Extended Data Table 1 Gaussian fit parameters

From: An early transition to magnetic supercriticality in star formation

  1. *Ipeak is the intrinsic peak Stokes I emission. We do not fit Ipeak for the HINSA because it is an absorption component.
  2. †τ is the central opacity. We do not fit τ for the WNM because it is a background component.
  3. ‡vLSR is the central LSR velocity.
  4. §σv is the Gaussian dispersion.
  5. ‖The order of the component along the line of sight. Order begins with 0, and increasing numbers mean increasing distance along the line of sight. We fix order to 0 for the HINSA as the Taurus cloud is one of the closest cloud to us. The orders of the other components are free parameters in the fitting.
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