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J/ApJS/171/249      Ultraviolet Spectral Atlas of VV Cephei       (Bauer+, 2007)

An ultraviolet spectral atlas of VV Cephei during total eclipse. Bauer W.H., Bennett P.D., Brown A. <Astrophys. J. Suppl. Ser., 171, 249-259 (2007)> =2007ApJS..171..249B
ADC_Keywords: Spectra, ultraviolet ; Atlases ; Binaries, spectroscopic Keywords: atlases - circumstellar matter - line: identification - line: profiles - stars: individual (VV Cep) - ultraviolet: stars Abstract: The first observations of the ultraviolet spectrum of the binary system VV Cep (M2Iab + B?) during total eclipse have been made with the HST. A rich emission-line spectrum is seen, with over two thousand emission features present. Shortward of 1600Å, a weak continuum presumably due to Rayleigh scattering of the hot component is present, strengthening markedly shortward of 1500Å. The continuum of the M supergiant becomes apparent longward of 2650Å. Numerous circumstellar and interstellar absorption features are also seen. We present an atlas of the spectrum from 1300-3160Å as observed near midtotality and at two epochs closer to egress, when gas surrounding the hot component has begun to emerge from eclipse and the flux on the short-wavelength edges of many emission lines has increased. This atlas has been annotated with line identifications. Circumstellar and interstellar absorption features seen out of eclipse remain in absorption during totality and are also annotated on the atlas. Well over 90% of the emission features have plausible identifications, but there are many blends. Only a few hundred features appear to be free enough from blending for useful measurement of the peak flux in the line. We present a list of these unblended features. Description: The spectrum from 1150-2155Å as been observed with the HST STIS FUV (far-ultraviolet) detector, and the spectrum from 1150-2155Å as been observed with the HST STIS NUV (near-ultraviolet) detector. These data were obtained with the medium and high-resolution modes of the STIS spectrograph. Objects: ---------------------------------------------------------- RA (2000) DE Designation(s) ---------------------------------------------------------- 21 56 39.1 +63 37 32 VV Cep = HR 8383 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table3.dat 67 5693 Emission lines selected from the database table5.dat 51 469 Unblended lines
See also: II/150A : Parameters of eclipsing binaries (Brancewicz+, 1980) J/A+A/357/225 : Mass loss of M supergiants (Josselin+, 2000) J/ApJS/143/513 : Spectral classification of close binaries. (Ginestet+, 2002) J/A+A/446/785 : Catalogue of eclipsing variables (Malkov+, 2006) Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 8 F8.3 0.1nm Wave Wavelength in Angstroms 10- 15 A6 --- Ion Ion designation (G1) 17- 20 F4.2 eV LowE Lower energy level 22- 26 F5.2 eV UpE Upper energy level 28- 32 F5.2 [-] log(gf) Log of the oscillator strength 34- 38 F5.2 --- LStr The "line strength" quantity (2) 39 A1 --- u_LStr Uncertainty flag on LStr (3) 41- 48 A8 --- Multi Multiplet number (if available) 50- 57 A8 --- LowT The lower term designation 59- 67 A9 --- UpT The upper term designation
Note (2): The difference between the line's log(gf) and the minimum log(gf) included for that upper level. If this quantity is negative, the transition was included because its log(gf) was within 1.0 of the minimum log(gf) for that upper level, and could explain a feature that would otherwise not have an identification. Note (3): the colon (:) indicates too few lines from that upper level for the strength quantity to be useful when comparing with line strengths from other elements or levels.
Byte-by-byte Description of file: table5.dat
Bytes Format Units Label Explanations
1- 8 F8.3 0.1nm Wave Wavelength in Angstroms 10 A1 --- f_Wave [b] Flag on Wave (2) 12- 17 A6 --- Ion Ion designation (G1) 19- 22 F4.2 eV LowE Lower energy level 24- 28 F5.2 eV UpE Upper energy level 30- 34 F5.2 [-] log(gf) Log of the oscillator strength 36- 43 A8 --- Multi Multiplet number (if available) 45- 49 F5.2 10-14W/m2/nm PFlux Peak flux (3) 51 A1 --- f_PFlux [c] Possible circumstellar absorption (4)
Note (2): 'b' indicates a line unblended for 100km/s on either side. Note (3): In units of 10-12erg/cm2/s/Angstrom. The continuum has not been subtracted. Note (4): 'c' indicates that the peak flux might be affected by circumstellar absorption.
Global Notes: Note (G1): The first two spaces are for the element's letter(s). The third space is blank. The Roman numeral for the ionization state begins in the fourth space; i.e, if the element is neutral, the final two spaces will be blank.
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 16-Apr-2009
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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