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Topic: Intergalactic medium

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	American Scientist Online - The Cosmic Web (Site not responding. Last check: 2007-10-21)
		At regular intervals, the computer records the density of the gas throughout the intergalactic medium, and these results are compared with actual observations of quasar spectra to test the accuracy of the physical models.
		Heavy-element enrichment in low-density regions of the intergalactic medium.
		The distribution of metallicity in the intergalactic medium at redshift 2.5: OVI and CIV the spectra of 7 QSOs.
	www.americanscientist.org /template/AssetDetail/assetid/29667/page/1?&print=yes (4478 words)

	Timeline of the interstellar medium and intergalactic medium... - Wikipedia, the free encyclopedia
		Timeline of the interstellar medium and intergalactic medium...
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	en.wikipedia.org /wiki/Timeline_of_the_interstellar_medium_and_intergalactic_medium... (61 words)

	Timeline of knowledge about the interstellar and intergalactic... - Wikipedia, the free encyclopedia
		Timeline of knowledge about the interstellar and intergalactic...
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	en.wikipedia.org /wiki/Timeline_of_knowledge_about_the_interstellar_and_intergalactic... (61 words)

	Carnegie Observatories Research: Michael Rauch (Site not responding. Last check: 2007-10-21)
		Combining observations with computer simulations, Michael Rauch uses quasar absorption lines in the intergalactic medium to study the nature and distribution of matter in the early universe.
		To study these clouds, known as the intergalactic medium (IGM), scientists have to observe the "shadows" they cast on the spectrum of a bright background light source.
		And the width and depth of the absorption lines indicate the changes in the mean temperature of the intergalactic medium as a function of time, and yield information about the history of cosmic ionization.
	www.ociw.edu /research/rauch.html (584 words)

	Double Lobed Radio Galaxies (Site not responding. Last check: 2007-10-21)
		The intergalactic medium tries to slow the jet, just like water slows a swimmer or a boat; this causes material to be dragged along with the jet, just like the wake of a boat.
		Because the jet is moving with a much higher speed than the medium, shocks form at the ends of the jet.
		As they travel through the intergalactic medium, these jets may become twisted by the motion of the galaxy itself or even be made to change direction due to the streaming motions of the medium.
	www.astro.umd.edu /education/astro/actgal/lobed.html (386 words)

	IAU Symposium 217 Abstracts
		This tidally liberated material is being recycled directly into the intergalactic population of stars, dwarf galaxies, globular clusters, and gas, which may have been largely built from a multitude of similar events over the life of the cluster.
		There is plenty of intergalactic HI gas without any obvious stellar content ranging from tidal tails (still attached to pairs of interacting or merging galaxies), tidal bridges (often found between interacting galaxies), and HI clouds (at varying distances from associated galaxies) but there are few or no isolated HI clouds.
		The implications of galactic winds on the formation and evolution of galaxies and the intergalactic medium are briefly discussed.
	www.uni-sw.gwdg.de /~paduc/IAUsymp/S217.prog.abstracts.html (17601 words)

	[No title] (Site not responding. Last check: 2007-10-21)
		Most of the intergalactic medium at z < 1 is likely to be in a warm, highly ionized state, with a mean overdensity of ~10.
		The best hope of detecting the medium, either in absorption or emission, is by studying intergalactic Oxygen.
		I discuss a re-evaluation of the ionization balance of intergalactic O, and prospects for detecting discrete emission and absorption.
	www.xray.mpe.mpg.de /~bol/xeus/paerels.txt (104 words)

	The Search for the Intergalactic Medium
		A principal scientific goal for HUT on the Astro-2 Mission will be an attempt to detect the primordial intergalactic medium, a tenuous gas believed to pervade the vast reaches of space between the galaxies.
		It is widely believed that the energy radiated by the quasars themselves, perhaps along with radiation from the first generation of galaxies and stars, was responsible for re-ionizing the intergalactic hydrogen gas.
		The Hopkins Ultraviolet Telescope is well-suited to the task of observing intergalactic helium.
	praxis.pha.jhu.edu /astro2/astro2_science/HS1700.html (954 words)

	SPACE.com -- Helium Cobweb Found in Vast Spaces Between Galaxies (Site not responding. Last check: 2007-10-21)
		As the light passed through intergalactic clouds, helium atoms in the gas absorbed specific colors of the light in the far-ultraviolet range of the spectrum.
		By comparing the absorption caused by intergalactic hydrogen, which is visible in spectra from ground-based telescopes like the Keck Observatory, to the helium absorption seen with FUSE, astronomers are able to achieve a better understanding of the energy source.
		The HUT observations, led by the late Arthur Davidsen of the Johns Hopkins University, gave the first inkling that the intergalactic medium was not a smooth distribution of gas between the galaxies.
	www.space.com /scienceastronomy/astronomy/fuse_results_010809.html (1037 words)

	Article Not Found - Open Encyclopedia (Site not responding. Last check: 2007-10-21)
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	open-encyclopedia.com /Timeline_of_the_interstellar_medium_and_interga... (88 words)

	DARK MATTER
		A prediction of the Compton effect interpretation of the red shift is that there should be what is called "reverse dispersion" in signals as the light travels through this transparent intergalactic medium.
		This is in agreement with the reverse dispersion in the light traveling billions of light years through a transparent intergalactic medium of electrons and positrons.
		Intergalactic space is thought to be too cold to allow ionization of hydrogen as a source.
	www.angelfire.com /az/BIGBANGisWRONG/darkmatter2.html (393 words)

	Timeline of knowledge about the interstellar and intergalactic medium - Wikipedia, the free encyclopedia
		Timeline of knowledge about the interstellar and intergalactic medium
		(Redirected from Timeline of the interstellar medium and intergalactic medium)
		1965 - James Gunn and Bruce Peterson use observations of the relatively low absorption of the blue component of the Lyman-alpha line from 3C9 to strongly constrain the density and ionization state of the intergalactic medium
	en.wikipedia.org /wiki/Timeline_of_the_interstellar_medium_and_intergalactic_medium (262 words)

	HUT OBSERVATIONS OF THE INTERGALACTIC MEDIUM (Site not responding. Last check: 2007-10-21)
		The HUT science team's highest priority science goal on Astro-2 was to detect and measure the characteristics of the primordial intergalactic medium (IGM), a hypothesized gas thought to be spread throughout the Universe between the galaxies.
		While this is not nearly enough material to "close" the Universe or account for the so-called "missing mass" in clusters of galaxies and elsewhere, it does say that only something like 20% of the material created in the Big Bang actually coalesced into the "structure" (galaxies and stars) that we see in the Universe today.
		The rest of it is "out there" between the galaxies in the form of the exceedingly tenuous intergalactic medium.
	praxis.pha.jhu.edu /science/igm.html (598 words)

	Space Astrophysics Lab
		The Space Astrophysics Laboratory is engaged in a variety of experimental and observational projects studying galaxy evolution, the dynamic interstellar medium, neutron star physics, and the the intergalactic medium.
		Cosmological simulations and quasar absorption line studies reveal an intergalactic medium, a "Cosmic Web", that has a profound effect on the formation and evolution of galaxies, and shows the influence of galactic feedback.
		The goals of the Intergalactic Medium Project are to develop new instrumentation and observational techniques to detect IGM emission from the ground and in space and use it to map and characterize the Cosmic Web and its relationship to galaxies and to the underlying distribution of Dark Matter.
	www.srl.caltech.edu /sal (266 words)

	CLUSTER ENVIRONMENTS
		The intragalactic medium (IGM) in clusters and groups of galaxies is an important large-scale feature of the universe.
		The medium is important in its own right as it offers an extreme environment in which to study plasma processes.
		Faraday rotation by the medium between us and the radio sources probes the line-of-sight magnetic field and the thermal electron density.
	www.cv.nrao.edu /vla/upgrade/node90.html (404 words)

	ScienceWeek (Site not responding. Last check: 2007-10-21)
		In contrast, the intergalactic medium has a density of only 10^(-6) particles per cubic centimeter --each atom inhabits a private box a meter on each side.
		Although galaxies are arranged into gravitationally bound clusters and superclusters, it is the galaxies themselves that are usually considered to be the fundamental macroscopic units of the Universe.
		Perhaps a good analogy concerning the distribution of galaxies is to consider a flask containing a rather dense culture of bacteria in a liquid medium.
	scienceweek.com /2004/sa040723-1.htm (2998 words)

	phot-26-02.html
		The southern jet rams into the intergalactic medium, thereby producing a "shock" with particularly strong synchrotron emission (the radio intensity contours in image "b").
		The central area (with the strongest emission) indicates where the jet from the galaxy hits the intergalactic medium; the two others represent synchrotron emission from electrons accelerated in secondary processes at these sites.
		The central area (with the strongest emission) is where the plasma jet from the galaxy centre hits the intergalactic medium.
	www.eso.org /outreach/press-rel/pr-2002/phot-26-02.html (1069 words)

	WHIM group: publications (Site not responding. Last check: 2007-10-21)
		We have identified a large scale structure of galaxies at z=0.8 in the Lockman Hole by means of multi-object spectroscopic observations.
		By using deep XMM images we have investigated the soft X-ray emission from the Warm-Hot Intergalactic Medium (WHIM) expected to be associated whit this large scale structure and set a tight upper limit to its flux in the very soft 0.2-0.4 keV band.
		Several popular cosmological models predict that most of the baryonic mass in the local universe is located in filamentary and sheet-like structures associated with groups and clusters of galaxies.
	www.arcetri.astro.it /~zappacos/WHIM_group/publications.html (479 words)

	Visible Matter: Once lost but now found: Science News Online, Aug. 10, 2002
		The absorption of the X rays, indicated by the troughs in the spectrum (blue line) of the quasar dubbed PKS 2155-304, discloses the presence of oxygen atoms.
		The new studies "reveal that most of the visible matter in the universe is in the intergalactic medium," says theorist Jeremiah P. Ostriker of the University of Cambridge in England.
		absorption from an overdense region in the intergalactic medium.
	www.sciencenews.org /articles/20020810/fob1.asp (657 words)

	GSFC Photo Release 99-004P
		The tenuous gas, known as the intergalactic medium, is colored to indicate how transparent the medium is to extreme-ultraviolet light (fl = opaque; white = transparent).
		The intergalactic helium gas closer to Earth (and thus observed as it existed more recently) is fully ionized and transparent to extreme ultraviolet light.
		The prong of brightness at a redshift of 3.05 arises from a locally transparent region in the intergalactic medium.
	www.gsfc.nasa.gov /news-release/releases/1999/99-004p.htm (669 words)

	Big Bang Cosmology Meets an Astronomical Death
		Hence, the greater the depth of the intergalactic medium through which a galaxy's light must pass toward the low-energy end of the spectrum - that is, toward the red.
		In that case, the greater the depth of the intergalactic medium between a galaxy and the observer, the more its light is shifted toward the low-energy (red) end of the spectrum.
		A redshift from the interaction of photons with atoms in the galactic and intergalactic media was previously denied: Most scientists are accustomed to thinking that when photons interact with the medium through which they pass, losing some energy in the process, some significant angular dispersion of the photons must result.
	www.newtonphysics.on.ca /BIGBANG/Bigbang.html (6143 words)

	Re: what fills in the empty space in outerspace? nitrogen?i am not sure.
		The density is pretty low, around 1 atom per cubic centimeter (compared to 10 billion billion molecules in a cubic centimeter of air at sea level), and it's mostly made up of hydrogen atoms.
		The interstellar medium is found in the space between stars within our Galaxy.
		It is even less dense than the interstellar medium, but there is so much space in between the galaxies that when you add up all the gas which is probably out there, it appears likely to be more mass than all the rest of the "ordinary" matter we find in galaxies.
	www.madsci.org /posts/archives/2000-12/976744281.As.r.html (408 words)

	[No title] (Site not responding. Last check: 2007-10-21)
		In order to study the intergalactic medium, the project observes high redshift QSOs at the redshift ranges from 2 to 5.
		Using the UV sensitive UVES, this project enables us to study the intergalactic medium statistically at the redshift ranges at 1.5 to 2 from high signal-to-noise and high resolution data for the first time.
		The evolution of the intergalactic medium (IGM), as traced by the Lyman-alpha forest, at the redshift ranges from 1.5 to 4.5, in particular the line number density evolution at the redshift ranges from 1.5 to 2.5
	www.eso.org /science/qsolp/uves.html (820 words)

	Measurement of the opacity of ionized helium in the intergalactic medium (Site not responding. Last check: 2007-10-21)
		Measurement of the opacity of ionized helium in the intergalactic medium
		DETERMINATION of the density and ionization state of diffuse primordial gas in the intergalactic medium (IGM) is an important step towards understanding the nature of dark matter and the formation of structure in the Universe.
		This implies that intergalactic hydrogen is both highly ionized and non-uniformly distributed
	www.nature.com /cgi-taf/DynaPage.taf?file=/nature/journal/v380/n6569/abs/380047a0.html (360 words)

	Research
		Polluting the surrounding intergalactic gas this way affects the formation of new galaxies because most of the normal matter in the universe has yet to cool down and condense into galaxies.
		The impact of this reheating, or feedback, on the galaxy population and the intergalactic medium is quite pronounced.
		Their work suggests most of the heavy elements synthesized by the starburst are expelled from the galaxy, a result which helps explain the overall high level of chemical enrichment observed in the intergalactic medium.
	www.physics.ucsb.edu /~cmartin/research.html (1262 words)

	[64.14] Supershells and the Intergalactic Medium (Site not responding. Last check: 2007-10-21)
		They also provide connections between galaxies, their halos, and the intergalactic medium (IGM).
		Massive stars and OB associations probably affect the ISM of intervening disk galaxies and intergalactic Lya absorbers.
		Large portions of the IGM are strongly influenced by local effects, through the radiative and energetic feedback from massive star formation in the first galaxies.
	www.aas.org /publications/baas/v31n3/aas194/117.htm (180 words)

	Kurt Adelberger : Galaxies and the Interstellar Medium at z ~ 3 (Site not responding. Last check: 2007-10-21)
		Comparing the locations of galaxies to the locations of HI and metals in the spectra of background QSOs shows that the intergalactic medium contains little HI or CIV within ~0.5 comoving Mpc of Lyman-break galaxies but a significant excess of both at slightly larger radii.
		The intergalactic medium within the largest galaxy overdensities at z~3---i.e., the presumed young intracluster medium---contains a wealth of HI and metals.
		These results may show that supernovae-driven winds are able to escape the galaxies' potential wells and drive ~1 comoving Mpc into the surrounding intergalactic medium.
	cfa-www.harvard.edu /~tad/events/2001-2002/s_abstracts/13.html (301 words)

	Headlines@Hopkins: Johns Hopkins University News Releases
		This gas - composed almost entirely of hydrogen and helium, the two lightest elements - is the material that was formed during the first few minutes after the Big Bang, some 10 billion to 20 billion years ago.
		This is because a helium atom has two electrons that are more tightly bound to its nucleus, and it is therefore more difficult to ionize completely.
		They are therefore much more likely to present a clear, unambiguous case for (or against) the existence of intergalactic helium.
	www.jhu.edu /news_info/news/hut/hutafd.html (1004 words)

	e-Prints Soton - Heating of the intergalactic medium by FR II radio sources
		Heating of the intergalactic medium by FR II radio sources
		Kaiser, Christian R. and Alexander, Paul (1999) Heating of the intergalactic medium by FR II radio sources.
		We present results of a numerical integration of the hydrodynamical equations governing the self-similar, two-dimensional gas flow behind the bow shock of an FR II radio source embedded in an intergalactic medium (IGM) with a power-law density profile.
	eprints.soton.ac.uk /14768 (381 words)

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