Planck intermediate results: LII. Planet flux densities

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Planck intermediate results : LII. Planet flux densities. / Akrami, Y.; Ashdown, M.; Aumont, J.; Baccigalupi, C.; Ballardini, M.; Banday, A. J.; Barreiro, R. B.; Bartolo, N.; Basak, S.; Benabed, K.; Bernard, J. P.; Bersanelli, M.; Bielewicz, P.; Bonavera, L.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Bucher, M.; Burigana, C.; Butler, R. C.; Calabrese, E.; Cardoso, J. F.; Carron, J.; Chiang, H. C.; Colombo, L. P.L.; Comis, B.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; De Bernardis, P.; De Rosa, A.; De Zotti, G.; Delabrouille, J.; Di Valentino, E.; Dickinson, C.; Diego, J. M.; Doré, O.; Ducout, A.; Dupac, X.; Elsner, F.; Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Fantaye, Y.; Kim, J.; Ma, Y. Z.; Savelainen, M.; Planck Collaboration.

In: Astronomy and Astrophysics, Vol. 607, A122, 01.11.2017.

Research output: Contribution to journalArticle

Harvard

Akrami, Y, Ashdown, M, Aumont, J, Baccigalupi, C, Ballardini, M, Banday, AJ, Barreiro, RB, Bartolo, N, Basak, S, Benabed, K, Bernard, JP, Bersanelli, M, Bielewicz, P, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bucher, M, Burigana, C, Butler, RC, Calabrese, E, Cardoso, JF, Carron, J, Chiang, HC, Colombo, LPL, Comis, B, Couchot, F, Coulais, A, Crill, BP, Curto, A, Cuttaia, F, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Di Valentino, E, Dickinson, C, Diego, JM, Doré, O, Ducout, A, Dupac, X, Elsner, F, Enßlin, TA, Eriksen, HK, Falgarone, E, Fantaye, Y, Kim, J, Ma, YZ, Savelainen, M & Planck Collaboration 2017, 'Planck intermediate results: LII. Planet flux densities', Astronomy and Astrophysics, vol. 607, A122. https://doi.org/10.1051/0004-6361/201630311

APA

Akrami, Y., Ashdown, M., Aumont, J., Baccigalupi, C., Ballardini, M., Banday, A. J., ... Planck Collaboration (2017). Planck intermediate results: LII. Planet flux densities. Astronomy and Astrophysics, 607, [A122]. https://doi.org/10.1051/0004-6361/201630311

Vancouver

Akrami Y, Ashdown M, Aumont J, Baccigalupi C, Ballardini M, Banday AJ et al. Planck intermediate results: LII. Planet flux densities. Astronomy and Astrophysics. 2017 Nov 1;607. A122. https://doi.org/10.1051/0004-6361/201630311

Author

Akrami, Y. ; Ashdown, M. ; Aumont, J. ; Baccigalupi, C. ; Ballardini, M. ; Banday, A. J. ; Barreiro, R. B. ; Bartolo, N. ; Basak, S. ; Benabed, K. ; Bernard, J. P. ; Bersanelli, M. ; Bielewicz, P. ; Bonavera, L. ; Bond, J. R. ; Borrill, J. ; Bouchet, F. R. ; Boulanger, F. ; Bucher, M. ; Burigana, C. ; Butler, R. C. ; Calabrese, E. ; Cardoso, J. F. ; Carron, J. ; Chiang, H. C. ; Colombo, L. P.L. ; Comis, B. ; Couchot, F. ; Coulais, A. ; Crill, B. P. ; Curto, A. ; Cuttaia, F. ; De Bernardis, P. ; De Rosa, A. ; De Zotti, G. ; Delabrouille, J. ; Di Valentino, E. ; Dickinson, C. ; Diego, J. M. ; Doré, O. ; Ducout, A. ; Dupac, X. ; Elsner, F. ; Enßlin, T. A. ; Eriksen, H. K. ; Falgarone, E. ; Fantaye, Y. ; Kim, J. ; Ma, Y. Z. ; Savelainen, M. ; Planck Collaboration. / Planck intermediate results : LII. Planet flux densities. In: Astronomy and Astrophysics. 2017 ; Vol. 607.

Bibtex - Download

@article{40dbfe32867a403ca34595b24c4ee41a,
title = "Planck intermediate results: LII. Planet flux densities",
abstract = "Measurements of flux density are described for five planets, Mars, Jupiter, Saturn, Uranus, and Neptune, across the six Planck High Frequency Instrument frequency bands (100-857 GHz) and these are then compared with models and existing data. In our analysis, we have also included estimates of the brightness of Jupiter and Saturn at the three frequencies of the Planck Low Frequency Instrument (30, 44, and 70 GHz). The results provide constraints on the intrinsic brightness and the brightness time-variability of these planets. The majority of the planet flux density estimates are limited by systematic errors, but still yield better than 1{\%} measurements in many cases. Applying data from Planck HFI, the Wilkinson Microwave Anisotropy Probe (WMAP), and the Atacama Cosmology Telescope (ACT) to a model that incorporates contributions from Saturn's rings to the planet's total flux density suggests a best fit value for the spectral index of Saturn's ring system of βring = 2.30 ± 0.03 over the 30-1000 GHz frequency range. Estimates of the polarization amplitude of the planets have also been made in the four bands that have polarization-sensitive detectors (100-353 GHz); this analysis provides a 95{\%} confidence level upper limit on Mars's polarization of 1.8, 1.7, 1.2, and 1.7{\%} at 100, 143, 217, and 353 GHz, respectively. The average ratio between the Planck-HFI measurements and the adopted model predictions for all five planets (excluding Jupiter observations for 353 GHz) is 1.004, 1.002, 1.021, and 1.033 for 100, 143, 217, and 353 GHz, respectively. Model predictions for planet thermodynamic temperatures are therefore consistent with the absolute calibration of Planck-HFI detectors at about the three-percent level. We compare our measurements with published results from recent cosmic microwave background experiments. In particular, we observe that the flux densities measured by Planck HFI and WMAP agree to within 2{\%}. These results allow experiments operating in the mm-wavelength range to cross-calibrate against Planck and improve models of radiative transport used in planetary science.",
keywords = "Cosmic background radiation, Cosmology: observations, Planets and satellites: general",
author = "Y. Akrami and M. Ashdown and J. Aumont and C. Baccigalupi and M. Ballardini and Banday, {A. J.} and Barreiro, {R. B.} and N. Bartolo and S. Basak and K. Benabed and Bernard, {J. P.} and M. Bersanelli and P. Bielewicz and L. Bonavera and Bond, {J. R.} and J. Borrill and Bouchet, {F. R.} and F. Boulanger and M. Bucher and C. Burigana and Butler, {R. C.} and E. Calabrese and Cardoso, {J. F.} and J. Carron and Chiang, {H. C.} and Colombo, {L. P.L.} and B. Comis and F. Couchot and A. Coulais and Crill, {B. P.} and A. Curto and F. Cuttaia and {De Bernardis}, P. and {De Rosa}, A. and {De Zotti}, G. and J. Delabrouille and {Di Valentino}, E. and C. Dickinson and Diego, {J. M.} and O. Dor{\'e} and A. Ducout and X. Dupac and F. Elsner and En{\ss}lin, {T. A.} and Eriksen, {H. K.} and E. Falgarone and Y. Fantaye and J. Kim and Ma, {Y. Z.} and M. Savelainen and {Planck Collaboration}",
year = "2017",
month = "11",
day = "1",
doi = "10.1051/0004-6361/201630311",
language = "English",
volume = "607",
journal = "Astronomy & Astrophysics",
issn = "0004-6361",

}

RIS - Download

TY - JOUR

T1 - Planck intermediate results

T2 - LII. Planet flux densities

AU - Akrami, Y.

AU - Ashdown, M.

AU - Aumont, J.

AU - Baccigalupi, C.

AU - Ballardini, M.

AU - Banday, A. J.

AU - Barreiro, R. B.

AU - Bartolo, N.

AU - Basak, S.

AU - Benabed, K.

AU - Bernard, J. P.

AU - Bersanelli, M.

AU - Bielewicz, P.

AU - Bonavera, L.

AU - Bond, J. R.

AU - Borrill, J.

AU - Bouchet, F. R.

AU - Boulanger, F.

AU - Bucher, M.

AU - Burigana, C.

AU - Butler, R. C.

AU - Calabrese, E.

AU - Cardoso, J. F.

AU - Carron, J.

AU - Chiang, H. C.

AU - Colombo, L. P.L.

AU - Comis, B.

AU - Couchot, F.

AU - Coulais, A.

AU - Crill, B. P.

AU - Curto, A.

AU - Cuttaia, F.

AU - De Bernardis, P.

AU - De Rosa, A.

AU - De Zotti, G.

AU - Delabrouille, J.

AU - Di Valentino, E.

AU - Dickinson, C.

AU - Diego, J. M.

AU - Doré, O.

AU - Ducout, A.

AU - Dupac, X.

AU - Elsner, F.

AU - Enßlin, T. A.

AU - Eriksen, H. K.

AU - Falgarone, E.

AU - Fantaye, Y.

AU - Kim, J.

AU - Ma, Y. Z.

AU - Savelainen, M.

AU - Planck Collaboration

PY - 2017/11/1

Y1 - 2017/11/1

N2 - Measurements of flux density are described for five planets, Mars, Jupiter, Saturn, Uranus, and Neptune, across the six Planck High Frequency Instrument frequency bands (100-857 GHz) and these are then compared with models and existing data. In our analysis, we have also included estimates of the brightness of Jupiter and Saturn at the three frequencies of the Planck Low Frequency Instrument (30, 44, and 70 GHz). The results provide constraints on the intrinsic brightness and the brightness time-variability of these planets. The majority of the planet flux density estimates are limited by systematic errors, but still yield better than 1% measurements in many cases. Applying data from Planck HFI, the Wilkinson Microwave Anisotropy Probe (WMAP), and the Atacama Cosmology Telescope (ACT) to a model that incorporates contributions from Saturn's rings to the planet's total flux density suggests a best fit value for the spectral index of Saturn's ring system of βring = 2.30 ± 0.03 over the 30-1000 GHz frequency range. Estimates of the polarization amplitude of the planets have also been made in the four bands that have polarization-sensitive detectors (100-353 GHz); this analysis provides a 95% confidence level upper limit on Mars's polarization of 1.8, 1.7, 1.2, and 1.7% at 100, 143, 217, and 353 GHz, respectively. The average ratio between the Planck-HFI measurements and the adopted model predictions for all five planets (excluding Jupiter observations for 353 GHz) is 1.004, 1.002, 1.021, and 1.033 for 100, 143, 217, and 353 GHz, respectively. Model predictions for planet thermodynamic temperatures are therefore consistent with the absolute calibration of Planck-HFI detectors at about the three-percent level. We compare our measurements with published results from recent cosmic microwave background experiments. In particular, we observe that the flux densities measured by Planck HFI and WMAP agree to within 2%. These results allow experiments operating in the mm-wavelength range to cross-calibrate against Planck and improve models of radiative transport used in planetary science.

AB - Measurements of flux density are described for five planets, Mars, Jupiter, Saturn, Uranus, and Neptune, across the six Planck High Frequency Instrument frequency bands (100-857 GHz) and these are then compared with models and existing data. In our analysis, we have also included estimates of the brightness of Jupiter and Saturn at the three frequencies of the Planck Low Frequency Instrument (30, 44, and 70 GHz). The results provide constraints on the intrinsic brightness and the brightness time-variability of these planets. The majority of the planet flux density estimates are limited by systematic errors, but still yield better than 1% measurements in many cases. Applying data from Planck HFI, the Wilkinson Microwave Anisotropy Probe (WMAP), and the Atacama Cosmology Telescope (ACT) to a model that incorporates contributions from Saturn's rings to the planet's total flux density suggests a best fit value for the spectral index of Saturn's ring system of βring = 2.30 ± 0.03 over the 30-1000 GHz frequency range. Estimates of the polarization amplitude of the planets have also been made in the four bands that have polarization-sensitive detectors (100-353 GHz); this analysis provides a 95% confidence level upper limit on Mars's polarization of 1.8, 1.7, 1.2, and 1.7% at 100, 143, 217, and 353 GHz, respectively. The average ratio between the Planck-HFI measurements and the adopted model predictions for all five planets (excluding Jupiter observations for 353 GHz) is 1.004, 1.002, 1.021, and 1.033 for 100, 143, 217, and 353 GHz, respectively. Model predictions for planet thermodynamic temperatures are therefore consistent with the absolute calibration of Planck-HFI detectors at about the three-percent level. We compare our measurements with published results from recent cosmic microwave background experiments. In particular, we observe that the flux densities measured by Planck HFI and WMAP agree to within 2%. These results allow experiments operating in the mm-wavelength range to cross-calibrate against Planck and improve models of radiative transport used in planetary science.

KW - Cosmic background radiation

KW - Cosmology: observations

KW - Planets and satellites: general

UR - http://www.scopus.com/inward/record.url?scp=85035810697&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201630311

DO - 10.1051/0004-6361/201630311

M3 - Article

VL - 607

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

M1 - A122

ER -

ID: 16605750