Transit Hunt for Young and Maturing Exoplanets (THYME) VIII: a Pleiades-age association harboring two transiting planetary systems from Kepler

Adam L. Kraus; Andrew Vanderburg; Andrew W. Mann; Benjamin M. Tofflemire; Daniel M. Krolikowski; Dylan A. Owens; Elisabeth R. Newton; Jonathan L. Bush; Madyson G. Barber; Matthew J. Fields

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Transit Hunt for Young and Maturing Exoplanets (THYME) VIII: a Pleiades-age association harboring two transiting planetary systems from Kepler

Madyson G. Barber, Andrew W. Mann, Jonathan L. Bush, Benjamin M. Tofflemire, Adam L. Kraus, Daniel M. Krolikowski, Andrew Vanderburg, Matthew J. Fields

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Elisabeth R. Newton, Dylan A. Owens, Pa Chia Thao

Earth and Planetary Astrophysics · Submitted 16 Jun 2022

abstract compiled · 2026-09-23 · no language-model review

The authors' main claim We describe a young association (MELANGE-3) in the Kepler field, which harbors two transiting planetary systems (Kepler-1928 and Kepler-970).

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arXiv ID2206.08383 (version 1)

Pith IDJUQDBRYH, Pith's permanent record of this paper and its review

CitationAdam L. Kraus, Andrew Vanderburg, Andrew W. Mann, Benjamin M. Tofflemire, Daniel M. Krolikowski, Dylan A. Owens, Elisabeth R. Newton, Jonathan L. Bush, Madyson G. Barber, Matthew J. Fields, Pa Chia Thao. "Transit Hunt for Young and Maturing Exoplanets (THYME) VIII: a Pleiades-age association harboring two transiting planetary systems from Kepler." arXiv:2206.08383 (2022). https://pith.science/paper/JUQDBRYH

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What the abstract itself states, as probabilities: claims first 0.04 · states limitation 0.35 · human participants 0.01 · controlled comparison 0.05 · randomized assignment 0.01 · states quantitative result 0.99 · compares with prior results 0.57 · mentions code or data availability 0.03.

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Young planets provide a window into the early stages and evolution of planetary systems. Ideal planets for such research are in coeval associations, where the parent population can precisely determine their ages. We describe a young association (MELANGE-3) in the Kepler field, which harbors two transiting planetary systems (Kepler-1928 and Kepler-970). We identify MELANGE-3 by searching for kinematic and spatial overdensities around Kepler planet hosts with high levels of lithium. To determine the age and membership of MELANGE-3, we combine new high-resolution spectra with archival light curves, velocities, and astrometry of stars near Kepler-1928 spatially and kinematically. We use the resulting rotation sequence, lithium levels, and color-magnitude diagram of candidate members to confirm the presence of a coeval $105\pm$10 Myr population. MELANGE-3 may be part of the recently identified Theia 316 stream. For the two exoplanet systems, we revise the stellar and planetary parameters, taking into account the newly-determined age. Fitting the 4.5 yr Kepler light curves, we find that Kepler-1928 b is a $2.0\pm0.1R_\oplus$ planet on a 19.58-day orbit, while Kepler-970 b is a $2.8\pm0.2R_\oplus$ planet on a 16.73-day orbit. Kepler-1928 was previously flagged as an eclipsing binary, which we rule out using radial velocities from APOGEE and statistically validate the signal as planetary in origin. Given its overlap with the Kepler field, MELANGE-3 is valuable for studies of spot evolution on year timescales, and both planets contribute to the growing work on transiting planets in young stellar associations.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	Young planets provide a window into the early stages and evolution of planetary systems.	background 1.00	0.04	0.03	asserted 1.00
s1	Ideal planets for such research are in coeval associations, where the parent population can precisely determine their ages.	background 1.00	0.05	0.03	asserted 0.99
s2	We describe a young association (MELANGE-3) in the Kepler field, which harbors two transiting planetary systems (Kepler-1928 and Kepler-970).	contribution 0.70	0.86	0.59	asserted 1.00
s3	We identify MELANGE-3 by searching for kinematic and spatial overdensities around Kepler planet hosts with high levels of lithium.	method 0.94	0.93	0.04	asserted 1.00
s4	To determine the age and membership of MELANGE-3, we combine new high-resolution spectra with archival light curves, velocities, and astrometry of stars near Kepler-1928 spatially and kinematically.	method 0.99	0.96	0.03	asserted 0.99
s5	We use the resulting rotation sequence, lithium levels, and color-magnitude diagram of candidate members to confirm the presence of a coeval $105\pm$10 Myr population.	result 0.87	0.96	0.21	asserted 1.00
s6	MELANGE-3 may be part of the recently identified Theia 316 stream.	interpretation 0.90	0.24	0.06	hedged possibility 1.00
s7	For the two exoplanet systems, we revise the stellar and planetary parameters, taking into account the newly-determined age.	contribution 0.77	0.94	0.09	asserted 1.00
s8	Fitting the 4.5 yr Kepler light curves, we find that Kepler-1928 b is a $2.0\pm0.1R_\oplus$ planet on a 19.58-day orbit, while Kepler-970 b is a $2.8\pm0.2R_\oplus$ planet on a 16.73-day orbit.	result 1.00	0.97	0.13	asserted 1.00
s9	Kepler-1928 was previously flagged as an eclipsing binary, which we rule out using radial velocities from APOGEE and statistically validate the signal as planetary in origin.	result 0.58	0.94	0.07	asserted 1.00
s10	Given its overlap with the Kepler field, MELANGE-3 is valuable for studies of spot evolution on year timescales, and both planets contribute to the growing work on transiting planets in young stellar associations.	interpretation 0.74	0.23	0.09	asserted 0.89

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from observation or experiment 0.60.

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Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

The paper

Original abstract

Young planets provide a window into the early stages and evolution of planetary systems. Ideal planets for such research are in coeval associations, where the parent population can precisely determine their ages. We describe a young association (MELANGE-3) in the Kepler field, which harbors two transiting planetary systems (Kepler-1928 and Kepler-970). We identify MELANGE-3 by searching for kinematic and spatial overdensities around Kepler planet hosts with high levels of lithium. To determine the age and membership of MELANGE-3, we combine new high-resolution spectra with archival light curves, velocities, and astrometry of stars near Kepler-1928 spatially and kinematically. We use the resulting rotation sequence, lithium levels, and color-magnitude diagram of candidate members to confirm the presence of a coeval $105\pm$10 Myr population. MELANGE-3 may be part of the recently identified Theia 316 stream. For the two exoplanet systems, we revise the stellar and planetary parameters, taking into account the newly-determined age. Fitting the 4.5 yr Kepler light curves, we find that Kepler-1928 b is a $2.0\pm0.1R_\oplus$ planet on a 19.58-day orbit, while Kepler-970 b is a $2.8\pm0.2R_\oplus$ planet on a 16.73-day orbit. Kepler-1928 was previously flagged as an eclipsing binary, which we rule out using radial velocities from APOGEE and statistically validate the signal as planetary in origin. Given its overlap with the Kepler field, MELANGE-3 is valuable for studies of spot evolution on year timescales, and both planets contribute to the growing work on transiting planets in young stellar associations.

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4 arXiv papers cite this in 11 sentences

Each citing sentence is taken from the citing paper's LaTeX source and typed by Pith's classifier. A label appears at probability 0.8 or more (0.95 for support), a contest at 0.7 or more; the quoted words are the citing authors'. How each label was checked · JSON

Papers citing it · 5 sentences without a confident label

Uses its method or tool 3 papers

We followed the method outlined in [ref] .

HIP 33609 b: An Eccentric Brown Dwarf Transiting a V=7.3 Rapidly Rotating B-Star · Measuring 's age · 1.00
We searched for additional planets using the Notch and LoCoR pipelines (). is described in further detail in [ref] [<https://github.com/arizzuto/Notch_and_LOCoR>] and has been used widely to search for young planets in light curves from [ref] , [ref] , and [ref] .

TESS Hunt for Young and Maturing Exoplanets (THYME) X: a two-planet system in the 210 Myr MELANGE-5 Association · Identification of the transit signals · 0.99
Parameters for running are identical to those described in [ref] .

TESS Hunt for Young and Maturing Exoplanets (THYME) IX: a 27 Myr extended population of Lower-Centaurus Crux with a transiting two-planet system · Observations of association members · 0.96

Compares with it 2 papers

The exception, MELANGE-3 had a 3.5$σ$ older variability age ($≃$300 Myr) compared to the age derived from lithium and rotation [ref] .

Using the Gaia excess uncertainty as a proxy for stellar variability and age · Testing the ages of groups · 0.85
Comparison to equivalent widths from [ref] , [ref] , and [ref] suggest these uncertainties are missing a systematic error term of $≃10$mA, which we added in on top of the MC uncertainties.

TESS Hunt for Young and Maturing Exoplanets (THYME) X: a two-planet system in the 210 Myr MELANGE-5 Association · Li Equivalent Widths · 0.89

What it cites · 9 sentences without a confident label

Uses the method or tool of 3 papers

We used a mixture model, as detailed in [ref] [<https://github.com/awmann/mixtureages>], based on the method outlined in [ref] , and wrapped in the Markov-Chain Monte-Carlo sampling algorithm [ref] .

Data analysis recipes: Fitting a model to data · Isochronal age · 1.00
We used a mixture model, as detailed in [ref] [<https://github.com/awmann/mixtureages>], based on the method outlined in [ref] , and wrapped in the Markov-Chain Monte-Carlo sampling algorithm [ref] .

TESS Hunt for Young and Maturing Exoplanets (THYME) VI: an 11 Myr giant planet transiting a very low-mass star in Lower Centaurus Crux · Isochronal age · 1.00
Then, we generated a Causal Pixel Model (CPM) of the telescope systematics using the package [ref] for each individual star.

The unpopular Package: a Data-driven Approach to De-trend TESS Full Frame Image Light Curves · Stellar rotation periods · 1.00

Uses data or values from 1 paper

lcccc 0pt Properties of and Parameter Source 4cName Gaia EDR3 2052827207364859264 2101379205604338688 [ref] KOI 3876 1838 [ref] KIC 3440118 5526527 [ref] TIC 122450696 122069243 [ref] 2MASS J19214575+3831248 J19183005+4042314 [ref] 4cAstrometry $α$ 290.440629 289.625218 Gaia EDR3 $δ$. 38.523572 40.708735 Gaia EDR3 $μ_α$ (mas yr$^-1$) -4.154$±$0.010 -2.739$±$0.020 Gaia EDR3 $μ_δ$ (mas yr$^-1$) 2.269$±$0.011 1.652$±$.024 Gaia EDR3 $π$ (mas) 3.0565$±$0.0093 3.0153$±$0.0186 Gaia EDR3 4cPhotometry $G_Gaia$ (mag) 12.6054$±0.0028$ 14.7876$±$0.0029 Gaia EDR3 $BP_Gaia$ (mag) 12.9642$±0.0033$ 15.4884$±$0.0049 Gaia EDR3 $RP_Gaia$ (mag) 12.0798$±0.0041$ 13.9759$±$0.0048 Gaia EDR3 $B$ (mag) $13.375 ±0.094$ … APASS $V$ (mag) $12.655 ±0.122$ … APASS $g$' (mag) $13.038 ±0.033$ … APASS $r$' (mag) $12.456 ±0.092$ … APASS $i$' (mag) $12.323 ±0.062$ … APASS $J$ (mag) $11.456 ±0.02$ 12.980$±$0.023 2MASS $H$

The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age · Stellar mass · 1.00

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