adsabs/AstroCLIMB huggingface dataset:
Paper: The Lyα Sky as Observed by New Horizons at 57 au
Authors: G. Randall Gladstone, J. Michael Shull, Wayne R. Pryor, Jonathan Slavin, Joshua A. Kammer, Tracy M. Becker, Tod R. Lauer, Marc Postman, John R. Spencer, Joel Wm. Parker, Kurt D. Retherford, Michael A. Velez, Maarten H. Versteeg, Michael W. Davis, Cynthia S. Froning, Camden D. Ertley, Nathaniel Cunningham, Jayant Murthy, Richard C. Henry, Seth Redfield, Carey M. Lisse, Kelsi N. Singer, Anne J. Verbiscer, Pontus C. Brandt, S. Alan Stern
Figure caption: The all-sky NH Lyα maps are constructed in the same way as for Figure 6, but show the residual brightness after subtracting a model prediction of the backscattered solar Lyα. Note that the range in brightness has been reduced to only 25–75 R in these residual maps.
Paper: The Lyα Sky as Observed by New Horizons at 57 au
Authors: G. Randall Gladstone, J. Michael Shull, Wayne R. Pryor, Jonathan Slavin, Joshua A. Kammer, Tracy M. Becker, Tod R. Lauer, Marc Postman, John R. Spencer, Joel Wm. Parker, Kurt D. Retherford, Michael A. Velez, Maarten H. Versteeg, Michael W. Davis, Cynthia S. Froning, Camden D. Ertley, Nathaniel Cunningham, Jayant Murthy, Richard C. Henry, Seth Redfield, Carey M. Lisse, Kelsi N. Singer, Anne J. Verbiscer, Pontus C. Brandt, S. Alan Stern
Figure caption: A 5 hr excerpt from the ∼150 hr of data is used to illustrate how the data were processed prior to making the all-sky map. The raw 10 Hz count-rate samples are shown in black. The blue line shows the expected count rate due to stars passing through the Alice slit, using the Velez et al. (2024) star catalog. We take any data at times where this expected stellar count rate is >50 counts s−1 (shown as a horizontal dashed blue line) as contaminated (here marked red) and remove them. We then smooth the remaining uncontaminated data using an instrument function which is approximately a smoothed boxcar of ∼40 s (i.e., ∼400 samples) length. The final count rate is shown in green, and is linearly interpolated across gaps due to star contamination. The horizontal red dashed line indicates the maximum Alice count rate during the all-sky map of 2576 counts s−1.
Paper: The Lyα Sky as Observed by New Horizons at 57 au
Authors: G. Randall Gladstone, J. Michael Shull, Wayne R. Pryor, Jonathan Slavin, Joshua A. Kammer, Tracy M. Becker, Tod R. Lauer, Marc Postman, John R. Spencer, Joel Wm. Parker, Kurt D. Retherford, Michael A. Velez, Maarten H. Versteeg, Michael W. Davis, Cynthia S. Froning, Camden D. Ertley, Nathaniel Cunningham, Jayant Murthy, Richard C. Henry, Seth Redfield, Carey M. Lisse, Kelsi N. Singer, Anne J. Verbiscer, Pontus C. Brandt, S. Alan Stern
Figure caption: The upper panel shows the estimated brightness of Hα emissions from the wall of the LHB that would result from EUV illumination by hot stars within the LHB, followed by local recombination and emission. The location of the outer edge of the LHB, as provided in T. J. O’Neill et al. (2024), was used in this calculation, along with the radiation field estimated using the stars in Table 6, which are labeled with dots sized according to the logarithm of their estimated H I photoionizing flux at a distance of 1 pc. The brightest regions are near the primary O-B associations mentioned above at the end of Section 4. The lower panel shows a high-resolution map of diffuse Hα emissions (D. P. Finkbeiner 2003); the lack of correlation with the model map of expected Hα from the interior wall of the LHB is likely due to the domination of contributions from beyond the outer wall of the LHB.
Paper: The Lyα Sky as Observed by New Horizons at 57 au
Authors: G. Randall Gladstone, J. Michael Shull, Wayne R. Pryor, Jonathan Slavin, Joshua A. Kammer, Tracy M. Becker, Tod R. Lauer, Marc Postman, John R. Spencer, Joel Wm. Parker, Kurt D. Retherford, Michael A. Velez, Maarten H. Versteeg, Michael W. Davis, Cynthia S. Froning, Camden D. Ertley, Nathaniel Cunningham, Jayant Murthy, Richard C. Henry, Seth Redfield, Carey M. Lisse, Kelsi N. Singer, Anne J. Verbiscer, Pontus C. Brandt, S. Alan Stern
Figure caption: Spectral images for the Alice observation of a dark region on the sky, referred to as NCOB01 (see M. Postman et al. 2024 and Table 5 for more information). Left: the count-rate spectral image of the sum of eight 1 hr histogram exposures of the sky, using all 32 rows and columns 535 through 555 of the Alice detector in order to display the spectral image in the Lyα vicinity. Approximate wavelengths are 120.3–123.9 nm; most of the signal is from diffuse Lyα filling the Alice slit. Center: same as left, but for the sum of the eight 1 hr interleaved dark exposures for observations NCOB01. Right: the net count rate of the sky (left) after subtracting the dark (center) spectral images, showing that the dark sky is completely dominated by diffuse Lyα at FUV wavelengths. The count rate is shown on a log scale in the color bar on the right.
Paper: The Lyα Sky as Observed by New Horizons at 57 au
Authors: G. Randall Gladstone, J. Michael Shull, Wayne R. Pryor, Jonathan Slavin, Joshua A. Kammer, Tracy M. Becker, Tod R. Lauer, Marc Postman, John R. Spencer, Joel Wm. Parker, Kurt D. Retherford, Michael A. Velez, Maarten H. Versteeg, Michael W. Davis, Cynthia S. Froning, Camden D. Ertley, Nathaniel Cunningham, Jayant Murthy, Richard C. Henry, Seth Redfield, Carey M. Lisse, Kelsi N. Singer, Anne J. Verbiscer, Pontus C. Brandt, S. Alan Stern
Figure caption: An example spectrum of wavelengths including the diffuse Lyα from the NCOB01 deep exposure, comprised of eight 1 hr exposures interleaved with eight 1 hr darks with the Alice instrument pointed at the direction ﹩(l,b)=(319\mathop{.}\limits^{^\circ }728,-60\mathop{.}\limits^{^\circ }293)﹩ (see Table 5 for other NCOB information). The observed net brightness spectrum is given by the black histogram, and the 1σ error of the net brightness is shown by the red histogram. As noted on the figure, for this observation the on-axis average diffuse Lyα brightness was 136.65 ± 4.71 R, and the corresponding analog net count rate was 485.68 ± 0.94 counts s−1. These values are combined to give a Lyα sensitivity for the Alice spectrograph of 3.55 ± 0.12 counts s−1 R−1 for this observation.
Paper: The Lyα Sky as Observed by New Horizons at 57 au
Authors: G. Randall Gladstone, J. Michael Shull, Wayne R. Pryor, Jonathan Slavin, Joshua A. Kammer, Tracy M. Becker, Tod R. Lauer, Marc Postman, John R. Spencer, Joel Wm. Parker, Kurt D. Retherford, Michael A. Velez, Maarten H. Versteeg, Michael W. Davis, Cynthia S. Froning, Camden D. Ertley, Nathaniel Cunningham, Jayant Murthy, Richard C. Henry, Seth Redfield, Carey M. Lisse, Kelsi N. Singer, Anne J. Verbiscer, Pontus C. Brandt, S. Alan Stern
Figure caption: Residual Lyα maps in Galactic coordinates, showing the polar regions (in satellite projection) for the north Galactic pole (NGP, upper) and south Galactic pole (SGP, lower). The typical diffuse brightness is ∼5–10 R larger in the north than in the south.
Paper: The Lyα Sky as Observed by New Horizons at 57 au
Authors: G. Randall Gladstone, J. Michael Shull, Wayne R. Pryor, Jonathan Slavin, Joshua A. Kammer, Tracy M. Becker, Tod R. Lauer, Marc Postman, John R. Spencer, Joel Wm. Parker, Kurt D. Retherford, Michael A. Velez, Maarten H. Versteeg, Michael W. Davis, Cynthia S. Froning, Camden D. Ertley, Nathaniel Cunningham, Jayant Murthy, Richard C. Henry, Seth Redfield, Carey M. Lisse, Kelsi N. Singer, Anne J. Verbiscer, Pontus C. Brandt, S. Alan Stern
Figure caption: The variation of the Alice spectrograph total analog count rate to observed diffuse Lyα brightness is plotted for the 15 NCOB observations. Using the 15 NCOB measurements, we find an average sensitivity for the Alice spectrograph of 3.67 ± 0.02 counts s−1 R−1, which is overplotted as a dashed line. This sensitivity is used to convert the analog count rates observed during the all-sky map into diffuse Lyα brightnesses in regions of the sky uncontaminated by UV-bright stars.
Paper: Stellar Population and Energy Feedback in the Supergiant Shell LMC 1
Authors: Guan-Hong Li, 冠宏 李, Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Po-Sheng Ou, 柏昇 歐, C.-H. Rosie Chen, 昌慧 陳, Konstantin Grishunin, Hsu-Tai Lee, 昫岱 李
Figure caption: Left: MCELS Hα image of SGS LMC 1. The OB association LH15 is marked in red. The H II regions are marked in blue with catalog numbers # from R. D. Davies et al. (1976), where the LMC H II regions are designated DEM L#. Right: MCELS Hα image marked with cluster ages from K. Glatt et al. (2010). The 1.7 Gyr-old globular cluster near the south rim of LMC 1 is NGC 1783.
Paper: Stellar Population and Energy Feedback in the Supergiant Shell LMC 1
Authors: Guan-Hong Li, 冠宏 李, Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Po-Sheng Ou, 柏昇 歐, C.-H. Rosie Chen, 昌慧 陳, Konstantin Grishunin, Hsu-Tai Lee, 昫岱 李
Figure caption: Left: MCELS Hα image of SGS LMC 1. The 25′ radius circular region is plotted in a red dashed line. The OB association LH15 is radially divided into A, B, and C regions. The stellar population is examined inside and outside LH15, and in the A, B, and C regions of LH15 separately to search for variations. Right: MCELS Hα image of SGS LMC 1 marked with main-sequence stars in the mass ranges of 10–15, 15–20, and 20–25 M⊙.
Paper: Stellar Population and Energy Feedback in the Supergiant Shell LMC 1
Authors: Guan-Hong Li, 冠宏 李, Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Po-Sheng Ou, 柏昇 歐, C.-H. Rosie Chen, 昌慧 陳, Konstantin Grishunin, Hsu-Tai Lee, 昫岱 李
Figure caption: MCELS Hα image of SGS LMC 1 superposed with green contours of 12CO(1–0) emission observed by NANTEN, and cyan contours of 12CO(3–2) emission observed by APEX. The YSOs from B. A. Whitney et al. (2008) and R. A. Gruendl & Y.-H. Chu (2009) are marked in filled red circles.
Paper: Stellar Population and Energy Feedback in the Supergiant Shell LMC 1
Authors: Guan-Hong Li, 冠宏 李, Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Po-Sheng Ou, 柏昇 歐, C.-H. Rosie Chen, 昌慧 陳, Konstantin Grishunin, Hsu-Tai Lee, 昫岱 李
Figure caption: Upper panel: the G vs. GBP − GRP CMD of stars overlaid with stellar evolutionary tracks and isochrones outside LH15. Stars are dereddened by an extinction of AV = 0.35. Lower panel: Same as above, but for stars inside LH15.
Paper: Stellar Population and Energy Feedback in the Supergiant Shell LMC 1
Authors: Guan-Hong Li, 冠宏 李, Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Po-Sheng Ou, 柏昇 歐, C.-H. Rosie Chen, 昌慧 陳, Konstantin Grishunin, Hsu-Tai Lee, 昫岱 李
Figure caption: Upper panel: the G vs. GBP − GRP CMD of stars overlaid with stellar evolutionary tracks and isochrones in Region A. Stars are dereddened by an extinction of AV = 0.35. Middle panel: same as above, but for stars in Region B. Lower panel: same as above, but for stars in Region C.
Paper: Stellar Population and Energy Feedback in the Supergiant Shell LMC 1
Authors: Guan-Hong Li, 冠宏 李, Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Po-Sheng Ou, 柏昇 歐, C.-H. Rosie Chen, 昌慧 陳, Konstantin Grishunin, Hsu-Tai Lee, 昫岱 李
Figure caption: Color composite of MCELS Hα image (green) and ATCA+Parkes H I column density map (red). The Hα emission originates from the ionized inner wall of the H I shell.
Paper: Stellar Population and Energy Feedback in the Supergiant Shell LMC 1
Authors: Guan-Hong Li, 冠宏 李, Chuan-Jui Li, 傳睿 李, You-Hua Chu, 有花 朱, Po-Sheng Ou, 柏昇 歐, C.-H. Rosie Chen, 昌慧 陳, Konstantin Grishunin, Hsu-Tai Lee, 昫岱 李
Figure caption: The 2nd moment map of the ATCA+Parkes H I 21 cm line data cube from S. Kim et al. (2003).
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: The left panel shows pixel-by-pixel visual extinction maps (Av) inferred from the jet emission, with the source name displayed above each map and the color bar on the right. There is a single color bar for all sources except IRAS 04302 (the only Class I source in the sample), which shows higher extinction values. The maps are arranged so that the left side is blueshifted while the right side is redshifted (Paper I). The dashed lines in the maps highlight the estimated source position along the jet. The right panel shows extinction as a function of the distance from the source (sources are arranged in the same order as the left panels), averaged across the jet. Blue and red points represent extinction on the blue- and redshifted sides, respectively.
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: Continuum-subtracted emission in the following lines: [Fe II] 1.257 μm, [C I] 0.985 μm, [S II] 1.032 μm, [N I] 1.040+1.041 μm, He I 1.083 μm, H I 4–3, and permitted C I 1.175 μm toward all four sources. For [N I], we integrate the emission over both 1.040 μm and 1.041 μm transitions to increase the S/N. The respective continuum emission is overlaid on the line emissions and is highlighted in green.
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: NIRSpec 0.97–1.82 μm (G140H/F100LP grating filter) spectra of all the sources summed over the entire field of view. The forbidden atomic lines are identified in the first panel, and other atomic and molecular lines in the second and third panels, respectively, but apply to all the panels. The strong dip in all the spectra between ∼1.408 and 1.486 μm corresponds to the detector gap and is highlighted in the first panel.
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: The left panel shows pixel-by-pixel electron density maps (ne) inferred from the jet emission, with the source name displayed above each map and the color bar on the right. There is a single color bar for all sources except HH 30, which shows higher electron densities. The right panel shows the average electron density as a function of the distance from the source (sources are arranged in the same order as the left panels). The vertical bars represent a 15% error as described in the text. Green dashed lines represent the extinction-corrected normalized [Fe II] 1.644 μm line fluxes. The maps are arranged so that the left side is blueshifted while the right side is redshifted. The dashed lines in the maps and the plots highlight the estimated source position along the jet.
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: Comparison of jet mass-loss rates between (i) the red- and blueshifted sides of the jet, (ii) three methods of calculating the jet mass-loss rates, (iii) different sources, and (iv) their literature estimates, when available. The estimates shown here are the median of the values plotted in Figure 14 along the jet. The blue and red points correspond to the blue- and redshifted lobes. The error bars correspond to the standard error of the distribution in Figure 14, and an additional error of at least 30% for HH 30 and FS TauB and 50% for Tau 042021 and IRAS 04302 needs to be considered. The dotted lines highlight 5 × 10−10 and 5 × 10−9 M⊙ yr−1, between which the majority of the points lie.
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: Top: He I, Paγ, and [Fe II] line ratios as diagnostics of the shock speed and pre-shock electron densities. Blue and red markers represent the blue- and redshifted jets, respectively, for each source. The He I/Paγ ratios are generated using the publicly available shock code MAPPINGS V (M. A. Dopita & R. S. Sutherland 2017; R. S. Sutherland & M. A. Dopita 2017; R. Sutherland et al. 2018). The curves represent increasing pre-shock densities from light gray to black. Growing circle sizes along each curve represent the following shock speeds: 20, 40, 60, 80, 100, 120 km s−1. Each line flux was calculated in the scattered-light-free region of the jet and was corrected for extinction before taking the ratio. Bottom: [Fe II] and Paβ line ratios as diagnostics of the shock speed and pre-shock electron densities. The curves are digitized and recreated from B.-C. Koo et al. (2016).
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: Extinction-corrected line ratios as a function of the distance from the source. The green dashed lines show the normalized [Fe II] 1.644 μm line flux. The gray bands highlight the scattered-light-dominated region, and since the He I and H I lines have a scattered emission component too (Figure 2), the ratios there are not representative of the jet. However, outside the gray bands are the jet-only ratios. For the redshifted side of HH 30, the Paβ/[Fe II] ratio should be considered as an upper limit, and the He I/Paβ ratio as a lower limit, as we could only estimate an upper limit for Paβ in this region (see Section 4.1).
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: All panels show the average electron density as a function of the distance from the source (with the source name at the top of each panel). In black are the electron densities derived using the [Fe II] line ratios, and in green, those using the [S II] line ratios. Each point has an error bar that corresponds to the standard deviation of the electron densities averaged at that offset. The maps are arranged so that the left side is blueshifted while the right side is redshifted. The dashed lines highlight the estimated source position along the jet.
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: Emission centroids and best-fit binary orbit model for the redshifted and the blueshifted jets of Tau 042021, fit simultaneously. The emission centroids and errors in these plots are the same as those shown in Figure 10 for Tau 042021. The negative x-axis indicates that it is tracing the redshifted jet.
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: In red are the mass accretion estimates from this work, calculated using the jet mass-loss rates acquired using three different methods. These estimates are placed alongside literature values of Taurus sources (in black) calculated using hydrogen recombination lines and/or UV excess by G. J. Herczeg & L. A. Hillenbrand (2008, 2014), L. Testi et al. (2022), and compiled by C. F. Manara et al. (2023).
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: Each panel shows the emission centroids across the jet as a function of the distance from the source. The name of the corresponding source is given at the top left. Blue points trace emission centers in the blueshifted jet lobe, whereas red points trace emission centroids in the redshifted lobe. Both the red and blueshifted emissions are placed on the same side of the source for easy comparison. The vertical position of the source (i.e., zero position on the y-axis) is determined as the average of the highest and lowest data points in the plot.
Paper: Class I/II Jets with JWST: Mass-loss Rates, Asymmetries, and Binary-induced Wigglings
Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page
Figure caption: Relation between the ionization fraction and shock speed for a pre-shock density of 1000 cm−3 and magnetic field strength of 100 μG. The relation is digitized and recreated from P. Hartigan et al. (1994) and was derived using the shock model predictions for [S II] line ratios.
Paper: Asymmetry and Dynamical Constraints in Two-limbs Retrieval of WASP-39 b Inferring from JWST Data
Authors: Zixin Chen, Jianghui Ji, Guo Chen, Fei Yan, Xianyu Tan
Figure caption: Comparison retrieved temperature of WASP-39 b of six hypotheses, arranged from left to right: 1D homogeneous clouds, 1D patchy clouds; 2D fixed 150 K temperature difference with homogeneous C/O and inhomogeneous cloud haze, both C/O and aerosol are inhomogeneous; 2D free temperature difference with homogeneous C/O and inhomogeneous cloud haze, both C/O and aerosol are inhomogeneous. Each hypothesis is marked using different symbols corresponding to the data sets used: circles represent the JWST/PRISM full data set, while JWST cutoff data set and the pre-JWST data set are shown in squares and triangles respectively. The upper panel describes the retrieved temperature parameter, a global temperature(in green) for 1D hypotheses, while morning temperature (in blue), evening temperature (in red) and the averaged temperature (in green) for 2D hypotheses. And the bottom shows the temperature difference correspondingly. Three gray dotted, dashed–dotted, and dashed line present the reference retrieved temperature, equilibrium temperature and skin temperature from L. Welbanks & N. Madhusudhan (2022) respectively. The red, blue, and purple solid line with shaded areas present the retrieved median and 1σ confidence intervals result from N. Espinoza et al. (2024).