adsabs/AstroCLIMB huggingface dataset:
Paper: Resolved UV and Optical Color Gradients Reveal Environmental Influence on Galaxy Evolution at Redshift z ∼ 1.6
Authors: W. J. Cramer, A. G. Noble, G. Rudnick, A. Pigarelli, G. Wilson, Y. M. Bahé, M. C. Cooper, R. Demarco, J. Matharu, T. B. Miller, A. Muzzin, J. Nantais, W. Sportsman, E. van Kampen, T. M. A. Webb, H. K. C. Yee
Figure caption: A comparison of the inner (orange) and outer (pink) NUV − r vs. FUV − NUV colors for the field sample and the cluster sample. Left-facing triangles show aperture fluxes at 3σ limits in either the FUV flux or the NUV flux. Downward-facing arrows show limits in just the NUV flux. Open circles show aperture fluxes with limit fluxes in both FUV and NUV. Contours based on a kernel density estimate are also shown to better illustrate the comparison. Six contour levels are shown, corresponding to ∼16% of the total plotted point distribution per contour level. Overall, the field sample shows a tighter overall distribution, while the cluster sample shows a wider range of values in the FUV − NUV color. Overall error levels on colors are quite low, averaging ∼0.05 mag for the field sample and ∼0.1 mag for the cluster sample.
Paper: Resolved UV and Optical Color Gradients Reveal Environmental Influence on Galaxy Evolution at Redshift z ∼ 1.6
Authors: W. J. Cramer, A. G. Noble, G. Rudnick, A. Pigarelli, G. Wilson, Y. M. Bahé, M. C. Cooper, R. Demarco, J. Matharu, T. B. Miller, A. Muzzin, J. Nantais, W. Sportsman, E. van Kampen, T. M. A. Webb, H. K. C. Yee
Figure caption: Stellar mass distributions for the SpARCS cluster sample, based on values from J. B. Nantais et al. (2016), and the field sample, based on values from H. V. Shipley et al. (2018). While the field sample has more lower-mass galaxies, repeating the analysis with more closely matched stellar mass samples by reducing the number of galaxies in the first two bins (shown in black) results in no statistically significant difference to the conclusions of this work.
Paper: Resolved UV and Optical Color Gradients Reveal Environmental Influence on Galaxy Evolution at Redshift z ∼ 1.6
Authors: W. J. Cramer, A. G. Noble, G. Rudnick, A. Pigarelli, G. Wilson, Y. M. Bahé, M. C. Cooper, R. Demarco, J. Matharu, T. B. Miller, A. Muzzin, J. Nantais, W. Sportsman, E. van Kampen, T. M. A. Webb, H. K. C. Yee
Figure caption: Quadratic fits to the predicted color from simple stellar population (SSP) and τ = 0.6 Gyr models produced at ages of 0.01, 0.05, 0.1, 0.2, 0.3, 0.4, 0.5, 0.8, 1.0, 1.5, 2.0, 3.0, 4.0, 5.0, and 6.0 Gyr by EzGal using a BC03 initial mass function (G. Chabrier 2003; see text for additional details). Axes are in units of AB magnitudes. With these fits, we establish a formula for converting the F435W to the F475W filter and the F606W to the F625W filter, based on the observed F435W − F606W color, in order to directly compare fluxes between the cluster and field.
Paper: Cascading Dark Energy
Authors: Kazem Rezazadeh, Amjad Ashoorioon, Daniel Grin
Figure caption: Residuals of the binned CMB power spectra relative to the reference ΛCDM model. The results of the ΛCDM (dashed black), single-field DE (long-dashed blue), rock 'n' roll (dotted red), and two-field CDE (short-dashed green) are compared with the binned Planck 2018 data points (gray; N. Aghanim et al. 2020a, 2020b, 2020c). We compared models using the best-fit parameters for all cases.
Paper: Cascading Dark Energy
Authors: Kazem Rezazadeh, Amjad Ashoorioon, Daniel Grin
Figure caption: Evolution of the f EDE as a function of cosmological redshift in the rock 'n' roll and two-field CDE models, with vertical dashed lines indicating z  c  in both models.
Paper: Cascading Dark Energy
Authors: Kazem Rezazadeh, Amjad Ashoorioon, Daniel Grin
Figure caption: 68% and 95% CL marginalized 1D likelihoods and 2D contours of z  c , f(z  c ), and H 0 for the rock 'n' roll model (red) and the two-field CDE model (blue).
Paper: Cascading Dark Energy
Authors: Kazem Rezazadeh, Amjad Ashoorioon, Daniel Grin
Figure caption: Evolution of the w DE as a function of cosmological redshift in the rock 'n' roll and two-field CDE models.
Paper: Toward Implementation of the Pressure-regulated, Feedback-modulated Model of Star Formation in Cosmological Simulations: Methods and Application to TNG
Authors: Sultan Hassan, Eve C. Ostriker, Chang-Goo Kim, Greg L. Bryan, Jan D. Burger, Drummond B. Fielding, John C. Forbes, Shy Genel, Lars Hernquist, Sarah M. R. Jeffreson, Bhawna Motwani, Matthew C. Smith, Rachel S. Somerville, Ulrich P. Steinwandel, Romain Teyssier
Figure caption: Schematic summary of the method used to measure the local galactic properties within 1 kpc scales for a random galaxy at z = 0 with a stellar mass M ⋆ = 3.2 × 1010 M ⊙. We start with the gas particle data to identify the angular momentum direction ﹩\hat{L}﹩ (top left), and rotate the three-dimensional coordinates and velocities to a face-on direction (top middle). We then create a grid with a pixel size of 1 kpc, and column heights of ±0.1 and ±10 kpc above/below the midplane (top right) to compute the midplane (e.g., pressure P) and integrated (e.g., surface density gas Σg) properties, respectively. We finally create all property maps by projecting the relevant particle properties. We show below resulting maps of gas surface density (Σ g , bottom right), stellar surface density (Σ⋆, bottom middle), and star formation rate density (ΣSFR, bottom left). We repeat the same procedure for all TNG50 galaxies at z = 0 and z = 2 within the mass range of M ⋆ = 107−11 M ⊙, and combine all maps to study the overall distributions of the local galactic properties in TNG50. These distributions will also be used to make predictions for the star formation using the PRFM model.
Paper: Toward Implementation of the Pressure-regulated, Feedback-modulated Model of Star Formation in Cosmological Simulations: Methods and Application to TNG
Authors: Sultan Hassan, Eve C. Ostriker, Chang-Goo Kim, Greg L. Bryan, Jan D. Burger, Drummond B. Fielding, John C. Forbes, Shy Genel, Lars Hernquist, Sarah M. R. Jeffreson, Bhawna Motwani, Matthew C. Smith, Rachel S. Somerville, Ulrich P. Steinwandel, Romain Teyssier
Figure caption: Distributions, weighted by contribution to the total SFR at each redshift, of various local environmental properties from all TNG50 galaxies at z = 0 (solid) and z = 2 (dashed). For each panel, we show ﹩{\mathrm{SFR}}_{\mathrm{tot}}^{-1}d\,\mathrm{SFR}/d{\mathrm{log}}_{10}{\rm{}}x﹩, where x represents the property on the x-axis. Measurements are within 1 proper kpc pixels in maps projected parallel to the direction of the angular momentum. Top panels show surface density of gas (Σg), stars (Σ*), and SFR (ΣSFR); bottom panels show stellar scale height (H *), volumetric density of stars ρ *, and dark matter ρ d. The distributions show a large decrease in characteristic densities from z = 2 to z = 0.
Paper: Follow-up Timing of 12 Pulsars Discovered in Commensal Radio Astronomy FAST Survey
Authors: D. Zhao, J. P. Yuan, N. Wang, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, Q. D. Wu, S. Q. Wang, S. N. Sun, F. F. Kou, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang, M. Xie, Y. X. Li, Y. B. Wang, Z. K. Luo, Z. Y. Gan, Z. Y. Sun, M. M. Chi, C. J. Wang
Figure caption: The MSPs with with light WD companions from PSRCAT (ver. 1.70). MSP−He WD systems are shown with gray circles. Top panel: the correlation between orbital period and eccentricity of MSP and light WD companion systems. Bottom panel: the correlation between orbital period and companion mass of MSP and light WD companion systems. The dashed lines are the numerical calculations of the MSP−He WD system by T. M. Tauris & G. J. Savonije (1999). The median companion mass estimation is given based on their mass functions assuming an orbital inclination of i = 60° and M psr = 1.4 M ⊙.
Paper: Follow-up Timing of 12 Pulsars Discovered in Commensal Radio Astronomy FAST Survey
Authors: D. Zhao, J. P. Yuan, N. Wang, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, Q. D. Wu, S. Q. Wang, S. N. Sun, F. F. Kou, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang, M. Xie, Y. X. Li, Y. B. Wang, Z. K. Luo, Z. Y. Gan, Z. Y. Sun, M. M. Chi, C. J. Wang
Figure caption: Panels (a) and (c) show the distributions of the mean flux density and the radio luminosity (L 1400) on spin-down luminosity (﹩\dot{E}﹩), respectively. Panels (b) and (d) show the dependence of the mean flux density and the radio luminosity on the distance from YMW16, respectively. The blue triangles represent pulsars reported in this work. The green crosses stand for CRAFTS pulsars in A. D. Cameron et al. (2020), and red stars are CRAFTS MSPs in C. C. Miao et al. (2023). Other known pulsars are represented by gray circles, and the data are from ATNF (ver. 1.70).
Paper: Follow-up Timing of 12 Pulsars Discovered in Commensal Radio Astronomy FAST Survey
Authors: D. Zhao, J. P. Yuan, N. Wang, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, Q. D. Wu, S. Q. Wang, S. N. Sun, F. F. Kou, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang, M. Xie, Y. X. Li, Y. B. Wang, Z. K. Luo, Z. Y. Gan, Z. Y. Sun, M. M. Chi, C. J. Wang
Figure caption: The distribution of the spin-down luminosity(﹩\dot{E}﹩) over characteristic age (τ  c ). The green stars represent pulsars reported in Q. D. Wu et al. (2023a). The red crosses stand for CRAFTS pulsars in A. D. Cameron et al. (2020). The purple circles represent pulsars reported in M. Cruces et al. (2021). The black diamonds stand for CRAFTS MSPs in C. C. Miao et al. (2023). The blue triangles represent pulsars reported in this work. Other known pulsars are represented by gray circles, and the data are from ATNF (ver. 1.70).
Paper: Follow-up Timing of 12 Pulsars Discovered in Commensal Radio Astronomy FAST Survey
Authors: D. Zhao, J. P. Yuan, N. Wang, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, Q. D. Wu, S. Q. Wang, S. N. Sun, F. F. Kou, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang, M. Xie, Y. X. Li, Y. B. Wang, Z. K. Luo, Z. Y. Gan, Z. Y. Sun, M. M. Chi, C. J. Wang
Figure caption: Flux density of PSR J1602−0611. The red solid line represents the flux density limit for FAST observation for 4 minutes.
Paper: Follow-up Timing of 12 Pulsars Discovered in Commensal Radio Astronomy FAST Survey
Authors: D. Zhao, J. P. Yuan, N. Wang, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, Q. D. Wu, S. Q. Wang, S. N. Sun, F. F. Kou, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang, M. Xie, Y. X. Li, Y. B. Wang, Z. K. Luo, Z. Y. Gan, Z. Y. Sun, M. M. Chi, C. J. Wang
Figure caption: A ﹩P-\dot{P}﹩ diagram of known pulsars and FAST’s newly discovered nulling pulsars. The gray circles are known pulsars. The red stars represent the published nulling pulsars discovered by FAST. The nulling pulsars in our study are represented by the blue triangles.
Paper: Follow-up Timing of 12 Pulsars Discovered in Commensal Radio Astronomy FAST Survey
Authors: D. Zhao, J. P. Yuan, N. Wang, D. Li, P. Wang, M. Y. Xue, W. W. Zhu, C. C. Miao, W. M. Yan, J. B. Wang, J. M. Yao, Q. D. Wu, S. Q. Wang, S. N. Sun, F. F. Kou, Y. T. Chen, S. J. Dang, Y. Feng, Z. J. Liu, X. L. Miao, L. Q. Meng, M. Yuan, C. H. Niu, J. R. Niu, L. Qian, S. Wang, X. Y. Xie, Y. F. Xiao, Y. L. Yue, S. P. You, X. H. Yu, R. S. Zhao, R. Yuen, X. Zhou, L. Zhang, M. Xie, Y. X. Li, Y. B. Wang, Z. K. Luo, Z. Y. Gan, Z. Y. Sun, M. M. Chi, C. J. Wang
Figure caption: The correlations between NF and pulsar period, τ  c , ﹩\dot{P}﹩, and ﹩\dot{E}﹩. The gray circles in the figure come from P. F. Wang et al. (2020).
Paper: No Redshift Evolution in the Fe II/Mg II Flux Ratios of Quasars across Cosmic Time
Authors: Danyang Jiang, Masafusa Onoue, Linhua Jiang, Samuel Lai, Eduardo Bañados, George D. Becker, Manuela Bischetti, Sarah E. I. Bosman, Rebecca L. Davies, Valentina D'Odorico, Emanuele Paolo Farina, Martin G. Haehnelt, Chiara Mazzucchelli, Jan-Torge Schindler, Fabian Walter, Yongda Zhu
Figure caption: The redshift—bolometric luminosity plane of the three quasar samples used in this work. The red circles, green diamonds, and blue pentagons represent the E-XQR-30 quasars at 6.0 ≤ z ≤ 6.6, the XQ-100 quasars at 3.5 ≤ z ≤ 4.8, and the low-redshift SDSS quasars, respectively. Their typical measurement errors of ﹩\mathrm{log}{L}_{\mathrm{bol}}﹩ are shown in the lower right corner. These quasars are among the most luminous quasar populations at these epochs (﹩47.0\lesssim \mathrm{log}{L}_{\mathrm{bol}}\ [{\mathrm{ergs}}^{-1}]\lesssim 48.0﹩).
Paper: No Redshift Evolution in the Fe II/Mg II Flux Ratios of Quasars across Cosmic Time
Authors: Danyang Jiang, Masafusa Onoue, Linhua Jiang, Samuel Lai, Eduardo Bañados, George D. Becker, Manuela Bischetti, Sarah E. I. Bosman, Rebecca L. Davies, Valentina D'Odorico, Emanuele Paolo Farina, Martin G. Haehnelt, Chiara Mazzucchelli, Jan-Torge Schindler, Fabian Walter, Yongda Zhu
Figure caption: Same as Figure 1 but for the low-redshift SDSS sample. The smoothed errors are not shown for SDSS spectra. The Fe II/Mg II ratios of SDSS 081946.32+414247.2 (upper panel) and SDSS 113448.31+333105.2 (lower panel) are ﹩{4.31}_{-0.10}^{+0.09}﹩ and ﹩{3.75}_{-0.07}^{+0.06}﹩, respectively.
Paper: Evolution of Tidal Disruption Event Disks with Magnetically Driven Winds
Authors: Mageshwaran Tamilan, Kimitake Hayasaki, Takeru K. Suzuki
Figure caption: Time evolution of the power-law indices of the mass accretion rate and mass-loss rate curves. The indices n and n  w  are given by Equations (25) and (26), respectively. The solid and dashed lines correspond to the cases M  i  = 0.5 and 0.005 M ⊙, respectively. The different colored lines indicate different models.
Paper: Estimating Dust Attenuation from Galactic Spectra. III. Radial Variations of Dust Attenuation Scaling Relations in MaNGA Galaxies
Authors: Niu Li, Cheng Li
Figure caption: Random Forest regression is employed to analyze the relationship between E(B − V)gas and galactic properties in the central region of galaxies. The histograms display the FI of the properties. Note that the maximum FI has been normalized to 1. Panel (a) excludes properties associated with Hα flux and [N II]/[S II], whereas panel (b) encompasses the entirety of the 15 properties under consideration. In each panel the solid/blue histogram and red histogram show the results respectively for the full sample and the subsample at z ≤ 0.03. The error bar shows the standard deviation of feature importance, estimated by bootstrap resampling of all the spaxels in the sample and retraining the Random Forest regression 100 times.
Paper: Estimating Dust Attenuation from Galactic Spectra. III. Radial Variations of Dust Attenuation Scaling Relations in MaNGA Galaxies
Authors: Niu Li, Cheng Li
Figure caption: (a) Radial profiles of correlations between E(B − V)gas and galactic properties. The x-axis represents the radial distance scaled by R  e  from the galactic center, while the y-axis depicts the Spearman rank correlation coefficients between E(B − V)gas and various galactic properties at different radii. (b) The symbols and lines are the same as in (a) but for E(B − V)star.
Paper: Estimating Dust Attenuation from Galactic Spectra. III. Radial Variations of Dust Attenuation Scaling Relations in MaNGA Galaxies
Authors: Niu Li, Cheng Li
Figure caption: The three rows describe correlations between E(B − V)gas and [O III]/[O II], [N II]/[S II], and σ Hα . The grayscale background in each panel represents the distributions of all ionized gas regions, with the median relation and 1σ scatter delineated by black lines. The Spearman rank correlation coefficients (ρ) and the range of distance to the galactic center scaled in R  e  are indicated in the upper left corner.
Paper: Estimating Dust Attenuation from Galactic Spectra. III. Radial Variations of Dust Attenuation Scaling Relations in MaNGA Galaxies
Authors: Niu Li, Cheng Li
Figure caption: Predicted [N II]/[S II] vs. the observed value for ionized gas regions in different radial bins as indicated in each panel. In the upper panels, the prediction is made by using Σ* and 12 + log10(O/H) as inputs to train a Random Forest regressor. In the lower panels, [O III]/[O II] is used in addition to Σ* and 12 + log10(O/H) for the prediction. In each panel, the dashed red line represents the 1:1 relation, while the solid thick and thin lines indicate the median and the 1σ scatter of the relation.
Paper: Estimating Dust Attenuation from Galactic Spectra. III. Radial Variations of Dust Attenuation Scaling Relations in MaNGA Galaxies
Authors: Niu Li, Cheng Li
Figure caption: (a), (c) Radial profiles of correlations between E(B − V)gas and galactic properties in Hα-faint regions with ΣHα  ≤ 1039 erg s−1 kpc−2 and Hα-bright regions with ΣHα  > 1039 erg s−1 kpc−2, respectively. (b), (d) Radial profiles of correlations between E(B − V)star and galactic properties in Hα-faint and Hα-bright regions, respectively. The symbols and lines are the same as in Figure 3.
Paper: Estimating Dust Attenuation from Galactic Spectra. III. Radial Variations of Dust Attenuation Scaling Relations in MaNGA Galaxies
Authors: Niu Li, Cheng Li
Figure caption: Random Forest regression is utilized to analyze the relationship between E(B − V)gas and galactic properties across various radial bins, as indicated in the legend, using units of R  e . The histograms depict the FI of the properties. Note that the maximum FI in each radial bin has been normalized to 1.
Paper: Tracking Outflow Using Line Locking (TOLL). I. The Case Study of Quasar J221531-174408
Authors: Chen Chen, Weimin Yi, Zhicheng He, Fred Hamann, Bo Ma
Figure caption: UVES spectrum of J221531-174408 at the rest-frame wavelengths (defined by the emission redshift z = 2.217) showing the absorption lines relative to the broad emission lines. The main emission lines are labeled across the top.
Paper: Estimating Dust Attenuation from Galactic Spectra. III. Radial Variations of Dust Attenuation Scaling Relations in MaNGA Galaxies
Authors: Niu Li, Cheng Li
Figure caption: The three rows depict correlations between E(B − V)star and ΣHα , sSFR, and t  L . The symbols and lines are the same as in Figure 4.
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: Simulated HH 48 NE ice band profiles (colors) compared to the spectrum observed with JWST (gray). Top: models of simple ice mixing scenarios in which the ices are assumed to be entirely pure (noninteracting), entirely mixed (interacting), or to have a polar (H2O) layer separate from a mixed apolar (CO2:CO) layer. Bottom: the preferred multicomponent model, including both polar and apolar components of CO2 and CO. Ice abundances for each model are listed in Table 5 with the model names in parentheses.
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: Top: Full near-IR spectrum from a radiative transfer model, including the wavelength ranges used to determine the local baselines for H2O (purple), CO2 (pink), and CO (orange). Circle markers show the wavelengths sampled for ray tracing. Bottom: As above, but for the observed JWST spectrum (J. A. Sturm et al. 2023a). The dashed blue line shows the radiative transfer model (with offset) used to predict the continuum around the H2O band. 4.08–4.19 μm is not covered by the observations.
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: Comparison of ice compositions across different evolutionary stages. Top: ratios of H2O, CO2, and CO with respect to H2O, shown for HH 48 NE as well as low-mass young stellar objects (LYSOs) and Solar System comets. For LYSOs (A. C. A. Boogert et al. 2015), the median is shown with a pink line, and the 25th–75th percentile range with a pink shaded bar. The ranges seen in Solar System comets (M. J. Mumma & S. B. Charnley 2011) are shown with an orange shaded bar, and those for 67P specifically (M. Rubin et al. 2019a) with an orange circle. Bottom: proportion of pure, polar, and apolar components of CO2 and CO measured toward LYSOs (median across the sample in K. I. Öberg et al. 2011a) and HH 48 NE.
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: Comparison of band profiles for different polar mixtures of CO2 and CO. The “H2O mixture” spectrum is the preferred multicomponent model shown in Figure 6 bottom. In the “CH3OH mixture” spectrum, the H2O:CO2 and H2O:CO components are replaced by CH3OH:CO2 and CH3OH:CO. In the left panel, the positions of CH3OH absorption features are indicated with black ticks. Ice abundances for each model are listed in Table 5 with the model names in parentheses.
Paper: JWST Ice Band Profiles Reveal Mixed Ice Compositions in the HH 48 NE Disk
Authors: Jennifer B. Bergner, J. A. Sturm, Elettra L. Piacentino, M. K. McClure, Karin I. Öberg, A. C. A. Boogert, E. Dartois, M. N. Drozdovskaya, H. J. Fraser, Daniel Harsono, Sergio Ioppolo, Charles J. Law, Dariusz C. Lis, Brett A. McGuire, Gary J. Melnick, Jennifer A. Noble, M. E. Palumbo, Yvonne J. Pendleton, Giulia Perotti, Danna Qasim, W. R. M. Rocha, E. F. van Dishoeck
Figure caption: Experimentally measured ice optical depth profiles (dark blue) compared to the band profiles following radiative transfer modeling (light blue). Spectra are shown for the H2O, CO2, and CO bands and for each of the single-component mixing scenarios described in Section 3.1.