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 present a range of new observations of the ‘broad absorption‐line radio galaxy’ 4C +72.26  ( z ≈ 3.5) , including sensitive rest‐frame ultraviolet integral field spectroscopy using the Gemini/GMOS‐N instrument and Subaru/CISCO  K ‐band imaging and spectroscopy. We show that 4C +72.26 is a system of two vigorously star‐forming galaxies superimposed along the line of sight separated by  ∼1300 ± 200 km s −1   in velocity, with each demonstrating spectroscopically resolved absorption lines. The most active star‐forming galaxy also hosts the accreting supermassive black hole which powers the extended radio source. We conclude that the star formation is unlikely to have been induced by a shock caused by the passage of the radio jet, and instead propose that a collision is a more probable trigger for the star formation. Despite the massive starburst, the ultraviolet‐mid‐infrared spectral energy distribution suggests that the pre‐existing stellar population comprises  ∼10 12  M ⊙   of stellar mass, with the current burst only contributing a further ∼2 per cent, suggesting that 4C +72.26 has already assembled most of its final stellar mass.

When galaxies collide: understanding the broad absorption‐line radio galaxy 4C +72.26