SIMULATING ASTRO-H OBSERVATIONS OF GALAXY CLUSTER GAS MOTIONS:

WHAT WE CAN EXPECT AND IMPLICATIONS FOR FUTURE MISSIONS

John ZuHone, MIT Kavli Institute

withEric Miller (MIT), Aurora Simionescu (ISAS/JAXA), Mark Bautz (MIT)

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

0.1

110

norm

aliz

ed c

ount

s s−

1 keV

−1

Energy (keV)

data and folded model

sekiya 6−Jun−2011 12:36

vturb = 0 km/svturb = 100 km/svturb = 300 km/svturb = 1000 km/s

6.7

w

xyz

jk

e

po

Perseus simulated spectrum (wabs＊bapec)

He-like Fe line at E0 ≈ 6.7 keV

CORE GAS SLOSHING

Markevitch & Vikhlinin 2007

ZuHone, Markevitch, & Johnson 2010

• 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?

LOOKING PERP TO PLANE

Inviscid

SB T

σμarXiv:1508.04426

LOOKING INTO THE

PLANE

Inviscid

SB T

σμarXiv:1508.04426

LOOKING PERP TO PLANE

Viscous

SB T

σμarXiv:1508.04426

LOOKING INTO THE

PLANE

Viscous

SB T

σμarXiv:1508.04426

INVISCID: IN THE PLANE

VISCOUS: IN THE PLANE

DIFFERENT VISCOSITY, SAME SHAPE

arXiv:1508.04426

DIFFERENT MOTIONS, SAME SHAPE (SOMETIMES)

arXiv:1508.04426

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

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

Predicted vs. RealVelocity

Distributions

arXiv:1508.04426

ACCOUNTING FOR PSF

SCATTERING

arXiv:1508.04426

A2319

200 kpc

A3667

200 kpc

�������Perseus

Where should

we look?

Astro-H

Athena

Shift Width

Shift Width

Inviscid

Viscous

Cluster at z = 0.05

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.)