1 / 27

INTEGRAL All-Sky Survey: Deep inside Galaxy and beyond

INTEGRAL All-Sky Survey: Deep inside Galaxy and beyond. R.Krivonos, M.Revnivtsev, S.Tsygankov, A. Lutovinov, E.Churazov, R.Sunyaev MPA, Garching, Germany IKI, Moscow, Russia Excellence Cluster Universe, Garching, Germany. INTEGRAL/IBIS

tala
Download Presentation

INTEGRAL All-Sky Survey: Deep inside Galaxy and beyond

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. INTEGRAL All-Sky Survey: Deep inside Galaxy and beyond R.Krivonos, M.Revnivtsev, S.Tsygankov, A. Lutovinov, E.Churazov, R.Sunyaev MPA, Garching, Germany IKI, Moscow, Russia Excellence Cluster Universe, Garching, Germany

  2. INTEGRAL/IBIS All-sky survey (Krivonos et. al., 2007, current state) ~600 detections: ~45% Galactic ~40% ExtraGal. ~15% Unident. SWIFT/BAT 36Month All-sky survey (Cusumano et. Al., 2009) ~1000 detections: ~20% Galactic ~55% ExtraGal. ~25% Unident.

  3. INTEGRAL/IBIS exposure map SWIFT/BAT sensitivity map: (Cusumano et. al., 2009)

  4. Source-free Sensitivity is strongly limited by systematic noise Galactic Center region 20 Msec 17-60 keV INTEGRAL/IBIS

  5. Having a large exposure accumulated in Galactic Plane, the survey sensitivity is significantly limited by systematic noise.The main constrains: Source projection model Source interplay in Galactic Center Galactic Background

  6. 1) Source projection model Source removal is not perfect, the residuals on detector can be 0.3-0.5% of the source flux

  7. Crab

  8. Sco X-1 7σ excess

  9. 1) Source projection model Residuals: Crab field: ~10 mCrab Sco X-1 field: ~5-7 mCrab GC region: ~1-0.5 mCrab Status: fixed at some sufficient level (mask pattern, screws, NOMEX support structure, etc.) Future:can be improved (pixel-to-pixel gain variations, dead time)

  10. 2) Source self-influence in GC …due to detector shared area between sources, and periodic mask Status: fixed at some sufficient level (correct solution cannot be found) Future:can not be significantly improved source subtraction order significantly change sky background: 4 Ms

  11. 2) Source self-influence in GC The insuperable difficulties in GC survey are detector shared area between sources, and periodic mask pattern (e.g. Swift/BAT has no such constrain)

  12. 3) Galactic X-Ray Background 150-200 mCrab / FOV / 17-60 keV

  13. 3) Galactic X-Ray Background

  14. Galactic Ridge intoduces at least 15-20% of systematic noise 300 ksec deep field of NGC4151 in staring mode +”Ridge like illumination” Status: fixed at some sufficient level (more efficient on special observing pattern) Future:can not be significantly improved

  15. Summary (not final) Source projection model: fixed/can be improved Source interplay in GC: fixed/cannot be improved Galactic Background: fixed/cannot be improved Generally we can’t significantly further improve IBIS/ISGRI imaging system, but we can remove systematic residuals from the reconstructed sky

  16. Non-parametric sky background approximation (wavelets) 300 ksec deep field of NGC4151 in staring mode Coded-mask can reconstruct on sky only point source, the other stuff is sky background (flat) and systematic residuals. The idea: use spatial freq. information to remove systematic noise

  17. Swift/XRT 2 days ago 300 ksec deep field of NGC4151 in staring mode SKY=Deconvolve(DET-SRCs) + SRCs SKY=WV(Deconvolve(DET-SRCs)) + SRCs Systematic noise (~30%) is removed Sensitivity is limited by pure statistics only! Immediate result: New source IGR J11203+4531 was detected (rev. 0074-0076)

  18. 5Ms deep field of 3C273

  19. 5Ms deep field of 3C273 S/N distribution is consistent with Gaussian σ=1 2 pix at -4.7σ (1.5 expected for total 557096 pix)

  20. Galactic Center region 20 Msec 17-60 keV

  21. Galactic Center region 20 Msec 17-60 keV

  22. Survey: statitsics (in process) (http://hea.iki.rssi.ru/integral/catalog) • 214 (144) AGN (statistically clear sample: N=115) • 80 (77) HMXB • 92 (89) LMXB • 39 (26) CV • 3 Clusters • and others… Total: 562 at >5σ Galactic: 239 Extragalactic: 217 Unidentified: 107 new hard X-Ray sources: IGR J18151-1052 0.54+/-0.10 mCrab HMXB IGR J17009+3559 0.96+/-0.20 mCrabAGN? IGR J11203+4531 3.68+/-0.58 mCrab … … Atels 2170,2193

  23. Revnivtsev et al. 2008 Survey: galactic LF New ultra-deep Galactic survey probes the low end of the LF: Llim=4e34 erg/s @8.5 kpc

  24. Survey: LogN-LogS Extragalactic: 115 AGNs used Slope: -1.5+/-0.1

  25. Volume density excess of nearby (<70 Mpc)‏ 40 AGNs: (INTEGRAL survey)‏ ~5,000 IR galaxies: (IRAS PSCz survey)‏ Convolved with INTEGRAL FOV

  26. b= bAGN = 1.0 bAGN = 0.80 ± 0.13 X-Ray AGN bias factor We use IRAS PSCz survey as matter tracer ( bIR≈1 ) Krivonos et al. in prep. => AGNs – good matter tracers on 10-70 Mpc scale => SMBH activity independent from density of galaxies

  27. Summary • INTEGRAL ultra-deep Galactic survey and excellent SWIFT/BAT extragalactic survey are great couple to complement each other in studying the hard X-ray sky • GC limited by ~20% systematics. We reduced systematic noise by ~30% and now sensitivity grows with exposure closely to the ideal case Flim~T-1/2 • Sensitivity of the INTEGRAL extragalactic survey is limited by pure statistics only. Ultra-deep extragalactic survey is possible. • 5σ Limiting flux in GC (20 Ms) is 0.3 mCrab(4.7e-12 erg/s/cm2) • INTEGRAL ultra-deep Galactic survey probes the low end of the LF: Llim=4e34 erg/s @8.5 kpc

More Related