Difference: SpireCalibrationWeb (98 vs. 99)

Revision 992013-10-30 - LucaConversi

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META TOPICPARENT name="WebHome"

SPIRE instrument and calibration web pages

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SPIRE Spectrometer Launch Pad version 1.7
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Photometer data reduction

 
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Overview
The best source of information for reducing SPIRE Photometer data is the SPIRE Data Reduction Guide available through the HIPE help. This runs through the User Pipeline scripts step by step, describes several other Useful Scripts, and offers advice for specific issues that might be encountered.
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Spectrometer data reduction

The best source of information for reducing SPIRE Spectrometer data is the SPIRE Data Reduction Guide available through the HIPE help. This runs through the User Pipeline scripts step by step, describes several other Useful Scripts, and offers advice for specific types of sources:

  • Faint (<10 Jy) and medium (<100 Jy) strength sources
  • Bright sources (>500 Jy)
  • Semi-extended sources
  • Spectral mapping observations
  • Observations with few repetitions

For faint sources, the subtraction of instrument, telescope and background emission is particularly important. Optimum subtraction can be performed in several ways (read the SPIRE Data Reduction Guide for details):

  1. Subtract the Dark Sky spectrum closest to your observation (use the "Background Subtraction" script in HIPE)
  2. Subtract the spectrum of surrounding detectors (use the "Background Subtraction" script in HIPE)
 
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New definition of Level-2 products
  • For versions of the HCSS prior to HIPE 10.0, a single point source calibrated (Jy/beam) map was provided in the Level 2 product for each of the PSW, PMW, PLW bands. However, for observations processed with HIPE 10.0 or later, more than one map calibration is made available within the Level 2 product. Maps are provided for the following scenarios for post HIPE v10.0 processing:
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Dark Sky observations are observed on every SPIRE Spectrometer OD, and are all public in the Archive.
 
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A listing of the available Dark Sky observations can be found here.
 
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Description New Name (HIPE10+) Original (pre-HIPE10) Name
Point Source (standard) Maps psrcPSW PSW
Extended Emission Maps extdPSW -
Solar System Object Maps ssoPSW -
Point Source Destriper Diagnostic psrcPSWdiag pddPSW
Extended Emission Destriper Diagnostic extdPSWdiag -
     
 
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  • psrcPxW are the previous PxW maps, calibrated for point source and in units of Jy/beam. Note that to do aperture photometry on such maps you'll first need to convert them to surface brightness (Jy/pixel, MJy/sr, etc.), although it is suggested to directly use the already extended emission calibrated extdPxW maps. Finally, bear in mind that SPIRE itself cannot measure the absolute sky flux, hence psrcPxW maps have an arbitrary offset having zero median.
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  • In all cases, SPIRE data is calibrated in the assumption of source having a spectral index equal to -1, i.e. νSν = const. To calibrate your data for other cases or convert to e.g. Jy/sr, please refer to section 5.7 of the SPIRE Data Reduction Guide.
 
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  • The SPIRE Photometer filter transmission curves, also known as Relative Spectral Response Functions (RSRF) are available here. For more details, please read the .readme file in this ftp folder.
 
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Photometer data reduction

 
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Data Processing Issues
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Overview

The best source of information for reducing SPIRE Photometer data is the SPIRE Data Reduction Guide available through the HIPE help. This runs through the User Pipeline scripts step by step, describes several other Useful Scripts, and offers advice for specific issues that might be encountered.

Data Processing Issues

  The main issues that you might find in your data are: undetected glitches, thermistor or detector jumps, and bad baseline removal.
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  • Quality flags in the quality context
    • Currently, the quality flags at the quality context inside the observation context are just meant for HSC/ICC internal evaluation of the quality of the products and not for the users. In case the data had some serious quality problem, the PI of the program has been contacted about it. Otherwise, only information in the quality summary, when available, should concern the observers.
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Known Issues in ODs 1304 & 1305
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Known Issues in ODs 1304 & 1305

 For (yet) unknown reasons, the three detectors PSW-B5, PSW-E9 and PSW-F8 - that use to behave well during the entire mission - were noisy during the two operational days 1304 and 1305. The result are stripes visible in the final PSW map which the current (HIPE 11) pipeline is not able to correct. The solution is to mask and exclude these detectors from the analysis. This could be done in 2 ways:
  1. You can use the SpireMaskEditor GUI as described in sec. 7.4.2 of the SPIRE Data Reduction Guide: write-click on your observation context variable and then select Level1_SpireMaskEditor and set to Master all samples in all scans (listed as BBID) for the detectors mentioned above.
  2. Alternatively, you can use these lines of code
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    * The official release of the report of SPIRE map-making test campaign (2013) can be downloaded as a PDF.
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Spectrometer data reduction

The best source of information for reducing SPIRE Spectrometer data is the SPIRE Data Reduction Guide available through the HIPE help. This runs through the User Pipeline scripts step by step, describes several other Useful Scripts, and offers advice for specific types of sources:

  • Faint (<10 Jy) and medium (<100 Jy) strength sources
  • Bright sources (>500 Jy)
  • Semi-extended sources
  • Spectral mapping observations
  • Observations with few repetitions

For faint sources, the subtraction of instrument, telescope and background emission is particularly important. Optimum subtraction can be performed in several ways (read the SPIRE Data Reduction Guide for details):

  1. Subtract the Dark Sky spectrum closest to your observation (use the "Background Subtraction" script in HIPE)
  2. Subtract the spectrum of surrounding detectors (use the "Background Subtraction" script in HIPE)

Dark Sky observations are observed on every SPIRE Spectrometer OD, and are all public in the Archive.

A listing of the available Dark Sky observations can be found here.

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Spectral Cube Analysis

Spectral cubes are produced by the Spectrometer pipeline for mapping observations. Some tips, suggestions and examples of spectral cube analysis for SPIRE data are provided here.

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