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method | Cu #x02013;O | Cu #x02013;NPy | Cu #x02013;NAm1 | Cu #x02013;NAm2 | Cu #x02013;O/N (avg.) | #x003c4;4b |
---|---|---|---|---|---|---|
XRD (this work) | 1.845(4) | 1.924(3) | 2.016(3) | 2.019(3) | 1.95 | 0.16 |
XRD (ref 1) | 1.9465(19) | 1.920(2) | 2.010(2) | 1.996(2) | 1.97 | 0.17 |
DFT (PBE0)c | 1.868 | 1.950 | 2.089 | 2.081 | 2.00 | 0.16 |
DFT (mPW)d | 1.863 | 1.947 | 2.078 | 2.080 | 1.99 | 0.16 |
EXAFS (ref 1) | 1.95 |
Fig. #8201;5 Each row shows a grey-scale image of the Spitzer 3.6 #8201; #956;m observations, superimposed with grey contours indicating the 1.4 #8201;GHz observations and black contours showing the 4.8 #8201;GHz (left panel) and 8.6 #8201;GHz (middle panel) observations. The IFRS are always the sources at the image centres. Contours start at 3 #963; and increase by factors of 2. The 1.4 #8201;GHz restoring beam and the 4.8 #8201;GHz/8.6 #8201;GHz restoring beams, which are the same size, are indicated with ellipses in the lower left corners of the images. The right panel shows the flux density measurements available for a source and 3 #963; upper limits where no detection was made (indicated with arrows). The solid line indicates the best available spectral index, and dashed lines indicate a power-law with an index 1 #963; larger and 1 #963; smaller than determined by the data. We note that all sources have a signal-to-noise ratio of more than 9 in the 1.4 #8201;GHz observations, so there is no doubt that they are real sources and not spurious. |
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Open with DEXTER | |
In the text |
Patinka | Sekti | Bendrinti | Daugiau |