#62. astrodeep200407 a g HUDF heic0611aa
#62. astrodeep200407 a g HUDF heic0611aa
Click on All Sizes button and select Original to see highest resolution image.
In the full HUDF view, saturating the colors reveals huge regions with very different overall colors -- this deserves research.
www.spacetelescope.org/images/html/zoomable/heic0611a.html Zoomable
The boxes are 3 arcsec wide, 100x100 pixels, with 0.03 arc-second per pixel. They are in order of apparent brightness, from 1 to 28.
The half-light galaxy diameters are about 1.6 kpc = 5220 Ly, as 1 kpc = 1000 parsecs = 3262 Ly. Our Milky Way galaxy is about 100,000 Ly wide.
notable bright blue tiny sources on darker 3D fractal web in HUDF VLT
ESO 28 images from 506 galaxies, z about 6 , RJ Bouwens, GD
Illingworth, JP Blakeslee, M Franx 2008.02.04 draft 36 page: Rich
Murray 2008.08.17
rmforall.blogspot.com/2008_08_01_archive.htm
Sunday, August 17, 2008
groups.yahoo.com/group/AstroDeep/26
groups.yahoo.com/group/rmforall/86
www.flickr.com/photos/rmforall/1363979470/in/photostream/
Double click on photo and click on All Sizes button and select Original to see highest resolution image, as well as some smaller images.
www.spacetelescope.org/images/html/zoomable/heic0611a.html Zoomable
The boxes are 3 arcsec wide, 100x100 pixels, with 0.03 arc-second per
pixel. They are in order of apparent brightness, from 1 to 28.
The HUDF is made of 0.03 arc-second pixels, 6200X6200, 186X186 arc-seconds, 3.1X3.1 arc-minutes, about a tenth of the width of the Moon or Sun, 0.5X0.5 degrees.
'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.'
Four wavelength filters collected the B435, V606, i775, z850 wavelength images for the observed blue, violet, near infrared, infrared images -- combined in this vast image with tiny 0.03 arc-second pixels.
'Galaxy sizes: Typical i-dropouts at z850,AB about 27 (from the HUDF-Ps and HUDF) have PSF-corrected half-light radii of about 0.8 kpc [2610 Ly] or about 0.14 arc-second (Figure 6: §3.7). [ So diameter is 1.6 kpc = 5220 Ly, as 1 kpc = 1000 parsecs = 3262 Ly. Our Milky Way galaxy is about 100,000 Ly wide. ]'
'The reheating, driven by the galaxies ultraviolet starlight, transformed the gas between galaxies from a cold, dark hydrogen soup to a hot, transparent plasma over only a few hundred million years.
With Hubble's help, astronomers are now beginning to see the kinds of galaxies that brought about the reheating.'
'The first 900 million years (Myr) to redshift z about 6 (the first seven per cent of the age of the Universe) remains largely unexplored for the formation of galaxies.'
'It is not at all clear how galaxies built up from the first stars when the Universe was about 300Myr old (z about 12-15) to z about 6, just 600Myr later.'
'The nearest galaxies -- the larger, brighter, well-defined spirals and ellipticals -- thrived about 1 billion years ago, when the cosmos was 13 billion years old.'
'The image required 800 exposures taken over the course of 400 Hubble orbits around Earth. The total amount of exposure time was 11.3 days, taken between Sept. 24, 2003 and Jan. 16, 2004.'
www.spacetelescope.org/images/html/heic0611a.html
Probing the distant Universe for young galaxies
This Hubble Space Telescope image shows 28 of the brightest of 506 young galaxies that existed when the universe was less than 1 billion years old.
The galaxies were uncovered in a study of two of the most distant surveys of the cosmos, the Hubble Ultra Deep Field (HUDF), completed in 2004, and the Great Observatories Origins Deep Survey (GOODS), made in 2003.
Just a few years ago, astronomers had not spotted any galaxies that existed significantly less than 1 billion years after the Big Bang.
The galaxies spied in the HUDF and GOODS surveys are blue galaxies brimming with star birth.
The large image at left shows the Hubble Ultra Deep Field, taken by the Hubble telescope.
The numbers next to the small blue boxes correspond to close-up views of 28 of the newly found galaxies at right. [ arranged by apparent brightness from 1 to 28 ]
The galaxies in the postage-stamp size images appear red because of their tremendous distance from Earth. The blue light from their young stars took nearly 13 billion years to arrive at Earth. During the journey, the blue light was shifted to red light due to the expansion of space.
Credit: NASA, ESA, R. Bouwens and G. Illingworth (University of California, Santa Cruz, USA)
www.spacetelescope.org/news/html/heic0611.html
News Release -- heic0611: Hubble finds hundreds of young galaxies in
the early Universe
21-Sep-2006: Astronomers analyzing two of the deepest views of the
cosmos made with the NASA/ESA Hubble Space Telescope have uncovered a
gold mine of galaxies, more than 500 that existed less than a billion
years after the Big Bang.
These galaxies thrived when the cosmos was less than 7 percent of its present age of 13.7 billion years.
This sample represents the most comprehensive compilation of galaxies in the early Universe, researchers said.
The discovery is scientifically invaluable for understanding the origin of galaxies, considering that just a decade ago early galaxy formation was largely uncharted territory.
Astronomers had not seen even one galaxy that existed when the Universe was a billion years old, so finding 500 in a Hubble survey is a significant leap forward for cosmologists.
The galaxies unveiled by Hubble are smaller than today's giant galaxies and very bluish in colour, indicating they are ablaze with star birth.
The images appear red because of the galaxies' tremendous distance from Earth.
The blue light from their young stars took nearly 13 billion years to arrive at Earth.
During the journey, the blue light was shifted to red light due to the expansion of space.
'Finding so many of these dwarf galaxies, but so few bright ones, is evidence for galaxies building up from small pieces -- merging together as predicted by the hierarchical theory of galaxy formation,' said astronomer Rychard Bouwens of the University of California, Santa Cruz, USA who led the Hubble study.
Bouwens and his team spied these galaxies in an analysis of the Hubble Ultra Deep Field (HUDF), completed in 2004, and the Great Observatories Origins Deep Survey (GOODS), made in 2003.
The results were presented on August 17 at the 2006 General Assembly of the International Astronomical Union, and will be published in the November 20 issue of the Astrophysical Journal.
The findings also show that these dwarf galaxies were producing stars at a furious rate, about ten times faster than is happening now in nearby galaxies.
Astronomers have long debated whether the hottest stars in early star-forming galaxies, such as those in this study, may have provided enough radiation to reheat the cold hydrogen gas that existed between galaxies in the early Universe.
The gas had been cooling since the Big Bang.
'Seeing all of these starburst galaxies provides evidence that there were enough galaxies 1 billion years after the Big Bang to finish reheating the Universe,' explained team member Garth Illingworth of the University of California, Santa Cruz. 'It highlights a period of fundamental change in the Universe, and we are seeing the galaxy population that brought about that change.'
In terms of human lifetimes, cosmic events happen very slowly.
The evolution of galaxies and stars, for example, occurs over billions of years.
Astronomers, therefore, rarely witness dramatic, relatively brief transitions that changed the Universe.
One such event was the Universe is 'reheating'.
The reheating, driven by the galaxies ultraviolet starlight, transformed the gas between galaxies from a cold, dark hydrogen soup to a hot, transparent plasma over only a few hundred million years.
With Hubble's help, astronomers are now beginning to see the kinds of galaxies that brought about the reheating.
Just a few years ago, astronomers did not have the technology to hunt for faraway galaxies in large numbers.
The installation of the Advanced Camera for Surveys (ACS) aboard the Hubble Space Telescope in 2002 allowed astronomers to probe some of the deepest recesses of our Universe.
Astronomers used the ACS to observe distant galaxies in the HUDF and GOODS public surveys.
Another major step in the exploration of the Universe's earliest years will occur if Hubble undergoes its next upgrade with the Wide Field Planetary Camera 3 (WFC3).
The WFC3's infrared sensitivity will allow it to detect galaxies that are so far away their starlight has been stretched to infrared wavelengths by the expanding Universe.
The galaxies uncovered so far promise that many more galaxies at even greater distances are awaiting discovery by the NASA/ESA/CSA James Webb Space Telescope (JWST), scheduled to launch in 2013.
Co-author Marijn Franx, member of the ESA JWST NIRSPEC science team,
explains: 'The JWST will be able to see even further back into the
early Universe, and glimpse the first objects that formed.
ESA's NIRSPEC instrument, can even measure the exact distances of
these objects.'
Notes for editors:
The Hubble Space Telescope is a project of international cooperation between ESA and NASA.
The members of the science team are Rychard Bouwens and Garth
Illingworth (University of California, Santa Cruz),
John Blakeslee (Washington State University),
and Marijn Franx (Leiden University).
NASA, ESA, R. Bouwens and G. Illingworth (University of California, Santa Cruz, USA)
NASA's press release
Contacts:
Marijn Franx
Leiden Observatory, Leiden, the Netherlands
Tel: +31-71-5275870
E-mail: franx@strw.leidenuniv;
Rychard Bouwens
University of California, Santa Cruz, California, USA
Tel: +1-831-459-5276
E-mail: bouwens@ucolick.org;
Garth Illingworth
University of California, Santa Cruz, California, USA
Tel: +1-831-459-2843
E-mail: gdi@ucolick.org;
John Blakeslee
Washington State University, Pullman, Washington, USA
Tel: +1-509-335-2414
E-mail: jblakes@wsu.edu;
Lars Lindberg Christensen
Hubble/ESA, Garching, Germany
Tel: +49-89-3200-6306
Cellular: +49-173-3872-621
E-mail: lars@eso.org;
Donna Weaver
Space Telescope Science Institute, Baltimore, Md., USA
Tel: +1-410-338-4493
E-mail: dweaver@stsci.edu;
Copyright-free material (more info).
hubblesite.org/newscenter/archive/releases/2004/07/image/a/
Hubble Ultra Deep Field Image Reveals Galaxies GaloreSTScI-PRC2004-07a
Galaxies, galaxies everywhere -- as far as NASA's Hubble Space Telescope can see. This view of nearly 10,000 galaxies is the deepest visible-light image of the cosmos. Called the Hubble Ultra Deep Field, this galaxy-studded view represents a 'deep' core sample of the universe, cutting across billions of light-years.
The snapshot includes galaxies of various ages, sizes, shapes, and colors.
The smallest, reddest galaxies, about 100, may be among the most distant known, existing when the universe was just 800 million years old.
The nearest galaxies -- the larger, brighter, well-defined spirals and ellipticals -- thrived about 1 billion years ago, when the cosmos was 13 billion years old.
In vibrant contrast to the rich harvest of classic spiral and elliptical galaxies, there is a zoo of oddball galaxies littering the field.
Some look like toothpicks; others like links on a bracelet.
A few appear to be interacting.
These oddball galaxies chronicle a period when the universe was younger and more chaotic.
Order and structure were just beginning to emerge.
The Ultra Deep Field observations, taken by the Advanced Camera for Surveys, represent a narrow, deep view of the cosmos.
Peering into the Ultra Deep Field is like looking through an eight-foot-long soda straw.
In ground-based photographs, the patch of sky in which the galaxies reside (just one-tenth the diameter of the full Moon) is largely empty.
Located in the constellation Fornax, the region is so empty that only a handful of stars within the Milky Way galaxy can be seen in the 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.
The image required 800 exposures taken over the course of 400 Hubble orbits around Earth. The total amount of exposure time was 11.3 days, taken between Sept. 24, 2003 and Jan. 16, 2004.
Object Names: Hubble Ultra Deep Field, HUDF
Image Type: Astronomical
Credit: NASA, ESA, S. Beckwith (STScI) and the HUDF Team
dipastro.pd.astro.it/venice06/oral/Bouwens_Venice06.ppt
RJB, GDI give 40 slide Power Point Import presentation in Venice
2006.03.31
arxiv.org/PS_cache/astro-ph/pdf/0509/0509641v6.pdf 36 page
Draft version February 4, 2008
Preprint typeset using LATEX style emulateapj v. 04/21/05
Galaxies at z about 6: the UV luminosity function and luminosity
density from 506 HUDF, HUDF-PS, and GOODS i-dropouts
Rychard J. Bouwens 3, bouwens@ucolick.org;
Garth D. Illingworth 3, www.ucolick.org/~gdi/ gillingw@ucsc.edu;
John P. Blakeslee 4, jblakes@wsu.edu;
Marijn Franx 5 franx@strw.leidenuniv.nl;
1 Based on observations made with the NASA/ESA Hubble Space Telescope,
which is operated by the Association of Universities for
Research in Astronomy, Inc., under NASA contract NAS 5-26555. These
observations are associated with programs #9803.
2 Observations have been carried out using the Very Large Telescope at
the European Southern Observatory (ESO) Paranal
Observatory under program ID: LP168.A-0485.
3 Astronomy Department, University of California, Santa Cruz, CA 95064
4 Department of Physics & Astronomy, Washington State University,
Pullman, WA 99164-2814 and
5 Leiden Observatory, Postbus 9513, 2300 RA Leiden, Netherlands.
Draft version February 4, 2008
ABSTRACT [ z = redshift due to increasing distance and time from us here and now, where z = 0 ]
We have detected 506 i-dropouts (z about 6 -- galaxies) in deep, wide-area HST ACS fields: HUDF, enhanced GOODS, and HUDF-Parallel ACS fields (HUDF-Ps).
The contamination levels are under 8% (i.e., over 92% are at z about 6).
With these samples, we present the most comprehensive, quantitative analyses of z about 6 -- galaxies yet and provide optimal measures of the UV luminosity function (LF) and luminosity density at z about 6, and their evolution to z about 3.
We redetermine the size and color evolution from z about 6 to z about 3.
Field-to-field variations (cosmic variance), completeness, flux, and contamination corrections are modeled systematically and quantitatively.
After corrections, we derive a rest-frame continuum UV (about 1350 A) LF at z about 6 that extends to M1350,AB about −17.5 (0.04L*, z=3).
There is strong evidence for evolution of the LF between z about 6 and z about 3, most likely through a brightening (0.6+-0.2 mag) of M* (at 99.7% confidence) though the degree depends upon the faint-end slope.
As expected from hierarchical models, the most luminous galaxies are deficient at z about 6.
Density evolution (phi*) is ruled out at over 99.99% confidence.
Despite large changes in the LF, the luminosity density at z about 6 is similar (0.82 ± 0.21x) to that at z about 3.
Changes in the mean UV color of galaxies from z about 6 to z about 3 suggest an evolution in dust content, indicating the true evolution is substantially larger: at z about 6 the star formation rate density is just about 30% of the z about 3 value.
Our UV luminosity function is consistent with z about 6 galaxies providing the necessary UV flux to reionize the universe.
Subject headings: galaxies: evolution -- galaxies: high-redshift
2.1. ACS HUDF
The B435V606i775z850 [colors blue, violet, near infrared, infrared]
images used for this analysis are the v1.0 reductions of the HUDF
(Beckwith et al. 2006), binned on a 0.03′′ pixel scale.
3.2. i-dropouts in the HUDF
Applying the above selection criteria to the HUDF results in a sample
of 122 i-dropouts.
Objects range in magnitude from z850,AB = 25.0 to 29.4 (the 8 d limit).
At z about 6, this corresponds to 0.04 - 2.2 times the characteristic rest-frame UV luminosity at z about 3 (Steidel et al. 1999).... V606i775z850 color cutouts are provided in Figure 1 for the brightest 28 i-dropouts from the HUDF.
Fig. 1. -- Postage stamps (V606i775z850 color images) of the brightest 28 i775-dropouts from the HUDF [ from the 122 galaxies found ].
Objects are ordered in terms of their z850-band magnitude. [infrared]
The z850-band magnitudes and object IDs are shown above and below each object, respectively.
Each postage stamp is 3.0′′ in size.
These high S/N images show definitive evidence for assymetries, mergers, and other interactions -- similar to that seen at lower redshifts (z about 2 - 5).
Galaxy sizes: Typical i-dropouts at z850,AB about 27 (from the HUDF-Ps and HUDF) have PSF-corrected half-light radii of about 0.8 kpc [2610 Ly] or about 0.14 arc-second (Figure 6: §3.7). [ So diameter is 1.6 kpc = 5220 Ly, as 1 kpc = 1000 parsecs = 3262 Ly. Our Milky Way galaxy is about 100,000 Ly wide. ]
www.ucolick.org/~gdi/docs/nature_05156.pdf 15 page
LETTERS
Vol 443, 14 September 2006 doi:10.1038/nature05156
Rapid evolution of the most luminous galaxies during the first 900 million years
Rychard J. Bouwens, Garth D. Illingworth
The first 900 million years (Myr) to redshift z about 6 (the first seven per cent of the age of the Universe) remains largely unexplored for the formation of galaxies.
Large samples of galaxies have been found at z about 6 (refs 1-4) but detections at earlier times are uncertain and unreliable.
It is not at all clear how galaxies built up from the first stars when the Universe was about 300Myr old (z about 12-15) to z about 6, just 600Myr later.
Here we report the results of a search for galaxies at z about 7-8, about 700Myr after the Big Bang, using the deepest near-infrared and optical images ever taken.
Under conservative selection criteria we find only one candidate galaxy at z about 7-8, where ten would be expected if there were no evolution in the galaxy population between z about 7-8 and z about 6.
Using less conservative criteria, there are four candidates, where 17 would be expected with no evolution.
This demonstrates that very luminous galaxies are quite rare 700Myr after the Big Bang.
The simplest explanation is that the Universe is just too young to
have built up many luminous galaxies at z about 7-8 by the
hierarchical merging of small galaxies.
____________________________________________________________
See similar images:
ubiquitous bright blue 1-12 pixel sources on darker 3D fractal web in
five 2007.09.06 IR and visible light HUDF images, Nor Pirzkal,
Sangeeta Malhotra, James E Rhoads, Chun Xu, -- might be clusters of
earliest hypernovae in recent cosmological simulations: Rich Murray
2008.08.17
rmforall.blogspot.com/2008_08_01_archive.htm
Sunday, August 17, 2008
groups.yahoo.com/group/AstroDeep/25
groups.yahoo.com/group/rmforall/85
bright blue 1-4 pixel sources on darker 3D fractal web in IR and
visible light HUDF images -- might be the clusters of earliest
hypernovae in the Naoki Yoshida and Lars Hernquist simulation: Rich
Murray 2008.07.31
rmforall.blogspot.com/2008_07_01_archive.htm
Thursday, July 31, 2008
groups.yahoo.com/group/AstroDeep/24
groups.yahoo.com/group/rmforall/84
Rich Murray, MA Room For All rmforall@comcast.net
505-501-2298 1943 Otowi Road Santa Fe, New Mexico 87505
groups.yahoo.com/group/rmforall/messages
groups.yahoo.com/group/AstroDeep/messages
____________________________________________________________
Comments and faves
rmforall@gmail.com (58 months ago | reply)
bright blue 1-4 pixel sources on darker 3D fractal web in IR and visible light HUDF images -- might be the clusters of earliest hypernovae in the Naoki Yoshida and Lars Hernquist simulation: Rich Murray 2008.07.31
groups.yahoo.com/group/AstroDeep/24
_____________________________________________ _______________
csaweb.yonsei.ac.kr/~sjyoon/JuniorSeminar/S_a nd_T/Stars_F...[bromm]dark_ages_first_stars.pdf
Out of the Dark Ages the First Stars, Volker Bromm,
Sky & Telescope, 2006 May, 7 pages pdf
www.space.com/scienceastronomy/080731-first-s tars.html
Jeremy Hsu, www.space.com How the first stars were born 2008.07.31
arxiv.org/PS_cache/arxiv/pdf/0807/0807.4928v1 .pdf
Protostar Formation in the Early Universe, Naoki Yoshida,
Kazuyuki Omukai, Lars Hernquist, Science 2008.08.01 13p
www.physics.uci.edu/Cosmology/Yoshida_Naoki.p df
From the first stars to the first galaxies, Naoki H Yoshida,
27 slides show
online.kitp.ucsb.edu/online/stars_c07/yoshida /
Second-Generation Star Formation in Proto-Galaxies, Naoki H Yoshida 2007.08.17 20 slides show
_____________________________________________ _______________
Hubble Infrared Ultra Deep Field clearly reveals deep cosmic background
fractal 3D mesh of H filaments lit by hypernovae: Murray 2006.11.21
groups.yahoo.com/group/AstroDeep/20
hubblesite.org/newscenter/archive/releases/20 04/07/image/b/
imgsrc.hubblesite.org/hu/db/2004/07/images/b/ formats/full...
7.34 MB tiff
www.flickr.com/photos/rmforall/
to access 62 deep sky astrophotos with texts
#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.
static.flickr.com/42/121113050_6b7c705fcb_o.p ng
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 fractal 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.p ng
#35. HUDF ir 1/16 area in low center,
400X400 pixels. 263 KB png
static.flickr.com/49/121113052_52157a78ca_o.p ng
#36. HUDF ir closer view. 180 KB png about 60 arc-sec wide
static.flickr.com/53/121150408_69845a7c53_o.p ng
#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.p ng
#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.p ng
# 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.jp g
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 fractal 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 The Virgo consortium
www.mpa-garching.mpg.de/galform/millennium/
www.mpa-garching.mpg.de/galform/millennium/ga lseq_D_063.jpg
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.pn g
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.
_____________________________________________ _______________
Rich Murray, MA Room For All rmforall@comcast.net
505-501-2298 1943 Otowi Road Santa Fe, New Mexico 87505
groups.yahoo.com/group/rmforall/messages
groups.yahoo.com/group/AstroDeep/messages
_____________________________________________ _______________
sally linsdell, nbccnn, Vincent Anton / aka Astrovine, vincor67, and vgratian added this photo to their favorites.