ライフサイエンスコーパス: quasar

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

2 c reflection features in a moderate-redshift quasar.

3 in the spectra of background sources such as quasars.

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

5 pports the unification scheme for radio-loud quasars.

6 polarization of gravitationally microlensed quasars.

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

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

9 kinetics and is spectrally orthogonal to the QuasArs.

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

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

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

13 These characteristics are unique among known quasars.

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

15 o spectrally separated fluorophores, FAM and Quasar 670.

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

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

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

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

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

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

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

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

24 Quasars are associated with and powered by the accretion

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

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

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

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

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

30 Quasars are rapidly accreting supermassive black holes a

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

32 Quasars are the most luminous non-transient objects know

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

65 of absorption line systems toward background quasars for decades.

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

95 absorption correlations in a sample of close quasar pairs.

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

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

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

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

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

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

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

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

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

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

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

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

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

109 from starburst galaxies or heavily filtered quasar radiation.

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

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

112 QuASAR reveals that CrvA asymmetrically patterns peptido

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

130 525150.3 at z approximately 6, which hosts a quasar, then our prospects for detecting the gas and dus

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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