COBE

DMR Images

The images below were created from the COBE DMR data products. Each image has been histogram equalized, giving a non-linear relation between color value and temperature. Use the data products for quantitative analysis. Additional images are available in the COBE Slide Set.

Before the full (four-year) DMR data set was calibrated and made into sky maps, preliminary maps based on 1-year and 2-year subsets of the data were created. While they have been superseded by the 4-year maps, these early renditions received much publicity. Thus we feature on this page both 2-year and 4-year DMR maps.

There is an important qualitative difference between the 2-year and 4-year maps having to do with the improved signal-to-noise ratio that results when more data are analyzed at once. The 4-year maps, which include twice as much data as the 2-year maps, have a signal-to-noise ratio roughly the square root of 2 (i.e., 1.4) times better than the 2-year maps. This modest improvement in map quality is sufficient to reveal individual features of the cosmic microwave background (CMB) in good contrast to the instrument noise. Due to the greater effect of instrument noise in the 2-year maps, those maps can be analyzed statistically to characterize the CMB fluctuations, but do not constitute accurate "pictures of the sky." However, in the final 4-year map, individual bright and faint spots represent actual CMB features. Illustrations of the major data analysis steps, and further explanations of the cosmic microwave background anisotropy (brightness fluctuations) are given below.

Maps Based on Two Years of DMR Observation

Cosmic microwave background temperature data were extracted from the released FITS files and then combined into two linear combinations. The first is a weighted sum of the 53 and 90 GHz channels which gives the highest signal-to-noise ratio for cosmic temperature variations but includes the Milky Way Galaxy as well. In the second linear combination, a multiple of the 31 GHz map is subtracted from a weighted sum of the 53 plus 90 GHz channels to give a "reduced map" that gives zero response to the observed Galaxy, zero response to free-free emission, but full response to variations in the cosmic temperature.

These maps have been smoothed with a 7 degree beam, giving an effective angular resolution of 10 degrees. An all-sky image in Galactic coordinates is plotted using the equal-area Mollweide projection. The plane of the Milky Way Galaxy is horizontal across the middle of each picture. Sagittarius is in the center of the map, Orion is to the right and Cygnus is to the left.

The following image is similar to the June 1992 Physics Today cover picture, with the map including the dipole and Galaxy on the top, the dipole removed map in the middle, and the reduced map on the bottom. The dipole, a smooth variation between relatively hot and relatively cold areas from the upper right to the lower left, is due to the motion of the solar system relative to distant matter in the universe. The signals attributed to this variation are very small, only one thousandth the brightness of the sky.

link to image of 3 maps
Click on the image to view the original

The following image just shows the reduced map (i.e., both the dipole and Galactic emission subtracted). The cosmic microwave background fluctuations are extremely faint, only one part in 100,000 compared to the 2.73 degree Kelvin average temperature of the radiation field. The cosmic microwave background radiation is a remnant of the Big Bang and the fluctuations are the imprint of density contrast in the early universe. The density ripples are believed to have given rise to the structures that populate the universe today: clusters of galaxies and vast regions devoid of galaxies.

link to CMB map with dipole and galactic emission subtracted
Click on the image to view the original

Maps Based on Observations Made Over the Entire 4-year Mission

Some of the features seen in the four-year maps below (i.e., dipole, Milky Way Galaxy) were described above. Like the two-year maps, the four-year maps have been smoothed to an effective angular resolution of 10 degrees. At this angular scale, the signal-to-noise ratio is sufficient (~2 per 10 degree patch) to portray for the first time an accurate visual impression of the cosmic microwave background (CMB) anisotropy.

The following image represents DMR data from the 53 GHz band (top) on a scale from 0 - 4 K, showing the near-uniformity of the CMB brightness, (middle) on a scale intended to enhance the contrast due to the dipole described above, and (bottom) following subtraction of the dipole component.

link to 3 DMR maps
Click on the image to view the original

The next image shows data obtained at each of the three DMR frequencies - 31.5, 53, and 90 GHz - following dipole subtraction.

link to an image of DMR maps at 3 frequencies
Click on the image to view the original

The following image shows the 53 GHz map (top) prior to dipole subtraction, (middle) after dipole subtraction, and (bottom) after subtraction of a model of the Galactic emission. The Galactic emission model is based on COBE/DIRBE far-infrared and Haslam et al. (1982) 408 MHz radio continuum observations (see Bennett et al. 1996, ApJ, 464, L1). Bennett et al. excluded an area around the Galactic plane referred to as the 'custom cut' region when they analyzed the CMB anisotropy. The excluded pixels are listed in two files that can be retrieved by anonymous ftp from the data/cobe/dmr/asds4 directory cmbdata.gsfc.nasa.gov.

link to image of 3 DMR maps at 53 GHz
Click on the image to view the original

Finally, here is the COBE-DMR "Map of the Early Universe." This false-color image shows tiny variations in the intensity of the cosmic microwave background measured in four years of observations by the Differential Microwave Radiometers on NASA's Cosmic Background Explorer (COBE). The cosmic microwave background is widely believed to be a remnant of the Big Bang; the blue and red spots correspond to regions of greater or lesser density in the early Universe. These "fossilized" relics record the distribution of matter and energy in the early Universe before the matter became organized into stars and galaxies. While the initial discovery of variations in the intensity of the CMB (made by COBE in 1992) was based on a mathematical examination of the data, the new picture of the sky from the full four-year mission gives an accurate visual impression of the data. The features traced in this map stretch across the visible Universe: the largest features seen by optical telescopes, such as the "Great Wall" of galaxies, would fit neatly within the smallest feature in this map. (Caption courtesy of Dr. Charles L. Bennett)

link to image of COBE-DMR map of the early universe
Click on the image to view the original




A service of the HEASARC and of the Astrophysics Science Division at NASA/GSFC
Goddard Space Flight Center, National Aeronautics and Space Administration
HEASARC Director: Dr. Alan P. Smale
LAMBDA Director: Dr. David T. Chuss
NASA Official: Dr. David T. Chuss
Web Curator: Mr. Michael R. Greason