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ABSTRACT  Optically very faint  ( R  &gt; 25.5)  sources detected by the  Spitzer Space Telescope  at 24 μm represent a very interesting population at redshift   z ∼ (1.5–3) . They exhibit strong clustering properties, implying that they are hosted by very massive haloes, and their mid‐infrared emission could be powered by either dust‐enshrouded star formation and/or by an obscured active galactic nucleus (AGN). We report observations carried out with the Max Planck Millimetre Bolometer (MAMBO) array at the IRAM 30‐m antenna on Pico Veleta of a candidate protocluster with five optically obscured sources selected from the 24‐μm  Spitzer  sample of the First‐Look Survey. Interestingly, these sources appear to lie on a high‐density filament aligned with the two radio jets of an AGN. Four out of five of the observed sources were detected. We combine these measurements with optical, infrared and radio observations to probe the nature of the candidate protocluster members. Our preliminary conclusions can be summarized as follows: the spectral energy distributions (SEDs) of all sources include both AGN and starburst contributions; the AGN contribution to the bolometric luminosities ranges between 14 and 26 per cent of the total. Such a contribution is enough for the AGN to dominate the emission at 5.8, 8 and 24 μm, while the stellar component, inferred from SED fitting, prevails at 1.25 mm and at  λ &lt; 4.5 μ m. The present analysis suggests a coherent interplay at high  z  between extended radio activity and the development of filamentary large‐scale structures.

MAMBO observations at 240 GHz of optically obscured Spitzer sources: source clumps and radio activity at high redshift