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 tructure is key to understanding the protein universe.

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

4 hydrogen in the very early evolution of the Universe.

5 let radiation backgrounds that reionized the universe.

6 damental plasma wave modes that permeate the universe.

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

8 se of its apparent absence in the observable Universe.

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

10 data sets provide new glimpses into the RNA universe.

11 eutron stars, and the expansion of the early Universe.

12 objective, classical reality in our quantum Universe.

13 about fluctuation spectra in the very early universe.

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

15 n for the apparent disappearance of half the Universe.

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

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

18 ber of neutrino species permeating the early Universe.

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

20 nsible for various eruptive phenomena in the universe.

21 has radiative access to the coldness of the universe.

22 e dense environment of galaxies of the early universe.

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

24 e would have led to a dramatically different universe.

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

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

27 pportunities for the expansion of the enzyme universe.

28 sequences in order to construct the protein universe.

29 capitulates the currently known protein fold universe.

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

31 through which heat can be dissipated to the universe.

32 also among the most abundant elements in the universe.

33 ot baryons in a representative volume of the Universe.

34 ng all proteins, or constructing the protein universe.

35 emical elements in galaxies during the early Universe.

36 emission from all stars and galaxies in the Universe.

37 day globular cluster population in the local Universe.

38 ties of the interstellar medium in the early Universe.

39 5 per cent of the mass-energy budget of the Universe.

40 epoch within a representative portion of the Universe.

41 change their topology, occurs throughout the universe.

42 may have been very inefficient in the early Universe.

43 are among the densest stellar systems in the Universe.

44 and giant elliptical galaxies in the nearby Universe.

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

46 ity to determine the baryonic content of the universe.

47 ception about the chemistry of carbon in our universe.

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

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

50 rguably the most complex system in the known universe.

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

52 ichment occurred early in the history of the Universe.

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

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

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

56 kely to be widely distributed throughout the universe.

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

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

59 on the origin of enantiomeric excess in the universe.

60 tition, cascade and conversion in the plasma universe.

61 hat abiogenesis is not extremely rare in the universe.

62 ovel method to realize the nature of protein universe.

63 so gives a direction for mapping the protein universe.

64 probing general relativity beyond our local universe.

65 abundances to probe the physics of the early Universe.

66 erved matter and antimatter asymmetry of the Universe.

67 dark matter and the baryon asymmetry in the Universe.

68 axy, contributing to the reionization of the Universe.

69 the star-formation-rate density in the early Universe.

70 e more common occurrence on Earth and in the universe.

71 w about the transformations of carbon in our universe.

72 ements to explain observed abundances in the Universe.

73 sive gravitationally bound structures in the Universe.

74 (CDM) constitutes most of the matter in the Universe.

75 ur most profound insights about the physical universe.

76 ormation of massive black holes in the early Universe.

77 80 per cent of the r-process content of the Universe.

78 ng well within the reionization epoch of the Universe.

79 in lower-metallicity galaxies in the nearby Universe.

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

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

82 and vaccinologists have existed in parallel universes.

83 est bound stellar structures observed in the Universe(1).

84 he most energetic explosive phenomena in the Universe(1).

85 nt for most of the r-process elements in the Universe(4).

86 or understanding the build-up of mass in the Universe(7).

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

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

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

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

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

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

93 he most massive virialized structures in the Universe and are formed through the gravitational accret

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

95 to the ever increasing entropic state of the universe and is fundamental in many branches of science

96 of the origin and evolution of the molecular universe and of carbon in our galaxy.

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

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

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

100 of the origin and evolution of the molecular universe and, in particular, of sulfur in our Galaxy.

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

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

103 ctions have allowed expansion of the protein universe, and how we can target them for therapeutic pur

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

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

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

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

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

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 g of how the most energetic particles in the universe are generated.

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

113 and their formation environment in the early Universe are still under debate, and their supposed rari

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

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

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

117 it is the only way to understand the complex universe around us and help society along the way".

118 hnologies that harvest the coldness from the universe as a new renewable energy source.

119 eus and to measure the expansion rate of the Universe as quantified by the Hubble constant.

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

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

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

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

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

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

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

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

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

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

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

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

132 erials shed heat from the ground to the cold universe by taking advantage of the terrestrial thermal

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

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

135 e of massive and dusty galaxies in the early Universe challenges our understanding of massive-galaxy

136 pattern of elements, the composition of the Universe changes over time as stars populate the periodi

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

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

139 The largest clusters of galaxies in the Universe contain vast amounts of dark matter, plus baryo

140 Cosmological simulations predict that the Universe contains a network of intergalactic gas filamen

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

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

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

144 he simplest and most abundant element in the Universe, develops a remarkably complex behaviour upon c

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

146 stem(1,3,14) and for the signatures of early Universe element synthesis in the Ga-Cd range found in t

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

148 prior belief on the frequency of life in the universe, even starting from a neutral or pessimistic st

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

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

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

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

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

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

155 he quark-gluon plasma until expansion of the universe freezes out the mass distribution to ~ 10(-24)

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

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

158 stry(1,2), when the temperature of the young Universe had fallen below some 4,000 kelvin, the ions of

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

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

161 r five per cent of the energy density of the Universe-has yet to be understood, given that the standa

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

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

164 Censuses of the nearby Universe have used absorption line spectroscopy(3,4) to

165 reflect an alternative ultimate rule of our universe, i.e., the principle of least action on a Finsl

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 would synchronize. It is now known that the universe is full of complex self-organizing systems, fro

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

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

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

185 The local expansion rate of the Universe is parametrized by the Hubble constant, [Formul

186 thway to find an ultimate rule governing our universe is to hunt for a connection among the fundament

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

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

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

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

191 O, and N are among the most abundant in the universe, many of these are organic in nature, including

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

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

194 mers that could plausibly govern life in the universe might inhabit a broad swath of chemical space.

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

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

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

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

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

200 inetic discrimination of isomers expands the universe of combinations.

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

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

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

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

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

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

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

208 flexible structures in the rapidly expanding universe of MOFs.

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

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

211 g new possibilities and applications for the universe of perovskite materials.

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

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

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

215 t specificity is vital, considering the vast universe of potential pHLA molecules that can be present

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

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

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

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

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

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

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

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

224 es that led to the discovery of an expanding universe of the components of the transcriptional and re

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

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

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

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

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

230 ext of life on Earth, however throughout the universe, other liquids may be able to support the emerg

231 the emergence of the classical realm of our Universe out of the quantum substrate.

232 ygen, the third most abundant element in the universe, plays a key role in the chemistry of condensed

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

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

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

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

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

238 o far unique role of our Solar System in the universe regarding its capacity for life raises fundamen

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

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

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

242 hree-quarters of the baryonic content of the Universe resides in a highly diffuse state that is diffi

243 matter(1), and an even larger amount of the Universe's energy content is attributed to dark energy(2

244 environment, neutral helium atoms formed the Universe's first molecular bond in the helium hydride io

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

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

247 or decades despite constituting ~ 85% of the universe's mass.

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

249 rrections and are insensitive to most of the Universe's volume and probably most of its mass.

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

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

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

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

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

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

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

257 s roughly five times more dark matter in the Universe than ordinary baryonic matter(1), and an even l

258 Half of all of the elements in the Universe that are heavier than iron were created by rapi

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

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

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

262 ned importance in the evolution of the early Universe, the HeH(+) ion has so far eluded unequivocal d

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

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

265 ere produced in the first few minutes of the Universe through a sequence of nuclear reactions known a

266 nd loss of energetic electrons in the plasma universe through resonant interactions with electrons.

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

268 ly studied in systems ranging from the early Universe to Bose-Einstein condensates(2-5), understandin

269 systems from longer than the lifespan of the universe to just minutes.

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

271 t a measurement of the baryon content of the Universe using the dispersion of a sample of localized f

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

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

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

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

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

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

278 ch of reionization, neutral gas in the early Universe was ionized by hard ultraviolet radiation emitt

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

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

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

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

283 ionally supported, cold disk galaxy when the Universe was only 1.5 billion years old favours formatio

284 galaxies at a mean redshift of 12, when the Universe was only 370 million years old.

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

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

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 considered in overdense regions of the early Universe, with a co-moving number density up to 10(-3) p

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