Spectra Precision Survey Pro 5.0 Crack
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Survey Office software is ideal for processing and analyzing GPS and GNSS, and optical survey data recorded in the field, and exporting it to a design package. The software provides numerous innovative and unique features, and it is easy to learn and use. With Survey Office software on your PC you have the ability to work with RTK and Static/PPK data to generate reports as well as identify and correct field errors. Import data from existing surveys or directly from the Internet and export data as points, or in CAD or XML format. Rest assured that your data is secure and reliable with built-in quality assurance and quality control features. The intuitive, integrated Survey Office program saves time with its short learning curve and powerful features.
Survey data acquired in the field using a total station and contained in a data file can be imported into the software and integrated as necessary with other data collected as part of a survey project (for example, GNSS or level data).
The Survey Office software provides surveyors and engineers with advanced technology, integrating common tasks into a single system. Process and review RTK, Static, FastStatic, and stop-and-go Kinematic data. Survey Office also performs data reduction, computation, QA/QC and network adjustment. Control data can be exported to the field software for use in the field.
Spectra Geospatial is an established brand known for delivering quality products to the survey, GIS and construction markets. Focusing on the specific needs of the conventional surveying market, the Spectra Geospatial brand offers a complete product portfolio including Global Navigation Satellite Systems (GNSS), Global Positioning Systems (GPS), optical total stations, data collection hardware, field and office software, as well as a wide range of construction tools.
Spectra Geospatial surveying equipment is an economical choice that utilizes technologies for optimal efficiency. With convenience and reliability as the foundation of the Spectra Geospatial brand, it is an ideal choice for value. The Spectra Geospatial brand is backed with the strong technical support that users have come to expect from a quality name in surveying and construction.
Spectra Geospatial motorized total station solutions combine high-speed, accuracy and precision in measurement with streamlined workflows to maximize productivity. Spectra digital levels determine accurate height information immediately and eliminate errors.
Spectra Geospatial field software solutions for surveying, GIS and mapping provide a clear and consistent data collection standard, optimized workflows and connectivity from field to office. Our office software solutions process the field data efficiently and accurately for quality results and implementation of design back to the field.
Spectra Precision Survey Office software is ideal for processing and analyzing GPS and GNSS, and optical survey data recorded in the field, and exporting it to a design package. The software provides numerous innovative and unique features, and it is easy to learn and use. With Spectra Precision Survey Office software on your PC you have the ability to work with RTK and Static/PPK data to generate reports as well as identify and correct field errors. Import data from existing surveys or directly from the Internet and export data as points, or in CAD or XML format. Rest assured that your data is secure and reliable with built-in quality assurance and quality control features. The intuitive, integrated Spectra Precision Survey Office program saves time with its short learning curve and powerful features.
The Spectra Precision Survey Office software provides surveyors and engineers with advanced technology, integrating common tasks into a single system. Process and review RTK, Static, FastStatic, and stop-and-go Kinematic data. Spectra Precision Survey Office also performs data reduction, computation, QA/QC and network adjustment. Control data can be exported to the field software for use in the field.
Spectra Precision has long been an established brand, belonging to Trimble Inc., known for delivering quality products to the survey and construction markets. Spectra Precision offers a complete survey equipment product portfolio including Global Navigation Satellite Systems (GNSS), Global Positioning Systems (GPS), optical total stations, laser systems, data collection hardware, field and office software, as well as a wide range of construction tools.
Spectra Precision surveying equipment is an economical choice that utilizes unique technologies for delivering maximum productivity with optimal efficiency. With convenience and reliability as the foundation of the Spectra Precision brand, it is an ideal choice for value. The Spectra Precision brand is backed with the strong technical equipment support that users have come to expect from a quality name in surveying and construction.
Everything contained in Survey Pro plus complete GPS/GNSS instrument support. Extensive data collection routines with easy to use, step-by-step setup features. Extensive support for projections and calibrations. All GNSS staking routines are supported. Support for RTK, Network RTK, static and PPK surveys.
Trimble and Spectra Precision provide their customers with a Stylesheet which can be used to convert conventional traverse data from the Trimble .job file or Spectra Precision Survey Pro .survey file directly to a STAR*NET format .dat file.
Survey Pro software is available in individual license modules that start with basic surveying project needs (Standard) and move into more advanced features and capabilities (Survey Pro). This can keep your costs down if you only need certain features in the field. You can also enable functionality with GPS / GNSS and robotic instruments by purchasing additional modules as necessary.
Featuring World Class Spectra Precision Field Software
Introducing the powerful Spectra Precision FOCUS 30 Total Station. This fully robotic motorized solution provides improved speed, accuracy and precision in measurement. A robotic instrument moves the power of the observer from the instrument to the range pole improving the quality of your work.
N2 - The Hobby-Eberly Telescope Dark Energy Experiment (HETDEX) is an unbiased, massively multiplexed spectroscopic survey, designed to measure the expansion history of the universe through low-resolution($R\sim750$) spectra of Lyman-Alpha Emitters. In its search for these galaxies, HETDEX will also observe a few 10$^5$ stars. In this paper, we present the first stellar value-added catalog within the internal second data release of the HETDEX Survey (HDR2). The new catalog contains 120,571 low-resolution spectra for 98,736 unique stars between$10 < G < 22$ spread across the HETDEX footprint at relatively high ($b\sim60^\circ$) Galactic latitudes. With these spectra, we measure radial velocities (RVs) for $\sim$42,000 unique FGK-type stars in the catalog and show that the HETDEX spectra are sufficient to constrain these RVs with a 1$\sigma$ precision of 28.0 km/s and bias of3.5 km/s with respect to the LAMOST surveys and 1$\sigma$ precision of27.5 km/s and bias of 14.0 km/s compared to the SEGUE survey. Since these RVs are for faint ($G\geq16$) stars, they will be complementary toGaia. Using t-Distributed Stochastic Neighbor Embedding (t-SNE), we also demonstrate that the HETDEX spectra can be used to determine a star'sT$\rmeff$, and log g and its [Fe/H]. With the t-SNE projection of the FGK-type stars with HETDEX spectra we also identify 416 newc andidate metal-poor ([Fe/H] $< -1$dex) stars for future study.These encouraging results illustrate the utility of future low-resolution stellar spectroscopic surveys.
AB - The Hobby-Eberly Telescope Dark Energy Experiment (HETDEX) is an unbiased, massively multiplexed spectroscopic survey, designed to measure the expansion history of the universe through low-resolution($R\sim750$) spectra of Lyman-Alpha Emitters. In its search for these galaxies, HETDEX will also observe a few 10$^5$ stars. In this paper, we present the first stellar value-added catalog within the internal second data release of the HETDEX Survey (HDR2). The new catalog contains 120,571 low-resolution spectra for 98,736 unique stars between$10 < G < 22$ spread across the HETDEX footprint at relatively high ($b\sim60^\circ$) Galactic latitudes. With these spectra, we measure radial velocities (RVs) for $\sim$42,000 unique FGK-type stars in the catalog and show that the HETDEX spectra are sufficient to constrain these RVs with a 1$\sigma$ precision of 28.0 km/s and bias of3.5 km/s with respect to the LAMOST surveys and 1$\sigma$ precision of27.5 km/s and bias of 14.0 km/s compared to the SEGUE survey. Since these RVs are for faint ($G\geq16$) stars, they will be complementary toGaia. Using t-Distributed Stochastic Neighbor Embedding (t-SNE), we also demonstrate that the HETDEX spectra can be used to determine a star'sT$\rmeff$, and log g and its [Fe/H]. With the t-SNE projection of the FGK-type stars with HETDEX spectra we also identify 416 newc andidate metal-poor ([Fe/H] $< -1$dex) stars for future study.These encouraging results illustrate the utility of future low-resolution stellar spectroscopic surveys.
The selection criteria for the subsample of CRATES sources observed by theOCRA-p are given in Section 2 of the reference paper (q.v.). Plots of themeasurements of each source over time and the aggregated source spectrabetween 26 MHz and 150 GHz are available online at the authors' web site: Bibcode2011MNRAS.410.2690PReferencesOne Centimetre Receiver Array-prototype observations of the CRATES sourcesat 30 GHz Peel M.W., Gawronski M.P., Battye R.A., Birkinshaw, M., Browne I.W.A., Davis R.J., Feiler R., Kus A.J., Lancaster K., Lowe S.R., Pazderka B.M., Pazderski E., Roukema B.F., Wilkinson P.N. =2011MNRAS.410.2690PProvenanceThis table was created by the HEASARC in May 2011 based on an electronicversion of Table 3 of the reference paper which was obtained from theauthors' web site Notice thatthe version here is the 10-Jan-2011 version which contains corrections to the30-GHz flux densities and their errors of 1% in the calibration and theapplication of the gain-elevation curve.ParametersName
The source designation in the generic style recommended by the Dictionary of Nomenclature of Celestial Objects, using the '[PGB2011]' prefix (for Peel, Gawronski, Battye 2011) and the J2000.0 equatorial coordinates truncated to 1 minute of time and 1 arcminute, e.g., '[PGB2011] J0954+7435'. No prefix is specified in the reference paper. By definition, these are all CRATES sources, but the CRATES source designation is higher precision in both coordinates: for example, the CRATES designation for this source is 'CRATES J095447+743549', hence the HEASARC created the '[PGB2011]' prefix.RA
The Right Ascension of the pointing for the 30-GHz observation in the selected equinox: this is that of the corresponding CRATES source, except for CRATES sources that have multiple components for which it is that of the brightest component. The position was given in J2000.0 equatorial coordinates to a precision of 0.1 seconds of time in the original table. For comparison, the OCRA beam is 1.2 arcminutes.Dec
The Declination of the pointing for the 30-GHz observation in the selected equinox: this is that of the corresponding CRATES source, except for CRATES sources that have multiple components for which it is that of the brightest component. The position was given in J2000.0 equatorial coordinates to a precision of 0.1 arcseconds in the original table. For comparison, the OCRA beam is 1.2 arcminutesLII
The Galactic Longitude of the 30-GHz pointing.BII
The Galactic Latitude of the 30-GHz pointing.Flux_20_cm
The flux density of the corresponding source in the CRATES Catalog at 1.4 GHz, in mJy.Flux_6_cm
The flux density of the corresponding source in the CRATES Catalog at 4.8 GHz, in mJy.Flux_3p6_cm
The flux density of the corresponding source in the CRATES Catalog at 8.4 GHz, in mJy.Flux_1_cm
The flux density of the source at 30 GHz as measured by the OCRA-p, in mJy.Flux_1_cm_Error
The uncertainty in the flux density of the source at 30 GHz as measured by the OCRA-p, in mJy. The methodology used for the OCRA-p flux density error calculation is discussed in Section 3 of the reference paper.Notes
This parameter can contain flags with various notes on the source properties. From an inspection of the NVSS (Condon et al. 1998, AJ, 115, 1693), Faint Images of the Radio Sky at Twenty Centimeters (FIRST; Becker, White and Helfand 1995, ApJ, 450, 559) and CLASS (Browne et al. 2003, MNRAS, 341, 13; Myers et al. 2003, MNRAS, 341, 1) data, it is clear that the majority of the CRATES sources are unresolved. A number do, however, show extension and/or multiple components; these are marked with a flag value of 'e'. Sources where multiple components listed in CRATES have been merged together are denoted by 'NC', where 'N' is the number of components. WMAP sources (Gold et al. 2011, ApJS, 192, 15) are marked with a 'w', CJF sources (Taylor et al. 1996, ApJS, 107, 37; Lowe et al. 2007, A&A. 474, 1093) are marked with a 'c' and Fermi point sources (Abdo et al. 2010, ApJS, 188, 405) are marked with an 'f' (see Section 5 of the reference paper for a fuller discussion of these issues). Potential gigahertz-peaked spectrum (GPS) sources are marked with a 'g (see Section 6 of the reference paper for a fuller discussion). The authors also note that there are two CLASS lens systems within the sample, J1609+6532 and J1938+6648 (Browne et al. 2003, MNRAS, 341, 13). There are 42 sources that appear variable within the OCRA measurements; these are marked with a 'v'. Sources were identified as variable if they were reasonably strong (> 20 mJy) and had two measurements which were 25% higher than the mean. Although sources with two measurements that are 25% lower than the mean could also be variable sources, these would be more contaminated by any sources with measurements that suffer from bad telescope pointing (and hence a reduced measured flux density) that have not been flagged. As such, the authors did not include these in the list of variable sources.Contact PersonQuestions regarding the CRATESOCRAP database table can be addressed to theHEASARC User Hotline.Page Author: Browse Software Development Team
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