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SIMULTANEOUS OBSERVATIONS OF H2O AND SIO MASERS TOWARD KNOWN EXTRAGALACTIC WATER MASER SOURCES
SIMULTANEOUS OBSERVATIONS OF H2O AND SIO MASERS TOWARD KNOWN EXTRAGALACTIC WATER MASER SOURCES
Journal of The Korean Astronomical Society. 2015. Dec, 48(6): 357-364
Copyright © 2015, Korean Astronomical Society
  • Received : November 16, 2015
  • Accepted : December 06, 2015
  • Published : December 31, 2015
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SE-HYUNG CHO
DONG-HWAN YOON
JAEHEON KIM
DO-YOUNG BYUN
JAN WAGNER

Abstract
We observe ten known 22GHz H 2 O maser galaxies during February 19–22, 2011 using the 21 m Tamna telescope of the Korean VLBI Network and a new wide-band digital spectrometer. Simultaneously we searched for 43GHz SiO v = 1, 2, J = 1–0 maser emission. We detect H 2 O maser emission towards five sources (M 33, NGC 1052, NGC 1068, NGC 4258, M 82), with non-detections towards the remaining sources (UGC 3193, UGC 3789, Antennae H 2 O-West, M 51, NGC 6323) likely due to sensitivity. Our 22GHz spectra are consistent with earlier findings. Our simultaneous 43GHz SiO maser search produced non-detections, yielding – for the first time – upper limits on the 43GHz SiO maser emission in these sources at a 3 σ sensitivity level of 0.018K–0.033K (0.24 Jy–0.44 Jy) in a 1.75 km s −1 velocity resolution. Our findings suggest that any 43GHz SiO masers in these sources (some having starburst-associated H 2 O kilomasers) must be faint compared to the 22GHz H 2 O maser emission.
Keywords
1. INTRODUCTION
Maser emission has been detected in our Galaxy from many molecular species. The same maser lines can also occur in external galaxies, yet only few have been detected. One issue is the sensitivity of the observing facilities. External galaxies are distant compared to Galactic maser sources, and typically only kilo-, mega-, or gigamasers, labeled according to the maser luminosities relative to Galactic counterparts, can be detected.
The first extragalactic detection was that of 22GHz H 2 O maser emission toward the giant H II region IC 133 in the disk of the galaxy M 33 (Churchwell et al. 1977) . After considerable improvements in sensitivity, extragalactic H 2 O masers have been detected towards over 150 galaxies (see web sites of the Water Maser Cosmology Project 1 and Megamaser Cosmology Project 2 ). The OH maser species is detected towards nearly 120 galaxies (Klockner et al. 2004 ; Impellizzeri 2008) . Four new H 2 O masers were added by Wagner (2013) in a study of dual-species (OH and H 2 O) maser galaxies. Recently, extragalactic masers of H 2 CO, CH 3 OH, and SiO molecules were found, and Wang et al. (2014) report the first triple-species maser galaxy.
Masers are good probes for studying extreme physical conditions and dynamics in different regions of, e.g., nuclear starbursts, merging galaxies, outflows in active galaxies, and accretion disks around supermassive black holes in active galactic nucleis (AGNs) using very long baseline interferometry (VLBI). Water megamasers allow to determine accurate supermassive black hole masses, galaxy distances, and an accurate Hubble constant (Braatz et al. 2008 ; Reid et al. 2009 ; Kuo et al. 2011 ; Humphreys et al. 2013) . A review of megamasers can be found in Lo (2005) . See also Tarchi (2012) .
With regard to SiO maser lines, which are very common in oxygen-rich, evolved stars in our Galaxy, only one extragalactic stellar SiO ( v = 1, J = 2–1) maser source has been detected towards the red supergiant IRAS 04553-6825 in the LMC (van Loon et al. 1996) . In 2014 the high vibrational state maser of SiO ( v = 3, J = 2–1) and a CH 3 OH maser were detected to-wards the nearby Seyfert 2 galaxy NGC 1068 using the IRAM 30m telescope (Wang et al. 2014) . Drawing upon similarities with the H 2 O maser line velocities in this “AGN disk/jet maser” galaxy (cf. Gallimore et al. 2001) , Wang et al. associated SiO and CH 3 OH megamasers with the AGN accretion disk and a jet-cloud interaction, respectively. While such an association needs to be confirmed by imaging, it also opens the question whether SiO masers might be common in H 2 O maser galaxies. The literature, however, finds no systematic searches for SiO masers in H 2 O maser galaxies. Thus, while carrying out test observations with the Tamna 21m telescope of the Korean VLBI Network (KVN) to test the performance of a new wide-band digital spectrometer, we also undertook a simultaneous search for SiO masers towards ten known H 2 O maser galaxies.
In this paper, we report the results of the H 2 O maser observation and SiO maser search. In Section 2, we present the source selection and observations. Observational results and a discussion including the comments on individual sources, and the operation and performance of the wide-band digital spectrometer, are given in Section 3. A summary is given in Section 4.
http://www.cfa.harvard.edu/~lincoln/demo/HoME/
http://safe.nrao.edu/wiki/bin/view/Main/MegamaserCosmologyProject
2. SOURCE SELECTION AND OBSERVATIONS
Our ten observed sources are listed in Table 1 . Nine sources with relatively strong H 2 O maser emission were selected from a catalog of galaxies detected in H 2 O maser emission 3 . The Antennae (H 2 O West) galaxy was selected from Brogan et al. (2010) . Columns 1, 2, and 3 of Table 1 list our source names and positions with regard to the right ascension (R. A.) and declination (Dec.). Column 4 lists the systemic velocity of the target source. The distance and its reference are given in Columns 5 and 6, respectively.
Ten Known Extragalactic H2O Maser Sources
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Notes. Vsys: Systemic velocities of the galaxies based on the optical velocity convention, measured with respect to the LSR.
We observed the H 2 O 6 16 −5 23 (22.235080GHz) and SiO v = 1, 2, J = 1–0 (43.122080GHz, 42.820587GHz) maser lines during February 19 to 22, 2011 using the KVN Tamna 21 m single-dish radio telescope on Jeju island. The KVN system has a unique quasi-optic system for observing simultaneously at four frequency bands (22, 43, 86 and 129GHz) using three dichroic low-pass filters (Han et al. 2008 , 2013) . We used 22GHz and 43GHz band cooled HEMT (High Electron Mobility Transistor) receivers adjusted to receive only left-circular polarized signals.
Our observation parameters are presented in Table 2 . The digital spectrometer was set up in wide-band mode with a bandwidth of 256 MHz, corresponding to a radial velocity coverage of approximately 3500 km s −1 (at 22GHz) and 1780 km s −1 (at 43GHz). The velocity resolution was 0.84 km s −1 and 0.43 km s −1 at 22 and 43GHz, respectively, and was adjusted to approximately 1.7 km s −1 using Hanning smoothing. The system noise temperatures were 114K–130K at 22GHz and 170K–218K at 43GHz depending on the elevation and weather conditions. The half power beam widths and aperture efficiencies of the KVN Tamna telescope were measured and found to be 122′′, 0.66 (at 22GHz) and 64′′, 0.60 (at 43GHz), respectively (Lee et al. 2011) . We observed in position switching mode. The pointing accuracy was checked every two hours using strong SiO maser sources located near our target sources. The on-source integration time was close to one hour.
Observation Parameters
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Notes. ∗After Hanning smoothing over 2 (at 22GHz) and 4 (at 43GHz) spectrometer channels.
The data were calibrated using the chopper wheel method, which corrects atmospheric attenuation and the antenna gain variations depending on the elevation, in order to determine antenna temperature
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. Detection upper limits at 3 σ noise levels were 0.018K–0.027K (0.22 Jy–0.33 Jy) at 22GHz and 0.018K–0.033K (0.24 Jy–0.44 Jy) at 43GHz. The conversion factors of the KVN Tamna telescope from antenna temperature to flux density were approximately 12.08 Jy K −1 at 22GHz, and 13.29 Jy K −1 at 43GHz.
http://www.nrao.edu/~jbraatz
3. OBSERVATIONAL RESULTS AND DISCUSSION
Simultaneously obtained spectra of the detected H 2 O 6 16 −5 23 maser lines and the non-detected SiO v = 1, 2, J = 1–0 maser lines from five sources are shown in Figure 1 . We detected H 2 O masers towards spiral galaxy M 33, elliptical galaxy NGC 1052, Seyfert 2 galaxies NGC 1068 and NGC 4258, and starburst galaxy M 82. The NGC 4258 disk megamasers had the strongest peak and showed a broad range of emission, although blue components were not detected at this epoch.
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Simultaneously obtained spectra of detected H2O 616 − 523 maser lines and non-detected SiO v = 1, 2, J = 1–0 maser lines from five extragalactic sources in Feb. 2011. Another M 33 H2O maser spectrum on the right side is enlarged from VLSR = −400 km s−1 to 0 km s−1.
The spectral features towards these maser sources are consistent with earlier detections, and exhibit the characteristic spectral properties that reflect the different maser origins in these galaxies (e.g., masing Keplerian accretion disk, jet-related masers, star-forming activity). As one of the first observations that used the new KVN wide-band digital spectrometer, this consistency also gave confidence in its correct operation.
Spectral line properties of our H 2 O maser detections, and upper limits for our SiO maser non-detections, are presented in Table 3 . The observed sources are given in Column 1. The peak antenna temperatures of the H 2 O masers and the 3 σ upper limits of these temperatures of the SiO masers are given in Columns 2 and 3, respectively. Column 4 provides the integrated antenna temperatures. Columns 5 and 6 give the equivalent isotropic luminosities of the H 2 O and SiO masers including their upper limits in terms of solar luminosity (cf., Bennert et al. 2009) . For the latter estimations we used the integrated antenna temperatures, detection upper limits, and distances of Table 1 , and assumed a SiO maser line width of 5 km s −1 similar to that of NGC 1068 (Wang et al. 2014) .
Results of the H2O and SiO Maser Observations
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Notes. B indicates Blue–shifted maser features, C Central maser features, and R Red-shifted maser features. Upper limits are 3σ.
The peak velocities of H 2 O maser features towards each source are listed in Table 4 . For five known H 2 O maser sources (UGC 3193, UGC 3789, Antennae H 2 O West, M 51, and NGC 6323), we did not detect H 2 O maser emissions within our 3 σ detection limits of between 0.018 K (0.22 Jy) and 0.027 K (0.33 Jy).
Line Velocities of Detected H2O Masers
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Notes. B indicates Blue–shifted maser features, C Central maser features, and R Red-shifted maser features.
The SiO v = 1,2, J = 1–0 maser lines were not detected towards any of these ten sources at a 3 σ detection limit of between ~ 0.018K (0.24 Jy) and ~0.033K (0.44 Jy). We expected that the SiO maser could be detected from the H 2 O maser sources if their SiO maser photon luminosities were higher than the H 2 O maser photon luminosities, as in the case of evolved stars in our Galaxy. The average values of SiO maser photon luminosities are higher than those of the H 2 O photon luminosities in Mira variables and OH/IR stars of our Galaxy. For example, the average values of the SiO ( v = 1, J = 1–0) photon luminosities of Mira variables are estimated to be 10 43.1 photon s −1 (10 −6.3 L ), while those of H 2 O photon luminosities are 10 42.8 photon s −1 (10 −6.6 L ) (Kim et al. 2014) . These results imply that the excitation condition of the SiO maser emission in the above five H 2 O maser-detected sources is different from that of our Galactic evolved stars. This particular excitation condition of SiO masers may be supported by the detection of the v = 3, J = 2–1 maser emission in the Seyfert 2 galaxy NGC 1068 (Wang et al. 2014) in spite of the marginal detection of the SiO v = 1, J = 2–1 maser and non-detection of v = 2, v = 2–1 maser. In our Galactic sources, SiO maser intensities normally decrease with increases in the vibrational state v for the same rotational transition J although the intensity of the SiO v = 2, J = 1–0 maser is stronger than that of the v = 1, J = 1–0 maser in fairly numerous post-AGB stars (Cho et al. 1996 ; Yoon et al. 2014) . Specifically, the intensity ratios among v = 1, 2, 3, J = 2–1 maser lines are 1 : 0.40 : 0.04 for the sole SiO v = 3, J = 2–1 maser detected source χ Cyg (Cho et al. 2007) . Wang et al. (2014) suggest that the SiO ( v = 3, J = 2–1) maser from the Seyfert 2 galaxy NGC 1068 likely originates from the nuclear disk and not from the hundreds of millions of χ Cyg like S-type Mira variables. One example of these different excitation conditions between AGNs and Galactic evolved stars may be a different radiation mechanism of infrared emission which is one of main factors of SiO maser pumping. Infrared emission from Galactic evolved stars is a thermal while that from AGNs is synchrotron radiation. This difference between them is well-known for optical emission lines (Veilleux & Osterbrock 1987) .
Concerning the non-detection of the SiO maser emission from our observed extragalactic sources, excitation conditions and locations, SiO abundance, and sensitivity should be considered. The SiO maser emission induced by radiative and/or collisional pumping (Bujarrabal et al. 1994 ; Humphreys et al. 2002) requires very high temperatures (> 1000K) and densities (> 10 9 cm −3 ) for its excitation; the v = 1 state is 1770K above the ground state (Elitzur et al. 1980) while the 22GHz H 2 O maser induced by collisional pumping (Yates et al. 1997) requires a temperature ranging from 300K to 1000K and densities ranging from 10 7 to 10 9 cm −3 (Benson & Little-Marenin 1996) . Therefore, the SiO masers arise from a region close to the central stars, i.e., between 2 and 4 stellar radii in Galactic evolved stars (Diamond et al. 1994) . These facts imply that the SiO masers from extragalactic sources also arise from regions of very high densities and temperatures, i.e., close to their galactic centers, for example, close to the AGNs; from the circumnuclear disk in the case of the NGC 1068 SiO maser emission. Furthermore, the abundance of SiO molecules in the nuclear region is enhanced by shocks and X-ray irradiation linked to nuclear activity as suggested by García-Burillo et al. (2010) in NGC 1068. They reported that the enhanced SiO abundance in the circumnuclear disk of NGC 1068 (García-Burillo et al. 2014 , 350 pc -size) is approximately one to two orders of magnitude higher than that in the starburst ring with a 1–1.5 kpc radius. Therefore, the most likely regions of SiO maser emission could be located at the circumnuclear disk regions close to the AGN, in which sufficient gas is accreted from the outer disk and where the molecular outflows are likely driven by the AGN similar to the small-scale SiO maser emission in the Orion KL (Matthews et al. 2010 ; Vaidya & Goddi 2013) . However, another important factor pertaining to the actual detection of SiO maser emissions will be the degree of a sensitivity. For the SiO maser detected source NGC 1068 (at 14.4 Mpc; Gallimore et al. 2001) , the peak intensities are close to 4 mK (17mJy) and 5.5 mK (23mJy) in the v = 1, 3, J = 2–1 maser lines (Wang et al. 2014) . Therefore, if the intensity ratio between the SiO J = 1–0 and J = 2–1 masers is assumed to be one in NGC 1068, we could not detect the SiO v = 1, 2, J = 1–0 masers from NGC 1068 within our upper limits of 0.024 K (0.32 Jy for v = 1) and 0.027 K (0.36 Jy for v = 2) using the KVN. An on-source integration time of approximately twelve hours is required to detect signals of SiO masers of approximately 0.021 Jy at 3 σ noise levels from NGC 1068.
- 3.1. Comments on Three Individual Sources
NGC 1068: The H 2 O maser emission from this prototypical Seyfert 2 barred galaxy was first detected by Claussen et al. (1984) . As shown in Figure 1 , we detected three H 2 O maser features which correspondingly peaked at 855, 1125, and 1434 km s −1 . These three features are nearly symmetric with respect to the recessional velocity of the galaxy (V LSR = 1137 km s −1 , Brinks et al. 1997) . The maser feature which peaked at 1125 km s −1 is associated with the core of the compact radio source, S1 as the nuclear masers (Gallimore et al. 1996 , 2001) . The red-shifted masers peaked at 1434 km s −1 and blue-shifted masers peaked at 855 km s −1 about the systemic velocity are also nuclear masers. However, possibly due to variability, we could not detect the “jet masers” near 900 km s −1 which are associated with radio jet continuum feature C.
NGC 4258: The systemic H 2 O maser features around the recessional velocity (V sys = 672 km s −1 , Cecil et al. 1992) of the galaxy were initially detected by Claussen et al. (1984) . The high-velocity features blue- and red-shifted with respect to the systemic velocity were discovered by Nakai et al. (1993) . VLBI studies showed that maser emission originates from a rotating disk (Greenhill et al. 1995) . A Keplerian rotation curve and warp in the disk structure were confirmed via VLBA observations (Miyoshi et al. 1995) . This archetypal circumnuclear H 2 O maser is used for measuring the accurate geometric distance to the active galaxy NGC 4258 (Argon et al. 2007 ; Humphreys et al. 2013) . As shown in Figure 1 , in 2011 February we could not detect blue-shifted maser features within our upper limits of 0.024K. In addition, SiO v = 1, 2, J =1–0 masers were not detected around the velocity of the central H 2 O maser features (around the systemic velocity of the galaxy) within our upper limits of 0.018K (0.22 Jy).
M 82 (NGC 3034): The H 2 O maser emission was initially detected by Claussen et al. (1984) . The galaxy M 82 is a starburst galaxy undergoing a massive star-forming episode (Wills et al. 1999) . A large-scale biconical outflow of hot gas was observed at X-ray and optical wavelengths from the nucleus of M 82 (Bregman et al. 1995 ; Shopbell & Bland-Hawthorn 1998) . We detected blue- and red-shifted H 2 O maser features with respect to the systemic velocity (V LSR = 200 km s −1 ). Hagiwara et al. (2004) associate these features with a molecular bipolar outflow. The broad feature occurring around V LSR = 109 km s −1 showed flaring with a luminosity similar to the maximum luminosity observed in the Galactic star forming region W 49N (Baudry et al. 1994) . In our observations, the red-shifted maser feature is narrow and shows a high intensity. The vertical filament feature of the SiO thermal emission with respect to the galaxy plane was referred to as the SiO chimney emanating from the disk by García-Burillo et al. (2001) . They explained this in terms of shock chemistry driven by a violent gas ejection from the starburst disk. We could not detect the SiO v = 1, 2, J = 1–0 maser emission within our upper limits of 0.024 K (0.32 Jy for v = 1) and 0.027 K (0.36 Jy for v = 2).
- 3.2. Operation and Performance ofWide-Band Digital Spectrometer
The digital spectrometer of the KVN has two types of input ports and selects one of them depending on the operation mode; narrow-band or wide-band mode. In narrow-band mode, it uses one VLBI Standard Interface (VSI) input from a digital filter unit that has a total frequency bandwidth of 256 MHz. This mode is mainly used for spectroscopic observations requiring high spectral resolution. In wide-band mode, the spectrometer uses VSI inputs from four digital samplers, each offering a frequency bandwidth of 512 MHz. The digital spectrometer can produce a maximum of 8 spectra of 8192 channels each, and its control software can take only 4096 channels for each spectrum. In wide-band mode, we can take 4096 channels across whole 512 MHz band-width after smoothing or binning every 2 channels. We can also get 256 MHz (sub)bandwidth by selecting a continuous 4096 out of 8192 available channels. The latter was used for our observations. For details on the backend and its available modes see Oh et al. (2011) .
We compared rms noise levels of spectra against values expected from system noise temperatures, integration time, quantization loss, and spectral resolution. We found that in 1–2 hour integrated spectra these are consistent within 6%. For the above comparison, we subtracted 1st or 2nd order polynomial baselines from the spectra. The measured rms noise levels were 4% higher than the expected values on average. There was no noticeable change in the excess noise ratio with the integration time from one minute to two hours. We confirmed that the rms noise levels decrease with 1/
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, where τ is the integration time. This indicates that the noise of a spectrum is dominated by random noise, and contribution of systemic noise such as residual baselines or spurious signals is much less than that of random noise components.
4. SUMMARY
We undertook simultaneous observations of H 2 O and SiO masers toward ten known extragalactic H 2 O maser sources in February 2011 using the Korean VLBI Network (KVN) single dish telescope. We also aimed at testing the performance of a wide band digital spectrometer at first stage of its operation. The results are summarized below.
  • 1. We detected the 22GHz H2O maser emission from five known extragalactic H2O maser sources; M 33, NGC 1052, NGC 1068, NGC 4258, and M 82. However, from another five known extragalactic H2O maser sources; UGC 3193, UGC 3789, Antennae (H2O W), M 51, and NGC 6323, we could not detect the H2O maser emission within 3σupper limits of 0.018–0.027 K (0.22–0.33 Jy).
  • 2. The detected H2O maser lines of five known extragalactic H2O maser sources exhibit central features around their systemic velocities and/or blue-and red-shifted features according to their originality as is previously known (i.e., central features around systemic velocities from spiral galaxy M 33 and elliptical galaxy NGC 1052, central features together with blue- and red-shifted features from Seyfert 2 galaxy NGC 1068, central features together with red-shifted features from the Seyfert 2 galaxy NGC 4258, and blue- and red-shifted features from the starburst galaxy M 82). The blue-shifted features from NGC 4258 were not detected within the upper limits of 0.024K (0.29 Jy).
  • 3. We could not detect the SiOv= 1, 2,J= 1–0 maser emission from any of the ten known extragalactic H2O maser sources within our upper limits of 0.018K–0.033K (0.24 Jy–0.44 Jy). The SiO maser emission in extragalactic sources is very faint or rare compared to the H2O maser. An on-source integration time of more than twelve hours is required to detect the ~20 mJy level SiO maser emission similar to that of NGC 1068 using the KVN single dish telescope.
  • 4. We confirmed that the digital spectrometer of the KVN is properly working in wide-band mode and the 22GHz and 43GHz receivers are stable enough to provide good baselines characteristics well fitted with first or second order polynomials over a 256 MHz frequency bandwidth. The detected H2O maser spectral features from five known extragalactic H2O maser sources are consistent with earlier detections. As one of the first observations that used the new KVN wide-band digital spectrometer, this consistency gave confidence in the correct operation of the new spectrometer.
Acknowledgements
This work was supported by the Basic and Fusion Research Programs (2011–2015) and also partially supported by the KASI–Yonsei Joint Research Program entitled the “Degree and Research Center Program” funded by the National Research Council of Science and Technology (NST). We are grateful to all of the staff members at KVN who helped to operate the array, operate the single dish telescope, and to correlate the data. The KVN is a facility operated by KASI (Korea Astronomy and Space Science Institute). The KVN operations are supported by KREONET (Korea Research Environment Open NETwork) which is managed and operated by KISTI (Korea Institute of Science and Technology Information).
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