SN Survey Simulation Results - 20130919t134637

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.

  1. The peak apparent magnitude of the object must be brighter than 21.5 mag
  2. The object must be detectable for long enough to complete a follow-up campaign of longer than 100 days within 1 survey year with any single filter.

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).

Results

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.

Cadence_Wheel_for_Simulated_Survey_plot
Cadence_Wheel_for_Simulated_Survey_plot
PISNe_Detected_Within_the_Suvrey_Year_plot
PISNe_Detected_Within_the_Suvrey_Year_plot
Redshift_Map_of_PISNe_Simulated_within_the_Survey_Volume_plot
Redshift_Map_of_PISNe_Simulated_within_the_Survey_Volume_plot
PS1_PISN_Survey___Relative_Detected_Rates_plot
PS1_PISN_Survey___Relative_Detected_Rates_plot