Terahertz spectroscopy systems use far-infrared radiation to extract molecular spectral information in an otherwise inaccessible portion of the electromagnetic spectrum. Materials research is an essential component of modern terahertz systems: novel, higher-power terahertz sources rely heavily on new materials such as quantum cascade structures. At the same time, terahertz spectroscopy and imaging provide a powerful tool for the characterization of a broad range of materials, including semiconductors and biomolecules.

Materials for terahertz science and technology

http://ideaexchange.uakron.edu/cgi/viewcontent.cgi?article=1230&context=chemengin_ideas

Surface Hydration: Principles and Applications Toward Low-fouling/nonfouling Biomaterials

Circumstellar dust exists around several hundred main sequence stars. For the youngest stars, that dust could be a remnant of the protoplanetary disk. Mostly it is inferred to be continuously replenished through collisions between planetesimals in belts analogous to the Solar System’s asteroid and Kuiper belts, or in collisions between growing protoplanets. The evolution of a star’s debris disk is indicative of the evolution of its planetesimal belts and may be influenced by planet formation processes, which can continue throughout the first gigayear as the planetary system settles to a stable configuration and planets form at large radii. Evidence for that evolution comes from infrared photometry of large numbers of debris disks, providing snapshots of the dust present at different evolutionary phases, as well as from images of debris disk structure. This review describes the theoretical framework within which debris disk evolution takes place and shows how that framework has been constrained by observations.

/pdf/evolution-of-debris-disks-vyvr2x26xs.pdf

Evolution of Debris Disks

▪ Abstract Until the late 1990s the rich Hyades and the sparse UMa clusters were the only coeval, comoving concentrations of stars known within 60 pc of Earth. Both are hundreds of millions of years old. Then beginning in the late 1990s the TW Hydrae Association, the Tucana/Horologium Association, the β Pictoris Moving Group, and the AB Doradus Moving Group were identified within ∼60 pc of Earth, and the η Chamaeleontis cluster was found at 97 pc. These young groups (ages 8–50 Myr), along with other nearby, young stars, will enable imaging and spectroscopic studies of the origin and early evolution of planetary systems.

/pdf/young-stars-near-the-sun-2c3pw8b328.pdf

Young Stars Near the Sun

SCUBA-2 is an innovative 10000 pixel bolometer camera operating at submillimetre wavelengths on the James Clerk Maxwell Telescope (JCMT). The camera has the capability to carry out wide-field surveys to unprecedented depths, addressing key questions relating to the origins of galaxies, stars and planets. With two imaging arrays working simultaneously in the atmospheric windows at 450 and 850µm, the vast increase in pixel count means that SCUBA-2 maps the sky 100–150 times faster than the previous SCUBA instrument. In this paper we present an overview of the instrument, discuss the physical characteristics of the superconducting detector arrays, outline the observing modes and data acquisition, and present the early performance figures on the telescope. We also showcase the capabilities of the instrument via some early examples of the science SCUBA-2 has already undertaken. In February 2012, SCUBA-2 began a series of unique legacy surveys for the JCMT community. These surveys will take 2.5years and the results are already providing complementary data to the shorter wavelength, shallower, larger-area surveys from Herschel. The SCUBA-2 surveys will also provide a wealth of information for further study with new facilities such as ALMA, and future telescopes such as CCAT and SPICA.

/pdf/scuba-2-the-10-000-pixel-bolometer-camera-on-the-james-clerk-36o4hmtmbk.pdf

SCUBA-2: the 10 000 pixel bolometer camera on the James Clerk Maxwell Telescope

Indirect detections of massive — presumably Jupiter-like — planets orbiting nearby Sun-like stars have recently been reported1,2. Rocky, Earth-like planets are much more difficult to detect, but clues to their possible existence can nevertheless be obtained from observations of the circumstellar debris disks of dust from which they form. The presence of such disks has been inferred3 from excess far-infrared emission but, with the exception of beta Pictoris4, it has proved difficult to image these structures directly as starlight dominates the faint light scattered by the dust5. A more promising approach is to attempt to image the thermal emission from the dust grains at submillimetre wavelengths6,7. Here we present images of such emission around Fomalhaut, beta Pictoris and Vega. For each star, dust emission is detected from regions comparable in size to the Sun's Kuiper belt of comets. The total dust mass surrounding each star is only a few lunar masses, so any Earth-like planets present must already have formed. The presence of the central cavity, approximately the size of Neptune's orbit, that we detect in the emission from Fomalhaut may indeed be the signature of such planets.

Submillimetre images of dusty debris around nearby stars

We present spectroscopic data of 3 isolated Vega-type systems which exhibit the 3.3 μm‘PAH’ feature ascribed to stretching of the C-H bonds in aromatic hydrocarbons. These are part of a sample of mainly hot stars. We discuss the implications of Vega-type stars having an organic component to their surroundings and compare them with the unique star, HD135344 (SAO 206462).

The 3.3 micron PAH feature in Vega-type stars

New photometry of main-sequence debris discs has been carried out at 850 and 450/μm; the derived SEDs indicate that the dust can lie in either thin rings or radially-extended discs, as seen directly in the few nearby objects which are resolvable. All such objects are consistent with a long wavelength opacity index β of 1.0±0.2 - similar to T Tauri stars, but significantly lower than embedded objects.

/pdf/spectral-energy-distributions-and-structures-of-debris-discs-10nw2id2ff.pdf

Spectral energy distributions and structures of debris discs

Further observations of the submillimetre CO lines in 3 Vega-type stars are reported and interpreted for the gas temperatures they imply. Very low gas temperatures (∽15K) are deduced for all three stars, consolidating the suggestion that, if the gas and dust are remnants of the molecular cloud from which the star system formed, then much of the CO in these systems may be locked up in ices on the surfaces of dust grains.

/pdf/gas-temperatures-in-vega-type-stars-34e099fjhq.pdf

D. Walther

Papers

Submillimetre images of dusty debris around nearby stars

The 3.3 micron PAH feature in Vega-type stars

Spectral energy distributions and structures of debris discs

Gas temperatures in Vega-type stars