JWST/NIRSpec insights into the circumnuclear region of Arp 220: A detailed kinematic study

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Volume 693 (January 2025)

A&A, 693 (2025) A36

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Table 3.

Properties of the high-velocity molecular and ionized outflows.

General properties of the Nuclei

	E Nucleus		W Nucleus
SFR(radio/FIR)⁽¹⁾	60–80		110–150
SFR(Paα)⁽²⁾	0.17		0.52
$L_{AGN}^{IR} (3)$ ${L_{\mathrm{AGN}}^{\mathrm{IR}}}^{(3)}$ [erg s⁻¹]	1.1 × 10⁴⁴		2.5 × 10⁴⁴
$L_{AGN}^{X} (4)$ ${L_{\mathrm{AGN}}^{X}} ^{(4)}$ [erg s⁻¹]	8.3 × 10⁴³		2.5 × 10⁴³
Hot-to-cold⁽⁵⁾	3 × 10⁻⁴		10⁻⁴

General properties of the outflows

	SEO	HGO	NWB	WNO
R_out⁽⁶⁾ [kpc]	0.4	0.6	1	0.15
n_e⁽⁷⁾ [10³ cm⁻³]	< 17	3.8 $_{- 1.3}^{+ 2.2}$ $_{-1.3}^{+2.2}$	< 1.8	5 $_{- 2}^{+ 2.5}$ $_{-2}^{+2.5}$
v_out⁽⁸⁾ [km s⁻¹]	600 ± 150	400 ± 140	600 ± 180	400 ± 70
t_dyn⁽⁹⁾ [Myr]	0.65	1.5	1.7	0.42
A_v⁽¹⁰⁾ [mag]	8.9	4.5	3	8

Hot molecular gas

M_out⁽¹¹⁾ [10⁴ M_⊙]	0.07	0.2	0.1
Ṁ_out [M_⊙ yr⁻¹]	0.001	0.001	0.0006
E_out⁽¹²⁾ [10⁵² erg s⁻¹]	0.2	0.3	0.36
${\dot{E}}_{out}^{(13)}$ $\dot {E}_{\mathrm{out}}^{(13)}$ [10⁴⁰ erg s⁻¹]	0.009	0.006	0.007

Ionized gas, assuming [Fe II]-based n_e

M_out [10⁴ M_⊙]	0.5	4	6	9
Ṁ_out [M_⊙ yr⁻¹]	0.007	0.025	0.03	0.26
E_out [10⁵² erg]	1.7	6	18	16
Ė_out [10⁴⁰ erg s⁻¹]	0.08	0.12	0.3	1.4

Ionized gas, assuming [S II]-based n_e = 170 cm⁻³

M_out [10⁴ M_⊙]	50	90	60	270
Ṁ_out [M_⊙ yr⁻¹]	0.7	0.6	0.4	8
E_out [10⁵² erg]	170	130	190	460
Ė_out [10⁴⁰ erg s⁻¹]	8	2.7	4	40

Total (ionized, hot and cold molecular)

M_out [10⁴ M_⊙]	400	2090	560	270
Ṁ_out [M_⊙ yr⁻¹]	5.7	12	3.2	8
E_out [10⁵² erg]	1170	3570	1940	460
Ė_out [10⁴⁰ erg s⁻¹]	53	71	39	40
μ⁽¹⁴⁾	0.08	0.09	0.05	0.06
Ė_out/ $L_{AGN}^{IR}$ $L_{\mathrm{AGN}}^{\mathrm{IR}}$	5 × 10⁻³	3 × 10⁻³	4 × 10⁻³	2 × 10⁻³
Ė_out/L_AGN^X	6 × 10⁻³	0.03	5 × 10⁻³	0.02
Ė_out/ ${\dot{E}}_{SFR}^{radio / far - IR}$ $\dot{E}_{\mathrm{SFR}}^{\mathrm{radio/far-IR}}$	0.009	0.007	0.006	0.004

Notes. (1) and (2) SFR computed from radio/FIR by Varenius et al. (2016) and Pereira-Santaella et al. (2021), and from Paα by Perna et al. (2024), respectively. (3) AGN luminosity from IR. (4) AGN luminosity from X-rays by Paggi et al. (2017). (5) Hot-to-cold ratio. (6) Outflow radius. (7) [Fe II]-based electron density. (8) Outflow velocity, calculated as the flux-weighted average of the velocity (defined as in Eq. (6)) of each spaxel and the associated errors. (9) Dynamical time. (10) Average attenuation. (11) Outflow mass. (12) Outflow kinetic energy. (13) Outflow kinetic power. (14) Outflow mass loading factor. The AGN luminosity refers to the nucleus from which the outflow originates. The SEO and NWB are attributed to the E nucleus, while the HGO and WNO to the W nucleus.

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