Revised SED of the triple protostellar system VLA 1623-2417
Nadia M. Murillo, Daniel Harsono, Melissa McClure, Shih-Ping Lai and, Michiel R. Hogerheijde

TL;DR
This study uses new ALMA Band 9 data to revise the spectral energy distribution of the triple protostellar system VLA 1623-2417, revealing that the secondary component B is more similar to A at shorter wavelengths than previously thought.
Contribution
The paper provides a revised analysis of the SED of VLA 1623-2417 using high-frequency ALMA data, challenging previous assumptions about the flux contributions of its components.
Findings
VLA 1623-2417 B's SED peaks at shorter wavelengths than previously thought.
Component B likely contributes significantly to flux at wavelengths below 450 μm.
The nature of VLA 1623-2417 B remains puzzling due to lack of circumstellar gas emission.
Abstract
VLA 16232417 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 16232417 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 16232417 and their inferred nature. Using dust continuum observations spanning from centimeter to near-infrared wavelengths, the SED of each component in VLA 16232417 is constructed and analysed. The ALMA Band 9 data presented here show that the SED of VLA 16232417 B does not peak at 850 m as previously expected, but instead presents the same shape as VLA 16232417 A at wavelengths shorter than 450 m. The…
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