Mapping the neutral atomic hydrogen gas outflow in the restarted radio galaxy 3C 236

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Table 3.

Properties of the kinematically disturbed HI clouds.

Component^a	^b 10¹⁹ cm ⁻² K⁻¹	N_HI^c (10¹⁹ cm⁻²)	d^d (pc)	n_HI^e (cm⁻³)	m_HI^f (10⁴M_⊙)	υ^g (km s⁻¹)	r_⋆^h (pc)	Ṁ_HIⁱ (M_⊙ yr⁻¹)
S4	0.18	18	≲36	30	0.65	640	≲40	1.2
S3	0.40	40	≲36	60	1.5	420	≲40	1.7
S2a	0.33	33	≲36	50	1.2	150	≲40	0.5
Nucleus	0.78	78	≲36	120	2.8	640	≲40	5
S2b	0.18	1.8	56 × 15	2	0.28	150	310	0.2

Notes.

^(a)

Label of the kinematic component (see Fig. 4). The values for “Nucleus” were obtained after integrating over S2a, S3, and S4.

^(b)

H I column density normalised by spin temperature.

^(c)

H I column density. For S4, S3, and S2a, T_spin = 1000 K is assumed, while for S2b T_spin = 100 K is assumed.

^(d)

Projected size of the components. For S2a, S3, and S4, a spherical geometry is assumed with an upper limit of the diameter based on the synthesized beam. For S2b, an ellipsoidal geometry is assumed, with the major and minor axis given.

^(e)

Density of the H I clouds. The same T_spin values as for the column density are assumed here.

^(f)

Mass of the H I clouds for the chosen T_spin values.

^(g)

Peak velocity of the H I clouds relative to the peak velocity of S1.

^(h)

Deprojected distance of the H I clouds relative to the nucleus.

⁽ⁱ⁾

Mass outflow rate following Heckman (2002) for the chosen T_spin values.

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