4 Comments regarding individual sources which have CS(2-1) integrated intensity greater than 10 K km s^-1

NGC 281-W. The integrated intensity is 14.4 K km s^-1. The profile is based on a pedestal. Bipolar outflow is weak (16 km s^-1 wing range, Snell et al. 1990). Maser emission at 44 GHz was not detected (Bachiller et al. 1990), but a weak Class II methanol maser was detected at the velocity of the bipolar outflow centre (Slysh et al. 1998). IRAS05329-0512. The source was taken from the list of bipolar outflows compiled by Xiang & Turner (1995). The coordinates are offset by $\Delta\alpha =65^{\prime\prime}$, $\Delta\delta =40^{\prime\prime}$from the centre of the strong Class I methanol maser OMC-2 (Haschick et al. 1990). The CS(2-1) integrated intensity is 11.6 K km s^-1. The profile is based on a pedestal. S233. The integrated intensity is 12.4 K km s^-1. The profile is based on a pedestal. IRAS 05358+3543 and a bipolar outflow (CO wing range 25 km s^-1, Snell et al. 1990) are observed in the direction of the HII region. The source was observed in CS(2-1) by Bronfman et al. (1996). The velocity of the CS line agrees with the velocity of the bipolar outflow centre within the limits of error. The methanol line at 44 GHz was not detected above the 10 Jy level (Kalenskii et al. 1992). S231. The integrated intensity is 14.0 K km s^-1. The profile is Gaussian. The source is known to be a Class I methanol maser at 44 GHz (Bachiller et al. 1990) and a strong Class II methanol maser at 6.7 GHz (Menten 1991). The velocity of the CS line is -16.5 km s^-1. S235B (GGD 5). A strong CS line with a red-shifted wing was detected. The integrated intensity is 27.4 K km s^-1. Bipolar outflow CO wings (22 km s^-1) were characterized by Bally & Lada (1983) as being average in range. The velocity of the CS line is -16.9 km s^-1. A Class I methanol maser was detected at -16.9 km s^-1 at 44 GHz at a position with $\Delta\alpha=12^{\prime\prime}$ and $\Delta\delta=23^{\prime\prime}$ offset (Haschick et al. 1990). AFGL5180 (S252, G188.9+0.9, S254-258). The region was included in our survey as a bipolar outflow (Snell et al. 1988) and also as a Class II methanol maser (Menten 1991) with $\Delta\alpha = 3^{\prime\prime}$ and $\Delta\delta = 12^{\prime\prime}$position difference. The CS line turned out to be stronger at the position of the bipolar outflow centre than on the position of the methanol maser. The CS integrated intensity is 23.1 K km s^-1 for AFGL 5180 and 13.8 K km s^-1 for G188.9+0.9. The velocity of the CS line, 3.2 km s^-1, is not coinciding with the velocity of the bipolar outflow 6.7 km s^-1, but is coinciding with the velocity 3.15 km s^-1 of the CS(1-0) line (Anglada et al. 1996) and with the velocity 3.1 km s^-1 of the CS(2-1) line (Bronfman et al. 1996). Snell et al. (1988) pointed out that it is difficult to evaluate the CO wing range of the bipolar outflow AFGL5180 at the velocity of 4 km s^-1 due to the second emission component of the line at 8 km s^-1 from S254-258 star forming region. A strong CS line was observed at 4 km s^-1 (AFGL 5180 and G188.9+0.9) and a weaker line (16.8 K km s^-1) was observed from the HII regions S254-258 at 7.5 km s^-1. The latter was observed in the CS(2-1) line by Zinchenko et al. (1994), at a velocity of 7.4 km s^-1. A Class II methanol maser was observed at the position of AFGL5180 with the offset $\Delta\alpha=6^{\prime\prime}$ and $\Delta\delta=5^{\prime\prime}$ (Caswell et al. 1995). GGD 12-15. The integrated intensity is 11.4 K km s^-1. It is a well known bipolar outflow with a wing range of 25 km s^-1 (Rodríguez et al. 1980; Rodríguez et al. 1982; Harvey et al. 1985; Little et al. 1990). The strong CS line has a main feature and is based on a pedestal. The line velocity, 11.7 km s^-1, is coinciding with the velocity of the bipolar outflow (11.6 km s^-1) (Rodríguez et al. 1982). No masers were detected, neither at 44 GHz (Bachiller et al. 1990), nor at 6.7 GHz (Slysh et al. 1998). NGC 2264. The molecular region NGC 2264 has a complex kinematic structure (Crutcher et al. 1978). NGC 2264F and NGC 2264G are two main regions (according to the CO line profile) - the southern and northern parts of the cloud, respectively. NGC 2264(IR) is located in the centre of the cloud and 4' north of a Bok globule (the Cone Nebula). A methanol maser at 44 GHz was detected by Haschick et al. (1990) at the position of NGC 2264(IR). A thermal methanol emission at 48 GHz was observed at the same position (Slysh et al. 1994) and absorption was observed at 6.7 GHz (Menten 1991). The youngest bipolar outflow (Outflow C.; Margulis & Snell 1988) out of the six observed in this region is close to the position of the observed CS line. The integrated intensity on the position of the IR source is 16.5 K km s^-1. The profile is Gaussian with a small blue-shifted wing. G9.62+0.19. An intense CS line with a strong pedestal was detected. The integrated intensity is 20.6 K km s^-1. There is no information about outflow activity. This is the strongest Class II methanol maser known (Menten 1991; Caswell et al. 1995). W33-Met. W33 is a giant and well studied HII region (Goldsmith & Mao 1983; Stier et al. 1984). The region contains H₂O and OH masers and far-infrared sources. No Class I methanol maser was detected in W33A and W33B (Haschick et al. 1990), but in both cases strong Class II methanol masers were detected by Menten (1991). Sources of Class I maser emission in W33-Met (Haschick et al. 1990) and a Class II weak maser (Menten 1991) were detected on the periphery of the central radio source W33C (a region of the brightest emission in both IR and CO). The rare methanol maser in the transition 9_-1-8_-2 E at 9.9 GHz was detected in W33-Met, which indicates high-density matter - up to 10⁶ cm^-3 (Slysh et al. 1993). Thermal methanol emission from W33-Met was not studied. From W33A and W33B thermal methanol emission was not detected (Slysh et al. 1994). A strong CS line was detected only at the positions of W33-Met and W33A, the integrated intensity is 41.5 K km s^-1 for W33-Met, 15.9 K km s^-1 for W33A, and 3.0 K km s^-1 for W33B. The velocity of the CS line at the position of both W33-Met and W33A (36 km s^-1) is the same as the main velocity of molecular gas, but the CS line from W33B has a velocity of -58 km s^-1, which corresponds to another group of gas velocities: the CO spectra of both W33A and W33B contain this group of velocities (Goldsmith & Mao 1983). The CS line profile consists of a single line, but the C³⁴S profile has two features, at 32 km s^-1 and at 36 km s^-1. These correspond to interferometric measurements in this source (Pratap & Menten 1992). G19.61-0.23. The CS line with integrated intensity 11.8 K km s^-1 was detected at 42.4 km s^-1. The source was included in our list as a Class I methanol maser, which was discovered by Bachiller et al. (1990). Caswell et al. (1995) discovered a weak Class II methanol maser at the position of a weak OH maser with $\Delta\alpha =9^{\prime\prime}$ and $\Delta\delta =42^{\prime\prime}$offset ($\sim$ HPBW). They pointed out, however, that the methanol maser was detected with a 39$^{\prime\prime}$ offset from the OH maser position measured with the VLA, which is in agreement with the position of a Class I methanol maser (Forster & Caswell 1989). L379IRS3. A broad and strong CS line described with a single Gaussian was detected. The integrated intensity is 12 K km s^-1. The bipolar outflow has strong wings (48.8 km s^-1) (Wilking et al. 1990). A strong Class I methanol maser was detected in this source at 44 GHz (Kalenskii et al. 1992). The velocity of the CS line, 17 km s^-1, is 1 km s^-1 less than the velocity of the maser component (18 km s^-1). A Class II methanol maser was discovered in this source in the 15-20 km s^-1 velocity interval by Caswell et al. (1995) at the position of an OH maser, which was discovered previously. G34.26+0.16. The profile of the CS line consists of a strong line at 57 km s^-1 and a weak component. The integrated intensity is 27.0 K km s^-1. The region is well studied in different molecules and transitions; this is a very dense region: $n_{\rm H_2}$ $\sim$10⁶ cm^-3 (Matthews et al. 1987; Fey et al. 1992; Carral & Welch 1992; Heaton et al. 1993). A Class I methanol maser line was detected at 44 GHz (Haschick et al. 1990). A Class II methanol maser was observed also at the position of the strong OH maser and ultracompact HII region in this source (Menten 1991; Caswell et al. 1995). The gas flow is displaced to the blue-shifted side of the spectrum with respect to the molecular cloud, and so is the ultracompact HII region. The ¹²CO emission line in the (1-0) transition was observed in the 40-70 km s^-1 velocity interval (Matthews et al. 1987). The cometary nebula G34.26+0.16 is displaced with respect to the molecular cloud and has the velocity 46 km s^-1 (Fey et al. 1992), but the velocity of the CS line ($\approx$59 km s^-1) is the same as for the molecular cloud (Fey et al. 1992). Class I methanol maser emission was observed at 56.4 km s^-1 and at 58.3 km s^-1 (Haschick et al. 1990). W49. This is a well studied region, which has strong bipolar outflow with a wing range of 60 km s^-1 (Scoville et al. 1986). It was observed in CS by Linke & Goldsmith (1980) at the same velocity (12.1 km s^-1), but the spectrum was not published. In our spectrum there is a double line with component velocities of 2.8 km s^-1 and 12.1 km s^-1 with integrated intensities 17.3 K km s^-1 and 5.8 K km s^-1, respectively. A weak maser component was observed in methanol at 44 GHz (Haschick et al. 1990) and at 6.7 GHz (Menten 1991). G45.07+0.13 and G45.47+0.05. These are compact HII regions from the catalogue of OH masers (Caswell & Haynes 1983). The CS line integrated intensities are 12.7 K km s^-1 and 10.4 K km s^-1, respectively. There is a small asymmetry in the line profile. A weak Class II methanol maser was observed (Menten 1991). W51. This is a well studied region of star formation (Turner et al. 1973; Liszt & Linke 1975; Linke & Goldsmith 1980; Pratap & Menten 1992). The parameters of the CS line, which were obtained previously, are in good agreement with the present results. It is a well known Class I and Class II source of maser emission (Haschick et al. 1990; Menten 1991). The CS line was observed at the position of both the Class II methanol maser W51 and the Class I methanol maser W51 e1/e2, which are very close. The CS line is stronger at the position of the Class I methanol maser, 114.7 K km s^-1 (72.4 K km s^-1 at the position of the Class II methanol maser). The velocities of the lines differ by 2 km s^-1. ON1. The integrated intensity is 11.1 K km s^-1. This is an isolated ultracompact HII region; the region of the first generation of star formation; one of the smallest in the Galaxy (approx. 0.02 pc) and one of the youngest (approx. 2000 years); the densest part of the molecular cloud has the density $n_{\rm H_2}\gt 10^4-10^5$ cm^-3; the region contains OH and H₂O masers; there is a bipolar outflow with a wing range of up to 30 km s^-1 (Israel & Wooten 1983; Zheng et al. 1985). The velocity of the main component of the CS profile, 11 km s^-1, is coinciding with the velocities of CO lines, of NH₃ lines, and of the group of OH masers. The velocity of the pedestal coincides with that of the H76$\alpha$ recombination line, 5.1 km s^-1 (Zheng et al. 1985). This is a source of Class I and Class II methanol maser emission; at 44 GHz the velocity is also approximately 11 km s^-1 (Haschick et al. 1990; Menten 1991).

  

Figure 1: Distributions of the CS(2-1) line intensities of bipolar outflows (BO), of Class I (MMI), and of Class II (MMII) methanol masers

ON2. There are two peaks of CO emission - central and north (Matthews et al. 1986). Bachiller et al. (1990) discovered a Class I methanol maser close to the position of the peak of CO emission and OH maser emission with $\Delta\delta =-36''$ offset. Menten (1991) discovered a Class II methanol maser at 6.7 GHz at the position of the Class I methanol maser. Thermal methanol emission was discovered at 48 GHz (Slysh et al. 1994). In our survey a strong CS line with an integrated intensity of 21.4 K km s^-1 was detected. The CO spectrum consists of three peaks at the position of the methanol maser. The CS profile has one component. No strong bipolar outflow has been detected (Matthews et al. 1986), but CO lines have wings at both the red and the blue-shifted side with a range of up to 30 km s^-1. DR21-West, DR21-Met C, W75N. This is a well known and well studied region in CS (Turner et al. 1973; Liszt & Linke 1975; Linke & Goldsmith 1980; Haschick et al. 1981; Plambeck & Menten 1990). The CO line from DR21 (bipolar outflow) was observed at the velocity of -3.0 km s^-1 and from W75N at -9 km s^-1. The red wing range of the CO line in DR21 is difficult to estimate due to the influence of the blue-shifted wing from W75N (Fisher et al. 1985). CS line parameters in our survey for DR21-West and DR21-Met C correspond to line parameters of the previous observations (Linke & Goldsmith 1980; Plambeck & Menten 1990). DR21-West, DR21-Met C, and W75N are the strongest Class I methanol masers (Haschick et al. 1990) and at the same time W75N is one of the strongest Class II methanol masers (Menten 1991). Integrated intensities of DR21-West, DR21-Met C, and W75N are 17.2 K km s^-1, 25.9 K km s^-1, and 22.7 K km s^-1, respectively. IRAS23032+5937. The integrated intensity is 10.5 K km s^-1. The CS line velocity corresponds to the velocity of the Perseus arm. The bipolar outflow has wings with a small range of 20 km s^-1  (Wouterloot et al. 1989). NGC 7538S. This is the southern part of a well known star forming region. There is no bipolar outflow (Fukui 1989). Haschick et al. (1990) discovered a group of methanol masers at this position. Emission lines are merged into a wide component at 44 GHz. The strong CS line profile is a simple Gaussian with a small asymmetry in the right wing. The CS integrated intensity is 35.9 K km s^-1.