adsabs/AstroCLIMB huggingface dataset:
Paper: Simulation of Thermal Nonequilibrium Cycles in the Solar Wind
Authors: Roger B. Scott, Jeffrey W. Reep, Mark G. Linton, Stephen J. Bradshaw
Figure caption: Time–distance plots of temperature (top), number density (middle), and linear particle flux (bottom) over a ﹩72\,\rm{hr}﹩ period during which the heating ratio ﹩\alpha ﹩ increases from ﹩3.45﹩ to ﹩3.5﹩, corresponding to footpoint heating rates of ﹩{{ \mathcal H }}_{b}\in \{6.9,7.0\}\times {10}^{-4}\,\mathrm{erg}\,{\mathrm{cm}}^{-3}\,{{\rm{s}}}^{-1}﹩. During the first ﹩24\,\rm{hr}﹩                      ﹩(\alpha =3.45)﹩, the plasma is in a steady state. Following the increase in footpoint heating ﹩(\alpha =3.5)﹩ at ﹩t=0﹩, the plasma undergoes two TNE cycles over the subsequent ﹩48\,\rm{hr}﹩ period.
Paper: Simulation of Thermal Nonequilibrium Cycles in the Solar Wind
Authors: Roger B. Scott, Jeffrey W. Reep, Mark G. Linton, Stephen J. Bradshaw
Figure caption: Profiles of plasma number density and temperature (topmost panel), pressure and wind speed (second panel), and rates of heating per particle (lower two panels) are depicted for two steady-state solutions with different footpoint heating rates. The values of ﹩\alpha \in \{0.0,1.0\}﹩ correspond to heating rates of ﹩{{ \mathcal H }}_{b}\in \{0.0,2.0\}\times {10}^{-4}\,\mathrm{erg}\,{\mathrm{cm}}^{-3}\,{{\rm{s}}}^{-1}﹩. The global heating in each case is ﹩{{ \mathcal H }}_{g}=2.0\times {10}^{-6}\,\mathrm{erg}\,{\mathrm{cm}}^{-3}\,{{\rm{s}}}^{-1}﹩.
Paper: Simulation of Thermal Nonequilibrium Cycles in the Solar Wind
Authors: Roger B. Scott, Jeffrey W. Reep, Mark G. Linton, Stephen J. Bradshaw
Figure caption: The dynamic cooling time, transit time, integrated cooling factor ﹩{\rm{\Gamma }}﹩, and minimum value of the temperature within the thermal sink are shown over a period of approximately ﹩36\,\rm{hr}﹩ that spans from just before the increase in heating from ﹩\alpha =3.45﹩ to ﹩\alpha =3.5﹩ at time ﹩t=0﹩ until just after the end of the first full condensation cycle.
Paper: WTP 19aalnxx: Discovery of a Bright Mid-infrared Transient in the Emerging Class of Low-luminosity Supernovae Revealed by Delayed Circumstellar Interaction
Authors: Charlotte Myers, Kishalay De, Lin Yan, Jacob E. Jencson, Nicholas Earley, Christoffer Fremling, Daichi Hiramatsu, Mansi M. Kasliwal, Ryan M. Lau, Morgan MacLeod, Megan Masterson, Christos Panagiotou, Robert Simcoe, Samaporn Tinyanont
Figure caption: ZTF optical (g and r band shown as green and red symbols, respectively) light curves and NEOWISE MIR (W1 and W2 shown as black and orange, respectively) of CCSNe from the BTS that exhibit late-time MIR brightenings in NEOWISE without reported spectroscopic signatures in their nominal classification. We show the nominal peak light spectroscopic classification of the source next to the source name in each panel. Solid symbols denote detections while hollow symbols indicate upper limits.
Paper: Simulation of Thermal Nonequilibrium Cycles in the Solar Wind
Authors: Roger B. Scott, Jeffrey W. Reep, Mark G. Linton, Stephen J. Bradshaw
Figure caption: The time evolution of ﹩n﹩, ﹩T﹩, and                          ﹩nuA﹩                       depicted during the precipitation phase, which lasts approximately ﹩1\,\rm{hr}﹩ for the case of marginal nonequilibrium, beginning with the formation of a cold condensation in the corona near ﹩{s}_{n}﹩, and ending with the upwelling of material at the base of the corona.
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Jet breakout conditions for injected jets with t d = 0.1 s and t d = 1 s after the merger. Top: L j = 1050 erg s−1; bottom: L j = 1051 erg s−1. The colored lines represent the energy required to collimate the jet to a certain opening angle according to Equation (3). In contrast, the black solid lines represent the energy required for a jet to escape as a function of the opening angle θ j derived from Equation (4). The dots represent the tested cases for θ j = 5° and 10°, with triangles (stars) representing successful (choked) jets. The black dashed lines in each panel, superposed on the colored lines, represent the fit for the collimation curve expressed by Equation (3).
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: An example of evolved jets in the BNS post-merger environment for the model t d = 1 s after 300  ms of continuous injection for three different cases: top—L = 1050 erg s−1 and θ = 5°; middle—L = 1051 erg s−1 and θ = 5°; and bottom—L = 1051 erg s−1 and θ j = 10°. We started the simulation at t = 1.06 s, which is roughly at t d = 1 s after the collapse of the HMNS. The time t j = 0.3 s indicates the time since the jet injection has started. The white line represents the opening angle of the jet. From left to right, the panels represent the Γβ factor, the density ρ, the pressure P, and the jet tracer (flagged cells with jet material advected with the fluid).
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Top: differential energy distribution with respect to the proper velocity Γβ of a relativistic jet with L j = 1050 erg s−1 and θ j = 5° injected into the ejecta. The different colors show the jet time evolution during the injection (cold colors for early times and hot colors for late times). The dotted colored lines represent the material associated with the jet. The black dashed line is the energy of the ejecta of the initial conditions. Note that we prolonged the simulation in this case to see the evolution of the distribution until the breakout time t bo ≃ 500 ms after the start of the injection. Bottom: different regions of the energy vs. velocity distribution after 550 ms of injection with respect to different thresholds of the jet scalar tracer Q j.
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Jet injection for the model t d = 0.1 s at t e = 100 ms after the injection (end of the injection) for two cases: top—L = 1050 erg s−1 and θ = 5°; and bottom—L = 1051 erg s−1 and θ j = 10°. The white lines and plotted physical quantities are the same as in the previous multipanel figures depicting simulation snapshots. For space reasons, we omit plotting the density map. The top panels correspond to the top row, second column, of Figure 2.
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Proper-velocity (Γβ) and jet scalar tracer maps of a jet initialized with a delay of t d = 1 s, a luminosity of L j = 1051 erg s−1, and an opening angle θ j = 5° at an early stage of its injection (taken after injecting for 0.025 s). At this stage, the jet is still in the innermost (and densest) part of the ejecta and has drilled through the polar funnel. We can see the shape of the collimation shock, which divides the unshocked jet material from the shocked material.
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Relativistic jets after we switched off the jet engine running for t e = 100 ms (top) and t e = 120 ms (bottom) and let the jet evolve until it reached R ej (post-injection phase) for L j = 1050 erg s−1 and θ j = 5° (top row) and L = 1051 erg s−1 and θ j = 10° (bottom row). The jet’s high-velocity material reaches the ejecta’s outer boundary after the jet engine shuts down, leaving jetted material that mixes with the BNS ejecta matter (rightmost panels). In both cases, the breakout happens at t j ≃ 0.5 s.
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Minimal engine time, t e, required for a jet to escape as a function of the injection angle, θ j, the luminosity, L j, and the time delay, t d, between the merger and jet launch. The lines represent the estimate from Equation (5). We can see that in the case of t d = 0.1 s, we get t e ≳ 0.05 s, while for t d = 1 s, this value increases to t e ≃ 0.1–0.3 s for jets with θ j = 5°–10°. All these values for t e are compatible with an sGRB.
Paper: Simulating Short Gamma-Ray Burst Jets in Realistic Late Binary Neutron Star Merger Environments
Authors: Matteo Pais, Tsvi Piran, Kenta Kiuchi, 建太 木内, Masaru Shibata, 田大 柴
Figure caption: Two-dimensional slice across the x–z plane passing through the center of the simulation box of the initial conditions taken at t = 1.06 s after the merger. Left: density slice in logarithmic units superposed on the streamlines of the velocity field. Right: pressure slice in logarithmic units. In both plots, we can notice the presence of the low-pressure/low-density polar funnel.
Paper: The Dark Energy Survey Supernova Program: Light Curves and 5 Yr Data Release
Authors: B. O. Sánchez, D. Brout, M. Vincenzi, M. Sako, K. Herner, R. Kessler, T. M. Davis, D. Scolnic, M. Acevedo, J. Lee, A. Möller, H. Qu, L. Kelsey, P. Wiseman, P. Armstrong, B. Rose, R. Camilleri, R. Chen, L. Galbany, E. Kovacs, C. Lidman, B. Popovic, M. Smith, P. Shah, M. Sullivan, M. Toy, T. M. C. Abbott, M. Aguena, S. Allam, O. Alves, J. Annis, J. Asorey, S. Avila, D. Bacon, D. Brooks, D. L. Burke, A. Carnero Rosell, D. Carollo, J. Carretero, L. N. da Costa, F. J. Castander, S. Desai, H. T. Diehl, J. Duarte, S. Everett, I. Ferrero, B. Flaugher, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, G. Giannini, K. Glazebrook, S. González-Gaitán, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, O. Lahav, S. Lee, G. F. Lewis, H. Lin, J. L. Marshall, J. Mena-Fernández, R. Miquel, J. Myles, R. C. Nichol, R. L. C. Ogando, A. Palmese, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, E. Sanchez, D. Sanchez Cid, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, B. E. Tucker, D. L. Tucker, V. Vikram, A. R. Walker, N. Weaverdyck
Figure caption: Difference in magnitudes for transients analyzed with SMP Y3 (B19) and SMP Y5 (this work). We expect subtle differences due to the improved catalogs, image processing and astrometry pipelines, and underlying photometric uncertainties. The trend seen in the i band is at 2σ significance, which is the largest out of all bands.
Paper: The Dark Energy Survey Supernova Program: Light Curves and 5 Yr Data Release
Authors: B. O. Sánchez, D. Brout, M. Vincenzi, M. Sako, K. Herner, R. Kessler, T. M. Davis, D. Scolnic, M. Acevedo, J. Lee, A. Möller, H. Qu, L. Kelsey, P. Wiseman, P. Armstrong, B. Rose, R. Camilleri, R. Chen, L. Galbany, E. Kovacs, C. Lidman, B. Popovic, M. Smith, P. Shah, M. Sullivan, M. Toy, T. M. C. Abbott, M. Aguena, S. Allam, O. Alves, J. Annis, J. Asorey, S. Avila, D. Bacon, D. Brooks, D. L. Burke, A. Carnero Rosell, D. Carollo, J. Carretero, L. N. da Costa, F. J. Castander, S. Desai, H. T. Diehl, J. Duarte, S. Everett, I. Ferrero, B. Flaugher, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, G. Giannini, K. Glazebrook, S. González-Gaitán, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, O. Lahav, S. Lee, G. F. Lewis, H. Lin, J. L. Marshall, J. Mena-Fernández, R. Miquel, J. Myles, R. C. Nichol, R. L. C. Ogando, A. Palmese, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, E. Sanchez, D. Sanchez Cid, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, B. E. Tucker, D. L. Tucker, V. Vikram, A. R. Walker, N. Weaverdyck
Figure caption: Rms for the flux pull on epochs free of transient flux (assuming a true flux of zero), as a function of the surface brightness of the galaxy host, exactly at the location of the transient. We include the distribution of host surface brightness for each filter in blue. The horizontal line indicates the expected rms = 1 for a unit dispersion Gaussian. We show the results for SMP (solid line) and DiffImg (dashed line).
Paper: The Dark Energy Survey Supernova Program: Light Curves and 5 Yr Data Release
Authors: B. O. Sánchez, D. Brout, M. Vincenzi, M. Sako, K. Herner, R. Kessler, T. M. Davis, D. Scolnic, M. Acevedo, J. Lee, A. Möller, H. Qu, L. Kelsey, P. Wiseman, P. Armstrong, B. Rose, R. Camilleri, R. Chen, L. Galbany, E. Kovacs, C. Lidman, B. Popovic, M. Smith, P. Shah, M. Sullivan, M. Toy, T. M. C. Abbott, M. Aguena, S. Allam, O. Alves, J. Annis, J. Asorey, S. Avila, D. Bacon, D. Brooks, D. L. Burke, A. Carnero Rosell, D. Carollo, J. Carretero, L. N. da Costa, F. J. Castander, S. Desai, H. T. Diehl, J. Duarte, S. Everett, I. Ferrero, B. Flaugher, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, G. Giannini, K. Glazebrook, S. González-Gaitán, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, O. Lahav, S. Lee, G. F. Lewis, H. Lin, J. L. Marshall, J. Mena-Fernández, R. Miquel, J. Myles, R. C. Nichol, R. L. C. Ogando, A. Palmese, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, E. Sanchez, D. Sanchez Cid, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, B. E. Tucker, D. L. Tucker, V. Vikram, A. R. Walker, N. Weaverdyck
Figure caption: DES light curves of SNe at different redshifts (z ∼ 0.3 and z ∼ 0.6) in the SN Deep and SN Shallow fields. Lines are the SALT3 model that best fits the light-curve data.
Paper: The Dark Energy Survey Supernova Program: Light Curves and 5 Yr Data Release
Authors: B. O. Sánchez, D. Brout, M. Vincenzi, M. Sako, K. Herner, R. Kessler, T. M. Davis, D. Scolnic, M. Acevedo, J. Lee, A. Möller, H. Qu, L. Kelsey, P. Wiseman, P. Armstrong, B. Rose, R. Camilleri, R. Chen, L. Galbany, E. Kovacs, C. Lidman, B. Popovic, M. Smith, P. Shah, M. Sullivan, M. Toy, T. M. C. Abbott, M. Aguena, S. Allam, O. Alves, J. Annis, J. Asorey, S. Avila, D. Bacon, D. Brooks, D. L. Burke, A. Carnero Rosell, D. Carollo, J. Carretero, L. N. da Costa, F. J. Castander, S. Desai, H. T. Diehl, J. Duarte, S. Everett, I. Ferrero, B. Flaugher, J. Frieman, J. García-Bellido, M. Gatti, E. Gaztanaga, G. Giannini, K. Glazebrook, S. González-Gaitán, R. A. Gruendl, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, D. J. James, K. Kuehn, O. Lahav, S. Lee, G. F. Lewis, H. Lin, J. L. Marshall, J. Mena-Fernández, R. Miquel, J. Myles, R. C. Nichol, R. L. C. Ogando, A. Palmese, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, A. Porredon, A. K. Romer, E. Sanchez, D. Sanchez Cid, I. Sevilla-Noarbe, E. Suchyta, M. E. C. Swanson, G. Tarle, B. E. Tucker, D. L. Tucker, V. Vikram, A. R. Walker, N. Weaverdyck
Figure caption: Comparison of flux residuals to SALT3 model fits for DiffImg and SMP DES-SN5YR light curves. We generally find a smaller amount of residual scatter for the SMP photometry in transients across the full redshift range.
Paper: On the Nature of Nonthermal Broadening of Spectral Lines Observed by IRIS
Authors: Kyuhyoun Cho, Bart De Pontieu, Paola Testa
Figure caption: Observational data and 2D histogram for region 1: (a) LOS magnetic field strength map; (b) AIA 1600 Å intensity map; (c) Si IV intensity map; (d) map of the cosine of the inclination between the magnetic field at the transition region and the LOS, where the red regions, or ﹩\cos i\simeq 1﹩, represent regions where the magnetic field is parallel to the LOS direction; (e) Si IV nonthermal velocity map; (f) Si IV Doppler velocity map; (g) 2D histogram between the cosine of the magnetic field inclination at the transition region and the Si IV nonthermal velocity; (h) 2D histogram between the cosine of the magnetic field inclination at the transition region and the Si IV Doppler velocity; and (i) 2D histogram between the Si IV Doppler velocity and Si IV nonthermal velocity. The blue contours and purple contours in (a)–(c) indicate the magnetic field strength masking and temporal masking, respectively. The unshaded areas in (d)–(f) indicate the major part of the intersection between the two maskings, the ROI. All analyses were conducted with the data within this unshaded area. The white arrows in (d)–(f) show the direction to the solar disk center. The linear fitting results are shown with the blue lines, and their coefficients and the Pearson correlation coefficients are exhibited in the upper left corner of every 2D histogram plot. The circles in (c), (e), and (f) indicate the positions of the sampled spectra in Figure 3.
Paper: On the Nature of Nonthermal Broadening of Spectral Lines Observed by IRIS
Authors: Kyuhyoun Cho, Bart De Pontieu, Paola Testa
Figure caption: (a) Si IV nonthermal velocity map from IRIS mosaic observations. (b) LOS magnetic field mosaic map from HMI observations. The blue numbers indicate the locations of the numbered (NOAA) active regions. (c) AIA 1600 Å intensity mosaic map from AIA observations. (d) Observation time for the IRIS mosaic data. The red boxes indicate the selected rectangular areas or regions of interest. The white color indicates regions that lack data (e.g., because of data dropouts or because of gaps between different mosaic pointings). Note that the selected regions span across different pointings, and especially the time difference between two successive horizontal sequences is usually greater than 1 hr.
Paper: On the Nature of Nonthermal Broadening of Spectral Lines Observed by IRIS
Authors: Kyuhyoun Cho, Bart De Pontieu, Paola Testa
Figure caption: An example of how we obtain an inclination map for region 3 in Figure 2. (a) An equidistant grid is superimposed on the HMI LOS magnetic field map. The yellow solid lines indicate every 50 grid points. The observing time of the HMI data is shown at the top of the panel. (b) The NLFFF extrapolated magnetic fields (green lines) in the local frame. The underlying image shows the equidistant grid data of the radial magnetic field in the photosphere. (c) The NLFFF extrapolated magnetic fields (green lines) superimposed on the AIA 171 map. The observing time of the AIA data is shown at the top of the panel. Considering that the coronal loops in the 171 Å image outline the coronal magnetic field lines, one can consider the goodness of the magnetic field extrapolation. (d) The cosine of the magnetic field inclination at transition-region heights (about 2200 km above the photosphere). A value of 1 indicates magnetic field lines that are parallel with the LOS.
Paper: On the Nature of Nonthermal Broadening of Spectral Lines Observed by IRIS
Authors: Kyuhyoun Cho, Bart De Pontieu, Paola Testa
Figure caption: A schematic illustration of the magnetic field configuration and its relation to the LOS direction at transition-region heights. The definition of the inclination i is described in several cases. If we assume that the active region located far from the disk center has a simple bipole configuration, the inclinations of the magnetic fields at the inner edge (i.e., toward disk center) of the farther polarity region are close to parallel to the LOS direction (the red circle). In contrast, the magnetic field inclination at the outer edge of the active region (i.e., toward the limb) is close to perpendicular to the LOS direction (the blue circle).
Paper: On the Nature of Nonthermal Broadening of Spectral Lines Observed by IRIS
Authors: Kyuhyoun Cho, Bart De Pontieu, Paola Testa
Figure caption: An example of an observed spectrum and a single Gaussian fit result. The location of the sampled spectrum is shown as the circles in Figure 6. The black histogram and gray dashed line indicate the observed spectrum and the rest wavelength of Si IV (1402.77 Å). The thick red solid line shows the result of a single Gaussian fitting. The red vertical line and red horizontal arrow show the Doppler shift (23.3 km s−1) and 1/e width (31.1 km s−1). The green line shows a spectrum with a thermal width corresponding to log T[K] = 4.8, the IRIS instrumental width, and a zero nonthermal width for comparison.
Paper: On the Nature of Nonthermal Broadening of Spectral Lines Observed by IRIS
Authors: Kyuhyoun Cho, Bart De Pontieu, Paola Testa
Figure caption: The same as Figure 6, but for region 2. The noisy patterns in the IRIS data were caused by cosmic-ray impacts on the detector, when IRIS passed through the South Atlantic Anomaly.
Paper: On the Nature of Nonthermal Broadening of Spectral Lines Observed by IRIS
Authors: Kyuhyoun Cho, Bart De Pontieu, Paola Testa
Figure caption: The same as Figure 6, but for region 3.
Paper: On the Nature of Nonthermal Broadening of Spectral Lines Observed by IRIS
Authors: Kyuhyoun Cho, Bart De Pontieu, Paola Testa
Figure caption: An example of a magnetic field inclination map from HMI observations. The white gray color (90°) indicates perpendicularity to the LOS direction.
Paper: CLASSY. X. Highlighting Differences between Partial Covering and Semianalytic Modeling in the Estimation of Galactic Outflow Properties
Authors: Mason Huberty, Cody Carr, Claudia Scarlata, Timothy Heckman, Alaina Henry, Xinfeng Xu, Karla Z. Arellano-Córdova, Danielle A. Berg, Stéphane Charlot, John Chisholm, Simon Gazagnes, Matthew Hayes, Weida Hu, Bethan L. James, R. Michael Jennings, Claus Leitherer, Crystal L. Martin, Matilde Mingozzi, Evan D. Skillman, Yuma Sugahara
Figure caption: Left: comparison between column densities derived using SALT and the partial covering fraction method from X. Xu et al. (2022). We report column densities for all three ionization states of silicon. The PCM Si II and Si IV column densities were computed directly from the data, while the Si III values were obtained using photoionization modeling. Right: comparison between the individual ion covering fractions computed with SALT and the average covering fraction computed using the PCM method. The two methods on average are positively correlated, with the black points representing the average SALT result across all ionization states.
Paper: CLASSY. X. Highlighting Differences between Partial Covering and Semianalytic Modeling in the Estimation of Galactic Outflow Properties
Authors: Mason Huberty, Cody Carr, Claudia Scarlata, Timothy Heckman, Alaina Henry, Xinfeng Xu, Karla Z. Arellano-Córdova, Danielle A. Berg, Stéphane Charlot, John Chisholm, Simon Gazagnes, Matthew Hayes, Weida Hu, Bethan L. James, R. Michael Jennings, Claus Leitherer, Crystal L. Martin, Matilde Mingozzi, Evan D. Skillman, Yuma Sugahara
Figure caption: Left: comparison between V out using the PCM from X. Xu et al. (2022) and a density-weighted average velocity as derived by SALT. Right: comparison between V out using the PCM from X. Xu et al. (2022) and a mass-weighted average velocity as derived by SALT. We report the individual ionization SALT velocities as well as the average ionization state SALT velocity in black. Both the mass and density weights are positively correlated with the PCM results, but it is the mass-weighted velocity that agrees most prominently with the PCM results. The density-weighted velocity is lower for SALT than for PCM, based on the fact that the power laws for density indicate a substantial component of material is contained within small radii of the outflow.