Mass and Light distributions in Clusters of Galaxies - Henry A ...

More documents

Recommendations

Info

Discussion range, 1 < z < 5. 5.2 Further application of the methods in other work By applying my methods to carefully separate and select background galaxies for a weak lensing study, we measured distortion effects in all four massive clusters studied in my work, A1689, A1703, A370 & RXJ1347, and derived the most accurate published mass profiles to date (Broadhurst et al. 2008). In producing these profiles, we combined the strong lensing information obtained from sets of multiple images found in high-quality HST/ACS imaging, with the weak lensing distortion to background galaxies in deep, wide-field, multi-band Subaru/Suprime-Cam imaging. The mass profiles all agree with the predicted form for CDM-dominated halos, with continuously steepening profiles, consistent with the expectation that DM is cold. In detail, however, these profiles are somewhat more concentrated than predicted, 8 < c vir < 15 (< c vir >= 10.39 ± 0.91). If this behavior proves to be typical it will require modification of the underlying model. In (Broadhurst et al. 2008) we also examined the lensing magnification effect, seen as a depletion in the surface number density profiles of red background galaxies near the cluster center. The measured depletion compared to the expected depletion for the best-fitting NFW density profile (derived from the corresponding distortion profiles) were found to be consistent, which strengthens our conclusions and more importantly establishes the utility of the background red galaxies for measuring magnification. By combining magnification and distortion we improve upon the accuracy of lensing mass determinations. Further implementation of the color-color selection method was used to study the mass structure of the galaxy cluster Cl0024+17 in Umetsu et al. (2009) and in Zitrin et al. (2009b). Based on deep Subaru BR c z ′ imaging and our recent comprehensive strong lensing analysis of HST/ACS/NIC3 142
5.3 Future work observations we obtained strong+weak lensing distortion and magnification profiles. Unlike previous lensing studies of this cluster, the weak and strong lensing were found to be in excellent agreement where the data overlap. This together with the anomalously low X-ray emission and complex internal dynamics strongly indicate that this cluster system is in a post collision state, which is consistent with our mass profile for a major merger occurring along the line of sight, viewed approximately 2 − 3 Gyr after impact when the gravitational potential has had time to relax in the center, but before the outer cluster region is virialized. 5.3 Future work I plan to continue and apply our robust approach to other X-ray (e.g., Ebeling et al. 2001, MACS) and SZ (e.g., Staniszewski et al. 2009, SPT; Geisbüsch et al. 2005, Planck) selected clusters. Such samples are arguably less prone to selection-biases than optically-selected, and therefore may provide a more secure determination of the concentration-mass relation for comparison with theoretical ΛCDM predictions. I have so far obtained and reduced data from the Subaru/Suprime-Cam archive, consisting of seven MACS cluster in multiple bands - B J , V J , R C , I C , z ′ , and at least a dozen more MACS clusters are available in the archive. Highresolution imaging of the central parts of the clusters will be required from space in order to determine the strong lensing properties of the cores. An integral part of this study will be to also determine the light properties of these clusters using the dilution method I have developed. I intend to further explore the declining M/L characteristic by examining the connection between morphology and the color-color plane. To that end higher resolution imaging and spectroscopy of close-by (z < 0.1) clusters will aid in identifying cluster galaxy morphologies. 143
Page 1:
TELAVIVUNIVERSITY SCHOOLOFPHYSICS&A
Page 5:
To my parents
Page 8 and 9:
1.2.3 Weak Gravitational Lensing .
Page 10 and 11:
5 Discussion 139 5.1 Summary . . .
Page 12 and 13:
negligibly contaminated by the clus
Page 15 and 16:
Acknowledgments I would like to tha
Page 17 and 18:
Chapter 1 Introduction Clusters of
Page 19 and 20:
1.1 Clusters of Galaxies The space
Page 21 and 22:
1.1 Clusters of Galaxies and a grav
Page 23 and 24:
1.1 Clusters of Galaxies to the sph
Page 25 and 26:
1.1 Clusters of Galaxies 1.1.5 X-ra
Page 27 and 28:
1.2 Gravitational Lensing increase
Page 29 and 30:
1.2 Gravitational Lensing Broadhurs
Page 31 and 32:
1.2 Gravitational Lensing If we ins
Page 33 and 34:
1.2 Gravitational Lensing Figure 1.
Page 35 and 36:
1.2 Gravitational Lensing 1.2.3.1 M
Page 37 and 38:
1.2 Gravitational Lensing a transfo
Page 39 and 40:
1.2 Gravitational Lensing effects c
Page 41:
1.3 The Structure of the Thesis 1.3
Page 44 and 45:
Weak Lensing Dilution in A1689 clus
Page 46 and 47:
Weak Lensing Dilution in A1689 beha
Page 48 and 49:
Weak Lensing Dilution in A1689 Figu
Page 50 and 51:
Weak Lensing Dilution in A1689 blue
Page 52 and 53:
Weak Lensing Dilution in A1689 gala
Page 54 and 55:
Weak Lensing Dilution in A1689 0.5
Page 56 and 57:
Weak Lensing Dilution in A1689 not
Page 58 and 59:
Weak Lensing Dilution in A1689 lens
Page 60 and 61:
2.5 Photometric redshifts Weak Lens
Page 62 and 63:
Page 64 and 65:
Weak Lensing Dilution in A1689 the
Page 66 and 67:
Page 68 and 69:
Weak Lensing Dilution in A1689 expe
Page 70 and 71:
Page 72 and 73:
Weak Lensing Dilution in A1689 et a
Page 74 and 75:
Weak Lensing Dilution in A1689 g +
Page 76 and 77:
Weak Lensing Dilution in A1689 Note
Page 78 and 79:
Weak Lensing Dilution in A1689 Usin
Page 80 and 81:
Weak Lensing Dilution in A1689 We a
Page 82 and 83:
Weak Lensing Dilution in A1689 limi
Page 84 and 85:
Weak Lensing Dilution in A1689 rela
Page 86 and 87:
Weak Lensing Dilution in A1689 To s
Page 88 and 89:
Weak Lensing Dilution in A1689 30 2
Page 91 and 92:
Chapter 3 Detailed Cluster Mass and
Page 93 and 94:
3.1 Introduction Stars are not expe
Page 95 and 96:
3.2 Subaru data reduction § 3.3 we
Page 97 and 98:
3.3 Sample selection from the color
Page 99 and 100:
Page 101 and 102:
Page 103 and 104:
3.4 Evolutionary color tracks 0.25
Page 105 and 106:
3.5 Depth estimation from SDF/COSMO
Page 107 and 108: 3.5 Depth estimation from SDF/COSMO
Page 109 and 110: 3.6 Weak lensing analysis 3.6 Weak
Page 111 and 112: 3.6 Weak lensing analysis where θ
Page 113 and 114: 3.8 Cluster light profiles 600 A168
Page 115 and 116: 3.9 M/L profiles Broadhurst et al.
Page 117 and 118: 3.9 M/L profiles 10 5 r [Mpc/h] bri
Page 119 and 120: 3.9 M/L profiles very moderate decl
Page 121 and 122: 3.9 M/L profiles 0.6 0.4 0.2 log 10
Page 123 and 124: 3.10 Cluster luminosity functions b
Page 125 and 126: 3.11 Discussion and conclusions Tab
Page 127 and 128: 3.11 Discussion and conclusions law
Page 129 and 130: Chapter 4 A Weak Lensing Determinat
Page 131 and 132: 4.1 Introduction Zitrin et al. 2009
Page 133 and 134: 4.3 Sample selection from the color
Page 139 and 140: 4.4 Weak lensing measurements objec
Page 141 and 142: 4.5 Results tion N i (z s ) of i-th
Page 143 and 144: 4.5 Results n [arcmin −2 ] 10 1 1
Page 145 and 146: 4.5 Results 3.5 3 2.5 4 3.5 3 B −
Page 147 and 148: 4.5 Results 0.4 0.35 0.3 0.25 foreg
Page 149 and 150: 4.5 Results Γ (g T amplitude ratio
Page 151 and 152: 4.5 Results 1.6 1.4 1.2 Γ (g T amp
Page 153 and 154: 4.7 Discussion and conclusions is t
Page 155 and 156: Chapter 5 Discussion 5.1 Summary In
Page 157: 5.1 Summary excluding the foregroun
Page 161 and 162: References Abadi, M. G., Moore, B.,
Page 163 and 164: REFERENCES Broadhurst, T., Umetsu,
Page 165 and 166: REFERENCES Gaidos, E. J. 1997, AJ,
Page 167 and 168: REFERENCES Kaiser, N. 1995, ApJ, 43
Page 169 and 170: REFERENCES Natarajan, P., Loeb, A.,
Page 171 and 172: REFERENCES Schrabback, T. et al. 20
Page 173 and 174: כפי שמתואר בפרק השל
Page 175 and 176: עבודה זו נעשתה בהנח
show all

Mass and Light distributions in Clusters of Galaxies - Henry A ...

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?