  VLA 1623$-$2417 is a triple protostellar system deeply embedded in Ophiuchus
A. Sources A and B have a separation of 1.1", making their study difficult
beyond the submillimeter regime. Lack of circumstellar gas emission suggested
that VLA 1623$-$2417 B has a very cold envelope and is much younger than source
A, generally considered the prototypical Class 0 source. We explore the
consequences of new ALMA Band 9 data on the spectral energy distribution (SED)
of VLA 1623$-$2417 and their inferred nature. Using dust continuum observations
spanning from centimeter to near-infrared wavelengths, the SED of each
component in VLA 1623$-$2417 is constructed and analysed. The ALMA Band 9 data
presented here show that the SED of VLA 1623$-$2417 B does not peak at 850
$\mu$m as previously expected, but instead presents the same shape as VLA
1623$-$2417 A at wavelengths shorter than 450 $\mu$m. The results presented
here indicate that the previous assumption that the flux in $Herschel$ and
Spitzer observations is solely dominated by VLA 1623$-$2417 A is not valid, and
instead, VLA 1623$-$2417 B most likely contributes a significant fraction of
the flux at $\lambda~<$ 450 $\mu$m. These results, however, do not explain the
lack of circumstellar gas emission and puzzling nature of VLA 1623$-$2417 B.
