adsabs/AstroCLIMB huggingface dataset:
Paper: Real-time Collision-free Motion Planning for Next-generation Fiber Positioners in LAMOST
Authors: Guifeng Chen, Zhen Zhang, Chunhui Su, YongGang Gu, Chao Zhai
Figure caption: The next-generation fiber positioner in LAMOST has two rotational axes, driven by independent gearmotors. Three positioners form a set with an electronics board.
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: Left: target confusion map ﹩{ \mathcal D }(\{{p}_{1},{p}_{2}\},{\rm{\Sigma }})﹩, where ﹩{p}_{1}=({{\boldsymbol{\theta }}}_{{p}_{1}}=({\delta }_{x,1}=0,{\delta }_{y,1}=0),{{\boldsymbol{F}}}_{{p}_{1}}={F}_{{p}_{1}})﹩ is a monochromatic point source at a fixed position and ﹩{p}_{2}=({{\boldsymbol{\theta }}}_{{p}_{2}}=({\delta }_{x,2},{\delta }_{y,2}),{{\boldsymbol{F}}}_{{p}_{2}}={F}_{{p}_{2}})﹩ is a monochromatic point source compared to the Airy disk in light green, where ﹩\delta ={({\delta }_{x,2}^{2}+{\delta }_{y,2}^{2})}^{1/2}﹩. Σ is a diagonal constant covariance matrix representing white background noise. When p1 and p2 are close, the output from P looks like one point source, i.e., ﹩{ \mathcal D }\gt 0﹩. When far apart, the output from P does not look like one point source, i.e., ﹩{ \mathcal D }\lt 0﹩. ﹩{F}_{{p}_{1}}/{F}_{{p}_{2}}﹩ is the luminosity flux ratio. Right: target confusion map ﹩{ \mathcal D }(\{{p}_{1},{p}_{2}\},{\rm{\Sigma }})﹩ of a configuration of two monochromatic point sources P = {p1, p2}, where ﹩{p}_{1}=({\delta }_{x,1}=0,{\delta }_{y,1}=0,{{\boldsymbol{F}}}_{{p}_{1}})﹩ is fixed for different luminosity flux ratios. In red is the resolution map ﹩{ \mathcal R }(\{{p}_{1}\},{F}_{{p}_{2}})﹩ for different luminosity flux ratios ﹩{F}_{{p}_{1}}/{F}_{{p}_{2}}﹩. At ﹩{F}_{{p}_{1}}={F}_{{p}_{2}}﹩, ﹩{ \mathcal R }={\delta }_{1}﹩. Spatial resolution δ1 ≈ 0.952 δRayleigh, where δRayleigh refers to the classical notion of resolution, i.e., the first zero of the Airy disk. This figure is a generalization of the plot in the left panel.
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: Conceptual examples of photobombing (left) and no photobombing (right) cases. “Output space” represents all images for traditional telescopes or time series for LIFE. “no ps” represents the output when there is no point source, i.e., a black image or flat time series. “1 ps space” represents all noiseless images/time series that one fixed point source can produce. Analogously, “2 ps space” represents all noiseless images/time series that two fixed point sources can produce. q⋆ is the one point source that minimizes the loss with P, i.e., P’s projection to the generated one point source subspace. In green is the smallest distance of the four distances according to the similarity notion, which is the loss. If the smallest distance, in green, is between P and q⋆, then ﹩{ \mathcal D }\gt 0﹩, and by definition, contamination can occur; otherwise, contamination does not occur. Similar to the Rayleigh criterion, the condition ﹩{ \mathcal D }\gt 0﹩ is more about the possibility and impossibility of contamination rather than contamination in the absolute sense. Notice that “no ps” ⊂ “1 ps” ⊂ “2 ps.”
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: Top: normalized target confusion map ﹩{ \mathcal D }﹩ (Equation (13)) for ﹩{p}_{1}=((0.6\cdot {\delta }_{\,\rm{null}\,},0),{{\boldsymbol{F}}}_{{p}_{1}})﹩ (black dot) with homogeneous luminosity flux ﹩{{\boldsymbol{F}}}_{{p}_{1}}={F}_{{p}_{1}}{\bf{1}}﹩ across the full wavelength range, λ from 4 μm to 18.5 μm, and a spectral resolution of 20. At each point where (δx, δy) is computed, the target confusion map is evaluated at P = {p1, p2}, where ﹩{p}_{2}=(({\delta }_{x},{\delta }_{y}),{{\boldsymbol{F}}}_{{p}_{2}}=0.5{F}_{{p}_{1}}{\bf{1}})﹩ with constant noise independent from P, i.e., σ(λ) = σ. When p2 is outside the red region, photobombing does not occur. The red region is independent from ﹩{F}_{{p}_{1}}﹩ and σ. In this case, bim = 6bnull and ﹩{ \mathcal R }\approx 0.08\,{\delta }_{\,\rm{null}\,}﹩. Middle: zoom in the region of local photobombing; i.e., two point sources look like one nonexisting point source, and they appear in close proximity. Bottom: zoom in the region of nonlocal photobombing; i.e., two point sources look like one nonexisting point source, and they do not appear in close proximity.
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: Top: normalized differential transmission map T at λ = λ0 = 10 μm (Equation (35)) compared to the apparent position of a star at the center and the apparent path of two exoplanets with an apparent angle of δr = 0.65δnull and δr = 0.88δnull from its star after rotating LIFE about the LIFE–star axis. The second and third plots are the normalized time series of the corresponding planets in the top plot. Bottom: normalized time series of the total signal of the planets in the top plot, where planet 1 (blue) has twice the luminosity of planet 2 (orange) at λ = 10 μm.
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: Normalized expected signal intensity for a blackbody radiating point source at temperature 280 K with a maximum semimajor axis angle of δr. Black is the signal intensity at λ = 10 μm and face-on, i.e., ϕ = 0. Blue is averaged over orbital angle θ face-on. Orange is averaged over orbital angle θ edge-on, i.e., ϕ = π/2 rad. Red is averaged over θ and ϕ. Without any information about ϕ, we set the baseline such that the apparent HZ center radius angle δHZ matches 0.91 ⋅ δnull.
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: Screen outputs from two point sources of light with an apparent angular distance between them of l, where x0 = δRayleigh.
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: X-architecture rotating interferometer setup. The current LIFE design has a scaling factor of q = 6 and nulling baseline bnull that can be adjusted from 10 m to 100 m. For details about this setup, see S. P. Quanz et al. (2022).
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: Conventional telescope setup with circular aperture. Far field approximation D > > L. Diameter d = 2s, where s is the radius of the circular aperture.
Paper: Potential Subsurface Lava Tube Skylight on the Western Flank of Elysium Mons, Mars
Authors: Ravi Sharma, Chunyu Ding, Yan Su, Zhonghan Lei, Changzhi Jiang, Jiangwan Xu, YuXiao Zhi, Zihang Liang, Jiawei Li, Xiaohang Qiu, Haoyu Chen, S. N. A. Jaaffrey
Figure caption: Elevation map of the western flank of Elysium Mons, integrating data from MOLA/MGS (D. E. Smith et al. 2001; D. Smith et al. 2003) and imagery from CTX/MRO (M. C. Malin et al. 2007). Contour lines at 100 m intervals illustrate the topographic gradient across the study area. The PCC, marked as a red star, is located within the AHv (K. Tanaka et al. 2014). The map highlights the PCC’s position at a relatively low elevation, enhancing its potential accessibility for future exploration.
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: Top: the detection probability for habitable planets for the entire LIFEsim survey (500 universes, ≈1700 systems each). The detection probability is the probability that a habitable planet has an S/N over 7 after 100 hr of observation, while assuming that the planet does not move during the observation. To better see the distribution, the left and right bars are cut off. They represent, respectively, 90.78% and 4.07% of the planets. A total of 7.93% of the planets have a detection rate over 50%. Bottom: the contamination probability for detectable habitable planets, i.e., detection probability >0%. The contamination probability is the probability of a detected planet being contaminated by another planet in the same system. Similarly, the first bar is cut off and represents 76.59% of cases.
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: Error δ1({λ}) − δC,11 in the number of iterations, where δC,11 is δ1({λ}) computed at 11 iterations. One iteration corresponds to steps 2 and 3 in the numerical method described in Section 2.6.
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: In red is the probability 1 − P2(T) to have contamination at time t + T after having contamination on the first visit at time t for TRAPPIST-1 e. Dashed red is 1 − PC, where PC is the contamination probability of TRAPPIST-1 e. In black is the probability 1 − PO(T) of no contamination during an observation of time T. We read that the uncorrelation time is 15 hr. We notice that 1 − PO(T > 2 days) ≈ 0. Hence, in this case, considering that the system does not change for observations, >15 hr is a bad approximation.
Paper: Potential Subsurface Lava Tube Skylight on the Western Flank of Elysium Mons, Mars
Authors: Ravi Sharma, Chunyu Ding, Yan Su, Zhonghan Lei, Changzhi Jiang, Jiangwan Xu, YuXiao Zhi, Zihang Liang, Jiawei Li, Xiaohang Qiu, Haoyu Chen, S. N. A. Jaaffrey
Figure caption: APC classified into their types (I, II, and III) based upon morphological investigation, adopted from G. E. Cushing et al. (2015).
Paper: Potential Subsurface Lava Tube Skylight on the Western Flank of Elysium Mons, Mars
Authors: Ravi Sharma, Chunyu Ding, Yan Su, Zhonghan Lei, Changzhi Jiang, Jiangwan Xu, YuXiao Zhi, Zihang Liang, Jiawei Li, Xiaohang Qiu, Haoyu Chen, S. N. A. Jaaffrey
Figure caption: Location map of the studied PCC on Mars, created using data from the Mars Cave Catalog (G. E. Cushing 2015) and overlaid on MOLA elevation data (D. E. Smith et al. 2001; D. Smith et al. 2003).
Paper: Potential Subsurface Lava Tube Skylight on the Western Flank of Elysium Mons, Mars
Authors: Ravi Sharma, Chunyu Ding, Yan Su, Zhonghan Lei, Changzhi Jiang, Jiangwan Xu, YuXiao Zhi, Zihang Liang, Jiawei Li, Xiaohang Qiu, Haoyu Chen, S. N. A. Jaaffrey
Figure caption: Illustration of the Sun–satellite geometry relative to the pit location, used to estimate the true vertical depth at the pit’s point location. The formulas and example images are adopted and modified from G. E. Cushing et al. (2015).
Paper: Photobombing for the Large Interferometer For Exoplanets (LIFE). A New Criterion for Target Confusion and Application to a Mid-infrared Rotating Nulling Interferometer
Authors: Drinor Cacaj, Daniel Angerhausen, Prabal Saxena, Romain Laugier, Jens Kammerer, Eleonora Alei, Sascha P. Quanz
Figure caption: Target confusion value ﹩{ \mathcal D }﹩ (blue) compared to the right-hand side term in Equation (12) (red) for different values of α. If ﹩{ \mathcal D }(P,{\rm{\Sigma }})\lt (\alpha -1)J(P,{Q}^{\star },{\rm{\Sigma }})﹩, then by definition of α, there is no contamination.
Paper: Thermal Variability in the Martian Upper Atmosphere within the Crustal Magnetic Field Region Induced by Gravity Wave Dissipation Due to Ion-drag Effect
Authors: Xing Wang, Xiaojun Xu, Jun Cui, Siqi Yi, Hao Gu, Zilu Zhou, Hengyan Man, Lei Luo, Peishan He, Pu Yang
Figure caption: Vertical profiles of electric conductivities and the characteristic frequencies in the altitude range of 80–300 km. (a). The Pedersen conductivity (σp) and Hall conductivity (σH) in the NCF region and strong CF region. (b). The characteristic damping frequency driven by the Pedersen and Hall conductivity marked by ωp and ωH, respectively. νni refers to the neutral-ion collisional frequency.
Paper: What if we Find Nothing? Bayesian Analysis of the Statistical Information of Null Results in Future Exoplanet Habitability and Biosignature Surveys
Authors: Daniel Angerhausen, Amedeo Balbi, Andjelka B. Kovačević, Emily O. Garvin, Sascha P. Quanz
Figure caption: Example of the posterior distributions resulting from one positive detection in 100 (perfect) observations, assuming different priors. While in linear space all priors seem to constrain the resulting value around 10−2 (or 1%), the logarithmic plot illustrates that the more “pessimistic” priors produces more statistical weight for values of ηobs much smaller than 10−2.
Paper: Thermal Variability in the Martian Upper Atmosphere within the Crustal Magnetic Field Region Induced by Gravity Wave Dissipation Due to Ion-drag Effect
Authors: Xing Wang, Xiaojun Xu, Jun Cui, Siqi Yi, Hao Gu, Zilu Zhou, Hengyan Man, Lei Luo, Peishan He, Pu Yang
Figure caption: Profiles of plasma gyro-frequency and collisional frequency in the (a) NCF region and (b) strong CF region. Electron and ion gyro-frequency marked by Ωe and Ωi, respectively; νen and νin refer to the electron-CO2 and O﹩{}_{2}^{+}﹩–CO2 collisional frequency, respectively. The shaded region illustrates the dynamo region, where Ωi ≪ νin and Ωe ≫ νen. The magnetic field strength in the NCF region and the CF region are assumed to be 20 nT and 500 nT, respectively.
Paper: Thermal Variability in the Martian Upper Atmosphere within the Crustal Magnetic Field Region Induced by Gravity Wave Dissipation Due to Ion-drag Effect
Authors: Xing Wang, Xiaojun Xu, Jun Cui, Siqi Yi, Hao Gu, Zilu Zhou, Hengyan Man, Lei Luo, Peishan He, Pu Yang
Figure caption: Vertical structures of the Martian background atmosphere in the altitude range of 80–300 km. (a). Number density profiles of the major neutral composition (CO2) and charged constituent (O﹩{}_{2}^{+}﹩). (b). Neutral background temperature denoted by T; sound speed is marked by cs; acoustic cut-off frequency and Brunt–Väisälä frequency are marked by ωa and ωb, respectively.
Paper: Thermal Variability in the Martian Upper Atmosphere within the Crustal Magnetic Field Region Induced by Gravity Wave Dissipation Due to Ion-drag Effect
Authors: Xing Wang, Xiaojun Xu, Jun Cui, Siqi Yi, Hao Gu, Zilu Zhou, Hengyan Man, Lei Luo, Peishan He, Pu Yang
Figure caption: (a) Altitude profile of wave-driven neutral density ratio. (b) Spatial distribution of the perturbed neutral density ratio. Input parameters of the selected wave mode are τ = 55.19 minutes, λx = 60 km, kz0 = −0.50 km−1, and cp =  18.12 m s−1.
Paper: What if we Find Nothing? Bayesian Analysis of the Statistical Information of Null Results in Future Exoplanet Habitability and Biosignature Surveys
Authors: Daniel Angerhausen, Amedeo Balbi, Andjelka B. Kovačević, Emily O. Garvin, Sascha P. Quanz
Figure caption: Comparison of results derived by this framework as function of the number of observations: differences in “best fit” and 99.9% upper limits between “optimistic” (flat) and “neutral/pessimistic” (Jeffreys/Kerman, extreme) prior analysis. N = 20–40 seems to be enough to be (relatively) independent of the choice of priors.
Paper: What if we Find Nothing? Bayesian Analysis of the Statistical Information of Null Results in Future Exoplanet Habitability and Biosignature Surveys
Authors: Daniel Angerhausen, Amedeo Balbi, Andjelka B. Kovačević, Emily O. Garvin, Sascha P. Quanz
Figure caption: Comparison to potential survey sizes of the HWO mission and LIFE concept (using Jeffrey’s prior).
Paper: What if we Find Nothing? Bayesian Analysis of the Statistical Information of Null Results in Future Exoplanet Habitability and Biosignature Surveys
Authors: Daniel Angerhausen, Amedeo Balbi, Andjelka B. Kovačević, Emily O. Garvin, Sascha P. Quanz
Figure caption: Left: comparison of the radius/insulation flux parameter spaces used in this paper to define the various exoplanet samples. Right: same as Figure 4 for LIFE but with a wider “optimistic habitable zone (optHZ)” sample.
Paper: A First Taste of MEAD (Measuring Extinction and Abundances of Dust). I. Diffuse Milky Way Interstellar Dust Extinction Features in JWST Infrared Spectra
Authors: Marjorie Decleir, Karl D. Gordon, Karl A. Misselt, Burcu Günay, Julia Roman-Duval, Sascha T. Zeegers
Figure caption: 3.4 μm (left) and 6.2 μm (right) hydrocarbon features, normalized to A(V) for all sightlines (in color). The average is shown in black and the standard error of the mean is shown in red. The purple dotted line shows the feature for the Quintuplet as fit by J. E. Chiar et al. (2013; C13). In the left plot, we divide the C13 profile by a factor of 2.5. The two sightlines with noisy MIRI spectra are not included in the right plot.
Paper: A First Taste of MEAD (Measuring Extinction and Abundances of Dust). I. Diffuse Milky Way Interstellar Dust Extinction Features in JWST Infrared Spectra
Authors: Marjorie Decleir, Karl D. Gordon, Karl A. Misselt, Burcu Günay, Julia Roman-Duval, Sascha T. Zeegers
Figure caption: Silicate features, ordered from weakest (bottom) to strongest (top). The skewed Gaussian fits are shown in red.
Paper: A First Taste of MEAD (Measuring Extinction and Abundances of Dust). I. Diffuse Milky Way Interstellar Dust Extinction Features in JWST Infrared Spectra
Authors: Marjorie Decleir, Karl D. Gordon, Karl A. Misselt, Burcu Günay, Julia Roman-Duval, Sascha T. Zeegers
Figure caption: 3 μm feature normalized to A(V) for HD073882 (left) and for the rest of the sample (right; in color). The average is shown in black and the standard error of the mean is shown in red. With the dashed and dotted lines, we show the renormalized profiles from M. Decleir et al. (2022) for the two dense sightlines (left) and for two diffuse sightlines with a tentative ice detection (right) from their sample.
Paper: A First Taste of MEAD (Measuring Extinction and Abundances of Dust). I. Diffuse Milky Way Interstellar Dust Extinction Features in JWST Infrared Spectra
Authors: Marjorie Decleir, Karl D. Gordon, Karl A. Misselt, Burcu Günay, Julia Roman-Duval, Sascha T. Zeegers
Figure caption: Silicate feature properties compared to A(V) and A(1500 Å), with literature measurements from K. D. Gordon et al. (2021) added in the right panels (in green).
Paper: A First Taste of MEAD (Measuring Extinction and Abundances of Dust). I. Diffuse Milky Way Interstellar Dust Extinction Features in JWST Infrared Spectra
Authors: Marjorie Decleir, Karl D. Gordon, Karl A. Misselt, Burcu Günay, Julia Roman-Duval, Sascha T. Zeegers
Figure caption: Peak wavelength, λ0, vs. peak optical depth, τ(λ0), compared to literature measurements from K. D. Gordon et al. (2021; in green). The gray data points correspond to the two sightlines with a noisy MIRI spectrum. The Spearman's rank correlation coefficients are shown in the corner (in black for the black data points, in gray for all the data points in this work, and in green for all the data points in this plot).
Paper: A First Taste of MEAD (Measuring Extinction and Abundances of Dust). I. Diffuse Milky Way Interstellar Dust Extinction Features in JWST Infrared Spectra
Authors: Marjorie Decleir, Karl D. Gordon, Karl A. Misselt, Burcu Günay, Julia Roman-Duval, Sascha T. Zeegers
Figure caption: Observed correlations between silicate feature properties. The gray data points correspond to the two sightlines with a noisy MIRI spectrum. The Spearman's rank correlation coefficients are shown in the corner of each panel (in black for only the black data points and in gray for all the data points).
Paper: A First Taste of MEAD (Measuring Extinction and Abundances of Dust). I. Diffuse Milky Way Interstellar Dust Extinction Features in JWST Infrared Spectra
Authors: Marjorie Decleir, Karl D. Gordon, Karl A. Misselt, Burcu Günay, Julia Roman-Duval, Sascha T. Zeegers
Figure caption: NIRCam and MIRI spectra (rebinned to a resolution λ/Δλ = 400) for all 9 stars in MEAD that were observed with JWST, multiplied by λ2 to flatten out the decreasing Rayleigh–Jeans tail of the stellar spectrum at these wavelengths, normalized to the mean flux*λ2 between 5 and 7.5 μm and ordered from flattest (bottom) to steepest (top) spectrum for convenient visualization.
Paper: A First Taste of MEAD (Measuring Extinction and Abundances of Dust). I. Diffuse Milky Way Interstellar Dust Extinction Features in JWST Infrared Spectra
Authors: Marjorie Decleir, Karl D. Gordon, Karl A. Misselt, Burcu Günay, Julia Roman-Duval, Sascha T. Zeegers
Figure caption: Silicate feature peak optical depth compared to hydrogen column densities and molecular hydrogen fraction.
Paper: Photometric Determination of Unresolved Main-sequence Binaries in the Pleiades: Binary Fraction and Mass-ratio Distribution
Authors: Rongrong Liu, Zhengyi Shao, Lu Li
Figure caption: Combined probability density function (PDF) of primary mass and mass ratio for our sample. The left panel shows the direct result, with grayscale representing probability density. The dashed blue line indicates the position of the binary star with a secondary mass of 0.09 ﹩{{ \mathcal M }}_{\odot }﹩. Binaries are located above this line, and single stars are below it. The solid blue line marks ﹩{{ \mathcal M }}_{1}=0.11﹩. The stars to the left of this line are incomplete and are thus excluded from the statistical analysis. The right panel presents a smoothed version of the left panel, displaying only the region for binary analysis, with color indicating probability density.
Paper: Photometric Determination of Unresolved Main-sequence Binaries in the Pleiades: Binary Fraction and Mass-ratio Distribution
Authors: Rongrong Liu, Zhengyi Shao, Lu Li
Figure caption: Comparison of binary fraction from this work with other works. The blue point indicates the comparison with a result using spectroscopic observations. Orange and green points represent comparisons with results using Gaia photometric data, with green points specifically showing high-mass-ratio binary fraction. Red points show comparisons with results that combined Gaia, 2MASS, and WISE photometric data. The black line indicates y = x.