SPIRE instrument and calibration web pages
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This page provides up-to-date information about using the SPIRE instrument: from preparing observations to reducing your data. This page also provides you with the latest calibration accuracies and known SPIRE calibration issues.
Documents explaining SPIRE
A quick guide to the SPIRE instrument is provided in the SPIRE fact sheet
Note that the SPIRE Spectrometer information in the fact sheet is outdate. Please use this up-to-date fact sheet
for the Spectrometer.
SPIRE Handbook and SPIRE Data Reduction Guide
Documents with relevance to the SPIRE calibration:
- Flux Calibration of Broadband Far Infrared and Submillimetre Photometric Instruments: Theory and Application to Herschel-SPIRE, Griffin et al., 2013, MNRAS, 434, 992
- Flux calibration of the Herschel-SPIRE photometer, Bendo et al., 2013, MNRAS, 433, 3062
- SPIRE point source photometry: within the Herschel interactive processing environment (HIPE), Pearson et al., 2014, ExA, 37, 175
- Systematic characterisation of the Herschel SPIRE Fourier Transform Spectrometer, Hopwood et al., 2015, MNRAS, 449, 2274
- Calibration of the Herschel SPIRE Fourier Transform Spectrometer, Swinyard et al., 2014, MNRAS, 440, 3658
- Observing extended sources with the Herschel SPIRE Fourier Transform Spectrometer, Wu et al., 2013, A&A, 556, 116
- Beam profile for the Herschel-SPIRE Fourier transform spectrometer, Makiwa et al., 2013, Applied Optics, 52, 3864
- Herschel SPIRE FTS relative spectral response calibration, Fulton et al. 2014, ExA, 37,381
- Herschel SPIRE FTS spectral mapping calibration, Benielli et al., 2014, ExA, 37, 357
- Herschel SPIRE fourier transform spectrometer: calibration of its bright-source mode, Lu et al., 2014, ExA, 37, 239
- Relative pointing offset analysis of calibration targets with repeated observations with Herschel-SPIRE Fourier-transform spectrometer, Valtchanov et al., ExA, 37, 207
- Herschel SPIRE FTS telescope model correction, Hopwood et al., 2014, ExA, 37, 195
- In-orbit performance of the Herschel/SPIRE imaging Fourier transform spectrometer: lessons learned, Naylor et al., 2014, SPIE, 9143E, 2
Some values on the performance and calibration in these papers are outdated. Please consult the latest SPIRE Data Reduction Guide
or the SPIRE Handbook
for most up to date information.
- The Herschel-SPIRE instrument and its in-flight performance, Griffin et al., 2010, A&A, 518, L3
- In-flight calibration of the Herschel-SPIRE instrument: Swinyard et al., 2010, A&A, 518, L4,
- Sensitivity of the SPIRE Detectors to Operating Parameters, Griffin M., 2007, SPIRE-UCF-DOC-002901
Detailed documents describing the pipeline algorithms:
AOT release notes
Reducing SPIRE data
Software and documentation
- We also provide access to the latest stable developer build (latest stable CIB).
- Beware These developer builds do not undergo the same in-depth testing as the user releases do. The latest developer build can be found here.
Please contact the Herschel helpdesk if you plan to use a developer build as there may be some additional information needed in order for you to properly make use of it.
- Within HIPE you can access all the SPIRE data reduction and HIPE-user documentation. The SPIRE Data Reduction Guide (SDRG) follows the user pipeline scripts and also explains the details of pipeline processing and data analysis. It is also available online here:
- SPIA: The SPIRE Photometer Interactive Analysis (SPIA) package is available in HIPE (previously it was a plugin). SPIA provides a structured GUI based access to the more intricate parts of the scan map photometer pipeline for SPIRE without the immediate need to resort to scripts. More information can be found in the SDRG or on the SPIA web page * Note: A bug that renders two deglitchers in the task spiaLevel1 unusable was found only recently. We have prepared a quick fix that will work on a standard HIPE 12.1 installation. Please see the SPIA web page for more information.
The SPIRE Launch Pads
- The SPIRE Launch Pads are single sheet quick entries (like a cheat sheet) into SPIRE data reduction and providing quick references to the relevant sections in the SPIRE Data Reduction Guide. There are launch pads for Data Access, SPIRE Photometer and Spectrometer data reduction.
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
- Subtract the Dark Sky spectrum closest to your observation (use the "Background Subtraction" script in HIPE)
- 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
Spectrometer Data Processing Issues
The SPIRE Spectrometer DP known issues listed here
Photometer data reduction
The best source of information for reducing SPIRE Photometer data is the SPIRE Data Reduction Guide
available as a standalone hyperlink document as well as 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.
Photometer Data Processing Issues
The SPIRE Photometer DP known issues listed here
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:
- You can use the
SpireMaskEditor GUI as described in Sec. 8.4 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.
- Alternatively, you can use these lines of code
- After either of those cases, you must then re-run level 1 to 2 steps on the newly modified level1 product. If your observation has been already re-reduced with HIPE 11, original and new level1s are already destriped, so you can directly run the naive map-maker on the new level1. Otherwise, you must run the destriper step: check the pipeline script for details.
Planck-HFI & Herschel-SPIRE cross calibration: absolute offset re-processing
As of HCSS 11, a new task named
is available to the users: this task calculates the absolute offset for a SPIRE map based on cross-calibration with HFI-545 and HFI-857 maps, colour-correcting HFI to SPIRE wavebands assuming a grey body function with fixed beta.
Details on how to run the task are available in the SPIRE Data Reduction Guide, Section 6.8
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.
Source Extraction and Photometry
- The current recommended method for photometry
sourceExtractorTimeline task (formerly known as the Timeline Fitter) which works on the detector timelines. The Map based algorithm
sourceExtractorSussex (SUSSEXtractor) providers good results and is useful on larger maps where the
sourceExtractorTimeline will be significantly slower.
sourceExtractorDaophot (DAOphot) also provides a reasonable estimate of the source flux but may require an aperture correction.
- Photometry on single direction fast scan parallel mode maps:
- The photometry on single scan direction fast parallel mode results in higher photometric errors of up to 5 percent for aperture photometry compared to nominal speed and cross linked maps. The best results are obtained using the Timeline Fitter. Wherever possible orthogonal and nominal direction parallel scans should be merged.
- Currently no astrometry correction is made during the merging process for parallel maps. For fast parallel mode an astrometry offset may be present which can in cases where there is a large offset, result in reduced photometers accuracy of the order of up to 25% compared to large cross-linked scan maps.
- In HIPE13 (and HIPE 11), the default 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 measured flux densities. If you use HIPE v12 we advise you to change the input PRF size using this script, in order to obtain the same photometry as in HIPE v13.
SPIRE report from the January 2013 HSC Map Making Workshop
- The official release of the report of SPIRE map-making test campaign (2013) can be downloaded as a PDF.
- A dedicated webpage to this matter is available at the NHSC website
Cookbooks are provided inside the SPIRE Data Reduction Guide (see above).
The standalone "Photometry Cookbook", is no longer maintained - it is being incorporated into the SPIRE DRG - please see the SDRG for photometry cookbook information, and raise a Helpdesk
ticket if you find something missing.
SPIRE calibration file versions
The available calibration trees for SPIRE are listed below (with the current operational version at the top).
Details of individual calibration products can be found here
- Any of the calibration trees can be retrieved in HIPE from the HSA using (e.g.)
cal = spireCal(calTree="spire_cal_13_1") etc. The default (applicable to the HIPE version in use) can be obtained with
cal = spireCal(calTree="spire_cal"). It can then be saved to a local pool right-clicking on the
cal variable and then selecting from the context menu Send To -> Local Pool.
- Alternatively, the latest calibration tree for SPIRE can be obtained as a jar file from Latest calibration trees. Then, you have to possibilities to read and save:
- The jar file can be load directly into HIPE with the command:
cal = spireCal(jarFile="PATH_TO_FILE/spire_cal_13_1.jar"). To save it to a local pool, proceed as described above, right-clicking on the
cal variable and then selecting from the context menu Send To -> Local Pool.
- The jar file can also be saved directly to a local pool without opening HIPE, running the following command in the terminal command line:
cal_import PATH_TO_FILE/spire_cal_13_1.jar. Then, to load the calibration tree in HIPE, simply type:
cal = spireCal(pool="spire_cal_13_1")
See the SPIRE Data Reduction Guide
for more details.
SPIRE calibration and performance
Photometer calibration and uncertainties
- SPIRE Photometer Calibration:
Full details of the SPIRE calibration can be found in the SPIRE Handbook and in dedicated publications: the calibration scheme is described in Griffin et al. (2013) and the implementation using Neptune as the primary calibration standard, is described in Bendo et al. (2013).
- Calibration uncertainties, which should be included in addition to the statistical errors of any measurement, are as follows:
- ± 4% absolute from Neptune model (this uncertainty is systematic and correlated across the three bands)
- ± 1.5% (random) from Neptune photometry
- Extended emission calibration
- In addition to the above uncertainties, there is an additional ±4% uncertainty due to the current uncertainty in the measured beam area
- SPIRE Photometer Beams:
- These are available in the SPIRE calibration context, at the standard map pixel size of (6,10,14) arcsec/pixel for (250,350,500) µm bands, and can be accessed in HIPE after a calibration context has been loaded (see above).
- A more detailed analysis of the SPIRE beam profile data was undertaken in 2012, leading to revised values for beam profile solid angles and derivation of a semi empirical wavelength dependent beam profile model. The results at a scale of 1 arcsec/pixel as well as the data needed for the model are available for download. A detailed description of the analysis is given as well.
- A final analysis of the SPIRE beam profiles was completed in Oct 2014, taking into account so called "shadow" observations that were taken after Neptune had moved away. This dramatically reduced the uncertainties in the beam profile solid angles to better than 1%. It also eliminated the need for a "static" part in the semi-empirical beam profile model. The results at a scale of 1 arcsec/pixel as well as the data needed for the model are available for download. A detailed description of the analysis is available too.
- SPIRE Photometer filter transmission curves:
- These are also available in the SPIRE calibration context (photRsrf) and can be accessed in HIPE after a calibration context has been loaded (See above).
- Neptune and Uranus models used for the SPIRE photometer flux calibration:
- The ESA2 models used up to HIPE v10 and
spire_cal_10_1, are available here.
- The ESA4 models used from HIPE v11 and
spire_cal_11_0, are available here.
Spectrometer calibration and uncertainties
- SPIRE Spectrometer Calibration:
Full details of the SPIRE FTS calibration can be found in the SPIRE Handbook, Swinyard et al., 2014 and Hopwood et al., 2015.
- Calibration uncertainties, which should be included in addition to the statistical errors of any measurement from HIPE v11 onwards, are as follows:
- Point sources observed on the centre detectors (SSWD4 and SLWC3): the measured repeatability is 6%, with the following contributions: (i) absolute systematic uncertainty in the models from comparison of Uranus and Neptune - determined to be ±3%; (i) the statistical repeatability determined from observations of Uranus and Neptune, with pointing corrected - estimated at ±1% (excluding the edges of the bands); (iii) the uncertainties in the instrument and telescope model, which lead to an additive continuum offset error of 0.4 Jy for SLW and 0.3 Jy for SSW and (iv) the effect of the Herschel APE.
- Sparse observations of significantly extended sources:
- the absolute uncertainty in intensity for a reasonably bright, fully extended object, observed in the central detectors is, in theory, ±1%, with the following contributions: (i) the systematic uncertainty in telescope model of 0.06%; (ii) the statistical repeatability estimated at ±1% and (iii) an additive continuum offset of 3.4x10-20 W/m2/Hz/sr for SLW and 1.1x10-19 W/m2/Hz/sr for SSW.
- In practice, truly extended sources tend to be faint and the uncertainty is therefore dominated by the additive offsets. When the source extent is larger than the main beam size, but not fully extended, or if there is structure inside the beam, then the uncertainties are dominated by the source-beam coupling (see Wu et al. 2013 ) and are significantly greater than 1%.
- Mapping mode: the variations between detectors becomes important and the overall repeatability has been measured as ±7% (see Benielli et al., 2014 for a full discussion of mapping mode observations). The off-axis detectors are less well calibrated, especially outside the unvignetted part of the field.
- Uranus model used for the SPIRE FTS point-source flux calibration:
- The ESA4 model, used from HIPE v10 onwards, is available here.
Interest groups and scripts
- The following interest groups relate to processing of observations taken with SPIRE. The links provided allow subscription to these interest groups.
- subscribe to the SPIRE Photometer interest group
- subscribe to the SPIRE and PACS parallel mode large map and point source extraction interest group
- subscribe to the SPIRE Spectrometer interest group
- subscribe to the PACS, SPIRE and HIFI spectral maps interest group
- User contributed scripts: Users are welcome to submit scripts and software that they believe could be of general interest to the community to the Herschel http://herschel.esac.esa.int/esupport/Helpdesk.
Contact the Helpdesk