- ID:
- ivo://nasa.heasarc/skyview/cdfs-less
- Title:
- LABOCA Extended Chandra Deep Field South Submillimetre Survey
- Short Name:
- CDFS LESS
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The LABOCA Extended Chandra Deep Field South (ECDFS) Submillimetre Survey (LESS) is a public legacy survey of the ECDFS at 870 μm using the LABOCA camera (Siringo et al. 2009) on the APEX telescope. <p> The LABOCA data presented here were obtained between 2007 May and 2008 November in excellent conditions using time from both ESO and Max Planck allocations. The mapping pattern was designed to uniformly cover the 30'x30' extent of the ECDFS, centered on 03:32:29.0, -27:48:47.0 (J2000). The project used a total of 310 hrs of observations to achieve a beam-smoothed noise of 1.2 mJy/beam over 900 sq. arcmin (and <1.6mJy/beam over 1260 sq. arcmin). The flux calibration of the map came from observations of Mars, Uranus and Neptune (as well as secondary calibrators) and is accurate to within 8.5%. Provenance: Data downloaded from ESO archive. This is a service of NASA HEASARC.
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- ID:
- ivo://nasa.heasarc/lpffiles
- Title:
- LISA Pathfinder Archive Data Summary
- Short Name:
- LPFFILES
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table provides an index for a time ordered set of files containing the telemetry from the the DRS system on the LISA Pathfinder mission. It gives the time in a variety of spacecraft modes for each file. Note that not all modes were explored during the LISA Pathfinder mission. The Disturbance Reduction System (DRS) was an experiment package aboard the European Space Agency (ESA) LISA Pathfinder spacecraft. LISA Pathfinder (LPF) launched from Kourou, French Guiana, on December 3, 2015. LPF successfully demonstrated the disturbance-free motion of two test masses at a noise level acceptable for a future gravitational wave (GW) observatory. Designated ST7, DRS is the NASA contribution to LPF with the goal of operating disturbance reduction technology in space applicable to GW missions and other future missions with challenging stability requirements. DRS flew two clusters of four, low-noise, colloid micro-thrusters (eight total) and a computer which implemented drag-free control laws. At specific times during the LPF mission, DRS operated as alternative to the ESA provided thrusters and control laws. The location of the test masses relative to the spacecraft and the attitude of the spacecraft were measured by ESA subsystems and provided to DRS as its sensors. The displacement and attitude of the spacecraft relative to the two test masses was controlled using the colloid thrusters and electrostatic forces on the TMs provided by the LPF systems. The key requirements for DRS were to show that the thrust noise was less than 0.1 micro-N, and the spacecraft position noise was less than 10nm/sqrt( Hz) in the measurement frequency band of 1 to 30 micro-Hz. ST7 also recorded the relative acceleration noise (delta-g) between the two test masses, a key metric for the GW application, but had no requirement did not optimize the delta-g performance because this is primarily dependent on the (ESA) inertial sensor. ST7 executed a primary mission in which the thrust noise of the thrusters and the performance of the drag free control were measured and a short extended mission which was used to optimize the performance and expand the operating range of the thrusters and control laws. This table was created by the HEASARC in February 2018 based on data files provided by Jacob Slutsky and Leonid Petrov, which were reformatted from the base files at the LISA Pathfinder archive at ESA. The reformatted data files are available at <a href="https://heasarc.gsfc.nasa.gov/FTP/lpf/data/fits/">https://heasarc.gsfc.nasa.gov/FTP/lpf/data/fits/</a> with summaries of the instrument mode intervals available in summary files in <a href="https://heasarc.gsfc.nasa.gov/FTP/lpf/data/summ/">https://heasarc.gsfc.nasa.gov/FTP/lpf/data/summ/</a>. This is a service provided by NASA HEASARC .
133. MAXI Master Catalog
- ID:
- ivo://nasa.heasarc/maximaster
- Title:
- MAXI Master Catalog
- Short Name:
- MAXIMASTER
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The MAXIMASTER database table records high-level information of the Monitor of All-sky X-ray Image (MAXI) observations and provides access to the data archive. MAXI is a Japanese experiment located at the International Space Station (ISS), designed to continuously monitor, through a systematic survey, X-ray sources as the ISS orbits Earth. MAXI was launched by the space shuttle Endeavour on 2009 July 16, then mounted on port No. 1 on JEM-EF on July 24. After the electric power was turned on, MAXI started nominal observations on 2009 August 3. The MAXI data are a copy of the MAXI data processing; the output of which is hosted at the DARTS archive located at ISAS (<a href="https://darts.isas.jaxa.jp/astro/maxi/">https://darts.isas.jaxa.jp/astro/maxi/</a>). This catalog is then generated at the HEASARC by collecting high-level information from the data and is updated regularly during operation. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/skyview/mellinger
- Title:
- Mellinger All Sky Mosaic: Red
- Short Name:
- MELLINGER
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This all sky mosaic was created by Axel Mellinger and is used in <i>SkyView</i> with his permission. A fuller description is available at the <a href="https://www.milkywaysky.com/">survey website</a>. <p> Between October 2007 and August 2009 a digital all-sky mosaic was assembled from more than 3000 individual CCD frames. Using an SBIG STL-11000 camera, 70 fields (each covering 40x27 degrees) were imaged from dark-sky locations in South Africa, Texas and Michigan. In order to increase the dynamic range beyond the 16 bits of the camera's analog-to-digital converter (of which approximately 12 bits provide data above the noise leve) three different exposure times (240s, 15s and 0.5 s) were used. Five frames were taken for each exposure time and filter setting. The frames were photometrically calibrated using standard catalog stars and sky background data from the Pioneer 10 and 11 space probes. the panorama has an image scale of 36"/pixel and a limiting magnitude of approximately 14. The survey has an 18 bit dynamic range. <p> The processing of these data used a custom data pipeline built using IRAF, Source Extractor and SWarp. <p> The data used here were converted to three independent RGB color planes of 8 bits each and provided to SkyView as a single 36000x18000x3 Cartesian projection cube. To allow users to efficiently sample data in a region of the sky, this cube was broken up into 2100x2100 pixel regions with a 50 pixel overlap between adjacent images. Tiles at the poles were 2100x2050. <p> In <i>SkyView</i> each color plane comprises a survey. The individual planes may be sampled as surveys independently as Mellinger-R, Mellinger-G and Mellinger-B. The color mosaics can be regenerated by creating an RGB image of all three surveys. Since <i>SkyView</i> may stretch the intensity values within each color, linear scaling and a minimum of 0 and maximum of 255 should be specified to keep the original intensity scalings. <p> The full spatial resolution data is used for images of less than 30 degrees on a side. If a user requests a larger region, data are sampled from a lower resolution 3600x1800x3 data cube. Please contact the survey author if you need to use the higher resolution data for larger regions. The Mellinger survey is only available in <i>SkyView</i> through the website. SkyView-in-a-Jar cannot access the underlying data. Provenance: Axel Mellinger. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/skyview/pmn
- Title:
- 4850 MHz Survey - GB6/PMN
- Short Name:
- PMN
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The 4850MHz data is a combination of data from three different surveys: Parkes-MIT-NRAO (PMN) Southern (-88&#176;; to -37&#176;; declination) and tropical surveys (-29&#176;; to -9&#176;; declination, and (86+87) Green Bank survey (0&#176;; to +75&#176;; declination). The data contains gaps between -27&#176;; to -39&#176;;, -9&#176;; to 0&#176;;, and +77&#176;; to +90&#176;; declination. The 4850MHz survey data were obtained by tape from J.J. Condon and are comprised of 576 images and are used by permission. Full information pertaining to these surveys are found in the references.<P> Provenance: NRAO, generated by J.J. Condon, J.J. Broderick and G.A. Seielstad, Douglas, K., and Gregory, P.C.. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/skyview/dss2
- Title:
- 2nd Digitized Sky Survey (Blue)
- Short Name:
- DSS2
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- <P> The native projection of these data is described as a high-order polynomial distortion of a gnomonic projection using the same terms as the DSS. Provenance: Data taken by ROE, AAO, and CalTech, Compression and distribution by Space Telescope Science Institute.. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/skyview/neat
- Title:
- Near-Earth Asteriod Tracking System Archive
- Short Name:
- NEAT
- Date:
- 29 Apr 2022
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The NEAT/SkyMorph survey provides access to the archives of the Near Earth Asteroid Tracking (NEAT) project. NEAT is designed to look for potentially hazardous asteroids, i.e., those whose orbits cross the Earth's. Over 200,000 images are available in the NEAT archive. <a href=https://skyview.gsfc.nasa.gov/skymorph/skymorph.html>SkyMorph</a> provides a Web interface to the NEAT images and allows users to select all images in which a given fixed or moving object is found. <p> Unlike most <i>SkyView</i> surveys, the NEAT data are extremely irregular in their spatial distribution. <i>SkyView</i>'s algorithms for mosaicking images together to form large images are not adequate for the NEAT data, so mosaicking is surpressed. Only data within a single NEAT image will be displayed. The system attempts to find the most recent image within which has a offset in both RA and Dec of less than 0.8 degrees. If no such image is found, then an image with the minimum offset is returned, or the search may fail altogether if there are no nearby plates. The NEAT telescope uses an array of 4 CCDs. The backgrounds of the CCDs may differ significantly. <p> The NEAT survey covers approximately 30% of the sky. Extreme southern and low-Galactic latitude regions are unsurveyed. Coverage is otherwise particularly dense in the ecliptic plane. <p> NEAT data consists primarily of groups of three images taken with separations of 20 minutes and almost identical positions. <i> SkyView </i> will normally return the last of a 'triplet'. The SkyMorph site can be used to display an overlay of triplets to look for targets which moved during the interval between images. <p> A catalog of objects detected in the NEAT/SkyMorph pages is accessible through the SkyMorph pages. 'Light-curves' from all images during which an object was in the NEAT field of view can also be generated. <P> The NEAT data values are in arbitrary density units. To enhance the display data are transformed such that all pixels below the median values are scaled linearly to values 0-20, while all pixels above the median are shifted (but not scaled) to values greater than 20.
138. NICER Master Catalog
- ID:
- ivo://nasa.heasarc/nicermastr
- Title:
- NICER Master Catalog
- Short Name:
- NICERMASTR
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This table records high-level information for the observations obtained with NICER (Neutron star Interior Composition ExploreR) and provides access to the NICER data archive. NICER is a NASA Explorer program Mission of Opportunity dedicated to the study of the neutron stars, exploring the exotic states of matter where density and pressure are higher than in atomic nuclei. NICER instrument is a payload aboard the International Space Station (ISS). It was launched on 3 June 2017 on a SpaceX Falcon 9 rocket and placed on the ISS. Normal operation started on 17 July 2017 after a commission phase to test the system and perform initial calibration. NICER's X-ray Timing Instrument (XTI) consists of an aligned collection of 56 X-ray "concentrator" optics (XRC) and silicon drift detector (SDD) pairs working in the energy range of 0.2-12 keV. Each XRC collects X-rays over a large geometric area from a roughly 30 arcmin<sup>2</sup> region of the sky and focuses them onto a small SDD. The SDD detects individual photons, recording both energies (with a 3% energy resolution at 6 keV) and high precision times (with 100 nanoseconds RMS relative to Universal Time). During one day of operation, NICER monitors several sources. For each observed source the data are divided into intervals of one day and labeled with a sequence number. This database table contains one record for each sequence number and includes parameters related to the observation. This contents of this database table are generated at the NICER Science and Mission Operations Center (SMOC) and updated regularly with new observations. Note that some fields have been added and are populated by the HEASARC. This is a service provided by NASA HEASARC .
- ID:
- ivo://nasa.heasarc/skyview/intgal1735e
- Title:
- Nine Year INTEGRAL IBIS 17\-35 keV Galactic Plane Survey: Exposure
- Short Name:
- INTGAL1735E
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This survey combines 9 years of INTEGRAL IBIS observations from December 2002 through January 2011 into a single Galactic Plane image. A total of 135 megaseconds of exposure is included in the observations used. Survey data is generated for the Galactic plane in the region |b| <= 17.5. The original flux data has been convolved with 5' seeing kernel. To minimize loss of resolution in transformations, the Lanczos sampler is suggested as the default, but may be overriden by the user. Both the preconvolved and standard convolved maps are available at the <a href="https://web.archive.org/web/20170620112312/https://hea.iki.rssi.ru/integral/nine-years-galactic-survey/index.php">Website</a>. <p> The exposure and sensitivity vary considerably over the coverage region, but 90% of the field has a limiting sensitivity better than 2.2 x 10<sup>-11</sup>ergs s<sup>-1</sup>cm<sup>-2</sup> or about 1.56 mCrab. Further details of the survey construction are given in the reference. <p> The flux and significance maps use the PSF convolved maps from the survey. The flux maps are in millicrab units. Exposure maps (with exposures in seconds) were from the exposure extension in the MAPDLD files and give the dead-time corrected exposure in seconds. <p> Links to the exposure and significance maps corresponding to the requested region will be given in the Web output. These maps can be generated directly in the CLI interface. For each waveband the flux, significance and exposure maps are available with just the end of the survey names distinguishing them (e.g., INT Gal 17-35 [Flux|Sig|Exp] or INTGal1735[F|S|E]) Provenance: <a href="https://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1205.3941">Krivonos et al., 2012</a><br> Based on observations with INTEGRAL, an ESA project with instruments and science data centre funded by ESA member states (especially the PI countries: Denmark, France, Germany, Italy, Switzerland and Spain), Poland, and participation of Russia and the USA.. This is a service of NASA HEASARC.
140. NRA) VLA Sky Survey
- ID:
- ivo://nasa.heasarc/skyview/nvss
- Title:
- NRA) VLA Sky Survey
- Short Name:
- NVSS
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- <i> SkyView </i> has copied the NVSS intensity data from the NRAO FTP site. The full NVSS survey data includes information on other Stokes parameters. <p> Observations for the 1.4 GHz NRAO VLA Sky Survey (NVSS) began in 1993 September and should cover the sky north of -40 deg declination (82% of the celestial sphere) before the end of 1996. The principal data products are: <ol> <li> A set of 2326 continuum map "cubes," each covering 4 deg X 4 deg with three planes containing Stokes I, Q, and U images. These maps were made with a relatively large restoring beam (45 arcsec FWHM) to yield the high surface-brightness sensitivity needed for completeness and photometric accuracy. Their rms brightness fluctuations are about 0.45 mJy/beam = 0.14 K (Stokes I) and 0.29 mJy/beam = 0.09 K (Stokes Q and U). The rms uncertainties in right ascension and declination vary from 0.3 arcsec for strong (S > 30 mJy) point sources to 5 arcsec for the faintest (S = 2.5 mJy) detectable sources. <li> Lists of discrete sources. </ol> The NVSS is being made as a service to the astronomical community, and the data products are being released as soon as they are produced and verified. <P> The NVSS survey is included on the <b>SkyView High Resolution Radio Coverage </b><a href="https://skyview.gsfc.nasa.gov/images/high_res_radio.jpg"> map</a>. This map shows coverage on an Aitoff projection of the sky in equatorial coordinates. <p> Provenance: National Radio Astronomy Observatory. The NVSS project includes J. J. Condon, W. D. Cotton, E. W. Greisen, Q. F. Yin, R. A. Perley (NRAO), and J. J. Broderick (VPI).. This is a service of NASA HEASARC.
