adsabs/AstroCLIMB huggingface dataset:
Paper: A Survey of Galaxy Pairs in the SDSS Photometric Images based on Faster-RCNN
Authors: Chen-hui Shi, 晨辉 史, Hai-feng Yang, 海峰 杨, Jiang-hui Cai, 江辉 蔡, Li-chan Zhou, 立婵 周, Yan-ting He, 艳婷 贺, Mei-hong Su, 美红 苏, Xu-jun Zhao, 旭俊 赵, Ya-ling Xun, 亚玲 荀
Figure caption: Some irregular physical galaxy pairs confirmed by photoz.
Paper: Spin–Orbit Coupling of the Ellipsoidal Secondary in a Binary Asteroid System
Authors: Hanlun Lei
Figure caption: Comparison of dynamical separatrices under different kernel Hamiltonian models (left panel) and resonant halfwidth of synchronous spin–orbit resonance as a function of a ref determined under Hamiltonian model #4 (right panel). The location of the resonant center and saddle point is marked. The red dashed line shown in the right panel shows the location of a ref = 10. A dynamical separatrix divides the entire phase space into regions of libration and circulation in terms of synchronous (1:1) spin–orbit resonance. The default parameters of system are set as a  s  = 1, b  s  = 0.95, c  s  = 0.85, α  m  = 0.05, a ref = 10, and ﹩{e}_{\max }=0.05﹩.
Paper: Spin–Orbit Coupling of the Ellipsoidal Secondary in a Binary Asteroid System
Authors: Hanlun Lei
Figure caption: Schematic diagram of variables, used for describing translational and rotational motions, in the binary asteroid system composed of a spherical primary with mass m  p  and an ellipsoidal secondary with mass m  s . The second-to-primary mass ratio is denoted as α  m  = m  s /m  p  < 1. In the planar problem, the X-axis directs toward an arbitrary fixed direction. The position vector from the primary toward the secondary is denoted by  r , the true longitude of the secondary is denoted by θ = f + ϖ where ϖ is the longitude of pericenter and f is the true anomaly, and the rotational angle of the secondary relative to the X-axis of an inertial frame is represented by ϕ. The relative angle is defined by ψ = ϕ − θ = (ϕ − ϖ) − f.
Paper: Spin–Orbit Coupling of the Ellipsoidal Secondary in a Binary Asteroid System
Authors: Hanlun Lei
Figure caption: Physically allowed regions corresponding to given Hamiltonian and total angular momentum, specified by the reference semimajor axis a ref and the maximum eccentricity e max (see Equations (15) and (16) for definition). The index shown in the color bar stands for the magnitude of eccentricity. For this example, the shape parameters of the secondary are taken as a  s  = 1, b  s  = 0.95, and c  s  = 0.85 and the mass ratio is assumed at α  m  = 0.05.
Paper: Spin–Orbit Coupling of the Ellipsoidal Secondary in a Binary Asteroid System
Authors: Hanlun Lei
Figure caption: Poincaré sections at different reference semimajor axes (left panel) and at different maximum eccentricities (right panel). The index shown in the color bar stands for the magnitude of eccentricity.
Paper: Spin–Orbit Coupling of the Ellipsoidal Secondary in a Binary Asteroid System
Authors: Hanlun Lei
Figure caption: Nominal location of high-order and secondary spin–orbit resonances (left panel) and comparison to Poincaré section (right panel). Red dashed lines stand for the dynamical separatrix of the synchronous (1:1) resonance.
Paper: Spin–Orbit Coupling of the Ellipsoidal Secondary in a Binary Asteroid System
Authors: Hanlun Lei
Figure caption: Poincaré sections at different mass ratios (left panel) and at different asphericity parameters (right panel). The index shown in the color bar stands for the magnitude of eccentricity.
Paper: Spin–Orbit Coupling of the Ellipsoidal Secondary in a Binary Asteroid System
Authors: Hanlun Lei
Figure caption: Time evolution of the old and new angular coordinates (i.e., before and after canonical transformation) for a librating cycle (left panel) and a circulating cycle (right panel).
Paper: Unveiling Subarcsecond Multiplicity in the Pleiades with Gaia Multicolor Photometry
Authors: Dmitry Chulkov
Figure caption: Color–color diagram for the Pleiades stars. The G − R  p  color is chosen for illustration; a similar pattern is observed with B  p  − G on the ordinate axis. Left: 54 outlying sources selected for further analysis. Right panel, red line: expected relation for single stars from the PARSEC isochrone (Section 3, Figure 6). The unreddened (absorption neglected) colors are chosen for a better fit with observational data. Other lines show binary populations with different mass ratios. Thin black line: q = 0.5, violet: q = 0.75, thick black: q = 1. Importantly, G flux is calculated for the primary star alone, while B  p  and R  p  are for the entire binary system. ◯ and □ mark components of resolved Gaia DR3 pairs; × indicate sources with unconfirmed multiplicity. Bare · denote unresolved Gaia sources whose multiplicity is known from ground-based observations (Table 4).
Paper: Unveiling Subarcsecond Multiplicity in the Pleiades with Gaia Multicolor Photometry
Authors: Dmitry Chulkov
Figure caption: Color–magnitude diagram for stars with δ μ < 5 mas yr−1 (Equation (1)). PPMXL data are used for the two-parameter Gaia DR3 solutions. Two entries marked by □ are unrelated to the Pleiades based on their parallaxes and radial velocities. The presence of a close neighbor in Gaia, potentially creating an artifact in c = B  P  − R  P  estimation, is color coded (Section 2.6).
Paper: Unveiling Subarcsecond Multiplicity in the Pleiades with Gaia Multicolor Photometry
Authors: Dmitry Chulkov
Figure caption: PARSEC (version 2.0; A. Bressan et al. 2012; C. T. Nguyen et al. 2022) isochrones with rotation Ω/Ω c  = 0.3 (inclination 60°) for ages t = 50, 100, and 200 Myr at solar metallicity. The model with enhanced [Fe/H] = 0.05, t = 100 Myr is adopted for further calculations. It provides reasonable agreement for sources with apparent magnitude G > 7mag, thus covering the binary systems considered in Table 4. A distance of 135 pc (5.65mag modulus) and an extinction of A  V  = 0.15mag are applied.
Paper: Unveiling Subarcsecond Multiplicity in the Pleiades with Gaia Multicolor Photometry
Authors: Dmitry Chulkov
Figure caption: Left: 18 unresolved binary systems with known mass ratios of components (color coded) in the color–magnitude diagram among other Pleiades members. The majority of objects are double-lined spectroscopic binaries from the G. Torres et al. (2021) survey. Two faint (G > 14mag) binaries were revealed by M. Kounkel et al. (2021). Triple-lined multiple systems are marked with a ×. The remaining are the astrometric-spectroscopic solutions for Atlas (N. Zwahlen et al. 2004) and V1282 Tau (G. Torres et al. 2020), which have ρ < 0.″05. Binaries with large q and triple systems are shifted above the main sequence. Right: the same unresolved systems in the color–color plot show no displacement.
Paper: Unveiling Subarcsecond Multiplicity in the Pleiades with Gaia Multicolor Photometry
Authors: Dmitry Chulkov
Figure caption: 351 isolated sources with no Gaia DR3 neighbors within 5″ considered probable Pleiades members. Stars with two-parameter solutions (marked by ×) are displaced toward brighter magnitudes, as expected for unresolved binary systems.
Paper: Search for Young Stellar Objects within 4XMM-DR13 Using CatBoost and SPE
Authors: Xiangyao Ma, Yanxia Zhang, Jingyi Zhang, Changhua Li, Zihan Kang, Ji Li
Figure caption: The known YSOs and YSO candidates in Galactic coordinates. The blue diamonds represent YSO candidates selected by SPE, and the red squares represent known YSOs.
Paper: Search for Young Stellar Objects within 4XMM-DR13 Using CatBoost and SPE
Authors: Xiangyao Ma, Yanxia Zhang, Jingyi Zhang, Changhua Li, Zihan Kang, Ji Li
Figure caption: The spectrum of LAMOST MRS med-59980-TD043724N254338B01_sp14-231.fits. It shows strong Hα emission at 6562.8 Å.
Paper: Search for Young Stellar Objects within 4XMM-DR13 Using CatBoost and SPE
Authors: Xiangyao Ma, Yanxia Zhang, Jingyi Zhang, Changhua Li, Zihan Kang, Ji Li
Figure caption: The spectrum of LAMOST LRS spec-56617-VB081S05V2_sp06-073.fits. It shows strong Hα emission at 6562.8 Å.
Paper: Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library
Authors: Aniket Sanghi, Jerry W. Xuan, Jason J. Wang, Dimitri Mawet, Brendan P. Bowler, Henry Ngo, Marta L. Bryan, Garreth Ruane, Olivier Absil, Elsa Huby
Figure caption: Free parameter optimization results. Left: histogram depicting the number of targets in the injection-recovery subset that yield the highest average S/N for the injected synthetic companion when a given image similarity metric is used for pre-frame ordering. MSE is strongly preferred, accounting for random Poisson uncertainty. Right: S/N map of the injected synthetic companions as a function of library size and PCs. Combinations where the number of PCs exceeds the number of reference frames in the library are set to a NaN value. The yellow star indicates the combination of library size and number of PCs that yields the maximum S/N in our tests.
Paper: Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library
Authors: Aniket Sanghi, Jerry W. Xuan, Jason J. Wang, Dimitri Mawet, Brendan P. Bowler, Henry Ngo, Marta L. Bryan, Garreth Ruane, Olivier Absil, Elsa Huby
Figure caption: Super-RDI vs. ADI for the young M-star survey: Average (black) and median (green) difference in Super-RDI (sRDI) and ADI contrast (units of Δmag) as a function of separation (units of arcseconds). A gray dashed line marks zero difference and corresponds to both techniques achieving the same sensitivity level. Positive differences indicate better Super-RDI performance and negative differences indicate better ADI performance. For the typical P.A. rotation of the young M-star survey (∼10°), Super-RDI outperforms a widely used implementation of ADI-based PSF subtraction at separations ≲0.″4, averaged across all observations.
Paper: Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library
Authors: Aniket Sanghi, Jerry W. Xuan, Jason J. Wang, Dimitri Mawet, Brendan P. Bowler, Henry Ngo, Marta L. Bryan, Garreth Ruane, Olivier Absil, Elsa Huby
Figure caption: Histograms summarizing distributions for key properties of targets in the sample (R.A. and decl.) and individual observations (W1 mag, total integration time, P.A. rotation, and seeing). The median values for the observations are as follows: 8.099 mag W1, 15 minutes of total integration time, 8.°6 P.A. rotation, and 0.″6 seeing.
Paper: Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library
Authors: Aniket Sanghi, Jerry W. Xuan, Jason J. Wang, Dimitri Mawet, Brendan P. Bowler, Henry Ngo, Marta L. Bryan, Garreth Ruane, Olivier Absil, Elsa Huby
Figure caption: A diagrammatic illustration of the metric covariance cube. This represents the data structure used to store image similarity metric values for each pair of science and reference frames. The red cube is an example location in the matrix where the metric value is stored, as described by three indices. The first two indices of the matrix uniquely identify the pair of frames for which the metric is calculated and the third index identifies the metric whose value is stored.
Paper: Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library
Authors: Aniket Sanghi, Jerry W. Xuan, Jason J. Wang, Dimitri Mawet, Brendan P. Bowler, Henry Ngo, Marta L. Bryan, Garreth Ruane, Olivier Absil, Elsa Huby
Figure caption: Gallery of 25 example sky-subtracted image cutouts (centered on target) drawn randomly from our NIRC2 vortex coronagraphic observations. The dimensions of each cutout are 101 × 101 pixels (1″ × 1″). The images are depicted in linear scale in normalized analog to digital units and are ordered left to right, top to bottom in ascending order of raw contrast level at a fixed radial separation (∼10−2 at 0.″15). The diversity of PSF shapes highlights the importance of using frame selection techniques to achieve optimal performance with the RDI strategy.
Paper: Efficiently Searching for Close-in Companions Around Young M Dwarfs Using a Multiyear PSF Library
Authors: Aniket Sanghi, Jerry W. Xuan, Jason J. Wang, Dimitri Mawet, Brendan P. Bowler, Henry Ngo, Marta L. Bryan, Garreth Ruane, Olivier Absil, Elsa Huby
Figure caption: “Optimal” 5σ contrast curves for 192 observations in the young M-star survey (gray curves) constructed by selecting the deepest achieved contrast as a function of separation from the combination of Super-RDI and ADI principal contrast curves. The median optimal contrast curve is plotted in black. A few contrast curves show irregularities due to the presence of point sources or image artifacts.
Paper:  Yuti: A General-purpose Transit Simulator for Arbitrary Shaped Objects Orbiting Stars
Authors: Ushasi Bhowmick, Vikram Khaire
Figure caption: Evolution of the residual feature obtained by Dyson Disk transit minus planet transit with transit parameters. Column (A) is for R pl/R st. The top panel shows the residuals for different values of R pl/R st, which are represented by the color-map. The bottom panel shows the variation of ΔF  m  with R pl/R st. ΔF  m  is the maximum difference observed between the light curves of the Dyson disk and planet. There is a sharp increase in ΔF  m  for values greater than 0.1, which implies greater detectability. Column (B) is for R orb/R st. Once again, a sharp increase is observed for orbits closer than 10 R st. Column (C) is for u 1. There is a linear decrease in ΔF  m . Column (D) is for b. There is an overall decrease in ΔF  m ; however, the shapes of the residuals vary significantly, as is observed in the top panel.
Paper:  Yuti: A General-purpose Transit Simulator for Arbitrary Shaped Objects Orbiting Stars
Authors: Ushasi Bhowmick, Vikram Khaire
Figure caption: Three simulated Dyson disk light curves with different limb-darkening parameters fitted with exoplanet models. The radius (0.1 R st), orbit (2 R st), and impact parameters (b = 0) are kept the same for all three examples. A 3D planet model with both quadratic as well as nonlinear limb darkening is fitted to the Dyson disk simulations. The top panels show the simulated light curves (green) and the fitted models. The bottom panels show the residual features (Simulation–Fit). The limb-darkening coefficients for the simulated Dyson disk light curve as well as the planet's fits are mentioned. From the residuals of the nonlinear fit (purple) and that of the quadratic fit (blue), the nonlinear law appears to fit slightly better than the quadratic law. Such a fit diminishes the residual feature, but kinks are observed at ingress and egress.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: FFT of whitened orbital frequency and its harmonics. The horizontal axis represents frequency (c/d), the vertical axis represents amplitude (amplitude in % of the mean brightness vs. frequency in μHz), and the dashed horizontal line refers to the 5σ detection threshold of local noise level. The upper panel is the FFT of the star located above the target star, while the lower panel is the FFT of the star located to the lower left of the target star.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The sFT of KIC 6362386 LC data with the white dashed line representing the frequency of 0.1642c/d and the black dashed line indicating the binary orbital frequency.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The fitting isochrones of KIC 6362386. The square and circle denote the locations of the primary and secondary, respectively. The solid lines show the isochrones with metallicity of [Fe/H], which is −0.16 dex derived from the spectra. The color of the line represents the logarithm of the age of the binary system ﹩\mathrm{log}t﹩. The dashed lines show the isochrones with metallicity of [Fe/H]± σ [Fe/H], which are −0.16 ± 0.14 dex.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The surrounding stars of KIC 6362386 made by tpfi (K. Xing et al. 2024). The image on the far left is the binary identification chart, while the others are the TPF files for each season. The red region indicates the default aperture mask, with the target denoted by a white cross symbol.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The corner diagram of the MCMC results.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The fast Fourier transform (FFT) of the removed binary orbital frequency of KIC 6362386 LC data. The red lines indicate the frequencies of the orbital frequency of KIC 6362386 and its harmonic frequencies.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The diagram of out-of-eclipse light curves. Each subplot corresponds to one quarter in Kepler LC data.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The light curves of KIC 6362386 from the Kepler SC photometry fitted under the optimal solution in the upper panel. The residuals are shown in the lower panel.
Paper: KIC 6362386: An Eclipsing Binary with γ Doradus–type Pulsations and Starspots
Authors: Mengqi Jin, Jianning Fu, Xiaobin Zhang, Weikai Zong, Jiaxin Wang, Xiaoyu Ma, Keyu Xing, Haotian Wang
Figure caption: The out-of-eclipse residuals of KIC 6362386. The top, middle, and bottom panels show the residuals from the Kepler LC photometry, the Kepler SC photometry, and the TESS photometry, respectively.
Paper: Formation of CN and CO Molecules in the Envelope of Nova V1391 Cas During the Near-maximum Phase
Authors: Hideyo Kawakita, James E. Lyke
Figure caption: Observed spectrum of V1391 Cas (black line) and synthesized emission spectra of CO (Δv = +1) (colored lines) for excitation temperatures of 2000, 2250, and 2500 K. The 13C/12C ratio in CO is assumed to be 0.5, as determined by R. J. Rudy et al. (2024) for the same nova. It is also assumed that the velocity of the CO emission system along the line of sight matches that of the Pa-β emission line observed in our data. The vertical thick bars indicate C I emission lines (refer to Figure 5).
Paper: Formation of CN and CO Molecules in the Envelope of Nova V1391 Cas During the Near-maximum Phase
Authors: Hideyo Kawakita, James E. Lyke
Figure caption: Paschen β emission line of V1391 Cas in our spectra (thin green line). The observed emission peak is at 12,821.64 Å in the heliocentric reference frame. The thick red dotted line represents a Gaussian profile with FWHM = 850 km s−1 (assuming a nova system velocity of 0 km s−1), combined with a narrower absorption feature at –160 km s−1 relative to the center wavelength of this emission. The thin dashed line is without the narrower absorption feature. Since the wavelengths near the Pa-β emission are mostly free from telluric absorption lines, the small absorption superimposed on the broad emission is not an artifact.
Paper: Formation of CN and CO Molecules in the Envelope of Nova V1391 Cas During the Near-maximum Phase
Authors: Hideyo Kawakita, James E. Lyke
Figure caption: Moderate-resolution (R ≈ 2700) spectra of V1391 Cas. This figure provides a close-up view of the wavelength region from 19,000 to 24,600 Å (the dashed line is the same as in Figure 1).
Paper: Formation of CN and CO Molecules in the Envelope of Nova V1391 Cas During the Near-maximum Phase
Authors: Hideyo Kawakita, James E. Lyke
Figure caption: Observed spectrum of V1391 Cas (black solid line) and a synthesized absorption spectrum of CN A-X (Δv = 0) band (violet dotted line). The synthesized CN spectrum, based on an excitation temperature of 5000 K and a constant continuum, serves as a guide. Note the weak emission lines from an unidentified source (at 11,057 Å) and Fe II (at 11,129 Å) observed on UT 2020 August 17.54 (R. J. Rudy et al. 2024), as shown in Figure 1. These emission lines, superimposed by the CN absorption lines, were likely present in our spectrum.
Paper: Formation of CN and CO Molecules in the Envelope of Nova V1391 Cas During the Near-maximum Phase
Authors: Hideyo Kawakita, James E. Lyke
Figure caption: Same as Figure 8, but plotted with the observed spectrum of V1391 Cas on UT 2020 August 17.54 reported by R. J. Rudy et al. (2024; with a logarithmic scale bias) and a modeled spectrum including the emission bands for 2500 K superimposed on the continuum with the absorption for 4000 K.
Paper: Formation of CN and CO Molecules in the Envelope of Nova V1391 Cas During the Near-maximum Phase
Authors: Hideyo Kawakita, James E. Lyke
Figure caption: A synthesized near-infrared spectrum of a typical A0 star, Vega (A0V) for the wavelength region considered in this article. The spectral resolution of this spectrum is R = 3000, matching to the observed spectra of V1391 Cas by NIRES. Vertical tick-marks show the wavelengths of relevant atomic hydrogen lines.
Paper: Formation of CN and CO Molecules in the Envelope of Nova V1391 Cas During the Near-maximum Phase
Authors: Hideyo Kawakita, James E. Lyke
Figure caption: Same as Figure 8, but with the absorption system incorporated into the model (see text for details).
Paper: Formation of CN and CO Molecules in the Envelope of Nova V1391 Cas During the Near-maximum Phase
Authors: Hideyo Kawakita, James E. Lyke
Figure caption: Moderate-resolution (R ≈ 2700) spectra of V1391 Cas. This figure provides a close-up view of the wavelength region from 14,000 to 18,500 Å.
Paper: Archetype-based Redshift Estimation for the Dark Energy Spectroscopic Instrument Survey
Authors: Abhijeet Anand, Julien Guy, Stephen Bailey, John Moustakas, J. Aguilar, S. Ahlen, A. S. Bolton, A. Brodzeller, D. Brooks, T. Claybaugh, S. Cole, A. de la Macorra, Biprateep Dey, K. Fanning, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, K. Honscheid, C. Howlett, S. Juneau, D. Kirkby, T. Kisner, A. Kremin, A. Lambert, M. Landriau, L. Le Guillou, M. Manera, A. Meisner, R. Miquel, E. Mueller, G. Niz, N. Palanque-Delabrouille, W. J. Percival, C. Poppett, F. Prada, A. Raichoor, M. Rezaie, G. Rossi, E. Sanchez, E. F. Schlafly, D. Schlegel, M. Schubnell, D. Sprayberry, G. Tarlé, C. Warner, B. A. Weaver, R. Zhou, H. Zou
Figure caption: DESI example spectra of BGS, LRG, ELG, and QSO targets. The colored lines show the three DESI cameras. The uncertainties in fluxes are shown in gray in each panel. We also label the expected location of absorption and emission lines in each spectrum.