Difference: DataProcessingWorkshop2013 (36 vs. 37)

Revision 372013-06-26 - PedroGarciaLario

Line: 1 to 1

Herschel Data Processing Workshop for Newcomers, 24-27 June 2013

Line: 373 to 373
 But I must confess I am not a CLEAN expert. One additional limitation is that there is not a single unique PSF for PACS, the PSF depends on the observation parameters (scan direction and speed) and data processing (map-making) used. Hope it helps.
SPIRE photometry

Q1: How much memory is needed for the reduction of a large SPIRE field (e.g. like a 2x2 degree Hi-GAL tile)?

A1: 8-10 GB is usually more than enough to reduce a large map like this. Small scan maps can be reduced without any problem with a 4GB laptop.

Q2: Are there any limitations in the reliability of the scripts used for determining the Planck offsets to be applied to SPIRE maps? In particular, I am interested in whether they can be applied to very small maps (since the corrections are based on the average absolute fluxes covered by the much bigger Planck maps)?

A2: In principle not, but it could be convenient to look at the special characteristics of the emission observed in your small field. If you have a particular sky field dominated by galactic cirrus emission it could be an issue. Raise a helpdesk ticket indicating the OBSID of the map you want to analyse and we will tell you whether we see any problem with applying the offset derived from Planck data.

SPIRE spectroscopy

Q1: Should the semi-extended correction be applied after all other steps (for instance improve background etc)?

A1: semi-extended correction should be applied as a last step after background subtraction because the galactic emission could make the source look as semi-extended

Q2: How do I find the appropriate dark observation to be used in the processing of a SPIRE FTS observation?

A2: You should look at the dark observations taken in the same operational day (OD) when your science observation was taken, or the nearest in time if there is none available on that particular OD. The OD number you can get it from the Observing Log or from the Archive (HSA). Once you know the OD, you query in HSA for all SPIRE FTS observations taken on that OD or a small range of ODs around the date when the observation was taken. There is also a list with all available dark observations taken (in the standard observing mode) throughout the mission at : http://herschel.esac.esa.int/twiki/bin/view/Public/SpireDailyDarkObservations

This site is powered by the TWiki collaboration platform Powered by Perl