HI power spectrum of the spiral galaxy NGC628

Abstract

We have measured the HI power spectrum of the nearly face-on spiral galaxy NGC628 (M74) using a visibility based estimator. The power spectrum is well fitted by a power law $P(U)=A{U}^{\alpha }$, with $\alpha =-1.6\pm 0.2$ over the length scale $800\mathrm{pc}\mathrm{to}8\mathrm{kpc}$. The slope is found to be independent of the width of the velocity channel. This value of the slope is a little more than one in excess of what has been seen at considerably smaller length scales in the Milky-Way, Small Magellanic Cloud (LMC), Large Magellanic Cloud (SMC) and the dwarf galaxy DDO210. We interpret this difference as indicating a transition from three dimensional turbulence at small scales to two dimensional turbulence in the plane of the galaxy's disk at length scales larger than galaxy's HI scale height. The slope measured here is similar to that found at large scales in the LMC. Our analysis also places an upper limit to the galaxy's scale height at $800\mathrm{pc}$ .

4 Pages, 2 Figures, 1 Table. Accepted for Publication in MNRAS LETTERS

References in corpus (2)

• Hierarchical Star Formation in the Spiral Galaxy NGC 628
• Power spectrum of HI intensity fluctuations in DDO 210

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