adsabs/AstroCLIMB huggingface dataset:
Paper: Spectroscopic Confirmation of the Nearby, Wide-separation L Dwarf Pair CWISE J061741.79+194512.8AB
Authors: Austin Humphreys, Aaron M. Meisner, Adam J. Burgasser, Chih-Chun Hsu, Adam C. Schneider, Christopher A. Theissen, Christian Aganze, Roman Gerasimov, Noah Schapera, J. Davy Kirkpatrick, Federico Marocco, Jacqueline K. Faherty, Dan Caselden, Marc J. Kuchner, Michael C. Cushing
Figure caption: Reduced Keck/NIRES spectra of J0617+1945A (top) and J0617+1945B (middle) with uncertainties in gray. Green curves show the corresponding smoothed NIRES standards (Theissen et al. 2022); blue curves show the corresponding low-resolution SPLAT standards (Burgasser 2007; Gagliuffi et al. 2014). Yellow shading indicates the region used for computing χ 2. The bottom panel illustrates one of our best-fit NIRSPEC models. The NIRSPEC spectrum is shown in black and the best-fit forward models with/without telluric absorption are shown in blue and green, respectively, and residual (data-model) in magenta.
Paper: ALMA Band-7 Flux Density Prediction of the Haumea Ring System for Ongoing Observations
Authors: Csilla E. Kalup, Csaba Kiss
Figure caption: ALMA band-7 flux density predictions of the simple ring model assuming normal optical depth of τ = 0.097, ring radius of r = 2287 km and width of w = 70 km. The red curve represents I/F = 0.09 and q = 0.26, while purple and blue lines correspond to I/F = 0.5, q = 0.6 and I/F = 0.05, q = 0.26, respectively. The minimum around 2003 is due to an edge-on observing geometry.
Paper: Exploring the Chemical Evolution of Nitrogen and Oxygen in Local Star-forming Galaxies
Authors: Mabel G. Stephenson, Karla Z. Arellano-Córdova, Danielle A. Berg, Matilde Mingozzi, Bethan L. James
Figure caption: The N/O vs. O/H relation for the CLASSY sample, shown as blue stars. For comparison, other galaxy samples are included; dwarf SFGs from Berg et al. (2012) and Berg et al. (2019), as well as extragalactic H II regions sampled of M101 from the CHemical Abundances Of Spirals (CHAOS, Croxall et al. 2016). Additionally, the N/O empirical fit reported in Nicholls et al. (2017) is shown in gray.
Paper: Deep DECam Y-band Follow-up of WISEA J153429.75–104303.3 (a.k.a. “The Accident”)
Authors: Aaron M. Meisner, Dan Caselden, Edward F. Schlafly, Ioana A. Zelko, J. Davy Kirkpatrick, Federico Marocco
Figure caption: 600 s DECam Y-band coadd, with a red square highlighting the predicted position of WISEA 1534−1043 at the relevant observing epoch, based on the motion solution of Kirkpatrick et al. (2021). The low-significance flux “blip” discussed in Section 3 is labeled with a blue circle. The field of view is approximately 1.′1 × 0.′5. East is left and north is up. Note that the color scale is inverted so that the blank sky looks relatively light in color, while compact sources appear black.
Paper: A Direct Connection between the Wake and the Former Host Galaxy of a Proposed Runaway Supermassive Black Hole
Authors: Pieter van Dokkum
Figure caption: Top: summed ACS F606W+F814W image of the linear feature and the compact galaxy GX, both at z = 0.964. The brightest emission is in orange. In van Dokkum et al. (2023) the linear feature is interpreted as young stars behind a runaway supermassive black hole that originated in GX. There is a gap between the feature and GX, and Sanchez Almeida et al. (2023) explore the alternative interpretation that they are two independent galaxies. Bottom: VLT B band image, sampling λ rest ∼ 0.22 μm. In the rest-frame far-UV there is no gap and the feature extends all the way to GX. This is consistent with what was seen in the observed u band and the [O III] line in vD23, and difficult to reconcile with the Sanchez Almeida et al. (2023) hypothesis. In the runaway black hole model the emission in the gap is shocked gas.
Paper: Comparative Study of Low-temperature Opacities with GARSTEC Models
Authors: Pedro Díaz Reeve, Aldo Serenelli
Figure caption: Left: comparison of the Rosseland mean opacity for ÆSOPUS and F05 for X = 0.70, Z = 0.004, 0.02 and 0.04. Gray vertical line shows the solar effective temperature ﹩\mathrm{log}T\simeq ﹩ 3.76, and gray shaded profile shows the range of variation for all ﹩\mathrm{log}R﹩ values. Right: Evolutionary tracks for stellar models computed with GARSTEC with Z = 0.01998, and for M/M ⊙ = 0.70 (red track), 1.00 (blue track) and 1.50 (black track).
Paper: Revisiting the Gas-phase Chemical Rate Coefficients at High Temperatures in CLOUDY
Authors: Gargi Shaw, Gary Ferland, M. Chatzikos
Figure caption: The upper panel shows the percentage of reaction rates applicable for the different upper limits of temperatures (provided by UDfA) for all the UDfA rate coefficients. Whereas, the lower panel shows the same for β > 0.
Paper: AGN’s Deadness Over Cosmic Time: UVJ Diagrams of X-Ray AGN
Authors: Rachel Cionitti, Brandon Coleman, Allison Kirkpatrick, Greg Troiani
Figure caption: The UVJ diagrams for all objects in the sample. The quiescent region falls in the upper left and is indicated by the solid black line. The greyscale is a 2D histogram representing the density of sources at each region. The colored points represent the locations of the most luminous X-ray sources (﹩\mathrm{log}\,{L}_{X}\gt 44.5﹩). The color bar demonstrates intensity in the hard X-ray band. We list the number of sources and the percentage of quiescent galaxies. We also list the percentage of galaxies in each region that are X-ray luminous.
Paper: Assessing the Accuracy of TESS Asteroseismology with APOGEE
Authors: Artemis Theano Theodoridis, Jamie Tayar
Figure caption: Top four: Offset between the spectroscopic and asteroseismic surface gravities (Seismic—Spectroscopic) compared to spectroscopic log(g), [α/M], mass, and [M/H]. The darkness is representative of the concentration of stars in a given area; slight trends can be seen with mass and metallicity and in the red clump (top right). Bottom left: Offset between the spectroscopic and asteroseismic results. A mean of 0.001 and uncertainty of 3.5% indicate excellent agreement between the measurements. Bottom right: Histogram comparing the measured offsets before the seismic and spectroscopic results scaled by the claimed uncertainties for each measurement. The distribution is much wider than the standard-normal distribution, suggesting that the claimed uncertainties are underestimated by a factor of 2.
Paper: Comment on the Feasibility of Carbon Burning in Betelgeuse
Authors: László Molnár, Meridith Joyce, Shing-Chi Leung
Figure caption: Visual (gray) and photometric (blue: V-band; red: SMEI) light curves of Betelgeuse. Updated from Figure 1 in Joyce et al. (2020).
Paper: Real-time Technosignature Strategies with SN 2023ixf
Authors: James R. A. Davenport, Sofia Z. Sheikh, Wael Farah, Andy Nilipour, Bárbara Cabrales, Steve Croft, Alexander W. Pollak, Andrew P. V. Siemion
Figure caption: Left: Color–magnitude diagram for 108 stars within 0.1 ly of the SETI Ellipsoid defined by SN 2023ixf as of MJD 60094 (black points), with the 100 pc Gaia sample for reference (blue contours). These Ellipsoid-crossing targets already span a range of stellar types. Right: Sky positions for the Ellipsoid-crossing stars (black points), which lay in a ∼3° region around SN 2023ixf (orange cross).
Paper: The Secondary Maximum of T CrB Caused by Irradiation of the Red Giant by a Cooling White Dwarf
Authors: Ulisse Munari
Figure caption: The secondary maximum of T CrB is accurately reproduced (orange line) by irradiating the red giant with the white dwarf companion cooling according to the temperature profile plotted in the top panel. The dashed line shows for reference the ellipsoidal modulation computed for the Roche-lobe filling red giant. The inset present the evolution of (B − V) color. Days are counted from primary maximum on JD 2431860.854 (=1946 February 9.354 UT), and phase ψ is reckoned from RG passage at superior conjunction (ψ = 0.0 on day +187 and JD 2432048). At the bottom, examples of the computed radiative models (the crosses highlight the position of the WD).
Paper: Solar Cycle 25 Will Be a Weak-moderate Cycle: an Update
Authors: V. M. S. Carrasco, J. M. Vaquero
Figure caption: (Top panel) Evolution of solar cycles from 1 to 25 according to its smoothed monthly sunspot number provided by SILSO (https://www.sidc.be/silso). (Lower panel) Comparison between the updated prediction made by the SC25PP (blue) and the smoothed monthly sunspot number values available by SILSO (red). Blue shadow is the smoothed monthly sunspot number range predicted by the SC25PP.
Paper: New Active Quasi-Hilda Asteroid 2004 CV50: A Citizen Science Discovery
Authors: Colin Orion Chandler, William J. Oldroyd, Chadwick A. Trujillo, William A. Burris, Henry H. Hsieh, Jay K. Kueny, Kennedy A. Farrell, Jarod A. DeSpain, Nima Sedaghat, Mark Jesus Mendoza Magbanua, Scott S. Sheppard, Michele T. Mazzucato, Milton K. D. Bosch, Tiffany Shaw-Diaz, Virgilio Gonano, Al Lamperti, Charles J. A. Dukes, Ivan A. Terentev, José A. da Silva Campos, Brian L. Goodwin
Figure caption: 2004 CV50 (at center) with a short, diffuse tail in these 120 s i-band DECam exposures (Prop. ID 2020A-0399, PI Zenteno, observer A. Diaz). Anti-motion (yellow arrow) and anti-solar (red-bordered black arrow) directions are indicated. The FOV is 32″ × 32″, with north up and east left. (a) UT 2020 February 15 at 08:47:22. (b) UT 2020 March 14 at 06:40:53. (c) UT 2020 March 14 at 06:44:38.
Paper: Photometry of Type II Supernova SN 2023ixf with a Worldwide Citizen Science Network
Authors: Lauren A. Sgro, Thomas M. Esposito, Guillaume Blaclard, Sebastian Gomez, Franck Marchis, Alexei V. Filippenko, Daniel O'Conner Peluso, Stephen S. Lawrence, Aad Verveen, Andreas Wagner, Anouchka Nardi, Barbara Wiart, Benjamin Mirwald, Bill Christensen, Bob Eramia, Bruce Parker, Bruno Guillet, Byungki Kim, Chelsey A. Logan, Christopher C. M. Kyba, Christopher Toulmin, Claudio G. Vantaggiato, Dana Adhis, Dave Gary, Dave Goodey, David Dickinson, David Koster, Davy Martin, Eliud Bonilla, Enner Chung, Eric Miny, Fabrice Mortecrette, Fadi Saibi, Francois O. Gagnon, Franois Simard, Gary Vacon, Georges Simard, Gerrit Dreise, Hiromi Funakoshi, Janet Vacon, James Yaniz, Jean-Charles Le Tarnec, Jean-Marie Laugier, Jennifer L. W. Siders, Jim Sweitzer, Jiri Dvoracek, John Archer, John Deitz, John K. Bradley, Keiichi Fukui, Kendra Sibbernsen, Kevin Borrot, Kevin Cross, Kevin Heider, Koichi Yamaguchi, Lea A. Hirsch, Liouba Leroux, Mario Billiani, Markus Lorber, Martin J. Smallen, Masao Shimizu, Masayoshi Nishimura, Matthew Ryno, Michael Cunningham, Michael Gagnon, Michael Primm, Michael Rushton, Michael Sibbernsen, Mike Mitchell, Neil Yoblonsky, Niniane Leroux, Olivier Clerget, Ozren Stojanović, Patrice Unique, Patrick Huth, Raymund John Ang, Regis Santoni, Robert Foster, Roberto Poggiali, Ruyi Xu, Ryuichi Kukita, Sanja Šćepanović, Sophie Saibi, Stefan Will, Stephan Latour, Stephen Haythornthwaite, Sylvain Cadieux, Thoralf Müller, Tze Yang Chung, Yoshiya Watanabe, Yvan Arnaud
Figure caption: Light curve of SN 2023ixf. Circles represent detections and triangles represent 3σ lower magnitude limits. Inset highlights the first 1.5 days after earliest detection.(The data used to create this figure are available.)
Paper: An Observational Upper Limit on the Rate of Gamma-Ray Bursts with Neutron Star–Black Hole Merger Progenitors
Authors: Sylvia Biscoveanu, Eric Burns, Philippe Landry, Salvatore Vitale
Figure caption: Posterior probability distributions on the local rate of GRBs with NSBH progenitors under the Gaussian (left) and power-law (right) mass ratio models. The colors indicate three different values of the minimum remnant mass that we require for a NSBH merger to potentially power a GRB. The dashed vertical lines indicate the 90th percentile for each value of the minimum remnant mass.
Paper: Non-LTE Abundances of Helium, Magnesium, and Silicon in the Atmosphere of the Bp He-weak Star HD 175156
Authors: Richard Monier
Figure caption: Left: NLTE synthesis of the He I at 4470 Å and the Mg II triplet at 4481.0 Å (observed spectrum in black, solar abundances in green, enhanced by a factor of 2 in red). Right: Synthesis of the Si III multiplet from 4550 to 4580 Å.
Paper: Selecting z ∼ 8 Galaxies with JWST Photometry in CEERS
Authors: Kaile Wang, Micaela B. Bagley, Steven L. Finkelstein
Figure caption: (Left) F150W magnitude vs. redshift for the 117 galaxies that are selected as z ∼ 8. (Right) 1.″5 × 1.″5 image stamps around an example z ∼ 8 galaxy in seven NIRCam bands and in two HST filters, F606W and F814W. The detection significance of the source was measured in the red circular aperture with 0.″3 diameter. The green elliptical aperture shows the region where fluxes were measured. The apertures are centered on the target, and the source disappears in the two dropout filters (i.e., F606W and F814W). The large image shows a 5″ × 5″ cutout of the F200W image around the source; the green square box in the large image is 1.″5 × 1.″5 in size. The P(z) distribution as a function of the redshift of the galaxy is also present. The data behind the first panel is available. This machine readable version also contains coordinates for each source.(The data used to create this figure are available.)
Paper: Modeling the Free Inclinations of the Classical Kuiper Belt with the von Mises–Fisher Distribution
Authors: Renu Malhotra, Supriya Roy
Figure caption: Free inclinations of non-resonant CKBOs and the best-fit two-component vMF model.
Paper: Pulsational Velocity Variations of the Radial Mode sdBV Star BPM 36430
Authors: Bennett C. Kirby, Bryce A. Smith, Brad N. Barlow
Figure caption: A 0.05 day section of the radial velocity curve (top panel) of the sdBVrs star BPM 36430, with the best–fitting sinusoid shown in red. The discrete Fourier transform (bottom panel) of the velocity curve, which we calculated using Period04 (Lenz & Breger 2014), shows a strong signal with amplitude just above 4 km s−1 and period consistent with the known radial mode pulsation.
Paper: The Late-Epoch, Matter-Bounded Spectrum of the Nova V1405 Cassiopeiae
Authors: Richard J. Rudy, John P. Subasavage, Jon C. Mauerhan
Figure caption: Optical and infrared spectrum of V1405 Cas from more than two years after discovery. The He II lines are particularly pronounced and marked in all three panels. Notable in the optical portion of the spectrum (top panel) are the exceptional strength of [Fe VII] 0.6087 and the absence of nebular lines such as [N II] and [O III]. Also absent are the optical He I lines. The only He I line with a clear detection is 1.0830, seen in the central panel. It is frequently the strongest infrared feature in novae, as it was previously in V1405 Cas (Woodward et al. 2022), but at this epoch is only a fraction of He II 1.0127. Also present in the middle panel are the infrequently seen near-infrared [Fe VI] lines. The unidentified feature at 1.1900 μmis seen in many novae that reach high excitation and probably includes a contribution from C IV. A similar unidentified lines is seen at 2.0996 μmin the bottom panel. That panel’s spectral range includes the two strongest coronal features: [S VI] 1.9645 and [Ca VIII] 2.3210.(The data used to create this figure are available.)
Paper: Discovery of Extensive [O III] Emission Near M31
Authors: Marcel Drechsler, Xavier Strottner, Yann Sainty, Robert A. Fesen, Stefan Kimeswenger, J. Michael Shull, Bray Falls, Christophe Vergnes, Nicolas Martino, Sean Walker
Figure caption: Top: Combined 48.6 hr [O III] 5007 Å exposure image showing the discovery of broad emission nebula southeast of M31. Bottom: Confirming 85.5 hr combined [O III] image. Note: Images are shown as obtained and unrotated. The bright object above the [O III] filaments is the 4.5 mag B5 V star ν And (HD 4727).
Paper: JWST-MIRI Synthetic Photometry Composition using 460 Spitzer-IRS Spectra of Nearby Galaxies
Authors: Cory M. Whitcomb, Karin Sandstrom, John-David T. Smith
Figure caption: Fractional contributions to MIRI photometric bands. Dust continuum (blue), PAHs (red), emission lines (black), and starlight (green). SINGS (left five panels) and BIGMAP (right five panels). The median and standard deviation of each distribution is indicated by the vertical and horizontal lines.
Paper: Repeating Outbursts from the Young Stellar Object Gaia23bab (=SPICY 97589)
Authors: Michael A. Kuhn, Robert A. Benjamin, Emille E. O. Ishida, Rafael S. de Souza, Julien Peloton, Michele Delli Veneri
Figure caption: (a) Gaia G-band light curve for Gaia23bab (=SPICY 97589). (b) ZTF g and r-band light curves. (c) Photometric measurements of the source during quiescence (circles). Filled circles were used for SED fitting, while open circles exhibit excess emission and were excluded from fitting. The orange curve is a representative reddened stellar photosphere model. (d) Spitzer/IRAC 3.6 (blue), 4.5 (green), and 8.0 (red) μm image of the cloud DOBASHI 1604 and cluster G38.3-0.9. YSOs from SPICY are circled in green. (e)–(f) Parallaxes and proper motions of YSOs in G38.3-0.9 (black circles), with SPICY 97589 indicated by the magenta star. The orange bars indicate the cluster’s estimated parallax and mean proper motions. In all panels (a)–(f), error bars are excluded if they are smaller than the point sizes.
Paper: 20 s Cadence TESS Photometry of HR 8799
Authors: Aldo G. Sepulveda, Daniel Huber, Gang Li, Timothy R. Bedding, Zhoujian Zhang, Michael C. Liu
Figure caption: (a): 20 s cadence TESS Sector 56 time series photometry of HR 8799 together with the residual photometry resulting from our frequency removal. (b): Amplitude spectrum of the 20 s data in log–log space. (c): Same as (b) but in linear–linear space, and zoomed in on the primary region of pulsations. (d): Kepler γ Dor stars from Li et al. (2020) that we used to infer the core rotation period of HR 8799. The median and 16th/84th percentiles are denoted in the inset histogram. See Sepulveda et al. (2022) for more details on the construction and interpretation of this subplot.
Paper: On the Discovery Claim of a New z > 7 Quasar
Authors: Sarah E. I. Bosman, Frederick B. Davies, Eduardo Bañados
Figure caption: Top: Motion of the contaminating asteroid in UKIDSS. The observing epoch is indicated above each panel; the central circle is 8″ across. The H and K band images are spatially offset from the J and Y bands by about 1′20″ (W1 circle is 20″ across). Bottom: photometry of the candidate object at times uncontaminated by the asteroid. The object is undetected in the UKIDSS J band; a detection in DELS z band conclusively rules out a redshift z > 7.3.
Paper: Photometric Observations of Nine High Mass X-Ray Binaries and Analysis of Potential Periodicities and Variations
Authors: David H. Hinzel
Figure caption: Composite Light Curve and Analysis of Potential Periodicities and Variations for HMXB 1H 1936+541.
Paper: New Jupiter and Saturn Satellites Reveal New Moon Dynamical Families
Authors: Scott S. Sheppard, David J. Tholen, Mike Alexandersen, Chadwick A. Trujillo
Figure caption: Outer moons where symbol size represents the Log of the moon size.
Paper: Scarlet Spectra: Two Red L Dwarfs Revealed by SOAR
Authors: Grady Robbins, Aaron M. Meisner, Adam C. Schneider, J. Davy Kirkpatrick, Dan Caselden, Adam J. Burgasser, Jacqueline K. Faherty, Marc J. Kuchner, Federico Marocco, Jonathan Gagné, Sarah Casewell
Figure caption: Top panel: The full resolution near-infrared spectrum of W0755−3259 (gray) and smoothed (black) compared to the L5 near-infrared spectral standard SDSS J083506.16+195304.4 (Chiu et al. 2006; Kirkpatrick et al. 2010) and L7 VL-G dwarf WISEA J114724.10-204021.3 (Schneider et al. 2016). Bottom panel: The full resolution near-infrared spectrum of W1659−3511 (gray) and smoothed (black) compared to the L7 near-infrared spectral standard 2MASSI J0825196+211552 (Kirkpatrick et al. 2000; Cruz et al. 2017) and L7 INT-G dwarf WISEP J004701.06+680352.1 (Gizis et al. 2012). All spectra are normalized between 1.27 and 1.29 μm.(The data used to create this figure are available.)
Paper: Gaia Astrometry and MIKE+PFS Doppler Data Joint Analysis Reveals that HD 175167b is a Massive Cold Jupiter
Authors: Tianjun Gan
Figure caption: Top panels: Time-series (left) and phase-folded (right) RV data from MIKE and PFS along with the best-fit model. Middle right panel: The orbit of the HD 175167b constructed based on the best-fit physical parameters using Rebound (Rein & Liu 2012). The parent star is located at the origin. Bottom panel: The posterior distributions of the joint-fit analysis. We follow the Gaia convention where t  p  is the Julian date of pericenter minus 2,457,389.
Paper: Constraints to Efficiently Find Interstellar Object Generated Craters on the Moon
Authors: Daniel Chang, Cheng-Han Hsieh, 承翰 謝, Gregory Laughlin
Figure caption: (a) shows the difference between the cumulative distribution functions of craters generated from solar system objects and ISOs. Most craters generated from solar system objects were formed in the first billion years, so that the ratio of the CDFs for craters with ages less than 3 Gyr is ∼20. (b) shows the cumulative probabilities of impact angles at various latitudes on the Moon for Near Earth Objects, calculated from the probability found in (Robertson et al. 2021). For latitudes 0° through 70°, there is a <10% probability that the crater is generated from vertical impact, while the probability is much higher at around 40% for latitudes 70°–90°.
Paper: Identifying SuperWASP Detected Candidate Variables with TESS 
Authors: Ai-Ying Zhou
Figure caption: Examples of the folded SuperWASP light curves (Left) compared with TESS light curves (Right). Top row: a known γ Dor star; 2nd row: a new γ Dor star; 3rd row: a new δ Sct star; 4th and 5th rows: two new RR Lyr stars; 6th row: a new RR Lyr in an eclipsing binary system; 7th row: a new rotating (ellipsoidal variable) star in an eclipsing binary system; 8th and 9th rows: two new rotating variables.
Paper: The Importance of Neural Network Hyperparameters in Determining Age Inference Quality
Authors: Jamie Tayar, Zachary R. Claytor, Quentin Fox, Liberty Mallison, Ezra Rader, Ryan Spivey, Denise Yudovich, Jack Moreland, Rachel Pinsky, Penelope Planet, Artemis Theodoridis, Jacod Williams, Caeli Benyacko, Sydney Phelps Comstock, Nadia Hansen, Marcus Mynatt, Ben C. Sherwin, Daniel Agharahimi, Amro Al-Wir, Jacob Boesger, JR Davis, Austin Fraley, Aaditya Kaushal, Trent La Sage, Anna Grace Lube, Rachel Prempeh, Sierra Sanne, Pae Swanson, Meridith Joyce
Figure caption: We show examples of the age predictions of an underfit (top left), well fit (top center), and overfit network (top right), and the two relatively similar subsets used for testing (bottom left). We find that the quality of the predictions does not depend significantly on the number of neurons per layer (middle left), the number of layers (middle center) or the number of iterations (middle right), although it does seem to be quite sensitive to the training set (bottom middle and right).
Paper: Mars-Crossing Minor Planet 2018 VL10: a Jupiter-family Comet Discovery via Citizen Science
Authors: Colin Orion Chandler, William J. Oldroyd, Chadwick A. Trujillo, Henry H. Hsieh, William A. Burris, Jay K. Kueny, Jarod A. DeSpain, Nima Sedaghat, 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: 2018 VL10 (at center) in these 32″ ×  32″ DECam 150 s VR-band exposures (Prop. ID 2018B-0122, PI Rest), with north up and east left. The anti-motion (red outlined black arrow) and anti-solar (yellow arrow) directions are indicated. (a) and (b): On UT 2018 December 31 (observer A. Zenteno) a diffuse tail spans between 12 and 2 o’clock. (c) and (d): On UT 2019 February 1 (observers A. Rest, A. Zenteno) diffuse comae and/or tail(s) are seen emanating roughly toward the anti-motion and anti-solar directions.