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Annual Parallax Distance and Secular Motion of the Water Fountain

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Annual Parallax Distance and Secular Motion of the Water Fountain PASJ: Publ. Astron. Soc. Japan , 1–??, c 2018. Astronomical Society of Japan. Annual Parallax Distance and Secular Motion of the Water Fountain Source IRAS 18286−0959 Hiroshi Imai1,2, Tomoharu Kurayama3, Mareki Honma4, and Takeshi Miyaji4 1Department of Physics and Astronomy, Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima 890-0065 [email protected] 2International Centre for Radio Astronomy Research, M468, The University of Western Australia, 35 Stirling Hwy, Crawley, Western Australia, 6009, Australia 3Center for Fundamental Education, Teikyo University of Science, 2525 Yatsusawa, Uenohara, Yamanashi 409-0193 4Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588 (Received 2012 April 28; accepted 2012 October 16) Abstract We report on results of astrometric observations of H2O masers in the “water fountain” source IRAS 18286−0959 (I18286) with the VLBI Exploration of Radio Astrometry (VERA). These observations yielded an annual parallax of IRAS 18286−0959, π =0.277 ± 0.041 mas, corresponding to a heliocentric +0.63 distance of D =3.61−0.47 kpc. The maser feature, whose annual parallax was measured, showed the ab- −1 solute proper motion of (µα,µδ) = (−3.2 ± 0.3, −7.2 ± 0.2)[mas yr ]. The intrinsic motion of the maser feature in the internal motions of the cluster of features in I18286 does not seem to trace the motion of the bipolar jet of I18286. Taking into account this intrinsic motion, the derived motion of the maser feature is roughly equal to that of the maser source I18286 itself. The proximity of I18286 to the Galactic midplane (z ≈10 pc) suggests that the parental star of the water fountain source in I18286 should be intermediate- mass AGB/post-AGB star, but the origin of a large deviation of the systemic source motion from that expected from the Galactic rotation curve is still unclear. Key words: masers — stars: AGB and post-AGB — stars: individual (IRAS 18286−0959) 1. Introduction AGB stars (e.g., Imai 2007). Here we report on the measurement of an annual par- −3 −1 Energetic mass loss (rate up to 10 M˙⊙yr ) has been allax of H2O masers in IRAS 18286−0959 (hereafter ab- observed from dying stars such as asymptotic giant branch breviated as I18286) with the VLBI Exploration of Radio (AGB) and post-AGB stars. The spatio-kinematics of Astrometry (VERA). The VERA astrometry for I18286 the mass-loss flows have been investigated in great de- was conducted in one of the VERA key science projects, tail by observations of maser emission such as SiO, H2O, which focuses on H2O maser sources at intermediate dis- and OH using very long baseline interferometry (VLBI). tances (2–5 kpc from the Sun) in order to extend the dis- These maser sources are associated with circumstellar en- tance scale for the VERA parallax measurements. The velopes (CSEs) of AGB stars, but in rare cases with highly result of the I18286 astrometry could be used as one of arXiv:1211.6207v2 [astro-ph.SR] 31 Jan 2013 collimated bipolar jets, so called “water fountains,” and the data points for exploring the Galactic dynamics if the CSE remnants around post-AGB stars or central objects motion of I18286 closely follows that of the Galactic ro- of planetary nebulae (PNe). In the latest decade, high tation (i.e. Reid et al. 2009; Honma et al. 2012). I18286 precision astrometry in very long baseline interferomery is a member of the class of water fountains, whose spatio- (VLBI) has enabled the measurement of trigonometric kinematics of H2O masers have been investigated in de- parallax distances and proper motions of maser sources. tail. Yung et al. (2011) suggest that most of the H2O Even in the rare cases mentioned above, the heliocentric masers in I18286 are associated with “double helices” of distances and three-dimensional secular motions of the highly collimated bipolar jets with speeds of ∼100 km s−1. water fountains, pre-PNe, and PNe have been measured, The formation of the double helices is expected from dis- in those cases where H2O masers could be detected (Imai continuous mass ejection from a moving star on a pe- et al. 2007c; Imai et al. 2011b; Tafoya et al. 2011). These riod of ∼30 yr. The annual parallax measurement for kinematic approaches have contributed to estimating the I18286 is the second case of parallax measurements for physical parameters of these parental stars and their evo- the water fountains after that for IRAS 19134+2131 (Imai lutionary properties. Taking into account their locations et al. 2007c). This paper discusses the galactic kinematical and 3D motions in the Milky Way, it has been suggested properties of I18286 in Sect. 3.2. However, the existence that these stars should be intermediate-mass AGB/post- of a low-velocity “equatorial flow” should be taken into 2 H. Imai et al. [Vol. , account when one interprets the observed secular motion improved for observations since 2007 by installing one of the maser feature in the cluster of features in I18286 to four artificial noise sources (Honma et al. 2008a). (Imai 2007). The argument of the equatorial flow will be Thirdly, fringe-fitting and self-calibration were performed described in a separate paper in more detail. using the continuum source data, whose solutions were applied in the data analysis of maser emission. Only the 2. Observations and data reduction solutions in the BBC at the same frequency as that for the H2O maser emission were valid for the fringe-phase The VERA observations of the I18286 H2O (JK−K+ = calibration. The accuracy of the phase-fluctuation 612 → 523, 22.235080 GHz) masers were conducted at 16 compensation and the coherence of the integration is epochs from 2007 October to 2009 September. Table 1 dependent on weather condition, particularly the humid- gives a summary of these observations, maser source map- ity, which is seasonally variable. These effects affect the ping, and astrometry. Out of 16 epochs, 14 produced final astrometric accuracy. Finally, image cubes of the scientifically meaningful output. At each epoch, the ob- maser source were obtained by deconvolution through servation was made for 6.7 hr in total. I18286 was ob- the CLEAN algorithm with a typical synthesized beam served together with the fringe-phase and position refer- of 0.9×2.5 in milliarcseconds (mas) in the case of full ence source, ICRF J183220.8−103511 (hereafter abbrevi- operation of VERA’s four antennas. Because the CLEAN ated as J1832), separated by 0◦.67 from I18286, simul- deconvolution was performed by automatically selecting taneously using VERA’s dual-beam system. They were local peaks of brightness in each of channel maps without tracked for 30–35 min out of every 40 min, followed by smaller CLEAN boxes, side lobes of the synthesized scans on other band-pass calibrator sources. The received beam pattern affected the final CLEAN image cube1. signals were digitized in four quantization levels, then di- Each maser spot (or velocity component) was identified vided into 16 base band channels (BBCs) with a band- as a Gaussian brightness component using the AIPS task width of 16 MHz each. One of the BBCs collected data SAD. from I18286 at the frequency band including the H2O In order to obtain higher quality maser maps, we also maser emission, while other BBCs from J1832 spanning adopted a normal procedures for maser source mapping. a total frequency band range of 480 MHz. The BBC out- Fringe-fitting and self-calibration were performed using puts had a recording data rate of 1024 Mbits s−1. The a spectral channel that contain bright maser emission. data correlation was made with the Mitaka FX correla- Column 4 in table 1 gives the local-standard-of-rest (LSR) tor with a correlation accumulation period of 1 s. The velocity of the spectral channel selected as phase- and correlation outputs consisted of 512 and 32 spectral chan- position-reference. The obtained solutions of calibration nels for the H2O maser and reference continuum emission, were applied to the data in all spectral channels. respectively. The former corresponds to a velocity spac- ing of 0.42 km s−1, which is narrow enough to resolve an 3. Results H O maser feature (corresponding to a maser gas clump), 2 3.1. The distribution and proper motions of H O maser which consists of two or more spectral channel components 2 features in IRAS 18286−0959 called maser spots. Data reduction was mainly made with the National Column 6 of table 1 gives the numbers of maser features Radio Astronomy Observatory (NRAO) Astronomical identified in the individual epochs. Figure 1 shows the dis- Image Processing System (AIPS) package. For astrom- tributions of H2O maser features at six out of 14 epochs. etry, we need special procedures described as follows The maser feature distribution was highly variable, with (see also e.g., Honma et al. 2007; Imai et al. 2007b). only a small fraction of the maser features having lifetimes Firstly, delay-tracking was repeated for the correlated longer than half year. Note that the VLBA observations data using better delay-tracking models calculated with conducted by Yung et al. (2011) and the VERA observa- the software equivalent to the CALC9 package developed tions reported in this paper, respectively, lasted for simi- by the Goddard Space Flight Center/NASA VLBI group. lar seasons, 2008 April–2009 May and 2007 October–2009 Throughout the whole data analysis, we adopted the coor- September, respectively. The latter observations identi- h m s dinates of the delay-tracking center: αJ2000 =18 31 22 fied most of the same maser features as found in Yung ◦ ′ ′′ .934, δJ2000 = −09 57 21 .70 for I18286 and et al.
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