Other satellite missions flown during the Planck mission

General information

• Launched on 14 May 2009 together with PLANCK aboard an Ariane 5 rocket
• Mission ends 2011-2012
• Operates from an orbit around the Lagrangian point L2 in the Sun/Earth system
  located approximately 1.5 million km away from the Earth in the antisunward direction

The key scientific objectives

• Study the formation of galaxies in the early universe and their subsequent evolution
• Investigate the creation of stars and their interaction with the interstellar medium
• Observe the chemical composition of the atmospheres and surfaces of comets, planets and satellites
• Examine the molecular chemistry of the universe

The HERSCHEL Instruments

HIFI - Heterodyne Instrument for the Far Infrared

• Very high resolution heterodyne spectroscopy spanning 480-1250 and 1410-1910 GHz
• Offers velocity resolution in the range 0.3-300 km/s

PACS - Photodetector Array Camera and Spectrometer

• Imaging photometer and integral field line spectrometer for wavelengths between 60-210 micrometers
• Point source detection limit 4-10*10^-18 W/m^2

SPIRE - Spectral and Photometric Imaging Receiver

• 3-band imaging photometer (simultaneous observation in 3 bands): wavelengths 250, 350, 500 um
• Imaging Fourier Transform Spectrometer (FTS): wavelengths 194-672 um

INTEGRAL

• The International Gamma-Ray Astrophysics Laboratory, ESA
  

General information

• INTEGRAL was launched on 17.10.2002
• Highly eccentric orbit (HEO)
• Mission extended to 31.12. 2012

The key scientific objectives

The scientific goals of Integral are addressed through the use of high resolution spectroscopy with fine imaging and accurate positioning of celestial sources in the gamma-ray domain.

• Compact Objects
• Extragalatic astronomy
• Stellar nucleosynthesis (eg in supernovae)
• Galactic structure and the Galactic centre
• Particle processes and acceleration
• Identification of high energy sources
• Monitor for transient sources

The INTEGRAL Instruments

Spectrometer SPI

• Performs spectral analysis of gamma-ray point sources and extended regions in the 20 keV - 8 MeV energy range
• Energy resolution of 2.2 keV (FWHM) at 1.33 MeV

Imager IBIS

• Provides diagnostic capabilities of fine imaging (12 arcmin FWHM), source identification and spectral sensitivity to both continuum and broad lines
• Energy range 15 keV - 10 MeV

X-Ray Monitor JEM-X

• Makes observations simultaneously with the main gamma-ray instruments and provides images with arcminute angular resolution
• Energy range 3 - 35 keV

Optical Monitoring Camera OMC

• Passively cooled CCD

Spitzer

General information

• Spitzer was launched on 25.8.2003
• An Earth-trailing, Heliocentric orbit
• Estimated lifetime 2.5 years (minimum); 5+ years (goal)

The key scientific objectives

• Search for brown dwarfs and super-planets
• Discovery and study of debris disks around nearby stars
• Study of ultraluminous infrared galaxies and active galactic nuclei
• Study of the early universe

The Spitzer Instruments

The Spitzer Space Telescope consists of a 0.85-meter diameter telescope and three cryogenically-cooled science instruments which will perform imaging and spectroscopy in the 3 - 180 micron wavelength range.

IRS - InfraRed Spectrograph

• Provides both high- and low-resolution spectroscopy at mid-infrared wavelengths
• Low-resolution, short-wavelength mode: 5.3-14 microns
• High-resolution, short-wavelength mode: 10-19.5 microns
• Low-resolution, long-wavelength mode: 14-40 microns
• High-resolution, long-wavelength mode: 19-37 microns

IRAC - Infrared Camera

• Provides imaging capabilities at near- and mid-infrared wavelengths
• Consists of 4 imaging arrays that provide simultaneous images at wavelengths of 3.6, 4.5, 5.8, and 8.0 microns
• Each of the four detector arrays are 256 x 256 pixels in size

The Multiband Imaging Photometer for Spitzer (MIPS)

• Provides imaging and limited spectroscopic data at far-infrared wavelengths
• 128 x 128 array for imaging at 24 microns
• 32 x 32 array for imaging at 70 microns, takes also spectra from 50 - 100 microns
• 2 x 20 array for imaging at 160 microns
• Field of view: from about 5x5 arcmin (shortest wavelength) to about 0.5x5 arcmin (longest wavelength)

Swift

Swift Main Index
NASA Swift Homepage

General information

• Swift was launched on 20.11.2004
• Circular low Earth orbit at 600km
• Mission duration is 2 years

The key scientific objectives

• Determine the origin of gamma-ray bursts (GRB)
• Classify gamma-ray bursts and search for new types
• Determine how the blastwave evolves and interacts with the surroundings
• Use gamma-ray bursts to study the early universe
• Perform the first sensitive hard X-ray survey of the sky

• Survey the hard x-ray sky to a sensitivity of 0.6 mCrab at high galactic latitude and 2 mCrab along the galactic plane
• Search for obscured Seyfert-2 type AGN

More about Swift's scientific objectives

The Swift Instruments

Three instruments will work together to observe GRBs and afterglows in the gamma-ray, X-ray, ultraviolet, and optical wavebands. BAT will detect and acquire locations for GRBs and then relay a 1-4 arc-minute position estimate to the ground within 15 seconds. After the initial burst detection, the spacecraft will quickly (20-75 seconds) and autonomously repoint itself to bring the burst location within the field of view of XRT and UVOT to observe the afterglow. Swift will provide redshifts for the bursts and multi-wavelength lightcurves for the duration of the afterglow.

BAT - Burst Alert Telescope

While searching for bursts, the BAT will perform an all-sky hard X-ray survey. Sky images are searched to detect and position sources.

• Detecting Area: 5200 cm2
• Field of View: 1.4 sr (partially coded)
• Location Accuracy: 1-4 arcminutes
• Energy Range: 15-150 keV

XRT - X-Ray Telescope

The XRT is designed to measure the fluxes, spectra, and lightcurves of GRBs and afterglows over a wide dynamic range covering more than 7 orders of magnitude in flux.
• Effective Area: 135 cm2 at 1.5 keV
• Field of View: 23.6 x 23.6 arcminutes
• Location Accuracy: 3-5 arcseconds
• Energy Range: 0.2-10 keV

UVOT - Ultraviolet/Optical Telescope

• The UVOT is uniquely capable for afterglow studies
• Telescope: 30 cm Ritchey-Chretien
• Detector: Intensified CCD
• Field of View: 17 x 17 arcminutes
• Location Accuracy: 0.3 arcseconds
• Wavelength Range: 170 nm - 650 nm

IXO/XEUS

• The International X-ray Observatory/X-Ray Evolving Universe Spectrometer, ESA/NASA/JAXA

XEUS is a follow-on to ESA's Cornerstone X-Ray Spectroscopy Mission (XMM-Newton). XEUS will be a permanent space-borne X-ray observatory with a sensitivity comparable to the most advanced planned future facilities such as JWST, ALMA and Herschel.

General information

• Planned launch in 2020-2021
• Estimated lifetime min. 5 years, goal 10 years
• XEUS will be placed into orbit at the second Earth-Sun Langrangian point L2

• Black holes and matter under extreme conditions
• Formation and evolution of galaxies, clusters and large scale structure
• Life cycles of matter and energy

• 3 m^2 of collecting area
• Baseline instrument concept

VSOP-2

• VLBI Space Observatory Program 2, JAXA (Japan)
  

VSOP-2 will be a spaceborne radio-interferometry satellite

General information

• Expected launch in 2012
• Estimated lifetime is 5 years

• Studies of super-luminal Sources
• Studies of nearby AGNs
• Cosmological test
• Extragalactic and galactic masers, and the interstellar matter

• Antenna diameter is 9.0 meters, design is a off-axis parabola.
• Observing bands 8 GHz, 22 GHz and 43 GHz.
• Resolution in microarcseconds 205 at 8GHz, 75 at 22 GHz
  and 38 at 43 GHz.
• System temperature is 60 K at 8 GHz, 30 K at 22 GHz and 40 K at 43 GHz.

James Webb Space Telescope

General information

• Will be launched 2013(earliest) by an Ariane V rocket
• Orbit in L2, 1.5 million km from Earth
• required lifetime 5 years, goal lifetime 10 years

• The End of the Dark Ages: First Light and Reionization
• Assembly of Galaxies
• The Birth of Stars and Protoplanetary Systems
• Planetary Systems and the Origins of Life

• Diameter of main mirror 6.5 meters, the mirror is deployable, thin, active and light
• Wavelength range 0.6-27 microns

NIRCam - Near Infrared Camera

• Near-IR and visible camera
• Sensitive over the 0.6-5 micron wavelength range
• 2.2 x 2.2 arcmin field of view

NIRSpec - Near Infrared Spectrograph

• Multi-object dispersive spectrograph (MOS)
• Sensitive over the 1-5 micron wavelength range
• 3.4 x 3.4 arcmin field of view

MIRI - Mid Infrared Instrument

• Mid-IR camera and Integral Field Unit (IFU) and long-slit spectrograph
• Sensitive over the 5-27 micron wavelength range
• 1.88 x 1.27 arcmin field of view imaging

FGS - Fine Guidance Sensor

• Fine Guidance System
• Enable stable pointing at the milli-arcsecond level

AGILE

• Astro-rivelatore Gamma a Immagini LEggero

AGILE is a Small Scientific Mission devoted to gamma-ray astrophysics supported by the Italian Space Agency (ASI).

General information

• Launched April 23, 2007.
• No other mission dedicated to gamma-ray astrophysics in the energy band 30 MeV - 30 GeV will be operational during that period

• Active Galactic Nuclei
• Gamma-Ray Bursts
• Pulsars
• Unidentified sources
• Supernova remnants
• Binary systems
• Diffuse emission
• Galaxies
• Fundamental physics

Gamma-Ray Imaging Detector

• Sensitive in the energy range ~30MeV - 50GeV
• Field of view: 3 sr

• Provides detection and imaging capabilities in the X-ray range

• Acts as AGILE' s calorimeter (GRID mode) or detects strong g transient events (BURST mode)
• Energy range for this non-imaging detector is 0.3-200 MeV

AKARI(ASTRO-F)

ASTRO-F(renamed AKARI after launch) is Japan's second satellite for infrared astronomy. A telescope with a 69 cm aperture, cooled down to 6 K.

General information

• Launched on 21 February, 2006
• Designed lifespan 550 days
• Sun-Synchronous orbit at 750 km altitude

• The Evolution of Galaxies
• The Life Cycle of Stars
• The Search for Brown Dwarves
• Seek out Planetary Systems Outside Our Own Solar System
• Discover New Comets

FIS - Far-Infrared Surveyor

• FIS is intended to make an all-sky survey at far-infrared wavelengths
• It is also used for pointing observations to detect faint objects or to perform spectroscopy using a Fourier transform spectrometer
• Wavelengths: 50 - 180 microns

IRC - InfraRed Camera

• The NIR camera: near-infrared wavelengths in the 2-5 micron range, field of view 10x10 arcmin
• MIR-S camera: mid-infrared wavelengths in the 6-14 micron range, field of view 9x10 arcmin
• MIR-L camera: mid-infrared wavelengths in the 12-27 micron range, field of view 10x10 arcmin

Updated: 2009-06-08 / ansuutar