± 2

6 ± 2

1 ⁺²

5 ± 2

8 ± 2

12 ± 3

N laor^c

1 ± 1

0⁺¹⁶

35 ± 21

15 ± 15

12 ± 6

18 ± 9

10 ± 8

14 ± 8

20 ± 8

8 ± 8

12 ± 8

36 ± 10

Notes. All spectra are fitted with χ²/ d.o.f. ~ 1.2.

^(a)

Ionisation parameter in 10^-9 Wm.

^(b)

Non-relativistic emission normalisation in 10⁵⁰ ph s^-1.

^(c)

Broad relativistic line normalisation in 10⁵⁰ ph s^-1.

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