ライフサイエンスコーパス: universe

1 ion years, or 3.6 per cent of the age of the Universe).

2 e would have led to a dramatically different universe.

3 s of star formation, especially in the early Universe.

4 nized-the last major phase transition in the Universe.

5 pportunities for the expansion of the enzyme universe.

6 sequences in order to construct the protein universe.

7 capitulates the currently known protein fold universe.

8 ities of dust observed in the distant, early universe.

9 also among the most abundant elements in the universe.

10 ot baryons in a representative volume of the Universe.

11 ng all proteins, or constructing the protein universe.

12 emission from all stars and galaxies in the Universe.

13 ties of the interstellar medium in the early Universe.

14 ng well within the reionization epoch of the Universe.

15 5 per cent of the mass-energy budget of the Universe.

16 epoch within a representative portion of the Universe.

17 change their topology, occurs throughout the universe.

18 in lower-metallicity galaxies in the nearby Universe.

19 may have been very inefficient in the early Universe.

20 are among the densest stellar systems in the Universe.

21 and giant elliptical galaxies in the nearby Universe.

22 ter of the hydrosphere during the age of the universe.

23 ity to determine the baryonic content of the universe.

24 have formed from metal-poor gas in the early Universe.

25 t source of stable r-process elements in the Universe.

26 rguably the most complex system in the known universe.

27 lk of star formation over the history of the Universe.

28 ichment occurred early in the history of the Universe.

29 to the true scale-relative structure of the universe.

30 a touchstone in the question of life in the universe.

31 dominant mode of r-process production in the Universe.

32 e life span of a mosquito and the age of the universe.

33 nds, and are the most luminous events in the universe.

34 hat result in C(60) formation throughout the Universe.

35 X-ray and gamma-ray transients in the local Universe.

36 on the origin of enantiomeric excess in the universe.

37 hat abiogenesis is not extremely rare in the universe.

38 ovel method to realize the nature of protein universe.

39 so gives a direction for mapping the protein universe.

40 probing general relativity beyond our local universe.

41 how proteins are distributed in the protein universe.

42 n plasma governed the expansion of the early Universe.

43 f the most extreme physical processes in the universe.

44 verwhelming majority of neutron stars in the Universe.

45 d not contribute to the re-ionization of the Universe.

46 se objects have not been found in the nearby Universe.

47 ion, bridging gaps in our map of the protein universe.

48 heory is a good description of our expanding Universe.

49 haracterizing the mass-energy content of the universe.

50 uclei (AGNs) over most of the history of the universe.

51 are unlike anything found in the present-day Universe.

52 ons for seeking extraterrestrial life in the Universe.

53 ates several hundred times that in the local Universe.

54 s contributed carbonaceous dust in the early universe.

55 cess in the search for life elsewhere in the universe.

56 ong the least luminous galaxies in the known Universe.

57 ryons that are expected to be present in the universe.

58 tructure is key to understanding the protein universe.

59 n capture (r-process) nucleosynthesis in the universe.

60 hydrogen in the very early evolution of the Universe.

61 let radiation backgrounds that reionized the universe.

62 damental plasma wave modes that permeate the universe.

63 chanism leading to formation of H3(+) in the universe.

64 se of its apparent absence in the observable Universe.

65 us processes in the laboratory, life and the universe.

66 data sets provide new glimpses into the RNA universe.

67 objective, classical reality in our quantum Universe.

68 about fluctuation spectra in the very early universe.

69 t a quasi-primitive environment in the early universe.

70 n for the apparent disappearance of half the Universe.

71 n a short period early in the history of the Universe.

72 e most vigorous star-forming galaxies in the Universe.

73 y parameter is the total mass density of the universe.

74 nsible for various eruptive phenomena in the universe.

75 has radiative access to the coldness of the universe.

76 e dense environment of galaxies of the early universe.

77 rgence of life on Earth and elsewhere in the Universe.

78 and vaccinologists have existed in parallel universes.

79 Among the hospital universe, 149 EDs were identified as the nearest ED to t

80 In the early Universe, a boost in H(2) emission by this process may h

81 As one of the most abundant elements in the Universe, a major by-product of oil refinery processes,

82 The observed matter in the universe accounts for just 5% of the observed gravity.

83 s of matter and antimatter in the primordial Universe after the Big Bang, but today's Universe is obs

84 he sources responsible for ionization of the Universe after the cosmic 'Dark Ages', when the baryonic

85 Magnetic fields pervade the entire universe and affect the formation and evolution of astro

86 a fundamental understanding of matter in the Universe and appear as collective phase or amplitude exc

87 minous, heavily star-forming galaxies in the Universe and are characterized by prodigious emission in

88 among the most luminous objects in the local Universe and are thought to be powered by intense star f

89 roach to a representative map of the protein universe and discuss its implications.

90 t question for both the study of life in the universe and for the development of evolutionary molecul

91 n as small density fluctuations in the early Universe and grow by in situ star formation and hierarch

92 and its scale dependence, and the age of the universe and of the first stars)--fits remarkably well a

93 n the earliest moments in the history of the universe and on possible new physics at energies many or

94 ed by nature between disparate realms of the universe and the amazing consequences of the unifying ch

95 ymmetry between matter and antimatter in our universe and the gravitational behaviour of antimatter.

96 It is the thinnest known material in the universe and the strongest ever measured.

97 finitive evidence for inflation in the early universe and would constrain new physics from the grand

98 ly on observations of the local, present-day universe) and describe prospects for the future.

99 is, moving nonrelativistically in the early universe) and interacts feebly if at all with normal mat

100 i.e., moves nonrelativistically in the early universe), and interacts only weakly with matter other t

101 ficient mass scale for star formation in the Universe, and is lower than that predicted by semi-analy

102 the unexplored regions of the small molecule universe, and it facilitates the mining of chemical libr

103 uman brain and of the evolution of the early Universe, and it is performed every day at major operati

104 rs and more exotic physical processes in the universe, and provides a crucial cosmological benchmark

105 al the full history of star formation in the universe, and simulations appear poised to accurately pr

106 ergy: evolution of the expansion rate of the Universe, and slow down in the rate of growth of cosmic

107 w-energy supernovae were common in the early Universe, and that such supernovae yielded light-element

108 lowest heavy-element abundance in the early universe, and thus are potential fuel for the most metal

109 man model provides a nexus between these two universes, and recent studies have begun to use this mod

110 ter playing a smaller part than in the local Universe; and second, the large velocity dispersion in h

111 he accreting supermassive black holes in the Universe are obscured by large columns of gas and dust.

112 dest and most luminous galaxies in the early Universe are surprisingly compact, having stellar masses

113 ty below 10% of the solar value in the local universe are the best analogues to investigating the int

114 Some "universes" are better fine-tuned than others to sustain

115 the Lorentzian spacetime of our accelerating universe, are more attractive as their predictions are m

116 he formation of large-scale structure in the universe, as well as the evolution of local structures i

117 Einstein equations, such that the Friedmann universe associated with the pure radiation phase of the

118 e intergalactic medium occurred in the early Universe at redshift z approximately 6-11, following the

119 n and as a result they enable studies of the Universe at the earliest cosmic epochs.

120 dark-matter haloes that should exist in the Universe at this epoch.

121 ive its age to be nearly half the age of the Universe at this redshift and the absorption line spectr

122 vitationally magnified galaxy from the early Universe, at a redshift of z = 9.6 +/- 0.2 (that is, a c

123 s that formed most of the stars in the early Universe, at redshifts z > 7, have been found in large n

124 entative of the cosmic matter content of the universe (baryons and dark matter).

125 ursors of the most massive structures in the Universe began to form shortly after the Big Bang, in re

126 oules per cm(3)) is prevalent throughout the Universe, being present in all types of stars and toward

127 'cosmic web' of galaxies that we see in the Universe, but failed to create a mixed population of ell

128 enormous potential to help characterize this universe, but is it ready to go for real world applicati

129 e for rare r-process enrichment in the early Universe, but only under the assumption that no gas accr

130 cores of giant molecular clouds in the local Universe, but they are about a hundred times larger and

131 st stars fundamentally transformed the early universe by emitting the first light and by producing th

132 They fundamentally transformed the early Universe by endowing it with the first sources of light

133 axies are insufficient to fully reionize the Universe by redshift z approximately 6, but low-mass, st

134 We show the protein universe can be realized as a protein space in 60-dimens

135 Further, the cold darkness of the Universe can be used as a renewable thermodynamic resour

136 iew that galaxies formed hierarchically in a Universe composed of cold dark matter.

137 hich drives the accelerated expansion of the universe, consists of a light scalar field, it might be

138 elds ranging from materials science to early-universe cosmology, and to engineering of laser beams.

139 n lifetimes of atoms and molecules in these "universes" depend strongly on the individual physical pr

140 knotted configurations influencing the Early Universe development, whereas in liquid crystals transie

141 timetre line of atomic hydrogen in the early Universe directly probe the history of the reionization

142 ogous in many ways to galaxies in the infant Universe during the early stages of black-hole growth an

143 In the local universe, dust forms primarily in the ejecta from stars,

144 st that baryons in the early (high-redshift) Universe efficiently condensed at the centres of dark-ma

145 Carbon, the basic building block of our universe, enjoys a vast number of allotropic structures.

146 ate the acceleration of the expansion of the Universe even though fundamental details, such as the na

147 t century, the parameters describing how our universe evolved from the Big Bang are generally known t

148 understanding of how the hot, smooth, early universe evolved into the complex and beautiful universe

149 Better understanding of how the protein universe evolved to its present form can be achieved by

150 c standpoint behave as individual "Minkowski universes" exhibiting different "laws of physics", such

151 But evidence from the local Universe favours the idea that r-process production occu

152 three Lorentzian manifolds corresponding to universes filled only with dark energy (de Sitter spacet

153 ty similar to random close packing and early universe fluctuations, but with arbitrary controllable d

154 The Chemical Universe Generated Databases up to 11 atoms of CNOF (GDB

155 rvations of the large-scale structure in the universe, gravitational lensing, and the cosmic microwav

156 The rapid expansion of the viral sequence universe has forced a recalibration of the data model to

157 ntimately related to the question of why the Universe has so little antimatter.

158 Hydrogen, the simplest element in the universe, has a surprisingly complex phase diagram.

159 t the most massive structures in the distant universe have a tremendous supply ( approximately 10(11)

160 Massive galaxies in the early Universe have been shown to be forming stars at surprisi

161 lie at the core of our understanding of the Universe have not yet been directly observed.

162 the first 'seed' black holes in the earlier Universe, however, is observationally unconstrained and

163 chemistry of the most common elements of the Universe (hydrogen, oxygen, nitrogen, and carbon).

164 ightest and the most abundant element in the universe, hydrogen is fascinating to physicists.

165 evidence that life might be abundant in the universe if early-Earth-like conditions are common, the

166 nology Department became a place, and little universe in itself, where young scientists from all over

167 masses and sizes of important objects in the universe in terms of just a few fundamental constants.

168 of 0.68% for a flat lambda cold dark matter universe in the era of third-generation ground-based det

169 ngs strengthen evidence for a picture of the Universe in which a large fraction of the missing baryon

170 The decomposition of the known structural universe into a finite set of compact TERMs offers excit

171 cally decompose the known protein structural universe into its basic elements, which we dub tertiary

172 ion schemes exist that partition the protein universe into structural units called folds.

173 inflationary or quantum gravity epoch of the universe intrinsically influences the phase difference i

174 luminous quasars that are observed when the universe is 1 billion years old.

175 was responsible for the reionization of the universe is a long-standing quest in astronomy.

176 e structure of spacetime in our accelerating universe is a power-law graph with strong clustering, si

177 on the basis that the expansion rate of the universe is accelerating at present - as was inferred or

178 annot tell us what the nature of the protein universe is concretely.

179 The science universe is dimmer after one of our brightest stars, Sus

180 er-abundance of very massive galaxies in the Universe is frequently attributed to the effect of galac

181 he laboratory, and most of the energy in the universe is in the form of "dark energy," energy associa

182 Most of the mass in the universe is in the form of dark matter--a new type of no

183 ial Universe after the Big Bang, but today's Universe is observed to consist almost entirely of ordin

184 Jacques Monod is "everything existing in the universe is the fruit of chance and necessity." While I

185 The protein universe is the set of all proteins of all organisms.

186 y-the first few hundred million years of the Universe-is challenging because it requires surveys that

187 In the local universe, it is possible to infer their properties from

188 Originally proposed as a symmetry of our universe, it still awaits experimental verification.

189 correct that if life exists elsewhere in the universe, it would have forms and structures unlike anyt

190 urvey of our size, suggesting that the early Universe may harbour a larger number of intense sites of

191 box for epoxide polymerization, a "polyether universe" may be envisaged that in its structural divers

192 The growing universe of "channelopathic pain" presents some interest

193 binds, we used Bayesian modeling within the universe of accessible chromatin.

194 These are extremes of a spectrum in a universe of activation states.

195 which represent extremes of a continuum in a universe of activation states.

196 e rearranged receptor genes to recognize the universe of antigens, natural killer (NK) cells are inna

197 elatively small chemical space into a larger universe of biological activities, as membrane-containin

198 o attain precise predictions that reduce the universe of candidate GIs to test in the lab.

199 the 20th century with attempts to narrow the universe of chemicals that might affect the disease by d

200 group, this algorithm drastically trims the universe of combinations while simultaneously guaranteei

201 inetic discrimination of isomers expands the universe of combinations.

202 innovation as a search for designs across a universe of component building blocks.

203 is, the Foundational Model of Connectivity's universe of discourse is the structural architecture of

204 We then apply EBC to map the complete universe of drug-gene relationships based on their descr

205 quisite for immune system recognition of the universe of foreign antigens, is generated in the first

206 to yield native-like models for the diverse universe of functionally important RNAs whose structures

207 We have just begun to probe the universe of human L1(Ta) polymorphisms, and as TIP-chip

208 pertoire with the potential to recognize the universe of infectious agents depends on proper regulati

209 ear at z > 6 (corresponding to an age of the Universe of less than 1 billion years).

210 es for 771 organisms spanned over the entire universe of life from viruses to humans.

211 In order to survey a universe of major histocompatibility complex (MHC)-prese

212 In recent years, the universe of modification-dependent enzymes has expanded

213 flexible structures in the rapidly expanding universe of MOFs.

214 The vast, diverse universe of organic pollutants is a formidable challenge

215 This finding expands the universe of p53 binding sites and demonstrates that even

216 n (defined as the number of samples out of a universe of plant samples reported to have groundwater c

217 rom a proteomics mixture, given the sequence universe of possible proteins and a target peptide profi

218 ire to have pre-existing specificity for the universe of potential pathogens.

219 s with sufficient diversity to recognize the universe of potential pathogens.

220 As the universe of prion diseases continues to expand, mouse mo

221 field can be used to explore efficiently the universe of protein folds with good accuracy and very li

222 evolutionary processes is a rich and complex universe of protein sequences and structures, with chara

223 tial functionally relevant clustering of the universe of protein sequences.

224 Although the universe of protein structures is vast, these innumerabl

225 structure space has implications for how the universe of protein structures might have originated, an

226 The amylome is the universe of proteins that are capable of forming amyloid

227 ging studies are greatly expanding the known universe of RNA-binding proteins, methods for the discov

228 ling model which has evolved in the parallel universe of spelling research resonates with Frost's rea

229 verse evolved into the complex and beautiful universe of stars and galaxies in which we now live.

230 These results greatly expand the universe of target cancer antigens and identify new tool

231 Well-annotated gene sets representing the universe of the biological processes are critical for me

232 mals (the microbiota) and in cataloguing the universe of the genes they carry (the microbiome).

233 al repertoire, enabling responses to a broad universe of unpredictable antigens while maintaining an

234 The sample is drawn from the universe of WIC sites nationally, excluding only those w

235 Our study expands the "genome universe" of P. aeruginosa and validates a technology th

236 A unique window on the universe opened on September 14, 2015, with direct detec

237 ent scales like the Higgs field in the early universe or quantum fluids in condensed matter systems.

238 Simulations of structure formation in the Universe predict that galaxies are embedded in a 'cosmic

239 ulations of structure formation in the early universe predict the formation of some fraction of stars

240 xies that stopped forming stars in the early Universe presents an observational challenge because the

241 ergers predicted to be common throughout the Universe probably have a similarly important role in sha

242 n massive star-forming galaxies in the early Universe produced many more low-mass stars than the IMF

243 the most extreme star-forming engines in the Universe, producing stars over about 100 million years (

244 iated with significant mass buildup in early-Universe proto-clusters, and that many submillimetre-bri

245 n of the first massive objects in the infant Universe remains impossible to observe directly and yet

246 of the mass that makes up dark matter in the Universe remains one of the prime puzzles of cosmology a

247 in of super-massive black holes in the early universe remains poorly understood.

248 The largest galaxies in the universe reside in galaxy clusters.

249 The Universe's largest galaxies reside at the centres of gal

250 r dark matter, which constitutes 85% of the universe's mass and which has been a mystery for decades

251 e that baryons account for 5 per cent of the Universe's total energy content.

252 inhabiting the farthest flung corners of the universe should age.

253 The "small molecule universe" (SMU), the set of all synthetically feasible o

254 ermal dust emission from an archetypal early Universe star-forming galaxy, A1689-zD1.

255 ries, yet fails to explain properties of the universe such as the existence of dark matter, the amoun

256 d in the interior of large ice bodies in the universe, such as Saturn and Neptune, where nonmolecular

257 ghtness fluctuations of quasars in the early Universe suggest that some were powered by black holes w

258 hydrogen (H(i)) have been found in the local Universe, suggesting that such structures have either di

259 r and oil; the distribution of matter in the universe; surface reconstruction in ionic crystals; and

260 were 1,000 times more abundant in the early Universe than at present.

261 d studied within a newly emergent conceptual universe (the 'Stockholm Paradigm'), embracing the inher

262 In the local Universe, the census of all observed baryons falls short

263 densest form of matter known to exist in our Universe, the composition and properties of which are st

264 del with only six parameters (the age of the universe, the density of atoms, the density of matter, t

265 In the local (low-redshift) Universe, the mass of dark matter within a galactic disk

266 yon fraction may be larger than in the local Universe, the systematic uncertainties (owing to the cho

267 s like the Leo ring were common in the early Universe, they may have produced a large, yet undetected

268 s function for substructure beyond the local Universe to be 1.1(+0.6)(-0.4), with an average mass fra

269 feasible paths in the entire known metabolic universe using a tailored heuristic search strategy.

270 In another universe, vaccinologists have relied on human clinical t

271 the individual physical properties of each "universe" via the Purcell effect.

272 ft z approximately 4 (refs 1, 2, 3; when the Universe was 1.5 billion years old) necessitates the pre

273 common in the host galaxies of AGN when the Universe was 2-6 billion years old, but that the most vi

274 of ionizing radiation from galaxies when the Universe was about 500 million years old, so that the hy

275 first galaxies during reionization when the Universe was about 500 million years old.

276 a spectrum of a quasar at z = 7.04, when the Universe was just 772 million years old (5.6 per cent of

277 At redshift z = 2, when the Universe was just three billion years old, half of the m

278 alaxies observed at redshift z > 6, when the Universe was less than a billion years old, thus far ver

279 The existence of such black holes when the Universe was less than one billion years old presents su

280 tory from the present day to a time when the Universe was less than one-tenth of its present age.

281 truly intergalactic, it would imply that the Universe was neither ionized by starlight nor chemically

282 nce of this supermassive black hole when the Universe was only 690 million years old-just five per ce

283 axies, which correspond to a period when the Universe was only approximately 800 million years old.

284 quasars are evolved objects even though the Universe was only seven per cent of its current age at t

285 nt galaxy at a redshift of z = 2.1, when the Universe was three billion years old.

286 that the first stars to appear in the early universe were very massive and formed in isolation.

287 ger supra-exponential accretion in the early universe, when a BH seed is bound in a star cluster fed

288 widely interpreted as relics from the early Universe, when all gas possessed a primordial chemistry.

289 ertainties about star formation in the early Universe, when the metallicity was generally low.

290 that accompanies star formation in the local Universe, where the dust-to-gas mass ratio is around one

291 imate of the size of the prokaryotic genomic universe, which appears to consist of at least a billion

292 s governing natural diversity of the protein universe, which make it capable of recognizing previousl

293 r moved at different velocities in the early Universe, which strongly suppressed star formation in so

294 m a binary neutron-star merger in the nearby Universe with a relatively well confined sky position an

295 rganization of the kinase inhibitor scaffold universe with respect to different activity and structur

296 y faint, dusty, star-forming galaxies in the Universe with star formation rates of a few hundred sola

297 ics of complex networks and spacetime in the universe, with implications to network science and cosmo

298 ark matter makes up 85% of all matter in the universe yet its microscopic composition remains a myste

299 ts for as much as 84.5% of all matter in our Universe, yet it has so far evaded all attempts at direc

300 ed to such high-density regions of the early Universe; yet dormant black holes of this high mass have