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

The extragalactic background light at far-infrared wavelengths originatesfrom optically-faint, dusty, star-forming galaxies in the universe withstar-formation rates at the level of a few hundred solar masses per year. Dueto the relatively poor spatial resolution of far-infrared telescopes, the faintsub-millimetre galaxies are challenging to study individually. Instead, theiraverage properties can be studied using statistics such as the angular powerspectrum of the background intensity variations. A previous attempt atmeasuring this power spectrum resulted in the suggestion that the clusteringamplitude is below the level computed with a simple ansatz based on a halomodel. Here we report a clear detection of the excess clustering over thelinear prediction at arcminute angular scales in the power spectrum ofbrightness fluctuations at 250, 350, and 500 microns. From this excess, we findthat sub-millimetre galaxies are located in dark matter halos with a minimummass of log[M_min/M_sun ]= 11.5^+0.7_-0.2 at 350 microns. This minimum darkmatter halo mass corresponds to the most efficient mass scale for starformation in the universe, and is lower than that predicted by semi-analyticalmodels for galaxy formation.

Sub-millimetre galaxies reside in dark matter halos with masses greater than 3x10^11 solar masses