Ne ew w T Ty yp pe es s o of f A As st tr ro on no - PowerPoint PPT Presentation

Ne ew w T Ty yp pe es s o of f A As st tr ro on no om mi ic ca al l N X- -r ra ay y T Te el le es sc co op pe es s X R. . H Hu ud de ec c a an nd d M M. . S Sk ku ul li in no ov vá á, , A As st tr ro on no om mi ic ca al l I In ns st ti it tu ut te e, , R Ac ca ad de em my y o of f S Sc ci ie en nc ce es s o of f t th he e C Cz ze ec ch h R Re ep pu ub bl li ic c, , O On nd dr re ej jo ov v, , A Cz ze ec ch h R Re ep pu ub bl li ic c C L. L . P Pí ín na a, , V V. T Ti ich hy y a an nd d L L. . _ _v vé éd da a, , C Cz zec ch h T Tec ch hn ni ic ca al l Un ni iv ve er rs si it ty y, , P Pr ra ag gu ue e, , C Cz ze ec ch h R Re ep pu ub bl li ic c U V. . M Ma ar r_ _í ík ko ov vá á a an nd d A A. . I In nn ne em ma an n, , R RI IT TE E, , P Pr ra ag gu ue e, , C Cz ze ec ch h V Re ep pu ub bl li ic c R 1 Vulcano Workshop 2010

New Trends in Astronomical New Trends in Astronomical X-ray Optics X-ray Optics  Achieving wide FOV: WF (Lobster) Optics  Achieving very fine angular resolution: Active X-ray Optics  Optics for large X-ray Telescopes with good angular resolution at affordable price: K-B Optics  Use of new materials e.g. Silicon wafers 2 Vulcano Workshop 2010

Lobster Eye X-ray Optics X-ray Optics Lobster Eye  Goal: sensitive all-sky X-ray monitoring  Improvement factor vs. RXTE: 100-1000  ! Important for many objects discussed here! 3 Vulcano Workshop 2010

Lobster Eye (LE) (LE) Lobster Eye  Novel Wide Field X-ray Telescopes  FOV of 100 sq. deg. and more easily possible (classical X-ray optics only 1 deg or less)  Analogy with lobster eyes The biomimetics – learning from the nature 4 Vulcano Workshop 2010

The biomimetics – learning from the nature The refractive eyes of a lobster 5 Vulcano Workshop 2010

„Real Real“ “ Lobster Eye Lobster Eye (LE) (LE) „ The eye of a lobster, viewed with a microscope. Right: close up of a small area of the eye. The eye consists of millions of square "channels"; each channel measures approximately 20 µ m (or two hundredths of a millimeter) across. 6 Vulcano Workshop 2010

Gain Gain number of photons detected inside the FWHM circle with the LE G = number of photons detected inside the FWHM circle without the LE Gain as a function of energy - for various designs (for E) The LE Optics can be designed for E = 0-10 keV. The gain can be ~ 1000 for low energies and ~100 for higher energies 7 Vulcano Workshop 2010

Micro LE: 3 x 3 x 14 mm module glass Foils 30 µ m thick separated by 70 µ m Focal image 8 keV The front wiew of the mini - lobster module, Schmidt arrangement, based on 100 micron thick plates spaced by 300 microns, 23 x 23 mm each The X-ray measurement at 8 keV in comparison with mathematical simulation model measured Modular concept to achieve large FOV 8 Vulcano Workshop 2010

LE Sky coverage per revolution LE Sky coverage per revolution • daily limiting flux 10 -12 erg/s/cm 2 • one module 2 x 195 plates 78 x 11.5 x 0.1 mm, 0.3 mm spacing • detector pixel size 150 µ m • total front area 1825 cm 2 • energy range 0.1 - 10 keV • FOV 180 x 6 degrees (30 modules 6 x 6 degrees) • angular resolution 3 - 4 arcmin • total mass < 200 kg 9 Vulcano Workshop 2010

Scientific goals 1. Alert System for X-ray transients fast recognition of new X-ray sources and/or sudden changes in X-ray flux of known sources, prompt emission study, precise positioning, alert system for narrow-field instruments  GRB prompt and afterglow X-ray emission (20-60 triggers/year)  X-ray flashes (> 8 triggers/year)  orphan GRBs (detectable in X-rays but not in gamma)  SNe prompt emission (thermal flash) 10-20 triggers/year  X-ray binary & CVs flux changes  Stellar events in the Sun's vinicity 10 Vulcano Workshop 2010

2. Long-term X-ray source monitoring long-term monitoring of large number of X-ray sources with sampling of hours to days (depending on the source flux). Light curves for all the sources together with rough spectra (continuum monitoring, strong lines, iron detectable). In the list below we assume the limiting flux of 10-12 erg/s/cm2 (but we can go deeper):  X-ray binaries ~ 700 triggers  Cataclysmic Variables ~ 200 triggers  stars ~ 600 triggers  AGN ~ 4 000 triggers  galaxy clusters ~ 400 triggers  SN remnants 11 Vulcano Workshop 2010

Tests in Palermo X-ray facility Tests in Palermo X-ray facility Tested lobster eye was Lobster eye P25 was tested in quasi parallel placed on device allowing beam full imaging mode using the 35 meters long remote controlled rotations X-ray beam line of INAF-OAPA in Palermo figured by red color. MCP (Italy). X-ray images at the focal plane have detector was placed on been taken with a MCP detector with spatial device allowing remote resolution 100µm. controlled translations in all directions. Gain as function of energy Estimated spatial 90 !"#$%&#$'()'*)"+&#$&,)-."',/#$'()&#).(.-01)234.5 80 resolution ~13arcmin. 70 "!!! ()*+,-)./.*0*/+1230). 4)30 &"!! 60 ()*+,-)./.*0*/+1230). &!!! -2510 FWHM 12~13arcmin at 50 Gain 6,7/83/9801 %"!! 40 %!!! :(#.("$#1 all energies (theoretical 5 30 $"!! $!!! 20 #"!! arcmin) 10 #!!! 0 "!! 0 1 2 3 4 5 6 7 8 9 ! '" '& '% '$ '# ! # $ % & " Energy [keV] 67+'"$#$'()8%%9 12 Vulcano Workshop 2010

X-ray images X-ray images 280eV 930eV 1500eV 280eV 930eV 1500eV 2900eV 2900eV 4500eV 4500eV 8000eV 8000eV 13 Vulcano Workshop 2010

Mini Lobster Telescope for Mini Lobster Telescope for picosatellite picosatellite  Goal: scientific payload for a picosatellite 10 x 10 x 30 cm 14 Vulcano Workshop 2010

LE Telescope on German Picosatellite LE Telescope on German Picosatellite Tests with Lobster Eye X-ray Optics & Medipix at 8 keV CTU Prague member of Medipix Collaboration The Medipix detector represents suitable imaging detector for use in space LE telescopes Feasibility study of small LE Based on UWE concept, Univ of Wurzburg, DE F=25 cm,L=30 cm X-ray telescope for Picosatellite Picosatellite 10 x 10 x 30 cm Technological experiment but still some science 15 Vulcano Workshop 2010

Active X-ray Optics Active X-ray Optics  Goal: ultra-precise angular resolution < 1 arcsec  Computer controlled substrates for ultraprecise X-ray optics (sub-arcsec)  Goal: super-precise optics (sub arcsec angular resolution) for NASA Project Generation X 16 Vulcano Workshop 2010

Arrangement of piezoelectric actuators on a Wolter I – principle of active X-ray optics. Technical challenge: the total number of piezoelectric elements must be of order of 100 000 – 1 000 000, due to large area of the mirror array Alternatives: (1) Piezoelectric actuators (2) Electrostatic shaping 17 Vulcano Workshop 2010

Future of X-ray Astronomy: IXO Future of X-ray Astronomy: IXO  Future space X-ray telescope such as IXO (International X-ray Observatory) require novel technologies: • Light-weight (large apertures, multiply nested) • Precise (angular resolutions better than 5 arcsec) • Low-cost, mass-production (need for huge geometrical area)  Old technologies cannot be used as they are either too heavy (thick glass ceramics, e.g. Chandra) or not enough accurate, or both (electroformed Ni, e.g. XMM Newton). • Key requirements: Effective area ~3 m 2 @ 1.25 keV Angular Resolution <= 5 arcsec • Single segmented optic with design optimized to minimize mass and maximize collecting area Vulcano Workshop 2010 18

Kirkpatrick-Baez Optics Kirkpatrick-Baez Optics  Goal: decrease expenses in future X-ray optics  High angular resolution ~5 arcses at affordable price Vulcano Workshop 2010 19

Kirkpatrick-Baez Optics Kirkpatrick-Baez Optics • Double reflection X-ray Optics consists of two mirror sets – one is aligned vertically and the second is aligned horizontally. • The quality of the focal spot image depend on quality of substrates (shape, microroughness). • Both mirrors are curved parabolically – the first mirror focuses in vertical plane and the second mirror focuses in horizontal plane. Single focal point is formed in the crossection of the two focal planes. Nested systems possible. • Technology is not necessarily based on precise and expensive mandrels hence • Cost-effective manufacture 20 Vulcano Workshop 2010

Focal length Wolter system KB system If W and KB have the same aperture, focal length of KB system is twice as large as Wolter system . 21 Vulcano Workshop 2010