venus-atm - User contributions [en]

Venus coordinated campaign

2010-05-19T13:07:12Z

145.238.174.192: /* Instrumentation and Techniques */

This site is intended as a tool to share information, comments and schedules for preparing the 2010 coordinated campaign of ground-based observations in the context of Venus Express and coming launch of Akatsuki mission.

The attached Google docs can be completed and modified according to the campaign progress.
__TOC__

==Map (under construction) ==

To have a general view of the sites and telescopes which are used to ground-based observations about Venus, this is a googlemap which resume all differents observatories and their instruments.

* [http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2 2010 Venus Coordinated Campaign, Telescopes sites]

==Coordination==

To prepare the campaign and coordinate telescope proposals with VEx MTPs, the attached table is under construction. Please do not hesitate to comment/modify and add more details on your plans.

[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr 2010 Venus Coordination]

== In-orbit observations ==

=== Venus Express ===

==== Instruments ====

[[Fichier:Instruments_of_venus_express.jpg|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

[http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=33964&fbodylongid=1441 More about the Venus Express Instruments]

=== Akatsuki ===

==== The Project====

The Venus Climate Orbiter mission (PLANET-C), one of the future planetary missions of Japan, aims at understanding the atmospheric circulation of Venus. Meteorological information will be obtained by globally mapping clouds and minor constituents successively with 4 cameras at ultraviolet and infrared wavelengths, detecting lightning with a high-speed imager, and observing the vertical structure of the atmosphere with radio science technique. The equatorial elongated orbit with westward revolution fits the observations of the movement and temporal variation of the Venusian atmosphere which rotates westward. The systematic, continuous imaging observations will provide us with an unprecedented large dataset of the Venusian atmospheric dynamics. Additional targets of the mission are the exploration of the ground surface and the observation of zodiacal light. The mission will complement the ESA's Venus Express, which also explores the Venusian environment with different approaches.

extract of: http://www.stp.isas.jaxa.jp/venus/top_english.html

The project, a link to
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html JAXA]

==== Instruments====
[[Fichier:Akatsuki_instrumentation.gif|400px|thumb|right|Instrumentation of Akatsuki, Credit: JAXA]]
* '''IR1''': 1-micron Camera
1.01µm
cloud (day-night), surface (nightside)

* '''IR2''': 2-micron Camera
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65µm

* '''UVI''': Ultraviolet Imager
283, 365 nm
SO2 - UV absorber (dayside)

* '''LIR''': Longwave Infrared Camera
10 µm
cloud top (day/nightside)

* '''LAC''': Lightning and Airglow Camera
Filters
777, 557, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)

[http://www.stp.isas.jaxa.jp/venus/E_instrument.html More about the Akatsuki Instruments]

==Coming meetings==
* [http://lesia.obspm.fr/venus2010/ Venus Conference, Aussois (France), 20-26 June 2010]
* [http://www.lesia.obspm.fr/venus-atm/International « After-Aussois Venus 2010 » workshop: 1st strategic workshop on Coordinated ground-based measurements and modeling of the Venus atmosphere, Paris Observatory, June 28-29, 2010]

Venus coordinated campaign

2010-05-19T12:22:04Z

145.238.174.192: /* Coordination */

This site is intended as a tool to share information, comments and schedules for preparing the 2010 coordinated campaign of ground-based observations in the context of Venus Express and coming launch of Akatsuki mission.

The attached Google docs can be completed and modified according to the campaign progress.
__TOC__

==Map (under construction) ==

To have a general view of the sites and telescopes which are used to ground-based observations about Venus, this is a googlemap which resume all differents observatories and their instruments.

* [http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2 2010 Venus Coordinated Campaign, Telescopes sites]

==Coordination==

To prepare the campaign and coordinate telescope proposals with VEx MTPs, the attached table is under construction. Please do not hesitate to comment/modify and add more details on your plans.

[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr 2010 Venus Coordination]

== In-orbit observations ==

=== Venus Express ===

==== Instruments ====

[[Fichier:Instruments_of_venus_express.jpg|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

[http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=33964&fbodylongid=1441 More about the Venus Express Instruments]

=== Akatsuki ===

==== The Project====

The Venus Climate Orbiter mission (PLANET-C), one of the future planetary missions of Japan, aims at understanding the atmospheric circulation of Venus. Meteorological information will be obtained by globally mapping clouds and minor constituents successively with 4 cameras at ultraviolet and infrared wavelengths, detecting lightning with a high-speed imager, and observing the vertical structure of the atmosphere with radio science technique. The equatorial elongated orbit with westward revolution fits the observations of the movement and temporal variation of the Venusian atmosphere which rotates westward. The systematic, continuous imaging observations will provide us with an unprecedented large dataset of the Venusian atmospheric dynamics. Additional targets of the mission are the exploration of the ground surface and the observation of zodiacal light. The mission will complement the ESA's Venus Express, which also explores the Venusian environment with different approaches.

extract of: http://www.stp.isas.jaxa.jp/venus/top_english.html

The project, a link to
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html JAXA]

==== Instrumentation and Techniques ====
[[Fichier:Akatsuki_instrumentation.gif|400px|thumb|right|Instrumentation of Akatsuki, Credit: JAXA]]
* '''IR1''': 1-micron Camera
1.01µm
cloud (day-night), surface (nightside)

* '''IR2''': 2-micron Camera
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65µm

* '''UVI''': Ultraviolet Imager
283, 365 nm
SO2 - UV absorber (dayside)

* '''LIR''': Longwave Infrared Camera
10 µm
cloud top (day/nightside)

* '''LAC''': Lightning and Airglow Camera
Filters
777, 557, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)

[http://www.stp.isas.jaxa.jp/venus/E_instrument.html More about the Akatsuki Instruments]

==Coming meetings==
* [http://lesia.obspm.fr/venus2010/ Venus Conference, Aussois (France), 20-26 June 2010]
* [http://www.lesia.obspm.fr/venus-atm/International « After-Aussois Venus 2010 » workshop: 1st strategic workshop on Coordinated ground-based measurements and modeling of the Venus atmosphere, Paris Observatory, June 28-29, 2010]

Venus coordinated campaign

2010-05-19T12:21:44Z

145.238.174.192: /* Coordination */

This site is intended as a tool to share information, comments and schedules for preparing the 2010 coordinated campaign of ground-based observations in the context of Venus Express and coming launch of Akatsuki mission.

The attached Google docs can be completed and modified according to the campaign progress.
__TOC__

==Map (under construction) ==

To have a general view of the sites and telescopes which are used to ground-based observations about Venus, this is a googlemap which resume all differents observatories and their instruments.

* [http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2 2010 Venus Coordinated Campaign, Telescopes sites]

==Coordination==

To prepare the campaign and coordinate telescope proposals with VEx MTPs, the attached table is under construction. Please do not hesitate to comment/modify and add more details on your plans.

Link on:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr 2010 Venus Coordination]

== In-orbit observations ==

=== Venus Express ===

==== Instruments ====

[[Fichier:Instruments_of_venus_express.jpg|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

[http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=33964&fbodylongid=1441 More about the Venus Express Instruments]

=== Akatsuki ===

==== The Project====

The Venus Climate Orbiter mission (PLANET-C), one of the future planetary missions of Japan, aims at understanding the atmospheric circulation of Venus. Meteorological information will be obtained by globally mapping clouds and minor constituents successively with 4 cameras at ultraviolet and infrared wavelengths, detecting lightning with a high-speed imager, and observing the vertical structure of the atmosphere with radio science technique. The equatorial elongated orbit with westward revolution fits the observations of the movement and temporal variation of the Venusian atmosphere which rotates westward. The systematic, continuous imaging observations will provide us with an unprecedented large dataset of the Venusian atmospheric dynamics. Additional targets of the mission are the exploration of the ground surface and the observation of zodiacal light. The mission will complement the ESA's Venus Express, which also explores the Venusian environment with different approaches.

extract of: http://www.stp.isas.jaxa.jp/venus/top_english.html

The project, a link to
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html JAXA]

==== Instrumentation and Techniques ====
[[Fichier:Akatsuki_instrumentation.gif|400px|thumb|right|Instrumentation of Akatsuki, Credit: JAXA]]
* '''IR1''': 1-micron Camera
1.01µm
cloud (day-night), surface (nightside)

* '''IR2''': 2-micron Camera
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65µm

* '''UVI''': Ultraviolet Imager
283, 365 nm
SO2 - UV absorber (dayside)

* '''LIR''': Longwave Infrared Camera
10 µm
cloud top (day/nightside)

* '''LAC''': Lightning and Airglow Camera
Filters
777, 557, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)

[http://www.stp.isas.jaxa.jp/venus/E_instrument.html More about the Akatsuki Instruments]

==Coming meetings==
* [http://lesia.obspm.fr/venus2010/ Venus Conference, Aussois (France), 20-26 June 2010]
* [http://www.lesia.obspm.fr/venus-atm/International « After-Aussois Venus 2010 » workshop: 1st strategic workshop on Coordinated ground-based measurements and modeling of the Venus atmosphere, Paris Observatory, June 28-29, 2010]

Venus coordinated campaign

2010-05-19T12:20:10Z

145.238.174.192: /* Map (under construction) */

This site is intended as a tool to share information, comments and schedules for preparing the 2010 coordinated campaign of ground-based observations in the context of Venus Express and coming launch of Akatsuki mission.

The attached Google docs can be completed and modified according to the campaign progress.
__TOC__

==Map (under construction) ==

To have a general view of the sites and telescopes which are used to ground-based observations about Venus, this is a googlemap which resume all differents observatories and their instruments.

* [http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2 2010 Venus Coordinated Campaign, Telescopes sites]

==Coordination==

To prepare the campaign and coordinate telescope proposals with VEx MTPs, the attached table is under construction. Please do not hesitate to comment/modify and add more details on your plans.

Link on:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr 2010 Coordination]

== In-orbit observations ==

=== Venus Express ===

==== Instruments ====

[[Fichier:Instruments_of_venus_express.jpg|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

[http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=33964&fbodylongid=1441 More about the Venus Express Instruments]

=== Akatsuki ===

==== The Project====

The Venus Climate Orbiter mission (PLANET-C), one of the future planetary missions of Japan, aims at understanding the atmospheric circulation of Venus. Meteorological information will be obtained by globally mapping clouds and minor constituents successively with 4 cameras at ultraviolet and infrared wavelengths, detecting lightning with a high-speed imager, and observing the vertical structure of the atmosphere with radio science technique. The equatorial elongated orbit with westward revolution fits the observations of the movement and temporal variation of the Venusian atmosphere which rotates westward. The systematic, continuous imaging observations will provide us with an unprecedented large dataset of the Venusian atmospheric dynamics. Additional targets of the mission are the exploration of the ground surface and the observation of zodiacal light. The mission will complement the ESA's Venus Express, which also explores the Venusian environment with different approaches.

extract of: http://www.stp.isas.jaxa.jp/venus/top_english.html

The project, a link to
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html JAXA]

==== Instrumentation and Techniques ====
[[Fichier:Akatsuki_instrumentation.gif|400px|thumb|right|Instrumentation of Akatsuki, Credit: JAXA]]
* '''IR1''': 1-micron Camera
1.01µm
cloud (day-night), surface (nightside)

* '''IR2''': 2-micron Camera
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65µm

* '''UVI''': Ultraviolet Imager
283, 365 nm
SO2 - UV absorber (dayside)

* '''LIR''': Longwave Infrared Camera
10 µm
cloud top (day/nightside)

* '''LAC''': Lightning and Airglow Camera
Filters
777, 557, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)

[http://www.stp.isas.jaxa.jp/venus/E_instrument.html More about the Akatsuki Instruments]

==Coming meetings==
* [http://lesia.obspm.fr/venus2010/ Venus Conference, Aussois (France), 20-26 June 2010]
* [http://www.lesia.obspm.fr/venus-atm/International « After-Aussois Venus 2010 » workshop: 1st strategic workshop on Coordinated ground-based measurements and modeling of the Venus atmosphere, Paris Observatory, June 28-29, 2010]

Venus coordinated campaign

2010-05-19T12:19:49Z

145.238.174.192: /* Map (under construction) */

This site is intended as a tool to share information, comments and schedules for preparing the 2010 coordinated campaign of ground-based observations in the context of Venus Express and coming launch of Akatsuki mission.

The attached Google docs can be completed and modified according to the campaign progress.
__TOC__

==Map (under construction) ==

To have a general view of the sites and telescopes which are used to ground-based observations about Venus, this is a googlemap which resume all different observatories and their instruments.

* [http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2 2010 Venus Coordinated Campaign, Telescopes sites]

==Coordination==

To prepare the campaign and coordinate telescope proposals with VEx MTPs, the attached table is under construction. Please do not hesitate to comment/modify and add more details on your plans.

Link on:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr 2010 Coordination]

== In-orbit observations ==

=== Venus Express ===

==== Instruments ====

[[Fichier:Instruments_of_venus_express.jpg|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

[http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=33964&fbodylongid=1441 More about the Venus Express Instruments]

=== Akatsuki ===

==== The Project====

The Venus Climate Orbiter mission (PLANET-C), one of the future planetary missions of Japan, aims at understanding the atmospheric circulation of Venus. Meteorological information will be obtained by globally mapping clouds and minor constituents successively with 4 cameras at ultraviolet and infrared wavelengths, detecting lightning with a high-speed imager, and observing the vertical structure of the atmosphere with radio science technique. The equatorial elongated orbit with westward revolution fits the observations of the movement and temporal variation of the Venusian atmosphere which rotates westward. The systematic, continuous imaging observations will provide us with an unprecedented large dataset of the Venusian atmospheric dynamics. Additional targets of the mission are the exploration of the ground surface and the observation of zodiacal light. The mission will complement the ESA's Venus Express, which also explores the Venusian environment with different approaches.

extract of: http://www.stp.isas.jaxa.jp/venus/top_english.html

The project, a link to
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html JAXA]

==== Instrumentation and Techniques ====
[[Fichier:Akatsuki_instrumentation.gif|400px|thumb|right|Instrumentation of Akatsuki, Credit: JAXA]]
* '''IR1''': 1-micron Camera
1.01µm
cloud (day-night), surface (nightside)

* '''IR2''': 2-micron Camera
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65µm

* '''UVI''': Ultraviolet Imager
283, 365 nm
SO2 - UV absorber (dayside)

* '''LIR''': Longwave Infrared Camera
10 µm
cloud top (day/nightside)

* '''LAC''': Lightning and Airglow Camera
Filters
777, 557, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)

[http://www.stp.isas.jaxa.jp/venus/E_instrument.html More about the Akatsuki Instruments]

==Coming meetings==
* [http://lesia.obspm.fr/venus2010/ Venus Conference, Aussois (France), 20-26 June 2010]
* [http://www.lesia.obspm.fr/venus-atm/International « After-Aussois Venus 2010 » workshop: 1st strategic workshop on Coordinated ground-based measurements and modeling of the Venus atmosphere, Paris Observatory, June 28-29, 2010]

Venus coordinated campaign

2010-05-19T12:06:57Z

145.238.174.192: /* Instrumentation and Techniques */

This site is intended as a tool to share information, comments and schedules for preparing the 2010 coordinated campaign of ground-based observations in the context of Venus Express and coming launch of Akatsuki mission.

The attached Google docs can be completed and modified according to the campaign progress.
__TOC__

==Map (under construction) ==

* [http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2 2010 Venus Coordinated Campaign, Telescopes sites]

==Coordination==

To prepare the campaign and coordinate telescope proposals with VEx MTPs, the attached table is under construction. Please do not hesitate to comment/modify and add more details on your plans.

Link on:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr 2010 Coordination]

== In-orbit observations ==

=== Venus Express ===

==== Instruments ====

[[Fichier:Instruments_of_venus_express.jpg|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

[http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=33964&fbodylongid=1441 More about the Venus Express Instruments]

=== Akatsuki ===

==== The Project====

The Venus Climate Orbiter mission (PLANET-C), one of the future planetary missions of Japan, aims at understanding the atmospheric circulation of Venus. Meteorological information will be obtained by globally mapping clouds and minor constituents successively with 4 cameras at ultraviolet and infrared wavelengths, detecting lightning with a high-speed imager, and observing the vertical structure of the atmosphere with radio science technique. The equatorial elongated orbit with westward revolution fits the observations of the movement and temporal variation of the Venusian atmosphere which rotates westward. The systematic, continuous imaging observations will provide us with an unprecedented large dataset of the Venusian atmospheric dynamics. Additional targets of the mission are the exploration of the ground surface and the observation of zodiacal light. The mission will complement the ESA's Venus Express, which also explores the Venusian environment with different approaches.

extract of: http://www.stp.isas.jaxa.jp/venus/top_english.html

The project, a link to
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html JAXA]

==== Instrumentation and Techniques ====
[[Fichier:Akatsuki_instrumentation.gif|400px|thumb|right|Instrumentation of Akatsuki, Credit: JAXA]]
* '''IR1''': 1-micron Camera
1.01µm
cloud (day-night), surface (nightside)

* '''IR2''': 2-micron Camera
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65µm

* '''UVI''': Ultraviolet Imager
283, 365 nm
SO2 - UV absorber (dayside)

* '''LIR''': Longwave Infrared Camera
10 µm
cloud top (day/nightside)

* '''LAC''': Lightning and Airglow Camera
Filters
777, 557, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)

[http://www.stp.isas.jaxa.jp/venus/E_instrument.html More about the Akatsuki Instruments]

==Coming meetings==
* [http://lesia.obspm.fr/venus2010/ Venus Conference, Aussois (France), 20-26 June 2010]
* [http://www.lesia.obspm.fr/venus-atm/International « After-Aussois Venus 2010 » workshop: 1st strategic workshop on Coordinated ground-based measurements and modeling of the Venus atmosphere, Paris Observatory, June 28-29, 2010]

Venus coordinated campaign

2010-05-19T12:06:23Z

145.238.174.192: /* Instruments */

This site is intended as a tool to share information, comments and schedules for preparing the 2010 coordinated campaign of ground-based observations in the context of Venus Express and coming launch of Akatsuki mission.

The attached Google docs can be completed and modified according to the campaign progress.
__TOC__

==Map (under construction) ==

* [http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2 2010 Venus Coordinated Campaign, Telescopes sites]

==Coordination==

To prepare the campaign and coordinate telescope proposals with VEx MTPs, the attached table is under construction. Please do not hesitate to comment/modify and add more details on your plans.

Link on:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr 2010 Coordination]

== In-orbit observations ==

=== Venus Express ===

==== Instruments ====

[[Fichier:Instruments_of_venus_express.jpg|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

[http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=33964&fbodylongid=1441 More about the Venus Express Instruments]

=== Akatsuki ===

==== The Project====

The Venus Climate Orbiter mission (PLANET-C), one of the future planetary missions of Japan, aims at understanding the atmospheric circulation of Venus. Meteorological information will be obtained by globally mapping clouds and minor constituents successively with 4 cameras at ultraviolet and infrared wavelengths, detecting lightning with a high-speed imager, and observing the vertical structure of the atmosphere with radio science technique. The equatorial elongated orbit with westward revolution fits the observations of the movement and temporal variation of the Venusian atmosphere which rotates westward. The systematic, continuous imaging observations will provide us with an unprecedented large dataset of the Venusian atmospheric dynamics. Additional targets of the mission are the exploration of the ground surface and the observation of zodiacal light. The mission will complement the ESA's Venus Express, which also explores the Venusian environment with different approaches.

extract of: http://www.stp.isas.jaxa.jp/venus/top_english.html

The project, a link to
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html JAXA]

==== Instrumentation and Techniques ====
[[Fichier:Akatsuki_instrumentation.gif|400px|thumb|right|Instrumentation of Akatsuki, Credit: JAXA]]
* IR1: 1-micron Camera
1.01µm
cloud (day-night), surface (nightside)

* IR2: 2-micron Camera
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65µm

* UVI: Ultraviolet Imager
283, 365 nm
SO2 - UV absorber (dayside)

* LIR: Longwave Infrared Camera
10 µm
cloud top (day/nightside)

* LAC: Lightning and Airglow Camera
Filters
777, 557, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)

[http://www.stp.isas.jaxa.jp/venus/E_instrument.html More about the Akatsuki Instruments]

==Coming meetings==
* [http://lesia.obspm.fr/venus2010/ Venus Conference, Aussois (France), 20-26 June 2010]
* [http://www.lesia.obspm.fr/venus-atm/International « After-Aussois Venus 2010 » workshop: 1st strategic workshop on Coordinated ground-based measurements and modeling of the Venus atmosphere, Paris Observatory, June 28-29, 2010]

Venus coordinated campaign

2010-05-19T12:05:35Z

145.238.174.192: /* Instruments */

This site is intended as a tool to share information, comments and schedules for preparing the 2010 coordinated campaign of ground-based observations in the context of Venus Express and coming launch of Akatsuki mission.

The attached Google docs can be completed and modified according to the campaign progress.
__TOC__

==Map (under construction) ==

* [http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2 2010 Venus Coordinated Campaign, Telescopes sites]

==Coordination==

To prepare the campaign and coordinate telescope proposals with VEx MTPs, the attached table is under construction. Please do not hesitate to comment/modify and add more details on your plans.

Link on:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr 2010 Coordination]

== In-orbit observations ==

=== Venus Express ===

==== Instruments ====

[[Fichier:Instruments_of_venus_express.jpg|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

[http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=33964&fbodylongid=1441 More about the Venus Express Instruments]

=== Akatsuki ===

==== The Project====

The Venus Climate Orbiter mission (PLANET-C), one of the future planetary missions of Japan, aims at understanding the atmospheric circulation of Venus. Meteorological information will be obtained by globally mapping clouds and minor constituents successively with 4 cameras at ultraviolet and infrared wavelengths, detecting lightning with a high-speed imager, and observing the vertical structure of the atmosphere with radio science technique. The equatorial elongated orbit with westward revolution fits the observations of the movement and temporal variation of the Venusian atmosphere which rotates westward. The systematic, continuous imaging observations will provide us with an unprecedented large dataset of the Venusian atmospheric dynamics. Additional targets of the mission are the exploration of the ground surface and the observation of zodiacal light. The mission will complement the ESA's Venus Express, which also explores the Venusian environment with different approaches.

extract of: http://www.stp.isas.jaxa.jp/venus/top_english.html

The project, a link to
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html JAXA]

==== Instrumentation and Techniques ====
[[Fichier:Akatsuki_instrumentation.gif|400px|thumb|right|Instrumentation of Akatsuki, Credit: JAXA]]
* IR1: 1-micron Camera
1.01µm
cloud (day-night), surface (nightside)

* IR2: 2-micron Camera
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65µm

* UVI: Ultraviolet Imager
283, 365 nm
SO2 - UV absorber (dayside)

* LIR: Longwave Infrared Camera
10 µm
cloud top (day/nightside)

* LAC: Lightning and Airglow Camera
Filters
777, 557, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)

[http://www.stp.isas.jaxa.jp/venus/E_instrument.html More about the Akatsuki Instruments]

==Coming meetings==
* [http://lesia.obspm.fr/venus2010/ Venus Conference, Aussois (France), 20-26 June 2010]
* [http://www.lesia.obspm.fr/venus-atm/International « After-Aussois Venus 2010 » workshop: 1st strategic workshop on Coordinated ground-based measurements and modeling of the Venus atmosphere, Paris Observatory, June 28-29, 2010]

Venus coordinated campaign

2010-05-19T12:03:43Z

145.238.174.192: /* Venus Express */

This site is intended as a tool to share information, comments and schedules for preparing the 2010 coordinated campaign of ground-based observations in the context of Venus Express and coming launch of Akatsuki mission.

The attached Google docs can be completed and modified according to the campaign progress.
__TOC__

==Map (under construction) ==

* [http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2 2010 Venus Coordinated Campaign, Telescopes sites]

==Coordination==

To prepare the campaign and coordinate telescope proposals with VEx MTPs, the attached table is under construction. Please do not hesitate to comment/modify and add more details on your plans.

Link on:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr 2010 Coordination]

== In-orbit observations ==

=== Venus Express ===

==== Instruments ====

[[Fichier:Instruments_of_venus_express.jpg|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

[http://sci.esa.int/science-e/www/object/index.cfm?fobjectid=33964&fbodylongid=1441 More about the Venus Express Instruments]

=== Akatsuki ===

==== The Project====

The Venus Climate Orbiter mission (PLANET-C), one of the future planetary missions of Japan, aims at understanding the atmospheric circulation of Venus. Meteorological information will be obtained by globally mapping clouds and minor constituents successively with 4 cameras at ultraviolet and infrared wavelengths, detecting lightning with a high-speed imager, and observing the vertical structure of the atmosphere with radio science technique. The equatorial elongated orbit with westward revolution fits the observations of the movement and temporal variation of the Venusian atmosphere which rotates westward. The systematic, continuous imaging observations will provide us with an unprecedented large dataset of the Venusian atmospheric dynamics. Additional targets of the mission are the exploration of the ground surface and the observation of zodiacal light. The mission will complement the ESA's Venus Express, which also explores the Venusian environment with different approaches.

extract of: http://www.stp.isas.jaxa.jp/venus/top_english.html

The project, a link to
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html JAXA]

==== Instrumentation and Techniques ====
[[Fichier:Akatsuki_instrumentation.gif|400px|thumb|right|Instrumentation of Akatsuki, Credit: JAXA]]
* IR1: 1-micron Camera
1.01µm
cloud (day-night), surface (nightside)

* IR2: 2-micron Camera
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65µm

* UVI: Ultraviolet Imager
283, 365 nm
SO2 - UV absorber (dayside)

* LIR: Longwave Infrared Camera
10 µm
cloud top (day/nightside)

* LAC: Lightning and Airglow Camera
Filters
777, 557, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)

[http://www.stp.isas.jaxa.jp/venus/E_instrument.html More about the Akatsuki Instruments]

==Coming meetings==
* [http://lesia.obspm.fr/venus2010/ Venus Conference, Aussois (France), 20-26 June 2010]
* [http://www.lesia.obspm.fr/venus-atm/International « After-Aussois Venus 2010 » workshop: 1st strategic workshop on Coordinated ground-based measurements and modeling of the Venus atmosphere, Paris Observatory, June 28-29, 2010]

Venus coordinated campaign

2010-05-18T09:13:58Z

145.238.174.192:

This wiki page is intended to support the coming coordinated Venus campaign of 2010, to give an overview of teams and techniques involved, and to serve as a tool for synchronized observations between VEx, Akatsuki with specific input or "wish list" from the modeling community.

The main drive of our coordinated ground-based activity is to study the dynamics of the Venus mesosphere (70-120 km) and lower thermosphere ( > 120 km) using techniques that can only be used from the Earth's ground (e.g. Doppler wind measurements on the day and night side of Venus, minor species distribution and abundance, requiring high spectral resolution in the visible, infrared and sub-millimeter range). Ground-based observations also bring a capability for uninterrupted monitoring of atmospheric structures and wave activity as well as other rapidly varying phenomena.

In recent meetings (Koeln, Brussels, Tokyo) we pointed out science objectives than can be reached out of significant coordination between ground-based and in-orbit measurements, such as continuous O2 1.27µm airglow emission mapping in both hemispheres, effects of planetary-scale waves on the nightglow distribution; strongly variable winds direction and amplitude in sub-mm CO and 10-µm non-LTE CO2 using IR heterodyne on the dayside, and their coupling with thermal field measurements (VEx/SPICAV and VeRa), as well as constrains on the vertical extent of cyclostrophic balance in the mesosphere.

__TOC__

==Map (under construction) ==

* [http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2 2010 Venus Coordinated Campaign telescope sites]

==Instrumentation and Techniques==

Link on the table:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdHQwaklWTlYtRFdocFZQZTd5U3BGY1E&hl=fr Instrumentation and Techniques]

==Observations and Operation Planning==

Link on the table:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr Observations and Operation Planning]

== In-orbit observations ==

=== Venus Express ===

==== Instruments ====

[[Fichier:Instruments_of_venus_express.jpg|300px|thumb|right|Instrumentation of Venus Express, Credit: ESA]]
* ASPERA : Analyser of Space Plasma and Energetic Atoms

* MAG : Venus Express Magnetometer

* SPICAV/SOIR : Ultraviolet and Infrared Atmospheric Spectrometer

* VeRa : Venus Radio Science Experiment

* VIRTIS : Ultraviolet/Visible/Near-Infrared mapping spectrometer

* VMC : Venus Monitoring Camera

=== Akatsuki ===

==== The Project====

The Venus Climate Orbiter mission (PLANET-C), one of the future planetary missions of Japan, aims at understanding the atmospheric circulation of Venus. Meteorological information will be obtained by globally mapping clouds and minor constituents successively with 4 cameras at ultraviolet and infrared wavelengths, detecting lightning with a high-speed imager, and observing the vertical structure of the atmosphere with radio science technique. The equatorial elongated orbit with westward revolution fits the observations of the movement and temporal variation of the Venusian atmosphere which rotates westward. The systematic, continuous imaging observations will provide us with an unprecedented large dataset of the Venusian atmospheric dynamics. Additional targets of the mission are the exploration of the ground surface and the observation of zodiacal light. The mission will complement the ESA's Venus Express, which also explores the Venusian environment with different approaches.

extract of: http://www.stp.isas.jaxa.jp/venus/top_english.html

The project, a link to
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html JAXA]

==== Instrumentation and Techniques ====
[[Fichier:Akatsuki_instrumentation.gif|400px|thumb|right|Instrumentation of Akatsuki, Credit: JAXA]]
* IR1
1.01um
cloud (day-night), surface (nightside)

* IR2
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65um

* UVI 283, 365 nm
SO2 - UV absorber (dayside)

* LIR
10 um
cloud top (day/nightside)

* LAC
777, 551, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)

[http://www.stp.isas.jaxa.jp/venus/E_instrument.html More about the Akatsuki Instruments]

==Coordination==

==Future meetings==

Venus coordinated campaign

2010-05-17T08:34:38Z

145.238.174.192:

It is intended to establish a 'wish list' of coordinated measurements to complement both VEx and Akatsuki's instrumentation in local time, altitude range, regional coverage and constrain mesosphere-thermosphere model parameters. It was noted in recent meetings (Koeln, Brussels, Tokyo) some science objectives can be reached out of significant coordination between ground-based and in-orbit measurements, such as continuous O2 1.27µm airglow emission mapping in both hemispheres, effects of planetary-scale waves on the nightglow distribution; strongly variable winds in sub-mm CO and 10-µm non-LTE CO2 using IR heterodyne on the dayside, and their coupling with thermal field measurements (VEx/SPICAV), constrains on the vertical extent of cyclostrophic balance in the mesosphere.

The main drive of this ground-based activity is to study the dynamics of the Venus mesosphere (70-120 km) and lower thermosphere ( > 120 km) using techniques that can only be accomplished from the ground and not feasible from Venus Express (e.g. Doppler wind measurements on the day and night side of Venus, minor species distribution and abundance, requiring high spectral resolution in the visible, infrared and sub-millimeter range), and with a capability for uninterrupted monitoring of atmospheric wave activity / rapidly varying phenomena.

* Obtain simultaneous measurements over several levels in Venus' upper atmosphere
* Obtain cross-validation of different measurement techniques
* Extended spatial (both hemispheres) and temporal scales
* Constrain modeling of the mesosphere, e.g. validity domain of cyclostrophic approximation

__TOC__

==Map==

* [http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2 2010 Venus Coordinated Campaign]

==Instrumentation and Techniques==

Link on the table:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdHQwaklWTlYtRFdocFZQZTd5U3BGY1E&hl=fr Instrumentation and Techniques]

==Observations and Operation Planning==

Link on the table:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr Observations and Operation Planning]

== In-orbit observations ==

=== Venus Express ===

==== Instruments ====

[[Fichier:Instruments_of_venus_express.jpg|300px|thumb|right|Instrumentation of Venus Express, Credit: ESA]]
* ASPERA : Analyser of Space Plasma and Energetic Atoms

* MAG : Venus Express Magnetometer

* SPICAV/SOIR : Ultraviolet and Infrared Atmospheric Spectrometer

* VeRa : Venus Radio Science Experiment

* VIRTIS : Ultraviolet/Visible/Near-Infrared mapping spectrometer

* VMC : Venus Monitoring Camera

=== Akatsuki ===

==== The Project====

The Venus Climate Orbiter mission (PLANET-C), one of the future planetary missions of Japan, aims at understanding the atmospheric circulation of Venus. Meteorological information will be obtained by globally mapping clouds and minor constituents successively with 4 cameras at ultraviolet and infrared wavelengths, detecting lightning with a high-speed imager, and observing the vertical structure of the atmosphere with radio science technique. The equatorial elongated orbit with westward revolution fits the observations of the movement and temporal variation of the Venusian atmosphere which rotates westward. The systematic, continuous imaging observations will provide us with an unprecedented large dataset of the Venusian atmospheric dynamics. Additional targets of the mission are the exploration of the ground surface and the observation of zodiacal light. The mission will complement the ESA's Venus Express, which also explores the Venusian environment with different approaches.

extract of: http://www.stp.isas.jaxa.jp/venus/top_english.html

The project, a link to JAXA:
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html JAXA]

==== Instrumentation and Techniques ====
[[Fichier:Akatsuki_instrumentation.gif|400px|thumb|right|Instrumentation of Akatsuki, Credit: JAXA]]
* IR1
1.01um
cloud (day-night), surface (nightside)

* IR2
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65um

* UVI 283, 365 nm
SO2 - UV absorber (dayside)

* LIR
10 um
cloud top (day/nightside)

* LAC
777, 551, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)

[http://www.stp.isas.jaxa.jp/venus/E_instrument.html More about the Akatsuki Instruments]

Accueil

2010-05-10T12:32:37Z

145.238.174.192: /* Venus Express */

Accueil

2010-05-10T12:32:15Z

145.238.174.192: /* The Project */

Accueil

2010-05-10T12:32:03Z

145.238.174.192: /* The Project */

Accueil

2010-05-10T12:31:36Z

145.238.174.192: /* The Project */

Accueil

2010-05-10T08:27:26Z

145.238.174.192: /* Instruments */

Accueil

2010-05-10T08:26:46Z

145.238.174.192: /* Instruments */

Accueil

2010-05-10T08:26:23Z

145.238.174.192: /* Instruments */

Accueil

2010-05-10T08:24:38Z

145.238.174.192: /* Instruments */

Accueil

2010-05-10T08:21:22Z

145.238.174.192: /* Map of the groundbased observations */

'''Overview of the Page venus-atm'''

Goal of Earth-based observations in the VEx-VCO/Akatsuki context

* Perform direct measurements not feasible by an orbiter
e. g. provide direct absolute wind measurements
* Obtain simultaneous measurements over several levels in Venus' upper atmosphere
* Obtain cross-validation of different measurement techniques
* Extended spatial (both hemispheres) and temporal scales
* Constrain modeling of the mesosphere, e.g. validity domain of cyclostrophic approximation

__TOC__

==Map==

Googlemap:
* [http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2 2010 Venus Coordinated Campaign]

$wgGoogleMapsKey = "ABQIAAAAlPAF_RpXQsb-9OA4bmfhuBROdUV6dnkNQ2wycpqjH1x_Q4S5MRRZCrmYQpMvvMzZ3_8K13uVJi0KhQ";
require_once( "$IP/extensions/GoogleMaps/GoogleMaps.php" );

==Instrumentation and Techniques==
Explanation of the table, contenu et but

Link on the table:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdHQwaklWTlYtRFdocFZQZTd5U3BGY1E&hl=fr Instrumentation and Techniques]

==Observations and Operation Planning==

Link on the table:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr Observations and Operation Planning]

== In-orbit observations ==

=== Venus Express ===

[[File:Venus Express in orbit.jpg⎮200px⎮thumb⎮left⎮ESA's Venus Express]]

==== Instruments ====
* Analyser of Space Plasma and Energetic Atoms ('''ASPERA''')

Led by Institute of Space Physics, Kiruna, Sweden

ASPERA will investigate the interaction between the solar wind and the atmosphere of Venus by measuring outflowing particles from the planet’s atmosphere and the particles making up the solar wind. It will study how the molecules and ions escape the planet.

* Venus Express Magnetometer ('''MAG''')

Led by IWF, Graz, Austria

Venus has no detectable internal magnetic field, and the field that exists around the planet is entirely due to the interaction between the solar wind and the atmosphere. The MAG magnetometer will study this process and will help in understanding the effect this has on Venus’s atmosphere, for instance the atmospheric escape process.

* Planetary Fourier Spectrometer ('''PFS''')

Led by IFSI-INAF, Rome, Italy

PFS will be able to measure the temperature of the atmosphere between altitudes of 55–100 kilometres at a very high resolution. It will also be able to measure the surface temperature and therefore be able to search for volcanic activity. In addition to its temperature measurements, PFS will be able to make composition measurements of the atmosphere.

* Ultraviolet and Infrared Atmospheric Spectrometer ('''SPICAV/SOIR''')

Led by Service d’Aeronomie du CNRS, Verriesres, France; Institute for Space Aeronomy, Belgium; IKI, Russia

SPICAV assists in the analysis of Venus’s atmosphere. In particular, it will search for the small quantities of water expected to exist in the Venusian atmosphere. It will also look for sulphur compounds and molecular oxygen in the atmosphere. It will determine the density and temperature of the atmosphere at 80–180 kilometres altitude.

* Venus Radio Science Experiment ('''VeRa''')

Led by Univ. der Bunderswehr, Munich, Germany

VeRa uses the powerful radio link between the spacecraft and Earth to investigate the conditions prevalent in the ionosphere of Venus. Scientists will also use it to study the density, temperature, and pressure of the atmosphere from 35–40 km up to 100 km from the surface, and to determine roughness and electrical properties of the surface. It will also allow investigations of the conditions of the solar wind in the inner part of the Solar System.

* Ultraviolet/Visible/Near-Infrared mapping spectrometer ('''VIRTIS''')

Led by CNR-IASF, Rome, Italy, and Observatoire de Paris, France

VIRTIS will be able to study the composition of the lower atmosphere between 40 kilometres altitude and the surface. It will track the clouds in both ultraviolet and infrared wavelengths and allow scientists to study atmospheric dynamics at different altitudes.

* Venus Monitoring Camera ('''VMC''')

Led by MPS, Katlenburg-Lindau, Germany

VMC is a wide-angle multi-channel camera that will be able to take images of the planet in the near infrared, ultraviolet and visible wavelengths. VMC will be able to make global images and will study the cloud dynamics and image the surface. In addition it will assist in the identification of phenomena seen by other instruments.

<gallery>

[[Fichier:http://esamultimedia.esa.int/images/venusexpress/31_AI3_H.jpg]]

</gallery>

[[File:venusexpress.jpg|200px|thumb|center|Venus Express]]

[[Fichier:http://www.stp.isas.jaxa.jp/venus/images/gallery/PLANET-C2.jpg]]

=== Akatsuki ===

==== The Project====

A short presentation of the project?

The project, a link to JAXA:
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html JAXA]

==== The Instrument and Techniques ====

* IR1
1.01um
cloud (day-night), surface (nightside)

* IR2
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65um

* UVI 283, 365 nm
SO2 - UV absorber (dayside)

* LIR
10 um
cloud top (day/nightside)

* LAC
777, 551, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)

[http://www.stp.isas.jaxa.jp/venus/E_instrument.html More about the Akatsuki Instruments]

Accueil

2010-05-10T07:51:06Z

145.238.174.192: /* In-orbit observations */

'''Overview of the Page venus-atm'''

Goal of Earth-based observations in the VEx-VCO/Akatsuki context

* Perform direct measurements not feasible by an orbiter
e. g. provide direct absolute wind measurements
* Obtain simultaneous measurements over several levels in Venus' upper atmosphere
* Obtain cross-validation of different measurement techniques
* Extended spatial (both hemispheres) and temporal scales
* Constrain modeling of the mesosphere, e.g. validity domain of cyclostrophic approximation

__TOC__

==Map of the groundbased observations==

Groundbased observations

Googlemap:
* [http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2 2010 Venus Coordinated Campaign]

http://www.evanmiller.org/maps/GoogleMaps-0.9.4.zip

$wgGoogleMapsKey = "ABQIAAAAlPAF_RpXQsb-9OA4bmfhuBROdUV6dnkNQ2wycpqjH1x_Q4S5MRRZCrmYQpMvvMzZ3_8K13uVJi0KhQ";
require_once( "$IP/extensions/GoogleMaps/GoogleMaps.php" );

<googlemap><iframe width="425" height="350" frameborder="0" scrolling="no" marginheight="0" marginwidth="0" src="http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-3.162456,11.601563&spn=104.451773,149.414063&z=2&output=embed"></iframe><br /><small>Afficher <a href="http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-3.162456,11.601563&spn=104.451773,149.414063&z=2&source=embed" style="color:#0000FF;text-align:left">2010 Venus Coordinated Campaign</a> sur une carte plus grande</small><googlemap/>

==Instrumentation and Techniques==
Explanation of the table, contenu et but

Link on the table:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdHQwaklWTlYtRFdocFZQZTd5U3BGY1E&hl=fr Instrumentation and Techniques]

==Observations and Operation Planning==

Link on the table:
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr Observations and Operation Planning]

== In-orbit observations ==

=== Venus Express ===

[[File:Venus Express in orbit.jpg⎮200px⎮thumb⎮left⎮ESA's Venus Express]]

==== Instruments ====
* Analyser of Space Plasma and Energetic Atoms ('''ASPERA''')

Led by Institute of Space Physics, Kiruna, Sweden

ASPERA will investigate the interaction between the solar wind and the atmosphere of Venus by measuring outflowing particles from the planet’s atmosphere and the particles making up the solar wind. It will study how the molecules and ions escape the planet.

* Venus Express Magnetometer ('''MAG''')

Led by IWF, Graz, Austria

Venus has no detectable internal magnetic field, and the field that exists around the planet is entirely due to the interaction between the solar wind and the atmosphere. The MAG magnetometer will study this process and will help in understanding the effect this has on Venus’s atmosphere, for instance the atmospheric escape process.

* Planetary Fourier Spectrometer ('''PFS''')

Led by IFSI-INAF, Rome, Italy

PFS will be able to measure the temperature of the atmosphere between altitudes of 55–100 kilometres at a very high resolution. It will also be able to measure the surface temperature and therefore be able to search for volcanic activity. In addition to its temperature measurements, PFS will be able to make composition measurements of the atmosphere.

* Ultraviolet and Infrared Atmospheric Spectrometer ('''SPICAV/SOIR''')

Led by Service d’Aeronomie du CNRS, Verriesres, France; Institute for Space Aeronomy, Belgium; IKI, Russia

SPICAV assists in the analysis of Venus’s atmosphere. In particular, it will search for the small quantities of water expected to exist in the Venusian atmosphere. It will also look for sulphur compounds and molecular oxygen in the atmosphere. It will determine the density and temperature of the atmosphere at 80–180 kilometres altitude.

* Venus Radio Science Experiment ('''VeRa''')

Led by Univ. der Bunderswehr, Munich, Germany

VeRa uses the powerful radio link between the spacecraft and Earth to investigate the conditions prevalent in the ionosphere of Venus. Scientists will also use it to study the density, temperature, and pressure of the atmosphere from 35–40 km up to 100 km from the surface, and to determine roughness and electrical properties of the surface. It will also allow investigations of the conditions of the solar wind in the inner part of the Solar System.

* Ultraviolet/Visible/Near-Infrared mapping spectrometer ('''VIRTIS''')

Led by CNR-IASF, Rome, Italy, and Observatoire de Paris, France

VIRTIS will be able to study the composition of the lower atmosphere between 40 kilometres altitude and the surface. It will track the clouds in both ultraviolet and infrared wavelengths and allow scientists to study atmospheric dynamics at different altitudes.

* Venus Monitoring Camera ('''VMC''')

Led by MPS, Katlenburg-Lindau, Germany

VMC is a wide-angle multi-channel camera that will be able to take images of the planet in the near infrared, ultraviolet and visible wavelengths. VMC will be able to make global images and will study the cloud dynamics and image the surface. In addition it will assist in the identification of phenomena seen by other instruments.

<gallery>

[[Fichier:http://esamultimedia.esa.int/images/venusexpress/31_AI3_H.jpg]]

</gallery>

[[File:venusexpress.jpg|200px|thumb|center|Venus Express]]

[[Fichier:http://www.stp.isas.jaxa.jp/venus/images/gallery/PLANET-C2.jpg]]

=== Akatsuki ===

==== The Project====

A short presentation of the project?

The project, a link to JAXA:
[http://www.jaxa.jp/projects/sat/planet_c/index_e.html JAXA]

==== The Instrument and Techniques ====

* IR1
1.01um
cloud (day-night), surface (nightside)

* IR2
1.73, 2.26, 2.32 (near-IR)
2.02 (CO2), 1.65um

* UVI 283, 365 nm
SO2 - UV absorber (dayside)

* LIR
10 um
cloud top (day/nightside)

* LAC
777, 551, 553, 558, 630 nm
O2/O airglow (night)
lightning (night)

[http://www.stp.isas.jaxa.jp/venus/E_instrument.html More about the Akatsuki Instruments]

Accueil

2010-05-06T14:39:13Z

145.238.174.192: /* Observations and Operation Planning */

'''Page venus-atm'''

Goal of Earth-based observations in the VEx-VCO/Akatsuki context

* Perform direct measurements not feasible by an orbiter
e. g. provide direct absolute wind measurements
* Obtain simultaneous measurements over several levels in Venus' upper atmosphere
* Obtain cross-validation of different measurement techniques
* Extended spatial (both hemispheres) and temporal scales
* Constrain modeling of the mesosphere, e.g. validity domain of cyclostrophic approximation

__TOC__

==Map==
Link on google map
* http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2

==Instrumentation and Techniques==

Link on the table
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdHQwaklWTlYtRFdocFZQZTd5U3BGY1E&hl=fr]

==Observations and Operation Planning==

Link on the table
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr]

==Venus Express==

Instruments:
* Analyser of Space Plasma and Energetic Atoms (ASPERA)

Led by Institute of Space Physics, Kiruna, Sweden

ASPERA will investigate the interaction between the solar wind and the atmosphere of Venus by measuring outflowing particles from the planet’s atmosphere and the particles making up the solar wind. It will study how the molecules and ions escape the planet.

* Venus Express Magnetometer (MAG)

Led by IWF, Graz, Austria

Venus has no detectable internal magnetic field, and the field that exists around the planet is entirely due to the interaction between the solar wind and the atmosphere. The MAG magnetometer will study this process and will help in understanding the effect this has on Venus’s atmosphere, for instance the atmospheric escape process.

* Planetary Fourier Spectrometer (PFS)

Led by IFSI-INAF, Rome, Italy

PFS will be able to measure the temperature of the atmosphere between altitudes of 55–100 kilometres at a very high resolution. It will also be able to measure the surface temperature and therefore be able to search for volcanic activity. In addition to its temperature measurements, PFS will be able to make composition measurements of the atmosphere.

* Ultraviolet and Infrared Atmospheric Spectrometer (SPICAV/SOIR)

Led by Service d’Aeronomie du CNRS, Verriesres, France; Institute for Space Aeronomy, Belgium; IKI, Russia

SPICAV assists in the analysis of Venus’s atmosphere. In particular, it will search for the small quantities of water expected to exist in the Venusian atmosphere. It will also look for sulphur compounds and molecular oxygen in the atmosphere. It will determine the density and temperature of the atmosphere at 80–180 kilometres altitude.

* Venus Radio Science Experiment (VeRa)

Led by Univ. der Bunderswehr, Munich, Germany

VeRa uses the powerful radio link between the spacecraft and Earth to investigate the conditions prevalent in the ionosphere of Venus. Scientists will also use it to study the density, temperature, and pressure of the atmosphere from 35–40 km up to 100 km from the surface, and to determine roughness and electrical properties of the surface. It will also allow investigations of the conditions of the solar wind in the inner part of the Solar System.

* Ultraviolet/Visible/Near-Infrared mapping spectrometer (VIRTIS)

Led by CNR-IASF, Rome, Italy, and Observatoire de Paris, France

VIRTIS will be able to study the composition of the lower atmosphere between 40 kilometres altitude and the surface. It will track the clouds in both ultraviolet and infrared wavelengths and allow scientists to study atmospheric dynamics at different altitudes.

<gallery>

[[Fichier:http://esamultimedia.esa.int/images/venusexpress/31_AI3_H.jpg]]

</gallery>

==Akatsuki==
Lancement
Projets

Accueil

2010-05-06T14:38:58Z

145.238.174.192: /* Observations and Operation Planning */

'''Page venus-atm'''

Goal of Earth-based observations in the VEx-VCO/Akatsuki context

* Perform direct measurements not feasible by an orbiter
e. g. provide direct absolute wind measurements
* Obtain simultaneous measurements over several levels in Venus' upper atmosphere
* Obtain cross-validation of different measurement techniques
* Extended spatial (both hemispheres) and temporal scales
* Constrain modeling of the mesosphere, e.g. validity domain of cyclostrophic approximation

__TOC__

==Map==
Link on google map
* http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2

==Instrumentation and Techniques==

Link on the table
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdHQwaklWTlYtRFdocFZQZTd5U3BGY1E&hl=fr]

==Observations and Operation Planning==

Link on the table

[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdGNENE56UU9WRVJodWZpMk81cE9aTWc&hl=fr]

==Venus Express==

Instruments:
* Analyser of Space Plasma and Energetic Atoms (ASPERA)

Led by Institute of Space Physics, Kiruna, Sweden

ASPERA will investigate the interaction between the solar wind and the atmosphere of Venus by measuring outflowing particles from the planet’s atmosphere and the particles making up the solar wind. It will study how the molecules and ions escape the planet.

* Venus Express Magnetometer (MAG)

Led by IWF, Graz, Austria

Venus has no detectable internal magnetic field, and the field that exists around the planet is entirely due to the interaction between the solar wind and the atmosphere. The MAG magnetometer will study this process and will help in understanding the effect this has on Venus’s atmosphere, for instance the atmospheric escape process.

* Planetary Fourier Spectrometer (PFS)

Led by IFSI-INAF, Rome, Italy

PFS will be able to measure the temperature of the atmosphere between altitudes of 55–100 kilometres at a very high resolution. It will also be able to measure the surface temperature and therefore be able to search for volcanic activity. In addition to its temperature measurements, PFS will be able to make composition measurements of the atmosphere.

* Ultraviolet and Infrared Atmospheric Spectrometer (SPICAV/SOIR)

Led by Service d’Aeronomie du CNRS, Verriesres, France; Institute for Space Aeronomy, Belgium; IKI, Russia

SPICAV assists in the analysis of Venus’s atmosphere. In particular, it will search for the small quantities of water expected to exist in the Venusian atmosphere. It will also look for sulphur compounds and molecular oxygen in the atmosphere. It will determine the density and temperature of the atmosphere at 80–180 kilometres altitude.

* Venus Radio Science Experiment (VeRa)

Led by Univ. der Bunderswehr, Munich, Germany

VeRa uses the powerful radio link between the spacecraft and Earth to investigate the conditions prevalent in the ionosphere of Venus. Scientists will also use it to study the density, temperature, and pressure of the atmosphere from 35–40 km up to 100 km from the surface, and to determine roughness and electrical properties of the surface. It will also allow investigations of the conditions of the solar wind in the inner part of the Solar System.

* Ultraviolet/Visible/Near-Infrared mapping spectrometer (VIRTIS)

Led by CNR-IASF, Rome, Italy, and Observatoire de Paris, France

VIRTIS will be able to study the composition of the lower atmosphere between 40 kilometres altitude and the surface. It will track the clouds in both ultraviolet and infrared wavelengths and allow scientists to study atmospheric dynamics at different altitudes.

<gallery>

[[Fichier:http://esamultimedia.esa.int/images/venusexpress/31_AI3_H.jpg]]

</gallery>

==Akatsuki==
Lancement
Projets

Accueil

2010-05-06T14:38:23Z

145.238.174.192:

'''Page venus-atm'''

Goal of Earth-based observations in the VEx-VCO/Akatsuki context

* Perform direct measurements not feasible by an orbiter
e. g. provide direct absolute wind measurements
* Obtain simultaneous measurements over several levels in Venus' upper atmosphere
* Obtain cross-validation of different measurement techniques
* Extended spatial (both hemispheres) and temporal scales
* Constrain modeling of the mesosphere, e.g. validity domain of cyclostrophic approximation

__TOC__

==Map==
Link on google map
* http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2

==Instrumentation and Techniques==

Link on the table
[http://spreadsheets.google.com/ccc?key=0Am6asZV0iMhhdHQwaklWTlYtRFdocFZQZTd5U3BGY1E&hl=fr]

==Observations and Operation Planning==

Link on the table

==Venus Express==

Instruments:
* Analyser of Space Plasma and Energetic Atoms (ASPERA)

Led by Institute of Space Physics, Kiruna, Sweden

ASPERA will investigate the interaction between the solar wind and the atmosphere of Venus by measuring outflowing particles from the planet’s atmosphere and the particles making up the solar wind. It will study how the molecules and ions escape the planet.

* Venus Express Magnetometer (MAG)

Led by IWF, Graz, Austria

Venus has no detectable internal magnetic field, and the field that exists around the planet is entirely due to the interaction between the solar wind and the atmosphere. The MAG magnetometer will study this process and will help in understanding the effect this has on Venus’s atmosphere, for instance the atmospheric escape process.

* Planetary Fourier Spectrometer (PFS)

Led by IFSI-INAF, Rome, Italy

PFS will be able to measure the temperature of the atmosphere between altitudes of 55–100 kilometres at a very high resolution. It will also be able to measure the surface temperature and therefore be able to search for volcanic activity. In addition to its temperature measurements, PFS will be able to make composition measurements of the atmosphere.

* Ultraviolet and Infrared Atmospheric Spectrometer (SPICAV/SOIR)

Led by Service d’Aeronomie du CNRS, Verriesres, France; Institute for Space Aeronomy, Belgium; IKI, Russia

SPICAV assists in the analysis of Venus’s atmosphere. In particular, it will search for the small quantities of water expected to exist in the Venusian atmosphere. It will also look for sulphur compounds and molecular oxygen in the atmosphere. It will determine the density and temperature of the atmosphere at 80–180 kilometres altitude.

* Venus Radio Science Experiment (VeRa)

Led by Univ. der Bunderswehr, Munich, Germany

VeRa uses the powerful radio link between the spacecraft and Earth to investigate the conditions prevalent in the ionosphere of Venus. Scientists will also use it to study the density, temperature, and pressure of the atmosphere from 35–40 km up to 100 km from the surface, and to determine roughness and electrical properties of the surface. It will also allow investigations of the conditions of the solar wind in the inner part of the Solar System.

* Ultraviolet/Visible/Near-Infrared mapping spectrometer (VIRTIS)

Led by CNR-IASF, Rome, Italy, and Observatoire de Paris, France

VIRTIS will be able to study the composition of the lower atmosphere between 40 kilometres altitude and the surface. It will track the clouds in both ultraviolet and infrared wavelengths and allow scientists to study atmospheric dynamics at different altitudes.

<gallery>

[[Fichier:http://esamultimedia.esa.int/images/venusexpress/31_AI3_H.jpg]]

</gallery>

==Akatsuki==
Lancement
Projets

Accueil

2010-05-06T14:33:05Z

145.238.174.192:

'''Page venus-atm'''

Goal of Earth-based observations in the VEx-VCO/Akatsuki context

* Perform direct measurements not feasible by an orbiter
e. g. provide direct absolute wind measurements
* Obtain simultaneous measurements over several levels in Venus' upper atmosphere
* Obtain cross-validation of different measurement techniques
* Extended spatial (both hemispheres) and temporal scales
* Constrain modeling of the mesosphere, e.g. validity domain of cyclostrophic approximation

__TOC__

==Map==
Link on google map
* http://maps.google.com/maps/ms?ie=UTF8&hl=fr&msa=0&msid=106784557914957315781.000481c7cd8ab690441fc&ll=-11.178402,-54.492187&spn=163.437297,68.554688&z=2

==Instrumentation and Techniques==

Link on the table

==Observations and Operation Planning==

Link on the table

==Venus Express==

Instruments:
* Analyser of Space Plasma and Energetic Atoms (ASPERA)

Led by Institute of Space Physics, Kiruna, Sweden

ASPERA will investigate the interaction between the solar wind and the atmosphere of Venus by measuring outflowing particles from the planet’s atmosphere and the particles making up the solar wind. It will study how the molecules and ions escape the planet.

* Venus Express Magnetometer (MAG)

Led by IWF, Graz, Austria

Venus has no detectable internal magnetic field, and the field that exists around the planet is entirely due to the interaction between the solar wind and the atmosphere. The MAG magnetometer will study this process and will help in understanding the effect this has on Venus’s atmosphere, for instance the atmospheric escape process.

* Planetary Fourier Spectrometer (PFS)

Led by IFSI-INAF, Rome, Italy

PFS will be able to measure the temperature of the atmosphere between altitudes of 55–100 kilometres at a very high resolution. It will also be able to measure the surface temperature and therefore be able to search for volcanic activity. In addition to its temperature measurements, PFS will be able to make composition measurements of the atmosphere.

* Ultraviolet and Infrared Atmospheric Spectrometer (SPICAV/SOIR)

Led by Service d’Aeronomie du CNRS, Verriesres, France; Institute for Space Aeronomy, Belgium; IKI, Russia

SPICAV assists in the analysis of Venus’s atmosphere. In particular, it will search for the small quantities of water expected to exist in the Venusian atmosphere. It will also look for sulphur compounds and molecular oxygen in the atmosphere. It will determine the density and temperature of the atmosphere at 80–180 kilometres altitude.

* Venus Radio Science Experiment (VeRa)

Led by Univ. der Bunderswehr, Munich, Germany

VeRa uses the powerful radio link between the spacecraft and Earth to investigate the conditions prevalent in the ionosphere of Venus. Scientists will also use it to study the density, temperature, and pressure of the atmosphere from 35–40 km up to 100 km from the surface, and to determine roughness and electrical properties of the surface. It will also allow investigations of the conditions of the solar wind in the inner part of the Solar System.

* Ultraviolet/Visible/Near-Infrared mapping spectrometer (VIRTIS)

Led by CNR-IASF, Rome, Italy, and Observatoire de Paris, France

VIRTIS will be able to study the composition of the lower atmosphere between 40 kilometres altitude and the surface. It will track the clouds in both ultraviolet and infrared wavelengths and allow scientists to study atmospheric dynamics at different altitudes.

<gallery>

[[Fichier:http://esamultimedia.esa.int/images/venusexpress/31_AI3_H.jpg]]

</gallery>

==Akatsuki==
Lancement
Projets

Accueil

2010-05-06T08:39:57Z

145.238.174.192:

Accueil

2010-05-05T13:55:46Z

145.238.174.192:

'''Page venus-atm'''

Goal of Earth-based observations in the VEx-VCO/Akatsuki context

- Perform direct measurements not feasible by an orbiter
e. g. provide direct absolute wind measurements
- obtain simultaneous measurements over several levels in Venus' upper atmosphere
- Obtain cross-validation of different measurement techniques
- Extended spatial (both hemispheres) and temporal scales
- Constrain modeling of the mesosphere, e.g. validity domain of cyclostrophic approximation

__TOC__

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