Astrometric observation of the Galactic LPVs with VERA; Mira and OH/IR stars

Akiharu Nakagawa; Tomoharu Kurayama; Gabor Orosz; Tomoaki Oyama; Takumi Nagayama; Toshihiro Omodaka

doi:10.1017/s174392131800635x

Astrometric observation of the Galactic LPVs with VERA; Mira and OH/IR stars

Proceedings of the International Astronomical Union ◽

10.1017/s174392131800635x ◽

2018 ◽

Vol 14 (S343) ◽

pp. 476-477

Author(s):

Akiharu Nakagawa ◽

Tomoharu Kurayama ◽

Gabor Orosz ◽

Tomoaki Oyama ◽

Takumi Nagayama ◽

...

Keyword(s):

Long Period ◽

Vlbi Observations ◽

Ir Stars ◽

Long Period Variables ◽

Astrometric Observation

AbstractWe present studies of Long Period Variables (LPVs) in our Galaxy based on astrometric VLBI observations of H2O and SiO masers. The Galactic Miras and OH/IR stars are our main targets. For Miras, we present the distribution of the LPVs on the MK – log P plane. Galactic Miras show consistency with PLR in the LMC except for some fainter sources. Parallaxes of the LPVs determined from VLBI and Gaia are compared. There seems to be some offset.

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The Galactic Distribution of OH/IR Stars

International Astronomical Union Colloquium ◽

10.1017/s0252921100069621 ◽

1977 ◽

Vol 42 ◽

pp. 399-433

Author(s):

H.J. Habing

Keyword(s):

Present Status ◽

Line Emission ◽

Microwave Line ◽

Late Type ◽

Maser Emission ◽

Long Period ◽

Ir Stars ◽

Long Period Variables ◽

Recent Compilation ◽

Galactic Distribution

In 1967 Wilson and Barrett (1968, 1970) discovered that some long period variables, very red and apparently very late type stars, emit OH microwave line emission that is especially strong in the 1612 MHz line at 18 cm. At present some 65 such OH-emitting stars have been identified - for a recent compilation see Bowers and Kerr (1977, M giants) and Baudry et al. (1977, M supergiants). Several stars show maser emission in H2O and SiO as well. At this colloquium Winnberg will review the present status of our knowledge of these stars.

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The galactic distribution of OH/IR stars

Symposium - International Astronomical Union ◽

10.1017/s0074180900014157 ◽

1979 ◽

Vol 84 ◽

pp. 29-34

Author(s):

B. Baud ◽

H. J. Habing ◽

J. H. Oort

Keyword(s):

Spectral Type ◽

Velocity Difference ◽

Double Peak ◽

Strong Emission ◽

Long Period ◽

Ir Stars ◽

Long Period Variables ◽

Galactic Distribution

Through systematic surveys (Johansson et al., Caswell and Haynes, Bowers, Baud, Caswell et al.) some 200 OH masers have been detected that are presumably associated with long period variables of very late spectral type (>M5). Tentatively these stars will be called “OH/IR stars”. They are characterized by their strong emission in the 1612 MHz line which shows a double peak due to the expansion of the shell surrounding these stars. The velocity difference ΔV between the peaks is generally between 10 and 50 km s−1.

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Long-period Variable Stars Near the Galactic Centre

Symposium - International Astronomical Union ◽

10.1017/s0074180900203501 ◽

1999 ◽

Vol 191 ◽

pp. 523-528 ◽

Cited By ~ 1

Author(s):

I.S. Glass ◽

S. Matsumoto ◽

B.S. Carter ◽

K. Sekiguchi

Keyword(s):

Variable Stars ◽

Galactic Centre ◽

Galactic Bulge ◽

Long Period ◽

Four Seasons ◽

Ir Stars ◽

Long Period Variables ◽

Period Variable

A second report on our 4-year survey for long-period variables (LPVs) in the central 24 × 24 arcmin2 of the Galactic Bulge is presented. All four seasons of data have now been reduced and ∼ 350 variables have been found. Preliminary periods have been obtained for most of them. Fifty-five out of 103 known OH/IR stars in the field have been recovered in the K-band.

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