adsabs/AstroCLIMB huggingface dataset:
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: Posterior distribution of orbital elements fit to NIRC2 astrometry of θ 1 Ori B2–B3. The fit displays a posterior distribution typical of short-arc visual orbit fits, with the same bimodal ω and Ω noted previously, normally distributed π and M tot, correlated semimajor axis, eccentricity, and inclinations that are otherwise relatively constrained. This orbit is so satisfyingly typical that I have petitioned for it act as the unofficial mascot of orbitize!, but I have not yet been humored thusly.
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: Posterior distribution of orbital elements fit to the astrometry of HD 142527 B. Here, ω and Ω show bimodal distributions with peaks spaced 180° apart; this a known degeneracy in visual orbits with a lack of RV constraints.
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: A corner plot illustrating the posterior distribution of BKA forward model fits to the 2013 April 11 Hα data, which are representative of all other epochs. Note that all marginal parameters are normally distributed, and the only correlation is a slight linear correlation between the X and Y positions.
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: A saturated image of HD 142527. The position of the instrumental ghost is marked with a black arrow. The Y-axis is in pixels, and the X-axis is labeled in milliarcseconds to illustrate the spatial extent of the 451 pixel crop and the position of the ghost.
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: Five hundred orbital fits to the NIRC2 astrometry of θ 1 Ori B2–B3 randomly drawn from the posterior distribution. Astrometry compiled in Table 7 is overplotted. Only the NIRC2 astrometry (orange triangles) was used to fit the orbit of the binary, and the corrected VisAO astrometry (red diamonds) falls along the fit orbits by design.
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: A gallery of BKA forward model best fits to HD 142527 B in the continuum filter, in chronological order from top to bottom. Data (left) are fit by BKA, yielding a best-fit forward model (center) and their difference (right).
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: A gallery of BKA forward model best fits to HD 142527 B in the Hα filter, in chronological order from top to bottom. Data (left) are fit by BKA, yielding a best-fit forward model (center) and their difference (right).
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: Galactic positions for MELANGE-2 (gray-blue), Group-X (orange), and Coma Ber (pink). TOI 2048, a Group-X candidate member, is marked by the green star. MELANGE-2 candidate members with rotation periods detected in TESS are outlined in black. Data for Coma Ber come from Tang et al. (2019). For Group-X, candidate members from Tang et al. and Fürnkranz et al. and Friends of TOI 2048 with ﹩{\rm{\Delta }}{v}_{\tan }\lt 2﹩ km s−1 are shown as filled orange circles. Open orange circles are Friends with ﹩{\rm{\Delta }}{v}_{\tan }\gt 2﹩ km s−1. There is some overlap between Group-X (especially Friends with ﹩{\rm{\Delta }}{v}_{\tan }\gt 2﹩ km s−1) and MELANGE-2.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: Rotation periods for Friends of TIC 224606446 (larger red-orange circles) showing both secure period detections (filled circles) and candidate periods (open circles). There is some overlap with Friends of TOI 2048. Also shown are rotation periods of benchmark clusters Pleiades (small blue circles) and Praesepe (small purple circles). Friends of TIC 224606446 generally lie along the sequence defined by Praesepe.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: Exoplanets from the NASA Exoplanet Archive (NASA Exoplanet Science Institute 2020) as a function of planet radius (R ⊕) and orbital period (days). Contours show all planets from Kepler and K2. Young (<1 Gyr), transiting planets that are part of open star clusters or associations are plotted in circles colored by their age; data for these planets are listed in Table 9. TOI 2048 b is outlined as a star and lands in the main distribution of its older counterparts.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: Individual transits for TOI 2048 b. Time is in days from transit center; the time of transit is given in the upper right in TJBD. Flux is in ppt with vertical offset applied. Small gray points show the TESS-SAP data after outliers have been removed. The larger red points show the binned data with error bars; the error bars are similar in size to the data points. Bins are 30 minutes; the points are the weighted average, and the error bars are the standard error on the means. The blue shaded region shows the 1σ range of the model (stellar variability Gaussian process plus transit).
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: Phase-folded transit light curve for TOI 2048 b, detrending using the stellar rotation model. Time is in units of days, and the flux is in ppt. Small gray points show the TESS-SAP data after outliers have been removed and the stellar variability model has been removed. The larger red points show the binned data with error bars; the error bars are similar in size to the data points. Bins are 20 minutes; the points are the weighted average, and the error bars are the standard error on the means. The blue shaded region shows the 1σ range of the transit model.
Paper: TESS Hunt for Young and Maturing Exoplanets (THYME). VII. Membership, Rotation, and Lithium in the Young Cluster Group-X and a New Young Exoplanet
Authors: Elisabeth R. Newton, Rayna Rampalli, Adam L. Kraus, Andrew W. Mann, Jason L. Curtis, Andrew Vanderburg, Daniel M. Krolikowski, Daniel Huber, Grayson C. Petter, Allyson Bieryla, Benjamin M. Tofflemire, Pa Chia Thao, Mackenna L. Wood, Ronan Kerr, Boris S. Safanov, Ivan A. Strakhov, David R. Ciardi, Steven Giacalone, Courtney D. Dressing, Holden Gill, Arjun B. Savel, Karen A. Collins, Peyton Brown, Felipe Murgas, Keisuke Isogai, Norio Narita, Enric Palle, Samuel N. Quinn, Jason D. Eastman, Gábor Fűrész, Bernie Shiao, Tansu Daylan, Douglas A. Caldwell, George R. Ricker, Roland Vanderspek, Sara Seager, Joshua N. Winn, Jon M. Jenkins, David W. Latham
Figure caption: Top panel: 1-day segment of the 2-minute light curve of TIC 137834492 showing multiperiodic, high-frequency pulsations characteristic of young δ Scuti stars. Bottom panel: amplitude spectrum of the full 2-minute light curve (sectors 16, 22, and 23) centered on the pulsations.
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: The visible-light contrast of HD 142527 B with respect to the continuum of HD 142527 A over time. Brown and green diamonds mark our Hα and continuum contrast measurements, respectively. The gray shaded region represents the 1σ standard deviation of our measurements of continuum contrast, centered on the median. The red and blue squares mark the contrasts measured in nearly equivalent filters by Cugno et al. (2019) using VLT/SPHERE/ZIMPOL. The amount of Hα excess appears to vary between many of the epochs, while the continuum contrast varies minimally and is consistent with uniformity within error bars.
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: Gallery of post-KLIP images showing the detections of HD 142527 B in Hα (top) and continuum (bottom). The colorbar is normalized to the peak pixel value of the companion in each image. The cyan circle indicates the nearest in time position of HD 142527 B reported in previous literature (Lacour et al. 2016; Claudi et al. 2019). The cyan star indicates the position of HD 142527 A. The innermost pixels have been masked to r ∼ 1 FWHM for each data set.
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: The orbit of HD 142527 B in context. The position of HD 142527 A is marked with a cyan star, and 250 randomly drawn orbits from fits to the astrometry of HD 142527 B are plotted with colors corresponding to their mutual inclination with the outer disk (θ ⋆−out). The outer image of the circumbinary disk is a Gemini/GPI scattered light polarized intensity H-band image reprocessed with an updated GPI pipeline and interpolated to VisAO’s platescale. The inner image is the post-KLIP 2015 May 15 Hα detection from VisAO (also shown in Figure 1). Both images are normalized to their respective maximum pixel values before combination.
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: Astrometric measurements of HD 142527 B relative to HD 142527 A (black star) from NACO, GPI, SPHERE, SINFONI, and VisAO (this work) between 2012 and 2018. The crosses represent the reported uncertainties on each measurement. The companion experiences significant orbital motion (Δθ ≈ 65°) and decreases substantially in separation (Δρ ≈ 30 mas) from 2016 to 2018. The VisAO values (yellow circles) agree well with astrometry from other instruments. Error bars on our measurements reflect the 1–2 mas accuracy achievable using pyklip forward modeling.
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: One hundred randomly drawn orbitize! orbits fit to the motion of HD 142527 B. Astrometry from Figure 3 is overplotted. Left: the orbits projected in RA and Dec, relative to HD 142527 A (black star). Right: the orbits in separation/position angle vs. time. The new VisAO astrometry does not add new coverage of the orbital arc, but the 2018 recovery adds more weight to the near-in-time SPHERE NRM astrometry.
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: Representative images of θ 1 Ori B2–B3 from NIRC2 (left, NB2.108 band) and MagAO (right, z′ band). All relative astrometry herein is conducted with respect to θ 1 Ori B2, which is centered at (0, 0).
Paper: Improved Orbital Constraints and Hα Photometric Monitoring of the Directly Imaged Protoplanet Analog HD 142527 B
Authors: William O. Balmer, Katherine B. Follette, Laird M. Close, Jared R. Males, Robert J. De Rosa, Jéa I. Adams Redai, Alex Watson, Alycia J. Weinberger, Katie M. Morzinski, Julio Morales, Kimberly Ward-Duong, Laurent Pueyo
Figure caption: Representative pyklip forward model fits for HD 142527 B. Shown are the 2013 April 11 Hα (top row) and continuum (bottom row) detections. Based on the PlanetEvidence analysis, the evidence ratios ﹩\mathrm{log}{Z}_{1}/{Z}_{0}﹩ are 266.30 and 75.89 in Hα and continuum, respectively. Both are considered extremely strong evidence in favor of the existence of the companion at this location.
Paper: A CHEOPS Search for Massive, Long-period Companions to the Warm Jupiter K2-139 b
Authors: Alexis M. S. Smith, Szilárd Csizmadia
Figure caption: Transit photometry of K2-139. The top panel shows the combined K2 and CHEOPS light curve, phase folded and with all the systematics and the red-noise wavelets subtracted. The original data points are plotted as small gray points, and the larger red circles are the same data binned in phase, with a bin width corresponding to 10 minutes. Below are the residuals to our best-fitting model. The lower panel shows the individual K2 and CHEOPS light curves, labeled with the corresponding instrument name and the UT date of midtransit, and vertically offset for clarity. In all cases, our best-fitting model is shown as a solid green line.
Paper: A CHEOPS Search for Massive, Long-period Companions to the Warm Jupiter K2-139 b
Authors: Alexis M. S. Smith, Szilárd Csizmadia
Figure caption: Comparison of Kepler/K2 (dashed line) and CHEOPS (solid line) instrument response as a function of wavelength. The Kepler data are taken from the Kepler Science Center, and the CHEOPS data from the ESA website.
Paper: A CHEOPS Search for Massive, Long-period Companions to the Warm Jupiter K2-139 b
Authors: Alexis M. S. Smith, Szilárd Csizmadia
Figure caption: CHEOPS photometry of K2-139 produced by the DRP using the OPTIMAL aperture.
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption: Left: “standard” analysis pipeline used to infer atmospheric K zz by generating a likelihood distribution from the abundance of key species. Right: schematic of the analysis pipeline used for the multivariate approach to identify optimal predictors. Inverse modeling, based on observational data, is used to create a model of a planet’s atmospheric chemistry. From this model, the list of thermodynamically favorable reactions and their rates is used to construct the chemical reaction network, for which topology, key species abundances, and Gibbs free energy are measured. The data then form the basis of an interpolation function, which is fed a selection of initial physical conditions, drawn from a Gaussian distribution, to determine what the corresponding network parameters are if a network was to be constructed using those initial physical conditions. The resulting distributions can then be used to quantitatively rank any given atmosphere with another in terms of distance from thermochemical disequilibrium and can provide target variables for development in future inverse modeling tools.
Paper: Toward a Data-driven Model of the Sky from Low Earth Orbit as Observed by the Hubble Space Telescope
Authors: Sarah E. Caddy, Lee R. Spitler, Simon C. Ellis
Figure caption: The SEDs of averaged sky measurements from fields that were selected using criteria given in Section 3.2 to have minimal stray light as well as fields selected to have a larger stray-light contribution. The standard deviation, normalized by the sample size of the observations, is also plotted as error bars on all data points. The normalized standard deviation of sky surface brightness for fields with higher stray-light contribution is larger as these exposures span a larger range of Sun altitudes and limb angles to ensure a larger sample size. The SED from the fields selected to have minimal stray light follow the Aldering (2002)-predicted zodiacal light SED model toward the GOODS North fields. The SED of the fields with stray light cannot be fitted with a zodiacal light, earthshine, or solar spectrum alone. A solar plus zodiacal spectrum also did not fit the relatively blue observed SED. To mimic the spectrum of stray light from earthshine, we combined a Rayleigh-scattered solar spectrum component with a zodiacal light spectrum and fit these to the data. This model is able to reproduce the F435W excess seen in the stray-light-contaminated data.
Paper: Inferring Exoplanet Disequilibria with Multivariate Information in Atmospheric Reaction Networks
Authors: Theresa Fisher, Hyunju Kim, Camerian Millsaps, Michael Line, Sara I. Walker
Figure caption: (a) The abundance of CH4, CO, NH3, and N2 as a function of the temperature of the atmosphere at constant pressure of 100 mbar, demonstrating the transition from abundant reduced species (CH4 and NH3) to abundant oxidized species (CO and N2) as temperatures increase. Increasing the K zz from equilibrium (left) to K zz = 1010 (right) leads to the transition occurring at higher temperatures than the equilibrium case. The dashed lines mark 600, 1200, and 1800 K, which are the temperatures of the corresponding networks shown in panel (b). (b) Network diagrams of the atmospheric chemical reaction network of a hot Jupiter over a range of temperatures, at solar metallicity and K zz = 0 (top) and K zz = 1010 (bottom), demonstrating how network topological properties measurably change as a function of physical parameters—in this case, irradiation temperature. The networks at irradiation temperatures 600, 1200, and 1800 K are represented by yellow, orange, and red, respectively. The size of the nodes represents the flux-weighted degree of each node, and the width of edges indicate their reaction rate. Both the size of nodes and edges are rescaled consistently and normalized at each temperature and K zz.