ライフサイエンスコーパス: baryon

1 and including all of the so-called 'missing baryons'.

2 n", which plays the role of a quintessential baryon.

3 observations should be able to detect these baryons.

4 inties, with the mass density of the missing baryons.

5 itive measure of the cosmological density of baryons.

6 he cosmic microwave background indicate that baryons account for 5 per cent of the Universe's total e

7 ized by a flat power spectrum with prominent baryon acoustic oscillations.

8 previous claims of the detection of warm-hot baryons along the line of sight to distant blazars and o

9 undergo fusion to produce the doubly charmed baryon and a neutron n (), resulting in an energy releas

10 atter profiles, because low-angular-momentum baryons and dark matter sink to the centres of galaxies

11 f the cosmic matter content of the universe (baryons and dark matter).

12 Finding the missing baryons and thereby producing a complete inventory of po

13 eviewed and demonstrate that the bulk of the baryons are dark and also that the bulk of the matter in

14 This suggests that the baryons are not missing, they are simply located in clus

15 The majority of baryons are still missing and are expected to be hidden

16 an by the spin of the black hole, and if the baryons can be accelerated to relativistic speeds, the j

17 proaches: a standard QED framework and heavy baryon chiral perturbation theory (an effective theory o

18 cent cosmological measurements indicate that baryons comprise about four per cent of the total mass-e

19 ravitational potential of a cluster, and the baryons confined by this potential radiate X-rays with a

20 h as a very large-scale inhomogeneity in the baryon content of the universe.

21 The baryon deficiency is typically observed in the central r

22 The BBN constraints on the cosmological baryon density are reviewed and demonstrate that the bul

23 e density, a density consistent with the low baryon density in the universe.

24 This reduced upper limit for the baryon density relieves any conflict with standard Big B

25 We calculate a baryon density that is 5% of the critical density requir

26 very robust conclusion of BBN regarding the baryon density.

27 ur own epoch (z < 2), however, the number of baryons detected add up to just over half (approximately

28 also in agreement with the actual number of baryons detected at early times (redshifts z > 2).

29 The number of baryons detected in the low-redshift (z < 1) Universe is

30 The primordial density of all baryons determined from the 3He data is in excellent agr

31 In a baryon-dominated jet only weak, tangled fields generated

32 high-redshift galaxy population was strongly baryon-dominated, with dark matter playing a smaller par

33 e local Universe, the census of all observed baryons falls short of this estimate by a factor of two.

34 ous results, our measurements of the cluster baryon fraction are consistent with the expected univers

35 mass in clusters to extrapolate the measured baryon fraction as a function of radius and as a functio

36 The apparent baryon fraction exceeds the cosmic mean at larger radii,

37 Although this implied baryon fraction may be larger than in the local Universe

38 We find that the baryon fraction reaches the cosmic value near the virial

39 parameters including mass, angular momentum, baryon fraction, age and size, as well as by the acciden

40 wer baryons (gas plus stars) than the cosmic baryon fraction.

41 , inferred from ancillary data, suggest high baryon fractions in the inner, star-forming regions of t

42 ers and continuous infall of dark matter and baryons from the cluster periphery produce long-lived "s

43 of galaxies suggest that they contain fewer baryons (gas plus stars) than the cosmic baryon fraction

44 ogical simulations indicate that the missing baryons have not condensed into virialized haloes, but r

45 or to estimate the total amount of warm-hot baryons in a representative volume of the Universe.

46 Most of the baryons in galaxy clusters reside between the galaxies i

47 tial evidence for the presence or absence of baryons in jets, and the only system in which they have

48 Qualitatively, the observations suggest that baryons in the early (high-redshift) Universe efficientl

49 measurement of the cosmic density of ionized baryons in the intergalactic medium of OmegaIGM = 4.9 +/

50 light, thereby establishing the presence of baryons in the jet.

51 for at most approximately 25 per cent of the baryons in the Universe.

52 The total mass of baryons in this medium is estimated to be up to approxim

53 ity of a previously undetected population of baryons, in the warm-hot phase of the intergalactic medi

54 ment, exothermic reaction in which two heavy baryons (Lambdac) undergo fusion to produce the doubly c

55 may not account for the bulk of the missing baryon matter predicted for the galactic halo according

56 show that up to two-thirds of the 'missing' baryons may have escaped detection because of their high

57 Here we show that the baryons may not actually be missing from clusters, but r

58 rmic nature of the fusion of two heavy-quark baryons might manifest itself.

59 provides the best estimate of the density of baryons (omegaB) in the Universe.

60 tes assume that the gravitational effects of baryons on dark matter substructure are small.).

61 tter is proposed in addition to the observed baryons plus radiation and thus the proposed density of

62 minor fraction of the energy is released in baryon-poor outflows from a differentially rotating open

63 We associate the energy emitted in baryon-poor outflows with gamma-ray bursts.

64 This "missing baryon" puzzle is especially surprising for the most mas

65 ter virial radius is gas-rich (with a gas-to-baryon ratio greater than 1%).

66 s are embedded in a 'cosmic web', where most baryons reside as rarefied and highly ionized gas.

67 rse in which a large fraction of the missing baryons reside in the filaments of the cosmic web.

68 hoto-ionized gas make up at most half of the baryons that are expected to be present in the universe.

69 luxes implies a mean cosmological density of baryons that is consistent with Big Bang nucleosynthesis

70 the lower values implying a high density of baryons that may be difficult to reconcile with both est

71 ters (including the density of matter and of baryons, the initial mass fluctuations amplitude and its

72 sis (BBN) depend only on the cosmic ratio of baryons to photons, a quantity inferred from observation

73 recent discovery of the first doubly charmed baryon , which contains two charm quarks (c) and one up