adsabs/AstroCLIMB huggingface dataset:
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Retrieval results for 1 Tmol yr−1N2O case.
Paper: Large Interferometer For Exoplanets (LIFE). XII. The Detectability of Capstone Biosignatures in the Mid-infrared—Sniffing Exoplanetary Laughing Gas and Methylated Halogens
Authors: Daniel Angerhausen, Daria Pidhorodetska, Michaela Leung, Janina Hansen, Eleonora Alei, Felix Dannert, Jens Kammerer, Sascha P. Quanz, Edward W. Schwieterman
Figure caption: Retrieval results for 10 Tmol yr−1N2O case.
Paper: The Long-term Activity of the Postnovae Q Cygni and BK Lyncis
Authors: Vojtěch Šimon
Figure caption: (a) The long-term activity of Q Cyg from 2012 to 2023. These observations are divided into Sets 1 (AAVSO data) and 2 (ZTF data). Only the 1 day means are plotted. Sizes of the error bars are often smaller than the symbol size. The smooth, thick line represents the two-sided moving averages (TMAs) for Q = 160 days of the 1 day means of brightness. The TMAs for AAVSO and ZTF data are separate (see the legend). The horizontal line marks the segment in panel (c). A vertical line represents a night series from panel (d). (b) Smoothed residuals, σ resMA, of the TMA of brightness. (c) Part of the light curve with a trend of brightness decrease and a subsequent plateau. While a considerable scatter of brightness is visible between JD 2 457 300 and JD 2 457 520, the scatter was smaller after JD 2 457 700. The smooth line represents TMAs with Q = 160 days running through the night-to-night fluctuations. (d) Intranight CCD light curve of Q Cyg. The error bars of the individual data points are marked. The horizontal lines and numbers at the edge of the panels represent M opt for its d and A  V . See Section 3 for details.
Paper: The Long-term Activity of the Postnovae Q Cygni and BK Lyncis
Authors: Vojtěch Šimon
Figure caption: Histograms of the brightness of Q Cyg from Figure 1(a). The division into Sets 1 and 2 is JD 258 400. AAVSO data in these histograms have JD < 258 400. ZTF data in these histograms have JD > 258 400. The bar widths are 0.1 mag in both plots. The vertical lines and numbers at the upper edge of panel (a) represent M opt for its d and A  V . The big  ×  symbol denotes maxima’s peaks of DN outbursts analyzed by Patterson (2011), appropriate to P orb of Q Cyg. The small  ×  symbols mark its error bars. (a) Individual 1 day means of CCD observations. (b) TMAs with Q = 160 days. See Section 3 for details.
Paper: Searching for Giant Exoplanets around M-dwarf Stars (GEMS) I: Survey Motivation
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Eric B. Ford, Ravit Helled, Dana E. Anderson, Alan Boss, William D. Cochran, Megan Delamer, Te Han, Jessica E. Libby-Roberts, Andrea S. J. Lin, Simon Müller, Paul Robertson, Gumundur Stefánsson, Johanna Teske
Figure caption: Left: Similar to Figure 4, we plot the EMD while comparing f(m, r∣stm = 0.75 M ⊙) with f(m, r∣stm = 1.0 M ⊙) in orange, and then f(m, r∣stm = 0.5 M ⊙) with f(m, r∣stm = 1.0 M ⊙) in red. As the K dwarf sample is fixed in sample size, it does not show any dependence on the M-dwarf sample size, whereas the red region converges. Right: To establish convergence of the EMD as a function of the sample size (i.e., the minimum sample size beyond which the improvement in EMD is marginal), we consider the distance between the central 68th percentile of the EMD distribution as a function of the sample size and the sample size where its fractional change goes below 1%. Takeaway: The EMD metric to ascertain the stellar dependence for f(m∣r = 1R  J , stm) starts to converge for a GEMS sample of ∼40.
Paper: Searching for Giant Exoplanets around M-dwarf Stars (GEMS) I: Survey Motivation
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Eric B. Ford, Ravit Helled, Dana E. Anderson, Alan Boss, William D. Cochran, Megan Delamer, Te Han, Jessica E. Libby-Roberts, Andrea S. J. Lin, Simon Müller, Paul Robertson, Gumundur Stefánsson, Johanna Teske
Figure caption: Green triangles show an estimate of the heavy-element content (M  Z ) of GEMS from planetary interior models (Thorngren et al. 2016) compared to the Class II disk dust mass (M  d ) estimates as orange squares (Manara et al. 2022) and the median (and 1σ) trend seen in the Lupus sample (Ansdell et al. 2016). The green arrows show the approximate expected disk dust masses required to form the green triangles assuming 10% formation efficiency (Liu et al. 2019b). The red line shows the range of dust masses for Class 0 and I disks from Tychoniec et al. (2020). Takeaway: The formation of GEMS necessitates disks with many 100 s of M ⊕ of heavy elements. This could be achieved by anomalously massive Class II disks with underestimated dust masses or Class 0/I disks.
Paper: Searching for Giant Exoplanets around M-dwarf Stars (GEMS) I: Survey Motivation
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Eric B. Ford, Ravit Helled, Dana E. Anderson, Alan Boss, William D. Cochran, Megan Delamer, Te Han, Jessica E. Libby-Roberts, Andrea S. J. Lin, Simon Müller, Paul Robertson, Gumundur Stefánsson, Johanna Teske
Figure caption: The solid line represents the median metric value, while the different shaded regions represent the 16%–84%, 5%–95%, and 1%–99% percentile regions, respectively. The vertical black line is the minimum sample size of transiting GEMS required based on the comparison of the distributions. Left: Welch’s t-test suggesting the need for about 20 GEMS if we solely wish to compare the median values of the two distributions assuming normality. Right: Earth-mover distance, which suggests the need for about 35 GEMS to distinguish between the two distributions agnostic of Gaussian assumptions. Takeaway: Identifying the minimum sample size required to distinguish between a sample of giant planets around FGK stars and GEMS based on their M-R distribution when the GEMS are about 60% in mass of the FGK planets, we require about 35 GEMS if we do not assume an underlying normal distribution and 20 GEMS if we do.
Paper: Searching for Giant Exoplanets around M-dwarf Stars (GEMS) I: Survey Motivation
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Eric B. Ford, Ravit Helled, Dana E. Anderson, Alan Boss, William D. Cochran, Megan Delamer, Te Han, Jessica E. Libby-Roberts, Andrea S. J. Lin, Simon Müller, Paul Robertson, Gumundur Stefánsson, Johanna Teske
Figure caption: The ∼1.0 million stars observed by TESS through Cycle 5 and contained in our cuts in Section 4.3. Previous studies have used an upper limit of 100 pc, which represents a small fraction (<20%) of our sample. Our sample spans the full range of color and magnitude for M0–M9. For reference, we indicate GJ 488 (M0V; square) and TRAPPIST-1 (M8V; triangle) in the CMD to approximately denote the two ends of the M-dwarf spectral type. The stellar radii, masses, and Teff are calculated from M − K  s  using relations from Mann et al. (2015, 2019), whereas the TICv8.2 contamination ratio is from Stassun et al. (2018).
Paper: Searching for Giant Exoplanets around M-dwarf Stars (GEMS) I: Survey Motivation
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Eric B. Ford, Ravit Helled, Dana E. Anderson, Alan Boss, William D. Cochran, Megan Delamer, Te Han, Jessica E. Libby-Roberts, Andrea S. J. Lin, Simon Müller, Paul Robertson, Gumundur Stefánsson, Johanna Teske
Figure caption: Planetary mass as a function of the stellar mass for GEMS. The transiting planets have true mass measurements, whereas M  p  sini is plotted for the nontransiting ones, with the exception of GJ 463 b which has a true mass measurement of ∼1140 M ⊕ (or ∼3.6 M  J ) from astrometry (Sozzetti 2023).
Paper: Searching for Giant Exoplanets around M-dwarf Stars (GEMS) I: Survey Motivation
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Eric B. Ford, Ravit Helled, Dana E. Anderson, Alan Boss, William D. Cochran, Megan Delamer, Te Han, Jessica E. Libby-Roberts, Andrea S. J. Lin, Simon Müller, Paul Robertson, Gumundur Stefánsson, Johanna Teske
Figure caption: The scatter plot shows the expectation value—f(m∣r, stm)—for Jovian-sized objects orbiting different stellar masses, whereas the orange line shows the linear fit, which we then extrapolate to lower stellar masses for M dwarfs.
Paper: Searching for Giant Exoplanets around M-dwarf Stars (GEMS) I: Survey Motivation
Authors: Shubham Kanodia, Caleb I. Cañas, Suvrath Mahadevan, Eric B. Ford, Ravit Helled, Dana E. Anderson, Alan Boss, William D. Cochran, Megan Delamer, Te Han, Jessica E. Libby-Roberts, Andrea S. J. Lin, Simon Müller, Paul Robertson, Gumundur Stefánsson, Johanna Teske
Figure caption: 2D joint probability distribution—f(m, r)  FGK — for ∼350 giant planets orbiting FGK stars shown in the background, where the black points are the real measurements of FGK planets, the red dots are an example simulation of 50 GEMS obtained via rejection sampling of the underlying FGK PDF, and the underlying color is their probability. Each of these simulated GEMS samples of planets is compared with the FGK sample to estimate the minimum sample size required for the survey as described in Section 4.1.1.
Paper: HPIC: The Habitable Worlds Observatory Preliminary Input Catalog
Authors: Noah W. Tuchow, Christopher C. Stark, Eric Mamajek
Figure caption: Stars selected for observation during a 6 month cool Jupiter detection survey. Points are color coded by survey completeness. Around 900 more stars were selected for observation that the baseline exo-Earth survey, many of which are fainter and at larger distances.
Paper: Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Timothy D. Brandt, Tara Fetherolf, Paul Robertson, Jinglin Zhao, Paul A. Dalba, Robert A. Wittenmyer, R. Paul Butler, Matías R. Díaz, Steve B. Howell, Jeremy Bailey, Brad Carter, Elise Furlan, Crystal L. Gnilka, Jonathan Horner, Hugh R. A. Jones, Simon O'Toole, Chris Tinney
Figure caption: Direct imaging visibility of the five planets in the HD 134606 system. Left panel: top-down view of the system with CHZ (bright green) and OHZ (dark green) overlaid. Right panel: sky-projected view of the system with 60° orbital inclination. IWA and IWA0.5 are represented by the bright and dark shaded disks, respectively. Orbits are color coded if they are above the 1 × 10−10 flux ratio with 60° inclination. The inner four planetary orbits are too compact to be shown with detail on this scale.
Paper: Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Timothy D. Brandt, Tara Fetherolf, Paul Robertson, Jinglin Zhao, Paul A. Dalba, Robert A. Wittenmyer, R. Paul Butler, Matías R. Díaz, Steve B. Howell, Jeremy Bailey, Brad Carter, Elise Furlan, Crystal L. Gnilka, Jonathan Horner, Hugh R. A. Jones, Simon O'Toole, Chris Tinney
Figure caption: Flux-ratio estimate as a function of the semimajor axis of the long-period companion based on random sampling of orbital parameters. The horizontal dashed line and the dotted–dashed line represent the required and optimistic contrast ratio limit of future space-based direct imaging missions, respectively.
Paper: Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Timothy D. Brandt, Tara Fetherolf, Paul Robertson, Jinglin Zhao, Paul A. Dalba, Robert A. Wittenmyer, R. Paul Butler, Matías R. Díaz, Steve B. Howell, Jeremy Bailey, Brad Carter, Elise Furlan, Crystal L. Gnilka, Jonathan Horner, Hugh R. A. Jones, Simon O'Toole, Chris Tinney
Figure caption: Dynamical simulation result of the HD 134606 system with five planets. Eccentricities for each planet were recorded for a simulation duration of 10 million years. The inner planets experience significant eccentricity variations.
Paper: Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Timothy D. Brandt, Tara Fetherolf, Paul Robertson, Jinglin Zhao, Paul A. Dalba, Robert A. Wittenmyer, R. Paul Butler, Matías R. Díaz, Steve B. Howell, Jeremy Bailey, Brad Carter, Elise Furlan, Crystal L. Gnilka, Jonathan Horner, Hugh R. A. Jones, Simon O'Toole, Chris Tinney
Figure caption: HARPS CCF FWHM and contrast data. The upper panels show the original time series of the two activity indicators, and the lower panels show data that have been corrected for the systematic drift due to the instrument de-focusing issue. The linear trends seen in the original FWHM and contrast time series are completely instrumental.
Paper: Revised Architecture and Two New Super-Earths in the HD 134606 Planetary System
Authors: Zhexing Li, Stephen R. Kane, Timothy D. Brandt, Tara Fetherolf, Paul Robertson, Jinglin Zhao, Paul A. Dalba, Robert A. Wittenmyer, R. Paul Butler, Matías R. Díaz, Steve B. Howell, Jeremy Bailey, Brad Carter, Elise Furlan, Crystal L. Gnilka, Jonathan Horner, Hugh R. A. Jones, Simon O'Toole, Chris Tinney
Figure caption: GLS periodogram of ASAS-3 photometry. The horizontal dashed lines are the 0.1% FAP thresholds. The upper and middle panel shows the periodogram before and after the subtraction of the 4600 day peak, respectively. The lower panel shows the window function of the photometry.
Paper: The Multilayer Nature of Molecular Gas toward the Cygnus Region
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Qing-Zeng Yan, Shaobo Zhang, Yan Sun, Xiaolong Wang, Haoran Feng, Yuehui Ma, Miaomiao Zhang, Zi Zhuang, Xin Zhou, Zhiwei Chen, Ji Yang
Figure caption: The multiple layers of gas structure with YSO candidates toward the Cygnus region. Similar to Figure 17, gray-scale maps are reconstructed by identified MC structures. The dashed ellipse shows a large-scale molecular loop with diameter of ∼56 pc at a distance of 800 pc. Red ellipses show OB associations and SNR, while boxes show the masers in Table 2. The overdensity of YSOs' candidates is shown as blue contours in each interval. The levels in different intervals are presented as follows: 3σ to 99.5% of the maximum value with an increased step of 25% in a logarithm scale for [500, 1000] pc. 3σ to 99.5% of the maximum value with an increased step of 20% in a logarithm scale for [1000, 1400] pc. 10σ to 99.5% of the maximum value with an increased step of 20% in a logarithm scale for ≳1400 pc. σ (∼15 deg−1) is the noise level of equivalent density map for each interval.
Paper: The Multilayer Nature of Molecular Gas toward the Cygnus Region
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Qing-Zeng Yan, Shaobo Zhang, Yan Sun, Xiaolong Wang, Haoran Feng, Yuehui Ma, Miaomiao Zhang, Zi Zhuang, Xin Zhou, Zhiwei Chen, Ji Yang
Figure caption: Distances measured by Model B for those 22 clouds in complicated extinction environments. The colorful bands denote gas layers we identified previously.
Paper: The Multilayer Nature of Molecular Gas toward the Cygnus Region
Authors: Shiyu Zhang, Yang Su, Xuepeng Chen, Min Fang, Qing-Zeng Yan, Shaobo Zhang, Yan Sun, Xiaolong Wang, Haoran Feng, Yuehui Ma, Miaomiao Zhang, Zi Zhuang, Xin Zhou, Zhiwei Chen, Ji Yang
Figure caption: The median and uncertainty of distances derived by different methods compared to this work.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Left: black points indicate the median magnitude, m med, vs. the median error, errmag, in the ZTF data. Red and green points indicate the median magnitude vs. the light-curve standard deviation, σ with red outline indicating stars that do not meet a threshold of standard deviation, σ mag, divided by median magnitude error, 2 × errmag, larger than two, and green those that do. Right: excess variability, plotted as standard deviation (σ mag) minus twice the median magnitude error (2 × errmag) vs. inverse von Neumann statistic. Variable stars are selected as those having inverse von Neumann <1 and σ mag > 2 × errmag.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Flux asymmetry (M) vs. quasiperiodicity (Q) plotted for our sample of 470 variable member sources. Primary variability classes are shown by the marker indicated in the legend. Sources with a secondary classification (multiperiodic or long timescale) are marked in addition to their primary class. The dotted lines show the limits in Q and M for the differing classes, with Q = 0.45 and Q = 0.82 dividing the periodic from quasiperiodic and quasiperiodic from stochastic sources, and M = −0.25 and M = +0.25 dividing the burster from symmetric and symmetric from dipper sources.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Distribution of most significant Lomb–Scargle peaks for all stars. The left panel shows the full distribution; the center panel is a zoom-in on the lower range of values that are most likely to be true rotation periods rather than a mix of rotation and other timescales associated with young star variability; the right panel shows a logarithmic format of the full period distribution.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Left: R.A.–decl. and PMRA–PMDec spaces for Mon R2 member stars that are not clustered (black) and associated with the three subcluster regions (red, green, blue). Subclusters are chosen by grouping within equal area 0.5 × 0.5 deg regions, centered at coordinates provided in Table 3. Right: density distribution for proper motions and parallax of the three clusters (red, green, blue curves) compared with those for all member stars (black dotted curves).
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Example sources with different Q–M classifications, as labeled. Top: observed light curves for the entire four seasons of ZTF data; error bars are shown. Bottom: phased light curves using the highest peak in a Lomb–Scargle periodogram (red points) with binned median magnitude (blue points); error bars are shown. Q and M values are indicated.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Light curves with errors for all LAVs that have burster classification (M < −0.25) ZTF_92.33017624_-6.69885234 or V899 Mon have been studied in more detail in Ninan et al. (2015) and Park et al. (2021). ZTF_88.42731129_-10.40019459 or V1818 Ori has been studied in more detail in Chiang et al. (2015).
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Light curves with errors for all LAVs that have symmetric classification. ZTF_92.618151_-6.150693 appears to have brightened recently, but over many epochs has shown both rising and dimming in brightness. Recent ZTF photometry has shown the magnitude has dimmed very quickly shortly after its rise.
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Light curves with errors for all LAVs that have dipper classification (M > 0.25). ZTF_91.84075009_-6.44193939 has been studied in Jiang & Hillenbrand (2022).
Paper: The Emerging Stellar Complex in Mon R2: Membership and Optical Variability Classification
Authors: Sally D. Jiang, Lynne A. Hillenbrand
Figure caption: Same as Figure 13, but example sources with secondary classification of L or MP.
Paper: Implication of the Velocity Dispersion Scalings on High-mass Star Formation in Molecular Clouds
Authors: An-Xu Luo, Hong-Li Liu, Sheng-Li Qin, Dong-ting Yang, Sirong Pan
Figure caption: Velocity-dispersion distribution of the 55 clumps that overlap between Traficante et al. (2018) and this work. The gray and red histograms represent the velocity dispersion distributions derived from the H13CO+ (1–0) line (see Section 3.1), and the N2H+ (1–0) line (Traficante et al. 2018), respectively. In turn, the gray and red dashed lines correspond to the mean values of the two distributions, respectively.
Paper: Implication of the Velocity Dispersion Scalings on High-mass Star Formation in Molecular Clouds
Authors: An-Xu Luo, Hong-Li Liu, Sheng-Li Qin, Dong-ting Yang, Sirong Pan
Figure caption: Luminosity–mass ratio distribution for different evolutionary phases of clumps, including the quiescent, protostellar, H II region, and PDR phases. The black vertical dashed line marks the median ratio for each phase. The median value for each phase is 2.0, 3.5, 19.5, and 12.8, respectively.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: Uniform prior fit with Efit5 and orbitize! for the new system mass of 0.38 M ⊙.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: Uniform prior fit with Efit5 and orbitize! for the new system mass of 0.38 M ⊙, new 2023A astrometry data point from NIRC2, and 2020 RV data point from KPIC.
Paper: Orbital and Atmospheric Characterization of the 1RXS J034231.8+121622 System using High-resolution Spectroscopy Confirms that the Companion is a Low-mass Star
Authors: Clarissa R. Do Ó, Ben Sappey, Quinn M. Konopacky, Jean-Baptiste Ruffio, Kelly K. O'Neil, Tuan Do, Gregory Martinez, Travis S. Barman, Jayke S. Nguyen, Jerry W. Xuan, Christopher A. Theissen, Sarah Blunt, William Thompson, Chih-Chun Hsu, Ashley Baker, Randall Bartos, Geoffrey A. Blake, Benjamin Calvin, Sylvain Cetre, Jacques-Robert Delorme, Greg Doppmann, Daniel Echeverri, Luke Finnerty, Michael P. Fitzgerald, Julie Inglis, Nemanja Jovanovic, Ronald A. López, Dimitri Mawet, Evan Morris, Jacklyn Pezzato, Tobias Schofield, Andrew Skemer, J. Kent Wallace, Jason J. Wang, Ji Wang, Joshua Liberman
Figure caption: Posteriors for Efit5 with the new data and uniform prior mass fit. Orbital parameters are fit with observable priors.