J/A+A/667/A14 Gaia-TESS transit candidates (Panahi+, 2022)
Gaia-TESS synergy: improving the identification of transit candidates.
Panahi A., Mazeh T., Zucker S., Latham D.W., Collins K.A., Rimoldini L.,
Evans D.W., Eyer L.
<Astron. Astrophys., 667, A14 (2022)>
=2022A&A...667A..14P 2022A&A...667A..14P (SIMBAD/NED BibCode)
ADC_Keywords: Binaries, eclipsing ; Optical ; Binaries, orbits
Keywords: binaries: eclipsing
Abstract:
The TESS team periodically issues a new list of transiting exoplanet
candidates based on the analysis of the accumulating light curves
obtained by the satellite. The list includes the estimated epochs,
periods, and durations of the potential transits. As the point spread
function (PSF) of TESS is relatively wide, follow-up photometric
observations at higher spatial resolution are required in order to
exclude apparent transits that are actually blended background
eclipsing binaries (BEBs).
The Gaia space mission, with its growing database of epoch photometry
and high angular resolution, enables the production of distinct light
curves for all sources included in the TESS PSF, up to the limiting
magnitude of Gaia. This paper reports the results of an ongoing
Gaia-TESS collaboration that uses the Gaia photometry to facilitate
the identification of BEB candidates and even to confirm on-target
candidates in some cases.
We inspected the Gaia photometry of the individual sources included in
the TESS PSF, searching for periodic dimming events compatible with
their ephemerides and uncertainties, as published by TESS. The
performance of the search depends mainly on the number of Gaia
measurements during transit and their precision.
Since February 2021, the collaboration has been able to confirm 126
on-target candidates and exclude 124 as BEBs. Since June 2021, when
our search methodology matured, we have been able to identify on the
order of 5% as on-target candidates and another 5% as BEBs.
This synergistic approach is combining the complementary
capabilities of two of the astronomical space missions of NASA and
ESA. It serves to optimize the process of detecting new planets by
making better use of the resources of the astronomical community.
Description:
The tables include the period and depth of the released TOIs, the
number of measurements in the Gaia light curve, N, the number of
in-transit measurements, NIT, and the derived depth of the Gaia
transit (or eclipse in case of a BEB).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 94 30 On-target confirmations in Phase I search
tablea2.dat 100 52 BEBs in Phase I search
tablea3.dat 94 96 On-target confirmations in Phase II
tablea4.dat 101 72 BEBs in Phase II
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See also:
IV/38 : TESS Input Catalog - v8.0 (TIC-8) (Stassun+, 2019)
I/355 : Gaia DR3 Part 1. Main source (Gaia Collaboration, 2022)
Byte-by-byte Description of file: tablea?.dat
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Bytes Format Units Label Explanations
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1 A1 --- Note [C] C for Transit confirmations in
binary systems
3- 4 I2 --- Seq Sequential number
6- 12 F7.2 --- TOI TOI designation
14- 23 I10 --- TIC TESS identification number
25- 35 F11.8 d Porb TESS Orbital period
37- 43 E7.2 d e_Porb TESS Orbital period error
45- 51 F7.5 d Dur TESS Transit duration
53- 59 F7.5 d e_Dur TESS Transit duration error
61- 68 F8.5 10-3 Depth TESS Transit depth (in ppt)
70- 76 F7.5 10-3 e_Depth TESS Transit depth error (in ppt)
78- 80 I3 --- N Number of measurements in Gaia light curve
82- 83 I2 --- NIT Number of in-transit measurement in
Gaia light curve
85- 88 F4.1 --- S/NT Gaia expected signal-to-noise ratio
90- 95 F6.2 10-3 DepthG Derived depth of the Gaia transit
(or eclipse in case of a BEB) (in ppt)
97-101 F5.2 10-3 e_DepthG ? Gaia transit depth error (in ppt) (1)
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Note (1): For tablea1.dat and tablea3.dat, as described in Sect. 4.2, we adopt a
uniform value of σd=6.5mmag for the Gaia transit depth uncertainty of
on-target confirmations.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 20-Feb-2023