References

1

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2

Albrecht, A., & Stebbins, A. 1992, Phys. Rev. Lett., 68, 2121. This paper computes the density power spectrum in a cosmic string seeded cold dark matter cosmology.

3

Alcock, C., et al. 1995, ApJ, 445, 133. This paper presents an analysis of the first year microlensing data from the MACHO collaboration. See Alcock's article in this book for a more recent review.

4

Abplanalp, M., et al. 1994, cond-mat preprint 9411072. A report on recent progress made by the Bern group in developing superconducting grain detectors.

5

Athanassopoulos, C., et al. 1995, Phys. Rev. Lett., 75, 2650. A description of recent results from the Los Alamos experiment suggesting evidence for neutrino oscillations. See also, the article by Hill.

6

Awaki, H., Mushotzky, R., Tsuru, T., Fabian, A., Fukazawa, Y., Loewenstein, M., Makishima, K., Matsumoto, H., Matsushita, K., & Mimara, T. 1994, PASJ, 46, 65. ASCA, the US-Japanese X-ray satellite, has enabled measurements of X-ray temperature profiles in galaxies. This paper discusses the gas and dark matter density distributions in elliptical galaxies as well as the chemical composition of the cluster gas. They conclude that elliptical galaxies are dark matter dominated at large radii.

7

Bahcall, J. N., Flynn, C., Gould, A., & Kirhakos, S. 19944, ApJ, 435, L51.

8

Bahcall, N., & Cen, R. 1994, ApJ, 426, L15. The formation of clusters and large scale structure in a low CDM dominated universe.

9

Bahcall, N., Lubin, L. M. & Dorman, V. 1995, ApJ, 447, L81. Recent discussion of the evidence for dark matter in clusters.

10

Battye, R. A., & Shellard, E. P. S. 1995, hep-ph preprint 9508301. The most recent analysis of axion production by cosmic strings. They conclude that this is likely to be the most important mechanism of axion production.

11

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12

Binney, J. & Tremaine, S. 1987, Galactic Dynamics (Princeton University Press: Princeton, NJ). An excellent graduate student text.

13

Bottino, A., et al. 1992, Phys. Lett. B, 295, 330. Rome-Beijing-Saclay NaI experiment.

14

Boute, D.A., & Canizares, C.R. 1996, ApJ, 457, 565. Hot gas comprises roughly 10 - 20 , then this baryon/dark matter ratio implies that .

15

Buckland, K., Lehner, M. J., Masek, G. E., & Mojaver, M. 1994, Phys. Rev. Lett., 73, 1067. San Diego TPC experiment which is sensitive to the direction of WIMP recoil.

16

Caldwell, D., et al. 1988, Phys. Rev. Lett., 61, 510. Limits from Germanium semiconductor experiment on halo SUSY particles and 4th Generation Neutrinos.

17

Carrignan, C., & Freeman, K. C. 1988. ApJ, 332, L33. DDO 240 is a gas and dark matter rich dwarf galaxies. The gas mass/stellar mass ratio in this galaxy is roughly 10:1 and the dark mass/(gas + stellar mass ratio) in the galaxy is also roughly 10:1.

18

Chiba, T., Sugiyama, N., & Suto, Y. 1993, ApJ, 429, 427. This paper compares the PIB model to then current experimental data. See also, Hu, W. and Sugiyama, N. 1994, ApJ, 436, 456. For more recent CMB data, see Bennett et al., astro-ph/9601067 and Netterfield et al., astro-ph/9601197.

19

Davis, R. L. 1986, Phys. Lett. B, 180, 225. This paper argues that axions may be produced predominantly through the decay of cosmic strings.

20

Davis, R. L., & Shellard, E. P. S. 1989, Nucl. Phys. B, 324, 167. Further exploration of axion production by cosmic strings.

21

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22

Dine, M., Fischler, W., & M. Srednicki, M. 1981, Phys. Lett. B, 104, 1955. One of the models for the "invisible axion".

23

Drukier, A., & Stodolsky, L. 1984, Phys. Rev. D, 30, 2295. This paper proposes the use of superconducting grains as a solar neutrino detector. It stimulated Goodman and Witten's and Wasserman's proposals for searches for non-baryonic halo dark matter.

24

Drukier, A., Freese, K., & Spergel, D. N. 1986, Phys. Rev. D, 30, 3495. This paper explores the use of a superconducting grain detector in dark matter searches. It shows how the Earth's motion around the Sun produces an annual modulation in the WIMP flux and in the detector signal.

25

Ellis, J., et al. 1984, Nucl. Phys. B, 238, 453 This paper shows that minimal SUSY models predict the existence of stable neutralinos and that these neutralinos have cosmologically interesting densities.

26

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27

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28

Gerhard, O. E., & Spergel, D. N. 1992, ApJ, 389, L9. Phase space constraints imply that neutrinos can not be the dark matter in dwarf galaxies.

29

Gerhard, O., & Silk, J. 1995, astro-ph preprint 9509149 and astro-ph preprint 9511036. They present a model in which halo dark matter in composed of a combination of low mass stars and very cold gas clouds.

30

Goldwirth, D., & Sasselov, D. 1995, ApJ, 444, 15. This paper shows that the systematic uncertainties in estimating the Helium abundances in low metallicity external galaxies are much larger than previously estimated. While many of my colleagues who study the physics of the interstellar medium agree with the conclusions of this paper, its implications have not been fully absorbed by the cosmology community.

31

Goodman, M. W., & Witten, E. 1985, Phys. Rev. D, 31, 3059. This seminal paper started the field of cold dark matter searches. I recommend this paper as the first article that someone interested in this field should read.

32

Gnedin, N., & Ostriker, J. P. 1991, ApJ, 400, 1. This paper proposed that the -rays produced by accretion onto black holes ionized the primordial Helium. See Mather et al. (1992) for limits on this model.

33

Hagmann, C., & Sikivie, P. 1991, Nucl. Phys. B, 363, 247. This paper argues that cosmic string production of axions has been overestimated in earlier papers.

34

Heidelberg-Moscow Experiment hep-ex/9502007. Best limits on the neutrino mass. These limits are based on limits on the rate of neutrinoless decays and apply only to Majorana neutrinos.

35

Hill, J. E. 1995, Phys. Rev. Lett., 75, 2654. This paper discusses the reported detection of Neutrino Oscillations (Athanassopoulos et al. 1995).

36

Hut, P. 1977, Phys. Lett. B, 69, 85. This paper shows how several GeV neutrinos could be the dark matter. These dark matter candidates are now experimentally ruled out (see Ahlen et al. 1987).

37

Jungman, G. U., Kamionkowski, M., & Griest, K. 1995, to appear in Physics Reports. This is an excellent up-to-date review of cold dark matter detection. It also contains several new results.

38

Kamionkowski, M., Griest, K., Jungman, G. & Sadoulet, B. 1995, Phys. Rev. Lett., 74, 5174. This paper compares the relative effectiveness of experiments that look for the decays of SUSY particles in the Sun and experiments that are sensitive to WIMP recoils.

39

Kim, J.-E. 1979, Phys. Rev. Lett., 43, 103. An invisible axion model.

40

Lauer, T., & Postman, M. 1994, ApJ, 425, 418. Lauer and Postman use the properties of the brightest galaxy in each cluster as a "standard candle" to probe the large scale distribution of matter. They find evidence for large-scale motions relative to the microwave background frame (but also see Reiss et al. 1995).

41

Lee, B. W., & Weinberg, S. 1977, Phys. Rev. Lett., 39, 165. This paper shows how several GeV neutrinos could be the dark matter. These dark matter candidates are now experimentally ruled out (see Ahlen et al. 1987).

42

Mather, J., et al. 1992, ApJ, 420, 439. The COBE FIRAS detector showed that the CMB spectrum did not deviate (within their experimental limits) from the predicted thermal spectrum. This experiment places important limits on any kind of energy release (winds from stars, particle decay, etc.) in the early universe.

43

Matsuki, S., et al. 1995, to appear in Proceeding of the XVth Moriond Workshop: Dark Matter in Cosmology, Clocks and Tests of Fundamental Laws, Villars-sur-Ollon, Switzerland, January 21, 1995. This paper describes a detection scheme for axions that uses Rydberg atoms.

44

Mulchaey, J.S., Davis, D.S., Mushotzky, R.F., & Burstein, D. 1993, ApJ (Letters), 404, L9. X-ray observations of a group of galaxies shows that baryons account for only 4% of the mass. The authors places an upper bound of 15% on the baryon content in this small group of galaxies. These observations are strong evidence that dark matter dominates in these small groups.

45

Paczynski, B. 1986, ApJ, 304, 1. This seminal paper describes how microlensing observations can be used to probe the composition of the halo.

46

Peccei, R.D. & H.R. Quinn 1977, Phys. Rev. D16, 1791. An important paper for understanding the role of the axion in CP conservation.

47

Peebles, P. J. E. 1987, ApJ, 315, L73. This paper introduces the baryon isocurvature model. See Peebles, P.J.E. 1994, ApJ, 432, L1 for a more recent discussion of the model.

48

Peterreins, T., et al. 1991, J. Appl. Phys., 69, 1791. This paper discusses the use of SIS junctions in WIMP detection.

49

Press, W. H., & Spergel, D. N. 1985, ApJ, 296, 679. This paper describes how the Sun will capture WIMPs. Once in the Sun, the WIMPs can annihilate (see Silk and Srednicki 1984).

50

Primack, J. R., Seckel, D., & Sadoulet, B. 1988, Ann. Rev. Nucl Part. Sci, 38, 751. A nice review of cold dark matter candidates and dark matter detection. See Jungman et al. (1995) for a more recent discussion.

51

Primack, J. R., Holtzman, J., Klypin, A., & Caldwell, D. O. 1995, Phys. Rev. Lett., 74, 2160. This paper discusses the galaxy and structure formation in the mixed dark matter cosmogony.

52

Raffelt, G. 1995, to appear in Proceeding of the XVth Moriond Workshop: Dark Matter in Cosmology, Clocks and Tests of Fundamental Laws, Villars-sur-Ollon, Switzerland, January 21, 1995 (hep-ph 9502358). This is an excellent introduction to axion dark matter physics.

53

Reiss, A., Kirshner, R. P., & Press, W. H. 1995, ApJ, 445, L91. This paper uses supernova as "standard candles" to probe the large-scale structure of the universe. It appears to contradict earlier work by Lauer and Postman.

54

Reusser, D., et al. 1991, Phys. Lett. B, 225, 143. Best limits on few GeV WIMPs as halo dark matter.

55

Sahu, K.C. 1994, P.A.S.P. 106, 942. This paper argues that the microlensing events in the LMC are better explained as being due to stars in the LMC than by MACHOs

56

Scodeggio, M., & Gavazzi, G. 1993, ApJ, 409, 110. A survey of 112 nearby galaxies that discusses the neutral gas content, and star formation rate as a function of environment.

57

Shifman, M. A., Vainshtein, A. I., & Zakharov, V. I. 1989, Nucl. Phys. B, 166, 493. A model for the invisible axion.

58

Shutt, T., et al. 1992, Phys. Rev. Lett., 69, 3425; ibid. 3531. This paper reports progress on the development of background rejection scheme for halo cold dark matter. See

59

Silk, J., & Srednicki, M. 1984, Phys. Rev. Lett., 53, 624. This paper describes the annihilation of WIMPs in the Sun and the possibility of detecting their annihilation signature.

60

Sikivie, P. 1983, Phys. Rev. Lett, 51, 1415.

61

Smith, P. F., & Lewin, J. D. 1990, Phys. Rep., 187, 203. A nice review of cold dark matter candidates and dark matter detection. See Jungman et al. (1995) for a more recent discussion.

62

Snowden-Ifft, D., et al. 1995, Phys. Rev. Lett., 74, 4133. This describes the use of Mica as a particle detector.

63

Spergel, D. N. 1988, Phys. Rev. D, 37, 1353. This paper shows how the Sun's motion through the Galaxy produces an asymmetric WIMP flux.

64

Spergel, D. N., & Bahcall, J. N. 1988, Phys. Lett. B, 200, 366. Limits on neutrino masses from SN 1987a.

65

Spooner, N., & Smith, P. F. 1993, Phys Lett. B, 314, 430. This paper reports progress in background rejection in a NaI detector.

66

Starkman, G. D., & Spergel, D. N. 1995, Phys. Rev. Lett., 74, 2623. This paper presents a new proposal for WIMP detection using WIMP coupling to bound electrons.

67

Strauss, M., & Willick, J. 1995, Physics Reports, 261, 271. A very nice review of efforts to probe the large-scale structure.

68

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69

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70

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71

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72

Walker, T. P., et al. 1991, ApJ, 376, 51. Standard big bang nucleosynthesis.

73

Wasserman, I. 1986, Phys. Rev. D, 33, 2071. This paper independently showed that supersymmetric dark matter and 4th generation neutrinos may be detectable experimentally.

74

Weinberg, S. 1978, Phys. Rev. Lett., 40, 223. This paper describes how the axion can solve the CP problem.

75

Wilczek, F. 1978, Phys. Rev. Lett., 40, 279. This paper describes how the axion can solve the CP problem.

76

Young, B. A., Cabrera, B. & Lee, A. T. 1990, Phys. Rev. Lett., 64, 2795. This paper describes the Stanford Silicon experiment.

77

Zhitnitsky, A. R. 1980, Sov. J. Nucl. Phys., 31, 260. A model for the invisible axion.