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1 r-rotators among blue galaxies (9 out of 489 galaxies).
2 he habitability of Earth-like planets in our Galaxy.
3 al engine is located in the core of the host galaxy.
4 de evidence for substructures in the lensing galaxy.
5 lation gamma-rays in the bulge region of our Galaxy.
6 tes a deficiency of interstellar dust in the galaxy.
7 gaelectronvolt continuum excess in the inner Galaxy.
8 Reticulum II is one such galaxy.
9 er ultraviolet observations of the Spiderweb galaxy.
10 ts thought to originate beyond the Milky Way galaxy.
11 rc seconds from the center of the foreground galaxy.
12 that detected in any other ultrafaint dwarf galaxy.
13 times as massive as the stellar mass of the galaxy.
14 e located in low-density regions of the host galaxy.
15 ch as an impact from a cosmic cloud or other galaxy.
16 cation within the central region of its host galaxy.
17 mation by a streamer of gas falling into the galaxy.
18 econd, it is the fastest unbound star in our Galaxy.
19 r cent of the population of the stars in the Galaxy.
20 a fast-spinning, rotationally supported disk galaxy.
21 shine brighter than any x-ray source in our Galaxy.
22 -velocity stars, which could even escape the galaxy.
23 ay between this feedback and the growth of a galaxy.
24 eing located within a prominent star-forming galaxy.
25 ure of space around matter in an intervening galaxy.
26 atics, to evolve into present-day elliptical galaxies.
27 be a pair of extremely massive star-forming galaxies.
28 ompact dwarf companions of parent elliptical galaxies.
29 gas acquisition in driving evolution of blue galaxies.
30 e Great Wall--the largest local structure of galaxies.
31 ave been detected only in three low-redshift galaxies.
32 ortance of external gas acquisition in these galaxies.
33 the star-formation rate observed in distant galaxies.
34 holes and the coevolution of black holes and galaxies.
35 ty to detect heavily obscured regions of the galaxies.
36 delling the spectral energy distributions of galaxies.
37 ) from standing shocks in the jets of active galaxies.
38 feedback and grow the bulges of present-day galaxies.
39 aryonic regions of the disks of star-forming galaxies.
40 e close relationship between black holes and galaxies.
41 s consideration of the rich phenomenology of galaxies.
42 opportunity to resolve the inner regions of galaxies.
43 s that grow into supermassive black holes in galaxies.
44 he star-forming interstellar medium of these galaxies.
45 s or the presence of peculiar field stars or galaxies.
46 way from the center of the Bullet cluster of galaxies.
47 which probably affect the properties of the galaxies.
48 ghtness similar to the integrated light from galaxies.
52 carbon monoxide, we show that the Spiderweb galaxy-a massive galaxy in a distant protocluster-is for
53 a supermassive black hole at the centre of a galaxy accretes matter, it gives rise to a highly energe
55 ion, the host galaxies of quasars, but these galaxies also host accreting supermassive (more than 10(
56 sible and reproducible, we implemented it in Galaxy - an open, web-based platform for data-intensive
58 l properties similar to massive star-forming galaxies and are embedded in enriched neutral hydrogen g
59 molecular gas lies between the protocluster galaxies and has low velocity dispersion, indicating tha
60 ion at radio frequencies in both clusters of galaxies and radio galaxies through non-thermal radiatio
62 nces of non-neutron-capture elements in this galaxy (and others like it) are similar to those in othe
63 the outer disks of six massive star-forming galaxies, and find that the rotation velocities are not
64 extragalactic, off-nucleus, point sources in galaxies, and have X-ray luminosities in excess of 3 x 1
65 ty dispersion of the spheroidal component of galaxies, and would contribute to the population of high
66 images of the z = 1.49 spiral supernova host galaxy, and a future appearance of the supernova elsewhe
67 s is set by the gas falling onto it from the galaxy, and the gas infall rate is regulated by the brig
68 uration radio signals originating in distant galaxies appear to have been discovered in the so-called
69 he presence of massive, quiescent early-type galaxies appearing as early as redshift z approximately
70 imal harvest date and late harvest date) on 'Galaxy' apple metabolism and quality after harvest and 9
72 ermassive black holes (SMBHs) and their host galaxies are generally thought to coevolve, so that the
75 However, these early, massive, quiescent galaxies are not predicted by the latest generation of t
76 dies of such phenomena in blue, star-forming galaxies are rare, leaving uncertain the role of externa
78 approximately 6, but low-mass, star-forming galaxies are thought to be responsible for the bulk of t
81 riggered by outflows or jets into their host galaxy, as a consequence of gas compression, evidence fo
82 wn SLSNe-I that reside in star-forming dwarf galaxies, ASASSN-15lh appears to be hosted by a luminous
83 y simpler, and more ancient ultrafaint dwarf galaxies assembled shortly after the first stars formed,
85 n difficult to identify and characterize the galaxies associated with these absorbers due to the intr
86 um line and dust-continuum emission from two galaxies associated with two such absorbers at a redshif
88 idence for populations of massive, quiescent galaxies at even higher redshifts and earlier times, usi
91 o find the ultraviolet luminosity density of galaxies at redshifts greater than 8 to be log rho(UV) =
93 gas shells is indirect and limited to radio galaxies at the centres of clusters, which are too rare
96 e the interstellar medium directly in normal galaxies at these redshifts have failed for a number of
97 at a wavelength of 158 micrometres) in four galaxies at z > 6 that are companions of quasars, with v
99 unt for the population of massive elliptical galaxies at z approximately 4 in terms of the density of
103 asurement of [Mg/Fe] for a massive quiescent galaxy at a redshift of z = 2.1, when the Universe was t
104 ine at a wavelength of 88 micrometers from a galaxy at an epoch about 700 million years after the Big
105 t the spectroscopic confirmation of one such galaxy at redshift z = 3.717, with a stellar mass of 1.7
107 this need, we have developed an extensible, Galaxy-based resource aimed at providing more researcher
109 ommand line tool, as a Galaxy Toolshed, on a Galaxy-based web server, and on a virtual cluster on the
110 nucleus of the Abell 2597 Brightest Cluster Galaxy (BCG), a nearby (redshift z = 0.0821) giant ellip
111 d today in the central regions ('bulges') of galaxies, because they formed in the largest over-densit
113 of massive (10(11) solar masses) elliptical galaxies by redshift z approximately 4 (refs 1, 2, 3; wh
115 lion years old, so that the hydrogen between galaxies changed from neutral to ionized-the last major
116 or low-energy cutoffs, for radio emission in galaxy clusters and radio galaxies, have not yet been de
118 (up to microgauss levels reported in nearby galaxy clusters, near equipartition with kinetic energy
119 NGC 4889 at the centres of the Leo and Coma galaxy clusters, which together form the central region
124 orbers due to the intrinsic faintness of the galaxies compared with the quasars at optical wavelength
126 rise to the observed synchrotron emission in galaxy cores and to the formation of relativistic jets,
131 consume data from diverse sources, including Galaxy, Distributed Annotation and IGB-specific Quickloa
133 tal abundances of the interstellar medium in galaxies during cosmic reionization are important for un
136 r density in the cores of massive elliptical galaxies extends over the same radius as the gravitation
137 r plots dynamically, export data directly to Galaxy for analysis, plus generate URL bookmarks of spec
141 commodated within the standard model only if galaxy formation becomes stochastic in halos below appro
142 Here we report a cosmological hydrodynamic galaxy formation simulation that is able to form a submi
143 ellar and cold-gas mass at the peak epoch of galaxy formation ten billion years ago, inferred from an
144 been explained by an improved generation of galaxy-formation models, in which they form rapidly at z
145 this galaxy is the most Mg-enhanced massive galaxy found so far, having twice the Mg enhancement of
147 ols2 suite can be easily deployed within any Galaxy framework via the toolshed repository, and we als
149 than helium in stellar atmospheres) in local galaxies, from 26,000 spectra, that clearly reveals that
150 hat six out of a sample of seven 'jellyfish' galaxies-galaxies with long 'tentacles' of material that
151 mption that no gas accretes into those dwarf galaxies; gas accretion favours continual r-process enri
152 new stars if they had orbited in their host galaxies' gaseous disks throughout the period between th
154 rough its gravitational effects on stars and galaxies, gravitational lensing of light around these, a
155 lated elliptical galaxy near the centre of a galaxy group at a distance of 64 megaparsecs from Earth.
158 europium abundance in some dwarf spheroidal galaxies has been suggested as evidence for rare r-proce
159 mes that of the Sun; the number of quiescent galaxies has increased by a factor of about 25 over the
160 emission at far-infrared wavelengths if the galaxies have become sufficiently enriched in dust and m
161 identify their counterparts (source or host galaxy) have relied on the contemporaneous variability o
163 These results are consistent with early galaxies having significantly less dust than typical gal
165 n of our previously published ImmunoGlobulin Galaxy (IGGalaxy) virtual machine that was developed to
167 Our results support the notion that giant galaxies in clusters formed from extended regions of rec
173 we show that the Spiderweb galaxy-a massive galaxy in a distant protocluster-is forming from a large
174 mation history of all stars currently in the galaxy, including younger and metal-poor stars that were
175 n of alternative transcripts; and a EuPathDB Galaxy instance for private analyses of a user's data.
178 that the acquisition of external gas in blue galaxies is possible; the interaction with pre-existing
187 n-thermal population of electrons in a radio galaxy jet/lobe, located at a significant distance away
188 uced by cluster mergers or injected by radio galaxy jets, which impacts the formation of large-scale
193 ar activity among heavily stripped jellyfish galaxies may be due to ram pressure causing gas to flow
195 Such systems are an expected consequence of galaxy mergers and can provide important constraints on
198 ASSN-15lh appears to be hosted by a luminous galaxy (MK approximately -25.5) with little star formati
199 These observations demonstrate that the galaxy must have formed the majority of its stars quickl
200 y NGC 1600--a relatively isolated elliptical galaxy near the centre of a galaxy group at a distance o
201 n to many publicly available tools including Galaxy, NEAT provides three main advantages: (1) Through
202 'active' black holes have been found in the galaxies NGC 3842 and NGC 4889 at the centres of the Leo
203 of the stellar velocity distribution in the galaxy NGC 1600--a relatively isolated elliptical galaxy
206 the merger occurred in the outskirts of the galaxy NGC 4993, at a distance of 40 megaparsecs from Ea
207 idly fading electromagnetic transient in the galaxy NGC 4993, which is spatially coincident with GW17
209 ing galaxies, which indicates that quiescent galaxies of less than 10(11) solar masses are on average
210 s at z > 6 are, with one exception, the host galaxies of quasars, but these galaxies also host accret
213 e galaxies contain a central black hole, and galaxies often merge, black-hole binaries are expected t
215 hysical processes that can remove gas from a galaxy, one of which is ram-pressure stripping by the ho
216 ar formation either by removing gas from the galaxy, or by heating it to temperatures that are too hi
218 cumentation for AmrPlusPlus, a user-friendly Galaxy pipeline for the analysis of high throughput sequ
223 large fraction of the massive high-redshift galaxy population was strongly baryon-dominated, with da
228 the 10-kiloparsec-scale environments of the galaxies, processing these environments into multiphase,
231 both supermassive black holes and their host galaxies, quenching star formation and explaining the cl
233 a rain of cold clouds that fall towards the galaxy's centre, sustaining star formation amid a kilopa
234 we calculate that the energy input from the galaxy's low-level active supermassive black hole is cap
236 escription languages, thus demonstrating how Galaxy's reproducible research features can be leveraged
237 field spectroscopy of a large representative galaxy sample, we find an appreciable fraction of counte
239 clusters will also be low mass, unless some galaxy-scale compression occurs, such as an impact from
241 having significantly less dust than typical galaxies seen at z < 3 and being comparable in dust cont
242 grew into the most massive local elliptical galaxies seen today, through mergers with minor companio
244 Ultraluminous x-ray sources (ULXs) in nearby galaxies shine brighter than any x-ray source in our Gal
246 matter cosmology, the baryonic components of galaxies-stars and gas-are thought to be mixed with and
249 oughly one-tenth the mass of the entire host galaxy, suggesting that it has grown much more efficient
250 molecular outflows in ultraluminous infrared galaxies support this quasar-feedback idea, because they
253 t are sensitive enough to detect the distant galaxies that act as signposts for these structures and
254 nificant surface density of fainter primeval galaxies that are below the point-source detection level
260 ulation that is able to form a submillimetre galaxy that simultaneously satisfies the broad range of
261 e of the ongoing formation of stars in these galaxies, the presence of molecular gas (which is known
262 ncies in both clusters of galaxies and radio galaxies through non-thermal radiation emission called s
263 previous indirect indications that the first galaxies to cease star formation must have gone through
264 ted into the open-source, web-based platform Galaxy to connect users with computational resources and
265 contribute to the morphological evolution of galaxies, to the evolution in size and velocity dispersi
268 lable for download in GitHub and as a set of Galaxy tools and workflows configured to execute on para
269 rational modes: as a command line tool, as a Galaxy Toolshed, on a Galaxy-based web server, and on a
271 peak (at about redshift z approximately 2), galaxies vigorously fed by cosmic reservoirs are dominat
273 of 600 to 3,000 solar masses per year, this galaxy was among the most vigorous star-forming galaxies
276 the event, which we use to identify the host galaxy; we measure the galaxy's redshift to be z = 0.492
278 billion years old, half of the most massive galaxies were extremely compact and had already exhauste
279 majority of the stars in massive elliptical galaxies were formed in a short period early in the hist
280 itated the escape of ionizing radiation from galaxies when the Universe was about 500 million years o
281 e than 10 kiloparsecs) outside the starburst galaxies (which have radii of less than 1 kiloparsec).
283 ifference between quiescent and star-forming galaxies, which indicates that quiescent galaxies of les
284 nd kinematics of a lensed z = 2.1478 compact galaxy, which-surprisingly-turns out to be a fast-spinni
286 le of four billion years, at least for local galaxies with a stellar mass less than 10(11) solar mass
287 he form of galactic-scale outflows of gas in galaxies with high rates of star formation, especially i
290 ng star formation dominate the population of galaxies with masses above 2 x 10(10) times that of the
292 lion years old) necessitates the presence of galaxies with star-formation rates exceeding 100 solar m
296 ), the primary tracer of molecular gas, in a galaxy with 7% solar metallicity, with additional detect
297 CO clouds in the local group dwarf irregular galaxy Wolf-Lundmark-Melotte (WLM), which has a metallic
299 stem that combines these two programs with a Galaxy workflow system accelerated with MPI and Python t
300 ombining the spectra of 24 massive quiescent galaxies, yielding an average [Mg/Fe] = 0.31 +/- 0.12.
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