adsabs/AstroCLIMB huggingface dataset:
Paper: A Secular Solar System Resonance that Disrupts the Dominant Cycle in Earth’s Orbital Eccentricity (g 2 − g 5): Implications for Astrochronology
Authors: Richard E. Zeebe, Margriet L. Lantink
Figure caption: Section of the ∼2.46 Ga Joffre Member exposed at Joffre Falls (Joffre Gorge, Karijini National Park, Western Australia). Photo credit: Frits Hilgen.
Paper: A Secular Solar System Resonance that Disrupts the Dominant Cycle in Earth’s Orbital Eccentricity (g 2 − g 5): Implications for Astrochronology
Authors: Richard E. Zeebe, Margriet L. Lantink
Figure caption: Mars’ inclination over the past 20 Myr (nearly identical in all solutions, reference frame: ECLIPJ2000).
Paper: Absolute Calibration. IV. Use of G-type Stars as Primary Calibrators
Authors: G. H. Rieke, Everett Schlawin, Charles R. Proffitt, Christopher Willmer
Figure caption: Comparison of the solar spectrum with the model for P330-E. The agreement is extremely good (in general, maximum differences are ≤0.3%), except for the shallower CO fundamental band in the model, which does not behave monotonically with spectral type. The small excursions in the P330-E model spectrum around 10 μm are from silicate absorption in the extinction law. The photometry is from Rieke et al. (2022) for K  S , Krick et al. (2021) for IRAC Band 1 (3.6 μm), Bohlin et al. (2022) for IRAC Bands 2–4 (see footnote in Section 4.1), and IRSA SEIP for the MIPS 24 μm point. All are based on the calibration of Rieke et al. (2023). The error bars are 1% at 2.2 and 3.6 μm, but larger at the longer wavelengths, where they show effects of increased statistical measurement errors (i.e., they are 2% for IRAC Bands 2 and 3, 3% for Band 4, and 4% at 24 μm. The NIRSpec prism spectrum is the version set as a ratio to the average of the white dwarf spectra and has been smoothed to suppress noise. Contrary to the model, it indicates that the CO fundamental is actually similar in strength to that in the Sun.
Paper: Absolute Calibration. IV. Use of G-type Stars as Primary Calibrators
Authors: G. H. Rieke, Everett Schlawin, Charles R. Proffitt, Christopher Willmer
Figure caption: The H-R diagram for the field containing NGC 2506. The main sequence is well defined, and most of the brighter detections off it are foreground stars (i.e., too bright for their g – r color). The vertical line is at the expected color difference for solar-type stars, and candidates are selected where they cross the main sequence.
Paper: Absolute Calibration. IV. Use of G-type Stars as Primary Calibrators
Authors: G. H. Rieke, Everett Schlawin, Charles R. Proffitt, Christopher Willmer
Figure caption: Comparison of the model for G-31 (red line), the NIRSpec prism spectrum (orange line), and the K  S -band photometric point.
Paper: Absolute Calibration. IV. Use of G-type Stars as Primary Calibrators
Authors: G. H. Rieke, Everett Schlawin, Charles R. Proffitt, Christopher Willmer
Figure caption: Comparison of the spectra of 18 Sco after joining, out to 1 μm. The spectrum of the Sun has been adjusted by the ratio of blackbody spectra at 5812 K (18 Sco) and 5772 K (Sun). It is hardly distinguishable from the BOSZ/solar spectrum.
Paper: Absolute Calibration. IV. Use of G-type Stars as Primary Calibrators
Authors: G. H. Rieke, Everett Schlawin, Charles R. Proffitt, Christopher Willmer
Figure caption: Ratio of the NIRSpec prism spectrum to the P330-E model. The two relevant photometric points are also shown, both with 1% error bars.
Paper: Absolute Calibration. IV. Use of G-type Stars as Primary Calibrators
Authors: G. H. Rieke, Everett Schlawin, Charles R. Proffitt, Christopher Willmer
Figure caption: An example G2V star in NGC 2420 found by mkclass (07:38:28.4 +21:33) is visually checked against spectral templates. Of particular importance for temperature classification are the Ca I 4226 Å, Hδ, Hγ, and Fe I lines highlighted above (Gray & Corbally 2009). Two standards (G2V and G1.5V) are shown for comparison.
Paper: Absolute Calibration. IV. Use of G-type Stars as Primary Calibrators
Authors: G. H. Rieke, Everett Schlawin, Charles R. Proffitt, Christopher Willmer
Figure caption: Difference of K magnitude from Casagrande et al. (2014) minus 2MASS K  S , vs. J − H.
Paper: Absolute Calibration. IV. Use of G-type Stars as Primary Calibrators
Authors: G. H. Rieke, Everett Schlawin, Charles R. Proffitt, Christopher Willmer
Figure caption: Comparison of photometry from Krick et al. (2021) and Bohlin et al. (2022) for IRAC Band 1 (3.55 μm).
Paper: Photometric and Spectroscopic Analysis of V583 Lyrae, an Algol with a g-mode Pulsating Primary and Accretion Disk
Authors: H.-T Zhang, S.-B Qian, W.-P Liao, B. Soonthornthum, N. Sarotsakulchai
Figure caption: Results for a set of assigned gainer rotation parameters F rot1 modeled from TESS and Kepler photometry. All minima fall between 4.7 and 5.3, and the best F rot1 = 4.8, implying essentially uniform gainer rotation.
Paper: Photometric and Spectroscopic Analysis of V583 Lyrae, an Algol with a g-mode Pulsating Primary and Accretion Disk
Authors: H.-T Zhang, S.-B Qian, W.-P Liao, B. Soonthornthum, N. Sarotsakulchai
Figure caption: All the spectra show the Hα profile. Fluxes are normalized to the continuum and heliocentric corrections have been applied.
Paper: Photometric and Spectroscopic Analysis of V583 Lyrae, an Algol with a g-mode Pulsating Primary and Accretion Disk
Authors: H.-T Zhang, S.-B Qian, W.-P Liao, B. Soonthornthum, N. Sarotsakulchai
Figure caption: Comparison of the Fourier periodograms of the TESS (blue), Kepler-SC (black), and Kepler-LC (red) light curves of V583 Lyr. There are no pulsations at higher frequencies up to the Nyquist frequency. The four frequency groups are labeled as Fg1–Fg4.
Paper: Photometric and Spectroscopic Analysis of V583 Lyrae, an Algol with a g-mode Pulsating Primary and Accretion Disk
Authors: H.-T Zhang, S.-B Qian, W.-P Liao, B. Soonthornthum, N. Sarotsakulchai
Figure caption: The shifts of the double peaks and the central absorption are plotted against the variation of the average peak separation.
Paper: Photometric and Spectroscopic Analysis of V583 Lyrae, an Algol with a g-mode Pulsating Primary and Accretion Disk
Authors: H.-T Zhang, S.-B Qian, W.-P Liao, B. Soonthornthum, N. Sarotsakulchai
Figure caption: Multifrequency fit for V583 Lyr. The residuals are shown after subtracting the eclipses in the Kepler (LC) observations and the synthetic curve. The lower panel presents a portion of the residuals denoted by the inset box in the upper panel. The red line indicates the synthetic curve computed using all the frequencies detected.
Paper: Photometric and Spectroscopic Analysis of V583 Lyrae, an Algol with a g-mode Pulsating Primary and Accretion Disk
Authors: H.-T Zhang, S.-B Qian, W.-P Liao, B. Soonthornthum, N. Sarotsakulchai
Figure caption: Upper panel: velocity curve of V583 Lyr based on elements from Table 4 and the best-fitting solution. The horizontal line marks the corresponding systemic velocity. Bottom panel: residuals from the fit.
Paper: Photometric and Spectroscopic Analysis of V583 Lyrae, an Algol with a g-mode Pulsating Primary and Accretion Disk
Authors: H.-T Zhang, S.-B Qian, W.-P Liao, B. Soonthornthum, N. Sarotsakulchai
Figure caption: The theoretical fit to the O − C data for V583 Lyr. The top panel shows the parabolic fit (dashed line), and the bottom panel shows the residuals from the fit.
Paper: Photometric and Spectroscopic Analysis of V583 Lyrae, an Algol with a g-mode Pulsating Primary and Accretion Disk
Authors: H.-T Zhang, S.-B Qian, W.-P Liao, B. Soonthornthum, N. Sarotsakulchai
Figure caption: Theoretical binary model fit of TESS (left panel) and Kepler (right panel) in semidetached mode.
Paper: Photometric and Spectroscopic Analysis of V583 Lyrae, an Algol with a g-mode Pulsating Primary and Accretion Disk
Authors: H.-T Zhang, S.-B Qian, W.-P Liao, B. Soonthornthum, N. Sarotsakulchai
Figure caption: The semidetached configuration of V583 Lyr at the phase = 0.25.
Paper: A Data-driven Approach for Mitigating Dark Current Noise and Bad Pixels in Complementary Metal Oxide Semiconductor Cameras for Space-based Telescopes
Authors: Peng Jia, Chao Lv, Yushan Li, Yongyang Sun, Shu Niu, Zhuoxiao Wang
Figure caption: The top and middle panels illustrate the detection accuracy and efficiency of both SExtractor and Faster R-CNN for stars with varying apparent magnitudes in the 47th frame of images. The bottom panels show how the detection accuracy and efficiency decrease with increasing temperature (frame sequence number).
Paper: A Data-driven Approach for Mitigating Dark Current Noise and Bad Pixels in Complementary Metal Oxide Semiconductor Cameras for Space-based Telescopes
Authors: Peng Jia, Chao Lv, Yushan Li, Yongyang Sun, Shu Niu, Zhuoxiao Wang
Figure caption: The schematic of the data-driven dark current noise model of the CMOS camera encompasses two essential steps: the pixel clustering step and the function fitting step. Initially, we collect test data following the observation strategy. Subsequently, we cluster the pixels based on their temperature (frame sequence number)–dark current relations. Using the clustering results, we fit functions to each cluster, representing the temperature (frame sequence number)–dark current relationship specific to the CMOS camera. In real observations, we start by acquiring the CMOS temperature (frame sequence number) using the grayscale values of noncelestial object pixels. This information enables us to determine the dark current for all pixels in the CMOS camera.
Paper: A Data-driven Approach for Mitigating Dark Current Noise and Bad Pixels in Complementary Metal Oxide Semiconductor Cameras for Space-based Telescopes
Authors: Peng Jia, Chao Lv, Yushan Li, Yongyang Sun, Shu Niu, Zhuoxiao Wang
Figure caption: Part of images in optical (top panels) and near-ultraviolet band (bottom panels) before and after being processed with our method. White boxes with solid lines indicate positions of true celestial objects that are above the detection limit. Red boxes with dashed lines indicate positions of candidates detected by SExtractor. As shown in this figure, SExtractor could better detect celestial objects after being processed by our method (with much lower false detection rates).
Paper: A Data-driven Approach for Mitigating Dark Current Noise and Bad Pixels in Complementary Metal Oxide Semiconductor Cameras for Space-based Telescopes
Authors: Peng Jia, Chao Lv, Yushan Li, Yongyang Sun, Shu Niu, Zhuoxiao Wang
Figure caption: The left panel displays the BIC values corresponding to various clusters. The right panel shows the distribution of pixels across different clusters.
Paper: A Data-driven Approach for Mitigating Dark Current Noise and Bad Pixels in Complementary Metal Oxide Semiconductor Cameras for Space-based Telescopes
Authors: Peng Jia, Chao Lv, Yushan Li, Yongyang Sun, Shu Niu, Zhuoxiao Wang
Figure caption: The top left panel shows the three methods (“Fit,” “Match,” “Per-fit”) for predicting the true frame rate of the image. The top right panel visualizes background levels of individual pixels within a single observation image for each cluster. The bottom panel shows the rms comparison with the original image after processing by both methods “Fit” and “Match.”
Paper: A Data-driven Approach for Mitigating Dark Current Noise and Bad Pixels in Complementary Metal Oxide Semiconductor Cameras for Space-based Telescopes
Authors: Peng Jia, Chao Lv, Yushan Li, Yongyang Sun, Shu Niu, Zhuoxiao Wang
Figure caption: The left panels display the original images, and the right panels display the processed images. The top panels show images obtained by the near-ultraviolet telescope, while the bottom panels show images obtained by the optical telescope.
Paper: A Data-driven Approach for Mitigating Dark Current Noise and Bad Pixels in Complementary Metal Oxide Semiconductor Cameras for Space-based Telescopes
Authors: Peng Jia, Chao Lv, Yushan Li, Yongyang Sun, Shu Niu, Zhuoxiao Wang
Figure caption: The left panel shows the relation between logarithm of dark current level and 1/frame sequence number. The right panel shows the relation between the dark current level and frame sequence number.
Paper: A Data-driven Approach for Mitigating Dark Current Noise and Bad Pixels in Complementary Metal Oxide Semiconductor Cameras for Space-based Telescopes
Authors: Peng Jia, Chao Lv, Yushan Li, Yongyang Sun, Shu Niu, Zhuoxiao Wang
Figure caption: The structure of the Faster R-CNN detection algorithm used in this paper.
Paper: Is the RSGC4 (Alicante 8) Cluster a Real Star Cluster? Peculiar Radial Velocities of Red Supergiant Stars
Authors: Sang-Hyun Chun, GyuChul Myeong, Jae-Joon Lee, Heeyoung Oh
Figure caption: Left: relative spatial distribution of RSG candidates in RSGC4 from the cluster center. The relative PM vectors are also indicated by arrows. The dotted circle indicates the region within ﹩3^{\prime} ﹩ of the cluster center. The ID numbers of candidates are indicated, and the approximate motions of candidates based on Φrel are indicated in parentheses (see text in Section 4.3). Right: distribution of Φrel as a function of μ rel for RSG candidates in RSGC4. The potential binary stars and the stars with RUWE < 1.4 are indicated by open squares and open circles, respectively. The red dashed lines indicate the angle criteria (±70° and ±110°) used to determine the approximate motions of RSG candidates. The KDE plot of Φrel is shown in the right panel.
Paper: Is the RSGC4 (Alicante 8) Cluster a Real Star Cluster? Peculiar Radial Velocities of Red Supergiant Stars
Authors: Sang-Hyun Chun, GyuChul Myeong, Jae-Joon Lee, Heeyoung Oh
Figure caption: Left: action space map of normalized (J hor, J ver) for the RSG candidates in the six RSGCs. The RSG candidates in RSGC4 with low J hor and J ver are indicated in the inset. The stars with RUWE < 1.4 are indicated by open circles. The potential binary stars in RSGC4 are indicated by open squares. The red dashed line shows the limits of the action space map. Right: map of inclination against eccentricity for the RSG candidates in the six RSGCs. The RSG candidates in RSGC4 with high eccentricity are shown in the inset.
Paper: Is the RSGC4 (Alicante 8) Cluster a Real Star Cluster? Peculiar Radial Velocities of Red Supergiant Stars
Authors: Sang-Hyun Chun, GyuChul Myeong, Jae-Joon Lee, Heeyoung Oh
Figure caption: Comparison of the H-band spectra of RSGC4-8, RSGC4-9 (peculiar RSGs), and RSGC4-5 (normal RSG). The spectra of V1016 Cyg (D-type) and AG Peg (S-type) symbiotic stars are also represented with orange solid lines to show similarities in spectral absorption features. Several atomic (Si, Ca, Ti, and Fe) and molecule (OH, CN, and CO) absorption lines are indicated by vertical lines of different colors.
Paper: Is the RSGC4 (Alicante 8) Cluster a Real Star Cluster? Peculiar Radial Velocities of Red Supergiant Stars
Authors: Sang-Hyun Chun, GyuChul Myeong, Jae-Joon Lee, Heeyoung Oh
Figure caption: The distributions of RSG candidates in six RSGCs in (Q1, Q2), (Q2, [3.6] − [4.5]), and (K  s  − [8.0], Q1) CCDs. The dashed lines indicate the criteria of RSGs established by Messineo et al. (2012), and the shaded region in each panel is where most Galactic RSGs are distributed. The peculiar RSG candidates with ID numbers in RSGC4 are located in the region where IR excesses are expected.
Paper: Is the RSGC4 (Alicante 8) Cluster a Real Star Cluster? Peculiar Radial Velocities of Red Supergiant Stars
Authors: Sang-Hyun Chun, GyuChul Myeong, Jae-Joon Lee, Heeyoung Oh
Figure caption: Comparison of the K-band spectra of RSGC4-8, RSGC4-9, and RSGC4-5.
Paper: How Well is the International Celestial Reference System Maintained in Official IAU Implementations?
Authors: Zinovy Malkin
Figure caption: Dependence of differences between the source positions (left panel) and normalized separation (right panel) in ICRF catalogs on the number of observations for 601 common sources in all three catalogs. Red lines show the level of D = 5 mas for the left panel and X = 5 for the right panel.
Paper: How Well is the International Celestial Reference System Maintained in Official IAU Implementations?
Authors: Zinovy Malkin
Figure caption: Sky distribution of the three radio ICRF catalogs and sources in common.
Paper: How Well is the International Celestial Reference System Maintained in Official IAU Implementations?
Authors: Zinovy Malkin
Figure caption: Transferring the ICRS to sequential radio (ICRF) and optical (Gaia-CRF) reference frames.
Paper: A Perfect Tidal Storm: HD 104067 Planetary Architecture Creating an Incandescent World
Authors: Stephen R. Kane, Tara Fetherolf, Zhexing Li, Alex S. Polanski, Andrew W. Howard, Howard Isaacson, Teo Močnik, Sadie G. Welter
Figure caption: Results of the injection-recovery test to determine the sensitivity of the RV data to planetary signatures as a function of planetary mass (﹩{M}_{p}\sin i﹩) and semimajor axis (a). The blue dots represent injected planetary signatures that were successfully recovered and the red dots represent those planets that were not recovered. The color scale shown on the right vertical axis corresponds to the probability contours of detecting a planet of a given mass and semimajor axis. The two detected planets are shown as large black dots.
Paper: A Perfect Tidal Storm: HD 104067 Planetary Architecture Creating an Incandescent World
Authors: Stephen R. Kane, Tara Fetherolf, Zhexing Li, Alex S. Polanski, Andrew W. Howard, Howard Isaacson, Teo Močnik, Sadie G. Welter
Figure caption: TESS 2 minute cadence photometry (left column), Lomb–Scargle periodogram (center column), and lightcurve phase-folded on the measured stellar rotation period (right column) for sectors 10 (top row), 36 (center row), and 63 (bottom row). The gray points in the left column panels show data points that were removed based on poor quality flags or 5σ outliers. The red curve represents the sinusoidal function that best-fits the lightcurve and represents the measured stellar rotation period. The black points in the right column represent the binned photometry.
Paper: A Perfect Tidal Storm: HD 104067 Planetary Architecture Creating an Incandescent World
Authors: Stephen R. Kane, Tara Fetherolf, Zhexing Li, Alex S. Polanski, Andrew W. Howard, Howard Isaacson, Teo Močnik, Sadie G. Welter
Figure caption: Eccentricity evolution for the three-planet model of the HD 104067 system, including the transiting planet candidate, TOI-6713.01 (top panel), the newly detected planet c (middle panel), and the previously known planet b (bottom panel). Data are shown for the first 105 yr of the full 107 yr integration.
Paper: A Perfect Tidal Storm: HD 104067 Planetary Architecture Creating an Incandescent World
Authors: Stephen R. Kane, Tara Fetherolf, Zhexing Li, Alex S. Polanski, Andrew W. Howard, Howard Isaacson, Teo Močnik, Sadie G. Welter
Figure caption: RV data for HD 104067, including those acquired from HARPS and HIRES on either side of the 2004 HIRES upgrade (HIRES1 and HIRES2), where the blue lines indicate the best fit to the data. The top panels show the full observational baseline and fit to the residuals. The bottom panels show the data fits for the individual planets, b and c.
Paper: A Perfect Tidal Storm: HD 104067 Planetary Architecture Creating an Incandescent World
Authors: Stephen R. Kane, Tara Fetherolf, Zhexing Li, Alex S. Polanski, Andrew W. Howard, Howard Isaacson, Teo Močnik, Sadie G. Welter
Figure caption: The eccentricity (top panel), tidal power (middle panel), and equilbrium temperature (bottom panel) evolution of the transiting planet candidate, TOI-6713.01. As for Figure 5, these results are shown for the first 105 yr of the dynamical simulation.
Paper: A Perfect Tidal Storm: HD 104067 Planetary Architecture Creating an Incandescent World
Authors: Stephen R. Kane, Tara Fetherolf, Zhexing Li, Alex S. Polanski, Andrew W. Howard, Howard Isaacson, Teo Močnik, Sadie G. Welter
Figure caption: Folded TESS lightcurve, where gray points are the raw data and blue represent the binned data. The median transit model is plotted as the black line. Residuals (data minus model) are shown in the lower panel.
Paper: Foreground Dust Properties toward the Cluster NGC 7380
Authors: Sadhana Singh, Jeewan C. Pandey, Thiem Hoang, Neelam Panwar, Biman J. Medhi, Vishal Joshi, Shashikiran Ganesh
Figure caption: The distributions of P (left panel) and θ (right panel) in the B, V, R, and I bands. Distributions for all observed and member stars are plotted with light and dark colors, respectively, in all bands.
Paper: Cloud–Cloud Collision and Cluster Formation in the W5-NW Complex
Authors: Namitha Issac, Anindya Saha, Saanika Choudhary, Aakash Chaudhary, Anandmayee Tej, Hong-Li Liu, Tie Liu, Maheswar Gopinathan
Figure caption: (a) Two-color composite image made with the 12CO(3 − 2) integrated intensity maps towards W5-NW. The blue and red correspond to the maps constructed within the velocity range −46.1 to −39.5 km s−1 (W5-NWa; Figure 2(a)) and −38.3 to −31.0 km s−1 (W5-NWb; Figure 2(c)), respectively. A grid of the 12CO(3 − 2) and 13CO(3 − 2) spectra over square regions of size ﹩2.3^{\prime} \times 2.3^{\prime} ﹩ are plotted in white and yellow, respectively. The 13CO(3 − 2) spectra are scaled up by 1.5 times and are boxcar smoothed by 20 channels, corresponding to a velocity smoothing of ∼1.1 km s−1. The dashed blue and red lines indicate the LSR velocities of W5-NWa and W5-NWb at −41.4 km s−1 and −36.3 km s−1, respectively. The green arrows labeled A, B, and C are the directions along which the PV slices are extracted, and the green circles mark the positions of the bridging features identified from the PV diagrams in Figure 5. (b) The 12CO(3 − 2) spectrum extracted over a bridging feature on the PV cut B shows a skewed single-emission profile.
Paper: Cloud–Cloud Collision and Cluster Formation in the W5-NW Complex
Authors: Namitha Issac, Anindya Saha, Saanika Choudhary, Aakash Chaudhary, Anandmayee Tej, Hong-Li Liu, Tie Liu, Maheswar Gopinathan
Figure caption:  12CO(3 − 2) (top panel) and 13CO(3 − 2) (bottom panel) integrated intensity maps of the region associated with the W5-NW complex. (a) 12CO(3 − 2) integrated intensity map over the velocity range −46.1 to −39.5 km s−1, corresponding to W5-NWa. (b) Same as (a) for the intermediate velocity range −39.5 to −38.3 km s−1. (c) Same as (a) with the integration velocity range −38.3 to −31.0 km s−1, corresponding to W5-NWb. The depression in W5-NWa and the peak in W5-NWb are marked as D and P, respectively. (d), (e), and (f) are for 13CO(3 − 2) in the same velocity ranges as (a), (b), and (c), respectively. The 13CO(3 − 2) integrated intensity maps are boxcar smoothed across 3 pixels. The schematic of the likely keyhole and key is shown in dashed lines in panels (a) and (c), respectively.
Paper: Cloud–Cloud Collision and Cluster Formation in the W5-NW Complex
Authors: Namitha Issac, Anindya Saha, Saanika Choudhary, Aakash Chaudhary, Anandmayee Tej, Hong-Li Liu, Tie Liu, Maheswar Gopinathan
Figure caption: Average spectra of 12CO(3 − 2) (blue) and 13CO(3 − 2) (red) towards W5-NW. The extracted spectra are averaged over the circular region shown in Figure 7 that covers the entire W5-NW complex. The 13CO(3 − 2) spectrum is scaled up by 1.5 times and is boxcar smoothed by 20 channels corresponding to a velocity smoothing of ∼1.1 km s−1. The double Gaussian fit to the 12CO(3 − 2) and 13CO(3 − 2) lines are depicted by dashed black and gray curves, respectively. The blue and red shaded regions highlight the velocity ranges over which the integrated intensity maps are constructed for W5-NWa and W5-NWb, respectively, and the vertical green lines indicate their LSR velocities.