J/ApJ/871/63 How to constrain your M dwarf. II. Nearby binaries (Mann+, 2019)
How to constrain your M dwarf.
II. The mass-luminosity-metallicity relation from 0.075 to 0.70 solar masses.
Mann A.W., Dupuy T., Kraus A.L., Gaidos E., Ansdell M., Ireland M.,
Rizzuto A.C., Hung C.-L., Dittmann J., Factor S., Feiden G., Martinez R.A.,
Ruiz-rodriguez D., Chia Thao P.
<Astrophys. J., 871, 63-63 (2019)>
=2019ApJ...871...63M 2019ApJ...871...63M (SIMBAD/NED BibCode)
ADC_Keywords: Parallaxes, trigonometric; Spectra, infrared; Stars, M-type;
Stars, dwarfs; Stars, double and multiple; Stars, masses;
Abundances, [Fe/H]
Keywords: binaries: visual; stars: late-type;
stars: low-mass stars: luminosity function, mass function
Abstract:
The mass-luminosity relation for late-type stars has long been a
critical tool for estimating stellar masses. However, there is growing
need for both a higher-precision relation and a better understanding
of systematic effects (e.g., metallicity). Here we present an
empirical relationship between MKs and M* spanning
0.075M☉<M*<0.70M☉. The relation is derived from 62
nearby binaries, whose orbits we determine using a combination of near
infra-red (Keck/NIRC2) imaging, archival adaptive optics data, and
literature astrometry. From their orbital parameters, we determine the
total mass of each system, with a precision better than 1% in the best
cases. We use these total masses, in combination with resolved Ks
magnitudes and system parallaxes, to calibrate the MKs-M*
relation. The resulting posteriors can be used to determine masses of
single stars with a precision of 2%-3%, which we confirm by testing
the relation on stars with individual dynamical masses from the
literature. The precision is limited by scatter around the best-fit
relation beyond measured M* uncertainties, perhaps driven by
intrinsic variation in the MKs-M* relation or underestimated
uncertainties in the input parallaxes. We find that the effect of
[Fe/H] on the MKs-M* relation is likely negligible for
metallicities in the solar neighborhood (0.0%±2.2% change in mass
per dex change in [Fe/H]). This weak effect is consistent with
predictions from the Dartmouth Stellar Evolution Database, but
inconsistent with those from modules for experiments in stellar
astrophysics (MESA) Isochrones and Stellar Tracks (MIST) (at
5σ). A sample of binaries with a wider range of abundances will
be required to discern the importance of metallicity in extreme
populations (e.g., in the Galactic halo or thick disk).
Description:
We obtained near infra-red (NIR) spectra for 58 of our 62 nearby
binary targets using the SpeX spectrograph on the NASA Infrared
Telescope Facility (IRTF) atop Maunakea. Observations were taken
between 2011 May and 2017 November (wavelength coverage from 0.9 to
2.5um and R∼2000).
We analyzed a mix of Adaptative Optics (AO) data from our own program
with Keck/NIRC2 and archival imaging from the Keck II Telescope, the
Canada-France-Hawaii Telescope (CFHT), the Very Large Telescope
(VLT), and the Gemini North Telescope.
As part of a long-term monitoring program with KeckII atop Maunakea,
between 2015 June and 2018 July we observed 51 of the 55 multistar
systems analyzed here. All observations were taken using the facility
AO imager NIRC2 (in K' (λc=2.124um) or narrow Kcont
(λc=2.271um) filter).
In addition to our own data, we downloaded images from the Keck
Observatory Archive (KOA), spanning 2002 March to 2015 November, all
of which were taken with the NIRC2 imager (in H- or K-band filters).
We obtained data for 34 of our targets from the Canadian Astronomy
Data Centre archive, all taken with the 3.6m Canada-France-Hawaii
Telescope (CFHT) using the Adaptive Optics Bonnette (AOB) and the KIR
infrared camera. A total of 239 data sets were included. Observations
spanned 1997 December to 2007 January. Images were taken using a range
of filters across JHK bands, but the majority used either the
narrowband Brγ or [FeII] filters.
We downloaded AO-corrected images from the European Southern
Observatory (ESO) archive taken with the Nasmyth Adaptive Optics
System Near-Infrared Imager and Spectrograph (NAOS-CONICA, or NaCo)
instrument on very large telescope (VLT). Data spanned 2002 November
to 2016 October, with about half of the 72 data sets taken from 2001
to 2005. Data covered 21 of our targets with a wide range of filters,
but the majority were taken either in broadband Ks and L or narrowband
[FeII] and Brγ filters.
We retrieved 36 data sets for eight of our targets from the Gemini
archive, all taken with the AO Near-Infrared imager (NIRI) on the
Frederick C. Gillett Gemini Telescope (Gemini North). All observations
were taken between 2004 August and 2011 February with the assistance
of the ALTtitude conjugate Adaptive optics for the InfraRed (ALTAIR).
Most observations were taken using broadband J-, H-, or K-band filters.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 104 62 Binary Sample
table2.dat 155 1142 Input astrometry and photometry
table5.dat 202 55 Orbital Parameters
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See also:
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+, 2003)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/AJ/106/773 : Mass-luminosity relation (Henry+, 1993)
J/A+A/385/87 : Speckle interferometry of nearby multiple stars (Balega+,2002)
J/A+A/398/239 : RI differential photometry of CU Cnc (Ribas, 2003)
J/ApJ/705/1416 : Volume-limited sample of M7-M9.5 dwarfs <20pc (Reiners+, 2009)
J/AJ/139/205 : 2007-2008 WIYN speckle observations of binaries (Horch+, 2010)
J/A+A/530/A138 : Geneva-Copenhagen survey re-analysis (Casagrande+, 2011)
J/AJ/141/45 : Speckle observations of HIP stars (Horch+, 2011)
J/AJ/141/157 : Speckle interferometry at USNO. XVI. (Mason+, 2011)
J/AJ/141/166 : HATNet variability survey of K and M dwarfs (Hartman+, 2011)
J/ApJ/728/48 : Multicolor eclipse data for 6 new binaries (Kraus+, 2011)
J/ApJ/748/93 : K-band spectra for 133 nearby M dwarfs (Rojas-Ayala+, 2012)
J/ApJ/750/L37 : Stellar parameters of low-mass KOIs (Muirhead+, 2012)
J/ApJ/754/44 : The AstraLux Large M-dwarf Survey (Janson+ 2012)
J/ApJS/201/19 : Hawaii Infrared Parallax Program. I. (Dupuy+, 2012)
J/A+A/556/A15 : Effective temperature scale of M dwarfs (Rajpurohit+, 2013)
J/AJ/145/52 : Abundances of K and M dwarfs in binary systems (Mann+, 2013)
J/AJ/145/102 : Spectroscopy of M dwarfs in the northern sky (Lepine+, 2013)
J/ApJ/779/188 : Spectra of nearby late K and M Kepler stars (Mann+, 2013)
J/MNRAS/429/859 : New companions to nearby low-mass stars (Jodar+, 2013)
J/AJ/147/20 : Spectroscopy of 447 nearby M dwarfs (Newton+, 2014)
J/AJ/147/94 : Solar neighborhood. XXXII. L and M dwarfs (Dieterich+, 2014)
J/ApJ/789/102 : Properties of late M-dwarfs (Janson+, 2014)
J/ApJ/791/54 : Nearby M Dwarfs parameters (Gaidos+, 2014)
J/MNRAS/443/2561 : CONCH-SHELL catalog of nearby M dwarfs (Gaidos+, 2014)
J/ApJ/800/85 : Teff, radii and luminosities of cool dwarfs (Newton+, 2015)
J/ApJ/804/64 : Empirical and model parameters of 183 M dwarfs (Mann+, 2015)
J/AJ/152/141 : Solar neighborhood. XXXVII. RVs for M dwarfs (Benedict+, 2016)
J/ApJS/225/32 : Extended abundance analysis of cool stars (Brewer+, 2016)
J/MNRAS/457/2877 : Kepler M dwarf stars revised properties (Gaidos+, 2016)
J/ApJ/836/167 : K2 planetary syst. around low-mass stars. I. (Dressing+, 2017)
J/AJ/154/224 : Transiting planets in young clusters from K2 (Rizzuto+, 2017)
J/AJ/155/114 : HAT-TR-318-007: a double-lined M dwarf binary (Hartman+, 2018)
J/AJ/155/225 : M dwarf rotational broadening measurements (Kesseli+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1 I1 --- Set [1/2] Sample code (1)
3- 12 A10 --- Name System identifier
14- 15 A2 --- m_Name Component pairing
17- 18 I2 h RAh Hour of Right Ascension (J2000)
20- 21 I2 min RAm Minute of Right Ascension (J2000)
23- 26 F4.1 s RAs Second of Right Ascension (J2000)
28 A1 --- DE- Sign of the Declination (J2000)
29- 30 I2 deg DEd Degree of Declination (J2000)
32- 33 I2 arcmin DEm Arcminute of Declination (J2000)
35- 36 I2 arcsec DEs Arcsecond of Declination (J2000)
38- 43 F6.3 mag Ksmag [3.1/13] System apparent 2MASS Ks band
magnitude (unless flagged)
45- 49 F5.3 mag e_Ksmag [0.01/0.05] Uncertainty in System Ksmag
51 A1 --- f_Ksmag [be] Flag on Ksmag (2)
53- 57 F5.3 mag DKsmag [0.001/4.3] Differential system Ks band
magnitude
59- 63 F5.3 mag e_DKsmag [0.01/0.075] Uncertainty in DKsmag
65- 71 F7.5 Msun Mass [0.14/1.6] System mass
73- 79 F7.5 Msun e_Mass [3.9e-4/0.18] Uncertainty in Mass
81- 85 F5.2 [Sun] [Fe/H] Metallicity (3)
87 A1 --- f_[Fe/H] [cd] Flag on [Fe/H] (4)
89- 95 F7.3 mas plx Parallax
97-101 F5.3 mas e_plx Uncertainty in plx
103-104 I2 --- r_plx Reference code for plx (5)
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Note (1): Set as follows :
1 = Systems analyzed in this paper
2 = Systems from Dupuy+ (2017, J/ApJS/231/15)
Note (2): Flags as follows :
b = Synthetic Ks magnitudes derived from spectra. All other Ks
magnitudes are from 2MASS.
e = Ks magnitude from 2MASS contains a third star, listed Ks
magnitude has third star's flux removed
Note (3): Errors on [Fe/H] are limited primarily by the calibration
(Mann+ 2013, J/AJ/145/52 and 2014AJ....147..160M 2014AJ....147..160M) and are 0.08dex
for all targets unless otherwise noted.
Note (4): Flags as follows :
c = Abundance derived from lower-resolution Infrared Telescope Facility
(IRTF) spectrum, e_[Fe/H] estimated to be 0.12dex.
d = L dwarfs are beyond the calibration range of Mann+ (2014AJ....147..160M 2014AJ....147..160M)
[Fe/H] values should be used with caution.
Note (5): References as follows :
1 = This work (MEarth)
2 = van Leeuwen (2007, I/311)
3 = Benedict+ (2016,J/AJ/152/141)
4 = Dupuy+ (2017, J/ApJS/231/15)
5 = van Altena+ (1995gcts.book.....V 1995gcts.book.....V)
6 = Finch+ (2016,J/AJ/151/160)
7 = Goldin & Makarov (2006ApJS..166..341G 2006ApJS..166..341G)
8 = Soderhjelm (1999, J/A+A/341/121)
9 = Bartlett+ (2017, J/AJ/154/151)
10 = Riedel+ (2010AJ....140..897R 2010AJ....140..897R)
11 = Gaia Collaboration+ (2016A&A...595A...2G 2016A&A...595A...2G)
12 = companion to star in Lindegren+ (2018A&A...616A...2L 2018A&A...616A...2L)
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name System identifier
12- 13 I2 h RAh Hour of Right Ascension (J2000)
15- 16 I2 min RAm Minute of Right Ascension (J2000)
18- 21 F4.1 s RAs Second of Right Ascension (J2000)
23 A1 --- DE- Sign of the Declination (J2000)
24- 25 I2 deg DEd Degree of Declination (J2000)
27- 28 I2 arcmin DEm Arcminute of Declination (J2000)
30- 31 I2 arcsec DEs Arcsecond of Declination (J2000)
33- 42 A10 "Y/M/D" Date UT Date of the observation (1)
44- 51 F8.3 mas Sep [35/3321] Separation (ρ)
53- 58 F6.3 mas e_Sep [0.04/80] Uncertainty in Sep
60- 66 F7.3 deg PA Position angle (θ)
68- 72 F5.3 deg e_PA [0.01/7.6] Uncertainty in PA
74- 80 A7 --- Filt Filter used in the observation
82- 87 F6.3 mag Dmag [-0.1/5.5]? Magnitude difference (Δm)
(2)
89- 93 F5.3 mag e_Dmag [0.01/0.9]? Uncertainty in Dmag
95-133 A39 --- Ref Observation reference (3)
142-155 A14 --- PI Principal investigator (4)
--------------------------------------------------------------------------------
Note (1): Dates from literature points may be off by 1 day due to inconsistency
in reporting UT versus local date.
Note (2): Errors are based on the scatter in individual images, and are
likely underestimated.
Note (3): Astrometry with source as Keck/NIRC2, CFHT/KIR, VLT/NaCo, or
Gemini/NIRI are from this paper. All other measurements list
the paper reference.
Note (4): For archive observatory (AO) data analyzed in this paper (from our
program or the archive) as it was listed in the image header.
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Byte-by-byte Description of file: table5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Name System identifier
12- 19 F8.5 yr Per [0.84/63] Orbital period
21- 27 F7.5 yr E_Per [1.4e-4/9.2] Upper uncertainty in Per
29- 35 F7.5 yr e_Per [1.4e-4/7.2] Lower uncertainty in Per
37- 43 F7.2 mas a [80/2447] Semi-major axis (α)
45- 50 F6.2 mas E_a [0.17/113] Upper uncertainty in a
52- 56 F5.2 mas e_a [0.17/84] Lower uncertainty in a
58- 64 F7.5 --- e [0.029/0.87] Eccentricity
66- 72 F7.5 --- E_e [1.3e-4/0.14]Upper uncertainty in e
74- 80 F7.5 --- e_e [1.3e-4/0.12] Lower uncertainty in e
82- 88 F7.3 deg i [12/167] Inclination
90- 94 F5.3 deg E_i [0.016/6.3] Upper uncertainty in i
96-100 F5.3 deg e_i [0.016/9.5] Lower uncertainty in i
102-108 F7.3 deg omega [1.4/350] Argument of periastron (ω)
110-116 F7.3 deg E_omega [0.02/332] Upper uncertainty in omega
118-123 F6.3 deg e_omega [0.02/60] Lower uncertainty in omega
125-131 F7.3 deg Omega [8/265] Position angle of the ascending
node (Ω)
133-138 F6.3 deg E_Omega [0.022/46] Upper uncertainty in Omega
140-146 F7.3 deg e_Omega [0.022/163] Lower uncertainty in Omega
148-155 F8.2 d MJD [51189/71033] Modified Julian Date of
periastron passage
157-164 F8.2 d E_MJD [0.23/12032] Upper uncertainty in MJD
166-172 F7.2 d e_MJD [0.23/3397] Lower uncertainty in MJD
174-182 E9.4 arcsec3/yr2 a3/P2 [2.9e-5/0.013] Semi-major axis cubed
dived by Period squared
184-192 E9.4 arcsec3/yr2 e_a3/P2 [1.3e-7/1.9e-4] Uncertainty in a3/P2
194-198 F5.1 --- chi2 [1.5/124] The χ2
200-202 I3 --- dof [3/105] Degrees of freedom
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History:
From electronic version of the journal
References:
Mann et al. Paper I. 2015ApJ...804...64M 2015ApJ...804...64M cat. J/ApJ/804/64
(End) Prepared by [AAS], Coralie Fix [CDS] 17-Feb-2020