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VLA 1623$-$2417 is a triple protostellar system deeply embedded in OphiuchusA. Sources A and B have a separation of 1.1", making their study difficultbeyond the submillimeter regime. Lack of circumstellar gas emission suggestedthat VLA 1623$-$2417 B has a very cold envelope and is much younger than sourceA, generally considered the prototypical Class 0 source. We explore theconsequences of new ALMA Band 9 data on the spectral energy distribution (SED)of VLA 1623$-$2417 and their inferred nature. Using dust continuum observationsspanning from centimeter to near-infrared wavelengths, the SED of eachcomponent in VLA 1623$-$2417 is constructed and analysed. The ALMA Band 9 datapresented here show that the SED of VLA 1623$-$2417 B does not peak at 850$\mu$m as previously expected, but instead presents the same shape as VLA1623$-$2417 A at wavelengths shorter than 450 $\mu$m. The results presentedhere indicate that the previous assumption that the flux in $Herschel$ andSpitzer observations is solely dominated by VLA 1623$-$2417 A is not valid, andinstead, VLA 1623$-$2417 B most likely contributes a significant fraction ofthe flux at $\lambda~<$ 450 $\mu$m. These results, however, do not explain thelack of circumstellar gas emission and puzzling nature of VLA 1623$-$2417 B.

Revised SED of the triple protostellar system VLA 1623-2417