Difference between revisions of "Planets related data"
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| − | + | The planet flux density measurements are described in a paper that is available on the arXiv: https://arxiv.org/abs/1612.07151 | |
| − | + | The raw data can be downloaded [[:File:Pla_v2.gz|here]]. The interpretation of these data should become apparent from reading the paper. However, the following list aims to provide accurate descriptions of each of the parameters that we provide. For any questions, please contact the corresponding author, Jon E. Gudmundsson: jon.gudmundsson@fysik.su.se / jegudmunds@gmail.com | |
| − | |||
| − | The data can be downloaded [[:File:Pla_v2.gz|here]]. The interpretation of these data should become apparent from reading the paper. However, | ||
| − | |||
| − | For any questions, please contact the corresponding author, Jon | ||
| − | E. Gudmundsson | ||
The results are contained in [[:File:Pla_v2.gz|21 data files]], one file for each planet observation made by Planck HFI. Each file contains 13 data columns. These data should allow the reader to reconstruct the Planck-HFI estimates of planet spectral radiance as well as associated uncertainties, both statistical and systematic. | The results are contained in [[:File:Pla_v2.gz|21 data files]], one file for each planet observation made by Planck HFI. Each file contains 13 data columns. These data should allow the reader to reconstruct the Planck-HFI estimates of planet spectral radiance as well as associated uncertainties, both statistical and systematic. | ||
The columns are: | The columns are: | ||
| − | |||
* '''Channel''' : The Planck-HFI detector name. | * '''Channel''' : The Planck-HFI detector name. | ||
* '''obs tims''' : The observation time [MJD] corresponding to the time when this detector is centred on the planet. | * '''obs tims''' : The observation time [MJD] corresponding to the time when this detector is centred on the planet. | ||
| − | * '''RA''' : Astrometric right ascension (ICRF/J2000) ephmeris corresponding to the location of the planet at the time of observation. Observer location is set to: Planck Space Observatory [500@-489] | + | * '''RA''' : Astrometric right ascension (ICRF/J2000) ephmeris corresponding to the location of the planet at the time of observation. <BR>Observer location is set to: Planck Space Observatory [500@-489] |
| − | * '''DEC''' : Astrometric declination (ICRF/J2000) ephmeris corresponding to the location of the planet at the time of observation. Observer location is set to: Planck Space Observatory [500@-489] | + | * '''DEC''' : Astrometric declination (ICRF/J2000) ephmeris corresponding to the location of the planet at the time of observation. <BR>Observer location is set to: Planck Space Observatory [500@-489] |
| − | * '''pda''' : Solid angle [arcsec^2] of the planet used in the brightness analysis. This corresponds to $\Omega _\mathrm{p}$ in the paper (see discussion in Section 2.1). | + | * '''pda''' : Solid angle [arcsec^2] of the planet used in the brightness analysis. <BR>This corresponds to $\Omega _\mathrm{p}$ in the paper (see discussion in Section 2.1). |
* '''dpda''' : Assumed error in planet solid angle [arcsec^2]. | * '''dpda''' : Assumed error in planet solid angle [arcsec^2]. | ||
| − | * '''T''' : Planet thermodynamic temperature [K] (see definition in paper) at the band reference frequency corresponding to 100, 143, 217, 353, 545, or 857 GHz (see discussion in Section 2.1). | + | * '''T''' : Planet thermodynamic temperature [K] (see definition in paper) at the band reference frequency <BR>corresponding to 100, 143, 217, 353, 545, or 857 GHz (see discussion in Section 2.1). |
* '''dT1''' : Statistical uncertainty in the determination of the thermodynamic temperature [K]. | * '''dT1''' : Statistical uncertainty in the determination of the thermodynamic temperature [K]. | ||
* '''dT2''' : Systematic uncertainty in the determination of the thermodynamic temperature [K]. | * '''dT2''' : Systematic uncertainty in the determination of the thermodynamic temperature [K]. | ||
| − | * '''flux''' : | + | * '''flux''' : Flux density [Jy] estimate at the reference frequency found by calculating the product of the planet <BR>solid angle and the Planck blackbody formula with the planet thermodynamic temperature and reference frequency as inputs. |
* '''dflux1''' : Statistical uncertainty in flux density [Jy]. | * '''dflux1''' : Statistical uncertainty in flux density [Jy]. | ||
* '''dflux2''' : Systematic uncertainty in flux density [Jy]. | * '''dflux2''' : Systematic uncertainty in flux density [Jy]. | ||
| − | * '''beam''' : Scanning beam solid angle [arcmin^2] used for this channel. This corresponds to $\Omega _\mathrm{b}$ in the paper (see discussion in Section 2.1). | + | * '''beam''' : Scanning beam solid angle [arcmin^2] used for this channel. <BR>This corresponds to $\Omega _\mathrm{b}$ in the paper (see discussion in Section 2.1). |
| − | * '''kappa1''' : Colour correction coefficient appropriate for this detector and planet. This corresponds to $\kappa _1$ in the paper (see definition in Section 2.1). | + | * '''kappa1''' : Colour correction coefficient appropriate for this detector and planet. <BR>This corresponds to $\kappa _1$ in the paper (see definition in Section 2.1). |
| − | * '''kappa2''' : Colour correction coefficient appropriate for this detector and planet. This corresponds to $\kappa _2$ in the paper (see definition in Section 2.1). | + | * '''kappa2''' : Colour correction coefficient appropriate for this detector and planet. <BR>This corresponds to $\kappa _2$ in the paper (see definition in Section 2.1). |
Revision as of 09:12, 22 December 2016
The planet flux density measurements are described in a paper that is available on the arXiv: https://arxiv.org/abs/1612.07151
The raw data can be downloaded here. The interpretation of these data should become apparent from reading the paper. However, the following list aims to provide accurate descriptions of each of the parameters that we provide. For any questions, please contact the corresponding author, Jon E. Gudmundsson: jon.gudmundsson@fysik.su.se / jegudmunds@gmail.com
The results are contained in 21 data files, one file for each planet observation made by Planck HFI. Each file contains 13 data columns. These data should allow the reader to reconstruct the Planck-HFI estimates of planet spectral radiance as well as associated uncertainties, both statistical and systematic.
The columns are:
* Channel : The Planck-HFI detector name. * obs tims : The observation time [MJD] corresponding to the time when this detector is centred on the planet. * RA : Astrometric right ascension (ICRF/J2000) ephmeris corresponding to the location of the planet at the time of observation.
Observer location is set to: Planck Space Observatory [500@-489] * DEC : Astrometric declination (ICRF/J2000) ephmeris corresponding to the location of the planet at the time of observation.
Observer location is set to: Planck Space Observatory [500@-489] * pda : Solid angle [arcsec^2] of the planet used in the brightness analysis.
This corresponds to $\Omega _\mathrm{p}$ in the paper (see discussion in Section 2.1). * dpda : Assumed error in planet solid angle [arcsec^2]. * T : Planet thermodynamic temperature [K] (see definition in paper) at the band reference frequency
corresponding to 100, 143, 217, 353, 545, or 857 GHz (see discussion in Section 2.1). * dT1 : Statistical uncertainty in the determination of the thermodynamic temperature [K]. * dT2 : Systematic uncertainty in the determination of the thermodynamic temperature [K]. * flux : Flux density [Jy] estimate at the reference frequency found by calculating the product of the planet
solid angle and the Planck blackbody formula with the planet thermodynamic temperature and reference frequency as inputs. * dflux1 : Statistical uncertainty in flux density [Jy]. * dflux2 : Systematic uncertainty in flux density [Jy]. * beam : Scanning beam solid angle [arcmin^2] used for this channel.
This corresponds to $\Omega _\mathrm{b}$ in the paper (see discussion in Section 2.1). * kappa1 : Colour correction coefficient appropriate for this detector and planet.
This corresponds to $\kappa _1$ in the paper (see definition in Section 2.1). * kappa2 : Colour correction coefficient appropriate for this detector and planet.
This corresponds to $\kappa _2$ in the paper (see definition in Section 2.1).
(Planck) High Frequency Instrument
