Kinematics of Red Variables in the Solar Neighborhood I. Basic Data Obtained by an SiO Maser Survey
aa r X i v : . [ a s t r o - ph . GA ] A ug PASJ:
Publ. Astron. Soc. Japan , 1– ?? , c (cid:13) Kinematics of Red Variables in the Solar Neighborhood I . Basic DataObtained by an SiO Maser Survey
Shuji
Deguchi , Tsuyoshi
Sakamoto ,andTakashi Hasegawa Nobeyama Radio Observatory, National Astronomical Observatory,Minamimaki, Minamisaku, Nagano 384-1305 Graduate University for Advanced Studies, National Astronomical Observatory,Minamimaki, Minamisaku, Nagano 384-1305 Bisei Space Guard Center, 1716-3 Ookura, Bisei, Ibara, Okayama 714-1411 Gunma Astronomical Observatory, 6860-86 Nakayama, Takayama, Agatsuma, Gunma 377-0702 (Received 2011 April 11; accepted 2011 August 9)
Abstract
In order to study the streaming motions of miras in the Solar neighborhood, we newly surveyed 379red variables in the SiO maser lines at 42.821 and 43.122 GHz with the Nobeyama 45m radio telescope.Accurate radial velocities were obtained for 229 (220 new) detected stars. The sample is selected fromoptical variables found by new automated surveys: the Northern Sky Variability Survey and the All SkyAutomated Survey. The new sample consists of the ”bluer” objects compared with those observed in theprevious SiO surveys. The distances to the objects are estimated using the period-luminosity relation, andthey are mostly less than 3 kpc from the Sun. The longitude-velocity diagram reveals three prominentgroups of stars deviant from the circular Galactic rotation with a flat rotation curve. In addition to theHercules group of stars which was studied before, we found two new deviant groups: one toward the Perseusarm and the other toward the Sagittarius arm. These two groups both exhibit anomalous motions towardthe Galactic center, which seem to be consistent with the noncircular motions of these spiral arms foundin the recent VLBI proper-motion measurements for maser gas clumps.
Key words:
Galaxy: disk, Galaxy: kinematics and dynamics, stars: AGB and post-AGB
1. Introduction
Moving groups are clumps of stars sharing the samespatial motion in the Solar neighborhood. They are oftenconsidered to be a fossil, which keeps past dynamical in-formation after its birth in the Galaxy. The coherent spa-tial motions of the moving groups are well studied in thepast based on the Hipparcos and the RAVE (the RadialVelocity Experiment; Zwitter et al 2008) databases (seeFamaey et al. 2005). In particular, the Hercules groupof stars, which was first identified by O. J. Eggen (see asummary by Eggen 1996), is a well studied moving groupwith rotational lag and outward motion of about 40 kms − and 50 km s − , respectively, to the Galactic rotation.It is inferred that a few percent of stars in the Solar neigh-borhood are members of this group (Bensby et al. 2007).The origin of the Hercules group is attributed to a rota-tional resonance of the bar-like Bulge, because the popu-lation of stars of this group is a mixture with different ages(Bensby et al. 2007). Feast & Whitelock (2000) investi-gated an outward motion of short-period Mira variablesnear the Sun, and attributed it to the resonance effect ofthe Bulge bar. Presumably the Hercules moving group,which was found in the Solar neighborhood, spreads spa-tially far from the Sun. Deguchi et al. (2010) found thata group of maser stars in the Galactic longitude range be- tween 20 ◦ and 40 ◦ , which are located at a few kpc fromthe Sun, have a distinctively large outward motion com-pared with the motions of usual stars under the Galacticrotation. They also attributed the large outward motionto the effect at the outer Lindblad and corotation res-onances of the central bar. The resonance effect of theGalactic bar should appear in areas near the resonancecircles in the Galactic plane. In particular, the old starswith ages several times longer than the rotational periodof the bar pattern reflect the resonance effect. Therefore,miras are ideal sample for studying the bulge-bar reso-nance effect because they are evolved stars with ages ofabout a few Gyr. In contrast, tidal streams of dwarf galax-ies, e.g., the Sgr dwarf stream (for example, Majewski etal. 2003), are often traced in a relatively limited area ofthe sky far from the Galactic plane because of their lowstellar density, though they still have been found in theGalactic disk using blue metal-poor stars (e.g., Belokurovet al. 2007).Radial velocities of OH and SiO maser sources havebeen used to investigate dynamics of stars in the disk(Jiang et al. 1996; Nakashima & Deguchi 2003; Ita etal. 2001) and the bulge of the Galaxy (Izumiura et al.1995; Sevenster et al. 2001). These maser stars are mostlymiras and semi-regular variables, i.e., O-rich evolved starsat the asymptotic-giant-branch (AGB) phase, though a Deguchi et al. [Vol. ,small amount of red supergiants are contaminated in thesample. Previous surveys of these stars by OH and SiOmaser lines were preferentially made for the highly red-dened, optically very faint stars because of their high de-tection rate in a color-selected sample (for example, seeDeguchi et al. 2004). These stars are located at relativelylarge distances in the Galactic disk, compared with a sam-ple of optical miras. Therefore, optical miras in the Solarneighborhood are missing in the previous samples of masersources [e.g., Nakashima & Deguchi (2003); Deguchi et al.(2007), except Jewell et al. (1991)]. Even though radialvelocities have been obtained for a large number of opticalmiras by optical spectroscopy, the accuracy in the mea-surement is quite limited. For example, if we compare theradial velocity of a mira in the RAVE database with thatof OH or SiO masers, we often find typically a 10 km s − or much larger difference between them. This is caused byseveral reasons: insufficient spectral resolution in opticalinstruments, phase dependency of optical line velocitieson mira pulsation (see, e.g., Scholz & Wood 2000), and avelocity shift of the optical lines due to scattering by mov-ing circumstellar dust (van Blerkom & Mao 1982). It isknown that the stellar velocities obtained in the maser linemeasurements are accurate within ∼ − [e.g., seesection 3.1 of Nakashima & Deguchi 2006]. Therefore, itis useful to measure the radial velocities of optical mirasin the Solar neighborhood in SiO maser lines even if opti-cal velocities are available for some stars. Moreover, theaccurate radial velocities of miras in the Solar neighbor-hood by the maser observations are essential to see if thedeviant stream is continuously connected with the streamthat is found previously in a large extension of the Galaxy(Feast & Whitelock 2000; Deguchi et al. 2010). In ad-dition, since precise measurements of proper motions willbe available by the phase-reference VLBI technique forSiO maser sources (Kobayashi et al. 2008), accurate 3dmotions in space will reveal in future for these objects.In this paper, we present the result of a new survey ofthe optical red variables in the SiO maser lines with the45m telescope at Nobeyama. A number of new variablestars were recently found by automated optical variabil-ity surveys: the Northern Sky Variability Survey (NSVS;Wo´zniak et al. 2004) and the All Sky Automated Survey(ASAS; Pojmanski et al. 2005). Though these newlyfound optical variables are much bluer in near-infrared(NIR) colors (such as H − K ) than the typical SiO masersources previously surveyed, they exhibit the characteris-tic optical variability of miras. Since the bluer color in-dicates the higher surface temperature and smaller massloss rate of the central star in general, the detection rateof SiO masers was expect to be very low for such a sample.However, contrary to our expectation, our preliminarysurvey made in 2009 resulted in a significantly high de-tection rate of SiO masers. Therefore, we have performeda new extensive observation in the SiO maser lines towardthese red variables, and have increased the data of our SiOradial velocity database. In this paper, we present the re-sult of the observations and give a limited discussion onthe kinematic properties of this sample, based mainly on the radial velocities. For all of the sampled stars, proper-motions have been measured optically (Roeser et al.2010). A kinematic study based on the proper motionswill be given in the future paper.
2. Observation, sample selection, and results
The observations were made with the 45m radio tele-scope at Nobeyama in 2009 March, 2010 March–May, and2010 December–2011 January in the SiO J = 1–0 v = 1 and2 transitions at 43.122 and 42.821 GHz, respectively. Afew data taken before 2009 were also added for the presentanalysis. A cooled HEMT receiver (H40) was used for the43 GHz observations with acousto-opt spectrometer ar-rays with 40 and 250 MHz bandwidths (with velocity res-olutions of about 0.3 and 1.8 km s − , respectively). Thesystem temperature was about 180 — 250 K for the SiOobservations, depending on weather conditions. The half-power beam width (HPBW) of the telescope was about40 ′′ at 43 GHz. A conversion factor of the antenna tem-perature to the flux density was about 2.9 Jy K − . Allof the observations were made by the position-switchingmode. Further details of observations using the NRO 45-m telescope have been described elsewhere (see Deguchi etal. 2000). The spectrometer arrays also covered the SiO J = 1–0 v = 0 and v = 3 lines at 43.424 GHz and 42.519GHz, respectively, the SiO J = 1–0 v = 0 line at 42.880GHz, and H53 α at 42.952 GHz. However, these lines weredetected in a few sources (shown in Appendix 1). The sample for the present SiO maser searches was cho-sen mainly from the ”Catalog of Red Variables in theNorthern Sky Variability Survey”(Williams et al. 2004).Because the coverage of this survey is heavily weighted onthe northern Galactic plane, we used an additional opticalcatalog of red variables selected from the ”ASAS VariableStars in Southern Hemisphere” (Pojmanski et al. 2005).These two catalogs listed up the red variables found inautomated sky surveys. They give period of optical lightcurve, classification code, optical magnitude and ampli-tude, coordinates of the stars with accuracy better than10 ′′ , and 2MASS and IRAS identifications. From thesecatalogs, we selected the objects with a classification codeof ”M” (mira) or ”SR+L” (semiregular and irregularvariables) and with a period longer than 80 d [which cov-ers enough for SiO maser stars at the short-period limit( ∼
150 d)]. Additionally, we applied the selection cri-teria to effectively squeeze out the stars enshrouded bycircumstellar dust;
K <
9, and H − K > .
6, the 12 µ mflux density brighter than 3 Jy, and the color − . < C [ ≡ log ( F /F )] < ∼ .
2, where H and K are 2MASS H and K s magnitudes, respectively (Cutri et al. 2003), and F and F are the IRAS flux densities in the 12 and 25 The variability type, ”semi-regular”, is applied to the variableswith smaller amplitude, shorter periods, and more irregular pul-sations than miras; some occasionally show multiple periodicity(Bedding & Zijlstra 1998). o. ] Kinematics of Red Variables I. Basic Data 3 -60-300 30 60 -180-120-60060120180
SiOno SiO
Fig. 1.
Distribution of the observed objects in the Galactic coordinates in the Hammer-Aitoff projection. Filled and unfilled circlesindicate SiO detection and no detection, respectively. µ m bands, respectively (Beichman et al. 1989) [the MSXbands C and E (Egan et al. 2003) were also consultedfor the | b | < ∼ ◦ sources. We applied the same criterion in C by translating log ( F E /F C ) to C without any cor-rection, where F C and F E are MSX 12 and 21 µ m fluxdensities. Detailed comparison of the MSX colors withthose of IRAS (Sjouwerma et al. 2009) showed that thecorrection is negligibly small around C = − . H − K and in C but havenot been surveyed before. We added these additional ob-jects to our results for completeness. We have observedall the red variables in the Williams et al. (2004)’s catalogdown to F = 7 Jy (though we could not consume all thebright objects in the ASAS catalog). The distribution ofthe observed stars in the sky is shown in Figure 1. Observational results are summarized in Tables 1 and 2for the SiO detections and no detections, respectively. Theobserved spectra of the SiO J = 1–0 v = 1 and 2 transitionsfor detected sources are given in Appendix 1, and theindividually interesting objects are also discussed there.Table 3 summarizes a few detections in the additional linesof SiO, i.e., the SiO v = 3 and v = 0 J = 1–0 and SiO v =0 J = 1–0 transitions [the spectra are shown in Appendix1]. Table 4 summarizes the infrared properties of all theobserved sources.Figure 2 shows the near- and middle-infrared color–magnitude diagrams for observed stars. If we comparethis, for example, with Figure 2 of Deguchi et al. (2010), -0.500.511.522.5-0.6 -0.4 -0.2 0SiOno SiO l og ( F / Jy ) C K ( m ag ) H-K
Fig. 2.
NIR color-magnitude and and MIR color-flux densitydiagrams for the sampled objects. Filled and unfilled circlesindicate SiO detection and no detection, respectively.
Deguchi et al. [Vol. , N u m be r Period (d) 1200
Fig. 3.
Histogram of period for SiO detections and no detec-tions. The filled and shaded areas indicate the SiO detectionand no detection, respectively. we can recognize that the present sample is weighted to-ward bluer colors than the previous SiO maser survey sam-ples; for example, the median of H − K for the presentsample is 0.72, while it is 1.09 for the former sample, andthe median of C in the present sample is − .
29, while itis − .
16 for the former sample. In addition, the objectsin the present sample are much brighter in K band thanthose in the previous samples. It suggests that the averagedistance from the Sun of the sampled stars is much smallerthan that of the previous SiO-survey samples with a typi-cal distance of ∼ ∼
80 %) for the objects that are bright inthe 12 µ m and K bands, but gradually decreases as theinfrared flux density decreases. Beyond K = 5, the num-ber of no detections exceeds that of detections because ofthe large distance to the sources. Such a high SiO detec-tion rate in SiO maser emission was an unexpected result,which apparently does not match up with the blue colorsof the sample. However, this apparent discrepancy couldbe explained for the following reasons. In the previous SiOsurveys, the variability indices of the IRAS catalog werenot considered in the selection criteria (except Jiang et al.1996). Therefore, the samples could include young stellerobjects (YSOs) and red giants (RGB stars) which maymimic IR colors of the AGB stars , but do not emit SiOmasers. On the contrary, the present sample is selectedfrom the optically visible variable stars. It assures thatthey are stars in the AGB or post-AGB phases exhibitingactive mass loss.Figure 3 shows a histogram of period for the detec-tions and no detections. The averaged period is 424( ± ± N u m be r D (kpc) 8
Fig. 4.
Histogram of luminosity distances computed usingthe PL relation. The filled and shaded area indicates theSiO detection and non detection. The average distance is2 . ± .
1) kpc for SiO detections and 2 . ± .
5) kpc for nodetections, where the parenthetic number is a standard devi-ation. riod less than 200 d occasionally exhibit a large deviantmotion from the Galactic rotation (Feast & Whitelock2000). However, above 4 objects (distributing in theGalactic longitude and latitude ranges of l = 46 – 110 ◦ and b = − ◦ ) spread only in the velocity range be-tween −
16 and 25 km s − . Therefore, we do not find anyanomalous kinematics for these 4 objects only from theirradial velocities.We estimated distances to the observed stars based onthe PL (Period-Luminosity) relation (Whitelock et al.2008). The detail of the distance estimation is given inAppendix 2. Figure 4 shows histogram of distances forthe detections and no detections. This figure indicatesthat most of objects in the sample are located within adistance of 3 kpc from the Sun except a few faint ones,though there is a considerable uncertainty in the distanceestimation. The average distance is 2.0 ( ± .
1) kpc for thedetections, and 2.2 ( ± .
5) kpc for the no detections.
3. Discussion
In Figure 5, we present the longitude-velocity diagramof the detections, in which filled and unfilled circles indi-cate the galactic latitude ranges of | b | < ◦ and | b | > ◦ ,respectively. Thick curves indicate the expected radialvelocities for the objects under a circular rotation at dis-tances, 1, 2, and 4 kpc from the Sun. Here we assumeda flat Galactic rotation curve of 220 km s − in the Solarneighborhood and the Sun–Galactic-center distance of 8kpc. We have also drawn the broken curves which areexpected for the Hercules and Arcturus moving groups ofstars near the Solar neighborhood (at the distance of 1kpc). For simplicity, we assumed that the rotational lagand radial motion of the streams to the Galactic rotationare kept the same everywhere near the Solar neighbor-hood. The curve for each moving group strongly dependson the assumed velocity law: see, for example, Figure 8o. ] Kinematics of Red Variables I. Basic Data 5and Appendix 3 of Deguchi et al. 2010).In Figure 5, we see notable concentrations of the starswith | b | < ◦ near the curve of 4 kpc distance; one around l = 25 – 45 ◦ and V lsr ≃ +40 – +80 km s − , and the otheraround l = 95 – 135 ◦ and V lsr ≃ −
70 – −
40 km s − . Inaddition, there is a group of stars in the area l = 20 – 50 ◦ and V lsr ≃ −
80 – −
20 km s − , which is deviant from theGalactic rotation by more than ∼
50 km s − . These de-viant groups of stars are surrounded by ellipses in Figure6 for clarity. They are overlaid on the CO l - v map (Dameet al. 2001) for comparison.The negative velocity feature around l = 20 – 50 ◦ ( V lsr ≃ −
80 – −
20 km s − ) has been discussed exten-sively by Deguchi et al. (2010). This is likely an ex-tension of the Hercules moving group of stars, which iscaused by outer Lindblad resonance of the Galactic barstructure. Bovy (2010() predicted that the member starsof the Hercules moving group would reveal most promis-ingly in the Galactic longitude range of 250 ◦ < ∼ l < ∼ ◦ .Unfortunately, stars in this longitude range are diffi-cult to observe from Nobeyama except for stars at highGalactic latitudes. Furthermore, SiO maser sources (O-rich evolved stars) are not populated much outside theSolar circle (e.g., Jiang et al. 1996). Therefore, it is hardto confirm such a prediction through only the present dis-cussion based on the longitude-velocity diagram. One of notable characteristics of Figure 5 is that a con-siderable number of objects exhibit radial velocities largerthan that expected from the 2 kpc distance; many starsfall around or beyond the curve of the 4 kpc distance.Because the objects in the present sample are optical vari-ables which are bright in K band ( K < l = 95 – 135 ◦ and V lsr ≃ −
70 – −
40 kms − coincides with a peak of CO emission feature for thePerseus spiral arm (see Dame et al. 2001). CO emission ismost prominent at around l = 111 ◦ and V lsr = −
45 km s − (toward the NGC7538 molecular cloud). The average dis-tance for the 18 objects in the ellipse of figure 5 (marked asPerseus) is estimated to be 1.94 kpc (with a standard de-viation of ± .
10 kpc) based on the period-luminosity (PL)relation. There is a large difference between the kinematicand luminosity distances for this group of stars. If we be-lieve the luminosity distance, the stars of this group areapproaching us with velocity larger than the velocity ex-pected by the standard circular rotation of the Galaxy.Note that the SiO maser sources have a velocity disper-sion of about 25 km s − from the average Galactic rotation[see the discussion in the last paragraph of Appendix 2 ofDeguchi et al. (2005)].The distance to the Perseus spiral arm was controver-sial in the past (Rickard et al. 1968; Roberts 1972).Recently parallax distances to the several masing objects in this spiral arm have been measured with Very LongBaseline Interferometric (VLBI) technique. For example,the distance to W3(OH) ( l = 134 ◦ ) is determined to be1 . ± .
04 kpc (Xu et al. 2006). A comprehensive sum-mary of the objects with annual parallax measurements isfound in Figure 11 of Asaki et al. (2010), which visualizespositions and peculiar motions of several objects in thisspiral arm. The Perseus spiral arm exhibits a systematicdeviation from the circular rotation by a ∼
30 km s − inthe longitude range l = 90 – 150 ◦ . Since the 18 red vari-ables toward the Perseus arm exhibit a similar kinematiccharacteristic, we conclude that these variables are asso-ciated with the Perseus spiral arm. An average period ofthe 18 red variables in the Perseus arm is 423 ( ± M ⊙ with age of 0.9 Gyr (see, e.g., Figure 20 of Vassiliadis &Wood 1993). Thus, the red variables in the Perseus armhas not left far from the birth place. As well as the Perseus spiral arm, we may consider apossibility of association of another deviant group at l = 25– 45 ◦ and V lsr ≃ +40 – +80 km s − with the Sagittarius-Crux arm. The average distance and period of 21 stars inthis group (the upper ellipse noted as Sgr group in Figure6) are 2.58 ( ± .
99) kpc and 489 ( ± D ∼ D ∼ D ∼ l ∼ ◦ .In the l - v diagram (see the overlaid color map of figure6), CO emission is very weak around ( l , V lsr ) ∼ (30 ◦ ,+60 km s − ), except in the direction of the HII region G .
257 + 0 . CO map (Leeet al. 2001). The kinematic distance of the HII region G .
257 + 0 .
155 was estimated to be 3.8 +0 . − . kpc (Fish etal. 2003) from the HI absorption feature assuming thestandard circular rotation. Recently the annual parallaxdistance was measured with VERA for the nearby infrareddark cloud, G .
43 + 00 .
24 (Kurayama, et al. 2011). Thedistance to the H O maser sources in this dark cloud is ∼ . ± .
12 kpc, which is considerably smaller than thekinematic distance of this cloud. Because the radial ve-locity of this cloud ( V lsr ∼
50 – 60 km s − ) is similar tothat of the HII region G .
257 + 0 . G .
257 + 0 .
155 may be overestimated. It is also likelythat our deviant group of stars, which has a similar radialvelocity in the same direction, is likely to be in the samespiral arm. Therefore, we call this group as the ”Sgr”deviant group because the average luminosity distance ofthe stars in this deviant group is close to the estimateddistance of the Sagittarius arm at l ∼ ◦ . Deguchi et al. [Vol. , Arcturus(1 kpc) -150-100-50050100150 060120180240300360 |b|<10°|b|>10° V l s r ( k m s - ) Galactic longitude (deg)4 kpc2 kpc1 kpc Hercules (1 kpc)
Fig. 5.
Longitude-velocity diagram for SiO detected sources in the present sample. Filled and unfilled circles indicate objects belowand above | b | = 10 ◦ . Three thick curves indicate radial velocities expected from the model with a flat rotation curve of 220 km s − for stars at distances, 1 , 2 , and 4 kpc from the Sun, respectively. Broken curves indicate radial velocities expected for the Herculesand Arcturus moving groups of stars (with a rotational lag of −
42 km s − and an outward velocity of 52 km s − for the Herculesgroup, and a rotational lag of −
120 km s − for the Arcturus group) at a 1 kpc distance from the Sun. -100-50050100 20406080100120140 |b|<10°|b|>10° V l s r ( k m s - ) Galactic longitude (deg) distant
Sgr groupHercules groupPerseus group
Fig. 6.
A part of figure 5 but overlaid on the CO longitude-velocity map taken from Dame et al. (2001). Filled and unfilled circlesindicate the SiO sources below and above | b | = 10 ◦ . The large ellipses indicate the deviant groups of stars toward the Sagittariusand Perseus arms, and for the Hercules group of stars. Small ellipse assigned as ”distant” indicates the distant stars which are notassociated with the Perseus deviant group. o. ] Kinematics of Red Variables I. Basic Data 7Reid et al. (2009) summarized the recent parallax mea-surements of massive star forming regions with VLBAand VERA by maser lines. Three star forming regions,G23.6 − − − G . − .
1) has a largeradial velocity of V lsr = +83 km s − (the kinematic dis-tance D Stdk = 5 .
04 kpc or D Revk = 4 . ± .
3) kpc for theirnew rotational parameters), but the parallax distance ofthis object is 3.19 kpc, which locates this objects verynear the far arm in this direction (the Scutum-Crux arm;see figure 5 of Reid et al. 2009). Another two source,G35.2 − − V lsr = +28 and +42 km s − ), for which the paral-lax distance roughly agrees with the kinematic distance (2– 3 kpc). From these facts and the 1.6 kpc distance of thedark cloud G .
43 + 00 .
24 (Kurayama, et al. 2011), weconclude that the spiral arm in this direction has a com-plicated velocity structure and a large noncircular motion.The exceeding velocity of the Sgr group of stars to thegalactic rotation suggests either (1) that these stars movefaster than the rotational velocity given by the flat rota-tion curve, or (2) that these stars move toward the galacticcenter (this inward motion causes the radial velocity in-crease in this direction). Because the directions of thesetwo motions appear in opposite sense in the proper mo-tion, VLBI observations of proper motions of objects inSagittarius arm can be a good test of above cases.Because the average period of this star group ( ∼
480 d)is considerably large compared with the average period ofoptical miras, they are relatively young objects comparedwith the field miras. Therefore it is likely that these starsare born in the Sagittarius arm and do not completelydepart from this arm yet.
Optical and infrared properties of the candidates forthe deviant groups are summarized in Table 5; it givesthe 2MASS name, period, variability type, R magnitude, R amplitude of the variability, 2MASS K s magnitude, er-ror in the K magnitude, quality flag for the K magni-tude, luminosity and kinematic distances. It involves afew stars with low photometric quality in the K band inthe 2MASS catalog. These objects have relatively largedistances compared with the average value of each group.Therefore the small average luminosity distances for thesetwo groups of stars are not due to the objects with poorphotometric accuracy.In the previous sections, we used the PL relation whichwas derived from the photometric measurements of themiras with periods between 100 and 400 d (Whitelocket al. 2008), and extended the linear relation to thelonger period up to 1000 d. However, it has been knownthat some miras with P >
400 d, especially for OH/IRsources, lie above the linear extrapolation of the PL re-lation (e.g., see Feast 2009). This may cause an errorin the distance estimation for the deviant group of stars.Therefore, we also applied the different PL relation for thestars with
P >
400 d, which was derived from the longer
Table 6.
Distance statistics for the deviant groups of stars
Group Quantity D k D L D Lc (number) (kpc) (kpc) (kpc)Perseus average 5.27 1.94 2.19(18) standard dev. 1.04 1.10 1.26 probability † — < − < − Sgr average 3.63 2.58 3.45(21) standard dev. 0.81 0.99 2.08 probability † — < − probability † — < − † : a probability of the Student’s t-test for the averagesof two sets of D K and D L (or D K and D Lc )being generated by the same distribution function.period miras in the Large Magellanic Cloud (LMC) (Ita& Matsunaga 2011). The detail of this correction wasdescribed in Appendix 3. The corrected distances (ap-plied for all of P >
400 d stars) are given in parentheticnumber in the 8th column of Table 5. In this case, theaverage distance is 2.2 ( ± .
3) kpc for the Perseus groupof stars, and it is 3.5 ( ± .
1) kpc for the Sgr group of stars,where the parenthetic number is the standard deviation.Therefore, such correction does not influence much for thedistance estimation for the Perseus group, but it increasesthe average distance considerably for the Sgr group, be-cause the latter group involves many stars with
P > P = 730 d) stars, which contaminate thissample. If we remove the 4 stars with P = 730 d, whichis the upper boundary as a result of insufficient data inthe NSVS survey (Williams et al. 2004), the average ofthe corrected luminosity distances of the Sgr group of 17deviant stars is 2.6 ( ± .
2) kpc. The average of the kine-matic distances of this reduced set is 3.5 ( ± .
7) kpc. TheStudent t-test gives a probability of 2 % for these two av-erages being produced by the same distribution function.In other words, with 98% confidence level, we can statethat the average distances of these two sets are signifi-cantly different. In table 6, we summarized the averagedistance and standard deviation, and the t probability ofthe Student’s t-test for the Perseus and Sgr (with smallernumber) groups. In summary, the discrepancy betweenkinematic and luminosity distances for the Perseus andSgr groups of stars are not removed by the correction inthe distance for the
P >
400 d, though evidence is slightlyweak for the case of the Sgr group. The present conclusion strongly depends on the luminosity dis-tance based on the PL relation. Further examination on the accu-racy of the distances will be given in the future paper, which alsodiscuss the validity of the optical proper motions for these objects. Of course, the smaller sets using only the miras with
P <
400 dgive luminosity distances, 1.9 ( ± .
2) kpc and 1.8 ( ± .
6) kpc forthe Perseus and Sgr groups, respectively. The difference betweenluminosity and kinematic distances is statistically significant inthe Student’s t-test for both groups, which are consistent withthe previous result including the
P >
400 d stars.
Deguchi et al. [Vol. ,
In this paper, we have given a preliminary analysis based on theobtained new radial velocities for a set of optical red variables, andhave shown that they provide useful information on the kinematicof the stars in the Galaxy.
4. Summary
We have observed 379 red variables in the SiO maser lines, ob-taining 229 (220 new) detections. Accurate radial velocities of thedetected sources are used for investigating the kinematics of stars inthe Solar neighborhood. Most of the observed stars locate within 3kpc from the Sun according to luminosity distances. The longitude-velocity diagram of the sample shows high number densities ofstars in two regions. The estimated luminosity distances suggestthat these groups of stars spatially collocate with the Perseus andSagittarius spiral arms. The result of the VLBI parallax measure-ments of the objects in these spiral arms seems to be consistent withthe present data. However, at the current moment, the number ofobjects observed with VLBI is too small to conclude the member-ship of objects to the Galactic spiral arms except for the objects inthe Perseus arm. In addition, we found a group of stars deviated bymore than 40 km s − in a Galactic longitude range of 20–40 ◦ , whichare likely to be members of the Hercules moving group. Proper mo-tion data are essential to reveal the 3d motions of these stars, andthe discussion based on the optically obtained proper motions willbe given in a forthcoming paper.We thank Dr. J. Nakashima, Univ. Hong Kong, for readingthe manuscripts and useful comments. This research was par-tially supported by a Grant-in-Aid for Scientific Research fromJapan Society for the Promotion of Sciences (20540234). This re-search made use of the SIMBAD and VizieR databases operatedat CDS, Strasbourg, France, and as well as use of data productsfrom Two Micron All Sky Survey, which is a joint project of theUniversity of Massachusetts and Infrared Processing and AnalysisCenter/California Institute of Technology, funded by the NationalAeronautics and Space Administration and National Science foun-dation. Appendix. 1. SiO maser spectra and short noteson individual objects
We show the SiO maser spectra (the J = 1–0 v = 1 and 2 tran-sitions) for detections in figures 8a–8m. We also show the spectraof other SiO maser transitions in figure 8. Individually interestingobjects are noted as follows. • J F = 34 . O maser emission hasbeen detected at V lsr = 0 . − (Lewis 1997), which isconsiderably shifted from the SiO radial velocity V lsr = − − measured in the present paper. OH maser searcheshave been negative (Nguyen-Q-Rieu et al. 1979; Lewis etal. 1995). The large velocity difference of about 30 km s − between H O and SiO maser lines suggests that this object islikely a water fountain source (Imai 2007). The central star,AG Cep, has a spectral type of M10, and a pulsation periodof 403 d in the NSVS catalog, which is slightly different fromthe period of 445 d in the SVS catalog (Samus et al. 2010).The IRAS LRS spectra of this source exhibits a very sharppeak at 9.8 µ m (LRS class 26), and Little-Marenin & Little(1990) classified the shape of silicate feature as ”Sil+”, whichhave high maser detection rate. • J µ m SiC feature; Volk et al. 1991), indicating a carbon star(Chen & Chen 2003). Searches for the 86.2 GHz SiO and88.6 GHz HCN emissions with the IRAM 30m telescope werenegative (Groenewegen et al. 2002). However, we detectedSiO masers in this star at V lsr = −
63 km s − . This result suggests that the LRS feature is a silicate absorption at 10 µ m typically seen in oxygen-rich evolved stars. • J J − , respectively, at the same Galactic lon-gitude l = 175 ◦ . The data points for these two stars are over-lapped in the longitude-velocity diagram (Figure 5), lying onon the broken curve of the Hercules moving group. In fact,they are at high Galactic latitudes and separated by 8 ◦ inGalactic latitude ( b = − . − . ◦ ). These two arelikely members of the Hercules moving group. • J F =21.1 Jy and IRAS LRS class of 13(feature less), but this star has been slipped out from the pastOH/IR and SiO maser surveys probably because of its ”blue”MIR color ( C = − . V lsr = − . − ) of this star at theGalactic coordinates of ( l,b ) = (170 . ◦ , − . ◦ ) indicates thatthis object is kinematically unusual. • J This is a faint IRAS source( F = 3 . V lsr = − . − in the present paper. • J V lsr = 53 . − at l = 70 . ◦ in SiO masers.OH and H O masers have been detected for this star (Lewiset al. 1995). The longitude-velocity diagram (Figure 6) showsthat several other stars also have similar (but slightly lower)radial velocities: J V lsr = 43 . − )and J V lsr = 31 . − ). These threestars fall in a circle of 3 degree diameter, and the estimateddistances are between 1.5 and 2.3 kpc (though the other twostars also fall near there in Figure 6, their distances are muchlarger). Because of their Galactic longitudes ( l ∼ ◦ ), it islikely that these stars are not associated with the Sagittariusspiral arm. They move faster than the Galactic rotation byabout 50 km s − . • J V lsr = − . − ; it is unusual as a star atthe Galactic coordinates (121.1 ◦ , 26.5 ◦ ); see Figure 5. Thisstar is located near the edge of the Polaris flare cloud in thelocal spur (Heithausen & Thaddeus 1990). The distance tothis flaring cloud is not very far from the Sun, possibly lessthan 0.5 kpc ( V lsr ∼ − − ). But this star is far awayfrom the CO cloud because the distance is estimated to be2.6 kpc. The pulsation period of this star is 338 d, and the2MASS K s magnitude is 4.3. IRAS 12 micron flux is 5.3 Jywith a color index C = − .
37. The spectral class is M8–9(Gigoyan & Hambaryan 1996). Therefore, It is likely thatthis is a deviant star in the Perseus arm, but not a star inthe Local spur.
Appendix. 2. Distance estimation using thePeriod–Luminosity relation
We estimated the luminosity distance from the observed K mag-nitudes using the Period-Luminosity (PL) relation (Whitelock et al.2008), M K = − . × [ log ( P ) − . − . . (1) http://heasarc.gsfc.nasa.gov/W3Browse/all/rittercv.html o. ] Kinematics of Red Variables I. Basic Data 9 The uncertainty of this formula is approximately 0.15 mag for themiras with a period between 150 and 400 d (Whitelock et al. 2008).The correction for stars with
P >
400 d will be discussed in Appendix3. The observed K magnitude can be corrected for the interstellarand circumstellar reddening (see equation (1) of Fujii et al. 2006) K c = K − A K /E ( H − K ) × [( H − K ) − ( H − K ) ] , (2)where we use A K /E ( H − K ) = 1 .
44 (Nishiyama et al. 2006), and( H − K ) is given by the empirical relation( H − K ) = 0 . × log ( P ) − .
597 (3)(Catchpole 1992). Then, we can compute the distance from thedifference between corrected and absolute K magnitudes, K c and M K , i.e.,( D L / pc) = 10 . K c − M K )+1 (4)Figure 4 is a histogram of the derived distances using PL relationfor the SiO detections and no detections. About 80% of the objectsare at the luminosity distances below 3 kpc.Accuracy of the obtained luminosity distance depends on twofactors: reliability of the measured pulsation period and errors inthe average K magnitude for a variable star. To check the reliabilityof the periods given by the NSVS catalog, we have cross-correlatedthe NSVS periods with those of the SVS catalog. Though the twoperiods derived from the NSVS and SVS catalogs coincide well forthe medium-period objects ( P <
600 d) in general, the coincidencebecomes worse for the longer period stars. Therefore, we have tobe careful to derive the distance based on the period given by theNSVS catalog. The present sample involves not only miras butsemi-regulars too. Though 75 percent of stars in the present sampleare of the variability type of mira, 20 percent of stars are of semi-regular type and 5 percent of stars are of other type (the lattertwo types are noted by symbols ” † ” and ” ‡ ” in the second columnof table 4). Moreover, some miras with SiO masers occasionallyexhibits a pulsation in a first overtone mode (Ita et al. 2006).Although it has been argued that semi-regulars may follow to a P – M K relation different from miras (for example, Bedding & Zijlstra1998), the current understanding attributes this phenomenon to themultiplicity of pulsation modes (Tabur et al. 2010). For a certainpercentage of stars with P <
250 d follows to the P – M K relation withalmost the same slope but approximately one magnitude brighterthan the standard sequence of the P – M K relation (sequence C in a P – M K diagram; Ita et al. 2004; Tabur et al. 2010). However, in thepresent analysis, we have used the single P – M K relation (1) for all ofthe observed stars, and estimated the distances. This is because it ishard to specify the pulsation mode for a particular star with P < ∼
13 %in the present semi-regular sample; see also Alcolea et al. 1990). Inthe present sample, only 18 stars with
P <
250 d were detected inall the 229 SiO detections. Therefore, the error in the distance inthe SiO detection sample is not severe. For the 18 Perseus group ofstars, no semiregular was involved. For the 21 Sgr group of stars,one semiregular with P = 351 d, which is likely in the sequence C,was involved. Therefore, the multiplicity of the P – M K relation forthe short period variables does not affect the discussions made insection 3.The K-band amplitude of pulsation reaches to 0.8 magnitude formiras (Whitelock et al. 2008). The 2MASS K s magnitude, whichwas measured at a single epoch, may differ from the average value ina pulsation period by about 1 mag [e.g., figure 11 of Messineo et al.2004]. Furthermore for bright stars with K <
4, the 2MASS mag-nitude involves relatively large uncertainty (up to 0.4 mag) (Cutriet al. 2003). Therefore, we deduce that the derived luminosity dis-tance may involve uncertainty of a factor of about 2 for individualobjects. However, we expect that the uncertainty do not producesevere systematic shift in the distance scale and the average valuefor a certain number of stars is meaningful. Therefore, we believethat the uncertainty of the distance do not mislead the discussionmade in the present paper. N u m be r D (kpc)0
Fig. 7.
Histogram of corrected luminosity distances com-puted using the PL relation (equation 5) for
P >
400 d .The filled and shaded area indicates the SiO detection andnon detection. The average distance is 2 . ± .
8) kpc for SiOdetections and 2 . ± .
2) kpc for no detections, where theparenthetic number is a standard deviation.
Appendix. 3. Distance correction for the starswith
P >
400 d.
It has been argued that the long-period variables with a periodlonger than 400 d lie systematically above a linear extrapolationof the PL relation of the miras with 100 < P <
400 d [see a nicesummary on this problem given by Feast (2009)]. Whitelock etal. (2003) concluded that all the luminous stars found by the earlyinvestigation of Hughes & Wood (1990) in the Large MagellanicCloud (LMC) follow an extrapolation of the PL relation except afew stars under the Hot Bottom Burning (HBB) stage. BecauseLithium is overabundant in many OH/IR (and SiO maser) stars(Garc´ıa-Hern´andez et al. 2007), it is very likely that the presentsample of SiO maser sources is contaminated by the luminous HBBstars. Therefore, we re-estimated the distances of stars introducingthe PL relation with a steeper gradient at
P >
400 d. We use forstars with
P >
400 d, M K = − . × [ log ( P ) − . − . , (5)and( H − K ) = 1 . × [ log ( P ) − .
6] + 0 . . (6)These equations are derived based on the JHK band observationsof the long period variables in the range 2 . < log ( P ) < .
95 in theLMC (Ita & Matsunaga 2011). The apparent H and K magnitudesin LMC are converted to M K with a distance modulus of 18.5 forLMC. Because the circumstellar extinction is negligibly small forthese LMC O-rich stars at log ( P ) < .
95 in their study, the linearfits of H and K against log(P) in their paper represent the H andK magnitudes without extinction. Therefore, the difference betweenthe H and K linear fits directly gives ( H − K ) . The uncertaintyof the linear fit in K is deduced to be about 0.36 mag (if we as-sume the deviation in K is the same as that in the LMC; Ita &Matsunaga 2011). From the above equations, we can compute thefinal correction factor for the distance for the stars with P >
400 das D Lc /D L = 10 . × [ log ( P ) − . . (7)where D Lc and D L are the corrected luminosity distance for P > P = 850 d. We gave the corrected distance for the Perseus andSgr groups of stars in parenthetic number at the 9th column of table5. The histogram of the luminosity distances in the present sample,which is corrected for all of the P >
400 d stars, is shown in Figure7.
The PL relation for the
P <
400 d stars does not exhibit a sig-nificant offset between the LMC and our Galaxy (Whitelock et al.2008). Therefore it is reasonably expected that, for the longer pe-riod stars (
P >
400 d), the same relation holds both in the LMC andin our Galaxy, except for a special environment such as the Galacticcenter (e.g., Ortiz et al. 2002).
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Observational results of SiO Masers.SiO J = 1–0 v = 1 maser line SiO J = 1–0 v = 2 maser line2MASS name T a V lsr L.F. rms T a V lsr L.F. rms obs. date (J—) (K) (km s −
1) (K km s −
1) (K) (K) (km s −
1) (K km s −
1) (K) (yymmdd.d) − − − − − − − − − − − − − † − − − − − − † − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − † † − − − − − − − − − − − − − − − − − − − − − − − − − − − − − o. ] Kinematics of Red Variables I. Basic Data 13 Table 1. (Continued.)SiO J = 1–0 v = 1 maser line SiO J = 1–0 v = 2 maser line2MASS name T a V lsr L.F. rms T a V lsr L.F. rms obs. date (J—) (K) (km s −
1) (K km s −
1) (K) (K) (km s −
1) (K km s −
1) (K) (yymmdd.d) − − − − − − − − − − − − † , − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − † − − − − − − − − − − − − − † − − − − − − − − − − − − Table 1. (Continued.)SiO J = 1–0 v = 1 maser line SiO J = 1–0 v = 2 maser line2MASS name T a V lsr L.F. rms T a V lsr L.F. rms obs. date (J—) (K) (km s −
1) (K km s −
1) (K) (K) (km s −
1) (K km s −
1) (K) (yymmdd.d) − − − − − − − − − − − † − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − o. ] Kinematics of Red Variables I. Basic Data 15 Table 1. (Continued.)SiO J = 1–0 v = 1 maser line SiO J = 1–0 v = 2 maser line2MASS name T a V lsr L.F. rms T a V lsr L.F. rms obs. date (J—) (K) (km s −
1) (K km s −
1) (K) (K) (km s −
1) (K km s −
1) (K) (yymmdd.d) − − − − − − − − − − − − − − − − † − − − − − − − − − − − − − − − − − − − − − − − − − − − − † ” indicates additional detections in the SiO v = 0 or 3, or SiO v = 0 J = 1–0 line. see table 3. previous detection of the SiO J = 2–1 v = 1 line (Haikala et al. 1994). previous detection of the SiO J = 1–0 v = 1 and 2 line by Deguchi et al. (2010), Deguchi et al. (2004), Jiang et al. (1999), Cho et al. (1996) , Zuckerman (1979), Hall et al. (1990), Kim et al. (2010)
Table 2.
Negative results for the SiO J = 1–0 v = 1 and 2 lines. v = 1 v = 22MASS name rms rms obs. date(J—) (K) (K) (yymmdd.d) − − − − − − − − − − − − − − − − − − − − − − − o. ] Kinematics of Red Variables I. Basic Data 17 Table 2. (Continued.) v = 1 v = 22MASS name rms rms obs. date(J—) (K) (K) (yymmdd.d) − − − Table 2. (Continued.) v = 1 v = 22MASS name rms rms obs. date(J—) (K) (K) (yymmdd.d) − Table 3.
Observational results for additional SiO lines2MASS name transition
T a V lsr
L.F. rms obs. date(J—) (K) (km s −
1) (K km s −
1) (K) (yymmdd.d) SiO v = 0 J = 1–0 0.382 − SiO v = 3 J = 1–0 0.316 − SiO v = 0 J = 1–0 0.521 2.2 0.835 0.084 10022205572394+4822417 SiO v = 3 J = 1–0 1.629 2.8 4.406 0.105 10022205581447+5002407 SiO v = 0 J = 1–0 0.305 − − SiO v = 0 J = 1–0 0.438 − − SiO v = 0 J = 1–0 0.728 − − SiO v = 0 J = 1–0 0.595 − SiO v = 0 J = 1–0 0.374 9.6 0.723 0.087 09030822071622+1153158 SiO v = 0 J = 1–0 0.836 23.3 0.542 0.095 09030922071622+1153158 SiO v = 3 J = 1–0 4.141 23.2 6.127 0.125 09030922071622+1153158 SiO v = 0 J = 1–0 0.334 19.1 0.505 0.104 090309 o. ] Kinematics of Red Variables I. Basic Data 19 Table 4.
Infrared properties of the observed objects2MASS name Period
K H − K F C V lsr ( SiO ) IRAS/MSX comment(J—) (d) mag. (Jy) (km s − name00074306+7414113 476 4.64 1.12 7.4 − − − − − − − − − − − − O , † − − − − − − † − − − − − − − − − − − − − − − − † − − − O − − − − − − − − † − − , H O − − − − † − − − − − − − − − − † − † − − − − − † − † − − † − − − − † − − † − † − − − − − † − − † − − † − − − † − − − − − − Table 4. (Continued.)2MASS name Period
K H − K F C V lsr ( SiO ) IRAS/MSX comment(J—) (d) mag. (Jy) (km s − name05001777+6046152 501 3.56 0.79 10.7 − − − − − − − − † − − − − − − † − − − † − − − − − − ‡ − − − − − † − − − − − − † − − † − − − − † − − ‡ − − − − ‡ − − − − † − − − − − − − ‡ − − − − − ‡ − − − ‡ − − ♯ − ‡ − − − − − − − − † − − − − − − − − − − ‡ − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − − ‡ − G − − − − ‡ − G − † − − ‡ − − G − − − − − − − − − − − − − − − − − − − − − O − − o. ] Kinematics of Red Variables I. Basic Data 21 Table 4. (Continued.)2MASS name Period
K H − K F C V lsr ( SiO ) IRAS/MSX comment(J—) (d) mag. (Jy) (km s − name16510590+1020515 303 3.02 0.65 10.5 − − − − − − − − † − − − − − − − − − − − − − − − − , H O − † − − − − − − − − − − − − − − − − − − − − − − − − − − − ‡ − ‡ − − − − − − − − − − − − − − − − − − − − − † − − − − − − − − − − † − − − − − † − − † − − − − − − − − − − − − − − † − − − − − − − − − − − − − − − − † − − − † − − − − − − † − − − − − − − − − Table 4. (Continued.)2MASS name Period
K H − K F C V lsr ( SiO ) IRAS/MSX comment(J—) (d) mag. (Jy) (km s − name19030960 − − − − − ♯ ♯ − − − † − − − − − − − † − − − − − − − − − − − − − − − − − − † − − − − − − − − − − − − − − − − − − − † − − † − − − − † − − − − − † − − − − − † − † − − † − − − † − † − − − − − † − − − − − − − ‡ − o. ] Kinematics of Red Variables I. Basic Data 23 Table 4. (Continued.)2MASS name Period
K H − K F C V lsr ( SiO ) IRAS/MSX comment(J—) (d) mag. (Jy) (km s − name20074663+3117241 281 3.77 1.00 14.5 − ‡ − † − − − − , H O † − − − † − † − − − − − − † − † − − − − − − − − † − † − − − − − − − † − − ♯ − − † − − − − − − − O − − − − − − − − − − − − − † − − − − − − − − − − − − − ♯ − − − † − − − ‡ − − − − † − † − − † − − − − − − − − ‡ − − Table 4. (Continued.)2MASS name Period
K H − K F C V lsr ( SiO ) IRAS/MSX comment(J—) (d) mag. (Jy) (km s − name21302607+5009190 730 4.75 0.68 6.5 − − − − − − − − − − − − − † − − − − † − † − † − − ♯ − − † − † † − − − † − † − − − − − − † − − − − − − − − − − − − † − † − † − − − ♯ − − − − † − − − − − − † − † − − − − − † : semiregular variables (SR+L), ‡ : the other type (MISC); ♯ G038.7780 − ♯ G037.3380 − ♯ G082.5317+01.4850, ♯ G084.2104 − ♯ G071.9088 − ♯ G084.2104 − ♯ G262.5919+18.5173, ♯ G239.6370+55.6395, ♯ G182.7804+72.0228, ♯ G055.3416-64.3560 ♭ In IRAS point source reject catalog (Beichman et al. 1989). Reference: Lewis (1997), Crocker & Hagen (1983), Engels et al. (1988), Eder et al. (1988), Engels & Lewis (1996) , Lewis (1994), Lewis et al. (1990), Lewis & Engels (1988), Benson & Little-Marenin (1996), Hall et al. (1990), Parimucha (2003), Cho & Kim (2010), Lewis et al. (1995) o. ] Kinematics of Red Variables I. Basic Data 25
Table 5.