| 42 | | |
| 43 | | == Reference versus Deep Stack == |
| 44 | | A requirements description for the needs in the different types of stacks would be useful to summarize. |
| 45 | | |
| 46 | | Reference stacks -- primarily for difference imaging for transient detection and necessary for magic destreaking. |
| 47 | | * Magic destreaking: a fairly clean reference stack (uses the convolved stack) with as much spatial area coverage as possible to enable release of non-stack data products. Particularly important is inclusion of older data on different pointings and of course a fairly balanced dither set. |
| 48 | | * Transient detection: a balance slanted towards best PSF but with some depth (1-1.5 magnitudes over nightly stacks) and also a fairly balanced dither set. |
| 49 | | |
| 50 | | Deep stacks -- for deep static sky science. |
| 51 | | * As deep as possible.. maximum FWHM allowance? minimum exposure time? specific request for at least ~10ks has been requested, with best FWHM possible and also a fairly balanced dither set.. |
| 52 | | |
| 53 | | See summary for each MD field reference stack for details on specifics for that field. Due to processing+time constraints/early mistakes, an attempt has been made to merge the similar criteria under the ''refstack'' label. |
| 54 | | |
| 55 | | Since magic destreaking uses the convolved stack, looking into a quickstack version of the unconvolved stacks for the transients reference and deep stack that will be faster to make with more inputs. |
| 56 | | |
| 57 | | For cases when a stack does not have a good sample of exposures with a reasonably small PSF FWHM, it should be possible to generate a reference stack with the fewer 'best' exposures for just SSdiffs and transient detection. MD02-g may be such a case. |
| 58 | | |
| 59 | | For fields with shifted centers from offset earlier exposures, inclusion of enough exposures to provide a reference stack for magic is necessary in order for data from those associated chips/skycells to be distributed (being older data, may not have the optimum quality). Mixing older and newer data may also be a detriment. |
| 60 | | |
| 61 | | Related to deep stacks, there needs to be enough inputs to obtain minimum depth that is as pixel contiguous as possible (see MD04 deep stack tests). |
| 62 | | |
| 63 | | How much of a varying IQ can go into a stack before ppSub has difficulty modeling the variations within a skycell? |
| 64 | | |
| 65 | | Deep stacks on hold until finish investigating overly large PSF in the convolved stacks dependent on the number of input warps. |
| 66 | | |
| 67 | | |
| 85 | | Difference Images: |
| | 59 | == Reference versus Deep Stack == |
| | 60 | A requirements description for the needs in the different types of stacks would be useful to summarize. |
| | 61 | |
| | 62 | Reference stacks -- primarily for difference imaging for transient detection and necessary for magic destreaking. |
| | 63 | * Magic destreaking: a fairly clean reference stack (uses the convolved stack) with as much spatial area coverage as possible to enable release of non-stack data products. Particularly important is inclusion of older data on different pointings and of course a fairly balanced dither set. |
| | 64 | * Transient detection: a balance slanted towards best PSF but with some depth (1-1.5 magnitudes over nightly stacks) and also a fairly balanced dither set. |
| | 65 | |
| | 66 | Deep stacks -- for deep static sky science. |
| | 67 | * As deep as possible.. maximum FWHM allowance? minimum exposure time? specific request for at least ~10ks has been requested, with best FWHM possible and also a fairly balanced dither set.. |
| | 68 | |
| | 69 | See summary for each MD field reference stack for details on specifics for that field. Due to processing+time constraints/early mistakes, an attempt has been made to merge the similar criteria under the ''refstack'' label. |
| | 70 | |
| | 71 | Since magic destreaking uses the convolved stack, looking into a quickstack version of the unconvolved stacks for the transients reference and deep stack that will be faster to make with more inputs. |
| | 72 | |
| | 73 | For cases when a stack does not have a good sample of exposures with a reasonably small PSF FWHM, it should be possible to generate a reference stack with the fewer 'best' exposures for just SSdiffs and transient detection. MD02-g may be such a case. |
| | 74 | |
| | 75 | For fields with shifted centers from offset earlier exposures, inclusion of enough exposures to provide a reference stack for magic is necessary in order for data from those associated chips/skycells to be distributed (being older data, may not have the optimum quality). Mixing older and newer data may also be a detriment. |
| | 76 | |
| | 77 | Related to deep stacks, there needs to be enough inputs to obtain minimum depth that is as pixel contiguous as possible (see MD04 deep stack tests). |
| | 78 | |
| | 79 | How much of a varying IQ can go into a stack before ppSub has difficulty modeling the variations within a skycell? |
| | 80 | |
| | 81 | Deep stacks on hold until finish investigating overly large PSF in the convolved stacks dependent on the number of input warps. |
| | 82 | |
| | 83 | |
| | 84 | |
| | 85 | = Difference Images = |
