Index of /hsa/legacy/HPDP/SPIRE/SPIRE-S/cal_targets

[ICO]NameLast modifiedSizeDescription

[DIR]Parent Directory  -  
[TXT]README.html02-Oct-2017 17:02 4.6K 
[TXT]SPIREspec_HPDP_calibrators_releaseNote.txt15-Dec-2016 09:01 3.7K 
[   ]SPIREspec_calibrators.tar.gz16-Dec-2016 16:37 23M 
[DIR]SPIREspec_calibrators/16-Dec-2016 16:37 -  
[TXT]observationList.csv15-Dec-2016 08:12 7.0K 
[DIR]postcards/15-May-2017 10:20 -  

SPIRE Spectrometer HPDP: Observations of the Spectrometer calibrators

Rosalind Hopwood

ESAC SPIRE Instrument and Calibration Scientist

13th December 2016, v1

Abstract

During Herschel’s mission the SPIRE Spectrometer took repeated observations of several calibration sources. Full details of the systematic programme of calibration observation can be found in Hopwood et al. 2015. Some of the data used in that paper received post-pipeline processing and where the quality of the data were improved (over the standard products available in the Herschel Science Archive, HSA), therefore these are provided as HPDPs.

Description of HPDP

Point-source calibrated high resolution SPIRE Spectrometer spectra of the primary and secondary calibration sources, which have received post-pipeline correction.

There are up to three corrections for each observation. 1. Correction for pointing offset, where the offset was assessed using the relative method described in Valtchanov et al. 2014. 2. Correction for partial extent, which was corrected using the Semi Extended Correction Tool in HIPE. 3. Removal of high-background emission, which was subtracted using the average spectra of off-axis detectors.

The CSV file “observationList.csv” lists the source name, observation and which of the corrections have been applied to the HPDP as

  1. “pointingOffsetCorr” for pointing offset correction
  2. “SECT” for semi-extended morphology correction
  3. “backgroundSubtracted” where background emission has been subtracted

These HPDPs were reduced with HIPE version 13, using spire_cal_13_1 and are presented in the standard pipeline generation final product form for sparse-mode SPIRE Spectrometer observations.

The data provided were all observed in high-resolution mode and are point-source calibrated in units of Jy. Any low resolution or extended-source calibrated data used in Hopwood et al. 2015 are not provided, as there were significant improvements to the associated calibration in HIPE version 14 (see Marchili et al. 2017 and Valtchanov et al. in preparation).

Each HPDP is provided as an individual gzipped FITS file in folder SPIREspec_calibrators, and are named as follows.

The prefix convention is:

OBSID_spectrometerCalibrator_, where OBSID is the observation ID number.

The suffix of the file depends on which of the three corrections have been applied:

For example, if the observation has been corrected for pointing offset and a high background the associated file name will be:

OBSID_spectrometerCalibrator_pointOffCorr_BGS.fits.gz

For several of the HPDPs, a further issue is addressed. There were a number of observations that tested the beam steering mirror, by using two different mirror angles within the same observation. These observations are not properly calibrated in the HSA, but were included in Hopwood et al. 2015, and are therefore provided with these HPDPs.

For such observations there are two products, where one filename has the suffix “bsmTwin1” and the second “bsmTwin2”. The calibration observations which are affected and included in this set of HPDPs are:

1342237017
1342246285
1342246280
1342227778

The corresponding HPDPs’s metadata may not be complete with respect to the metadata of HIPE v14.1 reduced data found in the archive.

The file size ranges from 113 to 208 KB.

All FITS files from folder SPIREspec_calibrators are also combined in a single tar.gz file.

The folder postcards contains the comparison of the current products in the Herschel Science Archive and this HPDP.

Purpose

These data have been made available as they improve on the standard products available in the HSA.

Caveats

Only the centre detectors of the bolometer arrays are present (SLWC3 and SSWD4).