Energetic feedback and 26Al from massive stars and their supernovae in the Carina region

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Table 3

Best-fit IMF of open clusters in our study.

Cluster	IMF (>15 M_⊙)	IMF (>25 M_⊙)	Mass range	No. of stars	Supernovae	Total No. (>15 M_⊙)
	Γ¹	Γ¹

Bochum 10	–	–	15–32	5	2.34	7.34
Bochum 11		–	15–120	6	0	6
Loden 153	–	–	15–45	2	0.43	2.43
NGC 3293	–	–	15–22	23	20.5	53.5
NGC 3324		–	15–120	3	0	3
Trumpler 14		–	15–120	13	0	13
Trumpler 15	–	–	15–40	11	3.08	14.08
Trumpler 16		1.3	15–120	54	0	54
All young²			15–120	76	0	76
All³			–	–	26.35	153.35

Notes. The upper limits on the mass ranges were estimated by the age of the host clusters. The number of stars inside the mass ranges were extrapolated using the Salpeter IMF to find the number of supernovae and the total number of initial stars.

⁽¹⁾

Slope of a single power-law fit.

⁽²⁾

Clusters young enough that no supernova explosions are believed to have occurred.

⁽³⁾

Clusters with maximum stellar masses ≥40 M_⊙ fitted in the 15–40 M_⊙ range.

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