1 INTRODUCTION
Methanol is an asymmetric top molecule with hindered internal rotation (Lees Reference Lees1973), a combination which produces a rich rotational spectrum at centimetre and millimetre wavelengths. Methanol is also a relatively common molecule in some interstellar environments. Two different types of methanol masers are observed in astrophysical environments, known as class I and class II. Class I methanol masers are produced by outflows and other low-velocity shocks, the most common transitions are the 36 and 44 GHz and the emission is distributed over regions of up to 1 pc (e.g. Voronkov et al. Reference Voronkov, Caswell, Ellingsen, Green and Breen2014). Class II methanol masers are produced by far infrared and submillimetre radiation, they are found close to young high-mass stars and the most common transitions are at 6.7 and 12.2 GHz. The empirical division of the maser transitions is consistent with maser modelling which shows that the class I masers arise in regions where collisional processes dominate (e.g. Sobolev et al. Reference Sobolev, Chapman and Baan2007; McEwen, Pihlström, & Sjouwerman Reference McEwen, Pihlström and Sjouwerman2014), whilst the class II masers are radiatively pumped (e.g. Sobolev & Deguchi Reference Sobolev and Deguchi1994; Cragg, Sobolev, & Godfrey Reference Cragg, Sobolev and Godfrey2005). Class I methanol masers are predominantly associated with high-mass star formation regions, but have been observed towards low-mass star formation regions (Kalenskii et al. Reference Kalenskii, Johansson, Bergman, Kurtz, Hofner, Walmsley and Slysh2010), supernova remnants (Pihlström et al. Reference Pihlström, Sjouwerman, Frail, Claussen, Mesler and McEwen2014), and starburst galaxies (Ellingsen et al. Reference Ellingsen, Chen, Qiao, Baan, An, Li and Breen2014; Chen et al. Reference Chen, Ellingsen, Baan, Qiao, Li, An and Breen2015). In contrast, class II methanol masers are only observed associated with high-mass star formation regions (Breen et al. Reference Breen, Ellingsen, Contreras, Green, Caswell, Stevens, Dawson and Voronkov2013).
To date, more than 30 different class II methanol maser transitions have been observed (see Ellingsen et al. Reference Ellingsen, Sobolev, Cragg and Godfrey2012, and references therein). However, compared to the common 6.7 and 12.2 GHz class II methanol transitions, the others are much less common, and where they are observed are weaker than the 6.7 and 12.2 GHz emission (e.g. Caswell et al. Reference Caswell, Yi, Booth and Cragg2000; Ellingsen et al. Reference Ellingsen, Cragg, Lovell, Sobolev, Ramsdale and Godfrey2004; Cragg et al. Reference Cragg, Sobolev, Caswell, Ellingsen and Godfrey2004; Ellingsen et al. Reference Ellingsen, Breen, Sobolev, Voronkov, Caswell and Lo2011). The output from the methanol maser models includes predictions of the brightness temperature for each of the different transitions. The strong, common class II methanol maser transitions (such as the 6.7 and 12.2 GHz) are predicted to produce intense maser emission for a wide range of gas temperatures, densities, and methanol column densities (Sobolev, Cragg, & Godfrey Reference Sobolev, Cragg and Godfrey1997b; Cragg et al. Reference Cragg, Sobolev and Godfrey2005). In contrast, the rarer, weaker methanol transitions are typically inverted over a much narrower range of physical conditions, and the majority of transitions are not expected to be masers. So the presence (or absence) of the rarer, weaker transitions then provides more stringent tests of maser models (Cragg et al. Reference Cragg, Sobolev, Caswell, Ellingsen and Godfrey2004). The relationship between the measured flux density S for emission and the brightness temperature
$T_{\text{b}}$
of a source is given by the equation
$$\begin{equation}
S[{\rm Jy}] = 5.65 \times 10^{-7}\ \nu ^2[{\rm GHz}]\ \theta ^2[{\rm arcsec}]\ T_{\text{b}}[{\rm K}],
\end{equation}$$
where ν is the frequency of the observations and θ is the angular scale of the emission region. For a source to be detectable at a particular frequency requires either a high brightness temperature, or emission over a large angular scale. Maser sources generally fall into the first of these categories with strong 6.7 and 12.2 GHz methanol masers having brightness temperatures in excess of 1010 K (e.g. Menten et al. Reference Menten, Reid, Pratap, Moran and Wilson1992). The majority of maser searches are made with single-dish telescopes with moderate (around 1 Jy) sensitivity limits; however, whilst these are efficient for detecting strong masers, they do not place strong upper limits on moderate or low brightness temperature masers (≲ 108 K). Sensitive, high resolution observations of some rare class II methanol maser transitions have shown that masers with brightness temperatures of less than 108 K are likely present in some sources (Krishnan et al. Reference Krishnan, Ellingsen, Voronkov and Breen2013). So rigorous tests of maser models require, sensitive, high resolution observations in order to detect, or limit moderate and low brightness temperature masers. The Australia Telescope Compact Array (ATCA) is an ideal instrument for undertaking such observations and in this paper, we report the results of a search for a number of methanol maser transitions which are predicted to exhibit weak maser emission under some physical conditions.
In order to test and refine maser models and potentially the physical conditions in the observed star formation regions, we selected a number of potential class II methanol maser transitions in the frequency range 5–9 GHz. A search for potential new maser transitions is a compromise between the number of different sources observed and the sensitivity of the observations. For the primary target transitions, we made observations of four high-mass star formation regions which are known to exhibit moderately strong emission from a range of different class II methanol maser transitions. For the secondary target transitions, we made observations of a single source G 345.01 + 1.79, as there are more class II methanol maser transitions detected towards that source than any other (Ellingsen et al. Reference Ellingsen, Sobolev, Cragg and Godfrey2012).
2 OBSERVATIONS AND DATA REDUCTION
We used the ATCA in the 6A configuration (baselines ranging from 337 to 5939 m) to undertake sensitive observations of five different methanol (CH3OH) transitions in the 5–9-GHz frequency range. The observations were made over a period of 13 h on 2000 August 30. The primary target transitions were the 124–133 A− and 124–133 A+ transitions, which have rest frequencies of 7.682232(50) and 7.830864(50) GHz, respectively (Tsunekawa et al. Reference Tsunekawa, Ukai, Toyama and Takagi1995, the numbers in brackets represent the uncertainty in the least significant figures). These two transitions were observed towards four high-mass star formation regions (G 339.88-1.26, G 345.01+1.79, NGC6334F, and W48), which all exhibit strong class II methanol maser emission in multiple transitions. The pointing centre for the observations of each source and the peak velocity of the class II methanol maser transitions is given in Table 1. For each transition, observations consisted of a series of scans of 5 min for each target source spread over a range of hour angles. Each scan on a target source was both preceded and followed by a 1 min scan on a nearby phase calibrator. The total observing time for each of the four target maser sources is around 45 min for each of the primary transitions.
Table 1. Class II methanol maser sources observed in the 124–133 A− and 124–133 A+ transitions, with the measured RMS noise for each transition, respectively. Distance references a Krishnan et al. (Reference Krishnan2015); b Green & McClure-Griffiths (Reference Green and McClure-Griffiths2011); c Wu et al. (Reference Wu2014).
Observations were also undertaken of secondary transitions 31A+–31A−, 17−2–18−3 E (vt = 1), and 41A+–41A− which have rest frequencies of 5.0053207(6), 6.181589(153), and 8.341622(4) GHz, respectively (Breckenridge & Kukolich Reference Breckenridge and Kukolich1995; Xu & Lovas Reference Xu and Lovas1997). These three transitions were observed only towards the G 345.01+1.79 star formation region with onsource durations of 4.2 min for each transition. Of the five transitions observed, the only one which has been detected astronomically is the 31A+–31A−, for which Robinson et al. (Reference Robinson, Brooks, Godfrey and Brown1974) report weak, broad emission towards Sgr B2.
The correlator was configured to the FULL_4_1024_POL mode which has 1 024 spectral channels across a 4 MHz bandwidth, with all polarisation products recorded. This corresponds to a velocity coverage of approximately 155 km s−1 at a frequency of 7.7 GHz and velocity resolution of approximately 0.18 km s−1. The data were reduced using miriad, applying the standard data reduction procedures for ATCA observations. The primary flux density calibration was with respect to the standard calibrator PKS B1934-638 using the in-built scale within miriad (Reynolds Reference Reynolds1994). The absolute flux density calibration is expected to be accurate to better than 10%. PKS B1934-638 was also used for bandpass calibration.
3 RESULTS
We imaged each of the four sources using the calibrated 4 MHz datasets for the 124–133 A− and 124–133 A+ transitions. Three of the four sources (all except G 339.88-1.26) have detectable radio continuum emission in both transitions. For these sources, we undertook self-calibration using a model formed from the cleaned images of the radio continuum emission. We found that a single iteration of phase-only self-calibration significantly improved the signal-to-noise ratio in the continuum images and we then used continuum subtraction to extract a spectral line dataset. We imaged a 10 km s−1 velocity range covering all the class II methanol maser emission in each source at a velocity resolution of 0.2 km s−1(see Table 1). Inspection of the image cubes for each of the sources did not reveal any emission in either of the two primary target transitions in any of the four source observed. The RMS noise level in 0.2 km s−1 spectral channels were in the range 27–37 mJy beam−1 for all sources and are listed in Table 1. Figure 1 shows the continuum images formed from the 124–133 A+ dataset after self-calibration for G 345.01+1.79 and NGC6334F. We do not show the continuum image for W48 because as it is very close to the equator, the ATCA as an East–West synthesis array has a very elongated synthesised beam and does not produce good images. Comparison of the images in Figure 1 with previous more sensitive observations of these sources at centimetre wavelengths (e.g. Ellingsen, Shabala, & Kurtz Reference Ellingsen, Shabala and Kurtz2005) shows similar structure and intensity. This demonstrates that despite both of these transitions lying outside the nominal frequency range of the ATCA receiver system (at the time of the observations), the system performed well and the non-detection of the spectral line emission is robust.
Figure 1. Radio continuum emission at 7.8 GHz for G 345.01+1.79 (left) and NGC6334F (right). For both sources, contour levels are at 2.5, 5, 10, 20, 40 and 80% of the image peak which is 217 and 776 mJy beam−1 for G 345.01+1.79 and NGC6334F, respectively. The RMS noise level as are 1.4 and 4.1 mJy beam−1 for G 345.01+1.79 and NGC6334F, respectively. The synthesised beam for these observations was approximately 2.0 arcsec × 1.8 arcsec.
The three secondary transitions (31A+–31A−, 17−2–18−3 E (vt = 1), and 41A+–41A−) were each observed for 4.2 min towards G 345.01+1.79. We have calibrated these data using the same approach as for the primary transitions; however, with a one-dimensional array configuration (such as the ATCA in the 6A array), it is not possible to image data from a single scan. We produced a vector averaged spectrum at the phase centre for each of the transitions and from this we obtained upper limits (3σ) on the intensity of any emission of 0.17, 0.15, and 0.25 Jy for the 31A+–31A−, 17−2–18−3 E (vt = 1), and 41A+–41A− transitions, respectively. The effective field of view for the vector averaged spectrum is the size of the synthesised beam (a few arcseconds), centred on the coordinates given for G 345.01+1.79 (Table 1). This is sufficient to encompass the class II methanol masers in this source which are observed to be confined to a single compact cluster with an angular extent of less than 0.5 arcsec (Krishnan et al. Reference Krishnan, Ellingsen, Voronkov and Breen2013).
4 DISCUSSION
Sobolev, Cragg, & Godfrey (Reference Sobolev, Cragg and Godfrey1997a) used the methanol maser pumping model of Sobolev et al. (Reference Sobolev, Cragg and Godfrey1997b) to predict which transitions are likely to show maser emission under a range of different physical conditions. In total six different pumping model input parameters were varied and the results for 10 different combinations are listed in Table 1 of Sobolev et al. (Reference Sobolev, Cragg and Godfrey1997a). The following model parameters were varied, the gas temperature (T kin), the gas density (n H), the maser beaming factor (ε), the dilution of continuum emission from a background Hii region (W HII ), the dust temperature (T d), and the methanol specific column density N M/ΔV. The 124–133 A− and 124–133 A+ transitions were predicted to exhibit weak maser emission (brightness temperatures of 104–105K) in 6 of the 10 models, more than any of the other methanol transitions at frequencies < 10 GHz which had not previously been detected. The most recent published class II methanol maser pumping model is that of Cragg et al. (Reference Cragg, Sobolev and Godfrey2005), which is based on the earlier work of Sobolev et al., but incorporates a number of improvements and refinements, including new collisional data and more energy levels. The Cragg et al. (Reference Cragg, Sobolev and Godfrey2005) model also suggests that the 124–133 A− and 124–133 A+ transitions are good candidates for weak masers, with six of the eight sets of input physical parameters they trialled yielding masers with brightness temperatures > 103 K, with three of them having brightness temperatures in excess of 104 K.
The four sources targeted for the current search are a subset of the 25 high-mass star formation regions which have been observed to show maser emission from the 107 GHz 31–40 A+ transition. Table 5 of Ellingsen et al. (Reference Ellingsen, Breen, Sobolev, Voronkov, Caswell and Lo2011) summarises the observed intensity, or measured upper limit for a dozen different class II methanol maser transitions towards these sources and shows that G 339.88−1.26, G 345.01 + 1.79, NGC6334F, and W48 have been detected in 6, 10, 8, and 5 of these dozen transitions, respectively. Comparing the class II methanol maser transitions observed in our four target sources with the results in Table 2 of Cragg et al. (Reference Cragg, Sobolev and Godfrey2005), they best match model 3, as it is the only model that predicts moderately strong 37.7 GHz methanol masers, which all these sources have. This model has T kin = 30K, T d = 175K, n H = 107 cm−3, N M/ΔV = 3 × 1011 cm−3s, and W HII = 0.002. This model predicts brightness temperatures of ~6.3 × 103 K for the 124–133 A− and 124–133 A+ transitions.
Table 1 shows that our most sensitive observations were of the 124–133 A+ transition at 7.83 GHz for which we obtained RMS noise levels in 0.2 km s−1 spectral channels of < 30 mJy beam−1 for three of the four sources (we had less time onsource for W48, so the RMS noise is higher). We can be confident that there is no emission stronger than 0.150 Jy beam−1 (5-σ) in this transition in the observed sources and from equation (1) that places an upper limit of ~1100 K on the brightness temperature of any emission on angular scales of 2 arcsec (the angular resolution of our observations). This is significantly less than the predicted brightness temperature in the Cragg et al. (Reference Cragg, Sobolev and Godfrey2005) model; however, maser emission generally occurs on much smaller angular scales than the 2 arcsec resolution of our synthesised beam. Very long baseline interferometry observations of class II methanol masers (e.g. Menten et al. Reference Menten, Reid, Pratap, Moran and Wilson1992; Minier, Booth, & Conway Reference Minier, Booth and Conway2002; Harvey-Smith & Cohen Reference Harvey-Smith and Cohen2006) show that the 6.7 GHz class II methanol masers generally have angular sizes in the range 5–50 milliarcsec. Rearranging equation (1) for the 124–133 A+ transition, our 0.15 Jy beam−1 upper limit on the flux of the emission from this transition implies θ2 Tb < 4330 K arcsec2. This corresponds to upper limits on the brightness temperature of 1.7 × 106 K for emission on scales of 50 milliarcsec or 1.7 × 108 K for emission on scales of 5 milliarcsec. These limits are both more than a order of magnitude higher than the predictions of any of the models of either Sobolev et al. (Reference Sobolev, Cragg and Godfrey1997a) or Cragg et al. (Reference Cragg, Sobolev and Godfrey2005) for this transition.
The observations of the 124–133 A− transition at 7.62 GHz are approximately 20% less sensitive than those for the 124–133 A+ transition. The lower sensitivity is believed to be due to poorer receiver performance at the frequency of that transition (at the time of our observations). The affect of this is that the limits for the 124–133 A− transition are 20% higher; however, this makes no significant difference to the conclusions we can draw.
It should be noted that the analysis undertaken here utilises data with a 0.2 km s−1 velocity resolution. This is close to optimal for Galactic maser work, as typical line widths are around 0.5 km s−1. Averaging several spectral channels would yield lower RMS noise levels in spectral line cubes; however, the resulting limits would be misleading, as they would not account for the dilution of narrow line emission.
From equation (1), we can estimate the minimum sensitivity for observations of the transitions targeted in this search that would be required to provide a stringent test of methanol maser pumping models. If we take a maximum likely size for the angular scale of the maser emission as 50 milliarcsec, then a maser brightness temperature of 104 K will result in a flux density of around 1 mJy. Robust detection of emission at this level in a 0.2 km s−1 spectral channel would require observations about two orders of magnitude more sensitive than those we report here. This level of sensitivity could be achieved with very long (of order days) integrations on sensitive telescopes with large collecting areas (e.g. the GBT, JVLA, or FAST); however, it more realistically lies within the realm of a future SKA survey of line emission in Galactic high-mass star formation regions.
5 CONCLUSION
We have searched for emission from a number of centimetre wavelength methanol transitions which are predicted to show weak maser emission towards high-mass star formation regions under some physical conditions. Our observations did not detect emission from any of the transitions in any of the four sources observed with upper limits of approximately 0.15 Jy. The observations reported here are approximately an order of magnitude more sensitive and an order of magnitude higher angular resolution than typical single dish searches for maser transitions and so they do represent a significant improvement on many searches for weak, rare class II methanol masers (e.g. Ellingsen et al. Reference Ellingsen, Cragg, Minier, Muller and Godfrey2003; Cragg et al. Reference Cragg, Sobolev, Caswell, Ellingsen and Godfrey2004). Previous observations have demonstrated that more sensitive observations can lead to the detection of weak maser lines, for example, Sobolev et al. (Reference Sobolev, Chapman and Baan2007) detected weak 23.1 GHz class II methanol masers after earlier unsuccessful searches by Cragg et al. (Reference Cragg, Sobolev, Caswell, Ellingsen and Godfrey2004). To significantly improve on the limits placed on the 31A+–31A−, 17−2–18−3 E (vt = 1), 124–133 A−, 124–133 A+, and 41A+–41A− transitions of methanol by the current observations will require next-generation radio astronomy facilities.
ACKNOWLEDGEMENTS
The Australia Telescope Compact Array is part of the Australia Telescope which is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO. This research has made use of NASA’s Astrophysics Data System Abstract Service. AC was funded by a University of Tasmania Dean’s Summer Research scholarship. AMS has been supported by the Ministry of Education and Science of the Russian Federation within the framework of state work ‘Organization of Execution of Scientific Research’. This work was also supported by Government of the Russian Federation Act 211, contract no 02.A03.21.0006.
