adsabs/AstroCLIMB huggingface dataset:
Paper: Substellar Hyades Candidates from the UKIRT Hemisphere Survey
Authors: Adam C. Schneider, Frederick J. Vrba, Jeffrey A. Munn, Scott E. Dahm, Justice Bruursema, Stephen J. Williams, Bryan N. Dorland, Jacqueline K. Faherty, Austin Rothermich, Emily Calamari, Michael C. Cushing, Dan Caselden, Martin Kabatnik, William Pendrill, Arttu Sainio, Nikolaj Stevnbak Andersen, Christopher Tanner
Figure caption: Right ascension vs. distance for the new substellar Hyades candidates in this work (red diamonds), recovered substellar Hyades members from our search (blue circles), and other suggested Hyades L and T members (yellow squares) compared to the 713 Hyades members within a 30 pc radius from the cluster center from the GCNS (Smart & Sarro et al. 2021b). The normalized histograms on the right show the 713 Hyades members from Smart & Sarro et al. (2021b) in gray, and the combined sample of all substellar candidates in green. The median values of each sample are marked with dashed lines.
Paper: Substellar Hyades Candidates from the UKIRT Hemisphere Survey
Authors: Adam C. Schneider, Frederick J. Vrba, Jeffrey A. Munn, Scott E. Dahm, Justice Bruursema, Stephen J. Williams, Bryan N. Dorland, Jacqueline K. Faherty, Austin Rothermich, Emily Calamari, Michael C. Cushing, Dan Caselden, Martin Kabatnik, William Pendrill, Arttu Sainio, Nikolaj Stevnbak Andersen, Christopher Tanner
Figure caption: The J2000 positions and proper motion vectors of our substellar Hyades candidates (red) and known, recovered L- and T-type members of the Hyades (blue) compared to all known Hyades members within the halo radius (18 pc) from the GCNS (Smart & Sarro et al. 2021b).
Paper: Hitting a New Low: The Unique 28 hr Cessation of Accretion in the TESS Light Curve of YY Dra (DO Dra)
Authors: Katherine L. Hill, Colin Littlefield, Peter Garnavich, Simone Scaringi, Paula Szkody, Paul A. Mason, Mark R. Kennedy, Aarran W. Shaw, Ava E. Covington
Figure caption: YY Dra light curves from ASAS-SN, ZTF, and DASCH. Top: overlaid ASAS-SN (blue circles) and ZTF (green triangles) light curves with including a deep low state observed by TESS shown in the cyan shaded region. The ASAS-SN light curve is relatively uniform for the first few years. However, multiple intermittent low states begin to appear around 2018–2019. The observed low states reach a consistent minimum magnitude. Bottom left: the DASCH light curve, with detections shown as circles and nondetections as dashes. As explained in the text, nondetections with limits brighter than magnitude 15 have been excluded. The quiescent magnitude is comparable to that observed by ZTF. While there are numerous outbursts throughout the observational period, no low states comparable to those in the ASAS-SN and ZTF data are present. Bottom right: enlargement of the ZTF observations obtained during the TESS light curve. The faintest datum (g = 17.37 ± 0.12) was obtained during the deep low state, when accretion was negligible.
Paper: Hitting a New Low: The Unique 28 hr Cessation of Accretion in the TESS Light Curve of YY Dra (DO Dra)
Authors: Katherine L. Hill, Colin Littlefield, Peter Garnavich, Simone Scaringi, Paula Szkody, Paul A. Mason, Mark R. Kennedy, Aarran W. Shaw, Ava E. Covington
Figure caption: Zoomed section of both a high and low state in YY Dra’s TESS light curve. Top: 2 day portion in the TESS light curve during the slow brightening at the beginning of the observation. This is representative of the first three weeks of the TESS light curve. Middle: 1.2 day deep low state during which accretion ceased. During this low state, the only periodic variability is from ellipsoidal variations. Bottom: YY Dra’s orbital light curve during the deep low state between BTJD = 1888–1889, phased according to Equation (1). The red stars represent bins with a width of 0.085. The data are repeated for clarity.
Paper: Hitting a New Low: The Unique 28 hr Cessation of Accretion in the TESS Light Curve of YY Dra (DO Dra)
Authors: Katherine L. Hill, Colin Littlefield, Peter Garnavich, Simone Scaringi, Paula Szkody, Paul A. Mason, Mark R. Kennedy, Aarran W. Shaw, Ava E. Covington
Figure caption: Top panel: TESS light curve of YY Dra, showing the SAP flux from the mission’s pipeline. The deep low state described in the text is apparent at BTJD = 1888. Bottom three panels: slices of YY Dra’s two-dimensional power spectrum near frequencies of interest, following the subtraction of a smoothed version of the light curve to suppress red noise. All periodic variation ceases during the deep low state except for the 2Ω signal, which we attribute to ellipsoidal variations by the donor star. The same intensity color map is used for all three panels.
Paper: Hitting a New Low: The Unique 28 hr Cessation of Accretion in the TESS Light Curve of YY Dra (DO Dra)
Authors: Katherine L. Hill, Colin Littlefield, Peter Garnavich, Simone Scaringi, Paula Szkody, Paul A. Mason, Mark R. Kennedy, Aarran W. Shaw, Ava E. Covington
Figure caption: Top: YY Dra’s power spectrum of the entire TESS light curve, with very clear Ω, 2Ω, ω-Ω, 2(ω-Ω), and 2ω frequencies. The spin frequency ω was below the noise level, but its expected position is labeled in red. The comparatively high intensity of ω-Ω and its harmonics relative to ω and 2ω is characteristic of stream-fed accretion in the Ferrario & Wickramasinghe (1999) models. Bottom: power spectrum during the 28 hr low state shown in Figure 2. The only remaining periodic variation occurs at 2Ω and is attributable to ellipsoidal variations.
Paper: WASP-35 and HAT-P-30/WASP-51: Reanalysis using TESS and Ground-based Transit Photometry
Authors: Lu Bai, Shenghong Gu, Xiaobin Wang, Leilei Sun, Chi-Tai Kwok, Ho-Keung Hui
Figure caption: Transit light curves of HAT-P-30 observed by TESS in Sector 7. The top row shows the raw light curves with the best-fitting transit + noise model, the middle row shows the detrended light curves with the best-fitting transit model, and the bottom row shows the corresponding residuals. Vertical shifts are added for visualization.
Paper: WASP-35 and HAT-P-30/WASP-51: Reanalysis using TESS and Ground-based Transit Photometry
Authors: Lu Bai, Shenghong Gu, Xiaobin Wang, Leilei Sun, Chi-Tai Kwok, Ho-Keung Hui
Figure caption: Transit light curves of WASP-35 observed by TESS in Sector 5. The top row shows the raw light curves with the best-fitting transit + noise model, the middle row shows the detrended light curves with the best-fitting transit model, and the bottom row shows the corresponding residuals. Vertical shifts are added for visualization.
Paper: WASP-35 and HAT-P-30/WASP-51: Reanalysis using TESS and Ground-based Transit Photometry
Authors: Lu Bai, Shenghong Gu, Xiaobin Wang, Leilei Sun, Chi-Tai Kwok, Ho-Keung Hui
Figure caption: The transit light curves of WASP-35 (left panel) and HAT-P-30 (right panel) observed using YO-1 m. The top row shows the raw light curves with the best-fitting transit + noise model, the middle row shows the light curves without the noise with the best-fitting transit model, and the bottom row shows the corresponding residuals.
Paper: WASP-35 and HAT-P-30/WASP-51: Reanalysis using TESS and Ground-based Transit Photometry
Authors: Lu Bai, Shenghong Gu, Xiaobin Wang, Leilei Sun, Chi-Tai Kwok, Ho-Keung Hui
Figure caption: The transit light curves of HAT-P-30 observed using FLWO-1.2 m. The top row shows raw light curves with the best-fitting transit + noise model, the middle row shows light curves without the noise with the best-fitting transit model, and the bottom row shows the corresponding residuals.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: Distributions of ﹩{\tilde{{ \mathcal H }}}_{\mathrm{col}}﹩, ﹩{\tilde{{ \mathcal H }}}_{a}﹩, ﹩{\tilde{{ \mathcal H }}}_{\mathrm{qs}}﹩, ﹩{\tilde{{ \mathcal H }}}_{\mathrm{hs}}﹩, and ﹩{\tilde{{ \mathcal H }}}_{\mathrm{tp}}﹩ lines with different i  m .
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption:                       ﹩\tilde{{ \mathcal H }}﹩ isosurface structure of the Sun–EMB CRTBP with i  m  = 20° in the torus space: (a) TP and QS surfaces, (b) TS surface, and (c) ﹩\tilde{{ \mathcal H }}﹩ isosurfaces and collision curves, which are denoted by black lines.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: Comparisons of 2020 XL5 and 3362 Khufu: (top) a curve, (middle) φ curve, and (bottom) c  k  distribution.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: (a) Distributions of e  r , ω  r , and φ with different i  m , and (b) frequency distribution histogram of i  m , where the 5th, 50th, and 95th percentiles of i  m  are indicated as black dashed lines.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: Distributions of (a) ﹩{\tilde{{ \mathcal H }}}_{o}﹩ and (b) ﹩\cos \varphi ﹩ values of the 221 potential ECOs, where the solid line corresponds to the L 4 and L 5 axial orbits, ⊕ : ﹩{{\mathscr{U}}}_{* }﹩, +: ﹩{{\mathscr{U}}}_{l}-{{\mathscr{U}}}_{* }﹩, ⊙ : ﹩{{\mathscr{U}}}_{c}-{{\mathscr{U}}}_{* }﹩, ▴: ﹩{{\mathscr{U}}}_{b}﹩, and •: ﹩{{\mathscr{U}}}_{a}-\left({{\mathscr{U}}}_{c}\cup {{\mathscr{U}}}_{l}\cup {{\mathscr{U}}}_{b}\right)﹩.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: Distributions of ﹩{\tilde{{ \mathcal H }}}_{p}﹩ values of the 221 potential ECOs, where definitions of the colored regions are identical to those in Figure 4.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption:                       ﹩\tilde{{ \mathcal H }}﹩ isosurface structure and collision curves of the Sun–EMB CRTBP with i  m  = 40°.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption:                    ﹩\tilde{{ \mathcal H }}﹩ values with i  m  = 20° and different φ and a 0 values in the Sun–EMB CRTBP, where the different colors of lines denote the different φ from 10° to 180°.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: Frequency distribution histograms of ﹩{\tilde{{ \mathcal H }}}_{o}﹩ and ﹩{\tilde{{ \mathcal H }}}_{p}﹩ of the 221 potential ECOs, where the percentiles of ﹩{\tilde{{ \mathcal H }}}_{o}﹩ and ﹩{\tilde{{ \mathcal H }}}_{p}﹩ are indicated by black and red dashed lines, respectively.
Paper: Stability Analysis of Earth Co-orbital Objects
Authors: Yi Qi, Dong Qiao
Figure caption: Schematic of the torus space.
Paper: L-band Integral Field Spectroscopy of the HR 8799 Planetary System
Authors: David S. Doelman, Jordan M. Stone, Zackery W. Briesemeister, Andrew J. I. Skemer, Travis Barman, Laci S. Brock, Philip M. Hinz, Alexander Bohn, Matthew Kenworthy, Sebastiaan Y. Haffert, Frans Snik, Steve Ertel, Jarron M. Leisenring, Charles E. Woodward, Michael F. Skrutskie
Figure caption: Left: background-subtracted PSF at 3.55 μm, using 10 PCA components of the 99 background frames. Residual structures indicate the presence of a ghost, some speckles, and a horizontal periodic structure. Right: same as left, but clipped at 2σ inside the area of a mask, indicated by the white lines in the left-hand image.
Paper: L-band Integral Field Spectroscopy of the HR 8799 Planetary System
Authors: David S. Doelman, Jordan M. Stone, Zackery W. Briesemeister, Andrew J. I. Skemer, Travis Barman, Laci S. Brock, Philip M. Hinz, Alexander Bohn, Matthew Kenworthy, Sebastiaan Y. Haffert, Frans Snik, Steve Ertel, Jarron M. Leisenring, Charles E. Woodward, Michael F. Skrutskie
Figure caption: Flowchart of the data reduction method.
Paper: L-band Integral Field Spectroscopy of the HR 8799 Planetary System
Authors: David S. Doelman, Jordan M. Stone, Zackery W. Briesemeister, Andrew J. I. Skemer, Travis Barman, Laci S. Brock, Philip M. Hinz, Alexander Bohn, Matthew Kenworthy, Sebastiaan Y. Haffert, Frans Snik, Steve Ertel, Jarron M. Leisenring, Charles E. Woodward, Michael F. Skrutskie
Figure caption: Removal of row and column discontinuities by fitting a third-order polynomial to every row and column.
Paper: Search for Stellar Flybys in the Sco-Cen OB Association with the Gaia DR2
Authors: Yilun Ma, 逸伦 马, Robert J. De Rosa, Paul Kalas
Figure caption: Closest approach distance as a function of closest approach time and closest approach angle for each of the flyby events involving detected debris disks. The crosses represent the median values of MC outputs; if the posterior distribution is bimodal, the median about each mode is marked by a red cross. The contours represent the 1σ and 2σ credible regions.
Paper: Search for Stellar Flybys in the Sco-Cen OB Association with the Gaia DR2
Authors: Yilun Ma, 逸伦 马, Robert J. De Rosa, Paul Kalas
Figure caption: Closest approach times and distances for the encounters and close encounters identified in the Sco-Cen sample. Orange diamonds mark the close encounters (d ca ≤ 0.5R H); blue stars mark encounters (0.5R H ≤ d ca ≤ R H); gray circles mark the pairs whose close approach distance is in neither star’s Hill radius. The dotted horizontal lines mark the 1st, 5th, and, 10th percentiles of the distribution of the separation of stars within the sample. The median separation of stars in the Sco-Cen sample is 5.60 pc.
Paper: Search for Stellar Flybys in the Sco-Cen OB Association with the Gaia DR2
Authors: Yilun Ma, 逸伦 马, Robert J. De Rosa, Paul Kalas
Figure caption: Color–magnitude diagram of the two samples created using optical photometry from Gaia DR2. Some stars that are not on the main sequence are not plotted. Isochrones from MIST at the ages of the three subgroups are also plotted for comparison. No extinction correction is applied to either the sample or the isochrones.
Paper: Search for Stellar Flybys in the Sco-Cen OB Association with the Gaia DR2
Authors: Yilun Ma, 逸伦 马, Robert J. De Rosa, Paul Kalas
Figure caption: The spatial distribution of the two samples, as well as the stars with identified flyby events, is plotted in the Galactic coordinates. The dashed boxes mark the boundaries of USCO, UCL, and LCC identified by de Zeeuw et al. (1999). The USCO sample is plotted within the inset.
Paper: Search for Stellar Flybys in the Sco-Cen OB Association with the Gaia DR2
Authors: Yilun Ma, 逸伦 马, Robert J. De Rosa, Paul Kalas
Figure caption: Closest approach times and distances for all the encounters and close encounters identified in the USCO sample. Legend is the same as that in Figure 4. The median separation of stars in this sample is 1.23 pc.
Paper: Search for Stellar Flybys in the Sco-Cen OB Association with the Gaia DR2
Authors: Yilun Ma, 逸伦 马, Robert J. De Rosa, Paul Kalas
Figure caption: The mass distributions of the samples are plotted. The full samples are plotted with solid lines; the mass distributions of USCO stars with RV are plotted with the dotted line. The bins are drawn in the logarithmic space.
Paper: Search for Stellar Flybys in the Sco-Cen OB Association with the Gaia DR2
Authors: Yilun Ma, 逸伦 马, Robert J. De Rosa, Paul Kalas
Figure caption: The comparison of the close approach distances of the events involving and not involving IR excess stars for the Sco-Cen sample.
Paper: Search for Stellar Flybys in the Sco-Cen OB Association with the Gaia DR2
Authors: Yilun Ma, 逸伦 马, Robert J. De Rosa, Paul Kalas
Figure caption: The comparison of relative velocity distributions between ScoCen−Field encounters (blue) and ScoCen−ScoCen encounters (orange) with d ca < 3 pc.
Paper: Search for Stellar Flybys in the Sco-Cen OB Association with the Gaia DR2
Authors: Yilun Ma, 逸伦 马, Robert J. De Rosa, Paul Kalas
Figure caption: The closest approach distance is plotted against relative velocity for ScoCen−Field encounters (blue) and ScoCen−ScoCen encounters (orange).
Paper: Search for Stellar Flybys in the Sco-Cen OB Association with the Gaia DR2
Authors: Yilun Ma, 逸伦 马, Robert J. De Rosa, Paul Kalas
Figure caption: The potential close approaches that would have happened within the USCO subgroup by simulating the effect of perfectly knowing the RV of stars without RV measurement. The dotted lines mark the 1st, 5th, 10th, and 50th percentiles of the distribution of the separation of stars within the sample.
Paper: The LHS 1678 System: Two Earth-sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc
Authors: Michele L. Silverstein, Joshua E. Schlieder, Thomas Barclay, Benjamin J. Hord, Wei-Chun Jao, Eliot Halley Vrijmoet, Todd J. Henry, Ryan Cloutier, Veselin B. Kostov, Ethan Kruse, Jennifer G. Winters, Jonathan M. Irwin, Stephen R. Kane, Keivan G. Stassun, Chelsea Huang, Michelle Kunimoto, Evan Tey, Andrew Vanderburg, Nicola Astudillo-Defru, Xavier Bonfils, C. E. Brasseur, David Charbonneau, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Tansu Daylan, John P. Doty, Courtney D. Dressing, Emily A. Gilbert, Keith Horne, Jon M. Jenkins, David W. Latham, Andrew W. Mann, Elisabeth Matthews, Leonardo A. Paredes, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Avi Shporer, Jeffrey C. Smith, Christopher Stockdale, Thiam-Guan Tan, Guillermo Torres, Joseph D. Twicken, Roland Vanderspek, Gavin Wang, Joshua N. Winn
Figure caption: Mass–radius diagram with LHS 1678 b and c, the rocky solar system planets, and small exoplanets with robust measurements of M < 2.5 M ⊕, R < 1.6 R ⊕, and errors of <20%. In order of increasing mass these are TRAPPIST-1 h, d, e, f, c, g, and b, LTT 1445 A c, L 231-32 b, GJ 1132 b, LHS 1140 c, Kepler-78 b, GJ 357 b, GJ 3473 b, L 98-59 d, L 98-59 c, LHS 1478 b, LTT 3780 b, K2-229 b, and LTT 1445 A b (properties and references in Table 8). LHS 1678 b and c are each labeled with three open circles with arrows connecting them from right to left to denote the 3-, 2-, and 1σ (99%, 97.7%, and 68%) mass upper limits. Lines of constant density for a variety of compositions are overlaid (Zeng et al. 2019). Planets with densities that lie beneath the collisional stripping curve (Marcus et al. 2010; Zeng et al. 2019) should be nonphysical, so that region is shaded. The collisional stripping mass upper limits of LHS 1678 b and c are 0.419 M ⊕ and 1.51 M ⊕, respectively. Notably, the majority of planets on this diagram are of similar density to an Earth-like rocky planet. This, combined with our mass constraints, indicates that the LHS 1678 planets are likely to be predominantly rocky. Of particular note, the 1σ mass upper limit for LHS 1678 c, which is in the “Venus zone”, places it identically with Venus on the mass–radius diagram within our error bars.
Paper: The LHS 1678 System: Two Earth-sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc
Authors: Michele L. Silverstein, Joshua E. Schlieder, Thomas Barclay, Benjamin J. Hord, Wei-Chun Jao, Eliot Halley Vrijmoet, Todd J. Henry, Ryan Cloutier, Veselin B. Kostov, Ethan Kruse, Jennifer G. Winters, Jonathan M. Irwin, Stephen R. Kane, Keivan G. Stassun, Chelsea Huang, Michelle Kunimoto, Evan Tey, Andrew Vanderburg, Nicola Astudillo-Defru, Xavier Bonfils, C. E. Brasseur, David Charbonneau, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Tansu Daylan, John P. Doty, Courtney D. Dressing, Emily A. Gilbert, Keith Horne, Jon M. Jenkins, David W. Latham, Andrew W. Mann, Elisabeth Matthews, Leonardo A. Paredes, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Avi Shporer, Jeffrey C. Smith, Christopher Stockdale, Thiam-Guan Tan, Guillermo Torres, Joseph D. Twicken, Roland Vanderspek, Gavin Wang, Joshua N. Winn
Figure caption: LS periodograms of HARPS RVs, activity indicators, and other diagnostics. The 5% and 1% FAPs are shown as solid and dashed horizontal lines. The periods of the TESS candidate planets derived from our joint modeling (Section 5) are plotted as vertical dotted–dashed (planet b) and dashed (planet c) lines. The RV periodogram exhibits no significant periodic signals at those orbital periods. The strongest signal in the RV data, with a 5% FAP, appears at 41.7 days (vertical dotted line). The signal may be associated with the stellar rotation period or a harmonic, but the data are insufficient to place a firm constraint. This candidate signal does not appear with any significance in the activity diagnostics. We note that several diagnostics exhibit significant peaks at ∼1 day, consistent with the observation cadence.
Paper: The LHS 1678 System: Two Earth-sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc
Authors: Michele L. Silverstein, Joshua E. Schlieder, Thomas Barclay, Benjamin J. Hord, Wei-Chun Jao, Eliot Halley Vrijmoet, Todd J. Henry, Ryan Cloutier, Veselin B. Kostov, Ethan Kruse, Jennifer G. Winters, Jonathan M. Irwin, Stephen R. Kane, Keivan G. Stassun, Chelsea Huang, Michelle Kunimoto, Evan Tey, Andrew Vanderburg, Nicola Astudillo-Defru, Xavier Bonfils, C. E. Brasseur, David Charbonneau, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Tansu Daylan, John P. Doty, Courtney D. Dressing, Emily A. Gilbert, Keith Horne, Jon M. Jenkins, David W. Latham, Andrew W. Mann, Elisabeth Matthews, Leonardo A. Paredes, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Avi Shporer, Jeffrey C. Smith, Christopher Stockdale, Thiam-Guan Tan, Guillermo Torres, Joseph D. Twicken, Roland Vanderspek, Gavin Wang, Joshua N. Winn
Figure caption: Ground-based transit observations of LHS 1678 b. Data points with uncertainties represent individual photometric measurements in each time series and white circles are data binned at 10 minutes cadence. The best-fit model is represented as a black line with 1σ uncertainties in gray shading. We note that the uncertainty in the transit times increases with time since the TESS observations, as expected.
Paper: The LHS 1678 System: Two Earth-sized Transiting Planets and an Astrometric Companion Orbiting an M Dwarf Near the Convective Boundary at 20 pc
Authors: Michele L. Silverstein, Joshua E. Schlieder, Thomas Barclay, Benjamin J. Hord, Wei-Chun Jao, Eliot Halley Vrijmoet, Todd J. Henry, Ryan Cloutier, Veselin B. Kostov, Ethan Kruse, Jennifer G. Winters, Jonathan M. Irwin, Stephen R. Kane, Keivan G. Stassun, Chelsea Huang, Michelle Kunimoto, Evan Tey, Andrew Vanderburg, Nicola Astudillo-Defru, Xavier Bonfils, C. E. Brasseur, David Charbonneau, David R. Ciardi, Karen A. Collins, Kevin I. Collins, Dennis M. Conti, Ian J. M. Crossfield, Tansu Daylan, John P. Doty, Courtney D. Dressing, Emily A. Gilbert, Keith Horne, Jon M. Jenkins, David W. Latham, Andrew W. Mann, Elisabeth Matthews, Leonardo A. Paredes, Samuel N. Quinn, George R. Ricker, Richard P. Schwarz, Sara Seager, Ramotholo Sefako, Avi Shporer, Jeffrey C. Smith, Christopher Stockdale, Thiam-Guan Tan, Guillermo Torres, Joseph D. Twicken, Roland Vanderspek, Gavin Wang, Joshua N. Winn
Figure caption: HARPS RV data folded on the candidate signal at 41.7 days, repeated across two full periods, with no binning, to better show the periodic nature. This signal may be consistent with the rotation period of LHS 1678 or a harmonic. Alternatively, the signal may be evidence of a longer-period planet in the system. To explore this hypothesis, we fit the signal with a Keplerian orbit model assuming broad input priors. We show random draws from the fit posterior as black curves. While the data can be fit with such a model, the true nature of the candidate signal at 41.7 days remains unconstrained with the available data.