adsabs/AstroCLIMB huggingface dataset:
Paper: A Potential Host Galaxy Association for FRB 20190605C
Authors: Obinna Modilim, Kaitlyn Shin, Kiyoshi Masui, Daniele Michilli, Adaeze L. Ibik, Michael Calzadilla, Mohit Bhardwaj
Figure caption: Top: DECaLS image of the baseband localization regions for FRB 20190605C. The 1σ, 2σ, and 3σ localization regions are marked with solid, dashed, and dotted ellipses. The PATH probabilities of both galaxies are labeled in red. Bottom: the observed (cyan) and modeled (black) spectrum of 2d-TGN109Z, with identified spectral lines labeled. The gray regions represent unreliable noisy data and a chip gap.
Paper: Discovery of Two New Eruptions of the Ultrashort Recurrence Time Nova M31N 2017-01e 
Authors: Allen W. Shafter, Jingyuan Zhao, 经远 赵, Kamil Hornoch, Hana Kučáková, Kenta Taguchi, Jiashuo Zhang, 家硕 张, Jia You, 嘉 游, Binyu Wang, 彬羽 王, Runwei Xu, 润玮 许, Weiye Wang, 炜晔 王, Yuqing Ren, 育庆 任, Lanhe Ding, 岚贺 丁, Xiaochang Yan, 小畅 严, Mi Zhang, 宓 张, Wei-Hao Wang, 为豪 王, Howard E. Bond, Robert Williams, Gregory R. Zeimann
Figure caption: Top Panel: the positions of M31N 2024-08c and 2014-06c (white) are compared with 2017-01e (black) in the left and right panels, respectively. The positions of the novae are coincident to an accuracy of less than 1″. Middle panel: the lightcurves for M31N 2024-08c and 2014-06c are shown in the left and right panels, respectively (symbol key given in Facilities section). The 2024-08c lightcurve shows that t 2 ∼ 5 days, which is consistent with other observed eruptions. The GIT point is from J. Basu et al. (2024). Bottom left panel: the O − C plot showing the times of the 6 observed eruptions of M31N 2017-01e. Bottom right panel: our HET spectrum of the putative quiescent optical counterpart, appearing to show a luminous B-type star.(The data used to create this figure are available.)
Paper: The Coronal Lines of the High-excitation, Fe II-type Nova V2467 Cygni
Authors: Richard J. Rudy, Ray W. Russell, Michael L. Sitko, David K. Lynch, Charles E. Woodward
Figure caption: Composite 0.47–5.2 μm spectrum of the nova V2467 Cygni from the period of maximum excitation. Data were acquired 2008 July 29 for the top panel and 2008 May 9 for other panels. Colored labels are used to distinguish among lines: red labels denote so-called coronal lines, collisionally excited lines from species with ionization energies of ≥100 eV. Blue labels denote lines that we have associated with C VI. In the third panel, tick marks indicate the H I Brackett lines. Emission lines whose identifications are uncertain are labeled with question marks, as are unknown lines that include the measured wavelength. The highest excitation lines, [S IX] 1.2523 μm, [Si X] 1.4305 μm, [Si IX] 3.9357 μm, have pronounced double-peaked profiles not seen in the lower excitation features. Low ionization features ([N II] 0.5754 μm and [O II] 0.7319 μm, 0.7329 μm) and lines from neutral species ([O I] 0.6300 μm, 0.6363 μm and [N I] 1.0405 μm) are present as well.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Confirmation of Recurrent Activity of Main-Belt Comet 456P/PANSTARRS (P/2021 L4)
Authors: Henry H. Hsieh, Scott S. Sheppard, Audrey Thirouin
Figure caption: Composite images of 456P from (a) Gemini, (b) Magellan, and (c) LDT, where the comet is at the center of each panel. North (N), East (E), and the projected antisolar (−⊙) and negative heliocentric velocity (−v) directions are shown in each panel.
Paper: Multiple Periods in the Dwarf Nova GZ Cancri
Authors: Albert Bruch
Figure caption: Top: ASAS-SN light curves of GZ Cnc in three observing seasons. Individual data points are connected by red dotted lines to guide the eye. The horizontal bars indicate time intervals covered by TESS light curves. Middle: TESS light curves LC#1 and LC#3 of GZ Cnc together with their time resolved power spectra drawn on the same timescale. The frequencies of the negative (Σ−) and positive (Σ+) superhumps, and of the orbital variations (Ω) are indicated at the right. Three one-day sections of LC#1 are amplified to highlight the different characteristics of distinct light curve phases. Bottom: TESS light curve LC#2 together with the time resolved power spectrum that exhibits periodic variations at the maxima and decline phases of the outbursts. The conventional power spectrum of the entire light curve shown in the lower left panel contains a broad feature composed of several narrow spikes close to the orbital frequency of GZ Cnc, caused by slight differences of the frequencies occurring during the individual outbursts (but all compatible with the orbital frequency within the error margins).
Paper: qCMOS Detectors and the Case of Hypothetical Primordial Black Holes in the Solar System, near Earth Objects, Transients, and Other High-cadence Observations
Authors: Martin M. Roth
Figure caption: Simulation of the image of a star (V = 19) showing results for qCMOS sensor (left) and CCD (right). In the example images on top, obtained for 10 s shutter open time for both sensors, the signal-to-noise ratio (SNR) is measured as 36 for the qCMOS, and 21 for the CCD. The scatter plots on the bottom present measured fluxes vs. time series effective integration time for a total of 10,000 realizations, illustrating how the CCD SNR rapidly degrades as the ROT becomes comparable to the time step.
Paper: The γ-Ray-emitting BL Lac 4FGL J1219.0+3653 in the Radio
Authors: Máté Krezinger, Krisztina Éva Gabányi, Sándor Frey
Figure caption: (a) Naturally weighted 7.6 GHz total intensity image of J1219+3657. The peak intensity is 11 mJy beam−1, the lowest contours are drawn at ±0.63 mJy beam−1, the positive levels increase by a factor of 2. The FWHM size of the elliptical Gaussian restoring beam is 2.2 mas × 0.9 mas at major axis position angle ﹩4\mathop{.}\limits^{^\circ }3﹩. Red cross marks the Gaia optical position, its size indicates the 1σpos uncertainty. (b) Total (black) and VLBI (blue) continuum radio spectra of J1219+3657. Shading represents 1σ uncertainty of the fits for power-law spectral indices.
Paper: Symmetry in Hyper Suprime-Cam Galaxy Spin Directions
Authors: Richard Stiskalek, Harry Desmond
Figure caption: Left: Sky distribution of the HSC DR3 galaxies in equatorial Mollweide projection, with galaxies spinning S-wise in blue and Z-wise in red. Right: Corner plot from the monopole–plus–dipole inference, indicating a dipole magnitude D consistent with 0 and a monopole M consistent with 0.5.
Paper: The Impact of AGN Jet Speed on the Lyα Forest Flux Power Spectrum
Authors: Megan Pirecki, Megan Taylor Tillman, Blakesley Burkhart
Figure caption: The redshift evolution of the Lyα forest 1D transmitted flux power spectrum for varying AGN jet speed. Top row: the predicted P1D. Bottom row: P1D ratios relative to the fiducial prediction. The black lines are the fiducial results, red corresponds to the highest value for AGN jet speed, and blue is the lowest value. The dashed gray line represents a 5% difference from fiducial.
Paper: Gas Dynamics in 3 “Dippers”: EPIC 203850058, EPIC 204638512, and EPIC 205151387 in 2017–2018
Authors: Michael L. Sitko, Ray W. Russell, Korash Assani, Ammar Bayyari, Dakotah Tyler, Carey M. Lisse, Carol A. Grady, William C. Danchi
Figure caption: The region around He I and Paγ for the three dippers. For EPIC 204638512, the He I line consists of a slightly blueshifted absorption line for all 4 epochs, suggesting an net outflowing gas. For EPIC 205151387, at its brightest state the He I and Paγ lines are in emission, while as the continuum flux drops due to increased dust extinction, the He I (and perhaps the Paγ line) evolves into a profile indicative of inflowing gas. For EPIC 203850058, in 2017, the He I line is in absorption with a red-degraded wing, indicating outflowing gas. On these nights, the Paγ is in emission. The single spectrum from 2018 shows no absorption in He I and no emission in the Paγ line. Dates are given in the format of yymmdd.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. XII. HD 7374 (87 Psc)
Authors: Richard Monier
Figure caption: Left: absence of the Hg II line at 5677.10 Å (observed mean ELODIE spectrum of 87 Psc in black), Right: synthesis of the 4500–4540 Å range (observed mean ELODIE spectrum in black, synthetic spectrum in red).
Paper: Emission-line Ratios and Ionization Conditions of CEERS Star-forming Galaxies with JWST/NIRSpec
Authors: Ansh R. Gupta, Allison Kirkpatrick, Vital Fernández, Pablo Arrabal Haro, Bren E. Backhaus, Nikko J. Cleri, Norman A. Grogin, Anton M. Koekemoer
Figure caption: Top panel: The SFG main sequence defined by D. Elbaz et al. (2011). We neglect dust attenuation, making these sSFR measurements lower limits. The sSFR error is dominated by stellar mass uncertainty. Populations above and below the MS (yellow stripe) reveal starbusting and quenching galaxies. Bottom 3 panels: [O III]λ5008/Hβ vs. [Ne III]λ3870/[O II]λ3728 line ratio diagrams, shaded by SFR, sSFR, and excess sSFR. The dashed black line is the empirical division at z ∼ 1.5 between SFGs (below) and AGN (above) (B. E. Backhaus et al. 2022). The line ratios appear most strongly correlated with sSFR.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: Robust Support for Semi-automated Reductions of Keck/NIRSPEC Data Using PypeIt
Authors: Adolfo S. Carvalho, Greg Doppmann, Kyle B. Westfall, Debora Pelliccia, J. Xavier Prochaska, Joseph Hennawi, Frederick B. Davies, Max Brodheim, Feige Wang, Ryan Cooke
Figure caption: Upper Left: a sample quality assurance plot from the wavelength calibration of Order 60 in the J band. Upper Right: order 60 of the A0V telluric standard spectrum (black) and the PHOENIX model (red) used to remove the Paβ line to produce a telluric absorption spectrum. Bottom Panel: a plot of Order 65 of the science spectrum (black), the telluric spectrum (green) and the telluric-corrected spectrum (red). Notice that the fringing is also removed by the division by the telluric absorption spectrum.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. V. HD 174933 (112 Her)
Authors: Richard Monier
Figure caption: Left: Synthesis of the 4500–4540 Å wavelength range (observed spectrum in black, synthetic in red) Right: Synthesis of the Hg II line at 5677.10 Å.
Paper: A Comment on the Solar Activity Level in 1744 by Diego de Torres Villarroel
Authors: A. J. P. Aparicio, J. M. Vaquero
Figure caption: Frontispiece of the booklet entitled “Juicio, y pronostico del nuevo cometa, que apareció sobre nuestro orizonte el dia siete de enero de este año de 1744” [Opinion and prognosis of the new comet that appeared on our horizon on January 7th of this year 1744] by Diego de Torres Villarroel.
Paper: Determination of the Abundance of Mercury from the Hg II Line at 5677.10 Å in Late B-type Stars. VI. HD 173524 (46 Dra)
Authors: Richard Monier
Figure caption: Left: Synthesis of the 4510–4530 Å wavelength range for 46 Dra A (observed spectrum in black, synthetic in red) Right: Synthesis of the Hg II line at 5677.10 Å.
Paper: Cometary Activity from Minor Planet 2015 VP51 Discovered with Citizen Science
Authors: Maxwell K. Frissell, Colin Orion Chandler, William J. Oldroyd, Chadwick A. Trujillo, Nima Sedaghat, William A. Burris, Jay K. Kueny, Jarod A. DeSpain, Kennedy A. Farrell, Henry H. Hsieh, 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: 2015 VP51 is at the center of these 63″ × 63″ images; North is up, East left. Red outlined black arrows and yellow filled arrows indicate the anti-motion and anti-solar directions, as project on the sky. (a) UT 2015 August 2: Co-addition of 3 × 240 s i-band exposures captured with the OmegaCAM instrument on the 2.6 m VLT Survey Camera (VST) atop Cerro Paranal (Chile) as part of the Kilo-Degree Survey (KiDS; K. Kuijken et al. 2019). (b) UT 2015 September 13: Co-addition of 3 (1 × 90 s g-band, 1 × 90 s r-band, 1 × 90 s i-band) DECam images (Prop. ID 2012B-0001, PI Frieman, observers Josh Frieman, Devon Hollowood, Ofer Lahav, Alex Kim). (c) UT 2015 October 18: Co-addition of 2 (1 × 90 s g-band, 1 × 90 s r-band) DECam images (Prop. ID 2012B-0001, PI Frieman, observers William Wester, Lucas Beaufore, Ann Elliott).
Paper: On the Plasma Quasi-thermal Noise in the Outer Heliosphere
Authors: Nicole Meyer-Vernet, Alain Lecacheux
Figure caption: Ratio of the drift speed v  D  to the electron thermal speed v TH observed by Voyager 2 as a function of time (in years) and heliocentric distance R, approximating the electron temperature by the proton one. The ratio v  D /v TH is close to unity in most of the outer heliosphere, until the crossing of the termination shock where it drops off abruptly.
Paper: The Hybrid Debris Disk Host Star HD 21997 is a High-frequency Delta Scuti Pulsator
Authors: Aldo G. Sepulveda, Timothy R. Bedding, Simon J. Murphy, Luca Matrà, Daniel Huber, Zhoujian Zhang
Figure caption: (a): TESS amplitude spectrum of HD 21997 zoomed in on the region of significant pulsations. Significant frequencies from our prewhitening procedure are denoted by black downward triangles. (b): Gaia DR3 color–magnitude diagram generated following Sepulveda et al. (2022). Orange diamonds are a sample of Kepler δ Scuti stars from Murphy et al. (2019) and small gray dots are non-pulsating KIC stars. HD 21997, whose color and absolute magnitude were calculated using A  V  = 0.075 (Chen et al. 2014), is overplotted as a large cyan star.
Paper: Intermediate Gas Phases within Turbulent Radiative Mixing Layers
Authors: Meg Georgina Blackburn, Ryan Jeffrey Farber
Figure caption: Upper: temperature distributions weighted by mass and volume for T cold = 400 K with an overdensity of χ = 3000 shown at 10.0 Myr. Lower: volume-weighted temperature distributions for T cold = 400 K, 103 K and 104K in descending order, with overdensities of χ = 100, 1000, 3000 at times of 0.0, 2.5 and 5.0 Myr.
Paper: SKYSURF-5: Probing the Integrated Galaxy Light with a SDSS-SKYSURF Cross-matched Catalog
Authors: Purvansh Bhatia, Timothy Carleton, Rogier A. Windhorst, Rolf A. Jansen, Rosalia O'Brien
Figure caption: A histogram of the r-band IGL for all SKYSURF images with SDSS overlap. The peak of this distribution is consistent with previous studies (accounting for SDSS incompleteness), but there is a significant tail toward higher IGL values. The identification of fields with high IGL values can be used to flag instances where HST was preferentially pointed to overdense regions of sky.
Paper: Do We Finally Know all Stellar and Substellar Neighbors within 10 pc of the Sun?
Authors: Ralf-Dieter Scholz, Alexey Mints
Figure caption: (a) Figure 1 of Henry et al. (1997) comparing observed cumulative numbers of systems (black dots) with expectations (black solid line) assuming complete knowledge within 5 pc and constant number density up to 10 pc. Overplotted are new numbers from Kirkpatrick et al. (2024) (red crosses). (b) New numbers from Kirkpatrick et al. (2024) (red crosses) and new expectations (blue solid line) using the same assumptions again. (c) Systems density as a function of distance from the Sun (black curve). Gray and light gray shaded areas show one and 2σ ranges assuming Poisson distribution of counts in each distance bin. The blue line indicates the mean system density (0.081 pc−3) within 10 pc.
Paper: Absorption in the Spectrum of a Background AGN by C II* by the Supernova Remnant G354-33
Authors: John C. Raymond, Connor Griscom
Figure caption: The C II wavelength region of the spectrum of J2017-4516. The absorption features at −50 km s−1 (−65 km s−1 LSR) are indicated by the dotted lines. Far stronger C II absorption from the ground state is also present. Absorption from the excited state at about −2 km s−1 is seen, but it is relatively weak compared to the highly saturated zero velocity absorption from the ground state. Strong absorption features of Ly 7 and Ly 8 at a redshift of 1.44 are also present.
Paper: Einasto Gravitational Potentials have Difficulty to Hold Spherically Symmetric Stellar Systems with Cores
Authors: Jorge Sánchez Almeida
Figure caption: (a) Stellar density profile with a core (the black line) together with the mass density giving rise to a NFW potential (the red line) and an Einasto potential (the blue line). (b) Distribution function required from the stellar profile to reside in the corresponding NFW potential (the red line) and in the Einasto potential (the blue line). In both cases, f(ϵ) becomes negative (the dashed lines). The parameters were chosen to represent a dwarf galaxy with M ⋆ ≃ 5 × 105 M ⊙.
Paper:  shock_cooling_curve: A Python-based Package for Extensive and Efficient Modeling of Shock Cooling Emission in Supernovae
Authors: Padma Venkatraman, Wynn Jacobson-Galán
Figure caption: Best-fit results with 1σ errors for SN2021gno obtained from MCMC sampling. The observed photometry is presented in AB magnitude system (Jacobson-Galán et al. 2022). Vertical red dashed line marks end of SCE timescale. Best-fit parameters along with the goodness-of-fit reduced chi-squared (﹩{\chi }_{\nu }^{2}﹩) value is provided at the top right. Filters are shown at the bottom of the figure.
Paper: An Enigmatic High Excitation Nebula in IC 1613 Dwarf Galaxy
Authors: S. Taibi, M. M. Roth, G. Battaglia, S. Kamann
Figure caption: Top: Emission-line map of the central MUSE pointing in IC 1613; H α  colored in red, [S II] in blue, and [O III] in green. The high excitation nebula is found in the top-right corner and highlighted in panel (A), while in panel (B) is shown the corresponding broad-band image, revealing no obvious hot star that could be ionizing the nebula. Bottom: Integrated spectrum of the [O III]-bright nebula in units of erg cm−2 s−1Å−1, typical for a high excitation planetary nebula.
Paper: Is the Far-ultraviolet Flux of 21 Com Anticorrelated to its Optical Brightness?
Authors: Richard Monier
Figure caption: Left: The variations of the FES counts of 21 Com between rotational phases ϕ = 0.00 and ϕ = 0.46, Right: The corresponding evolution of the FUV flux in a pseudo-continuum window at 1540 Å.
Paper: The Infrared Variability of V1647 Ori over 26 yr with Spitzer, (NEO)WISE, and ISO
Authors: Chinmay S. Kulkarni, Thomas Behling, Nathanael Burns-Watson, Jason Jones, Tyler Robbins, S. Thomas Megeath, Samuel Federman, William J. Fischer, Robert Gutermuth, Riwaj Pokhrel, Wafa Zakri, Savio B. Oliveira
Figure caption: Top: light curve of V1647 Ori at 4–8 μm showing change in Δm with MJD. This includes data from ISO, Spitzer, WISE, and NEOWISE. The blue vertical dashed line marks the initial outburst date (Briceño et al. 2004). The green vertical dashed lines mark the duration of the dip back to pre-outbursts levels seen in visible-light magnitudes (Fischer et al. 2023). Bottom: magnitude difference between ISO (1997) and Spitzer (2004) data of all detected YSOs in Orion with the median difference subtracted out. We used the difference between the 6.7 μm ISO band and the 5.8 μm (left) and 8.0 μm (center) Spitzer bands. The two Spitzer wavelength bands are combined on the rightmost plot (see text). The horizontal dotted lines mark the median absolute deviation of the difference at ±0.332, 0.236, 0.265 respectively from left to right. We use the combined value in the top plot, with the 5.8 and 8 μm values providing the displayed uncertainty range.(The data used to create this figure are available.)
Paper: James Webb Space Telescope Spectra of Cold Brown Dwarfs are Well-reproduced by Phosphine-free, Diabatic, ATMO2020++ Models
Authors: S. K. Leggett, Pascal Tremblin
Figure caption: JWST NIRSPEC and MIRI spectra are indigo and pink lines, respectively. The data are the MAST 1D extractions for program GO 2302. Cyan lines in the inset are HST spectra from Schneider et al. (2015). Yellow lines are the best fit phosphine-free solar-metallicity ATMO 2020++ synthetic spectra generated here. The green line is an earlier metal-poor model with PH3 (Meisner et al. 2023).
Paper: NE2001p: A Native Python Implementation of the NE2001 Galactic Electron Density Model
Authors: Stella Koch Ocker, James M. Cordes
Figure caption: Left: maximum DM vs. Galactic longitude in the Galactic plane (solid) and 5° above the plane (dashed) for the Fortran NE2001 (blue) and NE2001p (orange). Right: the cumulative distribution function (CDF) of fractional residuals (∣NE2001 − NE2001p∣/NE2001) for DM calculated from distance D (blue), SM from D (orange), and D from DM (green); see Section 2.
Paper: Anthropogenic Coal Ash as a Contaminant in an Underwater Search. II. Beyond Beryllium, Lanthanum, and Uranium
Authors: Patricio A. Gallardo
Figure caption: From top to bottom: (a) “BeLaU” average concentration, SRM 1633a and COALQUAL percentiles. (b) The “BeLaU pattern” of coal ash SRM 1633a using a chondritic normalization (black line and solid dots), gray lines show abundances of the 12 “BeLaU” spherules (data from L24v3). (c) Rare earth element abundances and their mean values. Note that in 9 cases of 16, the errorbar crosses unity as expected from random sampling (binomial p = 0.68, N = 16, PTE = 0.77). (d) The average abundance of the “BeLaU” samples normalized by the SRM 1633a. An arbitrary region of 10× has been drawn, note that no elements are richer than coal ash or 10×, deviations are deficits, only two elements are beyond 3σ the 1/10× line. This comparison does not account for water solubility of trace elements or statistical deviations in the reference sample.
Paper: Polarimetry of GRB 230818A
Authors: Denis Bernardes, Iain Steele, Helen Jermak, Callum McCall
Figure caption: From top to bottom, the first panel presents the magnitude in the R band as a function of time obtained for the target (blue dots). The blue line represents a broken power law adjusted for the target. The black dashed vertical line represents the time obtained for the transition between these regimes. The second panel presents the residuals resulting from the subtraction between the data and the linear adjustment. The third and fourth panels present the polarization percentage and polarization angle, respectively, as a function of time, for the target (red dots) and for some candidates (blue dots) found nearby.
Paper: Photometric Analysis of the Nucleus of the Main-belt Comet 2010 LH15
Authors: M. Mastropietro, H. Krishna, Y. Kim, J. Agarwal
Figure caption: Lightcurve profiles of 2010 LH15. Photometry not feasible between 08:25 and 08:41 on July 8 due to the presence of bright stars.
Paper: The Host Galaxy of a Dormant, Overmassive Black Hole at z = 6.7 may be Restarting Star Formation
Authors: Fabio Pacucci, Abraham Loeb, Ignas Juodžbalis
Figure caption: The condition for SMBH-driven star formation quenching developed in Pacucci & Loeb (2024) is applied to the galaxy JADES GN 1146115 (Juodžbalis et al. 2024), shown in the [M ⋆, M •/M ⋆] plane with its 1σ uncertainties. The dotted lines indicate how the range of  f Edd estimated for JADES GN 1146115 affects the threshold on M •/M ⋆. Galaxies hosting overmassive black holes in the green area experience reduced star formation as quasar feedback increases the gas temperature above the virial one. Local galaxies on the M •–M ⋆ relation (shown as a dashed line) are indicated with gray symbols (Reines & Volonteri 2015). The red arrow indicates the effect of an increasing host’s stellar mass in changing the location of the galaxy in the plane; the black arrow indicates the effect of a decreasing  f Edd in raising the threshold value of M •/M ⋆. Both changes would lead JADES GN 1146115 to a region where star formation is more efficient.