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 There is observational evidence at galactic and circumnuclear scales(4) that gas flows inwa

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 ity measurements taken over two years of the Galactic B-type star, LB-1.

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

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

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

9 be tidally interacting with the supermassive Galactic black hole, possibly enhancing its accretion ac

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

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

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

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

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

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

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

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

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

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

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

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

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

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

24 In this study, we used observations of the Galactic Center star S0-2 to test this prediction.

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

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

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

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

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

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

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

32 ose that these structures, which we term the Galactic Centre 'chimneys', constitute exhaust channels

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

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

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

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

37 The Galactic Centre contains a supermassive black hole with

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

39 On scales of 15 parsecs, the Galactic Centre has bipolar lobes that can be seen in bo

40 Fermi bubble' features(4), implying that our Galactic Centre has had a period of active energy releas

41 although the levels of star formation in the Galactic Centre have been approximately constant over th

42 The Galactic Centre hosts a puzzling stellar population in i

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

44 The Galactic Centre is the most active and heavily processed

45 arsecs), radio astronomers have observed the Galactic Centre lobe, an apparent bubble of emission see

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

47 below the plane, which appear to connect the Galactic Centre region to the Fermi bubbles.

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

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

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

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

52 r to the increased cosmic-ray density in the Galactic Centre, and is in turn the principal source of

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

54 i-continuous train of episodic events at the Galactic Centre, are transported from the central few pa

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

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

57 ity from the super-massive black hole at the Galactic Centre, which is coincident with the radio sour

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

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

60 tic plane and apparently associated with the Galactic Centre.

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

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

63 indicative of energy injection from near the Galactic Centre.

64 plying creation by an energetic event in the Galactic Centre.

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

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

67 warf galaxy Reticulum II(14), as well as the Galactic chemical enrichment of europium relative to iro

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

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

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

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

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

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

74 ly to endure higher levels of radiation from galactic cosmic radiation (GCR) and the possibility of a

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

94 understanding of the oncogenic potential of galactic cosmic rays.

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

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

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

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

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

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

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

102 ve stars; these are concentrated in the thin Galactic disk where the Sun resides.

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

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

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

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

107 presumably active galaxies seen through the Galactic disk.

108 nment that differs markedly from that of the Galactic disk.

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

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

111 ofiles of Halpha and ultraviolet emission in galactic disks.

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

113 edback-driven life cycles that vary with the galactic environment and collectively define how galaxie

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

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

116 llapse supernovae should be found in similar galactic environments.

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

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

119 probably existed, but were destroyed during Galactic evolution.

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

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

122 The recent detection of a Galactic fast radio burst in association with a soft gam

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

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

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

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

127 Models have shown that rapid collapse of pre-galactic gas (with a mass infall rate above some critica

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

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

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

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

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

133 The dominant gaseous structure in the Galactic halo is the Magellanic Stream.

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

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

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

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

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

139 We find that pre-galactic haloes and their associated gas clouds that are

140 s imply predominantly diffuse gas in massive galactic halos, even those hosting active supermassive b

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

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

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

144 ent bubble of emission seen only at positive Galactic latitudes(7,8), but again indicative of energy

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

146 n the ring-like central molecular zone(4) at Galactic longitude |l| < 0.7 degrees and latitude |b| <

147 a millisecond-duration radio burst from the Galactic magnetar SGR 1935+2154, with a fluence of 1.5 +

148 Recently, the Galactic magnetar SRG 1935+2154 entered an active phase

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

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

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

152 m on matter in extreme conditions, and probe galactic magnetic fields.

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

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

155 wed by gravitational collapse into blocks of galactic mass.

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

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

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

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

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

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

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

163 o the supermassive black hole in some active galactic nuclei (AGN) drives relativistic jets of plasma

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

190 ass and accretion properties, typical active galactic nuclei with higher-mass black holes can be expe

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

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

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

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

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

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

197 y quiescent in the broader context of active galactic nuclei, X-ray observations have provided eviden

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

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

200 ximately 100 times higher than bright active galactic nuclei.

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

202 Blazars are the most extreme active galactic nuclei.

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

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

205 despite strong feedback from stars or active galactic nuclei.

206 -population of mergers originate from active galactic nuclei.

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

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

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

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

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

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

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

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

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

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

217 ensing involve multiple imaging of an active galactic nucleus.

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

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

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

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

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

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

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

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

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

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

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

229 430 parsecs), extending above and below the Galactic plane and apparently associated with the Galact

230 hat the edges of these cavities close to the Galactic plane are bright in X-rays(4-6).

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

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

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

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

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

236 m of TYC 2597-735-1 and its proximity to the Galactic plane suggest that it is an old star, yet it ha

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

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

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

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

241 of extinction by interstellar dust along the Galactic plane.

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

243 gas and dust, tilted about 20 degrees to the Galactic plane.

244 high extinction in visible light within the Galactic plane.

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

246 om the centre, directed perpendicular to the Galactic plane.

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

248 ellar magnetic field thought to parallel the galactic plane.

249 with its axis oriented perpendicular to the Galactic plane.

250 ion of bright unidentified sources along the Galactic plane.

251 0 unidentified point sources found along the Galactic plane.

252 populate huge cavities on both sides of the Galactic plane.

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

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

255 a mass ratio q of 0.7 to 0.8)(5), the known Galactic population of merging double neutron-star syste

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

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

258 environment before they merge into the older Galactic population.

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

260 we constrain the rate of occurrence of their Galactic production sites to within about 1-100 per mill

261 ulsar-previously the source of the brightest Galactic radio bursts observed on similar timescales(7).

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

263 among patients with acute heart failure: the GALACTIC randomized clinical trial.

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

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

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

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

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

269 d, in contrast to their tight correlation on galactic scales(5).

270 ble of rapidly terminating star formation on galactic scales.

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

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

288 tudying the brighter and much faster varying Galactic systems.

289 xternal perturbers such as passing stars and Galactic tides.

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

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

292 difference between B-DNA and P-DNA, and the galactic virial mass.

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

294 er and energy from the disk in the form of a galactic wind(2).

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

296 Theory points to galactic winds as the primary source of the enriched and

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

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

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

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

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