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 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