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For any user of PACS data, it is necessary to have some information about the AOT -- the observing mode -- of the observation they are working on in order to know which of the SPG products to work with, which pipelines to use, and which calibration or other uncertainties to consider. All the relevant AOT details are held in the header keywords of the FITS files. Every FITS file in an HSA download has a complete copy of the keywords, and hence any Level >=2 product can be opened (e.g. in fv) to find the AOT. Tables containing the description of the AOT keywords can be found in the PACS Products Explained. | ||||||||
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< < | For photometry, almost all observations were of the scan-map mode and hence the same set of three maps are provided, where the key to knowing which to use is in the final chapter of the PACS Products Explained. For spectroscopy there were may more variations on the AOT: pointing mode, spectral mode, background sampling, type of mapping. In addition, the Level 2 and 2.5 products for spectroscopy are "sliced": each cube or table is for one wavelength range only, and the filenames differ only by an "s##" where more than one wavelength range was requested for that observation. This is also explained in the PACS Products Explained. In order to make it easier for an archive user to know, before having to open any FITS file, which FITS file they want, we have created a spreadsheet of AOT keyword data. In this table, you will find: the obsid; line/range spectroscopy; chop-nod or unchopped; pointed or mapping; if mapping, the raster details; the number of spectral lines or ranges requested or "sedxxx" to indicate that the observation is a full SED in the xxx band; line IDs given by the observer; and then four columns of slice number (the "s##" in the filename) and wavelength range: two columns (red and blue camera) for pointed observations where the search was done on the rebinned cube (one of the final products for this mode), and two columns (red and blue) for mapping observations where the search was done on the projected cubes (one of the final products for this mode). | |||||||
> > | For photometry, almost all observations were of the scan-map mode and hence the same set of three maps are provided, where the key to knowing which to use is in the final chapter of the PACS Products Explained. For spectroscopy there were may more variations on the AOT: pointing mode, spectral mode, background sampling, type of mapping. In addition, the Level 2 and 2.5 products for spectroscopy are "sliced": each cube or table is for one wavelength range only, and the filenames differ only by an "s##" where more than one wavelength range was requested for that observation. This is also explained in the PACS Products Explained. In order to make it easier for an archive user to know, before having to open any FITS file, which FITS file they want, we have created a spreadsheet of AOT keyword data. In this tarball (spreadsheet/readme), you will find: the obsid; line/range spectroscopy; chop-nod or unchopped; pointed or mapping; if mapping, the raster details; the number of spectral lines or ranges requested or "sedxxx" to indicate that the observation is a full SED in the xxx band; line IDs given by the observer; and then four columns of slice number (the "s##" in the filename) and wavelength range: two columns (red and blue camera) for pointed observations where the search was done on the rebinned cube (one of the final products for this mode), and two columns (red and blue) for mapping observations where the search was done on the projected cubes (one of the final products for this mode). | |||||||
All standard observations that processed to at least Level 2 in the SPG pipeline are included in this table. | ||||||||
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The FMT functionality is fully incorporated in HIPE 15, however it has not yet been tested on general users, and for this reason we recommend you to contact the Herschel helpdesk to ask for advice on running the code. In exchange for some one-on-one help, we would appreciate feedback on the scripts and the documentation provided in the FMT package. | ||||||||
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AOT table for PACS spectroscopyFor any user of PACS data, it is necessary to have some information about the AOT -- the observing mode -- of the observation they are working on in order to know which of the SPG products to work with, which pipelines to use, and which calibration or other uncertainties to consider. All the relevant AOT details are held in the header keywords of the FITS files. Every FITS file in an HSA download has a complete copy of the keywords, and hence any Level >=2 product can be opened (e.g. in fv) to find the AOT. Tables containing the description of the AOT keywords can be found in the PACS Products Explained. For photometry, almost all observations were of the scan-map mode and hence the same set of three maps are provided, where the key to knowing which to use is in the final chapter of the PACS Products Explained. For spectroscopy there were may more variations on the AOT: pointing mode, spectral mode, background sampling, type of mapping. In addition, the Level 2 and 2.5 products for spectroscopy are "sliced": each cube or table is for one wavelength range only, and the filenames differ only by an "s##" where more than one wavelength range was requested for that observation. This is also explained in the PACS Products Explained. In order to make it easier for an archive user to know, before having to open any FITS file, which FITS file they want, we have created a spreadsheet of AOT keyword data. In this table, you will find: the obsid; line/range spectroscopy; chop-nod or unchopped; pointed or mapping; if mapping, the raster details; the number of spectral lines or ranges requested or "sedxxx" to indicate that the observation is a full SED in the xxx band; line IDs given by the observer; and then four columns of slice number (the "s##" in the filename) and wavelength range: two columns (red and blue camera) for pointed observations where the search was done on the rebinned cube (one of the final products for this mode), and two columns (red and blue) for mapping observations where the search was done on the projected cubes (one of the final products for this mode). All standard observations that processed to at least Level 2 in the SPG pipeline are included in this table. | |||||||
Data reduction: HIPE, documentation, and useful links for data issuesHIPE (Herschel Interactive Processing Environment) is the tool used to inspect, reduce, and analyse Herschel data. | ||||||||
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The FMT has been developed in HIPE 15 to estimate the degree to which the fluxes are incorrect for any observation. As this differs for each observation -- it depends on the surface brightness distribution of the source and the pointing pattern of the observation (pointed, Nyquist mapping, oversampled mapping, tiling...) -- the correction is unique to each observation. To use the FMT it will be necessary to run HIPE. The most important input is a model of the surface brightness distribution of your source at the wavelength(s) of the observation. With this input, the surface brightness distribution that would have been observed with a completely uniform illumination is estimated by running the pipeline on the model. This output can be compared to your data. | ||||||||
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< < | The FMT is fully incorporated in HIPE 15, however it has not yet been tested on general users, and for this reason we recommend you to contact the Herschel helpdesk to ask for advice on running the code. In exchange for some one-on-one help, we would appreciate feedback on the scripts and the documentation provided in the FMT package. | |||||||
> > | The FMT functionality is fully incorporated in HIPE 15, however it has not yet been tested on general users, and for this reason we recommend you to contact the Herschel helpdesk to ask for advice on running the code. In exchange for some one-on-one help, we would appreciate feedback on the scripts and the documentation provided in the FMT package. | |||||||
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Some information about this is provided in the spectroscopy PACS Data Reduction Guide. A quick summary is:
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Although we are now in the post-operations phase of the mission, the PACS OM and the AOT release notes can still be useful to read for a background understanding on how PACS data were gathered. | ||||||||
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The PACS beam efficiencies describe the relative coupling of a point source to each spaxel as a function of the source's position in the FOV. The efficiencies are the ratio of the beam profile convolved with each detectors response and with the radiation pattern of a source, and the total power received. In order to characterise the PACS beam, Neptune raster maps at certain wavelengths were observed during the mission. Coarse 25x25 raster maps with raster step size 2.5" were obtained between ODs 174 and 751 in chopped mode covering all 25 spaxels. Also, fine Neptune 5x5 raster maps with raster step size 2” were executed on ODs 1311 and 1312. The combination of four such fine rasters, offset by 1", provide very high sampling for the central spaxel beam efficiency only. All raster maps were observed with only one chop -off position (aka, asymmetric chopNod). All these measurements were registered using least squares minimization in coordinates and gain, and a synthetic beam was constructed with the coarse raster outside the area covered by fine raster and from matched fine raster inside. Finally, this synthetic beam is interpolated into a 0.5" grid. Data were processed using the telescope background normalisation scheme to obtain the telescope-normalised signal per spaxel. The WCS associated with the beam is in sky coordinates for position angle 0. The final maps are a reconstruction of what each spaxel "sees" as the planet was rastered across each detector's aperture on the sky. Note the difference to a regular source map, where we reconstruct the spatial information as a function of position in the sky, even combining information coming from different spaxels. | ||||||||
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< < | Finally, the efficiencies were calculated normalising the raster maps in the following way:
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< < | Data processing known issues of standard products for photometry and spectroscopy: The Herschel Science Archive provides bulk-processed Level 2/2.5 products. This Data Processing Known Issues page describes typical problems and caveats the observer needs to be familiar when looking at the results of this "SPG" (standard product generation) processing. Aspects of product quality which can be further optimised by interactive processing are also summarised here. The document refers to the version of data processing pipeline currently being used for processing of incoming Herschel data. | |||||||
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< < | A brief introduction to reducing PACS data in HIPE. You can consult the PACS Data Reduction Guides (photometry and spectroscopy; available via HIPE) for more detail. | |||||||
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< < | Due to an oversight in the pipeline scripts of HIPE 13, the drizzled cubes for chop-nod line scan observations created by "SPG 13" have incorrect fluxes. Therefore you should not use the drizzled cubes downloaded from the HSA if the Meta datum "creator" is "SPG 13.0", whether they are within the ObservationContext at Level 2, or part of a Standalone Browse Product download. Drizzled cubes created for unchopped mode observations are unaffected, and for chop-nod range scan observations, drizzled cubes are not created by the SPG 13 pipeline.
This oversight has been corrected in HIPE/SPG 14. The drizzled cubes you get in an observation downloaded from the HSA with "creator" of "SPG 14.0" have correct fluxes. In HIPE 14 there is a dedicated script to produce these drizzled cubes. Therefore we recommend you use the SPG 14.0 products, or use the dedicated pipeline in HIPE 14 if you need your drizzled cubes before the SPG 14 products are available.
Photometry | |||||||
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< < | Some Unimap maps produced by SPG 13 and using HIPE 13 scripts show overshooting effects around very bright sources that are surrounded by a diffuse and relatively faint background. See, as an example, the blue image of NGC253 (obsID: 1342221743). This effect is due to a non-optimised convergence of the GLS algorithm and it will be corrected in HIPE/SPG14. | |||||||
> > | The relevant documentation to read before working on PACS data for the first time are the following: | |||||||
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< < | This has been corrected in HIPE 14, and products with "creator" of "SPG 14" have no overshooting effects.
Observing with PACS
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< < | Although we are now in the post-operations phase of the mission, the PACS OM and the AOT release notes can still be useful to read for a background understanding on how PACS data were gathered | |||||||
> > | Although we are now in the post-operations phase of the mission, the PACS OM and the AOT release notes can still be useful to read for a background understanding on how PACS data were gathered. | |||||||
Changed: | ||||||||
< < | The In-flight scientific capabilities of the PACS instrument are also given in this paper: The Photodetector Array Camera and Spectrometer (PACS) on the Herschel Space Observatory (1.5 Mb), Poglitsch et al., 2010, A&A, 518, L2 | |||||||
> > |
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PACS calibration and performance | ||||||||
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< < | Data processing known issues of standard products for photometry and spectroscopy: Bulk-processed Level 2/2.5 products are provided in the Herschel Science Archive. This Data Processing Known Issues page describes typical problems and caveats the observer needs to be familiar when looking at the results of this "SPG" (standard product generation) processing. Aspects of product quality which can be further optimised by interactive processing are also summarised here. The document refers to the version of data processing pipeline currently being used for processing of incoming Herschel data. | |||||||
> > | Data processing known issues of standard products for photometry and spectroscopy: The Herschel Science Archive provides bulk-processed Level 2/2.5 products. This Data Processing Known Issues page describes typical problems and caveats the observer needs to be familiar when looking at the results of this "SPG" (standard product generation) processing. Aspects of product quality which can be further optimised by interactive processing are also summarised here. The document refers to the version of data processing pipeline currently being used for processing of incoming Herschel data. | |||||||
Photometer calibration in scan maps | ||||||||
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Photometer map-makers | ||||||||
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< < |
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> > | Four fundamentally different map-makers are offered in HIPE 14 with interactive pipeline scripts, starting from Level 1. These map-makers are used in different ways to generate standard products ("SPG" product) provided by the Herschel Science Archive. High-pass filtering is applied to generate Level2 products, while Level2.5 products are generated by combining pairs of observations acquired in the scan plus cross-scan mode, using the Unimap, JScanam, and High-pass filtering mappers. Level3 products are mosaics of Unimap and Jscanam Level2.5 products that belong to the same sky field and to the same observing program.
| |||||||
Highpass filtering provides optimum sensitivity to point-sources while JScanam, Unimap and MadMap mappers all clean the dataset of systematic effects and remove the correlated 1/f noise, preserving at the same time the sky signal over large spatial scales. They are suited for analysing both point sources and extended emission.
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PACS calibration file versions | ||||||||
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Reducing PACS dataA brief introduction to reducing PACS data in HIPE. You can consult the PACS Data Reduction Guides (photometry and spectroscopy; available via HIPE) for more detail. | ||||||||
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HIPE, data reduction documentation, and useful links for data issues | ||||||||
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PACS instrument and calibration web pages | ||||||||
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< < | PACS spectrometer calibration | |||||||
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PACS spectrometer calibration | |||||||
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Introduction | ||||||||
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This oversight has been corrected in HIPE/SPG 14. The drizzled cubes you get in an observation downloaded from the HSA with "creator" of "SPG 14.0" have correct fluxes. In HIPE 14 there is a dedicated script to produce these drizzled cubes. Therefore we recommend you use the SPG 14.0 products, or use the dedicated pipeline in HIPE 14 if you need your drizzled cubes before the SPG 14 products are available.
Photometry | ||||||||
Changed: | ||||||||
< < | Some Unimap maps produced by SPG 13 and using HIPE 13 scripts show overshooting effects around very bright sources that are surrounded by a diffuse and relatively faint background. See, as an example, the blue image of NGC253 (obsID: 1342221743). This effect is due to a non-optimised convergence of the GLS algorithm and it will be corrected in HIPE/SPG14. | |||||||
> > | Some Unimap maps produced by SPG 13 and using HIPE 13 scripts show overshooting effects around very bright sources that are surrounded by a diffuse and relatively faint background. See, as an example, the blue image of NGC253 (obsID: 1342221743). This effect is due to a non-optimised convergence of the GLS algorithm and it will be corrected in HIPE/SPG14. | |||||||
This has been corrected in HIPE 14, and products with "creator" of "SPG 14" have no overshooting effects.
Observing with PACS | ||||||||
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Photometer calibration in scan maps
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Photometer map-makers
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> > | Highpass filtering provides optimum sensitivity to point-sources while JScanam, Unimap and MadMap mappers all clean the dataset of systematic effects and remove the correlated 1/f noise, preserving at the same time the sky signal over large spatial scales. They are suited for analysing both point sources and extended emission. | |||||||
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Cookbooks and interactive pipeline scripts
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PACS instrument and calibration web pages | ||||||||
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HIPE, data reduction documentation, and useful links for data issues | ||||||||
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PACS instrument and calibration web pages | ||||||||
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Cookbooks and interactive pipeline scripts
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Spectroscopy | ||||||||
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HIPE, data reduction documentation, and useful links for data issues
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Introduction | ||||||||
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You can also consult the PACS NHSC homepage![]() | ||||||||
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< < | Important message about drizzled cubes | |||||||
> > | Temporary notesSpectroscopy | |||||||
Changed: | ||||||||
< < | Due to an oversight in the pipeline scripts of HIPE 13, the drizzled cubes for chop-nod line scan observations created by "SPG 13" have incorrect fluxes. Therefore you should not use the drizzled cubes downloaded from the HSA if the Meta datum "creator" is "SPG 13.0", whether they are within the ObservationContext at Level 2, or part of a Standalone Browse Product download. Drizzled cubes created for unchopped mode observations are unaffected, and for chop-nod range scan observations, drizzled cubes are not created by the SPG 13 pipeline. | |||||||
> > | Due to an oversight in the pipeline scripts of HIPE 13, the drizzled cubes for chop-nod line scan observations created by "SPG 13" have incorrect fluxes. Therefore you should not use the drizzled cubes downloaded from the HSA if the Meta datum "creator" is "SPG 13.0", whether they are within the ObservationContext at Level 2, or part of a Standalone Browse Product download. Drizzled cubes created for unchopped mode observations are unaffected, and for chop-nod range scan observations, drizzled cubes are not created by the SPG 13 pipeline. | |||||||
This oversight has been corrected in HIPE/SPG 14. The drizzled cubes you get in an observation downloaded from the HSA with "creator" of "SPG 14.0" have correct fluxes. In HIPE 14 there is a dedicated script to produce these drizzled cubes. Therefore we recommend you use the SPG 14.0 products, or use the dedicated pipeline in HIPE 14 if you need your drizzled cubes before the SPG 14 products are available. | ||||||||
Added: | ||||||||
> > | Photometry | |||||||
Changed: | ||||||||
< < | FYI: Drizzled cubes can be found in an observation in the context called HPS3DD [R|B] (red and blue). They are also provided as standalone browse products in a context called HPS3DEQ [R|B] (red and blue, equidistant wavelength grid version of the drizzled cubes). On disk the FITS files for these cubes have the same set of letters in their name (but in lower case) and are at the Level 2 part of an observation.
For more information about the standard and the standalone browse cubes provided for PACS spectroscopy, see the PACS Products Explained HIPE help document, which is also available from the PACS documentation webpage and the HIPE download webpage, both off the Herschel Science Centre webpage.
Important message about Unimap maps | |||||||
> > | Some Unimap maps produced by SPG 13 and using HIPE 13 scripts show overshooting effects around very bright sources that are surrounded by a diffuse and relatively faint background. See, as an example, the blue image of NGC253 (obsID: 1342221743). This effect is due to a non-optimised convergence of the GLS algorithm and it will be corrected in HIPE/SPG14. | |||||||
Changed: | ||||||||
< < | Some Unimap maps produced by SPG 13 and using HIPE 13 scripts show overshooting effects around very bright sources that are surrounded by a diffuse and relatively faint background. See, as an example, the blue image of NGC253 (obsID: 1342221743). This effect is due to a non-optimised convergence of the GLS algorithm and it will be corrected in HIPE/SPG14. This has been corrected in HIPE 14, and products with "creator" of "SPG 14" have no overshooting effects. | |||||||
> > | This has been corrected in HIPE 14, and products with "creator" of "SPG 14" have no overshooting effects. | |||||||
Observing with PACS
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Photometer calibration in scan maps
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Photometer map-makers | ||||||||
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HIPE, data reduction documentation, and useful links for data issues | ||||||||
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Cookbooks and interactive pipeline scripts
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Tutorials and scripts | ||||||||
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PACS instrument and calibration web pages | ||||||||
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Photometer map-makers | ||||||||
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PACS instrument and calibration web pages | ||||||||
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Deleted: | ||||||||
< < | <!-- A new responsivity calibration (version) is deployed on the HCSS 7 track (this is explained in the internal report PICC-ME-TN-033 v1.01, where the associated encircled energy fraction [EEF] is given). This improves the accuracy of photometry to 3% in the blue channel and 5% in the red channel. "PACS photometer point-source flux calibration (3.1 Mb) (PICC-ME-TN-037), version 1.0, 12 April 2011. We refer to: PACS Photometer: chop/nod point-source & mini-scan map AOT release note: (2 Mb) version 2.0, 12 November 2010. We recommend you use the mini scan-map technique in all science cases related to point-sources, compact sources and also in cases of faint extended emission around point-sources. The chop/nod mode is no longer recommended for use * However, for a technical assessment of the original chop/nod mode sensitivity intended for point-sources, we refer to SAp-PACS-MS-0711-09 (5.5 Mb) and to the paper "The Herschel PACS photometer calibration - A time dependent flux calibration for the PACS chopped point-source photometry AOT mode" ![]() --> | |||||||
Photometer map-makers
| ||||||||
Line: 80 to 78 | ||||||||
| ||||||||
Changed: | ||||||||
< < | <!-- This is corrected for MADmap in HIPE 12 by the task convertToFixedPixelSize() at the end of level1. The flux difference come from the fact that the mean values of the optical flat are significantly different from 1, in other words it cannot be assumed by external map-makers that the pixel sizes is constant of the field of view at 3.2"/6.4 in the blue/red channel respectively. Scanamorphos and Unimap are also affected, but not JScanam that makes use of photProject.-->
PACS spectrometer calibration | |||||||
> > | PACS spectrometer calibration
| |||||||
|
Line: 1 to 1 | ||||||||
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PACS instrument and calibration web pages | ||||||||
Line: 10 to 10 | ||||||||
You can also consult the PACS NHSC homepage![]() | ||||||||
Changed: | ||||||||
< < | Important message about drizzled cubes in HIPE 13 | |||||||
> > | Important message about drizzled cubes | |||||||
Changed: | ||||||||
< < | Due to an oversight in the pipeline scripts of HIPE 13, the drizzled cubes you get for chop-nod line scan observations created by "SPG 13" will have incorrect fluxes. Therefore you should not use the drizzled cubes downloaded from the HSA if the Meta datum "creator" is "SPG 13.0", whether they are within the ObservationContext at Level 2, or part of a Standalone Browse Product download. Any drizzled cubes created for unchopped mode observations will be unaffected. For chop-nod range scan observations, drizzled cubes are not created by the SPG 13 pipeline anyway. This oversight will be corrected in HIPE/SPG 14. | |||||||
> > | Due to an oversight in the pipeline scripts of HIPE 13, the drizzled cubes for chop-nod line scan observations created by "SPG 13" have incorrect fluxes. Therefore you should not use the drizzled cubes downloaded from the HSA if the Meta datum "creator" is "SPG 13.0", whether they are within the ObservationContext at Level 2, or part of a Standalone Browse Product download. | |||||||
Changed: | ||||||||
< < | For the affected observations you have the following alternatives:
| |||||||
> > | Drizzled cubes created for unchopped mode observations are unaffected, and for chop-nod range scan observations, drizzled cubes are not created by the SPG 13 pipeline. | |||||||
Changed: | ||||||||
< < | For Your Information: Drizzled cubes FITS files, and their name as listed in an ObservationContext, are: HPS3DD [R|B] (red and blue) Standalone browse product drizzled cube FITS files, and their name as listed in an ObservationContext in the browse product section are: HPS3DEQ [R|B] (red and blue, equidistant wavelength grid version of the drizzled cubes). Projected cubes have the name: HPS3DP [R|B]. | |||||||
> > | This oversight has been corrected in HIPE/SPG 14. The drizzled cubes you get in an observation downloaded from the HSA with "creator" of "SPG 14.0" have correct fluxes. In HIPE 14 there is a dedicated script to produce these drizzled cubes. Therefore we recommend you use the SPG 14.0 products, or use the dedicated pipeline in HIPE 14 if you need your drizzled cubes before the SPG 14 products are available. | |||||||
Changed: | ||||||||
< < | For more information about the standard and the standalone browse cubes provided for PACS spectroscopy, see the PACS Products Explained HIPE help document (which is also linked as a PDF file in the Data Reduction section). | |||||||
> > | FYI: Drizzled cubes can be found in an observation in the context called HPS3DD [R|B] (red and blue). They are also provided as standalone browse products in a context called HPS3DEQ [R|B] (red and blue, equidistant wavelength grid version of the drizzled cubes). On disk the FITS files for these cubes have the same set of letters in their name (but in lower case) and are at the Level 2 part of an observation. | |||||||
Changed: | ||||||||
< < | Important message about Unimap maps in HIPE 13 | |||||||
> > | For more information about the standard and the standalone browse cubes provided for PACS spectroscopy, see the PACS Products Explained HIPE help document, which is also available from the PACS documentation webpage and the HIPE download webpage, both off the Herschel Science Centre webpage.
Important message about Unimap maps | |||||||
Changed: | ||||||||
< < | Some Unimap maps show overshooting effects around very bright sources that are surrounded by a diffuse and relatively faint background. See, as an example, the blue image of NGC253 (obsID: 1342221743). This effect is due to a not optimised convergence of the GLS algorithm and it will be corrected in HIPE/SPG14. | |||||||
> > | Some Unimap maps produced by SPG 13 and using HIPE 13 scripts show overshooting effects around very bright sources that are surrounded by a diffuse and relatively faint background. See, as an example, the blue image of NGC253 (obsID: 1342221743). This effect is due to a non-optimised convergence of the GLS algorithm and it will be corrected in HIPE/SPG14. | |||||||
Added: | ||||||||
> > | This has been corrected in HIPE 14, and products with "creator" of "SPG 14" have no overshooting effects. | |||||||
Observing with PACS
|
Line: 1 to 1 | ||||||||
---|---|---|---|---|---|---|---|---|
PACS instrument and calibration web pages | ||||||||
Line: 49 to 49 | ||||||||
Photometer calibration in scan maps | ||||||||
Changed: | ||||||||
< < |
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> > |
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|
Line: 1 to 1 | ||||||||
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PACS instrument and calibration web pages |
Line: 1 to 1 | ||||||||
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PACS instrument and calibration web pages | ||||||||
Changed: | ||||||||
< < | ||||||||
> > | ||||||||
Introduction | ||||||||
Line: 12 to 12 | ||||||||
Important message about drizzled cubes in HIPE 13 | ||||||||
Changed: | ||||||||
< < | Due to an oversight in the pipeline scripts of HIPE 13, the drizzled cubes you get for chop-nod line scan observations created by "SPG 13" will have incorrect fluxes. Therefore you should not use the drizzled cubes downloaded from the HSA if the Meta datum "creator" is "SPG 13.0", whether they are within the ObservationContext at Level 2, or part of a Standalone Browse Product download. Any drizzled cubes created for unchopped mode observations will be unaffected. For chop-nod range scan observations, drizzled cubes are not created by the SPG 13 pipeline anyway. This oversight will be corrected in HIPE/SPG 14. | |||||||
> > | Due to an oversight in the pipeline scripts of HIPE 13, the drizzled cubes you get for chop-nod line scan observations created by "SPG 13" will have incorrect fluxes. Therefore you should not use the drizzled cubes downloaded from the HSA if the Meta datum "creator" is "SPG 13.0", whether they are within the ObservationContext at Level 2, or part of a Standalone Browse Product download. Any drizzled cubes created for unchopped mode observations will be unaffected. For chop-nod range scan observations, drizzled cubes are not created by the SPG 13 pipeline anyway. This oversight will be corrected in HIPE/SPG 14. | |||||||
For the affected observations you have the following alternatives:
| ||||||||
Changed: | ||||||||
< < | For Your Information: Drizzled cubes FITS files, and their name as listed in an ObservationContext, are: HPS3DD [R|B] (red and blue) Standalone browse product drizzled cube FITS files, and their name as listed in an ObservationContext in the browse product section are: HPS3DEQ [R|B] (red and blue, equidistant wavelength grid version of the drizzled cubes). Projected cubes have the name: HPS3DP [R|B]. | |||||||
> > | For Your Information: Drizzled cubes FITS files, and their name as listed in an ObservationContext, are: HPS3DD [R|B] (red and blue) Standalone browse product drizzled cube FITS files, and their name as listed in an ObservationContext in the browse product section are: HPS3DEQ [R|B] (red and blue, equidistant wavelength grid version of the drizzled cubes). Projected cubes have the name: HPS3DP [R|B]. | |||||||
For more information about the standard and the standalone browse cubes provided for PACS spectroscopy, see the PACS Products Explained HIPE help document (which is also linked as a PDF file in the Data Reduction section).
Important message about Unimap maps in HIPE 13 | ||||||||
Changed: | ||||||||
< < | Some Unimap maps show overshooting effects around very bright sources that are surrounded by a diffuse and relatively faint background. See, as an example, the blue image of NGC253 (obsID: 1342221743). This effect is due to a not optimised convergence of the GLS algorithm and it will be corrected in HIPE/SPG14. | |||||||
> > | Some Unimap maps show overshooting effects around very bright sources that are surrounded by a diffuse and relatively faint background. See, as an example, the blue image of NGC253 (obsID: 1342221743). This effect is due to a not optimised convergence of the GLS algorithm and it will be corrected in HIPE/SPG14. | |||||||
Observing with PACS
| ||||||||
Line: 56 to 49 | ||||||||
Photometer calibration in scan maps | ||||||||
Changed: | ||||||||
< < | <--
| |||||||
> > |
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Line: 74 to 64 | ||||||||
| ||||||||
Changed: | ||||||||
< < | <-- A new responsivity calibration (version) is deployed on the HCSS 7 track (this is explained in the internal report PICC-ME-TN-033 v1.01, where the associated encircled energy fraction [EEF] is given). This improves the accuracy of photometry to 3% in the blue channel and 5% in the red channel. "PACS photometer point-source flux calibration (3.1 Mb) (PICC-ME-TN-037), version 1.0, 12 April 2011. We refer to: PACS Photometer: chop/nod point-source & mini-scan map AOT release note: (2 Mb) version 2.0, 12 November 2010. We recommend you use the mini scan-map technique in all science cases related to point-sources, compact sources and also in cases of faint extended emission around point-sources. The chop/nod mode is no longer recommended for use
| |||||||
> > | <!-- A new responsivity calibration (version) is deployed on the HCSS 7 track (this is explained in the internal report PICC-ME-TN-033 v1.01, where the associated encircled energy fraction [EEF] is given). This improves the accuracy of photometry to 3% in the blue channel and 5% in the red channel. "PACS photometer point-source flux calibration (3.1 Mb) (PICC-ME-TN-037), version 1.0, 12 April 2011. We refer to: PACS Photometer: chop/nod point-source & mini-scan map AOT release note: (2 Mb) version 2.0, 12 November 2010. We recommend you use the mini scan-map technique in all science cases related to point-sources, compact sources and also in cases of faint extended emission around point-sources. The chop/nod mode is no longer recommended for use * However, for a technical assessment of the original chop/nod mode sensitivity intended for point-sources, we refer to SAp-PACS-MS-0711-09 (5.5 Mb) and to the paper "The Herschel PACS photometer calibration - A time dependent flux calibration for the PACS chopped point-source photometry AOT mode" ![]() --> | |||||||
Photometer map-makers | ||||||||
Deleted: | ||||||||
< < | ||||||||
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Line: 102 to 77 | ||||||||
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< < |
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> > |
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< < | <-- This is corrected for MADmap in HIPE 12 by the task convertToFixedPixelSize() at the end of level1. The flux difference come from the fact that the mean values of the optical flat are significantly different from 1, in other words it cannot be assumed by external map-makers that the pixel sizes is constant of the field of view at 3.2"/6.4 in the blue/red channel respectively. Scanamorphos and Unimap are also affected, but not JScanam that makes use of photProject.--> | |||||||
> > | <!-- This is corrected for MADmap in HIPE 12 by the task convertToFixedPixelSize() at the end of level1. The flux difference come from the fact that the mean values of the optical flat are significantly different from 1, in other words it cannot be assumed by external map-makers that the pixel sizes is constant of the field of view at 3.2"/6.4 in the blue/red channel respectively. Scanamorphos and Unimap are also affected, but not JScanam that makes use of photProject.--> | |||||||
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< < | Data processing known issues of standard products for photometry and spectroscopy: Bulk-processed Level 2/2.5 products are provided in the Herschel Science Archive. This Data Processing Known Issues page describes typical problems and caveats the observer needs to be familiar when looking at the results of this "SPG" (standard product generation) processing. Aspects of product quality which can be further optimised by interactive processing are also summarised here. The document refers to the version of data processing pipeline currently being used for processing of incoming Herschel data. | |||||||
> > | Data processing known issues of standard products for photometry and spectroscopy: Bulk-processed Level 2/2.5 products are provided in the Herschel Science Archive. This Data Processing Known Issues page describes typical problems and caveats the observer needs to be familiar when looking at the results of this "SPG" (standard product generation) processing. Aspects of product quality which can be further optimised by interactive processing are also summarised here. The document refers to the version of data processing pipeline currently being used for processing of incoming Herschel data. | |||||||
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<-- This is corrected for MADmap in HIPE 12 by the task convertToFixedPixelSize() at the end of level1. The flux difference come from the fact that the mean values of the optical flat are significantly different from 1, in other words it cannot be assumed by external map-makers that the pixel sizes is constant of the field of view at 3.2"/6.4 in the blue/red channel respectively. Scanamorphos and Unimap are also affected, but not JScanam that makes use of photProject.--> | ||||||||
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For more information about the standard and the standalone browse cubes provided for PACS spectroscopy, see the PACS Products Explained HIPE help document (which is also linked as a PDF file in the Data Reduction section). | ||||||||
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> > | Important message about Unimap maps in HIPE 13Some Unimap maps show overshooting effects around very bright sources that are surrounded by a diffuse and relatively faint background. See, as an example, the blue image of NGC253 (obsID: 1342221743). This effect is due to a not optimised convergence of the GLS algorithm and it will be corrected in HIPE/SPG14. | |||||||
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> > | Important message about drizzled cubes in HIPE 13Due to an oversight in the pipeline scripts of HIPE 13, the drizzled cubes you get for chop-nod line scan observations created by "SPG 13" will have incorrect fluxes. Therefore you should not use the drizzled cubes downloaded from the HSA if the Meta datum "creator" is "SPG 13.0", whether they are within the ObservationContext at Level 2, or part of a Standalone Browse Product download. Any drizzled cubes created for unchopped mode observations will be unaffected. For chop-nod range scan observations, drizzled cubes are not created by the SPG 13 pipeline anyway. This oversight will be corrected in HIPE/SPG 14. For the affected observations you have the following alternatives:
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<--A new responsivity calibration (version) is deployed on the HCSS 7 track (this is explained in the internal report PICC-ME-TN-033 v1.01, where the associated encircled energy fraction [EEF] is given). This improves the accuracy of photometry to 3% in the blue channel and 5% in the red channel. --> | |||||||
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< < | The optical field distortion is not applied in level 1, as this calibration is applied by the native photProject task. As a result, external map-makers starting from level 1 have a systematic flux overestimate of 6-7% in the red channel and a lower underestimate (~2%) in the blue channel of the flux scale. This is corrected for MADmap in Hipe12 by introducing the new task convertToFixedPixelSize() at the end of level1. The flux difference come from the fact that the mean values of the optical flat are significantly different from 1, in other words it cannot be assumed by external map-makers that the pixel sizes is constant of the field of view at 3.2"/6.4 in the blue/red channel respectively. Scanamorphos and Unimap are also affected, but not JScanam that makes use of photProject. | |||||||
> > | <-- This is corrected for MADmap in HIPE 12 by the task convertToFixedPixelSize() at the end of level1. The flux difference come from the fact that the mean values of the optical flat are significantly different from 1, in other words it cannot be assumed by external map-makers that the pixel sizes is constant of the field of view at 3.2"/6.4 in the blue/red channel respectively. Scanamorphos and Unimap are also affected, but not JScanam that makes use of photProject.--> | |||||||
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< < | you the release note of the new calibration set, with details about the changes. This is further explained in the PDRGs (chap. 2). Clicking on 'Install' will install the latest calibration files. | |||||||
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< < | This page provides up-to-date information about using the PACS instrument: from preparing observations to reducing your data. This includes information on the PACS instrument, PACS data, reducing PACS data in HIPE, and post-pipeline processing, and links to tutorials and scripts that you can run in HIPE. The calibration accuracies and technical information about the spectrometer and photometer of PACS are also provided here, as well as information about what future calibration and processing improvements can be expected. | |||||||
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< < | A summary of the PACS instrument for an astronomerHere we provide a summary of instrumental and calibration details that a data-reducing astronomer often wants know. The summary provides a set of links or information about where to find the information. Spectroscopy
Reducing PACS dataBrief explanationA brief introduction to reducing PACS data in HIPE. You can consult the PACS Data Reduction Guides (photometry and spectroscopy) for more detail.
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> > | The In-flight scientific capabilities of the PACS instrument are also given in this paper: The Photodetector Array Camera and Spectrometer (PACS) on the Herschel Space Observatory (1.5 Mb), Poglitsch et al., 2010, A&A, 518, L2 | |||||||
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Reducing PACS dataA brief introduction to reducing PACS data in HIPE. You can consult the PACS Data Reduction Guides (photometry and spectroscopy; available via HIPE) for more detail.
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A summary of the PACS instrument for an astronomerHere we provide a summary of instrumental and calibration details that a data-reducing astronomer often wants know. The summary provides a set of links or information about where to find the information. Spectroscopy
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A report of the map-making working group compiled by Roberta Paladini is available: PACS map-making tools: analysis and benchmarking, 1 Nov. 2013. | ||||||||
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> > | An updated version of that report concentrating on JScanam, MADmap and Unimap in their latest versions is available in PACS Map-making Tools: Update on Analysis and Benchmarking, 30 March 2014. | |||||||
The optical field distortion is not applied in level 1, as this calibration is applied by the native photProject task. As a result, external map-makers starting from level 1 have a systematic flux overestimate of 6-7% in the red channel and a lower underestimate (~2%) in the blue channel of the flux scale. This is corrected for MADmap in Hipe12 by introducing the new task convertToFixedPixelSize() at the end of level1. The flux difference come from the fact that the mean values of the optical flat are significantly different from 1, in other words it cannot be assumed by external map-makers that the pixel sizes is constant of the field of view at 3.2"/6.4 in the blue/red channel respectively. Scanamorphos and Unimap are also affected, but not JScanam that makes use of photProject. | ||||||||
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Revision 1062014-03-17 - BrunoAltieri
Revision 1052014-03-11 - BrunoAltieri
Revision 1042014-03-11 - BrunoAltieri
Revision 1032014-02-14 - BrunoAltieri
Revision 1022013-12-11 - KatrinaExter
Revision 1012013-12-11 - KatrinaExter
Revision 1002013-12-10 - KatrinaExter
Revision 992013-11-19 - BrunoAltieri
Revision 982013-11-05 - BrunoAltieri
Revision 972013-09-30 - KatrinaExter
Revision 962013-08-22 - BrunoAltieri
Revision 952013-08-22 - MarkusNielbock
Revision 942013-08-08 - KatrinaExter
Revision 932013-07-29 - BrunoAltieri
Revision 922013-07-29 - BrunoAltieri
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