adsabs/AstroCLIMB huggingface dataset:
Paper: Deep HST/UVIS Imaging of the Candidate Dark Galaxy CDG-1
Authors: Pieter van Dokkum, Dayi David Li, Roberto Abraham, Shany Danieli, Gwendolyn M. Eadie, William E. Harris, Aaron J. Romanowsky
Figure caption: Top left and center: section of the 6-orbit F200LP image, centered on the four globular clusters that constitute CDG-1. No diffuse light is detected between the clusters. Top right: same as top center, with an artificial 5″ × 5″ patch of diffuse light added. The patch has the same total brightness as the four globular clusters. Bottom left: F200LP 2σ surface brightness depth as a function of spatial scale. Bottom right: corresponding upper limit on the fraction of the total light that is in a diffuse component.
Paper: Discovery of an [O III] Emission Shell around the X-Ray Binary CI Cam
Authors: Robert A. Fesen, Marcel Drechsler, Nicolas Martino, Yann Sainty
Figure caption: Top Left: [O III] λ5007+Hα + RGB color composite of the western portion of the Galactic supernova remnant G150.3+4.5 showing an emission shell centered on CI Cam in upper right corner (from Fesen et al. 2024) Top right panels: [O III] and Hα images of the CI Cam emission shell. Bottom Left: Blowup of color composite image of CI Cam’s emission shell. Bottom Right: Negative [O III] image stretched to show faint emission in the direction of and surrounding CI Cam.
Paper: Predicting the Number of Radio Sources seen by both VLASS and LSST
Authors: Alex Tellez, Yjan Gordon, Keith Bechtol
Figure caption: Panel (a) shows the distribution of angular separations for VLASS/HSC matches (blue line), with the expected and actual matches from random positions shown by the red dotted line and gray histogram respectively. The black solid line shows the estimated reliability of a match as a function of separation. Panel (b) shows the percentage of VLASS sources with an optical counterpart as a function of i-band depth. The upper histogram in panel (b) shows the i-band magnitude distribution for HSC.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. VII. HD 141556 (χ Lupi)
Authors: Richard Monier
Figure caption: Left: synthesis of the 4500–4530 Å wavelength range for χ Lupi A (observed spectrum in black, synthetic in red). Right: synthesis of the Hg II line at 5677.10 Å for χ Lupi A.
Paper:  NIFTY-LS: Fast and Accurate Lomb–Scargle Periodograms Using a Non-uniform FFT
Authors: Lehman H. Garrison, Dan Foreman-Mackey, Yu-hsuan Shih, Alex Barnett
Figure caption: Left panel:  performance with N  f   ≈ 12N  d . “ASTROPY fast” is the PR89 method. The three NIFTY-LS methods use FINUFFT (CPU), FINUFFT (multi-threaded CPU), and CUFINUFFT (CUDA GPU). Right panel:  periodogram accuracy. See Section 2.2 regarding “ASTROPY (worst case)”. Plotted N  d  values are staggered for clarity.
Paper: Two Intriguing Transits of HIP 23309 Observed by TESS
Authors: Giovanni A. Gollotti, Anastasios Tzanidakis, Tobin M. Wainer, James R. A. Davenport
Figure caption: Top: TESS and ASAS-SN (green) light curves for Sectors 35 and 62 centered on the dips. Bottom: Archival HARPS measurements are shown (blue points), while vertical lines represent the TESS transit epochs. The black line represents the best-fit sine function to the HARPS data, with 100 samples drawn from the maximum likelihood (orange curves). The derived RV jitter is also shown, which is used as an additional uncertainty.
Paper: Spectroscopic Analysis of CWISE J151044.74−524923.5, A Wide L Dwarf Companion to the L 262-74 System
Authors: Léopold Gramaize, Adam C. Schneider, Thomas P. Bickle, Jonathan Gagné, Austin Rothermich, Federico Marocco, Jacqueline K. Faherty, Aaron M. Meisner, J. Davy Kirkpatrick, Mark Popinchalk, Marc J. Kuchner
Figure caption: The SOAR/TripleSpec4 spectrum of W1510−5249 in full resolution (gray) and smoothed (black) compared to the L6 standard 2MASS J10101480−0406499 (J. D. Kirkpatrick et al. 2010) on the top panel, and to the L6β standard 2MASSI J0103320+193536 (J. K. Faherty et al. 2012; K. N. Allers & M. C. Liu 2013) on the bottom panel. All spectra are gaussian smoothed using a width of 10 pixels and normalized between 1.27 and 1.29 μm.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Discovery of a Unique Close Quasar–DSFG Pair Linked by a [C II] Bridge at z = 5.63
Authors: Yongda Zhu, Tom J. L. C. Bakx, Ryota Ikeda, Hideki Umehata, George D. Becker, Christopher Cain, Jaclyn B. Champagne, Xiaohui Fan, Yoshinobu Fudamoto, Xiangyu Jin, Hai-Xia Ma, Yang Sun, Tsutomu T. Takeuchi, Wei Leong Tee
Figure caption: (a) ALMA continuum image of the quasar-DSFG system. (b), (c), (d) [C II] emission from J1133c, the [C II] bridge, and the quasar host, with labeled velocity offsets (Δv). (e) Pan-STARRS z-band image. Green contours indicate 5σ/9σ/13σ continuum detections, with black contours in (c) showing 1σ and 2σ [C II] bridge detections. The ALMA beam size is shown in gray. (f) [C II] spectra of J1133c and the quasar with Gaussian fits.
Paper: Contamination in Exoplanet Transit Spectroscopy with a Changing Stellar Surface
Authors: Yike Qiao, Sharon X. Wang, Zitao Lin
Figure caption: Left: Schematic of the transit light source effect. Right: The thin yellow lines illustrate the range of contamination spectra for K2-18 b. The thick yellow, orange, and brown lines represented the contamination spectra produced with specific F and ﹩F^{\prime} ﹩ values, as labeled in legend. The molecular line data are from HITRAN (I. E. Gordon et al. 2022).
Paper: J115307.93+353528.2—Spectroscopic Twin Binary, Composed of Solar Like Stars. Orbital Solution from Poorly Resolved Double-line Structure
Authors: Mikhail Yu. Kovalev, Xuefei Chen, Zhanwen Han
Figure caption: Example of multiple-epoch fitting for two epochs (a), (b). RV values from individual (including contaminated) spectra and multiple epochs fits and orbital solution (c).
Paper: HD 34382: A Photometrically Identified Candidate Centrifugal Magnetosphere Star
Authors: Thaddaeus Kiker, Veronica Diaz, Luke G. Bouma, Matt Shultz, Alexandre David-Uraz, Colin P. Folsom
Figure caption: Sector 44 TESS light curve showing periodic variations (top). Phase-folded light curve (middle-left). Radial velocity measurements with predicted Keplerian curves for putative secondary masses of 0.05 M ⊙ and 0.1 M ⊙ (middle-right). Barycenter-corrected Keck/HIRES spectra with Gaussian smoothing highlight line profile variability between nights for the Fe II, Si II, and Hα lines, where darker line colors correspond to observations taken at instances closer to unity in phase space (bottom).
Paper: Exploring Viscosity Effects in Accretion Disk Simulations: A Code Comparison between FLASH and Athena
Authors: Georgia Amy Richardson, Ryan Jeffrey Farber
Figure caption: Plots of mass accretion rate over time, with varying y-axis limits between plots. The top panel shows simulations without viscosity across three different resolutions (128, 256 and 512). The middle panel shows all viscosity cases (10−3, 10−4, 10−5, 10−6) at resolution 128. The bottom panel shows all resolutions at viscosity 10−3.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. IV. HD 149121 (28 Her) and HD 178065
Authors: Richard Monier
Figure caption: Left: line synthesis of the Hg II line at 5677.10 Å of HD 178065 (observed spectrum in black, synthetic spectrum in red), Right: the Cr II line at 6158.62 Å is observed in emission in the same spectrum.
Paper: Determination of Surface Abundances for HD 129174 (π 1 Boo)
Authors: Richard Monier
Figure caption: Left: line synthesis of the Hg II line at 3983.93 Å of HD 129174 (coadded spectrum in black, synthetic spectrum in red), Right: spectral synthesis of the He I lines at 4471.48 Å and the Mg II lines at 4481.15 and 4481.33 Å.
Paper: OH and H2O Maser Activities Among Long-period Variables
Authors: Tian Wu, Graeme H. Smith
Figure caption: Distribution of maser variables in a CMD that plots infrared color (J − K  s ) vs. absolute K  s  magnitude ﹩({M}_{{K}_{s}})﹩. The black solid line is an H2O-maser division line and the black dashed line is an OH-maser division line, which depict the infrared CMD boundaries of circumstellar maser occurrence among LPVs.
Paper: The Abundance Pattern of The A2.5V Star HD 176687 (ζ Sagitarii A) In A Triple System
Authors: Richard Monier
Figure caption: Left: Comparison of the FUV SED of HD 176687 (in black) to that of α Lyr (in blue), θ Leo (in green) and α PsA (in red), Right: Synthesis of the O I lines from (observed spectrum in black, synthetic spectrum in red).
Paper: Ultraviolet and Blue Optical Imaging of UVCANDELS
Authors: Xin Wang, Harry I. Teplitz, Lei Sun, Marc Rafelski, Norman Grogin, Laura Prichard, Ben Sunnquist, Anahita Alavi, Rogier A. Windhorst, Anton M. Koekemoer, Teresa Ashcraft, Micaela Bagley, Ivano Baronchelli, Guillermo Barro, Alex Blanche, Gabriel Brammer, Adam Broussard, Timothy Carleton, Nima Chartab, Yingjie Cheng, Alex Codoreanu, Seth Cohen, James Colbert, Christopher Conselice, Y. Sophia Dai, Behnam Darvish, Romeel Davé, Laura DeGroot, Duilia De Mello, Mark Dickinson, Najmeh Emami, Henry Ferguson, Leonardo Ferreira, Keely Finkelstein, Steven Finkelstein, Jonathan P. Gardner, Eric Gawiser, Timothy Gburek, Mauro Giavalisco, Andrea Grazian, Caryl Gronwall, Yicheng Guo, Pablo Arrabal Haro, Nimish P. Hathi, Matthew Hayes, Shoubaneh Hemmati, Justin Howell, Kartheik Iyer, Rolf A. Jansen, Zhiyuan Ji, Sugata Kaviraj, Peter Kurczynski, Ilin Lazar, Ray A. Lucas, John MacKenty, Vihang Mehta, Kameswara Bharadwaj Mantha, Alec Martin, Garreth Martin, Tyler McCabe, Bahram Mobasher, Kalina V. Nedkova, Robert O'Connell, Charlotte Olsen, Lillian Otteson, Swara Ravindranath, Caleb Redshaw, Brant Robertson, Michael Rutkowski, Zahra Sattari, Claudia Scarlata, Brian Siana, Brent M. Smith, Emmaris Soto, Eros Vanzella, L. Y. Aaron Yung, Bonnabelle Zabelle
Figure caption: The UVCANDELS F275W coadded count-rate and exposure maps for the four premier CANDELS fields: GOODS-N, GOODS-S, COSMOS, and EGS, shown in panels (a), (b), (c), and (d) respectively. For all four fields, the exposure maps are on the same color scale represented by the color bar on the bottom. In all maps, we also overlay the footprints of the CANDELS F160W mosaics in magenta lines.
Paper: The Spectral ANalog of Dwarfs (SAND): New Model Atmospheres with Varying Chemistry for Galactic Archaeology with Ultracool Dwarfs
Authors: Efrain Alvarado, Roman Gerasimov, Adam J. Burgasser, Hunter Brooks, Christian Aganze, Christopher A. Theissen
Figure caption: Left: SAND spectral sequence with ﹩\mathrm{log}(g)=5.0﹩, [Fe/H] = −1.5, [α/Fe] = 0, and 800 K ≤ T eff ≤ 2400 K. Right: SAND spectral sequence with T eff = 1900 K, ﹩\mathrm{log}(g)=5.0﹩, and varying metallicity and alpha enrichment. In both panels, key molecular absorption bands (H2O, CH4, TiO), atomic lines of K, and the approximate wavelength range of collision-induced absorption by H2 are highlighted. The spectra were downsampled to R ∼ 1000 for clarity.
Paper: Galactic Archeology with Luminous Red Giant Oscillations in Gaia DR3 Photometry
Authors: Bryan Nnadi, Samuel Grunblatt
Figure caption: Distance estimation using the P–L relation of the LMC for the variable star 2MASS J06013711-6641042. (a) The lightcurve using Gaia photometric data. (b) The period spectrum using Lomb–Scargle (Astropy Collaboration et al. 2018; Cloutier et al. 2018), highlighting peak power in red. (c) The P–L relation for the LMC colored by oscillation amplitude, where the median, upper and lower uncertainties in absolute magnitude (horizontal lines) are inferred from the measured period (vertical line). (d) Histogram depicting the Gaia parallax distances and P–L distances. (e) Histogram comparing Gaia parallax and P–L distance uncertainties.
Paper: A Radio Galaxy Gravitational Lens in the COSMOS-Web Survey
Authors: Charlotte Moore, Mark Lacy
Figure caption: Left COSMOS 5914+1219, RGB color composite using the HST F606W (blue) and JWST F277W (green) and F444W (red) bands; middle best-fitting of COSMOS 5914+1219 and its companion in the F277W band. Right The masked emission from the lensed galaxy in the F277W band.
Paper: Lopsided Galaxy Distributions in Massive TNG300 Clusters
Authors: Kelsey A. Mangis, Tereasa G. Brainerd
Figure caption: Pairwise clustering statistic, P(Δϕ) for galaxies in the 280 most massive TNG300 clusters at z = 0. Dotted lines in each panel indicate P(Δϕ) for uniform circular distributions. Top: all cluster galaxies. Middle: red cluster galaxies (red circles) and blue cluster galaxies (blue circles). Bottom: galaxies in clusters with less than 60 members (squares) and galaxies in clusters with more than 150 members (crosses).
Paper: Discovery of Jupiter Family Comet 2011 UG104 Through AI Enhanced Citizen Science
Authors: Jarod A. DeSpain, Colin Orion Chandler, Nima Sedaghat, William J. Oldroyd, Chadwick A. Trujillo, William A. Burris, Henry H. Hsieh, Jay K. Kueny, Kennedy A. Farrell, Mark Jesus Mendoza Magbanua, Scott S. Sheppard, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano, Al Lamperti, José A. da Silva Campos, Brian L. Goodwin, Ivan A. Terentev, Charles J. A. Dukes
Figure caption: 2011 UG104 (center in each image) is shown in these archival DECam images. The field of view is 63″ × 63″, with north up and east left. The anti-motion (red arrow) and anti-solar (yellow arrow) directions are marked. (a) UT 2021 February 25, 90 s i-band (Prop. ID 2019A-0305, PI Drlica-Wagner, observers J. Carballo, D. James). A prominent tail is pointed primarily in the anti-solar direction. (b) UT 2021 March 29, 150 s Y-band (Prop. ID 2021A-0149, PI Zenteno, observer A. Zenteno). (c) UT 2021 April 26, 67 s Y-band (Prop. ID 2021A-0149, PI Zenteno, observer A. Zenteno).
Paper: Direct Imaging Detection of the Protoplanet AB Aur b at Wavelengths Covering Paβ 
Authors: Thayne Currie
Figure caption: My SCExAO/CHARIS and reprocessed Keck/NIRC2 AB Aurigae images (top panels): insets show the instrumental PSFs. (bottom-left) Keck/NIRC2 contrast curve for different source models. (bottom-right) Keck/NIRC2 image with injected point sources (pt) and extended sources (ext).
Paper: Satellite Visibility During the 2024 April Total Eclipse
Authors: Samantha M. Lawler, Hanno Rein, Aaron C. Boley
Figure caption: All-sky visibility plot for current Starlink satellites during totality, observed from Kingston, Ontario. Color shows visible g-magnitudes. Overall, satellites get gradually brighter toward zenith as the range decreases, with the shadow of the Moon causing fainter satellites close to the position of the Sun in the sky.
Paper: A Possible Cyclotron Feature of the Gamma-Ray Binary 4FGL J1405.1–6119
Authors: Sung-Chieh Chiu, Kwan-Lok Li
Figure caption: Data I and II correspond to (a) and (b), respectively. In both figure, the XMM-Newton detectors MOS1, MOS2 and PN represent with black, red and green color, and the fitting result is fixed at N H = 6.9 × 1022 cm2. The soft X-ray band (below 0.4 keV) of the PN observations is dominated by background. Thus, the binning effect (i.e., >20 counts bin−1) is not obvious.
Paper:  extrabol: A Python Package for Estimating Bolometric Light Curves of Thermal Transients
Authors: Ian Thornton, V. Ashley Villar, Sebastian Gomez, Griffin Hosseinzadeh
Figure caption: Example output plots of extrabol for SN 2010bc (data originally from Villar et al. 2020). Upper left: multiband Pan-STARRS Medium Deep Survey griz light curve (points). The GPR estimate is marked as solid lines, with 1σ uncertainty ranges given by shaded regions. Upper right: bolometric light curve estimate. Lower: estimated blackbody temperature and radius estimate over time. These estimates are used to generate the bolometric light curve.
Paper: Characterization of Instrumental Polarization in the MOPTOP Instrument
Authors: Denis Bernardes, Iain Steele, Helen Jermak, Callum McCall
Figure caption: Spatial distribution of the residual values obtained for the q (red dots) and u (blue dots) Stokes parameters, as a function of the filters BVRIL. The adjusted planes for the respective parameters are also presented. The constants A, B, and C of Equation (1) obtained for the adjustments are presented above the graph. We caution that the L band fits are not particularly well constrained.
Paper: Recent Outbursts of the High-mass X-Ray Binary CI Camelopardalis
Authors: David H. Hinzel
Figure caption: Light Curve HMXB CI Cam: The numbers 1–7 indicate the dates of the outbursts detected in the visual/Johnson V photometry as discussed above. The BRI data has little if any correlation to the outbursts.
Paper: New Pulsating Variable Stars and Eclipsing Binaries Around BL Cam 
Authors: Ai-Ying Zhou
Figure caption: Examples of newly identified TESS variables. Top row: a δ Sct star; Second row: a γ Dor star; Third row: a hybrid δ Sct-γ Dor stars; Rows 4–7: eight γ Dor stars; Row 8: two Algol-type (detached) eclipsing binaries: the left one exhibits δ Sct primary component. All graphs were generated through automated batch processing.
Paper: Exploration of Stellar Variability in 20 s Cadence TESS Data
Authors: Cooper DeVane-Prugh, Carmen Michaud, Jamie Tayar, Daniel J. Stevens, Rachael Beaton, Johanna Teske, Jennifer van Saders
Figure caption: For our sample (Top Left) we replicate the expected scaling between CDPP and magnitude (Top Middle) and show these scalings as a function of timescale (Top Right). Once we correct for the scaling with brightness (Bottom Left), we search for any residual correlations with stellar properties (Bottom Middle) and find that the CDPP as a function of surface gravity depends on the timescale of interest (Bottom Right).
Paper: Prospects for the Crossing by Earth of Comet C/2023 A3 Tsuchinshan-ATLAS’s Ion Tail
Authors: Samuel R. Grant, Geraint H. Jones
Figure caption: (Left) Impact parameters plotted for Earth and comet C/2023 A3 (Tsuchinshan-ATLAS) for purely radial solar wind velocities 200, 450, and 900 km s−1. In this case, slower solar wind speeds appear to increase the likelihood of a tail encounter. (Right) Relative positions of the Earth, Sun, and C/2023 A3, in a frame where the Sun–Earth line is fixed. The plane represents that of the ecliptic, with grid lines spaced at 0.1 au. The comet’s position is shown every 6 hr, with legs showing its 3D position relative to the ecliptic plane—orange when south of the ecliptic, red when north. Also shown in blue is the ion tail profile simulated for 2024 October 13 at 10:00 UTC, for a radial solar wind flow of 300 km−1. Under these circumstances, the ion tail axis would pass slightly north of Earth.
Paper: Direct Evidence for Preburst Stage of Gamma-Ray Burst from GRB 221009A Data
Authors: Qing Liu, Hanlin Song, Bo-Qiang Ma
Figure caption: Subfigure (a) shows the light curve of GRB 221009A from the observation of Fermi Gamma-ray Burst Monitor (GBM, NaI-n4, NaI-n6, NaI-n7 and NaI-n8, with photon energy range of 8–260 keV). The time bin is chosen as 64 ms. Subfigure (b) shows the multi-GeV photons of GRB 221009A from the observation of Fermi Large Area Telescope (LAT, with photon energy range of 0.1–100 GeV). The vertical dashed line denotes the trigger time of Fermi Gamma-ray Burst Monitor (S. Lesage et al. 2023). Subfigure (c) shows the released multi-TeV photons of GRB 221009A detected by KM2A detector of LHAASO (The LHAASO Collaboration 2023), with energies larger than 3 TeV and time period during −70 to 1400 s.
Paper:  At First Sight! Zero-shot Classification of Astronomical Images with Large Multimodal Models
Authors: Dimitrios Tanoglidis, Bhuvnesh Jain
Figure caption: The prompts used to instruct the multimodal models on the two classification tasks (upper part), as well as the resulting confusion matrices, obtained using the GPT-4o (middle part) and LLaVa-NeXT (lower part) models. The confusion matrices compare the predicted vs. the true labels for the example images in our test data sets. The numbers in parentheses correspond to the fraction of images with true label in class x that were predicted to belong to class y.
Paper: A Candidate Dark Matter Deficient Dwarf Galaxy in the Fornax Cluster Identified through Overluminous Star Clusters
Authors: Aaron J. Romanowsky, Enrique Cabrera, Steven R. Janssens
Figure caption: Panels (a), (b), (c): DECaLS DR10 images of NGC 1052-DF2, FCC 224, and FCC 316, on the same spatial and brightness scales. Panel (d): GC luminosity functions of FCC 316 (orange filled histogram), FCC 224 (blue open histogram), and a standard model (dashed curve). The 50% completeness limit is shown as a vertical dotted line. Panels (e), (f): HST/WFPC2 F555W images of FCC 224 and FCC 316. GC candidates brighter than M  V  ∼ − 8 are marked with dark blue circles.
Paper: Using the COSMIC Population Synthesis Code to Investigate How Metallicity Affects the Rates of Interacting Binaries
Authors: Ayanah L. Cason, Nicole Lloyd-Ronning, Roseanne Cheng
Figure caption: Left Panel: evolution time of our selected binary systems for our selection criteria) for six different metallicities. Right Panel: number of interacting binary systems composed of a massive star with a black hole companion divided by the total number of stars in the simulation vs. metallicity.
Paper: The Escape Probability of Photons Emitted in a Spherical Homogeneous Shell
Authors: Eli Dwek, Richard G. Arendt
Figure caption: Top panel: Cross section through the center of the homogeneous spherical shell, characterized by inner and outer radii R 1 and R 2, respectively. t depicts the path length traversed by photons exiting the shell at angle θ with respect to the normal at the exit point A. The figure represents three representative cases for the angle θ: θ less than, equal to, and greater than θ c, where ﹩{\theta }_{{\rm{c}}}=\arcsin ({R}_{1}/{R}_{2})﹩. Bottom panel: The escape probability as a function of the optical depth. The dashed red line represents the escape probability for a filled sphere, given by Equation (11). Other lines represent the escape probability from a sphere with increasingly larger cavities with radii R 1/R 2 ranging from 0 (green curve) to 0.99 (blue curve).
Paper: New Transit Timing Observations of WASP-12b from TESS Sectors 71 and 72
Authors: Zoutong Shen
Figure caption:  O − C diagram for WASP-12b transit (circles) and occultation (triangles) times.
Paper: Discovery of Raman-scattered C II Lines in V366 Carinae with GHOST/Gemini South
Authors: Jeong-Eun Heo, Miji Jeong
Figure caption: Top: The GHOST spectrum of V366 Car, showing the Raman O VI and C II features. Bottom: A zoom-in view of the Raman-scattered C II features, along with the fitting results. The blue and light-blue shaded regions represent the best-fit single Gaussian profiles for the Raman C II features.
Paper: LOFAR Non-detections of SN 2023ixf in its First Year Post-explosion
Authors: R. Timmerman, M. Arias, A. Botteon
Figure caption: Radio continuum detections of SN 2023ixf obtained at higher frequencies combined with the non-detections obtained from LOFAR observations indicated at the 3σ noise level.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Tentative Blazar Candidate EP240709A Associated with 4FGL J0031.5−5648: NICER and Archival Multiwavelength Observations
Authors: Mason Ng, Jeremy Hare, Gaurava K. Jaisawal, Christian Malacaria, Craig B. Markwardt, Andrea Sanna
Figure caption: (a) 0.4–3.0 keV background-subtracted NICER light curve (64 s bins); (b) Power law photon index; and (c) 0.3–10.0 keV unabsorbed flux in units of 10−12 erg s−1 cm−2. (d) variability index vs. curvature significance; and (e) curvature parameter and peak energy (in MeV).
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. IX. HD 27295 (53 Tau)
Authors: Richard Monier
Figure caption: Left: Line synthesis of the 4500–4540 Å range (UVES spectrum in black, synthetic spectrum in red), Right: Absence of Hg II line at 5677.10 Å in the UVES spectrum of 53 Tau.