adsabs/AstroCLIMB huggingface dataset:
Paper: SKYSURF: Constraints on Zodiacal Light and Extragalactic Background Light through Panchromatic HST All-sky Surface-brightness Measurements: II. First Limits on Diffuse Light at 1.25, 1.4, and 1.6 μm
Authors: Timothy Carleton, Rogier A. Windhorst, Rosalia O'Brien, Seth H. Cohen, Delondrae Carter, Rolf Jansen, Scott Tompkins, Richard G. Arendt, Sarah Caddy, Norman Grogin, Scott J. Kenyon, Anton Koekemoer, John MacKenty, Stefano Casertano, Luke J. M. Davies, Simon P. Driver, Eli Dwek, Alexander Kashlinsky, Nathan Miles, Nor Pirzkal, Aaron Robotham, Russell Ryan, Haley Abate, Hanga Andras-Letanovszky, Jessica Berkheimer, Zak Goisman, Daniel Henningsen, Darby Kramer, Ci'mone Rogers, Andi Swirbul
Figure caption: (a) [Top Left]: Spectral index distribution N(α) when interpolating the Kelsall et al. (1998) zodiacal sky-SB prediction of SKYSURF F160W pointings in the COBE/DIRBE J- and K-band filters. The median power-law spectral index and its 1σ range is α = 0.713 ± 0.023. (b) [Top Right]:  thermal dark signal corrections predicted by synphot in the WFC3 F125W, F140W, and F160W filters as a function of the change in telescope ambient temperature ΔT required to provide a best fit to the observed thermal dark signals shown in panels (c) and (d). The (ΔT, TD signal) numbers listed bracket the range of temperature and TD signal considered here (see Table 2). (c) [Bottom Left]: Mean Sky-SB values averaged over 500 WFC3/IR exposures in filters F098M, F105W, F110W, F125W, F127M, F139M, F140W, F159M, and F160W taken in distinct fields, subtracting various different thermal dark signal scenarios as a function of ambient temperature T ref. The lightly shaded points were affected by the geocoronal He II 1.083 μm-line (in F105W and F110W), or got too close to the Earth’s limb. The red asterisks show the zodiacal spectrum of Aldering (2001) at each filter’s effective central wavelength using Equation (4). All synphot thermal dark subtracted scenarios are normalized to the ratio at 1.25 μm, which is by definition unity. Blue squares and their median fit (blue solid line) assume that no thermal dark signal needs to be subtracted. The orange squares and green line assume T = T ref as the best fit, which is taken from the reference files. The green squares and green line assume the Aldering (2001) near-IR zodiacal spectral slope of α = 0.73 and an HST temperature T = T ref + 1.52 K. (d) [Bottom Right]: As in panel (c), but with the green squares and green line assuming a near-IR zodiacal spectral slope α = 0.65 and an HST temperature of T = T ref –1.62 K. The two ΔT cases in panels (b)–(d) bracket the likely range in HST telescope ambient temperatures, which are used to estimate the possible range in F125W–F160W thermal dark signal that needs to be subtracted from any diffuse sky-SB signal (Section 3.4).
Paper: SKYSURF: Constraints on Zodiacal Light and Extragalactic Background Light through Panchromatic HST All-sky Surface-brightness Measurements: II. First Limits on Diffuse Light at 1.25, 1.4, and 1.6 μm
Authors: Timothy Carleton, Rogier A. Windhorst, Rosalia O'Brien, Seth H. Cohen, Delondrae Carter, Rolf Jansen, Scott Tompkins, Richard G. Arendt, Sarah Caddy, Norman Grogin, Scott J. Kenyon, Anton Koekemoer, John MacKenty, Stefano Casertano, Luke J. M. Davies, Simon P. Driver, Eli Dwek, Alexander Kashlinsky, Nathan Miles, Nor Pirzkal, Aaron Robotham, Russell Ryan, Haley Abate, Hanga Andras-Letanovszky, Jessica Berkheimer, Zak Goisman, Daniel Henningsen, Darby Kramer, Ci'mone Rogers, Andi Swirbul
Figure caption: [(a) Top Left]: HST WFC3/IR sky-SB measurements in the F160W filter vs. ecliptic latitude after subtracting the best WFC3/IR thermal dark signal estimate for each exposure from Section 3.3 and the DGL signal from Section 3.5. Black dots indicate all observations from Figure 2, and red dots only those with Sun angle SA = 90° ± 10°. The COBE/DIRBE data, to which the models were fit, were taken at a comparable SA range. The blue points indicate the one-sided clipped medians of the SA = 90° ± 10° points in each 10° b Ecl bin, and the blue line indicates the best sech fit to these medians. [(b) Top Middle]: Kelsall et al. (1998) ZL model prediction for the same sky pointings and filters, observing day of the year, and Sun angles as the HST data in (a) with their medians and best-fit sech model. [(c) Top Right]: As in (b), but for the Wright (1998) zodiacal model prediction. [(d), (e), (f) Middle Row]: The clipped medians for each b Ecl bin from panels (a), (b), (c) are reproduced for clarity, respectively, with their errors plus the best sech fits and their coefficients. [(g) Bottom Middle]: Difference between each (HST–TD–DGL) data point from (a) and its Kelsall et al. (1998) ZL model prediction from (b), with the difference in their sech fits (blue line). The green dashed line indicates the two-sided 1σ clipped median for SA = 90° ± 10° and ∣b Ecl∣ ≳ 30° (Table 3). [(h) Bottom Right]: As in (g), but for the Wright (1998) zodiacal model prediction from (c).
Paper: SKYSURF: Constraints on Zodiacal Light and Extragalactic Background Light through Panchromatic HST All-sky Surface-brightness Measurements: II. First Limits on Diffuse Light at 1.25, 1.4, and 1.6 μm
Authors: Timothy Carleton, Rogier A. Windhorst, Rosalia O'Brien, Seth H. Cohen, Delondrae Carter, Rolf Jansen, Scott Tompkins, Richard G. Arendt, Sarah Caddy, Norman Grogin, Scott J. Kenyon, Anton Koekemoer, John MacKenty, Stefano Casertano, Luke J. M. Davies, Simon P. Driver, Eli Dwek, Alexander Kashlinsky, Nathan Miles, Nor Pirzkal, Aaron Robotham, Russell Ryan, Haley Abate, Hanga Andras-Letanovszky, Jessica Berkheimer, Zak Goisman, Daniel Henningsen, Darby Kramer, Ci'mone Rogers, Andi Swirbul
Figure caption: SKYSURF on the level of diffuse light compared with limits on diffuse light. As in Figure 10, purple triangles and blue open and filled circles are from Matsuura et al. (2017), Lauer et al. (2021), and Lauer et al. (2022) respectively. Also shown for context are iEBL estimates from Koushan et al. (2021) as the gray points, and the Driver et al. (2016) model fit to those measurements as the gray line. The large open orange circles with their error ranges are the SKYSURF diffuse light upper limits in the WFC3/IR filters F125W, F140W, and F160W, as discussed in Sections 3.1–3.6, Figures 5–9, and Tables 1–3, from which the iEBL+eEBL has already been subtracted. The shaded orange wedge indicates our diffuse light limits, given the current best knowledge of the HST temperature range and its resulting WFC3/IR thermal dark signal, along with the subtracted discrete iEBL+eEBL signal (Section 3). The synphot HST component temperature predictions can vary by ΔT ≃ ± 2 K from those in the HST engineering data and FITS headers. The best χ 2 fit occurs for an average (pysynphot–HST-header) difference of ΔT = –1.15 K. The ΔT value that is most consistent with the 1–2 μm Kelsall slope of the zodiacal spectrum (α = 0.713; see Section 3.4) is also indicated, and occurs for the (HST-header–synphot) temperature difference of ΔT = +0.90 K. Therefore, while our limits to the F125W and F140W diffuse light are a factor ∼3 above the best available discrete EBL counts of Koushan et al. (2021), any diffuse signal in the F160W filter could be fainter still, as indicated by the orange wedge. The upper limits of the orange wedge correspond to the limits derived from the SA90 method. Details are given in Sections 3 and 4. At 1.25 and 1.4 microns, the detection of diffuse light is not very dependent on the assumed thermal dark signal. While our fiducial F160W results are consistent with the F125W and F140W limits, the F160W limit depends much more strongly on the assumed thermal dark signal.
Paper: SKYSURF: Constraints on Zodiacal Light and Extragalactic Background Light through Panchromatic HST All-sky Surface-brightness Measurements: II. First Limits on Diffuse Light at 1.25, 1.4, and 1.6 μm
Authors: Timothy Carleton, Rogier A. Windhorst, Rosalia O'Brien, Seth H. Cohen, Delondrae Carter, Rolf Jansen, Scott Tompkins, Richard G. Arendt, Sarah Caddy, Norman Grogin, Scott J. Kenyon, Anton Koekemoer, John MacKenty, Stefano Casertano, Luke J. M. Davies, Simon P. Driver, Eli Dwek, Alexander Kashlinsky, Nathan Miles, Nor Pirzkal, Aaron Robotham, Russell Ryan, Haley Abate, Hanga Andras-Letanovszky, Jessica Berkheimer, Zak Goisman, Daniel Henningsen, Darby Kramer, Ci'mone Rogers, Andi Swirbul
Figure caption: SKYSURF F125W, F140W, and F160W sky-SB measurements from the HST data compared to the Kelsall COBE/DIRBE models [in Myr/sr] vs. ecliptic latitude b Ecl. Data in the bottom subpanels are restricted to the darkest Galactic regions with 20°≲∣ b II ∣ ≲ 60° (see Figure 1) and zoomed into the most relevant range. Left subpanels give the HST F125W/Kelsall 1.25 μm model flux density ratio, while the right subpanels give the linear flux difference between the HST data and the Kelsall COBE/DIRBE models for the same subsample. The orange sech functions and error wedges outline the darkest sky-SB measurements from Figure 2. The green wedges in the bottom subpanels illustrate the HST–Kelsall difference between sech fits from Figure 3, highlighting our best estimates of the Δ(HST data—Kelsall COBE/DIRBE model) of 0.0145 ± 0.007 MJy sr−1 for F125W, 0.025 ± 0.010 MJy sr−1 for F140W, and 0.048 ± 0.010 for F160W (Table 1). The bottom right subpanels best capture the linear SB difference between the HST sky-SB observations and the COBE/DIRBE Kelsall 1.25 μm model (magnify the PDF figure as needed to see the difference).
Paper: SKYSURF: Constraints on Zodiacal Light and Extragalactic Background Light through Panchromatic HST All-sky Surface-brightness Measurements: II. First Limits on Diffuse Light at 1.25, 1.4, and 1.6 μm
Authors: Timothy Carleton, Rogier A. Windhorst, Rosalia O'Brien, Seth H. Cohen, Delondrae Carter, Rolf Jansen, Scott Tompkins, Richard G. Arendt, Sarah Caddy, Norman Grogin, Scott J. Kenyon, Anton Koekemoer, John MacKenty, Stefano Casertano, Luke J. M. Davies, Simon P. Driver, Eli Dwek, Alexander Kashlinsky, Nathan Miles, Nor Pirzkal, Aaron Robotham, Russell Ryan, Haley Abate, Hanga Andras-Letanovszky, Jessica Berkheimer, Zak Goisman, Daniel Henningsen, Darby Kramer, Ci'mone Rogers, Andi Swirbul
Figure caption: [(a) Top Left]: HST WFC3/IR sky-SB measurements in the F125W filter vs. ecliptic latitude after subtracting the best WFC3/IR thermal dark signal estimate for each exposure from Section 3.3 and the DGL signal from Section 3.5. Black dots indicate all observations from Figure 2, and red dots only those with Sun angle SA = 90° ± 10°. The COBE/DIRBE data, to which the models were fit, were taken at a comparable SA range. The blue points indicate the one-sided clipped medians of the SA = 90° ± 10° points in each 10° b Ecl bin, and the blue line indicates the best sech fit to these medians. [(b) Top Middle]: Kelsall et al. (1998) ZL model prediction for the same sky pointings and filters, observing day of the year, and Sun angles as the HST data in (a) with their medians and best-fit sech model. [(c) Top Right]: As in (b), but for the Wright (1998) zodiacal model prediction. [(d), (e), (f) Middle Row]: The clipped medians for each b Ecl bin from panels (a), (b), (c) are reproduced for clarity, respectively, with their errors plus the best sech fits and their coefficients. [(g) Bottom Middle]: Difference between each (HST–TD–DGL) data point from (a) and its Kelsall et al. (1998) ZL model prediction from (b), along with the difference in their sech fits (blue line). The green dashed line indicates the two-sided 1σ clipped median for SA = 90° ± 10° and ∣b Ecl∣ ≳ 30° (Table 3). [(h) Bottom Right]: As in (g), but for the Wright (1998) zodiacal model prediction from (c).
Paper: SKYSURF: Constraints on Zodiacal Light and Extragalactic Background Light through Panchromatic HST All-sky Surface-brightness Measurements: II. First Limits on Diffuse Light at 1.25, 1.4, and 1.6 μm
Authors: Timothy Carleton, Rogier A. Windhorst, Rosalia O'Brien, Seth H. Cohen, Delondrae Carter, Rolf Jansen, Scott Tompkins, Richard G. Arendt, Sarah Caddy, Norman Grogin, Scott J. Kenyon, Anton Koekemoer, John MacKenty, Stefano Casertano, Luke J. M. Davies, Simon P. Driver, Eli Dwek, Alexander Kashlinsky, Nathan Miles, Nor Pirzkal, Aaron Robotham, Russell Ryan, Haley Abate, Hanga Andras-Letanovszky, Jessica Berkheimer, Zak Goisman, Daniel Henningsen, Darby Kramer, Ci'mone Rogers, Andi Swirbul
Figure caption: All SKYSURF sky-SB measurements vs. ecliptic latitude for HST data (left subpanels) and the Kelsall COBE/DIRBE models (right subpanels), but only for the darkest Galactic regions with 20° ≲ ∣ b II ∣ ≲ 60° (see Figure 1). As in Figure 1, the upper left plot is for F125W, the upper right plot is for F140W, and the lower left plot is for F160W. The orange and blue sech functions and error wedges outline the darkest ∼1% of the sky-SB measurements (magnify the PDF figure as needed to see this). Bottom panels give enlargements of the top panels.
Paper: SKYSURF: Constraints on Zodiacal Light and Extragalactic Background Light through Panchromatic HST All-sky Surface-brightness Measurements: II. First Limits on Diffuse Light at 1.25, 1.4, and 1.6 μm
Authors: Timothy Carleton, Rogier A. Windhorst, Rosalia O'Brien, Seth H. Cohen, Delondrae Carter, Rolf Jansen, Scott Tompkins, Richard G. Arendt, Sarah Caddy, Norman Grogin, Scott J. Kenyon, Anton Koekemoer, John MacKenty, Stefano Casertano, Luke J. M. Davies, Simon P. Driver, Eli Dwek, Alexander Kashlinsky, Nathan Miles, Nor Pirzkal, Aaron Robotham, Russell Ryan, Haley Abate, Hanga Andras-Letanovszky, Jessica Berkheimer, Zak Goisman, Daniel Henningsen, Darby Kramer, Ci'mone Rogers, Andi Swirbul
Figure caption: [(a) Top Left]: HST WFC3/IR sky-SB measurements in the F140W filter vs. ecliptic latitude after subtracting the best WFC3/IR thermal dark signal estimate for each exposure from Section 3.3 and the DGL signal from Section 3.5. Black dots indicate all observations from Figure 2, and red dots only those with Sun angle SA = 90° ± 10°. The COBE/DIRBE data, to which the models were fit, were taken at a comparable SA range. The blue points indicate the one-sided clipped medians of the SA = 90° ± 10° points in each 10° b Ecl bin, and the blue line indicates the best sech fit to these medians. [(b) Top Middle]: Kelsall et al. (1998) ZL model prediction for the same sky pointings and filters, observing day of the year, and Sun angles as the HST data in (a) with their medians and best-fit sech model. [(c) Top Right]: As in (b), but for the Wright (1998) zodiacal model prediction. [(d), (e), (f) Middle Row]: The clipped medians for each b Ecl bin from panels (a), (b), (c) are reproduced for clarity, respectively, with their errors plus the best sech fits and their coefficients. [(g) Bottom Middle]: Difference between each (HST–TD–DGL) data point from (a) and its Kelsall et al. (1998) ZL model prediction from (b), along with the difference in their sech fits (blue line). The green dashed line indicates the two-sided 1σ clipped median for SA = 90° ± 10° and ∣b Ecl∣ ≳ 30° (Table 3). [(h) Bottom Right]: As in (g), but for the Wright (1998) zodiacal model prediction from (c).
Paper: SKYSURF: Constraints on Zodiacal Light and Extragalactic Background Light through Panchromatic HST All-sky Surface-brightness Measurements: II. First Limits on Diffuse Light at 1.25, 1.4, and 1.6 μm
Authors: Timothy Carleton, Rogier A. Windhorst, Rosalia O'Brien, Seth H. Cohen, Delondrae Carter, Rolf Jansen, Scott Tompkins, Richard G. Arendt, Sarah Caddy, Norman Grogin, Scott J. Kenyon, Anton Koekemoer, John MacKenty, Stefano Casertano, Luke J. M. Davies, Simon P. Driver, Eli Dwek, Alexander Kashlinsky, Nathan Miles, Nor Pirzkal, Aaron Robotham, Russell Ryan, Haley Abate, Hanga Andras-Letanovszky, Jessica Berkheimer, Zak Goisman, Daniel Henningsen, Darby Kramer, Ci'mone Rogers, Andi Swirbul
Figure caption: A comparison of the HST F125W and COBE/DIRBE J-band filters to the solar spectrum in F  ν , which is fairly flat across these filters. For a zodiacal spectrum, the expected J-filter flux difference between HST WFC3/IR measurements and the COBE/DIRBE models due to small differences in their respective filter efficiency curves corresponds to –0.0061 AB-mag. We apply this ZP difference to our diffuse light estimates in the tables of Section 3.1. Note that the geocoronal 1.083 μm He II line is essentially suppressed in the wings of both filters.
Paper: A Transmission Spectrum of the Sub-Earth Planet L98-59 b in 1.1–1.7 μm
Authors: Mario Damiano, Renyu Hu, Thomas Barclay, Sebastian Zieba, Laura Kreidberg, Jonathan Brande, Knicole D. Colon, Giovanni Covone, Ian Crossfield, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Emily Gilbert, Christina L. Hedges, Edwin S. Kite, Ravi K. Kopparapu, Veselin B. Kostov, Caroline Morley, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Elisa V. Quintana
Figure caption: Top panel: transmission spectrum of L98-59 b in comparison with model scenarios. The scenarios of an H2O- or CO2-dominated atmosphere assume that the atmosphere does not have clouds or haze and has a temperature of the planet’s equilibrium temperature. The H2-dominated atmosphere model is the model calculated from the median of the posterior distribution shown in Figure 5. This model has HCN with a volume mixing ratio of 360 parts per million and clouds at 103 Pa in the atmosphere. Bottom panel: the HST data (Benneke et al. 2019; Tsiaras et al. 2019) comparing with atmospheric models of L98-59 b in the context of JWST observations. The dashed lines show the models with an H2-dominated atmosphere and solar-abundance water and methane for comparison—these models are ruled out by the current data. The models permitted by the transmission spectrum reported here can be distinguished with JWST observations in ∼1.5–5 μm.
Paper: A Transmission Spectrum of the Sub-Earth Planet L98-59 b in 1.1–1.7 μm
Authors: Mario Damiano, Renyu Hu, Thomas Barclay, Sebastian Zieba, Laura Kreidberg, Jonathan Brande, Knicole D. Colon, Giovanni Covone, Ian Crossfield, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Emily Gilbert, Christina L. Hedges, Edwin S. Kite, Ravi K. Kopparapu, Veselin B. Kostov, Caroline Morley, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Elisa V. Quintana
Figure caption: Posterior distributions of the retrieval on the 1D transmission spectrum of L98-59 b. The result suggests a light atmosphere (H2-dominated) with clouds or haze and also hints the presence of HCN. The volume mixing ratio (VMR) of HCN has a distribution peak toward high values, but is otherwise not well constrained. All the other gases considered in the fitting show VMR distributions toward low values or completely flat, suggesting their absence in the atmosphere or a presence below the cloud deck not detectable by transmission spectroscopy. The parameter R  p  in is defined as the radius at the bottom of the atmosphere, and therefore, when the atmosphere is more extended, the smaller this value must be to maintain consistency with the apparent radius of the planet.
Paper: A Transmission Spectrum of the Sub-Earth Planet L98-59 b in 1.1–1.7 μm
Authors: Mario Damiano, Renyu Hu, Thomas Barclay, Sebastian Zieba, Laura Kreidberg, Jonathan Brande, Knicole D. Colon, Giovanni Covone, Ian Crossfield, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Emily Gilbert, Christina L. Hedges, Edwin S. Kite, Ravi K. Kopparapu, Veselin B. Kostov, Caroline Morley, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Elisa V. Quintana
Figure caption: White-light curves of HST observations of L98-59 b transits. For each visit, the left panel shows the light curves from 2D images after correcting for systematics, and the right panel shows the residuals of the fit of the white-light curves. The dashed line depicts the best-fit transit model. A vertical shift of 0.001 is applied between the visits to better visualize the curves.
Paper: A Transmission Spectrum of the Sub-Earth Planet L98-59 b in 1.1–1.7 μm
Authors: Mario Damiano, Renyu Hu, Thomas Barclay, Sebastian Zieba, Laura Kreidberg, Jonathan Brande, Knicole D. Colon, Giovanni Covone, Ian Crossfield, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Emily Gilbert, Christina L. Hedges, Edwin S. Kite, Ravi K. Kopparapu, Veselin B. Kostov, Caroline Morley, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Elisa V. Quintana
Figure caption: Transmission spectra of L98-59 b using the two independent methods described in Section 2. Each of the two spectra is the weighted average of the five single visits.
Paper: A Transmission Spectrum of the Sub-Earth Planet L98-59 b in 1.1–1.7 μm
Authors: Mario Damiano, Renyu Hu, Thomas Barclay, Sebastian Zieba, Laura Kreidberg, Jonathan Brande, Knicole D. Colon, Giovanni Covone, Ian Crossfield, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Emily Gilbert, Christina L. Hedges, Edwin S. Kite, Ravi K. Kopparapu, Veselin B. Kostov, Caroline Morley, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Elisa V. Quintana
Figure caption: Colored: calculated 1D transmission spectrum of L98-59 b for each of the five HST visits resulting from the data analysis A described in Section 2. Black: weighted average combined transmission spectrum.
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: Average neighbor degree as a function of temperature and K zz, at 0.1, 1, 10, and 100 times solar metallicity. The x-axis is temperature, y-axis is K zz, and color corresponds to the weighted average neighbor degree (see color bar for each individual plot for scale).
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: Phi distributions over a range of uncertainties and K zz values, drawn from a 10,000-point normal distribution of initial conditions centered at 1200 K.
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: Average clustering coefficient as a function of temperature and K zz, at 0.1, 1, 10, and 100 times solar metallicity. The x-axis is temperature, y-axis is K zz, and color corresponds to the weighted average clustering coefficient (see color bar for each individual plot for scale).
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: Average shortest path length as a function of temperature and K zz, at 0.1, 1, 10, and 100 times solar metallicity. The x-axis is temperature, y-axis is K zz, and color corresponds to the weighted average shortest path length (see color bar for each individual plot for scale).
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: Node betweenness centrality as a function of temperature and K zz, at 0.1, 1, 10, and 100 times solar metallicity. The x-axis is temperature, y-axis is K zz, and color corresponds to the weighted node betweenness centrality (see color bar for each individual plot for scale).
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: Edge betweenness centrality as a function of temperature and K zz, at 0.1, 1, 10, and 100 times solar metallicity. The x-axis is temperature, y-axis is K zz, and color corresponds to the weighted edge betweenness centrality (see color bar for each individual plot for scale).