adsabs/AstroCLIMB huggingface dataset:
Paper: Detection of Metal Enrichment by SN 2011jm in NGC 4809
Authors: Yulong Gao, Qiusheng Gu, Ping Zhou, Yong Shi, Xiangdong Li
Figure caption: Gas-phase oxygen abundance (left) and nitrogen-to-oxygen ratio (N/O, right) maps around the SN 2011jm.
Paper: Diffuse Light in Milky Way–like Haloes
Authors: Emanuele Contini, San Han, Seyoung Jeon, Jinsu Rhee, Sukyoung K. Yi
Figure caption: Percentage of DL as a function of the stellar mass of the galaxies that contribute to it (top panel), for haloes in four different ranges of mass as indicated in the legend, and normalized to the halo mass in each range (bottom panel). The peak of the distributions moves toward the left (lower stellar mass) as the range in halo mass decreases, which means that the galaxies contributing to the DL are smaller and smaller as the halo mass decreases. If we focus on the contribution given by relative intermediate/massive galaxies (﹩9.5\lt \mathrm{log}{M}_{* }\lt 11﹩), we find that their contribution to the DL increases rapidly with increasing halo mass range, from around 16% in the lowest halo masses to 62% in the largest ones. This result is in line with what we found in Contini et al. (2014), i.e., that intermediate/massive galaxies contribute the most to the DL. However, when the halo mass decreases substantially, most of the contribution is given by galaxies with stellar mass lower or much lower than ﹩\mathrm{log}{M}_{* }\sim 9.5﹩. Once we scale the x-axis to the halo mass of host galaxies (bottom panel), the four distributions look similar and the peak lies between ﹩0.001\lt \mathrm{log}({M}_{\mathrm{gal}}/{M}_{\mathrm{halo}})\lt 0.003﹩.
Paper: Diffuse Light in Milky Way–like Haloes
Authors: Emanuele Contini, San Han, Seyoung Jeon, Jinsu Rhee, Sukyoung K. Yi
Figure caption: Full comparison between our results in Contini et al. (2023, 2024) and this work. In the top panel, we plot the DL fraction as a function of halo mass in the range ﹩11.5\lt \mathrm{log}{M}_{\mathrm{halo}}\lt 15.0﹩ by connecting the relation found in this work (black lines) and that in Contini et al. (2023; red lines). Similarly, in the bottom panel, we put together the relations between the DL/halo mass ratio and halo mass found here and in Contini et al. (2024). The DL fraction increases from very small scales to large clusters, while the DL/halo mass ratio, which we consider as the efficiency of haloes to form DL, increases from very small scales up to the peak in ﹩\mathrm{log}{M}_{\mathrm{halo}}\sim 13﹩, to decrease again toward large clusters. However, two important caveats must be noted, and the details are specified in the main text.
Paper: Distinguishing Oceans of Water from Magma on Mini-Neptune K2-18b
Authors: Oliver Shorttle, Sean Jordan, Harrison Nicholls, Tim Lichtenberg, Dan J. Bower
Figure caption: An outline of the methods followed to generate model atmospheric compositions and spectra of K2-18b as a magma ocean.
Paper: Distinguishing Oceans of Water from Magma on Mini-Neptune K2-18b
Authors: Oliver Shorttle, Sean Jordan, Harrison Nicholls, Tim Lichtenberg, Dan J. Bower
Figure caption: Best-fitting model transmission spectra of the atmospheres in the magma ocean scenario. The transmission spectra are generated, using petitRADTRANS, from the output photochemical-kinetics models when taking the atmosphere–magma ocean system output as a lower boundary condition (step 4, Figure 1). Data points from the observed transmission spectrum of K2-18b (Madhusudhan et al. 2023b) are plotted with their associated error estimates. The best-fitting model in the magma ocean scenario is shown in black and all models that agree with the observational data within 3σ are shown in blue.
Paper: Distinguishing Oceans of Water from Magma on Mini-Neptune K2-18b
Authors: Oliver Shorttle, Sean Jordan, Harrison Nicholls, Tim Lichtenberg, Dan J. Bower
Figure caption: The fraction of nitrogen in the planet’s atmosphere compared to the planet’s total inventory, as a function of magma ocean oxygen fugacity. As oxygen fugacity is decreased, nitrogen’s increased solubility depletes the atmosphere by orders of magnitude. Each colored circle represents a model run for a given set of parameters (Table 1); symbols have been colored by total atmospheric pressure (bar), and have been randomly displaced in the x-direction for ease of visualization. White squares are averages for runs of a given mantle mass (expressed as fractional mass of the planet) at a particular oxygen fugacity, and illustrate the important role mantle (or equivalently magma ocean) mass has in enabling significant N depletion.
Paper: Distinguishing Oceans of Water from Magma on Mini-Neptune K2-18b
Authors: Oliver Shorttle, Sean Jordan, Harrison Nicholls, Tim Lichtenberg, Dan J. Bower
Figure caption: Total atmospheric surface pressure (bar) and volume mixing ratio of NH3, and CO2 output from the atmosphere–magma ocean system over the parameter space that we have sampled, outlined in Table 1. This corresponds to the output of step 2 in the schematic presented in Figure 1. Points are color coded by the log of the planetary hydrogen budget, in units of parts per million of the planetary mass. Histograms of the distribution of NH3 mixing ratios (top left), CO2 mixing ratios (top right), and total surface pressures (lower right) from across the model runs are shown alongside.
Paper: Distinguishing Oceans of Water from Magma on Mini-Neptune K2-18b
Authors: Oliver Shorttle, Sean Jordan, Harrison Nicholls, Tim Lichtenberg, Dan J. Bower
Figure caption: Transmission spectra within 4.0–5.2 μm for four models demonstrating a range of CO2:CO ratios from the magma ocean scenario. Observational data from the observed transmission spectrum of K2-18b are shown with associated errors.
Paper: Diffuse Light in Milky Way–like Haloes
Authors: Emanuele Contini, San Han, Seyoung Jeon, Jinsu Rhee, Sukyoung K. Yi
Figure caption: Fraction of DL as a function of halo mass for haloes in different ranges of concentrations as shown in the legend, while the black solid and dashed lines indicate the mean and ±σ scatter of the distribution. Our results are compared with the predictions from Proctor et al. (2024; Eagle Project), Ahvazi et al. (2023; TNG50), and several observational measurements (Harmsen et al. 2017; Deason et al. 2019; Kluge et al. 2021; Ragusa et al. 2023). The DL fraction weakly increases toward larger haloes from about 0.1 in the low-mass end to 0.2 in the high-mass end, but the distribution also shows a ∼±0.1 scatter along the whole mass range. Considering the typical fractions found in groups and clusters (Contini et al. 2023, 2024), overall the DL fraction decreases quite importantly toward low-mass haloes, potentially becoming negligible on scales below those investigated here. It is important to highlight the role played by the concentration even in these scales: more concentrated, and so relaxed haloes, tend to host a higher fraction of DL, as shown by the red (average DL fraction in the highest bin in concentration) and blue (average DL fraction in the lowest bin in concentration) lines, respectively.
Paper: Diffuse Light in Milky Way–like Haloes
Authors: Emanuele Contini, San Han, Seyoung Jeon, Jinsu Rhee, Sukyoung K. Yi
Figure caption: Top panel: fraction of DL coming from the stellar stripping (black solid and dashed lines), and from the merger (purple solid and dashed lines) channels. In both cases, the solid and dashed lines indicate the mean and ±σ scatter of the distributions, while the circles with different colors represent haloes in different ranges of concentrations in the case of the stripping channel, as shown in the legend. Similarly to what was found in Contini et al. (2024) for groups and clusters, stellar stripping is responsible (even more in more concentrated haloes) for the bulk of the DL (95% on average), independently of the halo mass, while mergers play a marginal role (5% on average). Bottom panel: the same as in the top panel, for the case of the DL coming from preprocessing/accretion. Differently from their much larger counterparts, these haloes accrete, on average, 8% of the 100% of DL given by mergers and stripping, a number that highlights the fact that these haloes are still in the process of their formation and did not accrete much material from outside, having had, so far, a few minor or no relevant major mergers.
Paper: Diffuse Light in Milky Way–like Haloes
Authors: Emanuele Contini, San Han, Seyoung Jeon, Jinsu Rhee, Sukyoung K. Yi
Figure caption: Ratio between the amount of DL and the halo mass of its host, as a function of the latter. Circles with different colors represent haloes in different ranges of concentration, as indicated in the legend, while the black solid and dashed lines represent the mean and ±σ scatter of the distribution. This ratio, which can be considered as a sort of efficiency of haloes in producing DL, is an increasing function of halo mass, from around 0.3% (lowest halo mass) to 0.8% (highest halo mass). Putting together this result and its equivalent found in Contini et al. (2024) for groups and clusters, where the ratio is a weak decreasing function of halo mass, the net conclusion is that haloes with ﹩\mathrm{log}{M}_{\mathrm{halo}}\sim 13﹩ are the most efficient ones in producing DL. Once more, it is important to underline the role of the concentration: independently of the halo mass, more concentrated haloes are more efficient.
Paper: Diffuse Light in Milky Way–like Haloes
Authors: Emanuele Contini, San Han, Seyoung Jeon, Jinsu Rhee, Sukyoung K. Yi
Figure caption: Distribution of the DL formation time in our sample of haloes indicated by the black histogram, and its fit indicated by the red line. The formation time has been defined as the redshift when 50% of the DL at z = 0 was already formed. Exactly 50% of the haloes have formation times z form ≤ 0.5, and around a third of them (32%) have z form ≤ 0.3. These numbers, along with a simple comparison with the distribution found in Figure 7 of Contini et al. (2024) for groups and clusters, point out that these haloes are still in the process of their formation, and so is the DL they host.
Paper: Observation of GRB 221009A Early Afterglow in X-Ray/Gamma-Ray Energy Bands
Authors: Chao Zheng, Yan-Qiu Zhang, Shao-Lin Xiong, Cheng-Kui Li, He Gao, Wang-Chen Xue, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Wen-Xi Peng, Zheng-Hua An, Ce Cai, Ming-Yu Ge, Dong-Ya Guo, Yue Huang, Bing Li, Ti-Pei Li, Xiao-Bo Li, Xin-Qiao Li, Xu-Fang Li, Jin-Yuan Liao, Cong-Zhan Liu, Fang-Jun Lu, Xiang Ma, Rui Qiao, Li-Ming Song, Jin Wang, Ping Wang, Xi-Lu Wang, Yue Wang, Xiang-Yang Wen, Shuo Xiao, Yan-Bing Xu, Yu-Peng Xu, Zhi-Guo Yao, Qi-Bing Yi, Shu-Xu Yi, Yuan You, Fan Zhang, Jin-Peng Zhang, Peng Zhang, Shu Zhang, Shuang-Nan Zhang, Yan-Ting Zhang, Zhen Zhang, Xiao-Yun Zhao, Yi Zhao, Shi-Jie Zheng
Figure caption: Top: light-curve decay slopes before and after the jet break in different energy bands, with error bars indicating 1σ uncertainty. Bottom: the break time of early afterglow in different energy bands, with error bars indicating 1σ uncertainty. The results in the keV energy band are from joint analysis of GECAM-C and Fermi/GBM. Our fitting results of the jet break in the TeV energy band is consistent with LHAASO team (LHAASO-Collaboration et al. 2023) within 3σ uncertainty. Notably, the break time seems to be constant from keV to TeV within the error bar.
Paper: Observation of GRB 221009A Early Afterglow in X-Ray/Gamma-Ray Energy Bands
Authors: Chao Zheng, Yan-Qiu Zhang, Shao-Lin Xiong, Cheng-Kui Li, He Gao, Wang-Chen Xue, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Wen-Xi Peng, Zheng-Hua An, Ce Cai, Ming-Yu Ge, Dong-Ya Guo, Yue Huang, Bing Li, Ti-Pei Li, Xiao-Bo Li, Xin-Qiao Li, Xu-Fang Li, Jin-Yuan Liao, Cong-Zhan Liu, Fang-Jun Lu, Xiang Ma, Rui Qiao, Li-Ming Song, Jin Wang, Ping Wang, Xi-Lu Wang, Yue Wang, Xiang-Yang Wen, Shuo Xiao, Yan-Bing Xu, Yu-Peng Xu, Zhi-Guo Yao, Qi-Bing Yi, Shu-Xu Yi, Yuan You, Fan Zhang, Jin-Peng Zhang, Peng Zhang, Shu Zhang, Shuang-Nan Zhang, Yan-Ting Zhang, Zhen Zhang, Xiao-Yun Zhao, Yi Zhao, Shi-Jie Zheng
Figure caption: The early afterglow flux evolution from T AG+435 s to T AG+1635 s are given by Fermi/GBM and GECAM-C in five energy bands, namely 20–50 keV, 50–100 keV, 100–150 keV, 150–200 keV, and 200–300 keV from panels (a) to (e). The gray shaded area represents the fitting range. The orange lines show the posterior distribution of BPL, and the gray vertical lines show the posterior distribution of break time. The red dotted lines show the flux decay with the pre-break slope.
Paper: Observation of GRB 221009A Early Afterglow in X-Ray/Gamma-Ray Energy Bands
Authors: Chao Zheng, Yan-Qiu Zhang, Shao-Lin Xiong, Cheng-Kui Li, He Gao, Wang-Chen Xue, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Wen-Xi Peng, Zheng-Hua An, Ce Cai, Ming-Yu Ge, Dong-Ya Guo, Yue Huang, Bing Li, Ti-Pei Li, Xiao-Bo Li, Xin-Qiao Li, Xu-Fang Li, Jin-Yuan Liao, Cong-Zhan Liu, Fang-Jun Lu, Xiang Ma, Rui Qiao, Li-Ming Song, Jin Wang, Ping Wang, Xi-Lu Wang, Yue Wang, Xiang-Yang Wen, Shuo Xiao, Yan-Bing Xu, Yu-Peng Xu, Zhi-Guo Yao, Qi-Bing Yi, Shu-Xu Yi, Yuan You, Fan Zhang, Jin-Peng Zhang, Peng Zhang, Shu Zhang, Shuang-Nan Zhang, Yan-Ting Zhang, Zhen Zhang, Xiao-Yun Zhao, Yi Zhao, Shi-Jie Zheng
Figure caption: (a) The count rate spectra in 20–20,000 keV energy band from T 0+700 s to T 0+900 s. (b) The spectral energy distribution (vF v ) of CPL+PL model. (c)–(f) The residual distribution of CPL+PL, PL, CPL, and Band model.
Paper: Observation of GRB 221009A Early Afterglow in X-Ray/Gamma-Ray Energy Bands
Authors: Chao Zheng, Yan-Qiu Zhang, Shao-Lin Xiong, Cheng-Kui Li, He Gao, Wang-Chen Xue, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Wen-Xi Peng, Zheng-Hua An, Ce Cai, Ming-Yu Ge, Dong-Ya Guo, Yue Huang, Bing Li, Ti-Pei Li, Xiao-Bo Li, Xin-Qiao Li, Xu-Fang Li, Jin-Yuan Liao, Cong-Zhan Liu, Fang-Jun Lu, Xiang Ma, Rui Qiao, Li-Ming Song, Jin Wang, Ping Wang, Xi-Lu Wang, Yue Wang, Xiang-Yang Wen, Shuo Xiao, Yan-Bing Xu, Yu-Peng Xu, Zhi-Guo Yao, Qi-Bing Yi, Shu-Xu Yi, Yuan You, Fan Zhang, Jin-Peng Zhang, Peng Zhang, Shu Zhang, Shuang-Nan Zhang, Yan-Ting Zhang, Zhen Zhang, Xiao-Yun Zhao, Yi Zhao, Shi-Jie Zheng
Figure caption: The PL photon indices of the early afterglow from T 0+660 s to T 0+1870 s are derived from Fermi/GBM N8 and GECAM-C GRD05 in 20–300 keV energy range. It shows that the photon index first experienced hardening before the break and then softening after the break.
Paper: Observation of GRB 221009A Early Afterglow in X-Ray/Gamma-Ray Energy Bands
Authors: Chao Zheng, Yan-Qiu Zhang, Shao-Lin Xiong, Cheng-Kui Li, He Gao, Wang-Chen Xue, Jia-Cong Liu, Chen-Wei Wang, Wen-Jun Tan, Wen-Xi Peng, Zheng-Hua An, Ce Cai, Ming-Yu Ge, Dong-Ya Guo, Yue Huang, Bing Li, Ti-Pei Li, Xiao-Bo Li, Xin-Qiao Li, Xu-Fang Li, Jin-Yuan Liao, Cong-Zhan Liu, Fang-Jun Lu, Xiang Ma, Rui Qiao, Li-Ming Song, Jin Wang, Ping Wang, Xi-Lu Wang, Yue Wang, Xiang-Yang Wen, Shuo Xiao, Yan-Bing Xu, Yu-Peng Xu, Zhi-Guo Yao, Qi-Bing Yi, Shu-Xu Yi, Yuan You, Fan Zhang, Jin-Peng Zhang, Peng Zhang, Shu Zhang, Shuang-Nan Zhang, Yan-Ting Zhang, Zhen Zhang, Xiao-Yun Zhao, Yi Zhao, Shi-Jie Zheng
Figure caption: Left: the early afterglow flux light curve (50–300 keV) jointly observed by GECAM-C and Fermi/GBM. The gray shaded area represents the fitting range. The orange lines show the posterior distribution of BPL model, and the gray vertical lines show the posterior distribution of break time. The red dashed line shows the flux decay with the pre-break slope. Right: the corner plot represents the BPL fitting result of the flux light curve in the left panel.
Paper: Discovery of a Collimated Jet from the Low-luminosity Protostar IRAS 16253−2429 in a Quiescent Accretion Phase with the JWST
Authors: Mayank Narang, P. Manoj, Himanshu Tyagi, Dan M. Watson, S. Thomas Megeath, Samuel Federman, Adam E. Rubinstein, Robert Gutermuth, Alessio Caratti o Garatti, Henrik Beuther, Tyler L. Bourke, Ewine F. Van Dishoeck, Neal J. Evans, Guillem Anglada, Mayra Osorio, Thomas Stanke, James Muzerolle, Leslie W. Looney, Yao-Lun Yang, Pamela Klaassen, Nicole Karnath, Prabhani Atnagulov, Nashanty Brunken, William J. Fischer, Elise Furlan, Joel Green, Nolan Habel, Lee Hartmann, Hendrik Linz, Pooneh Nazari, Riwaj Pokhrel, Rohan Rahatgaonkar, Will R. M. Rocha, Patrick Sheehan, Katerina Slavicinska, Amelia M. Stutz, John J. Tobin, Lukasz Tychoniec, Scott Wolk
Figure caption: (a) The horizontal slices in green overlaid on top of the jet traced in [Fe II] at 5.34 μm mark slices that are 3 pixels wide along the jet direction. The jet width is computed from each of these green slices (see Section 3.2). The white circle represents the protostellar position. (b) The width (FWHM) of the jet as a function of distance from the central protostar. The negative distance corresponds to the northern jet, and the positive distance corresponds to the southern counterjet. (c) The deconvolved width (FWHM) of the jet as a function of distance from the central protostar. The fit to the jet width as a function of distance is shown as the red solid line. The green triangles in sub-figures (b) and (c) show the upper limits to the width at those points.
Paper: Discovery of a Collimated Jet from the Low-luminosity Protostar IRAS 16253−2429 in a Quiescent Accretion Phase with the JWST
Authors: Mayank Narang, P. Manoj, Himanshu Tyagi, Dan M. Watson, S. Thomas Megeath, Samuel Federman, Adam E. Rubinstein, Robert Gutermuth, Alessio Caratti o Garatti, Henrik Beuther, Tyler L. Bourke, Ewine F. Van Dishoeck, Neal J. Evans, Guillem Anglada, Mayra Osorio, Thomas Stanke, James Muzerolle, Leslie W. Looney, Yao-Lun Yang, Pamela Klaassen, Nicole Karnath, Prabhani Atnagulov, Nashanty Brunken, William J. Fischer, Elise Furlan, Joel Green, Nolan Habel, Lee Hartmann, Hendrik Linz, Pooneh Nazari, Riwaj Pokhrel, Rohan Rahatgaonkar, Will R. M. Rocha, Patrick Sheehan, Katerina Slavicinska, Amelia M. Stutz, John J. Tobin, Lukasz Tychoniec, Scott Wolk
Figure caption: (a) The Spitzer IRAC three-color (IRAC 3.6, 4.5, and 8 μm are red, green, and blue, respectively) image of the IRAS 16253−2429 field. The field of view is 2′ × 2′. The black square in the center represents a 6″ × 6″ field centered on the JWST observations. (b) A zoomed-in view of the NIRSpec and MIRI channel 1 short (A) field with the red representing continuum emission at 4.17 μm, the green showing H2 0-0 S(11) at 4.18 μm, and the blue depicting [Fe II] at 5.34 μm. A local continuum has been subtracted to make the line maps.
Paper: Discovery of a Collimated Jet from the Low-luminosity Protostar IRAS 16253−2429 in a Quiescent Accretion Phase with the JWST
Authors: Mayank Narang, P. Manoj, Himanshu Tyagi, Dan M. Watson, S. Thomas Megeath, Samuel Federman, Adam E. Rubinstein, Robert Gutermuth, Alessio Caratti o Garatti, Henrik Beuther, Tyler L. Bourke, Ewine F. Van Dishoeck, Neal J. Evans, Guillem Anglada, Mayra Osorio, Thomas Stanke, James Muzerolle, Leslie W. Looney, Yao-Lun Yang, Pamela Klaassen, Nicole Karnath, Prabhani Atnagulov, Nashanty Brunken, William J. Fischer, Elise Furlan, Joel Green, Nolan Habel, Lee Hartmann, Hendrik Linz, Pooneh Nazari, Riwaj Pokhrel, Rohan Rahatgaonkar, Will R. M. Rocha, Patrick Sheehan, Katerina Slavicinska, Amelia M. Stutz, John J. Tobin, Lukasz Tychoniec, Scott Wolk
Figure caption: The morphology of [Fe II] lines detected toward IRAS 16253−2429. All these lines trace the collimated jet launched from the protostar. All images are shown on the same spatial scale. The white solid circle is the MIRI MRS 14 μm continuum position. The scale bar corresponding to 100 au is shown in the bottom left corner.
Paper: Discovery of a Collimated Jet from the Low-luminosity Protostar IRAS 16253−2429 in a Quiescent Accretion Phase with the JWST
Authors: Mayank Narang, P. Manoj, Himanshu Tyagi, Dan M. Watson, S. Thomas Megeath, Samuel Federman, Adam E. Rubinstein, Robert Gutermuth, Alessio Caratti o Garatti, Henrik Beuther, Tyler L. Bourke, Ewine F. Van Dishoeck, Neal J. Evans, Guillem Anglada, Mayra Osorio, Thomas Stanke, James Muzerolle, Leslie W. Looney, Yao-Lun Yang, Pamela Klaassen, Nicole Karnath, Prabhani Atnagulov, Nashanty Brunken, William J. Fischer, Elise Furlan, Joel Green, Nolan Habel, Lee Hartmann, Hendrik Linz, Pooneh Nazari, Riwaj Pokhrel, Rohan Rahatgaonkar, Will R. M. Rocha, Patrick Sheehan, Katerina Slavicinska, Amelia M. Stutz, John J. Tobin, Lukasz Tychoniec, Scott Wolk
Figure caption: Morphology of the Br-α line and the other atomic FS lines detected toward IRAS 16253−2429. All images are shown on the same spatial scale. The white solid circle is the MIRI MRS 14 μm continuum position. The scale bar corresponding to 100 au is shown in the bottom left corner.
Paper: Discovery of a Collimated Jet from the Low-luminosity Protostar IRAS 16253−2429 in a Quiescent Accretion Phase with the JWST
Authors: Mayank Narang, P. Manoj, Himanshu Tyagi, Dan M. Watson, S. Thomas Megeath, Samuel Federman, Adam E. Rubinstein, Robert Gutermuth, Alessio Caratti o Garatti, Henrik Beuther, Tyler L. Bourke, Ewine F. Van Dishoeck, Neal J. Evans, Guillem Anglada, Mayra Osorio, Thomas Stanke, James Muzerolle, Leslie W. Looney, Yao-Lun Yang, Pamela Klaassen, Nicole Karnath, Prabhani Atnagulov, Nashanty Brunken, William J. Fischer, Elise Furlan, Joel Green, Nolan Habel, Lee Hartmann, Hendrik Linz, Pooneh Nazari, Riwaj Pokhrel, Rohan Rahatgaonkar, Will R. M. Rocha, Patrick Sheehan, Katerina Slavicinska, Amelia M. Stutz, John J. Tobin, Lukasz Tychoniec, Scott Wolk
Figure caption: The moment 1 map for the [Fe II] line at 5.34 μm. The white solid circle is the MIRI MRS 14 μm continuum position.
Paper: GJ 367b Is a Dark, Hot, Airless Sub-Earth
Authors: Michael Zhang, Renyu Hu, Julie Inglis, Fei Dai, Jacob L. Bean, Heather A. Knutson, Kristine Lam, Elisa Goffo, Davide Gandolfi
Figure caption: Left: eclipse depths inferred from the two individual eclipses, together with their average, which we adopt as the fiducial emission spectrum. Right: the average spectrum of the two eclipses, compared to the spectrum inferred by fitting the entire phase curve simultaneously. The two are consistent to 1σ at all wavelengths.
Paper: GJ 367b Is a Dark, Hot, Airless Sub-Earth
Authors: Michael Zhang, Renyu Hu, Julie Inglis, Fei Dai, Jacob L. Bean, Heather A. Knutson, Kristine Lam, Elisa Goffo, Davide Gandolfi
Figure caption: GJ 367b in the context of other rocky planets with thermal emission measurements. ﹩{T}_{\mathrm{rmd},\max }﹩ is the maximum possible dayside temperature, assuming a zero albedo, zero heat redistribution planet. The dashed horizontal line is at 0.78, the expected ratio for a zero albedo, maximum heat redistribution planet. The brightness temperature values come from Spitzer IRAC 4.5 μm for GJ 1252b, LHS 3844b, K2-141b, and 55 Cnc e (Crossfield et al. 2022) and from MIRI F1500W photometry for TRAPPIST-1b (Greene et al. 2023) and TRAPPIST-1c (Zieba et al. 2023). On the right, the gray region indicates temperatures high enough to melt all silicate rocks.
Paper: GJ 367b Is a Dark, Hot, Airless Sub-Earth
Authors: Michael Zhang, Renyu Hu, Julie Inglis, Fei Dai, Jacob L. Bean, Heather A. Knutson, Kristine Lam, Elisa Goffo, Davide Gandolfi
Figure caption: The data before removal of systematics. Left: spectroscopic light curves for each wavelength. The dark band at phase 0 is the transit, and it is the only evident astrophysical feature in this plot. Note the shadowed region (λ = 10.54–11.76 μm), the notch between λ = 8.04–8.14 μm and phases 0.68–0.74, the sudden flux drop at phase −0.685, and the odd–even effect. Right: the white light curve. Note the strong initial ramp and the sudden flux drop at phase −0.685. The vertical lines mark the boundaries between exposures.
Paper: GJ 367b Is a Dark, Hot, Airless Sub-Earth
Authors: Michael Zhang, Renyu Hu, Julie Inglis, Fei Dai, Jacob L. Bean, Heather A. Knutson, Kristine Lam, Elisa Goffo, Davide Gandolfi
Figure caption: Observed dayside emission spectrum, compared to selected self-consistent 1D forward models computed by HELIOS 3.1. The atmosphere models (left) have a metal-rich surface, while the surface models (right) have no atmosphere. We ignore the outlier 9.0 μm data point when comparing to models (but see Appendix F for the reasons it may be real).