J/A+A/682/A164 Double eclipsing binaries from ZTF (Vaessen+, 2024)
A systematic search for double eclipsing binaries in
Zwicky Transient Facility data.
Vaessen T., van Roestel J.
<Astron. Astrophys. 682, A164 (2024)>
=2024A&A...682A.164V 2024A&A...682A.164V (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Optical ; Binaries, orbits
Keywords: binaries: eclipsing - binaries: close - methods: data analysis
Abstract:
Double eclipsing binaries are gravitationally bound quadruple systems
in a '2+2' configuration where both of the binaries are eclipsing.
These systems are interesting objects to better understand stellar
formation, to investigate the dynamical interaction between the two
binary systems or to study certain stages of stellar evolution, such
as common-envelope events or Type Ia Supernovae.
With this work, we aim to determine if double eclipsing binaries can
be found using ZTF data and what the difficulties are in doing so.
Secondly, we aim to significantly increase the number of known double
eclipsing systems and determine how this sample differs from samples
of double eclipsing binaries found with other telescopes. Methods. We
develop a new method to systematically search for double eclipsing
binaries in sparsely sampled light curves. For this we use
Box-Least-Squares (BLS) to search for the period of the first binary
in the system. We then remove that signal from the light curves, and
search the residual light curve again with BLS to find the second
period. We applied this method to ZTF light curves of 575 526
eclipsing binaries known in the Gaia eclipsing binary catalogue.
We report the discovery of 198 new double eclipsing binary systems.
The shortest and longest orbital periods of the newly detected systems
are 0.11 days to 323 days respectively. Conclusions. We successfully
implemented a method that systematically searches for double eclipsing
binary systems in sparsely sampled data. In total 198 new double
eclipsing binary systems have been found in 575 526 light curves
(∼0.034%). The ZTF sample typically contains more short period
binaries compared to the TESS sample, but is also able to find systems
with longer periods than what is currently known. We expect that at
least three to four times more quadruples can be found by applying
this method to all ZTF stellar light curves, by increasing the number
of data points as a result of longer observations,and by implementing
an automatic detection mechanism that replaces visual inspection.
Description:
We have systematically searched sparsely sampled ZTF data to identify
new candidates for compact double eclipsing binaries. Our sample
consists of 198 double eclipsing binaries which is presented here for
detailed follow-up by astronomers.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 90 203 Parameters of the quadruple candidates
--------------------------------------------------------------------------------
See also:
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 F13.9 deg RAdeg Right ascension (J2000.0)
15- 29 F15.11 deg DEdeg Declination (J2000.0)
31- 49 I19 --- GaiaDR3 Gaia EDR3 identifier
51- 59 F9.6 d PerA Orbital period of A component
61- 70 E10.2 --- DepthA Eclipse depth of A component
72- 81 F10.6 d PerB Orbital period of B component
83- 90 F8.6 --- DepthB Eclipse depth of B component
--------------------------------------------------------------------------------
Acknowledgements:
Thomas Vaessen, thomas_vaessen7(at)hotmail.com
(End) Patricia Vannier [CDS] 14-Dec-2023