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Table 1: Observation IDs, times and positions of all six maps.

The last two "shadow" observations were made after Neptune had left the region 3 years later at about the same time of year to ensure the same observing geometry w.r.t the Zodiacal cloud. These were performed in a non-moving reference frame with the same narrow scan pattern as the Neptune observations. Each scan direction was executed only once. The duration of each map was equivalent to the corresponding ones on Neptune, i.e. spending a total of half the observing time that was used on Neptune.

(bis hier!)

HIPE 9.0.1782 and SPIA 1.8 were used. The map reconstruction was performed after median subtraction excluding a radius of 4 arcmin around the source. The maps have 1 arcsec sky bin size. Pointing for Neptune proper motion was corrected. The resulting original files are:

Array | Image | FITS |
---|---|---|

PSW | 0x5000241aL_PLW_pmcorr_1arcsec.fits | |

PSW | 0x5000241aL_PSW_pmcorr_1arcsec.fits | |

PSW | 0x5000241aL_PMW_pmcorr_1arcsec.fits |

Complications that arise when using these maps directly for derivation of beam profiles and solid angles were discussed in a presentation and led to a few corrections as follows.

0x5000241aL_PLW_pmcorr_1arcsec_bgfit.fits |

0x5000241aL_PSW_pmcorr_1arcsec_bgfit.fits |

0x5000241aL_PMW_pmcorr_1arcsec_bgfit.fits |

Overlaying the ecliptic coordinate system over the background fit (contours) shows that a an interpretation by a Zodiacal light gradient is at least qualitatively consistent.

Using IRSKY to obtain a rough estimate through extrapolation of its Zodiacal model to SPIRE wavelengths at the position of the observation and one degree towards the ecliptic pole, the following gradients were obtained.

Gradient over 0.4 deg | 0.085 | 0.108 | 0.252 |

PSW | PMW | PLW | |
---|---|---|---|

IRSKY Model Result | |||

Difference over 1 degree [MJy/sr] | 0.050 | 0.020 | 0.011 |

Gradient in [mJy/beam/deg] | 0.51 | 0.20 | 0.11 |

Fitted Background Map Result |

Array | Before Removal | After Removal | Source Positions |
---|---|---|---|

PLW | |||

PSW | |||

PMW |

neptune_omega_PLW4.pdf |

neptune_omega_PSW4.pdf |

neptune_omega_PMW4.pdf |

This map shows green rings at 600, 650, and 1000 arcsec radius. The maps become less reliable outside of about 700 arcsec due to decreasing coverage and S/N. The background seems to rise again in the plots of average annular signal vs. radius, which is likely to be due to the lower coverage.

The diagrams showing solid angle vs. radius show a plateau around 600 arcsec which may signal the end of significant contribution from the beam profile. At different integration radii, the following values in arcsec^2 result:

new analysis | 450 | 795 | 1665 | 600'' |
---|---|---|---|---|

PSW | PMW | PLW | Integration radius | |

analysis North&Griffin | 433 | 777 | 1632 | 500'' |

new analysis | 462 | 825 | 1690 | 1000'' |

These data are between 3.6 and 6.7% different from the North&Griffin numbers for 1000 arcsec integration radius and between 2.0 and 3.9% for 600 arcsec integration radius.

SPIRE plans to conduct shadow observations of the same region on the sky without Neptune in it in the fall of 2012. These will be used to determine whether the apparent rise outside 700 arcsec is real and they will improve the accuracy of the background level determination substantially, especially for the longer wavelength observations.

A presentation of this data was given to the HCalSG, the Hfi/Spire Cross Calibration Group and the SDAG.

Another presentation was given at the SDAG, which discussed various sources of uncertainties and concluded that an error of +/- 4% is a conservative estimate at this time.

It is important to point out that solid angles are color dependent. The FWHM of the beam varies with frequency proportional to nu^gamma. The most recent estimate from Griffin (priv. comm) for gamma is 0.78, 0.85, 0.85, respectively for PSW, PMW and PLW.

As the beam profiles and the solid angles were derived from a map of Neptune, there is a discrepancy to the n*Fnu = const. spectrum that all photometry is color corrected for.

To determine the magnitude of this variation, a radial beam profile model was derived from the final background subtracted 2D beam profiles, following the idea in Griffin et al. 2013. The radial beam profiles (download page) are split up into a constant and a variable core part whose radial scale varies with nu^gamma as mentioned above. The solid angle can be found by integrating the product of beam profile, relative spectral response function (RSRF) and source spectrum over radius and wavelength and dividing by the integral over RSRF and source spectrum. The source spectrum for Neptune was approximated by a power law with exponent -1.39. The ratio of the solid angles found for the Neptune power law and a power law with exponent -1 was used to correct the Neptune solid angles to the standard SPIRE reference spectrum.

Solid angles in [arcsec^2] | PSW | PMW | PLW |
---|---|---|---|

SPIRE photometer reference spectrum (nu*F_nu = const.) | 465 | 822 | 1768 |

Measured with Neptune spectrum | 450 | 795 | 1665 |

Summary of derived solid angles for Neptune spectrum and a standard reference spectum. Different numbers apply for other colors.

This diagram shows the frequency dependency of the solid angles of PSW, PMW, and PLW in comparison to conveniently scaled power law curves with different exponents.

Array | All data after background removal | PSF filtered and limited to 700" radius |
---|---|---|

PLW | ||

PSW | ||

PMW |

-- BernhardSchulz - 19 Mar 2015

Topic revision: r2 - 2015-03-20 - BernhardSchulz