The smoothed 0.3 - 8 keV map of the inner portion of the NGC 4410 group from the Chandra X-ray Telescope (color), after it has been divided by a smoothed weighted exposure map. The yellow/white regions are brightest in X-rays, the red fainter, and the blue faintest. The black region outside of the blue rectangular area was not observed by Chandra. The contours are from the optical Digitized Sky Survey.

The smoothed Chandra 0.3 - 1 keV map of the inner portion of the NGC 4410 group (color), after it has been divided by a smoothed 0.8 keV monochromatic exposure map. The contours are from the optical Digitized Sky Survey.

The 1 - 2.5 keV map, after it has been divided by a smoothed 1.5 keV monochromatic exposure map. The contours are from the optical Digitized Sky Survey.

The smoothed Chandra 2.5 - 8 keV map of the inner portion of the NGC 4410 group (color), after it has been divided by a smoothed 3 keV monochromatic exposure map. The contours are from the optical Digitized Sky Survey.

To see how different assumptions in making the exposure map affects the final Chandra image, click here.

To return to Beverly Smith's home page, click here
To look at my poster on NGC 4410 from the Gas and Galaxy Evolution Conference, click here.
To read my conference proceedings for that meeting, click here.
To read my paper on the atomic and molecular interstellar gas in the NGC 4410 galaxy group (Smith 2000, Ap. J., 541, 624), click here.
To read the Donahue, Smith, and Stocke paper on star formation in NGC 4410A+B, click here. (2002, AJ, 123, 1922).
Soon to come: Smith et al. (2003) paper on the Chandra observations of NGC 4410.

Last updated: 4/14/03