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Paper: A Gap-sharing Planet Pair Shaping the Crescent in HD 163296: A Disk Sculpted by a Resonant Chain
Authors: Juan Garrido-Deutelmoser, Cristobal Petrovich, Carolina Charalambous, Viviana V. Guzmán, Ke Zhang
Figure caption: Band 6 (λ ∼ 1.25 mm) comparison between dust continuum image from ALMA observation (Isella et al. 2018) and our synthetic observation after ≈4.8 × 105 yr. The synthesized beam are the same for both images (0.″038 × 0.″048, 82.°5), represented by white ellipse at the bottom left corner for each image. The synthetic image is projected with an inclination i = 46° and a position angle PA = 133°. The enumerated white dots indicate the position of potential planets associated with the following: (1) and (4) resonance angles in Laplace chains (see Section 5.1), (2) Lagrange point L 5 from the simulation, (3) velocity kink reported by Pinte et al. (2020). The white dashed lines denote the orbits of planets in the simulation. The right bottom Cartesian coordinate describes the prescription to estimate the azimuthal angles. The disk rotates in a clockwise direction.
Paper: A Gap-sharing Planet Pair Shaping the Crescent in HD 163296: A Disk Sculpted by a Resonant Chain
Authors: Juan Garrido-Deutelmoser, Cristobal Petrovich, Carolina Charalambous, Viviana V. Guzmán, Ke Zhang
Figure caption: Potential migratory history of the four-planet system locking the planets in a long orbital resonance chain leaving the outer three planets near a consecutive 2:1 commensurability and the innermost pair near 4:3 (panels (a) and (b)). The eccentricities remain small after the capture (panel (c)) and the three-body resonant angles ϕ 123 = 3λ 1 − 5λ 2 + 2λ 3 and ϕ 234 = 2λ 2 − 6λ 3 + 4λ 4 undergo small-amplitude libration (panel (d)). The bottom panel exhibits the corresponding combinations of the position angles in the system: PA123 = 3PA1 − 5PA2 + 2PA3 and PA234 = 2PA2 − 6PA3 + 4PA4.
Paper: A Gap-sharing Planet Pair Shaping the Crescent in HD 163296: A Disk Sculpted by a Resonant Chain
Authors: Juan Garrido-Deutelmoser, Cristobal Petrovich, Carolina Charalambous, Viviana V. Guzmán, Ke Zhang
Figure caption: Panels show a time evolution after 2000 orbits at 48 au (∼4.8 × 105 yr). (a) Surface density Σ maps in log-scale for a single Jupiter planet at 48 au. (b) The same as (a), but for a two-planet system with 85M ⊕ and 60M ⊕ instead the Jupiter. The crosses denote the position of the planets and the white lines indicate their orbits. The disk rotates in a clockwise direction. (c) Azimuthally averaged Σ/Σ0 profiles for both models.
Paper: A Gap-sharing Planet Pair Shaping the Crescent in HD 163296: A Disk Sculpted by a Resonant Chain
Authors: Juan Garrido-Deutelmoser, Cristobal Petrovich, Carolina Charalambous, Viviana V. Guzmán, Ke Zhang
Figure caption: Face-on gas and dust surface density Σ from the hydrodynamic model after ≈4.8 × 105 yr (2000 orbits at 48 au). The panels correspond to different fluids. The crosses denote the position of the planets and the white dashed lines indicate their orbits. The disk rotates in a clockwise direction.
Paper: A Gap-sharing Planet Pair Shaping the Crescent in HD 163296: A Disk Sculpted by a Resonant Chain
Authors: Juan Garrido-Deutelmoser, Cristobal Petrovich, Carolina Charalambous, Viviana V. Guzmán, Ke Zhang
Figure caption: Comparison of column density gap in C18O (2–1) line observation found by Zhang et al. (2021) with gas gaps derived from surface density profiles in this work.
Paper: A Gap-sharing Planet Pair Shaping the Crescent in HD 163296: A Disk Sculpted by a Resonant Chain
Authors: Juan Garrido-Deutelmoser, Cristobal Petrovich, Carolina Charalambous, Viviana V. Guzmán, Ke Zhang
Figure caption: Azimuthally averaged intensity profiles for synthetic and ALMA observations after ≈4.8 × 105 yr. The crosses denote the semimajor axes of the planets. The insert shows the ALMA observation in Band 6 with contours that reproduce the crescent and rings as well as the angular slice used for the azimuthal average denoted by ﹩\hat{\phi }﹩.
Paper: A Gap-sharing Planet Pair Shaping the Crescent in HD 163296: A Disk Sculpted by a Resonant Chain
Authors: Juan Garrido-Deutelmoser, Cristobal Petrovich, Carolina Charalambous, Viviana V. Guzmán, Ke Zhang
Figure caption: Black line denotes the convolved surface density profile of models and gray dashed line the respective smooth function. Panels (a) and (b) represent the single-planet case and two-planet case respectively. The crosses indicate the position of the planets.
Paper: A Gap-sharing Planet Pair Shaping the Crescent in HD 163296: A Disk Sculpted by a Resonant Chain
Authors: Juan Garrido-Deutelmoser, Cristobal Petrovich, Carolina Charalambous, Viviana V. Guzmán, Ke Zhang
Figure caption: Dust surface density Σ for 0.02 and 1.9 cm grain sizes. The crosses denote the position of the planets. The upper and bottom white rectangles indicate the Lagrange points L 4 and L 5 with respect to the outer planet.
Paper: Elucidating the Formation of Ethynylbutatrienylidene (HCCCHCCC; X1A′) in the Taurus Molecular Cloud (TMC-1) via the Gas-phase Reaction of Tricarbon (C3) with the Propargyl Radical (C3H3)
Authors: Alexander M. Mebel, Marcelino Agúndez, José Cernicharo, Ralf I. Kaiser
Figure caption: Upper panel: calculated fractional abundances of ethynylbutatrienylidene (HCCCHCCC) along with the tricarbon (C3) and propargyl radical reactants (C3H3). Observed values, indicated by horizontal dotted lines, were taken from Agúndez et al. (2022) for propargyl (C3H3) and Fuentetaja et al. (2022) for ethynylbutatrienylidene (HCCCHCCC). Lower panel: contributions of the reactions of l-HCCC+HCCCH and C3+C3H3 leading to ethynylbutatrienylidene (HCCCHCCC).
Paper: Elucidating the Formation of Ethynylbutatrienylidene (HCCCHCCC; X1A′) in the Taurus Molecular Cloud (TMC-1) via the Gas-phase Reaction of Tricarbon (C3) with the Propargyl Radical (C3H3)
Authors: Alexander M. Mebel, Marcelino Agúndez, José Cernicharo, Ralf I. Kaiser
Figure caption: Combined potential energy diagram for the l-CCCH + C3H2 and C3 + C3H3 reactions accessing the C6H3 PES. Relative energies are shown in kJ mol−1 with respect to C3 + C3H3. The red and blue lines respectively show the major and minor pathways leading to the formation of ethynylbutatrienylidene (HCCCHCCC, p3) plus atomic hydrogen.
Paper: Elucidating the Formation of Ethynylbutatrienylidene (HCCCHCCC; X1A′) in the Taurus Molecular Cloud (TMC-1) via the Gas-phase Reaction of Tricarbon (C3) with the Propargyl Radical (C3H3)
Authors: Alexander M. Mebel, Marcelino Agúndez, José Cernicharo, Ralf I. Kaiser
Figure caption: Minimal potential energy profiles for the initial recombination reaction steps C3 + C3H3 → i8 (a) and C3 + C3H3 → i7 (b) calculated at the ωB97XD/cc-pVTZ level of theory.
Paper: Optical Spectropolarimetry of Binary Asteroid Didymos–Dimorphos before and after the DART Impact
Authors: Stefano Bagnulo, Zuri Gray, Mikael Granvik, Alberto Cellino, Ludmilla Kolokolova, Karri Muinonen, Olga Muñoz, Cyrielle Opitom, Antti Penttilä, Colin Snodgrass
Figure caption: Spectropolarimetry obtained at the phase angles shown on the right-hand side of the plots. The bottom panels refer to data obtained prior to impact, and the top panels refer to data after the impact. The left panels show the polarization spectra P r(λ). The middle panels show the same spectra normalized to the values in the V filter. For display purposes, they are vertically offset by a quantity equal to the normalization factor. The right panels show the difference between each normalized polarization spectrum and the one obtained the night before the impact, September 26 at 07:26 UT), multiplied by 10. Again, for display purposes, these data have been offset by the normalization quantity P r(V). For clarity, among the group of postimpact spectra (top panels), error bars are shown only for one representative case. In the middle and right panels, we have omitted the polarization spectrum obtained on 2022 August 23 because, being taken close to the inversion angle, it would represent a noisy ratio between two small quantities.
Paper: Optical Spectropolarimetry of Binary Asteroid Didymos–Dimorphos before and after the DART Impact
Authors: Stefano Bagnulo, Zuri Gray, Mikael Granvik, Alberto Cellino, Ludmilla Kolokolova, Karri Muinonen, Olga Muñoz, Cyrielle Opitom, Antti Penttilä, Colin Snodgrass
Figure caption: Left panel: normalized polarization spectra of Didymos obtained just before impact on 2022 September 26 compared to that of other asteroids. The right panel shows the corresponding reflectance spectra. The three symbols after the asteroid name refer to the classification according to Tholen (1984), Bus & Binzel (2002a), and DeMeo et al. (2009), respectively.
Paper: Optical Spectropolarimetry of Binary Asteroid Didymos–Dimorphos before and after the DART Impact
Authors: Stefano Bagnulo, Zuri Gray, Mikael Granvik, Alberto Cellino, Ludmilla Kolokolova, Karri Muinonen, Olga Muñoz, Cyrielle Opitom, Antti Penttilä, Colin Snodgrass
Figure caption: Polarization spectra obtained with FORS2 at the phase angles before (red solid line) and after (blue solid line) impact, with scale on the left axis. Dotted lines show the approximate relative reflectance spectra (normalized to 1 at 550 nm), with scale on the right axis.
Paper: Optical Spectropolarimetry of Binary Asteroid Didymos–Dimorphos before and after the DART Impact
Authors: Stefano Bagnulo, Zuri Gray, Mikael Granvik, Alberto Cellino, Ludmilla Kolokolova, Karri Muinonen, Olga Muñoz, Cyrielle Opitom, Antti Penttilä, Colin Snodgrass
Figure caption: The N  Q  values calculated in the BVRI filters, offset by 0%, +0.5%, +1.0%, and +1.5%, respectively. Error bars are set to 0.05%.
Paper: Resurrection of Type IIL Supernova 2018ivc: Implications for a Binary Evolution Sequence Connecting Hydrogen-rich and Hydrogen-poor Progenitors
Authors: Keiichi Maeda, Tomonari Michiyama, Poonam Chandra, Stuart Ryder, Hanindyo Kuncarayakti, Daichi Hiramatsu, Masatoshi Imanishi
Figure caption: Radio light curves of SN 2018ivc. The high-frequency data are taken by ALMA at 100 (red circles) and 250 (blue squares) GHz, including the data from Maeda et al. (2023; small filled symbols), the new late-time data at >1000 days (large filled symbols), and the other archival data (open symbols). The late-time centimeter flux densities at 6.3/6.5 GHz (black open diamonds) are taken from Mutie et al. (2022). For band 3 data, the flux densities are corrected to those at 100 GHz, assuming the SED slope seen in a neighboring epoch when the SN was observed in both band 3 and band 6 (see Figure 2). The model curves at 100 (orange) and 250 (cyan) GHz in the earlier phase (≲200 days) are from Maeda et al. (2023). The four panels are shown with different models for the late-phase light curves at 6.5 (black), 100 (red), and 250 (blue) GHz with s = −2, 0, 1, and 2 for the CSM slope.
Paper: Resurrection of Type IIL Supernova 2018ivc: Implications for a Binary Evolution Sequence Connecting Hydrogen-rich and Hydrogen-poor Progenitors
Authors: Keiichi Maeda, Tomonari Michiyama, Poonam Chandra, Stuart Ryder, Hanindyo Kuncarayakti, Daichi Hiramatsu, Masatoshi Imanishi
Figure caption: Left: CSM distribution derived for SN 2018ivc. The inner structure at ≲2 × 1016 cm (black lines) is from Maeda et al. (2023). The CSM distributions adopted in the light-curve models (s = −2, 0, 1, and 2) for the late epochs (Figure 3) are shown by the gray lines, where the overlapping region (black diamond) is strongly constrained irrespective of the model details. Right: mass-loss history toward the SN (black line and point for SN 2018ivc). The mass-loss histories based on models 25 (peak at 5800 yr before the SN) and 28 (peak at ∼300 yr) of Ouchi & Maeda (2017) are shown for comparison, with model 28 (cyan) and model 25 shifted toward the SN by 5450 (blue) and 4300 (red) yr.
Paper: Resurrection of Type IIL Supernova 2018ivc: Implications for a Binary Evolution Sequence Connecting Hydrogen-rich and Hydrogen-poor Progenitors
Authors: Keiichi Maeda, Tomonari Michiyama, Poonam Chandra, Stuart Ryder, Hanindyo Kuncarayakti, Daichi Hiramatsu, Masatoshi Imanishi
Figure caption: The SED of SN 2018ivc on day ∼1300 (red circles), as constructed from the data at 6.3 (Mutie et al. 2022) and 100/250 (this work) GHz. For comparison, the SED on day 199 (black squares) is also shown (Maeda et al. 2023). The flux densities derived for the individual spectral windows (SPWs) are shown by open symbols, while the flux densities after combining the four continuum SPWs within each band are shown by filled symbols. The flux densities are shown with 1σ errors; the flux calibration error is included for the SPW-combined data, while it is omitted for the individual SPW data. The power-law fit to the ALMA data on day 1364 is shown by the dashed line. For demonstration purposes, the SED computed for the model with s = 1 is shown (magenta; see also Figure 3).
Paper: Resurrection of Type IIL Supernova 2018ivc: Implications for a Binary Evolution Sequence Connecting Hydrogen-rich and Hydrogen-poor Progenitors
Authors: Keiichi Maeda, Tomonari Michiyama, Poonam Chandra, Stuart Ryder, Hanindyo Kuncarayakti, Daichi Hiramatsu, Masatoshi Imanishi
Figure caption: ALMA band 3 (top) and band 6 (bottom) images of SN 2018ivc on days 199 (left; Maeda et al. 2023) and 1364 (right). The elliptical beam shape is shown in the bottom left corner in each panel.
Paper: COSMOS2020: Discovery of a Protocluster of Massive Quiescent Galaxies at z = 2.77
Authors: Kei Ito, Masayuki Tanaka, Francesco Valentino, Sune Toft, Gabriel Brammer, Katriona M. L. Gould, Olivier Ilbert, Nobunari Kashikawa, Mariko Kubo, Yongming Liang, Henry J. McCracken, John R. Weaver
Figure caption: Left panel: density map of quiescent galaxies with ﹩\mathrm{log}({M}_{\star }/{M}_{\odot })\gt 10.3﹩ at 2.74 < z phot < 2.94. The red shaded contours indicate −1σ, 0σ, 1σ, 2σ, 3σ, and 4σ overdensity. Gray regions correspond to the mask or the outside of the survey area (see Weaver et al. 2022). The dashed rectangle indicates the overdense structure reported in this paper. Right panel: zoom-in view of the overdense structure. The red and blue contours correspond to the density map of quiescent and star-forming galaxies with the same stellar mass cut, respectively. The number in these contours indicates the significance of the overdensity. The stars indicate the quiescent galaxies spectroscopically confirmed in this study, and the circles are photometrically selected ones at 2.74 < z phot < 2.94. They are color-coded by their stellar mass. The blue squares are star-forming galaxies in the same redshift slice. Black squares show the location of the MOSFIRE masks.
Paper: COSMOS2020: Discovery of a Protocluster of Massive Quiescent Galaxies at z = 2.77
Authors: Kei Ito, Masayuki Tanaka, Francesco Valentino, Sune Toft, Gabriel Brammer, Katriona M. L. Gould, Olivier Ilbert, Nobunari Kashikawa, Mariko Kubo, Yongming Liang, Henry J. McCracken, John R. Weaver
Figure caption: Left panels: spectra of four quiescent galaxies with significant absorption lines. The object spectra are shown with orange shading and the noise spectra with dark shading in each panel. In addition to QG301560 and QG280611, whose spectral analyses were conducted with binned spectra, the other spectra are also rebinned over four pixels just for illustrative purposes. The blue lines are the best fit from SLINEFIT. The gray masked regions are not observed or are largely affected by skylines and not used for the fitting. Right panels: blue and black lines indicate the probability distribution of the spectroscopic redshift from SLINEFIT and the photometric redshift from MIZUKI, respectively.
Paper: COSMOS2020: Discovery of a Protocluster of Massive Quiescent Galaxies at z = 2.77
Authors: Kei Ito, Masayuki Tanaka, Francesco Valentino, Sune Toft, Gabriel Brammer, Katriona M. L. Gould, Olivier Ilbert, Nobunari Kashikawa, Mariko Kubo, Yongming Liang, Henry J. McCracken, John R. Weaver
Figure caption: Left panel: Color–magnitude diagram for galaxies in the QO-1000 field. The vertical axis shows J − K  s , and the horizontal axis shows K  s -band magnitude. The red stars and open circles represent spectroscopic and photometric quiescent members of QO-1000, respectively. Blue circles are star-forming members. The gray crosses represent the other galaxies at 2.0 < z phot < 3.5 within the 2σ contour of Figure 1 in the projected space. The horizontal dashed lines show the J − K  s  color of the single-burst model of Bruzual & Charlot (2003) with different formation redshifts (z form = 3.0, 3.4, 3.7, and 6). Central panel: same as the left panel, but for galaxies at 2 < z phot < 3.5 randomly drawn from the entire COSMOS field apart from QO-1000. The same number of objects as in the QO-1000 field is drawn. Right panel: histogram of J − K  s  of all galaxies with K  s  < 22.5 mag in the QO-1000 field (red solid line) and randomly in the entire COSMOS field (gray dashed line).
Paper: COSMOS2020: Discovery of a Protocluster of Massive Quiescent Galaxies at z = 2.77
Authors: Kei Ito, Masayuki Tanaka, Francesco Valentino, Sune Toft, Gabriel Brammer, Katriona M. L. Gould, Olivier Ilbert, Nobunari Kashikawa, Mariko Kubo, Yongming Liang, Henry J. McCracken, John R. Weaver
Figure caption: Evolution of the host halo mass of the most massive quiescent galaxies in two structures similar to QO-1000 in TNG-300 (red lines). The evolution of the median halo mass of field quiescent galaxies with the same stellar mass in TNG-300 is shown by the gray line. The gray shaded region corresponds to the range between their 16th and 84th percentiles. The lower limit of the halo mass of QO-1000 (Section 3.4) is shown by the red star.
Paper: Prospective Implications of Extreme-ultraviolet Coronal Plumes for Magnetic-network Genesis of Coronal Heating, Coronal-hole Solar Wind, and Solar-wind Magnetic Field Switchbacks
Authors: Ronald L. Moore, Sanjiv K. Tiwari, Navdeep K. Panesar, Alphonse C. Sterling
Figure caption: Cradle-to-grave evolution of a typical EUV coronal plume (from Figure 6 of Avallone et al. 2018). Panel (a): swath of an AIA 211 Å full-Sun image, centered on the coronal hole of the plume, at the time of the plume’s maximum brightness in AIA 171 Å images, at 06:00 UT on 2011 July 6. The white box outlines the area of the 171 Å images in panel (b). Panel (b), top row: AIA 171 Å images centered on the plume’s foot (1) at the start of the plume’s birth, (2) during the plume’s growth, (3) during the plume’s maximum luminosity in AIA 171 Å images, (4) during the plumes decay, and (5) at the end of the plume’s decay. Panel (b), bottom row: HMI magnetograms of the same area at the times of the five 171 Å images, showing that the magnetic flux at the plume’s foot coalesces into a compact clump as the plume brightens in 171 Å emission and then disperses as the plume dies out.
Paper: Determining the IBEX Ribbon Transverse Profile from ENA Temporal Variations: A Proof of Concept for IMAP Observations
Authors: M. A. Dayeh, E. J. Zirnstein, D. J. McComas
Figure caption: (a) Azimuthal cut of the Ribbon at 315o azimuth showing the averaged ENA fluxes at 1.1 keV for P1 and P2. (b) Ribbon flux differences using data from (a); Red horizontal line marks the zero line of the difference flux, and vertical lines mark inferred Ribbon boundaries closest to the zero line. (c) Reconstruction of the GDF beneath the Ribbon; green shows the original surrounding GDF, orange shows the scaled GDF (see text for details). (d) Inferred Ribbon from the original data and the reconstructed GDF. (e) Determining peak and FWHM of the inferred Ribbon. (f) Contributions of the GDF and the Ribbon fluxes scaled to 100%.
Paper: Determining the IBEX Ribbon Transverse Profile from ENA Temporal Variations: A Proof of Concept for IMAP Observations
Authors: M. A. Dayeh, E. J. Zirnstein, D. J. McComas
Figure caption: ENA fluxes during the time periods P1 (green) and P2 (blue) studied here, along with their difference (red) for four different Ribbon transverse profiles (see gray arrows in Figures 1(a) and (b)). The figure highlights the distinctive transverse profiles that the Ribbon and its evolution over time could take. (a) shows a relatively symmetric flux change rate across the Ribbon; (b) and (c) show a one-sided skewed change and (d) shows a symmetric rate of change.
Paper: Determining the IBEX Ribbon Transverse Profile from ENA Temporal Variations: A Proof of Concept for IMAP Observations
Authors: M. A. Dayeh, E. J. Zirnstein, D. J. McComas
Figure caption: Time-averaged, Ribbon-frame maps of ENA fluxes at 1.1 keV during (a) period 1 (P1; 2009–2011 and (b) period 2 (P2; 2014–2015). (c) Difference flux maps showing the apparent evolution of the Ribbon fluxes. Gray arrows on the grid pointing inward mark the azimuths used for transverse profiles in Figure 2.
Paper: Determining the IBEX Ribbon Transverse Profile from ENA Temporal Variations: A Proof of Concept for IMAP Observations
Authors: M. A. Dayeh, E. J. Zirnstein, D. J. McComas
Figure caption: (a) Maximum Ribbon and GDF contributions to the total flux content across the sky in 2009–2011, centered on the azimuth intersecting the upwind direction (nose, see Figure 1). (b) inferred Ribbon-only FWHM, and (c) weighted Ribbon radius inferred using the derived Ribbon transverse profiles.
Paper: Unusual Hard X-Ray Flares Caught in NICER Monitoring of the Binary Supermassive Black Hole Candidate AT2019cuk/Tick Tock/SDSS J1430+2303
Authors: Megan Masterson, Erin Kara, Dheeraj R. Pasham, Daniel J. D'Orazio, Dominic J. Walton, Andrew C. Fabian, Matteo Lucchini, Ronald A. Remillard, Zaven Arzoumanian, Otabek Burkhonov, Hyeonho Choi, Shuhrat A. Ehgamberdiev, Elizabeth C. Ferrara, Muryel Guolo, Myungshin Im, Yonggi Kim, Davron O. Mirzaqulov, Gregory S. H. Paek, Hyun-Il Sung, Joh-Na Yoon
Figure caption: Multiwavelength light curve for AT2019cuk, with a zoom-in on the duration of the high-cadence NICER monitoring campaign. Top panel: full ZTF light curve from 2019 January to 2022 September. Red diamonds show the ZTF r-band data, offset by 0.8 mag, and yellow squares show the ZTF g-band data. The orange shaded region shows the prediction of the merger time from Jiang et al. (2022), using post-Newtonian modeling of both optical and X-ray data (see both Figure 3 and Extended Figure 9 of Jiang et al. 2022). The gray box represents the zoomed-in region shown in the lower four panels. Second panel: NICER (blue circles) and Swift XRT (green X’s) background-subtracted light curves in the 0.3–4 keV band. Swift data are scaled by a factor of 20 to account for the difference in effective area between the two telescopes. Third panel: Swift UVW1 light curve. Data have been corrected for Galactic extinction. Bottom two panels: optical light curves, with the fourth panel showing the ZTF g-band (yellow squares) and LOAO, MAO, and CBNUO B-band (light blue pentagons, triangles, and plus signs, respectively) data, and the fifth panel showing ZTF r-band (red diamonds) LOAO, MAO, and CBNUO R-band (light pink pentagons, triangles, and plus signs, respectively) data. There is a ≈9%–10% drop in the g- and B-band data in the fourth panel around MJD 59750 and a ≈3%–5% drop in the r- and R-band data at the same time, which corresponds to the time at which a large drop in the X-ray flux (≈50%) is also seen.