J/A+A/534/A133 Proxima Cen chromospheric emission lines (Fuhrmeister+, 2011)
Multi-wavelength observations of Proxima Centauri.
Fuhrmeister B., Lalitha S., Poppenhaeger K., Rudolf N., Liefke C.,
Reiners A., Schmitt J.H.M.M., Ness J.-U.
<Astron. Astrophys. 534, A133 (2011)>
=2011A&A...534A.133F 2011A&A...534A.133F
ADC_Keywords: Stars, variable ; Stars, late-type ; Spectroscopy
Keywords: stars: activity - stars: magnetic fields - stars: chromospheres -
stars: coronae - stars: late-type -
stars: individual: Proxima Centauri
Abstract:
We present an extensive identification catalog of chromospheric
emission lines in the optical range for a flare on Proxima Centauri.
The data were obtained with ESO's Kueyen telescope equipped with the
UVES spectrograph on March 9/10, 11/12, 13/14 in 2009. The instrument
was operated in dichroic mode (spectral coverage from 3290 to 4500 and
from 6400 to 10080Å). We tabulate measured wavelength, line flux
and FWHM for every line and also provide the rest wavelength from the
Moore catalog which was used for identification (Moore, 1972, Nat.
Stand. Ref. Data. Ser., 40). Few lines were identified with the NIST
database.
Objects:
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RA (2000) DE Designation(s)
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14 29 42.9 -62 40 46 Proxima Centaurus = V* V645 Cen
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table6.dat 93 474 Catalogue of chromospheric emission lines
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See also:
J/A+A/415/331 : HST/STIS spectra of alpha Cen A (Pagano+, 2004)
J/A+A/459/669 : JHKs photometry around α Cen (Kervella+, 2006)
J/A+A/464/373 : VRIZJHK photometry around Alpha Cen (Kervella+, 2007)
Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 7 F7.2 0.1nm lambda1 Measured wavelength
9- 12 F4.2 0.1nm sigma Line width sigma
14- 21 E8.3 mW/m2 Flux Line flux (in erg/cm2/s) (1)
23- 33 F11.5 0.1nm lambda2 Catalogued wavelength
35- 38 A4 --- Ion Ion name
40- 43 I4 --- Mult Multiplet number
45 I1 --- q_Mult [0/2] Identification status flag (2)
47- 93 A47 --- Rem Remarks (3)
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Note (1): Absolute errors are about a factor of 2,
differential errors are much smaller
Note (2): Line identification status as follows:
0 = secure line identification
1 = unsecure line identification
(mostly due to single line out of multiplet)
2 = single line out of multiplet but secure identification, since
line was secure identified in the megaflare of CN Leo
Note (3): Abbreviations used:
em = emission line core in absorption line
NIST = line was identified using NIST
no gaussian = line is fitted poorly by a Gaussian, flux has large errors
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Acknowledgements:
Birgit Fuhrmeister, bfuhrmeister(at)hs.uni-hamburg.de
(End) Birgit Fuhrmeister [Univ. Hamburg], Patricia Vannier [CDS] 25-Aug-2011