Turbulence within dust clouds (TB)

– Good Afternoon

Quendella Taylor

Northern Arizona University/Penn State

Turbulence within dust clouds (TB)

– Why should we study ‘TB’? Because turbulence may answers many of the fundamental questions . For example what conditions are desirable for star formation to occur, what happens in the vicinity of star forming areas, IMF ,etc.In addition we are developing tools in order to study diffuse emission, in the GLIMPSE survey regions.

– How can we study ‘TB’? By using the structure function SF(l) and the power spectrum P(k) to analyze images taken from 2mass and MSX .

– What are the SF(l) and P(k)? They are tools we are going to use in order to understand

‘TB’. By removing the stars from images we may be able to isolate the diffuse emission .

Power Spectrum & Structure Function

• P(k) measures the distribution of power on scales in a specific region. P(k)= |F {Q}|^2 ; Q[k]=F[Q] = integral (Q(x)e^(-ikx))dx

– Signature of turbulence : Q is proportional to k^beta ; beta= -1.66, -2.00

– F = Fourier transform , Q= intensity , k = wave length, x= spatial coordinate

• SF(l) measures the spatial differences in a specific region

– <(Q(x)-Q(x+1))^2> or integral ((Q(x)-Q(x+1))^2dx

– if Q(x)=Q(x+1), then SF(l)=0 l= spatial distance

Understanding the Outputs

Implanted objects

Conclusion

• Well , I think using the tools given, it does work.

• Improvements– we need to find other way to remove the stars

or mask the structure function.

• What the future could bring– GLIMPSE: different wavelength and higher

resolution

Thanks to the following individuals

• Thanks to the NSF – the people who funded this program

• Thanks to Remy Indebetouw

• Thanks to Fabian Heitsch

– by Quendella Taylor