adsabs/AstroCLIMB huggingface dataset:
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: The age differences between the HRD-based and CMD-based estimates for the Ophiuchus (red dots), US (blue dots), UCL/LCC (gray dots), and V1062 Sco (green dots) groups are plotted as a function of SPT. Ages are derived using the PARSEC models in conjunction with two sets of SPT-to-effective temperature conversions: PM13 and HH14 (top panels) and KH95 and L+03 (bottom panels).
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Comparison of SPT derived in this study with literature values for 2155 common objects (upper panel). The lower panel displays the robust standard deviation of SPT differences across SPTs, with error bars indicating the range of SPT bins employed to compute these dispersions.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Median ages of UCL/LCC (top) and US (bottom) within four spectral ranges: F type but later than F5, G types, K types, M types (M0−M5), derived with different stellar evolutionary tracks.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Same as Figure 8 but using the Baraffe models.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Same as Figure 8 but using the MIST models.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Mass distributions of the sources in the US group derived with different evolutionary models.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Comparison of stellar Lums as derived in this study and as reported in the literature. The dashed line represents the one-to-one relationship.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Age estimates for the US (upper panels) and UCL/LCC (lower panels) groups are plotted against SPT. For F/G-type stars, ages are derived using PISA models (gray); for K/M-type stars, SPOTS (green) and Baraffe (red) models are applied. These age calculations incorporate two SPT-to-effective temperature conversion data sets: PM13 and HH14 (left panels) and KH95 and L+03 (right panels). In each panel, the magenta filled squares shows the median age within the F5-G (the Pisa model) and K-M5 type (the SPOTS models) bins, with error bars indicating the 1σ uncertainty range. In the right panel, age distributions of the sources derived from the PISA (gray-filled histogram), SPOTS (green filled histogram), and Baraffe (red filled histogram) models are overlaid for comparison.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Three-dimensional spatial distribution of young stars in the Sco-Cen complex, with stellar ages color coded. Each star’s age is smoothed by averaging with the ages of its nine nearest neighbors. The Galactic XYZ coordinate system is adopted, with the Sun positioned at (0, 0, 0) and the Z = 0 plane aligned parallel to the Galactic plane.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Same as Figure 15 but showing the sources within different age bins in each panel.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Extinction-corrected infrared color excess vs. SPT for the sources in the Sco-Cen complex. In each panel, the blue filled circles are for the sources without the color excess and the red filled circles are for the ones with the color excess, and the magenta solid line marks the 3σExcess level.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: A comparison of SPTs derived in this work and in the literature for the sources used in the construction of spectral templates. The standard deviations on the SPT differences are 0.5, 0.8, 1.0, and 0.7 subclass for the sources with the SPTs later than M0, between K0 and M0, between G0 and K0, and earlier than G0, respectively. The color is represented by the normalized density.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Disk fractions of the Ophiuchus, US, UCL/LCC, and V1062 Sco groups as a function of their ages for the K/M-type sources.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: The timescale of disk decay estimated with different evolutionary models.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Same as Figure 11 but for the UCL/LCC group.
Paper: A Comprehensive Gaia Spectroscopic Study of Stars in the Scorpius-Centaurus Complex: Star Formation History and Disk Lifetime
Authors: Min Fang, Gregory J. Herczeg
Figure caption: Example spectral templates of Gaia XP spectra for young stars constructed in this work.
Paper: JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion
Authors: E. Baron, C. Ashall, J. M. DerKacy, P. Hoeflich, K. Medler, M. Shahbandeh, E. Fereidouni, C. M. Pfeffer, T. Mera, W. B. Hoogendam, S. Shiber, K. Auchettl, P. J. Brown, C. R. Burns, A. Burrow, D. A. Coulter, M. Engesser, G. Folatelli, O. Fox, L. Galbany, M. Guolo, J. T. Hinkle, Mark E. Huber, E. Y. Hsiao, T. de Jaeger, D. O. Jones, S. Kumar, J. Lu, P. A. Mazzali, N. Morrell, M. M. Phillips, A. Rest, N. B. Suntzeff, B. J. Shappee, Jennifer Shi, M. D. Stritzinger, L. Strolger, T. Temim, S. Tinyanont, M. Tucker, L. Wang, Q. Wang, Y. Yang
Figure caption: Panchromatic spectral comparison of SNe II observed with JWST (SNe 2022acko, 2023ixf, and 2024ggi) during the plateau phase and other historical SNe II (SNe 1987A D. K. Aitken et al. 1988) and (SN 2005af R. Kotak et al. 2006) observed in the MIR at similar phases. The SN 2022acko data shown here have been re-reduced using updated versions of the JWST pipeline (v1.18.0+jwst_1371.pmap and v1.17.1+jwst_1363.pmap for the NIRSpec and MIRI/MRS data, respectively) relative to the data first presented in M. Shahbandeh et al. (2024).
Paper: JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion
Authors: E. Baron, C. Ashall, J. M. DerKacy, P. Hoeflich, K. Medler, M. Shahbandeh, E. Fereidouni, C. M. Pfeffer, T. Mera, W. B. Hoogendam, S. Shiber, K. Auchettl, P. J. Brown, C. R. Burns, A. Burrow, D. A. Coulter, M. Engesser, G. Folatelli, O. Fox, L. Galbany, M. Guolo, J. T. Hinkle, Mark E. Huber, E. Y. Hsiao, T. de Jaeger, D. O. Jones, S. Kumar, J. Lu, P. A. Mazzali, N. Morrell, M. M. Phillips, A. Rest, N. B. Suntzeff, B. J. Shappee, Jennifer Shi, M. D. Stritzinger, L. Strolger, T. Temim, S. Tinyanont, M. Tucker, L. Wang, Q. Wang, Y. Yang
Figure caption: The full dereddened SED of SN 2024ggi. The UH88 optical spectrum was obtained on MJD 60470 (day ∼ 60); the IRTF spectrum was obtained on day 44. The NIRSpec spectrum was obtained on MJD 60466.46 (day 55), and the MIRI/LRS spectrum was obtained in the same visit as the NIRSpec. We note that the F700W and F2100W images were taken ∼9 days after the JWST spectra, which might explain the flux discrepancy between the photometry and the spectra.
Paper: JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion
Authors: E. Baron, C. Ashall, J. M. DerKacy, P. Hoeflich, K. Medler, M. Shahbandeh, E. Fereidouni, C. M. Pfeffer, T. Mera, W. B. Hoogendam, S. Shiber, K. Auchettl, P. J. Brown, C. R. Burns, A. Burrow, D. A. Coulter, M. Engesser, G. Folatelli, O. Fox, L. Galbany, M. Guolo, J. T. Hinkle, Mark E. Huber, E. Y. Hsiao, T. de Jaeger, D. O. Jones, S. Kumar, J. Lu, P. A. Mazzali, N. Morrell, M. M. Phillips, A. Rest, N. B. Suntzeff, B. J. Shappee, Jennifer Shi, M. D. Stritzinger, L. Strolger, T. Temim, S. Tinyanont, M. Tucker, L. Wang, Q. Wang, Y. Yang
Figure caption: A velocity-space comparison of some strong P-Cygni profiles found in JWST and ground-based observations of SNe 2022acko, 2023ixf, and 2024ggi.
Paper: JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion
Authors: E. Baron, C. Ashall, J. M. DerKacy, P. Hoeflich, K. Medler, M. Shahbandeh, E. Fereidouni, C. M. Pfeffer, T. Mera, W. B. Hoogendam, S. Shiber, K. Auchettl, P. J. Brown, C. R. Burns, A. Burrow, D. A. Coulter, M. Engesser, G. Folatelli, O. Fox, L. Galbany, M. Guolo, J. T. Hinkle, Mark E. Huber, E. Y. Hsiao, T. de Jaeger, D. O. Jones, S. Kumar, J. Lu, P. A. Mazzali, N. Morrell, M. M. Phillips, A. Rest, N. B. Suntzeff, B. J. Shappee, Jennifer Shi, M. D. Stritzinger, L. Strolger, T. Temim, S. Tinyanont, M. Tucker, L. Wang, Q. Wang, Y. Yang
Figure caption: A composite two-band color image constructed from the MIRI imaging of NGC 3621 using filters F700W and F2100W. The location of SN 2024ggi is highlighted with the turquoise circle.
Paper: JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion
Authors: E. Baron, C. Ashall, J. M. DerKacy, P. Hoeflich, K. Medler, M. Shahbandeh, E. Fereidouni, C. M. Pfeffer, T. Mera, W. B. Hoogendam, S. Shiber, K. Auchettl, P. J. Brown, C. R. Burns, A. Burrow, D. A. Coulter, M. Engesser, G. Folatelli, O. Fox, L. Galbany, M. Guolo, J. T. Hinkle, Mark E. Huber, E. Y. Hsiao, T. de Jaeger, D. O. Jones, S. Kumar, J. Lu, P. A. Mazzali, N. Morrell, M. M. Phillips, A. Rest, N. B. Suntzeff, B. J. Shappee, Jennifer Shi, M. D. Stritzinger, L. Strolger, T. Temim, S. Tinyanont, M. Tucker, L. Wang, Q. Wang, Y. Yang
Figure caption: The optical, ground-based NIR, and JWST SN 2024ggi spectra with prominent H I lines identified.
Paper: JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion
Authors: E. Baron, C. Ashall, J. M. DerKacy, P. Hoeflich, K. Medler, M. Shahbandeh, E. Fereidouni, C. M. Pfeffer, T. Mera, W. B. Hoogendam, S. Shiber, K. Auchettl, P. J. Brown, C. R. Burns, A. Burrow, D. A. Coulter, M. Engesser, G. Folatelli, O. Fox, L. Galbany, M. Guolo, J. T. Hinkle, Mark E. Huber, E. Y. Hsiao, T. de Jaeger, D. O. Jones, S. Kumar, J. Lu, P. A. Mazzali, N. Morrell, M. M. Phillips, A. Rest, N. B. Suntzeff, B. J. Shappee, Jennifer Shi, M. D. Stritzinger, L. Strolger, T. Temim, S. Tinyanont, M. Tucker, L. Wang, Q. Wang, Y. Yang
Figure caption: The observed day 55 SN 2024ggi ground-based and JWST spectrum, the PHOENIX model, and the PHOENIX model with all He I lines turned off. The one He I line that is prominent in the model spectrum is nearly coincident with the Huα line. Thus, there is no strong evidence for He I lines at this epoch and observed wavelength range.
Paper: JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion
Authors: E. Baron, C. Ashall, J. M. DerKacy, P. Hoeflich, K. Medler, M. Shahbandeh, E. Fereidouni, C. M. Pfeffer, T. Mera, W. B. Hoogendam, S. Shiber, K. Auchettl, P. J. Brown, C. R. Burns, A. Burrow, D. A. Coulter, M. Engesser, G. Folatelli, O. Fox, L. Galbany, M. Guolo, J. T. Hinkle, Mark E. Huber, E. Y. Hsiao, T. de Jaeger, D. O. Jones, S. Kumar, J. Lu, P. A. Mazzali, N. Morrell, M. M. Phillips, A. Rest, N. B. Suntzeff, B. J. Shappee, Jennifer Shi, M. D. Stritzinger, L. Strolger, T. Temim, S. Tinyanont, M. Tucker, L. Wang, Q. Wang, Y. Yang
Figure caption: A close-up of the P-Cygni features formed by Paγ and the C I 1.069 μm line (from the IRTF spectrum). Also indicated is the feature on the maximum of Paγ that is almost certainly due to the Mg II 1.0926 μm line (see Section 5). The insets show the velocity extent of the two P-Cygni lines.
Paper: JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion
Authors: E. Baron, C. Ashall, J. M. DerKacy, P. Hoeflich, K. Medler, M. Shahbandeh, E. Fereidouni, C. M. Pfeffer, T. Mera, W. B. Hoogendam, S. Shiber, K. Auchettl, P. J. Brown, C. R. Burns, A. Burrow, D. A. Coulter, M. Engesser, G. Folatelli, O. Fox, L. Galbany, M. Guolo, J. T. Hinkle, Mark E. Huber, E. Y. Hsiao, T. de Jaeger, D. O. Jones, S. Kumar, J. Lu, P. A. Mazzali, N. Morrell, M. M. Phillips, A. Rest, N. B. Suntzeff, B. J. Shappee, Jennifer Shi, M. D. Stritzinger, L. Strolger, T. Temim, S. Tinyanont, M. Tucker, L. Wang, Q. Wang, Y. Yang
Figure caption: The observed day 55 SN 2024ggi JWST spectrum, the PHOENIX model, and the PHOENIX model with all H I lines turned off. Most of the observed spectral features are due to H I lines.
Paper: JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion
Authors: E. Baron, C. Ashall, J. M. DerKacy, P. Hoeflich, K. Medler, M. Shahbandeh, E. Fereidouni, C. M. Pfeffer, T. Mera, W. B. Hoogendam, S. Shiber, K. Auchettl, P. J. Brown, C. R. Burns, A. Burrow, D. A. Coulter, M. Engesser, G. Folatelli, O. Fox, L. Galbany, M. Guolo, J. T. Hinkle, Mark E. Huber, E. Y. Hsiao, T. de Jaeger, D. O. Jones, S. Kumar, J. Lu, P. A. Mazzali, N. Morrell, M. M. Phillips, A. Rest, N. B. Suntzeff, B. J. Shappee, Jennifer Shi, M. D. Stritzinger, L. Strolger, T. Temim, S. Tinyanont, M. Tucker, L. Wang, Q. Wang, Y. Yang
Figure caption: Same as Figure 7 but with all the line opacity except for that due to Mg II turned off.
Paper: JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion
Authors: E. Baron, C. Ashall, J. M. DerKacy, P. Hoeflich, K. Medler, M. Shahbandeh, E. Fereidouni, C. M. Pfeffer, T. Mera, W. B. Hoogendam, S. Shiber, K. Auchettl, P. J. Brown, C. R. Burns, A. Burrow, D. A. Coulter, M. Engesser, G. Folatelli, O. Fox, L. Galbany, M. Guolo, J. T. Hinkle, Mark E. Huber, E. Y. Hsiao, T. de Jaeger, D. O. Jones, S. Kumar, J. Lu, P. A. Mazzali, N. Morrell, M. M. Phillips, A. Rest, N. B. Suntzeff, B. J. Shappee, Jennifer Shi, M. D. Stritzinger, L. Strolger, T. Temim, S. Tinyanont, M. Tucker, L. Wang, Q. Wang, Y. Yang
Figure caption: The line profiles of Hα (upper left panel), Ca IR triplet (upper right panel), Paα (lower left panel), and Pfα (lower right panel). Models with more extended velocity profiles capture the velocity extent of the optical features but do a poorer job of reproducing the shape of the NIR and MIR features. The synthetic spectra have been scaled for clarity. See Appendix B for more details.
Paper: JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion
Authors: E. Baron, C. Ashall, J. M. DerKacy, P. Hoeflich, K. Medler, M. Shahbandeh, E. Fereidouni, C. M. Pfeffer, T. Mera, W. B. Hoogendam, S. Shiber, K. Auchettl, P. J. Brown, C. R. Burns, A. Burrow, D. A. Coulter, M. Engesser, G. Folatelli, O. Fox, L. Galbany, M. Guolo, J. T. Hinkle, Mark E. Huber, E. Y. Hsiao, T. de Jaeger, D. O. Jones, S. Kumar, J. Lu, P. A. Mazzali, N. Morrell, M. M. Phillips, A. Rest, N. B. Suntzeff, B. J. Shappee, Jennifer Shi, M. D. Stritzinger, L. Strolger, T. Temim, S. Tinyanont, M. Tucker, L. Wang, Q. Wang, Y. Yang
Figure caption: The observed day 55 SN 2024ggi ground-based and JWST spectra compared to the PHOENIX model (see Section 4.2). In this and subsequent model plots, the synthetic spectrum has been scaled to the observed spectrum at 3 μm.
Paper: JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion
Authors: E. Baron, C. Ashall, J. M. DerKacy, P. Hoeflich, K. Medler, M. Shahbandeh, E. Fereidouni, C. M. Pfeffer, T. Mera, W. B. Hoogendam, S. Shiber, K. Auchettl, P. J. Brown, C. R. Burns, A. Burrow, D. A. Coulter, M. Engesser, G. Folatelli, O. Fox, L. Galbany, M. Guolo, J. T. Hinkle, Mark E. Huber, E. Y. Hsiao, T. de Jaeger, D. O. Jones, S. Kumar, J. Lu, P. A. Mazzali, N. Morrell, M. M. Phillips, A. Rest, N. B. Suntzeff, B. J. Shappee, Jennifer Shi, M. D. Stritzinger, L. Strolger, T. Temim, S. Tinyanont, M. Tucker, L. Wang, Q. Wang, Y. Yang
Figure caption: The three different line types seen in the models. Top panel: the strongly net-emission P-Cygni Hα line. Middle panel: a nearly pure emission line (transition). Bottom panel: a P-Cygni line that appears to be pure absorption in Figure 6. The line is essentially detached (see Section 4.3).
Paper: JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion
Authors: E. Baron, C. Ashall, J. M. DerKacy, P. Hoeflich, K. Medler, M. Shahbandeh, E. Fereidouni, C. M. Pfeffer, T. Mera, W. B. Hoogendam, S. Shiber, K. Auchettl, P. J. Brown, C. R. Burns, A. Burrow, D. A. Coulter, M. Engesser, G. Folatelli, O. Fox, L. Galbany, M. Guolo, J. T. Hinkle, Mark E. Huber, E. Y. Hsiao, T. de Jaeger, D. O. Jones, S. Kumar, J. Lu, P. A. Mazzali, N. Morrell, M. M. Phillips, A. Rest, N. B. Suntzeff, B. J. Shappee, Jennifer Shi, M. D. Stritzinger, L. Strolger, T. Temim, S. Tinyanont, M. Tucker, L. Wang, Q. Wang, Y. Yang
Figure caption: A SYNOW fit to the Hα line in SN 2024ggi. The optical depth is τ = 10, vphot = 3500 km s−1, the density profile is given by an exponential with ve = 2000 km s−1, and vmax = 20,000 km s−1.
Paper: JWST Observations of SN 2024ggi. I. Interpretation and Model Comparison of the Type II Supernova 2024ggi at 55 Days past Explosion
Authors: E. Baron, C. Ashall, J. M. DerKacy, P. Hoeflich, K. Medler, M. Shahbandeh, E. Fereidouni, C. M. Pfeffer, T. Mera, W. B. Hoogendam, S. Shiber, K. Auchettl, P. J. Brown, C. R. Burns, A. Burrow, D. A. Coulter, M. Engesser, G. Folatelli, O. Fox, L. Galbany, M. Guolo, J. T. Hinkle, Mark E. Huber, E. Y. Hsiao, T. de Jaeger, D. O. Jones, S. Kumar, J. Lu, P. A. Mazzali, N. Morrell, M. M. Phillips, A. Rest, N. B. Suntzeff, B. J. Shappee, Jennifer Shi, M. D. Stritzinger, L. Strolger, T. Temim, S. Tinyanont, M. Tucker, L. Wang, Q. Wang, Y. Yang
Figure caption: The fiducial model with vmax = 5900 km s−1 and a model with vmax = 12,250 km s−1.
Paper: A Face-on Accretion Disk Geometry Revealed by Millimeter-wave Periodicity in Sgr A∗
Authors: Kazuki Yanagisawa, Tomoharu Oka, Ryo Ariyama, Kazuki Yanagihara, Yuhei Iwata, Mikiya M. Takahashi
Figure caption: (a) Light curves of Sgr A∗ obtained over 77 epochs from 2015 to 2022. The red curves indicate datasets in which periodic variations were identified by I20+, while the magenta curve highlights the periodic variation newly identified in this study. The vertical gray dashed lines indicate the boundaries of the calendar years (UT) when the data were observed. (b) Light curve of Sgr A∗ observed on 2021 July 22 with ALMA at 229.5 (red), 231.2 (green), 231.9 (blue), and 232.6 GHz (cyan). The horizontal axis shows time in minutes relative to the observation start.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: General Implicit Runge–Kutta Integrators for Multifluid Gas–Dust Aerodynamic Drag
Authors: Giovanni Tedeschi-Prades, Til Birnstiel, Klaus Dolag, Barbara Ercolano, Mark Hutchison
Figure caption: Simulation outputs and analytical solutions for the three DUSTYBOX benchmark tests described in P. Huang & X.-N. Bai (2022). The system is composed of a gas fluid and two dust fluids. The simulation outputs are shown as dots, while the analytical solution is drawn as a continuous line. For the nonstiff Test A, the time step is chosen according to the CFL condition Equation (40), while for the stiff Tests B and C, the time step is, respectively, Δt = 0.005 and Δt = 0.05. The integrator used (GIRK with ﹩{{ \mathcal D }}_{{\rm{\Delta }}t/2}{{ \mathcal H }}_{{\rm{\Delta }}t}{{ \mathcal D }}_{{\rm{\Delta }}t/2}﹩ Strang splitting) is able to correctly capture the evolution of the mixture for all stiffness regimes. For Test C, we also show how much the integrator undershoots the analytical solution for the gas velocity before converging.
Paper: A Face-on Accretion Disk Geometry Revealed by Millimeter-wave Periodicity in Sgr A∗
Authors: Kazuki Yanagisawa, Tomoharu Oka, Ryo Ariyama, Kazuki Yanagihara, Yuhei Iwata, Mikiya M. Takahashi
Figure caption: (a) Light curve fitted with MCMC. Gray points represent the 232.6 GHz observations, and the red line shows the fit using Equation (3). (b) Corner plot for all eight parameters. Each panel displays the correlations between parameters, with the posterior distributions shown along the top. Contours correspond to 1σ, 2σ, and 3σ levels, and the indicated uncertainties represent 1σ. The posterior distribution of a* is flat, indicating that this parameter cannot be constrained by the current model. Note that r is expressed in units of rg.
Paper: A Face-on Accretion Disk Geometry Revealed by Millimeter-wave Periodicity in Sgr A∗
Authors: Kazuki Yanagisawa, Tomoharu Oka, Ryo Ariyama, Kazuki Yanagihara, Yuhei Iwata, Mikiya M. Takahashi
Figure caption: Top: fitting of the Doppler-boosted model to observational data. The best-fit parameters ﹩({T}_{\rm{min}\,},{\beta }_{\rm{min}}\sin {i}_{\,\rm{min}}),﹩ corresponding to the minimum reduced chi-square ﹩{\chi }_{\,\rm{red,min}\,}^{2}﹩, are shown with the blue curve, while the observed flux density at 232.6 GHz is plotted with red. Bottom: residuals between the model and observations. With residuals below 1% of the sinusoidal amplitude, the model shows strong consistency with the observations. The 232.6 GHz light curve is shown as a representative example as the same sinusoidal modulation is consistently seen in the other SpWs.
Paper: A Face-on Accretion Disk Geometry Revealed by Millimeter-wave Periodicity in Sgr A∗
Authors: Kazuki Yanagisawa, Tomoharu Oka, Ryo Ariyama, Kazuki Yanagihara, Yuhei Iwata, Mikiya M. Takahashi
Figure caption: GLS periodogram of the light curve observed on 2021 July 22. The black line shows the LS power of the observed light curve in this study. The FAP was estimated by generating 105 red-noise light curves and is indicated at the 3σ (blue dashed line) and 5σ (red dashed line) levels. Peaks in the LS power are marked with magenta points, with the corresponding FAP values indicated simultaneously.
Paper: A Face-on Accretion Disk Geometry Revealed by Millimeter-wave Periodicity in Sgr A∗
Authors: Kazuki Yanagisawa, Tomoharu Oka, Ryo Ariyama, Kazuki Yanagihara, Yuhei Iwata, Mikiya M. Takahashi
Figure caption: Schematic diagram of the hotspot model. The left panel illustrates a face-on view of the accretion disk surrounding Sgr A∗, while the right panel shows an edge-on perspective. The angle θ denotes the azimuthal position of the hotspot along its orbit, and i represents the inclination angle between the disk’s angular momentum vector and the line of sight (LoS).