Different Lines Of Sight Research Articles

Empirical line ratios for optical emission spectroscopy in low-temperature, low-density, magnetised Ar plasmas

Spectroscopic evaluation of electron temperature and density in low-temperature, low-density, magnetized plasmas can be difficult, but necessary in situations where chemical erosion and physical sputtering prevent the use of other diagnostics, such as Langmuir probes (LP). Further, in such cases, because of the low densities and temperatures, the vessel and environment involved, theoretical line ratios derived from Collisional-Radiative models may not be easily applicable. This is the case, for example, of low-temperature (<15 eV), low-density (<1011 cm−3), magnetised plasma used for plasma-material interaction studies where chemical erosion and physical sputtering can be significant. The aim of the present work is to define an empirical line ratio (ELR) method derived from an extensive calibration campaign with the two diagnostics, using LP measurements as a reference. The ELR method is useful to permit the use of optical emission spectroscopy independent of LP in conditions that are critical for the latter, resulting in an effective instrument for the evaluation of plasma parameters. Further, the use of two different lines of sight and the influence of the magnetic field intensity on the measurements are also discussed. The proposed ELR method is demonstrated here for pure Ar linear plasmas and is in principle applicable also to other similar cases.

3D scaling laws and projection effects in The300-NIKA2 Sunyaev-Zeldovich Large Program Twin Samples

The abundance of galaxy clusters with mass and redshift is a wellknown cosmological probe. The cluster mass is a key parameter for studies that aim to constrain cosmological parameters using galaxy clusters, making it critical to understand and properly account for the errors in its estimates. Subsequently, it becomes important to correctly calibrate scaling relations between observables like the integrated Compton parameter and the mass of the cluster. The NIKA2 Sunyaev-Zeldovich Large program (LPSZ) enables one to map the intracluster medium profiles in the mm–wavelength band with great details (resolution of 11 &amp; 17″ at 1.2 &amp; 2 mm, respectively) and hence, to estimate the cluster hydrostatic mass more precisely than previous SZ observations. However, there are certain systematic effects which can only be accounted for with the use of simulations. For this purpose, we employ The Three Hundred simulations which have been modelled with a range of physics modules to simulate galaxy clusters. The so-called twin samples are constructed by picking synthetic clusters of galaxies with properties close to the observational targets of the LPSZ. In particular, we use the Compton parameter maps and projected total mass maps of these twin samples along 29 different lines of sight. We investigate the scatter that projection induces on the total masses. Eventually, we consider the statistical values along different lines of sight to construct a kind of 3D scaling law between the integrated Compton parameter, total mass, and overdensity of the galaxy clusters to determine the overdensity that is least impacted by the projection effect.

Evolution of Galaxy Size in the FOGGIE Simulations

Cosmological simulations are a powerful tool to study galaxy evolution as they can span a substantial fraction of the cosmic time. In this research note, we use the Figuring Out Gas and Galaxies In Enzo simulations—cosmological hydrodynamic simulation of Milky Way-like galaxies—to measure the evolution of the radius of the galaxy disk. Additionally, we analyze the simulations along three different lines of sight. Lastly, we show that the disk size increases over time regardless of angle of projection.

Multi-wavelength spectroscopic study of shock-driven phenomena in explosive outbursts in symbiotic-like recurrent novae with an emphasis on RS Ophiuchi

Aims. Our goal is to detail the development of RS Ophiuchi and the other Galactic symbiotic-like recurrent novae throughout their outburst and quiescence, with a particular emphasis on the propagation of the shock wave during the outburst of the binaries. Methods. The spectral analysis has been performed using archival data according to the features of the individual datasets. Swift grism spectra were reduced and extracted using a combination of the pre-existing UVOTPY Python routine and newly written pipelines in Matlab. Other datasets were directly available in reduced form, already corrected for instrumental or background contamination, and calibrated in wavelength and flux or intensity. The work on these was done through pipelines suited for reading the data and elaborating them to extract quantities of interest for the analysis. Results. We find striking similarities in different outbursts of the same object and for different novae. For example, RS Oph 2021 was almost identical to the 2006 outburst, despite having occurred at a different orbital phase with the observations made from a different line of sight through the red giant wind. Despite the intrinsically different properties of the binaries, striking similarities are found for different systems of the same class, for instance, the trend of the electron density over time during outburst appears to follow a general temporal development.

A statistical analysis of the structure of the interstellar medium in the disc of the Milky Way

ABSTRACT We construct Convolutional Neural Networks (CNNs) trained on exponentiated fractional Brownian motion (xfBm) images, and use these CNNs to analyse Hi-GAL images of surface density in the Galactic Plane. The CNNs estimate the Hurst parameter, ${\cal H}$ (a measure of the power spectrum), and the scaling exponent, ${\cal S}$ (a measure of the range of surface densities), for a square patch comprising $[{\cal N}\times {\cal N}]=$ [128 × 128], [64 × 64], or [32 × 32] pixels. The resulting estimates of ${\cal H}$ are more accurate than those obtained using Δ-variance. We stress that statistical measures of structure are inevitably strongly dependent on the range of scales they actually capture, and difficult to interpret when applied to fields that conflate very different lines of sight. The CNNs developed here mitigate this issue by operating effectively on small fields (small ${\cal N}$), and we exploit this property to develop a procedure for constructing detailed maps of ${\cal H}$ and ${\cal S}$. This procedure is then applied to Hi-GAL maps generated with the ppmap procedure. There appears to be a bimodality between sightlines with higher surface density ($\gtrsim 32\, {\rm M}_{_\odot }\, {\rm pc^{-2}}$), which tend to have higher ${\cal H}\, (\gtrsim 0.8)$ and ${\cal S}\, (\gtrsim 1)$; and sightlines intercepting regions of lower surface density ($\lesssim 32\, {\rm M}_{_\odot }\, {\rm pc^{-2}}$), which tend to have lower ${\cal H}\, (\lesssim 0.8)$ and ${\cal S}\, (\lesssim 1)$; unsurprisingly the former sightlines are concentrated towards the Galactic Midplane and the Inner Galaxy. The surface density PDF takes the form dP/dΣ ∝ Σ−3 for $\Sigma \gtrsim 32\, {\rm M}_{_\odot }\, {\rm pc^{-2}}$, and on most sightlines this power-law tail is dominated by dust cooler than $\, \sim 20\, \rm {K}$, which is the median dust temperature in the Galactic Plane.

Study of pulsar flux density and its variability with Parkes data archive

ABSTRACT We present average flux density measurements of 151 radio pulsars at 1.4 GHz with the Parkes ‘Murriyang’ radio telescope. We recommend our results be included in the next version of the Australia Telescope National Facility Pulsar Catalogue. The large sample of pulsars together with their wide dispersion measure (DM) range makes this data set useful for studying variability of flux density, pulsar spectra, and interstellar medium (ISM). We derive the modulation indices and structure-function from the flux density time series for 95 and 54 pulsars, respectively. We suggest the modulation index also be included in the next version of the pulsar catalogue to manifest the variability of pulsar flux density. The modulation index of flow density and DM are negatively correlated. The refractive scintillation (RISS) time-scales or its lower bound for a set of 15 pulsars are derived. They are very different from theoretical expectations, implying the complicated properties of the ISM along different lines of sight. The structure-function for other pulsars is flat. The RISS parameters for some of these pulsars possibly could be derived with different observing strategies in the future.

Monitoring Horizontal and Vertical Components of SAMARCO Mine Dikes Deformations by DInSAR-SBAS Using TerraSAR-X and Sentinel-1 Data

This article presents an investigation of ground movement measurements based on a combination of TerraSAR-X and Sentinel-1 data, in opposite tracks, aiming to detect ground de-formation of the remaining dikes of Germano mine, after the Fundão dam collapse. The differential interferometry technique SBAS (Small Baseline Subset) was applied to obtain the deformation of the surface in different Line of Sight (LoS), in order to carry out the vector decomposition and generate the deformation measurements in the vertical and horizontal directions. A set of 37 single-look complex (SLC) images of TerraSAR-X (TSX), acquired during the period from 19 February 2016 to 15 May 2017, and 37 SLC images of Sentinel-1, acquired from 8 February 2016 to 15 May 2017, were used to perform this investigation. For the TerraSAR-X interferometric processing, a coherence threshold of 40%, 4 looks in range and 2 looks in azimuth, 1200 m of atmospheric filter, and 10 % of max normal baseline of the critical were used. For the Sentinel-1 interferometric processing a coherence threshold of 26%, 8 looks in range and 2 looks in azimuth, 1200 m of atmospheric filter, and 20% of the of max normal baseline of the critical were used. For both sensors a digital elevation model generated by Pleiades 1-A was used for removing the topographic phase component. The final results were consistent with the topographic in situ measurements, providing key information to make crucial decisions regarding risks, or even mitigation, repairs or emergency response, as well as for a better understanding of the on-going instability phenomena affecting the dikes and dams.

A study on the clustering properties of radio-selected sources in the Lockman Hole region at 325 MHz

ABSTRACT Studying the spatial distribution of extragalactic source populations is vital in understanding the matter distribution in the Universe. It also enables understanding the cosmological evolution of dark matter density fields and the relationship between dark matter and luminous matter. Clustering studies are also required for EoR foreground studies since it affects the relevant angular scales. This paper investigates the angular and spatial clustering properties and the bias parameter of radio-selected sources in the Lockman Hole field at 325 MHz. The data probes sources with fluxes ≳0.3 mJy within a radius of 1.8° around the phase centre of a 6° × 6° mosaic. Based on their radio luminosity, the sources are classified into Active Galactic Nuclei (AGNs) and Star-Forming Galaxies (SFGs). Clustering and bias parameters are determined for the combined populations and the classified sources. The spatial correlation length and the bias of AGNs are greater than SFGs- indicating that more massive haloes host the former. This study is the first reported estimate of the clustering property of sources at 325 MHz, intermediate between the pre-existing studies at high and low-frequency bands. It also probes a well-studied deep field at an unexplored frequency with moderate depth and area. Clustering studies require such observations along different lines of sight, with various fields and data sets across frequencies to avoid cosmic variance and systematics. Thus, an extragalactic deep field has been studied in this work to contribute to this knowledge.

Diagnosis of the imploding shell asymmetry in polar-direct-drive deuterium-tritium cryogenic target implosions on OMEGA.

We discuss the analyses of gated, x-ray imaging data from polar-direct-drive experiments with cryogenically layered deuterium-tritium targets on the OMEGA laser. The in-flight shell asymmetries were diagnosed at various times during the implosion, which was caused by the beam pointing geometry and preimposed variations in the energy partition between the different groups of laser beams. The shape of the ablation surface during the acceleration phase of the implosion was measured along two different lines of sight, and a Legendre mode (ℓ-mode) decomposition was applied for modes of up to ten to investigate shell asymmetries. A clear causal relationship between the imposed beam imbalance and the shape of the in-flight shell asymmetries was observed. The imploded shell with a balanced energy ratio shows smaller values of the amplitudes of ℓ-mode 2 compared to that from implosions with an imbalanced ring energy ratio. The amplitudes of ℓ-modes 4 and 6 are the same within the measurement uncertainty with respect to the change in beam energy ratio.

3D Hydrodynamics of Pre-supernova Outbursts in Convective Red Supergiant Envelopes

Eruptive mass loss likely produces the energetic outbursts observed from some massive stars before they become core-collapse supernovae (SNe). The resulting dense circumstellar medium may also cause the subsequent SNe to be observed as Type IIn events. The leading hypothesis of the cause of these outbursts is the response of the envelope of the red supergiant (RSG) progenitor to energy deposition in the months to years prior to collapse. Early theoretical studies of this phenomenon were limited to 1D, leaving the 3D convective RSG structure unaddressed. Using FLASH's hydrodynamic capabilities, we explore the 3D outcomes by constructing convective RSG envelope models and depositing energies less than the envelope binding energies on timescales shorter than the envelope dynamical time deep within them. We confirm the 1D prediction of an outward-moving acoustic pulse steepening into a shock, unbinding the outermost parts of the envelope. However, we find that the initial 2–4 km s−1 convective motions seed the intrinsic convective instability associated with the high-entropy material deep in the envelope, enabling gas from deep within the envelope to escape and increasing the amount of ejected mass compared to an initially “quiescent” envelope. The 3D models reveal a rich density structure, with column densities varying by ≈10× along different lines of sight. Our work highlights that the 3D convective nature of RSG envelopes impacts our ability to reliably predict the outburst dynamics, the amount, and the spatial distribution of the ejected mass associated with deep energy deposition.

Analysis of limited coverage effects on areal density measurements in inertial confinement fusion implosions

Accurate diagnosis of areal density (ρR) is critical for the inference of performance metrics in inertial confinement fusion implosions. One potential source of error in this diagnosis is the existence of low mode perturbations in the imploding target, which lead to asymmetries in the inference of the ρR from different lines of sight. Here, the error accrued as a result of limited coverage of the sphere due to a finite number of detectors is quantified, and the development of a forward scatter measurement from the OMEGA neutron time-of-flight detectors is motivated. A method by which the 1D-equivalent 4π-averaged ⟨ρR⟩ can be reconstructed, if accurate mode information can be diagnosed by other means, is validated.

Application of ground-based stereophotogrammetric survey in the technical inventory of real estate objects

The general methods of land survey for the purposes of technical inventory of real estate units don’t allow creating visual materials and forms of real estate objects elements that can have some errors. The new method of land survey with the stereo photography and GNSS coordinating of station is free of this weaknesses. The land surveys of object must be made with photogrammetric constructеs, which consist of 3, 4 or 6 snapshots. Stations must have noncollinear position. Minimal base lines must be calculated according to acceptable errors of buildings measurements. The research shows that all photogrammetric constructеs are of equal accuracy. The photographing with 4 or 6 stations is more informative because of different lines of sight. The result of this surveys is a 3D model. Measurements of forms of real estate objects elements with 3D models have high accuracy. The survey examples of different objects shows high accuracy results of 2D and 3D measurements, which are made with 3D model. The implementation of the method of land survey with the stereo photography for the purposes of technical inventory of real estate objects makes real progress in the creation of 3D cadaster.

Estimating anisotropy directly via neural timeseries

An isotropic dynamical system is one that looks the same in every direction, i.e., if we imagine standing somewhere within an isotropic system, we would not be able to differentiate between different lines of sight. Conversely, anisotropy is a measure of the extent to which a system deviates from perfect isotropy, with larger values indicating greater discrepancies between the structure of the system along its axes. Here, we derive the form of a generalised scalable (mechanically similar) discretized field theoretic Lagrangian that allows for levels of anisotropy to be directly estimated via timeseries of arbitrary dimensionality. We generate synthetic data for both isotropic and anisotropic systems and, by using Bayesian model inversion and reduction, show that we can discriminate between the two datasets – thereby demonstrating proof of principle. We then apply this methodology to murine calcium imaging data collected in rest and task states, showing that anisotropy can be estimated directly from different brain states and cortical regions in an empirical in vivo biological setting. We hope that this theoretical foundation, together with the methodology and publicly available MATLAB code, will provide an accessible way for researchers to obtain new insight into the structural organization of neural systems in terms of how scalable neural regions grow – both ontogenetically during the development of an individual organism, as well as phylogenetically across species.

Structural analysis of the optical hinge preliminary design for the ITER wide angle viewing system diagnostic

The ITER Visible/Infrared Wide Angle Viewing System (WAVS) is an optical diagnostic aimed at monitoring the first wall for machine protection purposes. The Optical Hinge (OH) and Optical Relay Unit (ORU) are the first two components in the interspace area and both share a common support structure. The WAVS will be composed by 15 different lines of sight (LoS) distributed around ITER vacuum vessel in Equatorial Ports (EP) 3, 9, 12 and 17. EP12 is currently at its preliminary design and has to be operational for the first plasma. Its development is being carried out by the Consortium constituted by CEA, CIEMAT and Bertin Technologies, within the Framework Partnership Agreement financed by F4E.The OH mission is to compensate the vertical displacement of the vacuum vessel during operation with respect to the building. Therefore each OH LoS consists of a pair of flat mirrors arranged vertically. The upper one is driven vertically while the other remains fixed. Both mirrors are provided with alignment capabilities to assure their correct installation. The three OH LoS are placed in the OH-ORU common support structure, which is in turn directly attached to the Interspace Support Structure.In order to assure the optical performance, the OH-ORU common support structure has to withstand thermal and inertial loads during normal operation and SL-1 seism with low deviation (0.3 mm) and tilt (0.5arcmin). In case of Category III and IV (higher seismic or accidental loads) its integrity has to be maintained as it is classified as an ITER Safety Relevant component.This work comprises the structural analyses performed by CIEMAT of the OH mechanical set to evaluate its optical performance and the ones of the OH-ORU common structure in EP12 to check its integrity in accordance with the RCC-MR Code.

The NANOGrav 12.5 yr Data Set: Polarimetry and Faraday Rotation Measures from Observations of Millisecond Pulsars with the Green Bank Telescope

Abstract In this work, we present polarization profiles for 23 millisecond pulsars observed at 820 and 1500 MHz with the Green Bank Telescope as part of the NANOGrav pulsar timing array. We calibrate the data using Mueller matrix solutions calculated from observations of PSRs B1929+10 and J1022+1001. We discuss the polarization profiles, which can be used to constrain pulsar emission geometry, and present both the first published radio polarization profiles for nine pulsars and the discovery of very low-intensity average profile components (“microcomponents”) in four pulsars. We obtain the Faraday rotation measures for each pulsar and use them to calculate the Galactic magnetic field parallel to the line of sight for different lines of sight through the interstellar medium. We fit for linear and sinusoidal trends in time in the dispersion measure and Galactic magnetic field and detect magnetic field variations with a period of 1 yr in some pulsars, but overall find that the variations in these parameters are more consistent with a stochastic origin.

A graph-matching approach for cross-view registration of over-view and street-view based point clouds

Wide-area 3D data generation for complex urban environments often needs to leverage a mixed use of data collected from both air and ground platforms, such as from aerial surveys, satellite, and mobile vehicles. On one hand, such kind of data with information from drastically different views (ca. 90° and more) forming cross-view data, which due to very limited overlapping region caused by the drastically different line of sight of the sensors, is difficult to be registered without significant manual efforts. On the other hand, the registration of such data often suffers from non-rigid distortion of the street-view data (e.g., non-rigid trajectory drift), which cannot be simply rectified by a similarity transformation. In this paper, based on the assumption that the object boundaries (e.g., buildings) from the over-view data should coincide with footprints of façade 3D points generated from street-view photogrammetric images, we aim to address this problem by proposing a fully automated geo-registration method for cross-view data, which utilizes semantically segmented object boundaries as view-invariant features under a global optimization framework through graph-matching: taking the over-view point clouds generated from stereo/multi-stereo satellite images and the street-view point clouds generated from monocular video images as the inputs, the proposed method models segments of buildings as nodes of graphs, both detected from the satellite-based and street-view based point clouds, thus to form the registration as a graph-matching problem to allow non-rigid matches; to enable a robust solution and fully utilize the topological relations between these segments, we propose to address the graph-matching problem on its conjugate graph solved through a belief-propagation algorithm. The matched nodes will be subject to a further optimization to allow precise-registration, followed by a constrained bundle adjustment on the street-view image to keep 2D-3D consistencies, which yields well-registered street-view images and point clouds to the satellite point clouds. Our proposed method assumes no or little prior pose information (e.g. very sparse locations from consumer-grade GPS (global positioning system)) for the street-view data and has been applied to a large cross-view dataset with significant scale difference containing 0.5 m GSD (Ground Sampling Distance) satellite data and 0.005 m GSD street-view data, 1.5 km in length involving 12 GB of data. The experiment shows that the proposed method has achieved promising results (1.27 m accuracy in 3D), evaluated using collected LiDAR point clouds. Furthermore, we included additional experiments to demonstrate that this method can be generalized to process different types of over-view and street-view data sources, e.g., the open street view maps and the semantic labeling maps. Codes will be made available through Github Repository.1https://github.com/GDAOSU/graph-matching-based-crossview-registration.1

Polarization signatures of the head-on collision model for Type Ia supernovae: how much asymmetry is too much?

ABSTRACT In a previous paper, we showed that the asymmetric ejecta produced by (zero impact parameter) head-on collisions of carbon–oxygen white dwarfs allow these progenitor models for Type Ia supernovae (SNe Ia) to cover the observed 2D distribution of Si ii line depths (Branch plot). In this paper, we study the polarization signature associated with the 2D asymmetric ejecta of the collision model and a double-detonation model using similar tardis radiative transfer simulations along different lines of sight with a spherical photosphere, combined with a new 3D Monte Carlo polarization code. We show that the polarization Q can be parametrized as a product Q = QmaxQx of a radial structure component Qmax , which is insensitive to the model specifics and is shown to be universally around $Q_{\max }\sim 5\,{{\mathrm{ per\,cent}}}$, and a cancellation component Qx, which depends on the asymmetry details. The continuum polarization is found to be low for both the collision and double-detonation models with $Q\sim 0.5\,{{\mathrm{ per\,cent}}}$. However, the irregular Si distribution in the 2D head-on collision model results in the Si ii line polarization reaching $Q\sim 3\,{{\mathrm{ per\,cent}}}$ ($Q_{{x}} \lesssim 50\,{{\mathrm{ per\,cent}}}$) in tension with observations (mostly $\lesssim 1.2\,{{\mathrm{ per\,cent}}}$). In contrast, we show that the double-detonation model also covers the Branch plot, and yet results in low line polarization $Q\lesssim 0.7\,{{\mathrm{ per\,cent}}}$ ($Q_{ {x}} \sim 10\,{{\mathrm{ per\,cent}}}$) consistent with previous results and most SNe Ia. These results strengthen the case for asymmetric explosions as progenitors of SNe Ia, emphasizing an additional requirement for large polarization cancellations to account for the low observed line polarizations.

Compton-thick AGN in the NuSTAR Era VI: The Observed Compton-thick Fraction in the Local Universe

Abstract We present the analysis of simultaneous Nuclear Spectroscopic Telescope Array (NuSTAR) and XMM-Newton data of eight Compton-thick active galactic nuclei (CT-AGN) candidates selected in the Swift-BAT 100 month catalog. This work is part of an ongoing effort to find and characterize all CT-AGN in the Local (z ≤ 0.05) Universe. We used two physically motivated models, MYTorus and borus02, to characterize the sources in the sample, finding five of them to be confirmed CT-AGN. These results represent an increase of ∼19% over the previous NuSTAR-confirmed, BAT-selected CT-AGN at z ≤ 0.05, bringing the total number to 32. This corresponds to an observed fraction of ∼8% of all AGN within this volume-limited sample, although it increases to 20% ± 5% when limiting the sample to z ≤ 0.01. Out of a sample of 48 CT-AGN candidates, selected using BAT and soft (0.3−10 keV) X-ray data, only 24 are confirmed as CT-AGN with the addition of the NuSTAR data. This highlights the importance of NuSTAR when classifying local obscured AGN. We also note that most of the sources in our full sample of 48 Seyfert 2 galaxies with NuSTAR data have significantly different lines of sight and average torus column densities, favoring a patchy torus scenario.

Radiative transfer of ionizing radiation through gas and dust: grain charging in star-forming regions

ABSTRACT The presence of charged dust grains is known to have a profound impact on the physical evolution of the multiphase interstellar medium (ISM). Despite its importance, this process is still poorly explored in numerical simulations due to its complex physics and the tight dependence on the environment. Here, we introduce a novel implementation of grain charging in the cosmological radiative transfer code crash. We first benchmark the code predictions on a series of idealized dusty H ii regions created by a single star, in order to assess the impact of grain properties on the resulting spatial distribution of charges. Secondly, we perform a realistic radiative transfer simulation of a star-forming region extracted from a dusty galaxy evolving in the Epoch of Reionization. We find that ∼13 per cent of the total dust mass gets negatively charged, mainly silicate and graphite grains of radius 10−3 $\mu$m. A complex spatial distribution of grain charges is also found, primarily depending on the exposure to stellar radiation and strongly varying along different lines of sight, as a result of radiative transfer effects. We finally assess the impact of grain properties (both chemical composition and size) on the resulting charge distribution. The new implementation described here will open up a wide range of possible studies investigating the physical evolution of the dusty ISM, nowadays accessible to observations of high- and low- redshift galaxies.

Multidimensional Parameter Study of Double Detonation Type Ia Supernovae Originating from Thin Helium Shell White Dwarfs

Abstract Despite the importance of Type Ia supernovae (SNe Ia) throughout astronomy, the precise progenitor systems and explosion mechanisms that drive SNe Ia are still unknown. An explosion scenario that has gained traction recently is double detonation, in which an accreted shell of He detonates and triggers a secondary detonation in the underlying white dwarf. Our research presents a number of high-resolution, multidimensional, full-star simulations of thin-He-shell, sub-Chandrasekhar-mass white dwarf progenitors that undergo a double detonation. This suite of thin-shell progenitors incorporates He shells that are thinner than those in previous multidimensional studies. We confirm the viability of the double detonation across a range of He-shell parameter space, as well as present bulk yields and ejecta profiles for each progenitor. The yields obtained are generally consistent with previous works and indicate the likelihood of producing observables that resemble SNe Ia. The dimensionality of our simulations allow us to examine features of the double detonation more closely, including the details of the off-center secondary ignition and asymmetric ejecta. We find considerable differences in the high-velocity extent of postdetonation products across different lines of sight. The data from this work will be used to generate predicted observables and may further support the viability of the double detonation scenario as an SN Ia channel, as well as show how the properties of the progenitor or viewing angle may influence trends in observable characteristics.