adsabs/AstroCLIMB huggingface dataset:
Paper: ALMA High-resolution Observation for the Transitional Disk Around IRAS 04125+2902
Authors: Ayumu Shoshi, Takayuki Muto, Quincy Bosschaart, Nienke van der Marel, Gijs D. Mulders, Mitsuki Omura, Kazuki Tokuda, Masahiro N. Machida
Figure caption: Spectrum of 12CO J = 2–1 emission integrated within the region in a radius of 1″ from the central star observed by ALMA. The black dotted line shows the central velocity of vcent = 7.7 km s−1.
Paper: Constraints on Emission Models by Broadband Observations of Soft Gamma-Ray Pulsar PSR B1509–58
Authors: W. T. Ye, P. F. Zhang, M. Y. Ge, L. Q. Qi, S. J. Zheng, Y. L. Tuo, D. W. Han, H. L. Peng, Y. X. Xiao, Q. C. Shui, F. J. Lu
Figure caption: The modeling of the pulse profiles of PSR B1509–58 for different energy bands. In the left part, the panels (a), (b), (c), and (d) show the soft X-ray, hard X-ray, soft γ-ray, and high-energy γ-ray pulse profiles, respectively. The black histograms show the observed pulse profiles with the superposed model fitting results. The right part shows the corresponding normalized photon sky maps with superposed blue lines at 20° representing the viewing angle. The viewing angle continuously intersects the region of the annular emission, which generates the broad single peak of the pulse profile. Moreover, the increase of θ causes the narrowing of the pulse profile.
Paper: Constraints on Emission Models by Broadband Observations of Soft Gamma-Ray Pulsar PSR B1509–58
Authors: W. T. Ye, P. F. Zhang, M. Y. Ge, L. Q. Qi, S. J. Zheng, Y. L. Tuo, D. W. Han, H. L. Peng, Y. X. Xiao, Q. C. Shui, F. J. Lu
Figure caption: The broadband high-energy spectrum of PSR B1509–58. Panel (a): The phase-averaged spectrum. Panel (b): The phase-resolved spectra for three different phase intervals. The triangle, diamond, square, and cross points represent the data from NICER, Insight-HXMT/ME, Insight-HXMT/HE, and Fermi/LAT data, respectively, in both panels. The solid lines represent the SuperExpCutoffPowerLaw model.
Paper: Constraints on Emission Models by Broadband Observations of Soft Gamma-Ray Pulsar PSR B1509–58
Authors: W. T. Ye, P. F. Zhang, M. Y. Ge, L. Q. Qi, S. J. Zheng, Y. L. Tuo, D. W. Han, H. L. Peng, Y. X. Xiao, Q. C. Shui, F. J. Lu
Figure caption: Pulse profiles (50 bins; arbitrary phase) observed by NICER, Insight-HXMT/HE, Fermi/GBM-NaI, and Fermi/LAT. Panels (a), (b), (c), (d) are the pulse profiles obtained from NICER (0.5–10 keV), Insight-HXMT/HE (30–150 keV), Fermi/GBM-NaI (150–800 keV), and Fermi/LAT (30 MeV–1 GeV), respectively. The red dashed lines are the fitting results, while the two black dashed lines represent the two Gaussian components.
Paper: Constraints on Emission Models by Broadband Observations of Soft Gamma-Ray Pulsar PSR B1509–58
Authors: W. T. Ye, P. F. Zhang, M. Y. Ge, L. Q. Qi, S. J. Zheng, Y. L. Tuo, D. W. Han, H. L. Peng, Y. X. Xiao, Q. C. Shui, F. J. Lu
Figure caption: Panel (a): the variations of angular distance δ between the viewing direction and the center of the radiation direction. The red line represents lower energy at θ = 50∘ while the blue line represents higher energy at θ = 60∘. Panel (b): The relative variations of Γs are shown by the green line. The blue crosses are the photon indexes of the phase-resolved spectrum observed by the Chandra telescope (C.-P. Hu et al. 2017).
Paper: Constraints on Emission Models by Broadband Observations of Soft Gamma-Ray Pulsar PSR B1509–58
Authors: W. T. Ye, P. F. Zhang, M. Y. Ge, L. Q. Qi, S. J. Zheng, Y. L. Tuo, D. W. Han, H. L. Peng, Y. X. Xiao, Q. C. Shui, F. J. Lu
Figure caption: The schematic view of the geometric modification according to the annular gap model (G. J. Qiao et al. 2004). For PSR B1509–58, the magnetic inclinations α and viewing angles β are chosen to be 30∘ and 20∘ as respectively discussed in Section 4.1. The radio emission emits in the direction of the magnetic axis. The angle between the high-energy radiation direction and the magnetic axis is θ.
Paper: Constraints on Emission Models by Broadband Observations of Soft Gamma-Ray Pulsar PSR B1509–58
Authors: W. T. Ye, P. F. Zhang, M. Y. Ge, L. Q. Qi, S. J. Zheng, Y. L. Tuo, D. W. Han, H. L. Peng, Y. X. Xiao, Q. C. Shui, F. J. Lu
Figure caption: The FWHM of the pulse profile of PSR B1509–58. The square, diamond, triangle, and cross points represent data from NICER, Insight-HXMT/HE, Fermi/GBM-NaI, and Fermi/LAT, respectively. The dashed line represents the power-law model. The fitting χ2/dof is 7.4/2.
Paper: Constraints on Emission Models by Broadband Observations of Soft Gamma-Ray Pulsar PSR B1509–58
Authors: W. T. Ye, P. F. Zhang, M. Y. Ge, L. Q. Qi, S. J. Zheng, Y. L. Tuo, D. W. Han, H. L. Peng, Y. X. Xiao, Q. C. Shui, F. J. Lu
Figure caption: Distribution of the MCMC fitting parameters. The joint parameter (emission beamwidth σ) and the respective parameters (emission angle θ and the flux modulation parameter a) are all fitted using the four pulse profiles simultaneously. Each parameter converges appropriately.
Paper: Constraints on Emission Models by Broadband Observations of Soft Gamma-Ray Pulsar PSR B1509–58
Authors: W. T. Ye, P. F. Zhang, M. Y. Ge, L. Q. Qi, S. J. Zheng, Y. L. Tuo, D. W. Han, H. L. Peng, Y. X. Xiao, Q. C. Shui, F. J. Lu
Figure caption: The Fermi/LAT profile fitted with a single Gaussian function. The red dashed line shows the best fit, with a χ2/dof is 62/46. The lower panel shows the residuals.
Paper: Constraints on Emission Models by Broadband Observations of Soft Gamma-Ray Pulsar PSR B1509–58
Authors: W. T. Ye, P. F. Zhang, M. Y. Ge, L. Q. Qi, S. J. Zheng, Y. L. Tuo, D. W. Han, H. L. Peng, Y. X. Xiao, Q. C. Shui, F. J. Lu
Figure caption: The θ evolution with energy, the emission angle increases with increasing energy.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: M. A. Dopita et al. (2018) shocked Hα-cloud regions displayed on the HST Hα (F658N) image with Chandra 2019–2020 (1.2–7.0 keV) contours in purple. Our expansion and spectral analysis regions are plotted in white. The inset shows an expanded view of the northeast. Cloud P01 shows indications of having interacted with the blast wave in the northeast—see the indentation in the X-ray contours in the inset and the X-ray enhancement in Figure 1. The small cloud P05 shows no indication of significant interaction in region S1.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: Trend of position errors of spatial fits vs. brightness of simulated point sources. Several point sources are placed at randomly selected azimuthal positions at different off-axis locations (see inset legend for point types corresponding to specific off-axis angles), with counts drawn from a uniform distribution ranging from 5 to 400, and are ray traced, and fitted. The narrow trend is well described by a power law, which we fit using a least absolute deviation (LAD) fit, which is robust to outliers. Vertical dashed lines mark one-eighth, one-quarter, and one-half of the ACIS pixel size to illustrate scale.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: Similar to Figure 13, but an illustration of how sources are selected for registration, using the example of ObsID 21365. Only the detected sources with fitted position errors < 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩3 (rightmost dashed vertical line) are shown. Neither the sources that fall outside the 5%–95% range of the distribution of deviations from the power-law LAD fit (empty squares), nor sources that are not present in other observations (empty circles), are used in the registration. The remaining sources are used for registration (filled circles; see Table 2). All the simulation points from Figure 13 are also shown as gray shaded points. A similar analysis is done for all ObsIDs.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: The QE and exposure time corrected profiles from Epoch A observations (2006) and one of the Epoch B observations (ObsID 21361, 2020). The range between green dashed lines has the events combination A0B1, the range between black dashed lines has the events combination A0B0, and the range between orange dashed lines has the events combination A1B0.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: The percentage of events on node 1 for Epoch A observations (2006) and one of the Epoch B observations (ObsID 21361, 2020). The range between green dashed lines has events combination A0B1, the range between black dashed lines has events combination A0B0, and the range between orange dashed lines has events combination A1B0.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: The spectrum of shock region N4 fit with a vpshock + power-law model and the background model. The black points and line are the spectral data and model, respectively. The green dashed line is the vpshock component. The blue line is the power-law component with an index of three. The red line is the background model.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: The 1D model results of the age vs. ejecta mass assuming explosion energies of 1.5–3 × 1051 erg (panels (a)–(d)) and an s = 0 ambient medium profile for the southern rim and northeastern regions. The green line and shaded area is the age estimated by C. J. Law et al. (2020) from optical data. The blue and red lines and shaded areas are the results of the 1D model for the southern rim and for the northeastern region respectively.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: The rectangular profile extraction regions in detector coordinates (CHIPX, CHIPY) for representative ObsIDs from each of the four roll groups. The upper left panel corresponds to Epoch A. The remaining panels show the Epoch B groups.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: The white rectangle shows the profile extraction region for calculating the initial values of QE difference normalization, plotted on the merged Epoch A observations (1.2–7 keV) in ACIS “sky” coordinates.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: Estimate of the systematic bias in the expansion measurement due to PSF differences. The data points are arranged similarly to Figure 6 with regions S1–S8 labeled sequentially from left to right. The apparent expansion derived from PSF simulations with the appropriate off-axis and azimuthal angles of the Epoch A and Epoch B observations of a nonmoving shock front at the locations marked in Figure 19 are shown, along with the sinusoidal fit (solid blue line) to all the points. This sinusoidal variation is attributable to the PSF bias.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: Estimate of the systematic bias in the expansion measurement due to an error in the assumed COE. The apparent expansion from Figure 20 is subtracted from the measured raw expansion shown in Figure 6, and a sinusoid is fit to account for an offset in the assumed expansion center (see Equation (C1); solid blue line). The final estimate of the expansion in Figure 7 accounts for this offset.
Paper: Chandra Large Project Observations of the Supernova Remnant N132D: Measuring the Expansion of the Forward Shock
Authors: Xi Long, Paul P. Plucinsky, Terrance J. Gaetz, Vinay L. Kashyap, Aya Bamba, William P. Blair, Daniel Castro, Adam R. Foster, Charles J. Law, Dan Milisavljevic, Eric Miller, Daniel J. Patnaude, Manami Sasaki, Hidetoshi Sano, Piyush Sharda, Benjamin F. Williams, Brian J. Williams, Hiroya Yamaguchi
Figure caption: The positions for the PSF simulations for the S1–S8 and N1–N6 regions. The red and green crosses are the PSF simulation centers and match the region color coding in Figure 20. The white sectors are the shock regions where we measure the expansion (see Table 5).
Paper: Sun-as-a-star Analysis of the Solar Eruption Source Region Using Hα Spectroscopic Observations of CHASE
Authors: Xiaofeng Liu, Yijun Hou, Ying Li, Ye Qiu, Ting Li, Yingjie Cai, Shihao Rao, Junyi Zhang, Chuan Li
Figure caption: Multiwavelength observations of the C4.9 flare, which occurred on 2024 August 20. (a1)–(a3) AIA 131 Å raw and running difference images taken at times corresponding approximately to those shown in panels (a1)–(a3) of Figure 9. (b) LASCO C2 running difference image at 18:00 UT. (c1)–(c2) AIA 171 Å running difference images taken at times corresponding approximately to those shown in panels (a2)–(a3) of Figure 9. (d) Irradiance variations of O V 629.7 Å. The vertical dashed lines mark the Hα (black) and GOES (blue) peak times. (e) Evolution of pre-event-subtracted O V spectra during this event. (f) Double Gaussian fitting result of the O V line profile near its peak time, showing distinct central and blueshifted emission components.
Paper: Sun-as-a-star Analysis of the Solar Eruption Source Region Using Hα Spectroscopic Observations of CHASE
Authors: Xiaofeng Liu, Yijun Hou, Ying Li, Ye Qiu, Ting Li, Yingjie Cai, Shihao Rao, Junyi Zhang, Chuan Li
Figure caption: Multiwavelength observations of the X9.0 flare, which occurred on 2024 October 3. (a1)–(a3) AIA 131 Å raw and running difference images taken at times corresponding approximately to those shown in panels (a1)–(a3) of Figure 7. (b) LASCO C2 running difference image at 13:48 UT, with a cyan arrow indicating the CME associated with this filament eruption event. (c1)–(c2) AIA 171 Å running difference images taken at times corresponding approximately to those shown in panels (a2)–(a3) of Figure 7. (d) Irradiance variations of O V 629.7 Å. The vertical dashed lines mark the Hα (black) and GOES (blue) peak times. (e) Evolution of pre-event-subtracted O V spectra during this event. (f) Double Gaussian fitting result of the O V line profile near its peak time, showing distinct redshifted and blueshifted emission components.
Paper: Sun-as-a-star Analysis of the Solar Eruption Source Region Using Hα Spectroscopic Observations of CHASE
Authors: Xiaofeng Liu, Yijun Hou, Ying Li, Ye Qiu, Ting Li, Yingjie Cai, Shihao Rao, Junyi Zhang, Chuan Li
Figure caption: The composite dynamic spectra of Hα and O V 629.7 Å. (a) The composite dynamic spectra for Event 3. The Hα spectra are the same as those in Figure 5, and the O V spectra with absolute change in irradiance larger than ﹩{\sigma }_{\max }﹩ are shown in gray (see Section 3.3 for the details of ﹩{\sigma }_{\max }﹩). (b)–(c) The same as (a) but for Events 4 and 5, respectively.
Paper: The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. II. Warm Molecular Hydrogen and Warm Dust
Authors: L. K. Hunt, B. T. Draine, M. G. Navarro, A. Aloisi, R. J. Rickards Vaught, A. Adamo, F. Annibali, D. Calzetti, S. Hernandez, B. L. James, M. Mingozzi, R. Schneider, M. Tosi, B. Brandl, M. G. del Valle-Espinosa, F. Donnan, A. S. Hirschauer, M. Meixner, D. Rigopoulou
Figure caption: 17″ × 17″ RGB image of I Zw 18 showing the apertures of interest overlaid in the right panel. As in the legend, red is the MIRI F1130W background-subtracted image, green is the F560W background-subtracted image, and blue is the HST F606W image astrometrically corrected to Gaia. In the right panel, the circles illustrate the apertures (0﹩\mathop{.}\limits^{^{\prime\prime} }﹩65 radius, ∼120 pc diameter) for spectral extraction; the rectangles correspond to the MRS/IFU FoVs of the two separate pointings in the four channels. The smallest FoV, Channel 1, is illustrated by a transparent shading; the two pointings overlap allowing the construction of a complete spectral map even at the shortest wavelengths. The MIRI 14 μm continuum sources are apparent as red knots in the SE, and the faint knot in the NW associated with VLA-NW-A. The horizontal line in the lower right corner corresponds to 100 pc.
Paper: The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. II. Warm Molecular Hydrogen and Warm Dust
Authors: L. K. Hunt, B. T. Draine, M. G. Navarro, A. Aloisi, R. J. Rickards Vaught, A. Adamo, F. Annibali, D. Calzetti, S. Hernandez, B. L. James, M. Mingozzi, R. Schneider, M. Tosi, B. Brandl, M. G. del Valle-Espinosa, F. Donnan, A. S. Hirschauer, M. Meixner, D. Rigopoulou
Figure caption: One-dimensional spectra extracted from the convolved cubes within the 0﹩\mathop{.}\limits^{^{\prime\prime} }﹩65-radius apertures shown in Figure 1. The vertical axis for flux density is in units of 10−17 W m−2 μm−1, and the horizontal wavelength axis in μm; the horizontal axis has been restricted to show only the relevant H2 lines. The gray curves show the spectra, while the heavy colored lines show the smoothed continua; the zero level for each spectrum is given as a horizontal dotted colored line. For better visibility of the spectra, the spectra are offset by small increments (in units of 10−17 W m−2 μm−1) as denoted in the figure. The vertical dotted lines correspond to the detected transitions given in Tables 5 and 6; to avoid overcrowding, not all lines are labeled. The spectra for VLA-NW-B and VLA-NW-C are missing the short-wavelength MIRI channels because part of the aperture falls outside the MIRI FoV at those wavelengths.
Paper: The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. II. Warm Molecular Hydrogen and Warm Dust
Authors: L. K. Hunt, B. T. Draine, M. G. Navarro, A. Aloisi, R. J. Rickards Vaught, A. Adamo, F. Annibali, D. Calzetti, S. Hernandez, B. L. James, M. Mingozzi, R. Schneider, M. Tosi, B. Brandl, M. G. del Valle-Espinosa, F. Donnan, A. S. Hirschauer, M. Meixner, D. Rigopoulou
Figure caption: Molecular hydrogen population diagrams for the apertures with five or more H2 detections at a 3σ level or greater, together with the best-fit models with Tu = 2000 K. Fits with OPR = 3 letting Tl and n vary are shown as blue curves, according to the MCMC sampler spread; the analogous fits letting OPR, Tl and n vary are shown as red curves (see Section 3.4). The total H2 column density shown in the legends is given by Equation (8).
Paper: The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. II. Warm Molecular Hydrogen and Warm Dust
Authors: L. K. Hunt, B. T. Draine, M. G. Navarro, A. Aloisi, R. J. Rickards Vaught, A. Adamo, F. Annibali, D. Calzetti, S. Hernandez, B. L. James, M. Mingozzi, R. Schneider, M. Tosi, B. Brandl, M. G. del Valle-Espinosa, F. Donnan, A. S. Hirschauer, M. Meixner, D. Rigopoulou
Figure caption: Corner plots for the (Tl, n) fits of the H2 population diagrams with Tu = 2000 K. For each region, the upper and right panels show the PDF, and the lower left panel shows the co-dependence of the two parameters. It can be seen that Tl and n are correlated, with an extension toward flatness particularly pronounced in JWST-SE-1 and VLA-NW-A.
Paper: The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. II. Warm Molecular Hydrogen and Warm Dust
Authors: L. K. Hunt, B. T. Draine, M. G. Navarro, A. Aloisi, R. J. Rickards Vaught, A. Adamo, F. Annibali, D. Calzetti, S. Hernandez, B. L. James, M. Mingozzi, R. Schneider, M. Tosi, B. Brandl, M. G. del Valle-Espinosa, F. Donnan, A. S. Hirschauer, M. Meixner, D. Rigopoulou
Figure caption: Corner plots for the (Tl, n, OPR) fits of the H2 population diagrams with Tu = 2000 K. As in Figure 4, for each region, the top and right-most panels show the PDF, and the lower corner panels show the co-dependence of the three parameters. As in Figure 4, Tl and n are correlated, but here the OPR is also correlated with Tl and n, with a tendency toward flatness (lower left subpanels) in JWST-SE-3 and SE; these are also the regions where OPR < 3.
Paper: The Interstellar Medium in I Zw 18 Seen with JWST/MIRI. II. Warm Molecular Hydrogen and Warm Dust
Authors: L. K. Hunt, B. T. Draine, M. G. Navarro, A. Aloisi, R. J. Rickards Vaught, A. Adamo, F. Annibali, D. Calzetti, S. Hernandez, B. L. James, M. Mingozzi, R. Schneider, M. Tosi, B. Brandl, M. G. del Valle-Espinosa, F. Donnan, A. S. Hirschauer, M. Meixner, D. Rigopoulou
Figure caption: OPR plotted against H2 column density Ntot. The different values of Tu are shown as open (magenta) circles and filled (blue) squares for Tu = 2000 K, 3500 K, respectively. The mean of the two determinations is shown as an open (gray) star. The horizontal dashed line corresponds to the LTE maximum OPR value of 3.