Mission Overview

NASA's Advanced X-ray Astrophysics Facility, (AXAF), renamed the Chandra X-ray Observatory in honor of Subrahmanyan Chandrasekhar, was launched and deployed by the Space Shuttle Columbia on the 23 of July 1999. The combination of high resolution, large collecting area, and sensitivity to higher energy X-rays will make it possible for Chandra to study extremely faint sources, sometimes strongly absorbed, in crowded fields. Chandra was boosted into an elliptical high-earth orbit that allows long-duration uninterrupted exposures of celestial objects.

The Chandra X-ray Observatory (formerly the Advanced X-ray Astrophysics Facility, or AXAF) was built around a high-resolution grazing incidence X-ray telescope which will make astrophysical observations in the 0.09 to 10.0 keV energy range. The principal science objectives of the mission were to determine the nature of celestial objects from normal stars to quasars, to understand the nature of physical processes which take place in and between astronomical objects, and to generally study the history and evolution of the universe. Observations will be made of X-rays from high energy regions such as supernova remnants, X-ray pulsars, black holes, neutron stars, and hot galactic clusters.

The spacecraft has a cone-shaped body with an octagonal structure surrounding the wide end. Two solar panel wings extend from opposite sides of the structure. The main opening is at the wide end covered by a sunshade door with a contamination cover. An aspect camera and stray light shade are mounted near the opening and two low-gain antennas and two fine Sun sensors are affixed to the outside structure. Thermal control is maintained by a radiator, insulators, heaters, and thermostats. Power generated by the solar panels is stored in three banks of batteries.

The X-ray telescope consists of four nested paraboloid-hyperboloid X-ray mirror pairs, arranged in concentric cylinders within the cone. The four instruments are located near the focus at the narrow end of the cone: the High Resolution Camera (HRC), the CCD Imaging Spectrometer (ACIS), High Energy Transmission Grating Spectrometer (HETGS), and the Low Energy Transmission Grating (LETG).

Lifetime: 23 July 1999 - (nominal 5 year mission)
Energy Range: 0.1-10 keV
Special Features: 64 Hours highly-eccentric Earth orbit.
Spatial resolution ‹ 1 arcsec
Launch Information
Launch Date: 1999-07-23 at 11:47:00 UTC
Launch Vehicle: Shuttle
Launch Site: Cape Canaveral, United States

Trajectory Description
Type: Orbiter
Central Body: Earth
Epoch start: 1999-07-23 13:55:12 UTC
Epoch stop: 1999-08-04 20:24:00 UTC

Orbital Parameters
Periapsis 9942.0 km
Apoapsis 140000.0 km
Period 64.0 hours
Inclination 28.5°
Eccentricity 0.7993800044059753

Type: Orbiter
Central Body: Earth
Epoch start: 1999-08-04 20:24:00 UTC

Orbital Parameters
Periapsis 10037.0 km
Apoapsis 140012.0 km
Period 64.19999694824219 hours
Inclination 28.459999084472656°
Eccentricity 0.7983499765396118

A single Wolter Type 1 grazing incidence iridium-coated imaging telescope with a ghost free FOV ~ 30´ diameter and an effective area of 800 and 400 cm2 @ 0.25 and 5 keV respectively. Four detectors could be inserted, one at a time, into the focal plane. Two of these were designed to be used primarily with the gratings.
• AXAF Charged Coupled Imaging Spectrometer (ACIS; 0.2-10 keV) 2 CCD arrays for a total of 10 chips. 8 chips are Front Illuminated (FI) and 2 are Back Illuminated (BI).
  FI: Eff area 340 cm2 @ 1 keV, E/dE = 20-50 @ 1 and 6 keV
  BI: Eff area 340 cm ‹ 2 @ 1 keV, E/dE = 9-35 @ 1 and 6 keV
    o ACIS-I. One 4-chip imaging array, all FI. FOV 16´ X 16´     o ACIS-S. One 6-chip spectroscopic array, 4 FI and 2 BI FOV 8´ X 48´. To be used primarily with the grating.

• High Resolution Camera (HRC; 0.1-10 keV) 2 micro-channel plate detectors.
    o HRC-I One 90mm square detector optimized for imaging. FOV ~30´ X 30´, eff. area 225 cm2 @ 1 keV, ~ 0.5 arcsec spatial resolution
    o HRC-S One 20 X 300 mm rectangular detector optimized for use with the LETG transmission gratings experiment. FOV 7´ X 97´
• High Energy Transmission Grating + ACIS-S (HETG; 0.5-10 keV) spectral resolving power (E/dE) 60-1000.
• Low Energy Transmission Grating + HRC-S (LETG; 0.08-6 keV) spectral resolving power (E/dE) 30-2000.


February 27, 2009

The oldest isolated pulsar ever detected in X rays has been found with NASA's Chandra X-ray Observatory. This very old and exotic object turns out to be surprisingly active.

The pulsar, PSR J0108-1431, is about 200 million years old. Among isolated pulsars - ones that have not been spun-up in a binary system - it is more than 10 times older than the previous record holder with an X-ray detection. At a distance of 770 light-years, it is one of the nearest pulsars known.

A pulsar is born when a star much more massive than the Sun collapses in supernova explosions, leaving behind a small, incredibly weighty core, known as a neutron star. At birth, these neutron stars, which contain the densest material known in the universe, are spinning rapidly, up to 100 revolutions per second. Distant observers see the rotating beams of their radiation as pulses, similar to a lighthouse beam. Astronomers call them "pulsars."

Astronomers observe a gradual slowing of the rotation of the pulsars as they radiate energy away. Radio observations of J0108 show it to be one of the oldest and faintest pulsars known, spinning only slightly faster than 1 revolution per second.

The surprise came when a team of astronomers led by George Pavlov of Penn State University observed J0108 in X rays with Chandra. They found that it glows much brighter in X rays than was expected for a pulsar of such advanced years.

Some of the energy that J0108 is losing as it spins more slowly is converted into X-ray radiation. The efficiency of this process for J0108 is found to be higher than for any other known pulsar.

"This pulsar is pumping out high-energy radiation much more efficiently than its younger cousins," said Pavlov. "So, although it's clearly fading as it ages, it is still holding its own with the younger generations."

It's likely that two forms of X-ray emission are produced in J0108: emission from particles spiraling around magnetic fields, and emission from heated areas around the neutron star's magnetic poles. Measuring the temperature and size of these heated regions can provide valuable insight into the extraordinary properties of the neutron star surface and the process by which the pulsar accelerates charged particles.

The younger, bright pulsars commonly detected by radio and X-ray telescopes are not representative of the full population of objects, so observing objects like J0108 helps astronomers see a complete range of behavior. At its advanced age, J0108 is close to the so-called "pulsar death line." Its pulsed radiation is expected to switch off, and it will become much harder, if not impossible, to observe.

"We can now explore the properties of this pulsar in a regime where no other pulsar has been detected outside the radio range," said co-author Oleg Kargaltsev of the University of Florida. "To understand the properties of 'dying pulsars,' it is important to study their radiation in X rays. Our finding that a very old pulsar can be such an efficient X-ray emitter gives us hope to discover new nearby pulsars of this class via their X-ray emission."

The extreme nature of J0108 was not fully apparent until a new distance to it was reported February 6 by Adam Deller from Swinburne University in Australia. The new distance is both larger and more accurate than the distance used in the Chandra paper, showing that J0108 was brighter in X rays than previously thought.

"Suddenly this pulsar became the record holder for its ability to make X rays," said Pavlov, "and our result became even more interesting without us doing much extra work."

The position of the pulsar seen by Chandra in X rays in early 2007 is slightly different from the radio position observed in early 2001. This implies that the pulsar is moving at a velocity of about 440,000 mph (708,000 km/h), close to a typical value for pulsars.

Currently, the pulsar is moving south from the plane of the Milky Way Galaxy, but, because it is moving more slowly than the escape velocity of the galaxy, it will eventually curve back toward the plane of the galaxy in the opposite direction.

The detection of this motion has allowed Roberto Mignani of University College London, in collaboration with Pavlov and Kargaltsev, to possibly detect J0108 in optical light, using estimates of where it should be found in an image taken in 2000. Such a multi-wavelength study of old pulsars is critical for understanding the long-term evolution of neutron stars, including how they cool with time and how their powerful magnetic fields evolve.