J/ApJ/888/34 Robo-AO Kepler asteroseismic survey. II. (Schonhut-Stasik+, 2020)
Robo-AO Kepler asteroseismic survey.
II. Do stellar companions inhibit stellar oscillations?
Schonhut-Stasik J., Huber D., Baranec C., Lamman C., Salama M.,
Jensen-clem R., Duev D.A., Riddle R., Kulkarni S.R., Law N.M.
<Astrophys. J., 888, 34-34 (2020)>
=2020ApJ...888...34S 2020ApJ...888...34S (SIMBAD/NED BibCode)
ADC_Keywords: Asteroseismology; Radial velocities; Stars, double and multiple;
Photometry, infrared; Spectral types; Stars, diameters
Keywords: asteroseismology; binaries: close; instrumentation: adaptive optics
methods: data analysis; methods: observational
stars: fundamental parameters; techniques: high angular resolution
Abstract:
The Kepler Space Telescope observed over 15000 stars for asteroseismic
studies. Of these, 75% of dwarfs (and 8% of giants) were found to show
anomalous behavior, such as suppressed oscillations (low amplitude) or
no oscillations at all. The lack of solar-like oscillations may be a
consequence of multiplicity, due to physical interactions with
spectroscopic companions or due to the dilution of oscillation
amplitudes from "wide" (AO detected; visual) or spectroscopic
companions introducing contaminating flux. We present a search for
stellar companions to 327 of the Kepler asteroseismic sample, which
were expected to display solar-like oscillations. We used direct
imaging with Robo-AO, which can resolve secondary sources at ∼0.15",
and followed up detected companions with Keck AO. Directly imaged
companion systems with both separations of ≤0.5" and amplitude
dilutions >10% all have anomalous primaries, suggesting these
oscillation signals are diluted by a sufficient amount of excess flux.
We also used the high-resolution spectrometer ESPaDOnS at the
Canada-France-Hawai'i Telescope to search for spectroscopic binaries.
We find tentative evidence for a higher fraction of spectroscopic
binaries with high radial velocity scatter in anomalous systems, which
would be consistent with previous results suggesting that oscillations
are suppressed by tidal interactions in close eclipsing binaries.
Description:
We used the Robo-AO robotic laser AO system, mounted on the 2.1m
telescope at Kitt Peak, Arizona, to obtain high angular resolution
images of our full target sample (327 stars). Robo-AO observations
took place between 2016 June 7 and 2017 May 28, across 20 nights, with
140 objects observed more than once. We took all observations in the
i' filter.
We used the NIRC2 infrared camera behind the Keck II AO system to
confirm all the wide companion candidates, and obtain supplementary
near-infrared photometry. We observed the targets on 2016 September
12, 13 and 2017 July 31. We used the J, K' and PK-continuum filters
(central wavelengths 1.248um, 2.124um, and 2.2706um, respectively).
We used ESPaDOnS, a high-resolution echelle spectrograph at CFHT on
Maunakea, Hawai'i, to obtain at least two epochs of spectroscopy
between 2017 and 2018 of a subsample (34 stars). Observations had an
average resolution of R∼80000. See Section 3.3.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 68 327 Full robo-AO observation list
table4.dat 49 125 Radial velocity shifts for spectroscopic data
table5.dat 96 39 Detected companion systems
table6.dat 111 73 Individual star information for companion systems
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See also:
B/sb9 : SB9: 9th Catalogue of Spectroscopic Binary Orbits (Pourbaix+ 2004-2014)
B/wds : The Washington Visual Double Star Catalog (Mason+ 2001-2020)
V/133 : Kepler Input Catalog (Kepler Mission Team, 2009)
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/A+A/356/590 : The CORALIE survey for extrasolar planets II (Udry+, 2000)
J/A+A/450/681 : Companions to close spectroscopic binaries (Tokovinin+, 2006)
J/AJ/134/2340 : Membership of Praesepe & Coma Berenices clusters (Kraus+, 2007)
J/AJ/136/312 : 2001-2006 WIYN binary stars speckle observations (Horch+, 2008)
J/ApJS/190/1 : A survey of stellar families (Raghavan+, 2010)
J/AJ/142/112 : KIC photometric calibration (Brown+, 2011)
J/AJ/142/160 : Kepler Mission. II. Eclipsing binaries in DR2 (Slawson+, 2011)
J/A+A/552/A64 : Gaia-RVS standards (Soubiran+, 2013)
J/ApJS/215/19 : APOKASC catalog of Kepler red giants (Pinsonneault+, 2014)
J/ApJ/791/35 : 715 Kepler planet candidates host stars (Law+, 2014)
J/AJ/152/18 : Robo-AO Kepler planetary candidate survey. II. (Baranec+, 2016)
J/AJ/153/117 : KOIs companions from high-resolution imaging (Hirsch+, 2017)
J/AJ/153/25 : Near-infrared observations of 84 KOI systems (Atkinson+, 2017)
J/AJ/153/66 : Robo-AO Kepler Planetary Cand. Survey. III. (Ziegler+, 2017)
J/ApJS/229/30 : Revised properties of Q1-17 Kepler targets (Mathur+, 2017)
J/MNRAS/469/3802 : Compact bin. syst. around Kepler red giants (Colman+, 2017)
J/AJ/155/161 : Stars nearby Robo-AO Kepler planetary cand. (Ziegler+, 2018)
J/AJ/156/83 : Effect of star companions on planetary systems (Ziegler+, 2018)
J/AJ/156/259 : Robo-AO detected close binaries in Gaia DR2 (Ziegler+, 2018)
J/ApJS/236/42 : Asteroseismology of ∼16000 Kepler red giants (Yu+, 2018)
J/ApJ/866/99 : Radii of KIC stars & planets using Gaia DR2 (Berger+, 2018)
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 [1430163/12555505] Kepler input catalog ID
10- 15 A6 --- KOI Kepler Object of Interest ID, if exists
17- 22 F6.3 mag pmag [6.8/14.1] Primary magnitude in Filt
24 A1 --- Filt [iK] Filter for pmag
26- 35 A10 "Y/M/D" Date Observation date (UT)
37- 64 A28 --- Comp Companion type and details (1)
66- 68 A3 --- pcat Category for the primary star (2)
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Note (1): What type of companion the primary star has and whether it
has been observed before. Wide = AO companion; Close = Spectroscopic
companion. Acronyms in parentheses correspond to papers who have
previously observed companions to these stars, although not necessarily
the same ones --
S11 = Slawson+ 2011, J/AJ/142/160
M01 = Mason+ 2001AJ....122.3466M 2001AJ....122.3466M ; Cat. B/wds
C82 = Couteau P. 1982A&AS...48..443C 1982A&AS...48..443C
C17 = Colman+ 2017, J/MNRAS/469/3802
H08 = Horch+ 2008, J/AJ/136/312
P04 = Pourbaix+ 2004A&A...424..727P 2004A&A...424..727P ; Cat. B/sb9
Z17 = Ziegler2017.
Note (2): Category for the primary star as follows:
DA = Dwarf, Anomalous;
DO = Dwarf, Oscillating;
GA = Giant, Anomalous;
GO = Giant, Oscillating;
G14 = Gaulme et al. (2014ApJ...785....5G 2014ApJ...785....5G).
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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- 8 I8 --- KIC [1571152/11709006] Kepler input catalog ID
10- 22 F13.7 d MJD Modified Julian Date for the observation
(JD-2400000.5)
24- 30 F7.3 km/s RVel [-43.41/65.42] Radial velocity (Barycentrics)
32 I1 --- sig [0/5]? Sigma likelihood for the system to
contain a close binary star
34- 39 F6.3 --- SDev [0.007/20]? Standard deviation between
the values of RV found for each observation
41- 43 I3 --- SNR [36/128] Signal to noise ratio
for each observation
48- 49 I2 --- SNRavg [52/99]? Mean SNR for all of the observations
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 8 I8 --- KIC [1571152/11551430] Kepler input catalog ID
10- 10 I1 --- m_KIC [1/3]? For systems with more than 1 companion,
stars are numbered in order of discovery
12- 15 F4.2 arcsec Sep [0.16/3.9] Separation
17- 17 I1 --- f_Sep [2]? Flag on Sep (1)
19- 22 F4.2 arcsec e_Sep [0.01/0.08] Uncertainty in Sep
24- 24 I1 --- f_PA [1]? Separation, Position angle source flag (1)
26- 30 F5.1 deg PA ? Position angle
32- 35 F4.1 deg e_PA [1.6/12]? Uncertainty in PA
37- 40 F4.2 mag dimag [0.1/6.6]? Magnitude difference, i' band
42- 45 F4.2 mag e_dimag [0.1/0.3]? Uncertainty in dimag
47- 51 F5.3 mag dKmag [0.1/6.8] Magnitude difference, K band
53- 56 F4.2 mag e_dKmag [0.1/1.9] Uncertainty in dKmag
58- 58 I1 --- f_dKmag [3]? flag on dKmag (1)
60- 60 A1 --- f_SNRi limit flag on iSNR
61- 65 F5.2 --- SNRi [3/35.4]? i' band detection significance
(σ)
67- 71 A5 --- SpT Spectral Type
73- 77 F5.2 % AmpD-i [0.2/45.6]? Amplitude dilution, i' band
79- 83 F5.3 % e_AmpD-i [0.004/4]? Uncertainty in AmpD-i
85- 89 F5.2 % AmpD-K [0.19/47.4] Amplitude dilution, K band
91- 96 F6.2 % e_AmpD-K [0.06/136.5] Uncertainty in AmpD-K
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Note (1): Flas as follows:
1 = Stars for which separation and position angle were determined
with a PSF subtracted image.
2 = Found in Keck image, not apparent in full or PSF Robo-AO image.
3 = dKmag measured on J-band image. KIC4999260 was taken in PK-continuum.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 I8 --- KIC Kepler input catalog ID
10- 10 A1 --- m_KIC [ABCD] Companion
12- 16 F5.2 mag imag [8.3/19]? i' band magnitude
18- 21 F4.2 mag e_imag [0.1/2.1]? Uncertainty in imag
23- 27 F5.2 mag Kmag [7/17.2] K band magnitude
29- 32 F4.2 mag e_Kmag [0.1/1.8] Uncertainty in K band
34- 38 A5 --- SpT Spectral Type
40- 40 A1 --- f_SpT [G ] Spectral type value calculated from
values on Gaia DR2 Database
42- 42 A1 --- r_Rad [B* ] Radius reference source(s) (1)
44- 47 F4.1 Rsun Rad [0.4/13.2]? Radius
49- 52 F4.2 Rsun E_Rad [0.04/3.1]? Upper or
symmetric uncertainty on Rad
54- 56 F3.1 Rsun e_Rad [0.1/3.8]? Lower uncertainty on Rad
58- 58 A1 --- f_Rad [G ] Radius value calculated from
values on Gaia DR2 Database
60- 60 A1 --- r_Dist [B* ] Distance reference sources (1)
62- 65 I4 pc Dist [52/4014]? Distance
67- 72 F6.1 pc E_Dist [0.1/1778]? Upper or
symmetric uncertainty on Dist
74- 78 F5.1 pc e_Dist [0.4/902]? Lower uncertainty on Dist
80- 80 A1 --- f_Dist [G ] Distance calculated from values
on Gaia DR2 Database
82- 85 I4 au SepAU [73/6626]? Physical separation
in astronomical units
87-100 A14 --- Assoc Physical Association (2)
102-111 A10 --- r_Assoc Method used for Association (3)
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Note (1): Source references as follows:
* = Value taken from the the Kepler Stellar Properties Catalog (KSPC;
Mathur+ 2017, J/ApJS/229/30)
B = Berger+ 2018, J/ApJ/866/99
Note (2): Likelihood of star not being physically associated.
Note (3): Physical association between the two stars in a system was determined
by calculating whether their distances agree within their
uncertainties to 1σ (see Section 4.1.5).
A17 = If the distance to a star was not available in Gaia, but we had a
K'- or PK-continuum band NIRC2 observation, we used the method
described in Atkinson+ 2017AJ....153...25A 2017AJ....153...25A
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History:
From electronic version of the journal
References:
Schonhut-Stasik et al. Paper I. 2017ApJ...847...97S 2017ApJ...847...97S
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 15-Jun-2021