학술논문
Near-Infrared Observations of Outflows and YSOs in the Massive Star-Forming Region AFGL 5180
Document Type
Working Paper
Author
Crowe, S.; Fedriani, R.; Tan, J. C.; Whittle, M.; Zhang, Y.; Garatti, A. Caratti o; Farias, J. P.; Gautam, A.; Telkamp, Z.; Rothberg, B.; Grudic, M.; Andersen, M.; Cosentino, G.; Garcia-Lopez, R.; Rosero, V.; Tanaka, K.; Pinna, E.; Rossi, F.; Miller, D.; Agapito, G.; Plantet, C.; Ghose, E.; Christou, J.; Power, J.; Puglisi, A.; Briguglio, R.; Brusa, G.; Taylor, G.; Zhang, X.; Mazzoni, T.; Bonaglia, M.; Esposito, S.; Veillet, C.
Source
Subject
Language
Abstract
Methods: Broad- and narrow-band imaging of AFGL 5180 was made in the NIR with the LBT, in both seeing-limited ($\sim0.5\arcsec$) and high angular resolution ($\sim0.09\arcsec$) Adaptive Optics (AO) modes, as well as with HST. Archival ALMA continuum data was also utilized. Results: At least 40 jet knots were identified via NIR emission from H$_2$ and [FeII] tracing shocked gas. Bright jet knots outflowing from the central most massive protostar, S4, are detected towards the east of the source and are resolved in fine detail with the AO imaging. Additional knots are distributed throughout the field, likely indicating the presence of multiple driving sources. Sub-millimeter sources detected by ALMA are shown to be grouped in two main complexes, AFGL 5180 M and a small cluster $\sim15\arcsec$ to the south, AFGL 5180 S. From our NIR continuum images we identify YSO candidates down to masses of $\sim 0.1\:M_\odot$. Combined with the sub-mm sources, this yields a surface number density of such YSOs of $N_* \sim 10^3 {\rm pc}^{-2}$ within a projected radius of about 0.1 pc. Such a value is similar to those predicted by models of both Core Accretion from a turbulent clump environment and Competitive Accretion. The radial profile of $N_*$ is relatively flat on scales out to 0.2~pc, with only modest enhancement around the massive protostar inside 0.05~pc. Conclusions: This study demonstrates the utility of high-resolution NIR imaging, in particular with AO, for detecting outflow activity and YSOs in distant regions. The presented images reveal the complex morphology of outflow-shocked gas within the large-scale bipolar flow of a massive protostar, as well as clear evidence for several other outflow driving sources in the region. Finally, this work presents a novel approach to compare the observed YSO surface number density from our study against different models of massive star formation.
Comment: Accepted to Astronomy & Astrophysics (A&A)
Comment: Accepted to Astronomy & Astrophysics (A&A)