Point source

About: Point source is a research topic. Over the lifetime, 5077 publications have been published within this topic receiving 94091 citations.

Absolute calibration of the JT‐60U neutron monitors using a 252Cf neutron sourcea)

Abstract: Absolutely calibrated measurements of the neutron yield are important for the evaluation of plasma performance such as the fusion gain Q in D–D operating tokamaks. The time‐resolved neutron yield is measured with 235U and 238U fission chambers and 3He proportional counters in the JT‐60U tokamak. The in situ calibration was performed by moving the 252Cf neutron source toroidally through the JT‐60 vacuum vessel. Detection efficiencies of three 235U and two 3He detectors were measured for 92 locations of the neutron point source in toroidal scans at two different major radii. The total detection efficiency for the torus neutron source was obtained by averaging the point efficiencies over the whole toroidal angle. The uncertainty of the resulting detection efficiency for the plasma neutrons is estimated to be ±11%.

The structure of the NGC1333-IRAS2 protostellar system on 500 AU scales: an infalling envelope, a circumstellar disk, multiple outflows, and chemistry

Abstract: This paper investigates small-scale structures of dense gas and dust around the low-mass protostellar binary NGC1333-IRAS2 using millimeter-wavelength aperture-synthesis observations from the OVRO and BIMA interferometers. The detected 3 mm continuum emission is consistent with models of the envelope around IRAS2A, based on previously reported submillimeter continuum images, down to the 3", or 500 AU, resolution of the interferometer data. Our data constrain the contribution of an unresolved point source to 22 mJy. Within the accuracy of the parameters describing the envelope model, the point source flux has an uncertainty by up to 25%. We interpret this point source as a cold disk of mass \gtrsim 0.3 M_\odot. The same envelope model also reproduces aperture-synthesis line observations of the optically thin isotopic species C34S and H13CO+. The more optically thick main isotope lines show a variety of components in the protostellar environment: N2H+ is closely correlated with dust concentrations as seen at submillimeter wavelengths and is particularly strong toward the starless core IRAS2C. We hypothesize that N2H+ is destroyed through reactions with CO that is released from icy grains near the protostellar sources IRAS2A and B. CS, HCO+, and HCN have complex line shapes apparently affected by both outflow and infall. In addition to the east-west jet from IRAS2A, a north-south velocity gradient near this source indicates a second, perpendicular outflow. This suggests the presence of a binary companion within 0.3" (65 AU) from IRAS2A as driving source of this outflow. Alternative explanations of the velocity gradient such as rotation in a circumstellar envelope or a single, wide-angle outflow are less likely.

VLT detection of a red supergiant progenitor of the type IIP supernova 2008bk

Abstract: We report the identification of a source coincident with the position of the nearby type II-P supernova (SN) 2008bk in high quality optical and near-infrared pre-explosion images from the ESO Very Large Telescope (VLT). The SN position in the optical and near-infrared pre-explosion images is identified to within about +-70 and +-40 mas, respectively, using post-explosion Ks-band images obtained with the NAOS CONICA adaptive optics system on the VLT. The pre-explosion source detected in four different bands is precisely coincident with SN 2008bk and is consistent with being dominated by a single point source. We determine the nature of the point source using the STARS stellar evolutionary models and find that its colours and luminosity are consistent with the source being a red supergiant progenitor of SN 2008bk with an initial mass of 8.5 +- 1.0 Msun.

Point source scanning apparatus and method

Abstract: A scanning display device (10) directly scans a light source (12) along at least one scanning path, rather than scanning a light beam emitted from such source (22) along such scanning path. By scanning the light source a smaller, lighter weight scanner without a mirror can be used to achieve light source scanning along the desired scan path. A resonant cantilever (44) translates one or more point sources (e.g., one for a monochromatic display; red, green and blue for an RGB display). The cantilever motion is driven by an electromagnetic drive circuit or by a piezoelectric drive actuator (82). The light source is one or more light emitting diode point sources (42), one or more fiber optic point sources (62), or one or more light emitting polymer light sources.