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Figure 1:
[OIII]
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Figure 2: Comparing our Pettini & Pagel (2004) empirically calibrated oxygen abundances with those directly measured by Izotov et al. (2006) via measuring the electron temperature reveals that our measurements are reliable with an rms scatter of 0.14 dex, the solid line depicting a one-to-one correspondence. Note the four outlying galaxies - see text for details. |
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Figure 3:
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Figure 4: Cumulative distribution of the combined CCSN rate from our HSFG and LSFG catalogues, measured against oxygen abundance. It is clear that as oxygen abundance increases so to does the rate of CCSNe. |
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Figure 5: Template lightcurves used within the Monte-Carlo simulation. Lightcurves for SNe of type IIP are according to 1999em, type IIL to 1998S, type Ib/c to 2002ap, type IIn/P to 1994Y and type IIn/L to 1999el. Note that allmagnitudes are in the AB system. |
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Figure 6: Percentage of CCSNe detected from our MCSs for a differing number of hours observing per night (labeled to the right of the plot). The percentage of CCSNe detected increases as the nightly observing time increases, as this increases the cadence of observations. As the individual exposure time per galaxies increases, the limiting magnitude of the search deepens but the cadence of observations decreases. There is therefore an optimal point at which the exposure time and cadence of observation are balanced to detect the maximum percentage of SNe. |
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Figure 7: Cumulative distribution of 1500 extinctions as measured through the fraction of the Galactic Plane which lies within the Pan-STARRS survey area. |
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Figure 8:
The galaxy distribution for the SDSS DR5 spectroscopic
survey galaxy sample. The solid curve represents the absolute magnitude
limit as a function of redshift given that the SDSS DR5 apparent magnitude
limit for the sample is r=17.77. An absolute magnitude limit of
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Figure 9: A schematic depicting the cadence of observation for any given point in the sky, taken from the Pan-STARRS observation strategy (Chambers & Denneau 2007). One Pan-STARRS year of 12 lunar months, approximately 352 days, is represented by a circle. With each observation epoch a double exposure is taken in order to identify Near Earth Objects. |
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Figure 10:
A third order polynomial is fitted to each set of K correction data,
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Figure 11:
The solid lines show CCSN detection distributions for PS1,
PS4 and LSST, the dashed lines the absolute magnitude limits of the surveys
as a function of redshift. At a absolute limiting magnitude of
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Figure 12: Of the 12 SNe discovered by the Nearby Supernova Factory that were hosted by SFGs in the SDSS DR5 catalogue, 5 were hosted by galaxies with 12 + log(O/H) < 8.4. The host shown are SDSS J140737.23+384047 (SN 2007fg), SDSS J160205.11+294338 (SN 2007fz), SDSS J135042.68 + 400208 (SNF20080324-010), SDSS J154404.32+275335 (SNF20080515-004) and SDSS J150031.40+552210 (SNF20080614-002). |
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