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Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: The same as Figure 6 but for β 1200.
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: The same as Figure 6 but for r 50.
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: The same as Figure 6 but for rest-frame Lyα EW.
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption:                       ﹩{F}_{{\rm{H}}\beta }^{\mathrm{mod}}/{F}_{\lambda 900}^{\mathrm{mod}}﹩ ratio predicted by instantaneous (left) and continuous (right) star formation histories from STARBURST99 (top) and BPASS (bottom) models for f esc LyC = 0 as a function of Hβ EW for a range of metallicities. Metallicity increases with increasing dash length over the interval Z = [0.001, 0.04], as shown by the arrow in the top-right panel. The change in F Hβ /F  λLyC with metallicity is due to the softening of stellar SEDs with increasing metallicity. The solid black line (top-left panel) indicates the Izotov et al. (2016b) relation. Symbols represent the inferred F Hβ /F  λLyC for f esc LyC = 0 for LCEs (circles) and nondetections (open triangles) implied by the measured F  λLyC, Hβ, ﹩12+{\mathrm{log}}_{10}\left(\tfrac{{\rm{O}}}{{\rm{H}}}\right)﹩, and f esc LyC for each set of models. Median uncertainties are shown in the bottom-left panel, increased by a factor of three for visualization.
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: Top: f esc LyC derived from fitting the COS UV spectrum compared to f esc LyC derived from Hβ using the STARBURST99 continuous star formation models. The shaded region indicates the rms log difference of the two f esc LyC values. Bottom: comparison of f esc LyC with F  λLyC/F  λ1100 for the combined sample of LzLCS and published LCEs. Open symbols represent f esc LyC derived from Hβ using the STARBURST99 continuous star formation models, while filled symbols represent f esc LyC derived from fits to the UV continuum. In both figures, symbol size corresponds to the LyC detection significance, and gray arrows indicate upper limits on f esc LyC. Error bars in the bottom right indicate the median uncertainty for objects with detected LyC (P(> N∣B) < 0.02275). The dashed line is 1:1 agreement.
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: Difference between f esc LyC calculated from BPASS instantaneous (open diamonds) and continuous (light gray squares) star formation or from STARBURST99 continuous star formation (dark gray circles) models and f esc LyC calculated using STARBURST99 instantaneous star formation models as compared to Hβ EW for f esc LyC derived from Hβ for the combined LzLCS and published samples. Symbol size corresponds to the LyC detection significance. Characteristic uncertainties are shown on the right. Increasing scatter with decreasing Hβ EW indicates the increasing effect of assumptions about star formation history on the inferred f esc LyC.
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: The same as Figure 6 but for f esc Lyα .
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: The same as Figure 6 but for the velocity separation of the blue and red peaks of the Lyα profile. No error bars are shown as insufficient uncertainties are reported in the literature.
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: The same as Figure 6 but for M ⋆.
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: The same as Figure 6 but for ΣSFR derived from Hβ.
Paper: The Low-redshift Lyman Continuum Survey. I. New, Diverse Local Lyman Continuum Emitters
Authors: Sophia R. Flury, Anne E. Jaskot, Harry C. Ferguson, Gábor Worseck, Kirill Makan, John Chisholm, Alberto Saldana-Lopez, Daniel Schaerer, Stephan McCandliss, Bingjie Wang, N. M. Ford, Timothy Heckman, Zhiyuan Ji, Mauro Giavalisco, Ricardo Amorin, Hakim Atek, Jeremy Blaizot, Sanchayeeta Borthakur, Cody Carr, Marco Castellano, Stefano Cristiani, Stephane De Barros, Mark Dickinson, Steven L. Finkelstein, Brian Fleming, Fabio Fontanot, Thibault Garel, Andrea Grazian, Matthew Hayes, Alaina Henry, Valentin Mauerhofer, Genoveva Micheva, M. S. Oey, Goran Ostlin, Casey Papovich, Laura Pentericci, Swara Ravindranath, Joakim Rosdahl, Michael Rutkowski, Paola Santini, Claudia Scarlata, Harry Teplitz, Trinh Thuan, Maxime Trebitsch, Eros Vanzella, Anne Verhamme, Xinfeng Xu
Figure caption: The same as Figure 6 but for M 1500. The dashed line indicates the characteristic ﹩{M}_{1600}^{* }=-20.87﹩ at z = 7 (Bouwens et al. 2015).
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Simulated spectra (left) and thermal structure (right) for HD 209458b. The blue data points are our original Iraclis reduced spectrum. The green points are the Line et al. (2016) data. The red points are the Iraclis observations offset by 160 ppm to match the Line et al. (2016) absolute depth. The same color scheme is applied for our retrievals on those different data sets. We also added forward-model spectra computed from two-stream self-consistent approximations in dashed lines: solar in purple, and metallicity 0.2 and C/O = 1 in orange.
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Recovered e− (left) and H2O (right) maps of our full retrieval performed on intentionally biased Spitzer data. Top: The noise of the Spitzer points has been doubled. Bottom: The eclipsed depth of the Spitzer points is offset by +100 ppm. While individual planet results can vary, the overall trends obtained from the unbiased Spitzer retrievals are conserved.
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Example spatial scan from the second eclipse observation of WASP-77 A b. The contributions from WASP-77 A and WASP-77 B can clearly be seen to overlap.
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: List of the free parameters and their uniform priors in the retrievals.
Paper: “Winged” Radio Sources from the LOFAR Two-meter Sky Survey First Data Release (LoTSS DR1)
Authors: Soumen Bera, Tapan K. Sasmal, Dusmanta Patra, Soumen Mondal
Figure caption: A comparison between NVSS, TGSS, VLA FIRST, and LOFAR images of the XRG J1243+5212. The first two images (from left) are from NVSS and TGSS ADR1 data, respectively. Unresolved structures are seen in both images due to the low resolution of NVSS and TGSS. The third image is the FIRST image, which shows an extension of the primary lobe in the northwest; no other extended emissions have been observed. Finally, the fourth image is from LoTSS DR1. This LOFAR image shows a clear picture of the X-shaped morphology.
Paper: “Winged” Radio Sources from the LOFAR Two-meter Sky Survey First Data Release (LoTSS DR1)
Authors: Soumen Bera, Tapan K. Sasmal, Dusmanta Patra, Soumen Mondal
Figure caption: LOFAR image of each X-shaped radio source (contours) overlaid on the DSS2 red image (gray scale). The relative radio contours are drawn from at least the 3σ level with an increment of ﹩\sqrt{2}﹩. Here, we use LOFAR 6″ full-resolution radio images for better resolved structure.
Paper: “Winged” Radio Sources from the LOFAR Two-meter Sky Survey First Data Release (LoTSS DR1)
Authors: Soumen Bera, Tapan K. Sasmal, Dusmanta Patra, Soumen Mondal
Figure caption: LOFAR image of each Z-shaped radio source (contours) overlaid on the DSS2 red image (gray scale). The relative radio contours are drawn from at least the 3σ level with an increment of ﹩\sqrt{2}﹩. Here, we use LOFAR 6″ full-resolution radio images for better resolved structure.
Paper: “Winged” Radio Sources from the LOFAR Two-meter Sky Survey First Data Release (LoTSS DR1)
Authors: Soumen Bera, Tapan K. Sasmal, Dusmanta Patra, Soumen Mondal
Figure caption: Color stamp images of the identified ZRG candidates.
Paper: “Winged” Radio Sources from the LOFAR Two-meter Sky Survey First Data Release (LoTSS DR1)
Authors: Soumen Bera, Tapan K. Sasmal, Dusmanta Patra, Soumen Mondal
Figure caption: Color stamp images of the identified XRG candidates.
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Retrieved abundances of e− vs. H2O at the dayside in our sample of 25 hot Jupiters recovered in the HST+Spitzer full runs. The colors on the data points indicate the retrieved atmospheric temperatures weighted by the contribution functions with the legend in the color bar. The shaded green region indicates the predicted abundances from equilibrium chemistry at solar metallicity (M = 1) and C/O (C/O = 0.55) between 1 bar and 0.01 bar, which is around the region probed by the observations. In orange, the metallicity is increased to 100 times solar. In red, the metallicity is decreased to 0.1 times solar. In blue, the metallicity is solar, and the C/O is increased to 1. The planets separate into three regimes: A solar hot-Jupiter regime where water vapor is detected in moderately hot atmospheres associated with a decreasing thermal profile (dashed green), an ultra-hot-Jupiter regime where thermal inversions and H− emission are detected in very hot atmospheres (dashed orange), and a high-C/O hot-Jupiter regime where temperatures remain moderate but where water is not detected (dashed blue).
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Correlations at the dayside between the H2O (top) and e− (bottom) abundances and the mean retrieved temperature weighted by the contribution function. The colors indicate the retrieved thermal gradient, defined as the temperature differences between the upper and lower quantiles of the contribution function. The shaded green region is the predicted abundances from equilibrium chemistry at solar metallicity and C/O between 1 bar and 0.01 bar. In orange, the metallicity is increased to 100 times solar. In red, the metallicity is decreased to 0.1 times solar. In blue, the metallicity is solar and the C/O is increased to 1. Note that in the e− plot (bottom), the solar and C/O = 1 cases overlap.
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Correlations between the retrieved abundances of optical absorbers (TiO, VO, FeH, and H−) and the thermal gradient in the atmosphere. The optical absorber abundances are estimated using the weighted average of the individually retrieved abundances for the detected molecules. If no optical absorber is detected, only an upper limit is available. The thermal gradient is the difference between atmospheric temperatures at 5% and 95% of the atmospheric contribution function. Colors on the data points represent averaged retrieved temperatures. Overall, planets with inverted thermal profiles have temperatures above 2000 K and possess optical absorbers (shaded orange region). Planets without thermal inversions have temperatures below 2500 K and do not possess optical absorbers (shaded green region).
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Averaged refractory element (TiO, VO, and FeH) abundances recovered in the HST+Spitzer full runs, weighted by their standard deviation, and plotted against the retrieved atmospheric temperature on the dayside. Green area: predictions from a solar composition and equilibrium chemistry between 1 bar and 0.01 bar. Orange area: the metallicity is assumed to be 100 times solar. Red area: the metallicity is assumed to be 0.1 times solar. Blue area: the metallicity is solar and C/O is assumed to equal 1.
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Best-fit spectra of the 25 planets considered in this study for the HST+Spitzer observations in eclipse. Individual analyses and additional retrievals, including a simpler blackbody fit, can be found in Appendix D. The planets are ordered in increasing atmospheric temperatures, which are traced by the colors (from blue to red). The retrieved atmospheric temperature is obtained by weighting the retrieved thermal profile by the contribution function. Unlabeled x-axes range from 1.1 to 2 μm.
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Day–terminator thermal gradient as a function of the e− abundance recovered using the free retrievals. Only planets that have both eclipse and transit spectra and for which the terminator temperature is constrained are shown in this plot.
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Best-fit spectra of the full runs for the planets observed in transit. The planets are ordered in increasing atmospheric temperatures, which are traced by the colors (from blue to red). Unlabeled x-axes range from 1.1 to 2 μm.
Paper: Five Key Exoplanet Questions Answered via the Analysis of 25 Hot-Jupiter Atmospheres in Eclipse
Authors: Q. Changeat, B. Edwards, A. F. Al-Refaie, A. Tsiaras, J. W. Skinner, J. Y. K. Cho, K. H. Yip, L. Anisman, M. Ikoma, M. F. Bieger, O. Venot, S. Shibata, I. P. Waldmann, G. Tinetti
Figure caption: Bayes factor between the full HST+Spitzer retrieval and the blackbody fit for the eclipses. The figure shows that a blackbody is rejected for all planets in the combined data set, except HAT-P-2 b.