A dedicated echelle spectrometer for the Anglo-Australian Telescope

Meaburn, J.; Blundell, B.G.; Carling, R.; Gregory, D. F.; Keir, D.; Wynne, C. G.

doi:10.1093/mnras/210.2.463

Cited by 74 publications

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“…Observations were made with the Manchester Echelle Spectrometer (MES-SPM -see Meaburn et al 1984Meaburn et al , 2003 combined with the 2.1-m San Pedro Martir, (B.C. Mexico) telescope on 2008 Oct. 26 to 28.…”

Section: Observations and Resultsmentioning

confidence: 99%

A high-speed bipolar outflow from the archetypical pulsating star Mira A

Meaburn

López

Boumis

et al. 2009

A&A

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Optical images and high-dispersion spectra have been obtained of the ejected material surrounding the pulsating AGB star Mira A. The two streams of knots on either side of the star, found in far-ultraviolet (FUV) GALEX images, have now been imaged clearly in the light of Hα. Spatially resolved profiles of the same line reveal that the bulk of these knots form a bipolar outflow with radial velocity extremes of ±150 km s −1 with respect to the central star. The south stream is approaching and the north stream receding from the observer. A displacement away from Mira A between the position of one of the south-stream knots in the new Hα image and its position in the previous Palomar Observatory Sky Survey (POSS I) red plate was noted. If interpreted as a consequence of expansion proper motions, the bipolar outflow is tilted at 69 • ± 15 • to the plane of the sky, has an outflow velocity of 160 ± 10 km s −1 and is ≈1000 y old.

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Section: Observations and Resultsmentioning

confidence: 99%

A high-speed bipolar outflow from the archetypical pulsating star Mira A

Meaburn

López

Boumis

et al. 2009

A&A

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“…The high-dispersion (HD) spectroscopy was obtained in 1999, June 29 and 30, with the Manchester Echelle Spectrometer (MES; Meaburn et al 1984) combined with the f/7.9 focus at the 2.1-m OAN telescope at the Sierra de San Pedro Mártir, B. C., Mexico. This spectrometer has no cross-dispersion.…”

Section: Observations and Resultsmentioning

confidence: 99%

Unveiling the structure of the planetary nebula M 2-48:

López‐Martín

López²,

Esteban³

et al. 2002

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Abstract. The kinematics and physical conditions of the bipolar planetary nebula M 2-48 are analysed from high and low dispersion long-slit spectra. Previous CCD narrow-band optical observations have suggested that this nebula is mainly formed by a pair of symmetric bow-shocks, an off-center semi-circular shell, and an internal bipolar structure. The bipolar outflow has a complex structure, characterised by a series of shocked regions located between the bright core and the polar tips. There is an apparent kinematic discontinuity between the bright bipolar core and the outer regions. The fragmented ring around the bright bipolar region presents a low expansion velocity and could be associated with ejection in the AGB-PN transition phase, although its nature remains unclear. The chemical abundances of the central region are derived, showing that M 2-48 is a type I planetary nebula (PN).

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“…The major nebula axis long-slit spectra were taken with the Anglo-Australian telescope (AAT) using the Manchester Echelle Spectrometer (MES; Meaburn et al 1984) between 26 and 28 March 1999. A slit width of 150 µm, which is equivalent to 1 arcsec, was used and limits the resolution in the spectral direction to be 11 km s −1 .…”

Section: Optical Images and Spectroscopymentioning

confidence: 99%

VLT observations of the asymmetric Etched Hourglass Nebula, MyCn 18

Clyne

Redman

Lloyd

et al. 2014

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Context. The mechanisms that form extreme bipolar planetary nebulae remain unclear. Aims. The physical properties, structure, and dynamics of the bipolar planetary nebula, MyCn 18, are investigated in detail with the aim of understanding the shaping mechanism and evolutionary history of this object. Methods. VLT infrared images, VLT ISAAC infrared spectra, and long-slit optical Echelle spectra are used to investigate MyCn 18. Morpho-kinematic modelling was used to firmly constrain the structure and kinematics of the source. A timescale analysis was used to determine the kinematical age of the nebula and its main components. Results. A spectroscopic study of MyCn 18's central and offset region reveals the detailed make-up of its nebular composition. Molecular hydrogen, atomic helium, and Bracket gamma emission are detected from the central regions of MyCn 18. ISAAC spectra from a slit position along the narrow waist of the nebula demonstrate that the ionised gas resides closer to the centre of the nebula than the molecular emission. A final reconstructed 3D model of MyCn 18 was generated, which provides kinematical information on the expansion velocity of its nebular components by means of position-velocity (P-V) arrays. A kinematical age of the nebula and its components were obtained by the P-V arrays and timescale analysis. Conclusions. The structure and kinematics of MyCn 18 are better understood using an interactive 3D modelling tool called SHAPE. A dimensional and timescale analysis of MyCn 18's major components provides a possible mechanism for the nebula's asymmetry. The putative central star is somewhat offset from the geometric centre of the nebula, which is thought to be the result of a binary system. We speculate that the engulfing and destruction of an exoplanet during the asymptotic giant branch phase may have been a key event in shaping MyCn 18 and generating of its hypersonic knotty outflow.

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A dedicated echelle spectrometer for the Anglo-Australian Telescope

Cited by 74 publications

References 0 publications

A high-speed bipolar outflow from the archetypical pulsating star Mira A

A high-speed bipolar outflow from the archetypical pulsating star Mira A

Unveiling the structure of the planetary nebula M 2-48:

VLT observations of the asymmetric Etched Hourglass Nebula, MyCn 18

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