adsabs/AstroCLIMB huggingface dataset:
Paper: The SSA22 H I Tomography Survey (SSA22-HIT). I. Data Set and Compiled Redshift Catalog
Authors: Ken Mawatari, Akio K. Inoue, Toru Yamada, Tomoki Hayashino, J. Xavier Prochaska, Khee-Gan Lee, Nicolas Tejos, Nobunari Kashikawa, Takuya Otsuka, Satoshi Yamanaka, David J. Schlegel, Yuichi Matsuda, Joseph F. Hennawi, Ikuru Iwata, Hideki Umehata, Shiro Mukae, Masami Ouchi, Yuma Sugahara, Yoichi Tamura
Figure caption: Magnitude distribution (bottom) and number fraction of the spectroscopically confirmed objects (bottom) for each of the five major categories. In each panel, the solid and dashed histograms represent the observed and spectroscopically confirmed objects in the given category, respectively. We used the ﹩i^{\prime} ﹩-band magnitudes for the T1, T2, and T3 categories, while the ﹩z^{\prime} ﹩-band magnitudes are used for the T4 and T5 categories.
Paper: Hazy with a Chance of Star Spots: Constraining the Atmosphere of Young Planet K2-33b
Authors: Pa Chia Thao, Andrew W. Mann, Peter Gao, Dylan A. Owens, Andrew Vanderburg, Elisabeth R. Newton, Yao Tang, Matthew J. Fields, Trevor J. David, Jonathan M. Irwin, Tim-Oliver Husser, David Charbonneau, Sarah Ballard
Figure caption: Detected population of all planets from Kepler and K2 as a function of the planet radius (R ⊕) and orbital period (days). Young (<1 Gyr), transiting planets that are members of clusters or stellar associations are plotted in circles colored by their age. K2-33b is outlined as a star and lands at the edge of the sub-Saturn desert. The youngest planets (yellow) have radii between Neptune and Jupiter, while no mature planets (purple) are located within this region. K2-33b is likely still evolving and offers an opportunity to observe an atmosphere in transition. Planet properties from the NASA Exoplanet Science Institute (2020).
Paper: Hazy with a Chance of Star Spots: Constraining the Atmosphere of Young Planet K2-33b
Authors: Pa Chia Thao, Andrew W. Mann, Peter Gao, Dylan A. Owens, Andrew Vanderburg, Elisabeth R. Newton, Yao Tang, Matthew J. Fields, Trevor J. David, Jonathan M. Irwin, Tim-Oliver Husser, David Charbonneau, Sarah Ballard
Figure caption: Left: typical raw HST image from Orbits 1–4. Right: typical raw image from Orbits 5–6. The telescope slewed so images from these orbits were discarded.
Paper: Zonal Winds of Uranus and Neptune: Gravitational Harmonics, Dynamic Self-gravity, Shape, and Rotation
Authors: Deniz Soyuer, Benno Neuenschwander, Ravit Helled
Figure caption: Top panels: contributions to the zonal gravitational harmonic perturbation ﹩{J}_{4}^{{\prime} }﹩ for Uranus and Neptune models, as a function of scale height H. The dashed lines show the difference between the observed and the model fourth-degree harmonic: ﹩{J}_{4}^{{\prime} }={J}_{4}^{\mathrm{obs}}-{\tilde{J}}_{4}﹩. Bottom panels: the relative impact of the self-gravity contribution with respect to the zonal wind contribution as a function of scale height H. Apart from the singular region where the perturbation changes signs, self-gravity has a contribution that is about one order of magnitude smaller than that of the zonal winds. Bottom panels: the scale height H, for which the condition ﹩{J}_{4}^{{\prime} }({\rho }^{{\prime} })={J}_{4}^{{\prime} }(\tilde{\rho })﹩ is satisfied, as a function of the missing dynamical contribution percentage from the model: ﹩| {J}_{4}^{{\prime} }(\tilde{\rho })/{J}_{4}^{\mathrm{obs}}| =| 1-{\tilde{J}}_{4}/{J}_{4}^{\mathrm{obs}}| ﹩. Since ﹩{\tilde{J}}_{4}/{J}_{4}^{\mathrm{obs}}\gt 1﹩, models lying further out in the x-axis have higher ﹩-{\tilde{J}}_{4}﹩ and require a higher ﹩{J}_{4}^{{\prime} }(\tilde{\rho })﹩ to match the observed ﹩{J}_{4}^{\mathrm{obs}}={\tilde{J}}_{4}+{J}_{4}^{{\prime} }(\tilde{\rho })﹩. These models correspond to those with lower surface densities, since r > 0.65R of the planet is represented by a single polytrope. Red (blue) dots represent solutions with (without) the contribution from dynamic self-gravity. The uncertainty of the inferred scale height limits for Neptune is larger due to the larger measurement uncertainty in the observed ﹩{J}_{4}^{\mathrm{obs}}﹩. Orange (purple) rectangles identify the three-layer models with the lowest (greatest) ﹩| {J}_{4}^{{\prime} }(\tilde{\rho })/{J}_{4}^{\mathrm{obs}}| ﹩ ratio. This color scheme is used in following plots as well.
Paper: Zonal Winds of Uranus and Neptune: Gravitational Harmonics, Dynamic Self-gravity, Shape, and Rotation
Authors: Deniz Soyuer, Benno Neuenschwander, Ravit Helled
Figure caption: Top panels: pressure vs. density profiles of various published interior structure models. Solid lines show the pressure vs. density profiles of the models, where the highlighted regions show the cores of the models, if it exists. The dotted black lines are arbitrarily normalized polytropes with a polytropic index of n = 1 to guide the eye. For Jupiter, a polytropic index n of unity is a relatively good fit for the model of Nettelmann et al. (2012) beneath 1 kbar (∼0.99R J), as also shown in Wicht et al. (2020). For Uranus and Neptune n = 1 seems to be a somewhat decent fit (Helled et al. 2011; Nettelmann et al. 2013). Bottom panels: solid lines show the calculated μ(r)R 2 for all models. The dashed line in the bottom left panel shows the ﹩\mu \sim {\pi }^{2}/{R}_{{\rm{J}}}^{2}﹩ approximation made by Wicht et al. (2020) for Jupiter. The dashed lines in the other bottom panels show the average value of μ(r)R 2 throughout the core exterior calculated here. Due to the relative complexity of the structure models shown here, the μ(r)R 2 value has nonmonotonous behavior, which is not the case for the polytropic models we consider in the following chapters.
Paper: Zonal Winds of Uranus and Neptune: Gravitational Harmonics, Dynamic Self-gravity, Shape, and Rotation
Authors: Deniz Soyuer, Benno Neuenschwander, Ravit Helled
Figure caption: The geoid shape as a function of colatitude for Uranus (top) and Neptune (bottom) for different configurations. Gray dashed lines show the inferred shapes after Voyager II radius measurements (Lindal et al. 1987, 1990). Black solid lines show the same geoid calculation, but with updated J 2 and J 4 values from Jacobson (2014, 2009). Black dotted lines show the geoid shape with updated harmonics as before, but also with an updated rotation period change according to Helled et al. (2010), where P U = 16.58h and P N = 17.46 h, instead of those in Table 1. The purple and orange lines correspond to the modifications to the shape given by the black curves due to density perturbations induced by zonal winds, as mentioned in Figure 6. Red errorbars show the radius measurements done by Voyager II. All curves are normalized such that the Voyager II measurements are matched.
Paper: Zonal Winds of Uranus and Neptune: Gravitational Harmonics, Dynamic Self-gravity, Shape, and Rotation
Authors: Deniz Soyuer, Benno Neuenschwander, Ravit Helled
Figure caption: Top panels: pressure vs. density profiles of Uranus and Neptune using polytropic empirical structure models where the innermost polytrope represents the core. The dotted black line represents a polytrope with index unity P ∝ ρ 2 to guide the eye. Bottom panels: solid lines represent the calculated μ(r)R 2 values for each model and the shaded yellow region shows the range of mean values 〈μ(r)〉R 2 for all the empirical density models. The mean values are computed for the outermost polytrope only. Models with a steeper (flatter) P vs. ρ curve than the index unity polytrope have a monotonously decreasing (increasing) μ(r)R 2 value.
Paper: Zonal Winds of Uranus and Neptune: Gravitational Harmonics, Dynamic Self-gravity, Shape, and Rotation
Authors: Deniz Soyuer, Benno Neuenschwander, Ravit Helled
Figure caption: Top and center panels: total density contours as a function of planetary radius r/R and colatitude θ of most extreme models of Uranus and Neptune. The top (center) panels are the models with the lowest (highest) ﹩{\tilde{J}}_{4}﹩ values (also shown in Figure 5). Bottom panels: densities averaged over the colatitude as a function of planetary radius. Solid curves show both density perturbations (lowest in orange, highest in purple), as well as all the other models in gray. Dashed curves show the hydrostatic densities of their respective models.
Paper: Zonal Winds of Uranus and Neptune: Gravitational Harmonics, Dynamic Self-gravity, Shape, and Rotation
Authors: Deniz Soyuer, Benno Neuenschwander, Ravit Helled
Figure caption: The ﹩{\tilde{J}}_{2}﹩ and the ﹩{\tilde{J}}_{4}﹩ values of Uranus (blue dots) and Neptune (orange dots) models used in this study. The bars represent the measured values and their errors for each planet. The hydrostatic ﹩{\tilde{J}}_{4}﹩ (or ﹩{\tilde{J}}_{2}﹩) of the models do not fit for the observed ﹩{J}_{4}^{\mathrm{obs}}﹩ (or ﹩{J}_{2}^{\mathrm{obs}}﹩) in order to account for the contribution of their dynamical counterparts ﹩{J}_{4}^{{\prime} }﹩ (or ﹩{J}_{2}^{{\prime} }﹩). Arrows indicate qualitatively the missing dynamical ﹩{J}_{4}^{{\prime} }﹩ counterpart to the observed ﹩{J}_{4}^{\mathrm{obs}}﹩ according to Equation (4).
Paper: Zonal Winds of Uranus and Neptune: Gravitational Harmonics, Dynamic Self-gravity, Shape, and Rotation
Authors: Deniz Soyuer, Benno Neuenschwander, Ravit Helled
Figure caption: Uranus and Neptune interior structure models generated with ±5 × 10−6 variation in the observed J 2 value (left). Zonal wind decay heights as a function of the J 2 offset (right). Allowing the interior models to have J 2 solutions in the ±5 × 10−6 range around the mean observed value has the same effect on the zonal wind decay heights as unconstrained, J 4.
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: The 12CO (integrated between −1 and +7 km s−1) and 13CO (integrated between 0.5 and 6.5 km s−1) emission contours of the observed Cassiopeia region, plotted on the 6 cm radio continuum image (from Sun et al. 2007). The 12CO contours (blue) start at 5σ and increase in a step of 3σ (1σ noise is ∼0.7–0.8 K km s−1), while the 13CO contours (green) start at 4σ and increase in a step of 2σ (1σ noise is ∼0.37 K km s−1). The 6 cm contours (white) correspond to 10, 15, 22, and 29 mK, and then increase by steps of 12 mK (1σ is ∼1.4 mK). The red dashed partial ellipse with a dimension of 3.°4 × 2.°8 shows a potential bubble suggested by the morphology and kinematics of both the shell and finger-like structures, while the yellow cross shows the bubble center suggested by the finger-like structures (l = 124.°06, b = 1.°15). The yellow dashed circles show the two supernova remnants in the region. The names of known H II regions are also labeled.
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: Top panel: the distribution of the 12CO line widths (moment 2 image) of the observed Cassiopeia region within the velocity range of [0, 7] km s−1. The unit of the scale bar is km s−1. Bottom panel: the same as the top panel, but for the 13CO emission. In the two panels, green squares, red, and blue stars show the positions of starless, prestellar, and protostellar cores detected in the Herschel Hi-Gal survey (see Elia et al. 2021), while the two dashed lines show the covered extent in the Hi-Gal survey. The Cassiopeia filament is observed in the velocity range of [+1, +4] km s−1, and the Herschel Hi-Gal cores are then selected with molecular gas velocities within [–1, +6] km s−1.
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: The multiwavelength radio continuum images of G120.0+1.4. The unit of the scale bar is Jy beam−1 for each panel. The red dashed circle shows the bubble center referred from the CO observations, while the blue-filled circle at the bottom right corner shows the beam size. (a) The comparison between the Green Bank (GB) 4850 MHz (6 cm) image (Condon et al. 1994) and Urumqi 6 cm image (Sun et al. 2007). The GB 4850 MHz contours represent 9 mJy emission (about 3σ), while the Urumqi 6 cm contours (white) represent 5, 10, 15, 22, and 29 mK emission. (b) The GB 4850 MHz image. (c) The NRAO VLA Sky Survey (NVSS) 1.4 GHz image (Condon et al. 1998). (d) The Westerbork Northern Sky Survey (WENSS) 325 MHz image (Rengelink et al. 1997). (e) The TIFR GMRT (Giant Metrewave Radio Telescope) Sky Survey (TGSS) 150 MHz image (Intema et al. 2017). (f) The VLA Low-Frequency Sky Survey (VLSS) 74 MHz image (Cohen et al. 2007; Lane et al. 2014).
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: Top panel: the velocity-integrated 12CO intensity map of the Milky Way obtained from the CfA 1.2 m survey (Figure 2 in Dame et al. 2001). Middle panel: also the CfA 1.2 m 12CO image, but the enlarged view toward the second quadrant (including the Cassiopeia region). Bottom panel: the MWISP 12CO image, integrated between −25 and +10 km s−1 (i.e., Local arm only). For each panel, the blue line shows the Cassiopeia Filament. Note that all CO images in this work are from the MWISP survey and only the two panels here are from the CfA 1.2 m survey (to provide a complete molecular gas view of the Milky Way).
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: Bottom panel: the CO longitude–velocity (LV) diagram for the second quadrant with b ≤ 5.°25 (see also Yan et al. 2021). The green dashed line shows the central mean velocity of the Local arm (∼8 km s−1). Middle panel: the enlarged view of the LV diagram for the Local arm. The red dashed box shows the longitude and velocity range of the Cassiopeia Filament (but integrated with b ≤ 5.°25). Top panel: the CO PV diagram along the Cassiopeia Filament (similar to Figure 10), with respect to the central mean velocity of the Local arm.
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: (a) The locations of the Cassiopeia Filament projected onto the Galactic plane. The Galaxy center (red solar symbol) is at (0, 0) kpc, while the Sun (black solar symbol) is at (0, 8.15) kpc. The solid and dashed curved lines denote the arm center and widths fitted by Reid et al. (2019). (b) The enlarged view of the area enclosed by the dashed square in the left panel. The viewing angle of the Cassiopeia Filament is roughly 10° (132.°0 ≥ l ≥ 122.°0). The distance of the east filament and west shell is measured to be 188 pc and 553 pc, respectively.
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: The CO position–velocity (PV) diagram along the Cassiopeia Filament (from east to west). The gray-scale background image represents the 12CO emission, with the 5σ contour (blue; 1σ ∼ 0.2 K). The green contour shows the 4σ 13CO emission (1σ ∼ 0.12 K).
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: Top panel: the 12CO velocity field (moment 1 image) of the observed Cassiopeia region within the velocity range of [0.5, 4.5] km s−1. The unit of the scale bar is km s−1. Bottom panel: the 12CO velocity field of the shell region within the velocity range of [0, 7] km s−1. The black arrow lines show the routings of the PV diagram of Fingers 2 and 4.
Paper: The Cassiopeia Filament: A Blown Spur of the Local Arm
Authors: Xuepeng Chen, Li Sun, Jiancheng Feng, Shiyu Zhang, Weihua Guo, Xiaoyun Xu, Yang Su, Yan Sun, Shaobo Zhang, Xin Zhou, Zhiwei Chen, Qing-Zeng Yan, Miaomiao Zhang, Min Fang, Ji Yang
Figure caption: The CO PV diagrams along Fingers 4 (left) and 2 (right). The gray-scale background image represents the 12CO emission. The 12CO contours (black) start from 1 K and increase by a step of 1 K (1σ ∼ 0.2 K). The 13CO emission contours (green) start from 0.4 K and increase by a step of 0.4 K (1σ ∼ 0.12 K). The red ellipse shows the fitting toward the PV diagram with a velocity radius of 6.5 km s−1.
Paper: Hazy with a Chance of Star Spots: Constraining the Atmosphere of Young Planet K2-33b
Authors: Pa Chia Thao, Andrew W. Mann, Peter Gao, Dylan A. Owens, Andrew Vanderburg, Elisabeth R. Newton, Yao Tang, Matthew J. Fields, Trevor J. David, Jonathan M. Irwin, Tim-Oliver Husser, David Charbonneau, Sarah Ballard
Figure caption: Illustration of the effect of spots on the observed stellar spectrum using BT-SETTL atmosphere models for a star with T surf = 3500 K and T spot = 2800 K and spot coverage fractions of 80% (green), 50% (blue), and 20% (green). The left panel shows a moderate-resolution optical–NIR spectrum (matching the wavelength coverage and resolution as our observational data). As spectra only generally provide relative flux measurements, each model is normalized to yield the same total luminosity. The change over the three models is small in the optical and could largely be fit out by assuming a cooler surface temperature or higher reddening. However, as large spots have a much larger impact on the NIR spectrum, the combined data set can provide strong constraints on both T surf and T spot.
Paper: Hazy with a Chance of Star Spots: Constraining the Atmosphere of Young Planet K2-33b
Authors: Pa Chia Thao, Andrew W. Mann, Peter Gao, Dylan A. Owens, Andrew Vanderburg, Elisabeth R. Newton, Yao Tang, Matthew J. Fields, Trevor J. David, Jonathan M. Irwin, Tim-Oliver Husser, David Charbonneau, Sarah Ballard
Figure caption: Best-fit model of a planet with a flat transmission spectrum crossing a heavily spotted star along a pristine transit chord (blue). The observed transit depths are plotted in red circles, and the labeled bars at the bottom indicate which instruments took those observations. The yellow lines show 100 random samples in T spot, f  S , and T surf taken from our fit to the IGRINS spectra (see Section 5.2.3). None of the results drawn from the spectroscopic constraints are consistent with the data; the only samples that come the closest to the optical data fail to reproduce the Spitzer data. The results are similar using the posterior from our fit to the SNIFS+SpeX data.
Paper: Hazy with a Chance of Star Spots: Constraining the Atmosphere of Young Planet K2-33b
Authors: Pa Chia Thao, Andrew W. Mann, Peter Gao, Dylan A. Owens, Andrew Vanderburg, Elisabeth R. Newton, Yao Tang, Matthew J. Fields, Trevor J. David, Jonathan M. Irwin, Tim-Oliver Husser, David Charbonneau, Sarah Ballard
Figure caption: Left: example results from Fleck, showing a portion of the light curve (black points) and best-fit models (purple curves). The model only captures the mean variability, failing to capture the peaks and troughs because it does not include long-term spot evolution. Middle: posteriors of f  S . Right: three example stellar surfaces randomly pulled from our fit posteriors. The colors correspond to two (blue), three (red), and four (gray) spots. To explain the low variability in the light curve and the inferred spot coverage, the spots must cover a large portion of the star and be located at the poles.
Paper: Hazy with a Chance of Star Spots: Constraining the Atmosphere of Young Planet K2-33b
Authors: Pa Chia Thao, Andrew W. Mann, Peter Gao, Dylan A. Owens, Andrew Vanderburg, Elisabeth R. Newton, Yao Tang, Matthew J. Fields, Trevor J. David, Jonathan M. Irwin, Tim-Oliver Husser, David Charbonneau, Sarah Ballard
Figure caption: Posteriors of the ratio of the planet radius to the star radius (R  p /R *) from the POET MCMC fits for Spitzer Channel 1 (left) and Channel 2 (right) with a bin size of 30. Each color represents a different transit (AOR), where gray is used to highlight the outlier transit in each channel (AOR 60658432 in Channel 1 had a flare and AOR 60656128 in Channel 2 had poor pointing). The green dashed vertical line is the ratio of the planet radius to the star radius for K2, which does not overlap with any of the Spitzer data points, except for the outlier transit in Channel 2.
Paper: Hazy with a Chance of Star Spots: Constraining the Atmosphere of Young Planet K2-33b
Authors: Pa Chia Thao, Andrew W. Mann, Peter Gao, Dylan A. Owens, Andrew Vanderburg, Elisabeth R. Newton, Yao Tang, Matthew J. Fields, Trevor J. David, Jonathan M. Irwin, Tim-Oliver Husser, David Charbonneau, Sarah Ballard
Figure caption: Corner plot of T spot and f  S  from fitting a flat planetary transmission spectrum to the observed transit depths and assuming a pristine transit chord (blue) compared to the same parameters constrained by fitting the stellar spectrum from IGRINS (black) or SNIFS+SpeX (red) spectra with a two-temperature model. Some solutions with low f  S  and low T spot values were trimmed for clarity.
Paper: Hazy with a Chance of Star Spots: Constraining the Atmosphere of Young Planet K2-33b
Authors: Pa Chia Thao, Andrew W. Mann, Peter Gao, Dylan A. Owens, Andrew Vanderburg, Elisabeth R. Newton, Yao Tang, Matthew J. Fields, Trevor J. David, Jonathan M. Irwin, Tim-Oliver Husser, David Charbonneau, Sarah Ballard
Figure caption: Top: Stacked phase-folded light curve of K2-33 observed in K2 (pink), MEarth (blue), Spitzer/Channel 1 (purple), Spitzer/Channel 2 (orange), and HST (green). The HST data here are the white light curve. The data points correspond to the light curve binned in phase using a bin size of 10, 200, 1500, and 1500 for K2, MEarth, Channel 1, and Channel 2, respectively. The solid line corresponds to the best-fit (highest-likelihood) model from our MCMC fit. Typical error bars are derived from the scatter in the out-of-transit data points. The transit depth for the optical wavelengths is ∼2 times deeper than the transit depth for the near-infrared wavelengths. Bottom: Residuals using the binned points.
Paper: Hazy with a Chance of Star Spots: Constraining the Atmosphere of Young Planet K2-33b
Authors: Pa Chia Thao, Andrew W. Mann, Peter Gao, Dylan A. Owens, Andrew Vanderburg, Elisabeth R. Newton, Yao Tang, Matthew J. Fields, Trevor J. David, Jonathan M. Irwin, Tim-Oliver Husser, David Charbonneau, Sarah Ballard
Figure caption: K2 light curve of K2-33 after removing signals from the pointing drift of the telescope (gray points). The pink shaded region shows the 3σ range of fits from the GP variability fit, while the pink solid line shows the combined GP and the transit model.
Paper: Hazy with a Chance of Star Spots: Constraining the Atmosphere of Young Planet K2-33b
Authors: Pa Chia Thao, Andrew W. Mann, Peter Gao, Dylan A. Owens, Andrew Vanderburg, Elisabeth R. Newton, Yao Tang, Matthew J. Fields, Trevor J. David, Jonathan M. Irwin, Tim-Oliver Husser, David Charbonneau, Sarah Ballard
Figure caption: White light curve of K2-33 observed with HST/WFC3. The top panel shows the raw normalized data (green circles) overplotted with the systematic model (gray line). The middle panel shows the best-fit model (gray line) from our MCMC fit overplotted with the systematic-corrected data (green circles). The bottom panel shows residuals from the light curve.