![]() ![]() ![]() VLASS will be able to detect ultracool dwarfs to 10–20 pc, active dwarf stars to a few tens of parsecs, and active binaries to slightly less than 2 kpc. By applying a series of “filters” such as spectral index, polarization and compactness, the large number of sources detected in VLASS can be reduced to a feasible number on which to conduct a periodicity search using single dish telescopes.Ĭoronal Magnetic Activity on Cool Stars: The radio emission from nearby active stars provides a unique probe of accelerated particles and magnetic fields that occur in them, which is useful for a broader understanding of dynamo processes in stars, as well as the particle environment around those stars. ![]() Further, there has been a host of surveys of the Galaxy at wavelengths that do penetrate deep into the Galaxy, from the infrared to γ -ray (e.g., with Spitzer, Herschel, Chandra, XMM-Newton, and Fermi ) that VLASS will complement, allowing for a rich multiwavelength characterization of sources detected. The following three topics will be further illuminated by the Galactic coverage afforded by the VLASS.Ĭompact Objects: The 2–4 GHz frequency of VLASS makes it especially sensitive to rare pulsar systems that are likely to be at low Galactic latitudes close to the Galactic Plane, and therefore have their emission highly scattered (e.g., PSR-BH binaries). eXtra-Large Proposals Expressions of InterestĪt visible wavelengths, dust obscuration and absorption e ff ects can be significant toward the Galactic plane, but these e ff ects are not problematic at radio wavelengths, and there is a rich history of using radio observations to find objects deep within the Galaxy (see Helfand et al. ![]()
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