The High Energy Astrophysics Science Archive Research Center (HEASARC) is the primary archive for NASA's (and other space agencies') missions studying electromagnetic radiation from extremely energetic cosmic phenomena ranging from black holes to the Big Bang. Since its merger with the Legacy Archive for Microwave Background Data Analysis (LAMBDA) in 2008, the HEASARC archive contains data obtained by high-energy astronomy missions observing in the extreme-ultraviolet (EUV), X-ray, and gamma-ray bands, as well as data from space missions, balloons, and ground-based facilities that have studied the relic cosmic microwave background (CMB) radiation in the sub-mm, mm and cm bands.

The HEASARC is a member of the NASA Astronomical Virtual Observatories (NAVO) where we work with other NASA archives to ensure comprehensive and consistent VO access to NASA mission datasets. Users may now query the HEASARC's catalogs using VO-enabled services and specialized tools. This page describes how to get to the HEASARC VO-enabled services and provides information on other HEASARC VO activities.

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Enter positions, times, missions, etc to query the HEASARC database.

Try ROSAT 3c273 1d to get ROSAT data within one degree of 3C273 or chanmaster bii>80 status='archived' to get archived Chandra observation data near the north galactic pole.

Note: For more than one target or when using any qualifier other than a mission, use quotes around targets that have embedded white space.(e.g., 'ar lac').

More information and examples


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Latest News
  • NuSTAR Probes Puzzling Galaxy Merger (28 Mar 2017)
    A supermassive black hole (SMBH) inside a tiny galaxy is challenging scientists' ideas about what happens when two galaxies merge. Was 49 is the name of a system consisting of a large disk galaxy, referred to as Was 49a, merging with a much smaller "dwarf" galaxy called Was 49b. The dwarf galaxy rotates within the larger galaxy's disk, about 26,000 light years from its center. Using NuSTAR, Secrest et al. (2017, ApJ, 836, 183), have discovered that the dwarf galaxy is so luminous in high-energy X-ray, it must host an SMBH much larger and more powerful than expected for such a lightweight.
  • BETA Pilot Multi-Epoch Continuum Survey of Spitzer SPT Deep Field (24 Mar 2017)
    This catalog of 3,722 radio source components detected by the Boolardy Engineering Test Array (BETA) prototype of the Australian Square Kilometre Array Pathfinder (ASKAP) in the 711-1015 MHz band in 150 sq. deg. covering two-thirds of the Spitzer South Pole Telescope Deep Field (from Heywood et al. 2016, MNRAS, 457, 4160) is now available in Browse and Xamin.
  • Andromeda's Bright Hard X-Ray Mystery Source Identified by NuSTAR (24 Mar 2017)
    The Milky Way's close neighbor galaxy Andromeda (M 31), features a dominant source of high-energy X-ray emission, but its identity has been mysterious until now. As reported in a new study by Yukita et al. (2017, ApJ, in press), NASA's NuSTAR (Nuclear Spectroscopic Telescope Array) mission has pinpointed the object responsible for this high-energy radiation to be Swift J0042.6+4112, a possible pulsar, the dense remnant of a dead star that is highly magnetized and spinning.
  • Viewing tool updated (23 Mar 2017)
    Swift's orbital pole constraints have been updated in the Viewing tool. The revised coefficients extrapolate the trend for the next year.
  • NICER expected launch date: May 14, 2017 (21 March 2017)
    NICER is currently scheduled for launch to the ISS on May 14, 2017 from the Kennedy Space Center.
  • NASA's Swift Mission Maps a Star's 'Death Spiral' into a Black Hole (21 Mar 2017)
    Some 290 Myrs ago, a star much like the sun wandered too close to the central black hole of its galaxy. Intense tides tore the star apart, which produced an eruption of optical, UV and X-ray light that first reached Earth in 2014. Now, a team of scientists using observations from Swift have mapped out how and where these different wavelengths were produced in the event, named ASASSN-14li, as the shattered star's debris circled the black hole: see Pasham et al. (2017, ApJ837, L30) for the full details.

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Last modified: Wednesday, 29-Mar-2017 00:30:08 EDT