adsabs/AstroCLIMB huggingface dataset:
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: Elemental abundance ratios [X/Fe] as a function of atomic number for stars in the GCs NGC 5139 (top left), NGC 6441 (bottom left, R. Gratton et al. 2006; J. C. Roediger et al. 2013), NGC 5927 (top right, A. Mura-Guzmán et al. 2017), and NGC 5634 (bottom right, E. Carretta et al. 2017), compared with HD 2665, HD 5916, HD 189349, and HD 218857, respectively. The dashed blue lines represent the mean abundance patterns of GCs, and the red dashed lines indicate the field star abundance. The colored symbols with error bars denote individual elemental abundances, and the panels below each plot show the residuals Δ[X/Fe] between the clusters and their corresponding comparison stars. Element symbols are labeled above their respective atomic numbers.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: Comparative chemical abundance patterns of elements (Mg to Y) relative to Fe in the stars of GCs NGC 6517 (orange dashed line) and NGC 6864 (blue dashed line) vs. field star HD 122956. The upper panels show individual abundance ratios [X/Fe] with associated uncertainties for each element, while the lower panel displays the differences Δ[X/Fe] between NGC 6517 − HD 122956 (orange) and NGC 6864 − HD 122956 (blue). The colored markers represent the observed data, with error bars indicating measurement uncertainties.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: An example for the determination of atmospheric parameters Teff and ξ using abundance (logϵ) as a function of both lower-level excitation potential (LEP, panels (a) and (b)) and reduced EW (REW; log (EW/λ), panels (c)) for HD 5916, HD 2665, and HD 218857. The solid line in each panel is the least-squares fit to the data.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: Corner plot displaying the posterior probability distributions for HD 5916, HD 2665, and HD 218857, with confidence levels marked at 68%, 90%, and 95%. The 1D marginal distributions indicate the median values, along with the 16th and 84th percentiles. The right side of each panel shows the corresponding positions of the stars on the Kiel diagram.
Paper: Stellar Ancestry Unlocked: Chemical and Orbital Clues Link Metal-poor Stars to Globular Clusters and the Galaxy’s Thick Disk
Authors: Gizay Yolalan, Timur Şahin, Selçuk Bilir, Olcay Plevne
Figure caption: Observed (black) and synthetic (blue) spectra of HD 5916, HD 122956, and HD 189349 near the Al  Iλ6696-6699 Å  line. The derived aluminum abundances (log ϵ(Al I)) are provided for each star. The dashed horizontal lines denote the continuum level, and wavelength ranges are truncated for clarity.
Paper: FAST Search for Circumstellar Atomic Hydrogen. III. Planetary Nebulae at Galactic Latitudes ∣b∣ ≥ 10°
Authors: Xu-Jia Ouyang, Yong Zhang, Albert Zijlstra, Chuan-Peng Zhang, Jun-ichi Nakashima, Quentin A. Parker, Xiao-Hu Li
Figure caption: H I spectra of PNe. For each subfigure, the top and bottom panels show the ON−OFF and OFF−OFF spectra, respectively. The arrows mark the systemic velocity position the PNe. The vertical dotted line indicates the velocities of the blue end of optical emission lines ([N II] or Hα lines), with the exception of IC 4846, where no such emission lines are found in the literature. A fitting to the potential circumstellar H I absorption is shown by the dashed curves.
Paper: FAST Search for Circumstellar Atomic Hydrogen. III. Planetary Nebulae at Galactic Latitudes ∣b∣ ≥ 10°
Authors: Xu-Jia Ouyang, Yong Zhang, Albert Zijlstra, Chuan-Peng Zhang, Jun-ichi Nakashima, Quentin A. Parker, Xiao-Hu Li
Figure caption: Positions of the our PN sample and the known HIPNe retrieved from the literature in the Galactic coordinate system. The filled circles represent HIPNe, with newly detected sources in this observation labeled by their names. The open circles represent PNe where H I is not detected in our observations. The background is an all-sky H I column density map integrated over the full velocity range of −600 km s−1 ≤ vLSR ≤  600 km s−1, adopted from HI4PI Collaboration et al. (2016).
Paper: FAST Search for Circumstellar Atomic Hydrogen. III. Planetary Nebulae at Galactic Latitudes ∣b∣ ≥ 10°
Authors: Xu-Jia Ouyang, Yong Zhang, Albert Zijlstra, Chuan-Peng Zhang, Jun-ichi Nakashima, Quentin A. Parker, Xiao-Hu Li
Figure caption: Integrated H I optical depth vs. linear radius of the ionized regions. The diagonal lines represent the results derived from theoretical calculations based on different mass-loss rates (as shown in the upper right corner).
Paper: WF-SwinUnet: A Window Fusion-based RFI Segmentation Model and Its Application in FAST
Authors: QingYun Li, MingHui Li, Dongjun Yu, Jie He
Figure caption: Structural composition of WF-SwinUnet. The patch partitioning process entails a reduction of the input data by a factor of four, subsequently followed by an increase in dimension. The linear embedding process refers to the implementation of a linear mapping of the number of channels to a designated dimension. Patch merging is achieved through a process of downsampling the intermediate data by a factor of two and increasing the dimension by a factor of two. Patch expansion involves upsampling the intermediate data by a factor of two and reducing the dimension by a factor of two. Linear projection is defined as the mapping of a specified dimension to a categorized number. The WF-Swin Transformer block is identified as the model’s primary structural element.
Paper: WF-SwinUnet: A Window Fusion-based RFI Segmentation Model and Its Application in FAST
Authors: QingYun Li, MingHui Li, Dongjun Yu, Jie He
Figure caption: The rectangles represent the various types of RFI present in the FAST observation data. The left panel in the top row indicates weak broadband RFI, with a signal strength of minimal intensity and a large number of channels affected. The center panel in the top row indicates weak narrowband RFI, characterized by its minimal signal intensity and limited coverage of channels. The right panel in the top row indicates transient RFI, defined by its short duration. The left panel in the bottom row shows strong broadband RFI, distinguished by its high signal strength and extensive range of channels, while the right panel in the bottom row represents strong narrowband RFI, characterized by a high signal strength and a more limited range of channels.
Paper: WF-SwinUnet: A Window Fusion-based RFI Segmentation Model and Its Application in FAST
Authors: QingYun Li, MingHui Li, Dongjun Yu, Jie He
Figure caption: Detailed figure showing the window fusion mechanism: Global information, obtained via the integration of the calculation outcomes from disparate branches, is processed in a pixel-by-pixel fashion. Following this, a fully connected network is employed for the calculation of the selection vector from the different branches, a process referred to as global pooling.
Paper: WF-SwinUnet: A Window Fusion-based RFI Segmentation Model and Its Application in FAST
Authors: QingYun Li, MingHui Li, Dongjun Yu, Jie He
Figure caption: Continuous window fusion Swin Transformer block figure. In this figure, ⨂ represents window fusion and ⊕ represents residual connection. Furthermore, W-MSA and SW-MSA are, respectively, the window multihead attention and the shifted window multihead self-attention module.
Paper: Updated Masses for the Gas Giants in the Eight-planet Kepler-90 System Via Transit-timing Variation and Radial Velocity Observations
Authors: David E. Shaw, Lauren M. Weiss, Eric Agol, Karen A. Collins, Khalid Barkaoui, Cristilyn N. Watkins, Richard P. Schwarz, Howard M. Relles, Chris Stockdale, John F. Kielkopf, Fabian Rodriguez Frustaglia, Allyson Bieryla, Joao Gregorio, Owen Mitchem, Katherine Linnenkohl, Adam Popowicz, Norio Narita, Akihiko Fukui, Michaël Gillon, Ramotholo Sefako, Avi Shporer, Adam Lark, Amelie Heying, Isa Khan, Beibei Chen, Kylee Carden, Donald M. Terndrup, Robert Taylor, Dasha Crocker, Sarah Ballard, Daniel C. Fabrycky
Figure caption: Comparison of the Kepler-90 system (gray) with our own solar system (blue). The size of each circle is proportional to the planet’s radius. Masses for the inner six Kepler-90 planets are estimated using their measured radii and an empirical mass–radius relation (L. M. Weiss & G. W. Marcy 2014). Error bars are generally too small to be seen on this scale. Lines of constant RV semiamplitude are drawn for a solar-mass star and circular orbit to approximately illustrate the RV signal induced by each planet.
Paper: A Metal-poor Atmosphere with a Hot Interior for a Young Sub-Neptune Progenitor: JWST/NIRSpec Transmission Spectrum of V1298 Tau b
Authors: Saugata Barat, Jean-Michel Désert, Sagnick Mukherjee, Jayesh M. Goyal, Qiao Xue, Yui Kawashima, Allona Vazan, William Misener, Hilke E. Schlichting, Jonathan J. Fortney, Jacob L. Bean, Swaroop Avarsekar, Gregory W. Henry, Robin Baeyens, Michael R. Line, John H. Livingston, Trevor David, Erik A. Petigura, James T. Sikora, Hinna Shivkumar, Adina D. Feinstein, Antonija Oklopčić
Figure caption: Simulated thermal evolution models for V1298 Tau b for two interior structure scenarios: pure H/He atmosphere (Section 5.7.1) and an envelop with silicate vapor in equilibrium with a rocky core (Section 5.7.2). These models have been calculated using the AIOLOS code (M. Schulik & R. A. Booth 2023). The evolution of three key parameters presented: the internal temperature, the transit radii, and the core-powered mass-loss rate are presented in the left, middle, and right panels, respectively. In each panel, the gold line represents the current age of the planet (20 Myr), while the star in the middle panel depicts its observed TESS radius (A. D. Feinstein et al. 2022). The red curve is an evolution of a standard, pure H/He atmosphere, using realistic temperature profiles from AIOLOS. The atmospheric mass fraction is f = 0.08, with an internal temperature of 105 K. The blue curve represents an evolution with atmospheric structure calculated allowing for chemical equilibrium of silicates and the resulting superadiabatic temperature profiles. In the pure H/He atmosphere scenario, our models predict rapid contraction with V1298 Tau b contracting by ∼50% compared to its current size within the next 100 Myr. In the silicate vapor case, the planet does not undergo significant evolution and can maintain its size over a Gyr timescale.
Paper: A Metal-poor Atmosphere with a Hot Interior for a Young Sub-Neptune Progenitor: JWST/NIRSpec Transmission Spectrum of V1298 Tau b
Authors: Saugata Barat, Jean-Michel Désert, Sagnick Mukherjee, Jayesh M. Goyal, Qiao Xue, Yui Kawashima, Allona Vazan, William Misener, Hilke E. Schlichting, Jonathan J. Fortney, Jacob L. Bean, Swaroop Avarsekar, Gregory W. Henry, Robin Baeyens, Michael R. Line, John H. Livingston, Trevor David, Erik A. Petigura, James T. Sikora, Hinna Shivkumar, Adina D. Feinstein, Antonija Oklopčić
Figure caption: Transmission spectrum of V1298 Tau b (upper panel) and fitted baseline quadratic polynomial coefficients (middle and lower panels), defined in Equation (C1). This transmission spectrum has been derived from an empirical model fit (Appendix C) to spectroscopic light curves derived from 10 pixel bins on the 1D stellar spectra from Eureka! data reduction (Appendix A). The light-curve models are described in Equation (C1). The model includes a quadratic polynomial function to model the low-frequency stellar baseline variability, a double exponential function to model the flare, a sinusoidal function to model the postflare oscillations, and a batman model for the planet transit. The solid red lines show a smoothed function, obtained by applying a Gaussian filter on the observed c2 (linear coefficient) and c3 (quadratic coefficient) values. The transmission spectrum derived using this approach exhibits prominent H2O, CH4, and CO2 absorption features, but shows significant scatter and multiple outliers (>5σ compared to neighboring data points). We find that c2 and c3 appear correlated with the transit depth: outliers in the transmission spectrum correspond to outliers in the c2 and c3. c2 and c3 show a strong wavelength dependence for NRS1, and are relatively wavelength independent for NRS2. The smoothed c2 and c3 coefficients are used for the data-driven detrending of the spectroscopic light curves in the second iteration of light-curve fits described in Appendix C.
Paper: A Metal-poor Atmosphere with a Hot Interior for a Young Sub-Neptune Progenitor: JWST/NIRSpec Transmission Spectrum of V1298 Tau b
Authors: Saugata Barat, Jean-Michel Désert, Sagnick Mukherjee, Jayesh M. Goyal, Qiao Xue, Yui Kawashima, Allona Vazan, William Misener, Hilke E. Schlichting, Jonathan J. Fortney, Jacob L. Bean, Swaroop Avarsekar, Gregory W. Henry, Robin Baeyens, Michael R. Line, John H. Livingston, Trevor David, Erik A. Petigura, James T. Sikora, Hinna Shivkumar, Adina D. Feinstein, Antonija Oklopčić
Figure caption: Density–radius profiles of three atmospheric structure models of V1298 Tau b, calculated using the AIOLOS code (M. Schulik & R. A. Booth 2023). See Section 5.7.1 for further description of the model. The outer radiative region is shown, with the radiative–convective boundary depicted by dots. Each color line represents a different corresponding atmospheric mass, given as a fraction of the total planet mass f: green is f  =  0.3, teal is f  = 0.08, and purple is f = 0.002. We assume a planet mass of 12 M⊕ from the free retrieval. All three profiles have been simulated assuming the retrieved atmospheric opacity from the observed transmission spectrum (Section 4.1). The transit radii (marked with a T and the yellow vertical line) are normalized at the TESS optical radius (A. D. Feinstein et al. 2022) for all three models. However, the three profiles correspond to different internal temperatures of 65, 105, and 500 K and core masses of 8 M⊕, 11 M⊕, and 12 M⊕, respectively.
Paper: A Metal-poor Atmosphere with a Hot Interior for a Young Sub-Neptune Progenitor: JWST/NIRSpec Transmission Spectrum of V1298 Tau b
Authors: Saugata Barat, Jean-Michel Désert, Sagnick Mukherjee, Jayesh M. Goyal, Qiao Xue, Yui Kawashima, Allona Vazan, William Misener, Hilke E. Schlichting, Jonathan J. Fortney, Jacob L. Bean, Swaroop Avarsekar, Gregory W. Henry, Robin Baeyens, Michael R. Line, John H. Livingston, Trevor David, Erik A. Petigura, James T. Sikora, Hinna Shivkumar, Adina D. Feinstein, Antonija Oklopčić
Figure caption: Upper panel: spectroscopic light curves of V1298 Tau b derived from the Eureka! data reduction (Appendix A) with the best-fit planetary transit and polynomial baseline removed (gray lines). These light curves have been derived by fitting the spectroscopic light curves with an empirical model (Equation (C1)) described in Appendix C. Subsequently, the observed spectroscopic light curves were divided by the best-fit planetary transit model and the quadratic baseline model, effectively leaving behind the astrophysical systematics (flare and oscillations). The light curves have been normalized at the peak of the flare for visual comparison. The light curves for all spectroscopic channels show similar temporal behavior, i.e., we do not see any wavelength-dependent temporal stretching. The solid black lines show the median of the individual flare-only light curves. Middle panel: best-fit flare model from white light-curve fits. The flare model is derived from Equation (C2) using the best-fit flare parameters from the white light-curve fits. This profile has been used in a second iteration fit to the spectroscopic light curves as described in Appendix C.2) Lower panel: residual oscillation profile from white light-curve fit. The residual oscillations are derived from the white light curves by removing the transit, baseline, and the best-fit flare model (middle panel). The solid black line shown in the lower panels has been derived by applying a Gaussian filter to the observed residual oscillation (gray points). The median residual oscillation profile has been used to detrend the spectroscopic light curves by multiplying with a scaling factor in a second iteration data-driven fit, as discussed in Appendix C.2.
Paper: A Metal-poor Atmosphere with a Hot Interior for a Young Sub-Neptune Progenitor: JWST/NIRSpec Transmission Spectrum of V1298 Tau b
Authors: Saugata Barat, Jean-Michel Désert, Sagnick Mukherjee, Jayesh M. Goyal, Qiao Xue, Yui Kawashima, Allona Vazan, William Misener, Hilke E. Schlichting, Jonathan J. Fortney, Jacob L. Bean, Swaroop Avarsekar, Gregory W. Henry, Robin Baeyens, Michael R. Line, John H. Livingston, Trevor David, Erik A. Petigura, James T. Sikora, Hinna Shivkumar, Adina D. Feinstein, Antonija Oklopčić
Figure caption: Mass–atmospheric metallicity diagram showing V1298 Tau b (red star with 1σ uncertainty) in the context of the solar system planets (orange points), and the exoplanet population with published atmospheric metallicity. We assume the mass and atmospheric metallicity of V1298 Tau b from the free chemistry atmospheric retrieval (Appendix D, Table 1). The retrieved atmospheric metallicity is converted into stellar units assuming a stellar metallicity of 0.10 ± 0.15 dex (A. Suárez Mascareño et al. 2021), and the uncertainties were propagated. We show exoplanets with metallicity measurements from HST in gray, taken from H. R. Wakeford & P. A. Dalba (2020), and with JWST (purple points). The JWST sample has been taken from Table 1 of S. Barat et al. (2024a). The red dashed line and the shaded region show the mass–metallicity relation derived in D. P. Thorngren et al. (2016). The atmospheric metallicity of V1298 Tau b is lower than what is expected from core-accretion formation models (J. B. Pollack et al. 1996; D. P. Thorngren et al. 2016) and what is typically seen for known sub-Neptune/super-Earth planets by more than 1 order of magnitude, indicating ongoing evolutionary mechanisms which are expected to enhance the atmospheric metallicity of V1298 tau b as it matures.
Paper: A Metal-poor Atmosphere with a Hot Interior for a Young Sub-Neptune Progenitor: JWST/NIRSpec Transmission Spectrum of V1298 Tau b
Authors: Saugata Barat, Jean-Michel Désert, Sagnick Mukherjee, Jayesh M. Goyal, Qiao Xue, Yui Kawashima, Allona Vazan, William Misener, Hilke E. Schlichting, Jonathan J. Fortney, Jacob L. Bean, Swaroop Avarsekar, Gregory W. Henry, Robin Baeyens, Michael R. Line, John H. Livingston, Trevor David, Erik A. Petigura, James T. Sikora, Hinna Shivkumar, Adina D. Feinstein, Antonija Oklopčić
Figure caption: Comparison between white light curves in NRS1 (upper panel) and NRS2 (lower panel) obtained from Eureka! data reduction (Appendix A) and SPARTA data reduction (Appendix B). The light curves and scatter are comparable in NRS1 (129 and 133 ppm for Eureka! and SPARTA, respectively). However, in NRS2, SPARTA shows a comparatively higher scatter (190 and 233 ppm for Eureka! and SPARTA, respectively). Both reductions show qualitatively similar light-curve features: a low-frequency temporal variability signal due to the rotational modulation of spots on the photosphere of the rapidly rotating (2.8 days) young T Tauri star, and high-frequency signal in the middle of the transit, which is due to a flare and prominent postflare oscillations, which continue even after egress, confirming that this periodic variability signal is due to the star and not spot crossings by the planet.
Paper: A Metal-poor Atmosphere with a Hot Interior for a Young Sub-Neptune Progenitor: JWST/NIRSpec Transmission Spectrum of V1298 Tau b
Authors: Saugata Barat, Jean-Michel Désert, Sagnick Mukherjee, Jayesh M. Goyal, Qiao Xue, Yui Kawashima, Allona Vazan, William Misener, Hilke E. Schlichting, Jonathan J. Fortney, Jacob L. Bean, Swaroop Avarsekar, Gregory W. Henry, Robin Baeyens, Michael R. Line, John H. Livingston, Trevor David, Erik A. Petigura, James T. Sikora, Hinna Shivkumar, Adina D. Feinstein, Antonija Oklopčić
Figure caption: Comparison between retrieved abundances of molecules in our free chemistry PICASSO retrieval (Appendix D), shown with colored circles and 1σ uncertainties, with molecular abundance profiles (solid lines of the same color) from the best-fit self-consistent PICASSO grid model (Appendix E). The shaded region around each profile from our grid represents the range of abundance profiles in the grid models, which have a probability of p(x) ≥ 1% (3σ confidence region). In our case, this represents the top 61 best-fitting grid models. Although the free retrieval finds SO2, the best-fit grid model does not seem to have a large SO2 abundance. The grid predicts OCS, which is also found in the free retrievals but at a 3σ lower VMR than predicted by the grid.
Paper: A Metal-poor Atmosphere with a Hot Interior for a Young Sub-Neptune Progenitor: JWST/NIRSpec Transmission Spectrum of V1298 Tau b
Authors: Saugata Barat, Jean-Michel Désert, Sagnick Mukherjee, Jayesh M. Goyal, Qiao Xue, Yui Kawashima, Allona Vazan, William Misener, Hilke E. Schlichting, Jonathan J. Fortney, Jacob L. Bean, Swaroop Avarsekar, Gregory W. Henry, Robin Baeyens, Michael R. Line, John H. Livingston, Trevor David, Erik A. Petigura, James T. Sikora, Hinna Shivkumar, Adina D. Feinstein, Antonija Oklopčić
Figure caption: Plausible self-consistently calculated T–P profiles for V1298 Tau b for different values of Tint using PICASSO. The light blue and red lines correspond to constant abundance CO and CH4 contours, respectively. The black dashed line shows the CO/CH4 equality line for 10× solar metallicity (J. J. Fortney et al. 2020). The solid blue line with its shaded region shows the methane abundance derived from the free retrieval and its 1σ uncertainty. The red star shows the CH4/CO quench point for the T–P profile with Tint = 500 K.
Paper: A Metal-poor Atmosphere with a Hot Interior for a Young Sub-Neptune Progenitor: JWST/NIRSpec Transmission Spectrum of V1298 Tau b
Authors: Saugata Barat, Jean-Michel Désert, Sagnick Mukherjee, Jayesh M. Goyal, Qiao Xue, Yui Kawashima, Allona Vazan, William Misener, Hilke E. Schlichting, Jonathan J. Fortney, Jacob L. Bean, Swaroop Avarsekar, Gregory W. Henry, Robin Baeyens, Michael R. Line, John H. Livingston, Trevor David, Erik A. Petigura, James T. Sikora, Hinna Shivkumar, Adina D. Feinstein, Antonija Oklopčić
Figure caption: Fitted linear limb darkening coefficient for V1298 Tau from the HST and JWST transit observations of V1298 Tau b (yellow data points with red 1σ error bars). The JWST limb darkening coefficients are measured at a higher spectral resolution compared to HST (by a factor of ∼10), which is why the JWST error bars are larger compared to HST. The continuous black curve is from a linear limb darkening model generated using ExoTiC-LD (D. Grant & H. Wakeford 2024) computed for a K1-type main-sequence star. The modeled linear limb darkening coefficients are found to be significantly smaller than the observed values, but the difference gets smaller at longer wavelengths.
Paper: Binary Analysis and Period Study of the Long-period, High-mass-ratio Contact Binary KIC 7766185
Authors: Conor M. Larsen, Andrej Prša
Figure caption: Distributions of the inferred parameters in the (a) LC run, (b) the RV run, and (c) the temperature run. The vertical dashed lines in the one-dimensional distributions represent the 68th percentile. The three contours in the two-dimensional distributions denote the 68th, 95th, and 99.7th percentiles.