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CHAPTER 5: LUMINOSITY FUNCTION OF XMS SOURCES the 1σ error bars to those calculated with a dividing value of N H = 10 22 cm −2 . [48] also found a fraction of absorbed AGN with L 2−10 ≥ 3 × 10 42 erg s −1 of 0.57 ± 0.11 which was in excellent agreement with the results obtained by a variety of SWIFT and INTEGRAL surveys (see Table 3 in [48]). The value predicted by our ultrahard N H function, converting 2-10 keV luminosities to 4.5-7.5 keV using Γ = 1.7, is 0.55 ± 0.18 using a dividing value of N H = 4 × 10 21 cm −2 , which fully agrees with that of [48]. Considering a dividing value of N H = 10 22 cm −2 , our predicted fraction decreases to 0.42 ± 0.18 which coincides with the INTEGRAL result of [201] (0.42 ± 0.09) who also used the latter dividing N H value between absorbed and unabsorbed AGN. The predicted fraction in the hard band at L 2−10 ≥ 3 × 10 42 erg s −1 is 0.39 ± 0.09, still consistent with the value of [201]. 5.3 Method In this section we will calculate the X-ray luminosity function of our sources in the soft, hard and ultrahard bands. Although the backbone of this study is the XMS sample, it is imperative to combine it with other complementary shallower and deeper surveys in order to cover a wider L x − z range. Shallower, wider area surveys will provide significant numbers of bright sources at low redshifts while deep pencil-beam surveys will probe fainter sources at greater distances. The accompanying surveys used in this chapter are summarized in Table 5.1 and they have been described in section 2.3. In order to have an optimal L X − z plane coverage (see Figure 5.5) we will constrain our analysis to those sources identified as AGN with redshifts in the range 0.01 < z < 3 in the soft and hard bands (spanning up to seven and six orders of magnitude in luminosity, respectively) and 0.01 < z < 2 in the ultrahard band (spanning up to four orders of magnitude in luminosity). The total sky area covered by these surveys is shown in Figure 5.6. For the purposes of this work and to avoid errors and biases caused by further classification, we have used the entire AGN population available (within the redshift limits stated above) irrespective of whether they were identified as Type-1 AGN or Type-2 AGN. The differential XLF measures the number of AGN per unit of comoving vol- 124
CHAPTER 5: LUMINOSITY FUNCTION OF XMS SOURCES Table 5.1 Summary of surveys used in this work, along with their flux limits, sky coverage, identification completeness and the number of identified AGN for each energy band. Soft (0.5-2 keV) Survey Flux limit (erg cm −2 s −1 ) Area (deg 2 ) Completeness (%) N AGN RBS 2.5×10 −12 20300 100 310 RIXOS8 8.4×10 −14 4.44 100 40 RIXOS3 3.0×10 −14 15.77 94 182 XMS 1.5×10 −14 3.33 96 178 RDS 5.5×10 −15 0.30 92 39 CDF-S 5.5×10 −17 0.12 100 a 226 Hard (2-10 keV) Survey Flux limit (erg cm −2 s −1 ) Area (deg 2 ) Completeness (%) N AGN AMSS 3.0×10 −13 68 99 79 XMS 3.3×10 −14 3.33 84 120 CDF-S 4.5×10 −16 0.11 100 a 236 Ultrahard (4.5-7.5 keV) Survey Flux limit (erg cm −2 s −1 ) Area (deg 2 ) Completeness (%) N AGN HBSS 7.0×10 −14 25.17 97 62 XMS 6.8×10 −15 3.33 86 57 a Including photometric redshifts (see section 2.3). 125
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Summary Since its discovery more th
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CONTENTS 1.6.1 The K-correction . .
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CONTENTS 5.3.2 Analytical model . .
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LIST OF FIGURES 4.6 Soft 1 − P µ
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Chapter 1 Introduction In the last
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CHAPTER 1: INTRODUCTION have confir
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CHAPTER 1: INTRODUCTION by this mis
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CHAPTER 1: INTRODUCTION Figure 1.2
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CHAPTER 1: INTRODUCTION to-noise ra
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CHAPTER 1: INTRODUCTION Compton up-
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CHAPTER 1: INTRODUCTION optically c
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CHAPTER 1: INTRODUCTION Figure 1.5
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CHAPTER 1: INTRODUCTION AGN are ess
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CHAPTER 2: AGN SURVEYS WITH XMM-New
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Chapter 3 Source counts of the AXIS
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CHAPTER 3: SOURCE COUNTS OF THE AXI
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61 Table 3.1 Maximum likelihood fit
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Page 206 and 207: REFERENCES [16] Barger, A. J., Cowi
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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
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