Discover the Hubble Ultra Deep Field: Deepest Portrait of the Visible Universe

[Brad_Ad23]

This is slightly off the topic directly of the HUDF, but it concerns a few things with it. 1) Does anyone have a rough idea of just how large the universe was at that epoch?
2)The dark energy acceleration of the universe, do we know if it is constant, or whether da/dt itself is growing larger or smaller as time goes, or if it is constant or zero?

 

[Loren Booda]

The redshift, Z=R(t₀)/R(t). Z=100 when the galaxies were "touching," and Z=1000 at the epoch of decoupling. I believe R(t₀) is present horizon radius, and R(t) the radius in question.

From Cosmology, by Rowan-Robinson, 3rd ed.

 

[Brad_Ad23]

Interesting, thanks.

Any idea about the dark energy question?

 

[wisp]

The paper referred to by ranyart is very good and discusses the formation of supermassive black holes (SMBHs) that were fully assembled early in the history of the universe.
Their masses were approx 10^9 greater than our sun (i.e. a billion times our sun's mass). The Hubble pictures show that galaxies had formed shortly after the big bang.
So I am convinced that these SMBH monsters were around early on and formed the seeds of galaxies.
But I am not convinced that "dark matter" played a part in their formation.
Why is it that we can see almost to the edge of our universe and yet nobody has ever found, seen, or can tell us what dark matter really is?
I think that this dark matter might just be an effect that results from the SMBHs presence and maybe these massive black holes were fragments blasted out during the big bang.

 

[Rich Murray]

Hubble Infrared Ultra Deep Field clearly reveals deep cosmic background
fractile 3D mesh of H filaments lit by hypernovae: Murray 2006.11.21

#33. Hubble Ultra Deep Field infrared view,
brightness +20, and both red and blue colors increased,
and green reduced, softness set to 3 of 12 levels, 4.07 MB png,
1600X1600 pixels. 4.07 MB png

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.
Click on All Sizes to view the Original.

The number of the myriad minute blue sources varies noticeably,
for instance,from higher south of the bright foreground star,
just left of center at the bottom, to lower towards the lower right.
This indicates that simple surveys can collect much detailed
information. (Use the All Sizes button and select Original.)

The value of this simple approach is evident,
if we take the tiny blue sources to be
the earliest massive hypernovae and GRBs,
markers that highlight the 3D fractile network distribution of mostly H
gas filaments, condensing by gravitational attraction,
as the universe bubble continued its expansion.
It became cool enough at 380,000 years to allow atoms to form within
the former ionized plasma.
Transparency emerged from opacity.
The intense ultraviolet radiation at 3,000 deg K was redshifted and
cooled with the thousand-fold expansion of space-time to
comprise our era's Cosmic Microwave Background at just 2.7 deg K,
ubiquitious, and uniform to a few parts in a hundred thousand.

See for yourself, Observer,
the deep tapestry of our astrophysical history,
hung hugely against the uniform red background
(downshifted cosmic ultraviolet),
the wooly open knit of cooled and condensed H filaments
(darkly silhouetting the background),
lit like Christmas trees with generations of tiny blue sources,
(the downshifted ultraviolet of immense fast-burning, short-lived
hypernovae,
and a few GRBs,
while some twin sources may be the two jet lobes of active galaxies),
with vistas of closer and cooler galaxies,
ranging from red, orange, yellow, green, blue, and white,
from early small clump cluster galaxies to far larger irregular,
spiral, and elliptical galaxies,
and the little kid in our own neighborhood,
the red foreground star with its diffraction spikes
from the Hubble Space Telescope,
just left of center at the bottom.

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: set at 3 of 12 levels, to slightly smooth out the pixels.
Color Adjustment: Cyan-Red +75, Magenta-Green -100, Yellow-Blue +50,
as empirically this created a pleasing, easy to view image with maximum
detail.
Brightness: increased from 0 to 20, to increase the dark background
details.
Gamma: unchanged at 1.00.#34. HUDF ir 1/4 area in low center,
800X800 pixels. 1.02 MB png

static.flickr.com/52/121113051_12b5e3b85c_o.png#35. HUDF ir 1/16 area in low center,
400X400 pixels. 263 KB png

static.flickr.com/49/121113052_52157a78ca_o.png#36. HUDF ir closer view. 180 KB png about 60 arc-sec wide

static.flickr.com/53/121150408_69845a7c53_o.png#37. HUDF ir closer view, to show levels of background structure:
distant red glow,
dark 3D fractile mesh that obscures the background red glow,
blue sources that light up the dark mesh of condensing H and He gas,
a few much closer red, white, and blue sources.
Click on All Sizes button for closeup.

static.flickr.com/44/121150409_efdb07b94d_o.png
#38. HUDF ir deepest view -- click on All Sizes button.
RTM-1 is the reddish feature that slants down to the lower right from
the center towards the bright galaxy -- not visible are the bright
objects at both ends of RTM-1, which may be a central ir source with
bipolar jets, seen from the side, that end quickly in a pair of big
expanded hot gas regions, very bright in the other HUDF
visible bands of light. See #31.

static.flickr.com/50/121150410_d95548c86f_o.png
# 19 The Millennium Simulation, announced 2005.06.02 by the Virgo
consortium,
used the largest supercomputer in Europe,
at the German Astrophysical Virtual Observatory,
for over a month to model the history of the Universe
in a cube over 2 billion light years on a side,
holding 20 million galaxies.

static.flickr.com/13/18135102_07a58fd89d_o.jpg

This image is a closeup of the results at redshift z = 0, showing a 15
MPC/h thick slice, showing the visible light distribution,
which closely follows the mass distribution.
The view is four times wider than in #18,
so that the width of the image is 1628 MLy.
The length of the central large and dense galaxy cluster
is about 60 MLy.

1024 X 768 pixels jpg 0.970950 MB

The distance measure Mpc/h has been used for decades to adjust to the
fact that the Hubble constant = H has not been exactly determined.
Mpc is megaparsecs.
A parsec is 3.26 light years.
The Millennium Simulation used the value 0.73
for the Hubble constant H.

To get the distance in Mpc,
we multiply their value by 100/H = 100/0.73 = 1.37 .

The huge, densely packed galaxy cluster,
holding thousands of galaxies,
for the greenish central region, has a length of about 60 MLy.
In contrast, the nearest large neighbor to our Milky Way galaxy is
Andromeda galaxy at 2.2 MLy distance.

The distribution of mass in the Universe is very fractile --
it looks just as complex and very much the same
at a very wide range of distance scales.

So, even though I do not know how wide this image would be in terms of
angular measures (degrees, minutes, seconds),
it is probably justified to compare it to the Capodimonte Deep Field
subtle background visible light images.

Many features are the same:
complex 3D fractile network,
with bright boundaries around both brighter (more dense) and dimmer
(more empty) regions,
and both brighter and thicker and thinner and dimmer lines,
marked by myriad tiny dense features.
I don't believe that the MS image includes gravitational lensing, which
must be a complex factor in the CDF images.

Click on All Sizes to view Original.

www.pparc.ac.uk/Nw/millennium_sim.asp[/URL] The Virgo consortium

[url]www.mpa-garching.mpg.de/galform/millennium/[/url]

[url]www.mpa-garching.mpg.de/galform/millennium/galseq_D_063.jpg[/url]

arxiv.org/abs/astro-ph/0504097
Simulating the joint evolution of quasars, galaxies and their
large-scale distribution

pil.phys.uniroma1.it/debate3.html
On the fractile structure of the universe
Sylos Labini, Montuori & Pietronero#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.