tokens: XTE J1752-223 discovered by the Rossi X-ray Timing Explorer ( RXTE ) and Swift satellites on 2009 October 23 (Markwardt et al. 2009b ) suggested that it is a black hole candidate (Markwardt et al. 2009a ; Nakahira et al. 2009 ; Remillard et al. 2009 ; Shaposhnikov et al. 2009 , 2010 ). Three days after the X-ray discovery, a bright optical counterpart was found by the Magellan Baade telescope (Torres et al. 2009b ). Also, a bright near-infrared (NIR) counterpart was identified immediately (Torres et al. 2009a ). Afterwards, a bright radio counterpart was discovered by the Australia Telescope Compact Array (ATCA) with a flux density of at both 5.5 and (Brocksopp et al. 2009 , 2010 ). The radio light curves of XTE J1752-223 at 5.5 and were measured by ATCA, the European VLBI (Very Long Baseline Interferometry) Network (EVN), the Very Long Baseline Array (VLBA), and the Expanded Very Large Array (Brocksopp et al. 2009 ; Yang et al. 2010 ; Miller-Jones et al. 2011 ). Furthermore, the X-ray outbursts during 2009 October and 2010 July were obtained by the Monitor of All-sky Image (MAXI), RXTE , and Swift (Nakahira et al. 2010 ; Shaposhnikov et al. 2010 ; Curran et al. 2011 ). The long baseline observations of XTE J1752-223 are shown in Figure 1 , in which four jet features marked as A, B, C, and D have been reported by Yang et al. ( 2011 ). Component A appeared first, and then components B1 and B2 emerged, which suggests that components farther from the core can be seen earlier than components nearer the core. Moreover, components A and B were observed after the peaks of the radio light curve. It is of interest to understand such a connection between jet features and light curve. Figure 1. The positions of the components A, B, and D of XTE J1752-223 from the VLBA images (Yang et al. 2011 ) for each observing epoch. Note that components B and C in Yang et al. ( 2011 ) are written as B1 and B2 here. NRAO 150, discovered in the radio band by Pauliny-Toth et al. ( 1966 ), is a prominent quasar from the millimeter to radio band at redshift z = 1.52 (Agudo et al. 2006 ). Observations of this source by VLBI from 2001 October to 2004 April and by VLBA from 1997 June to 2002 June have exhibited a moving core–jet structure as shown in the left panel of Figure 2 . The core–jet structure consists of three components, Q1, Q2, and Q3. The evolution of the relative position of these three components is plotted in the right panel of Figure 2 , where Q1, Q2, and Q3 moved in a counterclockwise direction with respect to the core. The projected angular speed of these components can be up to , which is the first superluminal motion found within the innermost region () of the jet in NRAO 150 (Agudo et al. 2007 ). Figure 2. The ridge line structure of the jet of quasar NRAO 150 and the evolution of the position of components Q1, Q2, and Q3 from left to right (Agudo et al. 2007 ). In this paper, the observations of the kinematics of XTE J1752-223 and NRAO 150 are
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