adsabs/AstroCLIMB huggingface dataset:
Paper: Refining the Masses and Radii of the Star Kepler-33 and its Five Transiting Planets
Authors: James Sikora, Jason Rowe, Daniel Jontof-Hutter, Jack J. Lissauer
Figure caption:  O−C diagram for planets c, d, e, and f. Black points are associated with the measured transit times as retrieved from DR25 (Thompson et al. 2018). Green/yellow lines correspond to the O−C values predicted by the photodynamics analysis.
Paper: Refining the Masses and Radii of the Star Kepler-33 and its Five Transiting Planets
Authors: James Sikora, Jason Rowe, Daniel Jontof-Hutter, Jack J. Lissauer
Figure caption: Same as Figure 1 but showing the TTV contributions from planet e (left) and planet f (right) by setting the mass of planet e and f to zero, respectively, and recalculating the models.
Paper: Toward the Automated Detection of Light Echoes in Synoptic Surveys: Considerations on the Application of Deep Convolutional Neural Networks
Authors: Xiaolong Li, Federica B. Bianco, Gregory Dobler, Roee Partoush, Armin Rest, Tatiana Acero-Cuellar, Riley Clarke, Willow Fox Fortino, Somayeh Khakpash, Ming Lian
Figure caption: Example of a template-subtracted (hereafter “difference”) image from the ATLAS survey (see Section 3 for details). The native resolution of the difference image is 1800 × 1800 pixels, corresponding to about 1 square degree. The images are template-subtracted to aid detectability of the faint, time-evolving LE features. The full-frame image (left) contains an LE in the top left corner, as well as stars and artifacts throughout. Because of the rarity of LEs, in order to mitigate class imbalance between stars and LEs in our data set, we split each ATLAS image into nine tiles and select only the tiles that contain LEs. The top left tile of this image that contains an LE is marked by an orange frame and is reproduced to the right with boxes corresponding to saturated stars, star streaks, and LEs are shown in blue, teal, and red, respectively.
Paper: Toward the Automated Detection of Light Echoes in Synoptic Surveys: Considerations on the Application of Deep Convolutional Neural Networks
Authors: Xiaolong Li, Federica B. Bianco, Gregory Dobler, Roee Partoush, Armin Rest, Tatiana Acero-Cuellar, Riley Clarke, Willow Fox Fortino, Somayeh Khakpash, Ming Lian
Figure caption: Slice of the geometry of the LE phenomenon (left) and its projection on the plane of the sky (right) in the case of a continuous dust sheet (top) and dust filaments (bottom). At each point in time, for every transient, there is an ellipsoidal surface with foci at the Earth and the transient. All points on the ellipsoid reflect light from the transient that arrive on Earth at the same time, and the ellipsoid itself expands over time. Due to the increase in path length, LEs reach the observer after the light from the original transient did. On the plane of the sky, we see the cross section of the reflection ellipsoid; yet not all LEs are circles: in most cases only a portion of the ellipsoid will have dust that reflects the light echo toward Earth. Most observed LEs are only arcs of a circle.
Paper: Toward the Automated Detection of Light Echoes in Synoptic Surveys: Considerations on the Application of Deep Convolutional Neural Networks
Authors: Xiaolong Li, Federica B. Bianco, Gregory Dobler, Roee Partoush, Armin Rest, Tatiana Acero-Cuellar, Riley Clarke, Willow Fox Fortino, Somayeh Khakpash, Ming Lian
Figure caption: Architecture of the YOLOv3. An input image is mapped to a tensor of shape S × S × N  b  × (5 + N  c ) through a deep neural network model as described in Section 4.1. Each cell of the S × S grid is responsible for both class prediction and bounding-box regression of objects whose centers fall inside the cell. The YOLOv3 model makes predictions at three size scales (1/8, 1/16, 1/32 of the image size).
Paper: Toward the Automated Detection of Light Echoes in Synoptic Surveys: Considerations on the Application of Deep Convolutional Neural Networks
Authors: Xiaolong Li, Federica B. Bianco, Gregory Dobler, Roee Partoush, Armin Rest, Tatiana Acero-Cuellar, Riley Clarke, Willow Fox Fortino, Somayeh Khakpash, Ming Lian
Figure caption: Distribution of number of bounding boxes per image (left) and bounding-box sizes across all images (right) for the three labeled classes: LEs, stars, and “other” (including satellite and star streaks and other artifacts). After augmentation (see Figure 4), the final data set contains 224 images, 584 boxes labeled as LEs, 1256 labeled as stars, and 648 as other. On average, each image contains 3 LEs, 6 stars, and 3 “other” objects. The size of the bounding boxes is measured as the ratio of the diagonal of the box to the diagonal of the image. In these units, the mean size of LE and “other” boxes is ∼0.1 (∼3′), while the stars are smaller, ∼0.06 (∼1.′8).
Paper: Toward the Automated Detection of Light Echoes in Synoptic Surveys: Considerations on the Application of Deep Convolutional Neural Networks
Authors: Xiaolong Li, Federica B. Bianco, Gregory Dobler, Roee Partoush, Armin Rest, Tatiana Acero-Cuellar, Riley Clarke, Willow Fox Fortino, Somayeh Khakpash, Ming Lian
Figure caption: Sky positions of 17 LEs contained in our final data set: 10 of them are from the Tycho SN, and 2 are from Cas A. The rest have positions and orientations that are inconsistent with both Tycho and Cas A and are of as-of-yet unknown origin. LEs are preferentially found in high-dust-content regions, such as near the Galactic plane, which is indicated by a thick blue line in this plot. The right panel shows a zoom-in view of the region containing the majority of the LEs recovered in our data. Table 3 contains the coordinate of each of the LEs in this figure.
Paper: Toward the Automated Detection of Light Echoes in Synoptic Surveys: Considerations on the Application of Deep Convolutional Neural Networks
Authors: Xiaolong Li, Federica B. Bianco, Gregory Dobler, Roee Partoush, Armin Rest, Tatiana Acero-Cuellar, Riley Clarke, Willow Fox Fortino, Somayeh Khakpash, Ming Lian
Figure caption: Image augmentations applied to the ATLAS data set: the images generated by subdividing the original ATLAS data are first flipped horizontally, and then rotated by 90°, 180°, and 270°. This augmentation increases our data set size by a factor of 8.
Paper: Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere
Authors: Li Zhou, Bo Ma, Yonghao Wang, Yinan Zhu
Figure caption: (a) The detector image of forward scan in the first visit. The zeroth order and first order can be seen, from which we extract the spectrum. Flux in the white region is estimated. The region in the white square is photometric aperture. (b) Extracted 1D spectrum using Iraclis.
Paper: Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere
Authors: Li Zhou, Bo Ma, Yonghao Wang, Yinan Zhu
Figure caption: Spectral light curves for the transmission spectra. Left panel: the detrended spectral light curves with best-fit model plotted. The right panel reveals the residuals. For each spectra, we present the values of σ, chi-square (χ 2), and the AC.
Paper: Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere
Authors: Li Zhou, Bo Ma, Yonghao Wang, Yinan Zhu
Figure caption: Vertical (Δy) and horizontal (Δx) shifts for each image relative to the first one, the sky ratio and raw flux of each image in the visit. Black: forward scan. Red: reverse scan. Here we take the first visit for example.
Paper: Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere
Authors: Li Zhou, Bo Ma, Yonghao Wang, Yinan Zhu
Figure caption: Panels (a) and (b) show the white light curves and residuals for best-fit models of five individual transit observations, respectively. Panel (c): transmission spectrum collected from each visit (colored data points) and the final combined transmission spectrum (black data points). Panel (d): uncertainty of each data point. Panel (e): deviation from the weighted-average spectrum, in unit of sigma, for each data point.
Paper: Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere
Authors: Li Zhou, Bo Ma, Yonghao Wang, Yinan Zhu
Figure caption: The spectrum of different atmospheric models of HST/WFC3.
Paper: Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere
Authors: Li Zhou, Bo Ma, Yonghao Wang, Yinan Zhu
Figure caption: Simulated spectrum of JWST/NIRISS GR700XD. Theoretic spectral model of L 98-59 b in the wavelength range of JWST/NIRISS GR700XD for a single transit visit. If HCN is present, JWST will be able to confirm its presence.
Paper: Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere
Authors: Li Zhou, Bo Ma, Yonghao Wang, Yinan Zhu
Figure caption: Contamination of the transmission spectrum of L 98-59 b from different stellar activity models. Lines with the same color represent stellar contamination models with different filling factors. The solid and dashed lines represent the transit light source effect for the maximum and mean spot or faculae filling factor, respectively.
Paper: Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere
Authors: Li Zhou, Bo Ma, Yonghao Wang, Yinan Zhu
Figure caption: The abundance of molecules range with different metallicity (0.1–1000×solar metallicity) using equilibrium chemistry model.
Paper: Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere
Authors: Li Zhou, Bo Ma, Yonghao Wang, Yinan Zhu
Figure caption: The abundance of molecules range with different C/O ratios using equilibrium chemistry model.
Paper: Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere
Authors: Li Zhou, Bo Ma, Yonghao Wang, Yinan Zhu
Figure caption: The atmospheric retrieval parameters of the best-fit model (model 4) for L 98-59 b.
Paper: Hubble WFC3 Spectroscopy of the Rocky Planet L 98–59 b: No Evidence for a Cloud-free Primordial Atmosphere
Authors: Li Zhou, Bo Ma, Yonghao Wang, Yinan Zhu
Figure caption: Same as Figure 6, but for the flatline pure cloudy model (model 5).
Paper: Characterizing and Mitigating Telluric Absorption in Precise Radial Velocities. II. A Study of an M2-type Star
Authors: Natasha Latouf, Sharon Xuesong Wang, Bryson Cale, Peter Plavchan
Figure caption: Telluric line–induced RV errors as a function of wavelength for each order in our simulation for the RV extraction methods listed in Section 2. In the top two plots, each point shows the rms value of the RVs extracted from one spectral order across one year (365 nights) each. The top left plot shows how using an incorrect line profile introduces more error into the analysis. The top right plot portrays how forward modeling generally has a lower rms than CCF + division, especially in the NIR. The bottom plot is the smoothed version of the top plots, for more clarity, with a window size of 11 orders and a moving average.
Paper: Characterizing and Mitigating Telluric Absorption in Precise Radial Velocities. II. A Study of an M2-type Star
Authors: Natasha Latouf, Sharon Xuesong Wang, Bryson Cale, Peter Plavchan
Figure caption: The relationship between the RV error and the stellar RV information content for both the M-dwarf and Kurucz solar models. The top left plot shows the M-dwarf RV error vs. the stellar RV information content, and the bottom left plot shows the solar RV error vs. the stellar RV information content. In the left plot, the “no correction” results are shown in gray, the K-profile division results are shown in orange, and the K-profile forward-model results are shown in blue.
Paper: Characterizing and Mitigating Telluric Absorption in Precise Radial Velocities. II. A Study of an M2-type Star
Authors: Natasha Latouf, Sharon Xuesong Wang, Bryson Cale, Peter Plavchan
Figure caption: Telluric-induced RV errors for each photometric band. The horizontal lines mark the photon-limited precision for S/N = 100 per pixel in each band. The lower ends of the vertical lines mark the RV rms shown in Table 2, and the upper ends of the lines mark the range of RV systematics (the 95% percentile range) from the simulation methods listed in Table 2.
Paper: Characterizing and Mitigating Telluric Absorption in Precise Radial Velocities. II. A Study of an M2-type Star
Authors: Natasha Latouf, Sharon Xuesong Wang, Bryson Cale, Peter Plavchan
Figure caption: RV signal as a function of time in units of days for the four RV extraction methods described in Section 2, for the broad optical (left) and the NIR (right), for an EFE spectrograph. Shown in purple is an RV analog of Earth’s signal (semi-amplitude of 25 cm s−1). We assume S/N = 100 per pixel for R = 120,000.
Paper: Characterizing and Mitigating Telluric Absorption in Precise Radial Velocities. II. A Study of an M2-type Star
Authors: Natasha Latouf, Sharon Xuesong Wang, Bryson Cale, Peter Plavchan
Figure caption: Extracted RVs from 365 nights as functions of airmass, PWV, and BC for three methods: no correction (left), CCF + division with the K-profile for tellurics (middle), and forward modeling with the K-profile for tellurics (right). Each data point is a weighted average of the reported RVs for all orders from 350 to 2500 nm, the entire wavelength range in our simulations. The weights assume S/N= 400 per pixel and combine photon noise with telluric-induced RV rms, as described in W22, Section 2, and as used in the presented data in Table 1.
Paper: Characterizing and Mitigating Telluric Absorption in Precise Radial Velocities. II. A Study of an M2-type Star
Authors: Natasha Latouf, Sharon Xuesong Wang, Bryson Cale, Peter Plavchan
Figure caption: Example spectral orders are shown on the left, with their corresponding RVs vs. BC on the right, when specifically ignoring tellurics during RV extraction, i.e., CCF + no correction. The left plots show the M-dwarf spectra in blue and the telluric spectra in orange, for each order, with the telluric absorption for order #28 shown in the top left panel being amplified by 10 in flux for better visibility.
Paper: Characterizing and Mitigating Telluric Absorption in Precise Radial Velocities. II. A Study of an M2-type Star
Authors: Natasha Latouf, Sharon Xuesong Wang, Bryson Cale, Peter Plavchan
Figure caption: The rms of the flux residuals vs. the telluric absorption depth from forward modeling iSHELL spectra at K band (2.8–2.41 μm), plotted with chunks of our simulations that match these wavelengths. Each point represents a residual flux rms that corresponds to a small range of telluric absorption (≈±1%).
Paper: Characterizing and Mitigating Telluric Absorption in Precise Radial Velocities. II. A Study of an M2-type Star
Authors: Natasha Latouf, Sharon Xuesong Wang, Bryson Cale, Peter Plavchan
Figure caption: Histograms of the best-fit telluric shift parameters for three iSHELL orders and corresponding best-fit normal distributions for the histograms (in units of m s−1). Order 5 (m = 216) has considerably more features from water than orders 9 (m = 220) and 17 (m = 228).
Paper: Adaptive Optics Imaging Can Break the Central Caustic Cusp Approach Degeneracy in High-magnification Microlensing Events
Authors: Sean K. Terry, David P. Bennett, Aparna Bhattacharya, Naoki Koshimoto, Jean-Philippe Beaulieu, Joshua W. Blackman, Ian A. Bond, Andrew A. Cole, Jessica R. Lu, Jean Baptiste Marquette, Clément Ranc, Natalia Rektsini, Aikaterini Vandorou
Figure caption: Close stellar binary mass–distance relation for OGLE-2011-BLG-0950L with constraints from the Keck K-band lens flux measurement in red and the angular Einstein radius from the direct measurement of μ rel in green. The individual masses are measured to be ﹩{M}_{{\rm{A}}}={1.12}_{-0.09}^{+0.11}﹩ and ﹩{M}_{{\rm{B}}}={0.47}_{-0.10}^{+0.13}\,{M}_{\odot }﹩.
Paper: Search for an Alien Message to a Nearby Star
Authors: Michaël Gillon, Artem Burdanov, Jason T. Wright
Figure caption: Left: 10′ by 10′ crop of the center of the stack (mean) of all images taken by TRAPPIST-South during the night of 2015 September 4–5. The position of the hypothetical FICD (under the assumptions of Section 2) between 2015 August 26 and 2016 August 26 is shown in red. This large motion on the sky is due the parallax effect combined with the compensation for the proper motion of Wolf 359. Right: 10″ by 10″ zoom-in on the path of the hypothetical FICD during the observations of TRAPPIST-South on 2015 September 4–5 (yellow line). The red plus sign shows the position that should have occupied the FICD at the inferior conjunction of Earth (i.e., in the middle of our planet’s transit as seen from the FICD). The bright spot at the east of the FICD location is a hot pixel cluster.
Paper: Search for an Alien Message to a Nearby Star
Authors: Michaël Gillon, Artem Burdanov, Jason T. Wright
Figure caption: Illustration of the Sun (black circle) as seen from the hypothesized FICD. The blue circle represents the ER, i.e., the ring for which photons from the FICD will reach the target receptor. Its actual thickness is a few centimeters. The small red circles represent the laser beams emitted by the FICD in the Sun’s plane. For this illustration, an impact parameter of 1.1 and a laser wavelength and waist of 500 nm and 1 m, respectively, were assumed. Each laser beam is ∼2.5 times wider than Earth.
Paper: Search for an Alien Message to a Nearby Star
Authors: Michaël Gillon, Artem Burdanov, Jason T. Wright
Figure caption: Evolution of the impact parameter of Earth as seen from the “solar gravitational line” (SGL) of Wolf 359 around the TRAPPIST-South observations of 2015. The red line corresponds to an impact parameter of 1.1. The green zone corresponds to the TRAPPIST-South observations. The intersection of the red and black lines corresponds to the crossing of the putative FICD’s beam by Earth.
Paper: Search for an Alien Message to a Nearby Star
Authors: Michaël Gillon, Artem Burdanov, Jason T. Wright
Figure caption: Sky-subtracted light curve of the source located approximately at the position of the hypothetical FICD in the TRAPPIST-South images. The points in red have a significant flux excess. The first group of red points is due to the passage of a g ∼ 19.5 asteroid in the aperture. We attributed the other outlier to a cosmic hit.
Paper: Search for an Alien Message to a Nearby Star
Authors: Michaël Gillon, Artem Burdanov, Jason T. Wright
Figure caption: Illustration showing the geometry of the hypothesized communication link from the solar system to the Wolf 359 system. The distances and sizes are not to scale. Wolf 359 is shown at three different positions. Position 1 corresponds to the time of the emission of the photons that we receive from it now. Position 2 corresponds to its current position. Position 3 corresponds to the time at which it will receive the photons emitted now by the transmitter T (R = receptor).
Paper: Search for an Alien Message to a Nearby Star
Authors: Michaël Gillon, Artem Burdanov, Jason T. Wright
Figure caption: Same as Figure 3, but for the 150 first images taken by SPECULOOS-South/Europa of 2018 September 4–5. The whole stack of the images (left) is smaller than 10′ × 10′ because of the shift of the images due to the tracking problem experienced by the telescope during the night.
Paper: More Evidence for Variable Helium Absorption from HD 189733b
Authors: Michael Zhang, P. Wilson Cauley, Heather A. Knutson, Kevin France, Laura Kreidberg, Antonija Oklopčić, Seth Redfield, Evgenya L. Shkolnik
Figure caption: Comparison of the average depth of the helium line that we find (in green) to literature values, measured by CARMENES and GIANO. All averages are computed between the end of ingress and beginning of egress in time, and between −20 and 20 km s−1 in planet-centric wavelength space.
Paper: More Evidence for Variable Helium Absorption from HD 189733b
Authors: Michael Zhang, P. Wilson Cauley, Heather A. Knutson, Kevin France, Laura Kreidberg, Antonija Oklopčić, Seth Redfield, Evgenya L. Shkolnik
Figure caption: Excess absorption in percent, as a function of time and wavelength. The diagonal red lines represent the wavelengths of the helium lines. The horizontal white light represent the beginning of ingress and end of egress in white light.(The data used to create this figure are available.)
Paper: More Evidence for Variable Helium Absorption from HD 189733b
Authors: Michael Zhang, P. Wilson Cauley, Heather A. Knutson, Kevin France, Laura Kreidberg, Antonija Oklopčić, Seth Redfield, Evgenya L. Shkolnik
Figure caption: Average in-transit excess absorption spectrum from beginning of ingress to end of egress, in the planetary frame. The red lines represent the wavelengths of the three helium lines.
Paper: More Evidence for Variable Helium Absorption from HD 189733b
Authors: Michael Zhang, P. Wilson Cauley, Heather A. Knutson, Kevin France, Laura Kreidberg, Antonija Oklopčić, Seth Redfield, Evgenya L. Shkolnik
Figure caption: Excess absorption spectra obtained by the three instruments averaged over three transits (CARMENES), five transits (GIANO-B), and one transit (NIRSPEC). CARMENES and GIANO-B spectra are convolved to the NIRSPEC resolution of 37,500, resulting in the artificial smoothness of the CARMENES spectrum. These spectra are computed from the end of ingress to beginning of ingress, unlike Figure 2, which is computed from the beginning of ingress to end of egress. CARMENES and GIANO-B spectra were kindly provided by the authors of the respective papers.
Paper: More Evidence for Variable Helium Absorption from HD 189733b
Authors: Michael Zhang, P. Wilson Cauley, Heather A. Knutson, Kevin France, Laura Kreidberg, Antonija Oklopčić, Seth Redfield, Evgenya L. Shkolnik
Figure caption: Reconstructed stellar spectrum using two methods. The two methods differ blueward of 1450 Å, where we use Lampón et al. (2021b) for method 1 and our own reconstruction for method 2. Note the large discrepancy in the EUV.
Paper: More Evidence for Variable Helium Absorption from HD 189733b
Authors: Michael Zhang, P. Wilson Cauley, Heather A. Knutson, Kevin France, Laura Kreidberg, Antonija Oklopčić, Seth Redfield, Evgenya L. Shkolnik
Figure caption: Relationship between maximum excess absorption depth in our 1D models and the stellar EUV flux at 1 au. Blue points represent XUV stellar spectra scaled from the spectrum of Lampón et al. (2021b), while red points represent XUV spectra scaled from our own spectrum.
Paper: More Evidence for Variable Helium Absorption from HD 189733b
Authors: Michael Zhang, P. Wilson Cauley, Heather A. Knutson, Kevin France, Laura Kreidberg, Antonija Oklopčić, Seth Redfield, Evgenya L. Shkolnik
Figure caption: Light curve of the region [−20, 15] km s−1 from the main helium peak, in the stellar frame. The beginning of ingress and end of egress are marked by the vertical black dotted and solid lines. Note the stellar activity that follows the transit.