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The MSFC mirror for SXT-I Scientific Case -- Star-forming regions --

This scientific case explores the use of X-ray flares from proto-stars to understand planet formation. The MSFC mirror's sharper PSF size offers a gain of x2 in positional accuracy, making it advantageous in crowded star-forming regions. The study aims to determine the size of flares and how proto-planetary disks are illuminated. Simulated spectra and images are used to analyze the reflection geometry and identify the source of the flare.

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The MSFC mirror for SXT-I Scientific Case -- Star-forming regions --

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  1. The MSFC mirror for SXT-I Scientific Case-- Star-forming regions -- Astro-H Science Team M. Tsujimoto (JASA/ISAS)

  2. MSFC vs. GSFC in SFRs • MSFC mirrors has the sharper PSF size (rPSF) by x3 at a sacrifice of the effective area (EA) smaller by x1/2 than GSFC mirrors. • Assume that the position determination accuracy is proportional to rPSF / (S/N) ~ rPSF / (EA)1/2. • A gain of x2 in the positional accuracy for MSFC. • This is a great advantage in star-forming regions, where 10-20 sources are crowded in the SXS FoV.

  3. A practical science case • X-ray flares from proto-stars (=young Suns) illuminate their circumstellar (proto-planetary) disks. • Crucial to unveil the initial condition of planet formation. • X-rays are a major ionization source of disks (Glassgold+ 1997). • It affects the disk chemistry and evolution (Nomura+ 2007). • An artists view (a video clip; SAO). Scientifically unproven. • It is known (Imanishi+ 2001; Tsujimoto+ 2005) that • Proto-stars commonly erupt flares occasionally (2-3/week). • Fe I Ka fluorescence line emission at 6.4 keV is (1) the direct proof of photo-ionization, (2) a useful diagnosis to reveal the illumination geometry. • It is unknown (and Astro-H will bring new big clues to) • How large the flares are? • How the proto-planetary disks are illuminated?

  4. 100 ks XMM-Newton view* (Imanishi+ 2001, ApJ) (Imanishi+ 2001, ApJ) r Oph cloud (D=120 pc) Fe I Ka fluorescence Any stars in SXS FoV can cause such flares once in 2-3 days. A 100 ks observation will catch some flares. *Stelzer, B. @ http://www.mpe.mpg.de/ixo/files/workshop_mpe_2008/ixo_MPE_v2.ppt.

  5. SXS Fe XXVI Ka Fe XXV Ka Fe I Ka SXI (GSFC) SXI (MSFC) Simulation: SXS/I spectra • Simulated spectra based on observed values in YLW16A (Imanishi+ 2001) • NH=4.7x1022/cm2 • kBT=10.7 keV • EW (Fe I Ka)=146 eV • Fx = 1.1x10-11 erg/s/cm2 Compton shoulder Direct emission Reflected emission EW (Fe I Ka) & CS are independent tools for the reflection geometry.

  6. Simulation: SXI image • Which star caused the SXS flare? XMM image smoothed with 1’.3. XMM image smoothed with 0’.4.

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