adsabs/AstroCLIMB huggingface dataset:
Paper: The Kinematic Bimodality: Efficient Feedback and Cold Gas Deficiency in Slow-rotating Galaxies
Authors: Bitao Wang, Yingjie Peng
Figure caption: An illustration of how disturbed cold gas away from a planar form can elevate feedback efficiency. This figure shows, from an edge-on perspective, a disk-dominated (left-hand side) and a spheroid-dominated (right-hand side) galaxy with four components including a central black hole (black blob), stellar body (silk), cold gas (blue), and plasma wind from an active galactic nucleus (red). A disk galaxy without much gravitational interference has its cold gas settled in a planar form over most of the evolution history. The biconical wind launched by the central black hole then has little surface of impact to drive massive gas outflows. A spheroidal galaxy, however, which must have experienced significant mergers over time, tends to possess volume-filling gas in hotter kinematics and therefore its gas couples well with the wind. Moreover, a more massive bulge/spheroid means a more massive black hole with higher energy output. The jet is not shown here but it would have the same effect. The wind/jet direction tends to be aligned more with the spin axis of fast-rotating galaxies than with slow-rotating galaxies that have little sense of bulk rotation (Beckmann et al. 2022).
Paper: The Kinematic Bimodality: Efficient Feedback and Cold Gas Deficiency in Slow-rotating Galaxies
Authors: Bitao Wang, Yingjie Peng
Figure caption: The dependence of the H I gas reservoir on the stellar rotation of galaxies. Upper row: H I to stellar mass ratio on logarithmic scale as a function of star formation level ΔMS, for the galaxy population of faster (black) and slower (red) rotations, respectively. Each column shows the relation in a certain stellar mass bin, with stellar mass increasing rightward. Small dots are for individual galaxies and include both detections and upper limits, while the solid lines and shaded envelopes show the running medians and uncertainties (standard deviation of 1000 bootstrap samples) in sequential ΔMS windows of width 0.8 dex at steps of 0.05 dex and of at least 10 galaxies. Large points show the mean gas fractions with uncertainties estimated via the standard stacking technique in the three broad ΔMS bins for star-forming (i.e., on the SFMS, the blue band), green valley, and passive galaxies defined in Section 2.1. The bins of galaxies fewer than 10 are not shown. Lower row: the H I detection ratio as a function of ΔMS for faster (black) and slower (red) populations with estimated uncertainty as the inner 68% of 1000 bootstrap samples.
Paper: The Kinematic Bimodality: Efficient Feedback and Cold Gas Deficiency in Slow-rotating Galaxies
Authors: Bitao Wang, Yingjie Peng
Figure caption: The galaxy number surface density on the ﹩({\lambda }_{{R}_{{\rm{e}}}},\varepsilon ﹩) diagram, based on full MaNGA excluding galaxies by the quality control described in Section 3.1. The density is calculated in a box of width 0.1 at a step of 0.002. The white solid curve is the TVT predicted locus for an oblate galaxy with ﹩{\lambda }_{R,\mathrm{intr}}=0.4﹩ and ﹩{\varepsilon }_{\mathrm{intr}}=0.525﹩ at anisotropy ﹩\delta =0.7{\varepsilon }_{\mathrm{intr}}=0.3675﹩, projected at all inclinations, and the white dotted line is a crude linear extension. Throughout this work, we define the galaxies above/below the white curve as faster/slower populations.
Paper: The Kinematic Bimodality: Efficient Feedback and Cold Gas Deficiency in Slow-rotating Galaxies
Authors: Bitao Wang, Yingjie Peng
Figure caption: The H I gas deficit of the slower populations, i.e., lg﹩\tfrac{{f}_{{\rm{H}}\,{\rm\small{I}},\mathrm{slow}}}{{f}_{{\rm{H}}\,{\rm\small{I}},\mathrm{fast}}}﹩ based on the stacking-derived quantities in Figure 3, as a function of stellar mass, for green valley (points) and passive (squares) galaxies, respectively. The error bars show propagated errors as the root of the quadratic sum of the errors for faster and slower populations, respectively.
Paper: The Kinematic Bimodality: Efficient Feedback and Cold Gas Deficiency in Slow-rotating Galaxies
Authors: Bitao Wang, Yingjie Peng
Figure caption: A comparison of seeing-corrected ﹩{\lambda }_{{R}_{{\rm{e}}}}﹩ between Graham et al. (2019) for MaNGA DR15 and this work for MaNGA DR17, excluding galaxies by the quality control described in the text. Each galaxy is represented by a red dot with a thick black edge. A robust linear fit to the relation and the standard deviation of the residuals are shown by the orange solid line and dashed lines, respectively. The best-fitting parameters are shown in the upper left corner.
Paper: The Kinematic Bimodality: Efficient Feedback and Cold Gas Deficiency in Slow-rotating Galaxies
Authors: Bitao Wang, Yingjie Peng
Figure caption: Spectra raw (i.e., without weighting) stacks of star-forming faster (upper row) and slower (lower row) populations. The number of galaxies in the stack is denoted in each panel.
Paper: Astrometric Accelerations as Dynamical Beacons: A Giant Planet Imaged inside the Debris Disk of the Young Star AF Lep
Authors: Kyle Franson, Brendan P. Bowler, Yifan Zhou, Tim D. Pearce, Daniella C. Bardalez Gagliuffi, Lauren I. Biddle, Timothy D. Brandt, Justin R. Crepp, Trent J. Dupuy, Jacqueline Faherty, Rebecca Jensen-Clem, Marvin Morgan, Aniket Sanghi, Christopher A. Theissen, Quang H. Tran, Trevor N. Wolf
Figure caption: Top: test for common proper motion based on the two epochs of relative astrometry between AF Lep A and b. The left panels show the predicted relative motion of a stationary source in separation (top) and P.A. (bottom) with respect to the first epoch of relative astrometry (blue circles). Gray shaded regions represent 1σ and 2σ uncertainties. The predicted position at 2023.090 is plotted as an open triangle, and the orange triangles are our measurements. Our 2023 observations significantly disagree with a stationary background source model at the 11σ-level in P.A. The right panel shows the same comparison but in ΔR.A. and Δdecl. instead of separation and P.A. Bottom: comparison of our ﹩L^{\prime} ﹩ photometry of AF Lep b to the M  L′–﹩(H-L^{\prime} )﹩ CMD. The gray regions show the 1σ and 2σ uncertainties on the ﹩L^{\prime} ﹩ magnitude from our 2023 imaging. The background points show L (red) and T (blue) dwarfs from The UltracoolSheet (Best et al. 2020). Sources marked as young or low surface gravity are plotted in yellow. Young objects in the compilation are sources with independent age constraints <300 Myr. Low surface gravity sources have spectroscopic features of youth based on near-infrared spectroscopy. We also add substellar companions with H and ﹩L^{\prime} ﹩ photometry compiled within the species package (Stolker et al. 2020). The ﹩L^{\prime} ﹩ photometry of AF Lep b implies an early T-dwarf spectral type.
Paper: Astrometric Accelerations as Dynamical Beacons: A Giant Planet Imaged inside the Debris Disk of the Young Star AF Lep
Authors: Kyle Franson, Brendan P. Bowler, Yifan Zhou, Tim D. Pearce, Daniella C. Bardalez Gagliuffi, Lauren I. Biddle, Timothy D. Brandt, Justin R. Crepp, Trent J. Dupuy, Jacqueline Faherty, Rebecca Jensen-Clem, Marvin Morgan, Aniket Sanghi, Christopher A. Theissen, Quang H. Tran, Trevor N. Wolf
Figure caption: Left: predicted mass as a function of separation for AF Lep b from its HGCA astrometric acceleration. This plot is generated following Franson et al. (2023). The blue curve shows the masses and separations most consistent with the astrometric acceleration. Due to orbital phase, companions can occupy separations and masses above but not below the curve. The dynamical mass and semimajor axis of AF Lep b is denoted by the gold star. The planet is consistent with causing the acceleration. Right: Keck/NIRC2 Imaging ﹩L^{\prime} ﹩ imaging of AF Lep b in 2021 December (left) and 2023 February (right). Here, S/N plots are displayed to enhance true sources over residual speckles. Note that the two images do not share the same color map. We apply a Gaussian filter with a standard deviation of 1.5 pixels to average over pixel-to-pixel noise. AF Lep b is detected with a significance of 7.5σ in the 2021 December epoch and 13.0σ in the 2023 February epoch.
Paper: Astrometric Accelerations as Dynamical Beacons: A Giant Planet Imaged inside the Debris Disk of the Young Star AF Lep
Authors: Kyle Franson, Brendan P. Bowler, Yifan Zhou, Tim D. Pearce, Daniella C. Bardalez Gagliuffi, Lauren I. Biddle, Timothy D. Brandt, Justin R. Crepp, Trent J. Dupuy, Jacqueline Faherty, Rebecca Jensen-Clem, Marvin Morgan, Aniket Sanghi, Christopher A. Theissen, Quang H. Tran, Trevor N. Wolf
Figure caption: Joint posterior distributions of M host, M comp, a, e, and i for the orbit fit of AF Lep b. The diagonal panels show the marginalized distribution for each parameter. The contours on off-diagonal panels denote 1σ, 2σ, 3σ, and 4σ levels in the joint posteriors. The upper right plots compare the separation and position angle of AF Lep b over time against a swarm of orbits drawn from the orbit fit, shown in gray. The black curves highlight the maximum-likelihood orbit.
Paper: Compressible Turbulence in the Near-Sun Solar Wind: Parker Solar Probe’s First Eight Perihelia
Authors: Manuel Enrique Cuesta, Rohit Chhiber, Xiangrong Fu, Senbei Du, Yan Yang, Francesco Pecora, William H. Matthaeus, Hui Li, John Steinberg, Fan Guo, Zhaoming Gan, Emma Conrad, Diana Swanson
Figure caption: (Left column) Compiled averages of density fluctuations ﹩\delta {{n}_{p}}_{\mathrm{rms}}/\langle {n}_{p}\rangle ﹩ as a function of turbulent Mach number M  t  spanning 9 days each for PSP encounters 1–8. Points represent 5 minute averages over nonoverlapping intervals whose quantities are computed via 5 minute rolling averages (see Section 2 for specifics on averaging techniques). (Right column) ﹩\delta {{n}_{p}}_{\mathrm{rms}}/\langle {n}_{p}\rangle ﹩ as a function of M  t  for individual simulations, adapted from Fu et al. (2022). Both the left and right plots are conditioned on ranges of cross helicity σ  c  and proton plasma beta β  p . Solid blue, dashed pink, and dotted green lines represent fits to blue circles, pink triangles, and green squares, respectively.
Paper: Compressible Turbulence in the Near-Sun Solar Wind: Parker Solar Probe’s First Eight Perihelia
Authors: Manuel Enrique Cuesta, Rohit Chhiber, Xiangrong Fu, Senbei Du, Yan Yang, Francesco Pecora, William H. Matthaeus, Hui Li, John Steinberg, Fan Guo, Zhaoming Gan, Emma Conrad, Diana Swanson
Figure caption: Overview of PSP observations in the inner heliosphere. Top: mean proton density 〈n  p 〉, rms density fluctuation ﹩\delta {{n}_{p}}_{\mathrm{rms}}﹩, and the ratio ﹩\delta {{n}_{p}}_{\mathrm{rms}}/\langle {n}_{p}\rangle ﹩ plotted as a function of heliocentric distance r. Data are aggregated from first eight PSP orbits and averaged within radial bins of size 5 R ⊙. Middle: proton plasma beta β p aggregated from first eight PSP orbits (squares) and mean values (filled red circles) within radial bins of size 5 R ⊙. Bottom: turbulent Mach number M t = δ v/c s aggregated from first eight PSP orbits (squares) and mean values (filled red circles) within radial bins of size 5 R ⊙. Vertical bars represent standard deviation about corresponding means within the 5 R ⊙ bins. Note that error bars that extend to negative values are not shown on logarithmic axes. Only radial bins with at least ten counts are included. Note that we focus on r ≲ 50 R ⊙ in our main analysis (Section 3).
Paper: Compressible Turbulence in the Near-Sun Solar Wind: Parker Solar Probe’s First Eight Perihelia
Authors: Manuel Enrique Cuesta, Rohit Chhiber, Xiangrong Fu, Senbei Du, Yan Yang, Francesco Pecora, William H. Matthaeus, Hui Li, John Steinberg, Fan Guo, Zhaoming Gan, Emma Conrad, Diana Swanson
Figure caption: Compiled averages of ﹩\delta {{n}_{p}}_{\mathrm{rms}}/\langle {n}_{p}\rangle ﹩ and M  t  spanning 9 days for encounters 1–8. Blue circles represent 5 minute averages over nonoverlapping intervals wherein statistical quantities are computed via 5 minute rolling averages (see Section 2 for specifics on averaging techniques). A fitted power law is given by the solid orange line and is equivalent to ﹩\delta {{n}_{p}}_{\mathrm{rms}}/\langle {n}_{p}\rangle \sim {M}_{t}^{1.18\pm 0.04}﹩. The red star represents the average of ﹩\delta {{n}_{p}}_{\mathrm{rms}}/\langle {n}_{p}\rangle ﹩ and M  t  over all intervals.
Paper: GRB 221009A: An Ordinary Nearby GRB with Extraordinary Observational Properties
Authors: Lin Lan, He Gao, An Li, Shuo Xiao, Shunke Ai, Zong-Kai Peng, Long Li, Chen-Yu Wang, Nan Xu, Shijie Lin, Wei-Hua Lei, Bing Zhang, Yan-Qiu Zhang, Chao Zheng, Jia-Cong Liu, Wang-Chen Xue, Chen-Wei Wang, Wen-Jun Tan, Shao-Lin Xiong
Figure caption: The isotropic gamma-ray energy E  γ,iso for our collected GRBs as a function of the redshift z. The blue circles, orange circles, blue stars, red stars, and green circles represent the sGRBs, lGRBs, GRB 130427A, GRB 221009A, and other energetic GRBs, respectively. The red horizontal dotted line represent E  γ,iso = 1054 erg. The histograms on top and right represent the E  γ,iso and z distribution for all GRBs, and the blue and red vertical lines represent GRB 130427A and GRB 221009A location, respectively.
Paper: GRB 221009A: An Ordinary Nearby GRB with Extraordinary Observational Properties
Authors: Lin Lan, He Gao, An Li, Shuo Xiao, Shunke Ai, Zong-Kai Peng, Long Li, Chen-Yu Wang, Nan Xu, Shijie Lin, Wei-Hua Lei, Bing Zhang, Yan-Qiu Zhang, Chao Zheng, Jia-Cong Liu, Wang-Chen Xue, Chen-Wei Wang, Wen-Jun Tan, Shao-Lin Xiong
Figure caption: Cumulative distribution of GRB isotropic energy for total samples (left panels) and pure Konus-Wind samples (right panels) in the low-redshift bins. The blue circles show the observed distribution, and the red solid lines, red dashed lines, and blue solid lines represent the best-fitting CPL model, BPL model, and PL model, respectively.
Paper: GRB 221009A: An Ordinary Nearby GRB with Extraordinary Observational Properties
Authors: Lin Lan, He Gao, An Li, Shuo Xiao, Shunke Ai, Zong-Kai Peng, Long Li, Chen-Yu Wang, Nan Xu, Shijie Lin, Wei-Hua Lei, Bing Zhang, Yan-Qiu Zhang, Chao Zheng, Jia-Cong Liu, Wang-Chen Xue, Chen-Wei Wang, Wen-Jun Tan, Shao-Lin Xiong
Figure caption: Similar to Figure 2, but for high-redshift bins.
Paper: GRB 221009A: An Ordinary Nearby GRB with Extraordinary Observational Properties
Authors: Lin Lan, He Gao, An Li, Shuo Xiao, Shunke Ai, Zong-Kai Peng, Long Li, Chen-Yu Wang, Nan Xu, Shijie Lin, Wei-Hua Lei, Bing Zhang, Yan-Qiu Zhang, Chao Zheng, Jia-Cong Liu, Wang-Chen Xue, Chen-Wei Wang, Wen-Jun Tan, Shao-Lin Xiong
Figure caption: The likelihood distribution of α and E c in the CPL model, from the total samples (left panel) and pure Konus-Wind samples (right panel) in different redshift bins.
Paper: GRB 221009A: An Ordinary Nearby GRB with Extraordinary Observational Properties
Authors: Lin Lan, He Gao, An Li, Shuo Xiao, Shunke Ai, Zong-Kai Peng, Long Li, Chen-Yu Wang, Nan Xu, Shijie Lin, Wei-Hua Lei, Bing Zhang, Yan-Qiu Zhang, Chao Zheng, Jia-Cong Liu, Wang-Chen Xue, Chen-Wei Wang, Wen-Jun Tan, Shao-Lin Xiong
Figure caption: The correlation between E X,iso and E  γ,iso. The red solid line and dashed lines are the best fit and the 95% confidence level of the fits, respectively. The blue circles, orange circles, blue star, red star, and green circles represent the sGRBs, lGRBs, GRB 130427A, GRB 221009A, and other energetic lGRBs, respectively.
Paper: GRB 221009A: An Ordinary Nearby GRB with Extraordinary Observational Properties
Authors: Lin Lan, He Gao, An Li, Shuo Xiao, Shunke Ai, Zong-Kai Peng, Long Li, Chen-Yu Wang, Nan Xu, Shijie Lin, Wei-Hua Lei, Bing Zhang, Yan-Qiu Zhang, Chao Zheng, Jia-Cong Liu, Wang-Chen Xue, Chen-Wei Wang, Wen-Jun Tan, Shao-Lin Xiong
Figure caption: Luminosity calculated with the L  γ,iso–E p,z–Γ0 relation reported by Liang et al. (2015) as a function of the observed luminosity for GRB 130427A, GRB 221009A, and other energetic GRBs as marked in the plot. The orange circles data from Liang et al. (2015), and the black solid and dashed lines mark the relation and its 3σ dispersion.
Paper: GRB 221009A: An Ordinary Nearby GRB with Extraordinary Observational Properties
Authors: Lin Lan, He Gao, An Li, Shuo Xiao, Shunke Ai, Zong-Kai Peng, Long Li, Chen-Yu Wang, Nan Xu, Shijie Lin, Wei-Hua Lei, Bing Zhang, Yan-Qiu Zhang, Chao Zheng, Jia-Cong Liu, Wang-Chen Xue, Chen-Wei Wang, Wen-Jun Tan, Shao-Lin Xiong
Figure caption: The L  γ,iso, E  γ,iso, and Γ0 relation reported by Lü et al. (2012) and Liang et al. (2010). The orange circles data from Lü et al. (2012; top panel) and Liang et al. (2015; bottom panel), and the GRB 130427A, GRB 221009A, and other energetic GRBs are marked with different colors and shapes in the plot. The orange solid line marks the relation.
Paper: GRB 221009A: An Ordinary Nearby GRB with Extraordinary Observational Properties
Authors: Lin Lan, He Gao, An Li, Shuo Xiao, Shunke Ai, Zong-Kai Peng, Long Li, Chen-Yu Wang, Nan Xu, Shijie Lin, Wei-Hua Lei, Bing Zhang, Yan-Qiu Zhang, Chao Zheng, Jia-Cong Liu, Wang-Chen Xue, Chen-Wei Wang, Wen-Jun Tan, Shao-Lin Xiong
Figure caption: Distribution of host galaxy properties of GRBs. The blue and orange circles represent sGRBs and lGRBs respectively. The green circles are energetic GRBs. The red stars mark GRB 221009A and the data are from Levan et al. (2023). The red dashed lines mark the position of 1054 erg.
Paper: Detection of Carbon Monoxide’s 4.6 Micron Fundamental Band Structure in WASP-39b’s Atmosphere with JWST NIRSpec G395H
Authors: David Grant, Joshua D. Lothringer, Hannah R. Wakeford, Munazza K. Alam, Lili Alderson, Jacob L. Bean, Björn Benneke, Jean-Michel Désert, Tansu Daylan, Laura Flagg, Renyu Hu, Julie Inglis, James Kirk, Laura Kreidberg, Mercedes López-Morales, Luigi Mancini, Thomas Mikal-Evans, Karan Molaverdikhani, Enric Palle, Benjamin V. Rackham, Seth Redfield, Kevin B. Stevenson, Jeff A. Valenti, Nicole L. Wallack, Keshav Aggarwal, Eva-Maria Ahrer, Ian J. M. Crossfield, Nicolas Crouzet, Nicolas Iro, Nikolay K. Nikolov, Peter J. Wheatley
Figure caption: Top panel: observed transmission spectra at native resolution (light green) and at 30 pixel resolution (black). Middle panel: model transmission spectrum fit to the data (dark blue) and the same model but with CO removed (gray). Bottom panel: model contribution from CO only (red).
Paper: Detection of Carbon Monoxide’s 4.6 Micron Fundamental Band Structure in WASP-39b’s Atmosphere with JWST NIRSpec G395H
Authors: David Grant, Joshua D. Lothringer, Hannah R. Wakeford, Munazza K. Alam, Lili Alderson, Jacob L. Bean, Björn Benneke, Jean-Michel Désert, Tansu Daylan, Laura Flagg, Renyu Hu, Julie Inglis, James Kirk, Laura Kreidberg, Mercedes López-Morales, Luigi Mancini, Thomas Mikal-Evans, Karan Molaverdikhani, Enric Palle, Benjamin V. Rackham, Seth Redfield, Kevin B. Stevenson, Jeff A. Valenti, Nicole L. Wallack, Keshav Aggarwal, Eva-Maria Ahrer, Ian J. M. Crossfield, Nicolas Crouzet, Nicolas Iro, Nikolay K. Nikolov, Peter J. Wheatley
Figure caption: Fits to the white light curve as well as example fits, centered on 4.7μm, to spectroscopic light curves at 30 pixels and native resolution. Shown are the corrected fluxes after the systematics model has been removed.
Paper: Detection of Carbon Monoxide’s 4.6 Micron Fundamental Band Structure in WASP-39b’s Atmosphere with JWST NIRSpec G395H
Authors: David Grant, Joshua D. Lothringer, Hannah R. Wakeford, Munazza K. Alam, Lili Alderson, Jacob L. Bean, Björn Benneke, Jean-Michel Désert, Tansu Daylan, Laura Flagg, Renyu Hu, Julie Inglis, James Kirk, Laura Kreidberg, Mercedes López-Morales, Luigi Mancini, Thomas Mikal-Evans, Karan Molaverdikhani, Enric Palle, Benjamin V. Rackham, Seth Redfield, Kevin B. Stevenson, Jeff A. Valenti, Nicole L. Wallack, Keshav Aggarwal, Eva-Maria Ahrer, Ian J. M. Crossfield, Nicolas Crouzet, Nicolas Iro, Nikolay K. Nikolov, Peter J. Wheatley
Figure caption: Top panel: example wavelength sector showing the model contribution from CO only. The model is shown at simulated resolution (gray, sampled every Ångstrom) and after being convolved with the observed point-spread function and rebinned onto the detector’s wavelength grid (black). Middle panel: visualization of our method for detecting CO sub-band structure. Red and blue portions indicate wavelengths that are in-band or out-of-band, respectively. Note these wavelength selections are refined in Figure 4. Bottom panel: model contributions per molecule, where H2O is the only significant molecular absorber in this wavelength sector other than CO.
Paper: Detection of Carbon Monoxide’s 4.6 Micron Fundamental Band Structure in WASP-39b’s Atmosphere with JWST NIRSpec G395H
Authors: David Grant, Joshua D. Lothringer, Hannah R. Wakeford, Munazza K. Alam, Lili Alderson, Jacob L. Bean, Björn Benneke, Jean-Michel Désert, Tansu Daylan, Laura Flagg, Renyu Hu, Julie Inglis, James Kirk, Laura Kreidberg, Mercedes López-Morales, Luigi Mancini, Thomas Mikal-Evans, Karan Molaverdikhani, Enric Palle, Benjamin V. Rackham, Seth Redfield, Kevin B. Stevenson, Jeff A. Valenti, Nicole L. Wallack, Keshav Aggarwal, Eva-Maria Ahrer, Ian J. M. Crossfield, Nicolas Crouzet, Nicolas Iro, Nikolay K. Nikolov, Peter J. Wheatley
Figure caption: Top panel: samples showing the number of sub-bands as a function of transit depth, δ, for in- and out-of-band CO. Middle panel: sampling distributions of the mean transit depths, ﹩\overline{\delta }﹩, for in- and out-of-band CO. These sampling distributions are modeled as Gaussians with means and standard deviations inferred from the measured samples shown in the top panel. Bottom panel: light-curve models visualizing the measured difference in transit depth for in- and out-of-band CO.
Paper: Detection of Carbon Monoxide’s 4.6 Micron Fundamental Band Structure in WASP-39b’s Atmosphere with JWST NIRSpec G395H
Authors: David Grant, Joshua D. Lothringer, Hannah R. Wakeford, Munazza K. Alam, Lili Alderson, Jacob L. Bean, Björn Benneke, Jean-Michel Désert, Tansu Daylan, Laura Flagg, Renyu Hu, Julie Inglis, James Kirk, Laura Kreidberg, Mercedes López-Morales, Luigi Mancini, Thomas Mikal-Evans, Karan Molaverdikhani, Enric Palle, Benjamin V. Rackham, Seth Redfield, Kevin B. Stevenson, Jeff A. Valenti, Nicole L. Wallack, Keshav Aggarwal, Eva-Maria Ahrer, Ian J. M. Crossfield, Nicolas Crouzet, Nicolas Iro, Nikolay K. Nikolov, Peter J. Wheatley
Figure caption: Graphical representation of the logic behind our in-band (red) and out-of-band (dark blue) definitions. The panels show the cuts in the models for the only-CO model (left-hand panel), the non-CO model (middle panel), and the resulting clear CO sub-bands model (right-hand panel).
Paper: Multiple Channels for Nitrogen Pollution by Metal-enriched Supermassive Stars and Implications for GN-z11
Authors: Chris Nagele, Hideyuki Umeda
Figure caption: Abundance ratios of nitrogen to oxygen, carbon to oxygen, and oxygen to hydrogen. The symbols denote each of the four models, while the color shows how much Z = 0.1 Z ⊙ ISM the yields from each model have mixed with. The gray regions show the conservative (lighter) and fiducial (darker) constraints on GN-z11 from the model of Cameron et al. (2023).
Paper: Multiple Channels for Nitrogen Pollution by Metal-enriched Supermassive Stars and Implications for GN-z11
Authors: Chris Nagele, Hideyuki Umeda
Figure caption: Log elemental yields, relative to Fe, relative to solar (Asplund et al. 2009), for each of the four models. For the 105 M ⊙ model, this includes not only wind-driven mass loss, but also the explosion ejecta.
Paper: Multiple Channels for Nitrogen Pollution by Metal-enriched Supermassive Stars and Implications for GN-z11
Authors: Chris Nagele, Hideyuki Umeda
Figure caption: Kippenhahn diagrams for the four models. The horizontal axis is time until the end of the simulation (for the two lower-mass models) or until the GR instability (for the two higher-mass models) while the vertical axes are mass coordinate and cumulative 14N ejected from the stellar wind. In the upper half of each panel the color shows the heating and [very small] cooling rate from nuclear and neutrino reactions. The hatches show convective (diagonal), radiative (dotted) and semiconvective (crossed) regions.