1 / 16

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 10 6 K Lx ~2x10 38 erg/ s. Li & Wan 2007. X-ray spectroscopy: He-like ions. R ( or W) : Resonance line (allowed)

enan
Download Presentation

X-ray Emission Line Spectroscopy of Diffuse Hot Plasma

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. 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

  2. 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.

  3. Solar Wind Charge Exchange From Dennerl 2010

  4. 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

  5. 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

  6. 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

  7. Chandra ACIS observations of nearby galaxies (Credit: NASA/CXC/SAO/R.DiStefano et al.) Soria& Wu (2002)

  8. 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.

  9. 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

  10. XMM-Newton Reflection Grating Spectrometers

  11. Spatially-resolved X-ray spectroscopy OVIII contours on HST image OVIII contours on OVII image

  12. NGC 4438 in the Virgo Cluster Ha+[NII] image (Kenney et al. 1995). Chandra 0.3-2 keV image, Machacek et al. 2004

  13. Operating X-ray Telescopes Chandra XMM-Newton SWIFT Suzaku

  14. Future X-ray telescopes eROSITA 2012 Astro-H, planned for launch in 2013 Athena???

  15. 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.

More Related