ライフサイエンスコーパス: milky

1 om 4000 to 6000 mg/dl, and the plasma turned milky.

2 ries was that of ripe fruit, followed by the milky and chemical series.

3 y nucleate in the whole drop, leading to its milky color that typifies the so-called "Ouzo effect." O

4 The presence of a milky, creamy appearing ascitic fluid with triglyceride

5 h-quality natural rubber in their latex, the milky cytoplasm of specialized cells known as laticifers

6 investigate 20 to 200 nm sized inclusions in milky diamonds from Rio Soriso, Juina area, Brazil.

7 ng beetle, Thermonectus marmoratus, ejects a milky fluid from its prothoracic defensive glands when d

8 Gpihbp1 knockout mice on a chow diet have milky plasma and plasma triglyceride levels of more than

9 (basalt, granite, hematite, magnetite, mica, milky quartz, and clear quartz) to quantify the capillar

10 lue-white veil, pink color, black color, and milky red/pink areas.

11 caused by luminous bacteria, but details of milky sea composition, structure, cause, and implication

12 e sensors detected a possible bioluminescent milky sea south of Java, Indonesia, spanning >100,000 km

13 e data, and assess their photography of this milky sea.

14 Milky seas are a rare form of marine bioluminescence whe

15 re, we show initial examples of DNB-detected milky seas based on a multi-year search.

16 f scientific observations, an explanation of milky seas has remained elusive.

17 est Indian Ocean and the Maritime Continent, milky seas have eluded rigorous scientific inquiry, and

18 ding water, resulting in a phenomenon called milky seas or sea sparkle.

19 ow help guide research vessels toward active milky seas to learn more about them.

20 ny light-emitting organism, these so-called "milky seas" are hypothesized to be manifestations of unu

21 "Milky seas" are massive swaths of uniformly and steadily

22 low-light imager, holds potential to detect milky seas, but the capability has yet to be demonstrate

23 se genetic background does not alter omental milky spot number and size, nor does it affect ovarian c

24 Similarly, medium conditioned by milky spot-containing adipose tissue caused 75% more cel

25 ell migration than did medium conditioned by milky spot-deficient adipose.

26 um also contains lymphoid aggregates, called milky spots (MSs), that contribute to peritoneal immunit

27 e present study shows the novel finding that milky spots and adipocytes play distinct and complementa

28 dings support a two-step model in which both milky spots and adipose have specific roles in colonizat

29 , we report that, in addition to the omental milky spots and fat-associated lymphoid clusters, in mic

30 ally associated with lymph nodes and omental milky spots have site-specific properties that equip the

31 Unlike conventional lymphoid organs, milky spots in the omentum developed in the absence of l

32 These results indicate that the milky spots of the omentum function as unique secondary

33 Omental milky spots readily concentrate intra-abdominal E. coli

34 Although the lymphoid architecture of milky spots was disrupted in lymphotoxin-deficient mice,

35 ue characterized by immune structures called milky spots, but the cellular dynamics that direct this

36 This tissue is unusual for its milky spots, comprised of immune cells, stromal cells, a

37 omental and splenoportal fat, which contain milky spots, rather than in peritoneal fat depots.

38 PWC5 variety of purple waxy corn at the milky stage had the highest values for all parameters, a

39 d higher expression level of OsNAC121 during milky stage in untransformed rice, compared to 14-day ol

40 TPC and TAC were highest at the milky stage, whereas TFC and AA were highest at the silk

41 Hybridization between milky stork (Mycteria cinerea) and painted stork (M. leu

42 I also estimate the age of the Milky Way (14.5(+2.8)(-2.2)Gyr in a way that is independ

43 ources further than the sun (both within the Milky Way and beyond) are expected to produce a flux of

44 00 K) foreground synchrotron emission in the Milky Way and extragalactic continuum sources.

45 enuation feature, which is well known in the Milky Way and galaxies at z 3 (refs.

46 ription of the Grand Rotation Curves for the Milky Way and M31 galaxies.

47 individual galaxies, for example, around the Milky Way and M82 (refs. (2,3)).

48 ered magnetic fields have been mapped in the Milky Way and nearby galaxies(1,2), but it is not known

49 nding of the globular cluster systems of the Milky Way and other galaxies point to a complex picture

50 ews recent studies of collisions between the Milky Way and smaller satellite galaxies.

51 expected for this line of sight through the Milky Way and the intergalactic medium, indicating magne

52 arm as it passes through the far side of the Milky Way and to validate a kinematic method for determi

53 Massive disk galaxies like the Milky Way are expected to form at late times in traditio

54 and the stellar and dark matter halo of the Milky Way are expected to give rise to disequilibrium ph

55 etic fields, cosmic rays produced within the Milky Way arrive at Earth from random directions.

56 at a rate more than 1,000 times that of the Milky Way at redshift 2.6, within 2.5 Gyr of the Big Ban

57 of the Local Group of galaxies to which the Milky Way belongs are shedding light on some of the proc

58 The Milky Way bulge underwent a rapid chemical enrichment du

59 vations of extremely metal-poor stars in the Milky Way bulge, including one star with an iron abundan

60 with diffuse emission of neutrinos from the Milky Way but could also arise from a population of unre

61 asonably well constrained in the disk of the Milky Way but we have very little direct information on

62 neralogically distinct from that towards the Milky Way centre.

63 If these black holes existed in the Milky Way dark matter halo, they would cause long-timesc

64 many more low-mass stars than the IMF in the Milky Way disk, and was probably slightly steeper than t

65 ace density of neutral hydrogen in the outer Milky Way disk, demonstrating that the Galaxy is a non-a

66 ost of the dark matter subhalos orbiting the Milky Way do not host visible galaxies.

67 But the Milky Way does not seem to have suffered any major colli

68 Otherwise Carina, the eighth most luminous Milky Way dwarf, would be expected to inhabit a signific

69 al-poor globular clusters in the halo of the Milky Way formed in dwarf galaxies, as is commonly belie

70 ation may indicate that galaxies such as the Milky Way gain much of their mass by accretion rather th

71 rbiting a few relatively normal stars in our Milky Way Galaxy and also at the centers of some galaxie

72 DNA and the Milky Way galaxy are examples of such structures, whose

73 The Milky Way galaxy contains a large, spherical component w

74 ner tens of light-years at the center of the Milky Way Galaxy contains five principal components that

75 The Milky Way galaxy has several components, such as the bul

76 The centre of the Milky Way Galaxy hosts a black hole with a solar mass of

77 stars in the central few light years of our Milky Way Galaxy indicate the presence of a dark object

78 rvations of stellar globular clusters in the Milky Way Galaxy, combined with revised ranges of parame

79 During the lifetime of our Milky Way galaxy, there have been something like 100 mil

80 kelvin interstellar medium component in the Milky Way Galaxy.

81 mmon in much older supernova remnants in the Milky Way Galaxy.

82 ation events thought to originate beyond the Milky Way galaxy.

83 ce of two flat-spectrum radio sources in the Milky Way globular cluster M22, and we argue that these

84 (>10(3)M((.)) pc(-)(2)), exceeding those of Milky Way globular clusters and young star clusters in n

85 other star ('black-hole/X-ray binaries') in Milky Way globular clusters, even though many neutron-st

86 e associated constraints on the shape of the Milky Way gravitational potential, treating the Sgr impa

87 dies of trends in chemical abundances in old Milky Way halo stars suggested that these elements are p

88 idence of the 3.5-keV line emission from the Milky Way halo.

89 ludes the dynamical effect of the LMC on the Milky Way halo.

90 the past and contributed their stars to the Milky Way halo.

91 ld in the central few hundred parsecs of the Milky Way has a dipolar geometry and is substantially st

92 The Milky Way has at least twenty-three known satellite gala

93 e velocities of stars near the centre of the Milky Way have provided the strongest evidence for the p

94 ystem is in almost all aspects comparable to Milky Way high-mass YSOs accreting gas from a Keplerian

95 The central 0.1 parsecs of the Milky Way host a supermassive black hole identified with

96 The centre of the Milky Way hosts several high-energy processes that have

97 We constructed a map of the Milky Way in three dimensions, based on the positions an

98 and scintillation from plasma screens in the Milky Way interstellar medium (ISM).

99 The Milky Way is a barred spiral galaxy, with physical prope

100 Like many galaxies of its size, the Milky Way is a disk with prominent spiral arms rooted in

101 Most of the matter in the Milky Way is invisible to astronomers.

102 be resolved by scintillating screens in the Milky Way ISM and will suppress the observed scintillati

103 Hubble's measurement of a galaxy beyond the Milky Way led to the discovery of cosmic expansion.

104 Little is known about the portion of the Milky Way lying beyond the Galactic center at distances

105 s the stellar mass, and by proxy (assuming a Milky Way molecular gas-to-dust ratio) 0.01 times the st

106 rate integrated over the entire disk of the Milky Way of approximately 1 solar mass per year can sol

107 xy have shaped the observed structure of the Milky Way on a variety of larger scales(1).

108 uter haloes of massive galaxies, such as the Milky Way or Andromeda.

109 dium pervading an extended corona around the Milky Way or the Local Group.

110 result demonstrates that the faintest of the Milky Way satellites are the most dark-matter-dominated

111 t been found in the chemical compositions of Milky Way stars.

112 The Milky Way Study enrolled 49 children (mean SD age: 5.2 0

113 Models of the chemical evolution of the Milky Way suggest that the observed abundances of elemen

114 und star clusters (globular clusters) in the Milky Way suggests that efficiencies were higher when th

115 we report simulations of the response of the Milky Way to the infall of the Sagittarius dwarf galaxy

116 The Milky Way underwent significant transformations in its e

117 city is approximately one-thousand times the Milky Way value.

118 lar gas is also low, about 3 per cent of the Milky Way value.

119 e times, progenitors of galaxies such as the Milky Way were about 10,000 times less massive.

120 a damped sinusoidal wave on the plane of the Milky Way with an average period of about 2 kiloparsecs

121 drogen content of luminous galaxies like the Milky Way within 100 million years.

122 lows us to constrain the warped shape of the Milky Way's disk.

123 dark matter halos and the properties of the Milky Way's dwarf galaxy satellites.

124 nces have been seen in selected stars in the Milky Way's halo and in two quasar absorption systems at

125 Our results show that the Milky Way's morphology is not purely secular in origin a

126 3.6(-2.3)(+3.8) x 10(8) Msun for one of the Milky Way's satellites: Carina.

127 urrent cosmological models indicate that the Milky Way's stellar halo was assembled from many smaller

128 o bursts) have been detected from beyond the Milky Way(1).

129 ture in their central regions, including our Milky Way(1,2).

130 4 x 10(6) solar masses at the centre of the Milky Way(1,2).

131 s that do not resemble those observed in the Milky Way(1-3) and whose origin is debated(4-6).

132 e two most massive satellite galaxies of the Milky Way(1-4).

133 ise to disequilibrium phenomena in the outer Milky Way(1-7).

134 9) that is bringing in metal-poor gas to the Milky Way(10).

135 ri, the most massive globular cluster of the Milky Way(3-5).

136 s-2112 can be considered a progenitor of the Milky Way(7-9), in terms of both structure and mass-asse

137 ole in a high-metallicity system (within the Milky Way) constrains wind mass loss from massive stars.

138 r for star formation in galaxies such as our Milky Way) remains unclear.

139 ts at the centres of galaxies similar to the Milky Way).

140 at a rate more than 2,000 times that of the Milky Way, a rate among the highest observed at any epoc

141 formed white dwarf stars in the halo of the Milky Way, and a separate analysis of archival data in t

142 Observations of globular clusters in the Milky Way, and a wide variety of other galaxies, have fo

143 All the known MYSO systems are in the Milky Way, and all are embedded in their natal material.

144 y four such maximal sources are known in the Milky Way, and the absorption of soft X-rays in the inte

145 star indicate that it is in the halo of the Milky Way, and the density of such objects implied by th

146 from a scattering screen located within the Milky Way, and the second originating from its host gala

147 hemically primitive stars in the halo of the Milky Way, because these objects retain the nucleosynthe

148 In the Milky Way, high-mass stars form in the dense cores of in

149 Observations of supernova remnants in the Milky Way, however, have hitherto revealed only 10(-7)-1

150 on of luminous and nonluminous matter in the Milky Way, in galaxies, and in galaxy clusters.

151 ared and X-ray emission at the centre of the Milky Way, is the closest example of this phenomenon, wi

152 supermassive black hole at the center of the Milky Way, known as Sagittarius A* (Sgr A*), may have af

153 t active and heavily processed region of the Milky Way, so it can be used as a stringent test for the

154 Unlike spiral galaxies such as the Milky Way, the majority of the stars in massive elliptic

155 of low-metallicity stars in the halo of the Milky Way, to determine the U/Th production ratio very p

156 ns of the Magellanic Clouds falling onto the Milky Way, we can reproduce the Magellanic Stream and it

157 sing on the largest known superbubble in the Milky Way, we identify groups of O-B2 stars at its perip

158 ith those measured from sources of CH in the Milky Way, we test the hypothesis that fundamental const

159 only through the interstellar medium of the Milky Way-indicate extragalactic origins and imply contr

160 absent beyond z = 1.5 in the progenitors of Milky Way-like galaxies(5,6).

161 ormation predict many more subhalos around a Milky Way-like galaxy than the number of observed satell

162 II, a high-resolution N-body simulation of a Milky Way-sized galaxy, to investigate the phase-space s

163 relatively rare in galaxies such as our own Milky Way.

164 be emitted by dark matter in the halo of the Milky Way.

165 probe the chemical enrichment history of the Milky Way.

166 greater than 30, in the early history of the Milky Way.

167 ss was temporarily the brightest star in the Milky Way.

168 be a nearby low-mass star in the disk of the Milky Way.

169 much of the 'dark matter' in the halo of the Milky Way.

170 e cloud that is falling into the disk of the Milky Way.

171 alaxies and in the extreme outer disk of the Milky Way.

172 ond-duration events detected from beyond the Milky Way.

173 one of the fastest superluminal jets in the Milky Way.

174 he closest massive satellite galaxies of the Milky Way.

175 c clouds are on their first orbit around the Milky Way.

176 nsitive probe of the mass of the LMC and the Milky Way.

177 at are similar to population II stars in the Milky Way.

178 es and column densities for CO clouds in the Milky Way.

179 s 50 per cent, tenfold that of clouds in the Milky Way.

180 n found in the outer regions ('halo') of the Milky Way.

181 ith a dust-to-gas ratio close to that of the Milky Way.

182 )-10(10 )Msun at the time they fell into the Milky Way.

183 factor of 100 greater than that seen in the Milky Way.

184 eir routes to the band of stars known as the Milky Way.

185 ittarius galaxy, which is a satellite of the Milky Way.

186 ar to that of the Sagittarius dwarf near the Milky Way.

187 al galaxies may not have the same IMF as the Milky Way.

188 sive black hole, SgrA*, at the centre of the Milky Way.

189 one of the most massive binary stars in the Milky Way.

190 th a spheroidal component, including our own Milky Way.

191 titude arcs observed in the same area of the Milky Way.

192 ld Phoenix stellar stream in the halo of the Milky Way.

193 population of 'dark dwarfs' should orbit the Milky Way: halos devoid of stars and yet more massive th

194 Our optical observations of its Milky-Way-sized, metal-rich host galaxy(10-12) show a ba