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In anattempt to study whether the formation of brown dwarfs (BDs) takes place as a scaled‐down version of low‐mass stars, we conducted Institut de Radioastronomie Millimetrique (IRAM) 30 m/MAMBO‐II observations at 1.2 mm in a sample of 12 proto‐BD candidates selected from  Spitzer /IRAC data in the B213‐L1495 clouds in Taurus. Subsequent observations with the Caltech Submillimetre Observatory at 350 μm, Very Large Array at 3.6 and 6 cm, and IRAM 30 m/EMIR in the  12 CO (1–0),  13 CO (1–0) and N 2 H +  (1–0) transitions were carried out towards the two most promising  Spitzer /IRAC source(s), J042118 and J041757. J042118 is associated with a compact (&lt;10 arcsec or &lt;1400 au) and faint source at 350 μm, while J041757 is associated with a partially resolved (∼16 arcsec or ∼2000 au) and stronger source emitting at centimetre wavelengths with a flat spectral index. The corresponding masses of the dust condensations are ∼1 and 5  M  Jup  for J042118 and J041757, respectively. In addition, about 40 arcsec to the north‐east of J041757, we detect a strong and extended submillimetre source, J041757‐NE, which is not associated with near‐infrared/far‐infrared emission down to our detection limits, but is clearly detected in  13 CO and N 2 H +  at ∼7 km s −1 , and for which we estimated a total mass of ∼100  M  Jup , close to the mass required to be gravitationally bound. In summary, our observational strategy has allowed us to find in B213‐L1495 two proto‐BD candidates and one pre‐substellar core candidate, whose properties seem to be consistent with a scaled‐down version of low‐mass stars.

A search for pre‐substellar cores and proto‐brown dwarf candidates in Taurus: multiwavelength analysis in the B213‐L1495 clouds