Star formation in M 33: the radial and local relations with the gas

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Table 3:

Pearson coefficients (r) and slopes (n) derived from the ``relative errors'' method for correlations between the two quantities shown in the first column.
	r	n	n₁
$\log \Sigma_{\rm SFR} - \log \Sigma_{\rm H_2}$	0.42	$2.22\pm 0.07$	1.46 $\pm$ 0.34
$\log \Sigma_{\rm SFR} - \log \Sigma_{\rm H_I}$	0.24	$1.62\pm 0.03$	1.11 $\pm$ 0.15
$\log \Sigma_{\rm SFR} - \log \Sigma_{\rm H_{tot}}$	0.43	$2.59\pm 0.05$	1.67 $\pm$ 0.25
$\log \Sigma_{\rm SFR} - \log \left(\Sigma_{\rm H_2}/\rho^{-0.5}_{\rm ISM}\right)$	0.62	$1.16\pm 0.04$	1.00 $\pm$ 0.01
$\log \Sigma_{\rm SFR} - \log \rho_{\rm ISM}$	0.71	$1.07\pm 0.02$	0.97 $\pm$ 0.01
$\log \Sigma_{\rm SFR} - \log \tau_{160}$	0.81	$1.13\pm 0.02$	1.01 $\pm$ 0.02

Notes. The SFR per unit area, $\Sigma _{\rm SFR}$ , is traced by the FUV emission corrected for extinction. Only positions where the CO luminosity is above the 2 $\sigma$ limit have been considered at a spatial resolution of 180 pc. The surface density of molecular, atomic and total gas are $\Sigma_{\rm H_2}$ , $\Sigma_{\rm H_I}$ and $\Sigma_{\rm H_{tot}}$ respectively. $\rho$ is the volume density of the ISM and $\tau_{160}$ the dust opacity. n₁ is the OLS slope as described in the text.

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