J/MNRAS/493/5382 Orbits for 10 new binaries with Kepler (Murphy+, 2020)
Finding binaries from phase modulation of pulsating stars with Kepler - VI.
Orbits for 10 new binaries with mischaracterized primaries.
Murphy S.J., Barbara N.H., Hey D., Bedding T.R., Fulcher B.D.
<Mon. Not. R. Astron. Soc., 493, 5382-5388 (2020)>
=2020MNRAS.493.5382M 2020MNRAS.493.5382M (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Binaries, orbits ; Stars, variable ;
Optical
Keywords: binaries: general - stars: oscillations -
stars: variables: δ Scuti - stars: variables: general
Abstract:
Measuring phase modulation in pulsating stars has proven to be a
highly successful way of finding binary systems. The class of
pulsating main-sequence A and F variables, known as δ Scuti
stars consists of particularly good targets for this, and the Kepler
sample of these has been almost fully exploited. However, some Kepler
δ Scuti stars have incorrect temperatures in stellar properties
catalogues, and were missed in previous analyses. We used an automated
pulsation classification algorithm to find 93 new δ Scuti
pulsators among tens of thousands of F-type stars, which we then
searched for phase modulation attributable to binarity. We discovered
10 new binary systems and calculated their orbital parameters, which
we compared with those of binaries previously discovered in the same
way. The results suggest that some of the new companions may be white
dwarfs.
Description:
We used a machine-learning algorithm to find δ Sct stars with
mischaracterized temperatures, manually verifying the
machine-automated shortlist of 1203 candidates to recover 960 known
and 93 new δ Sct stars. We searched these systems for binarity
using the phase-modulation method and found 10 new binaries. We also
searched for binaries among Kepler B stars with the same method, but
no new binaries could be confirmed. Since B stars are usually found in
binary or multiple systems, the low detection rate is probably because
B-type variable stars are generally not well suited to
phase-modulation analysis.
For the 10 new binaries, we determine the orbital parameters as the
medians of the marginalized posterior distributions from the MCMC
chains, which we give in Table 2.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 153 10 Orbital parameters for the PB1 systems
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See also:
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC KIC identifier
10- 17 F8.3 d P Orbital period
19- 24 F6.3 d E_P Upper error on P (1)
26- 31 F6.3 d e_P Lower error on P (1)
33- 38 F6.2 s a1sini/c Semimajor axis a1sini/c
40- 44 F5.2 s E_a1sini/c Upper error on a1sini/c (1)
46- 50 F5.2 s e_a1sini/c Lower error on a1sini/c (1)
52- 57 F6.4 --- e Eccentricity
59- 64 F6.4 --- E_e Upper error on e (1)
66- 71 F6.4 --- e_e Lower error on e (1)
73- 77 F5.3 rad varpi Argument of the periastron
79- 83 F5.3 rad E_varpi Upper error on varpi (1)
85- 89 F5.3 rad e_varpi Lower error on varpi (1)
91- 99 F9.1 d tp Time of periastron (BJD)
101- 104 F4.1 d E_tp Upper error on tp (1)
106- 109 F4.1 d e_tp Lower error on tp (1)
111- 117 F7.5 Msun fM Mass function
119- 125 F7.5 Msun E_fM Upper error on fM (1)
127- 133 F7.5 Msun e_fM Lower error on fM (1)
135- 140 F6.3 km/s K1 Radial velocity semi-amplitude (2)
142- 147 F6.3 km/s E_K1 Upper error on K1 (1)
149- 153 F5.3 km/s e_K1 Lower error on K1 (1)
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Note (1): The uncertainties are given as the upper and lower bounds that
encompass the central 68.2 per cent of the marginalized posteriors
Note (2): K1 is calculated from the other quantities and is convolved with sini
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History:
From electronic version of the journal
References:
Murphy et al., Paper I 2014MNRAS.441.2515M 2014MNRAS.441.2515M
Murphy et al., Paper IV 2016MNRAS.461.4215M 2016MNRAS.461.4215M
Murphy et al., Paper V 2018MNRAS.474.4322M 2018MNRAS.474.4322M, Cat. J/MNRAS/474/4322
(End) Ana Fiallos [CDS] 11-May-2023