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 Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

We provide the most accurate estimate yet of the bright end of the infrared(IR) luminosity functions (LFs) and the abundance of hyperluminous IR galaxies(HLIRGs) with IR luminosities > 10^13 L_solar, thanks to the combination of thehigh sensitivity, angular resolution, and large area of the LOFAR Deep Fields,which probes an unprecedented dynamic range of luminosity and volume. Wecross-match Herschel sources and LOFAR sources in Bootes (8.63 deg^2), LockmanHole (10.28 deg^2), and ELAIS-N1 (6.74 deg^2) with rms sensitivities of around32, 22, and 20 mJy per beam, respectively. We divide the matched samples intounique and multiple categories. For the multiple matches, we de-blend theHerschel fluxes using the LOFAR positions and the 150-MHz flux densities aspriors. We perform spectral energy distribution (SED) fitting, combined withmulti-wavelength counterpart identifications and photometric redshiftestimates, to derive IR luminosities. The depth of the LOFAR data allows us toidentify highly complete (around 92% completeness) samples of bright Herschelsources with a simple selection based on the 250 micron flux density (45, 40,and 35 mJy in Bootes, Lockman Hole, and ELAIS-N1, respectively). Most of thebright Herschel sources fall into the unique category (i.e. a single LOFARcounterpart). For the multiple matches, there is excellent correspondencebetween the radio emission and the far-IR emission. We find a good agreement inthe IR LFs with a previous study out to z around 6 which used de-blendedHerschel data. Our sample gives the strongest and cleanest indication to datethat the population of HLIRGs has surface densities of around 5 to 18 / deg^2(with variations due to a combination of the applied flux limit and cosmicvariance) and an uncertainty of a factor of 2. In comparison, the GALFORMsemi-analytic model significantly under-predicts the abundance of HLIRGs.

The bright end of the infrared luminosity functions and the abundance of hyperluminous infrared galaxies