Predicting HCN, HCO, multi-transition CO, and dust emission of star-forming galaxies - From local spiral and ultraluminous infrared galaxies to high-z star-forming and submillimeter galaxies

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Volume 602 (June 2017)

A&A, 602 (2017) A51

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Table B.4

High-z star-forming disk galaxies.

Galaxy name	v _rot ^c	l _flat	l _∗	M _∗		L _TIR	^d	Q ^b	δ ^b	Ṁ ^a	M _gas ^a
	(km s^-1)	(kpc)	(kpc)	(10¹⁰M_⊙)	(M_⊙ yr^-1)	(10¹¹L_⊙)	(^c)			(M_⊙ yr^-1)	(10⁹M_⊙)

EGS12004280	230	0.10	4.7	4.1	100	10.0	7.9	1.5	5.0	30.5	47.5
EGS12004754	215	0.10	6.5	9.3	53	5.3	4.7	1.5	5.0	5.8	39.2
EGS12007881	232	0.10	5.7	5.2	94	9.4	8.5	1.5	5.0	23.5	53.8
EGS12015684	233	0.10	4.0	4.6	113	11.3	5.8	1.5	5.0	30.5	41.3
EGS12023832	215	0.10	4.7	5.9	115	11.5	3.8	1.5	5.0	36.8	47.4
EGS12024462	253	0.10	8.6	6.0	78	7.8	5.8	1.5	5.0	12.9	73.5
EGS12024866	221	0.10	4.6	2.5	31	3.1	3.7	1.5	5.0	4.0	24.5
EGS13003805	387	0.10	5.7	17.0	200	20.0	24.0	1.5	5.0	9.7	70.9
EGS13004661	171	0.10	5.0	3.0	60	6.0	3.7	1.5	5.0	36.3	39.4
EGS13004684	295	0.10	5.0	11.0	42	4.2	9.5	1.5	5.0	1.4	27.7
EGS13011148	260	0.10	5.2	11.0	52	5.2	5.2	1.5	5.0	2.9	31.3
EGS13011155	296	0.10	7.8	12.0	201	20.1	13.0	1.5	5.0	35.2	106.5
EGS13011166	363	0.10	6.5	12.0	373	37.3	29.0	1.5	5.0	69.0	133.0
EGS13017614	346	0.10	4.5	13.0	88	8.8	13.0	1.5	5.0	2.9	36.0
EGS13017707	324	0.10	3.6	7.4	351	35.1	11.0	1.5	5.0	93.0	72.2
EGS13017843	227	0.10	4.2	4.0	35	3.5	6.3	1.5	5.0	3.3	22.2
EGS13017973	155	0.10	7.2	4.4	55	5.5	3.7	1.5	5.0	36.6	52.0
EGS13018632	319	0.10	1.9	5.2	82	8.2	3.9	1.5	5.0	3.9	15.1
EGS13019114	327	0.10	7.2	6.6	47	4.7	6.1	1.5	5.0	1.9	45.9
EGS13019128	194	0.10	5.2	4.4	87	8.7	4.9	1.5	5.0	39.6	48.1
EGS13026117	436	0.10	3.2	13.0	113	11.3	16.0	1.5	5.0	2.3	29.9
EGS13033624	301	0.10	5.3	8.9	148	14.8	10.0	1.5	5.0	17.0	59.6
EGS13033731	350	0.10	5.5	2.8	28	2.8	4.6	1.5	5.0	0.8	29.2
EGS13034339	299	0.10	3.0	6.6	86	8.6	6.0	1.5	5.0	5.4	24.4
EGS13034541	330	0.10	8.0	9.3	183	18.3	9.1	1.5	5.0	24.2	107.8
EGS13034542	195	0.10	4.0	5.2	61	6.1	1.8	1.5	5.0	11.9	26.7
EGS13035123	219	0.10	11.2	15.0	87	8.7	10.0	1.5	5.0	14.8	89.3
EGS13042293	167	0.10	5.2	3.9	55	5.5	3.0	1.5	5.0	24.2	36.0
zC406690	224	0.10	6.3	4.0	480	48.0	9.4	1.1	5.0	304.8	158.1
Q1623BX599	376	0.10	1.7	5.7	131	13.1	5.7	1.5	5.0	5.6	17.5
Q1700BX691	260	0.10	3.9	7.6	50	5.0	4.7	1.5	5.0	2.9	23.3
Q2343BX610	402	0.10	4.6	10.0	212	21.2	26.0	1.5	5.0	12.7	63.2
Q2343BX442	309	0.10	4.3	12.0	145	14.5	7.0	1.5	5.0	10.5	44.1
Q2343MD59	371	0.10	2.8	7.6	26	2.6	62.0	1.5	5.0	0.3	13.2
Q2346BX482se	285	0.10	2.4	0.6	34	3.4	9.2	1.5	5.0	3.9	15.8
BzK4171	261	0.10	4.5	4.0	101	10.1	19.0	1.5	5.0	20.2	45.4
BzK210000	292	0.10	4.7	7.8	231	23.1	20.0	1.5	5.0	54.3	72.2
BzK16000	258	0.10	4.0	4.3	82	8.2	14.0	1.5	5.0	11.9	34.4
BzK17999	238	0.10	4.7	3.9	450	45.0	15.0	1.2	5.0	351.0	122.8
BzK12591	361	0.10	4.5	11.0	267	26.7	29.0	1.5	5.0	26.7	69.4
BzK25536	254	0.10	3.0	3.3	62	6.2	10.0	1.5	5.0	7.4	22.2
J2135-0102	381	0.10	1.5	1.7	230	23.0	12.0	1.5	5.0	46.0	27.8

Notes.

^(a)

Calculated quantities;

^(b)

assumed quantities; all other columns are input quantities from Tacconi et al. (2013);

^(c)

if the assumed rotation velocity is ;

^(d)

in 10⁹ K km s^-1 pc².

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