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

More documents

Recommendations

Info

WL Determination of the Distance-Redshift Relation derived for the well studied multi-band field survey, COSMOS (Capak et al. 2007). For COSMOS, photometric redshifts have been derived by Ilbert et al. (2009) using 30 bands in the UV to mid-IR. Since the COSMOS photometry does not cover the Subaru R C band, we estimate R C -band magnitudes for it. For this we use the HyperZ (Bolzonella et al. 2000) template fitting code to obtain the best-fitting spectral template for each galaxy, from which the R C magnitude is derived with the transmission curve of the Subaru R C -band filter (see Umetsu et al. 2010). We then select samples by applying the same CC/magnitude limits as we did above for A370. This is shown in Fig. 4.5 (left) for the COSMOS catalog and plotted in terms of the same CC plane as A370. The color distribution of COSMOS field galaxies seen in this B, R, z ′ CC-space is very similar to that of A370, displaying the same morphology, including red, blue and dropout populations, but without the density peak associated with the massive cluster A370. We also show how redshift varies in this CC-plane by calculating the mean photo-z redshift from COSMOS in fine bins over the CC plane (Fig. 4.5, right), with the samples boundaries displayed as well. This demonstrates that the main overdensity in the CC plane near B J − R C ∼ 1 and R C − z ′ ∼ 0.3 has a mean redshift of around z 0.5, which agrees with our estimation for A370 where we found very little WL signal implying these object lie predominantly in the foreground of the cluster. We also see from this figure that the region where we picked “red” galaxies corresponds to z ∼ 1 − 1.5, and the “blue” galaxies occupy a region of mean redshift around z ∼ 2. Most notably, the top left corner of “dropout” galaxies corresponds to high-z with z 3.5. We further plot the redshift distribution of all the samples in Fig. 4.6. We calculate the median redshift of each sample and summarized in Table 4.2. However, if we look at the distribution of COSMOS redshifts of the dropout sample (Fig. 4.7, red), we find it is somewhat double-peaked, with most galaxies lying around z ∼ 3.5, but a significant fraction identified as having z ∼ 0.4. Since we are certain most of the galaxies in this region are in fact high redshift dropout galaxies, justified by the apparent high WL distortions measured for these galaxies (see Fig. 4.4) and by reference to deep 130
4.5 Results 0.4 0.35 0.3 0.25 foreground orange green−b green−f red−b red−f blue−b blue−f drops N(z) 0.2 0.15 0.1 0.05 0 0 0.5 1 1.5 2 2.5 3 3.5 4 4.5 z Figure 4.6 – Redshift distribution of all A370 samples: foreground (dashed gray), orange (dotted-dashed orange), green (green) bright (solid) and faint (dashed), red (red) bright (solid) and faint (dashed), blue (blue) bright (solid) and faint (dashed), and dropout (dotted-dashed magenta) using COSMOS photo-z’s. Figure 4.7 – Redshift distribution of the dropout-selected sample using COSMOS photoz’s (light red) and using GOODS-MUSIC photo-z’s (dark blue). The low-z peak seen more notably from the COSMOS photo-z’s is most likely due to misclassified galaxy redshifts, supported by the smaller numbers found when using the GOODS-MUSIC photo-z catalog.
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 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 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: 4.5 Results 3.5 3 2.5 4 3.5 3 B −
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 and 158: 5.1 Summary excluding the foregroun
Page 159 and 160: 5.3 Future work observations we obt
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?