adsabs/AstroCLIMB huggingface dataset:
Paper: Discovery and Timing of Millisecond Pulsars with the Arecibo 327 MHz Drift-scan Survey
Authors: Evan F. Lewis, Timothy E. E. Olszanski, Julia S. Deneva, Paulo C. C. Freire, Maura A. McLaughlin, Kevin Stovall, Manjari Bagchi, Jose G. Martinez, Benetge B. P. Perera
Figure caption: The TOA residuals as a function of orbital phase for the three binary pulsars in this paper, with 1σ error bars. Blue: Arecibo, 327 MHz; orange: Arecibo, 430 MHz; red: GMRT, 650 MHz; and black: Arecibo, 1.4 GHz. An orbital phase of 0.25 corresponds to a superior conjunction.
Paper: A Near-infrared-faint, Far-infrared-luminous Dusty Galaxy at z ∼ 5 in COSMOS-Web
Authors: Jed McKinney, Sinclaire M. Manning, Olivia R. Cooper, Arianna S. Long, Hollis Akins, Caitlin M. Casey, Andreas L. Faisst, Maximilien Franco, Christopher C. Hayward, Erini Lambrides, Georgios Magdis, Katherine E. Whitaker, Min Yun, Jaclyn B. Champagne, Nicole E. Drakos, Fabrizio Gentile, Steven Gillman, Ghassem Gozaliasl, Olivier Ilbert, Shuowen Jin, Anton M. Koekemoer, Vasily Kokorev, Daizhong Liu, R. Michael Rich, Brant E. Robertson, Francesco Valentino, John R. Weaver, Jorge A. Zavala, Natalie Allen, Jeyhan S. Kartaltepe, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Marko Shuntov, Sune Toft
Figure caption: F444W/F277W color–magnitude diagram for galaxies in COSMOS-Web. We show every galaxy over the 77 arcmin2 area in the background, with contours drawn at the 16th, 50th, and 84th percentiles. From within that sample, we highlight F444W sources that drop out of the F150W filter (purple circles), and 4 < z < 6,  M */M ⊙ > 1010 galaxies with counterparts in COSMOS2020 (diamonds; Weaver et al. 2022). SMGs with 3 GHz counterparts are shown with dark gray circles. Red tracks correspond to redshifted empirical SEDs between z = 2–4 (dashed) and z = 4–6 (solid) from the ALESS sample (da Cunha et al. 2015) at progressively higher A  V . We normalize the ALESS tracks such that the F444W flux is approximately that of the averaged optically faint ALESS SEDs for their mean redshift: ∼2 nJy for ﹩\langle z{\rangle }_{{OIR}-{faint}}^{{ALESS}}=3.7﹩ (da Cunha et al. 2015). AzTECC71 (black star) is among the reddest population of galaxies found in the first six pointings of COSMOS-Web, is redder than known 4 < z phot < 6 massive galaxies from COSMOS2020, and is brighter in F444W than most objects that drop out of F150W. AzTECC71 is also the faintest F444W source with F277W-F444W >0.2 and an FIR counterpart confirmed with an ALMA or VLA detection.
Paper: A Near-infrared-faint, Far-infrared-luminous Dusty Galaxy at z ∼ 5 in COSMOS-Web
Authors: Jed McKinney, Sinclaire M. Manning, Olivia R. Cooper, Arianna S. Long, Hollis Akins, Caitlin M. Casey, Andreas L. Faisst, Maximilien Franco, Christopher C. Hayward, Erini Lambrides, Georgios Magdis, Katherine E. Whitaker, Min Yun, Jaclyn B. Champagne, Nicole E. Drakos, Fabrizio Gentile, Steven Gillman, Ghassem Gozaliasl, Olivier Ilbert, Shuowen Jin, Anton M. Koekemoer, Vasily Kokorev, Daizhong Liu, R. Michael Rich, Brant E. Robertson, Francesco Valentino, John R. Weaver, Jorge A. Zavala, Natalie Allen, Jeyhan S. Kartaltepe, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Marko Shuntov, Sune Toft
Figure caption: 2″ × 2″ JWST/NIRCam cutouts from COSMOS-Web (M. Franco et al. 2023, in preparation; Casey et al. 2023) of AzTECC71. On each panel we show the elliptical aperture fit to the F444W detection (black dashed ellipse). The rightmost panel shows the residual between the F444W detection and a PSF-convolved 2D Sersic profile with r 1/2 = 0.″32 and n sersic = 0.74. Red circles denote the PSF for each band shown. The S/Ns of the flux densities extracted through the elliptical aperture are listed above each panel.
Paper: A Near-infrared-faint, Far-infrared-luminous Dusty Galaxy at z ∼ 5 in COSMOS-Web
Authors: Jed McKinney, Sinclaire M. Manning, Olivia R. Cooper, Arianna S. Long, Hollis Akins, Caitlin M. Casey, Andreas L. Faisst, Maximilien Franco, Christopher C. Hayward, Erini Lambrides, Georgios Magdis, Katherine E. Whitaker, Min Yun, Jaclyn B. Champagne, Nicole E. Drakos, Fabrizio Gentile, Steven Gillman, Ghassem Gozaliasl, Olivier Ilbert, Shuowen Jin, Anton M. Koekemoer, Vasily Kokorev, Daizhong Liu, R. Michael Rich, Brant E. Robertson, Francesco Valentino, John R. Weaver, Jorge A. Zavala, Natalie Allen, Jeyhan S. Kartaltepe, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Marko Shuntov, Sune Toft
Figure caption: 3.″6 × 3.″6 RGB image constructed from R = F444W, G = F277W, B = (F115W+F150W stack). White contours are ALMA Band 6 continuum at 1250 μm drawn at 5 through 10σ in increments of 1σ. The source is not spatially resolved by ALMA. The white circle corresponds to the centroid of the F444W image. The white + is the centroid of a 2D Gaussian fit to the ALMA detection.
Paper: A Near-infrared-faint, Far-infrared-luminous Dusty Galaxy at z ∼ 5 in COSMOS-Web
Authors: Jed McKinney, Sinclaire M. Manning, Olivia R. Cooper, Arianna S. Long, Hollis Akins, Caitlin M. Casey, Andreas L. Faisst, Maximilien Franco, Christopher C. Hayward, Erini Lambrides, Georgios Magdis, Katherine E. Whitaker, Min Yun, Jaclyn B. Champagne, Nicole E. Drakos, Fabrizio Gentile, Steven Gillman, Ghassem Gozaliasl, Olivier Ilbert, Shuowen Jin, Anton M. Koekemoer, Vasily Kokorev, Daizhong Liu, R. Michael Rich, Brant E. Robertson, Francesco Valentino, John R. Weaver, Jorge A. Zavala, Natalie Allen, Jeyhan S. Kartaltepe, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Marko Shuntov, Sune Toft
Figure caption: Corner plot showing the two-dimensional joint posterior distributions for dust SED fit parameters L IR and T dust derived using MCIRSED. The vertical dashed lines in the 1D histograms for each parameter show the 68% interquartile range (outer lines) and the median value (central line). The dust temperature and IR luminosity are highly covariant given the lack of rest-frame constraint straddling the dust SED peak.
Paper: Discovery and Timing of Millisecond Pulsars with the Arecibo 327 MHz Drift-scan Survey
Authors: Evan F. Lewis, Timothy E. E. Olszanski, Julia S. Deneva, Paulo C. C. Freire, Maura A. McLaughlin, Kevin Stovall, Manjari Bagchi, Jose G. Martinez, Benetge B. P. Perera
Figure caption: Polarization-calibrated composite profiles for PSRs J2116+1345 (left) and J2212+2450 (right), with polarization position angle, at 327 MHz (top), 430 MHz (middle), and 1380 MHz (bottom). The pulse profiles are centered at a pulse phase of 0.5. The y-axes are in arbitrary units. Black lines represent total intensity (Stokes I ), red lines represent linear polarization (Stokes L), and blue lines represent circular polarization (Stokes V ). The best-fit RMs have been applied to each profile as described in Section 3.
Paper: A Near-infrared-faint, Far-infrared-luminous Dusty Galaxy at z ∼ 5 in COSMOS-Web
Authors: Jed McKinney, Sinclaire M. Manning, Olivia R. Cooper, Arianna S. Long, Hollis Akins, Caitlin M. Casey, Andreas L. Faisst, Maximilien Franco, Christopher C. Hayward, Erini Lambrides, Georgios Magdis, Katherine E. Whitaker, Min Yun, Jaclyn B. Champagne, Nicole E. Drakos, Fabrizio Gentile, Steven Gillman, Ghassem Gozaliasl, Olivier Ilbert, Shuowen Jin, Anton M. Koekemoer, Vasily Kokorev, Daizhong Liu, R. Michael Rich, Brant E. Robertson, Francesco Valentino, John R. Weaver, Jorge A. Zavala, Natalie Allen, Jeyhan S. Kartaltepe, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Marko Shuntov, Sune Toft
Figure caption: Posterior (left) and cumulative (right) redshift distribution function from fitting only the IR SED with MMPz (black hatched), only the optical/NIR with CIGALE (dotted–dashed), the full optical through IR SED with CIGALE (blue shaded), and a CIGALE fit excluding JWST (dotted). We report the photometric redshift (z  p ) from the peak of the optical/NIR + FIR posterior distribution function and its 16th and 84th percentiles.
Paper: A Near-infrared-faint, Far-infrared-luminous Dusty Galaxy at z ∼ 5 in COSMOS-Web
Authors: Jed McKinney, Sinclaire M. Manning, Olivia R. Cooper, Arianna S. Long, Hollis Akins, Caitlin M. Casey, Andreas L. Faisst, Maximilien Franco, Christopher C. Hayward, Erini Lambrides, Georgios Magdis, Katherine E. Whitaker, Min Yun, Jaclyn B. Champagne, Nicole E. Drakos, Fabrizio Gentile, Steven Gillman, Ghassem Gozaliasl, Olivier Ilbert, Shuowen Jin, Anton M. Koekemoer, Vasily Kokorev, Daizhong Liu, R. Michael Rich, Brant E. Robertson, Francesco Valentino, John R. Weaver, Jorge A. Zavala, Natalie Allen, Jeyhan S. Kartaltepe, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Marko Shuntov, Sune Toft
Figure caption: Stellar mass posterior distribution from the full optical through IR SED with CIGALE (blue shaded), and a CIGALE fit excluding JWST (solid line). We report the stellar mass (M *) from the peak of the OIR  +  FIR CIGALE posterior and its 16th and 84th percentiles. Including JWST constraints shifts the most likely stellar mass down by ∼0.2 dex and lowers the uncertainty by a factor of 2.
Paper: A Near-infrared-faint, Far-infrared-luminous Dusty Galaxy at z ∼ 5 in COSMOS-Web
Authors: Jed McKinney, Sinclaire M. Manning, Olivia R. Cooper, Arianna S. Long, Hollis Akins, Caitlin M. Casey, Andreas L. Faisst, Maximilien Franco, Christopher C. Hayward, Erini Lambrides, Georgios Magdis, Katherine E. Whitaker, Min Yun, Jaclyn B. Champagne, Nicole E. Drakos, Fabrizio Gentile, Steven Gillman, Ghassem Gozaliasl, Olivier Ilbert, Shuowen Jin, Anton M. Koekemoer, Vasily Kokorev, Daizhong Liu, R. Michael Rich, Brant E. Robertson, Francesco Valentino, John R. Weaver, Jorge A. Zavala, Natalie Allen, Jeyhan S. Kartaltepe, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Marko Shuntov, Sune Toft
Figure caption: 80″  ×  80″ cutout of the SCUBA-2 S/N map (left) illustrating the deblending of the SCUBA-2 850 μm flux using ALMA Band 6 positional priors for AzTECC71 (red diamond) and the nearby z = 0.829 dusty galaxy (black circle). The model based on two scaled point sources fixed to the Band 6 positions is shown in the middle panel, with the residual shown in the far right.
Paper: Fermi Constraints on the Ejecta Speed and Prompt Emission Region of the Distant GRB 220101A
Authors: Lorenzo Scotton, Frédéric Piron, Nicola Omodei, Niccolò Di Lalla, Elisabetta Bissaldi
Figure caption: Fermi multidetector light curve of GRB 220101A prompt emission in increasing energy bands from top to bottom. The first four panels present count rates, while the last panel presents the energy of the LAT-observed events. The red dashed vertical line denotes the time of the trigger T 0, while the black dashed vertical lines indicate the time intervals chosen for the time-resolved spectral analysis, covering the main emission episode observed by the LAT.
Paper: Fermi Constraints on the Ejecta Speed and Prompt Emission Region of the Distant GRB 220101A
Authors: Lorenzo Scotton, Frédéric Piron, Nicola Omodei, Niccolò Di Lalla, Elisabetta Bissaldi
Figure caption: Left: light curve showing the two LLE peaks with the best-fit FRED2P function superimposed. Right: Γ γ γ  and ﹩{{\rm{\Gamma }}}_{\mathrm{Tr}}﹩ as a function of the ratio of the radii at which the high- and low-energy emissions were produced in time bins B and C.
Paper: Fermi Constraints on the Ejecta Speed and Prompt Emission Region of the Distant GRB 220101A
Authors: Lorenzo Scotton, Frédéric Piron, Nicola Omodei, Niccolò Di Lalla, Elisabetta Bissaldi
Figure caption: Left: GRB count spectra and residuals (upper panel) and SED (lower panel) from Band fits to GBM+LLE data in time bin B + C with pyXSPEC. Right: same for BandExpCut.
Paper: Fermi Constraints on the Ejecta Speed and Prompt Emission Region of the Distant GRB 220101A
Authors: Lorenzo Scotton, Frédéric Piron, Nicola Omodei, Niccolò Di Lalla, Elisabetta Bissaldi
Figure caption: Left: GRB count spectra and residuals (upper panel) and SED (lower panel) from ISSM fits to GBM+LLE data in time bin B + C with pyXSPEC. Right: same for ISSMExpCut.
Paper: Discovery and Timing of Millisecond Pulsars with the Arecibo 327 MHz Drift-scan Survey
Authors: Evan F. Lewis, Timothy E. E. Olszanski, Julia S. Deneva, Paulo C. C. Freire, Maura A. McLaughlin, Kevin Stovall, Manjari Bagchi, Jose G. Martinez, Benetge B. P. Perera
Figure caption: The orbital periods and median companion masses for recycled MSPs with known companion star types. The black dashed line represents the evolutionary models of NS binaries containing He WDs calculated by Tauris & Savonije (1999), and the He WDs (dark green circles) are shown to closely follow this relation. Black widows are shown with black triangles, and redbacks are shown with red squares. Figure and caption adapted from Strader et al. (2019) and Ray et al. (2022).
Paper: Discovery and Timing of Millisecond Pulsars with the Arecibo 327 MHz Drift-scan Survey
Authors: Evan F. Lewis, Timothy E. E. Olszanski, Julia S. Deneva, Paulo C. C. Freire, Maura A. McLaughlin, Kevin Stovall, Manjari Bagchi, Jose G. Martinez, Benetge B. P. Perera
Figure caption: Top panel: in gray, the distribution of spin-down luminosities (﹩\dot{E}﹩) for recycled pulsars with P < 100 ms and ﹩\dot{P}\lt {10}^{-17}﹩, with the distribution for AO327-discovered pulsars outlined in red and the pulsars from this work in blue. Bottom panel: the distribution of orbital periods for binary pulsars discovered by the PALFA (cyan), HTRU-North (red), HTRU-South (orange), and AO327 (black) surveys, with the pulsars from this work in blue. The total distribution from these four surveys is plotted in gray, and the vertical dashed black line represents an orbital period of 1 day.
Paper: Discovery and Timing of Millisecond Pulsars with the Arecibo 327 MHz Drift-scan Survey
Authors: Evan F. Lewis, Timothy E. E. Olszanski, Julia S. Deneva, Paulo C. C. Freire, Maura A. McLaughlin, Kevin Stovall, Manjari Bagchi, Jose G. Martinez, Benetge B. P. Perera
Figure caption: The radio timing positions for PSRs J2055+1545 (top) and J2116+1345 (bottom) are represented by red ellipses, plotted against the 68% (green dashed line) and 95% (blue dotted line) confidence ellipses for their potentially coincident Fermi sources. The ellipses representing the radio timing positions are roughly 2000 times the size of the 1σ uncertainties in the sky positions derived from pulsar timing.
Paper: Discovery and Timing of Millisecond Pulsars with the Arecibo 327 MHz Drift-scan Survey
Authors: Evan F. Lewis, Timothy E. E. Olszanski, Julia S. Deneva, Paulo C. C. Freire, Maura A. McLaughlin, Kevin Stovall, Manjari Bagchi, Jose G. Martinez, Benetge B. P. Perera
Figure caption: Composite pulse profiles of the four MSPs, with the colors indicating different observatories and observing frequencies. Profiles are centered at a pulse phase of 0.5 for clarity. From bottom to top—blue: Arecibo, 327 MHz; orange: Arecibo, 430 MHz; red: GMRT, 650 MHz; and black: Arecibo, 1.4 GHz. Each profile has been normalized, and is vertically offset from one another for clarity. The disparities in the pulsar flux and number of observations at each frequency cause some profiles to have a lower S/N than others.
Paper: Discovery and Timing of Millisecond Pulsars with the Arecibo 327 MHz Drift-scan Survey
Authors: Evan F. Lewis, Timothy E. E. Olszanski, Julia S. Deneva, Paulo C. C. Freire, Maura A. McLaughlin, Kevin Stovall, Manjari Bagchi, Jose G. Martinez, Benetge B. P. Perera
Figure caption:                    ﹩P\mbox{--}\dot{P}﹩ diagram of recycled pulsars from the ATNF catalog with P < 100 ms and ﹩\dot{P}\lt {10}^{-16}﹩. Pulsars from this work are shown and labeled in blue, and AO327-discovered pulsars are shown in red. Lines of constant minimum surface magnetic field (in Gauss) and spin-down luminosity (in erg s−1) are shown.
Paper: Discovery and Timing of Millisecond Pulsars with the Arecibo 327 MHz Drift-scan Survey
Authors: Evan F. Lewis, Timothy E. E. Olszanski, Julia S. Deneva, Paulo C. C. Freire, Maura A. McLaughlin, Kevin Stovall, Manjari Bagchi, Jose G. Martinez, Benetge B. P. Perera
Figure caption: Intensity vs. pulse phase and observation time for J2055 exiting its radio eclipse on MJD 57817, taken with Arecibo at 327 MHz. The pulsed radio emission is delayed from orbital phases 0.42–0.45. Two cycles of the pulse phase are shown.
Paper: Discovery and Timing of Millisecond Pulsars with the Arecibo 327 MHz Drift-scan Survey
Authors: Evan F. Lewis, Timothy E. E. Olszanski, Julia S. Deneva, Paulo C. C. Freire, Maura A. McLaughlin, Kevin Stovall, Manjari Bagchi, Jose G. Martinez, Benetge B. P. Perera
Figure caption: Top panel: phase-aligned integrated Fermi gamma-ray pulse profile (black) and 327 MHz Arecibo profile (red). Bottom panel: phase-time diagram for the gamma-ray pulsations from PSR J2116+1345. Two cycles of the pulse phase are shown.
Paper: Discovery and Timing of Millisecond Pulsars with the Arecibo 327 MHz Drift-scan Survey
Authors: Evan F. Lewis, Timothy E. E. Olszanski, Julia S. Deneva, Paulo C. C. Freire, Maura A. McLaughlin, Kevin Stovall, Manjari Bagchi, Jose G. Martinez, Benetge B. P. Perera
Figure caption: The TOA residuals as a function of observing date for the four pulsars in this paper, with 1σ error bars. Blue: Arecibo, 327 MHz; orange: Arecibo, 430 MHz; red: GMRT, 650 MHz; and black: Arecibo, 1.4 GHz.
Paper: A Near-infrared-faint, Far-infrared-luminous Dusty Galaxy at z ∼ 5 in COSMOS-Web
Authors: Jed McKinney, Sinclaire M. Manning, Olivia R. Cooper, Arianna S. Long, Hollis Akins, Caitlin M. Casey, Andreas L. Faisst, Maximilien Franco, Christopher C. Hayward, Erini Lambrides, Georgios Magdis, Katherine E. Whitaker, Min Yun, Jaclyn B. Champagne, Nicole E. Drakos, Fabrizio Gentile, Steven Gillman, Ghassem Gozaliasl, Olivier Ilbert, Shuowen Jin, Anton M. Koekemoer, Vasily Kokorev, Daizhong Liu, R. Michael Rich, Brant E. Robertson, Francesco Valentino, John R. Weaver, Jorge A. Zavala, Natalie Allen, Jeyhan S. Kartaltepe, Henry Joy McCracken, Louise Paquereau, Jason Rhodes, Marko Shuntov, Sune Toft
Figure caption: SED for AzTECC71. Observations are shown in blue, with circles denoting detections and arrows 3σ upper limits. The preferred z = 5.7 solution is shown for CIGALE with a black solid line. The optical/NIR-only fit is largely ruled out by the FIR/submillimeter data. The purple shaded region contains the uncertainty about the MCIRSED best fit (solid purple line). For comparison we show the average SED of z > 3 H − [4.5] selected galaxies from Wang et al. (2016) in blue (solid). The best-fit SED to COS-3 mm-1, a z ∼ 5 3 mm selected galaxy from Williams et al. (2019) is shown in orange. AzTECC71 is fainter in the optical than H − [4.5] selected massive and dusty star-forming galaxies from Wang et al. (2016), but brighter than this sample in the FIR if it were scaled to match AzTECC71 at z = 5.7 and 4.5 μm (blue dashed). Similar to the IR flux of COS-3 mm-1, AzTECC71 is likely part of a more IR-luminous population of massive galaxies at z > 4.
Paper: ALMA 300 pc Resolution Imaging of a z = 6.79 Quasar: No Evidence for Supermassive Black Hole Influence on the C II Kinematics
Authors: Romain A. Meyer, Marcel Neeleman, Fabian Walter, Bram Venemans
Figure caption: Top row: continuum emission and velocity-integrated [C II] emission maps of J0109–3047 at ∼300 pc resolution. The black crosses indicate the NIR position of J0109–3047 based on the Gaia-corrected positions of stars close to the quasar in the NIR images (Venemans et al. 2020). Bottom row: [C II] mean velocity and velocity dispersion fields. All maps are produced from the complete Cycles 1, 2, 3, and 8 data. The synthesized beam is 0.″049 × 0.″041. The continuum and [C II] velocity-integrated emission maps are produced using residual scaling. The contours are given at (3, 6, 9, 12)σ as black lines (no negative (−6, −3)σ emission is detected).
Paper: The Contribution and FIP Bias of Three Types of Materials inside ICMEs Associated with Different Flare Intensities
Authors: Hui Fu, Xinzheng Shi, Zhenghua Huang, Youqian Qi, Lidong Xia
Figure caption: The contributions of the three types of materials inside NFCs (panel (a)), LQFe–FCs (panel (b)), MQFe–FCs (panel (c)), and HQFe–FCs (panel (d)). The black plus signs represent the measures of ICMEs, and the horizontal and vertical white dashed lines denote the threshold for inferring the origination and generation mechanisms of the ICME materials. The subregions with sky blue, green, and red denote the corona materials (with lower Q Fe and A He), heated corona materials (with higher Q Fe and lower A He), and chromospheric evaporation materials (with higher Q Fe and A He), respectively. It is clear that the proportions of the three types of materials are significantly different for the ICMEs associated with different flare intensities.
Paper: The Contribution and FIP Bias of Three Types of Materials inside ICMEs Associated with Different Flare Intensities
Authors: Hui Fu, Xinzheng Shi, Zhenghua Huang, Youqian Qi, Lidong Xia
Figure caption: The FIP bias of the three types of materials inside NFCs (panel (a)), LQFe–FCs (panel (b)), MQFe–FCs (panel (c)), and HQFe–FCs (panel (d)). The distributions are normalized by the samples of the present type of materials, as we concentrate on the comparison of the distribution characteristics between different types of ICME materials. The blue, green, and red bars represent the corona materials, heated corona materials, and chromospheric evaporation materials, respectively. The black vertical lines in each panel denote the median FIP bias. The median and lower and upper quartiles of FIP bias are also presented in each panel. We can see that the FIP bias of chromospheric evaporation materials is higher than that of corona materials and heated corona materials in all three types of FCs.
Paper: Understanding the Lateral Drifting of an Erupting Filament with a Data-constrained Magnetohydrodynamic Simulation
Authors: J. H. Guo, 金涵 郭, Y. Qiu, 晔 邱, Y. W. Ni, 仪伟 倪, Y. Guo, 洋 郭, C. Li, 川 李, Y. H. Gao, 宇航 高, B. Schmieder, S. Poedts, P. F. Chen, 鹏飞 陈
Figure caption: Typical magnetic-field lines constructed from the NLFFF model at 10:00 UT, which are compared with (a), (c) SDO/AIA 171 Å, and (b) CHASE/HIS Hα line-center images. The yellow tubes represent the field lines of the erupting filament, the green tubes represent those of the chromosphere fibrils, and the pink tubes represent those of the overlying field. (a) Full-disk image of AIA 171 Å at 10:00 UT. Some selected field lines are overlaid in the simulated active region. (b) CHASE/HIS Hα line-center images at 09:33 UT. (c) Zoomed-in result of the red dotted box in panel (a). (d) The side view of the reconstructed magnetic structures.
Paper: Understanding the Lateral Drifting of an Erupting Filament with a Data-constrained Magnetohydrodynamic Simulation
Authors: J. H. Guo, 金涵 郭, Y. Qiu, 晔 邱, Y. W. Ni, 仪伟 倪, Y. Guo, 洋 郭, C. Li, 川 李, Y. H. Gao, 宇航 高, B. Schmieder, S. Poedts, P. F. Chen, 鹏飞 陈
Figure caption: Comparison between the simulated flux ropes and observed filaments at (a), (d) 10:23 UT, (b), (e) 10:38 UT, and (c), (f) 10:50. Panels (a)–(c) depict the magnetic structures that are back-projected onto the SDO/AIA 304 Å images. The insert figures in panels (a), (b), and (c) display the GONG/Hα line-center image, field lines in a γ-shaped morphology, and CHASE/HIS Hα red-wing image, respectively. Panels (d)–(f) show the SDO/AIA 171 Å running-difference images. The cyan oval in panel (f) represents the filament material that moves westward.
Paper: Understanding the Lateral Drifting of an Erupting Filament with a Data-constrained Magnetohydrodynamic Simulation
Authors: J. H. Guo, 金涵 郭, Y. Qiu, 晔 邱, Y. W. Ni, 仪伟 倪, Y. Guo, 洋 郭, C. Li, 川 李, Y. H. Gao, 宇航 高, B. Schmieder, S. Poedts, P. F. Chen, 鹏飞 陈
Figure caption: Panels (a)–(f) show the magnetic reconnection illustrations recognized by the field-line connectivity (panels (a), (c), and (e)) and J/B distributions (panels (b), (d), and (f)) in the x–z plane. The purple, cyan, and green lines represent the pre-reconnection field lines, newly formed flux ropes, and flare loops, respectively. The asterisk signs indicate the occurrence sites of magnetic reconnection. Panels (g) and (h) show the top and side views of the flare loops (yellow tubes) and the simulated flux rope (cyan tubes) at 10:50 UT, respectively. These field lines are overlaid on the CHASE/HIS Hα line-center images.