Difference: SpirePhotometerBeamProfile2 (1 vs. 6)

Revision 62017-09-15 - IvanV

Line: 1 to 1
 
META TOPICPARENT name="SpireCalibrationWeb"

SPIRE Photometer Beam Profiles

Line: 13 to 13
  The values in the first line were measured from a very finely sampled observation of Neptune as outlined below. Note that these are only accurate for a source of the same spectral shape. Since SPIRE flux densities for point sources are conventionally quoted for the reference wavelengths 250, 350, and 500 microns, assuming a source spectrum rising proportionally to wavelength (nu*F_nu=const.), we can adopt the same convention for (infinitely) extended sources. In this case the values in the second line apply. For sources of other colors a correction will have to be applied. The radial model beam profile is described in Griffin et al. 2013 and the data files given below can be used to calculate such beam profiles. This analysis showed that the static part of the model came from noise due to residual background galaxies and is not needed anymore. Rather the data show a well described fall-off with radius that is well described by a power-law. This fit is used to extrapolate beyond the measured radius.
Changed:
<
<

Normalized Beam Profile Products to Download

>
>

Normalized Beam Profiles

  The beam profile maps are available with all backgrounds subtracted and in a normalized form to the peak.

Detector Array PSW PMW PLW
Changed:
<
<
PSF with 1" pixel size and model extrapolation filling gaps and everything outside 750" radius (click on the image to enlarge)
PSF with 1" pixels as FITS file FITS file FITS file FITS file
PSF with standard pixel size (6", 10", 14") and model extrapolation filling gaps and everything outside 750" radius (click on the image to enlarge)
PSF with standard pixel size as FITS file FITS file FITS file FITS file
>
>
PSF with 1" pixel size and model extrapolation filling gaps and everything outside 750" radius (click on the image to enlarge)
PSF with 1" pixels as FITS file FITS file FITS file FITS file
PSF with standard pixel size (6", 10", 14") and model extrapolation filling gaps and everything outside 750" radius (click on the image to enlarge)
PSF with standard pixel size as FITS file FITS file FITS file FITS file
 These files can also be found in the photometer calibration context of a SPIRE observation.

Radial Beam Profile Model

Datasets to construct the radial beam profile model are available below. These allow to take into account the color dependent FWHM of the true beam profiles.

Changed:
<
<
An updated implementation of the beam profile model in IDL is available for download.
>
>
An updated implementation of the beam profile model in IDL is available for download.
  The radial beam profile model for SPIRE was developed and described by Griffin et al. 2013.
Changed:
<
<
Taking the shadow observations into account revealed that the wavelength independent component of the model was just noise from residual background galaxies. The shadow observation allowed an almost complete subtraction, making this part obsolete. The updated IDL model reflects this accordingly and we correct the formula for the peak normalized monochromatic flux, depending on the distance from the peak (Theta), as follows:
>
>
Taking the shadow observations into account revealed that the wavelength independent component of the model was just noise from residual background galaxies. The shadow observation allowed an almost complete subtraction, making this part obsolete. The updated IDL model reflects this accordingly and we correct the formula for the peak normalized monochromatic flux, depending on the distance from the peak (Theta), as follows:
 
Changed:
<
<
>
>
RadialBeamProfileModelFinal
  A value of -0.85 is adopted for gamma, which controls the dependence of the FWHM of the variable part of the beam on wavelength. The reference frequency nu_eff is the isophotal frequency for the product of the spectrum of Neptune and the respective SPIRE spectral filter profile. The frequencies 1224.0683, 873.06788, 609.86168 GHz for PSW, PMW, PLW respectively make the model beam profile consistent with the measured Neptune beam using the spectral indices 1.29, 1.42, 1.47 respectively to describe the Neptune SED in the three filter bands. For verification run the test procedure "test_hs_broadbpsf", returning the following table in excellent agreement with the measured values:
Line: 46 to 46
 
Radial beam profile model Values are given for radii in 1 arcsec steps starting at 0
Detector Radial beam profile
Changed:
<
<
PSW point_src_sim_PSW.fits.gz
PMW point_src_sim_PMW.fits.gz
PLW point_src_sim_PLW.fits.gz
>
>
PSW point_src_sim_PSW.fits.gz
PMW point_src_sim_PMW.fits.gz
PLW point_src_sim_PLW.fits.gz
 
Changed:
<
<
Updated IDL model
>
>
Updated IDL model
 

Analysis Details

Changed:
<
<
The interested reader can find a detailed description of the data analysis that led to the data products on this page.
>
>
The interested reader can find a detailed description of the data analysis that led to the data products.

META FILEATTACHMENT attachment="RadialBeamProfileModelFinal.png" attr="" comment="" date="1505465120" name="RadialBeamProfileModelFinal.png" path="RadialBeamProfileModelFinal.png" size="15662" user="IvanV" version="1"

Revision 52016-04-13 - IvanV

Line: 1 to 1
 
META TOPICPARENT name="SpireCalibrationWeb"

SPIRE Photometer Beam Profiles

Line: 19 to 19
 
Detector Array PSW PMW PLW
Changed:
<
<
PSF with 1" pixel size and model extrapolation filling gaps and everything outside 750" radius (click on the image to enlarge)
PSF with 1" pixels as FITS file FITS file FITS file FITS file
PSF with standard pixel size (6", 10", 14") and model extrapolation filling gaps and everything outside 750" radius (click on the image to enlarge)
PSF with standard pixel size as FITS file FITS file FITS file FITS file
>
>
PSF with 1" pixel size and model extrapolation filling gaps and everything outside 750" radius (click on the image to enlarge)
PSF with 1" pixels as FITS file FITS file FITS file FITS file
PSF with standard pixel size (6", 10", 14") and model extrapolation filling gaps and everything outside 750" radius (click on the image to enlarge)
PSF with standard pixel size as FITS file FITS file FITS file FITS file
 These files can also be found in the photometer calibration context of a SPIRE observation.

Radial Beam Profile Model

Line: 46 to 46
 
Radial beam profile model Values are given for radii in 1 arcsec steps starting at 0
Detector Radial beam profile
Changed:
<
<
PSW point_src_sim_PSW.fits
PMW point_src_sim_PMW.fits
PLW point_src_sim_PLW.fits
>
>
PSW point_src_sim_PSW.fits.gz
PMW point_src_sim_PMW.fits.gz
PLW point_src_sim_PLW.fits.gz
 
Changed:
<
<
Updated IDL model
>
>
Updated IDL model
 

Analysis Details

The interested reader can find a detailed description of the data analysis that led to the data products on this page.

Deleted:
<
<
-- BernhardSchulz - 19 Mar 2015

Revision 42015-10-08 - BernhardSchulz

Line: 1 to 1
 
META TOPICPARENT name="SpireCalibrationWeb"

SPIRE Photometer Beam Profiles

Changed:
<
<
Final beam profile derivation including shadow maps ( Bernhard Schulz, October 2014)
>
>
Final beam profile derivation including shadow maps including HIPE 14 update ( Bernhard Schulz, October 2015)
 

SPIRE Photometer Solid Angles

Solid angles in [arcsec^2] PSW PMW PLW
Changed:
<
<
Measured with Neptune spectrum 454+/-1 803+/-4 1687+/-12
SPIRE photometer reference spectrum (nu*F_nu = const.) 470+/-1 832+/-4 1793+/-12
>
>
Measured with Neptune spectrum 454.0+/-1.2 803.4+/-3.8 1700.0+/-13
SPIRE photometer reference spectrum (nu*F_nu = const.) 469.3+/-1.2 831.4+/-3.8 1804.3+/-13
  The values in the first line were measured from a very finely sampled observation of Neptune as outlined below. Note that these are only accurate for a source of the same spectral shape. Since SPIRE flux densities for point sources are conventionally quoted for the reference wavelengths 250, 350, and 500 microns, assuming a source spectrum rising proportionally to wavelength (nu*F_nu=const.), we can adopt the same convention for (infinitely) extended sources. In this case the values in the second line apply. For sources of other colors a correction will have to be applied. The radial model beam profile is described in Griffin et al. 2013 and the data files given below can be used to calculate such beam profiles. This analysis showed that the static part of the model came from noise due to residual background galaxies and is not needed anymore. Rather the data show a well described fall-off with radius that is well described by a power-law. This fit is used to extrapolate beyond the measured radius.
Line: 19 to 19
 
Detector Array PSW PMW PLW
Changed:
<
<
PSF with 1" pixel size and model extrapolation filling gaps and everything outside 750" radius (click on the image to enlarge)
PSF with 1" pixels as FITS file FITS file FITS file FITS file
PSF with standard pixel size (6", 10", 14") and model extrapolation filling gaps and everything outside 750" radius (click on the image to enlarge)
PSF with standard pixel size as FITS file FITS file FITS file FITS file
>
>
PSF with 1" pixel size and model extrapolation filling gaps and everything outside 750" radius (click on the image to enlarge)
PSF with 1" pixels as FITS file FITS file FITS file FITS file
PSF with standard pixel size (6", 10", 14") and model extrapolation filling gaps and everything outside 750" radius (click on the image to enlarge)
PSF with standard pixel size as FITS file FITS file FITS file FITS file
 These files can also be found in the photometer calibration context of a SPIRE observation.
Deleted:
<
<
 

Radial Beam Profile Model

Datasets to construct the radial beam profile model are available below. These allow to take into account the color dependent FWHM of the true beam profiles.

Line: 30 to 28
 

Radial Beam Profile Model

Datasets to construct the radial beam profile model are available below. These allow to take into account the color dependent FWHM of the true beam profiles.

Changed:
<
<
An updated implementation of the beam profile model in IDL is available for download.
>
>
An updated implementation of the beam profile model in IDL is available for download.
  The radial beam profile model for SPIRE was developed and described by Griffin et al. 2013.
Changed:
<
<
Taking the shadow observations into account revealed that the wavelength independent component of the model was just noise from residual background galaxies. The shadow observation allowed an almost complete subtraction, making this part obsolete. The updated IDL model reflects this accordingly and we correct the formula for the peak normalized monochromatic flux, depending on the distance from the peak (Theta), as follows:
>
>
Taking the shadow observations into account revealed that the wavelength independent component of the model was just noise from residual background galaxies. The shadow observation allowed an almost complete subtraction, making this part obsolete. The updated IDL model reflects this accordingly and we correct the formula for the peak normalized monochromatic flux, depending on the distance from the peak (Theta), as follows:
 
Changed:
<
<
>
>
  A value of -0.85 is adopted for gamma, which controls the dependence of the FWHM of the variable part of the beam on wavelength. The reference frequency nu_eff is the isophotal frequency for the product of the spectrum of Neptune and the respective SPIRE spectral filter profile. The frequencies 1224.0683, 873.06788, 609.86168 GHz for PSW, PMW, PLW respectively make the model beam profile consistent with the measured Neptune beam using the spectral indices 1.29, 1.42, 1.47 respectively to describe the Neptune SED in the three filter bands. For verification run the test procedure "test_hs_broadbpsf", returning the following table in excellent agreement with the measured values:

Modeled solid angles in [arcsec^2] PSW PMW PLW
Changed:
<
<
Neptune spectrum 454 803 1687
SPIRE photometer reference spectrum (nu*F_nu = const.) 470 832 1793
>
>
Neptune spectrum 454 803 1700
SPIRE photometer reference spectrum (nu*F_nu = const.) 469 831 1804
*These values were updated for the HIPE 14 calibration mainly due to a normalization issue of the PLW beam.
 
Radial beam profile model Values are given for radii in 1 arcsec steps starting at 0
Detector Radial beam profile
Changed:
<
<
PSW point_src_sim_PSW.fits
PMW point_src_sim_PMW.fits
PLW point_src_sim_PLW.fits
>
>
PSW point_src_sim_PSW.fits
PMW point_src_sim_PMW.fits
PLW point_src_sim_PLW.fits
 
Changed:
<
<
Updated IDL model
>
>
Updated IDL model
 

Analysis Details

Deleted:
<
<
The interested reader can find a detailed description of the data analysis that led to the data products on this page.
 
Added:
>
>
The interested reader can find a detailed description of the data analysis that led to the data products on this page.
  -- BernhardSchulz - 19 Mar 2015 \ No newline at end of file

Revision 32015-03-20 - BernhardSchulz

Line: 1 to 1
 
META TOPICPARENT name="SpireCalibrationWeb"

SPIRE Photometer Beam Profiles

Final beam profile derivation including shadow maps ( Bernhard Schulz, October 2014)
Line: 35 to 35
 The radial beam profile model for SPIRE was developed and described by Griffin et al. 2013. Taking the shadow observations into account revealed that the wavelength independent component of the model was just noise from residual background galaxies. The shadow observation allowed an almost complete subtraction, making this part obsolete. The updated IDL model reflects this accordingly and we correct the formula for the peak normalized monochromatic flux, depending on the distance from the peak (Theta), as follows:
Changed:
<
<
>
>
  A value of -0.85 is adopted for gamma, which controls the dependence of the FWHM of the variable part of the beam on wavelength. The reference frequency nu_eff is the isophotal frequency for the product of the spectrum of Neptune and the respective SPIRE spectral filter profile. The frequencies 1224.0683, 873.06788, 609.86168 GHz for PSW, PMW, PLW respectively make the model beam profile consistent with the measured Neptune beam using the spectral indices 1.29, 1.42, 1.47 respectively to describe the Neptune SED in the three filter bands. For verification run the test procedure "test_hs_broadbpsf", returning the following table in excellent agreement with the measured values:

Revision 22015-03-20 - BernhardSchulz

Line: 1 to 1
 
META TOPICPARENT name="SpireCalibrationWeb"
Deleted:
<
<

THIS PAGE IS UNDER CONSTRUCTION

 

SPIRE Photometer Beam Profiles

Final beam profile derivation including shadow maps ( Bernhard Schulz, October 2014)
Line: 21 to 19
 
Detector Array PSW PMW PLW
Changed:
<
<
PSF limited to 700" radius (click on the image to enlarge)
PSF as FITS file FITS file FITS file FITS file

Note that the position angle keyword posAngle is not set in the FITS headers. This is the position angle of the Z-axis of the spacecraft coordinate system projected onto the sky at the time of the observation. The Z-axis runs parallel to the short side of the SPIRE photometer FOV. For these observations the position angle is 250.6 degrees.

>
>
PSF with 1" pixel size and model extrapolation filling gaps and everything outside 750" radius (click on the image to enlarge)
PSF with 1" pixels as FITS file FITS file FITS file FITS file
PSF with standard pixel size (6", 10", 14") and model extrapolation filling gaps and everything outside 750" radius (click on the image to enlarge)
PSF with standard pixel size as FITS file FITS file FITS file FITS file
These files can also be found in the photometer calibration context of a SPIRE observation.
 

Radial Beam Profile Model

Datasets to construct the radial beam profile model are available below. These allow to take into account the color dependent FWHM of the true beam profiles.

Changed:
<
<
An implementation of the beam profile model in IDL is available for download.
>
>
An updated implementation of the beam profile model in IDL is available for download.
 
Changed:
<
<
The radial beam profile model for SPIRE was developed and described by Griffin et al. 2013. The peak normalized monochromatic flux, depending on the distance from the peak (Theta) can be described as:
>
>
The radial beam profile model for SPIRE was developed and described by Griffin et al. 2013. Taking the shadow observations into account revealed that the wavelength independent component of the model was just noise from residual background galaxies. The shadow observation allowed an almost complete subtraction, making this part obsolete. The updated IDL model reflects this accordingly and we correct the formula for the peak normalized monochromatic flux, depending on the distance from the peak (Theta), as follows:
 
Changed:
<
<

A value of -0.85 should be adopted for gamma, which controls the dependence of the FWHM of the variable part of the beam on wavelength. The reference frequency nu_eff is the isophotal frequency for the product of the spectrum of Neptune and the respective SPIRE spectral filter profile. The frequencies 1217.27, 867.75, 610.87 GHz for PSW, PMW, PLW respectively make the model beam profile consistent with the measured Neptune beam using the spectral indices 1.29, 1.42, 1.47 respectively to describe the Neptune SED in the three filter bands.

>
>
 
Added:
>
>
A value of -0.85 is adopted for gamma, which controls the dependence of the FWHM of the variable part of the beam on wavelength. The reference frequency nu_eff is the isophotal frequency for the product of the spectrum of Neptune and the respective SPIRE spectral filter profile. The frequencies 1224.0683, 873.06788, 609.86168 GHz for PSW, PMW, PLW respectively make the model beam profile consistent with the measured Neptune beam using the spectral indices 1.29, 1.42, 1.47 respectively to describe the Neptune SED in the three filter bands. For verification run the test procedure "test_hs_broadbpsf", returning the following table in excellent agreement with the measured values:
 
Changed:
<
<
PLW PLW_Core.csv PLW_Constant.csv
Radial beam profile model Values are given for radii in 1 arcsec steps starting at 0
Detector Core (variable) part Constant part
PSW PSW_Core.csv PSW_Constant.csv
PMW PMW_Core.csv PMW_Constant.csv
>
>
Modeled solid angles in [arcsec^2] PSW PMW PLW
Neptune spectrum 454 803 1687
SPIRE photometer reference spectrum (nu*F_nu = const.) 470 832 1793
 
Added:
>
>
PLW point_src_sim_PLW.fits
Radial beam profile model Values are given for radii in 1 arcsec steps starting at 0
Detector Radial beam profile
PSW point_src_sim_PSW.fits
PMW point_src_sim_PMW.fits
 
Deleted:
<
<
Solid angles derived from integrating this radial beam profile model over area and frequency were consistent with the numbers above within 1.5%.
 
Added:
>
>
Updated IDL model
 

Analysis Details

Changed:
<
<
The interested reader can find a detailed description of the data analysis that led to the data products on this page.
>
>
The interested reader can find a detailed description of the data analysis that led to the data products on this page.
 

-- BernhardSchulz - 19 Mar 2015 \ No newline at end of file

Revision 12015-03-19 - BernhardSchulz

Line: 1 to 1
Added:
>
>
META TOPICPARENT name="SpireCalibrationWeb"

THIS PAGE IS UNDER CONSTRUCTION

SPIRE Photometer Beam Profiles

Final beam profile derivation including shadow maps ( Bernhard Schulz, October 2014)

SPIRE Photometer Solid Angles

Solid angles in [arcsec^2] PSW PMW PLW
SPIRE photometer reference spectrum (nu*F_nu = const.) 470+/-1 832+/-4 1793+/-12
Measured with Neptune spectrum 454+/-1 803+/-4 1687+/-12

The values in the first line were measured from a very finely sampled observation of Neptune as outlined below. Note that these are only accurate for a source of the same spectral shape. Since SPIRE flux densities for point sources are conventionally quoted for the reference wavelengths 250, 350, and 500 microns, assuming a source spectrum rising proportionally to wavelength (nu*F_nu=const.), we can adopt the same convention for (infinitely) extended sources. In this case the values in the second line apply. For sources of other colors a correction will have to be applied. The radial model beam profile is described in Griffin et al. 2013 and the data files given below can be used to calculate such beam profiles. This analysis showed that the static part of the model came from noise due to residual background galaxies and is not needed anymore. Rather the data show a well described fall-off with radius that is well described by a power-law. This fit is used to extrapolate beyond the measured radius.

Normalized Beam Profile Products to Download

The beam profile maps are available with all backgrounds subtracted and in a normalized form to the peak.

Detector Array PSW PMW PLW
PSF as FITS file FITS file FITS file FITS file
PSF limited to 700" radius (click on the image to enlarge)

Note that the position angle keyword posAngle is not set in the FITS headers. This is the position angle of the Z-axis of the spacecraft coordinate system projected onto the sky at the time of the observation. The Z-axis runs parallel to the short side of the SPIRE photometer FOV. For these observations the position angle is 250.6 degrees.

Radial Beam Profile Model

Datasets to construct the radial beam profile model are available below. These allow to take into account the color dependent FWHM of the true beam profiles. An implementation of the beam profile model in IDL is available for download.

The radial beam profile model for SPIRE was developed and described by Griffin et al. 2013. The peak normalized monochromatic flux, depending on the distance from the peak (Theta) can be described as:

A value of -0.85 should be adopted for gamma, which controls the dependence of the FWHM of the variable part of the beam on wavelength. The reference frequency nu_eff is the isophotal frequency for the product of the spectrum of Neptune and the respective SPIRE spectral filter profile. The frequencies 1217.27, 867.75, 610.87 GHz for PSW, PMW, PLW respectively make the model beam profile consistent with the measured Neptune beam using the spectral indices 1.29, 1.42, 1.47 respectively to describe the Neptune SED in the three filter bands.

PLW PLW_Core.csv PLW_Constant.csv
Radial beam profile model Values are given for radii in 1 arcsec steps starting at 0
Detector Core (variable) part Constant part
PSW PSW_Core.csv PSW_Constant.csv
PMW PMW_Core.csv PMW_Constant.csv

Solid angles derived from integrating this radial beam profile model over area and frequency were consistent with the numbers above within 1.5%.

Analysis Details

The interested reader can find a detailed description of the data analysis that led to the data products on this page.

-- BernhardSchulz - 19 Mar 2015

 
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