adsabs/AstroCLIMB huggingface dataset:
Paper: The Hidden Clumps in VY CMa Uncovered by the Atacama Large Millimeter/submillimeter Array
Authors: Roberta M. Humphreys, A. M. S. Richards, Kris Davidson, A. P. Singh, L. Decin, L. M. Ziurys
Figure caption: An oblique plane in the image cube, similar to Figure 5. The vertical scale is frequency, represented by the 12CO Doppler velocity relative to the star. The horizontal axis is spatial position along a projected line oriented at position angle 120°; see Figure 4. The star’s position is marked by “+.” (a) Total observed intensity, 12CO emission plus continuum. The prominent vertical line just left of center is continuum emission from Clump C. (b) Same image after the formal continuum-subtraction process. An arrow marks the invalid dark spot shown in Figure 9 and explained in the text.
Paper: The Hidden Clumps in VY CMa Uncovered by the Atacama Large Millimeter/submillimeter Array
Authors: Roberta M. Humphreys, A. M. S. Richards, Kris Davidson, A. P. Singh, L. Decin, L. M. Ziurys
Figure caption: The continuum-subtracted 12CO line profiles at the projected centers of Clumps A, B, C, and D with a 1 pixel circular aperture. In the range −20 to −2 km s−1 on the left side, the shaded areas represent an opaque outlying shell which conceals the inner ejecta (Figure 8 and Section 6). As explained in the text, the two dashed curves represent locations 100 mas NW and SE of the center of Clump D (NW is brighter; see Figure 5). A fifth panel shows the intensity along the line of sight to the star, but this emission arises in circumstellar ejecta rather than the star.
Paper: The Hidden Clumps in VY CMa Uncovered by the Atacama Large Millimeter/submillimeter Array
Authors: Roberta M. Humphreys, A. M. S. Richards, Kris Davidson, A. P. Singh, L. Decin, L. M. Ziurys
Figure caption:  12CO spatial images at Doppler velocity V rel* −27 km s−1. At this frequency the outer ejecta are optically thick, hiding the inner ejecta. (a) Observed intensity, almost entirely 12CO emission. (b) Result of the formal continuum-subtraction procedure, which is valid at most other frequencies. The prominent central dark spot is an illusory negative image of continuum from Clump C. In both images the mottled mesh pattern is an artifact of the interferometry reduction process.
Paper: The Hidden Clumps in VY CMa Uncovered by the Atacama Large Millimeter/submillimeter Array
Authors: Roberta M. Humphreys, A. M. S. Richards, Kris Davidson, A. P. Singh, L. Decin, L. M. Ziurys
Figure caption: The historic light curve for VY CMa from Robinson (1970) with the estimated ejection dates and possible range of dates from the uncertainty in the expansion velocities for the four clumps.
Paper: Binary Fraction in Galactic Star Clusters: FSR 866, NGC 1960, and STOCK 2
Authors: L. Yalyalieva, A. Chemel, G. Carraro, E. Glushkova
Figure caption: CMD for Stock 2, NGC 1960, and FSR 866 open cluster based on stars with the membership probability P ≥ 0.95 for Stock 2, NGC 1960 and P ≥ 0.985 for FSR 866. Colors are preliminarily dereddened. Parameters are as follows (DMG is the distance modulus in the Gaia filter G). Stock 2: ﹩\mathrm{log}(\mathrm{Age}/\mathrm{yr})\,=\,﹩ 8.5, E(B − V)  =  0.336, DMG  =  9.2 mag, Distance = 463 pc; NGC 1960: ﹩\mathrm{log}(\mathrm{Age}/\mathrm{yr})\,=\,﹩ 7.48, E(B − V)  =  0.27, DMG  =  11.1 mag, Distance = 1202 pc; FSR866: ﹩\mathrm{log}(\mathrm{Age}/\mathrm{yr})\,=\,﹩ 9.57, E(B − V)  =  0.05, DMG  =  10.75 mag, Distance = 1331 pc.
Paper: Binary Fraction in Galactic Star Clusters: FSR 866, NGC 1960, and STOCK 2
Authors: L. Yalyalieva, A. Chemel, G. Carraro, E. Glushkova
Figure caption: Stars in the field of NGC 1960 in the proper motion space. Member stars of NGC 1960 itself are depicted with black dots, while stars of groups A and B with blue and red dots, respectively.
Paper: Binary Fraction in Galactic Star Clusters: FSR 866, NGC 1960, and STOCK 2
Authors: L. Yalyalieva, A. Chemel, G. Carraro, E. Glushkova
Figure caption: Area on the CMD for Stock 2, NGC 1960 and FSR 866 open cluster based on stars with the membership probability P  >  0.95, P  >  0.95 and P  >  0.985, respectively, where binary fraction were investigated. The dashed border indicates the boundaries of the study area. For more details on its determination see Section 4. Gray dots are stars beyond the area. The green part is the area below the line q = 0.6, while the red one is the area above the line q = 0.6, which is considered to contain binary MS stars. Colors are preliminarily dereddened.
Paper: Binary Fraction in Galactic Star Clusters: FSR 866, NGC 1960, and STOCK 2
Authors: L. Yalyalieva, A. Chemel, G. Carraro, E. Glushkova
Figure caption: Distance distribution for stars in the field of NGC 1960. Colors are the same as in Figure 3. Based on geometric distances from Bailer-Jones et al. (2021).
Paper: Binary Fraction in Galactic Star Clusters: FSR 866, NGC 1960, and STOCK 2
Authors: L. Yalyalieva, A. Chemel, G. Carraro, E. Glushkova
Figure caption: Color–magnitude diagram (CMD) of two studied groups in comparison with CMD of NGC 1960 (gray dots). Colors for two groups are the same as in Figure 3.
Paper: Binary Fraction in Galactic Star Clusters: FSR 866, NGC 1960, and STOCK 2
Authors: L. Yalyalieva, A. Chemel, G. Carraro, E. Glushkova
Figure caption: Proper-motion distribution for cluster members (red circles) and field stars (blue dots) in the field of Stock 2, NGC 1960, and FSR 866, derived on the basis of membership probability. The probability threshold for membership is 0.95, 0.95, and 0.985, respectively. Proper motions are from Gaia DR3. On the second panel, that corresponds to NGC 1960, two concentrations besides the cluster are visible, and are discussed in Section 2
Paper: Binary Fraction in Galactic Star Clusters: FSR 866, NGC 1960, and STOCK 2
Authors: L. Yalyalieva, A. Chemel, G. Carraro, E. Glushkova
Figure caption: Membership probability distribution for stars in the field of Stock 2, NGC 1960 and FSR 866. The final threshold probability level was chosen manually in the area where a sharp increase in the number of members begins. For Stock 2 and NGC 1960, this threshold is 0.95, and 0.985 for FSR 866.
Paper: Binary Fraction in Galactic Star Clusters: FSR 866, NGC 1960, and STOCK 2
Authors: L. Yalyalieva, A. Chemel, G. Carraro, E. Glushkova
Figure caption: Radial velocity measurements for the clusters. Single stars are depicted with blue color and double stars are with red. Large circles indicates the stars with more than three observations. The black line is a mean radial velocity, the other lines demonstrate the estimates from the literature that were mentioned in the Table 1, where *1—Dias et al. (2021), *2—Tarricq et al. (2021), *3—Zhong et al. (2020), 4*—Tarricq et al. (2021), 5*—Zhong et al. (2020), *6—(Dias et al. 2021), *7—Tarricq et al. (2021), *8—Alonso-Santiago et al. (2021), *9—Zhong et al. (2020), *10—Carrera et al. (2019), *11—Mermilliod et al. (2008).
Paper: Binary Fraction in Galactic Star Clusters: FSR 866, NGC 1960, and STOCK 2
Authors: L. Yalyalieva, A. Chemel, G. Carraro, E. Glushkova
Figure caption: Dependency of binary fraction on members selection for different values of the mass ratio q, determined by membership probability threshold, for Stock 2, NGC 1960, and FSR 866 open clusters. The plot covers a threshold range from 0.8 to 1.0. Black dashed line shows the membership probability threshold (0.95 for Stock 2 and NGC 1960, and 0.985 for FSR 866.)
Paper: Binary Fraction in Galactic Star Clusters: FSR 866, NGC 1960, and STOCK 2
Authors: L. Yalyalieva, A. Chemel, G. Carraro, E. Glushkova
Figure caption: CMD for Stock 2, NGC 1960, and FSR 866 open cluster, only stars with the membership probability P ≥ 0.95 for Stock 2, NGC 1960, and P ≥ 0.985 for FSR 866 are shown; blue color indicates stars with spectroscopic measurements.
Paper: Kepler Multitransiting System Physical Properties and Impact Parameter Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: An example for a nonlinear TbV pattern, which is superimposed on a secularly driven TbV linear pattern. (a) The evolution of the impact parameters of the planets in the system KOI-935 (Kepler-31) for the sample median parameter values, shifted by the initial b value, b initial, to make the trends visible at the same scale. (b) b resid, the residuals of this evolution after the removal of the linear trend (which is attributed to secular interactions). The thick lines show the residuals for the sample median parameter values, and the narrow lines represent the dynamics for 10 randomly selected parameter sets from our sample to highlight the nonlinear TbV pattern in this system seen in all solutions. The outermost pair, with orbital periods of roughly 42.63 and 87.65 days, reside near but just outside the 2:1 MMR, causing a super-period of roughly 1570 days, which is clearly seen in the nonlinear TbV signal. The largest nonlinear part of the TbV has a semiamplitude of 4 · 10−3 in the best-fitting solution. Such a small signal by itself might not have been detected by direct methods that aim to directly measure the impact parameter for each individual event; it was found here by integrating the information of all transit variations together (timing, duration, depth) in a single dynamical model. (c) The distribution of ﹩{\sigma }_{{b}_{\mathrm{resid}}}﹩ in the best-fitting parameters in the adopted dynamical solutions for 241 planets included in this work and in Paper II, and the linearly accumulated TbV over 1 yr for the same sample (using the median value of ﹩\dot{b}﹩ for each planet). The dashed lines indicate the median values of the two distributions; these differ by a factor of 10.
Paper: Kepler Multitransiting System Physical Properties and Impact Parameter Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: Planetary masses and radii obtained from this work. This figure shows the overall spread of masses and radii and the good agreement of planet masses with former literature values. (a) Mass–radius diagram. Each blue error bar is related to a single planet. The red lines are normalized histograms of the masses and radii obtained by summing up the pdf's of all points. As the sample is small and radii are well determined, the radius-weighted histogram appeared more as a collection of discrete values, so it was smoothed using a Gaussian kernel of width 0.3 R ⊕ to better show population-wide trends. The gray contours are constant-density curves. (b) Comparison of masses obtained in this work with literature values: JH21 values (blue) and upper limits (red); HL17 default mass prior, three of which show upper limits only (yellow); and high-mass prior (purple). We omit planets for which literature values are within less than 2σ of zero. For six objects labeled with their KOI numbers, the results obtained in this work disagree with the results of HL17 by more than 2σ; these are discussed in more detail in the text. The black line shows the identity function.
Paper: Kepler Multitransiting System Physical Properties and Impact Parameter Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: Distribution of mutual inclinations among all pairs in all our runs that passed the dynamical validity criterion σ Nbody < 1.5, and after shuffling over all configurations of the signs of I  x  and I  y . Each solid curve is obtained by averaging all empirical pdf's from all the runs passing the criterion above calculated over uniform bins in i  m  and shown in a logarithmic scale. The dashed lines indicate the best-fitting Gaussian for each curve: blue for systems with two or three planets, and red for systems with more than three planets. The vertical lines indicate the 99% confidence intervals of the expectation values of the fits (also listed in the legend), which are 2.°49 ± 0.°02 for systems with two or three planets and 2° ± 0.°04 for systems with more than three planets. This gives a qualitatively similar picture to that of He et al. (2020) in both the distribution shape and its dependence on multiplicity.
Paper: Kepler Multitransiting System Physical Properties and Impact Parameter Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: Overall statistics of mass estimates in terms of fractional mass error and TTV magnitude for the planets in this study and our former study (Paper II). (a) Distribution of relative error in planetary mass for the combined results of this study and our former study (Paper II; blue) and past literature (orange). The literature sources taken into account here are detailed in Figure 10 and in Judkovsky et al. (2022b, Figure 10). (b) Distribution of σ TTV, the standard deviation of the TTV signal, in the population of planets for which we obtained a dynamical solution and provided masses in this work and in Paper II.
Paper: Kepler Multitransiting System Physical Properties and Impact Parameter Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: Distribution of TbV magnitude in our 130-planet sample for which ﹩\dot{b}﹩ is predicted with a significance level larger than 2σ, listed in the Appendix and in Paper II. (a) The absolute value of TbV rate against the shortest-period companion for the 130 planets in our sample that display TbV to better than 2σ. (b) The empirical cumulative distribution function of the TbV magnitude in this sample, showing that the typical value is of order 10−2 yr−1, with red circles indicating the median and the percentiles equivalent to 1σ and 2σ in a normal distribution.
Paper: Kepler Multitransiting System Physical Properties and Impact Parameter Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: Comparison of the masses obtained from this work with past literature by KOI. In each subpanel, the planets in the system are sorted (left to right) by their orbital period. The numbers above are the suffix of the planets’ KOI designation; for instance, the first object in the plot is KOI-191.03. Dotted vertical lines separate different planets within a system. Bold underlined KOI numbers are used for systems with at least one planet without a previously reported mass constraint, as in Figure 3. The bold underlined KOI suffix represents a specific planet without a previously reported mass. The legend shows the colors and markers representing different literature sources. Arrows pointing down represent upper limits on mass.
Paper: Searching the SN 1987A SETI Ellipsoid with TESS
Authors: Bárbara Cabrales, James R. A. Davenport, Sofia Sheikh, Steve Croft, Andrew P. V. Siemion, Daniel Giles, Ann Marie Cody
Figure caption: TESS data obtained during Cycle 1 (left), Cycle 2 (center), and Cycle 3 (right) on the celestial plane. Common R.A. and decl. labels are displayed for the entire figure. Sources are color-coded by sector, highlighting the geometry of the TESS field of view and the overlap of all 13 sectors—per cycle—at the ecliptic poles (the CVZ). The circular area (bright orange) near the pole on each plot is composed of the targets observed in at least 11 overlapping sectors during that cycle and shows the data sample from which SETI Ellipsoid targets were selected.
Paper: Kepler Multitransiting System Physical Properties and Impact Parameter Variations
Authors: Yair Judkovsky, Aviv Ofir, Oded Aharonson
Figure caption: Measured impact parameter variation rates. (a) Timescale for transits to disappear (namely, number of orbital periods for b to change by 1) against an orbital period of 130 TbV-displaying planets. The radii of the circles represent the absolute planetary radii. (b) Absolute values of ﹩\dot{b}﹩ vs. orbital period. The values of ﹩\dot{b}﹩ are spread around ≈10−2 across the range of observed orbital periods. The correlation of ﹩| \dot{b}| ﹩ with P is weak.
Paper: Planetary Complexity Revealed by the Joint Differential Entropy of Eigencolors
Authors: Gary Segal, David Parkinson, Stuart Bartlett
Figure caption: Wavelength average statistical complexity vs. wavelength average differential entropy (top) and complexity vs. joint differential entropy of the eigencolors (bottom).
Paper: Planetary Complexity Revealed by the Joint Differential Entropy of Eigencolors
Authors: Gary Segal, David Parkinson, Stuart Bartlett
Figure caption: Dual horizontal axis showing both the wavelength average differential entropy (circle “o” shapes), and the JDE of the eigencolors (“x” shapes), aligning the horizontal axis at the respective values of the original Earth and the least complex synthetic world. The fixed point alignment of the horizontal axes changes the scale of each axis. The vertical axis shows the corresponding wavelength average statistical complexity for both measures. Perforated lines show the distinction between world types.
Paper: Planetary Complexity Revealed by the Joint Differential Entropy of Eigencolors
Authors: Gary Segal, David Parkinson, Stuart Bartlett
Figure caption: Off-diagonal frames contain pair-wise plots of individual PCs and the wavelength average statistical complexity classified by the world types presented in Table 1. The diagonal frames contain overlapping kernel density estimate (KDE) plots for each of the world types.
Paper: Planetary Complexity Revealed by the Joint Differential Entropy of Eigencolors
Authors: Gary Segal, David Parkinson, Stuart Bartlett
Figure caption: Scatter plot matrix showing colors 1–3 for both synthetic worlds from the toy model: High variance with correlated colors (orange) and Lower variance with uncorrelated colors (blue). The diagonal shows histograms for each of the colors.
Paper: Planetary Complexity Revealed by the Joint Differential Entropy of Eigencolors
Authors: Gary Segal, David Parkinson, Stuart Bartlett
Figure caption: Scatter plot matrix showing eigencolors 1–3 for both synthetic worlds from the toy model: High variance with correlated colors (orange) and Lower variance with uncorrelated colors (blue). The diagonal shows histograms for each of the eigencolors.
Paper: Circumstellar Disk Accretion Across the Lagoon Nebula: The Influence of Environment and Stellar Mass
Authors: Laura Venuti, Ann Marie Cody, Giacomo Beccari, Luisa M. Rebull, Michael J. Irwin, Apoorva Thanvantri, Sowmya Thanvantri, Silvia H. P. Alencar, Clara O. Leal, Geert Barentsen, Janet E. Drew, Steve B. Howell
Figure caption: Distribution of Lagoon Nebula members in the HR diagram. The model mass tracks (red) and isochrones (black) shown on the diagram were extracted from the MIST compilation (Choi et al. 2016; Dotter 2016), assuming solar metallicity and without rotation effects. The error bars at the bottom illustrate the SpT-dependent typical uncertainties on T eff and L bol values, as discussed in Sections 4.2 and 4.4.
Paper: Circumstellar Disk Accretion Across the Lagoon Nebula: The Influence of Environment and Stellar Mass
Authors: Laura Venuti, Ann Marie Cody, Giacomo Beccari, Luisa M. Rebull, Michael J. Irwin, Apoorva Thanvantri, Sowmya Thanvantri, Silvia H. P. Alencar, Clara O. Leal, Geert Barentsen, Janet E. Drew, Steve B. Howell
Figure caption: Mass distribution inferred for young stars in our Lagoon Nebula sample. The gray histogram refers to the entire population considered in this study, while the black dots and corresponding uncertainties trace the distribution of bona fide members alone. The IMF expressions presented in Chabrier (2003) for single stars (solid red line) and stellar systems (dash–dotted blue line) in the Galactic field are overlaid for comparison purposes, renormalized to the peak of the observed distribution. The dotted red lines trace the range of possible values around the single-star IMF ensuing from the uncertainties on the function parameters tabulated by Chabrier (2003).
Paper: Circumstellar Disk Accretion Across the Lagoon Nebula: The Influence of Environment and Stellar Mass
Authors: Laura Venuti, Ann Marie Cody, Giacomo Beccari, Luisa M. Rebull, Michael J. Irwin, Apoorva Thanvantri, Sowmya Thanvantri, Silvia H. P. Alencar, Clara O. Leal, Geert Barentsen, Janet E. Drew, Steve B. Howell
Figure caption: Diagnostics of accretion extracted for our target stars from the r − Hα color index on the dereddened (r − i, r − Hα) CCD (left) and (r − Hα, r) CMD (right). The colors and symbols are the same as in Figure 4. In the left panel, the red curve traces the SpT-dependent photospheric color sequence tabulated for main-sequence dwarfs in the VST/OmegaCAM filters by Drew et al. (2014). The spectral types, shifted downwards for clarity, are labeled along the reference sequence to guide the eye. In the right panel, the dashed and solid red curves trace the median reference color sequence extracted from our high-confidence disk-free population and a photometric range around the sequence (±0.02 mag) that takes into account the uncertainty on the reference fit, respectively. In both panels, the threshold curve adopted to select accreting stars is traced with a thicker green line. The stars selected as accretors are located above the green line in the CCD and to the right of the green line in the CMD.
Paper: Circumstellar Disk Accretion Across the Lagoon Nebula: The Influence of Environment and Stellar Mass
Authors: Laura Venuti, Ann Marie Cody, Giacomo Beccari, Luisa M. Rebull, Michael J. Irwin, Apoorva Thanvantri, Sowmya Thanvantri, Silvia H. P. Alencar, Clara O. Leal, Geert Barentsen, Janet E. Drew, Steve B. Howell
Figure caption: Accretion rate distribution as a function of stellar mass for Lagoon Nebula stars classified as accreting (black dots) or potential accretors (empty circles). Variability bars mark the full range of ﹩{\dot{M}}_{\mathrm{acc}}﹩ values measured during the VST/OmegaCAM monitoring. Upper limits, marked as downward arrows, are assigned to objects that were located in the nonaccreting regions of the various color excess diagrams at least in some epochs. The dashed red line traces a reference detection threshold, derived as a polynomial fit to the nominal ﹩{\dot{M}}_{\mathrm{acc}}﹩ values extracted for stars classified as nonaccreting following the criteria discussed in Section 5.4.
Paper: Circumstellar Disk Accretion Across the Lagoon Nebula: The Influence of Environment and Stellar Mass
Authors: Laura Venuti, Ann Marie Cody, Giacomo Beccari, Luisa M. Rebull, Michael J. Irwin, Apoorva Thanvantri, Sowmya Thanvantri, Silvia H. P. Alencar, Clara O. Leal, Geert Barentsen, Janet E. Drew, Steve B. Howell
Figure caption: Comparison between T eff estimates derived in this study as presented in Section 4.2 and the values obtained in Prisinzano et al. (2019) for objects in common between the two samples. The solid gray line traces the equality line on the diagram, while the dotted gray lines trace a difference between the two T eff sets that amounts to a factor of 1.2. The colored boxes mark the ranges in T eff associated with different spectral classes, as labeled in the legend. The overlapping corners between adjacent boxes correspond to the transition between the ninth subclass of the previous spectral group and the zeroth subclass of the following spectral group, while the delimiting T eff values take the uncertainties listed in Table 2 into account.
Paper: Circumstellar Disk Accretion Across the Lagoon Nebula: The Influence of Environment and Stellar Mass
Authors: Laura Venuti, Ann Marie Cody, Giacomo Beccari, Luisa M. Rebull, Michael J. Irwin, Apoorva Thanvantri, Sowmya Thanvantri, Silvia H. P. Alencar, Clara O. Leal, Geert Barentsen, Janet E. Drew, Steve B. Howell
Figure caption: Dereddened (u − r, r) CMD for Lagoon Nebula members in our sample with available u-band photometry. The objects classified as disk-free are highlighted as black dots (strong classification) and black circles (more uncertain classification). The gray dots without a contour correspond to disk-bearing sources. The dashed and solid red curves trace the median reference color sequence extracted from our high-confidence disk-free population and a photometric range around the sequence (±0.08 mag) that takes into account the uncertainty on the reference fit, respectively. The threshold adopted to select accreting stars is traced in green.