The g-band liming magnitudes of this simulated survey are:
Filter | Magnitude |
---|---|
i | 23.3 |
r | 23.3 |
z | 21.7 |
g | 23.3 |
A total of 200 PISNe where simulated in the survey, out to a redshift of 1.0. A constant galactic extinction of E(B-V) = 0.023
is used (the mean extinction of the 10 PS1 Medimum Deep Fields). The MDFs are visible for a fraction of 0.5 of the survey year and the typical fraction of survey time lost to weather of 0.4 is accounted for. Here are the relative rates and peak magnitude distributions of the SN used in the survey:
SN Type | Relative Rate | Peak Magnitude | Sigma Peak |
---|---|---|---|
SN2007bi | 0.5 | –17.08 | 0.001 |
SLSN | 0.5 | –20.21 | 0.001 |
If a PISN is detected by the simulated survey, extra constraints are placed upon the detected object to secure positive identification as a PISN.
The PISN rate for the survey volume is estimated by assuming a rate of 10e–5 times that of the CCSN rate (itself a fraction of 0.007 of the total SFR).
This simulated survey discovered a total of 1 PISNe per year. An extra 5 PISNe were detected but deemed too faint to constrain a positive PISN identification and a further 1 PISNe where detected but an observational campaign of more than 100 days could not be completed to ensure identification. See below for the various output plots.