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1 the molecular universe and of carbon in our galaxy.
2 uracy to localize them to an individual host galaxy.
3 ltraviolet photons must escape from the host galaxy.
4 that passes through the halo of a foreground galaxy.
5 e in star formation and the evolution of our galaxy.
6 he habitability of Earth-like planets in our Galaxy.
7 al engine is located in the core of the host galaxy.
8 rc seconds from the center of the foreground galaxy.
9 r cent of the population of the stars in the Galaxy.
10 a fast-spinning, rotationally supported disk galaxy.
11 shine brighter than any x-ray source in our Galaxy.
12 -velocity stars, which could even escape the galaxy.
13 ay between this feedback and the growth of a galaxy.
14 eing located within a prominent star-forming galaxy.
15 ure of space around matter in an intervening galaxy.
16 de evidence for substructures in the lensing galaxy.
17 niverse and, in particular, of sulfur in our Galaxy.
18 lation gamma-rays in the bulge region of our Galaxy.
19 ecular gas outflowing from the centre of our Galaxy.
20 e strongly affected the inner regions of our Galaxy.
21 star formation in the central regions of the Galaxy.
22 develops interactive training materials for Galaxy.
23 to represent the bulk population of massive galaxies.
24 adiation emitted by young stars in the first galaxies.
25 opportunity to resolve the inner regions of galaxies.
26 way from the center of the Bullet cluster of galaxies.
27 be a pair of extremely massive star-forming galaxies.
28 the star-formation rate observed in distant galaxies.
29 aryonic regions of the disks of star-forming galaxies.
30 s that grow into supermassive black holes in galaxies.
31 he star-forming interstellar medium of these galaxies.
32 s or the presence of peculiar field stars or galaxies.
33 which probably affect the properties of the galaxies.
34 ghtness similar to the integrated light from galaxies.
35 atics, to evolve into present-day elliptical galaxies.
36 ompact dwarf companions of parent elliptical galaxies.
37 gas acquisition in driving evolution of blue galaxies.
38 e Great Wall--the largest local structure of galaxies.
39 or haloes less massive than those of typical galaxies.
40 he extrapolation of structures seen in other galaxies.
43 be coincident with a compact over-density of galaxies(2) with photometric redshifts of 1.9 +/- 0.2.
46 These processes determine the properties of galaxies(3,4) but are poorly understood on the scale of
47 nd SMC are on their first passage around the Galaxy(5), that the Magellanic Stream is made up of gas
49 ve been localized and associated with a host galaxy(9-12), and just one of these four is known to emi
50 ting molecular gas through star formation in galaxies (about 2 billion years)(9,10) exceeds the cloud
51 a supermassive black hole at the centre of a galaxy accretes matter, it gives rise to a highly energe
52 ion, the host galaxies of quasars, but these galaxies also host accreting supermassive (more than 10(
53 th evolved stellar populations in the member galaxies and a hot, metal-rich gas composing the intracl
55 l properties similar to massive star-forming galaxies and are embedded in enriched neutral hydrogen g
61 ic outbursts have been detected from dormant galaxies and often attributed to the tidal disruption of
62 ion at radio frequencies in both clusters of galaxies and radio galaxies through non-thermal radiatio
63 e questions of the true abundance of massive galaxies and the star-formation-rate density in the earl
65 the outer disks of six massive star-forming galaxies, and find that the rotation velocities are not
67 ty dispersion of the spheroidal component of galaxies, and would contribute to the population of high
68 informatics workshops that introduce and use Galaxy, and develops interactive training materials for
69 alized to a low-metallicity, irregular dwarf galaxy, and the apparently non-repeating sources were lo
70 s is set by the gas falling onto it from the galaxy, and the gas infall rate is regulated by the brig
71 uration radio signals originating in distant galaxies appear to have been discovered in the so-called
72 he presence of massive, quiescent early-type galaxies appearing as early as redshift z approximately
73 imal harvest date and late harvest date) on 'Galaxy' apple metabolism and quality after harvest and 9
77 However, these early, massive, quiescent galaxies are not predicted by the latest generation of t
78 dies of such phenomena in blue, star-forming galaxies are rare, leaving uncertain the role of externa
80 approximately 6, but low-mass, star-forming galaxies are thought to be responsible for the bulk of t
83 bright objects at the centres (or nuclei) of galaxies, are thought to be produced through the accreti
85 riggered by outflows or jets into their host galaxy, as a consequence of gas compression, evidence fo
87 evelopments-including the discovery of dwarf galaxies associated with the Magellanic group(14-16), de
88 n difficult to identify and characterize the galaxies associated with these absorbers due to the intr
89 um line and dust-continuum emission from two galaxies associated with two such absorbers at a redshif
90 rvations of XLSSC 122 and identify 37 member galaxies at a mean redshift of 1.98, corresponding to a
91 ating that star formation commenced in these galaxies at a mean redshift of 12, when the Universe was
93 idence for populations of massive, quiescent galaxies at even higher redshifts and earlier times, usi
97 etres) detections of 39 massive star-forming galaxies at z > 3, which are unseen in the spectral regi
99 at a wavelength of 158 micrometres) in four galaxies at z > 6 that are companions of quasars, with v
100 unt for the population of massive elliptical galaxies at z approximately 4 in terms of the density of
102 o the largest star-forming region of a dwarf galaxy at a cosmological redshift of 0.19 (refs. (7-9)).
107 e near-ultraviolet continuum emission from a galaxy at a redshift of 4.2603, identified by detecting
108 asurement of [Mg/Fe] for a massive quiescent galaxy at a redshift of z = 2.1, when the Universe was t
109 ine at a wavelength of 88 micrometers from a galaxy at an epoch about 700 million years after the Big
113 t the spectroscopic confirmation of one such galaxy at redshift z = 3.717, with a stellar mass of 1.7
114 the framework, runs public servers that make Galaxy available via a web browser, performs and publish
115 this need, we have developed an extensible, Galaxy-based resource aimed at providing more researcher
119 of massive (10(11) solar masses) elliptical galaxies by redshift z approximately 4 (refs 1, 2, 3; wh
121 host galaxy with a moderate offset from the galaxy centre, as short gamma-ray bursts often do(15,16)
123 onfirm that XLSSC 122 is a remarkably mature galaxy cluster with both evolved stellar populations in
125 dge of radio emission connecting the merging galaxy clusters Abell 0399 and Abell 0401 with the Low-F
126 or low-energy cutoffs, for radio emission in galaxy clusters and radio galaxies, have not yet been de
132 matter in dense cosmic environments, such as galaxy clusters, is studied theoretically using cosmolog
133 NGC 4889 at the centres of the Leo and Coma galaxy clusters, which together form the central region
140 , an increasing number of regional and local Galaxy communities, and substantial growth in the Galaxy
141 orbers due to the intrinsic faintness of the galaxies compared with the quasars at optical wavelength
143 ation shows how ionizing photons escape this galaxy, contributing to the reionization of the Universe
144 cent numerical simulations suggest that such galaxies could form as early as a billion years after th
147 nety per cent of baryons are located outside galaxies, either in the circumgalactic or intergalactic
148 black-hole activity is occurring within the galaxies embedded in these structures, which are the lik
150 ons along the lines of sight and in the host-galaxy environments(11), and we derive a cosmic baryon d
152 r density in the cores of massive elliptical galaxies extends over the same radius as the gravitation
158 ellar and cold-gas mass at the peak epoch of galaxy formation ten billion years ago, inferred from an
159 form at late times in traditional models of galaxy formation(1,2), but recent numerical simulations
160 radiation hydrodynamics simulation of early galaxy formation(11,12) that produces metal-free haloes
163 been explained by an improved generation of galaxy-formation models, in which they form rapidly at z
164 this galaxy is the most Mg-enhanced massive galaxy found so far, having twice the Mg enhancement of
167 hat six out of a sample of seven 'jellyfish' galaxies-galaxies with long 'tentacles' of material that
168 mption that no gas accretes into those dwarf galaxies; gas accretion favours continual r-process enri
174 europium abundance in some dwarf spheroidal galaxies has been suggested as evidence for rare r-proce
175 mes that of the Sun; the number of quiescent galaxies has increased by a factor of about 25 over the
176 d energy from the central few parsecs of our Galaxy have shaped the observed structure of the Milky W
177 identify their counterparts (source or host galaxy) have relied on the contemporaneous variability o
178 n the Milky Way, and a wide variety of other galaxies, have found evidence for a 'metallicity floor',
180 onding to redshift z > 3) is mainly based on galaxies identified in rest-frame ultraviolet light(1).
181 n of our previously published ImmunoGlobulin Galaxy (IGGalaxy) virtual machine that was developed to
182 ally, it has been difficult to identify disk galaxies in emission at high redshift(5,6) in order to d
185 Such a high abundance of massive and dusty galaxies in the early Universe challenges our understand
189 n of alternative transcripts; and a EuPathDB Galaxy instance for private analyses of a user's data.
190 aging NCBI Blast+ commands, or via a managed Galaxy instance that can optionally run on a different h
201 n larger scales, approaching the size of the Galaxy itself, gamma-ray observations have revealed the
203 n-thermal population of electrons in a radio galaxy jet/lobe, located at a significant distance away
204 uced by cluster mergers or injected by radio galaxy jets, which impacts the formation of large-scale
206 owser, performs and publishes analyses using Galaxy, leads bioinformatics workshops that introduce an
208 We report a massive GC in the Andromeda Galaxy (M31), RBC EXT8, that is extremely depleted in he
209 ar activity among heavily stripped jellyfish galaxies may be due to ram pressure causing gas to flow
212 curring nova, M31N 2008-12a in the Andromeda galaxy (Messier 31 or NGC 224), which erupts annually(11
213 These observations demonstrate that the galaxy must have formed the majority of its stars quickl
214 'active' black holes have been found in the galaxies NGC 3842 and NGC 4889 at the centres of the Leo
217 the merger occurred in the outskirts of the galaxy NGC 4993, at a distance of 40 megaparsecs from Ea
218 idly fading electromagnetic transient in the galaxy NGC 4993, which is spatially coincident with GW17
220 s at z > 6 are, with one exception, the host galaxies of quasars, but these galaxies also host accret
223 hysical processes that can remove gas from a galaxy, one of which is ram-pressure stripping by the ho
224 cumentation for AmrPlusPlus, a user-friendly Galaxy pipeline for the analysis of high throughput sequ
226 ataset of bioinformatics analyses run on the Galaxy platform to demonstrate the feasibility of an onl
231 We propose a new visualization method, the galaxy plot, which can simultaneously present the effect
232 large fraction of the massive high-redshift galaxy population was strongly baryon-dominated, with da
234 the 10-kiloparsec-scale environments of the galaxies, processing these environments into multiphase,
236 Over the last two years, all aspects of the Galaxy project have grown: code contributions, tools int
239 the gravitationally lensed post-reionization galaxy PSZ1-ARC G311.6602-18.4624 (nicknamed the "Sunbur
241 on rates of 200 solar masses per year, these galaxies represent the bulk population of massive galaxi
242 of stars rich in such elements in the dwarf galaxy Reticulum II(14), as well as the Galactic chemica
243 a rain of cold clouds that fall towards the galaxy's centre, sustaining star formation amid a kilopa
245 we calculate that the energy input from the galaxy's low-level active supermassive black hole is cap
250 suming the black hole mass indicated by host galaxy scaling relations, these observations imply that
252 of activity nor star formation in the inner Galaxy seems to be a viable source for this material.
253 grew into the most massive local elliptical galaxies seen today, through mergers with minor companio
254 Ultraluminous x-ray sources (ULXs) in nearby galaxies shine brighter than any x-ray source in our Gal
255 lly associated with the oldest components of galaxies, so measurements of their composition can const
257 matter cosmology, the baryonic components of galaxies-stars and gas-are thought to be mixed with and
260 allicity, massive elliptical or star-forming galaxies, suggesting that perhaps the repeating and appa
261 t are sensitive enough to detect the distant galaxies that act as signposts for these structures and
264 ies represent the bulk population of massive galaxies that has been missed from previous surveys.
265 o bursts with four new localizations in host galaxies that have measured redshifts of 0.291, 0.118, 0
267 e of the ongoing formation of stars in these galaxies, the presence of molecular gas (which is known
269 ncies in both clusters of galaxies and radio galaxies through non-thermal radiation emission called s
270 previous indirect indications that the first galaxies to cease star formation must have gone through
271 contribute to the morphological evolution of galaxies, to the evolution in size and velocity dispersi
280 the event, which we use to identify the host galaxy; we measure the galaxy's redshift to be z = 0.492
282 billion years old, half of the most massive galaxies were extremely compact and had already exhauste
283 a massive, rotationally supported, cold disk galaxy when the Universe was only 1.5 billion years old
284 e than 10 kiloparsecs) outside the starburst galaxies (which have radii of less than 1 kiloparsec).
286 is known to under-represent the most massive galaxies, which have rich dust content and/or old stella
287 nd kinematics of a lensed z = 2.1478 compact galaxy, which-surprisingly-turns out to be a fast-spinni
288 (redshift 0.0337 +/- 0.0002) massive spiral galaxy, whose properties and proximity distinguish it fr
290 ng star formation dominate the population of galaxies with masses above 2 x 10(10) times that of the
291 chs(2-4), most of them are extreme starburst galaxies with star-formation rates exceeding 1,000 solar
292 lion years old) necessitates the presence of galaxies with star-formation rates exceeding 100 solar m
294 es in the outskirts of its star-forming host galaxy with a moderate offset from the galaxy centre, as
296 c Cloud has traditionally served as the best galaxy with which to calibrate Cepheid period-luminosity
298 s extending more than one megaparsec between galaxies within the SSA22 protocluster at a redshift of
299 erver in two use cases: (i) integration with Galaxy workflows and (ii) using Epiviz to create a custo
300 tion of emission from carbon monoxide in the galaxy yields a molecular mass that is consistent with t