M106 has also played an important role in calibrating the
cosmic distance ladder. Before,
Cepheid variables from other galaxies could not be used to measure distances since they cover ranges of
metallicities different from the Milky Way's. M106 contains Cepheid variables similar to both the metallicities of the Milky Way and other galaxies' Cepheids. By measuring the distance of the Cepheids with metallicities similar to our galaxy, astronomers are able to recalibrate the other Cepheids with different metallicities, a key fundamental step in improving quantification of distances to other galaxies in the universe. (*Wiki)
This was imaged with a Astro-Physics 155 EDFS. It's an oil filled 155mm objective with a 2.7 inch focuser.
9 x 600 secs IDAS D3
10 x 600 secs IDAS HUEIB
HISTORY 1 Stacking method SIGMA CLIP AVERAGE
HISTORY 2 De-mosaic bayer pattern used RGGB
HISTORY 3 Colour conversion: Bilinear interpolation interpolation.
EXPTIME = 11400. / Total luminance exposure time in seconds.
SET-TEMP = -5. / Set temperature used for luminance.
LUM_EXP = 600. / Average luminance exposure time.
LUM_CNT = 19. / Luminance images combined.
LUM_DARK = 40. / Darks used for luminance.
LUM_FLAT = 40. / Flats used for luminance.
LUM_BIAS = 80. / Flat-darks used for luminance.
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