X-ray telescope: Difference between revisions
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==Optical design== |
==Optical design== |
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X-ray telescopes can use a variety of different designs to image X-rays. The most common methods used in X-ray telescopes are [[Wolter telescope|grazing incidence mirrors]] and [[coded aperture]]s. The limitations of [[X-ray optics]] result in much narrower fields of view than visible or UV telescopes. |
X-ray telescopes can use a variety of different designs to image X-rays. The most common methods used in X-ray telescopes are [[Wolter telescope|grazing incidence mirrors]] and [[coded aperture]]s. The limitations of [[X-ray optics]] result in much narrower fields of view than visible or UV telescopes. |
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* a reasonable detection efficiency. |
* a reasonable detection efficiency. |
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The mirrors can be made of ceramic or metal foil<ref name=xraysMirror>{{ cite web |title=Mirror Laboratory |url=http://astrophysics.gsfc.nasa.gov/xrays/MirrorLab/xoptics.html }}</ref>. The most commonly used grazing angle incidence materials for X-ray mirrors are [[gold]] and [[iridium]]. The critical reflection angle is energy dependent. For gold at 1 keV, the critical reflection angle is 3.72 degrees. |
The mirrors can be made of ceramic or metal foil<ref name=xraysMirror>{{ cite web |title=Mirror Laboratory |url=http://astrophysics.gsfc.nasa.gov/xrays/MirrorLab/xoptics.html }}</ref>. The most commonly used grazing angle incidence materials for X-ray mirrors are [[gold]] and [[iridium]]. The critical reflection angle is energy dependent. For gold at 1 keV, the critical reflection angle is 3.72 degrees. |
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A limit for for this technology in the early 2000s with Chandra and XMM-Newton was about 15 keV light.<ref name=nustar1>[http://www.nustar.caltech.edu/about-nustar/instrumentation/optics NuStar: Instrumentation: Optics]</ref> Using new multi-layered coatings, computer aided manufacturing, and other techniques the x-ray mirror for the [[Nuclear Spectroscopic Telescope Array|NuStar]] telescope pushed this up to 79 keV light.<ref name=nustar1/> To reflect at this level, glass layers were multi-coated with Tungsten/Silicon or Platinum/SiliconCarbite.<ref name=nustar1/> |
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===Coded apertures=== |
===Coded apertures=== |
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Revision as of 22:32, 24 November 2010
An X-ray telescope (XRT) is a telescope that is designed to observe remote objects in the X-ray spectrum. In order to get above the Earth's atmosphere, which is opaque to X-rays, X-ray telescopes must be mounted on high altitude rockets or artificial satellites.
Optical design
X-ray telescopes can use a variety of different designs to image X-rays. The most common methods used in X-ray telescopes are grazing incidence mirrors and coded apertures. The limitations of X-ray optics result in much narrower fields of view than visible or UV telescopes.
Mirrors
The utilization of X-ray mirrors for extrasolar X-ray astronomy simultaneously requires:
- the ability to determine the location at the arrival of an X-ray photon in two dimensions and
- a reasonable detection efficiency.
The mirrors can be made of ceramic or metal foil[1]. The most commonly used grazing angle incidence materials for X-ray mirrors are gold and iridium. The critical reflection angle is energy dependent. For gold at 1 keV, the critical reflection angle is 3.72 degrees.
A limit for for this technology in the early 2000s with Chandra and XMM-Newton was about 15 keV light.[2] Using new multi-layered coatings, computer aided manufacturing, and other techniques the x-ray mirror for the NuStar telescope pushed this up to 79 keV light.[2] To reflect at this level, glass layers were multi-coated with Tungsten/Silicon or Platinum/SiliconCarbite.[2]
Coded apertures
Some X-ray telescopes use coded aperture imaging. This technique uses a flat aperture grille in front of the detector, which weighs much less than any kind of focusing X-ray lens, but requires considerably more post-processing to produce an image.
Telescopes
Exosat
The two low-energy imaging telescopes onboard Exosat used Wolter I X-ray optics and were equipped with two focal plane detectors:
- a position-sensitive proportional counter (PSD) and
- a channel multiplier array (CMA).[3]
Hard X-ray telescope
On board OSO 7 was a hard X-ray telescope. Its effective energy range: 7 - 550 keV, field of view (FOV) 6.5°, effective area ~64 cm2.
Filin telescope
The Filin telescope carried aboard Salyut 4, consisted of four gas flow proportional counters, three of which had a total detection surface of 450 cm2 in the energy range 2-10 keV, and one of which has an effective surface of 37 cm2 for the range 0.2-2 keV. The FOV was limited by a slit collimator to 3° x 10° FWHM. The instrumentation included optical sensors mounted on the outside of the station together with the X-ray detectors. The power supply and measurement units were inside the station. Ground based calibration of the detectors occurred along with in-flight operation in three modes: inertial orientation, orbital orientation, and survey. Data were collected in 4 energy channels: 2-3.1 keV, 3.1-5.9 keV, 5.9-9.6 keV, and 2-9.6 keV in the larger detectors. The smaller detector had discriminator levels set at 0.2 keV, 0.55 keV, and 0.95 keV.
SIGMA telescope
The hard X-ray and low-energy gamma-ray SIGMA telescope covered the energy range 35-1300 keV,[4] with an effective area of 800 cm2 and a maximum sensitivity field of view of ~5° × 5°. The maximum angular resolution was 15 arcmin.[5] The energy resolution was 8% at 511 keV.[6] Its imaging capabilities were derived from the association of a coded mask and a position sensitive detector based on the Anger camera principle.[7]
ART-P X-ray telescope
The ART-P X-ray telescope covered the energy range 4 to 60 keV for imaging and 4 to 100 keV for spectroscopy and timing. There were four identical modules of the ART-P telescope, each consisting of a position sensitive multi-wire proportional counter (MWPC) together with a URA coded mask. Each module had an effective area of approximately 600 cm², producing a FOV of 1.8° x 1.8°. The angular resolution was 5 arcmin; temporal and energy resolutions were 3.9 ms and 22% at 6 keV, respectively.[8] The instrument achieved a sensitivity of 0.001 of the Crab nebula source (= 1 "mCrab") in an eight-hour exposure. The maximum time resolution was 4 ms.[7][6]
Focusing X-ray telescope
The Broad Band X-ray Telescope (BBXRT) was flown on the Space Shuttle Columbia (STS-35) as part of the ASTRO-1 payload. BBXRT was the first focusing X-ray telescope operating over a broad energy range 0.3-12 keV with a moderate energy resolution (90 eV at 1 keV and 150 eV at 6 keV). The two Co-Aligned Telescopes with a segmented Si(Li) solid state spectrometer each (detector A and B) composite of five pixels. Total FOV 17.4´ diameter, Central pixel FOV 4´ diameter. Total area 765 cm2 at 1.5 keV, and 300 cm2 at 7 keV.
XRT on the Swift MIDEX mission
The XRT on the Swift MIDEX mission (0.2-10 keV energy range) uses a Wolter I telescope to focus X-rays onto a thermoelectrically cooled CCD.[9] It was designed to measure the fluxes, spectra, and lightcurves of Gamma-ray bursters (GRBs) and afterglows over a wide dynamic range covering more than 7 orders of magnitude in flux. The XRT can pinpoint GRBs to 5-arcsec accuracy within 10 seconds of target acquisition for a typical GRB and can study the X-ray counterparts of GRBs beginning 20-70 seconds from burst discovery and continuing for days to weeks.
The overall telescope length is 4.67 m with a focal length of 3.500 m and a diameter of 0.51 m.[9] The primary structural element is an aluminum optical bench interface flange at the front of the telescope that supports the forward and aft telescope tubes, the mirror module, the electron deflector, and the internal alignment monitor optics and camera, plus mounting points to the Swift observatory.[9]
The 508 mm diameter telescope tube is made of graphite fiber/cyanate ester in two sections. The outer graphite fiber layup is designed to minimize the longitudinal coefficient of thermal expansion, whereas the inner composite tube is lined internally with an aluminum foil vapor barrier to guard against outgassing of water vapor or epoxy contaminants into the telescope interior.[9] The telescope has a forward tube which encloses the mirrors and supports the door assmebly and star trackers, and an aft tube which supports the focal plane camera and internal optical baffles.[9]
The mirror module consists of 12 nested Wolter I grazing incidence mirrors held in place by front and rear spiders. The passively heated mirrors are gold-coated, electroformed nickel shells 600 mm long with diameters ranging from 191 to 300 mm.[9]
The X-ray imager has an effective area of >120 cm2 at 1.15 keV, a field of view of 23.6 x 23.6 arcmin, and angular resolution (θ) of 18 arcsec at half-power diameter (HPD). The detection sensitivity is 2 x 10-14 erg cm-2s-1 in 104 s. The mirror point spread function (PSF) has a 15 arcsec HPD at the best on-axis focus (at 1.5 keV). The mirror is slightly defocused in the XRT to provide a more uniform PSF for the entire field of view hence the instrument PSF θ = 18 arcsec.[9]
Normal incidence X-ray telescope
Like MSSTA, NIXT used normal incidence reflective multilayer optics.[10]
History of X-ray telescopes
The first X-ray telescope was used to observe the Sun. The first X-ray picture of the Sun was taken in 1963, by a rocket-borne telescope.
References
- ^ "Mirror Laboratory".
- ^ a b c NuStar: Instrumentation: Optics
- ^ Hoff HA (1983). "Exosat - the new extrasolar x-ray observatory". J Brit Interplan Soc (Space Chronicle). 36 (8): 363–7.
{{cite journal}}: Unknown parameter|month=ignored (help) - ^ "Overview of two-year observations with SIGMA on board GRANAT" (PDF). Astron Astrophys Supplement Series (97). 1993.
{{cite journal}}: Text "author-Mandrou P, Jourdain E. et al." ignored (help) - ^ Revnivtsev MG, Sunyaev RA, Gilfanov MR, Churazov EM, Goldwurm A, Paul J, Mandrou P, Roques JP (2004). "A hard X-ray sky survey with the SIGMA telescope of the GRANAT observatory". Astron Lett. 30: 527–33.
{{cite journal}}: CS1 maint: multiple names: authors list (link) - ^ a b "International Astrophysical Observatory "GRANAT"". IKI RAN. Retrieved 2007-12-05.
- ^ a b "GRANAT". NASA HEASARC. Retrieved 2007-12-05.
- ^ Molkov, S.V., Grebenev, S.A., Pavlinsky, M.N., Sunyaev. "GRANAT/ART-P OBSERVATIONS OF GX3+1: TYPE I X-RAY BURST AND PERSISTENT EMISSION", Mar 1999. 4pp. arXiv e-Print (astro-ph/9903089v1).
- ^ a b c d e f g Burrows DN, Hill JE, Nousek JA, Kennea JA, Wells A, Osborne JP, Abbey AF, Beardmore A, Mukerjee K, Short ADT, Chincarini G, Campana S, Citterio O, Moretti A, Pagani C, Tagliaferri G, Giommi P, Capalbi M, Tamburelli F, Angelini L, Cusumano G, Bräuninger HW, Burkert W, Hartner GD (2005). "The Swift X-ray Telescope". Space Sci Rev. 120 (3–4): 165–95. doi:10.1007/s11214-005-5097-2.
{{cite journal}}: Unknown parameter|month=ignored (help)CS1 maint: multiple names: authors list (link) - ^ Hoover RB; et al. (1991). "Solar Observations with the Multi-Spectral Solar Telescope Array". Proc. SPIE. 1546: 175.
{{cite journal}}: Explicit use of et al. in:|author=(help)
External links
- Hard X-ray microbeam experiments with a sputtered-sliced Fresnel zone plate and its applications
- Scientific applications of soft x-ray microscopy
See also
- List of telescope types
- Solar X-ray astronomy
- Sounding rocket X-ray astronomy
- Synchrotron X-ray tomographic microscopy
- X-ray astronomy
- Wolter telescope: A type of X-ray telescope built with glancing incidence mirrors.