Methanol masers are commonly found in star formation regions (SFRs). The methanol molecule has numerous transitions within the centimeter-and millimeter-wavelength ranges and hence provides a powerful tool for the study of star-forming regions. According to the empirical scheme of Menten (1991a) , methanol masers are divided into two categories. Class II methanol masers, such as the 6.7 GHz (5 1 -6 0 A + ) and 12.2 GHz (2 0 -3 −1 E) transitions (Batrla et al. 1987; Menten 1991b) , are found in close proximity to ultracompact H II regions, infrared sources, and OH masers (Walsh et al. 1998) , and are known to be pumped by radiative processes (Cragg et al. 1992 (Cragg et al. , 2005 . In contrast, class I methanol masers are thought to be tracers of shocked regions related to outflows and expanding Hii regions (e.g., Gan et al. 2013; Voronkov et al. 2014) and are produced by collisional pumping. On the basis of the latest class I methanol maser models (Leurini et al. 2016; Sobolev & Parfenov 2018) , such masers can be divided into several families: the (J+1) 0 -J 1 -A type, the (J+1) −1 -J 0 -E type, the J 2 -J 1 -E series at 25 GHz, and the J −2 -(J−1) −1 -E series at 9 GHz. Within the Milky Way, methanol maser emission from the 44 GHz 7 0 -6 1 A + (e.g., Morimoto et al. 1985; Kalenskii et al. 1992; Slysh et al. 1994 ) is the most widespread and strongest transition, with the 36 GHz 4 −1 -3 0 E (e.g., Haschick & Baan 1989; Liechti & Wilson 1996) , 84 GHz 5 −1 -4 0 E (e.g., Kalenskii et al. 2001; Breen et al. 2019) , and 95 GHz 8 0 -7 1 A + (e.g., Chen et al. 2011 Chen et al. , 2013 transitions also being relatively common.
The first detection of 44 GHz methanol masers was reported by Morimoto et al. (1985) . Subsequent single-dish surveys searching for 44 GHz methanol masers have targeted galactic SFRs (Haschick et al. 1990 ), water masers (Bachiller et al. 1990 ), cold Infrared Astronomical Satellite (IRAS) sources (Kalenskii et al. 1992) , H ii regions (Slysh et al. 1994) , 6.7 GHz methanol masers (Fontani et al. 2010) , intermediate-mass young stellar objects (YSOs; Bae et al. 2011) , and 2.122 µm emission (Lim et al. 2012 ). These searches have laid the crucial groundwork for establishing the nature of the 44 GHz methanol maser transition. Recently, a series of interferometric observations targeting outflows (Gómez-Ruiz et al. 2016 ) and high-mass protostellar objects (HMPOs; Rodríguez-Garza et al. 2017) , have revealed the relationship between the class I methanol masers and other star-forming phenomena at high angular resolution, which has allowed more detailed investigations of the evolutionary stage and the maser excitation conditions. In addition, variability of class I masers has only been the subject of limited studies, and to date, no detectable variability has been reported (e.g., Choi et al. 2012) .
The 8 0 -7 1 A + transition of methanol at 95 GHz is a member of the same transition family as the 44 GHz maser transition. Systematic searches for 95 GHz methanol masers toward Spitzer Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE) extended green objects (EGOs; Chen et al. 2011 Chen et al. , 2013 , molecular outflow sources (Gan et al. 2013) , cross-matching between the GLIMPSE point sources and the Bolocam Galactic Plane Survey (BGPS) sources (Chen et al. 2012) , and BGPS sources (Yang et al. 2017 ) have significantly increased the number of known 95 GHz methanol masers. Yang et al. (2017) compiled a catalog summarizing the past two decades of searches for 95 GHz methanol masers. This catalog contains 481 maser sources and a further 37 candidates, and it currently represents the largest and most complete catalog of 95 GHz methanol masers.
In this paper, we report a search for 44 GHz methanol masers targeting known 95 GHz masers. This search was made using the three 21 m antennas from the Korean very long baseline interferometry network (KVN) in singledish telescope mode. In Section 2 we describe the source selection and observations, then we give the results of the detections, compare them with the previous observations in Section 3, and follow this by discussing the flux density ratio between the two maser transitions and their occurrence at different stages of the star formation process (Section 4) and a summary in Section 5.
The 95 GHz methanol maser sources in which we searched for emission from the 44 GHz methanol transition were selected using the following criteria: (1) The sources are listed in the catalog of 95 GHz methanol masers and maser candidates (Yang et al. 2017 ). The Yang et al. (2017) catalog of 95 GHz methanol masers contains 481 sources and 37 maser candidates, identified in searches toward BGPS sources (version 1.0.1; Rosolowsky et al. 2010 ) and other searches undertaken over the past two decades (Kalenskii et al. 1994; Val'tts et al. 1995 Val'tts et al. , 2000 Ellingsen 2005; Kalenskii et al. 2006; Fontani et al. 2010; Chen et al. 2011 Chen et al. , 2012 Chen et al. , 2013 Gan et al. 2013) . Sources in which only broad spectral components (> 2.5 km s −1 ; Yang et al. 2017 ) are observed at 95 GHz were considered maser candidates.
(2) Sources with declination greater than −25 • (which are observable with the KVN 21m antennas).
(3) Sources with previously reported 44 GHz maser detections from single-dish observations were excluded (Haschick et al. 1990; Bachiller et al. 1990; Kalenskii et al. 1992; Slysh et al. 1994; Kalenskii et al. 2006; Pratap et al. 2008; Fontani et al. 2010; Bae et al. 2011; Lim et al. 2012; Kang et al. 2015) . (4) Sources with previous KVN observations, separated by less than 30 ′′ from a Yang et al. (2017) 95 GHz source from targeting of class I masers (private communication; Kurtz et al. 1994; Molinari et al. 1998; Pestalozzi et al. 2005; Rathborne et al. 2006; Pandian et al. 2007; Cyganowski et al. 2008; Caswell et al. 2010; Green et al. 2010 ) are also excluded. Based on these criteria, a total of 144 95 GHz methanol maser sources were identified (see Table 1 ). Of these, 123 (∼ 85%) are sources selected from Chen et al. (2012) and Yang et al. (2017) that target the position of peak emission of associated BGPS sources (version 1.0.1; Rosolowsky et al. 2010 ) whose beam-averaged H 2 column density is greater than 10 22.1 cm −2 , the others are targeting star-forming regions or outflow/EGO sources with a 95 GHz methanol maser detection. Ten of the 144 target sources are 95 GHz methanol maser candidates, and these are identified with a double dagger in Table 1 .
The observations of the 44.06943 GHz (7 0 -6 1 A + ) and 95.16946 GHz (8 0 -7 1 A + ) class I methanol maser transitions took place in the period 2016 October to December using the KVN 21m radio antennas in single-dish telescope mode. There are three KVN stations: KVN Yonsei telescope (Seoul), KVN Ulsan telescope (Ulsan), and KVN Tamna telescope (Jeju island). Each of the KVN antennas are equipped with a multifrequency receiving systems able to simultaneously operate in the 43 and 86 GHz bands, which enables observing 44 and 95 GHz methanol transitions at the same time. The beam size and antenna efficiency of each antenna are listed in Table 2 . Telescope pointing observations were performed at least once an hour, resulting in a pointing accuracy better than ∼6 ′′ . Digital spectrometers with 4096 spectral channels were used as back-ends, each with a bandwidth of 64 MHz, which provides velocity resolutions of 0.11 and 0.05 km s −1 at 44 GHz and 95 GHz, respectively.
A low-order polynomial baseline was fit to the line-free channels in the spectra. Hanning smoothing was applied once (twice) to improve the signal-to-noise ratio for the 44 GHz (95 GHz) methanol line spectra. This results in a velocitychannel width of 0.21 and 0.20 km s −1 for the 44 and 95 GHz transitions, respectively. The system temperature varied between 150 K and 300 K depending on the weather conditions and the elevation of the telescope. The on-source integration times were between 5 and 15 minutes, which achieved a typical 1σ noise level of between 0.4 and 1 Jy for both of the methanol transitions at the ∼0.2 km s −1 resolution obtained after smoothing. The data were reduced and analyzed using the GILDAS/CLASS package (Pety 2005) . To characterize the spectra, we undertook Gaussian fitting of each peak in the spectrum for each source.
Twenty-four sources which were observed in bad weather and were not reobserved. These sources are indicated by a dagger in Table 1 . These sources may have unreliable flux densities for any detected emission, and they have been excluded from our analysis of intensity ratios in Section 3.2.1, 4.1.2, 4.2, 4.3.1, and 4.3.2.
The current KVN search did not detect 95 GHz methanol emission toward a small number of targets for which detections of this transition have been reported previously (see Section 3.1 for details). The majority of 95 GHz methanol masers/candidates as KVN targets were detected using the Purple Mountain Observatory (PMO) 13.7m radio telescope with a typical on-source integration time of 10-20 minutes (Yang et al. 2017) , and have a peak flux density greater than 4 Jy. To eliminate potential effects due to different beam sizes and effectively determine whether these 95 GHz methanol masers show intrinsic intensity variability, we reobserved 13 sources using the PMO 13.7m radio telescope. All the 13 sources (see Table 3 ) were observed using the PMO 13.7m in previous studies with a 95 GHz peak flux density stronger than 4 Jy. Nine of them were not detected in the current KVN 21m observations, the other four sources were randomly selected among the KVN detections.
Observations toward thirteen 95 GHz class I methanol maser sources were made with the PMO 13.7m radio telescope in Delingha, China on 2018 December 4 and 6. A 3×3 multibeam sideband-separating superconducting spectroScopic array receiver system was used to observe the 95 GHz methanol transition. This receiver operates over a frequency range of 85-115 GHz, and the beam in the middle of the first row of the receiver was pointed at the target position in most cases. The spectra were recorded using a fast Fourier transform spectrometer with 16,384 spectral channels across a bandwidth of 1 GHz, yielding a frequency resolution of 61 kHz and an effective velocity resolution of 0.19 km s −1 for the 95 GHz methanol transition. The system temperature for the 95 GHz methanol maser observations was in the range 135-200 K, depending on the weather conditions and telescope elevation. Most sources were observed in a position-switching mode with an off-position offset by 15 ′ in R.A. For some sources, a different reference position was chosen to ensure that the reference spectrum was free from emission. The pointing rms was better than 5 ′′ . The standard chopper-wheel calibration technique (Ulich & Haas 1976 ) was applied to measure the antenna temperature, T * A , corrected for atmospheric absorption. The beam size of the telescope is approximately 55 ′′ at 95 GHz, with a main-beam efficiency η mb of 62%. The antenna efficiency is 48%, corresponding to a factor of 39.0 Jy K −1 to convert antenna temperature into flux density. An on-source integration time of 15 minutes for each source achieved rms noise levels of approximately 1.4 Jy for the 95 GHz methanol transition.
The data were reduced and analyzed using the GILDAS/CLASS package (Pety 2005) . The data reduction procedure was similar to that of the KVN observations. We only analyzed the data for the one beam used to track the target position. A low-order polynomial baseline subtraction and Hanning smoothing (the velocity resolution is ∼ 0.39 km s −1 after smoothing, reaching a typical rms noise levels of 0.9 Jy) were performed on the averaged spectrum for each target source.
We only consider a source/transition to be a detection where the peak intensity is greater than the 3σ noise level in the spectrum. A total of 144 sites were searched for 44 and 95 GHz methanol masers simultaneously, with 128 (89%) and 111 (77%) detections in the 44 and 95 GHz transitions, respectively. Table 1 summarizes the position of each of the target sources in equatorial coordinates (J2000), whether emission was detected for each transition, whether 44 GHz emission was a new detection, and the noise level for the 44 and 95 GHz spectra, respectively. Tables 4 and 5 contain the list of all detected sources along with the fitted Gaussian parameters of their spectral features. The spectra of the 144 observed sources are shown in Figure 1 .
After cross-matching the latest and largest class I methanol maser catalog (Ladeyschikov et al. 2019 ), a total of 106 detections at 44 GHz are the first reported observations of maser emission in the target sources. The exceptions are 17 sources detected in previous KVN observations ( Kang et al. 2016; Kim et al. 2018 Kim et al. , 2019 and 7 sources with previous interferometric observations (indicated in Table 1 ). One source, G033.390+00.008, which is detected to have weak 44 GHz emission (peak flux density 2 Jy) by Kim et al. (2018) , did not meet the criteria to be considered a detection in the current observations.
The The better velocity resolution of the current observations shows that nine of the sources at 95 GHz considered maser candidates by Yang et al. (2017, ∼ 0 .39 km s −1 after Hanning smoothing) because they only contained broad spectral components (line width of > 2.5 km s −1 ) do also exhibit narrower spectral components. With the exception of BGPS2190 (which is better fit with a single broad Gaussian profile), these sources have been fitted with multiple Gaussian components. From the current observations there are three sources (BGPS4048, BGPS5057, BGPS7208) at 44 GHz and six sources (BGPS2152, BGPS2190, BGPS4048, BGPS6502, NGC 7538IRAS11, BGPS7208) at 95 GHz that are best fit with only a single broad spectral component. BGPS7208 (also known as IRAS 23139+5939), has been observed with Very Large Array (VLA), which confirms that although the spectral profile is broad, it is still due to maser emission . Single-dish observations alone cannot identify whether these broad emission sources are due to maser or quasi-thermal emission, and future interferometric observations are required to determine this. For the purposes of our analysis, we have assumed that the detected 44 and 95 GHz methanol emission in these single broad profile sources is due to maser emission. In the unlikely event that all of these broader lines are found to be pure thermal emission, the number (fewer than 10) is too small to significantly influence our statistics.
In total, 107 sources have both 44 and 95 GHz emission, 21 sources have only 44 GHz emission, and 4 sources have only 95 GHz emission. Previous searches have only detected 95 GHz maser emission toward sources which also show 44 GHz masers (Fontani et al. 2010; Kim et al. 2018) . For the four sources where we have a 95 GHz methanol detection without corresponding 44 GHz emission (G183.72−3.66, G008.458−00.224, BGPS2190, BGPS7318), the 95 GHz emission is weak and only reaches the 3σ requirement. One of the sources, G183.72−3.66 (also known as GGD4), was observed at 44 GHz in 2007 March/April using the VLA in the D configuration (Gómez-Ruiz et al. 2016 ), but no emission was detected. Additional observations of these four sources are required to confirm the 95 GHz detection, and higher resolution observations will be required to determine whether it is maser emission or thermal emission.
A total of 33 sources were not detected in the 95 GHz methanol emission in the current KVN search. There are several potential reasons for nondetections: (1) The majority of nondetected sources were previously observed using the PMO 13.7 m radio telescope, which has a beam size at 95 GHz of ∼ 55 ′′ . This is similar to the beam size of the KVN 21m antennas at 44 GHz, but significantly larger than that at 95 GHz, so masing regions detected in previous searches could be located outside the KVN beam at 95 GHz, but within the beam at 44 GHz. There are 21 sources with 44 GHz maser detection but without 95 GHz detection. (2) For weak masers, the limited integration time means that there is emission with a signal-to-noise ratio lower than three. This emission cannot be unambiguously distinguished from the noise in the spectrum. (3) The source may have exhibited variability in the 95 GHz class I methanol maser emission. (4) Some of the sources where a previous detection has been claimed based on data with poor signal-to-noise ratio may have been incorrect, in which case we do not expect to detect either 95 GHz or 44 GHz emission in these sources.
Excluding the 24 sources with unreliable flux densities due to observations in bad weather conditions (see Section 2.2), there are 99 detected 95 GHz methanol masers, and of these, 95 were previously detected in observations with the PMO 13.7m, while the other 4 were previously detected in observations with the Mopra 22m telescope. These 99 sources in KVN observations were smoothed to a similar velocity resolution as the previous detections, i.e., ∼ 0.2 km s −1 for Mopra, and ∼ 0.4 km s −1 for PMO. Figure 2 shows the peak flux density ratio of the 95 GHz methanol masers detected in the current KVN observations compared to previous observations with either PMO or Mopra. More than 85% of the sources have a peak flux density ratio between the KVN observations and previous PMO observations (S pk,KVN /S pk,PMO ) that lies in the range 0.4-1.1. In addition to the flux calibration and pointing accuracy, which affect the ratio, different beam sizes during the observations will lead systematic bias in the ratio. The beam size of the PMO 13.7m is larger by a factor of two than that of the KVN 21m at 3 mm wavelength. This means that any maser emission that is offset from the pointing center of the observations will be relatively closer to the edge of the KVN beam than PMO beam. This will lower the value of S pk,KVN /S pk,PMO .
The beam size and velocity resolution of the Mopra 22m are ∼ 36 ′′ and 0.22 km s −1 , respectively, which are comparable to those of the KVN 21m. The Mopra observations (2009 August) were made approximately 7 yr prior to the KVN observations (2016 October-December). For the four sources observed with Mopra, the peak flux density ratio is close to one, suggesting no significant variability in the maser emission over that period.
In total, 13 sources that were previously detected in PMO observations were reobserved using the PMO 13.7m. Nine of them were not detected in the current KVN observations, and four were chosen randomly in the ratio of S pk,KVN /S pk,PMO . Table 3 compares the new PMO observations with the KVN results and previous PMO observations. Some sources were observed more than once in order to increase the on-source integration time to improve the signalto-noise ratio. Because there is no evidence of variability in the class I methanol masers, we averaged all the observed spectra. Figure 3 shows a comparison of the spectra for each source, with red and black representing the current and previous PMO spectra, respectively. Except for BGPS1917 and BGPS2011, whose peak flux densities are consistent between the two epochs of PMO observations, the peak flux densities of other sources are all slightly lower in the current data than before.
Of the nine sources that are not detected with the KVN at 95 GHz, five were detected in the current PMO 13.7m observations. This is consistent with the KVN nondetection arising because the class I methanol maser emission in these sources is offset from the pointing center and lies at the edge of or beyond the narrower KVN beam. For a further two sources (BGPS7252 and BGPS7351), the PMO peak flux density is significantly stronger than that of KVN data, and again, this is likely because the maser emission in these sources is offset from the pointing center and toward the edge of the KVN beam. Two sources (BGPS1917 and BGPS4252) that show a peak flux density in KVN observations that is twice as strong as the PMO detection. When we smooth the KVN spectra to the same velocity resolution as the PMO, the intensity is almost the same, suggesting that these sources have narrow spectral components.
No methanol emission was detected in the current PMO or KVN observations for four sources (BGPS2784, BGPS3319, BGPS4063, and G031.013+00.781). For BGPS3319 there was no detected 44 GHz methanol emission either, suggesting that this may not be a class I methanol maser source and that the previously reported detection may not be real, but a misidentification due to a poor signal-to-noise ratio. For the other three sources, we detect weak 44 GHz methanol emission, and when we take the typical intensity ratio between 44 and 95 GHz methanol two transitions into account, the 95 GHz emission might be too weak to be detected. While we cannot rule out that the uncertainty in the flux density calibration is partly responsible for differences in the measured flux densities between different epochs, an offset between the location of the detected maser emission and the pointing center of the observations appears to be the primary reason for the nondetection of some previously detected 95 GHz methanol masers in the current KVN observations.
To summarize, when we compare the previous 95 GHz detections with new observations of the same transitions made using PMO 13.7 m radio telescope, there is no clear evidence of variability on a timescale of six years (e.g., BGPS3322, BGPS7252, and BGPS7322 in Table 3 ).
For nine sources in our sample, 44 GHz interferometric observations from the VLA are available. These sources are indicated with an asterisk after the name in Table 1. G183.72−3.66 (GGD4). GGD4 is a low-mass SFR with a known outflow. This source was observed during 2007 March to April using the VLA in D configuration, but there was no detection of 44 GHz methanol emission (channel rms ∼ 52 mJy beam −1 Gómez-Ruiz et al. 2016 ). In the current observations, we do not detect any emission above the noise at 44 GHz. Gan et al. (2013) reported the detection of a weak 95 GHz class I methanol maser toward this source, and the current observations also show methanol emission at 95 GHz. Higher angular resolution observations are needed to determine whether the detected 95 GHz methanol emission is a maser or quasi-thermal. BGPS7501 (S255N). Kurtz et al. (2004) imaged the 44 GHz methanol masers in S255N on 2000 September 25 using the VLA in the D configuration. The current KVN observations have a similar velocity resolution as those of Kurtz et al. (2004) , with two major maser features. The strongest maser component has a velocity of 11 km s −1 and an intensity of about 250 Jy in the current KVN observations, compared to approximately 150 Jy in the VLA observations. The secondary maser feature at 10 km s −1 has a peak flux density of about 60 Jy in both the current and previous observations. An interferometric observation resolves out emission structures larger than a specific angular scale that is determined by the shortest baseline and the observing frequency. Jordan et al. (2017) analyzed the relative strength of compact maser emission (interferometric measurement) to diffuse emission (simultaneous singledish measurement), of a sample of 44 GHz class I methanol masers and found that class I methanol emission can be confined to compact structures, extended structures or a combination of the two. We cannot rule out the possibility that the single-dish KVN spectrum includes additional thermal or diffuse contributions that are resolved out in the interferometric observations, so that only additional high-resolution observations can determine whether this spectral component has varied or not. In addition to the main spectral features, the VLA observations show a series of weak methanol emission components in the velocity range 7-10 km s −1 , which are also seen in the KVN spectrum. The VLA image shows that the two strongest components are offset from the pointing center of the KVN observations by ∼ 11 ′′ . If the 95 GHz methanol masers are cospatial with the 44 GHz transition, the peak flux density of the 95 GHz methanol masers might be underestimated. The S255 molecular complex lies between two H ii regions, S255 and S257, and is at a distance of 1.59 kpc (Rygl et al. 2010) . It consists of three massive star forming regions, S255N, S255IR and S255S. The class I methanol maser emission is located near S255N, whose evolutionary stage is between that of S255IR (more evolved) and S255S (less eveolved). Outflow activity in this region has been studied through a number of different tracers, including CO, shocked H 2 and SiO emission (Miralles et al. 1997; Cyganowski et al. 2007; Wang et al. 2011) .
BGPS3016 (IRAS 18308−0841). Rodríguez-Garza et al. (2017) reported five 44 GHz methanol maser components in their VLA observations from 2008 September 7. The three components that are stronger than 6 Jy can be clearly seen in the KVN spectrum and are located approximately 11 ′′ from the pointing center of the KVN beam. The peak flux density of the 75.8 km s −1 , 76.4 km s −1 , and 76.9 km s −1 components measured with the VLA are about 6 Jy, 15 Jy, and 6 Jy, respectively, similar to the current KVN observations, which show 7 Jy, 15 Jy, and 7 Jy, respectively. Despite the different spatial resolution and flux density calibration uncertainties, we can see that with a similar velocity resolution (∼ 0.16 km s −1 ), there is no evidence for variability of the 44 GHz methanol masers in this source over a period of 8 yr (2008) (2009) (2010) (2011) (2012) (2013) (2014) (2015) (2016) . (Peretto et al. 2016) . The location of the class I methanol masers suggests that they may be located at the interface between an expanding H ii region and an infrared dark cloud (IRDC). On the other hand, Sridharan et al. (2002) were unable to confirm CO line outflows/wings in this source due to confusion with Galactic plane emission. Higher resolution observations are necessary to identify the possibility of the presence of outflow(s) and further confirm the origin of 44 GHz maser emission. The two maser components are separated from the KVN pointing center by only 1 ′′ , suggesting that the measured flux densities for both the 44 and 95 GHz transitions are reliable. The peak flux density ratio of the two transitions for both maser components is 0.7, suggesting similar environmental parameters, such as temperature and density. When we use the kinematic distance estimate of 3.7 kpc obtained from the model of Reid et al. (2014) , the linear separation between the two components is about 0.02 pc.
G058.471+00.433 (IRAS 19368+2239) . The KVN observations of this source were made in bad weather, leading to potentially unreliable flux density estimates. Gómez-Ruiz et al. (2016) detected 12 maser components in their VLA imaging of this source. The primary and secondary components from the VLA observations are at velocities of 37.9 km s −1 and 36.1 km s −1 , and the separation of these two components from the KVN pointing center are 19 ′′ and 21 ′′ , respectively. These offsets place two of the components beyond the FWHM of the KVN beam at 95 GHz, but strong emission at almost the same velocities was still detected.
G65 For the −52.7 km s −1 component, which is located 5 ′′ from the KVN beam center, the peak flux density detected by both the VLA and KVN is ∼4 Jy. Similarly, for the −54.7 km s −1 component, offset from the KVN beam center by 1 ′′ , the peak flux density measured in both single-dish and interferometric observations is 3.5 Jy. So once again, there is no evidence of variability in this source. The maser spots are close to the KVN beam center, and hence the measured flux densities of both the 95 and 44 GHz methanol masers will be reliable. When we assume that the 95 GHz methanol masers are cospatial with 44 GHz transition, the peak flux density ratio between the two transitions measured from the current observations can be considered reliable. The S pk,95 /S pk,44 for the −52.7 km s −1 component is about 0.5, while for the −54.7 km s −1 component, it is about 0.9. The difference in the flux density ratio between the two components may reflect a difference in the physical conditions of the environment hosting the two maser components. The angular separation of the two components is 6. ′′ 6, corresponding to a linear separation of about 0.1 pc for a parallax distance of 3.33 kpc (Choi et al. 2014 ). Figure 1 shows a wide variety of spectral profiles for the class I methanol masers. Some show a single, narrow, and strong maser feature, such as BGPS1509, BGPS1584, and BGPS2147, while others (e.g., BGPS3018, BGPS3026, and BGPS3212) contain multiple peaks. Some sources have broad spectral components, which could be quasi-thermal emission, indicating that the maser emission may in some cases be mixed the thermal emission. To reliably count the number of maser components, we only considered sources without broad emission components (line width > 2.5 km s −1 ), resulting in 111 and 96 methanol maser sources in our analysis for the 44 and 95 GHz transitions, respectively. For the 44 GHz methanol transition, the ratio of the number of sources with a singlep eak to those with multiple peaks is 0.66 (44/67). For the 95 GHz methanol transition, this ratio is 0.57 (35/61). It is not clear why some sources have a single peak of maser emission while others have multiple peaks, but possible reasons include (1) precession of the jet/outflow driven by the central object.
(2) multiple outflows, and (3) the distribution or structure of the ambient molecular clouds with which the outflow interacts. Figure 1 , it is clear that the 44 and 95 GHz methanol transitions typically cover the same velocity range with very similar radial velocities for individual maser components. This has been noted in several previous investigations that compared the emission from these two transitions (e.g., Val'tts et al. 2000; Kim et al. 2018 ).
In our sample, a total of 107 sources have detections for both the 44 and 95 GHz methanol transitions. We have smoothed the spectra from the two transitions to have the same velocity resolution (∼ 0.2 km s −1 ), and the peak velocity of each maser features were determined by Gaussian fitting. For sources that have the same number of maser features in each transition (e.g., BGPS3307), we matched all of the components individually to analyze the difference in peak velocity. For sources that have a different number of maser components for the 44 and 95 GHz transitions (e.g., BGPS1917), we compared the velocity of the strongest spectral feature. Figure 4 shows a comparison of the velocity of a total of 161 methanol peak velocities for the 44 and 95 GHz transitions. A very strong correlation exists between these two velocities with V pk,95 = (0.9998 ± 0.0010)V pk,44 − (0.0470 ± 0.0614), with the Pearson coefficient r = 0.9999. For 68% (109/161) of the maser components, the peak velocity of the two transitions agrees within 0.2 km s −1 , suggesting that the emission from the 44 and 95 GHz transitions arises in the same environment and is likely cospatial. The peak velocity difference between the 44 GHz masers and their 95 GHz counterparts, V pk,44 − V pk,95 , ranges from −3.15 to 1.37 km s −1 , with an average of 0.05 km s −1 and a median of 0.04 km s −1 . BGPS2718 shows the largest velocity deviation between the two transitions, with the strongest emission from the 44 GHz transition at ∼54 km s −1 , but the peak of the 95 GHz transition is at ∼57 km s −1 . There is a component at 54 km s −1 in the 95 GHz spectrum, but it is not the strongest emission from this transition. The large difference in the radial velocity of the strongest emission between two transitions in this source suggests that there may be significant environmental differences between the two components. The blue dots in Figure 4 highlight the 28 sources that have a single maser component for both transitions, which are not subject to the uncertainties caused by fitting multiple Gaussian components. In these sources, the peak emission velocities of two transitions has a tighter correlation, and the deviation ranges from −0.23 to 0.2 km s −1 , with a mean and median for both of ∼0.02 km s −1 .
Excluding the sources with unreliable flux densities, the flux density of each component of the 111 44 GHz maser sources was derived from Gaussian fitting of the spectra, ranging from 0.6 to 335 Jy (mean of 12.1 Jy, median 4.7 Jy). For the 95 GHz masers (99 sources), the flux density range is from 0.6 to 165.4 Jy (mean of 7.4 and median of 3.0 Jy). BGPS4252 and BGPS7501 are the 44 and 95 GHz methanol masers with the highest detected flux density in our sample, respectively. There are 95 sources with reliable flux densities in both transitions, and of these, 14 sources (∼ 15%) have a higher 95 GHz peak flux density than for the 44 GHz methanol maser counterpart.
Based on the discussion of the velocity difference in Section 4.1.1 and the velocity resolution of the spectra for the two transitions, we can confidently match the emission from the two transitions where there are components with a velocity difference within 0.2 km s −1 . Similar to the analysis we have undertaken of the peak velocity, for sources that have the same number of maser features in each transition, we matched all of the components individually to analyze the peak flux density ratio. For sources that have a different number of maser components for the 44 and 95 GHz transitions, we calculated the ratio of the strongest emission in each transition. In total, 119 pairs were investigated. Figure 5 compares their peak flux density and the corresponding integrated flux density. The peak flux density ratio, S pk,95 /S pk,44 , ranges from 0.1 to 2.8. G123.07−6.31 shows the highest ratio, while BGPS4258 has the lowest ratio.
The blue dots in Figure 5 highlight the 24 sources with a single maser component in both transitions that are not affected by Gaussian fitting, thus their flux density ratios are more reliable. There are four sources with a single maser component (∼ 17%) where the 95 GHz peak flux density surpasses the 44 GHz counterpart. The ratios, S pk,95 /S pk,44 , range from 0.3 to 1.4, with BGPS6547 having the highest value and G8.72−0.36 the lowest. The integrated flux density ratio, S 95 /S 44 , is significantly affected by Gaussian fitting, and so we decided to only investigate the range obtained from the sources with a single maser component. The integrated flux density ratio ranges from 0.36 to 2.5, and this encompasses the ratio for the majority components from the multiple-peak sources. Figure 5 shows strong correlations between the intensity of matched components from the two transitions. Linear fits yield the following results: Our linear fit for the peak emission is consistent with that obtained by Kim et al. (2018, which gives S pk,95 /S pk,44 of 0.56 ± 0.08), and slightly lower than the ratio of 0.71±0.08 found by Kang et al. (2015) . When we consider only the 24 sources with a single maser component, the correlation between the intensity of the two transitions becomes stronger, S pk,95 =(0.43±0.03)S pk,44 +(3.79±2.04), with a Pearson coefficient of 0.96. A recent investigation using interferometric data from the Australia Telescope Compact Array (ATCA) with an angular resolution of better than 6 ′′ for both transitions found S pk,95 /S pk,44 to be 0. We cannot rule out the possibility that some masers are close to the edge of the KVN beam at 95 GHz, but this will cause the detected flux density to be lower than the real value and hence lead to a peak flux density ratio of 95 and 44 GHz transitions that underestimates the real situation.
Class I maser pumping models (e.g., Leurini et al. 2016; Sobolev & Parfenov 2018) find that the line ratio between maser transitions is sensitive to the physical conditions of the environment. The different line ratios between the two transitions found in previous studies may be due to differences in the sample selection criteria. In addition, interferometric observations (Jordan et al. 2017 ) have found class I methanol emission can consist of only compact components, extended components, or a combination of the two. We cannot rule out that the single-dish spectra are a blend of maser and quasi-thermal emission in some sources, which may cause line ratio differences between interferometric and single-dish observations. The class I methanol masers reported in Kang et al. (2015) and McCarthy et al. (2018) all have an associated 6.7 GHz methanol maser, but the former were observed by the KVN in single-dish mode, while the latter were observed using ATCA, and the line ratio between the 95 and 44 GHz methanol transitions measured from the two studies is quite different.
It should be noted that S pk,95 /S pk,44 noticeably decreases as the flux density of the 44 GHz transition increases. Figure 6 shows S pk,95 /S pk,44 against the peak flux density of 44 GHz methanol emission. The best linear fit is S pk,95 /S pk,44 =(−0.45 ± 0.08)log(S pk,44 ) + (1.22 ± 0.08), with a Pearson coefficient of −0.47. As the 44 GHz peak flux density increases, the S pk,95 /S pk,44 decreases and flattens to an approximately constant value lower than one. From both Fig. 5 (left panel) and Fig. 6 , it is clear that when the peak flux density of the 44 GHz methanol maser is lower, the ratio of S pk,95 /S pk,44 has more scatter. In addition, for the 10 components (from 119 methanol transition pairs) where the peak flux density of the 44 GHz transition is greater than ∼ 40 Jy, there is no case where the 95 GHz methanol emission exceeds that of the 44 GHz counterpart. A possible explanation for this behavior is that the sensitivity of the 44 and 95 GHz transitions to the physical parameters is different, e.g., the methanol specific column density (see the definition in Sobolev & Deguchi 1994; Cragg et al. 2005) , which is a factor in the maser optical depth of the maser and therefore determines the maser brightness. Pumping models for class I methanol masers (A.M. Sobolev 2020, private communication, and S.Yu. Parfenov 2020, private communication) show that the 95 GHz transition becomes relatively weaker than the 44 GHz transition with the increase in maser flux. This dependence is not linear and is more pronounced when the masers have lower fluxes.
Because the angular resolution of the current single-dish observations is limited, we cannot study the infrared emission where the maser arises in depth, but only the overall infrared environment of the central YSOs that host the maser.
The Infrared Astronomical Satellite (IRAS 1 ) performed an unbiased sky survey at 12, 25, 60, and 100 µm, with an angular resolution ranging from 30 ′′ to 2 ′ . The data from this survey were used to create the IRAS Point Source Catalog (version 2.1) which we have used to analyze the environment of the maser host. Of the 128 detected 44 GHz methanol masers, 59 have an IRAS counterpart within 1 ′ , and Table 6 gives the angular separation and the name of the IRAS counterpart of each source, as well as the IRAS band fluxes, distance, and bolometric luminosity. We used F x to denote the flux density in the x µm IRAS band in Jy, and Q x to denote the corresponding flux quality, with values of 1, 2, and 3 representing an upper limit, moderate quality, and high quality, respectively. We also calculated the bolometric luminosity of the central object based on the IRAS fluxes (Connelley et al. 2007) . Distances for each of the target sources were tabulated by Yang et al. (2017) , primarily using kinematic distances calculated from the Reid et al. (2014) model.
The majority of the IRAS counterparts (93%; 55/59) has a bolometric luminosity greater than 10 3 L ⊙ , indicating that they are probably associated with high-mass star forming regions. About 83% (49/59) of the IRAS counterparts have F 12 < F 25 < F 60 < F 100 , which is characteristic of YSOs. Figure 7 shows IRAS color-color diagrams in which the youngest sources have the steepest spectra and are located toward the top right corner. As a source evolves, the infrared colors become bluer and sources shift toward the lower left corner. The green lines in the left panel depict the criteria of Wood & Churchwell (1989, hereafter WC89) which identify sources likely to be asscociated with an ultra-compact H ii (UCH ii) region, (log(F 25 /F 12 ) 0.57 and log(F 60 /F 12 ) 1.3). The left-hand panel in Fig. 7 shows that a significant fraction (61% ; 36/59) of sources meet the WC89 criteria region. This is a lower fraction than is observed for 6.7 GHz class II methanol masers (87%; Xu et al. 2003) . This seems to be consistent with the maser-based evolutionary sequence for high-mass star formation, which suggests that while both class I methanol masers and 6.7 GHz class II methanol masers can occur during the UCH ii phase, the class I methanol masers are thought to disappear earlier than those of class II and so have less overlap with the UCH ii phase (Breen et al. 2010) . However, there are a number of potential biases that may impact our analysis. First, the WC89 criteria are for UCH ii candidates, but many of them have been found to be HMPOs rather than UCHii regions (e.g., Molinari et al. 1996; Sridharan et al. 2002) . Secondly, the beam sizes of 6.7 GHz maser observations (e.g., 3 ′ -6 ′ ) were usually much larger than those (0. ′ 5-1 ′ ) of 44 or 95 GHz maser observations, and hence there were more likely to be two or more massive YSOs in different evolutionary stages within the beam of 6.7 GHz maser observations. The green line in the right panel of Fig. 7 represents an improved H ii region selection criterion (Yan et al. 2018) , and we find that 48 sources satisfy this. Note that in applying the Yan et al. (2018) criterion, we did not exclude sources with Q 60 = 1 or Q 100 = 1 as is suggested because under those circumstances the number of sources remaining is too small for a statistical analysis.
After the methanol masers with an unreliable flux density are removed, a total of 42 sources that have both 44 and 95 GHz class I methanol maser emission and an IRAS source counterpart. Fig.8 shows a plot of the isotropic maser luminosity as a function of the bolometric luminosity for the 44 GHz (left) and 95 GHz (right) methanol masers in our sample. The isotropic luminosities of the 44 and 95 GHz methanol masers (L 44 and L 95 ) can be calculated from the integrated flux density S v dv and the distance to the source (see, e.g., Bae et al. 2011 ). The black line in each panel marks the best linear fit to the data. The best fit for the 44 GHz methanol masers is log(L 44 ) = (0.77 ± 0.11) × log(L bol ) − (8.43 ± 0.45) with a Pearson coefficient of 0.75. The best fit for the 95 GHz methanol masers is log(L 95 ) = (0.60 ± 0.10) × log(L bol ) − (7.49 ± 0.43) with a Pearson coefficient of 0.68. Both L 44 and L 95 have a similar correlation with L bol , but the L 44 shows a slightly better correlation with L bol than L 95 .
For 44 GHz methanol masers, the relation between L 44 and L bol has been studied toward low-mass YSOs (L bol < . Combining the data from these previous studies with our sample, the best fit for all sources is log(L 44 ) = (0.56 ± 0.05) × log(L bol ) − (7.66 ± 0.22) with a Pearson coefficient of 0.63. Fig. 9 shows the isotropic maser luminosity as a function of the bolometric luminosity for all objects. The bolometric luminosity is a good measure of the central object mass. The correlation between maser luminosity and bolometric luminosity may arise when sources with higher mass sources drive more powerful outflows, or at least outflows that result in a larger volume of gas that produces class I methanol masers, where those outflows interact with the surrounding molecular environment (e.g., Bae et al. 2011; Kim et al. 2019 ).
It is widely accepted that the earliest stages of high-mass star formation often take place while the source is embedded within an IRDC . Investigation of molecular gas within IRDCs compared to HMPOs, shows that as the sources evolve, the temperatures increase and the densities and masses rise. The next evolutionary phase is associated with UCH ii regions, which are produced by young massive stars as they reach the main sequence (e.g., Motte et al. 2018) . Thus molecular clumps associated with IRDCs, HMPOs, and UCH iis represent an approximate evolutionary sequence of massive star formation. Ellingsen (2006) found that the infrared color of sources that are only associated with class I methanol masers are redder than the color of sources associated with both class I and class II methanol masers, indicating that the class I methanol masers trace an earlier stage than class II methanol masers. On the other hand, a few previous studies suggested that the detection rate of 44 GHz class I methanol masers increases as the central objects evolve (e.g., Bae et al. 2011; Kim et al. 2019) . These studies indicate that 44 GHz class I methanol masers can be associated with both early and late evolutionary stages of high-mass star formation, but the masers are more frequently detected in later evolutionary stages. Theoretical prediction and interferometric observations (e.g., Voronkov et al. 2014 ) also found that class I methanol maser could be pumped by expanding H ii regions, demonstrating that some class I methanol masers are associated with later stages of high-mass star formation. We would like to determine whether the current sample contains class I masers likely associated with both younger and older SFRs.
We investigated the infrared emission detected by the all-sky Wide-field Infrared Survey Explorer (WISE 2 ; Wright et al. 2010) toward each of our target sources. The WISE images can be used to determine which class I methanol maser sources may be associated with an infrared dark background or mid-infrared morphologies suggesting Hii regions.
WISE used a 40 cm telescope to image the entire sky in four mid-IR bands at 3.4, 4.6, 12 and 22 µm. From 3.4 to 22 µm, WISE achieved sensitivities for point sources of 0.08, 0.11, 1, and 6 mJy and angular resolution of 6 ′′ .1, 6 ′′ .4, 6 ′′ .5 and 12 ′′ .0 in the four bands, respectively. Mid-IR emission can be used to trace star-forming activity through polycyclic aromatic hydro-carbon emission, seen in the WISE 12µm band, and through the correlation with thermal emission from warm dust, predominantly see in the WISE 22 µm band.
We inspected the 12 ′ × 12 ′ three-color images for each of our target maser sources (see Figure 10 as an example). From our sample, we found that some class I methanol masers could be associated with IRDCs and some could be associated with H ii regions, suggesting that there are both younger and older class I methanol maser sources during star formation.
The IRDCs are seen as a dark silhouette against the bright background emission in images at wavelengths between 7 and 25 µm (e.g., Simon et al. 2006) . Investigations of molecular line and dust continuum emission shows that they are regions of dense, cold gas and have high column densities, consistent with the expectations for the initial conditions for high-mass star formation (e.g., Pillai et al. 2006; Rathborne et al. 2006) . Peretto & Fuller (2009) compiled an unbiased sample of candidate IRDCs (11303 in total) in the 10 • <| l |< 65 • , | b |< 1 • region of the Galactic plane using Spitzer 8 µm extinction. Subsequently, 76(±19)% of these cataloged SDCs were confirmed through association with a peak in Herschel column density maps constructed from 160 µm and 250 µm data from Herschel Galactic plane survey Hi-GAL (Peretto et al. 2016) .
In the WISE three-color images, 98% (125/128) have at least one WISE point source within 30 ′′ (about half of the beam size at 44 GHz) of the pointing center. Two of the exceptions are G208.97−19.37 (Orion-KL) and BGPS2152 (M17), where the three-color images are saturated and only one source (BGPS2054) has no close WISE point source in the AllWISE catalog. For the majority of sources with a 95 GHz class I methanol maser detection, we can surmise that the emission is located within the 15 ′′ of the targeted center (because the sensitivity of the observations drops very rapidly at larger separations). When Orion-KL and M17 are excluded, 25% (31/126) of the targeted locations have no WISE point source within 15 ′′ (about half of the beam size in 95 GHz) of the pointing center. We examined the WISE three-color images of these 31 masers and found that some of them show an absence of bright 22 µm emission, perhaps indicating the presence of an IRDC.
With the exception of IRDC18223-3 (where the observed target is a known IRDC), for the 31 sources without nearby (∼15 ′′ ) WISE counterparts, we cross-matched with the Herschel-confirmed SDC catalog, finding that 5 of them may be associated with IRDCs (See Table 7 ). The ratios, S pk,95 /S pk,44 , for the masers that may be associated with IRDCs are no greater than one, but for IRDC18223-3, the peak emission of the 95 GHz methanol maser is stronger than that of the 44 GHz counterpart of S pk,95 /S pk,44 ∼ 1.2. Anderson et al. (2014) compiled a catalog of more than 8000 Galactic Hii regions and candidates by visually and automatically searching for their characteristic mid-IR morphology using WISE data. Approximately 1500 of the midinfrared selected sample have been detected in RRL emission and are thus confirmed to be H ii regions. Furthermore, as a part of the Green Bank Telescope H ii Region Discovery Survey, new RRL observations are being undertaken (Anderson et al. 2015 (Anderson et al. , 2018 , expanding the catalog of confirmed H ii regions.
We cross-matched the class I methanol masers targeted in the current observations with the WISE catalog of Galactic H ii regions v2.0 from http://astro.phys.wvu.edu/wise/(see also Anderson et al. 2018) . The WISE name, coordinates, the approximate circular radius encompassing the WISE mid-IR emission and corresponding RRL velocity information were extracted from the catalog. We consider the class I methanol maser to be possibly associated with a H ii region when it meets the following criteria: (1) The angular separation between maser and H ii region is smaller than the radius of the corresponding H ii region. (2) To avoid including the effects from other complex environments, the angular separation between maser and H ii region is no greater than 60 ′′ (approximately the beam size at 44 GHz). It should be noted that this criterion may result in not identifying cases where the maser is located at the edge of an evolved and extended H ii region. (3) The H ii region has detected RRL emission, and the absolute difference between the velocity of the RRL and class I methanol maser is less than ∼ 10 km s −1 (Anderson et al. 2014) .
The criteria identified a total of 22 class I methanol masers (see Table 8 ) that may be associated with H ii regions, all of which also have BGPS 1.1 mm emission. There are multiple WISE H ii region counterparts within 30 ′′ (about half of the beam size in 44 GHz) of two masers (BGPS1116 and BGPS3155), suggesting that they are part of a larger H ii region complex. We listed all the possible WISE H ii regions, because when the accurate position of maser is unknown, we only interested in which masers may be associated with H ii regions rather than which specific H ii region it is associated with. Table 8 lists the names of the methanol masers, the possible associated WISE H ii regions, the angular separation between the BGPS source and Hii region, the angular sizes of the H ii regions, the velocity range of class I methanol masers and the velocity of the RRLs from H ii regions, as well as the ratio of the peak flux density for the two class I methanol transitions. For the source with an unreliable flux density or a 95 GHz nondetection, the ratio of the peak flux density between the two transitions is not listed. The ratios, S pk,95 /S pk,44 , for the masers that may be associated with H ii regions are all lower than one.
It should be noted that a large number of observations have shown that CO outflows are common toward both HMPOs and UCH iis (e.g., Shepherd, & Churchwell 1996; Zhang et al. 2001; Sridharan et al. 2002) , and numerous YSOs are observed at the peripheries of compact or extended H ii regions (e.g., Deharveng et al. 2008; Pomarès et al. 2009 ). Thus it is difficult to differentiate whether class I methanol masers are produced by the expansion of Hii regions or the outflows of associated YSOs, based on low-resolution radio and IR data. High-resolution observations are necessary to clarify the issue.
Four sources (BGPS1954, BGPS3026, BGPS3307, and BGPS4933) which may be associated with a H ii region and also a nearby IRDC (within ∼ 1 ′ ). The VLA observation of BGPS3307 (see Sec.3.2.2) shows that the maser components are located at the interface between a H ii region and an IRDC. For the other three sources, the exact position of the maser emission is unknown, and hence we cannot determine whether they are associated with an IRDC.
We have used the three KVN antennas in single-dish mode to simultaneously observed the 44 and 95 GHz class I methanol masers toward 144 sources with previous 95 GHz detections. The main results are listed below. 1. 128 44 GHz and 111 95 GHz methanol were detected, corresponding to detection rates of 89% and 77%, respectively. This is the first reported detection of 44 GHz class I methanol masers for 106 sites. 2. Through comparison with previous observations with PMO 13.7m new observations, no clear evidence was found for variability in 95 GHz methanol masers. 3. The 44 and 95 GHz methanol masers show a strong correlation in peak velocity, peak flux density, and integrated flux density. The peak flux density ratio S pk,95 /S pk,44 ranges from 0.1 to 2.8, and the best fit for S pk,95 /S pk,44 in our Figure 6 . The peak flux density ratio of S pk,95 /S pk,44 against with the peak flux density of the 44 GHz methanol maser. As shown before, the red dots represent the matched methanol emission component in sources with multiple peaks, and the blue dots represent the 24 sources with a single methanol emission peak. Error bars are shown in the peak flux density figure. The dash-doted orange line depicts where S pk,95 /S pk,44 equals 1 when the peak flux density of 44 GHz is stronger than 40 Jy (dashed green line). The solid black line denotes the best linear fit. (Wood & Churchwell 1989) , and the UCHii regions lie in the upper right corner. In the right-hand panel, the green line shows an improved Hii region selection criterion (Yan et al. 2018) , and the H ii regions lie above the green line. G123.07-6.31 Note-The sources marked with a dagger have unreliable flux densities due to poor weather. The sources with previous interferometric observations are marked with an asterisk. Ten sources were assigned as maser candidates (Yang et al. 2017) and are noted with a double dagger. Sources marked with a dagger and an asterisk are not given in this portion of Note-Column 1: the source name. Columns 2-3: the peak flux density and 1σrms noise of the new PMO observations. Columns 4-6: the observational dates, the peak flux density, and 1σrms noise of the previous PMO observations. Columns 7-8: the peak flux density of 44 and 95 GHz methanol masers of KVN observations. N indicates a nondetection. Note that the velocity resolutions of KVN data at both 44 and 95 GHz are ∼ 0.2 km s −1 . Column 9: the comments of each source, the detailed situations are listed below: a. The peak flux density is affected by a different velocity resolution. b. The maser could be out of the beam at 95 GHz or may be at the edge of the beam. c. The source could have week 95 GHz emission, but cannot be distinguished from noise. d. The source could have no 95 GHz emission, the previous detection might be a false detection. The velocity at peak V pk,44 , the line width ∆V44, the peak flux density S44, the integrated flux density S44 and corresponding fitting error for each of the maser features that have been estimated from Gaussian fits. Column 7: The total integrated flux density S44dv of the maser spectrum obtained by adding the integrated flux density of all maser features in the source.
(This table is available in the online material. A portion is shown here for guidance.) Note-Column 1: Source name. Column 2: The component(s) of each source at 95 GHz. Columns 3-6: The velocity at peak V pk,95 , the line width ∆V95, the peak flux density S pk,95 , the integrated flux density S95 and corresponding fitting error for each of the maser features that have been estimated from Gaussian fits. Column 7: The total integrated flux density S95dv of the maser spectrum obtained by adding the integrated flux density of all maser features in the source.
(This table is available in the online material. A portion is shown here for guidance.) Note-Column 1: the maser name. Column 2: the angular separation of KVN targeted center and possible associated IRAS source. Columns 3: IRAS name. Columns 4-7: the flux density in the four IRAS bands. Columns 8-11: the corresponding flux quality in the four IRAS band. Column 12: distance for each of the target sources (Yang et al. 2017) , primarily using kinematic distances calculated from Reid et al. (2014) . 