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This paper proposes a dual-parameter strain/displacement safety monitoring technology for railway tunnel lining structures. An integrated monitoring system with FBG (Fiber Bragg grating) and VDM (video displacement meter) components was used to monitor both the strain and deformation of the tunnel cross-section. Initially, a comprehensive experimental study was carried out using FBG strain sensors with temperature-compensated grating. The temperature-compensated grating was used to further improve the monitoring accuracy. The data show that the stability and accuracy were better than the traditional electronic strain sensor. Secondly, high-precision and multipoint monitoring of railway tunnel lining deformation was achieved by using VDM technology. Three months of case study results taken from the Gansu Railway Tunnel in China demonstrated a tunnel cross-section strain accuracy for microstrain and crown deformation at the submillimeter level, respectively. The technology provides a new high-precision way to monitor the condition of tunnel lining structures. [ABSTRACT FROM AUTHOR]

In this paper, a submillimetric/THz metasurface polarization/oblique independent absorber is designed and characterized. The absorber is designed using a periodic arrangement of a modified split ring resonator unit cell. The symmetric absorber is insensitive to the variation of incident angles and polarization angles. The results confirm that perfect absorption is achieved (close to 100%) for either TM or TE polarization at 300 GHz. Moreover, the absorber is efficient for normal and oblique incident angle (above 90% for 45° angle of incidence). In all the presented cases, the full width half maximum bandwidth is 20 GHz. The absorber unit cell size is only 0.0052 λ0 × 0.0052 λ0 and it has a low-profile thickness = 0.0002 λ0, at the operating frequency. Also, an absorber-based biosensor is presented. The sensing has proved the coating analyte thickness can be detected by shifting the absorption frequency. The maximum sensitivity is 24.9% RIU−1 with a low-profile maximum of 50 µm thickness. Analytical formulas for the frequency shift have been extracted. The presented results are discussed based on 3D full-wave EM simulations. [ABSTRACT FROM AUTHOR]

Spaceborne passive submillimeter instruments can provide higher sensitivity to a broader size range of ice hydrometeors than traditional millimeter and infrared observations. However, a plane‐parallel cloud assumption is commonly applied for simplicity in passive cloud retrieval algorithms, while observations from active instruments have already demonstrated the ice particle variabilities in the vertical dimension. This study is conducted to assess the impacts of ice cloud vertical inhomogeneity on passive submillimeter‐wave simulations. Specifically, a simplified two‐layer scheme for distributions of particle size and ice water content in ice clouds is utilized to explore the inhomogeneous effects on radiative‐transfer process via the brightness temperature differences at the top of the atmosphere. Then the effect is quantitively evaluated based on a generated synthetic ice cloud and compared under the assumption of five particle size distributions to simulate homogeneous and heterogeneous clouds. The simplified two‐layer model simulations show that before saturation, the upper layer generates a stronger brightness temperature depression due to scattering than does the lower layer, given the same ice water content (IWC). However, with increasing IWC or effective diameters, the saturation effect would lead to the opposite impact, especially for high‐frequency channels. The generated synthetic ice cloud simulations reveal that the average values and the root‐mean‐squared errors of the brightness temperature differences are between −6 and 8 K and within 10 K, respectively. The results in this study are of special significance for remote‐sensing ice hydrometeors from passive submillimeter observations for the upcoming Ice Cloud Imager (ICI), as well as for future assimilations of submillimeter radiances in all‐sky conditions. [ABSTRACT FROM AUTHOR]

Evolved stars on the asymptotic giant branch and red supergiants have multiple processes that can be studied in the (sub)mm, including stellar surfaces, circumstellar thermal gas and dust, and masers. Telescopes such as APEX and ALMA have opened the possibility to perform studies that are revealing new information on these, as well as on the role of binaries in shaping stellar winds and the evolution to planetary nebulae. Here, we discuss some recent results for (sub)mm observations towards evolved stars focusing particularly on masers. This includes SiO and water masers, as well as ALMA high angular resolution observations of HCN masers towards a carbon-rich star. [ABSTRACT FROM AUTHOR]

The presence of phosphine (PH3) in the atmosphere of Venus was reported by Greaves et al. (2021, https://doi.org/10.1038/s41550-020-1174-4), based on observations of the J = 1–0 transition at 267 GHz using ground‐based, millimeter‐wave spectroscopy. This unexpected discovery presents a challenge for our understanding of Venus's atmosphere, and has led to a reappraisal of the possible sources and sinks of atmospheric phosphorous‐bearing gases. Here we present results from a search for PH3 on Venus using the German REceiver for Astronomy at Terahertz Frequencies instrument aboard the Stratospheric Observatory for Infrared Astronomy aircraft, over three flights conducted in November 2021. Multiple PH3 transitions were targeted at frequencies centered on 533 and 1,067 GHz, but no evidence for atmospheric PH3 was detected. Through radiative transfer modeling, we derived a disk‐averaged upper limit on the PH3 abundance of 0.8 ppb in the altitude range 75–110 km, which is more stringent than previous ground‐based studies. Plain Language Summary: We performed observations using a unique, flying telescope—the Stratospheric Observatory for Infrared Astronomy—to search for a gas called phosphine (PH3) in the atmosphere of Venus, which has been suggested to be an indicator for life. Our observations showed no evidence of PH3, in contrast to the original claim, and we provide a stringent upper limit on its abundance. Two other recent studies using different telescopes also found no evidence for PH3 on Venus, in agreement with our present result. Key Points: A recent detection of phosphine (PH3) (a possible biomarker) on Venus at millimeter wavelengths has been called into question by subsequent workWe performed far‐infrared spectroscopic observations of Venus using the German REceiver for Astronomy at Terahertz Frequencies instrument onboard the Stratospheric Observatory for Infrared Astronomy aircraftPH3 was not detected, and a strict upper limit on its atmospheric abundance of 0.8 ppb was derived between 75 and 110 km [ABSTRACT FROM AUTHOR]

Cosmological and astrophysical surveys in various wavebands, in particular from the radio to the far-infrared, offer a unique view of the universe's properties and the formation and evolution of its structures. After a preamble on the so-called tension problem, which occurs when different types of data are used to determine cosmological parameters, we discuss the role of fast radio bursts in cosmology, in particular for the missing baryon problem, and the perspectives from the analysis of the 21 cm redshifted line from neutral hydrogen. We then describe the Planck Legacy Archive, its wealth of scientific information and next developments, and the promising perspectives expected from higher resolution observations, in particular for the analysis of the thermal Sunyaev–Zel'dovich effect. Three cosmological results of the Planck mission are presented next: the implications of the map of Comptonization fluctuations, the dipole analysis from cross-correlating cosmic microwave background anisotropy and Comptonization fluctuation maps, and the constraints on the primordial tensor-to-scalar perturbation ratio. Finally, we discuss some future perspectives and alternative scenarios in cosmology, such as the study of the Lorentz invariance violation with the cosmic microwave background polarization, the introduction of new gravitational degrees of freedom to solve the dark matter problem, and the exploitation of the magnification bias with high-redshift sub-millimeter galaxies to constrain cosmological parameters. [ABSTRACT FROM AUTHOR]

The gas electron multiplier (GEM) detector in combination with a solid converter has been widely used in the field of neutron detection in recent decades. Typically, the submillimeter is an important indicator for neutron detectors to satisfy many applications requiring a high spatial resolution. This article proposes a novel method to improve the spatial resolution of ceramic GEM detectors by adding a stopping layer on top of the solid 10B4C neutron converter. This will restrict the emission of the secondary ion products of large angles and consequently improve the spatial resolution. The Monte Carlo program FLUKA is used to validate the method, and the verification experiments are carried out at beam line #20 (BL20) of the China Spallation Neutron Source (CSNS). The experimental results are approximately in agreement with the simulations. The measured spatial resolution is 1.87 mm for the GEM neutron detector operated at ambient pressure with a 1 $\mu \text{m}$ -thick 10B4C converter and a drift gap of 4 mm, eventually, it is improved to ~0.8 mm by coating a 3 $\mu \text{m}$ -thick titanium on top of the 10B4C converter. [ABSTRACT FROM AUTHOR]

Background High-resolution ultrasound (HRUS) and magnetic resonance neurography (MRN) are considered complementary to clinical and neurophysiological assessment for neuropathies. Aims The aim of our study was to compare the accuracy of HRUS and MRN for detecting various peripheral nerve pathologies, to choose the correct investigation to facilitate prompt patient management. Materials and Methods This prospective study was done using HRUS with 14 MHz linear-transducer and 3 or 1.5T MR in cases referred for the assessment of peripheral nerve pathologies. Image interpretation was done using a scoring system (score 0–3 confidence level) to assess for nerve continuity/discontinuity, increased nerve signal/edema, fascicular change, caliber change, and neuroma/mass lesion. We determined the accuracy, sensitivity, and specificity of these modalities compared with the diagnostic standard determined by surgical and/or histopathological, if not performed then clinical and/or electrodiagnostic evaluation. Results The overall accuracy of MRN was 89.3% (specificity: 66.6%, sensitivity: 92.6%, negative predictive value [NPV]: 57.1%, positive predictive value [PPV]: 95%) and that of HRUS was 82.9% (specificity: 100%, sensitivity: 80.4%, NPV: 42.8, PPV: 100). The confidence level for detecting nerve discontinuity and change in nerve caliber was found to be higher on ultrasonography than magnetic resonance imaging (MRI) (100 vs. 70% and 100 vs. 50%, respectively). Pathology of submillimeter caliber nerves was accurately detected by HRUS and these could not be well-visualized on MRI. Conclusion HRUS is a powerful tool that may be used as the first-line imaging modality for the evaluation of peripheral nerve pathologies, and a better means of evaluation of peripheral nerves with submillimeter caliber. [ABSTRACT FROM AUTHOR]

Properties of galaxies, such as color, age, and star formation activity, appear to be associated with the environment in which they are immersed. To investigate how the environment‐galaxy relation is established, we study protoclusters, which are numerically dense environments of galaxies in the early Universe, and which give rise to galaxy clusters today. In this work, we use submillimeter galaxies (SMGs) ‐ which are very dusty and distant galaxies, with their copious infrared emission redshifted to the submillimeter wavelengths ‐ as lampposts to trace potential sites of protocluster regions. We undertook deep observations of the environment of SMGs with well‐established spectroscopic redshifts in the range of z ≃ 1–5. We made a combination of deep imaging and spectroscopic observations to identify Lyman‐alpha emitters (LAEs) as a means to assess the more typical star‐forming galaxies in these regions. We identified more than 300 LAE candidates in four potential protocluster regions. Of these, 200 have already been spectroscopically confirmed to be at the SMG redshifts. This is consistent with them being part of the same structure. By probing the redshift range z ≃ 1–5, which corresponds to ≥4 Giga years, we seek insights on the evolution of protoclusters over this time interval. [ABSTRACT FROM AUTHOR]

We present new constraints on the cosmic cold molecular gas evolution out to redshift 6 based on systematic mining of the public ALMA archive in the COSMOS field (A3 COSMOS). Our A3 COSMOS dataset contains ∼ 700 galaxies (0.3 ≲ z ≲ 6) with high-confidence ALMA detection and multi-wavelength SEDs. Combining with ∼ 1,200 CO-observed galaxies at 0 ≲ z ≲ 4 (75% at z < 0.1) in the literature, we parameterize galaxies' molecular gas depletion time and gas fraction each as a function of stellar mass, offset from the star-forming main-sequence and cosmic age. We propose a new functional form which provides a better fit and implies a "downsizing" effect and "mass-quenching". By adopting galaxy stellar mass functions and applying our gas fraction function, we obtain a cosmic cold molecular gas density evolution in agreement with recent CO blind field surveys as well as semi-analytic modeling. These together provide us a coherent picture of galaxy cold molecular gas, SFR and stellar mass evolution. [ABSTRACT FROM AUTHOR]

The spatial distribution of the dust and stars contains crucial information about the evolutionary pathways of galaxies. We present results of our study combing high-resolution ALMA and HST observations of z ∼ 2 bright sub-millimeter galaxies (SMGs). We have developed a two-dimensional extinction and age correction technique to obtain accurate stellar mass distributions from HST/CANDELS. For the first time, we can directly compare the spatial distribution of assembled stellar mass and ongoing star formation on kpc scales for distant SMGs, shedding light on their highly debated formation mechanisms. We find that the dust distribution is more compact than the stellar component, regardless if the SMG lies on the main sequence or at the starburst regime. Taking the dust emission as a proxy for dust-obscured star formation, our results imply that high-redshift SMGs are experiencing centrally enhanced star formation. These findings suggests that major galaxy interactions are not necessarily the main formation channel for SMGs with secular disk formation remaining a viable option as suggested by state-of-the-art cosmological simulations. The sizes and stellar densities of our z ∼ 2 SMGs agree well with the most compact early-type galaxies in the local Universe, strongly supporting the idea that the latter systems are indeed the descendants of massive SMGs at z ∼ 2. [ABSTRACT FROM AUTHOR]

Micro-Spec is a direct-detection spectrometer which integrates all the components of a diffraction-grating spectrometer onto a ≈ 10 -cm2 chip through the use of superconducting microstrip transmission lines on a single-crystal silicon substrate. The second generation of Micro-Spec is being designed to operate with a spectral resolution of at least 512 in the far-infrared and submillimeter (420–540 GHz, 714–555 μm) wavelength range, a band of interest for NASA's experiment for cryogenic large-aperture intensity mapping called EXCLAIM. EXCLAIM will be a balloon-borne telescope that is being designed to map the emission of redshifted carbon monoxide and singly-ionized carbon lines over a redshift range 0 < z < 3.5 and it will be the first demonstration of the Micro-Spec technology in a space-like environment. This work reviews the status of the Micro-Spec design for the EXCLAIM telescope, with emphasis on the spectrometer's two-dimensional diffractive region, through which light of different wavelengths is focused on kinetic inductance detectors along the instrument focal plane. An optimization process is used to generate a geometrical configuration of the diffractive region that satisfies specific requirements on size, operating spectral range and performance. An initial optical design optimized for EXCLAIM is presented in terms of geometric layout, spectral purity and efficiency. • Micro-Spec is a far-infrared spectrometer on a chip the size of a credit card. • High spectral purity is attained by using 3 stigmatic points on its focal plane. • Micro-Spec is designed to achieve a resolution of 512 and near-unity efficiency. • Multiple Micro-Spec modules coupled together enable multi-object spectroscopy. • Micro-Spec will be tested in a space-like environment on balloon-borne missions. [ABSTRACT FROM AUTHOR]

Powerful AGN have been detected up to very high redshifts (z ∼ 6–8), well within the Epoch of Reionization (EoR), but the lack of powerful radio-galaxies among such sources strongly disagrees with the expectations based on the known radio population up to z ∼ 5. Our group has been pursuing a detailed analysis of the faintest population of radio sources detected in the deepest fields searching for clues of these first radio galaxies. This paper describes our strategy and presents a highly confident candidate. The results, once follow-up of all candidates is completed, will have significant implications for the upcoming generation of all-sky deep radio surveys such as ASKAP-EMU, Westerbork-WODAN, and SKA itself. [ABSTRACT FROM AUTHOR]

We present 0.″2–0.″4 resolution ALMA images of the submillimeter dust continuum and the CO, H2O, and H2O+ line emission in a z = 3.63 strongly lensed dusty starburst. We construct the lens model for the system with an MCMC technique. While the average magnification for the dust continuum is about 11, the magnification of the line emission varies from 5 to 22 across the source, resolving the source down to sub-kpc scales. The ISM content reveals that it is a pre-coalescence major merger of two ultra-luminous infrared galaxies, both with a large amount of molecular gas reservoir. The approaching galaxy in the south shows no apparent kinematic structure with a half-light radius of 0.4 kpc, while the preceding one resembles a 1.2 kpc rotating disk, separated by a projected distance of 1.3 kpc. The distribution of dust and gas emission suggests a large amount of cold ISM concentrated in the interacting region. [ABSTRACT FROM AUTHOR]

Aminoacetonitrile (NH 2 CH 2 CN) was detected in the interstellar medium (ISM) one decade ago in the course of a spectral survey of the hot molecular core Sagittarius (Sgr) B2(N) with the IRAM 30 m telescope. With the advent of sensitive telescopes such as the Atacama Large Millimeter/submillimeter Array (ALMA), the degree of chemical complexity in the ISM can be further explored. In the family of aminoacetonitrile, the next stage in complexity with one additional CH 2 group is aminopropionitrile. This molecule has two structural isomers, a chain-like (3-aminopropionitrile, NH 2 CH 2 CH 2 CN) and a branched, chiral one (2-aminopropionitrile, CH 3 CH(NH 2 ) CN). The latter was studied in the laboratory a few years ago and was not detected in the IRAM 30 m survey. We present the search for both isomers in the EMoCA (Exploring Molecular Complexity with ALMA) survey, a sensitive spectral survey of Sgr B2(N) performed with ALMA. The rotational spectrum of 3-aminopropionitrile has been recorded in laboratory with a submillimeter spectrometer using solid-state sources. Helped by ab initio calculations performed for the different possible conformations, we present here the analysis based on a Watson Hamiltonian for an asymmetric one-top rotor in A-reduction performed in the frequency range 150–500 GHz for two conformers. More than 6200 lines of the ground-state and lowest excited vibrational states, corresponding to more than 8200 transitions, were assigned in the experimental spectrum. Partition functions, including the vibrational contribution of these states, and predictions in the JPL-CDMS catalog format were determined in order to search for both conformers of 3-aminopropionitrile in Sgr B2(N). Neither 3-aminopropionitrile, nor 2-aminopropionitrile are detected. The derived upper limits imply that they are at least 12 and 5 times less abundant than aminoacetonitrile, respectively. A comparison to ethyl cyanide and n-propyl cyanide detected in this source suggests that an improvement by a factor three in sensitivity may be sufficient to detect 3-aminopropionitrile, which should be within the range of our on-going follow-up project with ALMA. [ABSTRACT FROM AUTHOR]

Recent studies of the nearest star-forming clouds of the Galaxy at submillimeter wavelengths with the Herschel Space Observatory have provided us with unprecedented images of the initial conditions and early phases of the star formation process. The Herschel images reveal an intricate network of filamentary structure in every interstellar cloud. These filaments all exhibit remarkably similar widths – about a tenth of a parsec – but only the densest ones contain prestellar cores, the seeds of future stars. The Herschel results favor a scenario in which interstellar filaments and prestellar cores represent two key steps in the star formation process: first turbulence stirs up the gas, giving rise to a universal web-like structure in the interstellar medium, then gravity takes over and controls the further fragmentation of filaments into prestellar cores and ultimately protostars. This scenario provides new insight into the origin of stellar masses and the star formation efficiency in the dense molecular gas of galaxies. Despite an apparent complexity, global star formation may be governed by relatively simple universal laws from filament to galactic scales. [ABSTRACT FROM AUTHOR]

Testing of an 874 GHz submillimeter radiometer on meteorological satellites is being planned to improve ice water content retrievals. In this paper we study the optical properties of ice cloud particles in the 874 GHz band. The results show that the bulk scattering and absorption coefficients of an ensemble of ice cloud particles are sensitive to the particle shape and effective diameter, whereas the latter is also sensitive to temperature. The co-polar back scattering cross-section is not sensitive to particle shape, temperature, and the effective diameter in the range of 50–200 μm. [ABSTRACT FROM AUTHOR]

The pure rotational spectrum of mono-deuterated ethane, CH 3 CH 2 D, has been measured up to 1600 GHz and spectroscopic constants have been fit to 984 transitions in the ground state and 422 transitions in the first torsional excited state ( ν 18 ). Analyses of the ground state data were performed with the programs SPFIT, ERHAM and XIAM and of the first torsional state with SPFIT and ERHAM to extract molecular and spectroscopic constants. A combined fit of both states using ERHAM was used to determine ρ = 0.4344026(68), which in the symmetric limit is the ratio Iα/Iz and a measure of the periodicity of the internal rotation energy with K and the energy differences between the A and E torsional substates, Δ E ( E – A ), of 74.167(18) and −3382.23(34) MHz for the ground and excited states, respectively. Using these energy differences and the overtone transitions Δ v = 2 from Raman measurements in the literature, the coefficients V 3 and V 6 of the potential function of the internal rotation in CH 3 CH 2 D were determined as V 3 = 1004.56(4) cm −1 and V 6 = 7.09(12) cm −1 . This analysis lays the ground work for the assignment of the IR spectrum of CH 3 CH 2 D between (680–880 cm −1 ) which will help quantify isotopic ratios by remote sensing missions. [ABSTRACT FROM AUTHOR]

Out-of-field stray-light spots of the Herschel telescope optics relative to the PACS and SPIRE instrument apertures were modeled by ray tracing simulations with the Advanced Systems Analysis Program (ASAP, by Breault Research Organization) prior to launch. The predicted stray-light behaviour was verified by dedicated stray-light calibration observations in-flight. This resulted in a special feature of the Herschel Science Mission Planning Software, marking the sky positions of stray-light spots by the very bright infrared planetary sources Venus, Mars, Jupiter, and Saturn, as well as the Moon, thus avoiding contamination of scientific photometric observations by out-of-field stray-light of these sources. [ABSTRACT FROM AUTHOR]

Highlights: [•] High resolution measurements of the simplest Criegee intermediate up to 1THz. [•] Accurate distortion constants fitted from assignments up to J max =49 and =14. [•] Improved molecular parameters for prediction of the spectrum up to 2THz. [Copyright &y& Elsevier]

Highlights: [•] We model the fundamental limits of detection in the 0.1–10THz range. [•] We target the detection of high redshift dusty galaxies as a specific case. [•] We include noise from atmospheric, extraterrestrial and optical emissions. [•] We model various ground based, airborne and space based systems. [•] Large-aperture and cryogenic balloon-borne telescopes are also explored. [Copyright &y& Elsevier]

PILOT is a balloon-borne experiment designed to perform large-scale surveys of the polarized interstellar emission in the submillimeter. It is based on the use of an off-axis Gregorian type telescope, with a 1 m diameter primary mirror, and a large focal plane equipped with detectors arrays providing a $\sim 1\circ\times 1\circ$ field of view. All optical elements except the primary mirror are located inside a large liquid He cryostat, cooled down to 3 K. Strong constraints are then imposed on the alignment between the primary mirror and the cold optics. The characterization and optimization of the optical system performances are critical to the success of the mission. In this paper, we present the modelling and measurements performed on the primary mirror for this purpose. The optical and mechanical parameters of the as-built primary mirror have been determined using a method based on 3D measurements of the mirror surface. The deformations expected under flight conditions due to temperature variations and flexion under gravity have been estimated. We have also performed measurements using a submillimeter test bench in order to control the image quality and derive the main optical parameters. The parameters derived from the modeling using 3D measurements are in agreement with the requirements except for the conic constant. The best positioning of the mirror has been optimized consequently. The modeling has also allowed us to determine the pre-flight alignment parameters of the mirror as a function of the expected structure temperature at ceiling altitude. We have shown that this adjustment will enable to keep the tight requirements on the focus position ( $\pm $600 μm) within a range of $\pm 40\:\circ$C around the ceiling temperature value. The submillimeter measurements have validated the results derived from the 3D measurement based modeling. The image quality was investigated by performing a spatial exploration in azimuth and elevation around the nominal focus position, and along the optical axis. The deviation between the predicted and measured positions of the best focus are 80 μm and 11″ in translation along the optical axis and in rotation respectively. The best image pattern is also close to the nominal one, with a sphericity deviation lower than 2 μm RMS. These results will be used for the end-to-end tests of the integrated instrument, and for the optimization of the alignment before flight. [ABSTRACT FROM AUTHOR]

Abstract: Preliminary Atacama Large Millimeter/Submillimeter Array (ALMA) science verification data for a single pixel centered on the hot core of Orion KL (R. A.=05h 35m 14.35s, Dec=−05°22′35″ (J2000)) are available as this special issue on broadband spectroscopy is coming to press. As part of this verification process it is useful to compare simulations based on laboratory spectroscopy with ALMA results. This provides not only a test of instrumentation and analysis, but also a test of astrophysical assumptions such as local thermodynamic equilibrium (LTE) and the temperature variations within telescope beams. However, these tests are spectroscopically limited because it is well known that astrophysical spectra contain large numbers of unknown lines, many of which are presumably due to unanalyzed rotational spectra in excited vibrational states of a relatively few molecules. To address this issue we have previously discussed the use of broadband complete experimental spectra (CES) that is obtained from the analysis of several hundred intensity calibrated spectra taken over a range of temperatures. In this paper we will compare these CES with the similarly complete astrophysical spectra. [Copyright &y& Elsevier]

Abstract: Purpose: To evaluate the accuracy of 64-row-multidetector computed tomography (MDCT) with different slice thickness (0.625 vs. 1.25 mm) in assessing the cerebellar arteries. Materials and methods: A total of 21 consecutive patients who underwent computed tomography angiography (CTA) of the cervicocranial arteries (64-row MDCT; slice thickness, 0.625 mm) because of suspicion of cerebral ischemia were enrolled retrospectively. The MDCT data set was secondarily reconstructed to a slice thickness of 1.25 mm. The examinations were reviewed by three independent blinded observers. Recorded parameters for reconstructed slice thicknesses of 0.625 compared to 1.25 mm were visualization and edge enhancement (based on a developed phantom reference model) of the cerebellar arteries including anterior and posterior inferior cerebellar arteries and the superior cerebellar artery. Results: With 0.625-mm slices, significantly more vessel segments were visualized and edge enhancement was superior compared to 1.25-mm slices by the three readers, and a significant difference for the interaction between vessel segments and the slice thickness was found (P<.001). Furthermore, for a slice thickness of 1.25 mm, there was a significant difference in visualization (P=.0042) and edge enhancement (P=.0015) of vessel segments between the three readers, whereas for thinner slices (0.625 mm), no significant differences were found (P=.412, P=.465). Conclusions: MDCT with slice thickness of 0.625 mm is superior to 1.25 mm reconstructed slice thickness regarding the visualization of cerebellar arteries, representative for smallest assessable arteries in CTA. This is paralleled by a sharper edge enhancement of the vessel contours resulting from a reduced partial volume effect. Conclusively, cranial CTA protocols should be routinely optimized to generate submillimeter slices for diagnostic purposes and digital storage as additional diagnostic value can be expected. [Copyright &y& Elsevier]

Abstract: An investigation of the capabilities and science goals of a submillimeter-wave heterodyne sounder onboard a Titan orbiter is presented. Based on a model of Titan’s submillimeter spectrum, and including realistic instrumental performances, we show that passive limb observations of Titan’s submillimeter radiation would bring novel and unique information on the dynamical and chemical state of Titan’s atmosphere, particularly in the so far poorly probed 500–900km region. The 300–360, 540–660 and 1080–1280GHz spectral ranges appear especially promising, and could be explored with an instrument equipped with a tunable local oscillator system. Vertical temperature profiles can be determined up to ∼1200km using rotational lines of CH4, CO, and HCN. Winds can be measured over the 200–1200km altitude range with an accuracy of 3–5m/s from Doppler shift measurements of any strong optically thin line. Numerous molecular species are accessible, including H2O, NH3, CH3C2H, CH2NH, and several nitriles (HC3N, HC5N, CH3CN, and C2H3CN). Many of them are expected to be detectable in a large fraction of the atmosphere and in some cases at all levels, providing an observational link between stratospheric and thermospheric chemistry. Isotopic variants of some of these species can also be measured, providing new measurements of H, C, N, and O isotopic ratios. Mapping of the thermal, wind, and composition fields, best achieved from a polar orbit and with an articulated antenna, would provide a new view of the couplings between chemistry and dynamics over an extended altitude range of Titan’s atmosphere. Additional science goals at Saturn and Enceladus are briefly discussed. [ABSTRACT FROM AUTHOR]

Performances of 640-GHz Superconductor-Insulator-Superconductor (SIS) mixers developed for the Superconducting Submillimeter-Wave Limb-Emission Sounder (SMILES) mission are described. SMILES, launched in September 2009, is the first mission to observe atmosphere from space using superconducting mixers. Ground test performances of the SIS mixers show very flat gain and noise characteristics in their observation bands in compliance with the specifications required for SMILES. [ABSTRACT FROM AUTHOR]

We aim at understanding the statistical properties of luminous sub-millimeter (submm) galaxies (SMGs) in the context of cosmological structure formation. By utilizing a cosmological N-body simulation to calculate the distribution of dark halos in the Universe, we consider the dust enrichment in individual halos by Type II supernovae (SNe II). The SN II rate is estimated under a star formation activity which is assumed to occur on a dynamical timescale in the dark matter potential. Our simple framework successfully explains the luminosity function, the typical star formation rate, and the typical dust mass of an observational SMG sample at z∼3. We also examine the clustering properties of SMGs, since a positive cross correlation between SMGs and Ly α emitters (LAEs) is indeed observed by a recent observation. In the simulation, we select SMGs by FIR dust luminosity >10 L, while LAEs are chosen such that the age and the virial mass are consistent with the observed LAE properties. The SMGs and LAEs selected in this way show a spatial cross correlation whose strength is consistent with the observation. This confirms that the SMGs really trace the most clustered regions at z∼3 and that their luminosities can be explained by the dust accumulation as a result of their star formation activities. We extend our prediction to higher redshifts, finding that a statistical sample of submm galaxies at z≥6 can be obtained by ALMA with a 100 arcmin survey. With the same survey, a few submm galaxies at z∼10 may be detected. [ABSTRACT FROM AUTHOR]

Abstract: This article presents some aspects of the technology of terahertz heterodyne receiver front-ends dedicated to astrophysics, planetary and atmospheric sciences. It focuses on frequency multipliers and on Schottky mixers. Novel architectures of power-combined frequency multipliers at submillimeter-wavelengths, THz planar fundamental mixers, and integrated receivers will be discussed, as well as the fabrication of submillimeter-wave planar Schottky diodes in France. [ABSTRACT FROM AUTHOR]

We report on the design, fabrication, and characterization of an 840-900-GHz frequency multiplier chain that delivers more than 1 mW across the band at room temperature with a record peak power of 1.4 mW at 875 GHz. When cooled to 120 K, the chain delivers up to 2 mW at 882 GHz. The chain consists of a power amplifier module that drives two cascaded frequency triplers. This unprecedented output power from an electronic source is achieved by utilizing in-phase power-combining techniques. The first stage tripler uses four power-combined chips while the last stage tripler utilizes two power-combined chips. The source output was analyzed with a Fourrer transform spectrometer to verify signal purity. [ABSTRACT FROM AUTHOR]

Abstract: The FIR/submm window is amongst the least explored spectral regions of the electromagnetic spectrum. It is, however, a key to study the general properties of the interstellar medium of galaxies, as it contains important spectral line diagnostics from the neutral, ionized and molecular ISM. The Herschel Space Observatory, successfully launched on 14 May 2009, is the first observatory to cover the entire FIR/submm range between 57 and 672μm. We discuss the main results from the ISO era on FIR spectroscopy of galaxies and the enormous science potential of the Herschel mission through a presentation of its spectroscopic extragalactic key programs. [Copyright &y& Elsevier]

A novel slow-wave vacuum electron device circuit, consisting of a half-period-staggered double-vane array and a high-aspect ratio sheet electron beam, has been conceived for a high-power wideband submillimeter-wave generation. A particle-in-cell simulation, which is based on a finite-difference time- domain algorithm, has shown that this circuit has a very wide intrinsic bandwidth (in excess of 50 GHz around the operating frequency of 220 GHz) with a moderate gain of 13 dB/cm. Moreover, the saturated conversion efficiency is predicted to be 3%-5.5% over the operating band corresponding to an output power of 150-275 W, assuming a beam power of 5 kW. Of particular importance, this structure is based on the TE-fundamental mode interaction, thereby avoiding the complex overmoding instabilities that usually cause spurious signal oscillation in conventional high-aspect-ratio structures. This planar circuit has simple 2-D geometry that is thermally and mechanically robust as well as being compatible with conventional microfabrication techniques. This concept is expected to open numerous opportunities in potential applications of versatile electronic devices in the low-millimeter- and submillimeter-wave regions. [ABSTRACT FROM AUTHOR]

We report an overdensity of bright submillimetre galaxies (SMGs) in the 0.15 deg2 AzTEC/COSMOS survey and a spatial correlation between the SMGs and the optical-IR galaxy density at . This portion of the COSMOS field shows a overdensity of robust SMG detections when compared to a background, or ‘blank-field’, population model that is consistent with SMG surveys of fields with no extragalactic bias. The SMG overdensity is most significant in the number of very bright detections (14 sources with measured fluxes mJy), which is entirely incompatible with sample variance within our adopted blank-field number densities and infers an overdensity significance of . We find that the overdensity and spatial correlation to optical-IR galaxy density are most consistent with lensing of a background SMG population by foreground mass structures along the line of sight, rather than physical association of the SMGs with the galaxies/clusters. The SMG positions are only weakly correlated with weak-lensing maps, suggesting that the dominant sources of correlation are individual galaxies and the more tenuous structures in the survey region, and not the massive and compact clusters. These results highlight the important roles cosmic variance and large-scale structure can play in the study of SMGs. [ABSTRACT FROM AUTHOR]

Millimetron is a Russian-led 12 m diameter submillimeter and far-infrared space observatory which is included in the Space Plan of the Russian Federation for launch around 2017. With its large collecting area and state-of-the-art receivers, it will enable unique science and allow at least one order of magnitude improvement with respect to the Herschel Space Observatory. Millimetron will be operated in two basic observing modes: as a single-dish observatory, and as an element of a ground-space very long baseline interferometry (VLBI) system. As single-dish, angular resolutions on the order of 3 to 12 arc sec will be achieved and spectral resolutions of up to a million employing heterodyne techniques. As VLBI antenna, the chosen elliptical orbit will provide extremely large VLBI baselines (beyond 300,000 km) resulting in micro-arc second angular resolution. [ABSTRACT FROM AUTHOR]

Abstract: We present submillimeter observations of 12CO –2 and 2–1, and 13CO –1 lines of the Venusian mesosphere and lower thermosphere with the Heinrich Hertz Submillimeter Telescope (HHSMT) taken around the second MESSENGER flyby of Venus on 5 June 2007. The observations cover a range of Venus solar elongations with different fractional disk illuminations. Preliminary results like temperature and CO abundance profiles are presented. These data are part of a coordinated observational campaign in support of the ESA Venus Express mission. Furthermore, this study attempts to contribute to cross-calibrate space- and ground-based observations, to constrain radiative transfer and retrieval algorithms for planetary atmospheres, and to a more thorough understanding of the global patters of circulation of the Venusian atmosphere. [Copyright &y& Elsevier]

Abstract: These lecture notes provide an introduction to mm/submm extragalactic astronomy, focused on AGN studies, with the final goal of preparing students to their future exploitation of the ALMA capabilities. I first provide an overview of the current results obtained through mm/submm observations of galaxies and AGNs, both local and at high redshift. Then I summarize the main mm/submm facilities that are currently available. ALMA is then presented with a general description and by providing some details on its observing capabilities. Finally, I discuss some of the scientific goals that will be achievable with ALMA in extragalactic astronomy, and for AGN studies in particular. [Copyright &y& Elsevier]

Abstract: This paper is devoted to the measurement of pressure shift and broadening parameters of water-vapor lines of the pure rotational transition 110–101 in the ground vibrational state of H2 16O at 556.936GHz, H2 17O at 552.02GHz, H2 18O at 547.676GHz, and the vibrationally excited state v 2=1 line of H2 16O at 658.003GHz. The broadening coefficients of the line at 556.936GHz (for N2 and O2 as perturbing gases) coincide within the errors with the values obtained recently by Seta et al. [Pressure broadening coefficients of the water vapor lines at 556.936 and 752.033GHz. JQSRT 2008;109:144–50] by means of a very different technique (THz-TDS). Pressure shift and broadening for other lines were measured for the first time. Comparison of our results with previous measurements and theoretical calculations is presented. [Copyright &y& Elsevier]

Abstract: The air induced broadening coefficients of the pure rotational transitions of HO at 556.936GHz , and 752.033GHz were measured by terahertz time-domain spectroscopy. The air broadening coefficient was determined to be for the 556.936GHz line and for the 752.033GHz line, respectively. The present broadening coefficients for the 556.936 GHz water line are significantly smaller than those of Markov and Krupnov [Measurements of the pressure shift of the 1(10)–1(01) water line at 556.936GHz produced by mixtures of gases. J Mol Spect 1995:172;211–4] but relatively close to the values of the HITRAN database. The measured data may improve the accuracy of the abundance of water vapor retrieved from spectra obtained by the Odin/SMR satellite instrument. The effect on the satellite retrieval processing is discussed. [Copyright &y& Elsevier]

The submillimeter (submm) extragalactic background light (EBL) traces the integrated star formation history throughout the cosmic time. Deep blank-field 850 μm and 1.4 GHz surveys and optical follow-up have been only able to determine the redshift of ∼20% of the submm EBL. The majority (80%) of the submm EBL is still below the confusion and sensitivity limits of current submm and radio instruments. We break through these limits with stacking analyses on our deep 850 μm image in the GOODS-N and find that the submm EBL mostly comes from galaxies at redshifts around 1.0. This redshift is much lower than the redshift of z=2–3 previously implied from radio identified submm sources. This result significantly decreases the number of high redshift galaxies that may be seen by ALMA. [ABSTRACT FROM AUTHOR]

The Atacama Large Millimeter/Submillimeter Array (ALMA) is an international millimeter-wavelength radio telescope under construction in the Atacama Desert of northern Chile. ALMA will be situated on a high-altitude site at 5000 m elevation which provides excellent atmospheric transmission over the instrument wavelength range of 0.3 to 3 mm. ALMA will be comprised of two key observing components—a main array of up to sixty-four 12-m diameter antennas arranged in a multiple configurations ranging in size from 0.15 to ∼18 km, and a set of four 12-m and twelve 7-m antennas operating in a compact array ∼50 m in diameter (known as the Atacama Compact Array, or ACA), providing both interferometric and total-power astronomical information. High-sensitivity dual-polarization 8 GHz-bandwidth spectral-line and continuum measurements between all antennas will be available from two flexible digital correlators. At the shortest planned wavelength and largest configuration, the angular resolution of ALMA will be 0.005″. The instrument will use superconducting (SIS) mixers to provide the lowest possible receiver noise contribution, and special-purpose water vapor radiometers to assist in calibration of atmospheric phase distortions. A complex optical fiber network will transmit the digitized astronomical signals from the antennas to the correlators in the Array Operations Site Technical Building, and post-correlation to the lower-altitude Operations Support Facility where the array will be controlled, and initial construction and maintenance of the instrument will occur. ALMA Regional Centers in the US, Europe, Japan and Chile will provide the scientific portals for the use of ALMA; early science observations are expected in 2010, with full operations in 2012. [ABSTRACT FROM AUTHOR]

This paper presents a prospect for the observations of comets with ALMA. Thanks to unprecedented sensitivity, angular resolution and instantaneous uv-coverage, key measurements on a number of topics related to the chemical and physical properties of the coma and the nucleus will be obtained. These include (1) the identification of new molecular species and measurements of key isotopic ratios, (2) measurements of the composition of short-period comets coming from the trans-Neptunian scattered disc, to investigate chemical diversity within the whole comet population, (3) imaging of gas jets and their relationship with dust features, (4) the study of extended sources of gas in the coma, and (5) the study of the physical and outgassing properties of the nucleus. [ABSTRACT FROM AUTHOR]

The advent of ALMA is bound to improve our knowledge of OB star formation dramatically. Here, we present an overview of this topic outlining how high angular resolution and sensitivity may contribute to shed light on the structure of high-mass star forming regions and hence on the process itself of massive star formation. The impact of this new generation instrument will range from establishing the mass function of pre-stellar cores inside IR-dark clouds, to investigating the kinematics of the gas from which OB stars are built up, to assessing or ruling out the existence of circumstellar accretion disks in these objects. [ABSTRACT FROM AUTHOR]

Thanks to its sensitivity, spatial resolution and instantaneous uv-coverage, ALMA will permit many new studies related to the general topic of the couplings between chemistry and dynamics in planetary atmospheres. It will include: (1) three-dimensional mapping of composition, temperatures and winds in the atmospheres of Mars, Venus and Titan; (2) several aspects of Giant Planet composition and dynamics, such as the origin of oxygen, the evolution of Shoemaker–Levy 9 products in Jupiter’s atmosphere, and the deep atmosphere structure and meteorology; (3) the study of tenuous and distant atmospheres (Io, Enceladus, Pluto, Triton and other Kuiper Belt objects). [ABSTRACT FROM AUTHOR]

Highly-collimated outflows are believed to be the earliest stage in outflow evolution, so their study is essential for understanding the processes driving outflows. The BHR71 Bok globule is known to harbour such a highly-collimated outflow, which is powered by a protostar belonging to a protobinary system. Using the APEX telescope on Chajnantor, we mapped the BHR71 highly-collimated outflow in CO(3-2), and observed several bright points of the outflow in the molecular transitions CO(4-3), CO(7-6), 13CO(3-2), C18O(3-2), CH3OH(7-6) and H2CO(4-3). We use an LVG code to characterise the temperature enhancements in these regions. These observations are particularly interesting for investigating the interaction of collimated outflows with the ambient molecular cloud. In our CO(3-2) map, the second outflow driven by IRS2, which is the second source of the binary system, is completely revealed and shown to be bipolar. We also measure temperature enhancements in the lobes. The CO and methanol LVG modelling points to temperatures between 30 and 50 K in the two lobes. The methanol emission in the southern lobe bright knot is barely resolved with the APEX single-dish. ALMA will thus be a central tool to study the shock chemistry in these regions. [ABSTRACT FROM AUTHOR]

Abstract: The standard planar hybrid architecture, commonly used to construct near and mid-infrared focal-plane arrays, is not suitable for far IR detectors where readout glow, lack of efficient heat dissipation, and thermal mismatch between the detector and the readout could potentially limit their performance. In response, a new layered-hybrid structure was introduced to alleviate these problems and make possible the construction of large format far IR FPAs. To assess the viability of this design, we have fabricated and tested a prototype 2×16 Ge:Sb array coupled to a 1×32 SBRC190 cryogenic readout in a construction similar to the layered-hybrid. In this paper we present the results of our tests which prove the effectiveness of the layered-hybrid structure in blocking the readout glow and providing uniform cooling across the array. [Copyright &y& Elsevier]

Abstract: Future astronomical instruments call for large format and high sensitivity far infrared focal-plane arrays to meet their science objectives. Arrays as large as 128×128 with sensitivities equal to or better than 10−18 W/√Hz are set as targets for the far IR instruments to be developed within the next 10 years. These seemingly modest goals present a not-so-modest quantum leap for far IR detector technology whose progress is hampered by a number of complexities; chief among them the development of low noise readouts operating at deep cryogenic temperatures and a viable hybridization scheme suitable for far IR detectors. In an effort to incrementally develop large-format photoconductor arrays, we have fabricated a 2×16 Ge:Sb array using the SBRC190 readout – a cryogenic 1×32 CTIA readout multiplexer initially developed for SOFIA’s AIRES instrument. In this paper we report the results of the extensive parametric tests performed on this array showing an impressive noise performance of 2.2×10−18 W/√Hz and a DQE of 0.41 despite some design limitations. With such an encouraging performance, this prototype array will serve as a platform for our future developmental effort. [Copyright &y& Elsevier]

Abstract: We report results of a recently-completed pre-formulation phase study of SPIRIT, a candidate NASA Origins Probe mission. SPIRIT is a spatial and spectral interferometer with an operating wavelength range 25–400μm. SPIRIT will provide sub-arcsecond resolution images and spectra with resolution R =3000 in a 1′ field of view to accomplish three primary scientific objectives: (1) learn how planetary systems form from protostellar disks, and how they acquire their inhomogeneous composition; (2) characterize the family of extrasolar planetary systems by imaging the structure in debris disks to understand how and where planets of different types form; and (3) learn how high-redshift galaxies formed and merged to form the present-day population of galaxies. Observations with SPIRIT will be complementary to those of the James Webb Space Telescope and the ground-based Atacama Large Millimeter Array. All three observatories could be operational contemporaneously. [Copyright &y& Elsevier]

Abstract: The joint US and German SOFIA project to develop and operate a 2.5-meter infrared airborne telescope in a Boeing 747-SP is now in its final stages of development. Flying in the stratosphere, SOFIA allows observations through the infrared and submillimeter region, with an average transmission of greater than 80%. SOFIA is characterized by a wide instrument complement ranging from broadband imagers, through moderate resolution spectrographs capable of resolving broad features due to dust and large molecules, to high-resolution spectrometers suitable for kinematic studies of molecular and atomic gas lines at km/s resolution. This broad range in instruments will enable SOFIA to make unique contributions to a broad array of science topics. First science flights will begin in 2009 and the observatory is expected to operate for over 20 years. The sensitivity, characteristics, science instrument complement, and examples of first light spectroscopic science are discussed. [Copyright &y& Elsevier]