Various Coded Mask Telescope Missions

In Table 5.1, an overview is given about the main aperture modulation instruments and missions. The table is not nearly complete, giving only examples for those instruments that have either produced important scientific results or constituted a step

Table 5.1 Important aperture modulation telescopes

Year

Carrier

Instr.

No.of instr. &

Mode of

Energy

aperture

operation

[keV]

1970

Uhuru

2 Colla

Scanb

2-20

1971

OSO-7

4 Coll

Scan

1-1 000

1974

Ariel V

5 Coll, 1 RMCc

Spin,scan

0.3-40

1975

SAS-3

6 Coll, 2 RMC

Spin, pointd

0.1-60

1976

Rocket

SL1501

CM

Point

2-10

1977

HEAO-1

A1-A4

4 Coll(1 grid)e

Scan

0.2-10000

1983

Tenma

HXT

1 Coll, 1 CMf

Spinh

2-10

1985

Balloon

GRIP

CM

Point

30-600

1985

SL2

XRT

CM

Point

2-25

1987

Mir

TTM

CM

Point

1.8-30

1989

Granat

SIGMA

CM

Point

30-1300

ART-P

CM

4-60

ART-S

CM

3-100

WATCH

RMC

6-120

1991

CGRO

BATSE

Coll

Point, EaOcg

20-10000

1995

RXTE

ASM

CM

Scan

2-10

1996

BeppoSAX

WFC

CM

Point

2-30

2000

HETE-2

SXT

2 CM

Point

0.5-14

WXM

2 CM

Point

2-25

2002

INTEGRAL

JEM-X

CM

Point

3-35

IBIS

CM

15-10 000

SPI

CM

20-8 000

2004

Swift

BAT

CM

Point

15-150

For nonscanning missions simple collimated instruments are not mentioned

No individual references are given here. General information about X-ray astronomy satellites can be found in http://heasarc.gsfc.nasa.gov/docs, followed by the name of the satellite (e.g.,

"/heaol/heaol.html"). A useful web page for coded aperture is:

http://lheawww.gsfc.nasa.gov/docs/cai/coded.html

aSlat or tube collimators b Scanning cRotation modulation collimator (RMC)

dPointing eGrid collimators fCoded mask (CM)

gEarth occultations hSpinning satellite forward in technology. The reader is referred to the web addresses given in the footnote of Table 5.1.

The two most advanced satellites carrying Coded Mask instruments are INTEGRAL and Swift. While INTEGRAL, operating since November 2002, is devoted to pointed observations with combined high spatial, spectral and temporal resolution, the main scientific objective of Swift is to detect and accurately localize gamma-ray bursts and to perform fast response follow-up pointed observations at X-ray and UV/optical wavelengths.

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