adsabs/AstroCLIMB huggingface dataset:
Paper: Free-floating Planet Mass Function from MOA-II 9 yr Survey toward the Galactic Bulge
Authors: Takahiro Sumi, Naoki Koshimoto, David P. Bennett, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Extinction-free color–magnitude diagram of gb3-7-6. The orange curve is the isochrone matched to this subfield. The cyan square is the RCG centroid. The red circles with error bars are sources of the 13 FSPL events in this work. The blue filled circles indicate the two FFP candidates in this work. The black open and filled circles are FSPL events and FFP events from Gould et al. (2022), respectively. The purple triangle indicates the source of terrestrial FFP OGLE-2016-BLG-1928S (Mróz et al. 2020).
Paper: Free-floating Planet Mass Function from MOA-II 9 yr Survey toward the Galactic Bulge
Authors: Takahiro Sumi, Naoki Koshimoto, David P. Bennett, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Integrated detection efficiencies, ﹩\tilde{\epsilon }({t}_{{\rm{E}}};{\rm{\Gamma }})﹩, as a function of the timescale t E down to the source magnitude of I  s  < 21.4 mag for the criteria CR2. Red, black, green, and blue lines indicate the efficiencies of fields with the highest, high, medium, and low cadence, respectively.
Paper: Free-floating Planet Mass Function from MOA-II 9 yr Survey toward the Galactic Bulge
Authors: Takahiro Sumi, Naoki Koshimoto, David P. Bennett, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Observed cumulative distribution of θ E for 13 FSPL events from MOA (red line) and 29 FSPL events from KMTNet (black line; Gould et al. 2022). The blue line indicates θ E = 0.842 ± 0.064 for terrestrial-mass FFP candidate OGLE-2016-BLG-1928 (Mróz et al. 2020).
Paper: Free-floating Planet Mass Function from MOA-II 9 yr Survey toward the Galactic Bulge
Authors: Takahiro Sumi, Naoki Koshimoto, David P. Bennett, Nicholas J. Rattenbury, Fumio Abe, Richard Barry, Aparna Bhattacharya, Ian A. Bond, Hirosane Fujii, Akihiko Fukui, Ryusei Hamada, Yuki Hirao, Stela Ishitani Silva, Yoshitaka Itow, Rintaro Kirikawa, Iona Kondo, Yutaka Matsubara, Shota Miyazaki, Yasushi Muraki, Greg Olmschenk, Clément Ranc, Yuki Satoh, Daisuke Suzuki, Mio Tomoyoshi, Paul . J. Tristram, Aikaterini Vandorou, Hibiki Yama, Kansuke Yamashita
Figure caption: Posterior distributions of the parameters of the PL model for sample CR2. The vertical red dotted lines indicate the median and ±1σ. The vertical orange line indicates the best fit.
Paper: Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters
Authors: Xiaoying Pang, Yifan Wang, Shih-Yun Tang, Yicheng Rui, Jing Bai, Chengyuan Li, Fabo Feng, M. B. N. Kouwenhoven, Wen-Ping Chen, Rwei-ju Chuang
Figure caption: The correlation between the completeness-corrected binary fraction for q > 0.4 computed in Section 3.3 and the stellar density within the half-mass radius (a). The blue dots are clusters with ages less than 100 Myr, while the orange dots are older than 100 Myr. Two orange dots with black circles are outliers: the disrupted cluster Group X, which fragments into two overdensities, and the tidal tail cluster Mamajek 4, with very low central density. In panel (b), we display the radial binary fraction vs. the radial stellar density in each cluster, for regions with a binary number of more than five. The blue dots refer to the binary fraction and stellar density for stars within the half-mass radius r h; the orange dots to stars between r h and 2r h; and the green dots to stars between 2r h and 3r h. The gray dots show the mean values of each bin with the same number of clusters. The vertical error bar is the standard deviation of the binary fraction in each bin. The meanings of the quantities s and p are identical to those in Figure 2.
Paper: Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters
Authors: Xiaoying Pang, Yifan Wang, Shih-Yun Tang, Yicheng Rui, Jing Bai, Chengyuan Li, Fabo Feng, M. B. N. Kouwenhoven, Wen-Ping Chen, Rwei-ju Chuang
Figure caption: (a) The relation between the binary fraction for q > 0.4 identified in Section 3.1 (blue dots) and the distances of the clusters. The error bar of ﹩{f}_{\mathrm{bin}}^{q\gt 0.4}﹩ is estimated in Section 3.2. The orange dots are average values of cluster distance and ﹩{f}_{\mathrm{bin}}^{q\gt 0.4}﹩ for all 17 clusters in each bin, with the standard deviation indicated by the error bar. (b) Dependence of the completeness fraction on distance. f comp is estimated from Gaia’s angular resolution limit at a given distance taken from Table 2. (c) Binary fraction after incompleteness correction ﹩{f}_{\mathrm{binc}}^{q\gt 0.4}﹩ vs. cluster distance. The error bar of ﹩{f}_{\mathrm{binc}}^{q\gt 0.4}﹩ is propagated from the error estimated in Section 3.2. The computation scheme of the orange dots is identical to that in (a). The quantity s is the Spearman’s rank correlation coefficient, and p is the probability of the null hypothesis (that no correlation exists between two variables) of the correlation test. A p value of less than 0.1 means that the null hypothesis is rejected.
Paper: Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters
Authors: Xiaoying Pang, Yifan Wang, Shih-Yun Tang, Yicheng Rui, Jing Bai, Chengyuan Li, Fabo Feng, M. B. N. Kouwenhoven, Wen-Ping Chen, Rwei-ju Chuang
Figure caption: The radial dependence of the binary fraction on the clustercentric distance for the representative clusters of each of the four morphological types. These clusters are selected based on the number of both binary and single stars being greater than 28. The clustercentric distance is in the unit of half-mass radius r h. The types of clusters are marked with different colors. The horizontal dashed line indicates the value of ﹩{f}_{\mathrm{binr}}^{q\gt 0.4}﹩ for the first bin (within r h). The gray bars indicate the errors of the binary fraction of each annulus, which is the standard deviation of the sampling distribution of the binary fraction. The color coding is identical to that in Figure 5.
Paper: Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters
Authors: Xiaoying Pang, Yifan Wang, Shih-Yun Tang, Yicheng Rui, Jing Bai, Chengyuan Li, Fabo Feng, M. B. N. Kouwenhoven, Wen-Ping Chen, Rwei-ju Chuang
Figure caption: The stellar mass function for three regions along the semimajor axis d  a  of the best-fitting ellipsoid of each representative cluster shown in Figure 6. The 3D position of each star is transformed into the coordinate system spanned by d  a , d  b , and d  c , which are the the semimajor, semimediate, and semiminor axes of the best-fitted ellipsoid from Pang et al. (2022b). The blue curve represents the mass function in the inner region, a few parsecs away from the center in the d  a  direction. The orange and green curves are mass functions in the region on the left side (negative d  a  values) and right side (positive d  a  values) of the inner region along the d  a  direction. The best fit to the mass function of each region is indicated with the dotted colored lines, whose slopes, α, and corresponding uncertainties are indicated in the upper right corner of each panel. The vertical gray dashed line is the Gaia completeness limit at the distance of the cluster.
Paper: Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters
Authors: Xiaoying Pang, Yifan Wang, Shih-Yun Tang, Yicheng Rui, Jing Bai, Chengyuan Li, Fabo Feng, M. B. N. Kouwenhoven, Wen-Ping Chen, Rwei-ju Chuang
Figure caption: The distribution of the dispersion of the 1D tangential velocity, along the R.A. and decl. The velocity dispersion value is computed using the MCMC method (see Section 6). The circles indicate the dispersion values obtained from stars within the half-mass radius r h and the triangles indicate stars outside r h. The colors of the symbols are scaled with the cluster age (color bar). The dashed and dashed–dotted lines show the linear fits to the correlation of ﹩{\sigma }_{{\mu }_{\alpha }}﹩ and ﹩{\sigma }_{{\mu }_{\alpha }\cos \delta }﹩ for the regions outside and inside r h, respectively, with errors taken into consideration. The histograms in the upper and right panels represent the values of ﹩{\sigma }_{{\mu }_{\alpha }\cos \delta }﹩ and ﹩{\sigma }_{{\mu }_{\alpha }}﹩ for the stars inside r h (blue) and outside r h (red). The blue and red dashed lines in the upper and right panels denote the mean values of ﹩{\sigma }_{{\mu }_{\alpha }\cos \delta }﹩ and ﹩{\sigma }_{{\mu }_{\alpha }}﹩ for stars inside and outside r h, respectively.
Paper: Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters
Authors: Xiaoying Pang, Yifan Wang, Shih-Yun Tang, Yicheng Rui, Jing Bai, Chengyuan Li, Fabo Feng, M. B. N. Kouwenhoven, Wen-Ping Chen, Rwei-ju Chuang
Figure caption: The dependence of the radial binary fraction on clustercentric distance in the unit of half-mass radius r h in four types of clusters: filamentary (a), fractal (b), halo (c), and tidal tail (d). The three colored rectangles for each type indicate the values for stars within r h, between r h and 2r h, and between 2r h and 3r h. The colored rectangles indicate the inner quartile range (IQR, 75th percentile minus 25th percentile). The median value is indicated with a horizontal line. The upper and lower whiskers of each colored rectangle mark the maximum and minimum values within 1.5 IQR. Clusters outside 1.5 IQR (whiskers) are outliers indicated as open circles: Collinder 69 (blue circle) and Collinder 350 (green circle).
Paper: Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters
Authors: Xiaoying Pang, Yifan Wang, Shih-Yun Tang, Yicheng Rui, Jing Bai, Chengyuan Li, Fabo Feng, M. B. N. Kouwenhoven, Wen-Ping Chen, Rwei-ju Chuang
Figure caption: The relations between the completeness-corrected binary fraction for q > 0.4 identified in Section 3.3 and the age of the cluster (panel (a)) and the cluster total masses (panel (b)). The error bar of ﹩{f}_{\mathrm{binc}}^{q\gt 0.4}﹩ is propagated from the error estimated in Section 3.2. The orange dots represent the average values of the cluster distances and ﹩{f}_{\mathrm{binc}}^{q\gt 0.4}﹩ for all 17 clusters in each bin, with the standard deviation indicated with error bars. The Spearman's rank correlation coefficient s and the probability of the null hypothesis p are indicated in the upper right corner of each panel. The meanings of the quantities s and p are identical to those in Figure 2.
Paper: Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters
Authors: Xiaoying Pang, Yifan Wang, Shih-Yun Tang, Yicheng Rui, Jing Bai, Chengyuan Li, Fabo Feng, M. B. N. Kouwenhoven, Wen-Ping Chen, Rwei-ju Chuang
Figure caption: The dependence of the mean mass on clustercentric distance for the representative clusters of each of the four types shown in Figure 6. The size of each annulus is the half-mass radius r h of each cluster. Each dot represents the mean mass in the annulus, and the error bar indicates the standard deviation in each bin. The horizontal dashed line indicates the smallest mean mass value among all bins. The color coding is identical to that of Figure 6.
Paper: Binary Star Evolution in Different Environments: Filamentary, Fractal, Halo, and Tidal Tail Clusters
Authors: Xiaoying Pang, Yifan Wang, Shih-Yun Tang, Yicheng Rui, Jing Bai, Chengyuan Li, Fabo Feng, M. B. N. Kouwenhoven, Wen-Ping Chen, Rwei-ju Chuang
Figure caption: The dependence of the bias in the 1D tangential velocity along the decl. direction on the binary semimajor axis a and the mass ratio q. When calculating the bias, we assume a primary mass of 1 M ⊙. The color bar indicates the average 1D tangential velocity bias along the decl. direction.
Paper: Understanding the Capability of Future Direct-imaging Observations to Quantify Atmospheric Chemical Effects of Stellar Proton Events
Authors: Georgios P. Afentakis, Kyla Mullaney, Howard Chen, John Blalack, Jade Checlair, Dorian S. Abbot
Figure caption: NO2 S/N for the flare at days 58 in Figure 2 for different integration periods. We integrate the signal before the flare over 5 (dashed line) or 10 (solid line) days and after the flare has begun over a range of days (horizontal axis). We perform calculations both including clouds (blue) and without clouds (black).
Paper: Understanding the Capability of Future Direct-imaging Observations to Quantify Atmospheric Chemical Effects of Stellar Proton Events
Authors: Georgios P. Afentakis, Kyla Mullaney, Howard Chen, John Blalack, Jade Checlair, Dorian S. Abbot
Figure caption: NO2 S/N as a function of observing phase and distance for the O2-rich and O2-poor K-star scenarios. The black line marks a detectable S/N of 3. We use integration periods of 2 days after the flare and 10 days before the flare in this plot. These calculations include clouds.
Paper: A Comparison of the Composition of Planets in Single-planet and Multiplanet Systems Orbiting M dwarfs
Authors: Romy Rodríguez Martínez, David V. Martin, B. Scott Gaudi, Joseph G. Schulze, Anusha Pai Asnodkar, Kiersten M. Boley, Sarah Ballard
Figure caption: Left: Histograms of the [Fe/H] of the single-planet (purple) and multiplanet (pink) host stars for the full sample (top) and for the subsample excluding R  p  ≥ 6 R ⊕ planet host stars (bottom). The vertical dashed lines denote the median values of each distribution. Right: Empirical cumulative distribution functions of the samples, with their Kolmogorov–Smirnov statistic values overplotted. f threshold is explained in Section 4.3.
Paper: A Comparison of the Composition of Planets in Single-planet and Multiplanet Systems Orbiting M dwarfs
Authors: Romy Rodríguez Martínez, David V. Martin, B. Scott Gaudi, Joseph G. Schulze, Anusha Pai Asnodkar, Kiersten M. Boley, Sarah Ballard
Figure caption: Left: Core mass fraction as a function of the orbital period for the 24 likely rocky planets in our sample with M  p  < 10 M ⊕. The blue, and red horizontal dashed lines are the weighted average CMFs of the singles and multiples, respectively. We do not find any correlation between the CMF and period. The red and blue bands are 1σ confidence intervals on the mean. Right: Core/Water mass fractions as a function of the planet mass. The circles are multis and squares are singles. The Earth, with a CMF of 0.33, is plotted for reference in both plots.
Paper: A Comparison of the Composition of Planets in Single-planet and Multiplanet Systems Orbiting M dwarfs
Authors: Romy Rodríguez Martínez, David V. Martin, B. Scott Gaudi, Joseph G. Schulze, Anusha Pai Asnodkar, Kiersten M. Boley, Sarah Ballard
Figure caption: Left: Planet radius as a function of the stellar [Fe/H] metallicity for all planet hosts with measured metallicities. The points are color coded by planet multiplicity. Right: Planet radius as a function of the orbital period for the same sample on the left.
Paper: A Comparison of the Composition of Planets in Single-planet and Multiplanet Systems Orbiting M dwarfs
Authors: Romy Rodríguez Martínez, David V. Martin, B. Scott Gaudi, Joseph G. Schulze, Anusha Pai Asnodkar, Kiersten M. Boley, Sarah Ballard
Figure caption: Average [Fe/H] metallicity of M dwarfs hosting 1, 2, 3, and 4+ planets for our full sample (top) and for the subset of planets with R  p  < 6 R ⊕ (bottom). The error bars show the dispersion in the metallicity for each multiplicity. The shaded blue region shows the confidence interval for the slope.
Paper: A Comparison of the Composition of Planets in Single-planet and Multiplanet Systems Orbiting M dwarfs
Authors: Romy Rodríguez Martínez, David V. Martin, B. Scott Gaudi, Joseph G. Schulze, Anusha Pai Asnodkar, Kiersten M. Boley, Sarah Ballard
Figure caption: Left: Histograms of the rotation periods of single-planet (purple) and multiplanet (pink) host stars for the full sample (top) and for the subsample excluding R  p  ≥ 6 R ⊕ planet host stars (bottom). The vertical dashed lines denote the median values of each distribution. Right: Empirical cumulative distribution functions of the samples, with their Kolmogorov–Smirnov statistic values overplotted. f threshold is explained in Section 4.3.
Paper: Speckle Interferometry at SOAR in 2022
Authors: Brian D. Mason, Andrei Tokovinin, Rene A. Mendez, Edgardo Costa
Figure caption: Selected new orbital solutions, plotted together with all published data in the WDS database as well as the new data in Table 2. In each of these figures, micrometric observations are indicated by plus signs, interferometric measures by filled circles, conventional CCD by pink triangles, space-based measures are indicated by the letter “H,” new measures from Table 2 are plotted as a filled star. “O−C” lines connect each measure to its predicted position along the new orbit (shown as a thick solid line). A dotted–dashed line indicates the line of nodes, and a curved arrow in the lower right corner of each figure indicates the direction of orbital motion. The earlier orbit referenced in Table 5 is shown as a dashed ellipse. For the combined orbit of 17304−0104 = STF2173, plots of the relative astrometry and the radial velocity curve are provided.
Paper: Speckle Interferometry at SOAR in 2022
Authors: Brian D. Mason, Andrei Tokovinin, Rene A. Mendez, Edgardo Costa
Figure caption: Fragments of speckle ACFs of six newly resolved triple stars. The spatial and intensity scale is chosen for best representation of each system. Blue letters mark the ACF peaks corresponding to the components’ location, O marks the ACF center. The outer and inner separations are indicated.
Paper: The ﹩\dot{M}﹩–M disk Relationship for Herbig Ae/Be Stars: A Lifetime Problem for Disks with Low Masses?
Authors: Sierra L. Grant, Lucas M. Stapper, Michiel R. Hogerheijde, Ewine F. van Dishoeck, Sean Brittain, Miguel Vioque
Figure caption: The ﹩\dot{M}﹩–M disk relationship for the Herbig Ae/Be stars broken up by group classification (group I sources in red and group II sources in blue). Upper limits are the same as in Figure 1. ALMA continuum images from Stapper et al. (2022) are shown for each object with a 100 au scale bar and the beam at the bottom of each image. If the disk is unresolved in the ALMA observations, the beam is shown in red.
Paper: JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Marie Ygouf, Anthony Boccaletti, Thomas P. Greene, John Krist, Peter Plavchan, Marcia J. Rieke, Thomas L. Roellig, John Stansberry, John P. Wisniewski, Erick T. Young
Figure caption: Top: 5σ companion detection limits in mJy for both filters—computed as described in Section 5. The right y-axis provides the corresponding mass limits for each filter in Jupiter masses—using AMES-Cond and cloud-free petitCODE isochrones as outlined in Section 5. Middle: 5σ contrast curves for the same reductions, adopting the model-based stellar fluxes for AU Mic indicated in the upper right corner (see Section 5). Bottom: the ratio of the companion throughput for the RDI-LOCI and MCRDI procedures. The improvement for MCRDI persists up to approximately the edge of the outer optimization region used for construction of the starlight model (r = 2.″205 = 35 pixels). For all panels, the x-axis indicates the projected stellocentric separation of the measurement—in arcsec on the lower x-axis and in au on the upper x-axis. The relatively gentle slope of the coronagraph’s transmission profile permits some sensitivity to sources at smaller separations than the IWA of 0.″63 (dotted gray line).
Paper: JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Marie Ygouf, Anthony Boccaletti, Thomas P. Greene, John Krist, Peter Plavchan, Marcia J. Rieke, Thomas L. Roellig, John Stansberry, John P. Wisniewski, Erick T. Young
Figure caption: The absolute value of disk-model-subtracted images for MCRDI and classical RDI reductions in F444W, oriented as in Figure 1. Each image has been multiplied by the projected radial separation in units of arcsec and is presented with a linear color stretch. The dotted black contour outlines the extent of the disk model, with two previously identified background sources indicated by the blue and red dotted circles. As a reference for the depth of the imagery, based on Linder et al. (2019) models, the brightness of the background source circled in red would correspond to a foreground companion with a mass comparable to Saturn’s, while the brightness of the source circled in blue would correspond to a mass of ∼0.12 M  J .
Paper: JWST/NIRCam Coronagraphy of the Young Planet-hosting Debris Disk AU Microscopii
Authors: Kellen Lawson, Joshua E. Schlieder, Jarron M. Leisenring, Ell Bogat, Charles A. Beichman, Geoffrey Bryden, András Gáspár, Tyler D. Groff, Michael W. McElwain, Michael R. Meyer, Thomas Barclay, Per Calissendorff, Matthew De Furio, Marie Ygouf, Anthony Boccaletti, Thomas P. Greene, John Krist, Peter Plavchan, Marcia J. Rieke, Thomas L. Roellig, John Stansberry, John P. Wisniewski, Erick T. Young
Figure caption: Starlight-subtracted and roll-combined final images of AU Mic for the F356W (top row) and F444W (bottom row) filters using a variety of starlight subtraction techniques (as indicated by the column labels and described in 3.3). The black plus sign and dashed circle indicate the approximate coronagraph center and IWA, respectively. Interior to the IWA, coronagraph transmission decreases and is at least partially responsible for the intensity deficit. The images for a given filter are displayed with the same linear color stretch, as indicated by the colorbar at the end of each row. A mapping symmetric about zero is chosen to highlight the effects of RDI oversubtraction and speckle mismatch where present.