Issue 
A&A
Volume 584, December 2015



Article Number  A111  
Number of page(s)  10  
Section  Interstellar and circumstellar matter  
DOI  https://doi.org/10.1051/00046361/201526431  
Published online  01 December 2015 
Online material
Appendix A: Deriving the power spectrum of the SPIRE 250 μm beam
The power spectrum of the SPIRE 250 μm beam was derived from an empirical PSF image obtained by the SPIRE ICC from scan map data^{10} of Neptune in four directions. There are two sets of empirical PSFs available, one gridded at the nominal pixel size for each SPIRE passband and the other at a higher pixel resolution of 0.̋6. We used the latter product, but the angular extent of the footprint was only about 6.́0, corresponding to an angular frequency scale of ~0.3 arcmin^{1}, insufficient to correct for the beam convolution effect on large scales (i.e., small ). Therefore, to extend the angular frequency range of the beam power spectrum to lower values, we embedded the beam map of Neptune inside a larger map 25.́0 on a side, and then padded the pixels outside the central Neptune insert using the bestfit 2D Gaussian approximation to the beam.
The power spectrum of the SPIRE 250 μm beam as a function of angular frequency, , is shown in Fig. A.1. The power spectrum asymptotically converges to unity at small angular frequencies, but rapidly declines toward high angular frequencies (small angular scales). We caution that the SPIRE beam spectrum has a slight suppression of power around 0.2 arcmin^{1}<< 1.5 arcmin^{1} compared to a pure Gaussian shape. This problem led Martin et al. (2010) and MivilleDeschênes et al. (2010) to approximate the beam power spectrum using higherorder polynomial corrections to the Gaussian fit. The effective full width at half maximum (FWHM) of the SPIRE 250 μm beam power spectrum^{11} is about 2 arcmin^{1}, as shown by the dashed curve in Fig. A.1.
Fig. A.1
Power spectrum of the SPIRE 250 μm beam, (black solid curve). The dashed curve represents the power spectrum of a Gaussian beam with a FWHM equal to the nominal 18.̋2 HPBW of the SPIRE 250 μm beam. The dotted vertical line marks the FWHM of the corresponding power spectrum in the angular frequency domain. 

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Appendix B: Results from highresolution column density maps
Figure B.1 shows the power spectrum of the same filament already displayed in Fig. 2, but here derived from a highresolution column density map obtained using the multiscale decomposition scheme of Palmeirim et al. (2013). The power spectrum values at high spatial frequencies has more scatter than the one derived by converting I_{250} to H_{2}column density (see Fig. 4). This is primarily because the multiscale decomposition technique introduces fluctuations at small spatial scales which manifest themselves through enhanced scatter in the Fourier modes at high spatial frequencies. The distribution of power spectrum slopes derived from highresolution column density maps for the whole sample of filaments is shown in Fig. B.2. The mean power spectrum slopes before and after correcting for the beam effect are and , respectively. Within the quoted errors, these results are indistinguishable from those found in Sect. 5.1 using modified 250 μm maps.
Fig. B.1
Power spectrum of the linemass fluctuations along the Pipe filament shown in Fig. 2 as measured in the highresolution H_{2}column density map resulting from the multiscale decomposition technique of Palmeirim et al. (2013) Fig. 4. The powerlaw fits to the power spectra P_{obs}(s) (black plus symbols) and P_{true}(s) (cyan filled circles) have logarithmic slopes α_{obs} = −2.3 ± 0.2 and α_{corr} = −1.7 ± 0.3, respectively. 

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Fig. B.2
Distributions of power spectrum slopes measured in the highresolution H_{2}column density maps before beam correction (dashed histogram) and after beam correction (solid histogram). Similar to Fig. 7 but based on data from the highresolution column density maps instead of the modified 250 μm maps. Bestfit Gaussian curves to the two observed distributions are overplotted. The two distributions are centered on α_{obs} = −1.9 ± 0.3 and α_{corr} = −1.6 ± 0.45 for the uncorrected and beamcorrected power spectra, respectively. 

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© ESO, 2015
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