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ROSITA

ROSITA. ROSITA  ABRIXAS on ISS. RO entgen S urvey with an I maging T elescope A rray. Experimentvorstellung MPE 4.5.2001. Basic Scientific Idea. To extend the ROSAT survey up to 15 keV. X-ray Surveys. Survey. Pointing. ROSAT. ROSAT. 0.1-2 keV. ROSITA. XMM/Chandra. 0.5-15 keV.

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ROSITA

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  1. ROSITA ROSITA  ABRIXAS on ISS ROentgen Survey with an Imaging Telescope Array Experimentvorstellung MPE 4.5.2001

  2. Basic Scientific Idea To extend the ROSAT survey up to 15 keV

  3. X-ray Surveys Survey Pointing ROSAT ROSAT 0.1-2 keV ROSITA XMM/Chandra 0.5-15 keV

  4. ROSITA Survey 100 x 10000 x • All-Sky Survey • 3 Years Mission Time • S0.5-2=5.7 x 10-14 • S2-10 =1.7 x 10-13 • 42000 deg2 • NAGN=240,000 (0.5-2) / 50,000(2-10) • NCL =10,000 ROSITA Survey has two orders of magnitude higher sensitivity and angular resolution than previous survey in the same band.

  5. Scientific Goals NGC 6240 QSO average (Elvis et al.) ROSAT ROSITA ROSITA CMB CIB COB NGC 6240 ROSAT CXB • Absorbed AGN and the X-ray background

  6. HEAO-1 GRO MEGA IRAS 2MASS z=0.2 ROSAT FIRST ROSITA z=1 SDSS Chandra/XMM Deep Field z=5 FIRST (VLA) Elvis QSO template PLANCK NGC 6240

  7. Scientific Goals Star formation vs Black Hole activity „NGC6240“ Steidel et al., 1999 Hasinger et al., 1999 0.5-2 keV (ROSAT) • Absorbed AGN and the X-ray background • Cosmological Evolutionof AGN QSOs Seyfert Galaxies Starburst Galaxies What is the history of obscuration in the Universe? ROSITA needed as a local anchor to study evolution

  8. Scientific Goals ROSAT 0.1-2.4 keV ROSITA Clusters(expected) 20 cts ROSAT Clusters (already identified) 40 cts • Absorbed AGN and the X-ray background • Cosmological Evolutionof AGN • Clusters of Galaxies Clusters have harder X-ray spectra than AGN and ROSITA has sharper point-spread function than ROSAT => Clusters more easily identifiable.

  9. Evolution of Structure Klypin, Kravtsov, Gottlöber

  10. Large-Scale Structure T<105K 105<T<107K T>107K Cen & Ostriker 1999, ApJ 514, 1

  11. ROSAT Cluster Surveys Böhringer et al., 2000a-c; Collins et al., 2000; Sckuecker et al., 2000

  12. 3D-structure of clusters • Blue: Clusters in the • plane perpendicular • to the gal. Plane • (lII = 90 –270o) • Green: Clusters in • the foreground of • this plane • Need to break through the zone of avoidance!

  13. XMM: Cluster on Galactic Plane Nevalainen et al., 2001

  14. Large Nearby Clusters • Unlimited field-of-view • much lower particle • background than XMM • => ROSITA can determine temperature and metallicity out to much larger radii

  15. Scientific Goals • Absorbed AGN and the X-ray background • Cosmological Evolutionof AGN • Clusters of Galaxies • Galactic X-ray emission

  16. Creation of the elements Detailed Chemistry and plasma diagnostics possible with CCD resolution

  17. Tycho SNR

  18. Embedded Protostars Chandra Orion HST (visual) VLT (JHK) Look for Taurus/Auriga, Lupus ...

  19. Scientific Goals • Absorbed AGN and the X-ray background • Cosmological Evolutionof AGN • Clusters of Galaxies • Galactic X-ray emission • Monitoring of variable X-ray sources • Gamma Ray Bursts • etc.

  20. ABRIXAS Idea ABRIXAS 7 x 90 cm2 27 Shells f = 160 cm XMM 2000 cm2 58 Shells f = 750 cm MPE’s pn-CCD 6 x 6 cm2

  21. ABRIXAS Instrumentation

  22. ABRIXAS Field of Views 7  60 arcmin 7.5° separation

  23. Effective Area Gold /Nickel (ROSITA) Gold (ABRIXAS)

  24. MPE‘s Detector Development pn-CCD (XMM) XEUS10y 2001 advanced pn-CCD DEPFET pixel device

  25. New Detector Concept

  26. New Detector Concepts

  27. New Detector Concepts CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX FramestoreArea FramestoreArea FramestoreArea FramestoreArea FramestoreArea FramestoreArea FramestoreArea

  28. New Detector Concepts CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX FramestoreArea FramestoreArea FramestoreArea FramestoreArea FramestoreArea FramestoreArea FramestoreArea

  29. New Detector Concepts CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX FramestoreArea FramestoreArea FramestoreArea FramestoreArea FramestoreArea FramestoreArea FramestoreArea

  30. New Detector Concepts CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX CMX FramestoreArea FramestoreArea FramestoreArea FramestoreArea FramestoreArea FramestoreArea FramestoreArea

  31. ROSITA Field of Views 7  60 arcmin 4° separation

  32. Aluminum filter Deteiled thermal and mechanical design still under engineering study

  33. ROSITA on ISS ISS flies like an airplane ideally suited for a survey

  34. ROSITA viewing cone Flight direction

  35. Distanzplots für ESA-Modell Schwenk 60 Zenitdistanzdes TeleskopsZenitdistanz der Sonne Sonnendistanz des Teleskops 3 Jahre

  36. ESA Scan 3 Jahre

  37. ESA Scan 3 Jahre

  38. ISS tradeoff • Pro: • no attitude control • simple power supply • no antenna, transmitter • simple safe mode • commercial electronics • easy uplink, accommodation • Con: • viewing constraints • contamination? • limited telemetry? • mission life time • more complicated cooling • man-rating

  39. Currently... pre-phase A study with industry (KT) (mission analysis, accommodation, contamination etc.)

  40. Currently... pre-phase A study with industry (KT) (mission analysis, accommodation, contamination etc.) accommodation on ISS (location, uplink, collaborations)

  41. Currently... pre-phase A study with industry (KT)(mission analysis, accommodation, contamination etc.) accommodation on ISS (location, uplink, collaborations) new instrument concepts (smaller pixels, faster readout)

  42. Timing • ESA Columbus module > 2005 • ROSITA detector development > 2005 • Launch + Mission  2007-2009

  43. Summary (1) Field of View 7  60 arcmin total 5.5 deg2 Angular Resolution ~ 30 arcsec Mision Duration 3 years Average Exposure ~ 9.000 sec Sensitivity ~ 610-14 erg cm-2 s-1 Number of Sources 240.000 (0.5 – 2 keV) 360.000 (0.5 – 7 keV) 50.000 (2 – 7 keV) 100 times more sensitive than HEAO-1 (Piccinnotti)

  44. Summary (2) • compared to HEAO-1: • imaging, angular resolution x100 • sensitivity x100 • compared to ROSAT: • higher energy range • better angular resolution • better energy resolution • compared to ABRIXAS: • larger mirror area (Nickel coating) • better low-energy sensitivity (Al filter) • no FOV overlap (no ghost images) • detector technology demonstration for XEUS • scientific use for the Space Station

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