Gravitationally bound gas determines star formation in the Galaxy

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Volume 701 (September 2025)

A&A, 701 (2025) A152

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Table 1

Basic information for nearby star-forming clouds.

Clouds	Distance (pc)	$M_{A_{V} > 8}^{2 M A S S}$ $\[M_{\mathrm{A}_{\mathrm{V}}>8}^{2 \mathrm{MASS}}\]$ (M_⊙)	$M_{A_{V} > 8}^{Herschel}$ $\[M_{\mathrm{A_V}>8}^{\text {Herschel}}\]$ (M_⊙)	M_sgb (M_⊙)	SFR (10⁻⁶ M_⊙ yr⁻¹)	N_threshold (cm⁻²)
Aquila	278±13	16 034±2405	4993±749	$6434_{- 2573}^{+ 1286}$ $\[6434_{-2573}^{+1286}\]$	322.3±9.0	${6.69}_{- 0.04}^{+ 0.10}$ $\[6.69_{-0.04}^{+0.10}\]$ × 10²¹
California	454±22	3199±480	629±94	$6153_{- 1251}^{+ 1259}$ $\[6153_{-1251}^{+1259}\]$	70.0±4.2	${1.84}_{- 0.10}^{+ 0.07}$ $\[1.84_{-0.10}^{+0.07}\]$ × 10²¹
Cepheus I	336±16	6±1	209±31	$715_{- 71}^{+ 99}$ $\[715_{-71}^{+99}\]$	8.5±1.5	${1.35}_{- 0.05}^{+ 0.06}$ $\[1.35_{-0.05}^{+0.06}\]$ × 10²¹
Cepheus II	337±16	12±2	41±6	$86_{- 14}^{+ 10}$ $\[86_{-14}^{+10}\]$	0.0	${2.79}_{- 0.04}^{+ 0.23}$ $\[2.79_{-0.04}^{+0.23}\]$ × 10²¹
Cepheus III	341±17	41±6	42±7	$319_{- 16}^{+ 48}$ $\[319_{-16}^{+48}\]$	10.5±1.6	1.6 × 10²¹
Cepheus IV	359±17	0	50±8	$4_{- 1}^{+ 1}$ $\[4_{-1}^{+1}\]$	0.5±0.4	${17.47}_{- 2.83}^{+ 5.67}$ $\[17.47_{-2.83}^{+5.67}\]$ × 10²¹
Cepheus V	364±18	31±5	82±12	$1047_{- 185}^{+ 244}$ $\[1047_{-185}^{+244}\]$	4.8±1.1	${0.97}_{- 0.05}^{+ 0.04}$ $\[0.97_{-0.05}^{+0.04}\]$ × 10²¹
Cham I	210±14	176±26	263±39	$477_{- 47}^{+ 52}$ $\[477_{-47}^{+52}\]$	20.5±2.3	${2.94}_{- 0.03}^{+ 0.03}$ $\[2.94_{-0.03}^{+0.03}\]$ × 10²¹
Cham II	190±13	64±10	17±3	$344_{- 24}^{+ 52}$ $\[344_{-24}^{+52}\]$	6.0±1.1	3.2 × 10²¹
Cham III	161±11	0	12±2	$3_{- 1}^{+ 1}$ $\[3_{-1}^{+1}\]$	1.0±0.5	${10.80}_{- 1.61}^{+ 1.05}$ $\[10.80_{-1.61}^{+1.05}\]$ × 10²¹
Lupus I	151±10	75±8	19±3	245⁺³⁷	3.3±0.9	1.1 × 10²¹
Lupus III	197±13	163±24	24±4	$212_{- 51}^{+ 51}$ $\[212_{-51}^{+51}\]$	17.0±2.1	${1.61}_{- 0.04}^{+ 0.04}$ $\[1.61_{-0.04}^{+0.04}\]$ × 10²¹
Lupus IV	151±10	124±19	19±3	$453_{- 104}^{+ 133}$ $\[453_{-104}^{+133}\]$	3.0±0.9	${0.75}_{- 0.01}^{+ 0.01}$ $\[0.75_{-0.01}^{+0.01}\]$ × 10²¹
Musca	160±13	0	4±1	$253_{- 41}^{+ 44}$ $\[253_{-41}^{+44}\]$	3.0±0.9	${1.58}_{- 0.02}^{+ 0.02}$ $\[1.58_{-0.02}^{+0.02}\]$ × 10²¹
Ophiuchus	128±6	1209±181	466±70	$963_{- 201}^{+ 352}$ $\[963_{-201}^{+352}\]$	72.8±4.3	${3.25}_{- 0.07}^{+ 0.05}$ $\[3.25_{-0.07}^{+0.05}\]$ × 10²¹
Orion A	399±19	13721±2058	10205±1531	$26579_{- 9134}^{+ 4781}$ $\[26579_{-9134}^{+4781}\]$	715.5±13.4	${2.05}_{- 0.16}^{+ 1.95}$ $\[2.05_{-0.16}^{+1.95}\]$ × 10²¹
Orion B	415±22	7261±1074	3488±523	$8617_{- 602}^{+ 690}$ $\[8617_{-602}^{+690}\]$	158.8±6.3	${2.95}_{- 0.14}^{+ 0.14}$ $\[2.95_{-0.14}^{+0.14}\]$ × 10²¹
Perseus	256±12	1880±240	986±148	$4754_{- 991}^{+ 1178}$ $\[4754_{-991}^{+1178}\]$	149.5±6.1	${1.50}_{- 0.01}^{+ 0.01}$ $\[1.50_{-0.01}^{+0.01}\]$ × 10²¹
Pipe	180±9	178±27	30±5	$122_{- 24}^{+ 42}$ $\[122_{-24}^{+42}\]$	5.3±1.2	${4.18}_{- 0.01}^{+ 0.01}$ $\[4.18_{-0.01}^{+0.01}\]$ × 10²¹
Serpens	425±21	4213±632	1056±158	$4482_{- 1514}^{+ 2007}$ $\[4482_{-1514}^{+2007}\]$	56.0±3.7	${3.21}_{- 0.30}^{+ 0.26}$ $\[3.21_{-0.30}^{+0.26}\]$ × 10²¹
Taurus	156±7	1766±265	402±60	$3250_{- 652}^{+ 652}$ $\[3250_{-652}^{+652}\]$	83.8±4.6	${1.62}_{- 0.02}^{+ 0.02}$ $\[1.62_{-0.02}^{+0.02}\]$ × 10²¹

Notes. The masses derived from A_V extinction and star formation rates are from the following references: Lada et al. (2010) and Evans et al. (2014). The distance is from Zucker et al. (2020). $M_{A_{V} > 8}^{2 M A S S}$ $\[M_{\mathrm{A}_{\mathrm{V}}>8}^{2 \mathrm{MASS}}\]$ is the dense gas mass within the extinction contour of A_V = 8 mag, which is from Lada et al. (2010) and Evans et al. (2014); $M_{A_{V} > 8}^{Herschel}$ $\[M_{\mathrm{A_V}>8}^{\text {Herschel}}\]$ is the dense gas mass above N(H₂) = 7.4×10²¹ cm⁻² from Herschel column density maps. N_threshold is the threshold column density of the turning position between lognormal and power-law distribution in N-PDF, and the corresponding errors are from N-PDF fitting. M_sgb is the gas mass above N_threshold.

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