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- ID:
- ivo://nasa.heasarc/skyview/wfcf
- Title:
- ROSAT Wide Field Camera: F1
- Short Name:
- WFCF
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- This survey is a mosaic of images taken by the ROSAT Wide Field Camera and comprises of 12,743 seperates fields in each of two filters. Each field covers a region 2.6°; x 2.6°; with a 0.3°; overlap. Currently, this data is not a complete coverage of the sky; regions near the northern ecliptic pole are currently not included. Provenance: University of Leicester. This is a service of NASA HEASARC.
- ID:
- ivo://nasa.heasarc/skyview/rxte3_20k_flux
- Title:
- RXTE Allsky 3\-20 keV Flux
- Short Name:
- RXTE3_20k_flux
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- Rossi X-ray Timing Explorer was launched at the end of 1995 and up to now (2004) it has been successfully operating for more than 7 years. The mission was primarily designed to study the variability of X-ray sources on time scales from sub-milliseconds to years. The maneuvering capability of the satellite combined with the high photon throughput of its main detector (PCA) and high quality of background prediction (thanks to PCA intrumental group of LHEA, GSFC) has also made it possible to construct maps of the sky in energy band 3-20 keV. During its life time RXTE/PCA has collected a large amount of data from slew observations covering almost the entire sky. <p> We have utilized the slew parts of all RXTE/PCA observations performed from April 15, 1996-July 16, 2002 which amounts in total to approximately 50,000 observations. The exposure time at a given point in the map is typically between 200-500 seconds. The observational period before April 15, 1996 (High Voltage Epochs 1 and 2) was excluded from the analysis because during that time the PCA had significantly different gain and dependence of the effective area on energy. The data reduction was done using standard tools of the LHEASOFT with a set of packages written by M. Revnivtsev (HEAD/IKI, Moscow; MPA, Garching).<p> <p> The survey has several features. It has strongly different exposure times at different points on the sky that lead to strong variability of the statistical noise on images. Because of that the only meaningful representation of images is the map in units of statistical significance. After the detection of a source flux can be determined from the map in the 'flux' units. Map resolution is determined mainly by the slew rate of the RXTE (<0.05-0.1&#176;;/sec) and the time resolution of used data (16 sec, Std2 mode of the PCA). Sources can be detected down to the level of ~6e<sup>-12</sup> erg/s/cm<sup>2</sup>, but at this level the confusion starts to play an important role. Details of the survey are presented in the paper of Revnivtsev et al. (2004). Provenance: High Energy Astrophysics Department, Space Research Institute, Moscow, Russia; M PA, Garching, Germany. This is a service of NASA HEASARC.
- ID:
- ivo://org.gavo.dc/sasmirala/q/im
- Title:
- Sasmirala Subarcsecond mid-infrared atlas of local AGN
- Short Name:
- sasmirala atlas
- Date:
- 27 Dec 2024 08:31:05
- Publisher:
- The GAVO DC team
- Description:
- These FITS images were generated with the IDL package MIRphot [Asmus2014]_ by extraction (and combination) of the sub-images from the chopped/nodded total images from COMICS, Michelle, T-ReCS and VISIR (see [Asmus2014]_ for details). The FITS images contain the central ~4 arcsec of each source centered on the (putative) nuclear position with North being up and East to the left. The WCS registration has been performed after extraction by using coordinates of the nucleus from other wavelengths (mostly 2MASS and NED). The uncertainty of these reference position is usually less than 1 arcsec. In addition, the imprecision of the assignment itself is ~1px ~ 0.1". The FITS images are flux calibrated (unit is mJy) using the Gaussian 2D fits to the corresponding STD observation (where available, otherwise using the median conversion factor for the used instrument/filter settings). Therefore, correction factors have to be applied in case other flux measurement methods are applied to the images. The flux values given in the FITS headers should be regarded as approximate values. In particular for the instruments, VISIR and COMICS, they are not necessarily exactly equal to the values provided in the photometry results table, because many flux measurements were performed during the process of combining individual subimages (all in MIRphot), instead of in the final combined image, provided here. The used total images are available upon request. Note, however, that these are just the products of the observatory-delivered pipelines with default parameters. .. [Asmus2014] Asmus D., Hoenig S.F., Gandhi P., Smette A., Duschl W.: The subarcsecond mid-infrared view of local active galactic nuclei: I. The N- and Q-band imaging atlas, `2014MNRAS.439.1648A <http://ads.ari.uni-heidelberg.de/abs/2014MNRAS.439.1648A>`_
- ID:
- ivo://org.gavo.dc/plts/q/data
- Title:
- Scans of the Palomar-Leiden Trojan Survey Plates
- Short Name:
- plts.data
- Date:
- 27 Dec 2024 08:31:13
- Publisher:
- The GAVO DC team
- Description:
- This service publishes plate scans of the Palomar-Leiden Troian surveys conducted between 1960 and 1977. The surveys led to the discovery of more than 2,000 asteroids (1,800 with orbital information), with another 2,400 asteroids, including 19 Trojans, found after further analysis of the plates. Note that because of the large size of the plates, in this service each original plate is contained in two parts, marked with "_1" and "_2", respectively. The central parts of the two parts overlap.
- ID:
- ivo://nasa.heasarc/skyview/sfd
- Title:
- Schlegel, Finkbeiner and Davis dust\ map survey
- Short Name:
- SFD
- Date:
- 07 Mar 2025
- Publisher:
- NASA/GSFC HEASARC
- Description:
- The full sky 100 micron map is a reprocessed composite of the COBE/DIRBE and IRAS/ISSA maps, with the zodiacal foreground and confirmed point sources removed. Artifacts from the IRAS scan pattern were removed. The result of these manipulations is a map with DIRBE-quality calibration and IR AS resolution. Provenance: David J. Schlegel, Douglas P. Finkbeiner and Marc Davis, Princeton University and University of California, Berkeley. This is a service of NASA HEASARC.
- ID:
- ivo://chivo/alma_fits/q/siap-alma-fits
- Title:
- Simple Image Access for ALMA FITS
- Short Name:
- SIAP ALMA FITS
- Date:
- 06 Nov 2017 14:35:31
- Publisher:
- ChiVO
- Description:
- The resource contains the recommendations and requirements for ALMA FITS products of the Inter-ARC ALMA Science Archive Working Group (ASAWG) with the view to including a metadataset that is complete and easily accessible by the ChiVO Data Provider (CDP).
- ID:
- ivo://nasa.heasarc/skyview/skyview
- Title:
- SkyView Virtual Observatory
- Short Name:
- SkyView
- Date:
- 06 Apr 2021
- Publisher:
- NASA/GSFC HEASARC
- Description:
- SkyView is a Virtual Observatory on the Net. Astronomers can generate images of any portion of the sky at wavelengths in all regimes from radio to gamma-ray. Users tell SkyView the position, scale and orientation desired, and SkyView gives users an image made to their specification. The user need not worry about transforming between equinoxes or coordinate systesm, mosaicking submaps, rotating the image,.... SkyView handles these geometric issues and lets the user get started on astronomy.
- ID:
- ivo://sdss.jhu/services/SIAPDR4-Color
- Title:
- Sloan Digital Sky Survey DR4
- Short Name:
- SDSSDR4-Color
- Date:
- 14 Feb 2012 18:49:17
- Publisher:
- The Johns Hopkins Univer
- Description:
- The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey
- ID:
- ivo://sdss.jhu/services/SIAPDR3-Color
- Title:
- Sloan Digital Sky Survey DR3
- Short Name:
- SDSSDR3-Color
- Date:
- 14 Feb 2012 18:48:16
- Publisher:
- The Johns Hopkins Univer
- Description:
- The Sloan Digital Sky Survey is a project to survey a 10000 square degree area on the Northern sky over a 5 year period. A dedicated 2.5m telescope is specially designed to take wide field (3 degrees in diameter) images using a 5x6 mosaic of 2048x2048 CCD`s, in five wavelength bands, operating in drift scan mode. The total raw data will exceed 40 TB. A processed subset, of about 1 TB in size, will consist of 1 million spectra, positions and image parameters for over 100 million objects, plus a mini-image centered on each object in every color. The data will be made available to the public after the completion of the survey
