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1. Astrometric Accelerations as Dynamical Beacons: A Giant Planet Imaged inside the Debris Disk of the Young Star AF Lep

   https://doi.org/10.3847/2041-8213/acd6f6  

   Franson, Kyle ; Bowler, Brendan P. ; Zhou, Yifan ; Pearce, Tim D. ; Bardalez Gagliuffi, Daniella C. ; Biddle, Lauren I. ; Brandt, Timothy D. ; Crepp, Justin R. ; Dupuy, Trent J. ; Faherty, Jacqueline ; et al ( June 2023 , The Astrophysical Journal Letters)

   We present the direct-imaging discovery of a giant planet orbiting the young star AF Lep, a 1.2M_⊙member of the 24 ± 3 MyrβPic moving group. AF Lep was observed as part of our ongoing high-contrast imaging program targeting stars with astrometric accelerations between Hipparcos and Gaia that indicate the presence of substellar companions. Keck/NIRC2 observations in$L\prime$with the vector vortex coronagraph reveal a point source, AF Lep b, at ≈340 mas, which exhibits orbital motion at the 6σlevel over the course of 13 months. A joint orbit fit yields precise constraints on the planet’s dynamical mass of${3.2}_{-0.6}^{+0.7}$M_Jup, semimajor axis of${8.4}_{-1.3}^{+1.1}$au, and eccentricity of${0.24}_{-0.15}^{+0.27}$. AF Lep hosts a debris disk located at ∼50 au, but it is unlikely to be sculpted by AF Lep b, implying there may be additional planets in the system at wider separations. The stellar inclination (i_*=${54}_{-9}^{+11}°$) and orbital inclination (i_o=${50}_{-12}^{+9}°$) are in good agreement, which is consistent with the system having spin–orbit alignment. AF Lep b is the lowest-mass imaged planet with a dynamical mass measurement and highlights the promise of using astrometric accelerations as a tool to find and characterize long-period planets.

    

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2. The McDonald Accelerating Stars Survey: Architecture of the Ancient Five-planet Host System Kepler-444

   https://doi.org/10.3847/1538-3881/aca88c  

   Zhang 张周健, Zhoujian ; Bowler, Brendan P. ; Dupuy, Trent J. ; Brandt, Timothy D. ; Brandt, G. Mirek ; Cochran, William D. ; Endl, Michael ; MacQueen, Phillip J. ; Kratter, Kaitlin M. ; Isaacson, Howard T. ; et al ( January 2023 , The Astronomical Journal)

   We present the latest and most precise characterization of the architecture for the ancient (≈11 Gyr) Kepler-444 system, which is composed of a K0 primary star (Kepler-444 A) hosting five transiting planets and a tight M-type spectroscopic binary (Kepler-444 BC) with an A–BC projected separation of 66 au. We have measured the system’s relative astrometry using the adaptive optics imaging from Keck/NIRC2 and Kepler-444 A’s radial velocities from the Hobby-Eberly Telescope and reanalyzed relative radial velocities between BC and A from Keck/HIRES. We also include the Hipparcos-Gaia astrometric acceleration and all published astrometry and radial velocities in an updated orbit analysis of BC’s barycenter. These data greatly extend the time baseline of the monitoring and lead to significant updates to BC’s barycentric orbit compared to previous work, including a larger semimajor axis ($a={52.2}_{-2.7}^{+3.3}$au), a smaller eccentricity (e= 0.55 ± 0.05), and a more precise inclination ($i=85.°4_{-0.°4}^{+0.°3}$). We have also derived the first dynamical masses of B and C components. Our results suggest that Kepler-444 A’s protoplanetary disk was likely truncated by BC to a radius of ≈8 au, which resolves the previously noticed tension between Kepler-444 A’s disk mass and planet masses. Kepler-444 BC’s barycentric orbit is likely aligned with those of A’s five planets, which might be primordial or a consequence of dynamical evolution. The Kepler-444 system demonstrates that compact multiplanet systems residing in hierarchical stellar triples can form at early epochs of the universe and survive their secular evolution throughout cosmic time.

    

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3. 3D Selection of 167 Substellar Companions to Nearby Stars

   https://doi.org/10.3847/1538-4365/ac7e57  

   Feng, Fabo ; Butler, R. Paul ; Vogt, Steven S. ; Clement, Matthew S. ; Tinney, C. G. ; Cui, Kaiming ; Aizawa, Masataka ; Jones, Hugh R. A. ; Bailey, J. ; Burt, Jennifer ; et al ( August 2022 , The Astrophysical Journal Supplement Series)

   We analyze 5108 AFGKM stars with at least five high-precision radial velocity points, as well as Gaia and Hipparcos astrometric data, utilizing a novel pipeline developed in previous work. We find 914 radial velocity signals with periods longer than 1000 days. Around these signals, 167 cold giants and 68 other types of companions are identified, through combined analyses of radial velocity, astrometry, and imaging data. Without correcting for detection bias, we estimate the minimum occurrence rate of the wide-orbit brown dwarfs to be 1.3%, and find a significant brown-dwarf valley around 40M_Jup. We also find a power-law distribution in the host binary fraction beyond 3 au, similar to that found for single stars, indicating no preference of multiplicity for brown dwarfs. Our work also reveals nine substellar systems (GJ 234 B, GJ 494 B, HD 13724 b, HD 182488 b, HD 39060 b and c, HD 4113 C, HD 42581 d, HD 7449 B, and HD 984 b) that have previously been directly imaged, and many others that are observable at existing facilities. Depending on their ages, we estimate that an additional 10–57 substellar objects within our sample can be detected with current imaging facilities, extending the imaged cold (or old) giants by an order of magnitude.

    

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4. Wide post-common envelope binaries containing ultramassive white dwarfs: evidence for efficient envelope ejection in massive asymptotic giant branch stars

   https://doi.org/10.1093/mnras/stad4005  

   Yamaguchi, Natsuko ; El-Badry, Kareem ; Fuller, Jim ; Latham, David W. ; Cargile, Phillip A. ; Mazeh, Tsevi ; Shahaf, Sahar ; Bieryla, Allyson ; Buchhave, Lars A. ; Hobson, Melissa ( December 2023 , Monthly Notices of the Royal Astronomical Society)

   Post-common envelope binaries (PCEBs) containing a white dwarf (WD) and a main-sequence (MS) star can constrain the physics of common envelope evolution and calibrate binary evolution models. Most PCEBs studied to date have short orbital periods (Porb ≲ 1 d), implying relatively inefficient harnessing of binaries’ orbital energy for envelope expulsion. Here, we present follow-up observations of five binaries from 3rd data release of Gaia mission containing solar-type MS stars and probable ultramassive WDs ($M\gtrsim 1.2\ {\rm M}_{\odot}$) with significantly wider orbits than previously known PCEBs, Porb = 18–49 d. The WD masses are much higher than expected for systems formed via stable mass transfer at these periods, and their near-circular orbits suggest partial tidal circularization when the WD progenitors were giants. These properties strongly suggest that the binaries are PCEBs. Forming PCEBs at such wide separations requires highly efficient envelope ejection, and we find that the observed periods can only be explained if a significant fraction of the energy released when the envelope recombines goes into ejecting it. Our one-dimensional stellar models including recombination energy confirm prior predictions that a wide range of PCEB orbital periods, extending up to months or years, can potentially result from Roche lobe overflow of a luminous asymptotic giant branch (AGB) star. This evolutionary scenario may also explain the formation of several wide WD + MS binaries discovered via self-lensing, as well as a significant fraction of post-AGB binaries and barium stars.

    

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5. An Adaptive Optics Census of Companions to Northern Stars Within 25 pc with Robo-AO

   https://doi.org/10.3847/1538-3881/ac53fc  

   Salama, Maïssa ; Ziegler, Carl ; Baranec, Christoph ; Liu, Michael C. ; Law, Nicholas M. ; Riddle, Reed ; Henry, Todd J. ; Winters, Jennifer G. ; Jao, Wei-Chun ; Ou, James ; et al ( April 2022 , The Astronomical Journal)

   In order to assess the multiplicity statistics of stars across spectral types and populations in a volume-limited sample, we censused nearby stars for companions with Robo-AO. We report on observations of 1157 stars of all spectral types within 25 pc with decl. >−13° searching for tight companions. We detected 154 companion candidates with separations ranging from ∼0.″15 to 4.″0 and magnitude differences up to Δm${}_{i\prime }\le 7$using the robotic adaptive optics instrument Robo-AO. We confirmed physical association from Gaia EDR3 astrometry for 53 of the companion candidates, 99 remain to be confirmed, and two were ruled out as background objects. We complemented the high-resolution imaging companion search with a search for comoving objects with separations out to 10,000 au in Gaia EDR3, which resulted in an additional 147 companions registered. Of the 301 total companions reported in this study, 49 of them are new discoveries. Out of the 191 stars with significant acceleration measurements in the Hipparcos–Gaia catalog of accelerations, we detect companions around 115 of them, with the significance of the acceleration increasing as the companion separation decreases. From this survey, we report the following multiplicity fractions (compared to literature values): 40.9% ± 3.0% (44%) for FGK stars and 28.2% ± 2.3% (27%) for M stars, as well as higher-order fractions of 5.5% ± 1.1% (11%) and 3.9% ± 0.9% (5%) for FGK stars and M-type stars, respectively.

    

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