adsabs/AstroCLIMB huggingface dataset:
Paper: Mass Production of 2021 KMTNet Microlensing Planets. I
Authors: Yoon-Hyun Ryu, Youn Kil Jung, Hongjing Yang, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Kyu-Ha Hwang, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge
Figure caption: CMDs for each of the four planets reported here. The source positions (blue) and clump-giant centroids (red) are shown for all events.
Paper: Mass Production of 2021 KMTNet Microlensing Planets. I
Authors: Yoon-Hyun Ryu, Youn Kil Jung, Hongjing Yang, Andrew Gould, Michael D. Albrow, Sun-Ju Chung, Cheongho Han, Kyu-Ha Hwang, In-Gu Shin, Yossi Shvartzvald, Jennifer C. Yee, Weicheng Zang, Sang-Mok Cha, Dong-Jin Kim, Seung-Lee Kim, Chung-Uk Lee, Dong-Joo Lee, Yongseok Lee, Byeong-Gon Park, Richard W. Pogge
Figure caption: Light curve and model for KMT-2021-BLG-1372. The light curve shows a rounded dip, which is the classic signature of a minor-image perturbation for which the source misses the two planetary caustics. The anomaly is near peak, implying that the trajectory is roughly perpendicular to the planet–host axis and that there should be a classic “inner/outer” degeneracy (Gaudi & Gould 1997). These expectations are confirmed by the caustic structures shown in the insets.(The data used to create this figure are available.)
Paper: A Jupiter Analog Orbiting The Nearby M Dwarf GJ 463
Authors: Michael Endl, Paul Robertson, William D. Cochran, Phillip J. MacQueen, Brendan P. Bowler, Kyle E. Franson, Rae Holcomb, Corey Beard, Howard Isaacson, Andrew W. Howard, Jack Lubin
Figure caption: Predicted mass of the companion to GJ 463 as a function of semimajor axis based on its astrometric acceleration between Hipparcos and Gaia EDR3. Approximate thresholds for the deuterium-burning limit (13 M jup) and hydrogen-burning limit (75 M jup) are denoted by the black dashed lines. The minimum mass of GJ 463 b from the RV orbit fit is highlighted in red. The astrometric acceleration is fully consistent with the RV-detected companion GJ 463 b and indicates the true mass is likely in the planetary regime.
Paper: A Jupiter Analog Orbiting The Nearby M Dwarf GJ 463
Authors: Michael Endl, Paul Robertson, William D. Cochran, Phillip J. MacQueen, Brendan P. Bowler, Kyle E. Franson, Rae Holcomb, Corey Beard, Howard Isaacson, Andrew W. Howard, Jack Lubin
Figure caption: Star–planet contrast of GJ 463 b in reflected light assuming Lambertian scattering and a range of geometric albedos from A  g  = 0.1–0.9. In terms of contrast, Roman/CGI may be sensitive to GJ 463 b if it is a “bright” planet with albedos A  g  ≳ 0.5. Points represent equal-spaced intervals throughout the orbit.
Paper: A Jupiter Analog Orbiting The Nearby M Dwarf GJ 463
Authors: Michael Endl, Paul Robertson, William D. Cochran, Phillip J. MacQueen, Brendan P. Bowler, Kyle E. Franson, Rae Holcomb, Corey Beard, Howard Isaacson, Andrew W. Howard, Jack Lubin
Figure caption: One- and two-dimensional projections of the posterior probability distributions of parameters in our 1-planet fit.
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Different timescales involved in grain alignment, including super-Barnett relaxation with different iron inclusions (N cl) and inelastic relaxation, for suprathermally rotating grains by METs with s  d  = 0.25 (left) and s  d  = 0.5 (right). The gas damping time for three typical densities in protostellar environments is also shown for comparison. Super-Barnett and inelastic relaxation effects are faster for larger s  d .
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Variation of the maximum grain size for efficient internal alignment, ﹩{a}_{\,\max ,\mathrm{aJ}}﹩, with the gas density due to Barnett relaxation for the typical radiation strength U = 1, assuming grains rotating suprathermally by METs with s  d  = 0.25 (left panel) and 0.5 (right panel). Grains with different levels of iron clusters are considered. The internal alignment sizes increases with N cl and the drift parameter s  d .
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Variation of the minimum (﹩{a}_{\min ,\mathrm{aJ}}﹩, dashed lines) and maximum grain sizes (﹩{a}_{\,\max ,\mathrm{aJ}}﹩, solid lines) for efficient internal alignment with the gas density due to super-Barnett relaxation (BR, SPM) and inelastic relaxation (iER), assuming grains rotating suprathermally by RATs with γ rad = 0.5, ﹩\bar{\lambda }=10\,\mu {\rm{m}}﹩, and four values of U = 1, 102, 104, 106. Inelastic relaxation is more efficient than super-Barnett relaxation for U ≳ 104. Both effects become inefficient for increasing n H due to stronger gas damping and lower StRAT.
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Variation of the minimum (dashed line) and maximum sizes (solid line) for internal alignment by super-Barnett and inelastic relaxation for grains aligned at a high-J attractor by RATs for a protostellar disk with the surface density of Σ0 = 102 g cm−2 and μ Q = 108 erg cm−3. Inelastic relaxation is efficient for r > 100 au (shaded area), whereas super-Barnett relaxation is inefficient in the entire disk midplane.
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Schematic illustration of the grain precession in the presence of a magnetic field and a radiation beam, or a gas flow. In addition to radiative (or mechanical) precession, the grain experiences Larmor precession around the magnetic field ( B ). The fastest precession direction establishes the alignment axis by RATs (METs) in the presence of the magnetic field.
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Internal relaxation times by inelastic and super-Barnett relaxations for grains spun up by RATs in a radiation field of ﹩\bar{\lambda }=10\,\mu {\rm{m}},{\gamma }_{\mathrm{rad}}=0.5﹩ and gas density of n H = 108  cm−3 for U = 104 (left panel) and U = 106 (right panel). A sharp rise in the timescale at ﹩a\sim \bar{\lambda }/2﹩ is due to the change in the slope of RATs. Higher radiation strength increases the suprathermal rotation number StRAT and reduces the relaxation times, extending the range of grains with fast internal relaxation.
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Maximum size for internal alignment by super-Barnett relaxation for Σ0 = 100 (left) and Σ0 = 103 g cm−2 (right), assuming grains spun up by METs with s  d  = 0.25. The maximum size of internal alignment increases with the size of iron inclusions (N cl), but decreases with increasing Σ0 due to stronger gas damping.
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Same as Figure 8, but for grains subject to a stronger local radiation field of U = 104. The values of ﹩{a}_{\,\max ,\mathrm{aJ}}﹩ are smaller, especially for the case of large N cl, due to a decrease in the magnetic susceptibility with the dust temperature.
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Suprathermal rotation number (St) of dust grains spun up by RATs and METs as functions of the grain size (a). The values of StRAT are shown by the solid lines for the different radiation strength, U, and StMET values are shown by the broken lines for the different drift parameter, s d. The dashed horizontal line indicates St = 1. We assumed typical physical parameters with n H = 108  cm−3, ﹩\bar{\lambda }=10\,\mu {\rm{m}}﹩, and Q spinup = 10−3 for METs.
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Maximum size for magnetic alignment vs. disk radius for grains with different iron inclusions of N cl ≥ 100, assuming a disk surface mass density of Σ0 = 100 (left) and Σ0 = 103 g cm−2 (right).
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Expected polarization pattern of thermal dust emission from grains aligned with  J  along the magnetic field (magnetic alignment) in a disk with the toroidal magnetic field (blue lines). Both right IA (upper panels) and wrong IA (lower panels) are considered.
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Schematic illustration of internal alignment (IA) and external alignment of grains as a function of the grain size expected for protostellar environments, assuming grains are aligned by RATs (METs). The largest grains can experience k-RAT alignment (orange area) with two possible states of right and wrong IA. Smaller grains tend to experience B- RAT (-MET) alignment due to fast Larmor precession, with right IA (gray area) by inelastic relaxation (pink bar) and Barnett relaxation (green).
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Same as Figure 16 but for the alignment with  J  along the drift direction  v  d, which is assumed to be azimuthal due to the Keplerian motion. The polarization pattern is similar to Figure 16.
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Expected polarization pattern of thermal dust emission from aligned grains with  J  along the radiation direction  k  for the case of right IA (IA, upper) and wrong IA (lower panel).
Paper: On Internal and External Alignment of Dust Grains in Protostellar Environments
Authors: Thiem Hoang, Le Ngoc Tram, Vo Hong Minh Phan, Nguyen Chau Giang, Nguyen Thi Phuong, Nguyen Duc Dieu
Figure caption: Same as Figure 12 but for s  d  = 0.5. The maximum size for internal alignment is increased significantly due to stronger METs, and the ≳100 μm grains with large iron clusters can be internally aligned at r > 100 au.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Left: Recovery of TOI 451 c. Upper panel: PSF flux (in dark gray) and penalized spline trend (in blue). Lower panel: Detrended light curve (PSF flux divided by the trend). The multi-transit signature (in red) can be clearly seen. Right: Upper panel shows phase-folded light curve of TOI 451 c (gray data points) along with the best-fit model using EXOTIC (in red). Lower panel shows the residuals in parts per million.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Centroid tests for POIs/Potential Binaries in UCL.
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Centroid tests for single-planet systems
Paper: pterodactyls: A Tool to Uniformly Search and Vet for Young Transiting Planets in TESS Primary Mission Photometry
Authors: Rachel B. Fernandes, Gijs D. Mulders, Ilaria Pascucci, Galen J. Bergsten, Tommi T. Koskinen, Kevin K. Hardegree-Ullman, Kyle A. Pearson, Steven Giacalone, Jon Zink, David R. Ciardi, Patrick O'Brien
Figure caption: Centroid tests for multi-planet systems
Paper: Inhomogeneity within Local Interstellar Clouds 
Authors: Jeffrey L. Linsky, Seth Redfield, Diana Ryder, Adina Chasan-Taber
Figure caption: Left: plots of turbulent velocity vs. temperature for different ions, best fit (cross), and 1σ and 2σ contours about the best fit. Right: Doppler parameters vs. mass for each ion. The best-fit parameters and 1σ contours fitting the Doppler parameters are included. Data from E140M spectra are blue and data from E230H or E140H spectra are red.
Paper: Inhomogeneity within Local Interstellar Clouds 
Authors: Jeffrey L. Linsky, Seth Redfield, Diana Ryder, Adina Chasan-Taber
Figure caption: Distributions of sight-line temperatures for the full data set (left) and for only the sight lines that pass through the LIC (right). Temperatures are binned in 1000 K intervals. The solid curves are Gaussian fits to the weighted data points.
Paper: Inhomogeneity within Local Interstellar Clouds 
Authors: Jeffrey L. Linsky, Seth Redfield, Diana Ryder, Adina Chasan-Taber
Figure caption: Distributions of sight-line turbulent velocities for the full data set (left) and for only the sight lines that pass through the LIC (right). Turbulent velocities are binned in 0.5 km s−1 intervals. The solid curves are Gaussian fits to the weighted data points.
Paper: MOA-2020-BLG-135Lb: A New Neptune-class Planet for the Extended MOA-II Exoplanet Microlens Statistical Analysis
Authors: Stela Ishitani Silva, Clément Ranc, David P. Bennett, Ian A. Bond, Weicheng Zang, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Arisa Okamura, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Andreea Petric, Todd Burdullis, Pascal Fouqué, Shude Mao, Matthew T. Penny, Wei Zhu, Gioia Rau
Figure caption: The marginalized posterior distributions for our MCMC runs, correlating the parameters for the binary-lens single-source model (2L1S), and, in the diagonal, the one-dimension probability density function (PDF) of each parameter. The 68.3% (1σ), 95.5% (2σ), and 99.7% (3σ) confidence intervals are shown in dark blue, median blue, and light blue, respectively, in the posterior distribution plots. In the PDF plots, the black dot points out the median, and the thin line marks the 1σ confidence interval. For the separation s PDF plot, the additional red and yellow dots and lines also point out the median and the 1σ confidence interval, but now for each of the two regions, the close-separation (s < 1) in red and the wide-separation (s > 1) in yellow. In panel s vs. q/10−4, the two dashed lines show the theoretical limits of the three caustic topologies (close, resonant, and wide).
Paper: MOA-2020-BLG-135Lb: A New Neptune-class Planet for the Extended MOA-II Exoplanet Microlens Statistical Analysis
Authors: Stela Ishitani Silva, Clément Ranc, David P. Bennett, Ian A. Bond, Weicheng Zang, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Arisa Okamura, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Andreea Petric, Todd Burdullis, Pascal Fouqué, Shude Mao, Matthew T. Penny, Wei Zhu, Gioia Rau
Figure caption: The best-fit model for the MOA-2020-BLG-135 light curve in a magnification vs. time (﹩\mathrm{HJD}^{\prime} =\mathrm{HJD}﹩ −2,450,000) plot. The MOA-Red, MOA-V, and CFHT-i data are shown in brown, violet, and blue, respectively. The best single-source planetary model 2L1S (i.e., two lenses and one source) s > 1 is our best-fit model (see Section 3) and is displayed as a black solid line, while the point-source point-lens (PSPL) model is displayed as a dashed gray line. The main panel shows all the photometric data sets overlaid with the best-fit model. The upper left side of the figure, zooming near the peak of the event, shows the planetary perturbation, which is well covered by the MOA-Red data set, and the corresponding residuals. The lower panel shows the residuals of the best-fit model for each instrument—see the colored legend.(The data used to create this figure are available.)
Paper: MOA-2020-BLG-135Lb: A New Neptune-class Planet for the Extended MOA-II Exoplanet Microlens Statistical Analysis
Authors: Stela Ishitani Silva, Clément Ranc, David P. Bennett, Ian A. Bond, Weicheng Zang, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Arisa Okamura, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Andreea Petric, Todd Burdullis, Pascal Fouqué, Shude Mao, Matthew T. Penny, Wei Zhu, Gioia Rau
Figure caption: The caustic geometry and the source-lens trajectory. The caustic is represented in blue. The black straight solid line shows the source-lens trajectory and the arrow shows the direction of the source-lens relative motion. The source size is displayed as a black circle at its position at ﹩\mathrm{HJD}^{\prime} =9040.49﹩ (event peak), ﹩\mathrm{HJD}^{\prime} =9040.85﹩ for s < 1 and ﹩\mathrm{HJD}^{\prime} =9040.82﹩ for s > 1(source starts crossing the caustic), and ﹩\mathrm{HJD}^{\prime} =9041.00﹩ for s < 1 and ﹩\mathrm{HJD}^{\prime} =9041.34﹩ for s > 1 (source exiting the caustic). For (b), the source at ﹩\mathrm{HJD}^{\prime} =9041.71﹩ is also displayed to show when it is closest to the upper cusp. (a) Caustic geometry of the best-fit model for s <1, due to a close-separation planet. (b) Caustic geometry of the best-fit model for s >1, due to a wide-separation planet.
Paper: MOA-2020-BLG-135Lb: A New Neptune-class Planet for the Extended MOA-II Exoplanet Microlens Statistical Analysis
Authors: Stela Ishitani Silva, Clément Ranc, David P. Bennett, Ian A. Bond, Weicheng Zang, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Arisa Okamura, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Andreea Petric, Todd Burdullis, Pascal Fouqué, Shude Mao, Matthew T. Penny, Wei Zhu, Gioia Rau
Figure caption: (V—I, I) Color–magnitude diagram of the stars in the OGLE-III catalog within 90″ of MOA-2020-BLG-135. The black dots are the stars from the OGLE-III catalog, the blue dot indicates the source magnitude and color for the best-fit model (s > 1), and the red circle indicates the red clump giant centroid. For comparison, we added the green dots showing the Hubble Space Telescope color–magnitude diagram from Holtzman et al. (1998) shifted to the bulge distance and relevant extinction derived in Section 4. The source star is probably in a subgiant phase.
Paper: MOA-2020-BLG-135Lb: A New Neptune-class Planet for the Extended MOA-II Exoplanet Microlens Statistical Analysis
Authors: Stela Ishitani Silva, Clément Ranc, David P. Bennett, Ian A. Bond, Weicheng Zang, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Arisa Okamura, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Andreea Petric, Todd Burdullis, Pascal Fouqué, Shude Mao, Matthew T. Penny, Wei Zhu, Gioia Rau
Figure caption: Lens system properties derived from the Bennett et al. (2014) Galactic model using a power-law stellar mass function under the assumption that the hosting probability scales in proportion to the stellar mass, dP ∝ M dM. The 1σ and 2σ confidence intervals (i.e., 68.3% and 95.5%) are represented by dark blue and median blue, respectively, with the median marked as a solid black line. For comparison, the source magnitude is shown as a green line in the lens magnitude graphs.
Paper: MOA-2020-BLG-135Lb: A New Neptune-class Planet for the Extended MOA-II Exoplanet Microlens Statistical Analysis
Authors: Stela Ishitani Silva, Clément Ranc, David P. Bennett, Ian A. Bond, Weicheng Zang, Fumio Abe, Richard K. Barry, Aparna Bhattacharya, Hirosane Fujii, Akihiko Fukui, Yuki Hirao, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Naoki Koshimoto, Yutaka Matsubara, Sho Matsumoto, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Arisa Okamura, Nicholas J. Rattenbury, Yuki Satoh, Takahiro Sumi, Daisuke Suzuki, Taiga Toda, Paul. J. Tristram, Aikaterini Vandorou, Hibiki Yama, Andreea Petric, Todd Burdullis, Pascal Fouqué, Shude Mao, Matthew T. Penny, Wei Zhu, Gioia Rau
Figure caption: Lens system properties derived from the Bennett et al. (2014) Galactic model using a power-law stellar mass function with a prior uniform in M, dP ∝ dM, meaning all stars have an equal planet-hosting probability. The 1σ and 2σ confidence intervals (i.e., 68.3% and 95.5%) are represented by dark blue and median blue, respectively, with the median marked as a solid black line. For comparison, the source magnitude is shown as a green line in the lens magnitude graphs.
Paper: Simulating Spectral Kurtosis Mitigation against Realistic Radio Frequency Interference Signals
Authors: E. Smith, Ryan S. Lynch, D. J. Pisano
Figure caption: Flagging percentages for various data rates compared to the duty cycle of the RFI signal. BPSK on the top and 2-bit ASK on the bottom.
Paper: Simulating Spectral Kurtosis Mitigation against Realistic Radio Frequency Interference Signals
Authors: E. Smith, Ryan S. Lynch, D. J. Pisano
Figure caption: Examples of flagging a 200 ksps BPSK signal with a 4/W FIR cutoff frequency. (a) The unmitigated signal, (b) comparison mask, (c) single-scale ﹩\widehat{{SK}}﹩, (d) MS-42 ﹩\widehat{{SK}}﹩.