An Overview of the Performance and Scientific Results from the Chandra X‐Ray Observatory

By M. Weisskopf, B. Brinkman, C. Canizares, G. Garmire, S. Murray, L. V. Speybroeck. 2001

660 citations recorded by the source corpus.

The Chandra X‐Ray Observatory (CXO), the X‐ray component of NASA’s Great Observatories, was launched on 1999 July 23 by the space shuttle Columbia. After satellite systems activation, the first X‐rays focused by the telescope were observed on 1999 August 12. Beginning with the initial observation it was clear that the telescope had survived the launch environment and was operating as expected. Despite an initial surprise due to the discovery that the telescope was far more efficient for concentrating CCD‐damaging low‐energy protons than had been anticipated, the observatory is performing well and is returning superb scientific data. Together with other space observatories, most notably XMM‐Newton, it is clear that we have entered a new era of discovery in high‐energy astrophysics.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/9199931e93dc155f8b9e4b09f01abc1eb743b8b8

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Citations in the corpus

• THE CHANDRA COSMOS SURVEY. I. OVERVIEW AND POINT SOURCE CATALOG (2009, methodology): “– 5 – 0.9 sq.deg region of the COSMOS field (Fig.1, left), containing a wide range of cosmic overdensity (Fig.1, right), with the ACIS-I CCD imager (Garmire et al. 2003) on board the Chandra X-ray Observatory (Weisskopf et al. 2002).”
• The Cosmic Evolution of Hard X-Ray-selected Active Galactic Nuclei (2004, background): “The Chandra samples of Table 1 now contain 1165 spectroscopically observed sources and 715 spectroscopically identified sources.”
• 10 MK Gas in M17 and the Rosette Nebula: X-Ray Flows in Galactic H II Regions (2003, methodology): “3. chandraOBSERVATIONS AND ANALYSIS The HII regions were observed with the Imaging Array of Chandra’s Advanced CCD Imaging Spectrometer (ACIS-I); the observatory and instrument are described by Weisskopf et al. (2002).”
• An Overabundance of Transient X-Ray Binaries within 1 Parsec of the Galactic Center (2004, methodology): “The region within 10′ of Sgr A∗ has been observed sixteen times between 1999–2004 with the Advanced CCD Imaging Spectrometer imaging array (ACIS-I) aboard the Chandra X-ray Observatory (Weisskopf et al. 2002).”
• THE CHANDRA COSMOS LEGACY SURVEY: OVERVIEW AND POINT SOURCE CATALOG (2016, background): “Instead, for the faint and the high-z AGN population, that could be responsible for the re-ionization of the Universe (see Giallongo et al. 2015), Chandra (Weisskopf et al. 2002) is the preferred instrument.”
• The stellar rotation–activity relationship in fully convective M dwarfs (2018, methodology): “2.2 Chandra X-ray observations The targets were observed with the Advanced CCD Imaging Spectrometer (ACIS; Garmire et al. 2003) on board the Chandra Xray Observatory (Weisskopf et al. 2002) as part of programmes 14200934 (PI: Wright), 17200636 (PI: Williams), and 18200661 (PI: Wright).”
• A Neutron Star with a Massive Progenitor in Westerlund 1 (2005, methodology): “We observed Westerlund 1 with the Chandra X-ray Observatory Advanced CCD Spectrometer Spectroscopic array (ACIS-S)Weisskopf et al. (2002) on two occasions: 2005 May 22 for 18 ks (sequence 5411) and 2005 June 18 for 42 ks (sequence 6283).”
• THE CHANDRA COSMOS SURVEY. III. OPTICAL AND INFRARED IDENTIFICATION OF X-RAY POINT SOURCES (2012, methodology): “…observation strategy, now also used in otherChandrasurveys (e.g., Drake et al. 2009), combined with the sub-arcsecond on-axisChandrapoint spread function (PSF, Weisskopf et al. 2002), provides a rather uniform sensitivity in C-COSMOS (see Paper I and Puccetti et al. 2009, Paper II, for details).”
• Active galactic nuclei: what’s in a name? (2017, background): “Chandra (launched July 1999; Weisskopf et al. 2002) provides up-to subarcsecond imaging at ≈0.3–8 keV with sufficient collecting area for high S/N X-ray spectra of bright X-ray sources.”
• The X-Ray Observatory Suzaku (2007, positive): “Suzaku was designed to be highly complementary to the two large X-ray observatories that were already in orbit at launch, XMM-Newton (Jansen et al. 2001) and Chandra (Weisskopf et al. 2002).”
• An Exploratory Chandra Survey of a Well-defined Sample of 35 Large Bright Quasar Survey Broad Absorption Line Quasars (2006, methodology): “A Chandra Survey of 35 LBQS BAL Quasars 7 The lack of correlation between DI and ∆αox is surprising based on prior expectations from disk-wind models.”
• Diffuse X-Ray Emission in a Deep Chandra Image of the Galactic Center (2004, methodology): “The inner 20 pc of the Galaxy have been observed on twelve occasions as of June 2002 (Table 1) using the Advanced CCD Imaging Spectrometer imaging array (ACISI) aboard the Chandra X-ray Observatory (Weisskopf et al. 2002).”
• Occultation Measurement of the Size of the X-Ray-emitting Region in the Active Galactic Nucleus of NGC 1365 (2007, methodology): “All the observations were performed with the ACIS-S instrument (Weisskopf et al. 2002) in ’1/4 window’ mode in order to avoid possible pile-up.”
• Chandra Orion Ultradeep Project: Observations and Source Lists (2004, methodology): “The observations were obtained with the ACIS camera on-board Chandra, which are described by Weisskopf et al. (2002) and Garmire et al. (2003).”
• The X-Ray Telescope onboard Suzaku (2007, background): “Another type of X-ray telescope is one that achieves the ultimate imaging capability with accurate Wolter-I optics, which is onboard the Chandra X-ray Observatory (Weisskopf et al. 2002).”
• Advanced CCD imaging spectrometer (ACIS) instrument on the Chandra X-ray Observatory (2003, positive): “The Advanced CCD Imaging Spectrometer (ACIS) on board the Chandra X-ray Observatory(CXO) [1] is a powerful tool for conducting imaging, spectroscopic and temporal studies of celestial X-ray sources.”
• X-ray background measurements with XMM-Newton EPIC (2002, background): “In this case the recovered spectra are statistically identical with a large selection of observations made with ACIS outside the Chandra focal point (Biller et al 2002).”