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SN 1006 Supernova Remnant

Supernova remnants expand over time. Since the remnant from the SN 1006 event is near to us, we can see the outward expanision of the filament in the accompanying photo. This image of visible hydrogen emission in the NW filament of SN 1006 is from data taken with the Hubble ACS detector (Raymond et. al) in 2006. BY PLACING YOUR MOUSE IN THE IMAGE, you can now see the comparison image of H-alpha data taken at the CTIO 0.9m telescope (Winkler, et al.) in 1998. The stellar background remains constant and is from WFPC2 broadband B, V, and I data from 2008 (Hubble Heritage Team).

Illustration Credit: NASA, ESA, and L. Frattare (STScI)
Science Credit: Hubble data: NASA, ESA, and the Hubble Heritage Team (STScI/AURA); CTIO data: F.Winkler/Middlebury College and NOAO/AURA/NSF

(Roll mouse over image to see expansion motion.)

Full-shell Image of SN 1006 Showing Location of Hubble Observations

This image is a composite of visible (or optical), radio, and X-ray data of the full shell of the supernova remnant from SN 1006. The radio data show much of the extent that the X-ray image shows. In contrast, the visible light stems primarily from a small delicate filament along the northwest rim of the shell. The entire object has an angular size of roughly 30 arcminutes (0.5 degree, or about the size of the full moon), and a physical size of 60 light-years (18 parsecs) based on its distance of nearly 7,000 light-years. The small green box along the bright filament at the top of the image corresponds to the dimensions of the Hubble release image.

The optical data were obtained at the University of Michigan’s 0.9-meter Curtis Schmidt telescope at the National Science Foundation’s Cerro Tololo Inter-American Observatory (CTIO) near La Serena, Chile. CTIO is part of the National Optical Astronomy Observatory, which has its headquarters in Tucson, Ariz. H-alpha, continuum-subtracted data were provided by F. Winkler (Middlebury College) et al. The X-ray data were acquired from the Chandra X-ray Observatory’s AXAF CCD Imaging Spectrometer (ACIS) at 0.5-3keV, and were provided by J. Hughes (Rutgers University) et al. The radio data, supplied by K. Dyer and collaborators Maddalena and Cornwell (NRAO, Socorro), were a composite from the National Radio Astronomy Observatory’s Very Large Array (NRAO/VLA) in Socorro, New Mexico, along with NRAO's Green Bank Telescope (GBT) in Green Bank, West Virginia. These radio data were a mosaic at the 1.4 GHz frequency. Data of the supernova remnant were blended on a visible-light stellar background created using the Digitized Sky Survey’s Anglo-Australian Observatory (AAO2) blue and red plates.

Photo Credit: NASA, ESA, and Z. Levay (STScI)
Science Credit:
Radio: NRAO/AUI/NSF GBT+VLA 1.4 GHz mosaic (Dyer, Maddalena and Cornwell, NRAO);
X-ray: NASA/CXC/Rutgers/G. Cassam-Chenai and J. Hughes et al.;
Optical: F.Winkler/Middlebury College and NOAO/AURA/NSF; and DSS