adsabs/AstroCLIMB huggingface dataset:
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: F250M (red), F150W (green), and F090W (blue) three-color image of JWST ERS north field overlaid with type 1 objects (in FUV and near CO; red circles), type 2 objects (in FUV and away from CO; blue circles), type 3 objects (away from FUV and away from CO; yellow), resolved background galaxies (magenta circles), and CO cores (orange circles). The orientation of the image is such that north is up and east is to the left.
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: F250M (red), F150W (green), and F090W (blue) three-color image postage stamps of select type 1 objects (red circles) and the individual NIR sources within (gray, dashed circles) that we used to compare photometry between our larger objects and the smaller, individual sources within. We also overlay the CO cores (orange circles) inside the type 1 objects. The orientation of the image is such that north is up and east is to the left.
Paper: Probing the Relationship Between Early Star Formation and CO in the Dwarf Irregular Galaxy WLM with JWST
Authors: Haylee N. Archer, Deidre A. Hunter, Bruce G. Elmegreen, Monica Rubio, Phil Cigan, Rogier A. Windhorst, Juan R. Cortés, Rolf A. Jansen
Figure caption: Color–color diagram of F090W–F150W vs. F250M–F430M for type 1 objects (red circles) and resolved NIR sources within type 1 objects (gray diamonds). The black line corresponds to the effective temperature of a blackbody.
Paper: Motion Planning for the Robotic Fiber Positioners of the Large Sky Area Multiobject Fiber Spectrocopy Telescope
Authors: Feifan Zhang, Baolong Chen, Yu Wang, Zhenwan Peng, Zengxiang Zhou, Jianping Wang
Figure caption: Possible interference between the WR and its neighbors. (a; left) The WR is blocked from reaching its target by its neighbor. (b; right) When in a standstill at the home position, the WR will interfere with its neighbors.
Paper: Motion Planning for the Robotic Fiber Positioners of the Large Sky Area Multiobject Fiber Spectrocopy Telescope
Authors: Feifan Zhang, Baolong Chen, Yu Wang, Zhenwan Peng, Zengxiang Zhou, Jianping Wang
Figure caption: Schematic of the RRT algorithm.
Paper: Surviving Tidal Tails Around the Milky Way Bulge Globular Cluster NGC 6355
Authors: Andrés E. Piatti
Figure caption: Synthetic Milky Way color–magnitude diagram generated using the TRILEGAL code for a circular region centered on NGC 6355 and with a radius equals to the cluster radius. The red line is an isochrone for the cluster astrophysical properties (Souza et al. 2023), while the solid and dashed blue lines enclose the selected region and two control regions, respectively.
Paper: Surviving Tidal Tails Around the Milky Way Bulge Globular Cluster NGC 6355
Authors: Andrés E. Piatti
Figure caption: Milky Way synthetic stellar density map built from star counts of stars distributed within the red-giant-branch segment, generated using TRILEGAL (see text for details).
Paper: Surviving Tidal Tails Around the Milky Way Bulge Globular Cluster NGC 6355
Authors: Andrés E. Piatti
Figure caption: Interstellar extinction (E(B − V)) map across the observed NGC 6355 field. The black circle represents the cluster radius Piatti et al. (2019).
Paper: Surviving Tidal Tails Around the Milky Way Bulge Globular Cluster NGC 6355
Authors: Andrés E. Piatti
Figure caption: Color–magnitude diagram for all the measured stars in the field of NGC 6355, with their respective photometric errors. Black and gray dots represent stars located inside and outside a circle of radius equals to three times the cluster’s half-mass radius (0.022 deg), respectively. The red line is an isochrone for the cluster astrophysical properties (Souza et al. 2023).
Paper: Surviving Tidal Tails Around the Milky Way Bulge Globular Cluster NGC 6355
Authors: Andrés E. Piatti
Figure caption: Map of normalized background subtracted stellar densities. Only regions with η ≥3 are plotted (see text for details).
Paper: Surviving Tidal Tails Around the Milky Way Bulge Globular Cluster NGC 6355
Authors: Andrés E. Piatti
Figure caption: Same as Figure 4 using the present DECam observations.
Paper: Surviving Tidal Tails Around the Milky Way Bulge Globular Cluster NGC 6355
Authors: Andrés E. Piatti
Figure caption: Map of normalized background subtracted stellar densities of stars distributed within the red-giant-branch segment (see Figure 3). Contours for η = 4, 6, 8, and 10 are drawn with with to black lines, respectively. The arrows indicates the direction to the Milky Way center. The black circle represents the cluster radius (0.1 deg; Piatti et al. 2019), which is equivalent to 14.9 pc.
Paper: Surviving Tidal Tails Around the Milky Way Bulge Globular Cluster NGC 6355
Authors: Andrés E. Piatti
Figure caption: Spatial distribution of stars with action ratios within 1σ the cluster mean values. Data points arise from the Grondin et al. (2024)'s models.
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: The top plot shows the simulated flux time series of an active star drawn from the GP model described in Section 2.1. This data set corresponds to an observation of 4 days with an exposure time of 2 minutes. The mean of this signal consists of a periodic transit signal of period P = 0.7 days, duration D = 1.2 hr, and depth Δ = 2% (dark gray) plus an instrumental signal (blue). Correlated noise in the form of stellar variability is simulated with an SHO kernel of hyperparameters ω = π/6D, Q = 45, and σ = Δ. Finally, white noise with a standard deviation of 0.1% is added to the diagonal of the covariance matrix.
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Illustration of the effect of correlated noise on a single transit S/N. An hour-long transit of depth 0.5% is generated on top of white noise (standard deviation of 0.15%) as part of a 24 hr observation with an exposure time of 1 minute (top). Then, in the bottom plot, correlated noise is added, generated using a GP with an SHO kernel of hyperparameters ω = 60, Q = 0.5, and σ = Δ/4. The S/N on the right of each light curve is computed using Equation (2). Models used to simulate these data are provided in Section 2.1.
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Demonstration of the search of transiting exocomets in the TESS light curves of the star β Pictoris (2 minutes PDCSAP data from sector 33). This star is known to display rapid δ Scuti type photometric variations with a period of about 30 minutes (Lecavelier des Etangs et al. 2022). The GP kernel and its hyperparameters are chosen and optimized as in Section 4.2. Here, we simply used the linear search of nuance with a different base model, one that mimics the shape of transiting exocomets (with 20 trial durations), to compute the S/N time series of the signal over one sector. The maximum-S/N events are displayed at the bottom of the figure and match with the ones found by Lecavelier des Etangs et al. (2022).
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Study of nuance (black line) processing time against bi-weight+BLS (see Section 4.1, blue line). The gray curve shows the performance of nuance linear search when applied to chunks of 10,000 points continuous observations, instead of considering these observations all together. This study is performed on a single CPU core of an Apple M2 Max chip. While not being shown, we verify that both the BLS algorithm and nuance processing times scale linearly with the number of trial transit durations and orbital periods.
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Results of the transits injection–recovery on TIC 1019692 half-sector light curve. Left: cleaned light curve with computed trend overplotted in black (except for nuance where it corresponds to the mean of the GP model). Right: results of the transit search where a black square denotes a transit signal not detected, gray a signal detected at an alias period (P/2 or 2P), and white a signal detected with the correct period. On the right plots, secondary axes show the (τ, δ) relative parameter space. For each method, the upper right legend on the left plot indicates its ranking based on the percent of recovered transit signals (where a transit with an aliased period counts as being detected).
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Transit-search S/N periodograms of TOI-540 using bi-weight+BLS and nuance. After a first periodic search (left panel), the epochs corresponding to the maximum-S/N transit are masked before the second search is performed (right panel).
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Rate of true and false positives of nuance compared to other methods, as a function of the relative parameters τ and δ. The solid blue line corresponds to the maximum of true positives among all methods on the top panel (dominated by the harmonics+BLS method), and the minimum of false positives on the bottom panel (waned by the GP+BLS method, all other methods being above nuance).
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Rate of true and false positives of nuance compared to other methods, as a function of the injected planet’s radius. The solid blue line corresponds to the maximum of true positives among all other methods than nuance (dominated by the harmonics+BLS method).
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Sector 4 light curve of TOI-540. The cleaned signal (gray points) has been masked for flares (black points), and the black line corresponds to the mean of the GP model.
Paper:  nuance: Efficient Detection of Planets Transiting Active Stars
Authors: Lionel J. Garcia, Daniel Foreman-Mackey, Catriona A. Murray, Suzanne Aigrain, Dax L. Feliz, Francisco J. Pozuelos
Figure caption: Rate of true and false positives binned over the full parameter space (τ, δ) for all methods and all targets.
Paper: Dense Outflowing Molecular Gas in Massive Star-forming Regions
Authors: Yani Xu, 雅霓 徐, Junzhi Wang, 均智 王, Shu Liu, 姝 刘, Juan Li, 娟 李, Yuqiang Li, 郁强 李, Rui Luo, 睿 罗, Chao Ou, 超 欧, Siqi Zheng, 思琪 郑, Yijia Liu, 怡嘉 刘
Figure caption: The line wing spatial distributions of HCO+ 3-2. The source names are shown in the panels. Each panel shows the velocity integrated intensity distribution of blue and/or red wings traced by HCO+ 3-2. The grayscales illustrate the positions of cloud cores traced by H13CO+ 3-2. The cyan dotted line boxes indicate signal coverage. The detailed parameters for maps of this and other sources are presented in Table 2.
Paper: Dense Outflowing Molecular Gas in Massive Star-forming Regions
Authors: Yani Xu, 雅霓 徐, Junzhi Wang, 均智 王, Shu Liu, 姝 刘, Juan Li, 娟 李, Yuqiang Li, 郁强 李, Rui Luo, 睿 罗, Chao Ou, 超 欧, Siqi Zheng, 思琪 郑, Yijia Liu, 怡嘉 刘
Figure caption: The averaged spectral lines of HCN and HCO+ 3-2. The source names are shown in the panels. Each panel presents the spectra of HCO+ or HCN (black) and H13CO+ or H13CN (red) 3-2 after averaging all the spectral lines within the signal area. The blue and red line wing emissions are labeled with blue windows. The green line is the Gaussian fitting of the spectral line of H13CO+ or H13CN 3-2.
Paper: Spectroastrometric Survey of Protoplanetary Disks with Inner Dust Cavities
Authors: Stanley K. Jensen, Sean D. Brittain, Andrea Banzatti, Joan R. Najita, John S. Carr, Joshua Kern, Janus Kozdon, Jonathan Zrake, Jeffrey Fung
Figure caption: Modeled line profiles and SA signals for the sample. The SA signal and average line profile are plotted for each target (black lines in the upper and lower panels, respectively). The PA of the slit is indicated for the observation presented in the figure. The horizontal black bars indicate the instrumental resolution of the observation. The best-fit models are plotted in blue, and the residuals between the data and the fits are plotted above in red. The Doppler shift has been corrected for Earth’s motion and the radial velocity of the star using the values presented in Table 2. For the targets with multiple observations or epochs, those shown here are as follows: HD 169142 is averaged between 2017 April 20 and August 25; CQ Tau is from 2023 January 21; V892 Tau is from 2021 January 16; and AB Aur is from 2021 February 6. The velocity range affected by telluric correction of the low-J CO lines is indicated with vertical gray lines. For HD 169142, the data from two nights separated by 4 months were combined so two velocity ranges are indicated. The range containing telluric absorption for AB Aur falls outside of the plotted velocity range. The SA data provide a measure of the shift of the PSF (emission line and continuum) and should not be confused with the maximum spatial offset of the emission line.
Paper: Spectroastrometric Survey of Protoplanetary Disks with Inner Dust Cavities
Authors: Stanley K. Jensen, Sean D. Brittain, Andrea Banzatti, Joan R. Najita, John S. Carr, Joshua Kern, Janus Kozdon, Jonathan Zrake, Jeffrey Fung
Figure caption: HD 179218 line profile (top panel) and SA signal (lower panel). In the upper panel, the average profile of all three observations is presented (in black). The difference between the average profile and the profile from each observation is plotted above. The horizontal black line indicates the instrumental resolution of the observation. HD 179218 was observed in 2016 (Brittain et al. 2018) with the slit aligned with the semimajor axis (in red) and in 2020 with the slit aligned with the semimajor axis (in blue) and the semiminor axis (in green). There is no evidence of variability in the line profile—either temporally or due to changes in the orientation of the slit. In the lower panel, the SA signal for each date and PA are plotted using the same color scheme. The average of the SA signal measured with the slit aligned with the semimajor axis of the disk (in black) is also plotted. The SA signals measured in 2016 and 2020 are consistent.
Paper: Spectroastrometric Survey of Protoplanetary Disks with Inner Dust Cavities
Authors: Stanley K. Jensen, Sean D. Brittain, Andrea Banzatti, Joan R. Najita, John S. Carr, Joshua Kern, Janus Kozdon, Jonathan Zrake, Jeffrey Fung
Figure caption: LkHα 330 profile (black) and its reflection (blue) showing asymmetric structure. The velocity ranges covering the low-J v = 1−0 telluric lines are indicated in red. The horizontal black line indicates the instrumental resolution of the observation. The core of the line and the wings reveal a significant asymmetry. The half-width at zero intensity (HWZI) of the blue side of the line occurs near −20 km s−1, while the HWZI of the red side of the line falls near +30 km s−1. The core of the line shows an asymmetry in the opposite direction.
Paper: Spectroastrometric Survey of Protoplanetary Disks with Inner Dust Cavities
Authors: Stanley K. Jensen, Sean D. Brittain, Andrea Banzatti, Joan R. Najita, John S. Carr, Joshua Kern, Janus Kozdon, Jonathan Zrake, Jeffrey Fung
Figure caption: Comparison of the spectroscopic and SA profiles of CQ Tau observed in 2021 (black), 2022 (blue), and 2023 (red). The horizontal bars are scaled to the instrumental resolution of each observation. A narrow emission component persists in all three epochs, though its line/continuum ratio varies. The centroid of the PSF of the narrow component is extended when the slit is 47° east of north (2021 and 2023) and disappears when the slit PA is 137° east of north.
Paper: Spectroastrometric Survey of Protoplanetary Disks with Inner Dust Cavities
Authors: Stanley K. Jensen, Sean D. Brittain, Andrea Banzatti, Joan R. Najita, John S. Carr, Joshua Kern, Janus Kozdon, Jonathan Zrake, Jeffrey Fung
Figure caption: Comparison of AB Aur observed at three different slit PAs. The data are plotted with black lines, the model is blue and the residual is plotted above in red. The horizontal lines in the lower panels indicate the instrumental resolution of the observation. The model used to fit the profile and SA signal for the slit aligned with the semimajor axis of the disk (PA = 60°) was applied for two other PAs. While the profile could be fit reasonably well, the SA signal diverged significantly from the model. One way to account for this is for a nonaxisymmetric source of emission on the southern part of the disk.
Paper: Spectroastrometric Survey of Protoplanetary Disks with Inner Dust Cavities
Authors: Stanley K. Jensen, Sean D. Brittain, Andrea Banzatti, Joan R. Najita, John S. Carr, Joshua Kern, Janus Kozdon, Jonathan Zrake, Jeffrey Fung
Figure caption: Comparison of 2021 (black) and 2022 (red) average spectroscopic and SA profiles of V892 Tau. The horizontal bars indicate the instrumental resolution of each observation. The PA is offset by 35° between epochs. While the line profile is asymmetric in both epochs, the overall spectroscopic profile changed to exhibit a double-peaked structure, though still with an excess on the blue side. The SA signal is extended on the red and blue sides of the line, consistent with emission arising from an extended disk.
Paper: Resonant Chains and the Convergent Migration of Planets in Protoplanetary Disks
Authors: Ka Ho Wong, Man Hoi Lee
Figure caption: Same as Figure 6 but for a simulation with α = 0.931 and β = 1.552. This (α, β) combination is near the line of no migration, and the resonant chain is not broken by the very slow inward migration after 1 Myr.
Paper: The Weird and the Wonderful in Our Solar System: Searching for Serendipity in the Legacy Survey of Space and Time
Authors: Brian Rogers, Chris J. Lintott, Steve Croft, Megan E. Schwamb, James R. A. Davenport
Figure caption: Reconstruction scores for 3.1 million solar system objects across the reduced feature space. The color bar describes the reconstruction loss. More anomalous points are deeper in the red. The top 0.01% anomalies are enlarged for this plot. They lie distant from the majority of normal objects in blue.
Paper: The Weird and the Wonderful in Our Solar System: Searching for Serendipity in the Legacy Survey of Space and Time
Authors: Brian Rogers, Chris J. Lintott, Steve Croft, Megan E. Schwamb, James R. A. Davenport
Figure caption: The accuracy and F1 metrics for the XGBoost classifier for a given number of training labels. The horizontal red line is 95% of the score of the best-performing unsupervised method (KNN) on global anomalies. The green line is the 75th percentile performance of all unsupervised detection methods considered.
Paper: The Weird and the Wonderful in Our Solar System: Searching for Serendipity in the Legacy Survey of Space and Time
Authors: Brian Rogers, Chris J. Lintott, Steve Croft, Megan E. Schwamb, James R. A. Davenport
Figure caption: The latent space representation of the top ten anomalies and their nearest neighbors. These neighborhoods of anomalies are color coded and lie outside the dense blue distributions of normal objects in the latent space.
Paper: The Weird and the Wonderful in Our Solar System: Searching for Serendipity in the Legacy Survey of Space and Time
Authors: Brian Rogers, Chris J. Lintott, Steve Croft, Megan E. Schwamb, James R. A. Davenport
Figure caption: A schematic diagram of the general network architecture of an autoencoder. The input layer is followed by the encoder, which is made up of a number of hidden layers. In the center lies the latent representation, which can be transformed into an output using the decoder.
Paper: The Weird and the Wonderful in Our Solar System: Searching for Serendipity in the Legacy Survey of Space and Time
Authors: Brian Rogers, Chris J. Lintott, Steve Croft, Megan E. Schwamb, James R. A. Davenport
Figure caption: Visualization of the normalized autoencoder reconstruction loss vs. normalized anomaly score from the GMM. It can be seen with points (4) and (5) that outlying objects are suggested that would be missed by considering only the model-based approach.
Paper: Efficient Search and Detection of Faint Moving Objects in Image Data
Authors: Tam Nguyen, Deborah F. Woods, Jessica Ruprecht, Jonathan Birge
Figure caption: Illustration of the FaXT algorithm. FaXT transforms an input 3D data structure, such as an image stack, into an output 4D data structure, where each element represents the sum of input elements along a discretized linear track. FaXT consists of ﹩{\mathrm{log}}_{2}N﹩ stages. In each stage, basic shift-add operations are performed on the output of the previous stage, effectively generating longer tracks by combining previously generated short tracks. This process allows for each unit track to only be computed once and reused to form multiple longer tracks. For example, in the lower right, it can be seen that the unit track with endpoints (0, 0, 0) and (0, 0, 1), which was computed once in Stage 1, can be used to form four longer tracks (highlighted in blue) in Stage 2.
Paper: JWST MIRI MRS Observations of T Cha: Discovery of a Spatially Resolved Disk Wind
Authors: Naman S. Bajaj, Ilaria Pascucci, Uma Gorti, Richard Alexander, Andrew Sellek, Jane Morrison, Andras Gaspar, Cathie Clarke, Chengyan Xie, Giulia Ballabio, Dingshan Deng
Figure caption: Sketch for T Cha highlighting the argon and neon ionization mechanisms as well as the relative spatial extent of the disk wind emission traced by the two species. EUV ionizes argon, but it is blocked by the wind component traced by argon. However, X-rays can penetrate this component and ionize neon further out in the disk; see the more evolved disk/wind systems in Pascucci et al. (2020). The location of the planet candidate is from Huélamo et al. (2011), and the dust gap is from Hendler et al. (2018).
Paper: JWST MIRI MRS Observations of T Cha: Discovery of a Spatially Resolved Disk Wind
Authors: Naman S. Bajaj, Ilaria Pascucci, Uma Gorti, Richard Alexander, Andrew Sellek, Jane Morrison, Andras Gaspar, Cathie Clarke, Chengyan Xie, Giulia Ballabio, Dingshan Deng
Figure caption: The left panel shows the [Ne II]/[Ne III] ratio where the reference for each point is given in the legend, and the right panel shows the [Ar II]/[Ar III] ratio for T Cha. Upward arrows indicate the lower limits, and H&G 2009 refers to Hollenbach & Gorti (2009). The white region in the left panel refers to the hard EUV model, which can easily be ruled out as the ionization source for neon. However, for argon, the right panel suggests that the EUV model is preferred over X-rays for its ionization. Here, the EUV model combines both soft and hard EUV radiation.