VLBI懇談会シンポジウム 2019年11月24日 大妻女子大学

Extreme-OH/IR星の位置天文VLBI観測とSmall JASMINEやTAOとの連携
Akiharu NAKAGWA Kagoshima University

Aim of our study

・Confirming the PLR of the Galactic Miras
・Study the evolution from Miras to OH/IR stars

LPVs
・Initial Mass 0.8－8 M◎
・Period 100－1000 d
・Mass loss→Chemical evolution
・P-L relation → DistanceToday’s topics

https://www.cfa.harvard.edu/~mmarengo/me/agb.html(1): Astrometry of LPVs with VERA, VLBI and Gaia(2): Observations of LPVs to grasp its evolution from Miras to OH/IR stars(3): Collaboration with TAO, Small-Jasmine

65 project sources, ~30 parallaxes were measured.
ID

Src.

Type

R.A.

Dec.

IDSrc.

Type

R.A.

Dec.

123456789101112131415161718192021222324252627282930313233

W Hya
T Lep
RX_BooS_Crt
AP LynR UMa
WX_PscZ Pup
SY SclY Lib
VX UMaGX Mon
U Lyn
T UMa
S CrB
SW Lib
FS Lib
IRC-20540
IRC+10374
X Hya
R Cnc
FV_BooRU_Ari
RW_Lep
BW_CamBX_CamU_Ori
QX_Pup
RS_VirSY_AqlSV_Peg
R_TauOZ_Gem

SR
Mira
SRSR
Mira
Mira
Mira
Mira
Mira
Mira
Mira
Mira
Mira
Mira
Mira
Mira
Mira
Mira
Mira
Mira
Mira
SRSRSR
Mira
Mira
Mira
Mira
Mira
Mira
SRb
Mira
Mira

13h49m01.9980s
05h04m50.7999s
14h24m11.5998s
11h52m45.1000s
06h34m33.8999s
10h44m38.3999s
01h06m25.8998s
07h32m38.1000s
00h07m36.2000s
15h11m41.2999s
10h55m39.8999s
06h52m46.8999s
06h40m46.5000s
12h36m23.5000s
15h21m24.0000s
15h55m33.3999s
16h00m23.8000s
19h08m56.0000s
18h43m36.7000s
09h35m30.3000s
08h16m33.7999s
15h08m25.8000s
02h44m45.5000s
05h38m52.7000s
05h19m52.5600s
05h46m44.2999s
05h55m49.2000s
07h42m16.8298s
14h27m16.3998s
20h07m05.4000s
22h05m42.0850s
04h28m18.0000s
07h33m57.7500s-28d22m03.488-21d54m16.500+25d42m13.000-07d35m48.100+60d56m26.199+68d46m32.298+12d35m53.000-20d39m29.199-25d29m40.000-06d00m41.399+71d52m09.800+08d25m19.000+59d52m01.600+59d29m13.000+31d22m02.600-12d51m05.099-12d20m57.500-22d14m19.399+13d57m22.800-14d41m28.600+11d43m34.500+09d36m18.199+12d19m03.000-14d02m27.199+63d15m55.798+69d58m24.199+20d10m30.699-14d42m52.100+04d40m41.100+12d57m06.299+35d20m54.536+10d09m44.798+30d30m37.798

3435363738394041424344454647484950515253545556575859606162636465

V353_Pup
HU_PupHS_UMaR_LMi
BX_EriV637_Per
U_CVn
RU_HyaNSV17351
R_Peg
R_Hya
OH127.8
NSV25875
UU_Peg
R_Cas
S_Ser
W_Leo
OH32.8-0.3
V391CYGRAFGL5201
OH83.4-0.9
OH141.7+3.5
CU_Cep
DU_PupRAFGL2445
OH39.7+1.5
EUANDAWTAU
I17411-3154
OH26.5+0.6
OH42.3-0.1
TXCAM

SR
SR
LPV
Mira
SRSR
Mira
Mira
OHIR
Mira
Mira
OHIR
OHIR
Mira
Mira
Mira
Mira
OHIR
Mira
OHIR
OHIR
OHIR
OHIR
Mira
OHIR
OHIR
C
Mira
Mira
OHIR
OHIR
Mira

07h46m34.1510s
07h55m40.1600s
11h35m30.70408s
09h45m34.28304s
04h40m32.754s
03h54m02.28s
12h47m19.61s
14h11m34.39861s
07h07m49.38s
23h06m39.16689s
13h29m42.78187s
01h33 51.21s
22h19m27.48s
21h31m04.156s
23h58m24.87336s
15h21m39.53475s
10h53m37.43245s
18h52m24.682333s
19h40m52.394300s
06h34m28.052569s
20h50m58.619647s
03h33m30.618480s
22h11m31.882483s
07h35m03.978770s
19h44m07.000754s
18h58m30.094784s
23h19m58.881502s
05h47m30.209209s
17h44m24.003874s
18h37m32.51s
19h09m07.466221s
05h00m51.156996s-32d18m16.260-28d38m54.840+34d52m04.1775+34d30m42.7839-14d12m02.39+36d32m17.6+38d22m30.5-28d53m07.4089-10d44m05.9+10d32m36.0892-23d16m52.7747+62d26m53.2+59d51m21.7+11d09m13.24 92+51d23m19.7011+14d18m53.1002+13d42m54.3666-00d14m57.612+48d47m41.52658-05d03m42.85697+42d48m11.44793+60d20m08.85024+57d02'17.46857''-23d59'14.80023''+35d14'08.25184"+06d42'57.69806"+47d14'34.57638"+27d08'12.40939"-31d55'35.42862"-05d23'59.2"+08d16'22.70258"+56d10'54.09311"

Recent result of the period-Mk diagram of Miras in the Galaxy

Nakagawa et al. IAUS343 ProceedingVLBI and Gaia
●Mira, SRa●SRb○SRc■OH/IR

差分の評価指標

Peak: 0.29±0.35 σ
FWHM: 6.23

Parallax vs ParallaxNakagawa et al. in prep.

VLBI and Gaia

●VLBI
○Gaia

Parallax vs error

VLBI
y=(0.96±0.13)LogΠ – 1.20±0.06

Gaia

Gaia
y=(0.29±0.07)LogΠ – 0.72±0.04

VLBI

およそ190 pcを境に遠方はVLBIが有利, 近傍はGaiaが有利

Π = 5.20(D = 192 pc)

Nakagawa et al. in prep.

Observations of LPVs to grasp its evolution
from Miras to OH/IR stars
H2OとOH maserのスペクトル類似性
OH maser@1612MHzOH127.8+0.0

Similar characteristics
between H2O and OH
・Steep edges
・U-shaped hollow<Hypothesis>

Baud et al. 1979

H2O maser@22GHzNSV17351

H2O gas in NSV17351
has experienced anacceleration and reacheda terminal velocity in thelast 45 years.
H2O shell radius at theterminal velocity iscalculated to be >65 au.

Observations of LPVs to grasp its evolution
from Miras to OH/IR stars
H2O maser

膨張速度（小）進化① Mira型変光星

H2O maser

膨張速度（大）② Mira型変光星 ⇒ OH/IR星

OH maser

膨張速度（大・終端）③ OH/IR星

メーザーの種類

星周でH2Oメーザーが励起される

H2Oメーザーが加速を受けて外層へと広がる

H2Oメーザーが外縁部で光乖離されてOHメーザーが励起され始める

メーザーの速度ある速度で膨張次第に加速されて速度は速くなる

加速が終わり、速度は終端速度に達する

H2OメーザーH2Oメーザー

OHメーザー

膨張速度を反映したスペクトルの広がり。

加速により幅が徐々に広がる様子が見える。

加速が終わり終端速度に到達したOHメーザーが観測される。
切り立つエッジが特徴的。

可視から赤外まで広く輻射ありダストにより可視が抑えられ再放射による赤外の過多

メーザーのスペクトル

SEDの様子厚いダストによる中間赤外から遠赤外の過多が目立つ

VLBIobservationVLBI observation of extreme-OH/IR stars

VLBI and Gaia are complementary to each other.

OH127.8+0.0

DSS colored

ALLWISE volor Red(W4), Green(W2),Blue(W1) from raw Atlas Images

NSV25875
Peak 1.97 Jy/beam

2MSS color J(1.23um),H(1.66um),K(2.16um)

・43GHz astrometric observation
with VERA from Nov. 2017
・QSO: J2231+5922, ~240mJy@43GHz
・SiO
maser
(v=2), S/N=10AKARIFIS ColorWideL(140um),SideS(90um),N60(65um)

Phase referencing observation @43GHz, 2Gbps (512MHz BW for QSO)
Parallax = 0.38±0.13 mas, D = 2.60±0.85 kpc
RADEC

NSV25875

Sky plane

新しい観測結果

Parallax = 0.22±0.08 mas, D = 4.54±1.14 kpc(μx, μy) = (－1.18±0.12, －1.10±0.11) [mas/yr]

OH127.8+0.0

Sky plane

RADECSmall-Jasmine

・Verification of AGB star astrometry
・Single dish survey at Iriki (22, 43 GHz)

表面輝度構造変化の影響

116日

Chiavassa et al. 2018 (arXiv:1808.02548v1)
3D radiative-hydrodynamics simulations of convection
OH0.071-0.205
2.89 Jy
H2O maser

TAO

Short term and long term SED acquisition
H2O maser

膨張速度（小）MIMIZUKU
2－38μm

膨張速度（大）OH maser

膨張速度（大・終端）

進化① Mira型変光星② Mira型変光星 ⇒ OH/IR星

メーザーの種類

星周でH2Oメーザーが励起される

H2Oメーザーが加速を受けて外層へと広がる

H2Oメーザーが外縁部で光乖離されてOHメーザーが励起され始める

メーザーの速度ある速度で膨張

次第に加速されて速度は速くなる

加速が終わり、速度は終端速度に達する

H2OメーザーH2Oメーザー

OHメーザー

膨張速度を反映したスペクトルの広がり。

加速により幅が徐々に広がる様子が見える。

加速が終わり終端速度に到達したOHメーザーが観測される。
切り立つエッジが特徴的。

可視から赤外まで広く輻射あり

ダストにより可視が抑えられ再放射による赤外の過多

メーザーのスペクトルTAO

H2O maser

SEDの様子③ OH/IR星

厚いダストによる中間赤外から遠赤外の過多が目立つSummary:(1): Astrometry of LPVs with VERA, VLBI and Gaia
・PLR of the Galactic LPVs
・~30 parallaxes were determined from VERA・Parallaxes from VLBI and Gaia(2): Observations of LPVs to grasp its evolution
from Miras to OH/IR stars
・Acceleration found in H2O maser spectrum
・VLBI observation can determine parallaxof OH/IR stars to determine(3): Collaboration with TAO, Small-Jasmine
・TAO: Short term and long term SED monitoring
・Small-Jasmine: Verification of parallaxes from
infrared astrmetry