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Known Issues in ODs 1304 & 1305 | ||||||||
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Details on how to run the task are available in the SPIRE Data Reduction Guide, Section 6.8 | ||||||||
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> > | Be aware that for small size SPIRE maps, smaller than ~30 arcmin, the zero-offset can be rather uncertain, due to the large Planck beam (8 arcmin). In such cases the interpretation of the zero offset as the absolute zero level must to be treated with caution. | |||||||
<-- Herschel-SPIRE detectors are only sensitive to relative variations, and so as a consequence, the absolute brightness of the observed region is unknown and maps are constructed such that they have zero median. The Planck-HFI detectors are similar to the SPIRE ones, but the Planck observing strategy allowed it to (almost) observe a great circle on the sky every minute (having a 1 rpm spinning rate). By comparing the sky brightness as measured by COBE-FIRAS at the galactic poles (where the dust emission is lower), HFI is capable of setting an absolute offset to its maps. SPIRE and HFI share two channels with overlapping wavebands: SPIRE-PMW and HFI-857 have a similar filter profile, while SPIRE-PLW and HFI-545 are shifted by ~10%. --> | ||||||||
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<-- * In HIPE13 (and HIPE 11), the default size of the PRF used by SUSSEXtractor has a size of 5x5 pixels. In HIPE 12, a PRF of size 13x13 was used to allow a more complete coverage of the PRF edges, but this lead to some secondary effects that negatively affected the flux densities measured by SUSSEXtractor. The original HIPE11/13 results can be replicated by this script --> | |||||||
SPIRE report from the January 2013 HSC Map Making Workshop |