Check out these change background image images:
#30. astrodeep200407aecc
Image by rmforall@gmail.com
#30. (#24) field from Hubble Ultra Deep Field 832 X 833 p tif 2.72 MB png 1.86 MB
This field is 61 sec wide = 1 minute wide. RTM-1 is the pair of blue spots just above the large magenta galaxy in the lower left. There are six more suggestive blue spot pairs in this field.
RTM-1, closeup view in #21, is very like CSL-1, only blue and more separated, but with the similar equality of size and color. It turns out that there are so many easily found pairs of all sizes, down to single pixel bright spots separated by a pixel space, that statistical studies are appropriate. Views # 20 to 29 will explore the HUDF, and provide many helpful links.
The colors have been adjusted to reveal a few faint distant red sources, as well as a background of tiny blue sources, 1-2 pixel size, which are always on the background of dark tangled Murray mesh -- easier to see at first behind the red light scattered inside the Hubble Space Telescope by the much nearer bright star, and also behind the large blue white galaxy in the upper right. Click on All Sizes to view the Original.
I used an excellent low cost image processing program, MGI PhotoSuite 4.0, to adjust the colors to bring out the subtle background details:
Touchup feature: Soften: reduced from 3 to 0, as I wanted to maximize the raw detail.
Color Adjustment: Cyan-Red +100 Magenta-Green +25 Yellow-Blue +50,
as empirically this created a pleasing, easy to view image with maximum detail.
Brightness: increased from 0 to 50, to increase the dark background details.
Gamma: reduced from 1.00 to 0.80, to increase the dark background details.
Fix Colors: Hue: shifted 0 to -60, to accentuate the background of myriad minute
bright blue sources without losing information from the red end of the spectrum.
www.aip.de/groups/galaxies/sw/udf/index.php# The UDF Skywalker allows you to scan the entire HUDF with a movable magnifying glass that shows about this scale of detail. You can discern Murray mesh with it.
www.damtp.cam.ac.uk/user/gr/public/cs_interact.html
Cosmic String Dynamics and Evolution
'After formation, an initially high density string network begins to chop itself up by producing small loops. These loops oscillate rapidly (relativistically) and decay away into gravitational waves. The net result is that the strings become more and more dilute with time as the universe expands. From an enormous density at formation, mathematical modelling suggests that today there would only be about 10 long strings stretching across the observed universe, together with about a thousand small loops!
In fact the network dynamics is such that the string density will eventually stabilize at an exactly constant level relative to the rest of the radiation and matter energy density in the universe. Thus the string evolution is described as `scaling' or scale-invariant, that is, the properties of the network look the same at any particular time t if they are scaled (or multiplied) by the change in the time.'
If you inspect this carefully, especially holding a 4 inch reading glass close to both of your eyes, focussing on the tiny bright blue sources, you will easily discern many suggestive pairs, right down to the limit of two single pixel spots separated by a pixel, or even the many double pixel spots. The two sides of the convex reading glass function as opposed prisms, separating the reds and blues in such a way as to make the reds appear about a centimeter closer, creating a lovely, revealing 3D image, while moving the glass back and forth can flexibly adjust the smoothness and the sharpness of the image.
I found that using a 6X5 inch concave glass, which in effect has prisms opposed in the opposite direction of a convex lens, makes a smaller overall image in which the blues appear closer than the reds, which I surmise is the actual reality for these images for the background.
#24. astrodeep200407aecc.png
Image by rmforall@gmail.com
#24. (#30) field from Hubble Ultra Deep Field 832 X 833 p tif 2.72 MB png 1.86 MB
This field is 61 sec wide = 1 minute wide. RTM-1 is a pair of double blue spots just above the large magenta galaxy in the lower left. There are six more similar blue spot pairs in this field.
static.flickr.com/13/19717874_18d6b931b4_o.png
RTM-1, closeup view in #21, is very like CSL-1, only blue and more separated, but with the similar equality of size and color. It turns out that there are so many easily found pairs of all sizes, down to single pixel bright spots separated by a pixel space, that statistical studies are appropriate. Views # 20 to 29 will explore the HUDF, and provide many helpful links.
The colors have been adjusted to reveal a few faint distant red sources, as well as a background of tiny blue sources, 1-2 pixel size, which are always on the background of dark tangled Murray mesh -- easier to see at first behind the red light scattered inside the Hubble Space Telescope by the much nearer bright star, and also behind the large blue white galaxy in the upper right. Click on All Sizes to view the Original.
I used an excellent low cost image processing program, MGI PhotoSuite 4.0, to adjust the colors to bring out the subtle background details:
Touchup feature: Soften: reduced from 3 to 0, as I wanted to maximize the raw detail.
Color Adjustment: Cyan-Red +100 Magenta-Green +25 Yellow-Blue +50,
as empirically this created a pleasing, easy to view image with maximum detail.
Brightness: increased from 0 to 50, to increase the dark background details.
Gamma: reduced from 1.00 to 0.80, to increase the dark background details.
Fix Colors: Hue: shifted 0 to -60, to accentuate the background of myriad minute
bright blue sources without losing information from the red end of the spectrum.
www.aip.de/groups/galaxies/sw/udf/index.php# The UDF Skywalker allows you to scan the entire HUDF with a movable magnifying glass that shows about this scale of detail. You can discern Murray mesh with it.
www.damtp.cam.ac.uk/user/gr/public/cs_interact.html
Cosmic String Dynamics and Evolution
'After formation, an initially high density string network begins to chop itself up by producing small loops. These loops oscillate rapidly (relativistically) and decay away into gravitational waves. The net result is that the strings become more and more dilute with time as the universe expands. From an enormous density at formation, mathematical modelling suggests that today there would only be about 10 long strings stretching across the observed universe, together with about a thousand small loops!
In fact the network dynamics is such that the string density will eventually stabilize at an exactly constant level relative to the rest of the radiation and matter energy density in the universe. Thus the string evolution is described as `scaling' or scale-invariant, that is, the properties of the network look the same at any particular time t if they are scaled (or multiplied) by the change in the time.'
If you inspect this carefully, especially holding a 4 inch reading glass close to both of your eyes, focussing on the tiny bright blue sources, you will easily discern many suggestive pairs, right down to the limit of two single pixel spots separated by a pixel, or even the many double pixel spots. The two sides of the convex reading glass function as opposed prisms, separating the reds and blues in such a way as to make the reds appear about a centimeter closer, creating a lovely, revealing 3D image, while moving the glass back and forth can flexibly adjust the smoothness and the sharpness of the image.
I found that using a 6"X5" concave glass, which in effect has prisms opposed in the opposite direction of a convex lens, makes a smaller overall image in which the blues appear closer than the reds, which I surmise is the actual reality for these images for the background.
