J/ApJ/802/L10 M dwarf SpeX NIR spectroscopy (Terrien+, 2015)
M dwarf luminosity, radius, and α-enrichment from I-band spectral
features.
Terrien R.C., Mahadevan S., Bender C.F., Deshpande R., Robertson P.
<Astrophys. J., 802, L10 (2015)>
=2015ApJ...802L..10T 2015ApJ...802L..10T
ADC_Keywords: Equivalent widths ; Abundances ; Spectra, infrared ;
Radial velocities ; Stars, M-type ; Stars, diameters
Keywords: planets and satellites: fundamental parameters; stars: abundances;
stars: activity; stars: fundamental parameters; stars: low-mass;
techniques: spectroscopic
Abstract:
Despite the ubiquity of M dwarfs and their growing importance to
studies of exoplanets, Galactic evolution, and stellar structure,
methods for precisely measuring their fundamental stellar properties
remain elusive. Existing techniques for measuring M dwarf luminosity,
mass, radius, or composition are calibrated over a limited range of
stellar parameters or require expensive observations. We find a strong
correlation between the KS-band luminosity (MK), the observed
strength of the I-band sodium doublet absorption feature, and [Fe/H]
in M dwarfs without strong Hα emission. We show that the
strength of this feature, coupled with [Fe/H] and spectral type, can
be used to derive M dwarf MK and radius without requiring parallax.
Additionally, we find promising evidence that the strengths of the
I-band sodium doublet and the nearby I-band calcium triplet may
jointly indicate α-element enrichment. The use of these I-band
features requires only moderate-resolution near-infrared spectroscopy
to provide valuable information about the potential habitability of
exoplanets around M dwarfs, and surface gravity and distance for M
dwarfs throughout the Galaxy. This technique has immediate
applicability for both target selection and candidate planet-host
system characterization for exoplanet missions such as TESS and K2.
Description:
The 342 stars used here were observed in our IRTF-SpeX M dwarf survey.
Terrien et al. (2012ApJ...747L..38T 2012ApJ...747L..38T) detailed the observations on the
NASA IRTF/SpeX spectrograph, during 2011 August and November. We also
include spectra of nine nearby M dwarfs from Mann et al. (2013,
J/ApJ/779/188). All spectra have R∼2000 and span 0.8-2.4um.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 191 351 M dwarf parameters and measurements
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See also:
I/322 : UCAC4 Catalogue (Zacharias+, 2012)
I/311 : Hipparcos, the New Reduction (van Leeuwen, 2007)
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
III/145 : Radial Velocities in the Cardinal Directions (Sandage+ 1987)
J/ApJ/804/64 : Empirical and model parameters of 183 M dwarfs (Mann+, 2015)
J/ApJ/800/85 : Teff, radii and luminosities of cool dwarf (Newton+, 2015)
J/A+A/577/A132 : Stellar parameters of early M dwarfs (Maldonado+, 2015)
J/MNRAS/443/2561 : Trumpeting M dwarfs with CONCH-SHELL (Gaidos+, 2014)
J/AJ/147/20 : Spectroscopy of 447 nearby M dwarfs (Newton+, 2014)
J/ApJ/779/188 : Spectra of nearby late K and M Kepler stars (Mann+, 2013)
J/AJ/145/102 : Spectroscopy of M dwarfs in the northern sky (Lepine+, 2013)
J/AJ/145/52 : Abundances of late K-M dwarfs in binary systems (Mann+, 2013)
J/ApJ/757/112 : Stellar diameters. II. K and M-stars (Boyajian+, 2012)
J/ApJ/748/93 : K-band spectra for 133 nearby M dwarfs (Rojas-Ayala+, 2012)
J/AJ/143/67 : SLoWPoKES. II. Wide, low-mass binaries data (Dhital+, 2012)
J/AJ/141/97 : SDSS DR7 M dwarfs (West+, 2011)
J/other/A+ARV/18.67 : Accurate masses and radii of normal stars (Torres+, 2010)
J/ApJ/691/1400 : Absolute properties of CM Dra (Morales+, 2009)
J/AJ/136/452 : Astrometric studies of GAT stars (Gatewood, 2008)
J/AJ/132/1517 : Spectroscopy of M dwarfs in Praesepe (Kafka+, 2006)
J/AJ/132/866 : New M dwarfs in solar neighborhood (Riaz+, 2006)
J/ApJS/159/141 : Spectroscopic properties of cool stars. I. (Valenti+, 2005)
J/AJ/128/426 : Subdwarfs in the SDSS (West+, 2004)
J/ApJS/150/455 : New HIP-based parallaxes for 424 faint stars (Gould+, 2004)
J/AJ/123/3356 : Palomar/MSU nearby star spectrosc. survey. III. (Gizis+, 2002)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- 2MASS 2MASS identifier (HHMMSSss+DDMMSSs; J2000)
18- 25 F8.4 deg RAdeg Right Ascension in decimal degrees (J2000)
27- 34 F8.4 deg DEdeg Declination in decimal degrees (J2000)
36- 40 I5 mas/yr pmRA [-6768/3386]? Proper motion in RA (1)
42- 46 I5 mas/yr pmDE [-4766/10327]? Proper motion in Declination (1)
48- 54 I7 m/s RVel [-118240/136846]? Radial velocity
56- 61 I6 m/s e_RVel [70/15358]? Error in RVel (1)
63- 67 A5 --- r_RVel Reference for RVel (this work if blank) (2)
69- 74 F6.2 mas plx [19/549]? Parallax
76- 81 F6.2 mas e_plx [0.3/14.1]? Error in plx
83- 86 A4 --- r_plx Reference for plx (2)
88- 92 F5.2 0.1nm EWHa [-2.3/14]? H-α equivalent width;
in angstroms (3)
94- 97 A4 --- r_EWHa Reference for EWHa (2)
99-103 F5.2 [Sun] [Fe/H] [-0.7/0.7] Metallicity
105-108 F4.2 --- SpT [0.1/8.3] NIR M spectral subtype
110-114 F5.2 0.1nm EWNa [1.5/8.7] NaI 820nm equivalent width;
in angstroms (4)
116-119 F4.2 0.1nm e_EWNa [0.01/0.5] Error in EWNa
121-125 F5.2 0.1nm EWCa [-2.6/5.7] CaII 860nm equivalent width;
in angstroms (4)
127-130 F4.2 0.1nm e_EWCa [0.02/0.6] Error in EWCa
132-136 F5.3 Rsun R [0.1/0.7]? Boyaijian et al. 2012, J/ApJ/757/112,
interferometric radius
138-142 F5.3 Rsun e_R [0.001/0.03]? Error in R
144-148 F5.3 Rsun RK [0.1/0.7]? Predicted radius from K magnitude (5)
150-154 F5.3 Rsun e_RK [0.002/0.05]? Error in RKmag
156-160 F5.3 Rsun RNa [0.1/0.7]? Predicted radius from NaI equivalent
width (6)
162-166 F5.3 Rsun e_RNa [0.01/0.04]? Error in RNa
168-172 F5.2 [Sun] [a/Fe] [-0.09/0.4]? [α/Fe], α-element
abundance relative to iron
175-178 F4.2 [Sun] e_[a/Fe] [0.03]? Error in [a/Fe]
180-190 A11 --- r_[a/Fe] Reference(s) for [a/Fe] (2)
191 A1 --- sp [y] Flag if spectrum is from Mann et al. 2013,
J/ApJ/779/188
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Note (1): The e_Rvel for 00182549+4401376 and the pmRA and pmDE
for 22464232+1210214 are NaN and thus left blank.
Proper motions are compiled from Zacharias et al. 2013, I/322
Note (2): Reference as follows:
G02 = Gizis et al. (2002, J/AJ/123/3356);
G14 = Gaidos et al. (2014, J/MNRAS/443/2561);
R06 = Riaz et al. (2006, J/AJ/132/866)
D14 = Dittmann et al. (2014ApJ...784..156D 2014ApJ...784..156D);
A95 = van Altena et al. (1995, I/238);
L07 = van Leeuwen (2007, I/311);
G04 = Gould & Chaname (2004, J/ApJS/150/455);
AE12 = Anglada-Escude et al. (2012ApJ...746...37A 2012ApJ...746...37A);
G08 = Gatewood (2008, J/AJ/136/452);
vB11 = von Braun et al. (2011ApJ...729L..26V 2011ApJ...729L..26V);
REC = RECONS (www.recons.org);
N14 = Newton et al. (2014, J/AJ/147/20);
C12 = Chubak et al. (2012arXiv1207.6212C 2012arXiv1207.6212C);
CL09 = Chavez & Lambert (2009ApJ...699.1906C 2009ApJ...699.1906C);
WW05 = Woolf & Wallerstein (2005MNRAS.356..963W 2005MNRAS.356..963W);
VF05 = Valenti & Fischer (2005, J/ApJS/159/141).
M09 = Morales et al. (2009, J/ApJ/691/1400)
K10 = Khrutskaya et al. (2010AstL...36..576K 2010AstL...36..576K)
L13 = Lepine et al. 2013 (J/AJ/145/102)
Note (3): Positive = emission line.
Note (4): Negative = emission line.
Note (5): Interpolated at parallax-based MK and 5Gyr age
in Dartmouth model grid.
Note (6): Interpolated at predicted MK (see Section 3.1)
in Dartmouth model grid.
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History:
From electronic version of the journal
(End) Greg Schwarz [AAS], Emmanuelle Perret [CDS] 27-Jul-2015