Venus coordinated campaign
This wiki is provided as a tool to share information and schedules for the 2010 coordinated ground-based campaign of Venus. Please feel free to complete and modify the attached tables according to the campaign progress and your proposed observations.
Tools of the Venus coordinated campaign
Table
A list of proposed and actual observations : pre-conjunction (July 2010-Oct. 29, 2010), post conjunction (Oct. 29, 2010 - Feb. 2011)
Map of observatory sites and telescopes
Sites and telescopes used for ground-based observations, with a link to their instruments.
Instrumentation of the study of Venus
Ground-based instruments
- Sunspot Astronomy & Visitor Center
APO 3.5-m
ARCES
- Observatorio SOAR
Soar Telescope
- Observatoire du Pic du Midi de Bigorre
Bernard-Lyot 2-m
- Osservatorio Astronomico della Regione Autonoma Valle d'Aosta
- South African Astronomical Observatory
Southern African Large Telescope (SALT)
- Hanle Observatory
HCT
- National Central University Lulin Observatory
LOT Cassegrain/ SLT R-C/ 4 TAOS robotic
- Naroyo Observatory
Naroyo 1.6-m
- Siding Spring Observatory
Anglo-Australian 3.9-m
- Mount John University Observatory
1 m McLellan
MOA 1.8-m
0.6-m Optical Craftsmen
0.6-m Boller & Chivens
- Mauna Kea Observatory
IRTF (HIPWAC Heterodyne Instrument for Planetary Wind And Composition)
Keck 10-m
CFHT 3.6-m
SUBARU
JCMT
- Haleakala Observatory
AEOS
- Kitt Peak National Observatory
McMath-Pierce Solar Telescope
- THIS Tuneable Heterodyne Infrared Spectrometer
used at the:
- McMath-Pierce Solar Telescope on Kitt Peak in Arizona
- IRTF on Mauna Kea Hawaii
Venus Express instruments
400px|thumb|right|Instrumentation of Venus Express, Credit: ESA
- SPICAV/SOIR : Ultraviolet and Infrared Atmospheric Spectrometer
Atmospheric spectrometry by star or Sun occultation
UV 0.11 - 0.3 µm R ~ 300
IR 0.7 - 1.7 µm R ~ 1300
SOIR 2.3 - 4.2 µm R ~ 15000
- VeRa : Venus Radio Science Experiment
Radio sounding of atmosphere
- VIRTIS : Ultraviolet/Visible/Near-Infrared mapping spectrometer
Spectrographic mapping of atmosphere and surface
- VIRTIS-M mapping spectrometer
Vis 0.25 - 1.0 µm R ~ 100 - 200 ( IR 1 - 5 µm R ~ 100 - 200 )
- VIRTIS-H High-res
2 - 5 µm R ~ 1000 - 2000
- VMC : Venus Monitoring Camera
Ultraviolet and visible imaging
Filters :
UV 0.365 µm
Vis 0.513 µm
Near - IR1 0.965 µm
Near - IR2 1.010 µm
More about the Venus Express Instruments
Akatsuki instruments
400px|thumb|right|Instrumentation of Akatsuki, Credit: JAXA
Akatsuki successfully launched at 6:58:22 a.m. on May 21 (Japan Standard Time) !
More about VCO/Akatsuki mission
- IR1 : 1-micron Camera
Low stratus, vapor, active volcanism
1.01 µm cloud (day-night), surface (nightside)
- IR2 : 2-micron Camera
Low stratus, trace gasses, zodiacal light
1.73, 2.26, 2.32 (near-IR) 2.02 (CO2), 1.65 µm
- UVI : Ultraviolet Imager
Cloud-top ultraviolet absorber, SO2
283, 365 nm SO2 - UV absorber (dayside)
- LIR : Longwave Infrared Camera
Cloud-top temperature distribution
10 µm cloud top (day/nightside)
- LAC : Lightning and Airglow Camera
Lightening flash, high-stratus airglow emission
Filters 777, 557, 553, 558, 630 nm O2/O airglow (night) lightning (night)
More about the Akatsuki Instruments
Coordination meetings / meeting sessions
- Venus Conference, Aussois (France), 20-26 June 2010
- « After-Aussois Venus 2010 » workshop: 1st strategic workshop on Coordinated ground-based measurements and modeling of the Venus atmosphere, Paris, June 28-29, 2010
- 2010 VEXAG International Workshop: Venus, Our Closest Earth-like Planet, Madison (USA), 30 August - 2 September 2010
