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 luminosity functions at z < 4 - 5 suggest that most galaxies have arelatively low stellar mass (logM_star = 10) and a low dust attenuation (A_FUV= 1.0). The physical properties of these objects are quite homogeneous. We usedan approach where we combined their rest-frame far-infrared and submillimeteremissions and utilized the universe and the redshift as a spectrograph toincrease the amount of information in a collective way. From a subsample of 27ALMA-detected galaxies at z > 4.5, we built an infrared spectral energydistribution composite template. It was used to fit, with CIGALE, the 105galaxies (detections and upper limits) in the sample from the FUV to the FIR.The derived physical parameters provide information to decipher the nature ofthe dust cycle and of the stellar populations in these galaxies. The derived IRcomposite template is consistent with the galaxies in the studied sample. Adelayed star formation history with tau_main = 500 Myrs is slightly favored bythe statistical analysis as compared to a delayed with a final burst or acontinuous star formation history. The position of the sample in the starformation rate (SFR)- M_star diagram is consistent with previous papers. Theredshift evolution of the log M_star versus A_FUV relation is in agreement withevolution in the redshift of this relation. This evolution is necessary toexplain the cosmic evolution of the average dust attenuation of galaxies.Evolution is also observed in the L_dust/ L_FUV (IRX) versus UV slope beta_FUVdiagram: younger galaxies have bluer beta_FUV. We modeled the shift of galaxiesin the IRX versus the beta_FUV diagram with the mass-weighted age as a freeparameter, and we provide an equation to make predictions.

IR characteristic emission and dust properties of star-forming galaxies at 4.5 $<$ z $<$ 6.2