J/A+A/679/A116 M-star spectra FeH, CrH, and NiH line lists (Crozet+, 2023)
Correlations between laboratory line lists for FeH, CrH, and NiH and M-star
spectra collected with ESPaDOnS and SPIRou.
Crozet P., Morin J., Ross A.J., Bellotti S., Donati J.-F., Fouque P.,
Moutou C., Petit P., Carmona A., Kospal A., Adam A.G., Tokaryk D.W.
<Astron. Astrophys. 679, A116 (2023)>
=2023A&A...679A.116C 2023A&A...679A.116C (SIMBAD/NED BibCode)
ADC_Keywords: Atomic physics ; Spectroscopy ; Stars, M-type
Keywords: molecular data - stars: magnetic field - stars: atmospheres -
stars: low-mass - methods: laboratory: molecular
Abstract:
Molecular bands of metal oxides and hydrides dominate the optical and
near-infrared spectra of M dwarfs. High-resolution spectra of these
bands have immense potential for determining many properties of these
stars, such as effective temperature, surface gravity, elemental
abundances, radial velocity, or surface magnetic fields. Techniques
are being developed to do this but remain limited by the current
availability and accuracy of molecular data and spectral line lists.
This paper reports metal monohydride line lists selected from
near-infrared and visible laboratory data to show that specific bands
in several electronic transitions can be used to identify CrH, NiH,
and FeH in M stars and to determine radial velocities from Doppler
shifts. The possibility of measuring magnetic fields is also
investigated for FeH and CrH.
We used systematic cross-correlation analysis between unpolarised
spectra from a selection of M stars and state-specific laboratory line
lists. These lists were generated from a combination of existing data
and new laboratory laser-excitation spectra recorded at
Doppler-limited resolution, in zero-field conditions or in magnetic
fields up to 0.6 tesla. We show that transitions at visible
wavelengths in FeH and NiH, usually neglected in the analysis of the
spectra of M-type stars, do in fact contribute to the spectra, and we
demonstrate the influence of magnetic sensitivity on selected
transitions in CrH and FeH.
Although the new line lists focus on transitions recorded at
temperatures significantly lower than those of stellar objects, they
remain pertinent because they cover some band-head regions of high
spectral density. FeH bands can provide a useful supplement to atomic
lines for the analysis of high-resolution optical and near-infrared
spectra of M dwarfs. We demonstrate the influence of a magnetic field
on CrH signatures around 862nm.
Description:
We provide the FeH, CrH, and NiH line lists used in the paper for
cross-correlation calculations with M dwarf spectra. Each list
contains spectroscopic wavenumber (cm-1), vacuum wavelength (nm),
and -- when available -- relative line intensity.
Line lists for FeH (tables 1a, 1b, 2, 3) are selected from the
literature (see references below).
For CrH, table 4a is derived from laser-induced fluorescence
spectroscopy performed at ILM in Lyon without imposing an external
magnetic field. Tables 4b-4e are computed with Western's PGopher
program for 4 values of the magnetic field modulus in the Paschen-Back
regime (0.08 to 0.73T).
For NiH, table 5a is collated from previously published measurements
performed at ILM in Lyon (see references below). Tables 5b, 5c are
subsets of table 5a including only electronic transitions to the two
spin components of the 2Δ ground state.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1a.dat 30 2094 FeH E 4Π - X 4Δ transitions
(around 1.3µm) from NSO archival spectrum of
FeH, code 1983/01/19#2, referenced and analysed
by Balfour et al. (2004JChPh.121.7735B 2004JChPh.121.7735B).
table1b.dat 28 1613 FeH E 4Π - A 4Π transitions (around
1.6µm) from NSO archival spectrum of FeH,
code 1983/01/19#2, referenced and analysed by
Balfour et al. (2004JChPh.121.7735B 2004JChPh.121.7735B)
table2.dat 22 231 FeH e 6Π - a 6Δ transitions (around
0.53 µm) from
Goodridge et al. (1997JChPh.106.4823G 1997JChPh.106.4823G)
table3.dat 20 117 FeH g 6Φ - a 6Δ transitions
(around 0.49 µm) from
Carter & Brown (1994JChPh.101.2699C 1994JChPh.101.2699C) and
Wilson et al. (2001JChPh.115.5943W 2001JChPh.115.5943W)
table4a.dat 28 231 CrH A 6Σ - X 6Σ (0-0) transitions
(around 0.86 µm) derived from laser-induced
fluorescence spectroscopy performed at ILM in
Lyon without imposing an external magnetic field
table4b.dat 28 5726 CrH A 6Σ - X 6Σ (0-0) transitions
(around 0.86 µm) computed with the PGopher
program described in Western
(2017JQSRT.186..221W 2017JQSRT.186..221W) for a magnetic field
modulus B=0.08T
table4c.dat 28 7995 CrH A 6Σ - X 6Σ (0-0) transitions
(around 0.86 µm) computed with the PGopher
program described in Western
(2017JQSRT.186..221W 2017JQSRT.186..221W) for a magnetic field
modulus B=0.345T
table4d.dat 28 8165 CrH A 6Σ - X 6Σ (0-0) transitions
(around 0.86 µm) computed with the PGopher
program described in Western
(2017JQSRT.186..221W 2017JQSRT.186..221W) for a magnetic field
modulus B=0.453T
table4e.dat 28 8585 CrH A 6Σ - X 6Σ (0-0) transitions
(around 0.86 µm) computed with the PGopher
program described in Western
(2017JQSRT.186..221W 2017JQSRT.186..221W) for a magnetic field
modulus B=0.73T
table5a.dat 25 2167 NiH transitions in the spectral window 570-740nm
from Vallon et al. (2009ApJ...696..172V 2009ApJ...696..172V),
Ross et al. (2012MolPh.110.2019R 2012MolPh.110.2019R) and
Harker et al. (2013JMoSp.292...28H 2013JMoSp.292...28H)
table5b.dat 23 646 Subset of table 5a restricted to NiH transitions
originating from the v=0 and v=1 levels of the
X1 2Δ5/2 ground state
table5c.dat 23 576 Subset of table 5a restricted to NiH transitions
originating from the v=0 level of the
X2 2Δ3/2 state
files/* . 2 Configuration file for PGopher code and
description file for properties used to
modelisation of CrH molecule and
generation of tables 4b-4e
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table1a.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.4 cm-1 sigma Spectroscopic wavenumber (1)
11- 20 F10.5 nm lambda Vacuum wavelength
22- 30 F9.1 --- int Relative intensity (arbitrary unit)
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Note (1): estimated precision on sigma of 0.005 cm-1.
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Byte-by-byte Description of file: table1b.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.4 cm-1 sigma Spectroscopic wavenumber (1)
11- 20 F10.5 nm lambda Vacuum wavelength
22- 28 F7.5 --- int Relative intensity (arbitrary unit)
--------------------------------------------------------------------------------
Note (1): sigma estimated precision of 0.005 cm-1.
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.3 cm-1 sigma Spectroscopic wavenumber (1)
14- 22 F9.5 nm lambda Vacuum wavelength
--------------------------------------------------------------------------------
Note (1): sigma: estimated precision of 0.003 cm-1.
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.3 cm-1 sigma Spectroscopic wavenumber
12- 20 F9.5 nm lambda Vacuum wavelength (1)
--------------------------------------------------------------------------------
Note (1): sigma estimated precision of 0.006 cm-1.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4[abcde].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.3 cm-1 sigma Spectroscopic wavenumber
11- 18 E8.2 --- int Relative intensity (arbitrary unit)
20- 28 F9.5 nm lambda Vacuum wavelength (1)
--------------------------------------------------------------------------------
Note (1): sigma estimated precision of 0.003 cm-1.
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Byte-by-byte Description of file: table5a.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 9 F9.3 cm-1 sigma Spectroscopic wavenumber (1)
11- 15 F5.3 --- int Relative intensity (arbitrary unit)
17- 25 F9.5 nm lambda Vacuum wavelength
--------------------------------------------------------------------------------
Note (1): sigma estimated precision of 0.007 cm-1.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table5b.dat table5c.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
3- 11 F9.3 cm-1 sigma spectroscopic wavenumber
15- 23 F9.5 nm lambda vacuum wavelength
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Acknowledgements:
Patrick Crozet, patrick.crozet(at)univ-lyon1.fr
References:
Balfour W.J., Brown J.M. and Wallace L. 2004JChPh.121.7735B 2004JChPh.121.7735B
Carter R.T. and Brown J.M. 1994JChPh.101.2699C 1994JChPh.101.2699C
Goodridge D.M., Carter R.T., Brown J.M., Steimle T.C. 1997JChPh.106.4823G 1997JChPh.106.4823G
Harker H., Richard C., Tourasse G., Crozet P. Ross A.J. 2013JMoSp.292...28H 2013JMoSp.292...28H
Ross A.J., Crozet P., Richard C., Harker H.,
Ashworth S.H. Tokaryk D.W. 2012MolPh.110.2019R 2012MolPh.110.2019R
Vallon R., Richard C., Crozet P., Wannous G., Ross A. 2009ApJ...696..172V 2009ApJ...696..172V
Western C.M. 2017JQSRT.186..221W 2017JQSRT.186..221W
Wilson C., Cook H.M., Brown J.M. 2001JChPh.115.5943W 2001JChPh.115.5943W
(End) Patricia Vannier [CDS] 18-Oct-2023