1. Interstellar Scattering Joseph Lazio (Naval Research Laboratory) J. Cordes, A. Fey, S. Spangler, B. Dennison, B. Rickett, M. Goss, E. Waltman, M. Claussen, D. Jauncey, L. Kedziora- Chudczer, R. Ojha

2. Radio-wave Scattering   r e  n e ds Electron density fluctuations  Refractive index fluctuations  Corrugated phase fronts  Image distortions (cf. atmospheric seeing) Characterized by a scattering measure SM    n e 2 dx

3. Ionized Interstellar Medium H II regions EM > 10 4 pc cm -6 Powered by O or B star(s) Warm ionized medium (WIM) n ~ 0.1 cm -3 T ~ 8000 K f ~ 0.2 1/6 of O star luminosity WHAM survey

4. Scattering Observables Angular broadening –Pulsars –Extragalactic sources –Masers and other Galactic sources Intensity scintillations –Pulsars –Extragalactic sources Pulse broadening/scintillation bandwidth Pulsars (Spectral broadening) Scattering characterized typically by scattering measure SM    n e 2 dx Not really scattering observables, but related observables include Rotation measure Optical emission from diffuse gas (  EM =  n e 2 dx) Dispersion measure variations (DM =  n e dx) Diffuse gamma-ray emission?

5. Radio-wave Scattering Analyses    n e ds  ~ 2 SM Scattering physics –Density spectrum Spectral index Inner scale –Scattering genesis Distribution –“regional” –Galactic slope coefficient  SM

6. The Density Spectrum and Angular Broadening Point source at infinity V(b) = e -D(b)/2 Phase structure function D(b) =  [  (x) -  (x+b)] 2  D(b)   dq P  n (q)  [1–J 0 (bq)] P  n (q)  q -  (or …)

7. Density Fluctuation Power Spectrum Density spectrum in local interstellar medium Power law, with spectral index near Kolmogorov value –Notable exceptions! –Large dynamic range! Interstellar plasma has large Reynolds number.  Turbulent processes responsible for density fluctuations(?). Density spectrum elsewhere in Galaxy similar, probably. Armstrong, Rickett, & Spangler (1995) 1 pc1 AU

8. Extreme Scattering Events Events simultaneous at 2.2 and 8.1 GHz Duration of few weeks to months  intrinsic: T b  10 15 K  extrinsic: AU-sized refracting clouds in our Galaxy

9. ESE of 1741-038: 1992 June 20 (18 cm) Need a new monitoring program!

10. Density Fluctuation Power Spectrum Armstrong, Rickett, & Spangler (1995) 1 pc1 AU Density spectrum in local interstellar medium Power law, with spectral index near Kolmogorov value –Notable exceptions! –Large dynamic range! Interstellar plasma has large Reynolds number.  Turbulent processes responsible for density fluctuations(?). Density spectrum elsewhere in Galaxy similar, probably.

11. Turbulence Inner Scale If density fluctuations result from turbulence, inner scale would be a dissipation scale. Scattering resolved if b ~ /  d. Inner scale important if l 1 ~ b. Inner scale estimates are roughly 200 km. Spangler & Gwinn attribute it to the ion inertial length or ion Larmor radius.  Note gap in coverage from 30 km to 1000 km. Spangler & Gwinn (1990)

12. Sub-parsec magnetic fields NGC 6334B and Cyg X-3 show rotation of image shape with frequency: –Different frequencies sample different length scales in scattering medium.  Density fluctuations changing shape on these scales.  Magnetic fields aligning density fluctuations on this scale. Yet Sgr A* and B1849+005 do not…

13. Scattering Genesis Scattering traces star formation –NGC 6334B (Trotter et al.) –Cygnus region (many studies) Direct link more difficult to establish –Spangler et al. vs. Simonetti & Cordes and Spangler & Cordes Should be able to do much better today and in future 2013+370/G74.9+1.2 CTA 1

14. Where is the Scattering Medium? (“Regional”) Sources embedded in the medium are less scattered than background sources  Scattering must overcome the wavefront curvature. Distance ambiguity for Galactic sources No ambiguity for extragalactic sources  xgal = (D GC /  GC )  GC  Can solve for  GC.

15. Where is the Scattering Medium? B1849+005 PSR B1849+00

16. GC Scattered Images Sgr A* displays enhanced angular broadening OH/IR stars have maser spots with comparable diameters GC scattering diameter: 1" @ 1 GHz

17. GC Scattering—Where? Likelihood Results: xgal sources:  GC < 500 pc OH masers: 50 pc <  GC < 300 pc  GC  150 pc  xgal  75” @ 1 GHz Angular extent  1  (Note 1°  150 pc.) Inhomogeneous on  10–20 pc  X-ray emitting gas + molecular gas

18. Radial Extent of the WIM (“Galactic”) H I disks of nearby galaxies appear truncated Due to extragalactic ionizing flux?  H II disk extends much farther? Corbelli et al. 1989 H I H (= H I + H II )

19. Radial Extent of the WIM H I disks of nearby galaxies appear truncated; due to extragalactic ionizing flux?  H II disk extends much farther? Corbelli et al. 1989 Savage et al. 1995 C IV absorption toward H1821+643 suggests ionized gas at R ~ 25 kpc

20. Radial Extent and Warp of the WIM WIM radial extent equals or exceeds H I : H I disks truncated at R ~ 25–50 kpc (Galaxy a prototypical z = 0 Ly α cloud?) C IV absorption toward H1821+643, R ~ 25 kpc HVC models often require pressure support at R ~ 25 kpc

21. VLBA Survey 12 sources –7 with |b| < 1° –5 with l ~ 180° and |b| < 10° Cf. Dennison et al. 1984

22. Best-fit Radial Model  No Perseus spiral arm  Perseus spiral arm at 25% of TC93 truncated disk sech 2 disk

23. Sources of Scattering Truncated disk because of star formation? Molecular clouds show radial truncation; Star formation follows molecular clouds;  Scattering truncates where star formation does.  Similar to what is seen in other galaxies. Molecular cloud distribution from CO survey by Wouterloot & Brand 26 kpc

24. Ne2001 (Cordes & Lazio 2002, astro-ph/0207156) Number of data have nearly doubled. Modifications from TC93: –GC component added;  Diffuse component truncated at 20 kpc; –Diffuse component made thicker;  Spiral arms extrapolated;  Spiral arms made thicker; –Orion-Cygnus arm added; –Local Bubble and similar regions added;  “Clumps” and “voids” added.

25. Anomalous Scattering Effects Multiple media can lead to anomalous scattering effects – Phase  – Scattering angle  2 Effects occur because size of scattering region can become important in determining size of scattering disk. E.g., scattering of sources seen through other galaxies. Important for LOFAR? Infinitely extended scattering screen … Or not.

26. Cosmic Rays,  rays, and the WIM CRs are charged particles Smooth CR energy spectrum Magnetic irregularities scatter CRs Same magnetic irregularities cause scattering? 1 pc1 AU CR energy spectrum/gyroradii

27. Summary: Interstellar Scattering Exquisite probe of sub-parsec plasma physics –Density spectrum –Magnetic fields –Interstellar “clouds” (ESEs) –Cosmic rays? Galactic distribution of scattering –Large-scale tracer of Warm Ionized Medium (WIM) –Traces star formation See also –Intraday variability –Pulsar parallax and proper motions VLBA itself has been an immense step forward. VLBA + other telescopes is good. NMA will close gap around 100 km. LOFAR will be wonderful instrument for scattering studies ( 2 ). Difficult to avoid scattering at LOFAR frequencies! Space VLBI would be good, if frequency is low enough. SKA will be even better.

28. FINIS

29. Where is the Scattering Medium?

30. GC Scattering—Pulsars 10 7 –10 8 neutron stars:  Massive star formation  High-energy sources Selection Effects: – beaming & LF – velocities – background – pulse broadening

31. GC Scattering—Pulse Broadening  GC ~ 350 seconds GHz -4  Periodicity search: long-period, shallow spectra pulsars, > 8 GHz  Imaging search: steep-spectrum point sources, ~ 1” @ 1 GHz 10 seconds

32. Characterizing Scattering Strong scattering at SIRA (and LOFAR) frequencies: Fresnel radius R F = 3 x 10 12 cm (D/100 pc) 1/2 ( /1 MHz) -1/2 rms phase in Fresnel radius >> 1 Two characteristic regimes within strong scattering: oDiffractive oRefractive Rickett 1990

33. Refractive Effects Unimportant  time scales too long Refractive scintillation time scale  -2 666 6660  t r (@ 1 MHz in yr) Rickett et al. 1984

34. Diffractive Effects Diffractive scintillation seen commonly in pulsar observations at meter and centimeter wavelengths. Characteristic bandwidth,  d ~ 3 kHz (@ 1 MHz) Characteristic time,  t d ~ 60 s (@ 1 MHz for v ~ 100 km/s)  No objects will scintillate (twinkle). Frequency  Time  Scintille

35. Diffractive Effects Pulse broadening smears out pulsar pulses. At SIRA frequencies, extreme pulse broadening can be obtained.  Most pulsars will not be seen as pulsed objects.

36. Diffractive Effects Angular broadening distorts view of sources. Magnitude is large.  Current SIRA specs more than sufficient! Local Bubble

37. Optical Depth Electrons responsible for scattering also contribute to free- free optical depth. 0.24 MHz 0.4 MHz

38. Cosmic Rays and  rays Diffuse  -ray emission: –p + p ®    ®  –e + p ®  –e +  ® 

39. Cosmic Rays and  rays