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1,651 results for “Planes”
Bolocam Galactic Plane Survey Catalog v1
The Version 2 release (hereafter v2) of the BGPS data includes images and a catalog. It is described in Ginsburg et al (2013).The new images have improved fidelity and more uniform noise. The fields include all those in the original v1 release and some new data. There are new fields included in the BGPS v2 release, primarily in the outer galaxy but including some expansions in the inner galaxy. These include M17, IRAS 22172, a significant expansion in l and b around the l=110 region, Mon R2, NGC 2264, parts of the Orion A and B clouds, Sharpless 235, and scattered IRAS+CO selected fields at longitude 119, 123, 126, 129, 154, 169, 181, 182, 195, 201, and 217. IRSA provides a coverage map.There is a new catalog associated with the v2 images. The sources were extracted using Bolocat with parameters set in the same way as for the v1 catalog. There are many sources in v1 that are not in v2 and vice-versa. These discrepancies occur primarily for faint sources with low signal-to-noise. Objects in both catalogs are likely to be real since catalog parameters were selected to minimize false positives. Changing the quality of the images and the structure of the noise highlights some new objects and obscures others. The v2 catalog has about a 75% overlap with the v1 catalog. The differences are explored in more detail in the Ginsburg et al (2013).The flux calibration offset identified in the version 1 data is now understood. The version 2 data are brighter, on average, by approximately a factor 1.5, but the factor varies from source to source. The v2 catalog should be used instead of the v1 catalog. The source of the error was the incorrect application of a flux calibration solution.Contreras et al (2013) noted a 4.7 arcsecond offset between the BGPS v1 catalog and the ATLASGAL catalog. We believe this is caused by an offset of that magnitude (~3-4 arcseconds) in a few fields that have an inordinate number of sources extracted; the pointing accuracy in the vast majority of the BGPS fields, based on a comparison to Herschel Hi-Gal images, is better than 4 arcseconds, but the mean offset is within 2 arcseconds of zero.
Kepler K2 Ecliptic Plane Input Catalog
Launched in 2009, the Kepler Mission is surveying a region of our galaxy to determine what fraction of stars in our galaxy have planets and measure the size distribution of those exoplanets. Although Kepler completed its primary mission to determine the fraction of stars that have planets in 2013, it is continuing the search, using a more limited survey mode, under the new name K2. The K2 Ecliptic Plane Input Catalog is the primary source of information about objects observed as potential targets for the K2 mission, as the Kepler Input Catalog was used for the original Kepler mission.
ASCA Galactic Plane Survey of Faint X-Ray Sources
Sugizaki et al. (2001) have published a study of faint X-ray sources that were resolved in the ASCA Galactic Plane Survey and their contribution to the galactic ridge X-ray emission, and the present database contains their list of discrete sources. The X-ray emission from the central region of the Galactic plane, |l|<~45 degrees and |b|<~0.4 degrees, was studied in the 0.7 to 10 keV energy band with a spatial resolution of ~3' with the Advanced Satellite for Cosmology and Astrophysics (ASCA) observatory. The authors developed a new analysis method for the ASCA data to resolve discrete sources from the extended Galactic ridge X-ray emission (GRXE). Using the ASCA Gas Imaging Spectrometers (GISs), they successfully resolved 163 discrete sources with X-ray fluxes down to 10<sup>-12</sup>.5<sup>ergs/cm</sup>2/s and determined the intensity variations of the GRXE as a function of the Galactic longitude with a spatial resolution of about 1 degree. This database was created by the HEASARC in December 2001 based on the ADC/<a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/ApJS/134/77/table2">CDS Catalog J/ApJS/134/77/table2</a>.dat. This is a service provided by NASA HEASARC .
CFHT SR QUIRC RAW AND CALIBRATED RING PLANE CROSSING 1.O
This data set contains images of the Saturn system from the CANADA-FRANCE-HAWAII telescope with the Quick Infrared Camera in early August 1995.
WIYN S WI RAW RING PLANE CROSSING V1.0
This data set contains images of the Saturn system from the Wisconsin-Indiana-Yale-NOAO(WIYN) using the WIYN Imager in late November 1995. These observations were made during and immediately after the ring plane crossing.
HST SATURN WFPC2 3 RING PLANE CROSSING V1.0
This data set contains images of the Saturn system taken by the Wide Field/Planetary Camera 2 (WFPC2) aboard the Hubble Space Telescope (HST) through November 1995. This period includes all images taken during the Saturn ring plane crossings of 1995. (No WFPC2 images of Saturn were obtained during the last ring plane crossing in February 1996 because Saturn was too close to the Sun.)
ARC Code TI: X-Plane Communications Toolbox (XPC)
The X-Plane Communications Toolbox (XPC) is an open source research tool used to interact with the commercial flight simulator software X-Plane. XPC allows users to control aircraft and receive state information from aircraft simulated in X-Plane using functions written in C or MATLAB in real time over the network. This research tool has been used to visualize flight paths, test control algorithms, simulate an active airspace, or generate out-the-window visuals for in-house flight simulation software.
Bolocam Galactic Plane Survey Catalog v2.1
The Version 2 release (hereafter v2) of the BGPS data includes images and a catalog. It is described in Ginsburg et al (2013).The new images have improved fidelity and more uniform noise. The fields include all those in the original v1 release and some new data. There are new fields included in the BGPS v2 release, primarily in the outer galaxy but including some expansions in the inner galaxy. These include M17, IRAS 22172, a significant expansion in l and b around the l=110 region, Mon R2, NGC 2264, parts of the Orion A and B clouds, Sharpless 235, and scattered IRAS+CO selected fields at longitude 119, 123, 126, 129, 154, 169, 181, 182, 195, 201, and 217. IRSA provides a coverage map.There is a new catalog associated with the v2 images. The sources were extracted using Bolocat with parameters set in the same way as for the v1 catalog. There are many sources in v1 that are not in v2 and vice-versa. These discrepancies occur primarily for faint sources with low signal-to-noise. Objects in both catalogs are likely to be real since catalog parameters were selected to minimize false positives. Changing the quality of the images and the structure of the noise highlights some new objects and obscures others. The v2 catalog has about a 75% overlap with the v1 catalog. The differences are explored in more detail in the Ginsburg et al (2013).The flux calibration offset identified in the version 1 data is now understood. The version 2 data are brighter, on average, by approximately a factor 1.5, but the factor varies from source to source. The v2 catalog should be used instead of the v1 catalog. The source of the error was the incorrect application of a flux calibration solution.Contreras et al (2013) noted a 4.7 arcsecond offset between the BGPS v1 catalog and the ATLASGAL catalog. We believe this is caused by an offset of that magnitude (~3-4 arcseconds) in a few fields that have an inordinate number of sources extracted; the pointing accuracy in the vast majority of the BGPS fields, based on a comparison to Herschel Hi-Gal images, is better than 4 arcseconds, but the mean offset is within 2 arcseconds of zero.
XMM-Newton Survey Science Center Survey of the Galactic Plane
Many different classes of X-ray sources contribute to the Galactic landscape at high energies. Although the nature of the most luminous X-ray emitters is now fairly well understood, the population of low-to-medium X-ray luminosity (L<sub>X</sub> = 10<sup>27</sup> - 10<sup>34</sup> erg/s) sources remains much less studied, our knowledge being mostly based on the observation of local members. The advent of wide-field and high-sensitivity X-ray telescopes such as XMM-Newton now offers the opportunity to observe this low-to-medium L<sub>X</sub> population at large distances. This study reports the results of a Galactic plane survey conducted by the XMM-Newton Survey Science Centre (SSC). Beyond its astrophysical goals, this survey aims at gathering a representative sample of identified X-ray sources at low latitude that can be used later on to statistically identify the rest of the serendipitous sources discovered in the Milky Way. The survey is based on 26 XMM-Newton observations, obtained at |b| < 20 degrees, distributed over a large range in Galactic longitudes and covering a summed area of 4 deg<sup>2</sup>. The flux limit of this survey is 2 x 10<sup>-15</sup> erg/cm<sup>2</sup>/s in the soft (0.5 - 2 keV) band and 1 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s in the hard (2 - 1 2keV) band. A total of 1319 individual X-ray sources have been detected. Using optical follow-up observations supplemented by cross-correlation with a large range of multi-wavelength archival catalogs, the authors identify 316 X-ray sources. This constitutes the largest group of spectroscopically identified low-latitude X-ray sources at this flux level. The majority of the identified X-ray sources are active coronae with spectral types in the range A to M at maximum distances of ~1 kpc. The number of identified active stars increases towards late spectral types, reaching a maximum at K. Using infrared colors, the authors classify 18% of the stars as giants. The observed distributions of F<sub>X</sub>/F<sub>V</sub>, X-ray and infrared colors indicates that their sample is dominated by a young (100 Myr) to intermediate (600 Myr) age population with a small contribution of close main-sequence or evolved binaries. The authors find other interesting objects such as cataclysmic variables (d ~ 0.6 - 2 kpc), low-luminosity high-mass stars (likely belonging to the class of Gamma-Cas-like systems, d ~ 1.5 - 7 kpc), T Tauri and Herbig-Ae stars. A handful of extragalactic sources located in the highest Galactic latitude fields could be optically identified. For the 20 fields observed with the EPIC pn camera, the authors have constructed log N(>S) - log S curves in the soft and hard bands. In the soft band, the majority of the sources are positively identified with active coronae and the fraction of stars increases by about one order of magnitude from b = 60 degrees to b = 0 degrees at an X-ray flux of 2 x 10<sup>-14</sup> erg/cm<sup>2</sup>/s. The hard band is dominated by extragalactic sources, but there is a small contribution from a hard Galactic population formed by CVs, HMXB candidates or Gamma-Cas-like systems and by some active coronal stars that are also detected in the soft band. At b = 0 degrees, the surface density of hard sources brighter than 1 x 10<sup>-13</sup> erg/cm<sup>2</sup>/s steeply increases by one order of magnitude from l = 20 degrees to the Galactic center region (l = 0.9 degrees). This HEASARC table contains 739 X-ray sources detected in the 26 different fields observed in this study and listed in Tables 8 - 33, inclusive, of the reference paper. These 739 sources have the best XMM quality, i.e. the summary flag sum_flag which contains information about flags set automatically and manually for a given source is zero, meaning that there are no negative flags for the source detection, have either a 2MASS, USNO, GSC, or SDSS counterpart, whatever the probability of identification is, or have some information via SIMBAD or the authors own imaging or spectroscopic observations. For each X-ray source, its X-ray parameters are summarized, listing the pn count rates, and information on optical and infrared counterparts is provided. The properties of the 26 target fields are given in Table 1 of the reference paper, along with the breakdown of source classes in each field. This table was created by the HEASARC in May 2013 based on <a href="https://cdsarc.cds.unistra.fr/ftp/cats/J/A+A/553/A12">CDS Catalog J/A+A/553/A12</a>, the 26 files table8.dat to table33.dat, inclusive. This is a service provided by NASA HEASARC .
Data repository of the paper "Jones-vector multi-plane light conversion using adjoint-optimized metasurfaces"
<p>This data repository includes the requisite data and code for deriving the primary results from the paper, "Jones-vector multi-plane light conversion using adjoint-optimized metasurfaces."</p>
In-plane structural anisotropy in beta-gallium oxide single crystals
<p>GaOx_anisotropy_raw_data contains x-ray diffraction scans performed on commercial undoped and Sn-doped beta-gallium oxide wafers ((-201) oriented) grown using Edge-defined Film-fed Growth method by Tamura corporation and Si-doped beta-gallium oxide crystal ((100) oriented) grown using Optical Floating Zone technique at TIFR crystal growth facility.</p> <p>X-ray diffraction scans were performed at different phi angles to find in-plane structural anisotropy in beta-gallium oxide crystals. </p> <p>Scans were performed for (-603) plane for commercial wafers and (400) plane for lab-grown crystals.</p> <p>Rigaku Smartlab diffractometer was used to perform these scans and all data files are in .ras format.</p> <p>Scans include omega, 2theta-omega, chi, z which were performed to find exact Bragg peak at each phi. All scans performed to obtain optimized values are also present. (For Sn-doped sample, z optimization was not performed.)<br> 2theta, 2theta-theta and phi scans performed at optimized values are also present for Si-doped lab-grown sample and undoped commercial sample.</p> <p>Dataset also contains scans of Sn-doped wafer when chi optimization was not performed and can be used to compare with optimized peaks.</p> <p>Sn-doped commercial wafer scans - phi=0 to 360 with step of 15 degrees</p> <p>Si-doped lab grown crystal and undoped commercial wafer scans - phi=0 to 360 with step of 30 degrees</p>
On the Physics of Ultrasound Transmission for In-Plane Needle Tracking in Guided Interventions
<p>The authors provide all the datasets used in the publication below,</p> <p>G. Malamal and M. R. Panicker, “On the Physics of Ultrasound Transmission for In-Plane Needle Tracking in Guided Interventions,” in Biomedical Physics and Engineering Express. <a href="https://doi.org/10.1088/2057-1976/acc338">https://doi.org/10.1088/2057-1976/acc338</a> <strong>(Academic Reference to be Cited)</strong></p> <p><strong>Abstract:</strong></p> <p>In ultrasound (US) guided interventions, the accurate visualization and tracking of needles is a critical challenge, particularly during in-plane insertions. An inaccurate identification and localization of needles lead to severe inadvertent complications and increased procedure times. This is due to the inherent specular reflections from the needle with directivity depending on the angle of incidence of the US beam, and the needle inclination. Though several methods have been proposed for improved needle visualization, a detailed study emphasizing the physics of specular reflections resulting from the interaction of transmitted US beam with the needle remains to be explored. In this work, we discuss the properties of specular reflections from planar and spherical wave US transmissions respectively through multi-angle plane wave (PW) and synthetic transmit aperture (STA) techniques for in-plane needle insertion angles between 15°-50°.</p> <p><strong>Related Scripts: </strong><a href="https://github.com/gayathrimalamal/TxB_Needle_Ultrasound"> https://github.com/gayathrimalamal/TxB_Needle_Ultrasound </a></p> <p><strong>Details of Dataset: </strong><a href="https://drive.google.com/file/d/1QMDQH3QKS9ZRw5PWhPu4k3flrJU-kx-1/view?usp=sharing">Readme_Dataset.pdf</a></p> <p><strong>Request for Data: </strong><a href="https://drive.google.com/file/d/1RCrthqsLPIe5peGKIctPD1PpO7fCxFKw/view?usp=share_link">Data_Release_Agreement.pdf</a> (Contact: mahesh@iitpkd.ac.in)</p> <p> </p>
Riverside Plane Crash
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HST SATURN WFPC2 3 RING PLANE CROSSING V1.0
UNK
WHT S API ISIS RAW AND CALIBRATED RING PLANE CROSSING V1.0
Unknown
IRAS FOCAL PLANE ARRAY CHARACTERISTICS V1.1
Filter curves and detector parameters for the IRAS Focal Plane Array (FPA).
Data - Bedding Plane Geometry and Lithological Variations Influencing Rainfall-Triggered Landslide Dynamics in the Chittagong Fold Belt of Bangladesh
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MMS 4 Electric Double Probe (EDP) Axial Double Probe, Spin Plane Double Probe (ADP-SDP) Electric Double Probe, High-Frequency Electric Field Spectra, Level 2 (L2), Survey Mode, 16 s Data
Electric Double Probe, High-Frequency AC Electric Field Spectra, Level 2, Survey Data, Level 1B AC Electric Field Data
MMS 1 Electric Double Probe (EDP) Axial Double Probe, Spin Plane Double Probe (ADP-SDP) Electric Double Probe, High-Frequency Electric Field Spectra, Level 2 (L2), Survey Mode, 16 s Data
Electric Double Probe, High-Frequency AC Electric Field Spectra, Level 2, Survey Data, Level 1B AC Electric Field Data
MMS 3 Electric Double Probe (EDP) Axial Double Probe, Spin Plane Double Probe (ADP-SDP) Three-Dimensional HMFE Electric Field, Level 2 (L2), Burst Mode, 0.01525878906 ms Data
Electric Double Probe, Three-Dimensional HMFE Electric Field, Level 2, Burst Mode, Level 1B AC Electric Field Data
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OpenNeuro
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