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| Chandra Image of E6 Galaxy NGC 4697 |
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The adaptively smoothed Chandra X-ray image of the central region of the X-ray-faint elliptical galaxy NGC 4697. The image shows that most of the X-ray emission is resolved by Chandra into about 80 Low Mass X-ray Binary (LMXB) star systems, which contain accreting massive black holes and neutron stars (Sarazin, Irwin, & Bregman 2000, 2001) |
| Hydra A Chandra Image |
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| Chandra X-ray image of the central region of the cluster of galaxies (Abell 780) surrounding the radio galaxy Hydra A. This image shows a radio (green and maroon) overlay on the Chandra X-ray (pink and blue) image of Hydra A. It shows that the radio lobes are displacing and being confined by the 40 million degree X-ray gas in the cluster (McNamara et al. 2000). |
| Hydrodymical Simulation of Cluster Merger |
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| Hydrodynamical simulation of a merger of two identical clusters of galaxies. The colors show temperature (red=hotter, blue=cooler), while the contours are X-ray surface brightness. The red regions are merger shocks ( Ricker & Sarazin 2001a, 2002b). |
| Abell 2052 Chandra Image |
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| The Chandra X-ray Observatory image (false color) of the central part of the cooling flow cluster of galaxies Abell 2052, with contours of the radio emission overlaid. The radio source has blown "bubbles" in the hot X-ray gas. The radio source is in turn being confined by the X-ray gas (Blanton et al. 2001, 2003). |
| Chandra X-ray/Radio Overlay of Cluster Abell 133 |
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The adaptively smoothed Chandra X-ray image of the central region of the cluster Abell 133 is shown in red. The VLA radio image is shown in green. The yellow region to the lower left is the central cD galaxy, which is a radio source and a peak in the X-ray emission. A red "tongue" of X-ray emission extends from the cD galaxy to the spidery green radio relic source at the upper center (Fujita et al. 2002, 2003, 2004,). |
| Chandra Image of Merging Abell 85 Cluster of Galaxies |
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| The Chandra ACIS-I image of the merging cluster of galaxies Abell 85. Two smaller clusters to the southwest and south are merging with the main cluster, which as a cooling flow at its center. The southern subcluster has a "cold front" (a contact discontinuity with cooler gas from the subcluster core) at its northern edge. ( Kempner, Sarazin, & Ricker 2002a, 2002b, 2002c). |
| Chandra Image of Elliptical Galaxy NGC 4649 (M60) |
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| The Chandra ACIS-S image of the X-ray-bright elliptical galaxy NGC 4649 (M60). Both X-ray binary sources and diffuse gaseous X-ray emission are shown. (Randall, Sarazin, & Irwin 2004). |
| Chandra Image of E Galaxy/Group NGC 1600 |
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| The Chandra ACIS-S color image (red = soft, blue = hard) of the X-ray emission around the elliptical galaxy NGC 1600. The image shows galactic gas, group gas, a tail of gas stripped from NGC 1603 (group member), and very luminous X-ray sources, which may contain intermediate mass black holes. (Sivakoff, Sarazin, & Carlin 2004). |