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LEW01 - The Approaching Death of the OH/IR star IRAS 18455+0448

Short title: Lewis et al. (2001)
Authors: Lewis, B. M. Oppenheimer, B. D. Daubar, I. J.
Journal: The Astrophysical Journal, Volume 548, Issue 1, pp. L77-L80.
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Detection table: Show detection table (3 detection)

Abstract
1612 MHz observations of the OH/IR star IRAS 18455+0448 in 1998 June showed that its peak intensity had faded by a factor of 20 from its 2.09 Jy discovery intensity in 1988. Its peak intensity, when observed at constant resolution, has faded exponentially since by a further factor of 10, with an e-folding time of 319 days. This decline is seemingly inexorable, even though the main line OH masers are as yet largely unaffected, as the correlation between the expansion velocities and periods of OH/IR stars suggests a likely period of ~400 days for 18455+0448 as a long-period variable, and our observations cover 706 days. We argue that extant data are best understood if we are witnessing an early stage in the expansion of a fossil circumstellar shell around 18455+0448, prior to it becoming a planetary nebula.	Comments: Spectral type was set to: ""S"", where only one peak was found. ""D"", where two peaks were found. Velocity resolution: 0.22 and 0.44 km/s

Abstract

1612 MHz observations of the OH/IR star IRAS 18455+0448 in 1998 June showed that its peak intensity had faded by a factor of 20 from its 2.09 Jy discovery intensity in 1988. Its peak intensity, when observed at constant resolution, has faded exponentially since by a further factor of 10, with an e-folding time of 319 days. This decline is seemingly inexorable, even though the main line OH masers are as yet largely unaffected, as the correlation between the expansion velocities and periods of OH/IR stars suggests a likely period of ~400 days for 18455+0448 as a long-period variable, and our observations cover 706 days. We argue that extant data are best understood if we are witnessing an early stage in the expansion of a fossil circumstellar shell around 18455+0448, prior to it becoming a planetary nebula.

Comments:
Spectral type was set to:
""S"", where only one peak was found.
""D"", where two peaks were found.

Velocity resolution: 0.22 and 0.44 km/s

Input tables: Table 1 and 2
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Detection table from Lewis et al. (2001)

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ID	Obs. RA	Obs. Dec	l	b	Group id	Source name	Line	Frequency	V_range	V_peak	F_peak	List	Detection	Class	Dist. (parallax)	Ref.
	(J2000)	(J2000)	(deg.)	(deg.)			OH	(MHz)	(km/s)	(km/s)	(Jy)		Yes/No		(kpc)
1	18 48 2.1	+04 51 29	36.8722	2.9683	G36.873+2.968	IRAS 18455+0448	1612 MHz;	1612	27.8	27.8	0.040	ENG15	+H₂O +OH	EVOLVED		LEW01
2	18 48 2.1	+04 51 29	36.8722	2.9683	G36.873+2.968	IRAS 18455+0448	1665 MHz;	1665	12.5	27.9	0.454	ENG15	+H₂O +OH	EVOLVED		LEW01
3	18 48 2.1	+04 51 29	36.8722	2.9683	G36.873+2.968	IRAS 18455+0448	1667 MHz;	1667	12.6	27.7	0.733	ENG15	+H₂O +OH	EVOLVED		LEW01

Distribution of sources in all sky (l,b)

Distribution of sources in all sky using Aladin

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Distribution of sources in IRAS color-color diagram

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Original color diagram is taken form van der Veen & Habing (1987)

Type	Description
I	Oxygen-rich non-variable stars without circumstellar shells
II	Variable stars with "young" O-rich circumstellar shells
IIIa	Variable stars with more evolved O-rich circumstellar shells
IIIb	Variable stars with thick O-rich circumstellar shells
IV	Variable stars with very thick O-rich circumstellar shells
V	Planetary nebulae and non- variable stars with very cool circumstellar shells
VIa	Variable stars with relatively cold dust at large distances; a significant part of the stars is carbon-rich
VIb	Variable stars with relatively hot dust close to the star and relatively cold dust at large distances; Some of the objects have proven to be O-rich
VII	Variable stars with more evolved C-rich circumstellar shells
VIII	Different sort of objects

Distribution of the detection velocities versus galactic longitude from LEW01

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