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341. OSO8 A Detector Lightcurves
ID:
ivo://nasa.heasarc/oso8alc
Title:
OSO8 A Detector Lightcurves
Short Name:
OSO8ALC
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
This database accesses the FITS lightcurves obtained from the A detector part of the GSFC Cosmic X-ray Spectroscopy experiment (GCXSE) on board OSO8. The Orbiting Solar Observatory-I (OSO-8) was launched on 21 June 1975 into a 550 km circular orbit at 33 degrees inclination. While the primary objectives of the mission were solar in nature, there were 3 detectors (the GCXSE detectors A, B and C) which had exclusively non-solar objectives. The energy band was 2-60 keV for the A and C detector and 2-20 keV for the B detector. The spacecraft structure consisted of a rotating cylindrical base section called the "wheel" and a non-spinning upper section called the "sail". The GCXSE detectors were mounted in the rotating wheel and their fields-of-view were either aligned to the spin axis (B and C) or at small angles to it (A), hence they always viewed the portion of the sky at right angles to the earth-sun line. The GCXSE detectors obtained data until late September 1978. This is a service provided by NASA HEASARC .
342. OSO8B&CDetectorLightcurves
ID:
ivo://nasa.heasarc/oso8bclc
Title:
OSO8B&CDetectorLightcurves
Short Name:
OSO8BCLC
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
OSO8 B&C Detector Lightcurves This is a service provided by NASA HEASARC .
343. OSO8 GCXSE Raw PHA
ID:
ivo://nasa.heasarc/oso8pharaw
Title:
OSO8 GCXSE Raw PHA
Short Name:
OSO8PHARAW
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
The Orbiting Solar Observatory-I (OSO-8) was launched on 21 June 1975 into a 550 km circular orbit at 33 degrees inclination. Data were obtained from the mission until late September 1978. The spacecraft structure consisted of a rotating cylindrical base section called the "wheel" and a non-spinning upper section called the "sail". While the primary objectives of the mission were solar in nature, there were 3 detectors, the GSFC Cosmic X-ray Spectroscopy experiments (GCXSE detectors A, B, and C), mounted in the rotating wheel which had exclusively non-solar objectives. Their fields-of-view were either aligned to the spin axis or at small angles to it, hence they always view the portion of the sky at right angles to the earth-sun line. This database accesses the pha FITS datafiles for the A, B, and C GCXSE detectors. Data was accumulated every quarter of a rotation period (~2.56 s) for the A detector and every 40.96 s for the B and C detectors in the 2-60 keV energy band. This is a service provided by NASA HEASARC .
344. OSO8 GCXSE Raw Rates
ID:
ivo://nasa.heasarc/oso8rtraw
Title:
OSO8 GCXSE Raw Rates
Short Name:
OSO8RTRAW
Date:
07 Mar 2025
Publisher:
NASA/GSFC HEASARC
Description:
The Orbiting Solar Observatory-I (OSO-8) was launched on 21 June 1975 into a 550 km circular orbit at 33 degrees inclination. Data were obtained from the mission until late September 1978. The spacecraft structure consisted of a rotating cylindrical base section called the "wheel" and a non-spinning upper section called the "sail". While the primary objectives of the mission were solar in nature, there were 3 detectors, the GSFC Cosmic X-ray Spectroscopy experiments (GCXSE detectors A, B and C), mounted in the rotating wheel which had exclusively non-solar objectives. Their fields-of-view were either aligned to the spin axis or at small angles to it, hence they always view the portion of the sky at right angles to the earth-sun line. This database accesses the raw rates FITS datafile for the A, B and C GCXSE detectors, accumulated every 160 ms in the 2-60 keV energy band. This is a service provided by NASA HEASARC .
345. PACS Evolutionary Probe
ID:
ivo://irsa.ipac/Herschel/Images/PEP
Title:
PACS Evolutionary Probe
Short Name:
PEP
Date:
27 Oct 2022 19:00:00
Publisher:
NASA/IPAC Infrared Science Archive
Description:
The PACS Evolutionary Probe (PEP, Lutz et al. 2011) is a Herschel guaranteed time deep extragalactic survey (KPGT_dlutz_1) targeting six among the most popular "blank fields", ten lensing clusters of galaxies, and two z ~1 clusters at wavelengths of 100 and 160 microns. PEP includes SPIRE observations of the two z ~1 clusters at wavelengths of 250, 350, and 500 microns. SPIRE coverage of all other fields is available from the HerMES survey (Oliver et al. 2010). In addition, deep SPIRE GOODS-N data are provided by the GOODS-Herschel program (Elbaz et al. 2011).
346. PACS Highly Processed Data Products
ID:
ivo://irsa.ipac/Herschel/Images/PHPDP
Title:
PACS Highly Processed Data Products
Short Name:
PHPDP
Date:
27 Oct 2022 19:00:00
Publisher:
NASA/IPAC Infrared Science Archive
Description:
All Herschel observations are processed through an automatic pipeline, which corrects a number of instrumental artifacts. The Highly Processed Data Products (HPDP) have gone through additional interactive processing, and represent an improvement over the standard products. HPDP from Herschel's Photoconductor Array Camera and Spectrometer (PACS) are available for JScanam maps, Unimap maps, and Red Leak Spectra.
347. Palomar survey digitized by MAMA
ID:
ivo://padc.obspm.astro/posse/q/siap
Title:
Palomar survey digitized by MAMA
Short Name:
posse_siap
Date:
16 Jul 2024 00:01:13
Publisher:
Paris Astronomical Data Centre
Description:
Survey from Palomar Image plates Digitized using MAMA at Observatoire de Paris .All the image have been resampled and reprojected TAN
348. Panchromatic Hubble Andromeda Treasury (PHAT)
ID:
ivo://mast.stsci/phat
Title:
Panchromatic Hubble Andromeda Treasury (PHAT)
Short Name:
PHAT
Date:
23 Jul 2020 19:28:22
Publisher:
Space Telescope Science Institute Archive
Description:
The Panchromatic Hubble Andromeda Treasury is a Hubble Space Telescope Multi-cycle program to map roughly a third of M31's star forming disk, using 6 filters covering from the ultraviolet through the near infrared. With HST's resolution and sensitivity, the disk of M31 will be resolved into more than 100 million stars, enabling a wide range of scientific endeavors.
349. P60 GRBCam
ID:
ivo://irsa.ipac/P60/Images/GRBCam
Title:
P60 GRBCam
Short Name:
GRBCam
Date:
24 Aug 2023 19:31:00
Publisher:
NASA/IPAC Infrared Science Archive
Description:
During the years 2004 to 2017, the Palomar 60 inch telescope (P60) operated as a fully robotic facility to obtain targeted optical observations of gamma-ray burst (GRB) afterglows and other transient events. An automated pipeline reduced the data in real time. The raw, calibration, and pipeline-processed data are available here.
350. Planck 030 GHz Survey
ID:
ivo://nasa.heasarc/skyview/planck030
Title:
Planck 030 GHz Survey
Short Name:
Planck030
Date:
03 Dec 2018
Publisher:
NASA/GSFC HEASARC
Description:
Planck is ESA's third generation space based cosmic microwave background experiment, operating at nine frequencies between 30 and 857 GHz and was launched May 2009. Planck provides all-sky survey data at all nine frequencies with higher resolution at the 6 higher frequencies. It provides substantially higher resolution and sensitivity than WMAP. Planck orbits in the L2 Lagrange point. These data come from Release 1 of the Planck mission. <p> The original data are stored in HEALPix pixels. SkyView treats HEALPix as a standard projection but assumes that the HEALPix data is in a projection plane with a rotation of -45 degrees. The rotation transforms the HEALPix pixels from diamonds to squares so that the boundaries of the pixels are treated properly. The special HealPixImage class is used so that SkyView can use the HEALPix FITS files directly. The HealPixImage simulates a rectangular image but translates the pixels from that image to the nested HEALPix structure that is used by the HEALPix data. Users of the SkyView Jar will be able to access this survey through the web but performance may be poor since the FITS files are 150 to 600 MB in size and must be completely read in. SkyView will not automatically cache these files on the user machine as is done for non-HEALPix surveys. </p> Data from the frequencies of 100 GHz or higher are stored in a HEALPix file with a resolution of approximately 1.7' while lower frequencies are stored with half that resolution, approximately 3.4'.

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