J/ApJS/211/27 An atlas of FUV spectra of 31 Cyg (Bauer+, 2014)
An atlas of far-ultraviolet spectra of the zeta Aurigae binary 31 Cygni with
line identifications.
Bauer W.H., Bennett P.D.
<Astrophys. J. Suppl. Ser., 211, 27 (2014)>
=2014ApJS..211...27B 2014ApJS..211...27B
ADC_Keywords: Binaries, eclipsing ; Spectra, ultraviolet ; Line Profiles
Keywords: atlases; circumstellar matter; line: identification; line: profile;
stars: individual: 31 Cyg; ultraviolet: stars
Abstract:
The ζ Aurigae system 31 Cygni (K4 Ib + B4 V) was observed by the
FUSE satellite during total eclipse and at three phases during
chromospheric eclipse. We present the coadded, calibrated spectra and
atlases with line identifications. During total eclipse, emission from
high ionization states (e.g., Fe III and Cr III) shows asymmetric
profiles redshifted from the systemic velocity, while emission from
lower ionization states (e.g., Fe II and O I) appears more symmetric
and is centered closer to the systemic velocity. Absorption from
neutral and singly ionized elements is detected during chromospheric
eclipse. Late in chromospheric eclipse, absorption from the K star
wind is detected at a terminal velocity of ∼80km/s. These atlases will
be useful for interpreting the far-UV spectra of other ζ Aur
systems, as the observed FUSE spectra of 32 Cyg, KQ Pup, and VV Cep
during chromospheric eclipse resemble that of 31 Cyg.
Description:
31 Cyg was observed with The FUSE program D123 (PI: Bennett) in 2003
during total eclipse at two epochs during fairly deep chromospheric
eclipse and at one epoch at which only weak chromospheric lines were
seen. The FUSE satellite covered the wavelength range 900-1190Å.
The ultraviolet spectrum of this binary was also observed far from
eclipse with Hubble Space Telescope (HST) in 2001 and 2002.
Objects:
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RA (ICRS) DE Designation(s)
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20 13 37.91 +46 44 28.8 31 Cyg = HD 192577
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 83 7 FUSE observations of 31 Cygni
table6.dat 66 647 All absorption lines selected from Hirata and
Horaguchi (1995, Cat. VI/69)
fig5.dat 36 27801 The total eclipse atlas (spectrum in eclipse)
fig8.dat 40 83403 The chromospheric eclipse atlas (spectra at phases
0.989, 0.014 and 0.037)
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See also:
VI/129 : The FUSE Observation Log (FUSE, 1999-2007)
VI/110 : Final Merged Log of IUE Observations (NASA-ESA, 2000)
VI/69 : Atomic Spectral Line List (Hirata+ 1995)
III/86 : SKYLAB S-019 Far-UV Objective-Prism Spectrophotometry (Henize+ 1979)
J/ApJS/187/149 : StarCAT: STIS UV echelle spectra of stars (Ayres, 2010)
J/other/JAD/14.3 : Emission lines in 32 Cygni (Eaton, 2008)
J/ApJ/679/1490 : Phot. and Velocity of 3 ζ Aur binaries (Eaton+, 2008)
J/ApJS/171/249 : Ultraviolet Spectral Atlas of VV Cephei (Bauer+, 2007)
J/ApJS/119/83 : IUE sample of binaries with hot component (Parsons+, 1998)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Dataset Observation identification
10- 13 A4 --- Ap Aperture ("LWRS" (large) or "HIRS" (small))
15- 25 A11 "YYYY/MM/DD" Date UT date of observation
27- 32 F6.4 --- Phase Phase (1)
34- 37 I4 s Exp [58/3936] Exposure time
39- 83 A45 --- Comm Comment
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Note (1): Orbital phases were computed from the orbital solution of
Wright (1970VA.....12..147W 1970VA.....12..147W).
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 8 F8.3 0.1nm lambda [950.1/1187.5] Wavelength in Angstroms
10- 15 A6 --- Ion Ion Designation (1)
16- 20 F5.2 eV E0 [0/3.1] Lower energy level
21- 26 F6.2 eV E1 [10.6/15.8] Upper energy level
28- 32 F5.2 --- log(gf) [-5.9/0.8] Log of the oscillator strength
33- 37 F5.2 --- LStr [0/5.7] The "line strength" quantity (2)
38 A1 --- u_LStr Uncertainty flag on LStr (3)
40- 47 A8 --- Multi Multiplet number; if available
49- 56 A8 --- Term.0 The lower term designation
58- 66 A9 --- Term.1 The upper term designation
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Note (1): The first two spaces are for the element's letter(s). The third
space is blank. The Roman number for the ionization state begins in
the fourth space; i.e., if the element is neutral, the final two
spaces will be blank.
Note (2): The difference between the line's log(gf) and the minimum log(gf)
included for that lower level.
Note (3): The colon (:) indicates too few lines from that lower level for
the strength quantity to be useful when comparing with line strengths
from other elements or levels.
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Byte-by-byte Description of file: fig5.dat
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Bytes Format Units Label Explanations
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1- 7 F7.2 0.1nm lambda [910/1188] Wavelength in Angstroms
9- 17 E9.2 cW/m2/nm Flux Flux in erg/cm2/s/Å
19- 27 E9.2 cW/m2/nm e_Flux Error in Flux
29- 34 F6.2 cm2/ks Weight Effective area * Exposure time
36 I1 --- N Number of observations included in coadd
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Byte-by-byte Description of file: fig8.dat
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Bytes Format Units Label Explanations
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1- 5 F5.3 --- Phase [0/1] Orbital phase (1)
7- 13 F7.2 0.1nm lambda [910/1188] Wavelength in Angstroms
15- 23 E9.2 cW/m2/nm Flux Flux in erg/cm2/s/Å
25- 32 E8.2 cW/m2/nm e_Flux ?=0 Error in Flux
34- 38 F5.2 cm2/ks Weight [0/40.8]?=0 Effective area * Exposure time
40 I1 --- N [0/4] Number of observations included in coadd
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Note (1): The 0.037, 0.014 and 0.989 phases correspond to the top, middle and
bottom panels in Figure 8.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 07-May-2014