Evolution of the atomic component in protostellar outflows

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Table 1.

Target information.

Source	Class	Cloud	RA (J2000) ^(a)	Dec (J2000) ^(a)	D^(b)	L_bol^(c)	PA ^(h)
			(h m s)	(° ′ ″)	(pc)	(L_⊙)	(°)
IRAS 23011+6126 (Cep E)	0 ^(g)	Cepheus, OB3	23 03 12.8	+61 42 26	730	∼75 ^(d)	25
VLA 1 (HH 1)	0 ^(f)	Orion A, L1641	05 36 22.8	−06 46 06	430	∼46 ^(d)	145
IRAS 05413-0104 (HH 212)	0 ^(g)	Orion B, L1630	05 43 51.4	−01 02 53	420	∼13 ^(d)	30
L1551 IRS 5	I ^(g)	Taurus, L1551	04 31 34.2	+18 08 05	140	∼23 ^(e)	75

Notes.

^(a)

Taken from the Two Micron All Sky Survey (2MASS).

^(b)

Rounded from Zucker et al. (2019) based on Gaia DR2, except Cep E taken from Kun et al. (2008).

^(c)

We corrected the luminosities taken from the cited papers for our assumed distances: .

^(d)

van Dishoeck et al. (2011).

^(e)

Karska et al. (2018).

^(f)

AMI Consortium et al. (2012), Chini et al. (2001).

^(g)

Froebrich (2005).

^(h)

Position angle of the outflow.

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