The initial mass-remnant mass relation for core collapse supernovae

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Table C.1.

Results of the interpolation described in Sec. 2.3.

[Fe/H]	$M_{ZAMS}^{PPISN} (M_{⊙})$ $M_{\mathrm{ZAMS}}^{\mathrm{PPISN}} (\mathrm{M}_{\odot})$	$M_{preSN}^{PPISN} (M_{⊙})$ $M_{\mathrm{preSN}}^{\mathrm{PPISN}} (\mathrm{M}_{\odot})$	k₁	q₁(M_⊙)	k₂	q₂(M_⊙)
v = 0 km/s

0	N.A.	N.A.	N.A.	N.A.	N.A.	N.A.
-1	87.43	41.91	0.28	8.3	0.27	18.3
-2	87.66	83.27	0.53	-13.9	0.61	29.8
-3	87.01	87.01	0.48	-9.2	1.0	0.0

v = 300 km/s

0	N.A.	N.A.	N.A.	N.A.	N.A.	N.A.
-1	120.0	40.5	0.18	11.1	0.21	15.3
-2	65.19	39.89	0.39	7.9	0.48	8.6
-3	64.8	41.63	0.37	-0.6	0.37	8.7

Notes. Column 1: Metallicity, Column 2: M_ZAMS of the first progenitor undergoing PPISN, Column 3: Mass Pre-SN of the first progenitor undergoing PPISN. If the most massive progenitor of our grid is stable against PPISN, we cannot obtain such information. Thus, we labeled it as "Not Available" (NA), Column 4: Slope of Eq. 11, Column 5: Intercept of Eq. 11, Column 6: Slope of Eq. 12, Column 7: Intercept of Eq. 12.

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