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Topic: Galaxy filament

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	Dictionary of Meaning www.mauspfeil.net (Site not responding. Last check: 2007-10-20)
		The large elliptical galaxy at the centre is the [[Lenticular Galaxy M84; the elongated image of NGC 4388 (an active spiral galaxy) is in the lower left corner..html" title="Meaning of thumb250pxA sky field near some of the brighter galaxies in the Virgo cluster.
		The large elliptical galaxy at the centre is the [[Lenticular Galaxy M84; the elongated image of NGC 4388 (an active spiral galaxy) is in the lower left corner.">thumb250pxA sky field near some of the brighter galaxies in the Virgo cluster.
		The large elliptical galaxy at the centre is the [[Lenticular Galaxy M84; the elongated image of NGC 4388 (an active spiral galaxy) is in the lower left corner.
	www.mauspfeil.net /Virgo_cluster.html (879 words)

	Intergalaktische Wetterstation meldet Schockfront (Site not responding. Last check: 2007-10-20)
		The giant radio galaxy NGC 315 is one of the biggest known radio galaxies due to its several million lightyears long jets of radio gas (see Fig.
		An investigation of the galaxy distribution around NGC 315 reveals that the giant radio galaxy is located at a position within the Pisces-Perseus filament of galaxies (Fig.
		The galaxies of several sub filaments, which hit the main filament close to the position of NGC 315, are marked by colours.
	www.mpa-garching.mpg.de /HIGHLIGHT/2002/highlight0203_e.html (901 words)

	Optical Morphology
		The optical filaments associated with the minor axis outflow are visible across the entire field, to radial distances of at least 3.5 kpc to the north and 2 kpc to the south.
		The faintness of the northern filaments is almost certainly due to obscuration by the inclined disk of the galaxy (cf.
		This is consistent with the similar morphologies of the filaments beyond this radius in the north and south in Figure 8.
	www.astro.caltech.edu /~pls/papers/apj/m82_1/node13.html (780 words)

	Supercluster - Wikipedia, the free encyclopedia
		Superclusters are large groupings of smaller galaxy groups and clusters, and are among the largest structures of the cosmos.
		The existence of superclusters indicates that the galaxies in our Universe are not uniformly distributed; most of them are grouped together in groups and clusters, with groups containing up to 50 galaxies and clusters up to several thousand.
		Superclusters are frequently subdivided into groups of clusters called galaxy clouds.
	en.wikipedia.org /wiki/Supercluster (234 words)

	Sacramento Peak: Supercluster (Site not responding. Last check: 2007-10-20)
		Distances to galaxies and galaxy clusters are much more difficult to determine than the directions to those objects, so distances between such objects are usually much more accurate perpendicular to the radial direction than they are in the radial direction.
		A definition for superclusters that has less ambiguity would be a group of galaxy clusters that are bound together by gravity, just like the Sun, all the planets, and all other objects in the solar system are bound together by gravity.
		Our galaxy lies in the Canes Venatici cloud of galaxies on the outskirts of the Local Supercluster, of which the Virgo galaxy cluster is the central part [2].
	www.sunspot.noao.edu /sunspot/pr/tree/supercluster.html (451 words)

	Processed Images 2
		Comparing the luminosity profiles of a galaxy and a nebula has led me to conclude that their luminosity profiles are different.
		Using the isophotes method of contouring, I attempted to establish that the filament was connected to the bright spot.
		Contouring seemed to suggest that the bright spot was either a branch of the filament that was less intense then the original, or not part of the filament at all.
	home.cc.umanitoba.ca /~umhoepp3/Processed_Images_2.html (1812 words)

	The Extended Gaseous Medium Surounding Markarian 315 (Site not responding. Last check: 2007-10-20)
		We have mapped the HI associated with Markarian 315 using the VLA in the C-array and find it is located in a 60-100 kpc h^-1 filament which is displaced by 60 kpc h^-1 to the SE of the galaxy nucleus.
		The velocities of the neutral (HI) gas are interleaved with those of the ionized gas in the main body of the galaxy and those in the ionized filament.
		This close association between the ionized and neutral gas velocities suggests that the surounding gas is interacting with the galaxy but the disjoint morphology of the ionized and neutral gas implys that the interaction must be complex.
	www.aas.org /publications/baas/v28n2/aas188/abs/S004005.html (153 words)

	Astronomy Answers: Universe Family Tree: Supercluster (Site not responding. Last check: 2007-10-20)
		Usually it is decided which galaxy clusters together form a supercluster by looking at the distances between the galaxy clusters.
		Distances to galaxies and galaxy clusters are much more difficult to determine than the directions in which those objects are, so distances between such objects are usually much more accurate perpendicular to the radial direction than they are in the radial direction.
		The Virgo galaxy cluster is the only rich galaxy cluster in the Local Supercluster, and none of the listed galaxy clouds has its center further from the Virgo cluster than our own.
	www.astro.uu.nl /~strous/AA/en/boom/supercluster.html (388 words)

	Observing Galaxy Clusters (Site not responding. Last check: 2007-10-20)
		At a distance of roughly 40 million light years, the Virgo Cluster is the nearest rich aggregation of galaxies in the sky, and a target that will repay many evenings of careful study at the eyepiece.
		Among the brighter galaxy clusters here are the Hydra I Cluster (Abell 1060) around NGC 3309 and 3311, the Centaurus Cluster (RCG 3526) dominated by NGC 4696 and 4709, and the cluster around IC 4329.
		This huge filament of galaxy clusters extends from the Perseus Cluster (Abell 426) through Abell 347 and Abell 262 in Andromeda into the NGC 507 and NGC 383 galaxy groups in northern Pisces.
	www.angelfire.com /id/jsredshift/agcintro.htm (913 words)

	[No title]
		The central cD galaxy, a little South of the Northern peak of the filament, has a peculiar velocity of +350km/s with respect to the rest of the cluster galaxies, and is oscillating back and forth within the cluster core.
		Most of the Halpha gas in the filament has a velocity centred on the cluster mean velocity, and may also be sloshing in the cluster potential.
		The cooling filament is intimately related to the radio jets and lobes from the radiosource 4C+26.42 (van Breugel et al.
	aramis.obspm.fr /~galaxy/news2.html (1114 words)

	Bad Astronomy and Universe Today Forum - Anomalous red shifts and QSO-ejecting galaxies (Site not responding. Last check: 2007-10-20)
		Galaxies eject ultra-luminous X-ray (ULX) quasi-stellar objects (QSOs) whose red shift is anomalously high compared to its parent galaxy.
		Well, the angular diameter of the galaxy is about 80 arc seconds, so if you take a look at the first image of the galaxy, you can see that it must fall in the highest surface brightness part of the disk.
		He noted early on that not all galaxies in his atlas of peculiar galaxies were indicating evidence for association with quasars - they were found predominately among specific categories of peculiar galaxies #'s 100 to 160 in his catalog if I'm remembering right.
	www.badastronomy.com /phpBB/viewtopic.php?p=332541&highlight= (6398 words)

	Astronomy Update 1996 (Site not responding. Last check: 2007-10-20)
		The year was topped by the Hubble Deep Field, which revealed a spectacular number of galaxies within an area of sky 2.5 minutes of arc wide, a cascade of new planets (the result of dramatically improved technology), the resuscitation of the possibility of life on Mars, and of course the wonderfully popular Comet Hyakutake.
		The Young Galaxy Survey used a filter that was centered on the Lyman alpha line so that the investigators could pick up very distant galaxies that were emitting radiation as a result of their young stars.
		Galaxies seem to have formed almost at the same time the Big Bang was able to cool off to the point of allowing star formation.
	www.astro.uiuc.edu /~kaler/glpa/update96.html (7734 words)

	COLLECTED ABSTRACTS (Site not responding. Last check: 2007-10-20)
		All galaxies have redshifts in the range 2.16 \pm 0.02, centered around the redshift of the radio galaxy, and are within a projected physical distance of 1.5 Mpc from it.
		The direction of the filament is similar to that of the radio source axis, the large scale distribution of the other protocluster members, the 150 kpc-sized emission-line halo and the extended X-ray emission associated with the radio galaxy.
		The second galaxy is 1.3 $h_{50}^{-1}$ Mpc away from the radio-galaxy, is marginally resolved and, in addition to Ly$\alpha$ in emission, shows CIV in emission with a broad component indicating the contribution from an AGN.
	www.strw.leidenuniv.nl /~overzier/science/protoclusters.html (8876 words)

	Galaxy cluster cloud - Wikipedia, the free encyclopedia
		Wikimedia needs your help in the final days of its fund drive.
		In astronomy, a galaxy cluster cloud is a denser part of a galaxy supercluster, consisting of several galaxy clusters.
		The most well-known example is the Canes Venatici cloud of the Virgo supercluster, which harbours our own galaxy, the Milky Way.
	en.wikipedia.org /wiki/Galaxy_cluster_cloud (86 words)

	THE INFINITE UNIVERSE Chapter 5-4
		When AGNs descend from old galaxies or old g-galaxies (5-1) then part of the redshift of many AGNs (as well as other objects that originate from old galaxies or old g-galaxies, as may be the case with NGC 7603B, 5-4) may be due to gravitational redshift.
		The redshift quantization of quasars (5-4) may be due to galaxies or g-galaxies being in certain regions of space (5-4) (thus their distances may cause certain quantized amounts of tired light redshift).
		The foreground galaxy (with z=.04) that is in the middle of the 4 quasars (not shown in Fig.
	www.eitgaastra.nl /timesgr/part5/4.html (5741 words)

	The Formation of a Giant Elliptical Galaxy
		Three of the galaxies fall down a line which can be identified with the primordial filament apparent in the early formation of the dark matter cluster.
		The epoch around z=0.4 is marked by a period of intense activity in which many of the galaxies are merging and experiencing strong tidal perturbations resulting in tidal tails from close passes with the cluster center (Fig 4) and is an illustration of the galaxy harassment process (Moore et al.
		Of the 41 ``missing'' galaxies, 13 have merged to form the central massive elliptical galaxy.
	www.cita.utoronto.ca /~dubinski/bcg/node5.html (414 words)

	A Deep Optical Galaxy Search in the Southern ZOA
		Above this band, distinct filaments and round concentrations uncorrelated with the foreground dust can be recognized, thus they must have their origin in extragalactic large-scale structures.
		Lifting the obscuring veil of the Milky Way by correcting the observed properties of the galaxies for the foreground extinction would, in fact, reveal this cluster as the most prominent overdensity in the southern sky.
		Redshift measurements are required to map the galaxies in 3 dimensions.
	www.atnf.csiro.au /pasa/14_1/renee/paper/node2.html (449 words)

	Study of a field in the Coma Supercluster. I. Automated galaxies count
		The existence of a filament of galaxies was shown by Fontanelli (1984) in the Coma cluster region.
		The galaxy selection was made using a classical Bayesian classification based on the diagram of the integrated density versus the area.
		A histogram of all the galaxy magnitudes shows that the catalogue is apparently complete down to about the 19th magnitude.
	www.cs.wisc.edu /niagara/data/nasa/7159.xml (319 words)

	WHIM: filamentary evidences
		Scharf2000: Evidence for X-ray emission from a large-scale filament of galaxies ?
		Tittley2001: A Filament between Galaxy Clusters A3391 and A3395
		Bagchi2002: Evidence for Shock Acceleration and Intergalactic Magnetic Fields in a Large-Scale Filament of Galaxies ZwCl 2341.1+0000
	www.arcetri.astro.it /~zappacos/WHIM_filaments.html (70 words)

	[No title]
		Surveys undertaken over the past few decades to map the distribution of galaxies in the nearby universe have revealed a cosmic landscape of wondrous diversity, with richly populated galaxy clusters, filamentary and sheet-like superclusters and enormous voids.
		Clusters are often located at the vertices where multiple filaments merge; the cluster orientation is determined by the direction of the most prominent filament.
		In both cases a massive galaxy forms not by random isotropic mergers but instead by mergers which tend to occur along a preferred axis whose orientation is dictated by the surrounding large-scale filamentary structure.
	www.astro.ubc.ca /E-Cass/1997-DS/West/west-bil.html (3062 words)

	First Detection of CO in a Cooling Flow
		A large fraction of the mass in rich clusters of galaxies is under the form of diffuse hot gas (10 millions of degrees) observed in X-ray thermal emission.
		The rich cluster of galaxies Abell 1795 has been known for a long time to host a cooling flow; the gas temperature measured from X-ray emission is dropping by a factor 3 towards the core, at about 140kpc from the centre.
		In summary, the peculiar morphology of the cooling gas (X-ray, Halpha, blue continuum, molecular gas) appears to avoid the radio lobes, and is associated kinematically to the cluster as a whole, and not to the central cD galaxy.
	www.obspm.fr /actual/nouvelle/dec03/cool1795.en.shtml (1114 words)

	Imagine the Universe News - 03 April 2003
		The observation reveals distant and massive galaxies dotting the sky, clustered together under the gravitational attraction of deep, unseen pockets of dark matter.
		Galaxies and intergalactic gas are strung like pearls on unseen filaments of dark matter, which comprises over 85 percent of all matter.
		The galaxies that the team saw with Chandra were either dim or altogether undetectable with optical and radio telescopes.
	imagine.gsfc.nasa.gov /docs/features/news/03apr03.html (803 words)

	Chandra :: Photo Album :: Abell 1795 :: 04 Dec 00
		The filament was most likely caused when an enormous elliptical galaxy (white spot at the head of the filament) moved through the cluster core.
		Hot gas spread throughout the cluster is drawn by the gravitational field of the giant galaxy into a cosmic wake of cooling gas, which appears as the long string-like feature in the middle of this image.
		Most observed galaxies in the universe appear in groups ranging from simple pairs and trios to complex clusters of thousands.
	chandra.harvard.edu /photo/2000/0163 (308 words)

	Supercluster biography .ms (Site not responding. Last check: 2007-10-20)
		The superclusters dictates that the galaxies in our Universe are not uniformly distributed; most of them are grouped together in groups and clusters, with groups containing up to 50 and clusters several thousand galaxies.
		No clusters of superclusters are known, but the existence of bigger structures than supercluster is debated (see Filament (astronomy)).
		Interspersed among these superclusters are large voids of space in which few galaxies exist.
	supercluster.biography.ms (203 words)

	APOD: 2000 December 8 - Abell 1795: A Galaxy Cluster s Cooling Flow (Site not responding. Last check: 2007-10-20)
		clusters of galaxies millions of light-years across, are immersed within tenuous clouds of hot gas which glow strongly in x-rays.
		galaxy clusters, the gas appears to be cooling.
		At the very top of the filament is a large, x-ray bright galaxy.
	antwrp.gsfc.nasa.gov /apod/ap001208.html (202 words)

	SPACE.com -- Early Universe Was Spongy, Like Brain (Site not responding. Last check: 2007-10-20)
		These proto-galaxies stream along the filaments (red shows medium density) and meet at nodes, causing a buildup of galaxies.
		And they were found to lie within a tubular region of space -- a filament -- supporting a popular theory of the cosmic web, involving filaments stuffed with protogalaxies.
		Over billions of years, the filaments were replaced by large clusters of galaxies connected by bridges -- the remains of the largest of the original filaments.
	www.space.com /scienceastronomy/astronomy/spongy_universe_010522-1.html (608 words)

	[89.10] An 80 Mpc filament of galaxies at redshift z=2.38 (Site not responding. Last check: 2007-10-20)
		We present the detection of 34 Lyman-alpha emission-line galaxy candidates in a 80 x 80 x 60 co-moving Mpc region surrounding the known z=2.38 galaxy cluster J2143-4423.
		The distribution of galaxies suggests a filament or cross-section of a great wall at least 80 x 10 Mpc in transverse extent.
		Three of the candidate galaxies and one previously discovered galaxy have the large luminosities and extended morphologies of ``Lyman-alpha blobs''.
	www.aas.org /publications/baas/v35n5/aas203/1182.htm (233 words)

	Abell 3560, a galaxy cluster at the edge of a major merging event (Site not responding. Last check: 2007-10-20)
		We analyze also temperature maps, dividing the cluster into 4 sectors and deriving the temperature profiles in each sector: we find that the temperature drop is more sudden in the sectors which point towards the A3558 complex.
		From VLA radio data, at 20 and 6 cm, we find a peculiar bright extended radio source (J1332-3308), composed of a core (centered on the northern component of the Dumb-bell galaxy), two lobes, a "filament" and a diffuse component.
		The morphology of the source could be interpreted either by a strong interaction of the radio source with the intracluster medium or by the model of intermittency of the central engine.
	www.edpsciences.org /articles/aa/abs/2002/46/aa2704/aa2704.html (360 words)

	MM Papers: Gunn-Peterson test using a filament (Site not responding. Last check: 2007-10-20)
		Using CCD detectors onboard the forthcoming X-ray observatories Chandra and XMM, it is possible to devise a measurement of the absolute density of heavy elements in the hypothetical warm gas filling intercluster space.
		The proposed measurement would make use of a unique filament of galaxy clusters spanning over 700/h_50 Mpc (0.1
		A CCD moderate energy resolution (Delta E~ 100 eV) is adequate for detecting an absorption edge at a known redshift.
	hea-www.harvard.edu /~maxim/papers/sc (216 words)

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