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The Universe at High-z, Large-Scale Structure and the Cosmic Microwave Background: Proceedings of an Advanced Summer School Held at Laredo, Cantabria, ... 4-8 September 1995 (Lecture Notes in Physics)

Cosmology has dramatically evolved during the last decade and there has been vast development of, e.g., theories of galaxy formation in connection with the early universe or gravitational lensing. These new developments motivated the editors to organize a school covering all of these ideas and observations in a pedagogical way. The topics covered in the 26 lectures of this summer school include: QSO absorption systems, identification of objects at high redshift, radiogalaxies, galaxy formation and evolution, galaxy number counts, clustering, theories of structure formation, large-scale structure and streaming motions, gravitational lensing, and spectrum and anisotropies of the cosmic microwave background radiation. Observational developments, data analysis, and theoretical aspects are equally treated.

# 71 (#31, #21) astrodeep200407aecb.png 125 X 125 p, 3.75 X 3.75 arc-sec

Hubble closeup of "RTM-1", one of many noticeable blue galaxy pairs, just above yellow galaxy in lower left corner of #20 and #22, magenta in #23, and background of many tiny bright blue sources on a darker 3D fractal network, "Murray mesh".

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 arc-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 arc-sec. --
ten times less long than CSL-1 (now known to be simply a close pair of very similar
elliptical galaxies).

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

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

The infrared view in #37 is a close-up, about 30 arc-sec wide, of this same region, just to the lower left of the center of infrared view #36, which is about 60 arc-sec wide.
In it, the bright irregular white source in the lower right is this early smallish clump cluster galaxy, and just to the upper left of it is RTM-1, a reddish feature that seems to extend towards the clump cluster galaxy, but is very likely more distant.

The closest infrared view is #38.

In this view, #31, the visual field at twice the scale, RTM-1, appears as two close bright blue sources, probably very hot. It may be that the center of RTM-1 is a active black hole within an early, irregular galaxy, with the black hole heating its dust and gas clouds, while its two jets extend into the intergalatic medium and pile up in opposite directions to comprise the pair of very hot bright blue sources.

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.

and my head is going to become very worn out thinking about the conversation i had with victoria hammlet on the impossibility of meaning in anything with life and listening to her wonder that everything is pointless
and all i can think about is there is no way someone who plays the cello with as much conviction as you do could think that everything is pointless
or whose repressed sighs, endlessly harmonized "AHHHS" swirling and glowing inside of a dirty coffee cup and a bass drum
and i know your longing and my impatience is what is behind the science of an evolutionary need
FOR THE SEASONS TO CHANGE
i can sense the great depression of summer sweat salt and the winter coats weighing on y/our skin
is it really all the way until june until i'm myself again?
maybe never, maybe this summer was a fluke, like a stupid film
o exfoliate
o expatriate
i feel like it is my duty as a human being to convince you otherwise though i'm not entirely sure what the point of doing that is or whether or not anything is not meaningless if nothing is important then why are we talking about the possibility of nothing being important in the first place
if nothing is important then why is it important that nothing is important
there is a kind of tree that i like a lot that i think is sort of important
they are sort of like beech trees but they are not beech trees and you can peel off the bark horizontally like paper and dry it out on a table under the sun and staple or sew them together and use them to make small books or write letters to people if you want
this is not important i am going to pass out in a puddle of orange juice and i will stand up with a puddle of orange juice on my face
and people will say that is a large freckle on your face maureen
and my shirt will be orange and my pants will be orangey blue or something
and the internet says that the following things implode: light bulbs, galaxies, marshmallows
(when placed inside of microwaves which clearly have come from the mind of someone who wants to end the human race once and for all)

The lectures published in The Cosmic Microwave Background provide graduate students and young researchers with a survey of CMB radiation and an understanding of the latest research in this rapidly growing field. The lectures cover the anisotropy, spectrum and polarization of the CMB from both observational and theoretical viewpoints. The fundamental importance of the CMB is discussed in lectures on general relativity, inflation, structure formation, nucleosynthesis and primordial molecules. There is detailed coverage of statistical and data analysis techniques that are useful in CMB research.