&lt;title&gt;Characteristics of the flight model optics for the JET-X telescope onboard the Spectrum-X-Gamma satellite&lt;/title&gt;

Citterio, O.; Campana, S.; Conconi, P.; Ghigo, M.; Mazzoleni, Francesco; Poretti, E.; Conti, G.; Cusumano, G.; Sacco, B.; Braeuninger, Heinrich W.; Burkert, Wolfgang; Egger, R.; Castelli, C.; Willingale, R.

doi:10.1117/12.245112

Cited by 43 publications

(25 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…14) immediately shows the image quality of these mirrors and their capability to separate two nearby sources. The total effective area of a single unit is ∼159 cm 2 at 1.5 keV and ∼70 cm 2 at 8 keV, while the Half Energy Width (HEW) is ∼15 arcsec at 1.5 keV and ∼19 arcsec at 8 keV [56]. For the most recent results on the inflight calibrations of the mirror unit now flying onboard Swift see Moretti et al [57] and Romano et al [58].…”

Section: Opticsmentioning

confidence: 97%

POLARIX: a pathfinder mission of X-ray polarimetry

Costa¹,

Bellazzini

Tagliaferri

et al. 2010

Exp Astron

Self Cite

View full text Add to dashboard Cite

Since the birth of X-ray astronomy, spectral, spatial and timing observation improved dramatically, procuring a wealth of information on the majority of the classes of the celestial sources. Polarimetry, instead, remained basically unprobed. X-ray polarimetry promises to provide additional information procuring two new observable quantities, the degree and the angle of polarization. Polarization from celestial X-ray sources may derive from emission mechanisms themselves such as cyclotron, synchrotron and non-thermal bremsstrahlung, from scattering in aspheric accreting plasmas, such as disks, blobs and columns and from the presence of extreme magnetic field by means of vacuum polarization and birefringence. Matter in strong gravity fields and Quantum Gravity effects can be studied by X-ray polarimetry, too. POLARIX is a mission dedicated to X-ray polarimetry. It exploits the polarimetric response of a Gas Pixel Detector, combined with position sensitivity, that, at the focus of a telescope, results in a huge increase of sensitivity. The heart of the detector is an Application-Specific Integrated Circuit (ASIC) chip with 105,600 pixels each one containing a full complete electronic chain to image the track produced by the photoelectron. Three Gas Pixel Detectors are coupled with three X-ray optics which are the heritage of JET-X mission. A filter wheel hosting calibration sources unpolarized and polarized is dedicated to each detector for periodic on-ground and in-flight calibration. POLARIX will measure time resolved X-ray polarization with an angular resolution of about 20 arcsec in a field of view of 15 × 15 arcmin and with an energy resolution of 20% at 6 keV. The Minimum Detectable Polarization is 12% for a source having a flux of 1 mCrab and 105 s of observing time. The satellite will be placed in an equatorial orbit of 505 km of altitude by a Vega launcher. The telemetry down-link station will be Malindi. The pointing of POLARIX satellite will be gyroless and it will perform a double pointing during the earth occultation of one source, so maximizing the scientific return. POLARIX data are for 75% open to the community while 25% + SVP (Science Verification Phase, 1 month of operation) is dedicated to a core program activity open to the contribution of associated scientists. The planned duration of the mission is one year plus three months of commissioning and SVP, suitable to perform most of the basic science within the reach of this instrument. A nice to have idea is to use the same existing mandrels to build two additional telescopes of iridium with carbon coating plus two more detectors. The effective area in this case would be almost doubled

show abstract

Section: Opticsmentioning

confidence: 97%

POLARIX: a pathfinder mission of X-ray polarimetry

Costa¹,

Bellazzini

Tagliaferri

et al. 2010

Exp Astron

Self Cite

View full text Add to dashboard Cite

show abstract

“…1 Schematic of the Wolter telescope type I (left) and type II (right) [2] is of utmost importance, nested systems have been used (the EINSTEIN observatory [3] and [4], EXOSAT [5], ROSAT [6], ASCA [7] & [8] and Suzaku [9], the Chandra [10] and [11] and XMM-Newton [12] observatories, as well as the JET-X telescopes of the SWIFT mission [13] and [14]). For instance, each of the three X-ray telescopes on board of XMM-Newton [12] accommodates 58 nested paraboloid-hyperboloid Wolter type I mirror shell pairs.…”

Section: Wolter Telescopesmentioning

confidence: 99%

Realization of X-ray telescopes–from design to performance

Aschenbach

2009

Exp Astron

View full text Add to dashboard Cite

show abstract

“…The Ni electroforming replication method has been successfully used by Beppo-SAX, 1 JET-X, 2 SWIFT, 3 and XMM-Newton, 4 to produce the gold-coated xray mirrors. The main advantage of this approach is high imaging resolution, combined with the high throughput of the telescope design which is formed by many confocal thin mirror shells.…”

Section: Introductionmentioning

confidence: 99%

Investigation of direct replication techniques on periodic multilayers

et al. 2011

View full text Add to dashboard Cite

The direct replication of a periodic W/Si multilayer was investigated systematically. The W/Si multilayer was deposited by a high vacuum dc magnetron sputtering system. After deposition, the multilayer was transferred from the supersmooth mandrel onto a commercially available float glass substrate by the epoxy replication technique. The multilayer was characterized by the grazing incident x-ray reflectance (GIXR) measurement, atomic force microscope (AFM), and Zygo GPI interferometer before and after replication. The measured results showed that the multilayer structure and reflectivity were almost the same, and the surface roughness was 0.22 and 0.23 nm before and after replication, respectively. It was demonstrated that the W/Si multilayer was successfully replicated without modification of the structure, a significant increase of surface roughness, or apparent change of reflectivity. The optical figure of the substrate after replication experienced significant changes of many waves but was actually improved for this specific test. Future studies will focus on learning how to control the resulting optical figure of our replication process on a thin substrate. C 2011 Society of Photo-Optical Instrumentation Engineers (SPIE).

show abstract

<title>Characteristics of the flight model optics for the JET-X telescope onboard the Spectrum-X-Gamma satellite</title>

Cited by 43 publications

References 0 publications

POLARIX: a pathfinder mission of X-ray polarimetry

POLARIX: a pathfinder mission of X-ray polarimetry

Realization of X-ray telescopes–from design to performance

Investigation of direct replication techniques on periodic multilayers

Contact Info

Product

Resources

About