adsabs/AstroCLIMB huggingface dataset:
Paper: Cross-correlation of Luminous Red Galaxies with Machine Learning Selected Active Galactic Nuclei in HSC-SSP: Unobscured AGN Residing in More Massive Halos
Authors: Rodrigo Córdova Rosado, Andy D. Goulding, Jenny E. Greene, Grayson C. Petter, Ryan C. Hickox, Nickolas Kokron, Michael A. Strauss, Jahmour J. Givans, Yoshiki Toba, Cassandra Starr Henderson
Figure caption: Normalized dN/dz from all AGN subtype samples for cross-correlation in the wide redshift bin (z ∈ 0.7–1.0) for the L 6 μm > 3 × 1044 erg s−1 threshold, split by HSC field.
Paper: “SNe Ia Twins for Life”: Toward a Precise Determination of H 0 
Authors: P. Ruiz-Lapuente, J. I. González Hernández
Figure caption: (As in Figures 3 and 7.) Left-hand panel: result from the joint comparison of the two phases. Right-hand panel: individual phases and joint phase confidence regions from the comparison at 289 days after maximum and 344 days after maximum of SN 2018gv and SN 2011fe.
Paper: “SNe Ia Twins for Life”: Toward a Precise Determination of H 0 
Authors: P. Ruiz-Lapuente, J. I. González Hernández
Figure caption: Left-hand panel: spectra of the twins SN 2011fe and SN 2018gv at exactly the same phase of 289 days past maximum light. Right-hand panel: corner plot as in previous figures but for SN 2018gv at 289 days.
Paper: “SNe Ia Twins for Life”: Toward a Precise Determination of H 0 
Authors: P. Ruiz-Lapuente, J. I. González Hernández
Figure caption: Left-hand panel: final joint result from early (–2 days) and late-time spectra (361 days) of SN 2013aa and SN 2017cbv. Right-hand panel: the results showing the corner plots with the 1σ, 2σ, and 3σ confidence regions favored by each phase and those from the joint computation.
Paper: “SNe Ia Twins for Life”: Toward a Precise Determination of H 0 
Authors: P. Ruiz-Lapuente, J. I. González Hernández
Figure caption: As in Figure 3. Left-hand panel: final values favored by the joint phases both 46 days after maximum and 333 days after maximum of SN 2013dy with its twins. Right-hand panel: results for each phase and the joint phases.
Paper: “SNe Ia Twins for Life”: Toward a Precise Determination of H 0 
Authors: P. Ruiz-Lapuente, J. I. González Hernández
Figure caption: Left-hand panel: spectra of the twins SN 2011fe and SN 2018gv at exactly the same phase of 344 days past maximum light. Right-hand panel: as above but for 344 days past maximum.
Paper: “SNe Ia Twins for Life”: Toward a Precise Determination of H 0 
Authors: P. Ruiz-Lapuente, J. I. González Hernández
Figure caption: Comparison of the spectra of SN 2013aa and SN 2011fe at the same phase. The reddening of SN 2011fe has been placed at E(B − V) = 0.15 to compare it with SN 2013aa.
Paper: “SNe Ia Twins for Life”: Toward a Precise Determination of H 0 
Authors: P. Ruiz-Lapuente, J. I. González Hernández
Figure caption: Left-hand panel: comparison of early-time spectra of SN 2013dy and SN 2017cbv at −2 days before maximum light. Right-hand panel: 1σ, 2σ, and 3σ contours for this epoch.
Paper: “SNe Ia Twins for Life”: Toward a Precise Determination of H 0 
Authors: P. Ruiz-Lapuente, J. I. González Hernández
Figure caption: Left-hand panel: comparison of the spectrum of SN 2013dy and SN 2017cbv from late-time spectra at 333 days. Right-hand panel: contours for the 333 days phase.
Paper: “SNe Ia Twins for Life”: Toward a Precise Determination of H 0 
Authors: P. Ruiz-Lapuente, J. I. González Hernández
Figure caption: Left-hand panel: comparison of the spectra of SN 2013dy with SN 2013aa at 46 days past maximum light. Right-hand panel: as above but for the 46 days phase.
Paper: Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023
Authors: Kaushik Chatterjee, Santanu Mondal, Chandra B. Singh, Mutsumi Sugizaki
Figure caption: Variation of the (a) MAXI/GSC 2−20 keV count rate, (b) MAXI/GSC 2−6 and 6−20 keV count rates, and (c) hardness ratio with time. The HR is the ratio of the 6−20 keV count rate to the 2−6 keV count rate of the MAXI/GSC data.
Paper: Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023
Authors: Kaushik Chatterjee, Santanu Mondal, Chandra B. Singh, Mutsumi Sugizaki
Figure caption: Evolution of QPO frequencies (Hz) with time. Here we have shown three different plots for (a) LE, (b) ME, and (c) HE instruments. Panels (1)–(10) in each of the three of these plots (a, b, c) represent the ν qpo variation for the 10 observation IDs we used.
Paper: Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023
Authors: Kaushik Chatterjee, Santanu Mondal, Chandra B. Singh, Mutsumi Sugizaki
Figure caption: The model-fitted PDS using 0.01 s time-binned HE light curve from the observation ID P0614338004 (Exposure ID P061433800401-20230831-01-01).
Paper: Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023
Authors: Kaushik Chatterjee, Santanu Mondal, Chandra B. Singh, Mutsumi Sugizaki
Figure caption: Evolution of QPO frequency with time during the whole period of analysis for (a) LE, (b) ME, and (c) HE.
Paper: “SNe Ia Twins for Life”: Toward a Precise Determination of H 0 
Authors: P. Ruiz-Lapuente, J. I. González Hernández
Figure caption: A distance of 6.5 Mpc seems compatible with the late-time spectrum of SN 2011fe. Here a comparison is made with a theoretical spectrum with a 56Ni mass of 0.5 M ⊙ of the W7 class obtained with the code explained in P. Ruiz-Lapuente (1996).
Paper: “SNe Ia Twins for Life”: Toward a Precise Determination of H 0 
Authors: P. Ruiz-Lapuente, J. I. González Hernández
Figure caption: Comparison of SN 2017cbv/SN 2013aa with SN 2011fe at 2 days before maximum. The T eff of the photosphere of SN 2017cbv/2013aa is 2000 K higher than in SN 2011fe.
Paper: “SNe Ia Twins for Life”: Toward a Precise Determination of H 0 
Authors: P. Ruiz-Lapuente, J. I. González Hernández
Figure caption: Comparison of SN 2017cbv/SN 2013aa with SN 2011fe at 12 days past maximum. The T eff of the photosphere of SN 2017cbv is 2000 K higher than in SN 2011fe.
Paper: Constraining the Excitation of Molecular Gas in Two Quasar-starburst Systems at z ∼ 6
Authors: Fuxiang Xu, Ran Wang, Jianan Li, Roberto Neri, Antonio Pensabene, Roberto Decarli, Yali Shao, Eduardo Bañados, Pierre Cox, Frank Bertoldi, Chiara Feruglio, Fabian Walter, Bram P. Venemans, Alain Omont, Dominik Riechers, Jeff Wagg, Karl M. Menten, Xiaohui Fan
Figure caption: Line intensity maps of CO(8–7), (9–8), (10–9) (from left to right) and corresponding continuum of two objects observed by NOEMA. The top two row panels are for J2054-0005, and the bottom two rows are for J0129-0035. The green–yellow cross on the line intensity map and continuum represents the optical position. The shaded white ellipse in the bottom-left corner of each panel shows the FWHM of the beam. The contours denote the line map contours to [−2, 2, 3, 4, 6] ×σ and the continuum contours to [−2, 2, 4, 8, 16] ×σ.
Paper: Constraining the Excitation of Molecular Gas in Two Quasar-starburst Systems at z ∼ 6
Authors: Fuxiang Xu, Ran Wang, Jianan Li, Roberto Neri, Antonio Pensabene, Roberto Decarli, Yali Shao, Eduardo Bañados, Pierre Cox, Frank Bertoldi, Chiara Feruglio, Fabian Walter, Bram P. Venemans, Alain Omont, Dominik Riechers, Jeff Wagg, Karl M. Menten, Xiaohui Fan
Figure caption: Spectra of CO(8–7), (9–8), (10–9) (from top to bottom) of two objects (left: J2054-0005; right: J0129-0035) and the fitting results by one Gaussian mode. The dotted histograms mark the ±1σ range in the rms noise. The red lines show the best-fit model of the spectra. The yellow bins represent the velocity range within 1.5 × FWHM of the detected line.
Paper: Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023
Authors: Kaushik Chatterjee, Santanu Mondal, Chandra B. Singh, Mutsumi Sugizaki
Figure caption: Variation of spectrally fitted properties (a) hydrogen column density (n H), (b) inner disk temperature (T in in keV), (c) diskbb normalization, (d) Photon Index (Γ), (e) reflection fraction (R ref), and (f) cutoff energy (E cut) with time.
Paper: Constraining the Excitation of Molecular Gas in Two Quasar-starburst Systems at z ∼ 6
Authors: Fuxiang Xu, Ran Wang, Jianan Li, Roberto Neri, Antonio Pensabene, Roberto Decarli, Yali Shao, Eduardo Bañados, Pierre Cox, Frank Bertoldi, Chiara Feruglio, Fabian Walter, Bram P. Venemans, Alain Omont, Dominik Riechers, Jeff Wagg, Karl M. Menten, Xiaohui Fan
Figure caption: SED fitting results of J2054-0005. Open circles and errors are broadband photometric measurements from Herschel observation (black, C. Leipski et al. 2014), ALMA observation (orange, T. Hashimoto et al. 2019; B. P. Venemans et al. 2020; D. Salak et al. 2024; R. Tripodi et al. 2024), and NOEMA/PdBI observation (blue, R. Wang et al. 2008, 2013). The red–orange dashed line represents the best-fitted CAT3D model and the cyan dashed line shows the best-fitted host galaxy cold dust component.
Paper: Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023
Authors: Kaushik Chatterjee, Santanu Mondal, Chandra B. Singh, Mutsumi Sugizaki
Figure caption: Variation of shock properties with time in accordance with ν qpo. In (a) we show the variation of ν qpo with time, and in (b) and (c) we show the variations of the shock location (X  s ) and shock speed (v) with time.
Paper: Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023
Authors: Kaushik Chatterjee, Santanu Mondal, Chandra B. Singh, Mutsumi Sugizaki
Figure caption: The model-fitted spectrally analyzed unfolded spectra. (a) is or observation ID. P061433800501 (Exposure: P061433800501-20230902-01-01) for which the gabs model was required to achieve the best fit. (b) is for the observation ID. P061433800601 (exposure: P061433800601-20230904-01-01), for which the gabs model was not required to achieve the best fit.
Paper: Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023
Authors: Kaushik Chatterjee, Santanu Mondal, Chandra B. Singh, Mutsumi Sugizaki
Figure caption: Evolution of the QPO rms (%) with time (MJD) for (a) LE, (b) ME, and (c) HE.
Paper: Insight-HXMT View of the Black Hole Candidate Swift J1727.8–1613 during Its Outburst in 2023
Authors: Kaushik Chatterjee, Santanu Mondal, Chandra B. Singh, Mutsumi Sugizaki
Figure caption: Variation of photon index of power law (Γ) with QPO frequency (ν qpo) for (a) LE, (b) ME, and (c) HE instruments. Here, Γ is the spectral fitted index using combined LE+ME+HE data.
Paper: Constraining the Excitation of Molecular Gas in Two Quasar-starburst Systems at z ∼ 6
Authors: Fuxiang Xu, Ran Wang, Jianan Li, Roberto Neri, Antonio Pensabene, Roberto Decarli, Yali Shao, Eduardo Bañados, Pierre Cox, Frank Bertoldi, Chiara Feruglio, Fabian Walter, Bram P. Venemans, Alain Omont, Dominik Riechers, Jeff Wagg, Karl M. Menten, Xiaohui Fan
Figure caption: CO SLED fitted with PDR and/or XDR models. The black points with error bars represent the CO fluxes and the corresponding uncertainties of J2054-0005 and J0129-0035. The data and/or upper limits for CO(6–5), (8–7), (9–8), and (10–9) are from this work, with CO(6–5) obtained from ALMA observations (R. Tripodi et al. 2024), and (8–7), (9–8), and (10–9) from NOEMA observations. CO(2–1) data are sourced from Y. Shao et al. (2019). We determined the optimal parameter combination for the SLED of two sources by fitting the minimum χ 2 of the residuals. For J0129-0035, we considered the impact of upper limits on the fitting by incorporating an error function into the residuals. In the upper panel, from left to right, the fits include a single-PDR model of J2054-0005, low-density PDR+dense PDR models, and PDR+XDR modeling with the line constraints (﹩\mathrm{log}\,({n}_{{\rm{H}}}/{\mathrm{cm}}^{-3})=3.4﹩, ﹩\mathrm{log}\,{G}_{0}=3.9﹩). The lower panel presents similar cases for J0129-0035, with the line constraints of ﹩\mathrm{log}\,({n}_{{\rm{H}}}/{\mathrm{cm}}^{-3})=3.4﹩, ﹩\mathrm{log}\,{G}_{0}=3.9﹩. Blue lines represent the PDR component, red lines indicate the XDR component and gray lines depict the total contribution from both components.
Paper: Constraining the Excitation of Molecular Gas in Two Quasar-starburst Systems at z ∼ 6
Authors: Fuxiang Xu, Ran Wang, Jianan Li, Roberto Neri, Antonio Pensabene, Roberto Decarli, Yali Shao, Eduardo Bañados, Pierre Cox, Frank Bertoldi, Chiara Feruglio, Fabian Walter, Bram P. Venemans, Alain Omont, Dominik Riechers, Jeff Wagg, Karl M. Menten, Xiaohui Fan
Figure caption: (a) Grids of [C II]158 μm /[C I]369 μm intensity line ratio as a function of ﹩\mathrm{log}\,{G}_{0}﹩ and ﹩\mathrm{log}\,({n}_{{\rm{H}}}/{\mathrm{cm}}^{-3})﹩ in the PDRs. Gray contours indicate model values. The different color lines indicate the line ratio measured in the J2054-0005. The red solid line and gray region represent the [C II]158 μm/TIR luminosity ratio reported in B. P. Venemans et al. (2020). The blue dashed line means the upper limit of [C I]369 μm /TIR luminosity ratio where 3σ upper limit of [C I]369 μm in the J2054-0005 was reported in R. Decarli et al. (2022). The green dotted line indicates the lower limit of the [C II]158 μm /[C I]369 μm luminosity ratio. (b) Grids of [C II]158 μm/TIR intensity line ratio as a function of ﹩\mathrm{log}\,{G}_{0}﹩ and ﹩\mathrm{log}\,({n}_{{\rm{H}}}/{\mathrm{cm}}^{-3})﹩ in the PDRs. Gray contours indicate model values. The red solid line and the line width represent the [C II]158 μm/TIR luminosity ratio and the uncertainty reported in B. P. Venemans et al. (2020).
Paper: Constraining the Excitation of Molecular Gas in Two Quasar-starburst Systems at z ∼ 6
Authors: Fuxiang Xu, Ran Wang, Jianan Li, Roberto Neri, Antonio Pensabene, Roberto Decarli, Yali Shao, Eduardo Bañados, Pierre Cox, Frank Bertoldi, Chiara Feruglio, Fabian Walter, Bram P. Venemans, Alain Omont, Dominik Riechers, Jeff Wagg, Karl M. Menten, Xiaohui Fan
Figure caption: CO SLED normalized to CO(6–5) in normalized units of Jy km s−1. Left column: J2054-0005 (blue squares) and J0129-0035 (orange squares) in comparison with the mean of four galaxy samples: local (U)LIRGs (M. J. F. Rosenberg et al. 2015, green); local normal + starburst galaxies (D. Liu et al. 2015, brown); z ∼ 1.2–4.1 SMGs (M. S. Bothwell et al. 2013, red); and strongly lensed SMGs at z ∼ 2–4 (C. Yang et al. 2017, purple). Right column: J2054-0005 (blue squares) and J0129-0035 (orange squares) compared with high-z quasars. The plotted quasars are J2310+1855 (J. Li et al. 2020, green), PSOJ215.15 (J. Li et al. 2024, red), 1429+5447 (J. Li et al. 2024, purple), J1148+5251 (F. Bertoldi et al. 2003; F. Walter et al. 2003; A. Beelen et al. 2006; D. A. Riechers et al. 2009; S. Gallerani et al. 2014, brown), J0100+2802 (F. Wang et al. 2019, magenta), J0439+1634 (J. Yang et al. 2019, gray), and APM 08279+5255 (A. Weiß et al. 2007; D. A. Riechers et al. 2009; C. M. Bradford et al. 2011, yellow).
Paper: Constraining the Excitation of Molecular Gas in Two Quasar-starburst Systems at z ∼ 6
Authors: Fuxiang Xu, Ran Wang, Jianan Li, Roberto Neri, Antonio Pensabene, Roberto Decarli, Yali Shao, Eduardo Bañados, Pierre Cox, Frank Bertoldi, Chiara Feruglio, Fabian Walter, Bram P. Venemans, Alain Omont, Dominik Riechers, Jeff Wagg, Karl M. Menten, Xiaohui Fan
Figure caption: CO SLED fitting results for J2054-0005 ((a), left) and J0129-0035 ((b), right), employing priors obtained from best-fitting parameters through the least squares method with constrained PDR conditions and predicted line ratios. Blue (PDR) and red (XDR) lines represent the fitting results of the mode of the parameter posterior distribution (cyan). Black dots represent the observed data, and the gray line illustrates the combined PDR+XDR model.
Paper: Constraining the Excitation of Molecular Gas in Two Quasar-starburst Systems at z ∼ 6
Authors: Fuxiang Xu, Ran Wang, Jianan Li, Roberto Neri, Antonio Pensabene, Roberto Decarli, Yali Shao, Eduardo Bañados, Pierre Cox, Frank Bertoldi, Chiara Feruglio, Fabian Walter, Bram P. Venemans, Alain Omont, Dominik Riechers, Jeff Wagg, Karl M. Menten, Xiaohui Fan
Figure caption: Relation between the CO brightness temperature ratio r 96 and the AGN absolute magnitude M 1450 (a) and the FIR luminosity L FIR (b). The colored points indicate the value for high-z quasars. The hollow inverted triangle is the bold estimate of r 96 derived from r 106 for J0100+2802.
Paper: Constraining the Excitation of Molecular Gas in Two Quasar-starburst Systems at z ∼ 6
Authors: Fuxiang Xu, Ran Wang, Jianan Li, Roberto Neri, Antonio Pensabene, Roberto Decarli, Yali Shao, Eduardo Bañados, Pierre Cox, Frank Bertoldi, Chiara Feruglio, Fabian Walter, Bram P. Venemans, Alain Omont, Dominik Riechers, Jeff Wagg, Karl M. Menten, Xiaohui Fan
Figure caption: SED fitting results of J0129-0035. The left panel displays the variation of the fitting results with respect to different T dust and fixed β = 1.6. The right panel shows the variation of the fitting results for different β and fixed T dust = 47 K.
Paper: Supernova Shocks in Molecular Clouds: Shocks Driven into Dense Cores in IC 443 and 3C 391
Authors: William T. Reach, Le Ngoc Tram, Curtis DeWitt, Pierre Lesaffre, Benjamin Godard, Antoine Gusdorf
Figure caption: Modeled emissivity of the H2 S(1) and S(5) lines as a function of distance behind the model shocks listed in Table 3. The emissivities of the H2 lines are normalized to the peak value for each modeled transition. To show where molecules are dissociated, the fractional abundance of atomic H is shown in each panel, without normalization (so a value of 1 means complete dissociation of H2). Each panel is labeled with its shock designation from Table 3, abbreviated preshock density (cm−3), shock velocity (km s−1), and magnetic parameter β. The left column shows the C-type shock models, which become progressively more compact as the preshock density increases. The right column shows the J-type shock models. The dissociative J-type models (a, b, c, d) have a thin region just behind the shock front (2 × 10−7 pc), followed by a region where molecules are destroyed, then followed by a region of reformed molecules (around 10−3 pc). Note the two columns have different horizontal scales. The vertical dashed line shows the shock duration of 5000 yr, and vertical dotted lines show how far the shock developed in (from right to left) 3000, 1000, and 100 yr.
Paper: Supernova Shocks in Molecular Clouds: Shocks Driven into Dense Cores in IC 443 and 3C 391
Authors: William T. Reach, Le Ngoc Tram, Curtis DeWitt, Pierre Lesaffre, Benjamin Godard, Antoine Gusdorf
Figure caption: Modeled spectra of H2 emission in the S(1) and S(5) pure rotational lines, and the H2O 110–101 line, for C-type MHD shocks. Each panel is labeled with its shock designation from Table 3, abbreviated preshock density (cm−3), shock velocity (km s−1), and magnetic parameter β. All spectra are normalized by their peak values, which are reported in Table 4. Velocities are in the rest frame of the observer. The dashed line at 0 km s−1 indicates the preshocked gas velocity, and the modeled shock is propagating toward the observer (along the line of sight). Unlike Figure 6, the J-type models are not shown, because they are all simple Gaussians centered near zero.
Paper: Supernova Shocks in Molecular Clouds: Shocks Driven into Dense Cores in IC 443 and 3C 391
Authors: William T. Reach, Le Ngoc Tram, Curtis DeWitt, Pierre Lesaffre, Benjamin Godard, Antoine Gusdorf
Figure caption: Phase space of shock parameters. The three critical regimes (nondissociative C-type, dissociative J-type, and nondissociative J-type) are labeled (and shaded purple, green, and cyan, respectively). The input parameters for the shocks in Table 3 are indicated by their corresponding letter designations. Model (e) falls near the C- to J-type boundary and was found to be C type. This phase space is in accord with similar ones from (B. Godard et al. 2019; L. E. Kristensen et al. 2023) diagrams.
Paper: Supernova Shocks in Molecular Clouds: Shocks Driven into Dense Cores in IC 443 and 3C 391
Authors: William T. Reach, Le Ngoc Tram, Curtis DeWitt, Pierre Lesaffre, Benjamin Godard, Antoine Gusdorf
Figure caption: Slit spectrum of the H2 S(1) line from IC 443 B showing subtraction of residual sky emission. The upper panel shows one echellle order from standard nod subtraction. Sky lines from CO2 and N2O remain, with the N2O lines partially overlapping the region of celestial H2 S(1) emission. The lower panel shows the same order, after subtracting an additional small fraction of the sky spectrum. The H2 line is labeled below the lower panel. While the H2 line is visible in both panels, the suppression of sky features significantly improves the accuracy of measuring the line profile. The spectrum used for analysis was extracted from an 8″ portion of the slit near its center.
Paper: Supernova Shocks in Molecular Clouds: Shocks Driven into Dense Cores in IC 443 and 3C 391
Authors: William T. Reach, Le Ngoc Tram, Curtis DeWitt, Pierre Lesaffre, Benjamin Godard, Antoine Gusdorf
Figure caption: SOFIA spectra of H2 S(1) and S(5) and H2O 110–101 lines from IC 443 clumps B, C, G, and from 3C 391 at the positions listed in Table 1. The H2 lines are in units of Jy arcsec−2 and the H2O line is in units of brightness temperature (K). The S(5) and H2O spectra are vertically offset by 1 and 2 for clarity. All brightnesses for 3C 391 were doubled to be on the same scale.
Paper: Supernova Shocks in Molecular Clouds: Shocks Driven into Dense Cores in IC 443 and 3C 391
Authors: William T. Reach, Le Ngoc Tram, Curtis DeWitt, Pierre Lesaffre, Benjamin Godard, Antoine Gusdorf
Figure caption: Spectral image for the IC 443 B observations of the H2 S(5) line. Two orders of the echelle spectrum are shown, because they both cover part of the very broad celestial H2 line. The minimum and maximum wavenumber and velocity of each order are labeled on their lower and upper corners, respectively. An 8″ portion of the slit, toward the top, was extracted to match the region extracted for the S(1) line.
Paper: Supernova Shocks in Molecular Clouds: Shocks Driven into Dense Cores in IC 443 and 3C 391
Authors: William T. Reach, Le Ngoc Tram, Curtis DeWitt, Pierre Lesaffre, Benjamin Godard, Antoine Gusdorf
Figure caption: Diagram showing the context for SNRs IC 443 and 3C 391, produced by supernovae near or just inside the edges of molecular clouds. The blast wave propagates through lower-density gas making X-rays (blue), then into the molecular clumps (purple) and dense cores (red, labeled for those of IC 443).
Paper: Supernova Shocks in Molecular Clouds: Shocks Driven into Dense Cores in IC 443 and 3C 391
Authors: William T. Reach, Le Ngoc Tram, Curtis DeWitt, Pierre Lesaffre, Benjamin Godard, Antoine Gusdorf
Figure caption: Column density divided by statistical weight for the upper levels of the pure rotational S(0) through S(6) lines toward IC 443 C. The horizontal axis is the energy (expressed as a temperature) of the upper level. The observed values are in black. The predictions from shocks into moderate-density gas (combination of models (b p ) and (c p ) from Table 3), normalized to match the observed brightness of the S(5) line, are in blue. The predictions from a shock into higher-density gas (model (g) from Table 4), normalized to match the observed brightness of the S(0) line, is in orange. The left panel is for a shock into gas with statistical equilibrium populations of H2 (OPR = 3). The right panel is for a shock into gas that has remained cold and undisturbed (OPR = 0.006).
Paper: Supernova Shocks in Molecular Clouds: Shocks Driven into Dense Cores in IC 443 and 3C 391
Authors: William T. Reach, Le Ngoc Tram, Curtis DeWitt, Pierre Lesaffre, Benjamin Godard, Antoine Gusdorf
Figure caption: Same as Figure 7, but for only the three fastest C-type shocks a p , b p , and c p , at three different ages of 3000 yr (left), 1000 yr (center), and 100 yr (right). The velocity distribution skews away from zero if the shocks are younger, because the accelerated gas closer to the shock becomes a larger fraction of the emission.