Transient obscuration event captured in NGC 3227 - II. Warm absorbers and obscuration events in archival XMM-Newton and NuSTAR observations

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Volume 657 (January 2022)

A&A, 657 (2022) A77

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Table 4.

Estimated distances (r) of the four WAs (WA₁, WA₂, WA₃, and WA₄) of NGC 3227.

Parameter	WA₁	WA₂	WA₃	WA₄
Method 1 ^(*): Distance r ≥ thickness Δr
Ṗ_abs (10³³ erg m⁻¹) ^(a)	1.68	1.44	1.54	51.3
Ṗ_scat (10³² erg m⁻¹) ^(b)	9.6	1.1	0.5	0.7
C_v^(c)	0.049	0.039	0.011	0.006
r (pc) ^(d)	≲0.007	≲0.24	≲0.71	≲265

Method 2 ^(†): Outflow velocity v_out ≥ escape velocity v_esc
r (pc) ^(e)	≳0.03	≳0.2	≳0.3	≳4

Method 3 ^(‡): Recombination timescale method
⟨n_et_rec⟩ (10¹⁰ s cm⁻³)	5.6	5.4	3.9	7.2
t_rec (days) ^(f)	≲16	≲10	≲6	≲6
⟨n_e⟩ (10¹⁰ cm⁻³) ^(g)	≳4.0	≳6.3	≳7.5	≳14.0
r (pc) ^(h)	≲0.16	≲0.3	≲0.6	≲13

Notes.

^(*)

First method for estimating the distances of the WAs, based on the assumption that the thickness (Δr) of the WA cloud does not exceed its distance (r) (see Eqs. (2)–(5)).

^(a)

Momentum outflow rate from the radiation being absorbed.

^(b)

Momentum outflow rate from the radiation being scattered.

^(c)

Volume filling factor.

^(d)

The distances of the WAs that are estimated by the first method.

^(†)

The second method to estimate the distances of the WAs, which is based on the assumption that the outflow velocities of winds (v_out) are larger than or equal to their escape velocities (v_esc) (see Eq. (6)).

^(e)

Distances of the WAs that are estimated by the second method.

^(‡)

Third method to estimate the distances of the WAs, which is based on the recombination timescale (see Eq. (7)).

^(f)

Recombination time scale.

^(g)

Electron number density.

^(h)

Distances of the WAs that are estimated by the third method.

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