IRAS observations of OH/IR stars

Olnon, F. M.; Baud, B.; Habing, H. J.; Dejong, T; Harris, S.; Pottasch, [No Value]

doi:10.1086/161766

Cited by 82 publications

(40 citation statements)

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“…Most surveys for OH/IR stars after 1983 are based on the IRAS Point Source Catalog data base, exploiting the highly successful predictive property of the IRAS twocolour diagram for detecting OH/IR stars (Olnon et al 1984;Van der Veen & Habing 1988). Because of confusion in the GC, these surveys omit the GC area (however, see Taylor et al 1993 for a description of an "IRAS Galactic Center Catalog").…”

Section: Discussionmentioning

confidence: 99%

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: Discussionmentioning

confidence: 99%

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 IRAS colour-colour diagram has long been proved to be an efficient and simple tool for discussion of properties and evolutionary status of AGB stars (e.g., Olnon et al 1984;Zuckerman & Dyck 1986;Volk & Kwok 1988;van der Veen & Habing 1988;Kwok 1990). The log(F 60 /F 25 ) versus log(F 25 /F 12 ) colour-colour diagram for all OH/IR stars with the IRAS LRS spectra and good quality (Q = 3 or 2) IRAS PSC fluxes is presented in Fig.…”

Section: The Iras Colour-colour Diagram Of Oh/ir Starsmentioning

confidence: 99%

“…Kleinmann et al 1981), a very successful approach in finding new OH/IR stars was to search the IRAS Point Source Catalogue (1988, hereafter PSC) for sources with colours resembling those of the AGB stars with oxygen-rich envelops (see e.g. Olnon et al 1984). Several systematic surveys have been performed to detect OH emission from sources selected according to their colours: the Arecibo (hereafter AO) surveys (Eder et al 1988; Lewis et al 1990;Lewis 1992a;Chengalur et al 1993;Lewis 1994); the Dutch-Parkes (hereafter tL-H) surveys (te Lintel Hekkert 1990;te Lintel Hekkert et al 1991); the Nançay surveys Le Squeren et al 1992;David et al 1993;te Lintel Hekkert & Chapman 1996) and others (e.g.…”

Section: Introductionmentioning

confidence: 99%

Properties of OH/IR stars with IRAS LRS spectra

Chen

Szczerba

Kwok

et al. 2001

A&A

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Abstract. 1858 OH satellite line (1612 MHz) maser sources associated with the IRAS counterparts were assembled from the literature. Cross-correlation between collected OH/IR -IRAS sources and the recent catalogue of the IRAS LRS spectra (Kwok et al. 1997) allows us to subdivide 1024 of them (after excluding OH sources with uncertain IRAS associations) into 10 groups according to the Volk & Cohen (1989) classification scheme. We have found that sources with silicate emission form the largest group (about 57%), followed by the group with silicate absorption (only about 16%). For more sensitive individual OH maser surveys these numbers differentiate even more and the ratio between silicate emission and absorption sources reaches a value close to 6. Surprisingly, we found an association of OH maser emission with a small number of stars with carbon-rich atmospheres. The distribution of these subgroups of OH/IR stars in the IRAS colour-colour and the period-colour diagrams as well as histograms of some physical properties are presented. The galactic distribution of important parameters (periods, IRAS colours, expansion and stellar velocities) for different classes of OH/IR sources is analyzed from the point of view of the stars' evolutionary status. The correlations among the periods, colours, expansion and star velocities and the pumping efficiencies for selected subgroups of OH/IR stars are also investigated. These analyses allow us to demonstrate that a significant fraction of silicate emission group sources do not form an evolutionary sequence with the silicate absorption objects -as is suggested e.g. by the IRAS colour-colour diagram, but rather form a lower initial mass sequence, i.e. these sources will never develop sufficient mass loss to manifest silicate absorption.

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“…Olnon et al 1984;Bedijn 1987;van der Veen & Habing 1988). Due to the different properties of their dust shells, OH/IR stars, PPNe, and PNe occupy slightly different regions in the diagram (although there is also an overlap), and the diagram has been found to be especially useful in the selection of PPNe (e.g., Hu et al 1993a).…”

Section: Sio Masers In An Iras Two-color Diagrammentioning

confidence: 99%

SiO masers in OH/IR stars, proto–planetary and planetary nebulae

Nyman

Hall

Olofsson

1998

Astron. Astrophys. Suppl. Ser.

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Abstract. We present a search for SiO masers towards a sample of 126 objects including OH/IR stars, protoplanetary and planetary nebulae. All objects are classified as oxygen-rich, and most of them are associated with OH or H 2 O masers. SiO masers were found only in variable objects like the OH/IR stars and a few objects classified as proto-planetary nebulae, but with variable central stars that may be part of binary systems. In one object, OH 15.7+0.8, which appears to be varying irregularly and most likely recently left the AGB, an SiO maser was tentatively detected. Thus, we conclude that variability and SiO maser emission are closely linked, and that SiO masers disappear very soon after a star has reached the end of the AGB, when pulsation and mass loss cease.

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IRAS observations of OH/IR stars

Cited by 82 publications

References 0 publications

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

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

Properties of OH/IR stars with IRAS LRS spectra

SiO masers in OH/IR stars, proto–planetary and planetary nebulae

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