1
KaVA ESTEMA (Expanded Study on Stellar Masers) Hiroshi Imai *1 , Se-Hyung Cho *2 , Yoshiharu Asaki 3 , Yoon-Kyong Choi 2 , Jaeheon Kim 2 , Youngjoo Yun 2 , Naoko Matsumoto 5 , Cheul-Hong Min 4 , Tomoaki Oyama 4 , S.-C. Yoon 5 , D.-H. Kim 5 , Richard Dodson 6 , Maria J. Rioja 6 , Ross, A. Burns 1 , Gabor Orosz 1 , Miyako Oyadomari 1 , Akiharu Nakagawa 1 , James Chibueze O. 7 , Juni-ichi Nakashima 8 , and Andrey M. Sobolev 8 * co-PI; 1 Kagoshima Univ.; 2 KASI KVN; 3 NAOJ Chile; 4 NAOJ Mizusawa; 5 Seoul National Univ.; 6 ICRAR/UWA; 7 Univ. Nigeria; 8 Ural Fed. Univ. Time line and specification of the KaVA Large Programs on circumstellar masers Phase 1: ESTEMA (approved) during 2015 autumn2016, 2 years ×120 hours Snapshot imaging of H 2 O and SiO masers in circumstellar envelopes (Figure 1) around ~80 stars (source list in public) statistics of stellar masers i. maser spot sizes and shapes ii. distributions of H 2 O masers with respect to locations of SiO masers iii. correlation with kinematic parameters of circumstellar envelopes and stars yielding a larger sample of stars as targets of the Phase 2 project Phase 2: Intensive monitoring campaign during 20162024, 400500 hours/year 16—20 pulsating stars (P=300—1600 days) monitoring SiO and H2O masers in every 1/20 pulsation cycle over a few pulsation cycles for “stellar maser movie” synthesis detecting (both or either) i) propagation of pulsation-driven shock waves (Figure 2) ii) periodic change in physical conditions affected by stellar radiation Comprehensive synergy with ALMA, VLTI, Nano-JASMINE v=1 peak flux = 53.7 Jy channel /beam Levs = 0.54*(1, 2.6, 6.6, 16.8, 43, 69) Decl. offset (milliarcsecond) R.A. offset (milliarcsecond) 430 425 420 415 410 405 400 -235 -240 -245 -250 -255 -260 v=2 peak flux = 87.4 Jy channel /beam Levs = 0.88*(1, 2.600, 6.600, 16.80, 43, 69) SiO v=1 J=10 SiO v=2 J=10 BX Cam Figure 1 Schematic view of the spatial and density structure of a circumstellar envelope of an oxygen-rich (intermediate-mass) long-period pulsating star that hosts SiO and H2O masers. Gas ejected from the stellar surface forms molecules, then oxygen/silicon-rich dust (e.g. silicate and olivine). The dust particles are accelerated by stellar radiative pressure received through scattering of stellar infrared radiation. The microscopic (dust condensation) and macroscopic (turbulence, shock waves) process should be linked and explored in the KaVA projects. Distance from the star (stellar radus) Expansion velocity [km/s] 0 5 10 15 0 5 10 15 20 With shock waves SiO masers H 2 O masers shock wave propagation per year KaVA angular resolution at 1 kpc Without shock waves Figure 2 Schematic view of the radial velocity field of a circumstellar envelope of a pulsating star and the locations of the hosting SiO and H2O masers. Pulsation driven shock waves will be detectable by directly finding the velocity field and its time variation in the intensive KaVA monitoring program over a few stellar pulsation cycles. ESTEMA operation design Scan patterns in each session (Figure 3, 4) Two-day pairs of blocks for K&Q-bands with VERA for K/Q/W/D bands with KVN This yields a good (u,v) coverage (~60 min + ~120 min integration with VERA and KVN, respectively) Baseband channel allocation (Figure 5) Covering 1 H 2 O and 5 SiO (3, 1, 1 lines at Q-, W-, D-bands, respectively) lines Data analysis mission for multiple scientific outcomes 1. KaVA snapshot images of 1 H 2 O and 2 SiO (v=1 & J=10) maser lines 2. Astrometry (VERA dual beam & slow antenna nodding) 3. mm VLBI with KVN (SiO v=1 & J=21 and J=32 maser lines, with SFPR) Data analysis processing (using AIPS/ParselTongue/Python) a. ESTEMA ingest pipeline: amplitude calibration and data splitting for each mission b. Standard data calibration pipelines for KaVA imaging and astrometry c. Advanced data processing: SFPR d. Data archiving: calibrated visibilities, image cubes, important plots, pipeline inputs Figure 3 ESTEMA imaging demonstration resulted from the KaVA data of the SiO masers around BX Cam (including astrometric map registration). Figure 4 Scan patterns adopted in the KaVA ESTEMA sessions. The ESTEMA sessions suppose a block of 6 hours for 4 maser sources. Figure 5 Baseband channel allocations for ESTEMA.

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KaVA ESTEMA (Expanded Study on Stellar Masers)Hiroshi Imai*1, Se-Hyung Cho*2, Yoshiharu Asaki3, Yoon-Kyong Choi2, Jaeheon Kim2, Youngjoo Yun2, Naoko Matsumoto5, Cheul-Hong Min4, Tomoaki Oyama4, S.-C. Yoon5, D.-H. Kim5, Richard Dodson6, Maria J. Rioja6, Ross, A. Burns1, Gabor Orosz1, Miyako Oyadomari1, Akiharu Nakagawa1, James Chibueze O.7, Juni-ichi Nakashima8, and Andrey M. Sobolev8

*co-PI; 1Kagoshima Univ.; 2KASI KVN; 3NAOJ Chile; 4NAOJ Mizusawa; 5Seoul National Univ.; 6ICRAR/UWA; 7Univ. Nigeria; 8Ural Fed. Univ.

Time line and specification of the KaVA Large Programs on circumstellar masersPhase 1: ESTEMA (approved) during 2015 autumn̶2016, 2 years ×120 hoursSnapshot imaging of H2O and SiO masersin circumstellar envelopes (Figure 1) around ~80 stars (source list in public)● statistics of stellar masers i. maser spot sizes and shapes ii. distributions of H2O masers with respect to locations of SiO masers iii. correlation with kinematic parameters of circumstellar envelopes and stars● yielding a larger sample of stars as targets of the Phase 2 project

Phase 2: Intensive monitoring campaignduring 2016̶2024, 400̶500 hours/year16—20 pulsating stars (P=300—1600 days)monitoring SiO and H2O masers in every 1/20 pulsation cycle over a few pulsation cycles for “stellar maser movie” synthesis● detecting (both or either) i) propagation of pulsation-driven shock waves (Figure 2) ii) periodic change in physical conditions affected by stellar radiation● Comprehensive synergy with ALMA, VLTI, Nano-JASMINE

v=1 peak flux = 53.7 Jy channel /beam Levs = 0.54*(1, 2.6, 6.6, 16.8, 43, 69)

Dec

l. o

ffse

t (m

illia

rcse

con

d)

R.A. offset (milliarcsecond)430 425 420 415 410405 400

-235

-240

-245

-250

-255

-260

v=2 peak flux = 87.4 Jy channel /beam Levs = 0.88*(1, 2.600, 6.600, 16.80, 43, 69)

SiO v=1 J=1→0SiO v=2 J=1→0 BX Cam

Figure 1 Schematic view of the spatial and density structure of a circumstellar envelope of an oxygen-rich (intermediate-mass) long-period pulsating star that hosts SiO and H2O masers. Gas ejected from the stellar surface forms molecules, then oxygen/silicon-rich dust (e.g. silicate and olivine). The dust particles are accelerated by stellar radiative pressure received through scattering of stellar infrared radiation. The microscopic (dust condensation) and macroscopic (turbulence, shock waves) process should be linked and explored in the KaVA projects.

Distance from the star (stellar radus)

Exp

ansi

on v

elo

city

[km

/s]

0 5 10 15

0

5

10

15

20

With shock waves

SiO masers H2O masers

shock wave propagation per year

KaVA angular resolution at 1 kpc

Without shock waves

Figure 2 Schematic view of the radial velocity field of a circumstellar envelope of a pulsating star and the locations of the hosting SiO and H2O masers. Pulsation driven shock waves will be detectable by directly finding the velocity field and its time variation in the intensive KaVA monitoring program over a few stellar pulsation cycles.

ESTEMA operation designScan patterns in each session (Figure 3, 4)Two-day pairs of blocks for K&Q-bands with VERA for K/Q/W/D bands with KVNThis yields a good (u,v) coverage (~60 min + ~120 min integration with VERA and KVN, respectively)Baseband channel allocation (Figure 5)Covering 1 H2O and 5 SiO (3, 1, 1 lines at Q-, W-, D-bands, respectively) linesData analysis mission for multiple scientific outcomes1. KaVA snapshot images of 1 H2O and 2 SiO (v=1 & J=1→0) maser lines2. Astrometry (VERA dual beam & slow antenna nodding)3. mm VLBI with KVN (SiO v=1 & J=2→1 and J=3→2 maser lines, with SFPR)Data analysis processing (using AIPS/ParselTongue/Python)a. ESTEMA ingest pipeline: amplitude calibration and data splitting for each missionb. Standard data calibration pipelines for KaVA imaging and astrometryc. Advanced data processing: SFPRd. Data archiving: calibrated visibilities, image cubes, important plots, pipeline inputs

Figure 3 ESTEMA imaging demonstration resulted from the KaVA data of the SiO masers around BX Cam (including astrometric map registration).

Figure 4 Scan patterns adopted in the KaVA ESTEMA sessions. The ESTEMA sessions suppose a block of 6 hours for 4 maser sources. Figure 5 Baseband channel allocations for ESTEMA.