ライフサイエンスコーパス: cosmic

1 from Catalog of Somatic Mutations in Cancer (COSMIC), a large-scale database curated by the Wellcome

2 t is difficult to reconcile the low observed cosmic abundance of 3He with the predictions of both ste

3 , silicon, iron, and calcium) are present in cosmic abundances, with only small grain-to-grain variat

4 ese 'standardisable candles' indeed indicate cosmic acceleration.

5 d other theories that reproduce the observed cosmic acceleration.

6 at a redshift of z = 9.6 +/- 0.2 (that is, a cosmic age of 490 +/- 15 million years, or 3.6 per cent

7 tribution of the first stars at redshift 20 (cosmic age of around 180 million years), incorporating a

8 laxies (where the bulk of stars formed) at a cosmic age of less than about 500 million years (z less,

9 galaxies seem to be abundant at such a young cosmic age, suggesting that they may be the dominant sou

10 In addition, COSMIC also details more than six million noncoding muta

11 osity, suggests that GRB 031203 is the first cosmic analogue to GRB 980425.

12 The resistance of melanized fungi to cosmic and terrestrial ionizing radiation suggests that

13 e occupationally exposed to higher levels of cosmic and UV radiation than the general population, but

14 ns in human cancer has now been curated into COSMIC and while this is continually updated, a greater

15 he Catalogue of Somatic Mutations in Cancer (COSMIC) and the spatial information in the Protein Data

16 m OMIM, 587 873 cancer-related variants from COSMIC, and 1 484 045 SNPs from dbSNP.

17 ol regions, as well as links to Entrez Gene, COSMIC, and iHOP gene pages and the UCSC and Ensembl gen

18 sphere; they are inconsistent with volcanic, cosmic, anthropogenic, lightning, or authigenic sources.

19 of the cosmic microwave background with the Cosmic Background Imager from September 2002 to May 2004

20 on today, will demonstrate the presence of a cosmic background of hard X-rays at that early time.

21 t grains); this energy now forms part of the cosmic background radiation at wavelengths near 1 mm.

22 tain fewer baryons (gas plus stars) than the cosmic baryon fraction.

23 theories and are given by the areas of dual cosmic branes.

24 Among the mutated genes were almost 200 COSMIC Cancer Gene Census genes, many of which were recu

25 ely 470 million years ago one of the largest cosmic catastrophes occurred in our solar system since t

26 om the Cancer Cell Line Encyclopedia and the COSMIC Cell Lines Project to three renal cancer subtypes

27 compression occurs, such as an impact from a cosmic cloud or other galaxy.

28 tifies 15% redundant indels in dbSNP, 29% in COSMIC coding, and 13% in COSMIC noncoding datasets acro

29 ore redundant indels in dbSNP; 2,118 more in COSMIC coding, and 553 more in COSMIC noncoding indel da

30 Currently (v43, August 2009), COSMIC contains details of 1.5-million experiments perfo

31 COSMIC curates comprehensive information on somatic muta

32 ble for ionization of the Universe after the cosmic 'Dark Ages', when the baryonic matter was neutral

33 All information from the COSMIC database is available freely on the COSMIC websit

34 ine calls and comparison of somatic calls to COSMIC database variants.

35 on for approximately 10 000 mutations in the COSMIC database, the method does well in assigning highe

36 tely 2% of RCC patient samples in the Sanger COSMIC database.

37 ion years after the Big Bang, initiating the cosmic dawn.

38 esponding to the largest fluctuations in the cosmic density field.

39 ination, provide a direct measurement of the cosmic density of ionized baryons in the intergalactic m

40 inental crust (approximately 1.3) and mantle/cosmic dust (approximately 0.13).

41 In situ data from the Cosmic Dust Analyzer on board the Cassini spacecraft rev

42 This review discusses the magnitude of the cosmic dust input into the earth's atmosphere, and the r

43 Second, cosmic dust particles enter the atmosphere at high speed

44 s have terrestrial origins but also occur as cosmic dust particles.

45 esolution, glacial-to-interglacial record of cosmic dust using helium isotope analysis of the Europea

46 , soil erosion, eolian dust, sea-salt spray, cosmic dust, volcanic emissions, and for helium, hydrody

47 ar ice provides an archive for the influx of cosmic dust.

48 c, and cosmic materials, yet consistent with cosmic ejecta, supporting the hypothesis of extraterrest

49 in agreement with the accumulation rates of cosmic-enriched elements (Ir, Pt, Os and super-paramagne

50 d Strelka obtained the largest proportion of COSMIC entries as well as the lowest rate of dbSNP prese

51 cured to unobscured quasars as a function of cosmic epoch up to z congruent with 3 and show that a si

52 The relevance of this scenario at early cosmic epochs is not yet established.

53 scovered hundreds of galaxies at these early cosmic epochs, but their star-formation rates are more t

54 ve formed their dense stellar cores in early cosmic epochs.

55 of the IMF in other galaxies and at earlier cosmic epochs.

56 able studies of the Universe at the earliest cosmic epochs.

57 wed range of the Hubble constant, unless the cosmic equation of state is dominated by a component tha

58 dings do not preclude a terminal Pleistocene cosmic event.

59 emanates from a variety of sources, such as cosmic events, particle accelerators, nuclear reactors a

60 e constraint on the primordial abundance and cosmic evolution of lithium that is not susceptible to t

61 the Big Bang, and traces 13 billion years of cosmic evolution with 12 billion resolution elements in

62 city is the line-of-sight departure from the cosmic expansion and arises from gravitational perturbat

63 alaxies are inward after removal of the mean cosmic expansion and long range flows.

64 ervational programs can trace the history of cosmic expansion more precisely and over a larger span o

65 d arrivals of the supernova images probe the cosmic expansion rate, as well as the distribution of ma

66 rnovae good 'standard candles' for measuring cosmic expansion, but a correction must be applied to ac

67 be derived from the subtraction of the mean cosmic expansion, the product of distance times the Hubb

68 al lens could be used to measure the rate of cosmic expansion.

69 sion that arrives with the gamma-rays from a cosmic gamma-ray burst (GRB) is a signature of the engin

70 The explosion that results in a cosmic gamma-ray burst (GRB) is thought to produce emiss

71 appear to be a short-duration, hard-spectrum cosmic gamma-ray burst.

72 tion gamma-ray bursts are intense flashes of cosmic gamma-rays, lasting less than about two seconds,

73 pha emission, discovered during a survey for cosmic gas fluorescently illuminated by bright quasars a

74 This is based on the assumption that the cosmic gas was heated by stellar remnants-particularly X

75 tations such as the 1000 Genomes project and COSMIC give an opportunity to investigate general princi

76 he Catalogue of Somatic Mutations in Cancer (COSMIC), GraphPAC identifies new mutational clusters in

77 mic features has become a significant focus; COSMIC has begun curating full-genome resequencing exper

78 C risk prediction after exposure to high-LET cosmic heavy ion radiation exposure is hindered due to s

79 ions in the total production of photons over cosmic history and may contain faint, extended component

80 based and space-borne telescopes have probed cosmic history from the present day to a time when the U

81 s quickly, within the first billion years of cosmic history in a short, extreme starburst.

82 their centres, are the relics of a period in cosmic history when galaxies formed stars at remarkable

83 h in the young Universe and that, throughout cosmic history, black-hole growth occurs in the dusty, g

84 n tandem with their host galaxies throughout cosmic history, starting from the earliest times.

85 ast 20 years have revolutionized our view of cosmic history, transforming our understanding of how th

86 Star-forming galaxies trace cosmic history.

87 y galaxies probably induced a major event in cosmic history: the reionization of intergalactic hydrog

88 YDB objects with melt products from a known cosmic impact (Meteor Crater, Arizona) and from the 1945

89 ounger Dryas impact hypothesis posits that a cosmic impact across much of the Northern Hemisphere dep

90 en invigorated by a hypothesis implicating a cosmic impact at the Allerod-Younger Dryas boundary or Y

91 raters, and its presence strongly supports a cosmic impact event, further strengthened by its co-occu

92 act strewnfields and consistent with a major cosmic impact event.

93 mpelling evidence to accept the claim that a cosmic impact occurred approximately 12,800 y ago and ca

94 episode known as the Younger Dryas (YD) is a cosmic impact or airburst at the YD boundary (YDB) that

95 egafaunal extinction possibly triggered by a cosmic impact over North America at approximately 12,900

96 's typical surficial processes but common to cosmic impacts.

97 s, and magnetic microspherules attributed to cosmic impacts/airbursts.

98 scopes, they would have produced significant cosmic infrared background radiation in the near-infrare

99 omic information recently updated to GRCh37, COSMIC integrates many diverse types of mutation informa

100 0(6) non-synonymous mutations extracted from COSMIC, involving ~8000 genome-wide screened samples acr

101 as well as in the thermalization of both the cosmic IR and microwave background and in galactic cente

102 e of mutations in cancer, the information in COSMIC is curated by expert scientists, primarily by scr

103 bers of genomic rearrangements in cancer and COSMIC is now displaying details of these analyses also.

104 he catalogue of Somatic Mutations in Cancer (COSMIC) is the largest public resource for information o

105 Here we report on experiments from the Cosmics Leaving Outdoor Droplets chamber at the European

106 ticle formation experiments performed at the Cosmics Leaving Outdoor Droplets chamber at the European

107 ow, in experiments performed with the CLOUD (Cosmics Leaving Outdoor Droplets) chamber at CERN, that

108 ganic compounds conducted in the CERN CLOUD (Cosmics Leaving Outdoor Droplets) chamber.

109 we study nano-particle growth in the CLOUD (Cosmics Leaving OUtdoors Droplets) chamber, starting fro

110 Our findings reveal cosmic limits on the age synchronization of young binary

111 The microspherules were explained as either cosmic material ablation or terrestrial ejecta from a hy

112 ith anthropogenic, volcanic, authigenic, and cosmic materials, yet consistent with cosmic ejecta, sup

113 ich are expected to be representative of the cosmic matter content of the universe (baryons and dark

114 The apparent baryon fraction exceeds the cosmic mean at larger radii, suggesting a clumpy distrib

115 an a millikelvin) that marks the rise of the cosmic mean gas temperature above the microwave backgrou

116 As current detectors of the cosmic microwave background (CMB) already have sensitivi

117 stant supernovae and the fluctuations in the cosmic microwave background (CMB) indicate that the expa

118 c approach to TDA modeling in an analysis of cosmic microwave background (CMB) nonhomogeneity.

119 around these, and through its imprint on the Cosmic Microwave Background (CMB).

120 ons, which manifest in the anisotropy of the cosmic microwave background and the large-scale correlat

121 -ray binaries-to temperatures well above the cosmic microwave background at that time (about 30 kelvi

122 Observations of the cosmic microwave background indicate that baryons accoun

123 Recent cosmic microwave background polarization measurements in

124 a vital role across a range of systems: from cosmic microwave background polarization to superconduct

125 With recent precise measurements of the cosmic microwave background radiation, large galaxy reds

126 Age is the period between the time when the cosmic microwave background was emitted and the time whe

127 Polarization observations of the cosmic microwave background with the Cosmic Background I

128 teristic imprints in the polarization of the cosmic microwave background, or later with direct space-

129 the universe, gravitational lensing, and the cosmic microwave background.

130 This indicated that COSMIC mutational signature 24, previously hypothesized

131 ing: genomic conservation score, known SNPs, COSMIC mutations, disease associations and others.

132 Unresolved anisotropies of the cosmic near-infrared background radiation are expected t

133 s in dbSNP, 29% in COSMIC coding, and 13% in COSMIC noncoding datasets across all human chromosomes,

134 2,118 more in COSMIC coding, and 553 more in COSMIC noncoding indel dataset in addition to the ones r

135 COSMIC now details the genetics of drug resistance, nove

136 The cosmic optical background is an important observable tha

137 The cosmic origin of elements heavier than iron has long bee

138 vey of the outskirts of 42 galaxies with the Cosmic Origins Spectrograph onboard the Hubble Space Tel

139 s extensive application to a wide variety of cosmic phenomena.

140 before being driven more than 2 hours to the Cosmic Physics Laboratory at Chacaltaya (5200 m) where t

141 We estimate the cosmic production rate of helium relative to metals (Del

142 he Catalogue of Somatic Mutations in Cancer (COSMIC), QuartPAC is able to identify clusters which are

143 Cosmic radiation also disrupted synaptic integrity and i

144 Because messages require protection from cosmic radiation and small messages could be difficult t

145 Understanding the temporal variation of cosmic radiation and solar activity during the Holocene

146 ue opportunity to reconstruct the history of cosmic radiation and solar activity over many millennia.

147 Rodents exposed to cosmic radiation exhibit persistent hippocampal and cort

148 Of particular concern is the potential for cosmic radiation exposure to compromise critical decisio

149 ffects of heavy ionizing particles and other cosmic radiation need to be considered.

150 The new cosmic radiation record enables us to derive total solar

151 ion will result in an inevitable exposure to cosmic radiation that has been shown to cause cognitive

152 iomarker preservation against destruction by cosmic radiation.

153 enous thromboembolism and long-haul flights, cosmic-radiation exposure, jet lag, and cabin-air qualit

154 nmental radiation background, and monitoring cosmic radiations.

155 ang nucleosynthesis (BBN) depend only on the cosmic ratio of baryons to photons, a quantity inferred

156 many predictions, the intensity of anomalous cosmic ray (ACR) helium did not peak at the shock, indic

157 s linked with either ultraviolet or galactic cosmic ray (GCR) effects on atmospheric particles.

158 er risk is an important concern for galactic cosmic ray (GCR) exposures, which consist of a wide-ener

159 agnetic field causes an increase in galactic cosmic ray (GCR) flux.

160 er began making detailed measurements of the cosmic ray and energetic particle radiation environment

161 gh a variety of processes (such as solar and cosmic ray bombardment, micro-meteorite bombardment, and

162 by cosmic rays for different grain sizes and cosmic ray components.

163 he puzzle of the origin of ultra high energy cosmic ray electrons.

164 The presented (36)Cl Cosmic Ray Exposure ages demonstrate that the cliff over

165 The cosmic ray flux is reduced symmetrically at all latitude

166 The small intensity gradient of Galactic cosmic ray helium indicates that either the gradient is

167 hat for the processes studied, variations in cosmic ray intensity do not appreciably affect climate t

168 The cosmic ray intensity increased when B was relatively lar

169 liosheath or the local interstellar Galactic cosmic ray intensity is lower than expected.

170 rs in the interstellar medium in response to cosmic ray ionization is summarized, and a review of the

171 here was a simultaneous increase in Galactic cosmic ray ions and electrons, anomalous cosmic rays and

172 ned inside the heliosphere, the intensity of cosmic ray nuclei from outside the heliosphere abruptly

173 Newly constructed ultrahigh-energy cosmic ray observatories together with high-energy gamma

174 Local cosmic ray production is also enhanced, typically by a f

175 For data pretreatment, we developed a unique cosmic ray removal method and used an automated baseline

176 Cosmic ray sources are likely to involve the most energe

177 Stellar nucleosynthesis and cosmic ray spallation are ruled out as causes of the ano

178 Here we show that the cosmic ray-produced nuclides beryllium-10 and aluminum-2

179 ltogether in looking for isolated regions of cosmic-ray acceleration.

180 of tens to hundreds of megaelectronvolts) is cosmic-ray albedo neutron decay (CRAND).

181 The Pierre Auger Observatory is the largest cosmic-ray detector on Earth, and as such is beginning t

182 volts per nucleon and an increasing galactic cosmic-ray electron intensity down to ~10 x 10(6) electr

183 Here we consider neutrino and cosmic-ray emission from multiple emission regions since

184 The cosmic-ray exposure age of Ost 65 shows that it may be a

185 This interpretation relies mainly on cosmic-ray exposure dating of glacial deposits.

186 If such a high cosmic-ray flux is ubiquitous in diffuse clouds, the dis

187 paper we review the observables generated by cosmic-ray interactions with the interstellar medium, fo

188 ectrons (e-), the electron fraction, and the cosmic-ray ionization rate.

189 The origin of Galactic cosmic-ray ions has remained an enigma for almost a cent

190 sequent enrichment of the gas by stellar and cosmic-ray nucleosynthesis.

191 anisotropy maps of ground-based high-energy cosmic-ray observatories (Milagro, Asgamma, and IceCube)

192 The Galaxy is filled with cosmic-ray particles, mostly protons with kinetic energi

193 The unexpectedly high flux of cosmic-ray positrons detected at Earth may originate fro

194 Cosmic-ray produced radionuclides, such as (10)Be and (1

195 of stellar evolution, binary formation, and cosmic-ray production in the Galactic Centre.

196 ources, dark matter, or unknown processes of cosmic-ray secondary production.

197 After consideration of cosmic-ray spallation and degassing processes, our resul

198 nyl alcohol (C2H3OH) act as key tracers of a cosmic-ray-driven nonequilibrium chemistry leading to co

199 Cosmic-ray-produced (3)He, (21)Ne, and (36)Ar yield conc

200 700 years ago), based on new measurements of cosmic-ray-produced beryllium and aluminium isotopes ((1

201 s are not the only source of pulsed heating; cosmic rays also can heat interstellar grains in a pulse

202 iving interstellar chemistry via ionization, cosmic rays also interact with the interstellar medium i

203 on of high-energy (tera-electron volts, TeV) cosmic rays and diffusive propagation from supernova sou

204 tic cosmic ray ions and electrons, anomalous cosmic rays and low-energy ions.

205 rays', as well as to re-accelerate Galactic cosmic rays and low-energy particles from the inner Sola

206 ssess the damage caused to such materials by cosmic rays and neutrons, which pose a variety of hazard

207 nsoon connection is dominated most likely by cosmic rays and oceanic circulation (both associated to

208 ative termination shock is that of anomalous cosmic rays and of interstellar pick-up ions.

209 orbed dose and dose equivalent from galactic cosmic rays and solar energetic particles on the martian

210 cts of meteorites and micrometeorites and of cosmic rays and solar-wind particles are major causes of

211 Cosmic rays are charged particles arriving at the Earth

212 Cosmic rays are the highest-energy particles found in na

213 rse, demands a mechanism for ionization, and cosmic rays are the ideal candidate as they can operate

214 at hundreds to thousands of eV and galactic cosmic rays at tens of TeV has wide-ranging implications

215 the prime candidates to produce the observed cosmic rays at the highest energies.

216 yager 2 did not find the source of anomalous cosmic rays at the shock, suggesting that the source is

217 mation, and could guide a wind of hot gas or cosmic rays away from the central region.

218 ter while simultaneously being shielded from cosmic rays by overlying ice.

219 istance does not greatly exceed the distance cosmic rays can diffuse over this time, 1 kiloparsec.

220 expectations, the extragalactic component of cosmic rays contributes substantially to the total flux

221 We report the spectra of galactic cosmic rays down to ~3 x 10(6) electron volts per nucleo

222 Here, we calculate the heating by cosmic rays for different grain sizes and cosmic ray com

223 aelectron volt electrons, ACRs, and galactic cosmic rays have steadily increased since late 2004 as t

224 he detection of supernova-produced (60)Fe in cosmic rays implies that the time required for accelerat

225 It provides an example to study the youth of cosmic rays in a superbubble environment before they mer

226 We find that ions from Galactic cosmic rays increase the nucleation rate by one to two o

227 Cosmic rays initiate air showers--cascades of secondary

228 The origin of Galactic cosmic rays is a century-long puzzle.

229 Radio detection of cosmic rays is a rapidly developing technique for determ

230 y support the idea that the bulk of galactic cosmic rays is accelerated in such remnants by a Fermi m

231 We argue that the radial anisotropy of the cosmic rays is expected to be small in the foreshock reg

232 comes from accelerators capable of producing cosmic rays of these energies.

233 50-parsec-wide cocoon of freshly accelerated cosmic rays that flood the cavities carved by the stella

234 In this process, cosmic rays that reach the upper atmosphere interact wit

235 Iron-60 ((60)Fe) is a radioactive isotope in cosmic rays that serves as a clock to infer an upper lim

236 va remnants (SNRs) hint that they accelerate cosmic rays to energies close to ~10(15) electron volts.

237 nets, astronauts will be exposed to galactic cosmic rays which are composed of heavy particles (such

238 uare centimetre for air showers initiated by cosmic rays with energies of 10(17)-10(17.5) electronvol

239 Measurements of the mass composition of cosmic rays with energies of 10(17)-10(18) electronvolts

240 g nucleosynthesis, interactions of energetic cosmic rays with interstellar matter, evolved low-mass s

241 s shock is expected to accelerate 'anomalous cosmic rays', as well as to re-accelerate Galactic cosmi

242 August 2012, while those of galactic origin (cosmic rays) increased by 9.3% at the same time.

243 f interstellar clouds, the energy density of cosmic rays, and the formation of stars.

244 ns, to help determine the source of Galactic cosmic rays, and to date circumstellar grains.

245 pectral energy distribution of the anomalous cosmic rays, however, indicates that Voyager 1 still has

246 the most energetic particles ever observed, cosmic rays, will begin to be revealed in the next few y

247 i's classic result on the energy spectrum of cosmic rays, with the universal exponent -2, which is in

248 nding of the oncogenic potential of galactic cosmic rays.

249 using a ground-based analog for exposure to cosmic rays.

250 the termination shock, generating anomalous cosmic rays.

251 through observations of gamma-ray photons or cosmic rays.

252 les us to determine the mass spectrum of the cosmic rays: we find a mixed composition, with a light-m

253 s have had an important role in the epoch of cosmic reionization and the chemical evolution of early

254 f the interstellar medium in galaxies during cosmic reionization are important for understanding the

255 approximately 2), galaxies vigorously fed by cosmic reservoirs are dominated by gas and contain massi

256 Examination of COSMIC's data is primarily web-driven, focused on provid

257 sponsible for the most powerful and dramatic cosmic sources.

258 z approximately 4 in terms of the density of cosmic space.

259 we show that the FeNi metal in the resulting cosmic spherules was oxidized while molten, and quench-c

260 Starburst galaxies at the peak of cosmic star formation are among the most extreme star-fo

261 When cosmic star formation history reaches a peak (at about r

262 tation in galaxies during this peak epoch of cosmic star formation indicates that gas accretion is li

263 Despite the overall downturn in cosmic star formation towards the highest redshifts, it

264 For example, in cosmological theories, cosmic strings may have formed knotted configurations in

265 According to the current understanding of cosmic structure formation, the precursors of the most m

266 has been remarkably successful in explaining cosmic structure over an enormous span of redshift, but

267 ic particles, is consistent with large-scale cosmic structure.

268 count the milestones in our understanding of cosmic structure; summarize its impact on astronomy, cos

269 Previous simulations of the growth of cosmic structures have broadly reproduced the 'cosmic we

270 erse, and slow down in the rate of growth of cosmic structures.

271 the dynamo excitation of magnetic fields in cosmic systems; (ii) its bearing on the existence of Eul

272 COSMIC, the Catalogue Of Somatic Mutations In Cancer is

273 COSMIC, the Catalogue of Somatic Mutations in Cancer is

274 xies during the first three billion years of cosmic time (redshift z > 4) indicate a rapid evolution

275 sive black hole with its host galaxy through cosmic time is encoded in its spin.

276 rise and fall of star formation over 95% of cosmic time, back to the current observational frontier

277 the galaxy's properties in a brief period of cosmic time.

278 ge range in cluster radius, cluster mass and cosmic time.

279 ion of extragalactic magnetic fields through cosmic times (up to microgauss levels reported in nearby

280 observations find metal-enriched galaxies at cosmic times when the Universe was less than 1 Gyr old.

281 rophysical conditions and remain stable over cosmic timescales, giving unique insights on their exist

282 her important references such as GENCODE and COSMIC using the Google Cloud Platform.

283 lly on highly characterized drugs and genes, COSMIC v78 contains wide resistance mutation profiles ac

284 We find that the baryon fraction reaches the cosmic value near the virial radius for all groups and c

285 We queried the dbSNP and COSMIC variant databases and found numerous variants ind

286 alyses of YDB spherules suggest they are not cosmic, volcanic, authigenic, or anthropogenic in origin

287 , but reside throughout the filaments of the cosmic web (where matter density is larger than average)

288 a and constrain the net magnetization of the cosmic web along this sightline to <21 nanogauss, parall

289 challenges faced as we prepare to probe the cosmic web at new wavelengths.

290 Here we report observations of a cosmic web filament in Lyman-alpha emission, discovered

291 shocked gas streaming along filaments of the cosmic web into dark-matter halos--are important.

292 The thread-like structure of this 'cosmic web' has been traced by galaxy redshift surveys f

293 smic structures have broadly reproduced the 'cosmic web' of galaxies that we see in the Universe, but

294 rse predict that galaxies are embedded in a 'cosmic web', where most baryons reside as rarefied and h

295 forming a "cosmic web." The discovery of the cosmic web, especially through its signature of absorpti

296 oing growth of clusters from the surrounding cosmic web.

297 ssing baryons reside in the filaments of the cosmic web.

298 s, sheets, and knots collectively forming a "cosmic web." The discovery of the cosmic web, especially

299 e COSMIC database is available freely on the COSMIC website.

300 ed emission from these quasars generates the cosmic X-ray background, the spectrum of which has been