This online workshop aims to define the major science topics in Infrared/Submm astronomy for the next decade from a European perspective. Solar system to distant galaxies, continuum and spectroscopy observations from airborne platforms will be discussed.
Historically, the IGM motivated the search for FUV background which in turn led to a number of experiments and missions. Decades later the focus shifted to FUV as the primary heating and ionizing agent of the atomic phases (warm and cold neutral medium). The current view is that the diffuse FUV emission, at high latitudes, has three components: FUV light from hot stars in the Galactic plane reflected by dust grains (diffuse galactic light or DGL), FUV from other galaxies (extra-galactic background light, EBL) and a component of unknown origin.
Attendees of the upcoming 53rd Annual DPS Meeting will be able to attend the webinar: 'SOFIA: data and resources for planetary science', hosted at the USRA booth. The Stratospheric Observatory for Infrared Astronomy - SOFIA - is the only facility which can access the 5 - 600 microns wavelength range at a variety of spectral resolutions. Well suited to target thermal emission from Solar System bodies, SOFIA already observed a variety of asteroids, moons and planets.
As part of a cycle 7 SOFIA Legacy Program, we obtained imaging observations of some of the brightest infrared portions of the inner ~200 pc of our Galaxy at 25 and 37 microns. These data have provided new insights into some of the most complex regions within our galaxy, and specifically this talk will focus on the Sgr A region where the observations allow us to examine possible signs of nuclear activity.
Carbon stars dominate the observed production of dust in nearby metal-poor dwarf galaxies. To understand the chemical enrichment history and dust budgets of those galaxies, we must understandn the carbon stars. Infrared spectra from the Spitzer Space Telescope have shown that carbon stars form and dredge up enough of their own carbon to produce significant amounts of dust, no matter their initial metallicity.
At present epochs, stars dominate the baryonic mass of Galaxies, but at early ages the gas which fuels both star formation and AGN accretion must have been dominant. We have used ALMA archive data in the COSMOS 2-deg^2 field to measure the gas masses for samples of 700 and 10,000 galaxies at redshift 0.1 to 6, corresponding to a span of 12 Gyr. The range of measured gas masses is 10^9 - few x 10^11 solar masses -- the latter being ~ 100x that in the Milky Way.
Magnetic fields thread our Milky Way Galaxy, influencing interstellar physics from cosmic ray propagation to star formation. The magnetic interstellar medium is also a formidable foreground for experimental cosmology, particularly for the quest to find signatures of inflation in the polarized cosmic microwave background (CMB). Despite its importance across scientific realms, the structure of the Galactic magnetic field is not well understood.