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Turbulence within dust clouds (TB)

This study explores turbulence within dust clouds, aiming to answer fundamental questions about star formation conditions and dynamics in star-forming regions. We develop analytical tools, specifically Structure Function (SF(l)) and Power Spectrum (P(k)), to analyze data from 2MASS and MSX. By isolating diffuse emissions from stars, we can gain deeper insights into turbulence signatures and their implications for understanding cosmic processes. Future work includes improving methods to enhance resolution and observation capabilities in the GLIMPSE survey regions.

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Turbulence within dust clouds (TB)

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  1. Turbulence within dust clouds (TB) • Good Afternoon Quendella Taylor Northern Arizona University/Penn State

  2. 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 .

  3. 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

  4. Understanding the Outputs

  5. Implanted objects

  6. 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

  7. 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

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