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

We discuss the results of the relationships between the K-band and stellarmass, far-infrared luminosities, star formation rate, dust and gas masses ofnearby galaxies computing the bivariate K-band Luminosity Function (BLF) andbivariate K-band Mass Function (BMF) of the Herschel Reference Survey (HRS), avolume-limited sample with full wavelength coverage. We derive the BLFs andBMFs from the K-band and stellar mass, far-infrared luminosities, starformation rate, dust and gas masses cumulative distributions using a copulamethod which is outlined in detail. The use of the bivariate computed takinginto account the upper limits allows us to derive on a more solid statisticalground the relationship between the observed physical quantities. The analysisshows that the behaviour of the morphological (optically selected) subsamplesis quite different. A statistically meaningful result can be obtained over thewhole HRS sample only from the relationship between the K-band and the stellarmass, while for the remaining physical quantities (dust and gas masses, far-IRluminosity and star formation rate), the analysis is distinct for late-type(LT) and early-type galaxies (ETG). However, the number of ETGs is small toperform a robust statistical analysis, and in most of the case results arediscussed only for the LTG subsample. The Luminosity and Mass Functions (LFs,MFs) of LTGs are generally dependent on the K-band and the various dependenciesare discussed in detail. We are able to derive the corresponding LFs and MFsand compare them with those computed with other samples. Our statisticalanalysis allows us to characterise the HRS, that, although non homogeneouslyselected and partially biased towards low IR luminosities, may be considered asrepresentative of the local LT galaxy population.

The bivariate luminosity and mass functions of the local HRS galaxy sample. The stellar, dust, gas mass functions