two classes of readily noticeable common, ubiquitous, uniform bright blue sources in deep background (Murray mesh) of HUDF, dwarf galaxy luminous bare clumps, hyper novae?: 2005.04.01 BG and DM Elmegreen: Malcolm Fairbairn: Murray 2005.11.11

************************************************** ***********

http://groups.yahoo.com/group/AstroDeep/15
two classes of readily noticeable common, ubiquitous, uniform bright blue
sources in deep background (Murray mesh) of HUDF, dwarf galaxy luminous
bare clumps, hyper novae?: 2005.04.01 BG and DM Elmegreen:
Malcolm Fairbairn: Murray 2005.11.11

November 11, 2005 Hello Malcolm,

I hope it best answers your questions to give a long,detailed answer
that shows you how to access the 31 images on my Flickr.com archive,
and quotes the complete notes I wrote for each image,
moving in three steps from deepest closeup to the HUDF.

The public HUDF uses blue to represent received blue light.

It happens that RML-1 and many very similar pairs, are bright blue,
which I have emphasized by shifting the colors to emphasize blue,
without losing significant data for the red.

As a layman, I am guessing that these are very bright UV sources,
redshifted to blue.
Are they large ellipticals like CSL-1, small early galaxies, or smaller
"bare", "clump luminous masses", "gas-rich dwarf galaxies",
"small field objects are more the size of the z ~6 galaxies
studied by Bunker et al. (2004)."?

"These galaxies are members of a class dominated by 5 to 10 giant clumps,
and having no exponential disk or bulge.

The redshifts are found to be in the range from 1.6 to 3.

The clump emission is typically 40% of the total galaxy emission and the
luminous clump mass is 19% of the total galaxy mass.

The clump colors suggest declining star formation over the last ~0.3 Gy,
while the interclump emission is redder than the clumps,
corresponding to a greater age.

The clump luminous masses are typically 6 × 10E8 M(Sun) and their diameters
average 1.8 kpc, making their average density ~0.2 M(Sun) pc-3......

......or they could be captured as gas-rich dwarf galaxies,
flaring up with star formation at first and then dispersing.

Support for this second possibility comes from the high abundance of nearly
identical clumps in the UDF field, smaller than 6 pixels, whose
distributions on color-magnitude and color-color plots are the same as the
galaxy clumps studied here." 2005.04.01 Elmegreen BG, Elmegreen DM

From their text:
"4.2.2. Bare clumps in the UDF
What is the evidence for clumps like these outside of clump-cluster
galaxies, where they presumably existed before the accretion?
The UDF contains many isolated objects that resemble our clumps in both
luminosity and color.
The right-hand side of Figure 11 shows color-magnitude and color-color plots
of all the UDF objects smaller than 6 pixels in FWHM, as given in the
tabulation on the UDF web site (1).
This size limit was chosen because it roughly corresponds to the size of a
clump in a clump-cluster galaxy.
The left side of the figure shows the magnitudes and colors for the measured
clumps in the clump-cluster galaxies of this paper.
The distributions are essentially the same in the regions of overlap.
The UDF clumps can be much bluer than our clumps, suggesting either that
star formation begins to slow down
once a clump is ingested into a larger galaxy,
or the clump-cluster sample in our survey has too few clumps to include the
rare active ones seen in the general UDF field.
There are also much fainter clumps in the UDF field than those measured in
our survey, but the clump-cluster galaxies have much fainter clumps too
which we did not study.
We note that these small objects in the UDF field are not the well-studied
Lyman Break galaxies,
which tend to be more massive, blue, and luminous than our clumps even at
the same z ~2.5 - 3 (e.g., Papovich, Dickinson, & Ferguson 2001).
The small field objects are more the size of the z ~6 galaxies studied by
Bunker et al. (2004).
Most likely, most are low-mass and low-luminosity galaxies in about the same
range of redshifts as the clump-cluster galaxies studied here.....

[ Bunker, A., Spinrad, H., Stern, D., Thompson, R., Moustakas, L., Davis,
M., & Dey, A. 2000, in Galaxies in the Young Universe II, ed. H. Hippelein &
K. Meisenheimer (Berlin: Springer) ]

These considerations suggest that the clumps in some of our clump-cluster
galaxies could have been accreted as whole objects from the field."

The distance is greater, if the sources are smaller.
Predictions are that there are many more cosmic strings at earlier epoches.

The CMB is hotter with distance, and is ~3,000 deg K at age 380,000 years.
The initial H filaments have to cool down in order to collapse by gravity,
but then the first stars are ultramassive, ultrahot, short-lived extreme UV
sources that become hypernovae, quasars, and black holes.

As a layman, I conjecture that they are the myriad uniform
bright blue sources, 1-2 pixels,
always on a background fractile 3D dark mesh,
backlighted by a faint reddish glow,
which then would be redshifted CMB
prior to the formation of the mesh of H filaments.
The HUDF pixels are 0.03 arc-sec.

In that case, repeated exposures every few months of large fields
should show the rate of appearance and disappearance
of these extreme sources,
which have a lifetime on the order of 1 to 10 million years.

These are exciting vistas to appreciate,
immediately openning up a major frontier in astrophysics.

In mutual service, Rich

Rich Murray, MA Room For All 505-501-2298
1943 Otowi Road Santa Fe, New Mexico 87505 USA
http://groups.yahoo.com/group/AstroDeep/
************************************************** ***********

http://groups.yahoo.com/group/AstroDeep/12
more candidate cosmic string lens pairs in HUDF (re comment by Levon
Pogosian on astro-ph/0506400); also myriad minute bright blue sources,
always on dark background mesh: Murray 2005.11.10

http://groups.yahoo.com/group/AstroDeep/11
subtle background structure in deep astronomy photos; CSL-1 cosmic string
gravitational lens in Capodimonte Deep Field; Millennium Simulation of
evolving cosmic structure; AstroDeep group; Murray mesh; www.Flickr.com
photo archive: Murray 2005.06.10
************************************************** ***********

http://www.flickr.com/photos/rmforall/
31 images with detailed comments and links

Click in the lower left area just below Your Photos on Your Photo Page

Then click on the top photo #31 (#21) astrodeep200407aecb

Here is the text for this image, the most magnified closeup
I give from HUDF,
a view 3.75 X 3.75 arc-sec, with RML-1 0.4 X 0.2 sec --
ten times less long than CSL-1 :

#31 (#21) Closeup of possible cosmic string gravitational lens,
the blue galaxy pair, very similar to CSL-1,
just above yellow galaxy in lower left corner of #20 and #22,
magenta in #23. I call it RML-1, Rich Murray Lens 1.

The 125 X 125 pixel field was cropped from #23,
and expanded to fit the page,
and saved as tif 2.25 MB and this png .087 MB image.

The pixels are .03 arc-second each, so that the original
Hubble Ultra Deep Field, 6200 X 6200 pixels, is 186 X 186 arc-seconds,
3.1 X 3.1 arc-minutes, a tenth of the diameter of the Full Moon or the Sun,
0.5 degrees, 30 arc-minutes.

This view is 125 X 125 p, 3.75 X 3.75 sec.
The length of the dumbell shape of the two blue galaxies is
1/9 of the 125 p width of the view, 14 X 7 p, 0.4 X 0.2 sec. --
ten times less long than CSL-1.

Notice the background scatter of bright blue sources, 1 to 2 pixel size,
and the dark background 3D mesh.

The bright blue sources, like tiny Christmas lights,
are always on the dark 3D mesh.

The coding at some stage in the image processing
has produced prevalent vertical straight line artifacts.

hubblesite.org/newscenter/newsdesk/archive/releases/2004/...
Hubble reaches the final frontier: the dawn of galaxies

The Universe expanded from a tiny point 13.7 billion years ago.
By 380,000 years, time 0.000380 BY, the expanding hot atomic plasma,
made of electrons and protons, which had been opaque to light,
had cooled enough, 3,000 deg Kelvin,
to allow the free electrons to bind with the free protons
to form atoms of H, becoming a transparent gas --
by now these photons have cooled and redshifted
with the expanding space-time of the Universe
to become the ubiquitous 2.7 deg Kelvin cosmic microwave background, CMB.

But without stars, the universe was without light - the dark ages.

Gravity, very slowly at first, then faster and ever faster,
started pulling the initially slightly denser volumes of gas inward
to form complex fractile networks of increasingly dense filaments and nodes.

The first stars each formed within a single cloud of about a million solar
masses,
contracting to ignite a central mass of about 100 to 1000 solar masses.
These huge stars burned hotly and quickly for short lifespans
of a few million years,
and their intense ultraviolet light started to reionize the gas.
Many exploded as hypernovae, illuminating the Universe,
and venting huge amounts of heavier elements, called 'metals', into the
galactic gas.

Later stars, with increasing metal contents, were able to form more quickly
and were smaller, cooler, less bright, and much longer lived,
and so the masses of contracting gas
became clusters of hot, crooked dwarf galaxies.

This view may show this, with the ultraviolet light
from the early hyper novae
redshifted to the maroon color of the far background,
highlighting the complex 3D fractile dark network of condensing darker
filaments and nodes,
which in turn give birth to the hot, ultraviolet bright,
crooked dwarf galaxies, closer to us,
and so redshifted a lesser degree to bright blue.

arxiv.org/PS_cache/hep-th/pdf/0508/0508135.pdf
arXiv:hep-th/0508135 v2 25 Aug 2005
Cosmic strings: progress and problems. Alexander Vilenkin,
Institute of Cosmology, Department of Physics and Astronomy,
Tufts University, Medford, MA 02155, USA
' Another intriguing new development is the observation
of two nearly identical galaxies at redshift z = 0.46
with angular separation of 1.9 arc seconds [33].
The spectra of the two galaxies coincide at 99.9% confidence level [34].
The most plausible interpretation of the data appears to be
lensing by a cosmic string with Gµ ~ 4 × 10-7.
This estimate assumes a slowly moving string
orthogonal to the line of sight at a relatively low redshift (z ~0.1).
The issue is likely to be resolved by
Space Telescope observations later this year.


The next larger view is astrodeep200407aecc #30 (#24),
61 X 61 arc-sec :
[ astrodeep200407aecd # 25 is the same view, twice as dark ]

#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.
RML-1 is the probable cosmic string gravitational lens,
the double blue spots just above the large magenta galaxy in the lower left.
There are six more suggestive blue spot pairs in this field.

Rich Murray Lens 1, closeup view in #21, is very like CSL-1,
only blue and more separated,
but with the tell-tell 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 featu 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.

http://www.damtp.cam.ac.uk/user/gr/p..._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.



astrodeep200407aec # 23, 97.65 X 97.65" = 1.63 X 1.63'

#23 Part of bottom half of Hubble Ultra Deep Field,
255 X 255 pixels in the original HUDF,
[ cropped from its original 823 X 823 p when saved on
MGI PhotoSuite 4.0 as tif 112.618 MB ]
become 1911 X 1912 pixels in this expanded view,
tif 14.3 MB, uploaded as this png 9.83 MB,
just below the 10 MB Flickr limit.

Click on All Sizes to select Large and Original for much higher resolution.

The HUBF is described as 10,500 X 10,500 pixels,
at 0.03 arc-seconds/pixel,
giving a width of 315 arc-seconds = 5.25 arc-minutes,
oriented North at top and East to the left, with the center at
Right Ascension 03 hours 32 minutes 39.0 seconds
Declination -27 degrees 47 minutes 29.1 seconds

The previous photos #1-17 give the CSL-1 lens
and its subtle background in the Capodimonte Deep Field.
This field is 0.310 X 0.310 of the HUDF, 0.096 of its area,
the largest I could upload into Flickr. 97.65 X 97.65" = 1.63 X 1.63'

The 1-2 mm red and blue sources are much closer galaxies,
with their apparent colors determined by their actual temperature
and the amount of redshifting, which grows linearly with distance.
Much nearer to us, of course are the three 1-5 cm galaxies,
while the lower left red star is very much closer, in our own galaxy.



astrodeep200407aea # 20, the same view,
with the color settings of the public HUDF,
a freely available 110 MB TIFF image:

'In this image, blue and green correspond to colors that can be seen
by the human eye, such as hot, young, blue stars
and the glow of Sun-like stars in the disks of galaxies.
Red represents near-infrared light, which is invisible to the human eye,
such as the red glow of dust-enshrouded galaxies.'

hubblesite.org/newscenter/newsdesk/archive/releases/2004/...
highest resolution available public image 6200 X 6200 pixels TIFF 109.99 MB


#20 Part of bottom half of Hubble Ultra Deep Field,
255 X 255 pixels in the original HUDF,
[ cropped from its original 823 X 823 p
when saved on MGI PhotoSuite 4.0 as tif 112.618 MB ]
become 1911 X 1912 pixels in this expanded view, tif 14.3 MB,
uploaded as this png 9.83 MB, just below the 10 MB Flickr limit.

Click on All Sizes to select Large and Original for much higher resolution.

RML-1 is a tiny bright blue galaxy pair
just above the large yellow galaxy by the lower left edge.
Rich Murray Lens 1, closeup view in #21, is very like CSL-1,
only blue and more separated,
but with the tell-tell 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 previous photos #1-17 give the CSL-1 lens and its subtle background
in the Capodimonte Deep Field.

This field is 0.310 X 0.310 of the HUDF, 0.096 of its area,
the largest I could upload into Flickr. 97.65 X 97.65" = 1.63 X 1.63'

http://hubblesite.org/newscenter/new...hive/releases/
2004/07/text/"hubblesite.org/newscenter/newsdesk/archive/releases/2004/...
Hubble's Deepest View Ever of the Universe Unveils Earliest Galaxies
Release date: 2004.03.09 Images made 2003.09.24 -- 2004.01.16

'In this image, blue and green correspond to colors that can be seen
by the human eye, such as hot, young, blue stars
and the glow of Sun-like stars in the disks of galaxies.
Red represents near-infrared light, which is invisible to the human eye,
such as the red glow of dust-enshrouded galaxies.'

hubblesite.org/newscenter/newsdesk/archive/releases/2004/...
highest resolution available public image 6200 X 6200 pixels TIFF 109.99 MB

hubblesite.org/newscenter/newsdesk/archive/releases/2004/...
The Large view of the HUDF is a JPG size .0681 MB,
which shows RML-1 as a blue dot.
Enlarging it gives a 4 X 4 p white grey object
that has only a hint of something to its right.

hubblesite.org/newscenter/newsdesk/archive/releases/2004/...
This gives a fine TIFF view from HUDF of the RML-1 field,
a little smaller than my view here, 2.87 MB,
saved on my computer as a tif 2.942 MB.
A closeup of RML-1 in their view clearly shows a double galaxy,
with the L side slightly larger, about 12 X 12 pixels maximum,
and a brighter core of about 6 X 6 pixels: blue, green, brown.

Click on All Sizes to view Large and Original.
Notice the many bright blue pairs, and in Original the background haze
of myriad tiny blue spots, which I call Bright Blue Blazers,
with many pairs of BBB.

If you hold a 4 inch reading glass close to your face
and look through it with both eyes closely
at the monitor screen or a color print,
with the background lights turned off in your room,
you will see the different colors separated out as an apparent 3D image
about a centimeter deep, with red spots closer and the BBB in back,
against a 3D fractile network of tangled dark filaments.
Look close to the bright yellow-red star and the large blue-white galaxy
to see the dark background filaments.

The galaxy has many blue clumps inside it,
indicating that it grew by absorbing many blue dwarf galaxies.
xxx.lanl.gov/PS_cache/astro-ph/pdf/0504/0504032.pdf

arXiv:astro-ph/0504032 v1 1 Apr 2005 Stellar Populations in Galaxies
************************************************** ***********

From: "Malcolm Fairbairn"
To: "Rich Murray"
Subject: more candidate cosmic string lens pairs in HUDF
(re comment by Levon Pogosian on astro-ph/0506400);
also myriad minute bright blue sources, always on dark background mesh:
Murray 2005.11.10
Date: Friday, November 11, 2005 2:38 AM

Hello Rich Murray,

I don't have time to look in detail at all your information, so I'll focus
on one little point, apologies.

Regarding the image on your website page
http://www.flickr.com/photos/rmforal...deep200407aecd ,
where you claim to identify cosmic string lens candidates
in the Hubble deep field.
The reason why CSL-1 a is compelling is because we have spectra for
both images.

However, if there is a cosmic string then it will give rise to lensing
with a specific angle.

Do you know the angular separation of the objects or their redshifts?

best, Malcolm
--------------------------------------------------
http://www.physto.se/~malc/
Cosmology, Particle astrophysics and String theory
Department of Physics Stockholm University
AlbaNova University Center SE-106 91 Stockholm
Sweden Telephone +46 8 55 37 87 30
--------------------------------------------------
************************************************** ***********


http://arxiv.org/PS_cache/astro-ph/pdf/0511/0511085.pdf

arXiv:astro-ph/0511085 v2 3 Nov 2005
CSL-1: Lensing by a Cosmic String or a Dark Matter Filament?

Malcolm Fairbairn

Cosmology, Particle astrophysics and String theory, Department of Physics,
Stockholm University,
AlbaNova University Centre, SE-106 91, Stockholm, Sweden

The lens candidate CSL-1 has been interpreted
as evidence for a cosmic string.
Here we test the hypothesis that the lensing comes
from a tidally disrupted dark matter halo.
We calculate the mass-density relationship
that one would expect from structure formation theory
and come to the conclusion that in order to explain
the lensing using dark matter,
the halo would have to have a mass greater than the Milky Way.
There is apparently no such object seen in the data.
If the follow up observations confirm that the two objects
are indeed images of the same galaxy, then it seems
difficult to explain the lens using dark matter.
************************************************** ***********

ten clump-cluster galaxies in Hubble Ultra Deep Field, BG & DM Elmegreen
2005.04.01

arXiv: astro-ph/0504032 v1 1 Apr 2005
Stellar Populations in Ten Clump-Cluster Galaxies of the Ultra Deep Field
Bruce G. Elmegreen
IBM Research Division, T.J. Watson Research Center, P.O. Box 218,
Yorktown Heights, NY 10598, USA,
Debra Meloy Elmegreen
Vassar College, Dept. of Physics & Astronomy, Box 745, Poughkeepsie, NY
12604;

ABSTRACT

Color-color diagrams for the clump and interclump emission in 10
clump-cluster galaxies of the Ultra Deep Field are made from B,V,i, and z
images and compared with models to determine redshifts,
star formation histories, and galaxy masses.

These galaxies are members of a class dominated by 5 to 10 giant clumps,
and having no exponential disk or bulge.

The redshifts are found to be in the range from 1.6 to 3.

The clump emission is typically 40% of the total galaxy emission and the
luminous clump mass is 19% of the total galaxy mass.

The clump colors suggest declining star formation over the last ~0.3 Gy,
while the interclump emission is redder than the clumps,
corresponding to a greater age.

The clump luminous masses are typically 6 × 10E8 M(Sun) and their diameters
average 1.8 kpc, making their average density ~0.2 M(Sun) pc-3.

Including the interclump populations, assumed to begin forming at z = 6,
the total galaxy luminous masses average 6.5 × 10E10 M(Sun)
and their diameters average 19 kpc to the 2 sigma noise level.

The expected galaxy rotation speeds average ~150 km s-1 if they are
uniformly rotating disks.

The ages of the clumps are longer than their internal dynamical times by a
factor of ~8, so they are stable star clusters,
but the clump densities are only ~10 times the limiting tidal densities,
so they could be deformed by tidal forces.

This is consistent with the observation that some clumps have tails.

The clumps could form by gravitational instabilities in accreting disk gas
and then disperse on a ~1 Gy time scale,
building up the interclump disk emission,
or they could be captured as gas-rich dwarf galaxies,
flaring up with star formation at first and then dispersing.

Support for this second possibility comes from the high abundance of nearly
identical clumps in the UDF field, smaller than 6 pixels, whose
distributions on color-magnitude and color-color plots are the same as the
galaxy clumps studied here.

The distribution of axial ratios for the combined population of chain and
clump-cluster galaxies in the UDF is compared with models and shown to be
consistent with a thick disk geometry.

If these galaxies evolve into today's disk galaxies, then we are observing a
stage where accretion and star formation are extremely clumpy and the
resulting high velocity dispersions form thick-disks.

Several clump-clusters have disk densities that are much larger than in
local disks, however, suggesting an alternate model where they do not
survive until today, but get converted into ellipticals by collisions.

Subject headings: galaxies: formation - galaxies: evolution - galaxies: high
red-shift - galaxies: irregular
************************************************** ***********

I just wish the title and the content was a little bit longer!

Rich Murray wrote:

The public HUDF uses blue to represent received blue light.

I'm glad you clarified that point. It could have been very confusing
otherwise. What colors does it use to represent red and green?