J/A+A/523/A58 PDF Atlas and spectra of FeH molecule in LHS 2 (Wende+, 2010)
CRIRES spectroscopy and empirical line-by-line identification of FeH molecular
absorption in an M dwarf.
Wende S., Reiners A., Seifahrt A., Bernath P.F.
<Astron. Astrophys. 523, A58 (2010)>
=2010A&A...523A..58W 2010A&A...523A..58W
ADC_Keywords: Line Profiles ; Spectra, infrared; Spectroscopy ;
Stars, late-type ; Stars, M-type
Keywords: molecular data - line: identification - line: profiles -
stars: low-mass
Abstract:
We present an atlas for the iron-hydride molecule (FeH) in the z-range
(990nm to 1076.6nm).
We used high-resolution CRIRES spectra of the M-dwarf GJ1002, which is
an ideal target for the investigation of FeH, because it is only very
slow rotating (<3km/s) and exhibits only weak magnetic fields. The
identified lines stem mainly from the (0-0) and (1-1) vibronic
transitions, but also from the (1-0), (2-1), (2-2), (3-2), and (4-3)
transitions. For the confirmation of the identifications, we used
means of statistic and cross-correlation as well as the line
intensities. We corrected the theoretical positions if needed and
scaled the line intensities till they match the observations.
Description:
In the pdf atlas (fehatlas.pdf), the identified FeH lines, were
assigned with their molecular quantum numbers, which are in detail:
lower and upper vibrational state, branch, lower rotational state,
lower and upper omega, and the fraction to a possible blend. The
latter one is unity if the line is not blended. In the atlas, we
plotted the CRIRES spectrum of GJ1002 together with two computed
spectra for an M dwarf model with logg=5.0, Teff=3100K and solar
composition. One of the synthetic spectra is computed using the
original Einstein A values provided by Dulick et al.
(2003ApJ...594..651D 2003ApJ...594..651D) (red), the other one is computed with scaled
Einstein A values (green). For both computed spectra, the line
positions were adjusted. We also provide the spectra of GJ1002
(table2.dat), unscaled computations (table3.dat), and scaled
computations (table4.dat). All spectra are normalized to unity.
Objects:
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RA (2000) DE Designation(s)
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00 06 43.3 -07 32 15 GJ1002 = LHS 2
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 22 23000 GJ1002 CRIRES spectrum
sp-orig.dat 30 84263 Synthetic spectrum with original Einstein A
sp-scal.dat 30 84421 Synthetic spectrum with scaled Einstein A
table4.dat 126 1190 FeH line data
fehatlas.pdf 512 36531 pdf containing the plotted and labelled spectra
of observation and computation
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 F9.3 0.1nm lambdaO Observed position
15- 22 F8.6 - FluxO Observed normalised flux
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Byte-by-byte Description of file: sp-*.dat
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Bytes Format Units Label Explanations
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1- 14 F14.8 0.1nm lambdaC Computed position
21- 30 F10.8 - FluxC Computed normalised flux
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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- 10 F10.4 0.1nm lambdaO Observed position (vacuum wavelength)
13- 22 F10.4 0.1nm lambdaT Theoretical position (vacuum wavelength)
25 I1 --- vl Lower vibrational state
28 I1 --- vu Upper vibrational state
33- 35 F3.1 --- Omegal Lower Ω
40- 42 F3.1 --- Omegau Upper Ω
46- 49 F4.1 --- Jl Lower rotational state
53- 56 F4.1 --- Ju Upper rotational state
59 I1 --- B [1/3] Branch: 1=P-branch, 2=Q-branch, 3=R-branch
64- 72 F9.2 s-1 A Einstein A value
74- 81 F8.4 --- sA Scaling factor for A
84- 88 F5.3 eV El Lower level energy
91- 97 F7.4 0.1nm Dlambda Position correction
100-104 F5.3 --- Blend Blend fraction
107-108 A2 --- Cl Classification of the line (1)
110-126 A17 --- Comment Comment, if the line is blended by and atomic
feature, or if the classification of the line
did not agree with the scaling factor of the
Einstein A values (class ≠ sA)
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Note (1): Classification of line following Schaade (1964BAN....17..311S 1964BAN....17..311S):
P = the line is present, and its width agrees well with the straight
line of the diagram.
Pb = the line is present, but its width is too large, i.e. lies above
the straight line of the diagram. This could imply that the line
is blended by an other element (or that its computed line strength
is too small).
R = the line strength is presumably reduced by perturbations.
That means, that the computed line strength is too large,
and the data point lies below the line.
Q = we identified the line, but we can't verify its identification,
because we only investigate lines with ΔΩ=0 in plot.
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Acknowledgements:
Sebastian Wende, sewende(at)astro.physik.uni-goettingen.de
(End) Sebastian Wende [IAG, Germany], Patricia Vannier [CDS] 13-Aug-2010