pdf - SRON

More documents

Recommendations

Info

CHAPTER 5: LUMINOSITY FUNCTION OF XMS SOURCES d φ / d log L x 10 −11 10 −10 10 −9 10 −8 10 −7 10 −6 10 −5 10 −4 10 −3 0.01 0.01
CHAPTER 5: LUMINOSITY FUNCTION OF XMS SOURCES shape of our best-fit present day XLF would correspond to the average of the absorbed and unabsorbed present day XLF calculated in [48] thus lying inside the 1σ confidendence levels spanned by their parameters. Our best-fit value for the evolution parameter p 1 = 6.46 +0.69 −0.29 is in excellent agreement with that of [48] (p 1 = 6.5) and also with that of [22] obtained from a selected AGN sample in the optical range from the VIMOS-VLT survey (p 1 = 6.54) and that of the bolometric quasar luminosity function of [112] (p 1 = 5.95 ± 0.23). This value represents a much stronger evolution below the cut-off redshift than that obtained by [224] (p 1 = 4.23 ± 0.39) and [130] (p 1 = 4.62 ± 0.26) in the 2-10 keV band. Some works (i.e. [157], [104], [22]) suggest that the evolution parameter p 1 might depend linearly on the X-ray luminosity, increasing as the luminosity increases. Given the lack of deep surveys, which mainly account for intrincally faint objects, in the ultrahard band, this result could be biased towards highluminosity sources and hence provides higher evolution rates below the cut-off redshift. 5.4.2 Accretion history of the Universe The X-ray luminosity function of AGN, whose bolometric emission is directly linked to accretion power, constrains the history of the formation of the supermassive black holes that reside in the galactic centers along cosmic times. The comoving density of AGN as a function of redshift can be calculated straightforward from our best-fit XLF LDDE model: Φ(z) = ∫ L2 L 1 dΦ(L X , z) d log L X d log L X (5.4.1) As we can see in Figure 5.10, the most luminous AGN are formed before the less luminous ones in all bands, although this is difficult to say in the ultrahard band due to the limited statistics. AGN with log L X > 44 reach a maximum in density at redshift ∼1.5 while fainter AGN (log L X < 44) peak at z ∼ 0.7. Similarly to the comoving density, we can derive the luminosity density as a function of redshift in all bands and, from that, calculate the accretion rate density. Here we will assume that the accretion rate onto a supermassive black hole is related to the bolometric luminosity by a constant factor ɛ which is the 137
Page 3:
Universidad de Cantabria Departamen
Page 7:
A mis padres
Page 10 and 11:
explicar las altas luminosidades de
Page 12 and 13:
Además, una importante fracción (
Page 14 and 15:
ealizar estudios de espectroscopía
Page 16 and 17:
distribución diferencial que, al e
Page 18 and 19:
materia sobre el agujero negro cent
Page 20 and 21:
analizadas proviene de fuentes en t
Page 22:
Haciendo uso del segundo catálogo
Page 27:
With magic, you can turn a frog int
Page 30:
Un capítulo aparte merecen mis com
Page 33 and 34:
Summary Since its discovery more th
Page 36 and 37:
xxxiv
Page 38 and 39:
CONTENTS 1.6.1 The K-correction . .
Page 40 and 41:
CONTENTS 5.3.2 Analytical model . .
Page 42 and 43:
LIST OF FIGURES 4.6 Soft 1 − P µ
Page 45 and 46:
Chapter 1 Introduction In the last
Page 47 and 48:
CHAPTER 1: INTRODUCTION have confir
Page 49 and 50:
CHAPTER 1: INTRODUCTION by this mis
Page 51 and 52:
CHAPTER 1: INTRODUCTION Figure 1.2
Page 53 and 54:
CHAPTER 1: INTRODUCTION [161], [242
Page 55 and 56:
CHAPTER 1: INTRODUCTION tant contri
Page 57 and 58:
CHAPTER 1: INTRODUCTION to-noise ra
Page 59 and 60:
CHAPTER 1: INTRODUCTION Compton up-
Page 61 and 62:
CHAPTER 1: INTRODUCTION ([142]). It
Page 63 and 64:
CHAPTER 1: INTRODUCTION (NLR) and i
Page 65 and 66:
CHAPTER 1: INTRODUCTION optically c
Page 67 and 68:
CHAPTER 1: INTRODUCTION ber of AGN
Page 69 and 70:
CHAPTER 1: INTRODUCTION Figure 1.5
Page 71 and 72:
CHAPTER 1: INTRODUCTION 1.7.3 The X
Page 73 and 74:
CHAPTER 1: INTRODUCTION AGN are ess
Page 75:
CHAPTER 1: INTRODUCTION subjects ma
Page 78 and 79:
CHAPTER 2: AGN SURVEYS WITH XMM-New
Page 80 and 81:
Page 82 and 83:
Page 84 and 85:
R R OQP ONM 40 Table 2.1: Continued
Page 86 and 87:
Page 88 and 89:
Page 90 and 91:
Page 92 and 93:
Page 94 and 95:
Page 96 and 97:
Page 99 and 100:
Chapter 3 Source counts of the AXIS
Page 101 and 102:
CHAPTER 3: SOURCE COUNTS OF THE AXI
Page 103 and 104:
Page 105 and 106:
61 Table 3.1 Maximum likelihood fit
Page 107 and 108:
Page 109 and 110:
Page 111 and 112:
Page 113 and 114:
Page 115 and 116:
Page 117 and 118:
Page 119 and 120:
Page 121 and 122:
Page 123 and 124:
Page 125:
Page 128 and 129:
CHAPTER 4: CLUSTERING OF AXIS AND X
Page 130 and 131: CHAPTER 4: CLUSTERING OF AXIS AND X
Page 156: CHAPTER 4: CLUSTERING OF AXIS AND X
Page 159 and 160: Chapter 5 Luminosity function of XM
Page 161 and 162: CHAPTER 5: LUMINOSITY FUNCTION OF X
Page 179: CHAPTER 5: LUMINOSITY FUNCTION OF X
Page 192 and 193: CHAPTER 6: SUMMARY OF THE RESULTS s
Page 194 and 195: CHAPTER 6: SUMMARY OF THE RESULTS b
Page 196 and 197: CHAPTER 6: SUMMARY OF THE RESULTS F
Page 199 and 200: Appendix A Sensitivity maps The val
Page 201 and 202: APPENDIX A: SENSITIVITY MAPS clearl
Page 204 and 205: APPENDIX A: SENSITIVITY MAPS 160
Page 206 and 207: REFERENCES [16] Barger, A. J., Cowi
Page 208 and 209: REFERENCES [61] Ehle, M., Breitfell
Page 210 and 211: REFERENCES [107] Hawkins, M. R. S.
Page 212 and 213: REFERENCES [148] Matarrese, S., Col
Page 214 and 215: REFERENCES [190] Richstone, D., Ahj
Page 216: REFERENCES [236] Wisotzky, L., 1998
show all

pdf - SRON

Create successful ePaper yourself

Delete template?

Save as template?