![]() The system was operated in search mode, thus detections submitted to the MPC appear all over the detector field, not just the center. The optics produced significant astrometric distortion which PinPoint is able to automatically remove via adaptive higher-order solution. Back in 2002, IAU #333 used PinPoint with an 18" f/2.8 hyperbolic telescope and a 2K by 3K detector at 1.5 arcsec/pixel. PinPoint is used as the plate solving engine in many astronomy applications out there, including Diffraction Limited's MaxIm DL 6 and MaxPoint, CCDWare's FocusMax and PoleAlignMax, MainSequence's Sequence Generator Pro, Omega Labs Ricerca 7, CCDWare's CCD Autopilot, and of course our own ACP Expert Observatory Operating System. You can use Visual PinPoint with any FITS or POSS/DSS images. The package comes with Visual PinPoint, a point-and-click Windows program that has automated tools for hands-off asteroid and supernova hunting with optional blinking for validation. Typical uses include plate solving which gives precise pointing to telescope mounts, asteroid and comet searching, high-precision astrometry (detection and measurement of positions), and other more exotic uses such as space situational awareness. This is all automatic to you and to client programs that embed the engine. If you don't have an internet cdonnection, PinPoint can use the 'ansvr' local all-sky server by Andy Galasso. PinPoint automatically uses the cloud solving service of Astrometry.Net to find its initial solution, then it takes that as the starting point for a full PinPoint solution including distortion mapping. An internet connection is usually employed for this (see below). PinPoint 7 also has built-in all-sky plate solving, eliminating the requirement for approximate image centerpoint coordinates and plate scale at the cost of additional time. It is 70Gb for coverage down to magnitude 18 and 160 Gb for coverage down to magnitude 20. If you can afford the space, this is now the best catalog for all uses. ![]() This large, including Gaia stars and PanSTARRS/APASS magnitudes, has high quality magnitudes, it goes deep, and has proper motions. ![]() New with Version 7 is support for the ATLAS All-Sky Stellar Reference Catalog. Both 32- and 64-bit engines are available. A set of point-and-click tools (Visual PinPoint) for fast mass plate solving and survey-level asteroid and supernova hunting are included. Since hail can cause the rainfall estimates to be higher than what is actually occurring, steps are taken to prevent these high dBZ values from being converted to rainfall.Welcome to the web site for the PinPoint Astrometric Engine, a programmable engine that provides sensitive, robust, high-speed research-grade astrometric image processing for FITS files from any camera. Hail is a good reflector of energy and will return very high dBZ values. These values are estimates of the rainfall per hour, updated each volume scan, with rainfall accumulated over time. Depending on the type of weather occurring and the area of the U.S., forecasters use a set of rainrates which are associated to the dBZ values. The higher the dBZ, the stronger the rainrate. Typically, light rain is occurring when the dBZ value reaches 20. The scale of dBZ values is also related to the intensity of rainfall. The value of the dBZ depends upon the mode the radar is in at the time the image was created. ![]() Notice the color on each scale remains the same in both operational modes, only the values change. The other scale (near left) represents dBZ values when the radar is in precipitation mode (dBZ values from 5 to 75). One scale (far left) represents dBZ values when the radar is in clear air mode (dBZ values from -28 to +28). Each reflectivity image you see includes one of two color scales. The dBZ values increase as the strength of the signal returned to the radar increases. So, a more convenient number for calculations and comparison, a decibel (or logarithmic) scale (dBZ), is used. Reflectivity (designated by the letter Z) covers a wide range of signals (from very weak to very strong). "Reflectivity" is the amount of transmitted power returned to the radar receiver. The colors are the different echo intensities (reflectivity) measured in dBZ (decibels of Z) during each elevation scan. ![]()
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