Search

Start Over Subject surveys Resource Type Archive
11. Digitized First Byurakan Survey (DFBS) Plate Scans
ID:
ivo://org.gavo.dc/dfbs/q/i
Title:
Digitized First Byurakan Survey (DFBS) Plate Scans
Short Name:
DFBS plates
Date:
27 Dec 2024 08:31:04
Publisher:
The GAVO DC team
Description:
First Byurakan survey plate scan service
12. Digitized First Byurakan Survey (DFBS) Spectra Query Service
ID:
ivo://org.gavo.dc/dfbsspec/q/getssa
Title:
Digitized First Byurakan Survey (DFBS) Spectra Query Service
Short Name:
DFBS SSAP
Date:
27 Dec 2024 08:31:13
Publisher:
The GAVO DC team
Description:
The First Byurakan Survey (FBS) is the largest and the first systematic objective prism survey of the extragalactic sky. It covers 17,000 sq.deg. in the Northern sky together with a high galactic latitudes region in the Southern sky. The FBS has been carried out by B.E. Markarian, V.A. Lipovetski and J.A. Stepanian in 1965-1980 with the Byurakan Observatory 102/132/213 cm (40"/52"/84") Schmidt telescope using 1.5 deg. prism. Each FBS plate contains low-dispersion spectra of some 15,000-20,000 objects; the whole survey consists of about 20,000,000 objects.
13. Digitized Sky Survey
ID:
ivo://eso.org/dss
Title:
Digitized Sky Survey
Short Name:
DSS ESO
Date:
05 Jul 2021 08:18:13
Publisher:
ESO
Description:
The Online Digitized Sky Surveys (DSS1 & 2) server at the ESO/ST-ECF Archive provides access to the CD-ROM set produced by the Space Telescope Science Institute through its Guide Star Survey group. The images of these surveys are based on photographic data obtained using the Oschin Schmidt Telescope on Palomar Mountain and the UK Schmidt Telescope. The plates were processed into the present compressed digital form with the permission of these institutions. The photographic plates were scanned to a pixel scale of about 1.7 arcseconds per pixel for the POSS, SERC, and Palomar Quick-V surveys, and to about 1.0 arcseconds per pixel for the POSS-II surveys. Images of any part of the sky may be extracted from the DSS, in either FITS or GIF format.
14. DRAO 22 MHz Survey
ID:
ivo://nasa.heasarc/skyview/22mhz
Title:
DRAO 22 MHz Survey
Short Name:
22MHz
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
Roger et al. (1999) presented a map of the 22 MHz radio emission between declinations -28° and +80°, covering ~73% of the sky, derived from observations with the 22 MHz radiotelescope of the Dominion Radio Astrophysical Observatory (DRAO). The resolution of the telescope (EW x NS) is 1.2° x 1.7° secant(zenith angle). Roger et al. emphasize that the main value of the data lies in the representation of structure larger than the beam. The strongest point sources (Cas A, Cyg A, Tau A and Vir A) have been removed from the map. <p> The Centre d'Analyse de Données Etendues group used the data to form an all-sky HEALPix format map following the method described in Appendix A of Paradis et al. 2012, A&A, 543, 103, ADS. Their HEALPix map is mirrored here. The map is in units of K brightness temperature. Map pixels are set to a sentinel value of -32768.0 for unobserved regions and for regions affected by sidelobes around Cyg A, Tau A, and Vir A. Provenance: DRAO, MPI for Radio Astronomie. This is a service of NASA HEASARC.
15. Effelsberg-Bonn HI Survey
ID:
ivo://nasa.heasarc/skyview/ebhis
Title:
Effelsberg-Bonn HI Survey
Short Name:
EBHIS
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
The Effelsberg-Bonn HI Survey (EBHIS) is a 21-cm survey performed with the 100-m telescope at Effelsberg. It covers the whole northern sky out to a redshift of z ~ 0.07 and comprises HI line emission from the Milky Way and the Local Volume. This dataset is the atomic neutral hydrogen (HI) column density map derived from the Milky-Way part of EBHIS (|Vlsr| < 600 km/s). Provenance: Argelander-Institut f&uuml;r Astronomie (AIfA) and Max-Planck-Institut f&uuml;r Radioastronomie (MPIfR); data provided by B. Winkel. This is a service of NASA HEASARC.
16. Energetic Gamma-Ray Event Telescope: 10 channel data
ID:
ivo://nasa.heasarc/skyview/egret3d
Title:
Energetic Gamma-Ray Event Telescope: 10 channel data
Short Name:
EGRET3D
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
These data are from the Compton GRO EGRET team. Data are from all pointings of the EGRET instrument in the verification phase and phase 1-4 of the Compton mission. The maps exist in energies 30-100 MeV, 100-10000 MeV, and as a multi-dimensional, 10 channel survey. For the multi-dimensional survey, channels 1-3 comprise energies less than 100 MeV, and channels 4-10 comprise energies greater than 100 MeV. Note that the energies are not uniformly split among the channels. <P> The EGRET 3D map is comprised of ten channels with the following energy ranges: <UL> <LI>Channel 1 30-50 MeV <LI>Channel 2 50-70 MeV <LI>Channel 3 70-100 MeV <LI>Channel 4 100-150 MeV <LI>Channel 5 150-300 MeV <LI>Channel 6 300-500 MeV <LI>Channel 7 500-1000 MeV <LI>Channel 8 1000-2000 MeV <LI>Channel 9 2000-4000 MeV <LI>Channel 10 4000-10000 MeV </ul> <p> The default two dimensional image for the EGRET 3D survey is an average of Channels 4 - 10 (energies greater than 100 MeV). Provenance: EGRET Instrument team, NASA Goddard Space Flight Center. This is a service of NASA HEASARC.
17. Energetic Gamma-Ray Event Telescope: Hard
ID:
ivo://nasa.heasarc/skyview/egret
Title:
Energetic Gamma-Ray Event Telescope: Hard
Short Name:
EGRET
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
These data are from the Compton GRO EGRET team. Data are from all pointings of the EGRET instrument in the verification phase and phase 1-4 of the Compton mission. The maps exist in energies 30-100 MeV, 100-100000 MeV, and as a multi-dimensional, 10 channel survey. For the multi-dimensional survey, channels 1-3 comprise energies less than 100 MeV, and channels 4-10 comprise energies greater than 100 MeV. Note that the energies are not uniformly split among the channels. <P> The EGRET 3D map is comprised of ten channels with the following energy ranges: <UL> <LI>Channel 1 30-50 MeV <LI>Channel 2 50-70 MeV <LI>Channel 3 70-100 MeV <LI>Channel 4 100-150 MeV <LI>Channel 5 150-300 MeV <LI>Channel 6 300-500 MeV <LI>Channel 7 500-1000 MeV <LI>Channel 8 1000-2000 MeV <LI>Channel 9 2000-4000 MeV <LI>Channel 10 4000-10000 MeV </ul> <p> The default two dimensional image for the EGRET 3D survey is an average of Channels 4 - 10 (energies greater than 100 MeV). Provenance: EGRET Instrument team, NASA Goddard Space Flight Center. This is a service of NASA HEASARC.
18. Extreme Ultraviolet Explorer
ID:
ivo://archive.stsci.edu/euve
Title:
Extreme Ultraviolet Explorer
Short Name:
EUVE
Date:
22 Jul 2020 21:28:51
Publisher:
Space Telescope Science Institute Archive
Description:
Launched in June, 1992, The Extreme Ultraviolet Explorer (EUVE) conducted the first extreme ultraviolet (70-760 Angstroms) survey of the sky and subsequently began a Guest Observer Program of pointed
19. Extreme Ultraviolet Explorer: 83 A
ID:
ivo://nasa.heasarc/skyview/euve
Title:
Extreme Ultraviolet Explorer: 83 A
Short Name:
EUVE
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
The EUVE satellite surveyed the entire sky in the extreme ultraviolet through a set of four filters. The filters include: <UL> <LI>Lexan/Boron filter: peak at 83A (full range 50-180) <LI>Aluminium/Carbon/Titanium : 171A (160-240) <LI>Aluminium/Titanium/Antimony: 405A (345-605) <LI>Tin/SiO: 555A (500-740) </UL> <P> The data currently in <i>SkyView</i> is direct from the Center for EUVE. Provenance: Center for Extreme UV Astronomy, UCB. This is a service of NASA HEASARC.
20. Fermi Map: Band 1
ID:
ivo://nasa.heasarc/skyview/fermi
Title:
Fermi Map: Band 1
Short Name:
FERMI
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
This survey sums all data observed by the Fermi mission up to week 396. This version of the Fermi survey are intensity maps where the summed counts data are divided by the exposure for each pixel (in cm^2 s) and the area of the pixel. Data is broken into 5 energy bands <ul> <li> 30-100 MeV Band 1 </li> <li> 100-300 MeV Band 2 </li> <li> 300-1000 MeV Band 3 </li> <li> 1-3 GeV Band 4 </li> <li> 3-300 GeV Band 5 </li> </ul> The SkyView data are based upon a Cartesian projection of the counts divided by the exposure maps. In the Cartesian projection pixels near the pole have a much smaller area than pixels on the equator, so these pixels have smaller integrated flux. When creating large scale images in other projections users may wish to make sure to compensate for this effect the flux conserving clip-resampling option. Provenance: Fermi LAT instrument team, NASA Goddard Space Flight Center. This is a service of NASA HEASARC.