X ray emission line spectroscopy of diffuse hot plasma
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IRAC 8 micro K-band 0.5-2 keV. X-ray Emission Line Spectroscopy of Diffuse Hot Plasma. Chandra ACIS-I. XMM-Newton RGS Liu, Wang, Li, & Peterson 2010. T ~ 3 x 10 6 K Lx ~2x10 38 erg/ s. Li & Wan 2007. X-ray spectroscopy: He-like ions. R ( or W) : Resonance line (allowed)

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X-ray Emission Line Spectroscopy of Diffuse Hot Plasma

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X ray emission line spectroscopy of diffuse hot plasma

IRAC 8 micro

K-band

0.5-2 keV

X-ray Emission Line Spectroscopy of Diffuse Hot Plasma

Chandra ACIS-I

XMM-Newton RGS

Liu, Wang, Li, & Peterson 2010

T ~ 3 x 106 K

Lx~2x1038 erg/s

Li & Wan 2007


X ray spectroscopy he like ions

X-ray spectroscopy: He-like ions

  • R (or W): Resonance line (allowed)

    1s2p 1P11s21S0

    electronic dipole transition

  • I (or x+y): Intercombination line

    1s2p 3P1 1s2 1S0 (y)

    1s2p 3P21s2 1S0 (x)

    Triple or quadruplet

  • F (or z): Forbidden line

    1s2s 3S1 1s2 1S0

    relativistic magnetic dipole transition (Ajivery low)

R

I

F

Simplified Grotrian diagram

Porquet & Dubau (2000)

Photo-ionized plasma as seen in an AGN can have stronger forbidden lines.


Solar wind charge exchange

Solar Wind Charge Exchange

From Dennerl 2010


Solar wind charge exchange1

Solar Wind Charge Exchange

  • Charge exchange (CX) nature of comet X-ray emission is confirmed, spectroscopically and temporally.

  • CX has a cross-section of ~10-15 cm-2

  • PCX/Pthpropto 1/ne2 on scales of mean free path

CX is also expected at the heliosphere

Peter Beiersdorfer


Much of the diffuse soft x ray background may arise from the cx

Much of the diffuse soft X-ray background may arise from the CX!

4U1957+11

AGN

Futamoto et al. 2004, Wang et al. 05, Yao & Wang 05/06, Yao et al. 06/07/08

ROSAT all-sky survey in the ¾-keV band

X-ray binary


X ray absorption line spectroscopy of diffuse hot plasma

Fe XVII K

X-ray absorption line spectroscopy of diffuse hot plasma

  • Tracing all K transitions of metals  all three phases of the ISM.

  • Not affected by photo-electric absorption unbiased measurements of the global ISM.

LETG+HETG spectrum of LMXB 1820-303

Yao & Wang 2006, Yao et al. 2006, Futamoto et al 2004


Chandra acis observations of nearby galaxies

Chandra ACIS observations of nearby galaxies

(Credit: NASA/CXC/SAO/R.DiStefano et al.)

Soria& Wu (2002)


Xmm newton rgs spectrum of the nuclear starburst region of m51

XMM-Newton RGS spectrum of the nuclear starburst region of M51

Charge exchange may be responsible for much of diffuse soft X-ray emission in both normal and starburst galaxies.


Similar cx signatures are also observed in starburst galaxies

Similar CX signatures are also observed in starburst galaxies

Li, Mao, Wang 2011

Soft X-ray arises primarily from the interplay between a superwind and entrained cool gas clouds.

Composite of optical (HST), infrared (Spitzer), and X-ray (Chandra) images


Xmm newton reflection grating spectrometers

XMM-Newton Reflection Grating Spectrometers


Spatially resolved x ray spectroscopy

Spatially-resolved X-ray spectroscopy

OVIII contours on HST image

OVIII contours on OVII image


Ngc 4438 in the virgo cluster

NGC 4438 in the Virgo Cluster

Ha+[NII] image (Kenney et al. 1995).

Chandra 0.3-2 keV image, Machacek et al. 2004


Operating x ray telescopes

Operating X-ray Telescopes

Chandra

XMM-Newton

SWIFT

Suzaku


Future x ray telescopes

Future X-ray telescopes

eROSITA 2012

Astro-H, planned for launch in 2013

Athena???


Summary

Summary

  • X-ray spectroscopy is the future of the X-ray astronomy  X-ray astrophysics, providing key diagnostics of plasma in the Universe.

  • Much of the diffuse X-ray emission from galaxies may arise from the charge exchange.

  • A lot can already be done to understand the process, which traces the galactic feedback and the presence of cool gas, especially in low density environments.


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