adsabs/AstroCLIMB huggingface dataset:
Paper: The Hot Inner AU of V883 Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Ágnes Kóspál
Figure caption: Upper panel: the complete disk + scattering model (black) compared with the LRIS and SpeX spectra (magenta). The disk component is shown in red and the scattered light component is shown in blue. Historical photometry of the source is shown as green symbols: triangles for PanSTARRS, squares for 2MASS, and circles for WISE. The WISE photometry includes significant thermal emission from the dust surrounding V883 Ori, while the SpeX LXD spectrum is dominated by emission from only the inner disk. Lower panel: the dereddened SpeX spectrum and accompanying dereddened best-fit models, to better highlight the NIR fit. The AV used for dereddening the spectrum is 20.78 mag. As established from the joint model, this is much greater than AV (scatt), causing the rapid upward slope toward the visible.
Paper: The First Search for Optical Transient as a Counterpart of a Month-timescale IceCube Neutrino Multiplet Event
Authors: Seiji Toshikage, Shigeo S. Kimura, Nobuhiro Shimizu, Masaomi Tanaka, Shigeru Yoshida, Wataru B. Iwakiri, Tomoki Morokuma
Figure caption: Cumulative probability density of redshift distribution for the IC neutrino triplet sources depending on the total neutrino energy εν.
Paper: The Hot Inner AU of V883 Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Ágnes Kóspál
Figure caption: A light curve of V883 Ori, spanning the past 20 yr of observations. The arrows to the left of the plot mark the brightness of the source at 0.8, 3.5, and 4.8 μm, taken in 1963, 1975, and 1975, respectively (D. A. Allen et al. 1975). The source has remained at essentially the same brightness for at least the past 60 yr. The triangles mark points from Pan-STARRS, while * symbols mark points from ZTF. The tan and gray squares mark NEOWISE W1 and W2 points, respectively. The symbols on the plot are larger than the photometric uncertainties for all points except NEOWISE.
Paper: The Hot Inner AU of V883 Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Ágnes Kóspál
Figure caption: A diagram of the system showing the geometry of the scattering surfaces and obscuring the screen relative to the disk and the observer. The illustrated disk (in orange) angle is set to the 38﹩\mathop{.}\limits^{\unicode{x000b0}}﹩3 disk inclination. The vertical black arrow marks the 400 au projected spatial width of the LRIS trace on-sky, while the size of the disk illustration is the 100 au dust disk radius.
Paper: The First Search for Optical Transient as a Counterpart of a Month-timescale IceCube Neutrino Multiplet Event
Authors: Seiji Toshikage, Shigeo S. Kimura, Nobuhiro Shimizu, Masaomi Tanaka, Shigeru Yoshida, Wataru B. Iwakiri, Tomoki Morokuma
Figure caption: The direction of IceCube triplet event ICT-MJD59015 and ZTF coverage for the field = 396, ccdid = D15, and qid = 3. Here qid is the ID of the quadrant for each read-out area.
Paper: The Hot Inner AU of V883 Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Ágnes Kóspál
Figure caption: Posterior distributions for Lacc and ﹩{T}_{{\rm{\max }}}﹩ computed from the distributions of M*, ﹩\dot{M}﹩, and Rinner. The posterior distribution for AV for the disk component is shown for reference, as it is often covariant with ﹩{T}_{{\rm{\max }}}﹩. The lack of strong covariance of our posteriors indicates we have successfully broken the degeneracy typically present in SED fitting of accretion disk models.
Paper: The Hot Inner AU of V883 Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Ágnes Kóspál
Figure caption: The sources of heating in the V883 Ori disk. The heating from the central star is negligible since the disk dominates the luminosity of the system. The midplane viscous heating, while dominant in the inner 3 au of the disk, falls below the heating due to irradiation from the accretion luminosity of the disk.
Paper: The Hot Inner AU of V883 Ori
Authors: Adolfo S. Carvalho, Lynne A. Hillenbrand, Ágnes Kóspál
Figure caption: The posterior distributions of all 8 parameters of the disk + scattering models. They are all well-constrained and show minimal covariance.
Paper: Constraints on the Orbit of the Young Substellar Companion GQ Lup B from High-resolution Spectroscopy and VLTI/GRAVITY Astrometry 
Authors: Vidya Venkatesan, S. Blunt, J. J. Wang, S. Lacour, G.-D. Marleau, G. A. L. Coleman, L. Guerrero, W. O. Balmer, L. Pueyo, T. Stolker, J. Kammerer, N. Pourré, M. Nowak, E. Rickman, A. Sivaramakrishnan, D. Sing, K. Wagner, A.-M. Lagrange, R. Abuter, A. Amorim, R. Asensio-Torres, J.-P. Berger, H. Beust, A. Boccaletti, M. Bonnefoy, H. Bonnet, M. S. Bordoni, G. Bourdarot, W. Brandner, F. Cantalloube, P. Caselli, B. Charnay, G. Chauvin, A. Chavez, A. Chomez, E. Choquet, V. Christiaens, Y. Clénet, V. Coudé du Foresto, A. Cridland, R. Davies, R. Dembet, J. Dexter, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, N. M. Förster Schreiber, P. Garcia, R. Garcia Lopez, E. Gendron, R. Genzel, S. Gillessen, J. H. Girard, S. Grant, X. Haubois, G. Heissel, Th. Henning, S. Hinkley, S. Hippler, M. Houllé, Z. Hubert, L. Jocou, M. Keppler, P. Kervella, L. Kreidberg, N. T. Kurtovic, V. Lapeyrère, J.-B. Le Bouquin, D. Lutz, A.-L. Maire, F. Mang, A. Mérand, C. Mordasini, D. Mouillet, E. Nasedkin, T. Ott, G. P. P. L. Otten, C. Paladini, T. Paumard, K. Perraut, G. Perrin, S. Petrus, O. Pfuhl, D. C. Ribeiro, Z. Rustamkulov, J. Shangguan, T. Shimizu, A. Shields, J. Stadler, O. Straub, C. Straubmeier, E. Sturm, L. J. Tacconi, A. Vigan, F. Vincent, S. D. von Fellenberg, F. Widmann, T. O. Winterhalder, J. Woillez, S. Yazici
Figure caption: Posterior eccentricity and inclination distributions for GQ Lup B based on six orbital fits (see Table 5), grouped by inclusion of GRAVITY astrometry. The histograms show the relative probability of eccentricity and inclination values. Inclusion of GRAVITY and relative RV measurements substantially tightens the constraints. While the high-precision RV case (orange) provides the narrowest distribution, it may be biased due to stellar variability or unresolved companions. The adopted blue case (GRAVLowRV) incorporates GRAVITY astrometry and low-precision RV, offering a robust and physically plausible solution consistent with a moderately eccentric and inclined orbit.
Paper: Constraints on the Orbit of the Young Substellar Companion GQ Lup B from High-resolution Spectroscopy and VLTI/GRAVITY Astrometry 
Authors: Vidya Venkatesan, S. Blunt, J. J. Wang, S. Lacour, G.-D. Marleau, G. A. L. Coleman, L. Guerrero, W. O. Balmer, L. Pueyo, T. Stolker, J. Kammerer, N. Pourré, M. Nowak, E. Rickman, A. Sivaramakrishnan, D. Sing, K. Wagner, A.-M. Lagrange, R. Abuter, A. Amorim, R. Asensio-Torres, J.-P. Berger, H. Beust, A. Boccaletti, M. Bonnefoy, H. Bonnet, M. S. Bordoni, G. Bourdarot, W. Brandner, F. Cantalloube, P. Caselli, B. Charnay, G. Chauvin, A. Chavez, A. Chomez, E. Choquet, V. Christiaens, Y. Clénet, V. Coudé du Foresto, A. Cridland, R. Davies, R. Dembet, J. Dexter, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, N. M. Förster Schreiber, P. Garcia, R. Garcia Lopez, E. Gendron, R. Genzel, S. Gillessen, J. H. Girard, S. Grant, X. Haubois, G. Heissel, Th. Henning, S. Hinkley, S. Hippler, M. Houllé, Z. Hubert, L. Jocou, M. Keppler, P. Kervella, L. Kreidberg, N. T. Kurtovic, V. Lapeyrère, J.-B. Le Bouquin, D. Lutz, A.-L. Maire, F. Mang, A. Mérand, C. Mordasini, D. Mouillet, E. Nasedkin, T. Ott, G. P. P. L. Otten, C. Paladini, T. Paumard, K. Perraut, G. Perrin, S. Petrus, O. Pfuhl, D. C. Ribeiro, Z. Rustamkulov, J. Shangguan, T. Shimizu, A. Shields, J. Stadler, O. Straub, C. Straubmeier, E. Sturm, L. J. Tacconi, A. Vigan, F. Vincent, S. D. von Fellenberg, F. Widmann, T. O. Winterhalder, J. Woillez, S. Yazici
Figure caption: Orbit fit for Case GRAVLowRV (see Table 5), using astrometry including GRAVITY data and low-precision radial velocity measurement. The plot shows posterior samples from the orbit fit for GQ Lup B, generated using orbitize!. Blue ellipses represent 100 orbits randomly drawn from the posterior, and red points indicate the relative astrometric data. In the right panels, red points correspond to astrometric measurements from both the literature and new GRAVITY data included in the fit; gray lines trace the same 100 posterior orbits in separation and position angle. The results illustrate the power of GRAVITY data in improving the orbit solution for GQ Lup B.
Paper: Constraints on the Orbit of the Young Substellar Companion GQ Lup B from High-resolution Spectroscopy and VLTI/GRAVITY Astrometry 
Authors: Vidya Venkatesan, S. Blunt, J. J. Wang, S. Lacour, G.-D. Marleau, G. A. L. Coleman, L. Guerrero, W. O. Balmer, L. Pueyo, T. Stolker, J. Kammerer, N. Pourré, M. Nowak, E. Rickman, A. Sivaramakrishnan, D. Sing, K. Wagner, A.-M. Lagrange, R. Abuter, A. Amorim, R. Asensio-Torres, J.-P. Berger, H. Beust, A. Boccaletti, M. Bonnefoy, H. Bonnet, M. S. Bordoni, G. Bourdarot, W. Brandner, F. Cantalloube, P. Caselli, B. Charnay, G. Chauvin, A. Chavez, A. Chomez, E. Choquet, V. Christiaens, Y. Clénet, V. Coudé du Foresto, A. Cridland, R. Davies, R. Dembet, J. Dexter, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, N. M. Förster Schreiber, P. Garcia, R. Garcia Lopez, E. Gendron, R. Genzel, S. Gillessen, J. H. Girard, S. Grant, X. Haubois, G. Heissel, Th. Henning, S. Hinkley, S. Hippler, M. Houllé, Z. Hubert, L. Jocou, M. Keppler, P. Kervella, L. Kreidberg, N. T. Kurtovic, V. Lapeyrère, J.-B. Le Bouquin, D. Lutz, A.-L. Maire, F. Mang, A. Mérand, C. Mordasini, D. Mouillet, E. Nasedkin, T. Ott, G. P. P. L. Otten, C. Paladini, T. Paumard, K. Perraut, G. Perrin, S. Petrus, O. Pfuhl, D. C. Ribeiro, Z. Rustamkulov, J. Shangguan, T. Shimizu, A. Shields, J. Stadler, O. Straub, C. Straubmeier, E. Sturm, L. J. Tacconi, A. Vigan, F. Vincent, S. D. von Fellenberg, F. Widmann, T. O. Winterhalder, J. Woillez, S. Yazici
Figure caption: 1σ and 2σ joint posterior distributions of eccentricity and inclination for GQ Lup B under four cases (see Table 5) are shown by lines and dashed lines, respectively. The inclusion of GRAVITY astrometry significantly narrows the orbital parameter space, particularly by reducing the volume of the joint eccentricity–inclination posterior. Adding radial velocity measurements—especially in the GRAVLowRV and GRAVHighRV cases—further sharpens the constraints by reducing the eccentricity–inclination degeneracy, yielding a well-localized solution consistent with a moderately eccentric orbit.
Paper: Orbital and Pulsation Analysis of 42 Heartbeat Stars Discovered in TESS Data
Authors: Min-Yu Li, Sheng-Bang Qian, Ai-Ying Zhou, Li-Ying Zhu, Wen-Ping Liao, Lin-Feng Chang, Er-Gang Zhao, Xiang-Dong Shi, Fu-Xing Li, Qi-Bin Sun, Ping Li
Figure caption: Fit results of TIC 16791467. The K95+ model (solid red line) fitted to the phase-folded light curve (black dots) in the top panel. The lower panel shows the residuals of the fit. The dashed red line indicates a zero point. The unit of T0p is TBJD = BJD−2,457,000. Note: the plot shows phases 0−2 to make the fitting results clear, and phases 1−2 are an exact copy of phases 0−1.
Paper: Constraints on the Orbit of the Young Substellar Companion GQ Lup B from High-resolution Spectroscopy and VLTI/GRAVITY Astrometry 
Authors: Vidya Venkatesan, S. Blunt, J. J. Wang, S. Lacour, G.-D. Marleau, G. A. L. Coleman, L. Guerrero, W. O. Balmer, L. Pueyo, T. Stolker, J. Kammerer, N. Pourré, M. Nowak, E. Rickman, A. Sivaramakrishnan, D. Sing, K. Wagner, A.-M. Lagrange, R. Abuter, A. Amorim, R. Asensio-Torres, J.-P. Berger, H. Beust, A. Boccaletti, M. Bonnefoy, H. Bonnet, M. S. Bordoni, G. Bourdarot, W. Brandner, F. Cantalloube, P. Caselli, B. Charnay, G. Chauvin, A. Chavez, A. Chomez, E. Choquet, V. Christiaens, Y. Clénet, V. Coudé du Foresto, A. Cridland, R. Davies, R. Dembet, J. Dexter, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, N. M. Förster Schreiber, P. Garcia, R. Garcia Lopez, E. Gendron, R. Genzel, S. Gillessen, J. H. Girard, S. Grant, X. Haubois, G. Heissel, Th. Henning, S. Hinkley, S. Hippler, M. Houllé, Z. Hubert, L. Jocou, M. Keppler, P. Kervella, L. Kreidberg, N. T. Kurtovic, V. Lapeyrère, J.-B. Le Bouquin, D. Lutz, A.-L. Maire, F. Mang, A. Mérand, C. Mordasini, D. Mouillet, E. Nasedkin, T. Ott, G. P. P. L. Otten, C. Paladini, T. Paumard, K. Perraut, G. Perrin, S. Petrus, O. Pfuhl, D. C. Ribeiro, Z. Rustamkulov, J. Shangguan, T. Shimizu, A. Shields, J. Stadler, O. Straub, C. Straubmeier, E. Sturm, L. J. Tacconi, A. Vigan, F. Vincent, S. D. von Fellenberg, F. Widmann, T. O. Winterhalder, J. Woillez, S. Yazici
Figure caption: Corner plot of the posterior distributions for Case GRAVLowRV (see Table 5), which includes all available astrometry (including GRAVITY) and low-precision radial velocity measurement. The contours represent the 1σ, 2σ, and 3σ credible intervals, with individual posterior samples beyond the 3σ level shown as blue points. Strong covariances between eccentricity, inclination, and semimajor axis are apparent.
Paper: Orbital and Pulsation Analysis of 42 Heartbeat Stars Discovered in TESS Data
Authors: Min-Yu Li, Sheng-Bang Qian, Ai-Ying Zhou, Li-Ying Zhu, Wen-Ping Liao, Lin-Feng Chang, Er-Gang Zhao, Xiang-Dong Shi, Fu-Xing Li, Qi-Bin Sun, Ping Li
Figure caption: Corner plot of the MCMC fit procedure for TIC 16791467. Red vertical lines indicate the median values of the presented histograms for each parameter. Black vertical dashed lines show 1 σ uncertainties.
Paper: Constraints on the Orbit of the Young Substellar Companion GQ Lup B from High-resolution Spectroscopy and VLTI/GRAVITY Astrometry 
Authors: Vidya Venkatesan, S. Blunt, J. J. Wang, S. Lacour, G.-D. Marleau, G. A. L. Coleman, L. Guerrero, W. O. Balmer, L. Pueyo, T. Stolker, J. Kammerer, N. Pourré, M. Nowak, E. Rickman, A. Sivaramakrishnan, D. Sing, K. Wagner, A.-M. Lagrange, R. Abuter, A. Amorim, R. Asensio-Torres, J.-P. Berger, H. Beust, A. Boccaletti, M. Bonnefoy, H. Bonnet, M. S. Bordoni, G. Bourdarot, W. Brandner, F. Cantalloube, P. Caselli, B. Charnay, G. Chauvin, A. Chavez, A. Chomez, E. Choquet, V. Christiaens, Y. Clénet, V. Coudé du Foresto, A. Cridland, R. Davies, R. Dembet, J. Dexter, A. Drescher, G. Duvert, A. Eckart, F. Eisenhauer, N. M. Förster Schreiber, P. Garcia, R. Garcia Lopez, E. Gendron, R. Genzel, S. Gillessen, J. H. Girard, S. Grant, X. Haubois, G. Heissel, Th. Henning, S. Hinkley, S. Hippler, M. Houllé, Z. Hubert, L. Jocou, M. Keppler, P. Kervella, L. Kreidberg, N. T. Kurtovic, V. Lapeyrère, J.-B. Le Bouquin, D. Lutz, A.-L. Maire, F. Mang, A. Mérand, C. Mordasini, D. Mouillet, E. Nasedkin, T. Ott, G. P. P. L. Otten, C. Paladini, T. Paumard, K. Perraut, G. Perrin, S. Petrus, O. Pfuhl, D. C. Ribeiro, Z. Rustamkulov, J. Shangguan, T. Shimizu, A. Shields, J. Stadler, O. Straub, C. Straubmeier, E. Sturm, L. J. Tacconi, A. Vigan, F. Vincent, S. D. von Fellenberg, F. Widmann, T. O. Winterhalder, J. Woillez, S. Yazici
Figure caption: Inclination and longitude of ascending node (Ω) distributions for the GRAVLowRV-case orbit of GQ Lup B (blue), compared against the circumstellar disk (M. A. MacGregor et al. 2017), stellar spin axis (C. Broeg et al. 2007), and GQ Lup C’s disk (C. Lazzoni et al. 2020). The bottom panel shows the mutual inclination angle between the planet and each reference plane.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Radial gas mass flow rate in each radius from 60 pc to 10 kpc in three models. The solid black line shows the time-averaged gas flow rate, and the shaded area shows the standard deviation of the gas flow rate. To account for the SMBH’s motion, mass transport rates from 500 pc to 10 kpc were calculated in a coordinate system stationary with respect to the system’s center of gravity, whereas the rates from 60 pc to 500 pc were calculated in a coordinate system stationary with respect to the SMBH.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Radial gas mass flow rate in each radius from 60 pc to 10 kpc in three models. This figure is calculated using only high-density particles (nH > 700 cm−3), so this figure focuses only on the dense component of mass transport in Figure 6. The solid black line shows the averaged gas flow rate, and the shaded area shows the standard deviation. To account for the SMBH’s motion, mass transport rates from 500 pc to 10 kpc were calculated in a coordinate system stationary with respect to the system’s center of gravity, whereas the rates from 60 pc to 500 pc were calculated in a coordinate system stationary with respect to the SMBH.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Gas clump mass and specific angular momentum evolution in the fiducial model.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Gas clump orbits in a stationary system with respect to a bar potential fixed to the x-axis in the fiducial model. As the bar potential is fixed to the X-axis and rotates counterclockwise, the first and third quadrants are the regions subject to negative torque (blue) and the second and fourth quadrants to positive torque (red).
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Normalized gravitational torque map in three models. Columns, arranged left-to-right, show snapshots at 600 Myr, 800 Myr, and 1000 Myr; rows, ordered from top to bottom, correspond to bulge-to-stellar-disk mass ratios of Mbulge/Mdisk = 0.02,  0.10, and 0.20. The green contour shows the gas surface density at 50 M⊙ yr−1. Each panel shows a 12 kpc × 12 kpc region around a galactic center.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Mass distribution of gas clumps with varying FoF density thresholds in the fiducial model. ﹩{\bar{N}}_{{\rm{c}}}﹩ denotes the mean number of clumps per snapshot per logarithmic x-bin, averaged over 400 snapshots from 600 Myr to 1 Gyr at a temporal resolution of 1 Myr.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Final masses and lifetimes of gas clumps identified with an FoF density threshold of 700 cm−3 in the fiducial model between 600 Myr and 1 Gyr. The black solid line represents the average lifetime of clumps in each gas clump mass bin.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: Evolution of gas clump mass and specific angular momentum in the lower-resolution model with Mbulge/Mdisk = 0.02.
Paper: Dynamical Mechanism of Episodic Gas Accretion to the Central Region of Spiral Galaxies
Authors: Naomichi Yutani, Nozomu Kawakatu, Takayuki Saitoh, Keiichi Wada
Figure caption: The contribution of pressure gradient torque (∣τprg,z∣/(∣τprg,z∣ + ∣τG,z∣)) vs. gas number density at 600 Myr in the fiducial model.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Elemental spectrum of Ni calculated in models “c” with primary 2H and B (orange curves) compared with V1 (blue circles) and AMS-02 data (black diamonds). For details see Figure 24 caption.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Elemental spectra of H-F calculated in models “c” with primary 2H and B (orange curves) compared with V1 (blue circles) and AMS-02 data (black diamonds). The black dashed lines show GALPROP-HelMod VLISM spectra (M. J. Boschini et al. 2020, 2021a, 2022a, 2022b) tuned to AMS-02 data where available, otherwise they are tuned to ACE-CRIS and HEAO-3-C2 measurements. Red curves over AMS-02 data points show spectra modulated with HelMod (M. J. Boschini et al. 2020, 2021a, 2022a, 2022b) and corresponding to the period of data taking.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Elemental spectra of Ne-Ar calculated in models “c” with primary 2H and B (orange curves) compared with V1 (blue circles) and AMS-02 data (black diamonds). For details see the caption of Figure 24.
Paper: Voyager 1 Observations of Galactic Cosmic-Ray Isotopes in the Very Local Interstellar Medium: Evidence for Primary 2H and B
Authors: A. C. Cummings, I. V. Moskalenko, B. C. Heikkila, G. Jóhannesson, T. A. Porter
Figure caption: Elemental spectra of K-Co calculated in models “c” with primary 2H and B (orange curves) compared with V1 (blue circles) and AMS-02 data (black diamonds). For details see the caption of Figure 24.
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: Diagram showing the geometry of the graduated cylindrical shell model, reproduced from A. Thernisien (2011). Panel (a) is the axial plane cross-section and panel (b) is the edge-on cross-section.
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: 2013 April 11 CME observations and model fits. Panels (a) and (b) show the in situ data (black) with the HeXCor and cylindrical fittings overlaid (red). Panels (c)–(e) show all three geometries at approximately Earth-impact from the perspectives of the front or Earth view (heliographic longitude = 0°)), east side view (heliographic longitude = 270°), and top or north view (heliographic latitude = 90°), respectively. The pure GCS reconstruction is in green, HeXCor in red, and cylindrical model in blue. The Sun (yellow, not to scale), Earth (blue, not to scale), and solar equatorial plane are also shown.
Paper: Machine Learning Classification of COSMOS2020 Galaxies: Quiescent versus Star-forming
Authors: Vahid Asadi, Nima Chartab, Akram Hasani Zonoozi, Hosein Haghi, Ghassem Gozaliasl, Aryana Haghjoo, Bahram Mobasher
Figure caption: Distribution of total galaxies and the quiescent galaxy fraction as a function of redshift bins in the mock sample for MQG ≥ 109.5M⊙. The plot highlights the significant decline in the fraction of quiescent galaxies at z > 3.5.
Paper: Machine Learning Classification of COSMOS2020 Galaxies: Quiescent versus Star-forming
Authors: Vahid Asadi, Nima Chartab, Akram Hasani Zonoozi, Hosein Haghi, Ghassem Gozaliasl, Aryana Haghjoo, Bahram Mobasher
Figure caption: Overview of the data analysis pipeline used in this study.
Paper: Machine Learning Classification of COSMOS2020 Galaxies: Quiescent versus Star-forming
Authors: Vahid Asadi, Nima Chartab, Akram Hasani Zonoozi, Hosein Haghi, Ghassem Gozaliasl, Aryana Haghjoo, Bahram Mobasher
Figure caption: Redshift distributions of training and testing sets.
Paper: HeXCor: A Hybrid Magnetic Flux-rope Model of Coronal Mass Ejections Combining In Situ Measurements with Remote Sensing Observations
Authors: Matthew Dupertuis, Jie Zhang, Eleni Nikou, Suman K. Dhakal
Figure caption: Right-handed (s = 1) eastward (d = −1) for γ = 30°, 45°.