The VLA Orion A Large Survey (VOLS) large project will perform the deepest survey at subarcsecond resolution of the Orion A molecular cloud with the Karl G. Jansky Very Large Array (PI: G. Busquet, see https://vols.fqa.ub.edu). The superb sensitivity of the VLA combined with the large field of view of VOLS (~1 deg x 0.5 deg) requires a new strategy to identify regions of line emission. The VOLS project includes the emission lines of OH and CH3OH masers, 18 Hydrogen Radio Recombination lines and the line thermal emission of HC5N and SO molecules.
Astrophysics and Space Science
cOrion A is the nearest star-forming complex containing a broad range of environments populated by protostars and Young Stellar Objects (YSOs) with different masses and evolutionary stages, representing a testbed for star formation theories. The VLA Orion A Large Survey (VOLS, PI: G. Busquet; see https://vols.fqa.ub.edu) large project has been granted with 306 hours of observing time with the Karl G. Jansky Very Large Array to perform the deepest survey at subarcsecond resolution of the Orion A molecular cloud.
The formation process of stellar cluster requires a high degree of cloud fragmentation. Both simulations and observations show that cloud fragmentation leading to the formation of stellar cluster is controlled by a complex interaction of gravitational instability, turbulence, magnetic fields, cloud rotation, and stellar feedback. The infrared dark cloud G14.225-0.506 hosts two hubs harbouring two deeply embedded protoclusters.
The large-scale structure of the universe commonly refers to the distribution of galaxies at scales above 100Mpc, spanning across a wide range of redshifts, 0<z<3.
The quality of GaiaDR3 proper motions make them suitable for mapping for the first time the 3D velocity field of the Large Magellanic Cloud disc kinematics. These maps show a high degree of complexity and comparison with controlled N-body simulations becomes essential.
The gravitational interaction between the Large Magellanic Cloud (LMC) and the Small Magellanic Cloud is evident when GaiaDR3 reveals the shape of the Magellanic bridge in the young stellar evolutionary phase and the velocity flow also in older and evolved populations.
The radial and residual tangential velocity map in the Large Magellanic Cloud bar with GaiaDR3 data shows that the expected quadrupole pattern is asymmetric. We plan to analyse the cause of asymmetries using KRATOS simulations, a suite of 24 LMC-like N-body simulations.
Gamma-ray emitting binaries hosting a massive star are among the most efficient and powerful accelerators of the Galaxy. The closest vicinity of the binary is believed to be the region where electrons (and possibly protons and nuclei) are accelerated, reaching in some cases energies approaching 100 TeV. This implies that these sources are potential Pevatrons, in particular if protons and nuclei are also accelerated, as they are less affected by energy losses than electrons, close to the binary.