adsabs/AstroCLIMB huggingface dataset:
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: Parallaxes (left) and PMs (right) of member candidates. The left panel shows the distribution of the parallaxes and their associated errors for stars brighter than 18 mag in the GRP band. We searched for the genuine members between 1.0 and 2.5 kpc (dashed lines). The right panel displays the PMs of member candidates distributed between the upper and lower bounds on the distance. The ellipse (green) shows the region with PMs confined within three times the standard deviation from the weighted mean, where the inverse of the squared PM error is used as the weight value. The red dots represent the most probable members in M16.
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: Radial surface density profile. Poisson statistics was assumed to obtain the error for given surface density. The solid and dashed vertical lines indicate the positions of rh and rcl, respectively. The black curve was obtained from the parameters (μ0 = 21.1 ± 0.4, a = 1.5 ± 0.1, and γ = 2.8 ± 0.2) that best fit the model density profile (R. A. W. Elson et al. 1987).
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: Color–color diagram of early-type members (black dots). The blue solid curve represents the intrinsic color–color relation (H. Sung et al. 2013), while the red solid curve shows the same relation reddened by the mean reddening of 0.96. The reddening values obtained from the early-type members range from 0.78 to 1.32 (dashed curves). The red arrow indicates the reddening vector.
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: Color–color diagrams of IR sources from the GLIMPS survey (E. Churchwell et al. 2009). The red, green, and black dots represent Class 0/I sources, Class II sources, and other sources without definite IR excess emission.
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: CMD of members. Several member candidates (red crosses) below the orange solid lines are excluded from the final member list, while the other candidates are considered as genuine members.
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: Rotation of NGC 6611 within rcl. The upper panel represents the spatial variation of mean RVs that were computed within spatial bins of 7﹩\mathop{.}\limits{^{\prime} }﹩0. The cross and solid line indicate the center of NGC 6611 and the orientation of the projected rotational axis. The reference coordinate is the same as in Figure 5. In the lower panel, the dots represents the differences in the mean RVs between two regions divided by arbitrary axes passing through the center of the cluster. Θ is the position angle of the arbitrary axes. The blue curve shows the best-fit sinusoidal curve.
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: Kinematics of stars in M16. Left panel: the proper motion vectors of stars relative to NGC 6611. The grayscale in the right panel exhibits the integrated intensity map and position–velocity diagrams (grayscales) of the 13CO J = 1–0 line. The stars with RV measurements are superimposed on the figure. The vertical and horizontal lines in the position–velocity diagrams represent the errors of stellar RVs. The orange and blue boxes contain two prominent gas pillars that are likely to be physically associated with neighboring stars.
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: Map of proper motion vectors (upper) and the Φ distribution of the cluster members (lower). In the upper panel, the inner (solid) and outer (dashed) circles represent rh and rcl, respectively. The dashed line in the lower left panel corresponds to rh. The black dots, blue open squares, and red filled squares in the lower right panel show the histograms of Φ values for all cluster members, members within rh, and members beyond rh, respectively.
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: Integrated intensity maps and position–velocity diagrams of stars and gas in Regions 1 (left) and 2 (right). The symbols are the same as in Figure 14.
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: Color excess ratios of the early-type members (red dots). The black line shows the color excess ratios following the normal reddening law (RV = 3.1), while the blue line corresponds to RV = 4.5, which represents the abnormal reddening law.
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: CMDs in comparison with the MESA theoretical isochrones for three different ages: 1 Myr (blue), 2 Myr (orange), and 4 Myr (green; J. Choi et al. 2016; A. Dotter 2016). The isochrones are reddened by E(B − V) = 0.67, 0.78, and 1.32 in the left, middle, and right panels, respectively. The arrow indicates the reddening vector corresponding to AV = 1 mag.
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: Integrated intensity maps and position–velocity diagrams of the H2 1–0 S(1), Brγ, He I 2.059 μm, and [Fe II] 1.644 μm lines. A total of 28 slits cover the head of one southern pillar (see Figure 4). The red dashed lines represent the system RV of NGC 6611 for comparison.
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: Distance distribution of member stars (black). Stars with good astrometric parameters (RUWE < 1.4 and duplicate flag = 0) were used to compute distances. The red curve represents the Gaussian fit to the distance distribution. The distance to M16 is determined to be 1.7 ± 0.2 (s.d.) kpc from the Gaussian center.
Paper: Formation Process of the Young Stellar Population in Messier 16 from a Kinematic Perspective
Authors: Beomdu Lim, Hyeong-Sik Yun, Hyun-Jeong Kim, Yuna Lee, Jae-Rim Koo, Jongsuk Hong, Heeyoung Oh
Figure caption: Distributions of tangential velocities (VR.A. and Vdecl.) and RVs with respect to R.A. and decl. in M16. The vertical lines represents the errors of velocities.
Paper: Cocoon-to-butterfly Transformation in Protoplanetary Nebula: Detection of a Spherical Halo and a Barrel-shaped Torus in IRAS 06530–0213
Authors: Hao-Min Sun, Yong Zhang, Sheng-Li Qin
Figure caption: Channel maps of CO (J = 2–1). The upper panels cover ﹩14.5^{\prime\prime} \rm{}\,\rm{}\,\times 14\mathop{.}\limits^{^{\prime\prime} }5﹩, while the lower panels present a zoomed-in view spanning ﹩4\mathop{.}\limits^{^{\prime\prime} }1\times 4\mathop{.}\limits^{^{\prime\prime} }1﹩. Contour levels are individually defined for each channel by ten equally spaced lines between the channel’s intensity minimum and maximum. Crosses mark the phase center position, and LSR velocities are labeled in each panel. The object’s systemic velocity is 33 km s–1. The white ellipse in the bottom-left corner denotes the synthesized beam, with dimensions ﹩0\mathop{.}\limits^{^{\prime\prime} }72\times 0\mathop{.}\limits^{^{\prime\prime} }41﹩ and a position angle (PA) of 15°.
Paper: Cocoon-to-butterfly Transformation in Protoplanetary Nebula: Detection of a Spherical Halo and a Barrel-shaped Torus in IRAS 06530–0213
Authors: Hao-Min Sun, Yong Zhang, Sheng-Li Qin
Figure caption: Continuum emission at 1.3 mm wavelengths. The synthesized beams shown in the lower-left corner have a size of ﹩0\mathop{.}\limits^{^{\prime\prime} }7\times 0\mathop{.}\limits^{^{\prime\prime} }4﹩. The cross denotes the position of the phase center. Contour levels are set at 1σ intervals starting from 1σ, where the rms σ = 62.5 μJy beam−1.
Paper: Cocoon-to-butterfly Transformation in Protoplanetary Nebula: Detection of a Spherical Halo and a Barrel-shaped Torus in IRAS 06530–0213
Authors: Hao-Min Sun, Yong Zhang, Sheng-Li Qin
Figure caption: Flux density statistics of 13CO and CO moment 0 map in different regions. Left panels: 13CO and CO moment 0 map. Nine concentric annular regions centered at the phase center are outlined by white solid lines and black dashed lines; of these, the black dashed ring marks the halo position at the systemic velocity. Right panels: statistics of the normalized average flux within each ring from the left panel. Ring numbers 2–10 correspond to the concentric rings in the left panel, ordered from smallest to largest, with ring number 1 designating the central circular region. The red filled circles denote the positions of the spherical halo at the systemic velocity.
Paper: Cocoon-to-butterfly Transformation in Protoplanetary Nebula: Detection of a Spherical Halo and a Barrel-shaped Torus in IRAS 06530–0213
Authors: Hao-Min Sun, Yong Zhang, Sheng-Li Qin
Figure caption: Integrated intensity maps of the CO (J = 2–1) line over two different velocity ranges. The northeast (NE) direction is marked in the upper-left corner of the map. The black contours represent the continuum emission, as illustrated in Figure 3. The white ellipse at the bottom-left corner represents the synthesized beam, with a size of 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩72 × 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩41 and a PA of 15°.
Paper: Cocoon-to-butterfly Transformation in Protoplanetary Nebula: Detection of a Spherical Halo and a Barrel-shaped Torus in IRAS 06530–0213
Authors: Hao-Min Sun, Yong Zhang, Sheng-Li Qin
Figure caption: Three-dimensional mesh geometry of the SHAPE model viewed from two orthogonal directions. The upper panels depict the full nebular structure: the left panel presents a side-on view from the observer’s vantage point, whereas the right panel displays a front-facing view directed toward the observer. Red indicates the barrel-shaped torus, green represents the EE, and gray denotes the outer halo. The lower panels provide a close-up view of the barrel-shaped torus.
Paper: Cocoon-to-butterfly Transformation in Protoplanetary Nebula: Detection of a Spherical Halo and a Barrel-shaped Torus in IRAS 06530–0213
Authors: Hao-Min Sun, Yong Zhang, Sheng-Li Qin
Figure caption: SED and two-component fitting of IRAS 06530–0213.
Paper: Cocoon-to-butterfly Transformation in Protoplanetary Nebula: Detection of a Spherical Halo and a Barrel-shaped Torus in IRAS 06530–0213
Authors: Hao-Min Sun, Yong Zhang, Sheng-Li Qin
Figure caption: CO (J = 2–1) line profile and its isotopologue line profiles detected in IRAS 06530–0213, with the systemic velocity (33 km s−1) indicated by a vertical dashed line.
Paper: Cocoon-to-butterfly Transformation in Protoplanetary Nebula: Detection of a Spherical Halo and a Barrel-shaped Torus in IRAS 06530–0213
Authors: Hao-Min Sun, Yong Zhang, Sheng-Li Qin
Figure caption: Same as lower panels of Figure 5, but for 13CO J = 2−1.
Paper: Cocoon-to-butterfly Transformation in Protoplanetary Nebula: Detection of a Spherical Halo and a Barrel-shaped Torus in IRAS 06530–0213
Authors: Hao-Min Sun, Yong Zhang, Sheng-Li Qin
Figure caption: UV coverage acquired by combining the 12A and 10D configurations.
Paper: Cocoon-to-butterfly Transformation in Protoplanetary Nebula: Detection of a Spherical Halo and a Barrel-shaped Torus in IRAS 06530–0213
Authors: Hao-Min Sun, Yong Zhang, Sheng-Li Qin
Figure caption: P–V diagrams of the CO J = 2–1 transition from model predictions (upper panels) and observations (lower panels). The left panels depict the velocity structure along the major (symmetry) axis of the torus, aligned from NE to SW, where negative offsets correspond to the NE direction. The right panels display the velocity structure along the minor axis of the torus, aligned from SE to NW, with negative offsets corresponding to the SE direction.
Paper: Cocoon-to-butterfly Transformation in Protoplanetary Nebula: Detection of a Spherical Halo and a Barrel-shaped Torus in IRAS 06530–0213
Authors: Hao-Min Sun, Yong Zhang, Sheng-Li Qin
Figure caption: Modeled CO (J = 2–1) channel maps. The white ellipse in the lower-left corner of the image represents the synthesized beam. The angular size of each panel is identical to those in the lower panels of Figure 5.
Paper: Cocoon-to-butterfly Transformation in Protoplanetary Nebula: Detection of a Spherical Halo and a Barrel-shaped Torus in IRAS 06530–0213
Authors: Hao-Min Sun, Yong Zhang, Sheng-Li Qin
Figure caption: CO (J = 2–1) emission. The left panel displays the profile derived from averaging flux densities over a 12″ × 12″ area centered at the phase center. The right panel presents the channel maps corresponding to the pink mask (17.4–22.6 km s−1) and gray mask (38.2–43.4 km s−1) regions marked in the left panel.
Paper: Cocoon-to-butterfly Transformation in Protoplanetary Nebula: Detection of a Spherical Halo and a Barrel-shaped Torus in IRAS 06530–0213
Authors: Hao-Min Sun, Yong Zhang, Sheng-Li Qin
Figure caption: CO (J = 3–2) line in PN M3-35 (data taken from L. Guzman-Ramirez et al. 2018). The dashed line denotes the heliocentric velocity of PN M3-35, while the solid line marks the central velocity of the CO J = 3–2 line.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: Top panel: logarithm of the median flux in the traces of the two orders with the UVIS instrument after background subtraction and outlier correction for each pixel in the 3D data cube. The dotted lines mark the apertures (±20 pixels and ±24 pixels for +1 and −1 order, respectively) within which the flux is summed to obtain the 1D spectra. Higher-order traces enter the aperture and contaminate the flux from the primary order. Bottom panel: the total flux Ftotal within the aperture as well as the flux in orders 2 and 3 (﹩{F}_{2}={S}_{2}\,{F}_{* ,{\lambda }_{2}}{\rm{\Delta }}{\lambda }_{2}{t}_{{\rm{\exp }}}﹩ and ﹩{F}_{3}={S}_{3}\,{F}_{* ,{\lambda }_{3}}{\rm{\Delta }}{\lambda }_{3}{t}_{{\rm{\exp }}}﹩; see Equation (2)) for both the +1 and −1 orders from the UVIS data. The color of the lines indicates the wavelength of the different traces at any given pixel column. The flux in higher orders is derived by multiplying the respective calibrated sensitivities with the iteratively determined intrinsic flux of the star. At redder wavelengths for the ± 1 orders, the higher orders constitute a significant fraction of the total flux.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: The iteratively determined intrinsic flux of the star KELT-20 from the order +1 and −1 traces.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: Raw and processed images of the first exposures of the G102 and G141 visits. The white rectangles mark the regions from which the background count is estimated.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: The top and middle panels show the difference in the transit depths for the leading (morning) and the trailing (evening) limbs obtained by fitting the white light curve and the 0.2–0.4 μm light curve, respectively. The vertical lines show the predicted difference in the transit depths of the two limbs using general circulation models (GCMs; see Section 8.1). The bottom panel shows the mid-transit times for light curves binned in 0.1 μm-wide bandpasses. These measurements are shown relative to the mid-transit time of the white light curve, and the gray region marks the 1σ uncertainty of the white light curve’s mid-transit time.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: Median-fit spectra with the 1σ range from the free chemistry (red) and chemical equilibrium (blue) PETRA retrievals. In the calculation of the reduced-χ2 value, the best-fit offset of +10.7 and −130.1 ppm was applied to data points longward of 0.8 μm to the free chemistry and chemical equilibrium retrievals, respectively. This offset is shown by the gray points. The purple and gray shaded regions at short wavelengths show the contribution to the transit depth from 10 ppm of SiO and the best-fit abundance of Fe II, respectively. The approximate pressure is listed on the right axis, though the relationship between transit depth and pressure varies sample-to-sample as a function of temperature and atmospheric opacity.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: Comparison of the volume mixing ratio and 1σ range of Fe II, Fe I, SiO, and H2O from the chemical equilibrium retrieval with the H2O abundance from the free chemistry retrieval and the median fit from L. Finnerty et al. (2025).
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: Observed minus calculated mid-transit times of KELT-20 b. The period and T0 used to calculate the uncertainty region (gray lines) are from E. S. Ivshina & J. N. Winn (2022). Mid-transit times from this work as shown in black squares. T0 of the UVIS +1 and −1 order transits as well as the G141 transit are in exquisite agreement with the predicted T0. The WFC3 G102 visit does not cover either ingress or egress, and its measured T0 has the largest uncertainty out of the four light curves in our study.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: Fitted quadratic limb-darkening coefficients for the two UVIS orders compared to model quadratic coefficients from LDTK (H. Parviainen & S. Aigrain 2015).
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: The figure shows the raw white light curves (top panel), transit models and white light curves with the systematics removed (middle panel), and the residuals (bottom panel). For the G102 and G141 visits, the residuals window spans −200 to 200 ppm (2.5× Zoom). The UVIS transits are significantly deeper than the G102 and G141 transits.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: The 0.2–1.7 μm transmission spectrum of KELT-20 b measured with the WFC3 instrument in the G280 (UVIS), G102, and G141 bandpasses.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: Abundance posterior distributions for the free chemistry retrieval with PETRA.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: [Z/H] and [O/H] ratio posterior constraints from the chemical equilibrium retrieval with PETRA.
Paper: Strong NUV Refractory Absorption and Dissociated Water in the Hubble Transmission Spectrum of the Ultra Hot Jupiter KELT-20 b
Authors: Yayaati Chachan, Joshua Lothringer, Julie Inglis, Hayley Beltz, Heather A. Knutson, Jessica Spake, Bjorn Benneke, Ian Wong, Zafar Rustamkulov, David Sing, Katherine A. Bennett
Figure caption: Left panel: time-averaged temperature–pressure profiles for four regions of the 0G/drag-free GCM (solid lines) and the 5G active drag GCM (dashed lines). We can see that the active drag model has a slightly hotter dayside and a significantly cooler nightside. We also note that the east limb is hotter in the drag-free case due to more efficient heat transfer on the dayside. The western limb is hotter in the active drag case in the upper atmosphere due to differences in the flow patterns between the two models. Right panel: the GCM limb profiles are plotted along with the retrieved temperature–pressure profiles from PETRA, the 1D radiative-convective equilibrium (1D-RCE) model from PHOENIX assuming full heat redistribution, and the condensation curves for Fe and MgSiO3 from C. W. Visscher et al. (2010).