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Observations of Black Holes with MIRAX

Observations of Black Holes with MIRAX. João Braga - INPE. First Brazilian-led astronomical satellite project High-energy astrophysics observational window for the Brazilian community International collaboration  expertise in space missions and cost sharing

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Observations of Black Holes with MIRAX

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  1. Observations of Black Holes with MIRAX João Braga - INPE

  2. First Brazilian-led astronomical satellite project High-energy astrophysics observational window for the Brazilian community International collaboration  expertise in space missions and cost sharing Strong participation of Brazilian institutions and industry 100% public data  NASA HEASARC archive MIRAX mission

  3. João Braga, Flavio D’Amico, Chico Jablonski InstitutoNacional de PesquisasEspaciais - INPE, Brazil Rick Rothschild, John Tomsick Center for Astrophysics and Space Science - CASS/UCSD, USA RüdigerStaubert, EckhardKendziorra, Andrea Santangelo InstitutfürAstronomie und Astrophysik – IAA Tübingen, Germany JörnWilms University of Erlangen-Nurenberg, Germany Ron Remillard Kavli Institute for Astrophysics and Space Research - MIT, USA Erik Kuulkers Integral Science Operations Center, ESAC/ESA, Spain Collaborators: Eduardo Janot Pacheco IAG/USP, Brazil J. Renan de Medeiros UFRN, Brazil ThaisaStorchi-Bergmann UFRGS, Brazil MIRAX science team

  4. MIRAX baselineparameters

  5. Continuous broadband imaging spectroscopy of a large source sample (~9 months/yr)  Complete history of transient sources X-ray bursts – superburst recurrence times and emergence of normal bursts after superbursts Spectral state transitions and evolution on accreting compact objects Accretion torques on neutron stars  accreting pulsars, pulsed period evolution, ms-pulsar recurrent outbursts Relativistic jets on microquasars and other systems  X-ray light curves during radio ejections Flaring X-ray sources and fast transients (many INTEGRAL sources) Gamma-ray bursts (~1/month), especially XRFs  X-ray AGs seen immediately AGN variability (obscured AGNs) MIRAX SCIENCE

  6. Hard X-raysurvey of central Galactic plane with GC continuous monitoring Unique capability to detect, localize, identify, and study many (1000 square degrees) short-lived, rare, and/or unpredictable phenomena, including X-ray transients and fast X-ray novae, for a wide range of time scales (hours to months) Alert service for astronomers on all s; coordinated optical/IR and radio observations MIRAX Strategy

  7. 2 hard X-ray imaging cameras(10-200 keV) built by DAS/INPE in collaboration with CASS/IAAT - 58o x 26o FWHM FOV with cameras at 29o - 7 arcmin angular resolution Detectors developed at CASS/UCSD MIRAX instruments

  8. Energy range:10-200 keV Crossed-strip CZT (Cd0.9Zn0.1Te) detectors 0.5-mm spatial resolution 5 keV spectral resolution @ 60 keV 3x3 modules of 2x2 detectors  370 cm2 total area Provided by CASS/UCSD CZT detectors 7cm x 7cm x 10cm

  9. HXI concept Plastic Scintilator (6mm-thick) drawings by L.A.Reitano Pb-Sn-Cu shield CZT modules support flanges Pb-Sn-Cu shield (2mm-0.5mm-0.1mm) mask support flange coded mask

  10. HXIs: Background rejection: events on multiple, non-contiguous sites; low-energy deep interactions Background: ~20 counts s-1 per imager (MGGPOD/GEANT) (aperture flux dominates background) Sources in the central GP FOV: ~1 Crab  100 counts s-1 < 2 x 10-5 photons/cm2 s keV @ 100 keV (one day, 5 ) 2.2 mCrab/day, 20-200 keV (65% observing efficiency due to Earth occultation) ~40 times better than BATSE/CGRO (Earth occult. technique) CXD one-year “survey” sensitivity (syst. limit of 0.1% of bkg):  10-11 ergs/cm2 s (10-50 keV) (> 20 times better than HEAO-1 A4) SXI:we hope for ~10 times better than ASM/RXTE  ~5 mCrab/day, 2-10 keV MIRAX sensitivity

  11. Current or planned hard X-ray imaging missions

  12. spacecraft conceptPMM – multimission platform

  13. spacecraft concept

  14. spacecraft concept MIRAX

  15. 23 compact objects more massive than NSs have been identified using radial velocities in the optical -> 4-15 M๏ range They also lack pulsations and type-I bursts. 17 are transients! Black Hole Science with MIRAX 16 Galactic BHs (Jerry Orosz) Scaled, tilted, and colored for surface temp. of companion star.

  16. A number of other X-ray binaries(~27+) are suspected of harbouring a black hole by virtue of their X-ray spectral similarities with bona-fide black holes, temporal variability properties and lack of neutron star signatures. ~25+ are transients! Black Hole Science with MIRAX • In states of active accretion, black hole binaries usually show two spectral components with a large diversity in their relative strengths: a soft (~1 keV) thermal emission from the accretion disk and a hard power-law, commonly attributed to inverse Compton.

  17. BH States of Active Accretion Energy spectraPower density spectra Steep power law Disk + ?? thermal Hard state Energy (keV) Frequency (Hz)

  18. MIRAX will provide complete temporal coverage of the evolution of a large number of accreting BHs and will characterize in detail the spectral state transitions(timescales of 1 day or even less) with broadband spectral coverage. The nature of the nonthermal component, which is the dominant mechanism for radiative losses at the highest accretion rates, remains a fundamental mystery of accretion energetics in black hole binaries Relativisticjets in microquasars: AGN jetshavebeenknown for decades; since 1994, radio astronomers have also been discovering jets in X-ray binary systems, with occasional ballistic jets moving at speeds ~0.9c. Black Hole Science with MIRAX

  19. Such relativistic jets have been seen from 7 Galactic binaries (4 with dynamically established black holes), while jets with lower velocity (~0.2c) have been resolved in 4 other cases. Microquasars provide the unique opportunity to observe the formation and evolution of mass ejections on timescales of seconds to days, while such processes take years to millennia in AGN. Now it is clear that some of the radio flares from GRS 1915+105 and Cyg X-3, the two most prolific jet sources, are correlated with X-ray activity, while the overall behavior is exceedingly complex. The emergence of the jet is probably a consequence of the rapid disappearance of the inner accretion disk. Black Hole Science with MIRAX

  20. Do the larger, relativistic ejections arise from the same mechanism as the smaller ones? Is there a common mechanism producing the explosive jets in every source? Why do some X-ray novae exhibit radio jets only during the first days of outburst? What is the connection between the hard X-ray and radio emission? If the jets are powered by the black hole spin, how is this energy tapped? MIRAXwill help to answer these questions by providing long exposures of microquasars with high (~65%) duty cycle and bandwidth (1–200 keV). Questions:

  21. MIRAX FWHM Secondary target fields MIRAX fields ASM/RXTE all-sky map Sco X-1 Cyg X-1 Crab

  22. MIRAX key contributions • Large Discovery Space coverage - 1000 square degrees around the central GP for ~9 months. • Simultaneous broadband (1-200 keV) spectroscopic (DE/E ~60) observations of a large sample of Galactic black holes for long (~months) time scales. • Integral and Swift GC observations suffer from low duty cycles which make them unlikely to detect short-lived transients and unable to perform detailed studies of longer-lived phenomena • Fermi/GLAST does not do it and there will probably be no other mission

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