J/AJ/160/131 Compilation of 289 eclipsing binaries parameters (Bellotti+, 2020)
Detecting exoplanets using eclipsing binaries as natural starshades.
Bellotti S., Zabludoff A.I., Belikov R., Guyon O., Rathi C.
<Astron. J., 160, 131-131 (2020)>
=2020AJ....160..131B 2020AJ....160..131B (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple; Photometry, UBVRIJKLMNH;
Parallaxes, trigonometric; Spectral types; Exoplanets
Keywords: Eclipsing binary stars; Exoplanets; Direct imaging
Coronagraphic imaging
Abstract:
We investigate directly imaging exoplanets around eclipsing binaries
using the eclipse as a natural tool for dimming the binary and thus
increasing the planet to star brightness contrast. At eclipse, the
binary becomes pointlike, making coronagraphy possible. We select
binaries where the planet-star contrast would be boosted by >10x
during eclipse, making it possible to detect a planet that is ≳10x
fainter or in a star system that is ∼2-3x more massive than otherwise.
Our approach will yield insights into planet occurrence rates around
binaries versus individual stars. We consider both self-luminous (SL)
and reflected light (RL) planets. In the SL case, we select binaries
whose age is young enough so that an orbiting SL planet would remain
luminous; in U Cep and AC Sct, respectively, our method is sensitive
to SL planets of ∼4.5 and ∼9 MJ with current ground- or near-future
space-based instruments and ∼1.5 and ∼6 MJ with future ground-based
observatories. In the RL case, there are three nearby (≲50 pc)
systems-V1412 Aql, RR Cae, and RT Pic-around which a Jupiter-like
planet at a planet-star separation of ≳20mas might be imaged with
future ground- and space-based coronagraphs. A Venus-like planet at
the same distance might be detectable around RR Cae and RT Pic. A
habitable Earth-like planet represents a challenge; while the
planet-star contrast at eclipse and planet flux are accessible with a
6-8m space telescope, the planet-star separation is 1/3-1/4 of the
angular separation limit of modern coronagraphy.
Description:
We compile a list of 289 eclipsing binary systems; 58 from the Catalog
of Algol Type Binary Stars (Budding+, 2004, J/A+A/417/263) and 231
from the Catalog of Eclipsing Variables
(Malkov+, 2006, J/A+A/446/785).
Along with astrometry, Gaia DR2 provides stellar luminosities.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 89 289 Eclipsing binary systems with primary minimum
depth greater than or equal to 2.5.
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
J/A+A/417/263 : Catalogue of Algol type binary stars (Budding+, 2004)
J/A+A/446/785 : Catalogue of eclipsing variables (Malkov+, 2006)
J/AN/334/860 : Catalogue of eclipsing variables. Version 2 (Avvakumova+, 2013)
J/AJ/155/177 : Obliquities of planetary & eclipsing binary systems (Dai+,2018)
J/A+A/624/A68 : 47 single-line eclips. bin. BEBOP velocities (Martin+, 2019)
J/AJ/157/174 : Transiting planets Kepler-47 circumbinary system (Orosz+, 2019)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Name General Catalog of Variable Stars designation
11- 12 I2 h RAh Hour of Right Ascension (J2000) (1)
14- 15 I2 min RAm Minute of Right Ascension (J2000) (1)
17- 23 F7.4 s RAs Second of Right Ascension (J2000) (1)
25- 25 A1 --- DE- Sign of the Declination (J2000)(1)
26- 27 I2 deg DEd Degree of Declination (J2000) (1)
29- 30 I2 arcmin DEm Arcminute of Declination (J2000) (1)
32- 37 F6.3 arcsec DEs Arcsecond of Declination (J2000) (1)
39- 43 F5.2 mag mag [6.5/20.4] Magnitude at maximum brightness
45- 49 F5.2 mag Dmag [2.4/10.8] Depth of primary minimum
51- 52 A2 --- Filt Photometric filter used to obtain the light curve
54- 54 A1 --- Ref Reference of target, maximum brightness, primary
minimum, and filter (2)
56- 56 I1 --- Flag [0/1] Discrepancy flag (3)
58- 62 F5.2 mas Par [0.08/47.2]? Parallax, Gaia DR2
64- 69 F6.2 Lsun Lbol [0.28/632]? Maximum bolometric luminosity,
Gaia DR2
71- 85 A15 --- SpT Spectral type (4)
87- 89 A3 --- Class Evolutionary class
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Note (1): Positional information from Simbad.
Note (2): References as follows
B = Budding+, 2004, J/A+A/417/263
M = Malkov+, 2006, J/A+A/446/785
Note (3): If, for a given target, the catalogs report significantly
different values of Dmag in the same photometric filter, we exclude that
target from the analysis, but we report them here for completeness. A
value of 0 (245 occurrences) and 1 (44 occurrences) for the discrepancy
flag represents consistent and discrepant Dmag values respectively.
Note (4): Spectral type from Budding+, 2004, J/A+A/417/263,
Malkov+, 2006, J/A+A/446/785, and Avvakumova+, 2013, J/AN/334/860.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Coralie Fix [CDS], 09-Nov-2020