Supplementary Data for:

"Core-Collapse Supernovae from 9 to 120 Solar Masses Based on Neutrino-powered Explosions"

by Sukhbold, T., Ertl, T., Woosley, S., Brown, J., and Janka, H.-T. (2015, submitted to ApJ on 15 Oct).

doi:10.17617/1.b

- Detailed descriptions of calculations and models are provided in the paper, but please feel free to get in touch with any of us with questions.
- Please consider letting us know about your projects if you use our data
- Contact us, if you need something that is not provided here or if you have ideas on a potential collaboration

Contacts:

Tuguldur	Sukhbold	tuguldur.sgmail.com
Thomas	Ertl	tertlmpa-garching.mpg.de
Stan	Woosley	woosleyucolick.org
Justin	Brown	jumbrownucsc.edu
Thomas	Janka	thjmpa-garching.mpg.de

What follows are just brief, practical descriptions, for more details please see the paper: [arXiv.1510.04643]

Results as shown in Figure 7 and 8 (supplemented by the remaining calibrations) (294 KB)
Individual files: Z9.6+S19.8(txt, pdf); Z9.6+W15 (txt, pdf); Z9.6+W18 (txt, pdf); Z9.6+W20 (txt, pdf); Z9.6+N20 (txt, pdf)

Note: In the txt-version of the figures, "M_b,remnant" is the baryonic mass including fallback (which corresponds to the height of the orange bar of panel 4). In case of failed shock revival we list the baryonic He-core mass and the total mass at the onset of collapse, "M_He_core" and "M_total_precollapse", respectively. Be aware that whenever a value reaches the maximum value of the y-axis in the pdf-version, the value might be larger than that. You can find the exact value in the txt-version.

Progenitor Models (47 MB)
Progenitor properties: after the stellar evolution calculation (txt), at a central density of 5x10¹⁰ g/ccm (txt), at core bounce (txt).

These are the 200 progenitor models from 9 to 120 solar masses. Note that the mass increments are variable. Different pieces are taken directly or are based on models from previous studies:

WH15	9-13	=	based on Woosley & Heger (2015)	[arXiv:1505.06712]
SW14	13.1-14.9	=	based on Sukhbold & Woosley (2014)	[arXiv:1311.6546]
SW14	15-30	=	from Sukhbold & Woosley (2014)	[arXiv:1311.6546]
WH07	>30	=	from Woosley & Heger (2007)	[arXiv:astro-ph/0702176]

All models are calculated by the KEPLER code. Across different studies the code changes, but we assure that the changes are minimal for the above. In the paper we have presented several 'extra' models to demonstrate the agreement, especially between WH15 and SW14 models (Section 2). Those are not provided here, but feel free to request them if you are interested.

All explosion results (PHOTB) (19 KB)
Individual files: Z9.6 (txt); S19.8 (txt); W15 (txt); W18 (txt); W20 (txt); N20 (txt)

These are the outcomes after we process above 200 progenitors by the means of the following 'neutrino engines':

	9-12	=	processed by Z9.6 only
	>12	=	processed by W20, W15, W18, N20, S19.8

Here Z9.6 is calibrated to SN1054 (Crab) and the rest are calibrated to SN1987A. These results are similar to those published in Ertl et al. (2015) [arXiv:1503.0752], but they are *NOT* identical, especially for lower mass models. See Section 3 and 4 for the differences. When the star implodes, the explosion energy is 0.0 and other entries are empty. The fallback supernovae are noted by the large values of M_fallback and low values of M_outside(Ni) in the "With Fallback:" section. The "special trajectory:" and "With fallback:" section info are what we have used as lower and upper limits respectively, when we post-process the models using KEPLER.

Nucleosynthesis Yields (41 MB)

-	Z9.6, W18 and N20 engine results were post-processed with KEPLER to obtain these. The tables consist of two parts: 1) top segment lists ejecta and wind contributions for all stable isotopes. 2) bottom segment lists select 20 radioactive isotopes: c14, na22, al26, si32, cl36, ar39, k40, ca41, ca45, ti44, v49, mn53, mn54, fe55, fe60, co60, ni56, ni57, ni59, ni63 Most of these are picked on the basis that they have half-lives longer than ~ 1 year and are important to the light curve. Note that the top segment varies in size, and so the tables for different models are not necessarily of the same size. Please get in touch with us if you're interested in isotopes that are not listed in the bottom segment.
-	The imploded models contribute through their winds at least, and so these files list wind contributions for all implosions of the W18 engine. The Z9.6 engine did not have any implosions (everything exploded) and since the W18 engine is weaker than N20, these listed implosions include all of the imploded models from N20.
-	There are also full zonal yield information for four sample models, 200 seconds after the explosion (before any artificial mixing).

Light Curves (344 KB)

All explosion models based on Z9.6, W18 and N20 were post-processed with KEPLER until about 2.e7 seconds (~231 days) since the explosion, to obtain approximate bolometric luminosities. These tables are 'trimmed' versions, as the original calculation had many more points near the shock break-out and near the transition between plateau and nebular phases. Please get in touch with us if you are interested in those 'high resolution' tables.