English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Two major features of the prestellar CMF are: 1) a broad peak below 1 Msun,presumably corresponding to a mean gravitational fragmentation scale, and 2) acharacteristic power-law slope, very similar to the Salpeter slope of thestellar initial mass function (IMF) at the high-mass end. While recent Herschelobservations have shown that the peak of the prestellar CMF is close to thethermal Jeans mass in marginally supercritical filaments, the origin of thepower-law tail of the CMF/IMF at the high-mass end is less clear. Inutsuka(2001) proposed a theoretical scenario in which the origin of the power-lawtail can be understood as resulting from the growth of an initial spectrum ofdensity perturbations seeded along the long axis of filaments by interstellarturbulence. Here, we report the statistical properties of the line-massfluctuations of filaments in nearby molecular clouds observed with Herschelusing a 1-D power spectrum analysis. The observed filament power spectra werefitted by a power-law function $(P_{true}(s) \propto s^{\alpha})$ afterremoving the effect of beam convolution at small scales. A Gaussian-likedistribution of power-spectrum slopes was found centered at -1.6, close to thatof the one-dimensional velocity power spectrum generated by subsonicKolomogorov turbulence (-1.67). An empirical correlation, $P^{0.5}(s_0) \propto<N_{\rm H_2}>^{1.4 \pm 0.1} $, was also found between the amplitude of eachfilament power spectrum $P(s_0)$ and the mean column density along the filament$<N_{\rm H_2}>$. Finally, the dispersion of line-mass fluctuations along eachfilament $\sigma_{\rm M_{line}}$ was found to scale with the physical length$L$ of the filament, roughly as $\sigma_{M_{line}} \propto L^{0.7}$. Overall,our results are consistent with the suggestion that the bulk of the CMF/IMFresults from the gravitational fragmentation of filaments.

A possible link between the power spectrum of interstellar filaments and the origin of the prestellar core mass function