Chemical templates of the Central Molecular Zone - Shock and protostellar object signatures under Galactic Center conditions

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Table 2

Parameter space covered with UCLCHEM models.

	Parameter	Unit	Values	Notes
Stage 1: Collapse	n_{H, final}^(a)	cm⁻³	10⁴, 10⁵, 10⁶, 10⁷, 10⁸	n_{H, init} = 10² cm⁻³
	T_{init (gas, dust)}	K	15, 20, 25, 30, 35	...
	ζ/ζ₀	−	10¹, 10², 10³, 10⁴	ζ₀ = 1.31 × 10⁻¹⁷ s⁻¹
	G₀	Habing	10¹, 10², 10³, 10⁴	...
	A_{V, start}	mag	2	...
	X(Si)^(b)	−	1.78 × 10⁻⁸, 1.78 × 10⁻⁶^†	^†X(Si)_⊙ (Jenkins 2009)
	$R_{final}^{(c)}$ $\[R_{\text {final}}^{(c)}\]$	pc	0.5	...

Stage 2: Protostellar Objects	n_H^(a)	cm⁻³	10⁶, 10⁷, 10⁸	...
	G₀	Habing	10³, 10⁴	...
	T_{final (gas,dust)}	K	100, 150, 200, 250, 300, 350, 400, 450, 500	...
	M	M_⊙	10, 25	...

Stage 2: Shocks	n_{H, pre–shock}^(a)	cm⁻³	10⁴, 10⁵, 10⁶	...
	G₀	Habing	10¹, 10², 10³, 10⁴	...
	v_s	km s⁻¹	10, 15, 20, 25, 30, 35, 40	...
	$B_{0}^{(d)}$ $\[B_{0}^{(d)}\]$	μG	140, 450, 1400	$B_{0} = b m_{0} \sqrt{n_{H}}$ $\[B_{0}=b m_{0} \sqrt{n_{\mathrm{H}}}\]$

Notes. ^(a) Proton density, n_H, is defined as n(H) + 2n(H₂). ^(b) The models of protostellar objects utilize collapse models with depleted Si abundance with respect to the Solar abundance (e.g., Savage & Sembach 1996), while the shock models rely on those with the standard value of 1.78 × 10⁻⁶ (Jenkins 2009). ^(c) For consistency across models, we adopted a single radius. However, to evaluate the full impact of R_final on the chemistry of protostellar objects, we conducted an additional test with R_final = 0.05 pc (see Sect. 2.2.3). The results of this test suggest that our protostellar object models are also applicable to smaller objects, with R ≳ 0.05 pc. ^(d) Values of B₀ were not varied, as they depend on pre-shock densities. This work adopts bm₀ of 1.4 (Jiménez-Serra et al. 2008). The dagger signify the standard value and it’s origin.

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