Evolution of the atomic component in protostellar outflows

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Volume 650 (June 2021)

A&A, 650 (2021) A173

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Table 5.

Mass-loss rates of the observed targets.

Obj.	Region	θ	v_t			& component	Ṁ_acc^(e)
		(″)	(km s⁻¹)	(10⁻⁷ M_⊙ yr⁻¹)	(10⁻⁷ M_⊙ yr⁻¹)	(10⁻⁷ M_⊙ yr⁻¹)	(10⁻⁷ M_⊙ yr⁻¹)
Cep E	knot A	25	95 ^(a)	≲22.4−45.5	≲124.4−136.7	∼200 ^(j) & CO	170 ^(f)
	jet	35	60 ^(a)	≲7.2−14.7	≲87.5−99.0

HH 1	VLA 1	50	300 ^(b)	≲25.9−52.6	≲54.9−57.8	∼6 ^(k) & [Fe II]	290 ^(g)
	knot A	20	400 ^(b)	≲9.5−19.4	≲5.2−7.2	∼4 ^(k) & [S II]
						∼0.1 ^(k) & H₂
						∼15 ^(l) & CO

HH 212	knots A and B	30	150 ^(c)	3.9(−)7.9	8.0(−011.8	∼10 ^(m) & CO, SO, SiO	80 ^(h)
						≤3 ⁽ⁿ⁾ & CO, SiO
						∼1 ^(o) & H₂

L1551	IRS 5	25	120 ^(d)	5.8−11.8	4.9−5.4	≳100 ^(p) & CO, HCO⁺, swept-up gas	30 ⁽ⁱ⁾
						∼8.6 ^(q) & HI
						∼1.7 ^(r) & [Fe II]
						∼0.4 ^(r) & H₂

Notes. Column 5: Derived from jet geometry (i.e. Eq. (2)). Column 6: Derived from the Hollenbach & McKee (1989) shock model, that is Eq. (3). Column 7: Mass-loss rates from the literature that are connected to other outflow components, meaning they are traced by species other than [O I] as indicated. Mass accretion rates in Col. 8 are calculated from Eq. (4) unless stated otherwise.

^(a)

Proper motions from Noriega-Crespo et al. (2014).

^(b)

Proper motions from Bally et al. (2002).

^(c)

Proper motions from Noriega-Crespo et al. (2020).

^(d)

Proper motions from Fridlund & Liseau (1994).

^(e)

Calculated from their bolometric luminosities (see Sect. 4.4).

^(f)

Our estimate (see Sect. 4.4). From SED modeling, Velusamy et al. (2011) estimated a surprisingly high accretion rate for Cep E-mm of the order of 10⁻⁴ M_⊙ yr⁻¹.

^(g)

The stated value is in good agreement with Fischer et al. (2010). Therein, the source of the HH 1-2 outflow is labelled HOPS 203.

^(h)

The stated value is in good agreement with Lee et al. (2014).

⁽ⁱ⁾

The stated value is in good agreement with, for example, Osorio et al. (2003), Liseau et al. (2005), and Gramajo et al. (2007).

^(j)

Lefloch et al. (2015): This material is directly connected to the Cep E jet and not to swept-up gas.

^(k)

Nisini et al. (2005).

^(l)

From CO J = 1–0 observations undertaken by Tanabe et al. (2019), it is unclear if it is entrained material or not.

^(m)

Lee et al. (2007a), Podio et al. (2015), Lee et al. (2015), Lee (2020).

⁽ⁿ⁾

Cabrit et al. (2012).

^(o)

Davis et al. (2000).

^(p)

Hogerheijde et al. (1998), Fridlund et al. (2002), Yıldız et al. (2015).

^(q)

Giovanardi et al. (2000).

^(r)

Davis et al. (2003).

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