
	Where results make sense

Topic: Galaxy morphology

	Astronomy Online
		The Seyfert galaxy is a galaxy with such an active nucleus (probably powered by a large fl hole) and results in a brighter than usual bulge.
		In the constellation Canes Venatici, shining at a visible magnitude of 8.4 is the Whirlpool Galaxy, or M51.
		This galaxy is similar to M51 in that its distance is also 35 million light years away and its luminosity is also that of 10 billion Suns.
	astronomyonline.org /Astrophotography/GalaxyMorphology.asp (1775 words)

	Galaxy classification - Wikipedia, the free encyclopedia
		Astronomers classify galaxies based on their overall shape (elliptical, spiral or barred spiral) and further by the specific properties of the individual galaxy (for example degree of ellipse, number of spirals or definition of bar).
		From this, astronomers have constructed a theory of galaxy evolution which suggests that ellipticals are, in fact, the result of collisions between spiral and/or irregular galaxies, which strip out much of the gas and dust and randomize the orbits of the stars.
		Galaxies and the Universe - an introduction to galaxy classification
	en.wikipedia.org /wiki/Hubble_sequence (1031 words)

	Colour-Magnitude Relation for Elliptical Galaxies
		Another strong morphological correlation is between galaxy morphology and galaxy density - with early-type galaxies (E/S0/Sa) being preferentially found in regions of higher galaxy density (the cores of rich clusters of galaxies) and later-type spiral galaxies inhabiting the lower density surrounding regions (termed the ``Field'').
		The galaxy colours are measured from the apparent magnitudes of the galaxies in two different regions of their spectra: through a filter in the blue (B) around 4500Å and one in the infrared centred close to 8100Å, called the I band.
		The linear relation for the brighter galaxies indicates that most of the E and S0 galaxies within the cluster were formed via the same mechanism and that this mechanism couples the colour of the stars formed within the galaxy to the final mass of the galaxy.
	www.astro.su.se /~ostlin/ColMag/Source/colMag_intro.html (1365 words)

	[No title]
		Galaxies are fundamental units of matter in space, and determining how they formed and achieved their current state is of critical importance to many issues in astronomy.
		Galaxies at extremely large distances (several billion light years, where 1 light year is the distance light travels in one year) are being seen as they were when the Universe was considerably younger than it is now.
		It is expected that the morphology of galaxies would undergo significant changes during their formative period, and it is likely that very distant galaxies are showing the structures they had before a steady state had been achieved.
	bama.ua.edu /~rbuta/gvatlas/intro.html (1019 words)

	Galaxy Morphology
		Galaxies are collections of stars, and clouds of gas and dust that are bound together by their mutual gravity.
		But not all galaxies have these ferocious beasts at their cores, some merely have large clusters of young stars, while others have a nucleus that is dominated by large numbers of old stars.
		Galaxy collisions are quite frequent, and can generate a large amount of star formation as the gas and dust clouds are compressed as they run into each other.
	ganymede.nmsu.edu /astro/a110labs/labmanual/node14.html (5632 words)

	JRASC book reviews August 1999 (Site not responding. Last check: )
		Galaxy morphology is the study of such shapes; its thoughtful application can go far towards overcoming the limits imposed by biology.
		This aspect of morphology is much more amenable to automation than the subtleties of spiral arm patterns, which also do not occur in galaxies occupying high-density environments.
		The study of elliptical galaxy morphology, once considered boring (if you’ve seen one elliptical...) has blossomed with the help of detector technology into one of the most active areas of galaxy research.
	www.rasc.ca /reviews/jrascreview081999.html (2441 words)

	Galaxy Structure
		Studying the structure of galaxies can provide informations on their time of formation and, consequently, on the structure of the early Universe, the subsequent history and evolution, the distribution and amount of dark matter (thus posing costraints on its nature and composition).
		Studies of galaxy structures are concerned with measuring the intrinsic properties of the different components of these objects and their mutual relations both in the local Universe and at medium and high redshift.
		We are involved both in photometric studies, to detail the galactic morphology, and kinematic studies, to infer the mass distribution and the orbital structure, and decouple the different contribution of the different components.
	www.sissa.it /ap/GalStruc (310 words)

	Something and Nothing
		How were large galaxies able to form in the early stages of the Universe?
		Do all galaxies form at a single, well-defined epoch or is galaxy formation spread out in time?
		Why is there a correlation between the mass of the supermassive fl hole in the center of a galaxy
	www.idicalif.com (1622 words)

	[No title] (Site not responding. Last check: )
		Relationship of Galaxy Morphology to the Intra-cluster Medium: an NVO Demonstration Ray Plante and Jim Annis Version 2.0 Abstract The NVO is developing three demonstrations of VO principles as part of its first year efforts.
		Morphology will be characterized by three parameters--mean surface brightness, concentration index, and asymmetry index--which we will calculated directly from images of the galaxies.
		A galaxy's radio flux could be a further indicator of galaxy encounters which could be explored via a comparison with the morphological parameters.
	www.us-vo.org /pubs/files/morphdemo-plan2.txt (1352 words)

	[43.03] COSMOS Galaxy Morphology Pilot Project (Site not responding. Last check: )
		Morphology has been derived from both g and i ACS images in terms of bulge/disk ratio and Sersic index.
		These measures have been augmented by CAS and Gini coefficients as a way of identifying galaxies that are disturbed or interacting, or where the axisymmetric assumptions of GALFIT are not warranted.
		We present results on how morphology correlates with global quantities such as luminosity, scale length, and mean surface brightness as well as with various broad band color combinations, which serve as proxies for overall stellar populations and ages.
	www.aas.org /publications/baas/v36n2/aas204/570.htm (237 words)

	Exploring Galaxy Morphology with GalCrash
		Now try a simulation of the Cartwheel galaxy, which is shown in figure 23-17 of the textbook.
		A larger version of the Cartwheel Galaxy image is available from the Space Science Telescope Institute, that shows the Cartwheel along with two neighboring galaxies, each of which could possibly be the galaxy the cartwheel collided with.
		In section 23.2, the textbook discusses two possible ways to form an elliptical galaxy, the second of which is colliding two spiral galaxies together.
	www.uh.edu /~vanderse/astronomy/galcrash.html (712 words)

	[40.09] Classifying galaxy morphology with MatLab (Site not responding. Last check: )
		Using morphology classifications for galaxies provides a direct approach to probe galaxy populations back to an early stage in their lifetime, and hence to study many astrophysical problems such as large-scale structure, galaxy formation and galaxy evolution.
		Current galaxy classification systems are generally built on the visual characteristics of an image, such as magnitudes and colors and not on the shape of the galaxy.
		The galaxies used are face-on and large in spatial extent.
	www.aas.org /publications/baas/v36n2/aas204/782.htm (225 words)

	Phase 1 Proposal
		This sample of about 40 merging galaxy pairs will be compared with the parent sample of 800 galaxies to yield a clear estimate of the high redshift merger rate.
		The UV and blue light from galaxies is dominated by short-lived, high mass stars and is therefore a poor indicator of stellar mass.
		The actual SED of a galaxy is determined from its colours and compared to the synthetic SEDs to determine its star formation history and therefore its current stellar mass.
	astrowww.phys.uvic.ca /~gwyn/MMM/MMM.html (2938 words)

	[No title] (Site not responding. Last check: )
		Most galaxies in the universe are spiral signified by the abbreviation S followed by a lower case letter of the alphabet.
		A lenticular galaxy is a galaxy that appears lens-shaped.
		A lenticular galaxy is somewhere between a spiral galaxy and an elliptical galaxy and is signified by the abbreviation SO.
	home.cc.umanitoba.ca /~ummar143/morph.htm (130 words)

	Catalogue: J/ApJS/157/228/catalog
		Galaxy luminosity profiles are fitted with three models: exponential disk, de Vaucouleurs bulge, and a disk-plus-bulge hybrid model.
		The best fit is selected and produces a quantitative assessment of the morphology of each galaxy: the principal parameters derived being B/T, the ratio of bulge to total luminosity, the scale lengths and half-light radii, axial ratios, position angles, and surface brightnesses of each component.
		Note (4): The errors are mostly reliable for the single component models, and are given in the hybrid model case to indicate the average precision of the measurements.
	vizier.u-strasbg.fr /cgi-bin/Cat?J/ApJS/157/228/catalog (573 words)

	Galaxy Classification Lab - Astro 113 - Matthew A. Bershady
		Galaxies are some of the most beautiful and intriguing objects in the night sky.
		The problem with galaxies is, to quote one turn-of-the-century German astronomer: "Es gibt kein zwei Nebelflecken am Himmel, die sich gleichen" (Wolf 1908).
		Since no two galaxies are identical, when you classify other galaxies by comparing them to your reference sequence, you will have to estimate whether they are closer to one 'type' or another.
	www.astro.wisc.edu /~mab/education/astro113/galclass_lab.html (2607 words)

	Social Reasoning, Anxiety, and Collaboration with Rejected and Average Children Kimberly Crosby, M.A. Marcy ...
		If average is > 2 then it is labeled an irregular galaxy, if average is < 2 then it is labeled an elliptical galaxy.
		If armed structure are found (traced in red) using the profile vectors the galaxy is labeled a spiral.
		galaxies would become correct and some that were correct become incorrect.
	www.phys.ttu.edu /~diazabel/morphposter_files/slide0001.htm (612 words)

	[No title]
		The philosophy here is that galaxy morphology is not so mysterious that we cannot say anything about the physical meaning of observed features.
		The subtle morphological differences between the two galaxies in the upper panels and the two in the lower panels are highlighted with the notation in Figure 1.
		Galaxies later known as ``flocculent'' spirals by Elmegreen and Elmegreen (1987) were denoted high multiplicity, filamentary spirals by de Vaucouleurs (1956).
	bama.ua.edu /~rbuta/gvatlas/plan.html (2044 words)

	[No title]
		The PASP paper Near-Infrared Galaxy Morphology Atlas presents a full statistical analysis of the atlas.
		We then deduce the J and H peaks using the color of a "normal" galaxy (again, we have converted the mags to a calibrated flux unit).
		In a related case, there may be a bright foreground star near the core of the galaxy that fools the extended source processor and uses the star as the central position.
	www.ipac.caltech.edu /2mass/gallery/galmorph/2mass_galmorp.html (926 words)

	Observable physical properties of galaxies
		However, note that LSB galaxies tend to be later types, and, since these are not included, there may be a bias here.
		Galaxy luminosity functions: let's further consider the range of luminosities found in galaxies, both overall and as a function of morphological type.
		In addition, the luminosity function of galaxies is an important cosmological probe for evolution of the galaxy population, as we'll discuss more later.
	astronomy.nmsu.edu /holtz/a616/ay616/node3.html (1054 words)

	Galaxy Morphology and Classification - Cambridge University Press
		The classification of galaxies according to their shape is a fundamental tool in astronomy.
		It is through classification schemes that astronomers build a deeper understanding of how galaxies form and evolve.
		This long-awaited book by one of the pioneers of the field provides a concise and up-to-date summary of current ideas about galaxy morphology and classification.
	www.cambridge.org /catalogue/catalogue.asp?isbn=0521623359 (408 words)

	Morphology of Galaxy Mergers at Intermediate Redshift (Site not responding. Last check: )
		Rapid evolution in the surface brightness of tidal tails makes their use as an interaction signature limited; long tidal tails will only be detectable relatively early in the encounter, before the galaxies actually merge.
		Violent relaxation rapidly smooths isophotal irregularities after the galaxies merge, leaving the very low surface brightness tidal debris surrounding the remnant as the only sign of peculiarity after a few hundred Myr.
		This debris becomes indistinguishable from the main body of the remnant after 0.2 (z=1.0) to 1 (z=0.4) Gyr, leaving a morphologically normal elliptical galaxy behind.
	burro.astr.cwru.edu /preprints/morph.html (165 words)

	Galaxy Seminar & Journal Club
		It is a forum for informal talks given by members of these institutes, including students, and their guests.
		The seminar is intended to cover anything related to galaxies and their constituents, be it theoretical or observational.
		The Journal Club and Galaxy Seminar are held at the same timeslot: Fridays at 11:15 in the Seminar room (306) of the MPIA, on alternating weeks.
	www.mpia-hd.mpg.de /ORG/gal-morph.html (438 words)

	Poster Session - Astrostatistics Opening Workshop
		Such description will help scientists to study how galaxy morphology evolve over time, and the effect of environment toward the evolution.
		Clusters of galaxies play an important role in finding where the local structure fades away into a homogeneous and isotropic distribution.
		To extract connected components of the estimated level est, we propose to use a union of balls to approximate the estimated level set which is a modified version of Cuevas et al (2000).
	www.samsi.info /workshops/2005astro-posters200601.html (1006 words)

	The Galaxy Gallery Page 6: Comparative Morphology (Site not responding. Last check: )
		Here the Red passband is measuring the intensity and appearance of the galaxy in the light of 5 billion year old stars whereas the H-alpha image is measuring the distribution of stars with ages less than 10 Million years.
		NGC 3558 is a Southern Hemisphere spiral galaxy with a weakly defined disk.
		The fact that the disk is smooth in both the Visual and Infrared passbands indicates very little recent star formation and that the same stellar population dominates the light in both pass bands.
	zebu.uoregon.edu /morph.html (536 words)

	Matthew A. Bershady / Quantitative Galaxy Image Structure and Morphology (Site not responding. Last check: )
		Galaxy Form and Spectral-Type: A Physical Framework for Measuring Evolution, Bershady, M. 1999, to appear in "Toward a New Millennium in Galaxy Morphology," eds.
		Structural and Photometric Classification of Galaxies -- I. Calibration Based on a Nearby Galaxy Samplet, Bershady, M. Jangren, A., Conselice, C., to appear in June.
		The Symmetry, Color, and Morphology of Galaxies in the Hubble Deep Field, Conselice, C. and Bershady, M. 1999, in "After the Dark Ages: When Galaxies were Young (the Universe at 2 < z &l 5)," eds.
	www.astro.wisc.edu /~mab/research/ast9970780/imgstrc.html (220 words)

	surv (Site not responding. Last check: )
		The Morphology of Faint Galaxies in Medium Deep Survey Images using WFPC2(Griffiths, et al 94 ApJ 435 L19)
		Faintest Galaxy Morphology from HST WFPC2 Imaging of the Hawaii Survey Field(Cowie, Hu, & Songolia 95 AJ)
		Galaxy morphology to I=25 mag in the Hubble Deep Field(Abraham, etal 96 MNRAS (abstract))
	www.gb.nrao.edu /~koneil/defense/hst/surv.html (126 words)

	A HST Survey of the Mid-UV Morphology of Nearby Galaxies - Publications
		"A Systematic UBVRIJHK Survey of Nearby Galaxies to Classify Faint Galaxies from Deep HST Surveys", Burg, C.A.T.C., Windhorst, R.A., Odewahn, S.C., de Jong, R.S., and Frogel, J.A. 1997, in: "The Ultraviolet Universe at Low and High Redshift: Probing the Progress of Galaxy Evolution", eds.
		"Galaxy Counts versus Type for 19 < B < 29, and Galaxy Formation from Sub-galactic Clumps", Windhorst, R.A., Pascarelle, S., Odewahn, S., Cohen, S., Burg, C., Keel, W., and Driver, S. 1998, in: "The Hubble Deep Field: Proceedings of the STScI Symposium held May 6--9, 1997", eds.
		"The HST/WFPC2 B-Band Galaxy Counts vs. Type for 19 < B < 29 mag", Windhorst, R.A., Odewahn, S.C., Cohen, S.H., Burg, C.A., de Jong, R.S., Driver, S.P., Marzke, R.O., Tyson, J.A., and Dell'Antonio, I. 1997, in: "The Ultraviolet Universe at Low and High Redshift: Probing the Progress of Galaxy Evolution", eds.
	www.asu.edu /clas/hst/www/wfpc2/midUV/cy09publ.html (858 words)

	GalaxyDecompositionService - Main - Space Telescope Science Institute
		Quantitative galaxy morphology is widely used to address scientific questions such as:
		The galaxy photometric decomposition code fitgal essentially performs a chi^2 minimization between a user provided galaxy image and a multicomponent (bulge,disk,point etc.) model created using an analytical expression for the light distribution of each component.
		There already have been attempts to use a grid based approach for studying galaxy morphology (Deelman, 2003).
	chart.stsci.edu /twiki/bin/view/Main/GalaxyDecompositionService (651 words)

	Scientific Rationale (Site not responding. Last check: )
		Hubble deep field morphology compared to today's UV morphology of galaxies
		Morphology of Lyman break galaxies in the Hubble Deep Field
		X-ray morphology of galaxies: New results from AXAF; diffuse x-rays from the interstellar medium, compact x-ray sources and supernova remnants in spiral arms and the general disk.
	www.cam.wits.ac.za /origins99/galaxy.htm (213 words)

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