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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
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) (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: ------------------------------------------- RA (2000) DE Designation(s) ------------------------------------------- 00 06 43.3 -07 32 15 GJ1002 = LHS 2 ------------------------------------------- File Summary:
FileName Lrecl Records Explanations
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
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 9 F9.3 0.1nm lambdaO Observed position 15- 22 F8.6 - FluxO Observed normalised flux
Byte-by-byte Description of file: sp-*.dat
Bytes Format Units Label Explanations
1- 14 F14.8 0.1nm lambdaC Computed position 21- 30 F10.8 - FluxC Computed normalised flux
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
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)
Note (1): Classification of line following Schaade (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.
Acknowledgements: Sebastian Wende, sewende(at)astro.physik.uni-goettingen.de
(End) Sebastian Wende [IAG, Germany], Patricia Vannier [CDS] 13-Aug-2010
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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