Contents

A&A 485, 729-734 (2008)
DOI: 10.1051/0004-6361:200809472

A high-sensitivity 6.7 GHz methanol maser survey toward H2O sources[*]

Y. Xu1,2 - J. J. Li3 - K. Hachisuka3 - J. D. Pandian1 - K. M. Menten1 - C. Henkel1


1 - Max-Planck-Institute für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
2 - Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing 210008, PR China
3 - Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 20030, PR China

Received 28 January 2008 / Accepted 6 March 2008

Abstract
We present the results of a high sensitivity survey for 6.7 GHz methanol masers towards 22 GHz water masers using the 100 m Efflesberg telescope. A total of 89 sources were observed and 10 new methanol masers were detected. The new detections are relatively faint with peak flux densities of between 0.5 and 4.0 Jy. A nil detection rate from low-mass star forming regions enhances the conclusion that the masers are only associated with massive star formation. Even the faintest methanol maser in our survey, with a luminosity of $1.1 \times 10^{-9}~L_\odot$, is associated with massive stars, as inferred from its infrared luminosity.

Key words: masers - surveys - stars: formation - ISM: molecules

1 Introduction

The 51-60 A+ transition of methanol at 6.7 GHz produces the brightest known methanol masers. These masers are widespread in the Galaxy and more than 550 sources have been detected to date, including the compilations of Xu et al. (2003), Malyshev & Sobolev (2003) and Pestalozzi et al. (2005) and the new searches of Pandian et al. (2007) and Ellingsen (2007). The masers are not only a powerful tool to detect massive star-forming regions, but are also potentially useful for measuring distances using VLBI techniques, as has been demonstrated using their 12.2 GHz counterparts (Xu et al. 2006). Searches for 6.7 GHz methanol masers have been primarily targeted toward IRAS sources, OH masers, and ultracompact HII regions (e.g. Caswell et al. 1995; Walsh et al. 1997; Szymczak et al. 2000). In addition there have been a few blind surveys (Caswell et al. 1995; Ellingsen et al. 1996; Szymczak et al. 2002; Pandian et al. 2007). Unlike surveys in the Southern sky, most surveys in the Northern sky have a sensitivity limit of more than 1 Jy. The recent blind survey using the 305 m Arecibo radio telescope resulted in the discovery of numerous faint (<1 Jy) methanol masers (Pandian et al. 2007).


   
Table 1: The target sample of H2O maser sources.
00211+6549 $00259+5625^{\xi\dag } $ 00420+5530 00494+5617* 01134+6429 W3 (1)
02219+6152* $W3 (3)^{\xi}$ 02232+6138* 02395+6244 $02425+6851^{\dag }$ $02485+6902^{\dag }$
03101+5821 03167+5848 $ 03225+3034^{\dag }$ $03245+3002^{\dag }$ 04579+4703 05137+3919**
$05168+3634^{\xi}$ 05274+3345* $05302-0537^{\xi\dag }$ $05327-0457^{\xi}$ $KL IRC 2^{\xi}$ $05329-0508^{\xi\dag }$
$05329-0512^{\dag }$ 05335+3609 05345+3556 05345+3157 05358+3543* 05361+3539
05363+2454 $05375+3540^{\xi}$ NGC 2024$^{\xi}$ $05445+0020^{\dag }$ $05466+2316^{\xi\dag }$ 05553+1631
$06001+3014^{\xi\dag }$ $MON R2^{\xi}$ 06053-0622* 06055+2039* 06058+2138* 06061+2151*
$06067+2138^{\dag }$ 06099+1800* 06117+1350* 06127+1418 06291+0421 $06306+0437^{\dag }$
06437+0009 06446+0029** 06501+0143 $06579-0432^{\dag }$ $06584-0852^{\xi}$ 07006-0654
$18265+0028^{\dag }$ 18282-0951* 18290-0924* 18316-0602* 18319-0802** G23.44-0.18*
G23.01-0.41* OH24.7+0.2 18335-0713* 18341-0727* 18355-0650** 18359-0334
18360-0537 18385-0512 18403-0440** 18411-0338* 18434-0242* G29.91-0.05**
18449-0115* $W43 (M2)^{\xi}$ $18450-0148^{\xi}$ W43 (M3)* 18455-0200 18461-0136
18469-0132 18469-0041 18470-0049* 18479-0005** 18487-0015* 18507+0121*
18507+0110* 18517+0437* S76 W 18537+0749 $18538+0216^{\xi}$ $G35.05-0.52^{\xi}$
18556+0136* $18581+0409^{\xi}$ $18585+0407^{\xi}$ 18592+0108* $18593+0408^{\xi}$ $19008+0530^{\xi}$
19045+0813 19061+0652 19078+0901* $W49 S^{\xi}$ 19088+0902 19092+0841*
19095+0930* 19110+1045* 19181+1349 19207+1410 19209+1421 19213+1424*
19213+1723 $W51 M^{\xi}$ $19287+1816^{\dag }$ $19287+1845^{\xi\dag }$ 19303+1651* 19363+2018
19374+2352 19388+2357* 19410+2336* $19433+2743^{\dag }$ 19474+2637 19598+3324
$20050+2720^{\dag }$ 20056+3350 20062+3550* 20081+3122* 20110+3321* 20126+4104*
20144+3726 $20160+3911^{\xi}$ $20188+3928^{\xi}$ 20198+3716* ON 2 N $20215+3725^{\xi}$
$20227+4154^{\xi}$ $20231+3440^{\xi\dag }$ 20275+4001** $20286+4105^{\xi}$ W75 N* $W75 S(1)^{\xi}$
$W75 OH^{\xi}$ $W75 S(3)^{\xi}$ $21007+4951^{\xi\dag }$ 21008+4700 $21078+5211^{\xi}$ 21144+5430
21173+5450 $21206+5145^{\xi}$ 21228+5332 $G97.53+3.19^{\xi}$ 21306+5540** 21307+5049
21334+5039 21368+5502 21379+5106 21381+5000* $21391+5026^{\xi}$ $21391+5802^{\dag }$
21413+5442* 21418+6552 BFS 11-B $21479+5510^{\xi}$ 21527+5727 21553+5908
21558+5907 22142+5206 22176+6303** $22198+6336^{\dag }$ $22199+6322^{\dag }$ 22305+5803
22475+5939 $22517+6215^{\dag }$ 22543+6145* $22570+5912^{\xi}$ 23004+5642 23004+5642
$23030+5958^{\xi}$ 23116+6111* $S158^{\xi}$ 23138+5945    
* Previously known methanol masers.
** New detected methanol masers.
$^{\xi}$ Not observed due to constraints of observing time.
$^{\dag }$ Infrared luminosities less than 103 $L_{\odot}$.

Here, we report on the results of a sensitive survey for CH3OH masers targeted towards H2O maser sources, primarily in the Northern sky. Although there is no spatial correlation between 6.7 GHz CH3OH and 22 GHz H2O masers (Beuther et al. 2002; Breen et al. 2007), a high detection rate of both maser types in the same star forming regions indicates that the maser bearing phases for these two species overlap (Codella & Moscadelli 2000; Szymczak et al. 2005). The goals of our survey are two-fold: to find more CH3OH masers as astrometric targets for future VLBI observations to understand the spiral structure of the Galaxy. Further, since H2O masers are found towards both low-mass and high-mass star forming regions, we hope to verify the exclusive association of 6.7 GHz methanol masers with massive star formation.

2 Observations

The observations were made using the Effelsberg 100 m telescope[*] in February and May 2006. The rest frequency adopted for the 51-60 A+ transition was 6668.519 MHz (Breckenridge & Kukolich 1995). For the February observations, the spectrometer was configured to have a 10 MHz bandwidth with 4096 spectral channels yielding a spectral resolution of 0.11 km s-1 and a velocity coverage of 450 km s-1. In May, a bandwidth of 20 MHz was used giving a spectral resolution of 0.22 km s-1 and a velocity coverage of 900 km s-1. The half-power beam width was $\sim$2' and the telescope has an rms pointing error of 10''. The observations were made in position switched mode. The system temperature was typically around 35 K during our observations. The flux density scale was determined by observations of NGC 7027 (Ott et al. 1994). The absolute calibration for flux density is estimated to be accurate to $\sim$10%. The integration time on source was typically three minutes, which resulted in a mean rms noise level of $\sim$0.1-0.2 Jy in the spectra. When a source was detected, the integration time was increased to around 8 min (at the same position) with a velocity resolution of 0.11 km s-1 to obtain spectra with high signal to noise ratio.

The target sources were H2O masers selected from the Arcetri catalog (Comoretto et al. 1990; Brand et al. 1994), and are shown in Table 1. The sources were selected based on associations with star forming regions or HII regions, with declinations $\delta \geq
-10^{\circ}$. This gave us a sample of 178 sources of which 17 sources may be associated with low-mass young stellar objects (YSOs) with infrared luminosities less than $10^{3}~L_{\odot}$. 154 out of 178 sources are associated with IRAS point sources. We then excluded sources that had previous detections of methanol masers, which reduced our sample size to 131 sources. Of this, we observed a total of 89 sources within our observing time constraints. For all sources, the spectrometer was centered on the velocity of peak emission of the water maser. However, the wide velocity coverage precludes the possibility of methanol masers being missed due to their velocities being significantly offset from that of the water masers.

3 Results

Our observations resulted in the discovery of 10 new methanol masers, the properties of which are listed in Table 2. Since we did not attempt to refine the position of the methanol masers using a grid of observations, the positions quoted in Table 2 could have an error as high as $\sim$1'. The maser luminosities quoted in Table 2 are calculated from the integrated flux density assuming isotropic emission. Details of water maser sources that had non-detections of methanol masers are indicated in Table 3, which is available on-line. The peak flux densities of the methanol masers detected in our survey range from 0.5 to 4.0 Jy. Five sources are located beyond the solar circle, which is a significant addition to the number of such sources in the northern sky. It is interesting that the kinematic distance to the source 05137+3919 puts it at a distance of $\sim$14 kpc from the Sun and 20 kpc from the Galactic center. This is one of the farthest methanol masers (in terms of distance from the Galactic center) in the outer Galaxy, although the uncertainties in the rotation curve at these galactrocentric radii, and peculiar motions such as that observed in W3OH (Xu et al. 2006) translate into significant uncertainties in the kinematic distance. Measuring parallax distances to sources like 05137+3919 will be useful for measuring the rotation speed of the Galaxy at large galactocentric radii.


 

 
Table 2: Details of the newly detected 6.7 GHz CH3OH masers. The first column lists the source name (associated IRAS source or the galactic coordinates). The next two columns give their J2000 equatorial coordinates. Column (4) shows the distances. Columns (5) and (6) present the integrated flux density and peak flux density. Columns (7) and (8) show the radial velocity of peak emission and the radial velocity range. Columns (9)-(11) present the infrared, CH3OH and H2O luminosities. The maser luminosities are calculated assuming isotropic emission.
$\textstyle \parbox{20mm}{%
Source \\ name}$ $\textstyle \parbox{17mm}{%
RA(2000)\\
\mbox{${\rm (^h\;\;\;^m\;\;\;^s)}$ }}$ $\textstyle \parbox{17mm}{%
Dec(2000) \\
\mbox{$(\hbox{$^\circ$ }\;\;\;\hbox{$^\prime$ }\;\;\;\hbox{$^{\prime\prime}$ })$ }}$ $\textstyle \parbox{10mm}{%
$D$\space \\ (kpc)}$ $\textstyle \parbox{15mm}{%
$S_{\rm i}$\\ (Jy~km~s$^{-1}$ )}$ $\textstyle \parbox{10mm}{%
$S_{\rm p}$\\ (Jy)}$ $\textstyle \parbox{10mm}{%
$v_{\rm p}$\\ (km~s$^{-1}$ )}$ $\textstyle \parbox{12mm}{%
$\Delta v$\\ (km~s$^{-1}$ )}$ $\textstyle \parbox{10mm}{%
\par $L_{\rm IR}$\\ ($L_{\odot}$ )}$ $\textstyle \parbox{12mm}{%
\par $L_{{\rm CH}_{3}{\rm OH}}$\\ ($L_{\odot}$ )}$ $\textstyle \parbox{10mm}{%
\par $L_{{\rm H}_{2}{\rm O}}$\\ ($L_{\odot}$ )}$
05137+3919 $05\ 17\ 13.3$ +39 22 14 12.01 0.7 1.5 -16.2 -21.1, -16.0 6.1(4) 7.0(-7) 2.2(-4)
06446+0029 $06\ 47\ 12.9$ +00 26 07 6.01 2.8 1.6 48.6 42.7, 50.0 2.3(4) 7.0(-7) 1.5(-4)
18319-0802 18 34 38.2 -07 59 35 $2.8^{\ast}$ 2.2 2.1 35.7 31.0, 45.2 7.2(3) 1.2(-7) 4.5(-6)
18355-0650 18 38 14.3 -06 47 47 5.74 4.2 3.9 58.2 56.6, 62.1 7.4(5) 9.4(-7) 7.1(-6)
18403-0440 18 43 01.1 -04 36 41 3.34 0.3 1.0 20.1 19.8, 20.4 4.1(3) 2.3(-8) 3.2(-6)
G29.91-0.05 18 46 05.9 -02 42 27 $7.1^{\ast}$ 7.8 2.9 104.3 93.4, 105.3 -- 2.7(-6) 3.3(-5)
18479-0005 18 50 31.1 -00 01 54 13.02 1.3 1.5 27.4 24.9, 28.3 1.6(6) 1.5(-6) 9.0(-5)
20275+4001 20 29 24.9 +40 11 21 2.03 1.7 4.0 -6.9 -7.4, -6.5 6.7(4) 4.7(-8) 1.5(-5)
21306+5540 21 32 13.0 +55 52 56 8.61 1.5 1.1 -69.9 -73.7, -68.0 1.4(5) 7.8(-7) 9.9(-4)
22176+6303 22 19 18.3 +63 18 48 0.96 0.2 0.5 -2.0 -2.3, -1.1 2.4(4) 1.1(-9) 4.8(-7)
References for the distances:
1 Wouterloot et al. (1993). 2 Palagi et al. (1993). 3 Anglada et al. (1996). 4 van der Tak et al. (1999).
5 Wu et al. (2006). 6 Crampton & Fisher (1974).
$^{\ast}$ Heliocentric near kinematic distances.


3.1 Individual sources

The spectra of the CH3OH masers detected in our survey are shown in Fig. 1. The spectra have a velocity resolution of 0.11 km s-1. Here we present notes on individual sources.

05137+3919. There are two features that are separated by about 4.5 km s-1. The stronger feature is at an LSR velocity of -3.9 km s-1, while the weaker feature has a flux density of only 0.35 Jy. This region is associated with a 3.6 cm continuum source (Molinari et al. 2002).

06446+0029. There are at least five features over a velocity range of over 7 km s-1. The feature at 48.6 km s-1 is the strongest one. There is near infrared emission in this region as seen in the 2MASS data, and a non-detection of SiO masers (Harju et al. 1998).

18319-0802. There are several features spanning a velocity range of over 15 km s-1. The weakest feature is only about 0.2 Jy. An ultracompact (UC) HII region, separated by about 40'', could be associated with this region (Becker et al. 1994).

18355-0650. There are at least five features spanning a velocity range of about 6 km s-1. An UC HII region, separated by 17'', is associated with this region (Becker et al. 1994).

G29.91-0.05. Features span from 93.4 to 105.3 km s-1 with multiple features being blended together. There are at least two compact HII regions associated with this region within 2' (Wood & Churchwell 1989a; Becker et al. 1994). One of them, separated by about 80'', could be associated with this region.

18403-0440. This source primarily shows a single feature at +20.1 km s-1. No observations of this region have been reported, except for near infrared emission from the 2MASS data.

18479-0005. Walsh et al. (1997) did not detect maser emission within their 1 Jy limit (3$\sigma$). There are several features crowded within a velocity range of only 2 km s-1. A UC HII region is associated with this source (Kurtz et al. 1994).

20275+4001. This source displays a single feature at -6.9 km s-1, which matches the H13CO+ (4-3) peak of Hasegawa & Mitchell (1995). A bipolar outflow and a continuum source were also detected in this region (Hasegawa & Mitchell 1995; Trinidad et al. 2003). Mid-infrared images show that this source is surrounded by an optically thick dusty envelope (Marengo et al. 2000).

21306+5540. There are clearly five features in this source. Except for near infrared emission from the 2MASS data, no other observations have been reported in this region.

22176+6303 (S140). This source shows a double peaked structure and is the weakest source detected in this survey. At a distance of 910 pc (Crampton & Fisher 1974), the maser luminosity is very low ( $1.1~\times~10^{-9}~ L_{\odot}$). However, its infrared luminosity indicates that it is still associated with a massive star forming region (Table 2). A faint continuum source (Kurtz et al. 1994) and a CO outflow (Minchin et al. 1993) are associated with the region.


  \begin{figure}
\par\begin{tabular}{cccc}
\includegraphics[width=3.8cm,angle=-90]...
...udegraphics[width=3.8cm,angle=-90]{9472f1j.ps} &
\\
\end{tabular}
\end{figure} Figure 1: Spectra of the new 6.7-GHz CH3OH maser detections. The spectral resolution is 0.11 km s-1.

4 Discussion

We detected 10 methanol masers by targeting 89 sources, which results in a detection rate of $\sim$11%. However, to compare the statistics of H2O and methanol masers, we have to consider the entire original sample of 178 sources that satisfied our selection criteria ( $\delta \geq
-10^{\circ}$). 47 sources have previous detections of methanol masers, while 42 sources were not observed due to constraints of observing time. Hence, the overall detection rate of methanol masers in a water maser sample is at least $\sim$32%. Our sample includes 17 sources that are associated with low-mass YSOs and 10 of them were observed in this survey. A nil detection rate from these sources adds to the results of Minier et al. (2003) and Bourke et al. (2005), suggesting that 6.7 GHz methanol masers are only associated with massive star forming regions. Therefore, excluding the low-mass YSOs, the detection rate is at least $\sim$35%.

Figure 2 shows the color-color diagram of the IRAS sources associated with the sample of water masers. The box on the upper right corner shows the Wood & Churchwell (1989b, hereafter WC) criteria used to identify embedded massive stars and ultracompact HII regions. The stars and circles show the old and new methanol maser detections respectively. 113 out of 154 sources satisfy the WC criteria, of which 40 sources have methanol maser emission. Since 21 sources satisfying the WC criteria were not observed, the detection rate among IRAS sources satisfying WC criteria and hosting H2O masers is at least $\sim$35%. This detection rate is better than that of a survey based purely on IRAS sources satisfying WC criteria (e.g. see discussion of Ellingsen et al. 1996). It is to be cautioned that not all of these cases are true associations, as the IRAS source may point to the brightest far infrared source in the star forming region, and better positions for methanol masers may preclude some of the current associations (Ellingsen 2006; Pandian & Goldsmith 2007). There are also 12 methanol masers whose IRAS colors do not satisfy WC criteria. It can also be seen from Fig. 2 that there is no distinction between the IRAS sources associated with the new detections, and those associated with the previous detections (which are brighter), nor is there any distinction between the colors of sources with and without methanol masers. Thus, the low detection rate in our survey (11%) is not due to any systematic differences between in the infrared properties of the sources in our survey (versus the sources associated with previous detections of methanol masers). The lack of distinction of the IRAS source properties of bright versus faint methanol masers is also consistent with the observation of Pandian & Goldsmith (2007).


  \begin{figure}
\par\includegraphics[width=6.5cm,clip]{9472f2.eps}\end{figure} Figure 2: IRAS color-color diagram for 154 sources. The box in the upper right corner delineates the WC criteria for UCHII regions. Sources with no methanol maser detections are shown with open triangles. Previous and new detections of methanol masers are shown with stars and circles respectively.


  \begin{figure}
\par\begin{tabular}{ccc}
\includegraphics[width=7cm,clip]{9472f3a.eps} &
\includegraphics[width=7cm,clip]{9472f3a.eps} &
\end{tabular}\end{figure} Figure 3: Left panel - a) Methanol and water maser luminosities versus the infrared luminosity calculated from the IRAS data. The circles and triangles show the methanol and water masers respectively. Water masers without any methanol maser associations are excluded. Right panel - b) Water maser versus methanol maser luminosity. Previous and new detections of methanol masers are shown with stars and circles respectively.

There is only one detection with a peak flux density less than 1 Jy (this is also the only such source in the entire sample including previous detections). However, our sample is not from an unbiased survey, and hence it is not possible to discuss the implications of this in the context of the methanol maser population in the Galaxy. However, we note that this is consistent with the results of the simulation of van der Walt (2005) and the results of the Pandian et al. (2007). van der Walt (2005) using Monte Carlo simulations determined the completeness of surveys as a function of their flux densities, while the observational results of Pandian et al. (2007) corroborate the theoretical analysis with regard to the total number of methanol masers in the Galaxy. Moreover, Pandian et al. (2007) found that the distribution of peak flux densities drops at flux densities below $\sim$1 Jy. This could be one of the reasons why we did not detect many sources below 1 Jy. Figure 3a (left panel) shows the luminosity distributions for both maser types as a function of the infrared luminosity of the host IRAS sources and Fig. 3b (right panel) shows the the maser luminosities of the two species plotted against each other. Only sources that show emission in both species are shown in Fig. 3. The infrared flux $F_{\rm IR}$ (used to determine the infrared luminosity $L_{\rm IR}$) is calculated using the formula below (Casoli et al. 1986).

\begin{displaymath}F_{\rm IR} (10^{-13} ~\rm {W~m}^{-2}) = 1.75\left(\frac{{\it ...
... + \frac{{\it F}_{60}}{3.9} + \frac{{\it F}_{100}}{9.9}\right)
\end{displaymath} (1)

where F12, F25, F60 and F100 refer to the IRAS fluxes in 12, 25, 60 and 100 $\mu$m respectively. The distances are taken from the literature. For sources with no published distance, the near kinematic distance, computed from the peak velocity of 6.7 GHz emission using the galactic rotation curve of Wouterloot & Brand (1989), assuming R0 = 8.5 kpc and $\Theta_{0} = 220$ km s-1, is adopted. The near kinematic distance is used because it seems realistic (Sobolev et al. 2005).

Figure 3a shows that there is reasonably good correlation seen between the infrared luminosity and that of both H2O (Correlation coefficient R = 0.64, Probability p < 0.0001) and CH3OH masers (R = 0.56, p < 0.0001). This correlation has been found in the past by a number of groups (e.g. Wouterloot & Walmsley 1986; Szymczak et al. 2005), and the vertical scatter is normally attributed to the variability of the masers. However, it is not clear as to whether this correlation is physically meaningful. On the one hand, both maser types are spatially separated and have very different excitation requirements. H2O masers are collisionally pumped and occur in shocks along outflows, while CH3OH masers are produced by radiative pumping and originate from circumstellar disks or envelopes. Thus, it is not clear whether the correlation seen in Fig. 3a arises from a physical connection between the far-infrared luminosity and maser luminosity. Figure 3b shows that there is also a good correlation between methanol and water maser luminosities (R = 0.63, p < 0.0001). Since there is no physical connection between the two quantities, it is possible that the correlations are just a distance squared effect, as suggested by Palla et al. (1991) for the correlation between the water maser and the infrared luminosity. It is also curious that the water masers in our sample (that are associated with methanol masers) are an order of magnitude more luminous than the ones associated with the methanol maser sample of Szymczak et al. (2005). Some methanol masers detected in our survey have low luminosities with the faintest source having a maser luminosity of only 10-9$L_{\odot}$. However, the infrared luminosities of all sources range from 103 to 106 $L_{\odot}$, indicating that they are associated with massive star formation.

5 Summary

A survey for 6.7 GHz CH3OH masers was carried out toward 89 water masers and 10 new sources were detected, five of which are located beyond the solar circle. A nil detection rate from low-mass star forming regions enhances the conclusion that 6.7 GHz methanol masers are only associated with massive star forming regions. There is only one source maser with a peak flux density less than 1 Jy, which could be due to the nature of the methanol maser luminosity function. This paper presents only the results of the survey. In a separate paper, we will report on the environment around the masers, using ongoing observations of various molecules such as CO, HCO+, CN and NH3. This will also elucidate of any differences between faint masers and their bright counterparts.

Acknowledgements
We would like to thank the anonymous referee for many useful suggestions and comments, which improved this paper. This research is supported by NSFC under grants 10673024, 10733030, 10703010 and 10621303, and NBRPC (973 Program) under grant 2007CB815403.

References

 

  
6 Online Material


   
Table 3: H2O maser sources that have non detections for 6.7 GHz CH3OH maser emission. The columns show the source name, J2000 coordinates, central velocity for the spectrometer, $v_{\rm c}$, velocity range covered by the spectrometer, $v_{\rm min}$ and $v_{\rm max}$, the velocity resolution, $\delta (v)$, and the rms noise in the spectrum ($1\sigma $ limit on the maser flux density).

$\textstyle \parbox{19mm}{%
Source \\ name}$
$\textstyle \parbox{17mm}{%
RA(2000)\\
\mbox{${\rm (^h\;\;\;^m\;\;\;^s)}$ }}$ $\textstyle \parbox{17mm}{%
Dec(2000) \\
\mbox{$(\hbox{$^\circ$ }\;\;\;\hbox{$^\prime$ }\;\;\;\hbox{$^{\prime\prime}$ })$ }}$ $\textstyle \parbox{14mm}{%
$v_{\rm c}$\\ (km~s$^{-1}$ )}$ $\textstyle \parbox{18mm}{%
$v_{\rm min}$\\ (km~s$^{-1}$ )}$ $\textstyle \parbox{18mm}{%
$v_{\rm max}$\\ (km~s$^{-1}$ )}$ $\textstyle \parbox{14mm}{%
$\delta(v)$\\ (km~s$^{-1}$ )}$ $\textstyle \parbox{18mm}{%
rms\\ (Jy)}$

00211+6549
00 23 58.1 +66 06 03 -71.1 -296 154 0.11 0.14
00420+5530 00 44 57.5 +55 47 18 -47.8 -273 177 0.11 0.14
01134+6429 01 16 47.2 +64 45 39 -46.9 -272 178 0.11 0.10
W3 (1) 02 25 28.2 +62 06 58 -40.0 -265 185 0.11 0.10
02395+6244 02 43 29.1 +62 57 00 -67.1 -292 158 0.11 0.10
02425+6851 02 47 00.2 +69 04 11 -10.4 -461 440 0.22 0.05
02485+6902 02 53 07.2 +69 14 36 -10.4 -461 440 0.22 0.05
03101+5821 03 14 04.7 +58 33 08 -38.5 -489 412 0.22 0.05
03167+5848 03 20 44.3 +58 59 33 -55.6 -506 395 0.22 0.05
03225+3034 03 25 35.5 +30 45 21 2.6 -223 228 0.11 0.19
03245+3002 03 27 39.0 +30 13 00 4.4 -446 455 0.22 0.05
04579+4703 05 01 39.7 +47 07 23 -17.8 -243 207 0.11 0.10
05329-0512 05 35 27.5 -05 09 37 7.5 -218 233 0.11 0.19
05335+3609 05 36 52.5 +36 10 49 -17.3 -468 433 0.22 0.05
05345+3556 05 37 57.8 +35 58 41 -20.7 -471 430 0.22 0.05
05345+3157 05 37 53.1 +31 59 35 -20.0 -245 205 0.11 0.19
05361+3539 05 39 27.7 +35 40 43 -18.0 -469 433 0.22 0.05
05363+2454 05 39 28.2 +24 56 32 13.9 -437 464 0.22 0.05
05445+0020 05 47 05.4 +00 21 50 15.9 -209 241 0.11 0.19
05553+1631 05 58 13.9 +16 32 00 -7.6 -233 218 0.11 0.14
06067+2138 06 09 48.0 +21 38 11 3.2 -447 454 0.22 0.05
06127+1418 06 15 34.6 +14 17 10 11.3 -214 237 0.11 0.19
06291+0421 06 31 48.1 +04 19 31 9.6 -216 235 0.11 0.19
06306+0437 06 33 16.4 +04 34 57 10.1 -440 461 0.22 0.05
06437+0009 06 46 15.6 +00 06 19 33.6 -192 259 0.11 0.19
06501+0143 06 52 45.6 +01 40 15 52.0 -399 503 0.22 0.05
06579-0432 07 00 23.1 -04 36 38 26.3 -424 477 0.22 0.05
07006-0654 07 03 05.1 -06 58 28 29.1 -421 480 0.22 0.05
18265+0028 18 29 05.8 +00 30 36 5.3 -220 231 0.11 0.19
OH24.7+0.2 18 35 29.9 -07 13 10 25.9 -199 251 0.11 0.14
18359-0334 18 38 34.3 -03 32 06 -45.5 -271 180 0.11 0.14
18360-0537 18 38 41.6 -05 35 06 104.4 -121 330 0.11 0.19
18385-0512 18 41 12.0 -05 09 07 18.0 -207 243 0.11 0.24
18455-0200 18 48 08.8 -01 56 54 104.3 -130 320 0.11 0.19
18461-0136 18 48 45.2 -01 33 12 18.6 -207 244 0.11 0.19
18469-0132 18 49 32.8 -01 29 04 93.6 -132 319 0.11 0.24
18469-0041 18 49 32.2 -00 38 01 92.5 -133 318 0.11 0.19
S76 W 18 55 58.7 +07 53 42 -3.6 -229 222 0.11 0.19
18537+0749 18 56 11.8 +07 53 24 31.7 -194 257 0.11 0.19
19045+0813 19 06 59.7 +08 18 42 16.9 -208 242 0.11 0.19
19061+0652 19 08 36.8 +06 57 02 71.9 -153 297 0.11 0.19
19088+0902 19 11 15.8 +09 07 27 -5.1 -230 220 0.11 0.19
19181+1349 19 20 31.2 +13 55 24 34.1 -191 259 0.11 0.19
19207+1410 19 23 01.2 +14 16 40 68.6 -157 294 0.11 0.29
19209+1421 19 23 10.9 +14 26 38 52.1 -173 277 0.11 0.24
19213+1723 19 23 37.0 +17 28 59 -26.8 -252 198 0.11 0.14
19287+1816 19 30 58.3 +18 22 28 24.5 -201 250 0.11 0.19
19363+2018 19 38 31.6 +20 25 21 36.0 -189 261 0.11 0.19
19374+2352 19 39 33.2 +23 59 55 39.4 -186 265 0.11 0.19
19433+2743 19 45 20.8 +27 50 51 19.9 -205 245 0.11 0.19
19474+2637 19 49 32.5 +26 45 14 20.5 -205 246 0.11 0.19
19598+3324 20 01 45.5 +33 32 41 -19.4 -245 206 0.11 0.24
20050+2720 20 07 06.7 +27 28 53 0.9 -224 226 0.11 0.19
20056+3350 20 07 31.5 +33 59 39 10.4 -215 236 0.11 0.19
20144+3726 20 16 15.8 +37 35 40 -56.7 -507 394 0.22 0.05
ON 2 N 20 21 43.9 +37 26 39 2.4 -448 453 0.22 0.05
21008+4700 21 02 32.3 +47 12 36 -49.6 -500 401 0.22 0.05
21144+5430 21 15 55.8 +54 43 31 -83.2 -534 367 0.22 0.05
21173+5450 21 18 53.1 +55 03 19 -82.8 -533 368 0.22 0.05
21228+5332 21 24 29.0 +53 45 34 -97.4 -548 353 0.22 0.05
21307+5049 21 32 31.4 +51 02 23 -46.7 -272 179 0.11 0.10
21334+5039 21 35 09.1 +50 53 09 -43.9 -269 181 0.11 0.19
21368+5502 21 38 25.8 +55 16 33 -83.2 -308 142 0.11 0.19
21379+5106 21 39 40.5 +51 20 32 -41.6 -267 184 0.11 0.19
21391+5802 21 40 42.3 +58 16 10 -5.0 -230 220 0.11 0.10
21418+6552 21 43 04.0 +66 05 57 -31.2 -256 194 0.11 0.10
BFS 11-B 21 43 06.0 +66 06 57 -14.9 -240 210 0.11 0.05
21527+5727 21 54 21.5 +57 41 14 -70.3 -296 155 0.11 0.10
21553+5908 21 56 59.3 +59 22 39 -87.8 -538 363 0.22 0.05
21558+5907 21 57 24.5 +59 21 56 -89.6 -315 136 0.11 0.05
22142+5206 22 16 10.4 +52 21 25 -37.4 -488 413 0.22 0.05
22198+6336 22 21 27.5 +63 51 46 -21.3 -247 204 0.11 0.10
22199+6322 22 21 33.2 +63 37 22 -9.0 -460 442 0.22 0.05
22305+5803 22 32 24.2 +58 18 58 -53.0 -278 172 0.11 0.19
22475+5939 22 49 29.5 +59 55 37 -54.5 -280 171 0.11 0.10
22517+6215 22 53 43.4 +62 31 46 -9.0 -234 216 0.11 0.19
23004+5642 23 02 34.9 +56 58 55 -53.5 -504 397 0.22 0.05
23004+5642 23 02 32.1 +56 57 51 -53.5 -279 172 0.11 0.19
23138+5945 23 16 04.4 +60 01 34 -44.5 -270 181 0.11 0.19



Copyright ESO 2008