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The H II Regions’ Molecular Law of Star Formation

  • Authors: Daniela Calzetti, Drew Lapeer, Robert C. Kennicutt, Bruce Elmegreen, Sean T. Linden, Mark R. Krumholz, Angela Adamo, Daniel A. Dale, Karin Sandstrom, Giacomo Bortolini, Michele Cignoni, Matteo Correnti, Ana Duarte-Cabral, Helena Faustino Vieira, John S. Gallagher, Kathryn Grasha, Mark Heyer, Leslie K. Hunt, Kelsey E. Johnson, Ralf S. Klessen, Thomas S.-Y. Lai, Desika Narayanan, Göran Östlin, Alex Pedrini, Elena Sabbi, John-David T. Smith, Linda J. Smith, Monica Tosi, Varun Bajaj, Martha Boyer, Tony D. Weinbeck

Daniela Calzetti et al 2026 The Astrophysical Journal 1008 .

  • Provider: AAS Journals

Caption: Figure 6.

The efficiency per freefall time, ϵff, for the regions in our sample as a function of ΣSFR (top left), Σmol (top right), the gas velocity dispersion σv (bottom left), and the gas peak temperature Tpeak (bottom right). The areas excluded by the limits Log(ΣSFR) ≥ −1.8 and Log(Σmol) ≥ 0.5 are marked as black lines with gray shaded regions. The horizontal dark-red line shows the location of constant ϵff = 0.01. The purple shaded areas in the two top panels show the 1σ range of possible slopes returned by a forward modeling approach to the data distribution (see the text). For the ϵff–versus–ΣSFR plot, the best-fit line (blue solid) and its scatter (shaded blue) from the LINMIX algorithm are also shown.

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