PHYS08200605006 D.K. Hazra - Homi Bhabha National Institute
PHYS08200605006 D.K. Hazra - Homi Bhabha National Institute
PHYS08200605006 D.K. Hazra - Homi Bhabha National Institute
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2.4. THE SCALAR AND THE CMB ANGULAR POWER SPECTRA<br />
<br />
<br />
l(l+1) C l TT /(2π) µK 2<br />
<br />
<br />
<br />
<br />
<br />
<br />
<br />
l<br />
<br />
<br />
Figure 2.4: The CMBTT angular power spectra corresponding to the best fit values of the<br />
inflationary models for the WMAP seven-year data without and with the step. The solid<br />
blue and the solid red curves correspond to the quadratic potential without and with the<br />
step, respectively. The dashed green curve corresponds to the best fit small field model<br />
with the step. We find that the results for the tachyon model behave in exactly the same<br />
fashion. The black dots with error bars denote the WMAP seven-year data. It is visually<br />
evident that, with the introduction of the step, the models lead to a better fit to the data<br />
near the multipole moments ofl = 22 and 40.<br />
39