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Spectral Analysis of the Cool and Warm Perseus data
1 Gain Calibration - zopt = 0. 179 for Perseus
Figure 1: Spectral analysis of cool portion of the Perseus observation in the 5.0-8.0 keV energy band. The best-fit redshift and 1 σ and 90% uncertainties are z=0.0164, (0.0142-0.0173) and (0.0116-0.0179). This gives ∆z =0.15%, ∆z 1 σ =0.06%, and ∆z90% =0.0%
Figure 2: Spectral analysis of warm portion of the Perseus observation in the 5.0-8.0 keV energy band. The best-fit redshift and 1 σ and 90% uncertainties are z=0.0132, (0.0096-0.0152) and (0.0092-0.0167). This gives ∆z =0.47%, ∆z 1 σ =0.27%, and ∆z90% =0.12%
Figure 3: ACIS-I spectrum of the cool portion of the Perseus observation along with the best-fit phabs*apec model.
Figure 4: ACIS-I spectrum of the warm portion of the Perseus observation along with the best- fit phabs*apec model.
Table 3: Spectral Analysis Results (2.0-7.0 keV) - tcticorr Detector Temp kT z (keV) Cool 4.30 (4.15-4.38)(4.12-4.44) 0.0135 (0.0126-0.0168)(0.0121-0.0184) Warm 4.13 (4.06-4.22)(4.01-4.27) 0.0121 (0.0112-0.0156)(0.0109-0.0168)
Notes: Best-fit kT and redshift (along with their 1 σ and 90% uncertainties) obtained by fitting an absorbed thermal model (phabs*apec) to the Perseus spectra.
Table 4: Spectral Analysis Results (2.0-7.0 keV) - ape Detector Temp kT z (keV) Cool 4.04 (3.90-4.20)(3.82-4.30) 0.0260 (0.0247-0.0268)(0.0233-0.0277) Warm 4.07 (3.93-4.14)(3.87-4.19) 0.0259 (0.0241-0.0262)(0.0230-0.0276)
Notes: Best-fit kT and redshift (along with their 1 σ and 90% uncertainties) obtained by fitting an absorbed thermal model (phabs*apec) to the Perseus spectra.
