ライフサイエンスコーパス: quasar

1 mponents for both a sample and an individual quasar.

2 observe in hours what would take months in a quasar.

3 c reflection features in a moderate-redshift quasar.

4 es, extragalactic jets in radio sources, and quasars.

5 These characteristics are unique among known quasars.

6 in the spectra of background sources such as quasars.

7 lations of galaxies, BL Lacertae objects, or quasars.

8 pports the unification scheme for radio-loud quasars.

9 traviolet (UV) absorption towards background quasars.

10 of hydrogen and helium atoms in a sample of quasars.

11 polarization of gravitationally microlensed quasars.

12 l Seyfert galaxies and a few higher-redshift quasars.

13 greater than those of previously known z > 6 quasars.

14 kinetics and is spectrally orthogonal to the QuasArs.

15 al spectra and light-variability of two such quasars.

16 emission in a sample of 21 z approximately 6 quasars.

17 se have only been observed in starbursts and quasars(11,12).

18 rburst galaxies(8-12) and companions of rare quasars(13,14).

19 ssed using the SCOT cohort for discovery and QUASAR 2 cohort for validation.

20 oxaliplatin-based chemotherapy, and from the QUASAR 2 trial (ISRCTN45133151), which compared adjuvant

21 cases from the SCOT trial and 1069 from the QUASAR 2 trial in our analysis.

22 tage II or III R0 colorectal cancer from the QUASAR 2 trial was used for validation; these patients w

23 E)-FoxP3(IS) was confirmed in cases from the QUASAR 2 trial, both as a continuous variable (aHR(75 vs

24 For the open-label, randomised, controlled QUASAR 2 trial, which was done at 170 hospitals in seven

25 Low-luminosity quasars(4-6) from the Hyper Suprime-Cam Subaru Strategic

26 o spectrally separated fluorophores, FAM and Quasar 670.

27 hole seeds(6) and one of the first luminous quasars(7).

28 es for the cool gas in the CGM can reconcile quasar absorption measurements (from which we infer the

29 ted stars in the Milky Way's halo and in two quasar absorption systems at redshift z = 3 (ref. 4).

30 a primordial origin of variations of D/H in quasar absorption systems.

31 r and atomic line-excitation temperatures in quasar absorption-line systems, but are model dependent(

32 ~ 2), the peak of global star formation and quasar activity(3,4).

33 nown as microquasars, mimic the behaviour of quasars and active galactic nuclei.

34 ndipitous; they are close to their companion quasars and appear bright in the far-infrared.

35 ve recently been discovered in high-redshift quasars and galaxies corresponding to a time when the Un

36 n lines present in the spectra of background quasars and gamma-ray bursts(5-10).

37 rs varies on much shorter timescales than in quasars and occasionally produces exceptionally bright X

38 ve galaxies that can be observed as luminous quasars and starbursts.

39 systematically assessed Arch(D95N), Archon, QuasAr, and the eFRET sensors MacQ-mCitrine and QuasAr-m

40 highest-redshift submillimetre galaxies and quasars, and a likely progenitor for the dense, ancient

41 of galaxies, narrow pencil-beam surveys, and quasars, appear to be yielding a consistent picture of t

42 Quasars are associated with and powered by the accretion

43 puzzling result suggests that these distant quasars are evolved objects even though the Universe was

44 Thus z approximately 6 quasars are indeed at an early evolutionary stage, with

45 the mass of the black hole, and the brighter quasars are inferred to have black holes with masses of

46 The two hot-dust-free quasars are likely to be first-generation quasars born i

47 As typical quasars are not, however, undergoing intense star format

48 Quasars are rapidly accreting supermassive black holes a

49 But because these episodes are brief, quasars are rare objects typically separated by cosmolog

50 Quasars are the most luminous non-transient objects know

51 optical and radio observations of radio-loud quasars are the result of different viewing angles.

52 Quasars are thought to be powered by the accretion of ga

53 Active galactic nuclei and quasars are thought to be scaled-up versions of Galactic

54 helium (He II) absorption in the spectra of quasars are unique probes of structure in the early univ

55 than 13 megaparsecs and contains a luminous quasar as well as a system rich in molecular gas.

56 the ratio of heavily obscured to unobscured quasars as a function of cosmic epoch up to z congruent

57 of the mass of the black hole in a luminous quasar at a redshift of 2, with a look back in time of 1

58 deep observation of a gravitationally lensed quasar at z = 0.658.

59 heavy-element absorption in a spectrum of a quasar at z = 7.04, when the Universe was just 772 milli

60 In a spectroscopic search of 62 quasars at a redshift of about 2, we have discovered lar

61 ilar in size from luminous type 1 and type 2 quasars at concordant redshift.

62 dust-enshrouded galaxies or a population of quasars at extremely high redshift.

63 Nz7q is an antecedent to unobscured luminous quasars at later epochs.

64 faintness of the galaxies compared with the quasars at optical wavelengths.

65 smic gas fluorescently illuminated by bright quasars at redshift z approximately 2.3.

66 s of light known at present are galaxies and quasars at redshift z congruent with 6, and their spectr

67 nd near-infrared observations of a sample of quasars at redshifts 5.8 z 6.6.

68 factor of three smaller than is typical for quasars at redshifts between 6.0 and 6.4.

69 tical images and spectroscopy of two HSC-SSP quasars at z > 6 with the JWST.

70 The red optical colours of outflow quasars at z 5.8 indeed suggest that these systems are d

71 d gas nebulae surrounding three luminous red quasars at z ~ 0.4 from Gemini integral field unit obser

72 sion from the infrared-luminous 'Cloverleaf' quasar (at a redshift zeta = 2.5579).

73 ee quasars are likely to be first-generation quasars born in dust-free environments and are too young

74 strate that the hot-dust abundance in the 21 quasars builds up in tandem with the growth of the centr

75 een resolved into individual sources (mainly quasars), but these sources do not have the spectral ene

76 ctrum resulting from the integrated light of quasars, but ratios of >100 in many locations indicate a

77 ed black-hole growth in the form of 'type-2' quasars, but their numbers are fewer than expected from

78 re, with one exception, the host galaxies of quasars, but these galaxies also host accreting supermas

79 lines imprinted on the spectra of background quasars, but these have typically yielded measurements o

80 frared and radio emissions characteristic of quasars, but which are faint at near-infrared and optica

81 ocess ensures that haloes capable of forming quasars by a redshift of z > 6 produce massive seeds.

82 that then transition to unobscured luminous quasars by expelling gas and dust(5).

83 Absorption of radiation from distant quasars by intervening clouds of gas offers a means of p

84 stellar absorption lines in the more massive quasar, confirming the detection of the host.

85 Each quasar contains a black hole with a mass of about one bi

86 masses) of dust observed in the most distant quasars could have been produced within only 700 million

87 orated amplification signal reporters, read "quasar"), does not significantly reduce the amplificatio

88 Quasar-driven outflows on galactic scales are a routinel

89 provide unambiguous evidence for galaxy-wide quasar-driven outflows, in parallel with the quasi-spher

90 ction of starlight from the host galaxies of quasars during the reionization epoch (z > 6) has been e

91 Pairs of quasars, each with a massive black hole at the centre of

92 we discovered a physical association of four quasars embedded in a giant nebula.

93 te an evolutionary sequence of dust-reddened quasars emerging from heavily dust-obscured starbursts t

94 ocity-broadened gas in the vicinity of these quasars enables measurements of their black hole masses

95 These outflows carry ~1% of the total quasar energy, while their kinematics are consistent wit

96 reconciled with theory by the hypothesis of quasar "evolution," which, however, appears incapable of

97 e(1,2) since it was discovered that luminous quasars existed only 700 million years after the Big Ban

98 onserving mechanism that is the basis of the quasar feedback in active galactic nuclei that lack powe

99 ultraluminous infrared galaxies support this quasar-feedback idea, because they directly trace the ga

100 of absorption line systems toward background quasars for decades.

101 udies of the progenitor halo of a primordial quasar found that it favours the formation of such seeds

102 The summed emission from these quasars generates the cosmic X-ray background, the spect

103 bined analysis of the Zeeman measurements of quasar H I absorption, H I emission, OH emission and HIN

104 This quasar has a bolometric luminosity of 4 x 10(13) times t

105 (6)), a transitioning quasar has not been found at similar redshifts owing to

106 ll as the luminosity density provided by the quasars, has therefore been substantially overestimated.

107 imaged, periodicities in the light curves of quasars have been interpreted as evidence for binaries,

108 probe to higher redshifts, however, because quasars have historically been identified in optical sur

109 Quasars have long been known to be variable sources at a

110 Such apparently hot-dust-free quasars have no counterparts at low redshift.

111 ic nuclei-the low-luminosity counterparts of quasars-have been observed in low-redshift mergers(2), n

112 rer observations of the line of sight to the quasar HE2347-4342 in the 1000 to 1187 angstrom band at

113 The current highest redshift quasar host detected(3), at z = 4.5, required the magnif

114 Observations of molecular hydrogen in quasar host galaxies at high redshifts provide fundament

115 rbon monoxide has been detected in about ten quasar host galaxies with redshifts z > 2; the record-ho

116 The inferred abundance of quasar host galaxies, as well as the luminosity density

117 Optically luminous quasars host the most prodigious accreting black holes i

118 The most luminous quasars, however, are not confined to such high-density

119 oles (SMBHs), which may be witnessed as dual quasars if both SMBHs are rapidly accreting.

120 -shear environments could have created these quasars if they were 10(4)-10(5) solar masses at birth,

121 rces are similar to the host galaxies of the quasars in [C ii] brightness, linewidth and implied dyna

122 ponential growth during which we see them as quasars in the distant Universe.

123 luminosities and brightness fluctuations of quasars in the early Universe suggest that some were pow

124 distinguishable from those of lower-redshift quasars in the rest-frame ultraviolet/optical and X-ray

125 different sequencing depths demonstrate that QuASAR is a powerful tool for ASE analysis when genotype

126 he chance probability of finding a quadruple quasar is estimated to be approximately 10(-7), implying

127 low-redshift mergers(2), no unambiguous dual quasar is known at cosmic noon (z ~ 2), the peak of glob

128 e quasars seen in a direction from which the quasar is obscured, and there is some limited direct evi

129 The phase transition between galaxies and quasars is often identified with the rare population of

130 n lines on the spectra of distant background quasars known as the Lyman-alpha forest.

131 The most distant quasars known, at redshifts z approximately 6, generally

132 at of the Sun have been detected in luminous quasars less than one billion years after the Big Bang,

133 3, identified by detecting its absorption of quasar light.

134 ses when mergers drive gas infall that feeds quasar-like events.

135 or about 80 per cent of the emission, with a quasar-like luminosity of 1.5 x 10(46) ergs per second.

136 envector 1 has long been suspected to be the quasar luminosity normalized by the mass of the hole (th

137 nes in the ultraviolet spectra of background quasars lying near the LMC.

138 Every radio-loud quasar may have blazar activities, according to a unifie

139 ray polarization of a cosmologically distant quasar microlensed by the random star field in a foregro

140 sAr, and the eFRET sensors MacQ-mCitrine and QuasAr-mOrange, in the nematode Caenorhabditis elegans A

141 es associated with the much brighter compact quasar nuclei (separated by 0.46" or 3.8 kpc) and low-su

142 n early massive black holes and the luminous quasars observed at z = 6.

143 ming visible over intergalactic distances as quasars or active galactic nuclei (AGN).

144 Quasar outflows may play a crucial role in regulating th

145 e host galaxy, although the spatial scale of quasar outflows remain a major enigma, with their accele

146 absorption correlations in a sample of close quasar pairs.

147 the broadband x-ray spectra of the luminous quasar PDS 456.

148 dic signal in the optical variability of the quasar PG 1302-102 with a mean observed period of 1,884

149 across the broad Halpha emission line in the quasar PG 1700+518 originate close to the accretion disk

150 selkumab induction given intravenously (from QUASAR phase 2b and phase 3 induction studies) were rand

151 The QUASAR Phase 2b Induction Study evaluated the efficacy a

152 d, double-blind, placebo-controlled studies (QUASAR phase 3 induction and maintenance) included rando

153 ation has been shut down, perhaps during the quasar phase of rapid accretion onto a supermassive blac

154 galaxies once passed through a hyperluminous quasar phase powered by accretion onto a supermassive bl

155 r mass), there must have been an earlier pre-quasar phase when these black holes grew (mass range app

156 rom accretion onto the black hole during its quasar phase(4-6).

157 During the quasar phase, a huge luminosity is released as matter fa

158 is consistent with that expected for the pre-quasar phase.

159 r results show that most of the diversity of quasar phenomenology can be unified using two simple qua

160 How quasars powered by supermassive black holes formed less

161 Bright quasars, powered by accretion onto billion-solar-mass bl

162 ights into new astronomical phenomena (e.g., quasars, pulsars, and the 3 degrees cosmic background ra

163 ogen column density in the cloud towards the quasar Q1937 - 1009, for which one of the low D/H values

164 osomal interactions, and novel ones, such as QuASAR-QC, to identify low-quality experiments.

165 o quantify how curvature forms, we developed QuASAR (quantitative analysis of sacculus architecture r

166 We present QuASAR, quantitative allele-specific analysis of reads,

167 ndicating that the coupling between dust and quasar radiation may produce powerful feedback that is c

168 from starburst galaxies or heavily filtered quasar radiation.

169 vidence of absorption of the spectrum of the quasar redwards of the Lyman alpha emission line (the Gu

170 luding HiCRep, GenomeDISCO, HiC-Spector, and QuASAR-Rep.

171 of this model, every obscured and unobscured quasar represents two distinct phases that result from a

172 QuASAR reveals that CrvA asymmetrically patterns peptido

173 his program, designed to detect very distant quasars, reveals the powers and limitations of charged-c

174 nt observation are made for the Large Bright Quasar Sample.

175 Here we report CO emission from the quasar SDSS J114816.64 + 525150.3 at z = 6.42.

176 Here we report that the quasar SDSS J153636.22+044127.0 is a plausible example o

177 we report the discovery of an ultraluminous quasar, SDSS J010013.02+280225.8, at redshift z = 6.30.

178 naroff-Riley type 2 (FR2) radio galaxies are quasars seen in a direction from which the quasar is obs

179 This quasar shows two broad-line emission systems, separated

180 ence of supermassive BHs that power luminous quasars so soon after the Big Bang.

181 About half of the quasar spectra reveal broad, blueshifted absorption line

182 lysing carbon and oxygen absorption lines in quasar spectra that allows us to probe the heavy-element

183 In particular, quasar spectroscopy is sensitive either to the very smal

184 luated in the Quick and Simple and Reliable (QUASAR) study.

185 therefore coexists with the peak activity of quasars, suggesting a close relationship between the gro

186 y polarized photons emitted by high-redshift quasars suggests similar magnetic fields are present in

187 missivity and escape fractions (f(esc)) from quasars support their role in driving cosmic reionizatio

188 panions in four out of the twenty-five z > 6 quasars surveyed, a fraction that needs to be accounted

189 vey (SDSS) J0749 + 2255 as a kpc-scale, dual-quasar system hosted by a galaxy merger at cosmic noon (

190 mass BH seeds into the supermassive luminous quasars that are observed when the universe is 1 billion

191 They are analogues of quasars that contain supermassive black holes of 10(6) t

192 orption lines in the spectra of more distant quasars that lie along the same line of sight-provides t

193 easurement of time delays in multiply imaged quasars, the Sunyaev-Zel'dovich effect in clusters, and

194 525150.3 at z approximately 6, which hosts a quasar, then our prospects for detecting the gas and dus

195 e ionized proximity zone associated with the quasar to be about 26 million light years, larger than f

196 herapy are similar, allowing NNTs derived in QUASAR to be updated using contemporary, nonrandomized d

197 Tumor tissue from 868 patients in the QUASAR trial (adjuvant fluorouracil/folinic acid v obser

198 The aim of the QUASAR trial was to determine the size and duration of a

199 up B 9581 and Quick and Simple and Reliable (QUASAR) trials.

200 Despite extensive efforts, however, the quasar ULAS J1120 + 0641 at redshift z = 7.09 has remain

201 Here we report observations of the quasar ULAS J134208.10 + 092838.61 (hereafter J1342 + 09

202 Here we report observations of a quasar (ULAS J112001.48+064124.3) at a redshift of 7.085

203 n-alpha emission surrounding the radio-quiet quasar UM 287 extends well beyond the virial radius of a

204 he outflows, owing to the long timescales of quasar variability.

205 ew data sets for a systematic exploration of quasar variability.

206 Recently one z approximately 6 quasar was shown not to have any detectable emission fro

207 s spectral energy distributions of gamma-ray quasars, we find a seed factor distribution which peaks

208 nd subtracting the light from the unresolved quasars, we find that the host galaxies are massive (ste

209 The first quasars were thus a natural consequence of structure for

210 Quasars, which are exceptionally bright objects at the c

211 detection of a population of distant type-2 quasars, which is at least comparable in size to the wel

212 ived superbubble "break-out" phase, when the quasar wind drives the bubbles to escape the confinement

213 r 247,000 known, spectroscopically confirmed quasars with a temporal baseline of about 9 years.

214 years, larger than found with other z > 6.1 quasars with lower luminosities.

215 So far, roughly 40 quasars with redshifts greater than z = 6 have been disc

216 lack holes; the detection of highly luminous quasars with redshifts greater than z = 6 suggests that

217 the Big Bang, as revealed by observations of quasars with redshifts of less than 6.5.

218 Exceptionally bright quasars with redshifts up to z = 6.28 have recently been

219 The fraction of quasars with such outflow winds at z 5.8 is ~2.4 times h

220 Here we show that up to one-third of known quasars with z approximately equal to 6 will have had th

221 our galaxies at z > 6 that are companions of quasars, with velocity offsets of less than 600 kilometr

222 Here we report the discovery of a second quasar without hot-dust emission in a sample of 21 z app

223 ll also confirm the strong gravity nature of quasar X-ray emission.

224 rossing events using the first simulation of quasar X-ray microlensing polarization light curves.