Planet models and observations Splinter summary Outline Observations

Planet models and observations Splinter summary

Outline • Observations re-calibration • Planet Models • Herschel observations: cross-calibration • Other observations

Observations • Mars’ model (Rudy or Lellouch) calibrated versus WMAP within 2% • Need to re-calibrate the existing observations of Uranus and Neptune in the cm/mm/submm vs. Mars model. Data : • Hofstadter (VLA), Orton and Griffin 1993, 1987, Sandel and Dowel 2005, IRAM and SMA 2004 -2007, ISO

URANUS H 2 S, same model (PH 3 might also work but is a less likely candidate on the basis of chemical equilibrium) Sandel & Dowell data (2005)

Uranus mm-submm spectrum

Uranus Variability • Uranus cm/mm time variability link to geometrical and seasonal effect separate the observations between 2 epochs : pole-on (Voyager) and equator-on (Herschel) • Compare with planet models • Maybe constrain 2 deep thermal structures slightly different ~ 2 -3 K (not necessary easy: ∆~2%)

Possible Uranus amplitude variation during Herschel period

Planets Models • Comparison between Orton and Moreno models with thermal profile of Spitzer/ISO (Uranus and Neptune) • Optimize these P(T) in order to fit both HD lines of PACS and Spitzer. • Models to be also compared with recalibrated observations at cm/mm/submm-λ

T(p) models for Neptune Herschel PACS (Lellouch et al. 2010) Spitzer IRS (Line et al. 2008) ISO + ground-based (Burgdorf et al. 2003) Akari (Fletcher et al. 2010) Voyager RSS - - (Lindal et al. 1990)

Herschel observations: cross-calibration Comparison between HIFI/SPIRE of Neptune/Uranus at the same period ( Oct-Dec 2011). + PACS? Measure Uranus and Neptune maps with HIFI at 648 and 1012 GHz (band 2 a and 4 a) and also Mars in the same period (5. 5” on mid- Oct. 2011 ) Idea: Compare/transfer the Mars absolute calibration of HIFI with SPIRE using Uranus/Neptune observations. HIFI is calibrated versus Mars Model (OK with WMAP to 1%). Expected Absolute error from WMAP ~ 1% ν < 100 GHZ and ~ 3% in the 350 GHz < ν < 550 GHZ

Other observations • SOFIA/FORCAST observations of Uranus and Neptune, to constrain T(p) further, as well as He/H 2 and para-H 2/ortho-H 2 ratio in approved program. Follow up with spectroscopy in 2012, or whenever available. (~ 19 -37 μm) – Proposal G. Orton Uranus Neptune

Other observations • WISE filtered observations in the same region (see Amanda Mainzer, 3. 2 -22 μm) • Use planet observations from Planck when available (mm/submm) • CH 4 and CO lines on Neptune (HIFI, PACS, SPIRE, SPITZER) Constraint P(T).