Deciphering the radio–star formation correlation on kpc scales - II. The integrated infrared–radio continuum and star formation–radio continuum correlations

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Volume 667 (November 2022)

A&A, 667 (2022) A30

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Table B.2.

Ultraluminous infrared galaxies.

Galaxy Name	v_max	l_flat^(b)^(f)	l_*	M_*	Ṁ_∗ ^(e)	log(L_TIR)^(d)	Q^(b)	Ṁ^(a)	M_gas^(a)
	(km s⁻¹)	(kpc)	(kpc)	(10¹⁰ M_⊙)	(M_⊙yr⁻¹)	L_⊙)		(M_⊙yr⁻¹)	(10⁹ M_⊙)
IRAS17208-0014	260	0.02	0.5	0.8	435	12.39	1.2	313.3	14.8
Mrk231	345	0.02	0.4	1.3	595	12.50	1.5	499.8	16.5
Arp220D	330	0.02	0.4	1.2	52	11.49	2.5	15.8	3.8
Mrk273	280	0.02	0.4	0.9	253	12.21	1.5	182.4	8.4
IRAS23365+3604	260	0.02	0.6	1.0	258	12.13	1.5	242.9	14.4
VIIZw31	290	0.02	1.1	2.2	164	12.00	1.5	28.0	13.7
Arp193	230	0.02	0.7	0.9	81	11.73	1.5	18.8	6.5
Arp220W	300	0.01	0.1	1.2	79	11.66	2.0	34.8	1.1
Arp220E	350	0.01	0.1	1.9	52	11.49	2.8	22.1	1.3

Notes.

^(a)

calculated quantities; the mean CO(1-0)–H₂ conversion factor is α_CO = 1.7 ± 0.4 M_⊙(K km s⁻¹ pc²)⁻¹ (Vollmer et al. 2017).

^(b)

assumed quantities; all other columns are input quantities from Downes & Solomon (1998).

^(c)

Arp220D, Arp220W, and Arp220E refer to the Disk, Western, and Eastern components, respectively.

^(d)

Garcia-Carpio et al. (2008)

^(e)

A conversion factor of Ṁ_∗/L_TIR = 1.7 × 10⁻¹⁰ M_⊙ yr⁻¹ was assumed

^(f)

A rotation curve of the form v_rot = v_max(1 − exp(−R/l_flat)) was assumed.

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