J/A+AS/139/135 The Optical Spectrum of RR Tel (Crawford+ 1999)
Line identifications and intensities for the optical spectrum of
RR Telescopii between 3180 and 9455 Å
Crawford F.L., McKenna F.C., Keenan F.P., Aller L.H., Feibelman W.A.,
Ryan S.G.
<Astron. Astrophys. Suppl. Ser. 139, 135 (1999)>
=1999A&AS..139..135C 1999A&AS..139..135C
ADC_Keywords: Stars, variable ; Novae ; Spectroscopy
Keywords: binaries: symbiotic - line: identifications -
stars: individual: RR Tel
Abstract:
The symbiotic nova RR Telescopii has been observed with the 3.9 m
telescope at the Anglo-Australian Observatory (AAO), using the
University College London Echelle Spectrograph (UCLES) in conjunction
with a Tek CCD. It displays a rich emission line spectrum, ranging in
excitation from NI to NiVIII. We present a list of 811 measured lines,
with their suggested identifications and absolute line intensities,
covering a wavelength range from 3180 to 9455 A. The absolute line
intensities have been derived by comparing the high resolution data
with a flux-calibrated low resolution spectrum taken with the
Australian National University 2.3 m telescope. All of the lines have
been successfully identified. Comparing our results with those of
previous studies indicates that the RR Tel system is advancing towards
higher degrees of ionisation.
Objects:
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RA (2000) DE Designation(s)
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20 00 20.2 -55 52 04 RR Tel
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 50 643 Line list for RR Telescopii, with absolute flux
calibrated intensities shown, for the
wavelength range 3490 - 5530Å
table3.dat 50 235 Line list for RR Telescopii, in the wavelength
range 3183 - 3488Å and 5550 - 9456Å, with
intensities flux calibrated using the HeII
recombination line ratios of Hummer and Storey
(1987MNRAS.224..801H 1987MNRAS.224..801H) and Storey and Hummer
(1995MNRAS.272...41S 1995MNRAS.272...41S)
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Byte-by-byte Description of file: table[23].dat
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Bytes Format Units Label Explanations
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1- 7 F7.2 0.1nm LambdaMea Measured wavelength
9- 11 I3 km/s DeltaV Velocity FWHM
12 A1 --- n_DeltaV [h] Note on DeltaV (2)
14- 19 F6.3 10-12mW/m2 Int Measured intensity
21- 26 F6.3 10-12mW/m2 Intc Corrected intensity (1)
27 A1 --- n_Intc [efgkl] Note on Intc (2)
29- 36 A8 --- Line Identity of line
37 A1 --- n_Line [j] Note on line (3)
38- 44 F7.2 0.1nm LambdaLab Laboratory wavelength
45 A1 --- n_LambdaLab [bcgi] Note on labLam (2)
47- 49 I3 --- Mult ? Multiplet number
50 A1 --- F [F] F: forbidden line
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Note (1): Measured intensities corrected for interstellar extinction using
E(B-V) = 0.08 (Jordan, Murset & Werner 1994A&A...283..475J 1994A&A...283..475J)
Note (2): a: Measured intensities corrected for interstellar extinction using
E(B-V)=0.08.
b: Observed in the spectrum of a gaseous nebula (see McKenna et al.,
1997ApJS..109..225M 1997ApJS..109..225M).
c: Observed in the spectrum of eta Car (see McKenna et al.,
1997ApJS..109..225M 1997ApJS..109..225M).
d: In the case where more than one identification is listed for a
given line, the first is taken to be the primary contributor to
the blend.
e: The estimated error in the line intensity is between 15 and 40%.
k: The estimated error in the line intensity is between 20 and 40%.
f: The estimated error in the line intensity is greater than 40%.
g: It is possible that there may be some OVI at 3811.36 and
3834.24Å, but with the current data this is not definite.
l: This HeII line is blended and so could not be used for calibration
using line intensity ratios.
h: There are several lines very close together here which could not be
individually resolved, and so they are given as one line.
i: These very wide features appear to be the Raman-scattered OVI lines
at 6825 and 7082 Å, as shown by Espey et al.
(1995ApJ...454L..61).
Note (3): j: The intrinsically stronger [NeV] line at 3426 is not detected, as
it falls in a region between echelle orders.
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Acknowledgements: Fergal Crawford
(End) Patricia Bauer [CDS] 29-Jul-1999