tokens: For instance, a source with ∼4 Jy in VLBI and ∼1 Jy in single-dish flux densities has been known as a variable, J0238+1636, which had strong flux variations of around 5 Jy from 2007 to 2010. 6 6 F-GAMMA project: http://www3.mpifr-bonn.mpg.de/div/vlbi/fgamma/fgamma.html . In addition, a source with ∼0.3 Jy (VLBI) and ∼3 Jy (single dish) is J1849+6705. This has also been known as a variable and shows year-scale variations (see footnote 8). Therefore, these variables were not considered for the fit in K band. At SI ≥ 3, on the other hand, the linear fit results were calculated with all sources because the number of sources was small to fit. The slope for the compact sources is 1.07 ± 0.065, while that of extended sources is 0.66 ± 0.006 in K band. We infer that most of the radiation from the compact sources (SI 3) comes from the compact core region, whereas the extended sources (SI ≥ 3) have missing flux. In the Q band, because there are few common sources, the weighted linear fit was applied to all 76 sources. We expect that most of the radiation (∼80%) comes from the compact component, although about 20% of the flux density in the Q band is missing. Figure 6. Top: flux–flux relationship of 232 common sources in K band between single-dish observations from the KVNCS and VLBI observations from (Charlot et al. 2010 ) according to the structure index (SI). The error bar of each source indicates the 1 σ measurement error. Regions (1) and (2) are separated by the median flux densities (the first dotted line) of the KVNCS in K band. Regions (2) and (3) are separated by 1 Jy (the second dotted line) arbitrarily. Red (SI 3) and blue (SI ≥ 3) lines show the weighted linear fit results obtained using the data in (2) and those from all extended sources, respectively (black line: proportional case). Bottom: flux–flux relationship of 76 common sources in the Q band. The error bar of each source indicates the 1 σ measurement error. The green line shows the weighted linear fit result obtained using the all data, regardless of the SI (black line: proportional case). 4.3. Spectral Index Distributions Table 3 shows the statistics of α for 1533 sources in K band and 553 sources in the Q band, and 513 sources simultaneously detected in the K and Q bands. As expected, many of our sources have flat spectra in both the S and X and the K and Q bands. The distributions of the spectral indices of the S and X ( α SX ), X and K ( α XK ), X and Q ( α XQ ), and the K and Q ( α KQ ) bands are shown in Figure 7 . The top panel shows the distributions of α SX and α XK for 1533 sources and α XQ for 553 sources. The distribution of α XK becomes broader than that of α SX , but ∼88% of the α SX values and ∼70% of the α XK values belong to the flat-spectrum ranges. In addition, the distribution of α XQ is similar, and we expect that these are relatively bright sources. In the bottom panel, the distribution of α XK is broader than the other distributions and shifts toward
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