adsabs/AstroCLIMB huggingface dataset:
Paper: Impact of Galaxy Clusters on the Propagation of Ultrahigh-energy Cosmic Rays
Authors: Antonio Condorelli, Jonathan Biteau, Remi Adam
Figure caption: Interaction and escape lengths as a function of magnetic rigidity at the center of a prototypical galaxy cluster: photohadronic interaction times (dashed–dotted lines), spallation times (dashed lines), and diffusion times (solid lines) for protons (red) and nitrogen nuclei (green). The Hubble radius (corresponding to the age of the Universe) is shown as a long-dashed line. Length scales have been calculated assuming the following parameters: R 500 = 1 Mpc, B = 1 μG, l  c  = 10 kpc, n ICM = 1 · 10−4 cm−3.
Paper: Impact of Galaxy Clusters on the Propagation of Ultrahigh-energy Cosmic Rays
Authors: Antonio Condorelli, Jonathan Biteau, Remi Adam
Figure caption: Thermal-proton density profiles for the Coma cluster: the blue line indicates the best-fit model to the ROSAT data (Briel et al. 1992), the red line indicates the density obtained from the Ghirardini et al. (2019) polytropic relation combined with the Arnaud et al. (2010) UPP profile, the green and orange lines indicate the UDP from Pratt et al. (2022) and Ghirardini et al. (2019), respectively.
Paper: Impact of Galaxy Clusters on the Propagation of Ultrahigh-energy Cosmic Rays
Authors: Antonio Condorelli, Jonathan Biteau, Remi Adam
Figure caption: Magnetic field strength profiles for Coma cluster: the blue line (and shaded region) indicates the best-fit model (and the constrained range) as obtained from the Faraday-rotation measure (Bonafede et al. 2010), the red and orange lines indicate the model obtained when scaling the magnetic field strength to the UPP and using β pl = 200 and β pl = 77, respectively, the orange line indicates our model when scaling the magnetic field strength to the gas density, with the UDP from Pratt et al. (2022).
Paper: Impact of Galaxy Clusters on the Propagation of Ultrahigh-energy Cosmic Rays
Authors: Antonio Condorelli, Jonathan Biteau, Remi Adam
Figure caption: Escaping proton spectra from a cluster of M = 1014 M ⊙ as a function of the injection point. Positive (negative) y values correspond to positions closer to the nearest (furthest) edges of the cluster. The spectra are normalized to that expected without interactions in the ICM. The vertical line shows the ankle energy.
Paper: Impact of Galaxy Clusters on the Propagation of Ultrahigh-energy Cosmic Rays
Authors: Antonio Condorelli, Jonathan Biteau, Remi Adam
Figure caption: Transparency as a function of energy for protons, helium, and nitrogen nuclei for different cluster magnetic fields (see the legend), assuming an injection point at the center of the environment. The points show the results obtained from the simulations with errors resulting from the number of injected particles. The solid lines display the proposed parameterization. The vertical line shows the ankle energy.
Paper: Impact of Galaxy Clusters on the Propagation of Ultrahigh-energy Cosmic Rays
Authors: Antonio Condorelli, Jonathan Biteau, Remi Adam
Figure caption: Escaping proton spectra from a cluster of different magnetic field values at the center, taken at 1 kpc (see the legend), assuming injection at the center of the cluster. The spectra are normalized to that expected without interactions in the ICM. The vertical line shows the ankle energy.
Paper: Internal Shock with a Background Magnetic Field for the Prompt Emission of Gamma-Ray Bursts—A Case Study of GRB 211211A
Authors: Li Zhou, Da-Bin Lin, Xing Yang, Guo-Yu Li, Kuan Liu, Jing Li, En-Wei Liang
Figure caption: Radiation spectra of our model with different f B, i.e., f B = 0 (black), 10−4 (magenta), 10−3 (cyan), 10−2 (green), and 10−1 (wine), where L obs = 1052erg s−1, R dis = 1015 cm, p = 3.5, α B = 1, ﹩{\gamma }_{{\rm{m}}}^{{\prime} }=3\times {10}^{3}﹩, and z = 1 are taken. In this figure, the Band radiation spectrum with E p = 400 keV, α = −1, and β = −2.3 (gray solid line) and the power-law spectra with spectral index ﹩\hat{{\rm{\Gamma }}}=1/3﹩ (gray dotted line) or ﹩\hat{{\rm{\Gamma }}}=-1/2﹩ (gray dashed–dotted line) are also shown for comparison.
Paper: Internal Shock with a Background Magnetic Field for the Prompt Emission of Gamma-Ray Bursts—A Case Study of GRB 211211A
Authors: Li Zhou, Da-Bin Lin, Xing Yang, Guo-Yu Li, Kuan Liu, Jing Li, En-Wei Liang
Figure caption: Radiation spectra of our model with different parameters, where the fiducial case (green solid line) in each panel is the same as that in Figure 1. (a) Different values of α B are indicated by different dashed lines, i.e., α B = 0 (black), 0.5 (red), 2 (blue), and 4 (wine). (b) Different values of p are indicated by different dashed lines, i.e., p = 2.5 (black), 3 (red), and 4 (blue). (c) Different values of R dis are indicated by different dashed lines, i.e., R dis = 1014 (black), 3 × 1014 (blue), 3 × 1015 (red), and 1016 cm (gray). (d) Different values of ﹩\gamma {{\prime} }_{{\rm{m}}}={10}^{4}﹩ (blue dashed line), or Y 0 = 2 (red dashed line), or ﹩t{{\prime} }_{\mathrm{end}}=3﹩ (orange dashed line), or τ B = 0.001 (magenta dashed line) are adopted.
Paper: Properties Underlying the Variation of the Magnetic Field Spectral Index in the Inner Solar Wind
Authors: J. R. McIntyre, C. H. K. Chen, A. Larosa
Figure caption: The dependence of (a) the solar wind speed, V sw; (c) the sampling angle, θ BV; (e) the magnitude of the magnetic field fluctuations, δ B, squared and (g) the normalized fluctuation magnitude, δ B/B 0, squared on the heliocentric distance, r. (b) The gradient from a least-squares linear fit, γ, of the spectral index, α B, against V sw for sets of intervals binned by r, with 95% confidence intervals, and the equivalent for γ of α B against (d) θ BV, (f) δ B 2 and (h) ﹩\delta {B}^{2}/{B}_{0}^{2}﹩. The data points for the largest r bin in panels (b) and (d) are not shown owing to having large associated confidence intervals, to allow the confidence intervals of other bins to be seen clearly.
Paper: Internal Shock with a Background Magnetic Field for the Prompt Emission of Gamma-Ray Bursts—A Case Study of GRB 211211A
Authors: Li Zhou, Da-Bin Lin, Xing Yang, Guo-Yu Li, Kuan Liu, Jing Li, En-Wei Liang
Figure caption: Spectral fitting results in the time slice of [6.25, 6.5] s of GRB 211211A, where the left and right panels are the fitting results with the Band function and our model, respectively.
Paper: Internal Shock with a Background Magnetic Field for the Prompt Emission of Gamma-Ray Bursts—A Case Study of GRB 211211A
Authors: Li Zhou, Da-Bin Lin, Xing Yang, Guo-Yu Li, Kuan Liu, Jing Li, En-Wei Liang
Figure caption: Light curve of the hard main emission of GRB 211211A (black curve) and the time slices, marked with two red vertical dashed lines and labels “a”–“p”, for our spectral analysis.
Paper: Properties Underlying the Variation of the Magnetic Field Spectral Index in the Inner Solar Wind
Authors: J. R. McIntyre, C. H. K. Chen, A. Larosa
Figure caption: The velocity field spectral index, α v, of 1 hr PSP intervals against the absolute cross helicity, ∣σ c∣. The red line is a 50-point running mean. The dashed lines mark the spectral index values −3/2 and −5/3.
Paper: Sesquinary Catastrophe for Close-in Moons with Dynamically Excited Orbits
Authors: Matija Ćuk, Douglas P. Hamilton, David A. Minton, Sarah T. Stewart
Figure caption: The approximate velocity of ejecta returning to the moon as sesquinary impactors normalized to the escape velocity (q  v , Equation (1)) for each of the small inner moons as numbered in Table 1. Point colors indicate the parent planet: Mars (red), Jupiter (purple), Saturn (orange), Uranus (green), and Neptune (cyan). Black circles indicate satellites in a resonance with a more massive moon. Only the moons with q  v  > 0.1 are included in this plot.
Paper: Sesquinary Catastrophe for Close-in Moons with Dynamically Excited Orbits
Authors: Matija Ćuk, Douglas P. Hamilton, David A. Minton, Sarah T. Stewart
Figure caption: The approximate velocity of ejecta returning to the moon as sesquinary impactors normalized to the escape velocity (q  v ) vs. the radius for our sample of small, close-in planetary satellites. Point colors indicate the parent planet: Mars (red), Jupiter (purple), Saturn (orange), Uranus (green), and Neptune (cyan). Black circles indicate satellites in a resonance with a more massive moon. Only the moons with q  v  > 0.1 are included in this plot.
Paper: Sesquinary Catastrophe for Close-in Moons with Dynamically Excited Orbits
Authors: Matija Ćuk, Douglas P. Hamilton, David A. Minton, Sarah T. Stewart
Figure caption: The approximate velocity of ejecta returning to the moon as sesquinary impactors normalized to the escape velocity (q  v ) vs. the timescale for reimpact (τ, Equation (2)) for small, close-in planetary satellites. Point colors indicate the parent planet: Mars (red), Jupiter (purple), Saturn (orange), Uranus (green), and Neptune (cyan). Black circles indicate satellites in a resonance with a more massive moon. Only the moons with q  v  > 0.1 are included in this plot.
Paper: Sesquinary Catastrophe for Close-in Moons with Dynamically Excited Orbits
Authors: Matija Ćuk, Douglas P. Hamilton, David A. Minton, Sarah T. Stewart
Figure caption: The approximate velocity of ejecta returning to the moon as sesquinary impactors normalized to the escape velocity (q  v ) vs. dynamical excitation (﹩\eta =\sqrt{{e}^{2}+{\sin }^{2}i}﹩) for the same set of small, close-in moons as in Figure 1. Point colors indicate the parent planet: Mars (red), Jupiter (purple), Saturn (orange), Uranus (green), and Neptune (cyan). Black circles indicate satellites in a resonance with a more massive moon. Only the moons with q  v  > 0.1 are included in this plot.
Paper: Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies
Authors: Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu
Figure caption: Kinematic properties of LRG–CGM systems. Left panel: centroid velocities (dv) vs. virial mass for our Mg II-LRGs (orange stars), our Baseline LRGs (red diamonds), and literature LRGs (magenta circles). The error bars denote velocity extents Δv 90,Lyα . For two LRGs, we also show additional line components. For these line components we show the full velocity range included in analysis instead of Δv 90,Lyα . The gray line denotes v = 0 km s−1. Blue dashed–dotted lines denote escape velocity at 30 kpc and at 400 kpc. We note that velocities of the LRG–CGM gas are consistent with being within the escape velocity of the host halos. Right panel: average rest-frame EWs per wavelength interval for H I 1215 for Mg II-LRGs (orange line with stars) and Baseline LRGs (red line with diamonds). For Mg II-LRGs, average rest-frame EWs per wavelength interval are scaled so that the area below the function is the same for Mg II-LRGs and for Baseline LRGs. We include only data points that are inside the analyzed velocity intervals for H I 1215 lines, and two additional velocity components that are also shown in the left panel. We note that Mg II-LRGs show a shallower profile than Baseline LRGs.
Paper: Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies
Authors: Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu
Figure caption: Covering fraction of H I (C  F ) in the LRG–CGM compared to the other data. The data include CGM measurements around: Virgo cluster (orange square; Yoon et al. 2012), LRGs (our Baseline LRGs combined with literature LRGs), QSO hosts (green circle Prochaska et al. 2013), non-star-forming COS-Halos (blue triangle; Tumlinson et al. 2013), and non-star-forming COS-Dwarfs (violet diamond; Bordoloi et al. 2014). The error bars on the C  F  correspond to the calculated Wilson score intervals. Left: covering fraction vs. redshift, for massive halos at different redshifts. The most-massive halos show smaller C  F  at lower redshifts. Typical (average) R ⊥/R vir for Virgo cluster, LRGs, and QSO hosts are 0.5, 0.3, and 1, respectively. Right: covering fraction vs. halo mass, for non-star-forming galaxies at z ∼ 0–0.5. The typical (average) R ⊥/R vir for COS-Halos and COS-Dwarfs galaxies are 0.3 and 0.5, respectively. All covering fractions are calculated for EW﹩{}_{\min }﹩ (H I 1215) >0.3 Å (upper filled symbols). Covering fractions for LRGs, QSO hosts, non-star-forming COS-Halos, and non-star-forming COS-Dwarfs are also calculated for EW﹩{}_{\min }﹩ (H I 1215) >1 Å (lower open symbols).
Paper: Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies
Authors: Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu
Figure caption: Left: EW(O VI 1031) vs. stellar mass for LRGs and red COS-Halos galaxies, with and without at least one blue NG. Our Baseline and literature LRGs are marked with diamonds, while Mg II-LRGs are marked with stars, and COS-Halos are marked with circles. Blue and red symbols correspond to galaxies with at least one and without blue NGs, respectively. Measurements for blended O VI transitions are shown with fainter colors. Typically, galaxies with strong CGM O VI absorption have a blue NG. All (100%) galaxies with measured EW(O VI 1031) >0.24 Å that are not upper limits have a blue NG, while for galaxies with EW(O VI 1031) <0.24 Å the percent of galaxies that have a blue NG is 52%, or twice as small. The gray dashed line denotes EW(O VI 1031) = 0.24 Å. Right: fraction of galaxies with (blue line) and without (red line) blue NGs that show EW(O VI 1031) greater than EW﹩{}_{\mathrm{lim}}﹩, for different EW﹩{}_{\mathrm{lim}}﹩, in the combined sample of LRGs and red COS-Halos galaxies. We note that for all EW﹩{}_{\mathrm{lim}}﹩ between 0.05 and 0.4, the fraction of galaxies with EW(O VI 1031)﹩\,\gt {\mathrm{EW}}_{\mathrm{lim}}﹩ is higher for galaxies with blue NGs than for galaxies without blue NGs.
Paper: Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies
Authors: Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu
Figure caption: CGM H I as a function of stellar mass. Top: log EW (H I 1215) corrected for the impact parameter as a function of stellar mass, for our Baseline LRGs (red diamonds), literature LRGs (magenta circles), COS-Halos (blue squares), and COS-Dwarfs (blue diamonds). The full gray line shows relation derived by Bordoloi et al. (2018). Black open diamonds are median values for all data points inside stellar mass bins ﹩\mathrm{log}{M}_{* }﹩ of [8,9], [9,9.5], [9.5,10], [10,10.5], [10.5,11], [11,11.5], and [11.5,12]. Some of the data points would be below the y-axes limits. These points are shown as upper limits at a fixed value of −1. The vertical gray dashed line corresponds to ﹩\mathrm{log}{M}_{* }\sim 11.5﹩. Bottom: covering fraction for the detection of EWcorr higher than minimum EW﹩{}_{\mathrm{corr},\min }=0﹩ for galaxies in stellar mass bins with width in ﹩\mathrm{log}{M}_{* }﹩ intervals of 0.5. While the EWcorr(H I 1215) increases with stellar mass for ≲L* galaxies, the most-massive galaxies show smaller EWcorr(H I 1215).
Paper: Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies
Authors: Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu
Figure caption: CGM O VI as a function of color and halo mass. Left panel: comparison of EW(O VI 1031) vs. M  u  − M  r  color for our Baseline LRGs and COS-Halos. M  u  and M  r  are absolute SDSS magnitudes. Open symbols denote upper limits. Right panel: EW(O VI 1031) vs. halo mass for LRGs (our Baseline LRGs combined with literature LRGs) and COS-Halos. We detect O VI 1031 in only one of eight LRG–CGM systems (LRG_0855+5615). However, when detected, EW(O VI 1031) might exceed that of the CGM of red ∼L* z ∼ 0.2 galaxies.
Paper: Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies
Authors: Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu
Figure caption: EW (H I 1215) as a function of impact parameter, for our Mg II-LRGs (red stars), compared to other CGM data. Other CGM data shown include: COS-Halos (blue open squares), QSO host galaxies (orange open circles), and our Baseline LRGs (red open diamonds). The blue line denotes predicted EW(H I 1215) relation from Bordoloi et al. (2018) for average ﹩\mathrm{log}{M}_{* }﹩ for COS-Halos. The orange line denotes average EW(H I 1215) for QSO hosts. Some of the data points would be below the y-axes limits. These points are shown as upper limits at a fixed value of −1. In the left panel, impact parameters are not scaled, while in the right panel, impact parameters are scaled to the virial radii. In the left panel, we note that Mg II-LRGs and QSO host galaxies show similar CGM properties, and that the CGM of LRGs and QSO host galaxies might be evolutionary connected.
Paper: Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies
Authors: Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu
Figure caption: H I column densities as a function of impact parameter scaled to the virial radius, for our LRGs and literature LRGs. For the four Mg II-LRGs with a lower limit from the LL decrement, the measurements represent medians of the lower limit (from the LL flux decrement) and the upper limit (from the curve of growth). Four Baseline LRGs with EW detection and with upper limits from the LL flux decrement are circled and shown as full diamonds upper limits. Some of the data points would be below the y-axes limits, and these points are shown as upper limits at a fixed value 15.2. We do not show data points beyond R ⊥/R vir = 0.7. Column density in H I in LRG−CGM decreases with the impact parameter scaled to the virial radius.
Paper: Circumgalactic Medium at High Halo Masses—Signatures of Cold Gas Depletion in Luminous Red Galaxies
Authors: Marijana Smailagić, Jason Xavier Prochaska, Joseph Burchett, Guangtun Zhu
Figure caption: Number of neighboring galaxies (NGs) inside <200 kpc from the QSO sight lines. Red and blue NGs are labeled in red and blue, respectively (see the text for the definition that we use). Different bins correspond to different LRGs. LRGs are sorted from the maximum to the minimum EW(H I 1215). ID numbers from 0–14 correspond to the following LRGs: LRG_1520+2534 (0), LRG_1059+4039 (1), LRG_1102+4543 (2), LRG_1144+0714 (3), LRG_1121+4345 (4), LRG_1440-0157 (5), LRG_1351+2753 (6), LRG_1217+4931 (7), LRG_0855+5615 (8), LRG_1237+1106 (9), LRG_1106-0115 (10), LRG_0226+0014 (11), LRG_1549+0701 (12), LRG_1251+3025 (13), and LRG_1306+3421 (14). NGs do not include LRGs. In our sample, LRGs have zero to six NGs, which include both blue and red galaxies. It can also be seen that there is no correlation between EW(H I 1215) and the number of NGs or blue NGs.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Modeled abundances and column densities of 1-cyanonaphthalene (﹩{{\rm{C}}}_{10}{{\rm{H}}}_{7}\mathrm{CN}﹩; maroon), 2-cyanonaphthalene (C10CNH7; pink), and C6H5 (gray) as a function of time. The dotted lines represent the observed column densities in TMC-1, with the shaded areas signifying an error of 1σ. The dashed lines represent modeled abundances from GOTHAM DR1, and the solid lines are the modeled abundances with the updated model presented in this work. As the formation pathways and observed TMC-1 abundances of the two cyanonaphthalene isomers are very similar, the plotted curves for one isomer are overlapping with those of the other.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Modeled abundances and column densities of CH2CCH for different values of the (a) CH2CCH + C, (b) CH2CCH + N, (c) CH2CCH + O, (d) CH2CCH + OH, (e) ﹩{\mathrm{CH}}_{2}\mathrm{CCH}+\mathrm{CN}﹩, and (f) CCH + CH3 rate constants. The dashed lines are networks where this rate constant has been modified by the factors in the legend. The base network (presented in this paper) is shown for comparison as a solid line, as well as a network where this reaction is removed entirely. The color gradient corresponds with the magnitude of the factor of change.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Modeled abundances and column densities of CNCH2CCH for different values of the ﹩\mathrm{CN}+{\mathrm{CH}}_{2}\mathrm{CCH}﹩ rate constant. The dashed lines are networks where this rate constant has been modified by the factors in the legend. The base network (presented in this paper) is shown for comparison as a solid line, as well as a network where this reaction is removed entirely. The color gradient corresponds with the magnitude of the factor of change. As with the previous figures, a dotted horizontal line is plotted representing the observed abundance of CNCH2CCH in TMC-1, with the shaded region signifying an error of 1σ.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Modeled abundances and column densities of (a) CH2CCH and (b) C6H5 for different values of the CH2CCH + CH2CCH rate constant. The dashed lines are networks where this rate constant has been modified by the factors in the legend. The base network (presented in this paper) is shown for comparison as a solid line, as well as a network where this reaction is removed entirely. The color gradient corresponds with the magnitude of the factor of change.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Modeled abundances and column densities of CH2CCH for different values of the CH2CCH + H rate constant. The dashed lines are networks where this rate constant has been modified by the factors in the legend. The base network (presented in this paper) is shown for comparison as a solid line, as well as a network where this reaction is removed entirely. The color gradient corresponds with the magnitude of the factor of change. The dotted line represents the observed column density in TMC-1, with the shaded area signifying an error of 1σ.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Modeled abundances and column densities of CH2CCH2 for different values of the CH2CCH + H rate constant. The dashed lines are networks where this rate constant has been modified by the factors in the legend. The base network (presented in this paper) is shown for comparison as a solid line, as well as a network where this reaction is removed entirely. The color gradient corresponds with the magnitude of the factor of change.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Reaction rates for key destruction pathways of (a) CH2CCH, (b) CH3CCH, and (c) CH2CCH2 as a function of time. For more information on these reactions, including product channels, refer to Tables 4–8.
Paper: Astrochemical Modeling of Propargyl Radical Chemistry in TMC-1
Authors: Alex N. Byrne, Ci Xue, Ilsa R. Cooke, Michael C. McCarthy, Brett A. McGuire
Figure caption: Modeled abundances and column densities of the phenyl radical from 1 to 104 yr. The dashed line represents modeled abundances from GOTHAM DR1, and the solid line represents the modeled abundances of the updated model presented in this work.