Long-period variable AGB stars in a field towards the galactic bulge

Blommaert, J. A. D. L.; Brown, A. G. A.; Habing, H. J.; Veen, W. E. C. J. van der; Ng, Y. K.

doi:10.1007/978-94-011-0922-2_23

Cited by 23 publications

(39 citation statements)

References 4 publications

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“…The solid line is the distribution of previously known OH/IR stars in our survey, new detections are distributed according to the dotted line. The striking resemblance of both distributions is in large contrast to the expansion velocity distributions of OH/IR stars with a different metallicity, for example in the outer Galaxy and Galactic plane (dashed: Blommaert et al 1993plus Blommaert et al 1994, multiplied by three for display purposes) velocity in Fig. 9.…”

Section: Expansion Velocity Distributionmentioning

confidence: 90%

A new sample of OH/IR stars in the Galactic center

Sjouwerman

Langevelde

Winnberg³

et al. 1998

Astron. Astrophys. Suppl. Ser.

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113

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Abstract. Two independent, largely overlapping 1612 MHz data sets were searched for OH/IR stars in the Galactic center. One set, taken with the Very Large Array in the period 1988 to 1991, consists of 17 epochs monitoring data of Van Langevelde et al. (1993). The other set was observed in 1994, using the Australia Telescope Compact Array. This article describes the data reduction procedures as well as a different way of searching image cubes for narrow line sources, and lists 1 a total of 155 double peak OH maser detections within 18 or 40 projected parsecs of Sagittarius A*, the compact radio continuum source in the Galactic nucleus. Presented are 65 formerly unseen double peaked 1612 MHz emitters, of which 52 are OH/IR stars. Also given are 3 single peak sources, which we believe to be masers of OH/IR stars. Apart from being less bright in their 1612 MHz OH maser line, the previously unknown OH/IR stars do not seem to be different from the previously known population of OH/IR stars in the Galactic center. We find that the OH/IR star OH maser luminosity distribution peaks at L OH ≈ 10 43.4 photons per second. Further physical and kinematical analysis of the new sample will be presented in additional papers.

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Section: Expansion Velocity Distributionmentioning

confidence: 90%

A new sample of OH/IR stars in the Galactic center

Sjouwerman

Langevelde

Winnberg³

et al. 1998

Astron. Astrophys. Suppl. Ser.

Self Cite

113

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“…The 22 objects listed as O-rich stars in RowanRobinson et al (1986), Epchtein, Le Bertre, & Lepine (1990), Lewis et al (1990), Le Squeren et al (1992, Blommaert, van der Veen, & Habing (1993), Chengalur et al (1993), Kastner et al (1993), Whitelock et al (1994), and Guglielmo, Le Bertre, & Epchtein (1998) are carbon stars. These stars are listed in the General catalog of galactic carbon stars (GCGCS) by Stephenson (Alksnis et al 2001) or classified as IRAS LRS class C (Kwok et al 1997).…”

Section: (A) O-rich Starsmentioning

confidence: 99%

A Catalog of Agb Stars in Iras PSC

Suh

Kwon²

2009

Journal of The Korean Astronomical Society

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We make a new catalog of AGB stars in our Galaxy from the sources listed in the Infrared Astronomical Satellite (IRAS) point source catalog (PSC) compiling the lists of previous works with verifying processes. We verify the class identification of AGB stars into oxygen-rich and carbon-rich stars using the information from recent investigations. For the large sample of AGB stars, we present infrared two-color diagrams from the observations at near infrared bands and IRAS PSC. On the two-color diagrams, we plot the tracks of theoretical radiative transfer model results with increasing dust shell optical depths. Comparing the observations with the theoretical tracks, we discuss the meaning of the infrared two-color diagrams.

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“…A.1 of the Appendix, excluding IRAS 17347-3139 and IRAS 17411-3154. We added K band photometry from the 2MASS and DENIS (Epchtein et al 1997) near-infrared surveys, and from the literature (Hyland et al 1972;Manchado et al 1989;Persi et al 1990;van der Veen & Habing 1990;Blommaert et al 1993;Noguchi et al 1993;Xiong et al 1994;Jiang et al 1996). Whenever a model light curve was fitted to the observational data (see the following section) this is also shown.…”

Section: Near-infrared Photometrymentioning

confidence: 99%

Near-IR variability properties of a selected sample of AGB stars

Jiménez-Esteban

García-Lario

Engels

et al. 2006

A&A

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We present the results of a near-infrared monitoring programme of a selected sample of stars, initially suspected to be Mira variables and OH/IR stars, covering more than a decade of observations. The objects monitored cover the typical range of IRAS colours shown by O-rich stars on the asymptotic giant branch and show a surprisingly large diversity of variability properties. Sixteen objects are confirmed as large-amplitude variables. Periods between 360 and 1800 d and typical amplitudes 1 m < ∼ ∆K < ∼ 2 m could be determined for nine of them. In three light curves, we find a systematic decrease in the mean brightness, and two light curves show pronounced asymmetry. One source, IRAS 07222-2005, shows infrared colours typical of Mira variables, but it pulsates with a much longer period (≈1200 d ) than a normal Mira. Two objects are either close to (IRAS 03293+6010) or probably in (IRAS 18299-1705) the post-AGB phase. In IRAS 16029-3041 we found a systematic increase in the H − K colour of ≈1 m , which we interpret as evidence of a recent episode of enhanced mass loss. IRAS 18576+0341, a heavily obscured luminous blue variable was also monitored. The star showed a continued decrease in brightness over a period of 7 years (1995)(1996)(1997)(1998)(1999)(2000)(2001)(2002).

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Long-period variable AGB stars in a field towards the galactic bulge

Cited by 23 publications

References 4 publications

A new sample of OH/IR stars in the Galactic center

A new sample of OH/IR stars in the Galactic center

A Catalog of Agb Stars in Iras PSC

Near-IR variability properties of a selected sample of AGB stars

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