How many stars form in compact clusters in the local Milky Way?

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Volume 701 (September 2025)

A&A, 701 (2025) L2

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Table 1.

Surface density star formation rates (∑_SFR, OC) derived from the completeness-corrected mass function of compact OCs from HR24.

Parameter	Value	Units
∑_SFR, OC (power law)	$791_{- 191}^{+ 162}$ $791^{+162}_{-191}$	M_⊙ Myr⁻¹ kpc⁻²
∑_{SFR, OC, CST ≥ 5} (power law)	$736_{- 176}^{+ 159}$ $736^{+159}_{-176}$	M_⊙ Myr⁻¹ kpc⁻²
∑_SFR, OC/∑_SFR	$86_{- 24}^{+ 14}$ $86^{+14}_{-24}$ %
∑_{SFR, OC, CST ≥ 5}/∑_SFR	$80_{- 22}^{+ 17}$ $80^{+17}_{-22}$ %

∑_SFR, OC (cluster count)	$875_{- 35}^{+ 34}$ $875^{+34}_{-35}$	M_⊙ Myr⁻¹ kpc⁻²
∑_{SFR, OC, CST ≥ 5} (cluster count)	$846_{- 35}^{+ 34}$ $846^{+34}_{-35}$	M_⊙ Myr⁻¹ kpc⁻²
∑_SFR, OC/∑_SFR	$95_{- 14}^{+ 4}$ $95^{+4}_{-14}$ %
∑_{SFR, OC, CST ≥ 5}/∑_SFR	$92_{- 14}^{+ 4}$ $92^{+4}_{-14}$ %

Notes. The first value corresponds to the ∑_SFR, OC derived from the power-law fit of the mass function (Section 2.1), whereas the second value stands for the ∑_SFR, OC derived through a cluster count for OCs within 1 kpc (Section 2.2). For each value, we have also displayed the ratio compared with the ∑_SFR of $922_{- 1}^{+ 133}$ $922^{+133}_{-1}$ M_⊙ Myr⁻¹ kpc⁻² from Q25.

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