adsabs/AstroCLIMB huggingface dataset:
Paper: A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z ph > 7
Authors: Chenxiaoji Ling, Bangzheng Sun, Cheng Cheng, Nan Li, Zhiyuan Ma, Haojing Yan
Figure caption: Fitting of COSBO-7's optical-to-mid-IR SED to derive its photometric redshift based on four different SED fitting tools. The data points (filled symbols) and upper limit are from the JWST photometry listed in Table 2, and the corresponding passbands are labeled at the bottom. The cases for the F090W upper limit of 28.43 mag and 26.98 mag are shown in the top four and the bottom four panels, respectively. In the cases of LePhare, EAZY, and X-CIGALE, the superposed spectrum is that of the best-fit template, and the inset shows the probability distribution function (PDF) of redshift (P(z)). In the case of Bagpipes, the spectrum is the 50th percentile posterior spectrum, and the inset shows the distribution of the posterior redshifts. In all cases, the open symbols are the synthesized magnitudes of the superposed spectrum at the corresponding bands. See Section 4.2 for details.
Paper: A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z ph > 7
Authors: Chenxiaoji Ling, Bangzheng Sun, Cheng Cheng, Nan Li, Zhiyuan Ma, Haojing Yan
Figure caption: Images of COSBO-7 and its vicinity, with the coordinates labeled. From left to right, these are in ALMA Band 7 (870 μm) and the JWST NIRCam SW and LW channels, respectively. The white ellipse in the left panel indicates the beam size in 870 μm. The bright 870 μm source has a close, fainter companion in its southeastern direction, and their centers are only 1.″25 apart. The NIRCam images are color composites made of F090W (blue), F115W (green), and F200W (red) in SW and F277W (blue), F356W (green), and F444W (red) in LW, respectively. The positions of the bright 870 μm source and its weak companion are labeled as the black plus signs and crosses in these two images, respectively. Apparently, this is a strong gravitational lensing system: the NIRCam counterpart of the bright 870 μm source is the very red arc around the bright disk galaxy at z = 0.359, which must be an image of a background source produced by this disk galaxy as the lens. The weak 870 μm source is likely the counterimage of the brighter one; however, its NIRCam counterpart is swamped by the lens galaxy.
Paper: A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z ph > 7
Authors: Chenxiaoji Ling, Bangzheng Sun, Cheng Cheng, Nan Li, Zhiyuan Ma, Haojing Yan
Figure caption: Deblending of the Herschel SPIRE images. From top to bottom, the three rows show the case in 250, 350, and 500 μm, respectively. The images are 2′ on a side. The first panel shows the VLA positions of the three blended sources overlaid on the SPIRE image: COSBO-7 (red symbols) and H1 and H2 (green symbols). The second–fourth panels show the original image, the GALFIT-constructed model image by fitting PSFs at the fixed VLA positions, and the residual image after subtracting the model from the original image.
Paper: A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z ph > 7
Authors: Chenxiaoji Ling, Bangzheng Sun, Cheng Cheng, Nan Li, Zhiyuan Ma, Haojing Yan
Figure caption: Comparison of the dust emission as detected by ALMA and the starlight as detected by JWST NIRCam. The background image is a color composite of the NIRCam residual images in F150W (blue), F277W (green), and F444W (red) after the removal of the foreground lens. The left panel shows the contours of the ALMA Band 7 image (cyan), which coincide the contours of the VLA 3 GHz image (white). The middle panel shows the contours of the ALMA Band 4 image (yellow). The peak positions of the ALMA Band 7 and 4 emissions as well as of the VLA 3 GHz emissions are marked as plus signs in the right panel using the same color coding.
Paper: A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z ph > 7
Authors: Chenxiaoji Ling, Bangzheng Sun, Cheng Cheng, Nan Li, Zhiyuan Ma, Haojing Yan
Figure caption: Removal of the foreground lens galaxy using GALFIT in the eight NIRCam and two MIRI bands. For each band, the original image, the best-fit model from GALFIT, and the residual image after the model subtraction are shown from left to right. The MIRI bands only require one (F1800W) or two (F770W) Sérsic profiles, while the NIRCam bands require a four-component model (see Section 3.3 for details).
Paper: A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z ph > 7
Authors: Chenxiaoji Ling, Bangzheng Sun, Cheng Cheng, Nan Li, Zhiyuan Ma, Haojing Yan
Figure caption: Polygon apertures used for photometry in the ALMA images, indicated in red. In Band 7, the main image and its counterimage are separated. In Band 4, the two are not separable, and a larger polygon aperture is adopted.
Paper: Comprehensive Synthesis of Magnetic Tornado: Cospatial Incidence of Chromospheric Swirls and Extreme-ultraviolet Brightening
Authors: Hidetaka Kuniyoshi, Souvik Bose, Takaaki Yokoyama
Figure caption: Panels (a) and (b): the probability distributions of the xy-averaged temperature 〈T〉 and mass density 〈ρ〉 for t and z. Panels (c)–(f): snapshots (t = 1278 s) of magnetic field lines, B  y , S  z , and v  z  on the xz-plane at x = 4.2 Mm in the presence of the magnetic tornado. The black contours in panels (d)–(f) indicate the transition region height where T = 80,000 K.
Paper: Interstellar Neutral Hydrogen in the Heliosphere: New Horizons Observations in the Context of Models
Authors: P. Swaczyna, M. Bzowski, K. Dialynas, L. Dyke, F. Fraternale, A. Galli, J. Heerikhuisen, M. Z. Kornbleuth, D. Koutroumpa, I. Kowalska-Leszczyńska, M. A. Kubiak, A. T. Michael, H.-R. Müller, M. Opher, F. Rahmanifard
Figure caption: Top panel: the trajectory of New Horizons (red line) projected on the ecliptic plane shown on top of the density modulation of ISN hydrogen calculated with the WTPM (Tarnopolski & Bzowski 2009; Sokół et al. 2015). The solid portion represents the almost continuous observations between 22 and 52 au used in our study. The orange and magenta ellipses show the Jupiter and Pluto trajectories, respectively. The black arrow indicates the ISN hydrogen flow direction. The green line represents the line along which the PUIs accumulated for observations at 45 au from the Sun. Bottom panels: column density (left panel) and local density (right panel) of ISN hydrogen in the heliosphere based on the New Horizons/SWAP observations of PUIs. The color of the data points corresponding to each day of SWAP observations represents the cooling index value (see Swaczyna et al. 2020). The averages over 1 au wide bins are shown using points with error bars (gray—excluded from the model fits; black—included in the model fits; see text). The cold model fit from Swaczyna et al. (2020) is shown with dashed gray lines. The new fit using a cold model and a model with a gradient (see text) are shown using purple and orange lines, respectively.
Paper: Interstellar Neutral Hydrogen in the Heliosphere: New Horizons Observations in the Context of Models
Authors: P. Swaczyna, M. Bzowski, K. Dialynas, L. Dyke, F. Fraternale, A. Galli, J. Heerikhuisen, M. Z. Kornbleuth, D. Koutroumpa, I. Kowalska-Leszczyńska, M. A. Kubiak, A. T. Michael, H.-R. Müller, M. Opher, F. Rahmanifard
Figure caption: ISN hydrogen density along New Horizons trajectory for the three models (in columns). The numerical results are presented using the green line. The cold model and the model with a gradient fitting the models over the limited range are shown using purple and orange lines, respectively. The bottom panels magnify the portion within 90 au from the Sun for easier comparison.
Paper: Interstellar Neutral Hydrogen in the Heliosphere: New Horizons Observations in the Context of Models
Authors: P. Swaczyna, M. Bzowski, K. Dialynas, L. Dyke, F. Fraternale, A. Galli, J. Heerikhuisen, M. Z. Kornbleuth, D. Koutroumpa, I. Kowalska-Leszczyńska, M. A. Kubiak, A. T. Michael, H.-R. Müller, M. Opher, F. Rahmanifard
Figure caption: The ISN hydrogen density profiles predicted by the hot models and analytic formulas. The left and right panels show the column and local ISN hydrogen densities, respectively, as a function of distance from the Sun along the New Horizons trajectory. The hot models are scaled by a constant factor to match the data. The hot models do not explain the negative slope.
Paper: Interstellar Neutral Hydrogen in the Heliosphere: New Horizons Observations in the Context of Models
Authors: P. Swaczyna, M. Bzowski, K. Dialynas, L. Dyke, F. Fraternale, A. Galli, J. Heerikhuisen, M. Z. Kornbleuth, D. Koutroumpa, I. Kowalska-Leszczyńska, M. A. Kubiak, A. T. Michael, H.-R. Müller, M. Opher, F. Rahmanifard
Figure caption: ISN hydrogen density profiles (colored lines) from the fit analytic models and scaled numerical models used in this study compared to the observations (dots with error bars). The bottom panel shows the density profiles within the range covered by the New Horizons observations. The fiducial point distance and density are marked with dashed lines (see text).
Paper: A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z ph > 7
Authors: Chenxiaoji Ling, Bangzheng Sun, Cheng Cheng, Nan Li, Zhiyuan Ma, Haojing Yan
Figure caption: Lensing modeling of COSBO-7. The left panel shows the reconstructed image in the source plane. The middle panel overlays the source model, shown as the blue contour, on the same reconstructed image. The green curve represents the caustics of the lensing system. The right panel superposes the modeled lensed images in blue contours on the observed F444W image, and the red curve represents the critical curve of the strong-lensing system. The blue contours in both the middle and right panels correspond to 25% maximum of the F444W observation. In addition, the white symbols (square, cross, and triangle) mark the positions of the three clumps in the F444W data (right panel) and the reconstructed source image (middle panel), respectively. The small blue contour within the critical curve in the right panel is the counterimage of the arc predicted by our lensing model, and the red plus sign indicates the peak of the main image in the ALMA 870 μm data. Note that the effect of PSF smearing is included in the right panel but not in the other two panels.
Paper: A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z ph > 7
Authors: Chenxiaoji Ling, Bangzheng Sun, Cheng Cheng, Nan Li, Zhiyuan Ma, Haojing Yan
Figure caption: Single-temperature MBB fit of the far-IR-to-millimeter SED using three different choices of the emissivity value (β) as noted. The fit is done at the fixed redshift of 7.455 (see Appendix B). The data points in each panel show the measurements in Herschel SPIRE 250, 350, and 500 μm; ALMA 870 μm; MAMBO-2 1.2 mm; and ALMA 2.07 mm. These measurements are the combined values of the two lensed images, whose flux density ratio in ALMA 870 μm is 5.3:1. The red curve is the best-fit MBB model, and the corresponding dust temperature (T mbb) as well as the total far-IR luminosity (L FIR) are labeled. The L FIR value is for the two lensed images combined and is not demagnified.
Paper: A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z ph > 7
Authors: Chenxiaoji Ling, Bangzheng Sun, Cheng Cheng, Nan Li, Zhiyuan Ma, Haojing Yan
Figure caption: ALMA Band 3 spectrum of COSBO-7 that reveals the line of the double-peak feature. If the line is due to the CO (7–6) transition (at the rest frame 806.65 GHz), the corresponding redshift is z = 7.455 and is consistent with the z ph determined in Section 4.2. The gray region represents the frequency ranges not covered by the observations.
Paper: A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z ph > 7
Authors: Chenxiaoji Ling, Bangzheng Sun, Cheng Cheng, Nan Li, Zhiyuan Ma, Haojing Yan
Figure caption: SED fitting results for the foreground lens galaxy at z = 0.36, obtained following the same procedures as in Figure 6.
Paper: A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z ph > 7
Authors: Chenxiaoji Ling, Bangzheng Sun, Cheng Cheng, Nan Li, Zhiyuan Ma, Haojing Yan
Figure caption: Same as Figure 7 but done at z = 4.
Paper: A Strongly Lensed Dusty Starburst of an Intrinsic Disk Morphology at a Photometric Redshift of z ph > 7
Authors: Chenxiaoji Ling, Bangzheng Sun, Cheng Cheng, Nan Li, Zhiyuan Ma, Haojing Yan
Figure caption: Same as Figure 6 but with the limit of z ≤ 6 when running the fitting codes to obtain low-z solutions.
Paper: Comprehensive Synthesis of Magnetic Tornado: Cospatial Incidence of Chromospheric Swirls and Extreme-ultraviolet Brightening
Authors: Hidetaka Kuniyoshi, Souvik Bose, Takaaki Yokoyama
Figure caption: The horizontal slices (z = 7.3 Mm) of temperature T, ∣∇ ×  B ∣/B and vertical velocity v  z  in color, with horizontal magnetic field (B  x , B  y ) or horizontal velocity field (v  x , v  y ) in arrows at t = 1278 s.
Paper: An IXPE-led X-Ray Spectropolarimetric Campaign on the Soft State of Cygnus X-1: X-Ray Polarimetric Evidence for Strong Gravitational Lensing
Authors: James F. Steiner, Edward Nathan, Kun Hu, Henric Krawczynski, Michal Dovčiak, Alexandra Veledina, Fabio Muleri, Jiri Svoboda, Kevin Alabarta, Maxime Parra, Yash Bhargava, Giorgio Matt, Juri Poutanen, Pierre-Olivier Petrucci, Allyn F. Tennant, M. Cristina Baglio, Luca Baldini, Samuel Barnier, Sudip Bhattacharyya, Stefano Bianchi, Maimouna Brigitte, Mauricio Cabezas, Floriane Cangemi, Fiamma Capitanio, Jacob Casey, Nicole Rodriguez Cavero, Simone Castellano, Elisabetta Cavazzuti, Sohee Chun, Eugene Churazov, Enrico Costa, Niccolò Di Lalla, Alessandro Di Marco, Elise Egron, Melissa Ewing, Sergio Fabiani, Javier A. García, David A. Green, Victoria Grinberg, Petr Hadrava, Adam Ingram, Philip Kaaret, Fabian Kislat, Takao Kitaguchi, Vadim Kravtsov, Brankica Kubátová, Fabio La Monaca, Luca Latronico, Vladislav Loktev, Christian Malacaria, Frédéric Marin, Andrea Marinucci, Olga Maryeva, Guglielmo Mastroserio, Tsunefumi Mizuno, Michela Negro, Nicola Omodei, Jakub Podgorný, John Rankin, Ajay Ratheesh, Lauren Rhodes, David M. Russell, Miroslav Šlechta, Paolo Soffitta, Sean Spooner, Valery Suleimanov, Francesco Tombesi, Sergei A. Trushkin, Martin C. Weisskopf, Silvia Zane, Andrzej A. Zdziarski, Sixuan Zhang, Wenda Zhang, Menglei Zhou, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Riccardo Ferrazzoli, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Jeffery J. Kolodziejczak, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Ikuyuki Mitsuishi, Chi-Yung Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Nicholas E. Thomas, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Fei Xie
Figure caption: The best-fitting comprehensive spectral model for epoch 5, showing contributions from the Comptonized disk and reflection components. Each NICER GTI contains 5–30 million counts; the IXPE, NuSTAR, and INTEGRAL spectra contain ∼2–4 million counts apiece. For clarity, the ratios of data to best-fit model are split between the lower two panels. The middle panel shows NuSTAR FMPA (dark gray) and FMPB (light gray); IXPE DU1 (red), DU2 (green), and DU3 (blue); and INTEGRAL IBIS (cyan). The lower panel shows the ratio of the spectra from the different NICER GTIs. The same color scheme is used for the unfolded data sets and model in the upper panel.
Paper: An IXPE-led X-Ray Spectropolarimetric Campaign on the Soft State of Cygnus X-1: X-Ray Polarimetric Evidence for Strong Gravitational Lensing
Authors: James F. Steiner, Edward Nathan, Kun Hu, Henric Krawczynski, Michal Dovčiak, Alexandra Veledina, Fabio Muleri, Jiri Svoboda, Kevin Alabarta, Maxime Parra, Yash Bhargava, Giorgio Matt, Juri Poutanen, Pierre-Olivier Petrucci, Allyn F. Tennant, M. Cristina Baglio, Luca Baldini, Samuel Barnier, Sudip Bhattacharyya, Stefano Bianchi, Maimouna Brigitte, Mauricio Cabezas, Floriane Cangemi, Fiamma Capitanio, Jacob Casey, Nicole Rodriguez Cavero, Simone Castellano, Elisabetta Cavazzuti, Sohee Chun, Eugene Churazov, Enrico Costa, Niccolò Di Lalla, Alessandro Di Marco, Elise Egron, Melissa Ewing, Sergio Fabiani, Javier A. García, David A. Green, Victoria Grinberg, Petr Hadrava, Adam Ingram, Philip Kaaret, Fabian Kislat, Takao Kitaguchi, Vadim Kravtsov, Brankica Kubátová, Fabio La Monaca, Luca Latronico, Vladislav Loktev, Christian Malacaria, Frédéric Marin, Andrea Marinucci, Olga Maryeva, Guglielmo Mastroserio, Tsunefumi Mizuno, Michela Negro, Nicola Omodei, Jakub Podgorný, John Rankin, Ajay Ratheesh, Lauren Rhodes, David M. Russell, Miroslav Šlechta, Paolo Soffitta, Sean Spooner, Valery Suleimanov, Francesco Tombesi, Sergei A. Trushkin, Martin C. Weisskopf, Silvia Zane, Andrzej A. Zdziarski, Sixuan Zhang, Wenda Zhang, Menglei Zhou, Iván Agudo, Lucio A. Antonelli, Matteo Bachetti, Wayne H. Baumgartner, Ronaldo Bellazzini, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Niccolò Bucciantini, Chien-Ting Chen, Stefano Ciprini, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Riccardo Ferrazzoli, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Svetlana G. Jorstad, Vladimir Karas, Jeffery J. Kolodziejczak, Ioannis Liodakis, Simone Maldera, Alberto Manfreda, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Ikuyuki Mitsuishi, Chi-Yung Ng, Stephen L. O'Dell, Chiara Oppedisano, Alessandro Papitto, George G. Pavlov, Abel L. Peirson, Matteo Perri, Melissa Pesce-Rollins, Maura Pilia, Andrea Possenti, Simonetta Puccetti, Brian D. Ramsey, Oliver J. Roberts, Roger W. Romani, Carmelo Sgrò, Patrick Slane, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Nicholas E. Thomas, Alessio Trois, Sergey S. Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Fei Xie
Figure caption: (Left) IXPE 2–8 keV PD and PA for each soft state (S1–S5; red) in comparison to previous hard-state observations (H1–H2; blue). (Right) Energy-dependent polarization of the soft-state data composite. Contours show 68% confidence intervals.
Paper: Influence of Orbit and Mass Constraints on Reflected Light Characterization of Directly Imaged Rocky Exoplanets
Authors: Arnaud Salvador, Tyler D. Robinson, Jonathan J. Fortney, Mark S. Marley
Figure caption: Fiducial-model-generated (synthetic) reflected light spectrum of an Earth-like planet at quadrature (i.e., at a planetary phase angle α = 90°; see Table 1 for fiducial input values). The colored areas indicate the spectral impact of the gas species by showing the difference between the baseline spectrum (black line) and the spectrum obtained if they were absent from the atmosphere. The top of the figure shows the two wavelength ranges considered and their spectral resolving power: red bandpass (λ = [0.87, 1.05] μm, ﹩\mathrm{res}=140;﹩ see Appendix B) and visible (λ = [0.45, 1] μm, ﹩\mathrm{res}=140﹩) + NIR (λ = [1, 1.80] μm, ﹩\mathrm{res}=70﹩). The error bars show the nonrandomized, wavelength-independent noise corresponding to specific S/N at the reference wavelengths λ = 0.45 μm for the vNIR range, and λ = 0.88 μm for the red bandpass.
Paper: Influence of Orbit and Mass Constraints on Reflected Light Characterization of Directly Imaged Rocky Exoplanets
Authors: Arnaud Salvador, Tyler D. Robinson, Jonathan J. Fortney, Mark S. Marley
Figure caption: Planet radius (R p), water vapor mixing ratio (﹩{f}_{{{\rm{H}}}_{2}{\rm{O}}}﹩), surface pressure (p surf), and cloud fraction (f c) posterior distributions for the different levels of color-coded prior knowledge, at different S/N values (10, 15, and 20) in the vNIR. The “mass constrained” case (i.e., where only the mass is constrained; in red) is shown for S/N = 20 only. Earth-like input values are depicted with dashed horizontal lines. The density has been normalized across all kernel density plots such that each have the same area. Apart from the planet radius inference, which is significantly improved by prior knowledge of the orbit, increasing the S/N is more beneficial for atmospheric characterization; as illustrated by the shrinking tails of the posterior distributions and their narrowing toward the fiducial values with increasing S/N (see also Tables 2, 3, and 4 for the retrieval results).
Paper: Influence of Orbit and Mass Constraints on Reflected Light Characterization of Directly Imaged Rocky Exoplanets
Authors: Arnaud Salvador, Tyler D. Robinson, Jonathan J. Fortney, Mark S. Marley
Figure caption: Mass–radius diagram (center) and marginal univariate posterior distributions (top and right side) for the different scenarios of prior knowledge (same as Figure 3) considering a narrower spectral bandpass centered on “red” wavelengths (λ = [0.87, 1.05] μm, ﹩\mathrm{res}=140;﹩ see Figure 1) and S/N = 10. The contours of the 2D posterior distributions denote the 1σ, 2σ, and 3σ levels, encompassing 68%, 95%, and 99.7% of the observed values, respectively. Earth-like input values are depicted with dashed horizontal and vertical lines. The small images of Earth and Neptune indicate their positions in the diagram. For comparison, mass–radius relationships representative of different bulk compositions and interior structures are shown (pure H2O assuming 1 mbar surface pressure level at 300 K, Earth-like rocky: 32.5% Fe + 67.5% MgSiO3, and pure iron; from Zeng et al. 2019). Retrieval results are given in Table 5.
Paper: Influence of Orbit and Mass Constraints on Reflected Light Characterization of Directly Imaged Rocky Exoplanets
Authors: Arnaud Salvador, Tyler D. Robinson, Jonathan J. Fortney, Mark S. Marley
Figure caption: Mass–radius diagram (center) and marginal univariate posterior distributions (top and right side) for the different scenarios of prior knowledge and for the vNIR and S/N = 20 case. The contours of the 2D posterior distributions denote the 1σ, 2σ, and 3σ levels, encompassing 68%, 95%, and 99.7% of the observed values, respectively. Earth-like input values are depicted with dashed horizontal and vertical lines. The small images of Earth and Neptune indicate their positions in the diagram. For comparison, mass–radius relationships representative of different bulk compositions and interior structures are shown (pure H2O assuming 1 mbar surface pressure level at 300 K, Earth-like rocky: 32.5% Fe + 67.5% MgSiO3, and pure iron; from Zeng et al. 2019 (https://lweb.cfa.harvard.edu/~lzeng/planetmodels.html#mrrelation). Retrieval results are given in Table 2.