J/A+A/415/331 HST/STIS spectra of alpha Cen A (Pagano+, 2004)
HST/STIS High Resolution Echelle Spectra of alpha Centauri A (G2 V).
Pagano I., Linsky J.L., Valenti J., Duncan D.K.
<Astron. Astrophys. 415, 331 (2004)>
=2004A&A...415..331P 2004A&A...415..331P
ADC_Keywords: Stars, double and multiple ; Spectra, ultraviolet ; Line Profiles
Keywords: stars: individual (alpha Cen A) - stars: chromospheres -
Description:
This table is part of a paper is which a study of the alpha Cen A
spectrum recorded with the E140 grating by HST/STIS between 1140 and
1670Å is presented. In this spectrum the authors have identified a
total of 662 emission features of which 77 are due to blends of two or
more lines, 71 are due to unidentified transitions, and 514 are
identified as due to single emission lines.
Objects:
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RA (2000) DE Designation(s)
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14 39 36.5 -60 50 02 alpha Cen A = HD 128620
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4.dat 156 662 Line identifications, velocity shifts, FWHM,
and fluxes
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- LineID Line identification(s)
18- 25 F8.3 0.1nm LabWav ? Laboratory wavelength (1)
26 A1 --- --- [/]
27- 34 F8.3 0.1nm LabWav2 ? Laboratory wavelength when more than one ID
35 A1 --- --- [/]
36- 43 F8.3 0.1nm LabWav3 ? Laboratory wavelength when more than one ID
44 A1 --- --- [/]
47- 55 F9.4 0.1nm ObsWav Observed wavelength
57- 62 F6.4 0.1nm e_ObsWav Error on Observed wavelength
64- 67 F4.1 km/s RVshift ? Radial velocity shift (2)
69- 71 F3.1 km/s e_RVshift ? Error on velocity shift
73- 80 F8.1 mW/m2 Flux Flux at ObsWav (line 5)
82- 86 F5.1 mW/m2 e_Flux Error on flux
88- 92 F5.1 km/s FWHM ? Line full-width at half-maximum
94- 97 F4.1 km/s e_FWHM ? Error on FWHM
98- 99 A2 --- n_FWHM [UL] Note on FWHM (3)
102-156 A55 --- Notes Notes (4)
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Note (1): The laboratory wavelengths listed in table are from Sandlin et al.
(1986ApJS...61..801S 1986ApJS...61..801S), unless otherwise noted in the notes.
Note (2): Radial velocity shifts corrected for the stellar radial velocity of
-23.45 km/s, computed using the orbital parameters and ephemeris
given by Pourbaix et al. (2002A&A...386..280P 2002A&A...386..280P).
Note (3): For unresolved lines where the flag 'UL' has been used
Note (4): We use Gaussian fits to the line profiles to measure wavelengths,
FWHM, and fluxes for single or blended emission lines which do not
show central reversals.
For the lines which have interstellar absorption components or central
reversals, i.e. the most intense optically thick chromospheric lines
of C I, O I, Si II, and C II, we instead integrated the flux contained
in a suitable wavelength interval and tabulated the FWHM of the
observed profile. These lines are indicated with "CR" in the column
"Notes" .
The strongest transition region lines show broad wings, and therefore
do not have a Gaussian profile. For these lines, we list the line
centroid, the FWHM of the observed profile and the flux integrated in
a suitable wavelength interval.
Absorption features due to the interstellar medium have been measured
in a number of lines originating in transitions from the ground level.
Such lines are indicated with "ISM" in the column "Notes".
Not identified lines present also in the solar spectrum, and
classified by Sandlin et al. (1986ApJS...61..801S 1986ApJS...61..801S ) in four classes,
are listed with the name Sandlin-class number and the observed
wavelength in the Solar spectrum
Abbreviations:
CR: line with Central Reversal
ISM: presence of an absorption component due to interstellar medium
absorption
emd: the line was used to derive the differential emission measure
distribution
NB+BC: line profile can be fitted by a broad plus a narrow components.
NIST: line has been identified according to the NIST Atomic Spectra
Datbase, NIST Standard Reference Database #78
http://physics.nist.gov/cgi-bin/AtData/main_asd
e: For the laboratory wavelengths of [O IV] and [S IV] lines in the
1400Å region, see Harper (1999MNRAS.303L..41H 1999MNRAS.303L..41H).
Kelly (1982): Kelly, 1982, in Atomic and Ionic Spectrum Lines
Below 200Å, ORNL-592
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Acknowledgements: Isabella Pagano
(End) Patricia Bauer [CDS] 04-Nov-2003