ライフサイエンスコーパス: galactic

1 high Galactic latitudes after the effects of Galactic absorption are considered.

2 development of structure in the universe on galactic and larger scales is the challenge that drives

3 However, recent analyses of structure on galactic and subgalactic scales have suggested discrepan

4 Two ring-like wrappings emerge towards the Galactic anti-Centre in our model that are reminiscent o

5 sars are thought to be scaled-up versions of Galactic black hole binaries, powered by accretion onto

6 ptical, x-ray, and radio observations of the Galactic black hole system V404 Cygni, showing a rapid s

7 ether active galactic nuclei (AGN) vary like Galactic black hole systems when appropriately scaled up

8 ove their Eddington limit, analogous to some Galactic black holes at peak luminosity.

9 nd in the X-ray variations from both AGN and Galactic black holes, but whether it is physically meani

10 So AGN really are just scaled-up Galactic black holes.

11 laxies, recent studies claimed that the true Galactic building blocks must have been vastly different

12 The gas is concentrated around the galactic bulge and disk on scales of a few kiloparsec.

13 erved against the dense stellar field of the Galactic bulge presents ideal conditions for such observ

14 erformed in a rich stellar field towards the Galactic bulge.

15 in the Galaxy, and transport of stars to the galactic center also appears unlikely during their lifet

16 he portion of the Milky Way lying beyond the Galactic center at distances of more than 9 kiloparsec f

17 Keck Observatory has been used to image the galactic center at the highest angular resolution possib

18 In reconstructing its trajectory, the Galactic center becomes very unlikely as an origin, whic

19 he cosmic IR and microwave background and in galactic center dimming between 3 and 9 micrometers.

20 parsec of the supermassive black hole in the galactic center is challenging for theories of star form

21 ed the intrinsic size of Sagittarius A*, the Galactic center radio source associated with a supermass

22 lve the linearly polarized emission from the Galactic Center supermassive black hole, Sagittarius A*.

23 y interactions between the components at the Galactic center will improve our understanding of the na

24 at large distances ( 1 kiloparsec) from the galactic center.

25 mplex life within a few kiloparsecs from the galactic center.

26 oxide (CH3CHCH2O), in absorption toward the Galactic center.

27 0,000-year-old Sagittarius A East SNR at the Galactic center.

28 ither stalled or dramatically accelerated by galactic-center environments and that higher-cadence and

29 latively unprocessed metal-poor gas into the Galactic Centre (at the rate inferred by Wakker).

30 , chemical evolution models predict that its Galactic Centre abundance relative to hydrogen is D/H =

31 relative strengths of these DIBs towards the Galactic Centre and the Cygnus OB2 diffuse cloud are con

32 t magnetic field was recently found near the Galactic Centre black hole.

33 We conclude that the observed Galactic Centre deuterium is cosmological, with an abund

34 The Galactic Centre hosts a puzzling stellar population in i

35 haracterization of the magnetic field at the Galactic Centre is important because it can affect the o

36 The Galactic Centre is the most active and heavily processed

37 ately wide-field monitoring programme of the Galactic Centre region at 0.33 GHz.

38 e that they originate almost entirely in the Galactic Centre region, a considerably warmer and harshe

39 emission is more sharply peaked towards the Galactic Centre than is the surface brightness of the so

40 sults of a large-scale imaging survey of the Galactic Centre that resolves these components.

41 ccount for the funnelling of gas towards the galactic centre to feed the black hole.

42 Our model implies that planets form in the Galactic centre, and that tidal debris from proto-planet

43 If located in or near the Galactic Centre, its brightness temperature (approximate

44 r bulge stars are on tight orbits around the Galactic Centre, rather than being halo stars passing th

45 mately 20 faint sources appears north of the Galactic Centre, which is part of a broader class of fai

46 h-extinction sightlines towards stars in the Galactic Centre.

47 of gas onto a supermassive black hole at the Galactic Centre.

48 n a molecular cloud only 10 parsecs from the Galactic Centre.

49 formation, and cosmic-ray production in the Galactic Centre.

50 ight X-ray and optical/ultraviolet flares in galactic centres.

51 the interstellar medium (after allowing for Galactic chemical evolution), and indicates that the abs

52 of a few hundredfold for objects the size of galactic clusters a few megaparsecs in size.

53 a larger scale, initiating the formation of galactic clusters and still larger structures.

54 Ultimately structures larger than galactic clusters outran the diffusion of the gravitons

55 ations from those for dwarf galaxies through galactic clusters.

56 ents indicate the existence of an additional galactic component, to account for the light composition

57 iously reported bursts and, accounting for a Galactic contribution to the dispersion and using a mode

58 accretion phase, supermassive black holes in galactic cores are known to emit very high levels of ion

59 g galaxy, have long been sought as probes of galactic cores too distant to resolve with ordinary obse

60 mechanisms linked with either ultraviolet or galactic cosmic ray (GCR) effects on atmospheric particl

61 Cancer risk is an important concern for galactic cosmic ray (GCR) exposures, which consist of a

62 the geomagnetic field causes an increase in galactic cosmic ray (GCR) flux.

63 The small intensity gradient of Galactic cosmic ray helium indicates that either the gra

64 in the heliosheath or the local interstellar Galactic cosmic ray intensity is lower than expected.

65 in that there was a simultaneous increase in Galactic cosmic ray ions and electrons, anomalous cosmic

66 us cosmic rays', as well as to re-accelerate Galactic cosmic rays and low-energy particles from the i

67 f the absorbed dose and dose equivalent from galactic cosmic rays and solar energetic particles on th

68 IBEX ENAs at hundreds to thousands of eV and galactic cosmic rays at tens of TeV has wide-ranging imp

69 results from spallation reactions (in which Galactic cosmic rays break apart larger nuclei in the in

70 We report the spectra of galactic cosmic rays down to ~3 x 10(6) electron volts p

71 ly 10-megaelectron volt electrons, ACRs, and galactic cosmic rays have steadily increased since late

72 ess caused by variations in the intensity of galactic cosmic rays in the atmosphere.

73 We find that ions from Galactic cosmic rays increase the nucleation rate by one

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

75 bservatory support the idea that the bulk of galactic cosmic rays is accelerated in such remnants by

76 nizing HZE particles (high charge and energy galactic cosmic rays were observed, yielding an overall

77 other planets, astronauts will be exposed to galactic cosmic rays which are composed of heavy particl

78 alculations, to help determine the source of Galactic cosmic rays, and to date circumstellar grains.

79 understanding of the oncogenic potential of galactic cosmic rays.

80 electron volts per nucleon and an increasing galactic cosmic-ray electron intensity down to ~10 x 10(

81 The origin of Galactic cosmic-ray ions has remained an enigma for almo

82 It is thought that Galactic cosmic-ray nuclei are gradually accelerated to

83 The search for the origin(s) of Galactic cosmic-ray nuclei may be closing in on the long

84 nic Cloud (LMC) to determine the fraction of Galactic dark matter contained in massive compact halo o

85 As the Earth moves through the galactic dark matter halo, interactions with domain wall

86 ) Universe, the mass of dark matter within a galactic disk increases with disk radius, becoming appre

87 en wave propagating vertically away from the Galactic disk, driven by rotation of the magnetized circ

88 r impact event as a trivial influence on the Galactic disk.

89 presumably active galaxies seen through the Galactic disk.

90 l existence of million-degree gas within the Galactic disk.

91 bound from one another and spread across the Galactic disk.

92 ive their births, instead dispersing to form galactic disks or bulges.

93 extend for dozens of kiloparsecs beyond the galactic disks-host an active nucleus, and two of them a

94 ofiles of Halpha and ultraviolet emission in galactic disks.

95 rved galactic rotation curves and explaining galactic dynamics without the need of dark matter.

96 Our results indicate that the external galactic environment strongly imprints the heliosphere.

97 axies, and that star formation rates in some galactic environments may have been systematically under

98 llapse supernovae should be found in similar galactic environments.

99 that travels at a velocity greater than the Galactic escape velocity and whose peculiar atmosphere i

100 H to constrain the more flexible stellar and galactic evolution models (although the question of pote

101 their primordial values by using stellar and galactic evolution theories.

102 ning to provide a quantitative diagnostic of galactic evolution, and of the epoch of formation of the

103 he door to alternative probes of stellar and galactic evolution, cosmology and fundamental physics.

104 thetic processes in stars and the effects of Galactic evolution.

105 was depleted, or as an isotopic 'memory' of Galactic evolution.

106 Our results suggest that galactic feedback, coupled jointly to turbulence and gra

107 ent can be derived for large numbers of cool Galactic field stars.

108 These patterns constitute a "galactic" form of prehistoric urbanism, sharing features

109 We speculate that most unidentified Galactic gamma-ray sources associated with star-forming

110 Chandra has now observed over 80 Galactic globular clusters, and these observations have

111 trometric satellite on distance estimates of galactic globular clusters.

112 the missing baryon matter predicted for the galactic halo according to the standard cosmology.

113 ir distances are key for placing them in the galactic halo and unraveling their role.

114 the sensitivity required to detect directly galactic halo dark matter through their interactions wit

115 ations, and represents a direct detection of galactic halo dark matter.

116 and 50 per cent of the baryonic mass of the Galactic halo is in the form of MACHOs, but removing the

117 ur times that measured in the atmospheres of Galactic halo stars.

118 recent abundance measurements of metal-poor galactic halo stars.

119 d the metals found in dwarf galaxies and the Galactic halo.

120 investigate the phase-space structure of the galactic halo.

121 ucture even in the very inner regions of the Galactic halo.

122 ment and similarity to the progenitor of the Galactic helium nova V445 Puppis suggest that SN 2012Z w

123 losest and most easily studied sample of the Galactic interstellar medium, an understanding of which

124 point sources is comparable to that at high Galactic latitudes after the effects of Galactic absorpt

125 millisecond flashes, found primarily at high Galactic latitudes, with dispersion measures much larger

126 cted to contain cold nonsolar plasma and the galactic magnetic field.

127 shift of the magnetic field, the strength of galactic magnetic fields at redshifts z > 0 remains unce

128 The standard model for the origin of galactic magnetic fields is through the amplification of

129 e >/= 10(6) times more luminous than typical galactic maser sources.

130 he formation of galaxies, down to the lowest galactic mass scales.

131 wed by gravitational collapse into blocks of galactic mass.

132 ly of Li from evolved stellar objects to the Galactic medium has hitherto been found.

133 ary supermassive black holes are produced by galactic mergers as the black holes from the two galaxie

134 r massive black holes, through accretion and galactic merging.

135 ion by factors of 4 to 15 relative to smooth galactic models.

136 Recent observations have revealed massive galactic molecular outflows that may have the physical c

137 e hot gas is a product of stellar and active galactic nuclear feedback--the least understood part in

138 ivistic jets of material ejected from active galactic nuclei (AGN) and the 'microquasars' located in

139 formed stars at remarkable rates and active galactic nuclei (AGN) shone brightly as a result of accr

140 A long-standing question is whether active galactic nuclei (AGN) vary like Galactic black hole syst

141 elativistic plasma jets found in many active galactic nuclei (AGN).

142 intergalactic distances as quasars or active galactic nuclei (AGN).

143 , and at the center of some galaxies [active galactic nuclei (AGN)].

144 peaks of the broad emission lines in active galactic nuclei (AGNs) are significantly blueshifted or

145 anding of the majority populations of active galactic nuclei (AGNs) over most of the history of the u

146 other astrophysical sources, such as active galactic nuclei and proto-stars.

147 Active galactic nuclei and quasars are thought to be scaled-up

148 ome unification of different types of active galactic nuclei and quasi-stellar objects (QSOs).

149 rvational evidence that outflows from active galactic nuclei are launched from the disks.

150 Powerful winds driven by active galactic nuclei are often thought to affect the evolutio

151 Massive outflows driven by active galactic nuclei are widely recognized to have a key role

152 between binary black hole mergers and active galactic nuclei as hosts, even if only a sub-population

153 arbour supermassive black holes, which power galactic nuclei by converting the gravitational energy o

154 monstrate that their association with active galactic nuclei can be made through a statistical spatia

155 a survey of ultraviolet emission from active galactic nuclei decreases significantly when the vector

156 Approximately 10% of active galactic nuclei exhibit relativistic jets, which are pow

157 the intracluster gas, supernovae, and Active Galactic Nuclei feedback) likely contribute to this expa

158 has a crucial role as one of only two active galactic nuclei for which black hole mass measurements b

159 l improve our understanding of the nature of galactic nuclei in general, and will provide us with a b

160 In at least some cases, input from active galactic nuclei is dynamically important, so pure stella

161 The properties of lensed active galactic nuclei make them promising systems for astrophy

162 unds for believing that outflows from active galactic nuclei originate as disk winds, observational v

163 er photometry of eight x-ray-absorbed active galactic nuclei that have luminosities and redshifts cha

164 s the basis of the quasar feedback in active galactic nuclei that lack powerful radio jets (such jets

165 ormation, the evolution of star clusters and galactic nuclei, and the formation of galaxies and clust

166 poch of star formation in radio-quiet active galactic nuclei, similar to that seen in radio galaxies.

167 e component has been observed in many active galactic nuclei, there have hitherto been no significant

168 ve black holes (SMBHs) and star formation in galactic nuclei, uncertainties exist in our understandin

169 Active galactic nuclei, which are powered by long-term accretio

170 Blazars are active galactic nuclei, which are powerful sources of radiation

171 s with rare host galaxy types-such as active galactic nuclei-can nevertheless be identified statistic

172 in the form of long-term accretion in active galactic nuclei.

173 ximately 100 times higher than bright active galactic nuclei.

174 -population of mergers originate from active galactic nuclei.

175 s, mimic the behaviour of quasars and active galactic nuclei.

176 Blazars are the most extreme active galactic nuclei.

177 imation, and propagation of jets from active galactic nuclei.

178 an indicated by estimates based on models of galactic nuclei.

179 k-hole binaries are expected to be common in galactic nuclei.

180 despite strong feedback from stars or active galactic nuclei.

181 unresolved discrete sources, such as active galactic nuclei; the remainder appears to constitute a t

182 clusters of galaxies and the role of active galactic nucleus (AGN) heating.

183 gas flow in the X-ray spectrum of the active galactic nucleus IRAS 13224-3809, at 0.236 +/- 0.006 tim

184 The active galactic nucleus is responsible for about 80 per cent of

185 The brightness of an active galactic nucleus is set by the gas falling onto it from

186 which contributes, together with the active galactic nucleus it harbours, to its high infrared lumin

187 o be co-located with a low-luminosity active galactic nucleus or a previously unknown type of extraga

188 Many of these galaxies contain an active galactic nucleus powered by accretion of gas onto a supe

189 infrared luminosities result from the active galactic nucleus, from bursts of massive star formation

190 ensing involve multiple imaging of an active galactic nucleus.

191 to a highly energetic phenomenon: an active galactic nucleus.

192 is regulated by the brightness of the active galactic nucleus; this feedback loop is the process by w

193 essential to understanding whether they have galactic or extragalactic sources.

194 of >10(3) on 25 August 2012, while those of galactic origin (cosmic rays) increased by 9.3% at the s

195 onsistent with the fast radio burst having a Galactic origin or its source being located within a pro

196 m the interstellar plasma, which is of local Galactic origin.

197 guously reveal star formation occurring in a galactic outflow at a redshift of 0.0448.

198 evidence for star formation occurring within galactic outflows is still missing.

199 tar formation may also be occurring in other galactic outflows, but may have been missed by previous

200 High-velocity galactic outflows, driven by intense bursts of star form

201 will survive exposure to levels of solar and galactic particle radiation encountered during a flight

202 The Galactic plane is a strong emitter of hard x-rays (2 to

203 use, which indicates omnipresence within the Galactic plane of a hot plasma, the energy density of wh

204 Molecular gas has been detected outside the galactic plane of the archetypal starburst galaxy M82 (r

205 the field was thought to be parallel to the Galactic plane or inclined by 38-60 degrees or 60-90 deg

206 rried out the deepest hard x-ray survey of a Galactic plane region that is devoid of known x-ray poin

207 nresolved X-ray emission extending along the Galactic plane, is dominated by accreting white dwarf sy

208 Despite having a similar distribution in the Galactic plane, the DIB 8620 carrier has a significantly

209 avitationally bound ensemble of stars in the Galactic plane--are typically only about 0.01 to 0.05 ov

210 high extinction in visible light within the Galactic plane.

211 is at an angle of about 30 degrees from the Galactic plane.

212 roximately 60 degrees to 90 degrees from the galactic plane.

213 ellar magnetic field thought to parallel the galactic plane.

214 with its axis oriented perpendicular to the Galactic plane.

215 ion of bright unidentified sources along the Galactic plane.

216 0 unidentified point sources found along the Galactic plane.

217 ately 40 per cent of the 1/4-keV flux in the Galactic plane.

218 of extinction by interstellar dust along the Galactic plane.

219 transients all more than 40 degrees from the Galactic plane.

220 a "pencil-beam" geometry of galaxies at the galactic poles indicated strong clustering, with a provo

221 lanets in nearly coplanar orbits, yielding a Galactic population of at least several million.

222 sent, their ephemeral nature implies a total Galactic population significantly exceeding that of the

223 stage in the evolution of the oldest stellar galactic population, occurring either as field halo star

224 environment before they merge into the older Galactic population.

225 Our analysis of the galactic position and velocity relative to the cluster s

226 local standard of rest frame) are within one galactic radius of the Sun and have enough mass to maint

227 ults appear to favor rapid merging at modest galactic redshifts.

228 The Galactic ridge hard x-ray emission is diffuse, which ind

229 raction follows a 1/R law, matching observed galactic rotation curves and explaining galactic dynamic

230 an active nucleus, and two of them also have galactic-scale ionization cones.

231 Observations reveal feedback in the form of galactic-scale outflows of gas in galaxies with high rat

232 ble of rapidly terminating star formation on galactic scales.

233 Recent surveys show that virtually all galactic sites of high-mass star formation have similarl

234 tars begin to form relatively quickly in sub-galactic-sized building blocks called haloes which are s

235 of gamma-rays during a giant flare from the Galactic soft gamma-ray repeater, SGR 1806-20, reopened

236 and mixing, and that there is no significant Galactic source of deuterium.

237 ion measures much larger than expected for a Galactic source.

238 X-ray and radio emission are coupled in such Galactic sources; the radio emission originates in a rel

239 These measurements allow us to shed light on Galactic spiral structure by locating the Scutum-Centaur

240 e vector is transformed to the frames of the Galactic Standard of Rest and the Local Group of galaxie

241 velocity clouds (iHVCs) in the foreground of galactic stars.

242 ng differences of a factor of up to three in galactic stellar mass.

243 uires distinct stellar origins: steady-state galactic stellar nucleosynthesis for (182)Hf and late-st

244 have a typical set of properties not seen in Galactic stellar-mass black holes.

245 y have a similarly important role in shaping galactic structure.

246 as it is crucial to our understanding of how galactic structures form and evolve.

247 hur from the gas phase, and with the average Galactic sulphur/silicon abundance ratio.

248 Modeling of the x-ray spectra of the Galactic superluminal jet sources GRS 1915+105 and GRO J

249 y 2-4M(o) of cold dust in the youngest known Galactic supernova remnant, Cassiopeia A.

250 tudying the brighter and much faster varying Galactic systems.

251 xternal perturbers such as passing stars and Galactic tides.

252 Its gas-to-dust ratio is lower than the Galactic value, which we attribute to dust enrichment by

253 agate through the satellite constellation at galactic velocities 300 km s(-1).

254 s overpressurized and drives M82's prominent galactic wind into the intergalactic medium.

255 Although ionized galactic winds are readily observable, most of the expel

256 We show that the galactic winds sustain turbulence in the 10-kiloparsec-s

257 riginate in dense shock waves powered by hot galactic winds.

258 se is frequently attributed to the effect of galactic winds.

259 ndard thin disk accretion that powers bright Galactic X-ray binaries, or both.

260 Soft-gamma-ray repeaters (SGRs) are galactic X-ray stars that emit numerous short-duration (