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Using Pulsars to probe the interstellar mediumPowerPoint Presentation

Using Pulsars to probe the interstellar medium

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Using Pulsars to probe the interstellar medium

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Barney Rickett,

University of California San Diego

Department of Electrical & Computer Engineering

Presentation at PAC 2012 - KIAA/PKU October 2012

- FAST sensitivity and sky coverage => More pulsars and DMs (DM = ∫ ne dl)
- Pulsar HI absorption measurements => new pulsar distances
- More pulsars, DMs & distances
- => Better model for electron distribution in Galaxy
- => Better model for 3D distribution of pulsars

- Pulsar Rotation Measures + better electron model
- => Better model for Galactic Magnetic Fields

- DM = ∫ Lp ne dl = ∫ Zp ne(z) dz/sinb
- DM sinb = ∫ Zpne(z)dz
- if Zp < Hne DM => Lp ne(0) Lp
- if Zp > Hne DM sinb => DM90 = ∫ ∞ne(z)dz ~ ne(0) Hne

z

*

Zp

Hne

Lp

*

ne(z)

20/sinb

DM = ∫ ne dl = ∫ ne(z)dz/sinb < DM90 /sinb

DM sinb = ∫ Zpne(z)dz < DM90

Possibility to determine the temperature and number of cool HI clouds.

emission

absorption

delay

Cygnus Region

SMC LMC

Ia ~ ∫ ne2 dl = EM (cm-6 pc)

Large Iacan be a lower bound to EM (due to saturation)

FAST: ZA< 40deg

AO: ZA< 20deg

Psrs & high DM in LMC & SMC

FAST: ZA< 40deg

AO: ZA< 20deg

- Modelling the electrons in the Galaxy:
- Taylor & Cordes 1993; Cordes & Lazio 2001-2006
- Questions:
- Are pulsars concentrated in spiral arms?
- At 100 km/sec a psr moves 1kpc in 107 years

- a spiral arm? or due to AO observational (sensitivity) bias

42 deg

Cordes & Lazio 2006

Need to compare

distributions of

Plasma and Pulsars

Neutron star distribution as history of star formation ?

- Small-scale structure in the ISM scatters radiowaves
- Refractive index deviation l2
- Scattering is typically consistent with Kolmogorov turbulence over scales from 1000 km -> 100 AU (Armstrong et al. 1995)
- But turbulence level is very inhomogeneous i.e. “patchy”
- see the Ha maps

- Turbulence is often anisotropic
- Probe by pulsar scattering:
- DM variation
- Pulse Broadening time & ISS bandwidth
- Scattering hides pulsars (esp. MSPs)

- Scintillation Arcs (Stinebring et al.)

From Radio Galaxy Quasar or AGN

2000

pc

The solid line gives the best fit line with power law index a =1.66 ±0.04 consistent with Kolmogorov a = 5/3

Ramachandran et al 2006:

Slope = 1.66

pulsar

zp

scattering layer

zo

q

Scattered Image Brightness = B(q,b)

Scattered Pulse shape:

P(t) = ∫ 02πB[q=√(2ct/zeff),b] db

zeff = (zo+zp)(zp/zo)

Pulse Broadening timetscatt= zeffq2 /2c f -4.4

Kolmogorov:

Inner scale < 10km

loge[P(t)]

Detailed shape is a diagnostic of scattering at high wavenumbers (ie due to very small scales)

Conclude linner ~ 75 km

Allowing for anisotropy makes this a lower limit

This requires very high signal to noise ratio (ie FAST)

Inner scale > 1000km

The uniform Kolmogorov model predicts:tscatt DM2.2

But the observations show a much steeper dependence on DM. They imply that at larger distances through the electron layer, there is an increasing chance of encountering regions of high density and high turbulence.

This result is built in to the Galactic electron model of Cordes & Lazio (2003) as a high level of patchy turbulence in the inner Galaxy

Note that tscatt responds to a column of density-variance (related to emission measure). Since we expect dne ~ne , tscatt picks out the highest densities along a line of sight.

dnd

Scintillation Arcs

dtd

tscatt= 1/(2π dnd)

“Secondary Spectrum” (S2) with

three scintillation arcs

Primary Dynamic Spectrum

delay t (µsec)

Doppler Frequency fD (mHz)

Hill, Stinebring et al. (2005) showed this example of the arcs observed for pulsar B0834+06. In addition to the main forward arc (following the dotted curve) there are “reverse arclets”. Those labelled a-d are particularly striking.

They observed them over 25 days and found that they moved in Delay and Doppler, precisely as expected for the known pulsar proper motion.

Doppler Frequency fD (mHz)

334 MHz

321 MHz

Predicted for plasma refraction

The right plot shows how fD varies with observing frequency.

Remarkably this shows that the spatial location of the scatterers is independent of frequency. They DO NOT show the expected shift due to the dispersive nature of plasma refraction.

The left plot shows the angular position of the structures (in mas) responsible for each reverse arclet, mapped from the Doppler frequency fD . The lines have the slope expected for the known pulsar proper motion.

Note reverse arclets and one group at delay of 1 msec

Note the faint offset scattering responsible for the “1 msec” arclet

Scattered image reconstructed by mapping from the secondary spectrum. The phase provides orientation in RA/Dec

(J-J Gao PhD UCSD)

Dqdec (mas)

DqRA (mas)

Doppler Frequency fD (mHz)

Blue line shows the axis derived from VLBI by Brisken, Gao et al.

Scattered Brightness is Anisotropic, Asymmetrical & Intermittent

- New tool for study of ISM
- Thin screen model is often remarkably successful => ISM is patchy
- Examples of thin arcs and multiple “reverse arclets” require:
- a) Highly anisotropic scattering
- b) very patchy distribution of “turbulence”
- Intense turbulent regions ~10 AU dominate in a path of 108 AU !
- Together these upset the assumptions of isotropy and uniformity in a turbulent & ionized ISM. Instead we have anisotropy and intermittency in the turbulence.
- It leaves us with fascinating puzzles:
- What are the astro-physical sites that cause peaks in the scattering?
- What is the cause of the 1-D fine structure ? What role for magnetic field?
- What consequences for MSP timing ?

- New ideas from Cyclo-Stationary spectral analysis
- New facilities GBT, EVLA, LOFAR, FAST

- The sensitivity of the FAST telescope will explore the ISM on the large scale:
- Spatial distribution of Pulsars
- Inside and outside of spiral arms
- More associations with supernova remnants

- New distance measurements by sensitive HI absorption
- Delay spectrum as a new probe of HI

- New DMs improve the modelling of plasma in the Galaxy (Ne2020?)
- What ionizes the ISM?
- Influence of HII regions and supernova remnants

- New Rotation Measures improve knowledge of the Galactic Magnetic Field
- RM from pulsars, extra-galactic sources and diffuse synchrotron emission
Scattered pulse shapes and secondary spectra will explore the ISM on the small scale:

- RM from pulsars, extra-galactic sources and diffuse synchrotron emission
- Monitoring the non-uniform ISM for corrections to pulsar timing
- DM variation of MSPs for timing correction

- Particular discrete regions of scattering
- What is their physical origin?
- What is their density in interstellar space?

- Study of turbulence in the interstellar plasma

PSR B1737+13 mjd 53857 Arecibo 320 MHz Stinebring

In the 1-D scattering we find secondary spectrum:

S2(t,fD) µ B(t/AfD+AfD) x B(t/AfD-AfD) / |fD|

in terms of the 1-D brightness function B(q) and a scaling constant A

Hence from observations of S2 one can fit the observations S2 to a 1-D model and so estimate B(q)

PSR B1737+13 mjd 53857 Arecibo 320 MHz Stinebring

PSR B1737+13

mjd 53857 1700 MHz

1-dim Scattered Power

Scattered Brightness is Anisotropic, Asymmetrical & Intermittent

ft

Relative to a center time t0 and frequency n0, the interference term is:

Cos[2πfn(n-n0) + 2πft(t-t0)+Df0]

fn = dt1- dt2 = [q12- q12] (z/2c)

ft = dn1- dn2 = (q1x- q2x)V/l

t-t0

fn

2DFT

x

x

S1

S2

n-n0

scattering screen

I = |E1 + E2|2 if E1 and E2 are coherent at frequency n:

= |E1|2 + |E2|2 + 2E1E2cos(Df)

where Df = 2π(n1t1-n2t2)+f01-f02

t1 = t+dt1,n1 = n+dn1

Df = 2π[n(dt1- dt2)+(dn1- dn2)t .. + ..O(dn,dt) + f01-f02]

V

where

dt1 = zq12/2c is the relative time delay

dn1 = n(V.q1)/c is the relative Doppler frequency

V

q

2

z

q

1

scattering screen

t= dt1- dt2 = [q12- q22] (z/2c)

fD = dn1- dn2 = (q1x- q2x)V/l

With q2 fixed there is a quadratic relation between t and fD which depends on q1y2. If in addition q1x and q1y lie on a straightline (ie 1-D scattered brightness) the relation is a parabola through the origin => reverse arclet

b

In that case the visibility phase on baseline b corresponds to the mean position of the two angles => π (q1+ q2). b/l

Apex of parabola is where q2=0, hence visibility phase at an apex gives astrometric measure of q1.

Proper motion ~30 mas/yr

Psr distance 4.8 kpc (DM)

Angle units ~ mas

Proper motion predicts

0.5 mas per week

No coherent shifts seen

Some decorrelation even over half-hour

Individual scattering centers

Background of distributed turbulence

Perpendicular Geometry

Anisotropic & intermittent - spaghetti-like filaments in SN remnants

Separate offset feature also needed

Parallel Geometry

Isotropic scatterers clumped linearly

Other clumps too far from line of sight

~4 pc

Bright shell:

EM ~ 100 pc cm-3

dL ~ 1 pc

=> max ne ~ 10 cm-3

Ha intensity ± 5 deg latitude