SiO, 29SiO, and 30SiO emission from 67 oxygen-rich stars. A survey of 61 maser lines from 7 to 1 mm
aa r X i v : . [ a s t r o - ph . S R ] F e b Draft version February 9, 2021
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SiO, SiO, and SiO emission from 67 oxygen-rich stars.A survey of 61 maser lines from 7 to 1 mm
J. R. Rizzo,
1, 2
J. Cernicharo, and C. Garc´ıa-Mir´o Centro de Astrobiolog´ıa (INTA-CSIC), Ctra. M-108, km. 4, E-28850 Torrej´on de Ardoz, Madrid, Spain ISDEFE, Beatriz de Bobadilla 3, E-28040 Madrid, Spain Grupo de Astrof´ısica Molecular, Instituto de F´ısica Fundamental (IFF-CSIC), C/ Serrano 121, E-28006 Madrid,Spain Joint Institute for VLBI ERIC (JIVE), Oude Hoogeveensedijk 4, 7991 PD Dwingeloo, The Netherlands
Submitted to Astrophysical Journal Supplement SeriesABSTRACTCircumstellar environments of oxygen-rich stars are among the strongest SiO maseremitters. Physical processes such as collisions, infrared pumping and overlaps favorsthe inversion of level population and produce maser emission at different vibrationalstates. Despite numerous observational and theoretical efforts, we still do not have anunified picture including all the physical processes involved in the SiO maser emission.The aim of this work is to provide homogeneous data in a large sample of oxygen-richstars. We present a survey of 67 oxygen-rich stars from 7 to 1 mm, in their rotationaltransitions from J = 1 → J = 5 →
4, for vibrational numbers v from 0 to 6 inthe three main SiO isotopologues. We have used one of the 34 m NASA antennas atRobledo and the IRAM 30 m radio telescope. The first tentative detection of a v = 6line is reported, as well as the detection of new maser lines. The highest vibrationallevels seem confined to small volumes, presumably close to the stars. The J = 1 → v = 2 line flux is greater than the corresponding v = 1 in almost half of the sample,which may confirm a predicted dependence on the pulsation cycle. This database ispotentially useful in models which should consider most of the physical agents, timedependency, and mass-loss rates. As by-product, we report detections of 27 thermalrotational lines from other molecules, including isotopologues of SiS, H S, SO, SO , andNaCl. Keywords:
ISM: molecules — masers – stars: circumstellar matter — stars: evolution— stars: winds, outflows — surveys INTRODUCTION
Corresponding author: Ricardo [email protected]
Evolved oxygen-rich stars are among the mostpowerful maser emitters known to date. Maseremission in SiO rotational transitions of vibra-tionally excited states is ubiquitous and very in-tense in these sources. Rotational transitions up
Rizzo et al. to J = 7 → v = 1 , , SiO and SiO (e.g. Deguchi et al. 1983;Cernicharo et al. 1991; Alcolea & Bujarrabal1992; Cernicharo & Bujarrabal 1992;Gonz´alez-Alfonso et al. 1996).Despite the large amount of observationaldata available in the literature, SiO maser emis-sion has complex aspects that deserve furtherobservational and theoretical effort. Besides theoverall inversion of the rotational levels in eachvibrational ladder, the SiO emission displays in-triguing anomalies in some specific rotationallines, such as drastic changes in intensity fromone rotational line to the next within the same v -state. Although the general inversion pro-cess seems to be relatively well understood (e.g.Bujarrabal 1994a,b), the differences in the emis-sion of adjacent rotational lines are difficult toexplain upon standard radiative and collisionalpumping models.Such anomalies, which are particularly impor-tant for the high- v states of SiO, also applyto the less-abundant isotopologues SiO and SiO in v = 0 , , SiO, SiO and SiO (Gonz´alez-Alfonso & Cernicharo 1997;Herpin & Baudry 2000). The excitation ofthe vibrational levels depends on the amountof dust in the envelope and on the effectivetemperature of the star photosphere. Fur-thermore, an overlap between SiO and H Ohas been proposed to explain the v = 2 J = 2 → SiO (Olofsson et al. 1981,1985; Langer & Watson 1984; Bujarrabal et al.1996). Optical pumping is also a possible mechanismto account for the observed features in theselines. Rausch et al. (1996) have modelled syn-thetic atmospheres of M-stars immersed in ex-panding envelopes and show that optical pump-ing may account for some features of maseremission even without collisions; moreover, theregions of inversion may be different from oneisotopologue to another, depending on the ve-locity difference between the photosphere andthe emitting volume. Optical pumping throughthe A Π-X Σ electronic transition could be veryefficient in stars with moderate/low mass lossrate and hot photospheres in which photons at250 nm could excite the Π state. Excitationthrough the triplet states of SiO could also oc-cur at 330 nm.The excitation of the SiO masers throughcollisions with H and He is a subject stillopen. Before the work of Dayou & Balan¸ca(2006), who performed new potential energysurface calculations of the system SiO/He/p-H , there were not accurate ro-vibrational colli-sional rates. Recently, Balan¸ca & Dayou (2017)extended the computation of collisional rateswith He in the temperature range 300 – 6 000 K,for the first six vibrational levels and up to therotational states J = 40.Despite the many years since the discovery ofSiO masers, robust and realistic models whichtake into account all the possible mechanismsfor pumping are still necessary. To distinguishbetween the different physical processes leadingto the population inversion of the SiO energylevels, and to retrieve key information aboutthe physical conditions of the gas in the regionbetween the photosphere and the dust growthzone, it is necessary to gather the most com-plete, simultaneous and homogeneous sampleof the SiO rotational emission in the differentvibrational states. The current availability ofwideband backends spanning several GHz of in-stantaneous bandwidths make possible nowa- iO, SiO, and SiO in oxygen-rich stars SiO in6 evolved stars by Schwartz et al. (1982), theline survey in the red supergiant VY CMa byCernicharo et al. (1993), the study of 12 sourcesby Pardo et al. (1998), the survey by Cho et al.(1996) of six J = 1 → SiO and SiO, andthe study of the J = 1 → v = 1 and 2 linesdone by Kim et al. (2010). Most of the otherstudies, however, have been carried out in dif-ferent epochs, with different instruments and,sometimes, without a complete coverage of therotational transitions from different vibrationallevels. Due to the variability of the SiO maseremission and to the complexity of the physicsof stellar pulsation (which is in turn associatedto the line pumping), the observations gatheredin different epochs cannot be compared to inferrobust conclusions about the excitation of SiO.In this paper, we report a survey of SiO, SiO, and SiO maser lines towards 67 evolvedoxygen-rich stars. The selected sources spandifferent mass losses, temperatures, and C/Oabundance ratio . As a by-product, this workalso provides valuable information about themolecular content of these objects in the sur-veyed frequency ranges. The survey was done The C/O abundance ratio is < >
1, exhibit SiO thermalemission but not maser lines. using one of the 34 m antenna of the MadridDeep Space Communications Complex (here-after MDSCC) and the IRAM 30 m radio tele-scope at Pico Veleta. A total of 61 transitionsfrom J = 1 → →
4, and v = 0 to 6 wasobserved in the whole sample. In Sect. 2 we de-scribe the observations. We present the resultsin Sect. 3. In Sect. 4 we discuss some global re-sults of the survey, including polarization, vari-ability, some special cases and the identificationof other spectral lines. We summarize the mainfindings in Sect. 5. In a follow up paper, we planto use this database to model the circumstellarenvelopes (CSEs), using an already developednon-local radiative transfer code which includesinfrared overlaps between the three silicon iso-topes of SiO, collisional pumping, and opticaland infrared excitation. OBSERVATIONS2.1.
Overview, sources and strategy
As said in the previous section, we have donea survey of 67 oxygen-rich evolved stars intheir SiO, SiO, and SiO maser line emission.The DSS-54 antenna of the Madrid Deep SpaceCommunications Complex (MDSCC) was usedin the first part of the survey to observe the J = 1 → ∼
43 GHz). Based on these initial results,we observed the most relevant sources in the J = 2 → →
4, at wavelengths of 3, 2 and1 mm, using the 30 m IRAM radio telescope atPico Veleta (Spain). The MDSCC observationswere done between March and July 2012, andthe IRAM observations in August 2012.We have chosen the observing modes and thebands in order to optimize the tuning of thelargest possible number of simultaneous lines.The lines observed (61 in total) and their cor-responding frequencies are indicated in Table1. The frequencies have been obtained from the
Rizzo et al.
CDMS (M¨uller et al. 2001, 2005) and the JPL (Pickett et al. 1998) catalogues. We also usedinformation from MADEX (Cernicharo 2012)when the above mentioned catalogues did notprovided sufficient precision. The list of the ob-served sources are presented in Table 2, togetherwith some useful information, such as the dateof observation, transitions, observing modes, ve-locity spacing, integration time, rms noise, andpolarization recorded. The DSS-54 antenna isable to record both circular polarizations, whilethe 30 m radio telescope records lineal polariza-tions.The half-power beam width (HPBW) of bothtelescopes at the different frequencies are in-dicated in Table 3, together with sensitivitiesand efficiencies. The spectra have been cor-rected for atmospheric opacity and elevationgain ( T ∗ a scale) during the observation, and con-verted to flux density ( S scale) during the re-duction process. The conversion from T ∗ a tomain-beam temperature ( T MB ) can be done by T MB = T ∗ a /η MB , being η MB the main beam effi-ciency, also depicted in Table 3. Unless specif-ically stated, we use the flux density scale (inJy) throughout all the paper, and in the onlinetables. 2.2. MDSCC observations
We used the NASA DSS-54 antenna of theMDSCC to observe the J = 1 → http://spec.jpl.nasa.gov/ftp/pub/catalog/catform.html https://nanocosmos.iff.csic.es/madex/ backend (Rizzo et al. 2012). The observationswere done in 14 different sessions betweenMarch 23 and July 26, 2012. At the begin-ning, the backend had the capacity to pro-cess a single circular polarization, with a band-width of 1.5 GHz, 8192 channels, and a fre-quency spacing of ∼
183 kHz (equivalent to1.28 km s − ). At some point during the sur-vey, a second FFTS board were incorporated,allowing the possibility of observing both cir-cular polarizations simultaneously and to use ahigh-resolution mode, which provided 500 MHzof bandwidth, 16384 channels, and a frequencyspacing of ∼
31 kHz (equivalent to 0.21 km s − ).The broad band FFTS backend was centeredat 42.75 GHz, which allowed to simultaneouslyobserve the 10 lines indicated in Table 1. The500 MHz bandwidth FFTS was always centeredat 42.97 GHz, in order to simultaneously ob-serve the J = 1 → v = 1 , SiO v = 0. This setup is indicated as1 − ∗ in Table 2.A total of 56 stars have been observed us-ing this telescope with the largest bandwidth(1.5 GHz), 11 of those during two or more daysfor cross-checking and to study possible vari-ability. A number of 28 out of those 56 targetstars have also been observed with the high-resolution mode (i.e., 500 MHz bandwidth) toincrease details about the line profiles.We corrected the observed positions by assum-ing the standard pointing model for this an-tenna in Q-band, which is accurate to within8 ′′ . This model was also regularly checked andimproved at specific sessions in the epoch of ob-servations, and we estimate that pointing er-rors can account intensity uncertainties alwaysbelow 10%. At the beginning of each observ-ing session, we also cross-checked the pointingby means of the observation of sources includedin the paper of Rizzo et al. (2012). Focus wasoptimized for Q-band using specific calibrationsessions, and automatically corrected during ob- iO, SiO, and SiO in oxygen-rich stars ′ in azimuth. In 38 cases, we observedin frequency-switching mode, with a frequencythrow of 13.2 MHz to avoid ripples. The at-mospheric opacity was always between 0.07 and0.1. 2.3. IRAM observations
We used the IRAM 30 m radio telescope inPico Veleta, Spain, to observe the J = 2 → → ∼
195 kHz. Four of these units were alwaysused at the 3 mm band, tuned at 85.045 GHz(the central frequency of the J = 2 → J = 3 → → J = 4 → v = 4 to 6, SiOat v = 2 to 5, and SiO at v = 0 to 3; this ad-ditional mode is indicated as “4 − ∗ ” in Table2. The 3 mm unit centered at 88.775 GHz wasused to search of other molecules.The observations were done in wobbler switch-ing mode (which provides very flat baselines), with a throw at 90 ′′ at a rate of 2 Hz. Systemtemperatures varied in the ranges 110–220 K,134–360 K, 770–3080 K, and 390–1300 K for the J = 2 → → − . ′′ . Every day, wealso observed W3(OH) as a line calibrator(Mauersberger et al. 1989). Focus was checkedand corrected at the beginning of each sessionand after sunset.A total of 38 sources have been observed, 11of them not included in the MDSCC sample. RESULTS3.1.
Overview
All detections are presented in Table 4. Ineach row, the table depicts the observation ID,the source name, the transition detected, theparameters of the lines, and individual com-ments (if any). The transitions in each entrycontains the isotopologue, the rotational quan-tum numbers J → J −
1, and the vibrationalstate. The parameters include the line flux ( F ),the flux-weighted velocity ( V LSR ), and the veloc-ity range of emission above 3-sigma ( V min and V max ) . F and V LSR were computed in the veloc-ity range ( V min , V max ). Some relevant informa-tion are also added in several entries to Table4 as individual comments. These remarks aremostly referred to the cases when data smooth-ing has been applied to improve the signal-to-noise ratio. In other cases information aboutpolarization and line blending is included. The V min and V max were determined by the first and last oc-currences of two consecutive channels with temperaturesabove 3-sigma. Rizzo et al. only instrumental feature that we noted lies ∼
20 MHz apart from the J = 5 → v = 3 lineof SiO; although the detection and parametersare fairly well determined, the cases in which thespurious feature is observed are commented inthe table.For some cases, improvement of the signal-to-noise ratio was necessary to achieve clear de-tections; this was done by the average of datagathered during different days and/or from dif-ferent polarizations. These cases are shown inTable 5, in the same format as Table 4. Theseaveraged spectra not only allowed the detectionof lines, but also permitted us to identify widecomponents in at lest two cases: the J = 2 → v = 0 line of SiO in S Per and in the J = 2 → v = 0 line of SiO in IRC+60154 (see commentsin Table 5).As an example, the Fig. 1 depicts thefull range spectrum of one of the sources(IRC+10011 = WX Psc) in the J = 1 → Some examples of individual features
In the following, a series of figures illustratessome of the properties found in the sample, par-ticularly with respect to line shapes, variabilityand polarization.
Line profiles . The physical conditions topump masers are so restrictive that the emit-ting volumes are relatively small; therefore, oneof the fingerprints of the maser emission is thatthe velocity components are narrow, typically1 km s − or even less.Depending on the pumping mechanisms andthe physical conditions, the maser emittingregions dramatically change from one sourceto another, and also from one line to an-other (Gray et al. 2009). This trend is con-firmed by high angular resolution observa-tions (see, for example, Soria-Ruiz et al. 2007;Wittkowski et al. 2007). When these kind ofsources are observed by single dishes, though, the different emitting regions and physical con-ditions are reflected in a variety of line profiles.Figure 2 shows six representative examples ofthe line shapes present in the catalog. For eachpanel, source name is indicated on the upperleft and the transition (in abridged format) inthe upper right corner. In the case of S Perthe spectrum is dominated by two peaks, but isthe result of a superposition of several individ-ual blended components. In the case of S Cas,the shape of a truncated parabolic and wide lineis indicative of thermal emission from the CSEas a whole. In O Cet the SiO J = 4 → v = 2 line displays a component at ∼
57 km s − which is right outside the velocity range of thethermal line; the J = 4 → v = 1 line (lowerleft panel) has a Gaussian shape, and is cen-tered at the star velocity. The line depicted forIRC+10011 is representative of a typical verynarrow maser line. And finally, the line dis-played for NML Tau ( SiO J = 3 → v = 0)seems the result of the superposition of both theCSE thermal component and at least one masercomponent. Variability . Most of the SiO and isotopo-logues maser lines in evolved stars develop ahigh degree of variability on scales from daysto years (Humphreys et al. 2002; Pardo et al.2004). The J = 1 → v = 1 and v = 2 lines,respectively. It is remarkable the case of µ Cep,which presents a dramatic variation where thehighest fluxes roughly double the lowest ones.In order to provide more details, Fig. 4 shows iO, SiO, and SiO in oxygen-rich stars v = 1 and v = 2 lines.Another clear example of line variability isshown in Fig. 5, where the SiO J = 1 → v = 0 line of VX Sgr significantly changed injust two weeks. Polarization . A significant part of the maserlines are often linearly and circularly po-larized due to intrinsic magnetic fields (e.g.Shinnaga et al. 2004; Vlemmings, et al. 2011;Shinnaga et al. 2017). The IRAM spectra con-tains valuable information about lineal polariza-tion of these sources, although it is not possibleto derive the Stokes parameters with the presentobservations. Even though, the simultaneousobservations of both lineal polarizations duringfour consecutive nights allowed the discovery ofhighly polarized components. Two examplesare shown in Fig. 6: in IRC+10011, the SiO J = 2 → v = 0 line depicts in the horizon-tal polarization a component at ∼
10 km s − )which is virtually absent in the vertical polariza-tion; the second example is VY CMa, where theSiO J = 4 → v = 3 line displays significantlydifferences between the two linear polarizationin the two principal velocity components.3.3. Identification of other spectral lines
For a significant fraction of the sample, a fre-quency range of up to ≈
30 GHz has been sur-veyed. This large bandwidth permits also thesearch for other molecules. For each source,we averaged the spectra corresponding to alldates and polarizations, and looked for molecu-lar species other than SiO and its isotopologues. A total of 27 lines have been detected. Table 6provides the list of those spectral lines togetherwith some useful information, such as the fre-quencies, quantum numbers, and energies of theupper levels. For the sake of brevity, we labeledthe spectral lines by a letter followed by a num-ber; the letter indicates the molecular species,while the number designates the transition de-tected, ordered by isotopologue and frequency.Detections are presented in the Table 7. Atotal of 20 stars with detections of some of theabove mentioned 27 thermal lines are included.In all cases spectra have been smoothed to a ve-locity resolution of 2 km s − . Positive detectionsare labeled by “Y”, negative results by “N”, anddetections after further smoothing by “S”.A brief analysis of the results are presented inSect. 4 below. DISCUSSION4.1.
The highest vibrationally excited lines
R Cas is one of the strongest SiO maseremitter, and has been the subject of numeroussingle-dish and interferometric observations upto v = 3 (see, for example Phillips, et al. 2001;Phillips et al. 2003; McIntosh & Hayes 2008;McIntosh & Patriat 2010; Assaf, et al. 2011,2013). We report here the first tentative de-tection of a v = 6 line, corresponding to therotational transition J = 4 →
3. The line, dis-played in Fig. 7 (left panel), is very narrow andhas been significantly detected after averagingthe two lineal polarizations (Table 5).We also report the tentative detection of an-other v = 6 line, the one corresponding to J = 2 → χ Cyg (ID 348 in Table4). The line, very narrow, is also depicted inFig. 7 (right panel). χ Cyg also displays theonly v = 5 line of the whole survey. This alsocorresponds to the J = 2 → J = 2 → Rizzo et al. highly vibrationally excited lines have been de-tected in only one scan. Taken into account thatboth lines are detected at ≈ σ level, χ Cyg de-serves further observations, because both highlyvibrationally excited lines may be polarized andrapidly variable, as has been suggested by recentobservations of the intense J = 2 → v = 1line (G´omez-Garrido et al. 2020).In χ Cyg, the intraday variability claimedby G´omez-Garrido et al. (2020) is confirmed byour data in the v = 1 and v = 2, J = 2 → J = 1 → J = 2 → v = 1 and v = 2 line fluxes are very dispersed around themean value, with departures from the averageup to 20 %. This is clearly illustrated in Fig. 8,where the integrated fluxes of the three lines areplotted as a function of the scan IDs; the fluxesare integrated between − − andnormalized to the average of the six scans (345to 350).To our knowledge, there is only one reporteddetection of a v = 5 line, which is thatcorresponding to J = 8 → J = 11 → v = 4 line has been re-ported in the high-mass young stellar objectOrion Source I (Hirota et al. 2018; Kim et al.2019). In an evolved star, however, there is onlyone detection of a v = 4 line SiO maser: the J = 5 → J = 3 → v = 4 line in VY CMa and for thefirst time in other four sources: IRC+10011,R Leo, VX Sgr, and S Per. As expected, theline is very narrow and highly polarized, beingVY CMa the only source where the line wasdetected in both lineal polarizations; the signif-icant detection in S Per was reached after av-eraging both polarizations. The narrowness ofthe lines is not unusual, but the significance of the detections should be monitored carefully. Itis worth noting that the maser emission of thisline was predicted by Herpin & Baudry (2000)as the result of infrared line overlaps.4.2. About the emitting region
Masers request different physical conditionsto invert the level population. It is there-fore expected that the emitting volumes changefrom one maser to another. This is con-firmed by interferometry at low v -states (e. g.Gonidakis et al. 2010; Kami´nski et al. 2013;Richter et al. 2013). Such restrictive physicalconditions are met through different mecha-nisms (radiative pumping, collisional pumping,overlaps), as explained in Sect. 1. In addition,we are dealing with pulsating stars, which addsthe time dependency of such conditions.As our survey contains almost simultaneousobservations of all masers, it is particularly suit-able to get an idea about the overall distributionof the emitting regions. A first approach is pro-vided in Fig. 9, where we plot the normalizedcumulative frequencies of the vibrational levels0 to 3, as a function of the velocity range ofemission. As v increases, the lines are moreconcentrated to smaller velocity ranges. As-suming that the velocity dispersion is corre-lated with the emitting volume, this tendencystrongly suggests that the emitting region isconfined to smaller volumes for larger v . As ex-pected, this result also indicates that the physi-cal conditions (temperature and density, IR ra-diative field) to produce maser emission becomemore restrictive as v increases.Yun & Park (2012) simulated SiO maser emis-sion in Mira-type stars under non-LTE condi-tions, considering different velocity gradients,and covering a complete pulsation cycle. Oneof the most robust results is the prediction ofthe J = 1 → , v = 2 line being more intensethan the corresponding v = 1 in half of the pul-sation cycle, and the opposite in the other half.We can test this prediction with our sample, iO, SiO, and SiO in oxygen-rich stars v = 1 line and other two with detections of the v = 2 line. The Fig. 10 sketches the main find-ings. In the left panel –Fig. 10(a)–, we plotthe flux ratio of the v = 2 to v = 1 lines as afunction of the scan ID, while in the right panel–Fig. 10(b)–, it is shown the distribution of thesame line ratio in bins of 0.2 width. The me-dian (0.84) and mean (0.11) of the sample arealso indicated in the figure, which helps to in-fer a rather uniform distribution of the ratiosaround values close to one, i.e., without a cleardominance of one line over the other.We have counted a total of 33 sources (44%)where F( v = 2) is greater than F( v = 1), and 42cases (56%) with the opposite behavior. Over-all results of this rather simple analysis seemto confirm the prediction made by Yun & Park(2012), although a more thorough and case-by-case analysis should be performed to provide afirm confirmation.4.3. “Bonus” thermal lines In order to provide an overall view aboutthe thermal lines detected, we divided theminto four groups. The first group is con-stituted by the C-bearing molecules HCO + ,HNC, HCN and H CN. HCO + (A1 in Ta-ble 6) is a wide spread molecule besides H and CO, abundant in a variety of astronomi-cal sources such as comets, diffuse clouds, andmolecular clouds, but with abundances belowthe predicted values in AGB stars (Glassgold1996). HCO + was firstly discovered in VY CMa(Ziurys et al. 2007) and later in other sources(e.g. Pulliam et al. 2011), including TX Camand NML Cyg. We detect HCO + in 10 sources.HNC (B1 in Table 6) was first tentatively re-ported by Lindqvist et al. (1988) in TX Cam,and later detected by Ziurys et al. (2009) in VY CMa. We detect HNC in TX Cam,NML Tau, and NML Cyg, but not in VY CMaprobably due to a high noise level. HCN (C1 inTable 6) is the most common molecule found inthe survey, detected in 19 out of the 20 sources.It was already detected by several authors (e.g.Lindqvist et al. 1988; Nercessian et al. 1989;Ziurys et al. 2009) in some of the stars ofour sample (IRC+10011, NML Tau, TX Cam,VY CMa, VX Sgr, NML Cyg, and R Cas). Itsisotopologue H CN (C2 and C3 in Table 6)is less abundant and therefore hardly detected;it was reported and analyzed in IRC+10011,NML Tau (= IK Tau), VY CMa and NML Cyg(Nercessian et al. 1989; Tenenbaum et al. 2010;Velilla Prieto, et al. 2017).The second group (lines D and E in Ta-ble 6) is constituted by the sulfur-bearingmolecules SiS and H S, and some of their iso-topologues. Around evolved stars, SiS andH S are tracers of warm gas, probably above100 K (S´anchez Contreras et al. 2015, and ref-erences therein), and are good tracers of thedust formation zones (Cernicharo et al. 2011).SiS was firstly reported by Lindqvist et al.(1988) in TX Cam, and later in NML Tau(Bujarrabal et al. 1994); we confirm here thosedetections and add other six to the list:IRC+10011, S Cas, VY CMa, VX Sgr,V111 Oph, and NML Cyg.H S was firmly detected by Omont et al.(1993) in IRC+10011, NML Tau, VY CMa,and NML Cyg; a tentative detection wasalso reported by Danilovich et al. (2017) inV1111 Oph. We add here the detection of H Sin TX Cam.The third group (lines F and G in Table 6) isformed by sulfur oxides. Together with the SiOmaser lines, sulfur oxides are the most abundantmolecules in oxygen-rich CSEs. SO (F1 to F5lines in Table 6) and SO (G1 to G5 in the sametable) have been detected since the first molecu-lar studies of these sources. Omont et al. (1993)0 Rizzo et al. detected up to three lines of SO in IRC+10011,NML Tau, VY CMa, RX Boo, and NML Cyg,none of them coincident to those reported inour survey. Later, Tenenbaum et al. (2010)performed a sensitive survey of VY CMa at1mm and reported several S-bearing moleculesin this source. A similar spectral survey to-wards NML Tau, but with a high spectral cov-erage (from 79 to 356 GHz) was recently pub-lished (Velilla Prieto, et al. 2017) with similarfindings. We detected SO and SO in the samesources as in the Omont et al. (1993) article,and also in VX Sgr and R Cas. The less abun-dant isotopologue SO (line F5) is detectedonly in NML Cyg. The 16 , − , line ofSO (G5), with the highest upper energy level(147.8 K) is only detected in VY Cma and NMLCyg.The fourth group is constituted by NaCland its isotopologue Na Cl. Four lines havebeen clearly identified, labeled as H1 to H4in Table 6. Since the first identification inCSEs (Cernicharo & Guelin 1987), this metalrefractory molecule has been firmly observedin IK Tau and VY CMa (Milam et al. 2007;Tenenbaum et al. 2010; Kami´nski et al. 2013;Decin et al. 2016; Velilla Prieto, et al. 2017);recently, it was tentatively detected in R Dor(De Beck, & Olofsson 2018), although not con-firmed with ALMA data (Decin et al. 2018).We failed to detect NaCl in IK Tau and VYCMa, although report the first detection inNML Cyg, as shown in Fig. 11. Besides thelines quoted in Table 7, the observed frequen-cies include also the J = 10 → → Cl (also shown in Fig. 11), not de-tected probably due to insufficient noise level. CONCLUSIONSThis work reports the results of a nearly com-plete survey of SiO, SiO, and SiO emissionfor J = 1 → →
4, in 67 oxygen-richstars. The stars have been chosen to span alarge range of mass-loss rates, from 10 − up to 10 − M ⊙ yr − . In all rotational transitions, wesurveyed simultaneously the vibrational levels v from 0 to 6, completing a list of 61 maser lines.A total of 1474 detections is reported.The observations were made in a relativelyshort time (weeks for the J = 1 → v = 6line in R Cas and χ Cyg. χ Cyg also displaysthe only v = 5 line detected. The v = 4 vibra-tional state only depicts rotational lines in the J = 3 → + and HCN), refractorymolecules (like SiS), S-bearing molecules (H S,SO, SO ) and the less observed NaCl, detectedfor the first time in NML Cyg (Fig. 11).SiO plays a key role in the process of dustformation under the appropriate physical con-ditions. The database generated by this surveywould be the basis of ambitious modeling of SiOmaser emission and the overall evolution of thecircumstellar envelopes. iO, SiO, and SiO in oxygen-rich stars
Facilities:
MDSCC:DSS-54, IRAM:30mREFERENCES
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Figure 1.
A full range spectrum, aiming to show the complexity of lines. This example corresponds tothe source IRC+10011, in the J = 1 → SiO, SiO, and SiO,respectively. For each isotopomer, vibrational number v increases from botton to top, starting at zero. Inthis example, six out of ten possible lines were detected. iO, SiO, and SiO in oxygen-rich stars Figure 2.
A sample of six different line profiles, representative of the catalogue. Source name are indicatedat the upper left corner of each panel, while the lines (abridged) are shown in the upper right corner. Rizzo et al.
Figure 3.
Variability of the J = 1 → v = 1 and v = 2 line fluxes corresponding to the eleven starsobserved in two or more different days. Fluxes are normalized to their respective averages. Red and bluemarks represent fluxes corresponding to the v = 1 and v = 2 lines, respectively. In most cases the variabilityis clearly noted on time scales of several days to few weeks. The variability of µ Cep is remarkable, wherethe highest fluxes in both lines are almost two times the other values (see text and Fig. 4). iO, SiO, and SiO in oxygen-rich stars Figure 4.
Variability of µ Cep. Lower and upper rows correspond to the J = 1 → v = 1 and v = 2lines, respectively. Observation dates and circular polarizations are indicated on top. The emission does notseem significantly polarized (second and third columns). The notable increment experienced in the last day(fourth column) arise from different velocity components in the two maser lines. Figure 5.
An example of variability. The SiO J = 1 → v = 0 line of VX Sgr has been observed twotimes, with a time separation of only two weeks, but resulting in very different spectra. Rizzo et al.
Figure 6.
Two examples of highly linearly polarized velocity components. The cases shown are the SiO J = 2 → v = 0 line towards IRC+10011 and the SiO J = 4 → v = 3 line towards VY CMa. iO, SiO, and SiO in oxygen-rich stars Figure 7.
First tentative detections of v = 6 SiO maser lines. They correspond to R Cas ( J = 4 →
3; leftpanel) and χ Cyg ( J = 2 →
1; right panel). Both v = 6 lines are very narrow and displayed in red. Tovisualize the velocity range of emission of the other SiO lines, the corresponding v = 0 line (not to scale)are displayed in grey. Rizzo et al.
Figure 8.
Intraday variability of χ Cyg. Fluxes of the thermal HCN J = 1 → J = 2 → v = 1 , − − ) are normalized to their respective average values. Scan IDs are explained in Table2, and correspond to both linear polarizations observed during August 1, 2, and 4. Note that the HCNnormalized flux (black marks) remains well within ± iO, SiO, and SiO in oxygen-rich stars Figure 9.
Normalized cumulative frequencies of the different vibrational levels for the whole sample, as afunction of the velocity range of emission. Rizzo et al.
Figure 10.
Relative intensities of the J = 1 → v = 1 and v = 2 lines. (a) Flux ratios v = 2 /v = 1plotted as a function of the scan ID; blue line indicates the median of the sample. (b) Distribution of thesame ratios, expressed in absolute (left axis) and relative (right axis) frequencies; the median (0.84) and themean (0.11) of the sample are also plotted as blue arrows. iO, SiO, and SiO in oxygen-rich stars Figure 11.
NaCl and Na Cl lines in NML Cyg. Transitions are indicated at the top left of each panel.Lines are shaded in the velocity range of emission of other lines in this source. Two other close lines (HCO + and SiO) fall inside the plot, as indicated. Rizzo et al.
Table 1.
Frequencies of the observed lines (in MHz)SiO v J = 1 → J = 2 → J = 3 → J = 4 → J = 5 →
40 43423.85163 86846.9600 130268.6100 173688.3100 217104.98001 43122.07310 86243.3700 129363.2400 172481.1500 215595.95002 42820.58624 85640.4600 128458.8872 171275.2800 214088.54003 42519.38333 85038.0464 127555.2739 170070.3500 212582.60004 42218.45653 84436.1911 126652.4901 168866.6332 211077.87005 83834.8731 167663.99456 83234.0760 166462.3977 SiO v J = 1 → J = 2 → J = 3 → J = 4 → J = 5 →
40 42879.94655 85759.1990 128637.0500 171512.8027 214385.75771 42583.82840 85166.9603 127748.6912 170328.3228 212905.15542 42287.99473 84575.2900 126861.1851 169144.9799 211425.97443 83984.1744 167962.7457 209948.17934 166781.60005 165602.4900 SiO v J = 1 → J = 2 → J = 3 → J = 4 → J = 5 →
40 42373.42369 84746.1702 127117.5479 169486.8766 211853.47361 42082.54453 84164.4095 168323.3529 210399.06652 83583.2041 167160.93963 165999.6090 i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 2 . Sources observedID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy1 Y Cas 00:03:21.40 +55:40:52.2 − − − − − − − − − − − − − − − − ∗ e PSw 0.21 15 0.16 RCP14 IRC+10011 01:06:25.98 +12:35:53.0 9.0 07-19 1 − − ∗ PSw 0.21 9 0.18 RCP16 08-01 2 − − − − − − − Table 2 continued R i zz o e t a l . Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy23 08-03 3 − − − − ∗ f WSw 0.35 13 0.57 HLP27 08-04 4 − ∗ WSw 0.35 13 0.51 VLP28 08-04 5 − − − − − ∗ PSw 0.21 9 0.04 RCP32 H2O125.6 01:16:37.16 +64:50:39.1 − − − ∗ PSw 0.21 15 0.26 RCP34 S Cas 01:19:41.99 +72:36:40.8 − − − ∗ PSw 0.21 4 0.43 RCP36 07-19 1 − − ∗ PSw 0.21 13 0.21 RCP38 08-01 2 − − − − − − − − − Table 2 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy47 06-23 1 − ∗ PSw 0.21 13 0.29 RCP48 W And 02:17:33.24 +44:18:23.0 − − − ∗ PSw 0.21 15 0.33 RCP50 O Cet 02:19:20.78 − − − ∗ PSw 0.21 16 0.26 RCP52 08-01 2 − − − − − − − − − − − ∗ WSw 0.35 8 0.77 HLP63 08-04 4 − ∗ WSw 0.35 8 0.69 VLP64 08-04 5 − − − − − ∗ PSw 0.21 18 0.37 RCP68 07-02 1 − − ∗ PSw 0.21 11 0.26 RCP70 08-02 2 − Table 2 continued R i zz o e t a l . Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy71 08-02 2 − − − − − − − − − − ∗ WSw 0.35 8 0.58 HLP81 08-04 4 − ∗ WSw 0.35 8 0.52 VLP82 08-04 5 − − − − ∗ PSw 0.21 24 0.19 RCP86 02395+624 02:43:28.10 +62:57:05.6 − − − ∗ PSw 0.21 10 0.28 RCP88 02404+215 02:43:16.20 +22:03:34.6 − − − ∗ PSw 0.21 10 0.24 RCP90 RU Ari 02:44:45.18 +12:19:08.2 20.0 07-26 1 − − ∗ PSw 0.21 9 0.26 RCP92 T Ari 02:48:19.74 +17:30:33.8 − − − − Table 2 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy95 08-03 2 − − − − − − − − − − − − ∗ PSw 0.21 14 0.26 RCP106 AFGL 490 03:27:37.61 +58:46:58.0 33.0 07-02 1 − − ∗ PSw 0.21 12 0.26 RCP108 NML Tau 03:53:28.87 +11:24:21.7 33.0 08-01 2 − − − − − − − − − − − ∗ WSw 0.35 11 0.52 HLP
Table 2 continued R i zz o e t a l . Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy119 08-04 4 − ∗ WSw 0.35 11 0.48 VLP120 08-04 5 − − − − − − − − − − − − − − − − − − − − − − − − − Table 2 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy143 08-03 3 − − − − − − − − − − − − − − ∗ WSw 0.35 12 0.48 HLP157 08-04 4 − ∗ WSw 0.35 12 0.43 VLP158 08-04 5 − − − − − − − − − Table 2 continued R i zz o e t a l . Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy167 08-01 4 − − − − − α Ori 05:55:10.31 +07:24:25.0 3.0 05-11 1 − − − − − − − − − − − − − − − − − − − − − Table 2 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy191 08-04 2 − − − − − − − ∗ WSw 0.35 6 2.52 HLP198 08-04 4 − ∗ WSw 0.35 6 2.30 VLP199 08-04 5 − − − − − − − − − − − − − − − − − Table 2 continued R i zz o e t a l . Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy215 08-03 3 − − − − − ∗ WSw 0.35 8 1.46 HLP220 08-04 4 − ∗ WSw 0.35 8 1.35 VLP221 08-04 5 − − − − − − − − − − − − − ∗ PSw 0.21 7 0.50 RCP230 T Com 12:58:38.92 +23:08:21.5 28.0 03-23 1 − − − − − − − − − Table 2 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy239 RT Vir 13:02:37.78 +05:11:07.5 13.0 04-16 1 − − − − − − − − − − − − − − − − − − − ∗ WSw 0.35 10 0.70 HLP254 08-03 4 − ∗ WSw 0.35 10 0.65 VLP255 08-03 5 − − − − − − − − Table 2 continued R i zz o e t a l . Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy263 08-02 3 − − − − − − − − − − − − − − − − − − − − − − − ∗ PSw 0.21 14 0.41 RCP284 08-02 2 − − − Table 2 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy287 08-03 2 − − − − − − − − − − − − − − − − − − − − − ∗ PSw 0.21 17 0.29 RCP305 06-22 1 − ∗ PSw 0.21 6 0.45 LCP306 06-22 1 − ∗ PSw 0.21 5 0.52 RCP307 07-31 2 − − − − Table 2 continued R i zz o e t a l . Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy311 08-03 2 − − − − − − − − − − − − − − − − − − − − − − − − − − Table 2 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy335 08-01 2 − − − − − − − − − − χ Cyg 19:50:33.92 +32:54:50.6 8.3 05-28 1 − − ∗ PSw 0.21 9 0.40 RCP345 08-01 2 − − − − − − − − − − − ∗ WSw 0.35 13 1.18 HLP356 08-04 4 − ∗ WSw 0.35 13 1.09 VLP357 08-04 5 − − Table 2 continued R i zz o e t a l . Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy359 TW Aql 19:51:00.83 +13:59:14.2 38.0 05-28 1 − − ∗ PSw 0.21 4 0.44 RCP361 RR Aql 19:57:36.06 − − − ∗ PSw 0.21 12 0.23 RCP363 08-01 2 − − − − − − − − − − − − ∗ PSw 0.21 11 0.28 RCP373 07-26 1 − − ∗ PSw 0.21 11 0.23 RCP375 NML Cyg 20:46:25.54 +40:06:59.4 − − − − − − − − − Table 2 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy383 08-03 3 − − − − ∗ WSw 0.35 11 0.76 HLP387 08-04 4 − ∗ WSw 0.35 11 0.71 VLP388 08-04 5 − − − − − ∗ PSw 0.21 9 0.29 RCP393 08-01 2 − − − − − − − − µ Cep 21:43:30.46 +58:46:48.2 24.0 05-21 1 − − − ∗ PSw 0.21 7 0.35 RCP404 07-21 1 − ∗ PSw 0.21 19 0.22 LCP405 08-01 2 − − Table 2 continued R i zz o e t a l . Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy407 08-03 2 − − − − − − − − − ∗ WSw 0.35 11 0.59 HLP416 08-04 4 − ∗ WSw 0.35 11 0.53 VLP417 08-04 5 − − − − − − − − − − − − − − − ∗ WSw 0.35 12 0.56 HLP
Table 2 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy431 08-04 4 − ∗ WSw 0.35 12 0.51 VLP432 R Aqr 23:43:49.46 − − − − ∗ PSw 0.21 5 0.40 RCP434 08-01 2 − − − − − − − − − − − ∗ PSw 0.21 13 0.26 RCP445 08-01 2 − − − − − − − − − − Table 2 continued R i zz o e t a l . Table 2 (continued)
ID Source RA (J2000) Dec (J2000) V LSR
Date a J → J − b vel. spacing t i nt rms c Pol. d hh:mm:ss.ss ± dd:mm:ss.s km s − mm-dd km s − min. Jy455 08-04 4 − ∗ WSw 0.35 11 0.51 HLP456 08-04 4 − ∗ WSw 0.35 11 0.46 VLP457 08-04 5 − − Note —Table 2 is entirely published in the electronic edition of the
Astrophysical Journal SupplementSeries . A portion is shown here for guidance regarding its form and content. a All dates in year 2012. b PSw: position switching. FSw: frequency switching. WSw Wobbler switching. c σ rms value. d Polarizations: LCP = Left circular; RCP = Right circular; HLP = Horizontal linear; VLP = Verticallinear. e − ∗ includes only the v = 1 and 2 lines of SiO, and the v = 0 line of SiO. f − ∗ includes the v = 4 to 6 lines of SiO, the v = 2 to 5 lines of SiO, and the v = 0 to 3 lines of SiO. iO, SiO, and SiO in oxygen-rich stars Table 3.
Efficiencies and intensity conversionsFrequency HPBW
S/T ∗ a η MB η a GHz ” Jy/K43 48 6.41 0.57 0.4686 29 5.89 0.81 0.63129 19 6.28 0.76 0.57172 14 6.80 0.70 0.54216 11 7.52 0.62 0.49 R i zz o e t a l . Table 4 . DetectionsID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(4 − SiO(4 − − . Polarized. SiO(4 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(1 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
25 IRC+10011 SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − − .29 IRC+10011 SiO(5 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − − .30 IRC+30021 SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(3 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − − .44 S Cas SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(1 − − .48 W And SiO(1 − SiO(1 − SiO(1 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
57 O Cet SiO(2 − SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(4 − SiO(4 − SiO(4 − − . SiO(4 − − .61 O Cet SiO(4 − SiO(4 − SiO(4 − SiO(4 − − .64 O Cet SiO(5 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(5 − SiO(5 − − . SiO(5 − − .65 O Cet SiO(5 − SiO(5 − SiO(5 − − . SiO(5 − − .66 S Per SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − − . Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
70 S Per SiO(2 − SiO(2 − SiO(2 − − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
76 S Per SiO(3 − SiO(3 − SiO(3 − SiO(3 − − . SiO(3 − − .77 S Per SiO(3 − SiO(3 − SiO(3 − SiO(3 − − . SiO(3 − − . SiO(3 − − .78 S Per SiO(4 − − . SiO(4 − SiO(4 − − . SiO(4 − SiO(4 − SiO(4 − − . SiO(4 − SiO(4 − SiO(4 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
81 S Per SiO(4 − − . SiO(4 − − .82 S Per SiO(5 − SiO(5 − SiO(5 − − . SiO(5 − − . SiO(5 − SiO(5 − SiO(5 − − . SiO(5 − − . SiO(5 − SiO(1 − SiO(1 − − .90 RU Ari SiO(1 − SiO(1 − SiO(1 − SiO(1 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
92 T Ari SiO(2 − − SiO(2 − − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(3 − SiO(4 − SiO(4 − SiO(2 − SiO(2 − SiO(2-1)v0 1.20 0.57 15.88 2.70 14.6 17.3 Smoothed to 2.7 km s − . Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2-1)v1 14.16 0.11 16.14 0.23 12.4 18.5105 IRC+20052 SiO(1 − − .108 NML Tau SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
115 NML Tau SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − − . SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − − . SiO(4 − SiO(4 − SiO(4 − SiO(4 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
119 NML Tau SiO(4 − − SiO(4 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(2 − SiO(2 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
130 S Tau SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(3 − SiO(3 − SiO(3 − SiO(4 − − .146 TX Cam SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − − SiO(4 − SiO(4 − SiO(4 − SiO(4 − − SiO(4 − SiO(4 − SiO(4 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
158 TX Cam SiO(5 − SiO(5 − − . SiO(5 − − .159 TX Cam SiO(5 − SiO(5 − − . SiO(5 − − .160 IRC+60154 SiO(2 − − SiO(2 − SiO(2 − − SiO(2 − SiO(2 − SiO(2 − − .162 IRC+60154 SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
164 IRC+60154 SiO(3 − SiO(3 − SiO(3 − SiO(3 − − .165 IRC+60154 SiO(3 − SiO(3 − SiO(3 − SiO(3 − − .166 IRC+60154 SiO(4 − SiO(4 − − . SiO(4 − SiO(1 − SiO(1 − SiO(1 − − . SiO(1 − −
24 km s − .178 U Ori SiO(2 − SiO(2 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
179 U Ori SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − −
15 km s − .184 U Ori SiO(4 − − . SiO(4 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(4 − SiO(4 − − .185 U Ori SiO(4 − − . SiO(4 − SiO(4 − SiO(4 − SiO(4 − − .186 VY CMa SiO(1 − SiO(1 − SiO(1 − SiO(1 − − .187 VY CMa SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
189 VY CMa SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − − . SiO(4 − − .196 VY CMa SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − − . Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(1 − SiO(1 − − . Very narrow line. Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
203 R LMi SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
207 R Leo SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(3 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − − .218 R Leo SiO(4 − SiO(4 − SiO(4 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(4 − SiO(4 − SiO(4 − − .220 R Leo SiO(4 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(1 − − . SiO(1 − SiO(1 − SiO(1 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
227 R Vir SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − − . SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
239 RT Vir SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
249 RX Boo SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(4 − SiO(4 − SiO(4 − − . SiO(4 − SiO(4 − SiO(4 − SiO(4 − − . SiO(4 − SiO(4 − SiO(4 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
255 RX Boo SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(4 − SiO(4 − SiO(4 − SiO(1 − SiO(1 − SiO(1 − − .268 WX Ser SiO(2 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − − .274 WX Ser SiO(4 − − .275 WX Ser SiO(4 − SiO(1 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − − . Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
285 U Her SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − − .287 U Her SiO(2 − SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − − . Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
290 U Her SiO(4 − − . SiO(4 − − . SiO(4 − − .291 U Her SiO(4 − − . SiO(4 − − .292 R UMi SiO(1 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(3 − − . SiO(3 − − . Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(3 − − .298 R UMi SiO(3 − SiO(3 − − . SiO(3 − − .299 R UMi SiO(4 − SiO(4 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(1 − SiO(1 − SiO(1 − SiO(1 − − .306 VX Sgr SiO(1 − SiO(1 − SiO(1 − − .307 VX Sgr SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
310 VX Sgr SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − − . Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(3 − SiO(3 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − − . SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − − . SiO(4 − − . SiO(4 − SiO(5 − SiO(5 − − . SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − − . Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(5 − SiO(5 − SiO(5 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − − . Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
323 V1111 Oph SiO(2 − SiO(2 − SiO(2 − SiO(2 − − .324 V1111 Oph SiO(2 − SiO(2 − SiO(2 − SiO(2 − − .325 V1111 Oph SiO(2 − SiO(2 − SiO(2 − SiO(2 − − .326 V1111 Oph SiO(2 − SiO(2 − SiO(2 − SiO(2 − − .327 V1111 Oph SiO(3 − SiO(3 − SiO(3 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(4 − SiO(4 − − . SiO(4 − SiO(4 − SiO(4 − − .330 V1111 Oph SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − − . Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
331 V1111 Oph SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − − . SiO(5 − SiO(5 − SiO(5 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − − .337 R Aql SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(3 − SiO(4 − SiO(4 − SiO(4 − − .341 R Aql SiO(4 − SiO(4 − SiO(4 − − .343 χ Cyg SiO(1 − SiO(1 − SiO(1 − SiO(1 − χ Cyg SiO(1 − SiO(1 − SiO(1 − χ Cyg SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2 − χ Cyg SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − χ Cyg SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − χ Cyg SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − χ Cyg SiO(2 − SiO(2 − SiO(2 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2 − SiO(2 − χ Cyg SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − χ Cyg SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − χ Cyg SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − χ Cyg SiO(4 − SiO(4 − SiO(4 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(4 − SiO(4 − χ Cyg SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − χ Cyg SiO(4 − − .356 χ Cyg SiO(4 − − .357 χ Cyg SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − χ Cyg SiO(5 − SiO(5 − SiO(5 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − − . SiO(2 − − .364 RR Aql SiO(2 − SiO(2 − SiO(2 − − .365 RR Aql SiO(2 − SiO(2 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
366 RR Aql SiO(2 − SiO(2 − SiO(2 − − .367 RR Aql SiO(3 − SiO(3 − SiO(3 − SiO(3 − − . SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − − . SiO(3 − SiO(4 − − . SiO(4 − SiO(4 − SiO(4 − SiO(4 − − . SiO(4 − SiO(4 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(4 − − .371 IRC-10529 SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − − SiO(2 − − SiO(2 − SiO(2 − SiO(2 − − . SiO(2 − − .378 NML Cyg SiO(2 − SiO(2 − SiO(2 − − . SiO(2 − − .379 NML Cyg SiO(2 − SiO(2 − SiO(2 − − . Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2 − − .380 NML Cyg SiO(2 − SiO(2 − SiO(2 − SiO(2 − − .381 NML Cyg SiO(2 − SiO(2 − SiO(2 − SiO(2 − − . SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(4 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(4 − SiO(4 − − .385 NML Cyg SiO(4 − SiO(4 − SiO(4 − − .386 NML Cyg SiO(4 − − .387 NML Cyg SiO(4 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(1 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(3 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − − . SiO(3 − SiO(4 − SiO(4 − − .400 T Cep SiO(4 − − . SiO(4 − µ Cep SiO(1 − SiO(1 − µ Cep SiO(1 − SiO(1 − µ Cep SiO(1 − SiO(1 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − µ Cep SiO(1 − SiO(1 − µ Cep SiO(2 − µ Cep SiO(2 − − SiO(2 − µ Cep SiO(2 − SiO(2 − µ Cep SiO(2 − SiO(2 − µ Cep SiO(2 − − SiO(2 − µ Cep SiO(2 − SiO(2 − µ Cep SiO(3 − µ Cep SiO(3 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − µ Cep SiO(4 − SiO(4 − µ Cep SiO(4 − SiO(4 − − .417 µ Cep SiO(5 − − . SiO(5 − SiO(5 − SiO(5 − µ Cep SiO(5 − − . SiO(5 − SiO(5 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
422 AFGL 2999 SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − − .424 AFGL 2999 SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(3 − − . SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(4 − − . SiO(4 − − . Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(4 − SiO(4 − − .429 AFGL 2999 SiO(4 − − . SiO(4 − SiO(4 − SiO(4 − SiO(4 − − . Polarized. SiO(4 − SiO(4 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
437 R Aqr SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(4 − SiO(4 − SiO(4 − − .441 R Aqr SiO(4 − SiO(4 − SiO(4 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s −
443 R Cas SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(1 − SiO(2 − SiO(2 − SiO(2 − − SiO(2 − − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(2 − SiO(2 − − . SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(2 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(3 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − Table 4 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − SiO(4 − − .457 R Cas SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − SiO(5 − − . SiO(5 − SiO(5 − SiO(5 − − . Table 4 continued R i zz o e t a l . Table 4 (continued)
ID Source Transition a Flux Error V LSR
Error V min V max Individual commentsJy km s − km s − km s − Note —Table 4 is entirely published in the electronic edition of the
Astrophysical Journal SupplementSeries . A portion is shown here for guidance regarding its form and content. a Transition name includes the isotopomer, the rotational transition and the vibrational state. As anexample, the transition SiO(4 − J = 4 → SiO species,at the vibrational state v = 2. i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 5 . Detections after averagesAveraged Source Transition a Flux Error V LSR
Error V min V max Individual commentsIDs Jy km s − km s − km s − − SiO(2 − −
25 IRC+10011 SiO(4 − −
41 S Cas SiO(2 − − .38 −
41 S Cas SiO(2 − − .44 −
45 S Cas SiO(4 − −
45 S Cas SiO(4 − − .52 −
57 O Cet SiO(2 − −
57 O Cet SiO(2 − −
63 O Cet SiO(4 − SiO(1 − SiO(1 − − .70 −
75 S Per SiO(2 − −
75 S Per SiO(2 − − .76 −
77 S Per SiO(3 − − .76 −
77 S Per SiO(3 − − .98 −
99 T Ari SiO(4 − − .108 −
113 NML Tau SiO(2 − −
119 NML Tau SiO(4 − − .154 −
155 TX Cam SiO(4 − − .158 −
159 TX Cam SiO(5 − − .160 −
163 IRC+60154 SiO(2 − −
163 IRC+60154 SiO(2 − Table 5 continued R i zz o e t a l . Table 5 (continued)
Averaged Source Transition a Flux Error V LSR
Error V min V max Individual commentsIDs Jy km s − km s − km s − −
167 IRC+60154 SiO(4 − − .235 −
236 T Com SiO(3 − −
262 S Crb SiO(2 − −
262 S Crb SiO(2 − −
266 S Crb SiO(4 − −
266 S Crb SiO(4 − − .265 −
266 S Crb SiO(4 − − .268 −
271 WX Ser SiO(2 − − .272 −
273 WX Ser SiO(3 − − .274 −
275 WX Ser SiO(4 − − .284 −
287 U Her SiO(2 − − .293 −
296 R UMi SiO(2 − − .299 −
300 R UMi SiO(4 − − .299 −
300 R UMi SiO(4 − − .307 −
312 VX Sgr SiO(2 − −
330 V1111 Oph SiO(4 − − .361 −
362 RR Aql SiO(1 − −
370 RR Aql SiO(4 − − .369 −
370 RR Aql SiO(4 − −
398 T Cep SiO(3 − − µ Cep SiO(2 − − µ Cep SiO(2 − − µ Cep SiO(3 − − .420 −
425 AFGL 2999 SiO(2 − − . Table 5 continued i O , S i O , an d S i O i n o xy g e n - r i c h s t a r s Table 5 (continued)
Averaged Source Transition a Flux Error V LSR
Error V min V max Individual commentsIDs Jy km s − km s − km s − −
425 AFGL 2999 SiO(2 − −
437 R Aqr SiO(2 − −
450 R Cas SiO(2 − −
456 R Cas SiO(4 − − .455 −
456 R Cas SiO(4 − −
456 R Cas SiO(4 − − . Note —Table 5 is entirely published in the electronic edition of the
Astrophysical Journal SupplementSeries . A portion is shown here for guidance regarding its form and content. a Transition name includes the isotopomer, the rotational transition and the vibrational state. As anexample, the transition SiO(4 − J = 4 → SiO species,at the vibrational state v = 2. Rizzo et al.iO, SiO, and SiO in oxygen-rich stars
Table 6.
Other molecular lines: identificationSpecies and Molecule Transition Frequency E u line ID MHz KA1 HCO + CN 1–0 86339.9214 4.2C3 H CN 2–1 172677.8512 12.4D1 SiS 5–4 90771.5643 13.1D2 SiS 7–6 127076.1860 24.4D3 SiS 5–4 89103.7489 12.8D4 SiS 12–11 213816.1396 66.7D5 Si S 5–4 88285.8282 12.7E1 H S 1 , –1 , S 2 , –2 , S 1 , –1 , –1 –2 –3 –4 SO 6 –5 , –8 , , –12 , , –11 , , –10 , , –16 , Cl 7–6 89220.1148 17.1H4 Na Cl 17-16 216531.3010 93.4
Note —C1 line (HCN J = 1 →
0) is composed of threehyperfine components; quoted frequency corresponds to themost intense one. R i zz o e t a l . Table 7 . Other molecular lines: detections
Source LineA1 B1 C1 C2 C3 D1 D2 D3 D4 D5 E1 E2 E3 F1 F2 F3 F4 F5 G1 G2 G3 G4 G5 H1 H2 H3 H4IRC+10011 Y N Y Y S Y Y S S Y Y N S Y Y N S N Y N N Y N N N N NS Cas N N Y S S S S N · · · N · · · · · · · · · N N N · · · · · ·
N N N N · · · N · · · N · · · O Cet Y N N N N N N N N N N N N N N N N N N N N N N N N N NS Per N N Y N N N N N N N N N N N N N N N N N N N N N N N NNML Tau Y Y Y Y Y Y Y S N S Y N S Y Y Y Y N Y Y Y Y N N N N NTX Cam Y Y Y Y S Y Y N N Y Y N N Y Y N N N Y N N N N N N N NIRC+60154 N N Y N N N N N · · · N · · · · · · · · · N N N · · · · · ·
N N N N · · · N · · · N · · · HK Ori N N Y N N N ... N · · · N · · · · · · · · · N · · · N · · · · · · N · · · · · · · · · · · · · · · · · · N · · · VY CMa Y N Y Y N Y Y N N N N N N Y Y S a Y N Y Y b S Y S N N N NR Leo N N Y N N N N N N N N N N Y Y N Y N N N N N N N N N NRX Boo N N Y N N N N N N N N N N Y Y Y S N Y N S Y N N N N NU Her N N Y N N N N N · · · N · · · · · · · · · N S N · · · · · ·
N N N N · · · N · · · N · · · VX Sgr Y N Y N N S S N N N · · · N · · · S Y S Y N S Y N S N N · · ·
N NV1111 Oph Y N Y Y N Y Y N N N · · · N · · · S S N Y N Y N N S N N · · ·
N NR Aql N N Y N N N N N · · · N · · · · · · · · · Y Y S · · · · · ·
Y N Y Y · · · N · · · N · · · χ Cyg N N Y Y Y N N N N N N N N N N N N N N N N N N N N N NRR Aql N N Y N N N N N · · · N · · · · · · · · · N S S · · · · · ·
Y S S S · · · N · · · N · · · NML Cyg Y S Y Y S Y Y N N N Y Y Y Y Y Y Y S Y Y Y Y S Y Y Y S µ Cep Y N Y N N N N N N N N N N Y N N N N N N N N N N N N NR Cas Y N Y Y N N N N N N N N N Y Y Y Y N Y S Y Y N N N N N
Note —All spectra have been averaged and smoothed down to ≈ − .Y: detected. N: not detected. S: detected after smoothing worse than 2 km s − . a Instrumental problems close in frequency, but clear detection. b Blended with SiO(3–2) vv