4 Notes on individual new sources

05382+3547. The source lies $36.9^{\prime}$ from the known object 05358+3543 which exhibits both OH and H₂O maser lines (Wouterloot et al. 1988). The OH 1665 MHz and H₂O 22 GHz features from 05358+3543 were observed at velocities higher than -16 and -20 km s^-1 respectively, but at some epoch the water maser emission was also detected near -30 km s^-1 (Wouterloot et al. 1988). We made observations of 05382+3547 and 05358+3543 at the same epoch. It appeared that 05358+3543 has only the 1665 MHz right circularly polarized emission with the peak flux density of 3.4 Jy at -10.3 km s^-1, while 05382+3547 shows the 1665 MHz completely circularly polarized emission at velocities lower than -21 km s^-1. Therefore, we conclude that 05382+3547 is an OH source. The velocity of the 6.7 GHz methanol maser feature of -24.1 km s^-1 (Szymczak et al. 2000) is just within the range of the velocities of L and R 1665 MHz features. CO emission at -19.2 km s^-1 was observed by Wouterloot & Brand (1989). No water maser emission was found towards 05382+3547 at three different epochs (Wouterloot et al. 1993). Furthermore, no ammonia lines were detected (Molinari et al. 1996).
18512+0029. This is the strongest new OH source with a high degree of circular polarization up to 100% for 64.6 km s^-1 feature at 1667 MHz. The adjacent OH source 18507+0110, first discovered by Caswell & Haynes (1983b) as OH34.26+0.15, during our survey had the maser emission blueshifted relatively to the maser features from 18512+0029. Thus, it is unlikely that OH features towards 18512+0029 are sidelobe responses to 18507+0110 source. Turner (1979) did not search for OH emission in the direction of 33.70-0.26. He found an OH mainline emission near 60 and 59 km s^-1 towards neighbourhood points 33.6+0.0 and 33.9+0.0 respectively. The velocities of most of the OH emission peaks observed in our survey are exactly in the middle of the velocity range of the 6.7 GHz methanol maser (Szymczak et al. 2000).
19191+1538. We detected a broad 1667 MHz feature near 42 km s^-1. It is redshifted relatively to the 6.7 GHz methanol maser and the thermal CS line by about 12 and 16 km s^-1 respectively (Szymczak et al. 2000; Bronfman et al. 1996). This source is associated with a spherical ultracompact HII region of the flux density of 87.3 mJy at 6 cm (Wood & Churchwell 1989).
19282+1814. Towards this source a weak ( $\sim3\sigma$) 1665 MHz emission is seen within the velocity range of about 20 km s^-1. The 1667 MHz emission peak at about 24 km s^-1 is redshifted with respect to the 6.7 GHz methanol maser by about 6 km s^-1 (Szymczak et al. 2000). The CS emission detected at 23.6 km s^-1(Bronfman et al. 1996), ammonia emission near 24.1 km s^-1 (Molinari et al. 1996) and HCO⁺ emission at 24.4 km s^-1 (Richards et al. 1987) coincide in velocity with the OH 1667 MHz emission. No H₂O maser emission was detected (Palla et al. 1991). It is unclear whether the 1667 MHz feature near -4.1 km s^-1 is related to the source. An unresolved HII region with the flux density of 1.5 mJy at 3.6 cm was found by Kurtz et al. (1994).
19366+2301. A weak ( $\sim 3-4\sigma$) OH emission with peaks near 32.5 and 33.7 km s^-1 at 1665 and 1667 MHz respectively was detected in our survey. These velocities are virtually the same as the velocity of CS emission of 32.9 km s^-1 (Bronfman et al. 1996) and the central velocity of the 6.7 GHz methanol maser of 34 km s^-1 (Szymczak et al. 2000).
20062+3550. We detected only the 1667 MHz emission at the velocity -2.4 km s^-1. The strongest methanol maser feature was observed exactly at the same velocity (Slysh et al. 1999; Szymczak et al. 2000). The water maser emission peaks near -1.6 km s^-1 (Brand et al. 1994). The CS emission was found at 1.1 km s^-1 (Bronfman et al. 1996).
21074+4949. Two peaks of the 1665 MHz emission at -72.5 and -76 km s^-1 are blueshifted relatively to the velocity of the 6.7 GHz maser (Szymczak et al. 2000). No CS emission was detected (Bronfman et al. 1996).
22272+6358. An OH emission was found at both mainlines. In 1993 no OH emission was detected to the $3\sigma$ upper limit of about 0.15 Jy (Slysh et al. 1994). This suggests considerable variations of the source. The velocity range of the OH emission is similar to that observed for the 6.7 GHz methanol maser (Szymczak et al. 2000). The thermal emission of HCO⁺ found at the velocity of -9.9 km s^-1 (Richards et al. 1987) is very close to the velocities of maser lines.

 

 

Table 2: List of non-detections

02455+6034	06061+2151	18494+0002	18527+0301
18572+0057	18577+0358	19012+0505	19031+0621
19048+0705	18049+0712	19097+0847	19120+0917
19186+1440	19189+1520	19266+1745	19270+1750
19388+2357	22566+5830	23139+5939