Minutes from IOPW Steering Committee meeting, 2007 October 9, 12:10 - 1:20 pm
Cafe Gaugin, Rosen Center Hotel, Orlando, Florida

Present: Glenn Orton (chair), Chris Russell, Paul Steffes, Kevin Baines,
Ricardo Hueso (for Agustin Sanchez-Lavega), Imke de Pater

Absent from DPS: Tom Stallard (rotating member), John Clarke (auroral, etc.
discipline), Henry Roe (present only starting on Tuesday night)

MIA: Heidi Hammel, Robert West

Heidi later related that she was in a conference call that went into overtime.
Agustin Sanchez-Lavega was participating as a backup information source in the
New Horizons press conference.

Discipline Reports:

John Clarke, Aurora, Magnetospheres, Torus Discipline (by email before the
meeting)

Hi Glenn,

My report for the first year of the combined Aurora, Magnetospheres, and Torus
section of the IOPW is to draw your attention to the web site we have created:
http://www.bu.edu/csp/PASS/iopw_main.html

I think a large part of the benefit of this web site is the page of
publications, with links to more than 100 pubs in this subject area.

Then, the results of the large HST program for auroral observations with quick
look data are posted at:
http://www.bu.edu/csp/PASS/main.html

Have a good meeting on Tues., sorry I am not there.

Cheers, John

Frank Marchis, Satellites

We continued to monitor Io regularly when it is observable using the  Keck AO
instrument.  Two official programs conducted by J. Spencer with VLT/NACO and F.
Marchis with GEMINI/ALTAIR were submitted and accepted to observe in correlation
and after the NH flyby. Both programs were merged and F. Marchis will be
presenting the result at the AGU Fall meeting.  K. Jessup got funding with NASA
PAST to study the SO2 gas absorption  with ground based telescopes. She
submitted a proposal at Keck NASA using NIRC2 and the AO system. In
collaboration with E. Lellouch, and she also submitted a similar proposal to
characterize the SO2 gas distribution using CRIRES R=30,000-50,000 resolution
spectrometer  (CRIRES) combined with MACAO at VLT.

Agustin Sanchez-Lavega, Jupiter and Saturn atmospheres discipline:

Substantial work was done, both in continuing support of the Cassini mission,
but also to support the New Horizons flyby and the NTB and SEB outbreaks which
occurred in the spring.

Monday night, October 8, there was what ended up as a combined Jupiter and
Saturn, plus Uranus and Neptune atmospheres meeting, starting at 6:30 which went
past 9 pm. The addition of Uranus and Neptune discussion was unexpected, but
enough people turned out to be interested that these items were added to the
agenda.  There were 30-40 people at the meeting, substantially larger than
almost any preceeding meeting, and there were some complaints later that it went
too long.  The presentations were extensive; most did not recapitulate items
presented in oral or poster talks during the meeting.

INTERNATIONAL OUTER PLANET WATCH GIANT AND ICY PLANETS DISCIPLINE MEETING
DPS (Orlando, October 8) Agenda:

Introduction
* A. Sanchez-Lavega.  New webmaster IOPW-PVOL

Uranus and Neptune (H. Hammel)
* P. Irwin. Near Infrared Observations of the Latitudinal Variation of Vertical
    Cloud Structure in Uranus' Atmosphere prior to its Equinox.
* L. Sromosvsky. Uranus and Neptune observations.
* G. Orton. Neptune pole.

Jupiter
* Ch. Go. Jupiter upheavel in 2007
* A. Sanchez-Lavega. Jupiter Southern Hemisphere Disturbances in 2007
* G. Orton. Jupiter Observations 2007
* A. Sanchez-Lavega. New measurements and simulations of BA-GRS
* S. Perez-Hoyo. NTB Disturbance: Clouds and aerosols.
* R. Hueso. NTB Disturbance: Dynamical Models

Saturn
* G. Orton.  Non-seasonal oscillations in Saturn between the equator and low
     latitudes.
* K. Sayanagi. Zonal Jets on Jupiter and Saturn: their formation and stability.

Future observing plans
* G. Orton et al.
* A. Sanchez-Lavega. Grantecan and CanariCam

From Agustin's presentation:

Spain is building the largest telescope in the world, at over 10 m diameter
(using a Keck-like array of segmented mirrors).

Applications will be solicited for the second semester of 2008.

The first instrument will be a mid-infrared camera/spectrometer built by Charlie
Telesco's group at U. Florida. Details follow:

Canari-Cam is a mid-infrared imager with spectrogroscopic, coronagraphic, and
polarimetric capabilities, which will be mounted initially at the Nasmyth focus
of the 10-m Gran Telescopio Canarias at the Roque de los Muchachos Observatory
in La Palma (Canary Islands, Spain). In the future, when the Cassegrin focus of
the telescope is commissioned, we expect CanariCam to move to this focus, which
will provide superior performance with the instrument. CanariCam is designed as
a diffraction-limited imager. It is optimised as an imager, and although it will
offer a range of other observing modes, these will not compromise the imaging
capability. The fact that CanariCam offers polarimetry and coronagraphy in
addition to the more standard imaging and spectroscopic modes makes it an
extremely versatile and powerful instrument that is unique in the world.

Wavelength range (optimised science)    8-25 microns
Wavelength range (engineering)          2-25 microns
Pixel size                             0.08 (+- 5%) arcseconds
Field of view                           25.6 x 19.2 (+- 5%) arcseconds
Image quality at 8 microns              80% of energy within 2x2 pixel square
Optical throughput                      >75% at 10 microns (not incl. filters)
Goal:                                   >90% from 8-24 microns (not incl.
filters)

Ghost images                            Goal: <0.01% of primary image intensity
Cosmetic quality of detector            <1% of defective pixels
Number of filter positions              23 broad and narrow band
Maximum image distortion                2 pixels at edge of field
Sensitivity 10 microns (short exposure) ~11.5 (5 sigma in 100s)
0.9 mJy (5 sigma in 100s)

Sensitivity 10 microns (deep exposure)  ~14.2 (5 sigma in 4 hours)
80 microJy (5 sigma in 4 hours)

Observing modes:
Direct imaging.
Long slit spectroscopy.
Imaging polarimetry.
Imaging coronagraphy.

http://www.iac.es/proyecto/CCam/
http://www.astro.ufl.edu/CanariCam/canaricam_home.htm

Uranus & Neptune Report for the IOPW, DPS October 2007
Submitted by H. B. Hammel

Uranus

Uranus Atmosphere.     There were a substantial number of
observations of the Uranus system in 2007.  Two of the three Earth
Ring-Plane Crossing (RPX) events took place; still to come are the
Sun RPX - a.k.a. the Equinox - on 7 Dec 2007, and a final RPX in
early 2008 (not observable due to Uranus solar conjunction).
Telescopes around the world observed the atmosphere, rings, and
satellites, including Hubble, the Keck II, the VLT, Palomar, IRTF,
and many other facilities.

Keck and HST results, with supporting low resolution observations
from VLT, Palomar and other facilities, show continued evolution of
both the banded structure and the number and type of discrete
features.  The bright southern polar collar --  encircling the
previously sunlit southern pole - is demonstrably darkening, while
the similar northern band is brightening.   The southern feature
dubbed "Monster Berg" now seems to show nearly continuous
high-altitude activity, including some instance of multiple bright
points.   The phase lag of symmetry with respect to the equinox is
predicted to of order 3-5 years; continued observations are required
to confirm this.

Longer-wavelength measurements at radio and sub-mm indicate symmetry
or uniform disks.  The turnover point between this deeper symmetric
atmosphere and the upper more asymmetric atmosphere is not clearing
identified yet, but is certainly deeper than 3-5 bars, and possibly
even deeper than 7-10 bars.

Spectroscopy and multi-wavelength observations are beginning to yield
quantitative understanding of the vertical aerosol structure and
cloud composition.  One conclusion is that the observed cloud deck is
probably not due methane condensation, contradicting past
conventional wisdom.  It appears to be too deep, closer to 5-7 bars
rather than 1 bar.  Rather than methane, it may be ammonia, or even
ammonium hydrosulfide.  This has not been confirmed
spectroscopically.

Results from HST multi-wavelength images are suggesting that the
hazes or aerosol layers may not be tightly confined to altitude
layers, but rather exhibit gentle gradients of opacity through the
tropopause and down into the troposphere.  There does seem to be an
inflection near the expected 1-bar methane condensation level,
suggesting methane haze plays a role, but perhaps not a dominant
role.  That work only probes down toe about 3 bar.

There has not yet been an update on the ionospheric observations for Uranus.

Uranus Rings.     Keck and Hubble images at and near RPX are
revealing substantial variation of ring brightnesses, as predicted
from basic understanding of scattering as a function of optical
depth.  Detailed analysis of the changes, however, suggests
significant changes in the dust distribution within the main rings
since the Voyager flyby.

Uranus Satellites.     A few mutual events have been observed,
analysis in progress.   Hubble and Keck data are being used to detect
smaller moons in order to define their orders, and perhaps extract
wavelength-dependent photometric measurements, which may be
indicative of surface composition (e.g., whether the signature of
water is seen on faint moons like Mab).

Continued Observations

Continued observations of the Uranus system through 2008 are planned
at many facilities.  Final equinoctial observations will be made for
the rings and moons, and post-equinoctial observations of the
atmosphere will continue to document the seasonal variations
underway.   The Keck observations will be severely curtailed due to
NASA HQ programmatic choices (see Requested Action below).  We
continue to solicit verbal support from IOPW for these activities.

Neptune

Both Keck and Hubble continued their observations programs of Neptune
imaging.  Most progress in the past year has been in the field of
mid-infrared imaging.  Papers appeared for mid-IR imaging from both
Gemini and VLT, showing that the mid-IR emission is predominantly
from the southern pole, along with limb brightening.  There has also
been evidence for discrete thermal features. Continued observations
also will be made of Neptune whenever feasible.

Action Requested from IOPW

A decision from NASA administration has serious impacted the ability
of NASA researchers to use the Keck telescope for outer planet
observations.  Virtually all NASA time on Keck is being devoted to
interferometry, with almost no time for single-dish work. All other
NASA science is restricted to just 6 nights of Keck time for the
entire year 2008.

While that is bad enough for time-critical programs like our Uranus
equinox observations, even more chilling is the possibility that this
is a prelude to NASA completely pulling out of supporting the Keck
Telescope.

There has been an enormous body of excellent NASA-supported science
accomplished with the NASA time on the Keck Telescopes, and it would
be a serious blow to lose the access.  Much of the work simply cannot
be done at any other facility, since it requires the high quality and
deep sensitivity afforded by the diffraction-limited imaging produced
by the Keck AO system.

My specific request would be that we, as the IOPW Steering Committee,
send a letter regarding the issue of NASA-supported observations
using Keck single-dish time to a number of key individuals listed
below.  The letter might mention the ongoing research, its
productivity, its significant return for relatively little investment
of funds, and your hopes that the means can be found to permit such
top-ranked research to continue in the coming years, in order to
supported NASA's science and research goals.

(Please note:  need to verify these titles prior to sending anything....)

Dr. Richard Binzel, Chair NASA Keck/IRTF MOWG.
Dr. Jon Morse, Director, Universe Division
Dr. James Green, Planetary Science Division
Dr. Alan Stern, SMD Associate Administrator

Please cc Dr. Taft Armandroff, Keck Director.  I would be happy to
assist in drafting such a letter.

Titan Discipline, Henry Roe
(transmitted 2007 Oct 25; Henry was unable to make the DPS
  in time for the IOPW Steering Committee meeting on Tuesday)

Ground-based monitoring of Titan continues with IRTF spectra, and
Gemini and Keck imaging and integral field spectroscopy.  After more
than a year of low levels of cloud activity the mid-latitude (-40
degree south) clouds became suddenly prominent and common again in April
and May of 2007.  The new Titan observing season starts in October 2007
and we will see the status of these clouds at that time.

Paul Steffes, laboratory support discipline

Paul expressed regret that he'd not done much specifically for this discipline.
He did note, however, that his own work would be continuing on support for the
JUNO mission in the radio would be continuing with  NH3-H2 absorption.  It was
noted that there were several sets of laboratory oriented posters and talks at
the DPS, but the organizers interspersed them within the sessions appearing to
be the most relevant and receptive to their results. There will also be more
reported at NASA's Planetary Atmospheres workshop early in November in Maryland.


Notes from rotating member Tom Stallard (via email transmitted Oct. 3)

Not a lot to say about the Cassini-Hubble ground-based support program we ran
this year, other than to say it was pretty successful and we have a lot of
interesting results that need analysis.  The Uranus program is developing nicely
too - last year showed some very interesting data and we're following it up with
now observations right now.

More importantly, let me know if more needs to be done on the Uranus and Neptune
Discipline website.

Also, a brief word about Europlanet - since it seems no-one outside Europe
generally knows about it.

The European planetary network (Europlanet) is currently submitting a case to
the European Union for continued funding, having completed the first four-year
period of funding.  The overall objectives of the network are to increase the
productivity of planetary projects with European investment, with emphasis on
major planetary exploration missions; initiate long-term integration within the
European planetary science community; improve European scientific
competitiveness, develop and spread expertise in this research area; and to
improve public understanding of planetary environments.

The significance of this is that the EU has provided funds for inter-European
collaborations and meetings, as well as paying for Europlanet members to travel
internationally. This has been used to good effect within the outer planetary
community, especially in developing ties between space-based and ground-based
observations of solar system and planetary objects. The network also lead to the
formation of a new international planetary meeting -  the European Planetary
Science Congress - which first opened in 2006.

Hopefully the EU will decide to continue this important funding stream for
European researchers.