TY - JOUR
T1 - Characterising the multiple protostellar system VLA 1623-2417 with JWST, ALMA and VLA
T2 - outflow origins, dust growth and an unsettled disk
AU - Radley, Isaac C.
AU - Busquet, Gemma
AU - Ilee, John D.
AU - Liu, Hauyu Baobab
AU - Pineda, Jaime E.
AU - Pontoppidan, Klaus M.
AU - Macías, Enrique
AU - Maureira, María José
AU - Bianchi, Eleonora
AU - Bourke, Tyler L.
AU - Codella, Claudio
AU - Forbrich, Jan
AU - Girart, Josep M.
AU - Hoare, Melvin G.
AU - Garnica, Ricardo Hernández
AU - Jiménez-Serra, Izaskun
AU - Loinard, Laurent
AU - Ordóñez-Toro, Jazmín
AU - Podio, Linda
N1 - Accepted for publication in ApJ. 35 pages, 10 figures
PY - 2025/1/31
Y1 - 2025/1/31
N2 - Utilising JWST, ALMA and the VLA we present high angular resolution (0.06''- 0.42''), multi-wavelength (4 micron - 3cm) observations of the VLA 1623-2417 protostellar system to characterise the origin, morphology and, properties of the continuum emission. JWST observations at 4.4 micron reveal outflow cavities for VLA 1623 A and, for the first time, VLA 1623 B, as well as scattered light from the upper layers of the VLA 1623 W disk. We model the millimetre-centimetre spectral energy distributions to quantify the relative contributions of dust and ionised gas emission, calculate dust masses, and use spectral index maps to determine where optical depth hinders this analysis. In general, all objects appear to be optically thick down to ~90 GHz, show evidence for significant amounts (10's - 100's M_Earth) of large (>1 mm) dust grains, and are dominated by ionised gas emission for frequencies ~
AB - Utilising JWST, ALMA and the VLA we present high angular resolution (0.06''- 0.42''), multi-wavelength (4 micron - 3cm) observations of the VLA 1623-2417 protostellar system to characterise the origin, morphology and, properties of the continuum emission. JWST observations at 4.4 micron reveal outflow cavities for VLA 1623 A and, for the first time, VLA 1623 B, as well as scattered light from the upper layers of the VLA 1623 W disk. We model the millimetre-centimetre spectral energy distributions to quantify the relative contributions of dust and ionised gas emission, calculate dust masses, and use spectral index maps to determine where optical depth hinders this analysis. In general, all objects appear to be optically thick down to ~90 GHz, show evidence for significant amounts (10's - 100's M_Earth) of large (>1 mm) dust grains, and are dominated by ionised gas emission for frequencies ~
KW - astro-ph.SR
KW - astro-ph.EP
KW - astro-ph.GA
M3 - Article
SN - 0004-637X
JO - The Astrophysical Journal
JF - The Astrophysical Journal
ER -