Simulating Astro-H Observations of Galaxy Cluster Gas Motions: What We Can Expect and Implications for Future Missions
•
0 gefällt mir•375 views
Talk given to the "The Universe in High-resolution X-ray Spectra" meeting in Cambridge, MA, August 2015.
Empfohlen
Empfohlen
Weitere ähnliche Inhalte
Was ist angesagt?
Was ist angesagt? (20)
Ähnlich wie Simulating Astro-H Observations of Galaxy Cluster Gas Motions: What We Can Expect and Implications for Future Missions
Ähnlich wie Simulating Astro-H Observations of Galaxy Cluster Gas Motions: What We Can Expect and Implications for Future Missions (20)
Mehr von John ZuHone
Mehr von John ZuHone (6)
Kürzlich hochgeladen
Kürzlich hochgeladen (20)
Simulating Astro-H Observations of Galaxy Cluster Gas Motions: What We Can Expect and Implications for Future Missions
- 1. SIMULATING ASTRO-H OBSERVATIONS OF GALAXY CLUSTER GAS MOTIONS: WHAT WE CAN EXPECT AND IMPLICATIONS FOR FUTURE MISSIONS John ZuHone, MIT Kavli Institute with Eric Miller (MIT),Aurora Simionescu (ISAS/JAXA), Mark Bautz (MIT)
- 2. ASTRO-H MISSION • To be launched early next year • Soft X-ray Spectrometer (SXS): • 3’x3’ FOV • ~5 eV spectral resolution • ~1’ spatial PSF 6.4 6.5 6.6 0.1110 normalizedcountss−1 keV−1 Energy (keV) data and folded model sekiya 6−Jun−2011 12:36 vturb = 0 km/s vturb = 100 km/s vturb = 300 km/s vturb = 1000 km/s 6.7 w xyz j k e po Perseus simulated spectrum (wabs＊bapec) He-like Fe line at E0 ≈ 6.7 keV
- 3. CORE GAS SLOSHING Markevitch &Vikhlinin 2007 ZuHone, Markevitch, & Johnson 2010
- 4. • Can we detect these sloshing motions with Astro-H? • If so, what effect will these motions have on the shift and shape of spectral lines? • Can we use this spectral analysis to tell us something about microphysics?
- 12. DIFFERENT MOTIONS, SAME SHAPE (SOMETIMES) arXiv:1508.04426
- 13. SYNTHETIC OBSERVATIONS ZuHone et al 2014, arXiv:1407.1783 SIMX http://www.youtube.com/watch?v=fUMq6rmNshc http://yt-project.org http://hea-www.harvard.edu/simx/ + PHOX http://www.mpa-garching.mpg.de/~kdolag/Phox/ (Biffi et al 2012, 2013, MNRAS) event lists: RA, Dec, E “real” event files
- 14. FITTING SPECTRA Model 1: Single-T APEC model, w/ thermal broadening only exposure time = 200 ks Model 2: Single-T APEC model, w/ thermal and Gaussian velocity broadening exposure time = 200 ks
- 18. Astro-H Athena Shift Width Shift Width Inviscid Viscous Cluster at z = 0.05
- 19. SUMMARY • Astro-H will be able to measure line shifts and widths from sloshing motions in nearby galaxy clusters • It will be difficult to distinguished line broadening from sloshing motions vs. turbulent motions • Constraints on viscosity are probably limited • Must worry about systematics—Gaussian models for non-Gaussian velocity distributions, PSF scattering from core • What do we need? Better spatial resolution! (Athena, X-ray Surveyor, etc.)