
	Where results make sense

Topic: Subclump

	Image with caption (Site not responding. Last check: 2007-10-23)
		Note that the cold front associated with the merging sub-cluster appears behind the merger shock front to the left of two sub-clusters (z=0.43 panel).
		Note also the cold front associated with the merging subclump at z=0 to the left of the cluster center and the adjacent compressed region of enhanced temperature.
		The subclump is trailed by a relatively cold (~1-2 keV) intergalactic gas accreted along a filament.
	astro.uchicago.edu /~daisuke/Research/Tmp/Captions/cap_xray.html (119 words)

	dmtree2
		The evolution of subclumps in the DM merging trees.
		The dark spots represent the subclumps surving as overdens DM clumps (galactic DM haloes) with mass m inside the host haloes with mass M. Their evolution is explained in the text.
		The initial condition (at the bottom of the tree) is set assuming m=M. We shall refer to the subclumps as galactic clumps.
	lbc.mporzio.astro.it /menci/galtree1.html (592 words)

	Uncovered Structures and the Cluster Abell 3627
		Note the alignment of the subclump with the radio emission.
		The redshift data are yet too sparse to allow a kinematical analysis of this cluster, however, the redshifts in the subclump tend to be higher, suggesting that this subgroup is in front of the main cluster and falling towards it.
		The lack of distortion of the radiolobes of both radio galaxies and the compactness of the subclump imply that the suspected merger must be in an early stage.
	www.atnf.csiro.au /pasa/14_1/renee/paper/node4.html (737 words)

	Elliptical galaxy M 49 (Site not responding. Last check: 2007-10-23)
		M49 (NGC 4472) is by some measures the optically brightest galaxy in the Virgo cluster (about 60 million light-years away), slightly outshining M87.
		It lies in a subclump of the cluster about 4 degrees south of the cluster center.
		This pseudocolor image is from a red-light CCD frame taken with the Lowell Observatory 1.1-meter telescope (actually, it was taken to calibrate some narrow-band filters on a galaxy with no detectable H-alpha emission).
	www.astr.ua.edu /gifimages/m49r.html (72 words)

	[No title]
		Four b-galaxies are located within one subclump of galaxies in the cluster.
		Leir (1976) notes that a bright foreground galaxy is superimposed on the northern part of the cluster.
		472 Subclumps of galaxies are elongated in the approximate direction of the major axis of the cluster.
	cdsweb.u-strasbg.fr /ftp/cats/VII/96/notes (21751 words)

	7 Discussion
		It has a bright core and at least two faint extensions, similar to the morphology of the compact cores in the field sample of Steidel et al.
		The main subclump displays a compact morphology, which is not resolved in width on the WFPC2 images, thus implying length scales of the order of
		Its morphology and the equivalent (rest frame) width of Ly are similar to those of H5, one of the multiple images at z=4.05 identified in the core of A2390 (Pelló et al.
	aanda.u-strasbg.fr:2002 /papers/aa/full/2001/41/aa1416/node7.html (748 words)

	Scatter in the X-ray scaling relations
		Some of these contain subclumps that are falling into the cluster for the first time and which have raised its mass without yet significantly altering the emission-weighted temperature; others are clusters which are undergoing a core-bounce after a merger and for which the temperature is temporarily slightly too low.
		This has several advantages: the number of clusters showing substructure is reduced, the properties are measured at radii that are more accessible to X-ray observations, and the substructure that is measured is more directly related to subclumps that are interacting strongly with the intracluster medium and that will be influencing the X-ray properties.
		This cluster was even further from the line in the original plot (the topmost large triangle) but did not show up as having substructure because the subclump was too close to the centre.
	www.pact.cpes.sussex.ac.uk /~drr21/resim/node14.html (1144 words)

	Introduction
		They will have some amount of substructure, may be rotating and could collide with more than one subclump at a time.
		Therefore to find out what kind of mergers clusters tend to undergo and the effect this has on the complex ICM, full cosmological simulations need to be carried out.
		MBL03 undertook radiative simulations of a sample of two clusters and showed that the traditional model of smooth accretion onto clusters is inaccurate in that clusters accrete gas in subclumps which bring precooled gas direct to the core of a cluster.
	astronomy.sussex.ac.uk /~drr21/resim/node1.html (657 words)

	[No title]
		A possible explanation for such a lack of faint Coma members in this particular region of the cluster could be their tidal disruption in the core of the cluster, as described by S97.
		B95 reported the discovery of an optical subclump of galaxies (approximatively at
		Almost all of them correspond to the peak at z = 0.5 seen in Figure 2, and the corresponding spatial extension is 360 kpc at z = 0.5107 (mean redshift of the structure).
	www.cfht.hawaii.edu /Reference/Bulletin/Bull39/bulleti3.htm (1525 words)

	X-Ray Multimodality in A2151 (Site not responding. Last check: 2007-10-23)
		As also seen in the Einstein image of this cluster, this peak is bimodal, with no corresponding feature in the galaxy distribution.
		The western subclump, apparent in the optical contour map is indistinguishable from the main clump in velocity space and is only a 2$\sigma$ enhancement of the X-ray background, The three group partition of the optical data is a significant improvement over the one group fit, at a $>99.9$\% confidence level.
		X-ray spectra derived from the central peak of emission yield a best-fit temperature of 1.6 keV.
	www.aas.org /publications/baas/v25n4/aas183/abs/S506.html (283 words)

	Intracluster Stars and the Structure of the Virgo Galaxy Cluster
		The number of intracluster planetaries varies significantly from field to field, generally dropping off with distance from the cluster center.
		The intracluster planetaries in subclump A of Virgo (Fields 1, 3, 4, 5) are a few Mpc less distant from us than those in subclump B (2 and 6).
		Although the presence of intracluster stars complicates the distance determination of the Virgo cluster, the same stars can serve as a powerful probe of the structure and history of the cluster itself.
	www.noao.edu /noao/noaonews/dec98/node2.html (814 words)

	Jacqueline van Gorkom - Research
		Based on the HI kinematics we conclude (surprisingly) that ram pressure stripping is ongoing at this large distance from the center.
		Perhaps this is due to subclump merging and a first hint of "preprocessing" before the galaxy falls into the cluster.
		This illustrates that detailed observations of galaxies in a nearby cluster can constrain the mechanisms that affect the evolution of the galaxy.
	www.astro.columbia.edu /~jvangork/research.html (744 words)

	Citebase - Exploring Cluster Physics with High-Resolution Sunyaev-Zel'dovich Effect Images and X-Ray Data: The Case of ...
		We demonstrate that the combined analysis yields a unique probe of complex structures in the intracluster medium, offering determinations of their temperature, density, and line-of-sight extent.
		For a subclump in RX J1347-1145, previously discovered in our SZE map, the temperature inferred after removing the foreground and background components is well in excess of 20 keV, indicating that the cluster has recently undergone a violent merger.
		Excluding the region around this subclump, the SZE signals in submillimeter to centimeter bands (350, 150, and 21 GHz) are all consistent with those expected from Chandra X-ray observations.
	www.citebase.org /cgi-bin/citations?id=oai:arXiv.org:astro-ph/0311574 (319 words)

	3 Results and discussion
		The galaxy masses alone are not sufficient to produce the observed multiple images, however indicate the same substructure as a "guess by the eye'' lens modelling would derive for the dark matter distribution.
		Next we admitted three additional dark matter distributions (modelled by EISC) at the southern and northern subclump of the center of E0657, and at the brighter one of the two galaxies west of the arc.
		The positions of these dark matter distributions were allowed to vary as well, however did not change much from the optically guessed center.
	aanda.u-strasbg.fr:2002 /papers/aa/full/2001/43/aa1304/node3.html (2782 words)

	Essay (Site not responding. Last check: 2007-10-23)
		Although M87 is most often taken as the center of the Virgo Cluster, it is off the center (density peak) of A by approximately 1° in the direction toward C.
		Rather, the central part of the Virgo Cluster seems to consist of a small number of subclumps of galaxies, one of which is defined by M87 alone.
		However, as a result of "dynamical friction," the subclumps will rapidly merge.
	www.astro.bas.bg /~petrov/galaxies_files/clustgal.html (3293 words)

	XMM-Newton observation of the most X-ray-luminous galaxy cluster RX J1347.5-1145 (Site not responding. Last check: 2007-10-23)
		We present the first temperature map of this cluster, which shows a complex structure.
		It identifies the cool core and a hot region at radii 50-200 kpc to south-east of the main X-ray peak, at a position consistent with the subclump seen in the X-ray image.
		This structure is probably an indication of a submerger event.
	www.edpsciences.org /articles/aa/abs/2004/43/aagg161/aagg161.html (227 words)

	Worlds.com \| Gamma Documentation \| Advanced Development
		The subclump ordering is determined by rwxtobod when it creates the
		It is important that the hierarchy and labels of this model are exactly right; review the actual RWX file in a text editor before proceeding to ensure that the subclumps are all in the proper hierarchy and labeled correctly.
		Follow the instructions above in “Custom Avatar Language” to create a string that describes what textures are applied to which limbs and subclumps of the model.
	www-static.us.worlds.net /private/GammaDocs/Gamma_Advanced.html (10321 words)

	THE ROSAT PSPC OBSERVATIONS OF A85 CLUSTER OF GALAXIES: THE BARYONIC AND DARK MATTER DISTRIBUTIONS
		We could follow the intracluster gas emission with 3
		We derived the density profile of the intracluster gas (after excluding a southern subclump from the profile fit), which we used, together with the best fit ASCA GIS temperature of the gas, to calculate the profile of total gravitating mass M, using an equation for hydrostatic equilibrium.
		Galaxies are the most centrally concentrated mass component, while the gas mass density profile is quite flat, and the dark matter profile is intermediate between the two.
	www.astro.helsinki.fi /abstracts/jukkan/jukka.html (260 words)

	Purpose Verses - Chapter 17
		I'm not sure if it's bad or if it's just normal that local gatherings of Christians tend to clump together by socioeconomic groupings.
		I suspect it's just normal that when a whole bunch of people share a belief, they will tend to subclump into groups where they are most similar in other ways as well.
		In a setting where there are fewer believers, there is greater diversity in a given clump.
	www.purposeverses.com /17.aspx (2851 words)

	Varosi vlib AstroContrib Library
		Procedure returns two arrays: Clump_Beg and Clump_End which specify all the consecutive runs in the input array SubScripts.
		The consecutive subscripts are then given by the Loop: for j=0,n_elements(Clump_Beg)-1 do begin SubClump = SubScripts(Clump_Beg(j):Clump_End(j))
		INTERLEAVE Determine the interleaving of two arrays of numbers, by returning subscripts of the interleaving elements, basically binning the array B into bins defined by array A. Note that the input arrays can be in any order (non-sorted), but for using result of this function you probably want A sorted first.
	www.astro.washington.edu /deutsch/idl/htmlhelp/slibrary21.html (7016 words)

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