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Parmentier & Pasquali (2020)

San Diego State University

The big idea

Two clouds with the same dense-gas mass MdgM_\mathrm{dg} can form stars at different rates if their density gradients differ: a centrally-concentrated clump has more of its mass at high density, where the local free-fall time τff∝ρ−1/2\tau_\mathrm{ff}\propto\rho^{-1/2} is short, so it forms stars faster than a uniform (“top-hat”) clump of the same mass. PP20 capture this geometric boost with a single magnification factor ζ\zeta, so that

SFRdgMdg=ζ ϵff,int⟨τff,dg⟩(their Eq. 7).\frac{\mathrm{SFR}_\mathrm{dg}}{M_\mathrm{dg}} = \zeta\,\frac{\epsilon_\mathrm{ff,int}}{\langle\tau_\mathrm{ff,dg}\rangle} \qquad\text{(their Eq. 7).}

ζ=1\zeta=1 is the top-hat lower limit; ζ>1\zeta>1 for any centrally-concentrated profile.

Physical & observational context (Sections 1–3)

The dense-gas star-formation law — NYSO∝MdgN_\mathrm{YSO}\propto M_\mathrm{dg}, equivalently SFR∝Mdg\mathrm{SFR}\propto M_\mathrm{dg} — is observationally near-linear (Lada et al. 2010 find NYSO=0.18 MdgN_\mathrm{YSO}=0.18\,M_\mathrm{dg}) but carries real scatter. PP20’s thesis is that the scatter is not purely random: it partly tracks the cloud’s internal density gradient. Steeper gradients (larger pp) push more mass into the short-free-fall-time inner region, raising SFR/Mdg\mathrm{SFR}/M_\mathrm{dg}. The two key inputs PP20 separate (their Eq. 2) are the intrinsic efficiency per free-fall time ϵff,int\epsilon_\mathrm{ff,int} (a true SF-physics number) and the purely geometric boost ζ\zeta — so that measuring a cloud’s gradient unlocks its ζ\zeta and lets one read ϵff,int\epsilon_\mathrm{ff,int} cleanly from the data.

The radial slope pp is inferred observationally from the cloud ρ\rho-pdf or projected Σ\Sigma-pdf: for a power-law tail of index nn in the Σ\Sigma-pdf, p=1+2/np = 1 + 2/n (Kritsuk et al. 2011); p≡κp\equiv\kappa in the Kainulainen et al. (2014) notation. The Kainulainen sample has a mean p≈1.67p \approx 1.67 (range 1<p<2.21<p<2.2), which is the canonical observational anchor: ζ(1.67)≈1.79\zeta(1.67)\approx1.79. PP20 also apply the framework to the Central Molecular Zone (CMZ), whose clouds sit ~10× below the nearby-cloud locus in (p, SFR/Mdg)(p,\,\mathrm{SFR}/M_\mathrm{dg}).

Core equations

Why ζ\zeta has this form. The dense-gas SFR is the mass-weighted free-fall rate, ∝⟨ρ1/2⟩mass\propto\langle\rho^{1/2}\rangle_\mathrm{mass}, while the “naive” rate uses the mean density, ∝⟨ρ⟩1/2\propto\langle\rho\rangle^{1/2}. Hence

ζ=⟨ρ1/2⟩mass⟨ρ⟩1/2=∫ρ3/2 dV  (∫dV)1/2(∫ρ dV)3/2.\zeta = \frac{\langle\rho^{1/2}\rangle_\mathrm{mass}}{\langle\rho\rangle^{1/2}} = \frac{\int \rho^{3/2}\,dV\;(\int dV)^{1/2}}{(\int \rho\,dV)^{3/2}} .

Closed form for a power-law sphere ρ∝r−p\rho\propto r^{-p} (Eq. 6, in Eq. 9). Performing the integrals over the sphere gives

ζ(p)=(3−p)3/233/22 (2−p)=(3−p)3/22.6 (2−p),0≤p<2.\zeta(p) = \frac{(3-p)^{3/2}}{\tfrac{3^{3/2}}{2}\,(2-p)} = \frac{(3-p)^{3/2}}{2.6\,(2-p)} , \qquad 0 \le p < 2 .

PP20 print the constant as the rounded 2.6; the exact value is 33/2/2=2.5983^{3/2}/2 = 2.598, fixed by the physical top-hat limit ζ(0)=1\zeta(0)=1. The factor (2−p)(2-p) in the denominator means ζ\zeta diverges only as p→2p\to2 — there is no pole at p=1.3p=1.3 (a previously caught transcription fabrication). Spot values:

pp011.51.67
ζ(p)\zeta(p)1 (exact)1.0892=1.414\sqrt2 = 1.414 (exact)1.79

Forbidden regions (their Fig. 1). Equation (6) is the upper limit on ζ\zeta (pure power law), and ζ=1\zeta=1 is the lower limit (top-hat); real cored profiles lie between. For p≥2p\ge2 a pure power law would drive the central density — and the SFR — to infinity, so PP20 add a flat inner core: a cored profile ρ(r)=ρc[1+(r/rc)2]−p/2\rho(r)=\rho_c[1+(r/r_c)^2]^{-p/2} has a finite ζ\zeta even for p≥2p\ge2, obtained by numerically integrating the ratio above over r/R∈[0,1]r/R\in[0,1]. The core damps the boost: a relative core size rc/rclump>0.1r_c/r_\mathrm{clump}>0.1 already reduces ζ\zeta significantly (their Fig. 1), because it shrinks the centre-to-edge density contrast.

Link to BM19. The PDF slope α\alpha (Burkhart & Mocz) and the radial slope pp are the same quantity: p=κ=3/αp = \kappa = 3/\alpha. So α∈[1.5,3]⇔p∈[1,2]\alpha\in[1.5,3]\Leftrightarrow p\in[1,2].

Use in progenax

Validation: anchors ζ(0)=1, ζ(1)=1.089, ζ(1.5)=2, ζ(1.67)=1.79\zeta(0)=1,\ \zeta(1)=1.089,\ \zeta(1.5)=\sqrt2,\ \zeta(1.67)=1.79 to <0.1%<0.1\% (AC3); the direct field estimator matches the analytic ζ(p)\zeta(p) to ∼3%\sim3\% on a sampled power law (AC4).

Notes

References
  1. Parmentier, G., & Pasquali, A. (2020). A new parameterization of the star formation rate–dense gas mass relation: Embracing gas density gradients. The Astrophysical Journal, 903, 56. 10.3847/1538-4357/abb8d3