adsabs/AstroCLIMB huggingface dataset:
Paper: Dual Origins of Rapid Flare Ribbon Downflows in an X9-class Solar Flare
Authors: Ryan J. French, William H. Ashfield, Cole A. Tamburri, Maria D. Kazachenko, Marie Dominique, Marcel Corchado Albelo, Amir Caspi
Figure caption: Top: HXR spectra (black markers) from ASO-S/HXI, within the time windows of 12:15:00–12:15:30 UT (left panel) and 12:25:16–12:25:46 UT (right panel). These time periods encapsulate part of our two stages of interest, with the former focusing on the peak of the HXR emission and the latter centered around the strongest Si IV downflow observed in the later stage. In the second panel, we label in the data the locations of residual background emission from 241Am (see text) and the residual background noise level. The red curve in each panel presents the total spectral fit, consisting of two isothermal components and a nonthermal component (cyan, blue, and orange, respectively), with key parameters as noted in the legend; a photospheric albedo correction (gray curve) is also included. Bottom: the fit residuals (the differences between black markers and red curves) normalized by respective uncertainties in each energy bin.
Paper: Dual Origins of Rapid Flare Ribbon Downflows in an X9-class Solar Flare
Authors: Ryan J. French, William H. Ashfield, Cole A. Tamburri, Maria D. Kazachenko, Marie Dominique, Marcel Corchado Albelo, Amir Caspi
Figure caption: Si IV 1402.77 Å line profile and triple-Gaussian fit for a selection of the fastest-redshift pixels across the sit-and-stare raster (plotted as green circles in Figure 1). Black line plots the spectral data (with error bars), green the sum of the triple-Gaussian fit, and yellow/orange/red the individual Gaussian fit profiles. The pixel position and velocity of the redmost Gaussian are noted in the top-right corner of each panel.
Paper: Under Pressure: Decoding the Effect of High Densities on Derived Nebular Properties
Authors: Zorayda Martinez, Danielle A. Berg, Bethan L. James, Karla Z. Arellano-Córdova, Daniel P. Stark, Peter Senchyna, Evan D. Skillman, Noah S. J. Rogers, John Chisholm
Figure caption: The Cloudy model relationship between O+2/O+ and ﹩\mathrm{log}U﹩. The left panel shows 3D plots of the bicubic fits for each grid of models, and the marker color denotes ne ranging from 102 to 106 cm−3. In the right panel, we show a 2D projection where the range of ne is shown by the shaded region. The metallicities range between 0.05 Z⊙ and 0.40 Z⊙ as indicated by the color bar in the upper-right plot. Additionally, the solid lines show the fits at ne = 102 cm−3 and the dotted lines mark where the fits are at ne = 106 cm−3. The effect of ne on O+2/O+ is minimal making this probe of ﹩\mathrm{log}U﹩ extremely robust.
Paper: Dual Origins of Rapid Flare Ribbon Downflows in an X9-class Solar Flare
Authors: Ryan J. French, William H. Ashfield, Cole A. Tamburri, Maria D. Kazachenko, Marie Dominique, Marcel Corchado Albelo, Amir Caspi
Figure caption: Top: K-means clustering map of Si IV 1402.77 Å spectra, marking the locations of the colored grouped spectra from panels below. Bottom: forty clustering groups of Si IV 1402.77 Å spectra. Profiles are ordered by the full width at 30% of maximum, sorted from lowest to highest.
Paper: Dual Origins of Rapid Flare Ribbon Downflows in an X9-class Solar Flare
Authors: Ryan J. French, William H. Ashfield, Cole A. Tamburri, Maria D. Kazachenko, Marie Dominique, Marcel Corchado Albelo, Amir Caspi
Figure caption: Top: 120 s detrended Si IV Doppler velocity within the southern flare ribbon (detrended version of the red maximum velocity curve in Figure 2). Bottom left: wavelet power spectrum of time series plotted in top panel (on a log color scale). Orange lines mark the cone of influence. Bottom right: global wavelet power for the same dataset. The red line marks the 95% confidence threshold.
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: Superposed epoch analysis of the normalized magnetic field fluctuations over the ten 30 minute subintervals within Alfvénic slow solar wind interval. Top-left panel: parallel (z) magnetic field fluctuations for forward (black curve) and backward (orange curve; ±) fast MS modes ﹩\delta {B}_{z}^{{f}^{\pm }}/{B}_{0}﹩. Middle-left two panels: forward and backward transverse magnetic field fluctuations ﹩\delta {B}_{x,y}^{{f}^{\pm }}﹩ for fast MS modes. Bottom-left panel: forward (black curve) and backward (orange curve) Alfvén ﹩\delta {B}_{x}^{{A}^{\pm }}﹩ and advected magnetic island ﹩(\delta {B}_{x}^{i}﹩, green curve) modes. Top-right panel: parallel (z) magnetic field fluctuations for forward (black curve) and backward (orange curve; ±) slow MS modes ﹩\delta {B}_{z}^{{s}^{\pm }}/{B}_{0}﹩. Middle-right two panels: forward and backward transverse velocity fluctuations ﹩\delta {B}_{x,y}^{{s}^{\pm }}﹩ for slow MS modes. Bottom-right panel: forward (black curve) and backward (orange curve) Alfvén ﹩\delta {B}_{y}^{{A}^{\pm }}﹩ and advected magnetic island ﹩(\delta {B}_{y}^{i}﹩, green curve) modes.
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: Data corresponding to an Alfvénic slow (left panels) and fast wind (right panels) period. From top to bottom: the field magnitude, B (in nT); the solar wind bulk speed, Vsw(in kilometers per second); the proton number density, Np (in cm−3); the angle, θBV (in degrees) between the magnetic and flow velocity vectors; the plasma beta, βp; the mach number, MA; and correlation coefficient between the velocity and magnetic fluctuation in z-component. The ten 30 minute Alfvénic slow and eight 30 minute fast intervals are highlighted with vertical dashed lines.
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: Superposed epoch analysis of the normalized velocity field fluctuations over the ten 30 minute subintervals within Alfvénic slow solar wind. Top-left panel: parallel (z) velocity component for forward (black curve) and backward (orange curve; ±) fast MS modes ﹩\delta {u}_{z}^{{f}^{\pm }}/{U}_{0}﹩. Middle-left two panels: forward and backward transverse velocity fluctuations ﹩\delta {u}_{x,y}^{{f}^{\pm }}﹩ for fast MS modes. Bottom-left panel: forward (black curve) and backward (orange curve) Alfvén ﹩\delta {u}_{x}^{{A}^{\pm }}﹩ modes. Top-right panel: parallel (z−) velocity component for forward (black curve) and backward (orange curve; ±) slow MS modes ﹩\delta {u}_{z}^{{s}^{\pm }}/{U}_{0}﹩. Middle-right two panels: forward and backward transverse velocity fluctuations ﹩\delta {u}_{x,y}^{{s}^{\pm }}﹩ for slow MS modes. Bottom-right panel: forward (black curve) and backward (orange curve) Alfvén ﹩\delta {u}_{y}^{{A}^{\pm }}﹩ modes.
Paper: Investigation of Turbulent Fluctuations in the Fast and Alfvénic Slow Solar Wind at 1 au
Authors: Monika Karki, Gary P. Zank, Laxman Adhikari, Ashok Silwal, Sujan Prasad Gautam, Prashrit Baruwal, Prashant Baruwal, Ismita Tasnim, Lingling Zhao, Alexander Pitňa
Figure caption: Superposed epoch analysis showing the time series of the normalized density fluctuations over the ten 30 minute subintervals for an Alfvénic slow solar wind stream. Top panel: normalized density fluctuations for the entropy modes. Middle panel: normalized density fluctuations for the forward (blue curve) and backward (orange curve) fast MS modes. Bottom panel: normalized density fluctuations for the forward (blue curve) and backward (orange curve) slow MS modes. All fluctuating quantities are normalized to the mean density as labeled.
Paper: Extreme Geoeffectiveness by the Turbulent Sheath of the ICME of the 2024 October Space Weather Event
Authors: Smitha V. Thampi, Ankush Bhaskar, Indu Venugopal, Shibotosh Biswas, Vipin K. Yadav
Figure caption: Observations by MMS-1. (a) AE index (black) and solar wind dynamic pressure (yellow) during the period (derived from OMNI database), (b) the total magnetic field and its components, (c) densities of H+ and O+ ions measured by HPCA, (d) plasma beta, (e) bulk velocity components of O+ ions, (f) bulk velocity components of H+ ions, (g)–(i) fluxes of H+, O+, and He++ measured by HPCA.
Paper: Extreme Geoeffectiveness by the Turbulent Sheath of the ICME of the 2024 October Space Weather Event
Authors: Smitha V. Thampi, Ankush Bhaskar, Indu Venugopal, Shibotosh Biswas, Vipin K. Yadav
Figure caption: Left panel: schematic (not to scale) showing Earth’s sheath turbulence mapping to the ground magnetometer through open magnetic field lines and possible inference of magnetopause distance. Right panel: ground magnetometer observations of magnetic field perturbations as seen in the northward component. The geographic latitude, longitude, and L-shell values are shown with the station IDs. The distinct variation in magnetic field fluctuation marks open and closed field-line regions of the magnetosphere on 2024 October 10.
Paper: A Luminous and Hot Infrared through X-Ray Transient at a 5 kpc Offset from a Dwarf Galaxy
Authors: Jean J. Somalwar, Vikram Ravi, Raffaella Margutti, Ryan Chornock, Priyamvada Natarajan, Wenbin Lu, Charlotte Angus, Matthew J. Graham, Erica Hammerstein, Edward Nathan, Matt Nicholl, Kritti Sharma, Robert Stein, Frank Verdi, Yuhan Yao, Eric C. Bellm, Tracy X. Chen, Michael W. Coughlin, David Hale, Mansi M. Kasliwal, Russ R. Laher, Reed Riddle, Jesper Sollerman
Figure caption: Summary of emission from 24puz. The left panel shows the ZTF lightcurve on the top panel, the radio/millimeter upper limits in the middle panel, and the 0.3–10 keV Swift/XRT and XMM-Newton lightcurves in the bottom panel. The X-ray fluxes are computed as the unabsorbed, observed 0.3–10 keV flux assuming a Γ = 1.77 power law. The two Swift/XRT observations that are joined together by a line were individually nondetections, so we show the flux measured by stacking the two observations, which is significant. Dates of Keck I/LRIS spectroscopy are shown as dashed lines. The top right panels show the optical spectral sequence, which no significant features detected. The solid lines are smoothed by a Gaussian with width of 5 pix. The faded lines show the unsmoothed spectra. Commonly detected transient lines are shown as dashed blue lines; none are detected. The apparent line in the red, MJD 60520 spectrum near 4000 Å is a poorly subtracted sky line. The bottom right panel shows a zoom-in on the detected absorption lines, with the lines labeled in gray.
Paper: Extreme Geoeffectiveness by the Turbulent Sheath of the ICME of the 2024 October Space Weather Event
Authors: Smitha V. Thampi, Ankush Bhaskar, Indu Venugopal, Shibotosh Biswas, Vipin K. Yadav
Figure caption: The location of the GOES-16, GOES-18, and MMS spacecraft with respect to Earth’s bow shock and magnetopause boundaries on 2024 October 10 at 18:00 UT. The dashed circle represents the geosynchronous orbit, which is consistent with the in situ observations of fields and particles on board both GOES satellites.
Paper: Extreme Geoeffectiveness by the Turbulent Sheath of the ICME of the 2024 October Space Weather Event
Authors: Smitha V. Thampi, Ankush Bhaskar, Indu Venugopal, Shibotosh Biswas, Vipin K. Yadav
Figure caption: Magnetic field component Bz and electron flux data from GOES-16 (panels (a) and (b)) and GOES-18 (panels (c) and (d)). Note that the magnetic field shown here is a local field in GSM coordinates at geostationary orbit (GEO) altitudes, inside Earth’s magnetosheath.
Paper: Extreme Geoeffectiveness by the Turbulent Sheath of the ICME of the 2024 October Space Weather Event
Authors: Smitha V. Thampi, Ankush Bhaskar, Indu Venugopal, Shibotosh Biswas, Vipin K. Yadav
Figure caption: AMPERE-derived FACs corresponding to ICME sheath and MC phases (global polar maps), and the magnetic field observations from MAG/Aditya-L1 and SYM-H index (line plots respectively).
Paper: Extreme Geoeffectiveness by the Turbulent Sheath of the ICME of the 2024 October Space Weather Event
Authors: Smitha V. Thampi, Ankush Bhaskar, Indu Venugopal, Shibotosh Biswas, Vipin K. Yadav
Figure caption: Solar wind parameters and the geomagnetic SYM-H index for the period 2024 October 10–11 . The panels are (a) solar wind velocity, (b) proton density, (c) temperature, (d), (e), (f) total IMF and its y and z components, and (g) geomagnetic SYM-H index.
Paper: Eclipsing Stellar Flare on the Demon Star Algol Binary System Observed during the MAXI–NICER Follow-up Campaign in 2018
Authors: Kazuya Nakayama, Wataru Buz Iwakiri, Teruaki Enoto, Shun Inoue, Yuta Notsu, Keith Gendreau, Zaven Arzoumanian, Kenji Hamaguchi, Tatehiro Mihara
Figure caption: NICER (blue circles, sky-blue triangles) and MAXI (orange squares, red diamonds) count rates and luminosity in the 2.0–5.0 keV band of Algol, which are binned at 64 and 211 s (each MAXI scan) in the left and right panels, respectively. The MAXI data are added after being converted to the corresponding NICER count rate by PIMMS, assuming that the MAXI spectrum can be represented by a power law and the temperature was 4 keV. The time zero of MJD 58300.0 corresponds to 2018 July 1, 00:00 UT. The blue dotted line and green dotted line show the 2.0–5.0 keV NICER count rate and luminosity in the quiescent state on 2018 August 11, 2.0 counts s−1 and 9.5 × 1029 erg s−1 in the left and right panels, respectively.
Paper: Eclipsing Stellar Flare on the Demon Star Algol Binary System Observed during the MAXI–NICER Follow-up Campaign in 2018
Authors: Kazuya Nakayama, Wataru Buz Iwakiri, Teruaki Enoto, Shun Inoue, Yuta Notsu, Keith Gendreau, Zaven Arzoumanian, Kenji Hamaguchi, Tatehiro Mihara
Figure caption: Time evolutions of the best-fit NICER spectral parameters. (a) Absorbed flux in the 0.3–2.0 keV (blue circle), 2.0–10.0 keV (red square), and total (0.3–10.0 keV; orange diamond) bands. (b) Temperatures of the two plasma components. (c) EM calculated from the normalization of the vapec components, i.e., EM = 4πd2k × 1014, where d is the distance to the source (cm) assuming d = 28.8 pc = 8.9 × 1019 cm for Algol, and ﹩k=\frac{1{0}^{-14}}{4\pi {d}^{2}}\int {n}_{e}{n}_{{\rm{H}}}dV﹩, where ne and nH are the electron and hydrogen densities (cm−3), respectively, which is the normalization derived in Xspec. (d) Hydrogen-equivalent column density (NH). The last four points are not shown since the spectra are fitted well without the ISM absorption component.
Paper: Eclipsing Stellar Flare on the Demon Star Algol Binary System Observed during the MAXI–NICER Follow-up Campaign in 2018
Authors: Kazuya Nakayama, Wataru Buz Iwakiri, Teruaki Enoto, Shun Inoue, Yuta Notsu, Keith Gendreau, Zaven Arzoumanian, Kenji Hamaguchi, Tatehiro Mihara
Figure caption: Background-subtracted Algol flare spectra in the 0.3–8.0 keV band for the first NICER observation on MJD 58303.83 (ObsID 1200260101, exposure time 1068 s, panel (a)), before the eclipse on MJD 58304.34 (ObsID 1200260102, exposure time 1104 s, panel (b)), during the eclipse on MJD 58304.47 (ObsID 1200260102, exposure time 1104 s, panel (c)), and quiescent on MJD 58341.76 (ObsID 1200260104, exposure time 1024 s, panel (d)). The flare spectra are fitted with the tbabs (vapec + vapec + vapec + vapec) model. The quiescent spectrum is fitted with the two-temperature CIE plasma model, and its best-fit result is included in each flare fit with fixed parameters. The additional two collisionally ionized components of the flare are fitted, with the best-fit models shown by the solid red line, composed of low-temperature (blue dashed), high-temperature (green dashed–dotted), and an added Gaussian at the Fe-L line (purple dotted). The residuals, (data − model)/error, are shown in the bottom panels. The expected NICER background spectra (black dotted) are calculated with the SCORPEON model and shown for comparison.
Paper: Eclipsing Stellar Flare on the Demon Star Algol Binary System Observed during the MAXI–NICER Follow-up Campaign in 2018
Authors: Kazuya Nakayama, Wataru Buz Iwakiri, Teruaki Enoto, Shun Inoue, Yuta Notsu, Keith Gendreau, Zaven Arzoumanian, Kenji Hamaguchi, Tatehiro Mihara
Figure caption: Optical observation of Algol by TESS on MJD 58793.2–58795.8 (Photometer, 600–1000 nm wavelength, blue dot) folded at the orbital period of Algol (Porb in Table 1). The inset figure shows this TESS observation covering the entire orbital period. The 2.0–10.0 keV absorbed flux from the NICER flare observations is overlaid. The red shaded areas show the eclipse start and end times of X-rays. The blue horizontal dotted line shows the 2.0–10.0 keV NICER flux at the quiescent level of 1.4 × 10−11 erg cm−2 s−1. It should be noted that the TESS and NICER observations were not conducted simultaneously.
Paper: Callisto’s Nonresonant Orbit as an Outcome of Circum-Jovian Disk Substructure
Authors: Teng Ee Yap, Konstantin Batygin
Figure caption: Schematic of the circum-Jovian decretion disk. Gas and dust from the circumsolar accretion disk are subsumed into the Jovian disk from approximately one hydrostatic scale height via meridional flows and move outward beyond the magnetospheric truncation radius. Decretion ﹩\dot{M}﹩ is driven by turbulence manifesting as a macroscopic viscosity, and parametrized by the Shakura–Sunyaev α parameter. The four Galilean moons are envisioned to form beyond the ice line and pressure bump, and undergo Type I migration inward. The bump serves as a migration trap, preventing Callisto from convergent migration into resonance with Io, Europa, and Ganymede.
Paper: Callisto’s Nonresonant Orbit as an Outcome of Circum-Jovian Disk Substructure
Authors: Teng Ee Yap, Konstantin Batygin
Figure caption: Final simulation outcomes from exploration of Rα–w parameter space. Three main regimes are discerned: (red) for thin and tall disks to the top left, the bump is too “stiff” a trap, ultimately leading to a dynamical instability; (orange) for short and wide disks to the bottom right, the bump fails to trap the moons, leading to the formation of a 6:3:2:1 resonant chain; (green) between (red) and (orange) lies a “Goldilocks” zone wherein the bump can both function as a trap, and allow the moons to be “pushed” across it by migration in lockstep following resonant capture. This zone corresponds roughly to bump aspect ratios Δh between 0.45 and 0.6. Along its former boundary are simulations wherein alternatives to the resonant chain in (orange) are realized (light green: 8:4:2:1; and white: e.g., 12:6:3:2). The green star corresponds to the fiducial case discussed in Section 4.1. See Section 4.2 for a discussion.
Paper: Callisto’s Nonresonant Orbit as an Outcome of Circum-Jovian Disk Substructure
Authors: Teng Ee Yap, Konstantin Batygin
Figure caption: Plots of (a) the surface density and temperature profile of the disk, as well as (b) the disk aspect ratio and the characteristic Type I timescale for two hypothetical moons (one with ∼50 ppm and the other ∼100 ppm of Jupiter’s mass), where Rα = 2 and w = h0. Inset in (a) depicts a close-up view of the pressure bump, just beyond (i.e., 1.25 times) the ice line (r0 ∼ 0.04RHill). As discussed in Section 2.3, larger bodies migrate and have their eccentricities damped faster. Simulation results corresponding to these Σ(r) and h(r)/r profiles are discussed in Section 4.3 and presented in Figure 4.
Paper: Callisto’s Nonresonant Orbit as an Outcome of Circum-Jovian Disk Substructure
Authors: Teng Ee Yap, Konstantin Batygin
Figure caption: Simulation results for Rstop = 0.03RHill > RT = 5RJ and r0 = 0.18RHill, assuming fiducial Rα = 2.5 and w = 1.25h0. Panels indicate the (a) semimajor axes and (b) eccentricities of the moons, (c) their outer-inner period ratios, and (d) resonant arguments between Io, Europa, and Ganymede. Key resonant captures are denoted by vertical lines. See Section 4.1 for a discussion.
Paper: Callisto’s Nonresonant Orbit as an Outcome of Circum-Jovian Disk Substructure
Authors: Teng Ee Yap, Konstantin Batygin
Figure caption: Simulation results for Rstop = 0.03 RHill and r0 = 0.18 RHill, with Rα = 3.75 and w = 2h0. Panels indicate the (a) semimajor axes and (b) eccentricities of the moons, as well as (c) their outer-inner period ratios. Key resonant captures are denoted by vertical lines. This simulation, culminating in an 8:4:2:1 resonance, is an example of those constituting the “soft” transition between the regimes wherein (i) the intended result (i.e., 4:2:1 resonance between I, E, and G; C trapped at bump) and (ii) a 6:3:2:1 resonance between the four moons are achieved (see Figure 3). Variations on simulation outcomes at the “soft” transition (at Δh/w ∼ 0.45) include 12:6:3:2, 16:8:6:3, and 9:6:4:2 resonances. See Section 4.2 for a discussion.
Paper: Callisto’s Nonresonant Orbit as an Outcome of Circum-Jovian Disk Substructure
Authors: Teng Ee Yap, Konstantin Batygin
Figure caption: Simulation results for Rstop = 0.03 RHill and r0 = 0.18 RHill, with Rα = 4.5 and w = 1.25h0. Panels indicate the (a) semimajor axes of the moons and (b) their outer-inner period ratios. Key resonant captures are denoted by vertical lines. Here, the bump is too “sharp” (i.e., tall/thin; Δh/w ≳ 0.6) to allow for the trapped moon (i.e., I) to be “pushed” across once resonance is established, even with G. Eccentricities are “pumped” until a collision between E and G takes place, terminating the simulation. See Section 4.2 for discussion, and Figure 3 for all Rα–w pairs explored that correspond to resonant pileups at the bump, and eventual instability.
Paper: Callisto’s Nonresonant Orbit as an Outcome of Circum-Jovian Disk Substructure
Authors: Teng Ee Yap, Konstantin Batygin
Figure caption: Simulation results for Rstop = 0.03 RHill and r0 = 0.18 RHill, with Rα = 2.5 and w = 2h0. Panels indicate the (a) semimajor axes of the moons and (b) their outer-inner period ratios. Key resonant captures are denoted by vertical lines. Here, the bump is too “flat” (i.e., short/wide; Δh/w ≲ 0.45) to function as a migration trap. As such, all four moons individually make it past the bump, establishing a 6:3:2:1 resonance interior to it. See Section 4.2 for a discussion, and Figure 3 for all Rα–w pairs explored that correspond to this final outcome.
Paper: Callisto’s Nonresonant Orbit as an Outcome of Circum-Jovian Disk Substructure
Authors: Teng Ee Yap, Konstantin Batygin
Figure caption: Simulation results for Rstop = RT = 5RJ and r0 just beyond (i.e., 1.25 times) the ice line (r0 ∼ 0.04RHill), with Rα = 2 and w = h0. Panels indicate the (a) semimajor axes of the moons and (b) their outer-inner period ratios. Key resonant captures are denoted by vertical lines. See Section 4.3 for a discussion.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: The cumulative curves quantify the total line flux for each source, aiding comparison between knots and the central core.
Paper: The ALMA-ATOMS-QUARKS Survey: Resolving a Chemically Rich Massive Protostellar Outflow
Authors: Jiahang Zou, Tie Liu, Fengwei Xu, Xindi Tang, Dezhao Meng, Yan-Kun Zhang, Aiyuan Yang, Tapas Baug, Chang Won Lee, L. Viktor Tóth, Ariful Hoque, Sami Dib, Pablo Garcia, Hong-Li Liu, Prasanta Gorai, Swagat R. Das, Guido Garay, Patricio Sanhueza, Li Chen, Di Li, Jihye Hwang, Dongting Yang
Figure caption: CH3OH 4−2,3–3−1,2 channel map.