Observational characteristics of dense cores with deeply embedded young protostars
arXiv:astro-ph/0511095 · doi:10.1002/asna.200510453
Abstract
Class 0 objects, which are thought to be the youngest protostars, are identified in terms of NIR or radio emission and/or the presence of molecular outflows. We present combined hydrodynamic and radiative transfer simulations of the collapse of a star-forming molecular core, which suggest two criteria for identifying dense cores with deeply embedded very young protostars that may not be observable in the NIR or radio with current telescopes. We find that cores with protostars are relatively warm (T>15K) with their SEDs peaking at wavelengths <170 micron, and they tend to appear circular.
Accepted in the 'Astronomical Notes' for the special issue with the proceedings of the "Ultra low-mass star formation and evolution" workshop
References in corpus (13)
- 2-D Radiative Transfer in Protostellar Envelopes: I. Effects of Geometry on Class I Sources
- Tracing the Mass during Low-Mass Star Formation. II. Modelling the Submillimeter Emission from Pre-Protostellar Cores
- The initial conditions of isolated star formation - VI. SCUBA mapping of prestellar cores
- Simulating star formation in molecular cloud cores I. The influence of low levels of turbulence on fragmentation and multiplicity
- A "Starless" Core that Isn't: Detection of a Source in the L1014 Dense Core with the Spitzer Space Telescope
- Tracing the Mass during Low-Mass Star Formation. III. Models of the Submillimeter Dust Continuum Emission from Class 0 Protostars
- The dust temperature distribution in prestellar cores
- Dust emissivity in the Submm/Mm: SCUBA and SIMBA observations of Barnard 68
- Monte Carlo Radiative Transfer in Embedded Prestellar Cores
- How to identify the youngest protostars
- Why do starless cores appear more flattened than protostellar cores?
- Monte Carlo radiative transfer in SPH density fields
- Radiative transfer models of non-spherical prestellar cores