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

Ultraviolet (UV) galaxies have been selected from the  Galaxy Evolution Explorer  deep imaging survey. The presence of a far‐UV (FUV) drop‐out in their spectral energy distributions (SEDs) proved to be a very complete (83.3 per cent) but not very efficient (21.4 per cent) tool for identifying Lyman break galaxies (LBGs) at  z ∼ 1. In this paper, we explore the physical properties of these galaxies and how they contribute to the total star formation rate (SFR). We divide the LBG sample into two subclasses: red LBGs (RLBGs) detected at  λ= 24 μm  which are mainly luminous infrared (IR) galaxies (LIRGs) and blue LBGs (BLBGs) undetected at  λ= 24 μm  down to the MIPS/GTO limiting flux density of 83 μJy. Two of the RLBGs are also detected at 70 μm. The median SED of the RLBGs is similar (above  λ∼ 1 μm ) to that of a luminous dusty starburst at   z ∼ 1.44 , HR10. However, unlike local luminous and ultraluminous IR galaxies, RLBGs are UV bright objects. We suggest that these objects contain a large amount of dust but that some bare stellar populations are also directly visible. The median SED of the BLBGs is consistent with their containing the same stellar population as the RLBGs (i.e. a 250–500 Myr old, exponentially decaying star formation history) but with a lower dust content. The luminosity function (LF) of our LBG sample at   z ∼ 1  is similar to the LF of near‐UV (NUV) selected galaxies at the same redshift. The integrated luminosity densities of   z ∼ 1  LBGs and NUV‐selected galaxies are very consistent. Making use of the RLBG sample, we show that SFRs estimated from UV measurements and corrected using the IRX−β method provide average total SFR TOT  in agreement with the sum of the UV and IR contributions: SFR  UV + SFR  dust . However, IRX−β‐based SFR TOT  shows a large dispersion. Summing up the detected UV (1150‐Å rest‐frame) and IR‐based SFRs of the detected objects, we find that only one‐third of the total (i.e. UV + dust) LBG SFR resides in BLBGs and two‐thirds in RLBGs, even though most LBGs at  z ∼ 1 are BLBGs. On the other hand, the total SFR of LBGs accounts for only 11 per cent of the total SFR at   z ∼ 1 . Finally, we observe a regular decrease in the luminosity ratio  L  dust / L  FUV  from   z = 0  to   z ≈ 2  for UV‐selected samples.

Lyman break galaxies at z ∼ 1 and the evolution of dust attenuation in star‐forming galaxies with redshift