# Intra-Day Variability Observations of Two Dozens of Blazars at 4.8 GHz
## 3 Results and Discussion
### Comment on Individual Sources
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0300 + 470 & BL\({}^{\star}\) & 21 & 2.548 \(\pm\) 0.029 & 1.14/0.91 & 2.81 & 60.1 & 3.0 & 6.8 \(\times\) 10\({}^{-6}\) (9) \({}^{\star}\) & 0.475 & mm (1) \\ BZ 040 + 362 & FSRQ & 10 & 0.452 \(\pm\) 0.005 & 1.11/0.00 & 2.70 & 9.5 & 1.1 & 3.9 \(\times\) 10\({}^{-6}\) (10) & 1.484 & yyyy (1) \\ PKS 0507 + 199 & FSRQ & 15 & 0.584 \(\pm\) 0.008 & 1.37/0.94 & 3.63 & 30.6 & 2.2 & 6.4 \(\times\) 10\({}^{-6}\) (9) & 0.41 & 7 yyy (1) \\ PKS 0528 + 134 & FSRQ & 22 & 1.710 \(\pm\) 0.034 & 1.99/1.83 & 5.64 & 149.8 & 7.1 & 1.9 \(\times\) 10\({}^{-21}\) (9) & 2.06 & myyy (1) \\
0624 + 496 & FSRQ & 23 & 2.532 \(\pm\) 0.027 & 1.06/0.79 & 2.52 & 55.6 & 2.9 \(\times\) 10\({}^{-6}\) (9) & 3.96 & mm (1) \\
0716 + 714 & BL & 43 & 1.255 \(\pm\) 0.016 & 1.27/0.99 & 3.30 & 112.6 & 2.7 \(\times\) 10\({}^{-6}\) (9) & 0.3 & y (2) \\
0748 + 126 & FSRQ & 24 & 2.599 \(\pm\) 0.057 & 2.23/1.14 & 6.40 & 237.9 & 10.3 & 1.3 \(\times\) 10\({}^{-30}\) (9) & 0.889 & myyy (1) \\
0917 + 624 & FSRQ & 44 & 1.123 \(\pm\) 0.018 & 1.60/1.37 & 4.40 & 186.0 & 4.3 & 1.1 \(\times\) 10\({}^{-10}\) (9) & 1.446 & mm (1) \\
0954 + 688 & FSRQ & 43 & 1.183 \(\pm\) 0.017 & 1.53/1.99 & 4.15 & 164.3 & 3.9 & 2.2 \(\times\) 10\({}^{-10}\) (9) & 0.368 & myyy (1) \\
1004 + 719 & FSRQ & 15 & 2.881 \(\pm\) 0.005 & 1.36/1.15 & 3.58 & 57.5 & 4.1 & 3.3 \(\times\) 10\({}^{-6}\) (9) & 1.15 & mm (1) \\
1156 + 295 & FSRQ & 26 & 1.248 \(\pm\) 0.013 & 1.04/0.70 & 2.45 & 45.4 & 1.8 & 7.5 \(\times\) 10\({}^{-6}\) (9) & 0.72469 & yyyy (1) \\
02129 + 376 & FSRQ & 24 & 0.918 \(\pm\) 0.011 & 1.20/0.00 & 3.03 & 47.8 & 2.1 & 1.8 \(\times\) 10\({}^{-6}\) (9) & 3.81908 & n.a \\
1357 + 769 & FSRQ & 51 & 0.461 \(\pm\) 0.025 & 5.4/2.82 & 16.15 & 972.4 & 1.8 \(\times\) 10\({}^{-6}\) (9) & 1.858 & n.a. \\ PKS 1502 + 106 & FSRQ & 9 & 0.791 \(\pm\) 0.005 & 0.63/0.00 & 0.00 & 4.1 & 0.5 & 8.5 \(\times\) 10\({}^{-6}\) (10) & 1.8831 & n (n) \\
1367 + 574 & FSQ & 39 & 1.308 \(\pm\) 0.016 & 1.22/0.93 & 3.12 & 86.0 & 2.3 & 1.4 \(\times\) 10\({}^{-6}\) (9) & 0.7566 & mm (1) \\ \hline WISE J092153.43 + 501336.0 & BL\({}^{\star}\) & 10 & 0.342 \(\pm\) 0.013 & 3.80/3.50 & 11.24 & 83.3 & 9.3 & 3.6 \(\times\) 10\({}^{-14}\)(9) & 0.3709 & yyyy (1) \\ BZ  
**WISE J092915.43 + 501336.0 (J0929 + 5013, B0925 + 504)**: the BL Lac object exhibits fast IDV in both sessions (bottom panel of Figure 1), \(m^{\prime}\) increases from 3.50 in session 1 to 7.13 in session 2. Its mean flux density is slightly increased from session 1 to session 2. The blazar has previously shown fast IDV with Urumqi 25 m and Efferslberg 100 m telescope, its IDV timescales can be fitted with the annual modulated ISS model [36; 37]. **BZQ J1128 + 5925**: the blazar shows a strong fast IDV in both sessions (middle panel of Figure 1), its \(m^{\prime}\) increases from 3.54 in session 1 to 5.18 in session 2. Its mean flux density increases slightly from 0.621 \(\pm\) 0.023 Jy in session 1 to 0.630 \(\pm\) 0.033 Jy in session 2. This fast IDV was first found with Urumqi 25 m telescope, and it has shown seasonal variations of IDV timescales and can be well fitted with the annual modulation model [35]. **J2311 + 4543**: the blazar shows a strong IDV in both sessions with both the \(m^{\prime}\) and mean flux density slightly increased from session 1 to session 2.