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.3.

Submillimeter galaxies.

Galaxy Name	v_max	l_flat^(b)^(d)	l_*	M_*^(c)	Ṁ_∗ ^(e)	log(L_TIR^(f))	Ṁ^(a)	M_gas^(a)
	(km s⁻¹)	(kpc)	(kpc)	(10¹⁰ M_⊙)	(M_⊙ yr⁻¹)	(L_⊙)	(M_⊙ yr⁻¹)	(10⁹ M_⊙)
SMM J02399-013	590	0.10	3.5	10.0	2294	13.1;–;13.4;13.0;–	1927.0	318.5
SMM J09431+470	295	0.10	0.9	10.0	1746	12.9;–;13.0;–;–	1117.4	39.1
SMM J105141+57	457	0.10	2.1	10.0	1296	12.8;–;–;–;13.1	423.4	98.2
SMM J123549+62	442	0.10	0.6	24.0	1794	13.0;–;–;–;–	71.8	17.1
SMM J123634+62	343	0.10	2.8	10.0	930	12.7;–;–;12.7;–	737.8	117.0
SMM J123707+62	317	0.10	1.9	24.0	1016	12.7;–;–;12.8;–	135.5	45.6
SMM J131201+42	430	0.10	2.1	10.0	1340	12.8;12.9;–;–;–	589.6	99.5
SMM J131232+42	346	0.10	1.4	10.0	1016	12.7;–;–;–;–	257.4	41.5
SMM J163650+40	523	0.10	1.6	46.0	1772	12.9;12.7;–;–;–	59.1	50.8
SMM J163658+41	590	0.10	0.5	52.0	2248	13.1;12.9;–;–;–	28.5	16.0

Notes.

^(a)

calculated quantities; the mean CO(1-0)–H₂ conversion factor is α_CO = 1.4 ± 0.7 M_⊙(K km s⁻¹ pc²)⁻¹ (Vollmer et al. 2017).

^(b)

assumed quantities; all other columns are input quantities from Genzel et al. (2010).

^(c)

we assumed M_* = 10¹¹ M_⊙ for galaxies whose mass is not given in Genzel et al. (2010).

^(d)

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

^(e)

Twice the SFRs from Genzel et al. (2010) who used Ṁ_∗/L_TIR = 1.0 × 10⁻¹⁰ M_⊙ yr⁻¹.

^(f)

Genzel et al. (2010), Kovács et al. (2006), Valiante et al. (2009), Magnelli et al. (2012), and Chapman et al. (2010).

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