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J/ApJS/71/983 UV spectrum of eta Car (Viotti+ 1989)
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The ultraviolet spectrum of eta Carinae
Viotti R., Rossi L., Cassatella A., Altamore A., Baratta G.B.
<Astrophys. J. Suppl. Ser. 71, 983 (1989)>
=1989ApJS...71..983V
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ADC_Keywords: Stars, variable; Spectra, ultraviolet; Equivalent widths;
Line Profiles
Keywords: line identifications - line profiles - stars: emission-line -
stars: individual - ultraviolet: spectra
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2 69 480 Spectrum
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Byte-by-byte Description of file: table2
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Bytes Format Units Label Explanations
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1- 6 F6.1 0.1nm Obs Observed wavelength (vacuum wavelength
below 2000A=200nm)
7 A1 --- u_Obs [:?] Uncertainty flag on Obs
11 A1 --- A/E Nature of the line: A=Absorption, E=Emission
15- 18 F4.1 0.1nm W Total width (in A) of the measured feature
22- 27 F6.2 0.1nm Weq Equivalent width (in A) or integrated line
flux (in 10-15W/m2 = 10-12 erg.cm-2.s-1 not
dereddened) of the absorption or emission
feature respectively
28 A1 --- u_Weq [:?] Uncertainty flag on Weq
30- 33 F4.1 10-15W/m2 Cont Estimated level of the continuum local to the
feature (in 10-12 erg.cm-2.s-1.A-1 not
dereddened)
34 A1 --- u_Cont [:?] Uncertainty flag on Cont
37- 41 A5 --- ION Identification of the ion(s) contributing to
the feature
43- 49 F7.2 0.1nm Lab Laboratory wavelength.
50 A1 --- n_Lab [K,-] Note to Lab:
K refers to a transition listed by Kurucz
, or - indicates a second part (Lab2)
51- 56 A6 --- Lab2 Second part of the line
57 A1 --- u_Lab2 [:?] Uncertainty flag on Lab2
58- 69 A12 --- Rem Remarks (1)
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Note (1): the following abbreviations are used:
I.S. = Interstellar Line;
I.S.RED = Redshifted interstellar component;
PGYG ABS = Violet shifted absorption of a P Cygni profile;
EM PEAK = narrow emiss component;
BROAD EM = broad emiss including any emiss peak;
BLEND = blend of two or more lines;
DB/MULT = double or multiple structure of the feature;
FL = possible fluorescent line; see also notes:
Individual Notes:
1233.0-33.3 Laboratory wavelength of SI from Rossi and Panagia (1989)
1285.2-97.4 The region from 1284 to 1298 A is dominated by the
blending of the multiplets UV 1 and 2 OF Ti III. The 0.00 eV
interstellar (I.S.) narrow absorption lines are possibly present.
1300-1306 The OI triplet and the Si II 1304.37 line are strongly
blended. The emission components of the OI 1302.17 line and of the
Si II 1304.37 + OI 1304.86 blend are completely absorbed by the
P Cygni absorption of Si II 1304.37 + OI 1304.86 respectively
1388.0, 1397.0 Possible high velocity absorption component of the
Si IV doublet
1453.5 A broad absorption is also present in KQ Pup, probably a blend
of many lines. Ti II is another possible contributor
1545-1551 The several absorption features can be attributed to the two
interstellar components of CIV at 0 and +100 km/s, and to the P
Cygni absorptions of CIV and FeII 1550.26. The actual contribution
of the CIV P Cygni profiles is very uncertain
1631-1643 The whole spectral region from 1600 to 1650 A was compared
with KQ Pup in order to identify the main Fe II contributors to the
observed emission and absorption features. It turned clearly out
that the 1640.5 double peak in eta Car cannot be attributed to the
Fe II 1640.17 line alone, and that the stronger redward component
of the emission is He II 1640.43
1657 In the violet edge of the broad Fe II P Cygni absorption
1747-1753 Very strong emission of the N III intercombination multiplet.
Ni II multiplet UV 4 is a possible contributor to this feature
1785-87 FeII UV multiplet 191 with a very broad emission and two
narrow peaks corresponding to the 1785.26 and 1786.74 A transitions
while the 3rd component at 1788.00 A has no prominent emission peak
1907.0 This absorption line is not evident in the less exposed
SWP4433 image where a weak narrow emission is visible with a flux
of about 1.5x10-12 erg.cm-2.s-1. We cannot decide whether the
difference between the two spectra are instrumental effects or due
to real spectral variation of the CIII intercombination line
2227.1 The region from 2200 to 2300 A is strongly depressed by broad
and intense P Cygni absorption lines of FeII
2320-2408 Also this region is very difficult to analyze for the
crowding of the FeII lines
2506-2508 The strongest emission feature in the (not dereddened) UV
spectrum of eta Car includes a broad emission due to the blend of
the high excitation FeII lines at 2506.80, 07.59, 07.68, and 08.34.
the two narrow peaks are the fluorescent transitions at 2506.80
and 2508.34 A
2601.0 The emission component of the FeII resonance line is strongly
modified by the P Cygni absorption of MnII 2605.70. The same effect
is present in MgII 2795.52
2795.8 This line is a blend of 2 absorptions at 2795.7 A and 2796.5 A
with an equivalent width of about 0.84 and 0.30 A, respectively
corresponding to the central and red shifted I.S. lines of MgII
2843.6 The other FeI fluorescent line aT 2823.28 A is not present
3185.3 there is a gap in the spectrum from 3186 A to 3192 A. This
region includes the FeII 3186.74 line
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(End) Francois Ochsenbein [CDS] 19-Feb-1993