H2 formation and excitation in the Stephan's Quintet galaxy-wide collision

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Volume 502 / No 2 (August I 2009)

A&A, 502 2 (2009) 515-528

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Table 2:

Overview of the emission of the SQ postshock gas, from observations and model predictions^a. The models are the same as those used in Fig. 5.
					F LUX OF S PECTRAL F EATURES (10^-18 W m^-2)
	Mass Flow	$P/k_{\rm B}$	$V_{\rm s}$ ^b	Cooling Time^c	O I [ $63~\mu$ m]	$\rm H_2$ rot.^d	$\rm H_2$ 1-0 S(1)	O I 6300 Å^e	$\rm H_{\alpha}$ ^e
	[ $M_{\odot}$ yr^-1]	[K cm^-3]	[km s^-1]	[yr]	O I [ $63~\mu$ m]	$\rm H_2$ rot.^d	$\rm H_2$ 1-0 S(1)	O I 6300 Å^e	$\rm H_{\alpha}$ ^e
Observations						$55 \pm 3$		3.6	5.3
Isobaric Cooling	100 (WIM, H $_\alpha$ )^f	$2 \times 10^5$		$1.2 \times 10^4$	3.9	1.4	0.05	0.5	5.3
Isobaric Cooling	640 (WNM, O I)^g	$2 \times 10^5$		$1.5 \times 10^5$	25.8	9.1	0.3	3.6
Shock Models	$5.7 \times 10^3$	$4.5 \times 10^7$	5	$1.8 \times 10^4$	13	27	0.3	10^-5
Shock Models	270	$5.6 \times 10^8$	20	$3.7 \times 10^3$	0.04	25	0.01	$5 \times 10^{-3}$

^a All line fluxes are scaled to the aperture ${\cal A} = 11.3$ $\times$ 4.7 arcsec². For isobaric cooling calculations, the pressure is set to the SQ postshock gas value. For MHD shock models, both contributions of the 2 shock velocities to the emission are indicated, as well as the pressure for the warm $\rm H_2$ phase in the shock.
^b MHD Shock velocity.
^c Cooling time computed down to 50 K.
^d Sum of the $\rm H_2$ S(0) to S(5) rotational lines (from Appleton et al. 2006).
^e From optical observations by Xu et al. (2003).
^f Mass flow derived from H $~ \alpha$ observations, ignoring ionization. It represents the isobaric cooling of the recombining H II gas.
^g Cooling mass flow derived from O I observations and model calculations at the ambient SQ pressure. This mass flow does not depend much on the pressure since the critical density of the O I line is high (2 $\times$ 10⁶ cm^-3).

Source LaTeX | All tables | In the text

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