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: Results for Proxima-type star in 100 days.
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: Results for Proxima-type star in 10 days.
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: Results for K6V-type star in 100 days.
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: Results for K6V-type star in 10 days.
Paper: The DECam Ecliptic Exploration Project (DEEP). VI. First Multiyear Observations of Trans-Neptunian Objects
Authors: Hayden Smotherman, Pedro H. Bernardinelli, Stephen K. N. Portillo, Andrew J. Connolly, J. Bryce Kalmbach, Steven Stetzler, Mario Jurić, Dino Bektešević, Zachary Langford, Fred C. Adams, William J. Oldroyd, Matthew J. Holman, Colin Orion Chandler, Cesar Fuentes, David W. Gerdes, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: Cumulative (top) and differential (bottom) histograms of semimajor axis distribution of the predicted CFEPS detections (orange) given our survey biases and our recovered classical objects (blue), limited to the 40 < a < 48 au range. The differential histogram was normalized to the number of real objects, and we also include Poisson error bars in the counts of the real objects.
Paper: The DECam Ecliptic Exploration Project (DEEP). VI. First Multiyear Observations of Trans-Neptunian Objects
Authors: Hayden Smotherman, Pedro H. Bernardinelli, Stephen K. N. Portillo, Andrew J. Connolly, J. Bryce Kalmbach, Steven Stetzler, Mario Jurić, Dino Bektešević, Zachary Langford, Fred C. Adams, William J. Oldroyd, Matthew J. Holman, Colin Orion Chandler, Cesar Fuentes, David W. Gerdes, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: Eccentricity vs. semimajor axis (top) and inclination vs. semimajor axis (bottom) for the 110 objects from the DEEP B1 fields. Color denotes dynamical classifications. Vertical dotted lines correspond to the approximate location of select Neptunian p:q mean-motion resonance. Curved dotted lines (top panel only) correspond to lines of constant pericenter.
Paper: The DECam Ecliptic Exploration Project (DEEP). VI. First Multiyear Observations of Trans-Neptunian Objects
Authors: Hayden Smotherman, Pedro H. Bernardinelli, Stephen K. N. Portillo, Andrew J. Connolly, J. Bryce Kalmbach, Steven Stetzler, Mario Jurić, Dino Bektešević, Zachary Langford, Fred C. Adams, William J. Oldroyd, Matthew J. Holman, Colin Orion Chandler, Cesar Fuentes, David W. Gerdes, Hsing Wen Lin, 省文 林, Larissa Markwardt, Andrew McNeill, Michael Mommert, Kevin J. Napier, Matthew J. Payne, Darin Ragozzine, Andrew S. Rivkin, Hilke Schlichting, Scott S. Sheppard, Ryder Strauss, David E. Trilling, Chadwick A. Trujillo
Figure caption: Inverse variance-weighted mean H magnitudes of the 110 detected real objects. This is computed using an H-G model with an assumed value of G = 0.15.
Paper: Precise Mass Measurement of OGLE-2013-BLG-0132/MOA-2013-BLG-148: A Saturn-mass Planet Orbiting an M Dwarf
Authors: Natalia E. Rektsini, Virginie Batista, Clément Ranc, David P. Bennett, Jean-Philippe Beaulieu, Joshua W. Blackman, Andrew A. Cole, Sean K. Terry, Naoki Koshimoto, Aparna Bhattacharya, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: Light curve of OGLE-2013-BLG-0132. The right panel shows the enlargement of the caustic-crossing part of the light curve. The best-fit model is indicated by the black curve. The bottom panel shows the residual from the best-fit model and the OGLE and MOA data. The figures were made using the software described in Ranc (2020).
Paper: Precise Mass Measurement of OGLE-2013-BLG-0132/MOA-2013-BLG-148: A Saturn-mass Planet Orbiting an M Dwarf
Authors: Natalia E. Rektsini, Virginie Batista, Clément Ranc, David P. Bennett, Jean-Philippe Beaulieu, Joshua W. Blackman, Andrew A. Cole, Sean K. Terry, Naoki Koshimoto, Aparna Bhattacharya, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: Bayesian posterior probability distributions for the planetary companion mass, host mass, their separation, and the distance to the lens system are shown with only light-curve constraints in blue and with the additional constraints from our Keck follow-up observations in red. The central 68.3% (1σ) of the distributions are shaded in darker colors (dark magenta and dark cyan), and the remaining central 95.4% (3σ) of the distributions are shaded in lighter colors. The vertical black line marks the median of the probability distribution for the respective parameters. We show that the medians of the Bayesian probability are within 2σ of the constrained parameter distributions.
Paper: Precise Mass Measurement of OGLE-2013-BLG-0132/MOA-2013-BLG-148: A Saturn-mass Planet Orbiting an M Dwarf
Authors: Natalia E. Rektsini, Virginie Batista, Clément Ranc, David P. Bennett, Jean-Philippe Beaulieu, Joshua W. Blackman, Andrew A. Cole, Sean K. Terry, Naoki Koshimoto, Aparna Bhattacharya, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: Mass–distance estimate for the lens. The purple curve represents the constraint from the K-band measurement of lens flux, the sea green curve shows the measurement of Einstein angular radius, and the gray curve represents the microlensing parallax calculated using the (AO) constraints. The intersection between the three curves defines the estimated solution of the lens physical parameters.
Paper: Precise Mass Measurement of OGLE-2013-BLG-0132/MOA-2013-BLG-148: A Saturn-mass Planet Orbiting an M Dwarf
Authors: Natalia E. Rektsini, Virginie Batista, Clément Ranc, David P. Bennett, Jean-Philippe Beaulieu, Joshua W. Blackman, Andrew A. Cole, Sean K. Terry, Naoki Koshimoto, Aparna Bhattacharya, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: The marginalized posterior distributions of the light-curve best-fit model. On the diagonal we show the one-dimensional cumulative density function of each parameter. The 68.3% (1σ), 95.5% (2σ), and 99.7% (3σ) confidence intervals are represented by dark, median, and light violet respectively.
Paper: Precise Mass Measurement of OGLE-2013-BLG-0132/MOA-2013-BLG-148: A Saturn-mass Planet Orbiting an M Dwarf
Authors: Natalia E. Rektsini, Virginie Batista, Clément Ranc, David P. Bennett, Jean-Philippe Beaulieu, Joshua W. Blackman, Andrew A. Cole, Sean K. Terry, Naoki Koshimoto, Aparna Bhattacharya, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: Two-dimensional parallax distribution based on the Galactic model (genulens). The color scale shows the relative probability; the black cross indicates the microlensing parallax predicted using our (AO) Keck constraints.
Paper: Precise Mass Measurement of OGLE-2013-BLG-0132/MOA-2013-BLG-148: A Saturn-mass Planet Orbiting an M Dwarf
Authors: Natalia E. Rektsini, Virginie Batista, Clément Ranc, David P. Bennett, Jean-Philippe Beaulieu, Joshua W. Blackman, Andrew A. Cole, Sean K. Terry, Naoki Koshimoto, Aparna Bhattacharya, Aikaterini Vandorou, Thomas J. Plunkett, Jean-Baptiste Marquette
Figure caption: Left panel: close-up frame (400 × 420 mas) of the three-star group selection by DAOPHOT. Right panel: residual of the three-star PSF fit.
Paper: Helium in the Extended Atmosphere of the Warm Superpuff TOI-1420b
Authors: Shreyas Vissapragada, Michael Greklek-McKeon, Dion Linssen, Morgan MacLeod, Daniel P. Thorngren, Peter Gao, Heather A. Knutson, David W. Latham, Mercedes López-Morales, Antonija Oklopčić, Jorge Pérez González, Morgan Saidel, Abigail Tumborang, Stephanie Yoshida
Figure caption: Large-scale model of the planetary outflow from TOI-1420b. The upper panel shows the logarithm of the mass density ﹩{\mathrm{log}}_{10}(\rho )﹩ of a slice through the orbital plane of the 3D hydrodynamic model. A small bubble of unshocked mass loss around the planet is truncated by the star’s tidal gravitational field, after which the outflow extends into leading and trailing tails ahead and behind the planet in its orbital path, respectively. The lower panel shows the corresponding excess absorption in the WIRC helium bandpass as a function of time during a transit, and shaded regions denote the 1σ (dark gray) and 2σ (light gray) uncertainties on the measured mid-transit excess absorption. Despite the extended tails, most of the absorption comes during the optical transit (approximately ±0.07 day, indicated by vertical lines) with a gradual return to very low levels of excess absorption outside of ±0.1 day. This indicates that most of the optical depth contributing to the excess absorption lies in dense regions at the base of the planetary outflow near the planet—not from the large-scale structure, which is mostly transparent.
Paper: Helium in the Extended Atmosphere of the Warm Superpuff TOI-1420b
Authors: Shreyas Vissapragada, Michael Greklek-McKeon, Dion Linssen, Morgan MacLeod, Daniel P. Thorngren, Peter Gao, Heather A. Knutson, David W. Latham, Mercedes López-Morales, Antonija Oklopčić, Jorge Pérez González, Morgan Saidel, Abigail Tumborang, Stephanie Yoshida
Figure caption: WIRC (left) and phase-folded TESS (right) light curves of TOI-1420b. The data are shown unbinned in gray (with circles and triangles denoting points from the first and second nights of WIRC observations, respectively) and binned to 10 minute cadence in black. MAP light-curve models are overplotted in the solid curves for WIRC (red) and TESS (blue), with the shaded regions denoting the 68% credible intervals. The TESS light-curve model is recalculated using the helium bandpass limb-darkening coefficients on the WIRC plot, showing that differences in limb darkening cannot explain the increased depth at mid-transit.(The data used to create this figure are available.)
Paper: Helium in the Extended Atmosphere of the Warm Superpuff TOI-1420b
Authors: Shreyas Vissapragada, Michael Greklek-McKeon, Dion Linssen, Morgan MacLeod, Daniel P. Thorngren, Peter Gao, Heather A. Knutson, David W. Latham, Mercedes López-Morales, Antonija Oklopčić, Jorge Pérez González, Morgan Saidel, Abigail Tumborang, Stephanie Yoshida
Figure caption: (Left) Masses and equilibrium temperatures of low-density (ρ < 0.3 g cm−3) planets on the NASA Exoplanet Archive as of 2023 September 10 (Akeson et al. 2013) with masses measured to better than 30%. Planets on grazing orbits have been removed. TOI-1420b is highlighted with a red star. The shading indicates planetary density, and the dotted lines demarcate the bounds of the plot shown on the right. (Right) Same as left, but focused on the lower-mass superpuff population with individual systems labeled.
Paper: Helium in the Extended Atmosphere of the Warm Superpuff TOI-1420b
Authors: Shreyas Vissapragada, Michael Greklek-McKeon, Dion Linssen, Morgan MacLeod, Daniel P. Thorngren, Peter Gao, Heather A. Knutson, David W. Latham, Mercedes López-Morales, Antonija Oklopčić, Jorge Pérez González, Morgan Saidel, Abigail Tumborang, Stephanie Yoshida
Figure caption: Temperature (top panel, solid curves), mean molecular weight (top panel, dashed curves), and metastable helium number density (middle panel) profiles for the high-activity (blue), medium-activity (red), and low-activity (green) ATES+Cloudy models. The solid curves in the bottom panel show the predicted metastable helium features at high dispersion in air wavelengths in the observatory rest frame. The dotted curve shows the filter transmission function. The text annotations give the corresponding excess transit depth values (after integrating through the filter transmission function) compared to the observed absorption.
Paper: Helium in the Extended Atmosphere of the Warm Superpuff TOI-1420b
Authors: Shreyas Vissapragada, Michael Greklek-McKeon, Dion Linssen, Morgan MacLeod, Daniel P. Thorngren, Peter Gao, Heather A. Knutson, David W. Latham, Mercedes López-Morales, Antonija Oklopčić, Jorge Pérez González, Morgan Saidel, Abigail Tumborang, Stephanie Yoshida
Figure caption: Allan deviation plots for the two WIRC light curves. The black curves indicate the rms scatter as a function of the bin size on each night, the solid red curves indicate the expectations from photon noise, and the dashed red curves are the solid red curves scaled up to match the first point of the black curve, i.e., the expectation if our data binned down exactly like white noise.
Paper: Relative Velocities between 13CO Structures within 12CO Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Xuepeng Chen, Yang Su, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Min Fang, Fujun Du, Yan Sun, Hongchi Wang, Ye Xu
Figure caption: Upper panel: number distributions of relative velocities (ΔV LOS) between each two 13CO structures in the MC samples having triple 13CO structures and their ratios with internal velocity dispersions of 13CO structures (ΔV LOS/﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{in}}﹩). Lower panel: number distributions of the maximum relative velocity (﹩{\rm{\Delta }}{V}_{\max }﹩) within each MC and their ratios with internal velocity dispersions (﹩{\rm{\Delta }}{V}_{\max }﹩/﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{in}}﹩). The vertical dashed lines show their median values. In the upper-right corner of each panel, the corresponding normalized probability densities are presented. The normalized probability densities are presented as log scales, and the values in the x-axis are binned as linear scales.
Paper: Relative Velocities between 13CO Structures within 12CO Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Xuepeng Chen, Yang Su, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Min Fang, Fujun Du, Yan Sun, Hongchi Wang, Ye Xu
Figure caption: Number distributions of the relative velocities (ΔV LOS) and their ratios with internal velocity dispersions of 13CO structures (ΔV LOS/﹩{\sigma }_{{}^{13}\mathrm{CO},\mathrm{in}}﹩) for MCs with double 13CO structures. The “Near” represents MCs with central velocities ranging from −30 to 25 km s−1, and the “Far” means clouds with central velocities in a range of −95 to −30 km s−1. The vertical dashed lines denote the corresponding median values. In the upper-right corner of each panel, the corresponding normalized probability densities are presented. The normalized probability densities are presented as log scales, and the values in the x-axis are binned as linear scales.
Paper: Relative Velocities between 13CO Structures within 12CO Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Xuepeng Chen, Yang Su, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Min Fang, Fujun Du, Yan Sun, Hongchi Wang, Ye Xu
Figure caption: Relative velocities along the line of sight between 13CO structures (ΔV LOS) in MCs with double and triple 13CO structures. A single MC with double 13CO structures has one ΔV LOS. A single MC with triple 13CO structures has three ΔV LOS between each of two 13CO structures or two ΔV MST between each pair of 13CO structures connected by the MST algorithm.
Paper: Relative Velocities between 13CO Structures within 12CO Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Xuepeng Chen, Yang Su, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Min Fang, Fujun Du, Yan Sun, Hongchi Wang, Ye Xu
Figure caption: Distribution of relative velocities between 13CO structures for 185 MCs in the “triple” regime. The gray histograms represent the whole 555 ΔV LOS from the arbitrary two 13CO structures within 185 samples. The green histograms mean the 370 ΔV MST between the 13CO structures connected through the MST algorithm, there are two ΔV MST within a cloud. The corresponding vertical dashed lines show their median values. In the upper-right corner of each panel, the corresponding normalized probability densities are presented. The normalized probability densities are presented as log scales, and the values in the x-axis are binned as linear scales.
Paper: Relative Velocities between 13CO Structures within 12CO Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Xuepeng Chen, Yang Su, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Min Fang, Fujun Du, Yan Sun, Hongchi Wang, Ye Xu
Figure caption: Histogram of the number of clouds along the line of sight in each pixel. The y-axis is given in fractions of the total number of pixels in the region of 104.°75 < l < 50.°25, ∣b∣ < 5.°25. The “All” means the line of sight with −95 < V LSR < 25 km s−1, the “Near” is along the line of sight with −30 < V LSR < 25 km s−1, and the “Far” is in a range of −95 < V LSR < −30 km s−1.
Paper: Relative Velocities between 13CO Structures within 12CO Molecular Clouds
Authors: Lixia Yuan, Ji Yang, Xuepeng Chen, Yang Su, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Min Fang, Fujun Du, Yan Sun, Hongchi Wang, Ye Xu
Figure caption: Schematic illustrations of the two kinds of combination modes for MCs with triple 13CO structures.
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: Big picture of multiple gas layers toward the Cygnus region. We divide clouds with distance measurement (see Tables 1, 2, and 3) into three intervals: [500, 1000] pc in red, [1000, 1400] pc in green, and [1400, 3000] pc in black. Lighter contours indicate nearer distance for each layer, while the darker shows the farther distances. Gray-scale maps are reconstructed by identified clouds from ACORNS, while their boundaries are delineated using a low-pass filtering method (butterworth in Python). The dashed ellipse shows a large-scale molecular loop with diameter of ∼56 pc at a distance of 800 pc. Different layers are also annotated in the [500, 1000] pc map. Middle map includes two layers, the ≈1 kpc clouds in light green, and ∼1.3 kpc clouds in green. Clouds in ≥1.4 kpc layer without contours are MCs associated with masers and/or mid-IR bright features in Tables 2 and 3. 7 clouds in Table 1 are successfully measured in this layer. Blue ellipses show OB associations and SNR, while boxes show the masers in Table 2.
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: Left panel: 13CO (white contours in [5, 15, 25, 35, 45, 55]×σ, σ is the noise level of intensity map) and C18O emission (colormap) in [−3, 3] km s−1 toward S106. 5% system error of the distances is labeled for identified 13CO structures. The location of H II region (yellow circle) and maser (white box) are also labeled on the map. Right panel: the different velocity structures labeled in black and red dots in the velocity–latitude coordinates from Gaussian decomposition (see details in Section 5.5). The blue square with error represents the observed maser from Xu et al. (2013).
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: A validation of coherent structures (ID 118 in Table 1) identified by ACORNS based on Gaussian decomposition. We chose substructures of the large MC structure by manually marked boxes and hierarchical trunks (colored contours). Their distances are marked by blue squares and green triangles, respectively, while their confidence intervals (added 5% system error of Gaia) are denoted by error bars. The 1σ confidence interval of distance is plotted in gray area of panel (c). In lower right panel, it is a 3D PPV scatter plot of centroid velocities of the cloud. All structures (other colors) overlaid with the cloud (in green) along LOS are also drawn, showing coherent velocity structures in PPV space.
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: Upper panel: 13CO (white contours in [5, 15, 25, 35, 45, 55] × σ, σ is the noise level of intensity map) and C18O emission (colormap) in [0, 6] km s−1 toward L914. 5% system error of the distances is labeled for identified 13CO structures. Lower panel: moment 1 map of centroid velocities extracted from Gaussian decomposition for the above velocity 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: The same as Figure A1, but for MC L889 toward the Cygnus X South region.
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: (a) Deviation between distances derived from emcee and preset distances in a relation with increasing ΔA  G . (b) Uncertainties of distances derived from emcee in a relation with increasing ΔA  G .
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: Comparison of distance measurements with different sampling modules. (a) The emcee module vs. Pymc3 module in our samples. (b) Distance derived from different modules vs. preset distance in mock data.
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: Two examples of measuring distance with mock data based on the Bayes model. Details in the panels can be seen in the caption of Figure 4, but points in lower panel are for the mock data.
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: All on-cloud stars (red+black region in Figure 4) vs. overlap-removed on-cloud stars (red region in Figure 4).