J/AJ/155/114 HAT-TR-318-007: a double-lined M dwarf binary (Hartman+, 2018)
HAT-TR-318-007: a double-lined M dwarf binary with total secondary eclipses
discovered by HATNet and observed by K2.
Hartman J.D., Quinn S.N., Bakos G.A., Torres G., Kovacs G., Latham D.W.,
Noyes R.W., Shporer A., Fulton B.J., Esquerdo G.A., Everett M.E., Penev K.,
Bhatti W., Csubry Z.
<Astron. J., 155, 114 (2018)>
=2018AJ....155..114H 2018AJ....155..114H (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Stars, dwarfs ; Stars, M-type ; Photometry ;
Radial velocities ; Spectroscopy ; Stars, double and multiple ;
Equivalent widths ; Abundances ; Effective temperatures
Keywords: binaries: eclipsing - stars: fundamental parameters -
stars: individual (HAT-TR-318-007, EPIC 211432946) - stars: late-type
Abstract:
We report the discovery by the HATNet survey of HAT-TR-318-007,
a P=3.34395390±0.00000020 day period detached double-lined M dwarf
binary with total secondary eclipses. We combine radial velocity (RV)
measurements from TRES/FLWO 1.5 m and time-series photometry from HATNet,
FLWO 1.2 m, BOS 0.8 m, and NASA K2 Campaign 5, to determine the masses
and radii of the component stars: MA=0.448±0.011 M☉N,
MB=0.2721-0.0042+0.0041 M☉N,
RA=0.4548-0.0036+0.0035 R☉N, and
RB=0.2913-0.0024+0.0023 R☉N. We obtained a FIRE/Magellan
near-infrared spectrum of the primary star during a total secondary
eclipse, and we use this to obtain disentangled spectra of both components.
We determine spectral types of STA=M3.71±0.69 and STB=M5.01±0.73
and effective temperatures of Teff,A=3190±110 K and
Teff,B=3100±110 K for the primary and secondary star, respectively.
We also measure a metallicity of [Fe/H]=+0.298±0.080 for the system.
We find that the system has a small, but significant, nonzero eccentricity
of 0.0136±0.0026. The K2 light curve shows a coherent variation at
a period of 3.41315-0.00032+0.00030 days, which is slightly longer
than the orbital period, and which we demonstrate comes from the primary
star. We interpret this as the rotation period of the primary. We perform
a quantitative comparison between the Dartmouth stellar evolution models
and the seven systems, including HAT-TR-318-007, that contain M dwarfs
with 0.2 M☉N<M<0.5 M☉N, have metallicity measurements,
and have masses and radii determined to better than 5% precision.
Discrepancies between the predicted and observed masses and radii are
found for three of the systems.
Description:
HAT-TR-318-007 was initially detected as a candidate transiting planet
system by the HATNet survey (Bakos et al. 2004PASP..116..266B 2004PASP..116..266B). The
available HATNet observations data of this system are provided in Table 2.
In order to determine the atmospheric parameters for the individual
components of HAT-TR-318-007, we obtained medium-resolution NIR spectra
using the Folded-port InfraRed Echellette (FIRE) spectrograph
(Simcoe et al. 2013PASP..125..270S 2013PASP..125..270S) on the 6.5 m Magellan Baade telescope
at Las Campanas Observatory in Chile. Observations were conducted during
the last ∼4 hr before twilight on the UT nights of 2011 December 09,
10, and 11, with a total secondary eclipse occurring during the night
of 2011 December 10. We observed HAT-TR-318-007 continuously over an
83-minute period encompassing the secondary eclipse and on each of the
nights before and after the eclipse. For calibration we also observed
a number of M dwarf standard stars. The data are provided in Table 6.
Objects:
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RA (ICRS) DE Designation(s) (Period)
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08 50 32.96 +12 08 23.6 HAT-TR-318-007 = EPIC 211432946 (P=3.34395390)
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 97 90164 Time-series photometry data for HAT-TR-318-007
table4.dat 43 14 Relative radial velocities for HAT-TR-318-007
from FLWO 1.5 m/TRES
table6.dat 42 20752 Disentangled FIRE/Magellan spectra of
HAT-TR-318-007
table9.dat 107 11 Equivalent widths and inferred metallicities
from FIRE/Magellan following Terrien et al.
(2012ApJ...747L..38T 2012ApJ...747L..38T)
table10.dat 86 11 Equivalent widths and inferred spectral types
and metallicities from FIRE/Magellan following
Rojas-Ayala et al. (2012, J/ApJ/748/93)
table11.dat 37 11 Atmospheric parameters from FIRE/Magellan based
on cross-correlation with BT-Settl synthetic
templates
table12.dat 166 25 *Literature M dwarfs in eclipsing binary systems
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Note on table12.dat: Literature M dwarfs in eclipsing binary systems with masses
between 0.2 M☉N<M<0.5 M☉N, and with masses and radii
determined to better than 5% precision.
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See also:
J/AJ/141/166 : HATNet variability survey of K and M dwarfs (Hartman+, 2011)
J/ApJ/748/93 : K-band spectra for 133 nearby M dwarfs (Rojas-Ayala+, 2012)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- ID Object identifier (1)
12- 24 A13 --- Fac Facility identifier (2)
26- 27 A2 --- Filter [Kp r i] Filter used
29- 39 F11.6 d BJD [811.024/3214.432269] Barycentric Julian Date
(TDB; BJD-2454000) (3)
41- 47 F7.4 mag Rawmag [-1/15.7704]?=0 Raw magnitude in Filter (4)
49- 54 F6.4 mag e_Rawmag [0.0004/6.6063]? Error in Rawmag
56- 63 F8.5 mag Cormag [13.5346/15.4047]? Corrected magnitude in Filter
(5)
64- 71 F8.5 d T-Tc [-0.09421/0.1824]? Time from eclipse center (6)
73- 79 F7.5 --- S [0.1002/0.4297]? The S parameter (7)
81- 88 F8.5 --- D [-0.026/0.012]? The D parameter (7)
90- 97 F8.5 --- K [-0.0113/0.0212]? The K parameter (7)
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Note (1): Either "HTR318-007" to indicate that this is a measurement for
HAT-TR-318-007, or "TFA??" to indicate that this is a measurement for one
of the TFA trend vectors. The first digit in names of the form "TFA??" is
either 0, 1, or 2 to indicate if it is a trend used for the KeplerCam
observations, the BOS observations, or the K2 observations respectively. The
second digit indicates which trend vector this measurement is associated with
(1-20 for KeplerCam, 1-5 for BOS, or 1-12 for K2). For the K2 observations
these trends are the sin and cos components of a harmonic series to sixth
order with a period equal to the time-spanned by the full quarter.
Note (2): Either "kepcam" for KeplerCam observations, "bos" for BOS
observations, "K2/Campaign5" for K2, "kepcam binned" for the time-binned
out-of-eclipse KeplerCam observations, or "HAT/G???" to indicate HATNet
observations. In the latter case the last three digits in the name indicate
the HATNet field from which these observations were obtained. The K2
observations have been cleaned as described in Section 2.3.
Note (3): On the TDB system, and we have corrected the times for the
light-travel time effect as described in Appendix A.
Note (4): For KeplerCam, BOS and K2 observations of HAT-TR-318-007 this is the
measured magnitude without application of EPD or TFA. For HATNet this is the
magnitude after application of EPD and TFA run in signal-search mode. For TFA
trend measurements this is the value of the TFA vector at the specified time.
Note (5): For KeplerCam, BOS and K2 observations of HAT-TR-318-007 this is the
magnitude after application of EPD and TFA. For other observations this value
is undefined.
Note (6): This is used as an EPD term to second order for the KeplerCam and BOS
observations of HAT-TR-318-007. For other observations this value is left
undefined.
Note (7): These describe the shape of the PSF, and are provided for KeplerCam
and BOS observations of HAT-TR-318-007, for which they are used as EPD terms
to first order. Here we assume an elliptical Gaussian PSF parameterized by
the form: exp{-1/2(S(x2+y2)+D(x2-y2)+K(2xy))}, with x and y being the
distance in pixels from the PSF center.
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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- 12 F12.4 d BJD Barycentric Julian Date
13 A1 --- n_BJD [e] Note on BJD (1)
15- 20 F6.2 km/s RVA [91.86/187.85] Primary radial velocity (2)
22- 25 F4.2 km/s e_RVA [0.6/1.39] Uncertainty in RVA (3)
27- 32 F6.2 km/s RVB [62.07/220.2]? Secondary radial velocity (2)
34- 37 F4.2 km/s e_RVB [1.68/3.69]? Uncertainty in RVB (4)
39- 43 F5.3 --- C [0.343/0.792] Normalized cross-correlation peak
height
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Note (1): Note as follows:
e = This observation was obtained near eclipse. A separate velocity for the
secondary component could not be resolved from the primary velocity.
Note (2): RVs are measured relative to Barnard's star.
Note (3): Primary star RV uncertainties have been scaled by a factor of 0.81 as
determined in Section 3.2.
Note (4): Secondary star RV uncertainties have been scaled by a factor of 0.96
as determined in Section 3.2.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 9 F9.3 0.1nm Wave [8321.04/24137.6] Wavelength (Å)
11- 17 F7.5 --- PFlux [0.28879/4.03168] Primary's flux (1)
19- 25 F7.5 --- e_PFlux [0.00257/0.26515] Error in PFlux (2)
27- 34 F8.5 --- SFlux [-0.26764/1.09283] Secondary's flux (1)
36- 42 F7.5 --- e_SFlux [0.00262/0.44873] Error in SFlux (2)
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Note (1): The spectra have been flux-calibrated using observations of telluric
standards. The fluxes have units of power per wavelength, but are on an
arbitrary scale.
Note (2): Uncertainties based on photon-counting statistics for the individual
observations of HAT-TR-318-007, propagated through the spectral disentangling
procedure via a Monte Carlo simulation.
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Byte-by-byte Description of file: table9.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Target Target name
15 A1 --- m_Target [AB] Multiplicity index on Target
17 A1 --- n_Target [ab] Note on Target (G1)
19- 22 F4.2 0.1nm EW(Ca)H [0.56/3.47] Ca equivalent width in the H band
(Å)
24- 27 F4.2 0.1nm e_EW(Ca)H [0.22/0.4] Uncertainty in EW(Ca)H (Å)
29- 33 F5.3 0.1nm EW(K)H1 [0.481/2.881] K equivalent width in the H1 band
(Å)
35- 39 F5.3 0.1nm e_EW(K)H1 [0.055/0.108] Uncertainty in EW(K)H1 (Å)
41- 44 F4.2 0.1nm EW(Na)K [4.34/7.96] Na equivalent width in the K band
(Å)
46- 49 F4.2 0.1nm e_EW(Na)K [0.09/0.19] Uncertainty in EW(Na)K (Å)
51- 54 F4.2 0.1nm EW(Ca)K [1.05/5.59] Ca equivalent width in the K band
(Å)
56- 59 F4.2 0.1nm e_EW(Ca)K [0.12/0.27] Uncertainty in EW(Ca)K (Å)
61- 65 F5.3 --- H2O-H [0.727/0.944] H2O-H spectral index
67- 71 F5.3 --- e_H2O-H [0.012/0.021] Uncertainty in H2O-H
73- 77 F5.3 --- H2O-K [0.797/0.979] H2O-K spectral index
79- 83 F5.3 --- e_H2O-K [0.019/0.034] Uncertainty in H2O-K
85- 89 F5.2 [-] [Fe/H]H [-0.64/0.43] Metallicity in the H band
91- 94 F4.2 [-] e_[Fe/H]H [0.08/0.14] Uncertainty in [Fe/H]H
96-101 F6.3 [-] [Fe/H]K [-0.294/0.498] Metallicity in the K band
103-107 F5.3 [-] e_[Fe/H]K [0.016/0.036] Uncertainty in [Fe/H]K
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Byte-by-byte Description of file: table10.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Target Target name
15 A1 --- m_Target [AB] Multiplicity index on Target
17 A1 --- n_Target [ab] Note on Target (G1)
19- 22 F4.2 0.1nm EW(Na)K [3.64/8.64] Na equivalent width in the K band
(Å)
24- 27 F4.2 0.1nm e_EW(Na)K [0.36/0.7] Uncertainty in EW(Na)K (Å)
29- 32 F4.2 0.1nm EW(Ca)K [1.1/6.2] Ca equivalent width in the K band
(Å)
34- 37 F4.2 0.1nm e_EW(Ca)K [0.19/0.85] Uncertainty in EW(Ca)K (Å)
39- 43 F5.3 --- H2O-K [0.67/0.967] H2O-K spectral index
45- 49 F5.3 --- e_H2O-K [0.008/0.016] Uncertainty in H2O-K
51- 55 A5 --- SpType MK spectral type
57- 60 F4.2 --- e_SpType [0.18/0.38] Uncertainty in SpType
62- 67 F6.3 [-] [Fe/H] [-0.408/0.634] [Fe/H] metallicity
69- 73 F5.3 [-] e_[Fe/H] [0.046/0.143] Uncertainty in [Fe/H]
75- 80 F6.3 [-] [M/H] [-0.282/0.45] Overall metallicity
82- 86 F5.3 [-] e_[M/H] [0.035/0.103] Uncertainty in [M/H]
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Byte-by-byte Description of file: table11.dat
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Bytes Format Units Label Explanations
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1- 14 A14 --- Target Target name
15 A1 --- m_Target [AB] Multiplicity index on Target
17 A1 --- n_Target [ab] Note on Target (G1)
19- 22 I4 K Teff [2050/3870] Effective temperature
24- 26 I3 K e_Teff [100/110] Uncertainty in Teff
28- 32 F5.2 [-] [Fe/H] [-0.31/0.27] Metallicity
34- 37 F4.2 [-] e_[Fe/H] [0.13/0.15] Uncertainty in [Fe/H]
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Byte-by-byte Description of file: table12.dat
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Bytes Format Units Label Explanations
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1- 21 A21 --- Star Star name (1)
22 A1 --- m_Star [ABC] Multiplicity index on Star
24 A1 --- n_Star [abcdef] Note on Star (2)
26- 32 F7.5 Msun Mass [0.20255/0.499] Mass (in M☉N) (3)
34- 40 F7.5 Msun e_Mass [0.00066/0.019] Uncertainty in Mass
42- 48 F7.5 Rsun Rad [0.22623/0.5087] Radius (in R☉N) (3)
50- 56 F7.5 Rsun E_Rad [0.00059/0.013] Upper limit uncertainty in Rad
58- 64 F7.5 Rsun e_Rad [0.00059/0.013] Lower limit uncertainty in Rad
66- 69 I4 K Teff [2950/3730]? Effective temperature
71- 73 I3 K e_Teff [30/180]? Uncertainty in Teff
75- 79 F5.2 [-] [Fe/H] [-0.3/0.15]? Metallicity
81- 84 F4.2 [-] e_[Fe/H] [0.03/0.2]? Uncertainty in [Fe/H]
86-125 A40 --- Ref Reference(s)
127-166 A40 --- Bibcode Bibcode(s) of the reference(s)
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Note (1): Except where noted, stars are components of double-lined eclipsing
binary systems. We exclude stars with white dwarf binary companions; such
systems may have undergone significant mass transfer.
Note (2): Note as follows:
a = WOCS 23009B is the secondary component of a single-lined binary system
with an M=1.468±0.030 M☉N evolved primary star. This binary
system is a member of the open cluster NGC 6819. The listed [Fe/H] is the
value for the cluster;
b = PTFEB132.707+19.810 is a member of the Praesepe open cluster, and the
adopted metallicity is the value for the cluster. Note that Gillen et al.
(2017ApJ...849...11G 2017ApJ...849...11G) independently identified this as a binary, which
they label AD 3814. They measure masses of 0.3813±0.0074 M☉ and
0.2022±0.0045 M☉ and radii of 0.3610±0.0033 R☉ and
0.2256-0.0049+0.0063 R☉ for the primary and secondary stars,
respectively;
c = The metallicity of the LP 661-13 eclipsing binary system was not
determined spectroscopically, but was estimated using the absolute Ks
magnitude and the MEarth-KS broadband color following Dittmann et al.
(2016ApJ...818..153D 2016ApJ...818..153D);
d = KOI-126B and KOI-126C are components of a triply eclipsing hierarchical
triple system. The primary star has a mass of M=1.347±0.032 M☉N.
Only light from the primary star has been detected in the spectrum. The
listed [Fe/H] is the value determined spectroscopically for the primary.
The triple eclipses, together with the RVs for the primary star, enable a
determination of the masses and radii of both stars that is independent
of stellar evolution models;
e = Feiden & Chaboyer (2014A&A...571A..70F 2014A&A...571A..70F) argue that CM Dra has [Fe/H]∼0 dex
and [α/Fe]≳+0.2 dex;
f = Kepler-16B is the secondary component of a binary system with an
M=0.6897±0.0035 M☉N primary star. Light from the secondary star
has not been detected within the spectrum; however, there is a transiting
circumbinary planet whose transits around each stellar component, in
conjunction with the observed RVs for the primary star, allow a
determination of the masses and radii of both stars that is independent of
stellar evolution models. The listed [Fe/H] is the [M/H] value determined
spectroscopically for the primary.
Note (3): We adopt the nominal solar conversion constants from IAU 2015
Resolution B3 as listed in Prsa et al. (2016AJ....152...41P 2016AJ....152...41P), using the
suggested notation M☉N, R☉N for these constants.
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Global notes:
Note (G1): Note as follows:
a = Based on the combined spectrum obtained during total secondary eclipse;
b = Based on the disentangled primary and secondary spectra.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 30-Oct-2018