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</ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.10109">arXiv:2411.10109</a> <span> [<a href="https://arxiv.org/pdf/2411.10109">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Artificial Intelligence">cs.AI</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Human-Computer Interaction">cs.HC</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> </div> </div> <p class="title is-5 mathjax"> Generative Agent Simulations of 1,000 People </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Park%2C+J+S">Joon Sung Park</a>, <a href="/search/?searchtype=author&query=Zou%2C+C+Q">Carolyn Q. Zou</a>, <a href="/search/?searchtype=author&query=Shaw%2C+A">Aaron Shaw</a>, <a href="/search/?searchtype=author&query=Hill%2C+B+M">Benjamin Mako Hill</a>, <a href="/search/?searchtype=author&query=Cai%2C+C">Carrie Cai</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Meredith Ringel Morris</a>, <a href="/search/?searchtype=author&query=Willer%2C+R">Robb Willer</a>, <a href="/search/?searchtype=author&query=Liang%2C+P">Percy Liang</a>, <a href="/search/?searchtype=author&query=Bernstein%2C+M+S">Michael S. Bernstein</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.10109v1-abstract-short" style="display: inline;"> The promise of human behavioral simulation--general-purpose computational agents that replicate human behavior across domains--could enable broad applications in policymaking and social science. We present a novel agent architecture that simulates the attitudes and behaviors of 1,052 real individuals--applying large language models to qualitative interviews about their lives, then measuring how we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10109v1-abstract-full').style.display = 'inline'; document.getElementById('2411.10109v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.10109v1-abstract-full" style="display: none;"> The promise of human behavioral simulation--general-purpose computational agents that replicate human behavior across domains--could enable broad applications in policymaking and social science. We present a novel agent architecture that simulates the attitudes and behaviors of 1,052 real individuals--applying large language models to qualitative interviews about their lives, then measuring how well these agents replicate the attitudes and behaviors of the individuals that they represent. The generative agents replicate participants' responses on the General Social Survey 85% as accurately as participants replicate their own answers two weeks later, and perform comparably in predicting personality traits and outcomes in experimental replications. Our architecture reduces accuracy biases across racial and ideological groups compared to agents given demographic descriptions. This work provides a foundation for new tools that can help investigate individual and collective behavior. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10109v1-abstract-full').style.display = 'none'; document.getElementById('2411.10109v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.10597">arXiv:2410.10597</a> <span> [<a href="https://arxiv.org/pdf/2410.10597">pdf</a>, <a href="https://arxiv.org/format/2410.10597">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> SOFIA/HAWC+ Far-Infrared Polarimetric Large-Area CMZ Exploration Survey. IV. Relative Magnetic Field Orientation Throughout the CMZ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Par%C3%A9%2C+D+M">Dylan M. Par茅</a>, <a href="/search/?searchtype=author&query=Chuss%2C+D+T">David T. Chuss</a>, <a href="/search/?searchtype=author&query=Karpovich%2C+K">Kaitlyn Karpovich</a>, <a href="/search/?searchtype=author&query=Butterfield%2C+N+O">Natalie O. Butterfield</a>, <a href="/search/?searchtype=author&query=Iulliano%2C+J+I">Jeffrey Inara Iulliano</a>, <a href="/search/?searchtype=author&query=Pan%2C+X">Xing Pan</a>, <a href="/search/?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</a>, <a href="/search/?searchtype=author&query=Zhang%2C+Q">Qizhou Zhang</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Nilsson%2C+M">Matthilda Nilsson</a>, <a href="/search/?searchtype=author&query=Zhao%2C+R+J">Roy J. Zhao</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.10597v2-abstract-short" style="display: inline;"> The nature of the magnetic field structure throughout the Galactic Center (GC) has long been of interest. The recent Far-InfraREd Polarimetric Large-Area CMZ Exploration (FIREPLACE) Survey reveals preliminary connections between the seemingly distinct vertical and horizontal magnetic field distributions previously observed in the GC. We use the statistical techniques of the Histogram of Relative O… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.10597v2-abstract-full').style.display = 'inline'; document.getElementById('2410.10597v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.10597v2-abstract-full" style="display: none;"> The nature of the magnetic field structure throughout the Galactic Center (GC) has long been of interest. The recent Far-InfraREd Polarimetric Large-Area CMZ Exploration (FIREPLACE) Survey reveals preliminary connections between the seemingly distinct vertical and horizontal magnetic field distributions previously observed in the GC. We use the statistical techniques of the Histogram of Relative Orientation (HRO) and the Projected Rayleigh Statistic (PRS) to assess whether the CMZ magnetic field preferentially aligns with the structure of the CMZ molecular clouds or the morphology of the non-thermal emission of the GC NTF population. We find that there is a range of magnetic field orientations throughout the population of CMZ molecular clouds, ranging from parallel to perpendicular orientation. We posit these orientations depend on the prevalence of gravitational shear in the GC in contrast with what is observed in Galactic Disk star-forming regions. We also compare the magnetic field orientation from dust polarimetry with individual prominent NTFs, finding a preferred perpendicular relative orientation. This perpendicular orientation indicates that the vertical field component found in the FIREPLACE observations is not spatially confined to the NTFs, providing evidence for a more pervasive vertical field in the GC. From dynamical arguments, we estimate an upper limit on the magnetic field strength for this vertical field, finding B less than or equal to 4 mG. A field close to this upper limit would indicate that the NTFs are not local enhancements of a weaker background field and that the locations of the NTFs depend on proximity to sites of cosmic ray production. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.10597v2-abstract-full').style.display = 'none'; document.getElementById('2410.10597v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.16745">arXiv:2408.16745</a> <span> [<a href="https://arxiv.org/pdf/2408.16745">pdf</a>, <a href="https://arxiv.org/format/2408.16745">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> A VLA Study of Newly-Discovered Southern Latitude Non-Thermal Filaments in the Galactic Center: Polarimetric and Magnetic Field Properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pare%2C+D+M">Dylan M. Pare</a>, <a href="/search/?searchtype=author&query=Lang%2C+C+C">Cornelia C. Lang</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.16745v1-abstract-short" style="display: inline;"> A population of structures unique to the Galactic Center (GC), known as the non-thermal filaments (NTFs), has been studied for over 40 years, but much remains unknown about them. In particular, there is no widely-accepted and unified understanding for how the relativistic electrons illuminating these structures are generated. One possibility is that there are compact and extended sources of Cosmic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.16745v1-abstract-full').style.display = 'inline'; document.getElementById('2408.16745v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.16745v1-abstract-full" style="display: none;"> A population of structures unique to the Galactic Center (GC), known as the non-thermal filaments (NTFs), has been studied for over 40 years, but much remains unknown about them. In particular, there is no widely-accepted and unified understanding for how the relativistic electrons illuminating these structures are generated. One possibility is that there are compact and extended sources of Cosmic Rays (CRs), which then diffuse along magnetic flux tubes leading to the illumination of the NTFs through synchrotron emission. In this work, we present and discuss the polarimetric distributions associated with a set of faint NTFs in the GC that have only been studied in total intensity previously. We compare the derived polarized intensity, rotation measure, and intrinsic magnetic field distributions for these structures with the results obtained for previously observed GC NTFs. The results are then used to enhance our understanding of the large-scale polarimetric properties of the GC. We then use the derived polarimetric distributions to constrain models for the mechanisms generating the relativistic electrons that illuminate these structures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.16745v1-abstract-full').style.display = 'none'; document.getElementById('2408.16745v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.06312">arXiv:2408.06312</a> <span> [<a href="https://arxiv.org/pdf/2408.06312">pdf</a>, <a href="https://arxiv.org/format/2408.06312">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41550-024-02362-0">10.1038/s41550-024-02362-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A magnetised Galactic halo from inner Galaxy outflows </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Zhang%2C+H">He-Shou Zhang</a>, <a href="/search/?searchtype=author&query=Ponti%2C+G">Gabriele Ponti</a>, <a href="/search/?searchtype=author&query=Carretti%2C+E">Ettore Carretti</a>, <a href="/search/?searchtype=author&query=Liu%2C+R">Ruo-Yu Liu</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Haverkorn%2C+M">Marijke Haverkorn</a>, <a href="/search/?searchtype=author&query=Locatelli%2C+N">Nicola Locatelli</a>, <a href="/search/?searchtype=author&query=Zheng%2C+X">Xueying Zheng</a>, <a href="/search/?searchtype=author&query=Aharonian%2C+F">Felix Aharonian</a>, <a href="/search/?searchtype=author&query=Zhang%2C+H">Haiming Zhang</a>, <a href="/search/?searchtype=author&query=Zhang%2C+Y">Yi Zhang</a>, <a href="/search/?searchtype=author&query=Stel%2C+G">Giovanni Stel</a>, <a href="/search/?searchtype=author&query=Strong%2C+A">Andrew Strong</a>, <a href="/search/?searchtype=author&query=Yeung%2C+M">Micheal Yeung</a>, <a href="/search/?searchtype=author&query=Merloni%2C+A">Andrea Merloni</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.06312v1-abstract-short" style="display: inline;"> Large-scale magnetic fields are observed off the midplanes of disk galaxies, indicating that they harbour magnetised halos. These halos are crucial to studies of galaxy evolution, galactic-scale outflows, and feedback from star formation activity. Identifying the magnetised halo of the Milky Way is challenging because of the potential contamination from foreground emission arising in local spiral… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.06312v1-abstract-full').style.display = 'inline'; document.getElementById('2408.06312v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.06312v1-abstract-full" style="display: none;"> Large-scale magnetic fields are observed off the midplanes of disk galaxies, indicating that they harbour magnetised halos. These halos are crucial to studies of galaxy evolution, galactic-scale outflows, and feedback from star formation activity. Identifying the magnetised halo of the Milky Way is challenging because of the potential contamination from foreground emission arising in local spiral arms. Additionally, it is unclear how our magnetic halo is influenced by recently revealed large-scale structures such as the X-ray emitting eROSITA Bubbles, which, according to previous simulations, might be transient structures powered by the Galactic Center or the Galaxy's star-forming ring. Here we report the identification of several kpc-scale magnetised structures based on their polarized radio emission and their gamma-ray counterparts, which can be interpreted as the radiation of relativistic electrons. These non-thermal structures extend far above and below the Galactic plane and are spatially coincident with the thermal X-ray emission from the eROSITA Bubbles. The morphological consistency of these structures suggests a common origin, which can be sustained by Galactic outflows driven by the active star-forming regions located at 3-5 kpc from the Galactic Centre. These results reveal how X-ray-emitting and magnetised halos of spiral galaxies can be related to intense star formation activities and suggest that the X-shaped coherent magnetic structures observed in their halos can stem from galaxy outflows. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.06312v1-abstract-full').style.display = 'none'; document.getElementById('2408.06312v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Initially submitted on March 2nd, 2024</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature Astronomy (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.03467">arXiv:2408.03467</a> <span> [<a href="https://arxiv.org/pdf/2408.03467">pdf</a>, <a href="https://arxiv.org/format/2408.03467">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/ad6cd6">10.3847/1538-3881/ad6cd6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Galactic Center in Color: Measuring Extinction with High-Proper-Motion Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Haggard%2C+Z">Z. Haggard</a>, <a href="/search/?searchtype=author&query=Ghez%2C+A+M">A. M. Ghez</a>, <a href="/search/?searchtype=author&query=Sakai%2C+S">S. Sakai</a>, <a href="/search/?searchtype=author&query=Gautam%2C+A+K">A. K. Gautam</a>, <a href="/search/?searchtype=author&query=Do%2C+T">T. Do</a>, <a href="/search/?searchtype=author&query=Lu%2C+J+R">J. R. Lu</a>, <a href="/search/?searchtype=author&query=Hosek%2C+M">M. Hosek</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">M. R. Morris</a>, <a href="/search/?searchtype=author&query=Granados%2C+S">S. Granados</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.03467v1-abstract-short" style="display: inline;"> The Milky Way's central parsec is a highly extinguished region with a population of high-proper-motion stars. We have tracked 145 stars for $\sim$10 years at wavelengths between 1 and 4 microns to analyze extinction effects in color-magnitude space. Approximately $30\%$ of this sample dims and reddens over the course of years, likely from the motion of sources relative to an inhomogeneous screen o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03467v1-abstract-full').style.display = 'inline'; document.getElementById('2408.03467v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.03467v1-abstract-full" style="display: none;"> The Milky Way's central parsec is a highly extinguished region with a population of high-proper-motion stars. We have tracked 145 stars for $\sim$10 years at wavelengths between 1 and 4 microns to analyze extinction effects in color-magnitude space. Approximately $30\%$ of this sample dims and reddens over the course of years, likely from the motion of sources relative to an inhomogeneous screen of dust. We correct previous measurements of the intrinsic variability fraction for differential extinction effects, resulting in a reduced stellar variability fraction of $34\%$. The extinction variability sub-sample shows that the extinguishing material has sub-arcsecond scales, much smaller variations than previously reported. The observed extinction events imply a typical cross-section of 500 AU and a density of around $3 \times 10^{4} \ \mathrm{atoms/cm^{3}}$ for the extinguishing material, which are consistent with measurements of filamentary dust and gas at the Galactic Center. Furthermore, given that the stars showing extinction variability tend to be more highly reddened than the rest of the sample, the extinction changes are likely due to material localized to the Galactic Center region. We estimate the relative extinction between 1 and 4 microns as, $\mathrm{A}_{\mathrm{H}}:\mathrm{A}_{\mathrm{K'}}:\mathrm{A}_{\mathrm{L'}} = 1.67 \pm 0.05:1:0.69 \pm 0.03$. Our measurement of extinction at longer wavelengths -- L' (3.8 $渭$m) -- is inconsistent with recent estimations of the integrated extinction towards the central parsec. One interpretation of this difference is that the dust variations this experiment is sensitive to -- which are local to the Galactic Center -- are dominated by grains of larger radius than the foreground. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03467v1-abstract-full').style.display = 'none'; document.getElementById('2408.03467v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">49 pages, 30 figures, accepted for publication in The Astronomical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.03136">arXiv:2408.03136</a> <span> [<a href="https://arxiv.org/pdf/2408.03136">pdf</a>, <a href="https://arxiv.org/format/2408.03136">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3390/galaxies12040044">10.3390/galaxies12040044 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Dust-Scattering Model for M1-92: A Revised Estimate of the Mass Distribution and Inclination </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Li%2C+Y+Q">Yun Qi Li</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Sahai%2C+R">Raghvendra Sahai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.03136v2-abstract-short" style="display: inline;"> Preplanetary nebulae (PPNe) are formed from mass-ejecting late-stage AGB stars. Much of the light from the star gets scattered or absorbed by dust particles, giving rise to the observed reflection nebula seen at visible and near-IR wavelengths. Precursors to planetary nebulae (PNe), PPNe generally have not yet undergone any ionization by UV radiation from the still-buried stellar core. Bipolar PPN… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03136v2-abstract-full').style.display = 'inline'; document.getElementById('2408.03136v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.03136v2-abstract-full" style="display: none;"> Preplanetary nebulae (PPNe) are formed from mass-ejecting late-stage AGB stars. Much of the light from the star gets scattered or absorbed by dust particles, giving rise to the observed reflection nebula seen at visible and near-IR wavelengths. Precursors to planetary nebulae (PNe), PPNe generally have not yet undergone any ionization by UV radiation from the still-buried stellar core. Bipolar PPNe are a common form of observed PPNe. This study lays the groundwork for future dynamical studies by reconstructing the dust density distribution of a particularly symmetric bipolar PPN, M1-92 (Minkowski's Footprint, IRAS 19343$+$2926). For this purpose, we develop an efficient single-scattering radiative transfer model with corrections for double-scattering. Using a V-band image from the Hubble Space Telescope (HST), we infer the dust density profile and orientation of M1-92. These results indicate that M1-92's slowly expanding equatorial torus exhibits an outer radial cutoff in its density, which implicates the influence of a binary companion during the formation of the nebula. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03136v2-abstract-full').style.display = 'none'; document.getElementById('2408.03136v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 8 figures, accepted for publications in Galaxies</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Galaxies 2024, 12(4), 44 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.08054">arXiv:2407.08054</a> <span> [<a href="https://arxiv.org/pdf/2407.08054">pdf</a>, <a href="https://arxiv.org/format/2407.08054">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> SOFIA/FORCAST Galactic Center Source Catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Cotera%2C+A+S">Angela S. Cotera</a>, <a href="/search/?searchtype=author&query=Hankins%2C+M+J">Matthew J. Hankins</a>, <a href="/search/?searchtype=author&query=Bally%2C+J">John Bally</a>, <a href="/search/?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/?searchtype=author&query=Battersby%2C+C+D">Cara D. Battersby</a>, <a href="/search/?searchtype=author&query=Hatchfield%2C+H+P">H Perry Hatchfield</a>, <a href="/search/?searchtype=author&query=Herter%2C+T+L">Terry L. Herter</a>, <a href="/search/?searchtype=author&query=Lau%2C+R+M">Ryan M. Lau</a>, <a href="/search/?searchtype=author&query=Longmore%2C+S+N">Steven N. Longmore</a>, <a href="/search/?searchtype=author&query=Mills%2C+E+A+C">Elisabeth A. C. Mills</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Radomski%2C+J+T">James T. Radomski</a>, <a href="/search/?searchtype=author&query=Simpson%2C+J+P">Janet P. Simpson</a>, <a href="/search/?searchtype=author&query=Stephens%2C+Z">Zachary Stephens</a>, <a href="/search/?searchtype=author&query=Walker%2C+D+L">Daniel L. Walker</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.08054v1-abstract-short" style="display: inline;"> The central regions of the Milky Way constitute a unique laboratory for a wide swath of astrophysical studies, consequently the inner $\sim$400 pc has been the target of numerous large surveys at all accessible wavelengths. In this paper we present a catalog of sources at 25 and 37 $渭$m located within all of the regions observed with the SOFIA/FORCAST instrument in the inner $\sim$200 pc of the Ga… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.08054v1-abstract-full').style.display = 'inline'; document.getElementById('2407.08054v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.08054v1-abstract-full" style="display: none;"> The central regions of the Milky Way constitute a unique laboratory for a wide swath of astrophysical studies, consequently the inner $\sim$400 pc has been the target of numerous large surveys at all accessible wavelengths. In this paper we present a catalog of sources at 25 and 37 $渭$m located within all of the regions observed with the SOFIA/FORCAST instrument in the inner $\sim$200 pc of the Galaxy. The majority of the observations were obtained as part of the SOFIA Cycle 7 Galactic Center Legacy program survey, which was designed to complement the Spitzer/MIPS 24 $渭$m catalog in regions saturated in the MIPS observations. Due to the wide variety of source types captured by our observations at 25 and 37 $渭$m, we do not limit the FORCAST source catalog to unresolved point sources, or treat all sources as if they are point-like sources. The catalog includes all detectable sources in the regions, resulting in a catalog of 950 sources, including point sources, compact sources, and extended sources. We also provide the user with metrics to discriminate between the source types. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.08054v1-abstract-full').style.display = 'none'; document.getElementById('2407.08054v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 13 figures, Accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.09264">arXiv:2406.09264</a> <span> [<a href="https://arxiv.org/pdf/2406.09264">pdf</a>, <a href="https://arxiv.org/format/2406.09264">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Human-Computer Interaction">cs.HC</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Artificial Intelligence">cs.AI</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computation and Language">cs.CL</span> </div> </div> <p class="title is-5 mathjax"> Towards Bidirectional Human-AI Alignment: A Systematic Review for Clarifications, Framework, and Future Directions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Shen%2C+H">Hua Shen</a>, <a href="/search/?searchtype=author&query=Knearem%2C+T">Tiffany Knearem</a>, <a href="/search/?searchtype=author&query=Ghosh%2C+R">Reshmi Ghosh</a>, <a href="/search/?searchtype=author&query=Alkiek%2C+K">Kenan Alkiek</a>, <a href="/search/?searchtype=author&query=Krishna%2C+K">Kundan Krishna</a>, <a href="/search/?searchtype=author&query=Liu%2C+Y">Yachuan Liu</a>, <a href="/search/?searchtype=author&query=Ma%2C+Z">Ziqiao Ma</a>, <a href="/search/?searchtype=author&query=Petridis%2C+S">Savvas Petridis</a>, <a href="/search/?searchtype=author&query=Peng%2C+Y">Yi-Hao Peng</a>, <a href="/search/?searchtype=author&query=Qiwei%2C+L">Li Qiwei</a>, <a href="/search/?searchtype=author&query=Rakshit%2C+S">Sushrita Rakshit</a>, <a href="/search/?searchtype=author&query=Si%2C+C">Chenglei Si</a>, <a href="/search/?searchtype=author&query=Xie%2C+Y">Yutong Xie</a>, <a href="/search/?searchtype=author&query=Bigham%2C+J+P">Jeffrey P. Bigham</a>, <a href="/search/?searchtype=author&query=Bentley%2C+F">Frank Bentley</a>, <a href="/search/?searchtype=author&query=Chai%2C+J">Joyce Chai</a>, <a href="/search/?searchtype=author&query=Lipton%2C+Z">Zachary Lipton</a>, <a href="/search/?searchtype=author&query=Mei%2C+Q">Qiaozhu Mei</a>, <a href="/search/?searchtype=author&query=Mihalcea%2C+R">Rada Mihalcea</a>, <a href="/search/?searchtype=author&query=Terry%2C+M">Michael Terry</a>, <a href="/search/?searchtype=author&query=Yang%2C+D">Diyi Yang</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Meredith Ringel Morris</a>, <a href="/search/?searchtype=author&query=Resnick%2C+P">Paul Resnick</a>, <a href="/search/?searchtype=author&query=Jurgens%2C+D">David Jurgens</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.09264v3-abstract-short" style="display: inline;"> Recent advancements in general-purpose AI have highlighted the importance of guiding AI systems towards the intended goals, ethical principles, and values of individuals and groups, a concept broadly recognized as alignment. However, the lack of clarified definitions and scopes of human-AI alignment poses a significant obstacle, hampering collaborative efforts across research domains to achieve th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.09264v3-abstract-full').style.display = 'inline'; document.getElementById('2406.09264v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.09264v3-abstract-full" style="display: none;"> Recent advancements in general-purpose AI have highlighted the importance of guiding AI systems towards the intended goals, ethical principles, and values of individuals and groups, a concept broadly recognized as alignment. However, the lack of clarified definitions and scopes of human-AI alignment poses a significant obstacle, hampering collaborative efforts across research domains to achieve this alignment. In particular, ML- and philosophy-oriented alignment research often views AI alignment as a static, unidirectional process (i.e., aiming to ensure that AI systems' objectives match humans) rather than an ongoing, mutual alignment problem. This perspective largely neglects the long-term interaction and dynamic changes of alignment. To understand these gaps, we introduce a systematic review of over 400 papers published between 2019 and January 2024, spanning multiple domains such as Human-Computer Interaction (HCI), Natural Language Processing (NLP), Machine Learning (ML). We characterize, define and scope human-AI alignment. From this, we present a conceptual framework of "Bidirectional Human-AI Alignment" to organize the literature from a human-centered perspective. This framework encompasses both 1) conventional studies of aligning AI to humans that ensures AI produces the intended outcomes determined by humans, and 2) a proposed concept of aligning humans to AI, which aims to help individuals and society adjust to AI advancements both cognitively and behaviorally. Additionally, we articulate the key findings derived from literature analysis, including literature gaps and trends, human values, and interaction techniques. To pave the way for future studies, we envision three key challenges and give recommendations for future research. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.09264v3-abstract-full').style.display = 'none'; document.getElementById('2406.09264v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">proposing "bidirectional human-AI alignment" framework after a systematic review of over 400 alignment papers</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.04446">arXiv:2406.04446</a> <span> [<a href="https://arxiv.org/pdf/2406.04446">pdf</a>, <a href="https://arxiv.org/format/2406.04446">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Artificial Intelligence">cs.AI</span> </div> </div> <p class="title is-5 mathjax"> Can Language Models Use Forecasting Strategies? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pratt%2C+S">Sarah Pratt</a>, <a href="/search/?searchtype=author&query=Blumberg%2C+S">Seth Blumberg</a>, <a href="/search/?searchtype=author&query=Carolino%2C+P+K">Pietro Kreitlon Carolino</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Meredith Ringel Morris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.04446v1-abstract-short" style="display: inline;"> Advances in deep learning systems have allowed large models to match or surpass human accuracy on a number of skills such as image classification, basic programming, and standardized test taking. As the performance of the most capable models begin to saturate on tasks where humans already achieve high accuracy, it becomes necessary to benchmark models on increasingly complex abilities. One such ta… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.04446v1-abstract-full').style.display = 'inline'; document.getElementById('2406.04446v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.04446v1-abstract-full" style="display: none;"> Advances in deep learning systems have allowed large models to match or surpass human accuracy on a number of skills such as image classification, basic programming, and standardized test taking. As the performance of the most capable models begin to saturate on tasks where humans already achieve high accuracy, it becomes necessary to benchmark models on increasingly complex abilities. One such task is forecasting the future outcome of events. In this work we describe experiments using a novel dataset of real world events and associated human predictions, an evaluation metric to measure forecasting ability, and the accuracy of a number of different LLM based forecasting designs on the provided dataset. Additionally, we analyze the performance of the LLM forecasters against human predictions and find that models still struggle to make accurate predictions about the future. Our follow-up experiments indicate this is likely due to models' tendency to guess that most events are unlikely to occur (which tends to be true for many prediction datasets, but does not reflect actual forecasting abilities). We reflect on next steps for developing a systematic and reliable approach to studying LLM forecasting. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.04446v1-abstract-full').style.display = 'none'; document.getElementById('2406.04446v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.04022">arXiv:2406.04022</a> <span> [<a href="https://arxiv.org/pdf/2406.04022">pdf</a>, <a href="https://arxiv.org/format/2406.04022">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The SKA Galactic Centre Survey -- A White Paper </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Schoedel%2C+R">Rainer Schoedel</a>, <a href="/search/?searchtype=author&query=Alberdi%2C+A">Antxon Alberdi</a>, <a href="/search/?searchtype=author&query=Jimenez-Serra%2C+I">Izaskun Jimenez-Serra</a>, <a href="/search/?searchtype=author&query=Yusef-Zadeh%2C+F">Farhad Yusef-Zadeh</a>, <a href="/search/?searchtype=author&query=Gardini%2C+A">Angela Gardini</a>, <a href="/search/?searchtype=author&query=Kramer%2C+M">Michael Kramer</a>, <a href="/search/?searchtype=author&query=Torres%2C+M+P">Miguel Perez Torres</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Forbrich%2C+J">Jan Forbrich</a>, <a href="/search/?searchtype=author&query=Ingallinera%2C+A">Adriano Ingallinera</a>, <a href="/search/?searchtype=author&query=Nogueras-Lara%2C+F">Francisco Nogueras-Lara</a>, <a href="/search/?searchtype=author&query=Henshaw%2C+J+D">Jonathan D. Henshaw</a>, <a href="/search/?searchtype=author&query=Longmore%2C+S+N">Steven N. Longmore</a>, <a href="/search/?searchtype=author&query=Moldon%2C+J">Javier Moldon</a>, <a href="/search/?searchtype=author&query=Heywood%2C+I">Ian Heywood</a>, <a href="/search/?searchtype=author&query=Rammala%2C+I">Isabella Rammala</a>, <a href="/search/?searchtype=author&query=Montenegro%2C+L+V">Lourdes Verdes Montenegro</a>, <a href="/search/?searchtype=author&query=Exposito%2C+S+S">Susana Sanchez Exposito</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.04022v1-abstract-short" style="display: inline;"> With its extreme density of stars and stellar remnants, dense young massive clusters, high specific star formation rate, intense radiation field, high magnetic field strength, and properties of the interstellar medium that resemble those in high redshift galaxies and starbursts, the Galactic Centre is the most extreme environment that we can observe in detail. It is also the only nucleus of a gala… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.04022v1-abstract-full').style.display = 'inline'; document.getElementById('2406.04022v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.04022v1-abstract-full" style="display: none;"> With its extreme density of stars and stellar remnants, dense young massive clusters, high specific star formation rate, intense radiation field, high magnetic field strength, and properties of the interstellar medium that resemble those in high redshift galaxies and starbursts, the Galactic Centre is the most extreme environment that we can observe in detail. It is also the only nucleus of a galaxy that we can observe with a resolution of just a few milli parsecs. This makes it a crucial target to understand the physics of galactic nuclei and star formation, as well as the connection between them. It enables studies of a large number of otherwise rare objects, such as extremely massive stars and stellar remnants, at a well-defined distance, thus facilitating the interpretation of their properties. The Galactic Centre has been and is being studied intensively with the most advanced facilities. In this White Paper, we advocate for a large-area, multi-wavelength survey with the Square Kilometre Array of an area of about 1.25x0.3 deg**2 (180x40 pc**2), centered on the massive black hole Sagittarius A* and for repeated deep observations of the nuclear star cluster over a decade, which will allow the community to address multiple science problems with a single data set. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.04022v1-abstract-full').style.display = 'none'; document.getElementById('2406.04022v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.16244">arXiv:2404.16244</a> <span> [<a href="https://arxiv.org/pdf/2404.16244">pdf</a>, <a href="https://arxiv.org/format/2404.16244">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computers and Society">cs.CY</span> </div> </div> <p class="title is-5 mathjax"> The Ethics of Advanced AI Assistants </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gabriel%2C+I">Iason Gabriel</a>, <a href="/search/?searchtype=author&query=Manzini%2C+A">Arianna Manzini</a>, <a href="/search/?searchtype=author&query=Keeling%2C+G">Geoff Keeling</a>, <a href="/search/?searchtype=author&query=Hendricks%2C+L+A">Lisa Anne Hendricks</a>, <a href="/search/?searchtype=author&query=Rieser%2C+V">Verena Rieser</a>, <a href="/search/?searchtype=author&query=Iqbal%2C+H">Hasan Iqbal</a>, <a href="/search/?searchtype=author&query=Toma%C5%A1ev%2C+N">Nenad Toma拧ev</a>, <a href="/search/?searchtype=author&query=Ktena%2C+I">Ira Ktena</a>, <a href="/search/?searchtype=author&query=Kenton%2C+Z">Zachary Kenton</a>, <a href="/search/?searchtype=author&query=Rodriguez%2C+M">Mikel Rodriguez</a>, <a href="/search/?searchtype=author&query=El-Sayed%2C+S">Seliem El-Sayed</a>, <a href="/search/?searchtype=author&query=Brown%2C+S">Sasha Brown</a>, <a href="/search/?searchtype=author&query=Akbulut%2C+C">Canfer Akbulut</a>, <a href="/search/?searchtype=author&query=Trask%2C+A">Andrew Trask</a>, <a href="/search/?searchtype=author&query=Hughes%2C+E">Edward Hughes</a>, <a href="/search/?searchtype=author&query=Bergman%2C+A+S">A. Stevie Bergman</a>, <a href="/search/?searchtype=author&query=Shelby%2C+R">Renee Shelby</a>, <a href="/search/?searchtype=author&query=Marchal%2C+N">Nahema Marchal</a>, <a href="/search/?searchtype=author&query=Griffin%2C+C">Conor Griffin</a>, <a href="/search/?searchtype=author&query=Mateos-Garcia%2C+J">Juan Mateos-Garcia</a>, <a href="/search/?searchtype=author&query=Weidinger%2C+L">Laura Weidinger</a>, <a href="/search/?searchtype=author&query=Street%2C+W">Winnie Street</a>, <a href="/search/?searchtype=author&query=Lange%2C+B">Benjamin Lange</a>, <a href="/search/?searchtype=author&query=Ingerman%2C+A">Alex Ingerman</a>, <a href="/search/?searchtype=author&query=Lentz%2C+A">Alison Lentz</a> , et al. (32 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.16244v2-abstract-short" style="display: inline;"> This paper focuses on the opportunities and the ethical and societal risks posed by advanced AI assistants. We define advanced AI assistants as artificial agents with natural language interfaces, whose function is to plan and execute sequences of actions on behalf of a user, across one or more domains, in line with the user's expectations. The paper starts by considering the technology itself, pro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.16244v2-abstract-full').style.display = 'inline'; document.getElementById('2404.16244v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.16244v2-abstract-full" style="display: none;"> This paper focuses on the opportunities and the ethical and societal risks posed by advanced AI assistants. We define advanced AI assistants as artificial agents with natural language interfaces, whose function is to plan and execute sequences of actions on behalf of a user, across one or more domains, in line with the user's expectations. The paper starts by considering the technology itself, providing an overview of AI assistants, their technical foundations and potential range of applications. It then explores questions around AI value alignment, well-being, safety and malicious uses. Extending the circle of inquiry further, we next consider the relationship between advanced AI assistants and individual users in more detail, exploring topics such as manipulation and persuasion, anthropomorphism, appropriate relationships, trust and privacy. With this analysis in place, we consider the deployment of advanced assistants at a societal scale, focusing on cooperation, equity and access, misinformation, economic impact, the environment and how best to evaluate advanced AI assistants. Finally, we conclude by providing a range of recommendations for researchers, developers, policymakers and public stakeholders. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.16244v2-abstract-full').style.display = 'none'; document.getElementById('2404.16244v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.12542">arXiv:2404.12542</a> <span> [<a href="https://arxiv.org/pdf/2404.12542">pdf</a>, <a href="https://arxiv.org/format/2404.12542">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Pinwheel Outflow induced by Stellar Mass Loss in a Coplanar Triple System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kim%2C+H">Hyosun Kim</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Kim%2C+J">Jongsoo Kim</a>, <a href="/search/?searchtype=author&query=He%2C+J">Jinhua He</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.12542v1-abstract-short" style="display: inline;"> We develop a physical framework for interpreting complex circumstellar patterns whorled around asymptotic giant branch (AGB) stars by investigating stable, coplanar triple systems using hydrodynamic and particle simulations. The introduction of a close tertiary body causes an additional periodic variation in the orbital velocity and trajectory of the AGB star. As a result, the circumstellar outflo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.12542v1-abstract-full').style.display = 'inline'; document.getElementById('2404.12542v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.12542v1-abstract-full" style="display: none;"> We develop a physical framework for interpreting complex circumstellar patterns whorled around asymptotic giant branch (AGB) stars by investigating stable, coplanar triple systems using hydrodynamic and particle simulations. The introduction of a close tertiary body causes an additional periodic variation in the orbital velocity and trajectory of the AGB star. As a result, the circumstellar outflow builds a fine non-Archimedean spiral pattern superimposed upon the Archimedean spiral produced by the outer binary alone. This fine spiral can be approximated by off-centered circular rings that become tangent to each other at the location of the Archimedean spiral. The superimposed fine pattern fades out relatively quickly as a function of distance from the center of the system, in contrast to the dominant Archimedean spiral pattern, which presents a much slower fractional density decrease with radius. The different rates of radial decrease of the density contrast in the two superimposed patterns, coupled with their different time and spatial scales, lead to an apparent, but illusory radial change in the observed pattern interval, as has been reported, for example, in CW Leo. The function describing the detailed radial dependence of the expansion velocity is different in the two patterns, which may be used to distinguish them. The shape of the circumstellar whorled pattern is further explored as a function of the orbital eccentricity and the inner companion's mass. Although this study is confined to stable, coplanar triple systems, the results are likely applicable to moderately noncoplanar systems and open interesting avenues for studying noncoplanar systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.12542v1-abstract-full').style.display = 'none'; document.getElementById('2404.12542v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 7 figures, 1 table, ApJ in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.07808">arXiv:2404.07808</a> <span> [<a href="https://arxiv.org/pdf/2404.07808">pdf</a>, <a href="https://arxiv.org/format/2404.07808">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> A broad linewidth, compact, millimeter-bright molecular emission line source near the Galactic Center </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ginsburg%2C+A">Adam Ginsburg</a>, <a href="/search/?searchtype=author&query=Bally%2C+J">John Bally</a>, <a href="/search/?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/?searchtype=author&query=Battersby%2C+C">Cara Battersby</a>, <a href="/search/?searchtype=author&query=Budaiev%2C+N">Nazar Budaiev</a>, <a href="/search/?searchtype=author&query=Butterfield%2C+N+O">Natalie O. Butterfield</a>, <a href="/search/?searchtype=author&query=Caselli%2C+P">Paola Caselli</a>, <a href="/search/?searchtype=author&query=Colzi%2C+L">Laura Colzi</a>, <a href="/search/?searchtype=author&query=Dutkowska%2C+K+M">Katarzyna M. Dutkowska</a>, <a href="/search/?searchtype=author&query=Garc%C3%ADa%2C+P">Pablo Garc铆a</a>, <a href="/search/?searchtype=author&query=Gramze%2C+S">Savannah Gramze</a>, <a href="/search/?searchtype=author&query=Henshaw%2C+J+D">Jonathan D. Henshaw</a>, <a href="/search/?searchtype=author&query=Hu%2C+Y">Yue Hu</a>, <a href="/search/?searchtype=author&query=Jeff%2C+D">Desmond Jeff</a>, <a href="/search/?searchtype=author&query=Jim%C3%A9nez-Serra%2C+I">Izaskun Jim茅nez-Serra</a>, <a href="/search/?searchtype=author&query=Kauffmann%2C+J">Jens Kauffmann</a>, <a href="/search/?searchtype=author&query=Klessen%2C+R+S">Ralf S. Klessen</a>, <a href="/search/?searchtype=author&query=Levesque%2C+E+M">Emily M. Levesque</a>, <a href="/search/?searchtype=author&query=Longmore%2C+S+N">Steven N. Longmore</a>, <a href="/search/?searchtype=author&query=Lu%2C+X">Xing Lu</a>, <a href="/search/?searchtype=author&query=Mills%2C+E+A+C">Elisabeth A. C. Mills</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Nogueras-Lara%2C+F">Francisco Nogueras-Lara</a>, <a href="/search/?searchtype=author&query=Oka%2C+T">Tomoharu Oka</a>, <a href="/search/?searchtype=author&query=Pineda%2C+J+E">Jaime E. Pineda</a> , et al. (15 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.07808v2-abstract-short" style="display: inline;"> A compact source, G0.02467-0.0727, was detected in ALMA \threemm observations in continuum and very broad line emission. The continuum emission has a spectral index $伪\approx3.3$, suggesting that the emission is from dust. The line emission is detected in several transitions of CS, SO, and SO$_2$ and exhibits a line width FWHM $\approx160$ \kms. The line profile appears Gaussian. The emission is w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07808v2-abstract-full').style.display = 'inline'; document.getElementById('2404.07808v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.07808v2-abstract-full" style="display: none;"> A compact source, G0.02467-0.0727, was detected in ALMA \threemm observations in continuum and very broad line emission. The continuum emission has a spectral index $伪\approx3.3$, suggesting that the emission is from dust. The line emission is detected in several transitions of CS, SO, and SO$_2$ and exhibits a line width FWHM $\approx160$ \kms. The line profile appears Gaussian. The emission is weakly spatially resolved, coming from an area on the sky $\lesssim1"$ in diameter ($\lesssim10^4$ AU at the distance of the Galactic Center; GC). The centroid velocity is $v_{LSR}\approx40$-$50$ \kms, which is consistent with a location in the Galactic Center. With multiple SO lines detected, and assuming local thermodynamic equilibrium (LTE) conditions, $T_\mathrm{LTE} = 13$ K, which is colder than seen in typical GC clouds, though we cannot rule out low-density, subthermally excited, warmer gas. Despite the high velocity dispersion, no emission is observed from SiO, suggesting that there are no strong ($\gtrsim10~\mathrm{km~s}^{-1}$) shocks in the molecular gas. There are no detections at other wavelengths, including X-ray, infrared, and radio. We consider several explanations for the Millimeter Ultra-Broad Line Object (MUBLO), including protostellar outflow, explosive outflow, collapsing cloud, evolved star, stellar merger, high-velocity compact cloud, intermediate mass black hole, and background galaxy. Most of these conceptual models are either inconsistent with the data or do not fully explain it. The MUBLO is, at present, an observationally unique object. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.07808v2-abstract-full').style.display = 'none'; document.getElementById('2404.07808v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.14480">arXiv:2403.14480</a> <span> [<a href="https://arxiv.org/pdf/2403.14480">pdf</a>, <a href="https://arxiv.org/format/2403.14480">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202449527">10.1051/0004-6361/202449527 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Periodicity from X-ray sources within the inner Galactic disk </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mondal%2C+S">Samaresh Mondal</a>, <a href="/search/?searchtype=author&query=Ponti%2C+G">Gabriele Ponti</a>, <a href="/search/?searchtype=author&query=Bao%2C+T">Tong Bao</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">Frank Haberl</a>, <a href="/search/?searchtype=author&query=Campana%2C+S">Sergio Campana</a>, <a href="/search/?searchtype=author&query=Hailey%2C+C+J">Charles J. Hailey</a>, <a href="/search/?searchtype=author&query=Mandel%2C+S">Shifra Mandel</a>, <a href="/search/?searchtype=author&query=Mereghetti%2C+S">Sandro Mereghetti</a>, <a href="/search/?searchtype=author&query=Mori%2C+K">Kaya Mori</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Rea%2C+N">Nanda Rea</a>, <a href="/search/?searchtype=author&query=Sidoli%2C+L">Lara Sidoli</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.14480v1-abstract-short" style="display: inline;"> For many years, it has been claimed that the Galactic ridge X-ray emission at the Galactic Center (GC) is truly diffuse in nature. However, with the advancement of modern X-ray satellites, it has been found that most of the diffuse emission is actually comprised of thousands of previously unresolved X-ray point sources. Further, many studies suggest that a vast majority of these X-ray point source… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.14480v1-abstract-full').style.display = 'inline'; document.getElementById('2403.14480v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.14480v1-abstract-full" style="display: none;"> For many years, it has been claimed that the Galactic ridge X-ray emission at the Galactic Center (GC) is truly diffuse in nature. However, with the advancement of modern X-ray satellites, it has been found that most of the diffuse emission is actually comprised of thousands of previously unresolved X-ray point sources. Further, many studies suggest that a vast majority of these X-ray point sources are magnetic cataclysmic variables (mCVs) and active binaries. One unambiguous way to identify these mCVs and other sources is by detecting their X-ray periodicity. Therefore, we systematically searched for periodic X-ray sources in the inner Galactic disk, including the GC region. We have used data from our ongoing XMM-Newton Heritage survey of the inner Galactic disk ($350^{\circ}\lesssim l\lesssim+7^{\circ}$ and $-1^{\circ}\lesssim b\lesssim +1^{\circ}$) plus the XMM-Newton archival observations of the GC. We computed the Lomb-Scargle periodogram of the light curves for the periodicity search. We fitted the energy spectra of the sources using a simple power-law model plus three Gaussians at 6.4, 6.7, and 6.9 keV for the iron $K$ emission complex. We detected periodicity in 26 sources. For 14 of them, this is the first discovery of periodicity. For the other 12 sources, we found periods similar to those already known, indicating no significant period evolution. We also searched for the Gaia counterparts of the periodic sources to estimate their distances using the Gaia parallax. We found a likely Gaia counterpart for seven sources. We have classified the sources into four categories based on the periodicity, hardness ratio, and the equivalent width of Fe $K$ line emission. Of the 14 sources where we detect the periodicity for the first time, four are likely to be intermediate polars, five are likely to be polars, two are neutron star X-ray binaries, and three are of unknown nature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.14480v1-abstract-full').style.display = 'none'; document.getElementById('2403.14480v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 9 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A125 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.13048">arXiv:2403.13048</a> <span> [<a href="https://arxiv.org/pdf/2403.13048">pdf</a>, <a href="https://arxiv.org/format/2403.13048">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450035">10.1051/0004-6361/202450035 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Magnetic field morphology and evolution in the Central Molecular Zone and its effect on gas dynamics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Tress%2C+R+G">R. G. Tress</a>, <a href="/search/?searchtype=author&query=Sormani%2C+M+C">M. C. Sormani</a>, <a href="/search/?searchtype=author&query=Girichidis%2C+P">P. Girichidis</a>, <a href="/search/?searchtype=author&query=Glover%2C+S+C+O">S. C. O. Glover</a>, <a href="/search/?searchtype=author&query=Klessen%2C+R+S">R. S. Klessen</a>, <a href="/search/?searchtype=author&query=Smith%2C+R+J">R. J. Smith</a>, <a href="/search/?searchtype=author&query=Sobacchi%2C+E">E. Sobacchi</a>, <a href="/search/?searchtype=author&query=Armillotta%2C+L">L. Armillotta</a>, <a href="/search/?searchtype=author&query=Barnes%2C+A+T">A. T. Barnes</a>, <a href="/search/?searchtype=author&query=Battersby%2C+C">C. Battersby</a>, <a href="/search/?searchtype=author&query=Bogue%2C+K+R+J">K. R. J. Bogue</a>, <a href="/search/?searchtype=author&query=Brucy%2C+N">N. Brucy</a>, <a href="/search/?searchtype=author&query=Colzi%2C+L">L. Colzi</a>, <a href="/search/?searchtype=author&query=Federrath%2C+C">C. Federrath</a>, <a href="/search/?searchtype=author&query=Garc%C3%ADa%2C+P">P. Garc铆a</a>, <a href="/search/?searchtype=author&query=Ginsburg%2C+A">A. Ginsburg</a>, <a href="/search/?searchtype=author&query=G%C3%B6ller%2C+J">J. G枚ller</a>, <a href="/search/?searchtype=author&query=Hatchfield%2C+H+P">H P. Hatchfield</a>, <a href="/search/?searchtype=author&query=Henkel%2C+C">C. Henkel</a>, <a href="/search/?searchtype=author&query=Hennebelle%2C+P">P. Hennebelle</a>, <a href="/search/?searchtype=author&query=Henshaw%2C+J+D">J. D. Henshaw</a>, <a href="/search/?searchtype=author&query=Hirschmann%2C+M">M. Hirschmann</a>, <a href="/search/?searchtype=author&query=Hu%2C+Y">Y. Hu</a>, <a href="/search/?searchtype=author&query=Kauffmann%2C+J">J. Kauffmann</a>, <a href="/search/?searchtype=author&query=Kruijssen%2C+J+M+D">J. M. D. Kruijssen</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.13048v2-abstract-short" style="display: inline;"> The interstellar medium in the Milky Way's Central Molecular Zone (CMZ) is known to be strongly magnetised, but its large-scale morphology and impact on the gas dynamics are not well understood. We explore the impact and properties of magnetic fields in the CMZ using three-dimensional non-self gravitating magnetohydrodynamical simulations of gas flow in an external Milky Way barred potential. We f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13048v2-abstract-full').style.display = 'inline'; document.getElementById('2403.13048v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.13048v2-abstract-full" style="display: none;"> The interstellar medium in the Milky Way's Central Molecular Zone (CMZ) is known to be strongly magnetised, but its large-scale morphology and impact on the gas dynamics are not well understood. We explore the impact and properties of magnetic fields in the CMZ using three-dimensional non-self gravitating magnetohydrodynamical simulations of gas flow in an external Milky Way barred potential. We find that: (1) The magnetic field is conveniently decomposed into a regular time-averaged component and an irregular turbulent component. The regular component aligns well with the velocity vectors of the gas everywhere, including within the bar lanes. (2) The field geometry transitions from parallel to the Galactic plane near $z=0$ to poloidal away from the plane. (3) The magneto-rotational instability (MRI) causes an in-plane inflow of matter from the CMZ gas ring towards the central few parsecs of $0.01-0.1$ M$_\odot$ yr$^{-1}$ that is absent in the unmagnetised simulations. However, the magnetic fields have no significant effect on the larger-scale bar-driven inflow that brings the gas from the Galactic disc into the CMZ. (4) A combination of bar inflow and MRI-driven turbulence can sustain a turbulent vertical velocity dispersion of $蟽_z \simeq 5$ km s$^{-1}$ on scales of $20$ pc in the CMZ ring. The MRI alone sustains a velocity dispersion of $蟽_z \simeq 3$ km s$^{-1}$. Both these numbers are lower than the observed velocity dispersion of gas in the CMZ, suggesting that other processes such as stellar feedback are necessary to explain the observations. (5) Dynamo action driven by differential rotation and the MRI amplifies the magnetic fields in the CMZ ring until they saturate at a value that scales with the average local density as $B \simeq 102 (n/10^3 cm^{-3})^{0.33}$ $渭$G. Finally, we discuss the implications of our results within the observational context in the CMZ. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.13048v2-abstract-full').style.display = 'none'; document.getElementById('2403.13048v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A303 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.01662">arXiv:2402.01662</a> <span> [<a href="https://arxiv.org/pdf/2402.01662">pdf</a>, <a href="https://arxiv.org/ps/2402.01662">ps</a>, <a href="https://arxiv.org/format/2402.01662">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computers and Society">cs.CY</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Artificial Intelligence">cs.AI</span> </div> </div> <p class="title is-5 mathjax"> Generative Ghosts: Anticipating Benefits and Risks of AI Afterlives </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Morris%2C+M+R">Meredith Ringel Morris</a>, <a href="/search/?searchtype=author&query=Brubaker%2C+J+R">Jed R. Brubaker</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.01662v3-abstract-short" style="display: inline;"> As AI systems quickly improve in both breadth and depth of performance, they lend themselves to creating increasingly powerful and realistic agents, including the possibility of agents modeled on specific people. We anticipate that within our lifetimes it may become common practice for people to create a custom AI agent to interact with loved ones and/or the broader world after death; indeed, the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.01662v3-abstract-full').style.display = 'inline'; document.getElementById('2402.01662v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.01662v3-abstract-full" style="display: none;"> As AI systems quickly improve in both breadth and depth of performance, they lend themselves to creating increasingly powerful and realistic agents, including the possibility of agents modeled on specific people. We anticipate that within our lifetimes it may become common practice for people to create a custom AI agent to interact with loved ones and/or the broader world after death; indeed, the past year has seen a boom in startups purporting to offer such services. We call these "generative ghosts," since such agents will be capable of generating novel content rather than merely parroting content produced by their creator while living. In this paper, we reflect on the history of technologies for AI afterlives, including current early attempts by individual enthusiasts and by startup companies to create generative ghosts. We then introduce a novel design space detailing potential implementations of generative ghosts, and use this taxonomy to ground discussion of the practical and ethical implications of various approaches to designing generative ghosts, including potential positive and negative impacts on individuals and society. Based on these considerations, we lay out a research agenda for the AI and HCI research communities to better understand the risk/benefit landscape of this novel technology so as to ultimately empower people who wish to create and interact with AI afterlives to do so in a safe and beneficial manner. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.01662v3-abstract-full').style.display = 'none'; document.getElementById('2402.01662v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">version 3, updated to include new references and examples</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.12555">arXiv:2401.12555</a> <span> [<a href="https://arxiv.org/pdf/2401.12555">pdf</a>, <a href="https://arxiv.org/format/2401.12555">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> An Estimate of the Binary Star Fraction Among Young Stars at the Galactic Center: Possible Evidence of a Radial Dependence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gautam%2C+A+K">Abhimat K. Gautam</a>, <a href="/search/?searchtype=author&query=Do%2C+T">Tuan Do</a>, <a href="/search/?searchtype=author&query=Ghez%2C+A+M">Andrea M. Ghez</a>, <a href="/search/?searchtype=author&query=Chu%2C+D+S">Devin S. Chu</a>, <a href="/search/?searchtype=author&query=Hosek%2C+M+W">Matthew W. Hosek Jr.</a>, <a href="/search/?searchtype=author&query=Sakai%2C+S">Shoko Sakai</a>, <a href="/search/?searchtype=author&query=Naoz%2C+S">Smadar Naoz</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Ciurlo%2C+A">Anna Ciurlo</a>, <a href="/search/?searchtype=author&query=Haggard%2C+Z">Zoe Haggard</a>, <a href="/search/?searchtype=author&query=Lu%2C+J+R">Jessica R. Lu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.12555v2-abstract-short" style="display: inline;"> We present the first estimate of the intrinsic binary fraction of young stars across the central $\approx$ 0.4 pc surrounding the supermassive black hole (SMBH) at the Milky Way Galactic center (GC). This experiment searched for photometric variability in 102 young stars, using 119 nights of 10"-wide adaptive optics imaging observations taken at Keck Observatory over 16 years in the K'- and H-band… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.12555v2-abstract-full').style.display = 'inline'; document.getElementById('2401.12555v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.12555v2-abstract-full" style="display: none;"> We present the first estimate of the intrinsic binary fraction of young stars across the central $\approx$ 0.4 pc surrounding the supermassive black hole (SMBH) at the Milky Way Galactic center (GC). This experiment searched for photometric variability in 102 young stars, using 119 nights of 10"-wide adaptive optics imaging observations taken at Keck Observatory over 16 years in the K'- and H-bands. We photometrically detected three binary stars, all of which are situated more than 1" (0.04 pc) from the SMBH and one of which, S2-36, is newly reported here with spectroscopic confirmation. To convert the observed binary fraction into an estimate of the underlying binary fraction, we determined experiment sensitivity through detailed light curve simulations, incorporating photometric effects of eclipses, irradiation, and tidal distortion in binaries. The simulations assumed a population of young binaries, with stellar ages (4 Myr) and masses matched to the most probable values measured for the GC young star population and underlying binary system parameters similar to those of local massive stars. The detections and simulations imply young, massive stars in the GC have a stellar binary fraction $\geq$ 71% (68% confidence), or $\geq$ 42% (95% confidence). This inferred GC young star binary fraction is consistent with that typically seen in young stellar populations in the solar neighborhood. Furthermore, our measured binary fraction is significantly higher than that recently reported by Chu et al. (2023) based on RV measurements of young stars <~1" of the SMBH. Constrained with these two studies, the probability that the same underlying young binary fraction extends across the entire region is <1.4%. This tension provides support for a radial dependence of the binary star fraction and, therefore, for the dynamical predictions of binary merger and evaporation events close to the SMBH. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.12555v2-abstract-full').style.display = 'none'; document.getElementById('2401.12555v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">51 pages, 27 figures, 7 tables. Accepted for publication in The Astrophysical Journal. Abstract revised for final manuscript</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.05317">arXiv:2401.05317</a> <span> [<a href="https://arxiv.org/pdf/2401.05317">pdf</a>, <a href="https://arxiv.org/format/2401.05317">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad4462">10.3847/1538-4357/ad4462 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SOFIA/HAWC+ Far-Infrared Polarimetric Large-Area CMZ Exploration (FIREPLACE) Survey III: Full Survey Data Set </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Par%C3%A9%2C+D">Dylan Par茅</a>, <a href="/search/?searchtype=author&query=Butterfield%2C+N+O">Natalie O. Butterfield</a>, <a href="/search/?searchtype=author&query=Chuss%2C+D+T">David T. Chuss</a>, <a href="/search/?searchtype=author&query=Guerra%2C+J+A">Jordan A. Guerra</a>, <a href="/search/?searchtype=author&query=Iuliano%2C+J+I">Jeffrey I. Iuliano</a>, <a href="/search/?searchtype=author&query=Karpovich%2C+K">Kaitlyn Karpovich</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Wollack%2C+E">Edward Wollack</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.05317v3-abstract-short" style="display: inline;"> We present the second data release (DR2) of the Far-Infrared Polarimetric Large-Area CMZ Exploration (FIREPLACE) survey. This survey utilized the Stratospheric Observatory for Infrared Astronomy (SOFIA) High-resolution Airborne Wideband Camera plus (HAWC+) instrument at 214 $渭$m (E-band) to observe dust polarization throughout the Central Molecular Zone (CMZ) of the Milky Way. DR2 consists of obse… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.05317v3-abstract-full').style.display = 'inline'; document.getElementById('2401.05317v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.05317v3-abstract-full" style="display: none;"> We present the second data release (DR2) of the Far-Infrared Polarimetric Large-Area CMZ Exploration (FIREPLACE) survey. This survey utilized the Stratospheric Observatory for Infrared Astronomy (SOFIA) High-resolution Airborne Wideband Camera plus (HAWC+) instrument at 214 $渭$m (E-band) to observe dust polarization throughout the Central Molecular Zone (CMZ) of the Milky Way. DR2 consists of observations that were obtained in 2022 covering the region of the CMZ extending roughly from the Brick to the Sgr C molecular clouds (corresponding to a roughly 1$^{\circ}$ $\times$ 0.75$^{\circ}$ region of the sky). We combine DR2 with the first FIREPLACE data release to obtain full coverage of the CMZ (a 1.5$^{\circ}$ $\times$0.75$^{\circ}$ region of the sky). After applying total and polarized intensity significance cuts on the full FIREPLACE data set we obtain $\rm\sim$65,000 Nyquist-sampled polarization pseudovectors. The distribution of polarization pseudovectors confirms a bimodal distribution in the CMZ magnetic field orientations, recovering field components that are oriented predominantly parallel or perpendicular to the Galactic plane. These magnetic field orientations indicate possible connections between the previously observed parallel and perpendicular distributions. We also inspect the magnetic fields toward a set of prominent CMZ molecular clouds (the Brick, Three Little Pigs, 50 km s$\rm^{-1}$, Circum-nuclear Disk, CO 0.02-0.02, 20 km s$\rm^{-1}$, and Sgr C), revealing spatially varying magnetic fields that generally trace the morphologies of the clouds. We find evidence that compression from stellar winds and shear from tidal forces are prominent mechanisms influencing the structure of the magnetic fields observed within the clouds. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.05317v3-abstract-full').style.display = 'none'; document.getElementById('2401.05317v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35 pages, 23 figures, 3 tables. Article is accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 969 (2024) 150 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.01983">arXiv:2401.01983</a> <span> [<a href="https://arxiv.org/pdf/2401.01983">pdf</a>, <a href="https://arxiv.org/format/2401.01983">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> SOFIA/HAWC+ Far-Infrared Polarimetric Large Area CMZ Exploration (FIREPLACE) II: Detection of a Magnetized Dust Ring in the Galactic Center </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Butterfield%2C+N+O">Natalie O. Butterfield</a>, <a href="/search/?searchtype=author&query=Guerra%2C+J+A">Jordan A. Guerra</a>, <a href="/search/?searchtype=author&query=Chuss%2C+D+T">David T. Chuss</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Pare%2C+D">Dylan Pare</a>, <a href="/search/?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</a>, <a href="/search/?searchtype=author&query=Costa%2C+A+H">Allison H. Costa</a>, <a href="/search/?searchtype=author&query=Hankins%2C+M+J">Matthew J. Hankins</a>, <a href="/search/?searchtype=author&query=Staguhn%2C+J">Johannes Staguhn</a>, <a href="/search/?searchtype=author&query=Zweibel%2C+E">Ellen Zweibel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.01983v2-abstract-short" style="display: inline;"> We present the detection of a magnetized dust ring (M0.8-0.2) in the Central Molecular Zone (CMZ) of the Galactic Center. The results presented in this paper utilize the first data release (DR1) of the Far-Infrared Polarimetric Large Area CMZ Exploration (FIREPLACE) survey (i.e., FIREPLACE I; Butterfield et al. 2023). The FIREPLACE survey is a 214 $渭$m polarimetic survey of the Galactic Center usi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.01983v2-abstract-full').style.display = 'inline'; document.getElementById('2401.01983v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.01983v2-abstract-full" style="display: none;"> We present the detection of a magnetized dust ring (M0.8-0.2) in the Central Molecular Zone (CMZ) of the Galactic Center. The results presented in this paper utilize the first data release (DR1) of the Far-Infrared Polarimetric Large Area CMZ Exploration (FIREPLACE) survey (i.e., FIREPLACE I; Butterfield et al. 2023). The FIREPLACE survey is a 214 $渭$m polarimetic survey of the Galactic Center using the SOFIA/HAWC+ telescope. The M0.8-0.2 ring is a region of gas and dust that has a circular morphology with a central depression. The dust polarization in the M0.8-0.2 ring implies a curved magnetic field that traces the ring-like structure of the cloud. We posit an interpretation in which an expanding shell compresses and concentrates the ambient gas and magnetic field. We argue that this compression results in the strengthening of the magnetic field, as we infer from the observations toward the interior of the ring. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.01983v2-abstract-full').style.display = 'none'; document.getElementById('2401.01983v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.01532">arXiv:2312.01532</a> <span> [<a href="https://arxiv.org/pdf/2312.01532">pdf</a>, <a href="https://arxiv.org/format/2312.01532">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Human-Computer Interaction">cs.HC</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computation and Language">cs.CL</span> </div> </div> <p class="title is-5 mathjax"> Using Large Language Models to Accelerate Communication for Users with Severe Motor Impairments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Cai%2C+S">Shanqing Cai</a>, <a href="/search/?searchtype=author&query=Venugopalan%2C+S">Subhashini Venugopalan</a>, <a href="/search/?searchtype=author&query=Seaver%2C+K">Katie Seaver</a>, <a href="/search/?searchtype=author&query=Xiao%2C+X">Xiang Xiao</a>, <a href="/search/?searchtype=author&query=Tomanek%2C+K">Katrin Tomanek</a>, <a href="/search/?searchtype=author&query=Jalasutram%2C+S">Sri Jalasutram</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Meredith Ringel Morris</a>, <a href="/search/?searchtype=author&query=Kane%2C+S">Shaun Kane</a>, <a href="/search/?searchtype=author&query=Narayanan%2C+A">Ajit Narayanan</a>, <a href="/search/?searchtype=author&query=MacDonald%2C+R+L">Robert L. MacDonald</a>, <a href="/search/?searchtype=author&query=Kornman%2C+E">Emily Kornman</a>, <a href="/search/?searchtype=author&query=Vance%2C+D">Daniel Vance</a>, <a href="/search/?searchtype=author&query=Casey%2C+B">Blair Casey</a>, <a href="/search/?searchtype=author&query=Gleason%2C+S+M">Steve M. Gleason</a>, <a href="/search/?searchtype=author&query=Nelson%2C+P+Q">Philip Q. Nelson</a>, <a href="/search/?searchtype=author&query=Brenner%2C+M+P">Michael P. Brenner</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.01532v1-abstract-short" style="display: inline;"> Finding ways to accelerate text input for individuals with profound motor impairments has been a long-standing area of research. Closing the speed gap for augmentative and alternative communication (AAC) devices such as eye-tracking keyboards is important for improving the quality of life for such individuals. Recent advances in neural networks of natural language pose new opportunities for re-thi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.01532v1-abstract-full').style.display = 'inline'; document.getElementById('2312.01532v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.01532v1-abstract-full" style="display: none;"> Finding ways to accelerate text input for individuals with profound motor impairments has been a long-standing area of research. Closing the speed gap for augmentative and alternative communication (AAC) devices such as eye-tracking keyboards is important for improving the quality of life for such individuals. Recent advances in neural networks of natural language pose new opportunities for re-thinking strategies and user interfaces for enhanced text-entry for AAC users. In this paper, we present SpeakFaster, consisting of large language models (LLMs) and a co-designed user interface for text entry in a highly-abbreviated form, allowing saving 57% more motor actions than traditional predictive keyboards in offline simulation. A pilot study with 19 non-AAC participants typing on a mobile device by hand demonstrated gains in motor savings in line with the offline simulation, while introducing relatively small effects on overall typing speed. Lab and field testing on two eye-gaze typing users with amyotrophic lateral sclerosis (ALS) demonstrated text-entry rates 29-60% faster than traditional baselines, due to significant saving of expensive keystrokes achieved through phrase and word predictions from context-aware LLMs. These findings provide a strong foundation for further exploration of substantially-accelerated text communication for motor-impaired users and demonstrate a direction for applying LLMs to text-based user interfaces. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.01532v1-abstract-full').style.display = 'none'; document.getElementById('2312.01532v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.16394">arXiv:2311.16394</a> <span> [<a href="https://arxiv.org/pdf/2311.16394">pdf</a>, <a href="https://arxiv.org/format/2311.16394">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> High-Resolution, Mid-Infrared Color Temperature Mapping of the Central 10 Arcseconds of the Galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Dinh%2C+C+K">Cuc K. Dinh</a>, <a href="/search/?searchtype=author&query=Cuirlo%2C+A">Anna Cuirlo</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Sch%C3%B6del%2C+R">Rainer Sch枚del</a>, <a href="/search/?searchtype=author&query=Ghez%2C+A">Andrea Ghez</a>, <a href="/search/?searchtype=author&query=Do%2C+T">Tuan Do</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.16394v1-abstract-short" style="display: inline;"> The neighborhood of the Galactic black hole boasts a plethora of extended interstellar gas and dust features as well as populations of compact (unresolved, or marginally resolved) features such as the G objects. Most are well manifested in the infrared. To disentangle and characterize the infrared structure of extended features and identify compact sources, we used 3.8~$渭$m (L' filter) data from t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.16394v1-abstract-full').style.display = 'inline'; document.getElementById('2311.16394v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.16394v1-abstract-full" style="display: none;"> The neighborhood of the Galactic black hole boasts a plethora of extended interstellar gas and dust features as well as populations of compact (unresolved, or marginally resolved) features such as the G objects. Most are well manifested in the infrared. To disentangle and characterize the infrared structure of extended features and identify compact sources, we used 3.8~$渭$m (L' filter) data from the NIRC2 imager at the Keck Observatory and 8.6~$渭$m (PAH1 filter) data from the VISIR imager at the Very Large Telescope (VLT) to produce the highest-resolution mid-IR color-temperature map of the inner half-parsec of the Galactic Center to date. From this map, we compile a catalog of features that stand out from their background. In particular, we identify 33 compact sources that stand out against the local background temperature, 11 of which are newly identified and are candidates for being members of the G objects population. Additionally, we resolve and newly characterize the morphology of several known extended features. These results prepare the way for ongoing and future JWST studies that have access to a greater range of mid-infrared wavelengths, and thus will allow for refined estimation of the trends of dust temperatures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.16394v1-abstract-full').style.display = 'none'; document.getElementById('2311.16394v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 14 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.15948">arXiv:2311.15948</a> <span> [<a href="https://arxiv.org/pdf/2311.15948">pdf</a>, <a href="https://arxiv.org/format/2311.15948">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> A First Look with JWST Aperture Masking Interferometry (AMI): Resolving Circumstellar Dust around the Wolf-Rayet Binary WR 137 beyond the Rayleigh Limit </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lau%2C+R+M">Ryan M. Lau</a>, <a href="/search/?searchtype=author&query=Hankins%2C+M+J">Matthew J. Hankins</a>, <a href="/search/?searchtype=author&query=Sanchez-Bermudez%2C+J">Joel Sanchez-Bermudez</a>, <a href="/search/?searchtype=author&query=Thatte%2C+D">Deepashri Thatte</a>, <a href="/search/?searchtype=author&query=Soulain%2C+A">Anthony Soulain</a>, <a href="/search/?searchtype=author&query=Cooper%2C+R+A">Rachel A. Cooper</a>, <a href="/search/?searchtype=author&query=Sivaramakrishnan%2C+A">Anand Sivaramakrishnan</a>, <a href="/search/?searchtype=author&query=Corcoran%2C+M+F">Michael F. Corcoran</a>, <a href="/search/?searchtype=author&query=Greenbaum%2C+A+Z">Alexandra Z. Greenbaum</a>, <a href="/search/?searchtype=author&query=Gull%2C+T+R">Theodore R. Gull</a>, <a href="/search/?searchtype=author&query=Han%2C+Y">Yinuo Han</a>, <a href="/search/?searchtype=author&query=Jones%2C+O+C">Olivia C. Jones</a>, <a href="/search/?searchtype=author&query=Madura%2C+T">Thomas Madura</a>, <a href="/search/?searchtype=author&query=Moffat%2C+A+F+J">Anthony F. J. Moffat</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Onaka%2C+T">Takashi Onaka</a>, <a href="/search/?searchtype=author&query=Russell%2C+C+M+P">Christopher M. P. Russell</a>, <a href="/search/?searchtype=author&query=Richardson%2C+N+D">Noel D. Richardson</a>, <a href="/search/?searchtype=author&query=Smith%2C+N">Nathan Smith</a>, <a href="/search/?searchtype=author&query=Tuthill%2C+P">Peter Tuthill</a>, <a href="/search/?searchtype=author&query=Volk%2C+K">Kevin Volk</a>, <a href="/search/?searchtype=author&query=Weigelt%2C+G">Gerd Weigelt</a>, <a href="/search/?searchtype=author&query=Williams%2C+P+M">Peredur M. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.15948v2-abstract-short" style="display: inline;"> We present infrared aperture masking interferometry (AMI) observations of newly formed dust from the colliding winds of the massive binary system Wolf-Rayet (WR) 137 with JWST using the Near Infrared Imager and Slitless Spectrograph (NIRISS). NIRISS AMI observations of WR 137 and a point-spread-function calibrator star, HD~228337, were taken using the F380M and F480M filters in 2022 July and Augus… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.15948v2-abstract-full').style.display = 'inline'; document.getElementById('2311.15948v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.15948v2-abstract-full" style="display: none;"> We present infrared aperture masking interferometry (AMI) observations of newly formed dust from the colliding winds of the massive binary system Wolf-Rayet (WR) 137 with JWST using the Near Infrared Imager and Slitless Spectrograph (NIRISS). NIRISS AMI observations of WR 137 and a point-spread-function calibrator star, HD~228337, were taken using the F380M and F480M filters in 2022 July and August as part of the Director's Discretionary Early Release Science (DD-ERS) program 1349. Interferometric observables (squared visibilities and closure phases) from the WR 137 "interferogram" were extracted and calibrated using three independent software tools: ImPlaneIA, AMICAL, and SAMpip. The analysis of the calibrated observables yielded consistent values except for slightly discrepant closure phases measured by ImPlaneIA. Based on all three sets of calibrated observables, images were reconstructed using three independent software tools: BSMEM, IRBis, and SQUEEZE. All reconstructed image combinations generated consistent images in both F380M and F480M filters. The reconstructed images of WR 137 reveal a bright central core with a $\sim300$ mas linear filament extending to the northwest. A geometric colliding-wind model with dust production constrained to the orbital plane of the binary system and enhanced as the system approaches periapsis provided a general agreement with the interferometric observables and reconstructed images. Based on a colliding-wind dust condensation analysis, we suggest that dust formation within the orbital plane of WR 137 is induced by enhanced equatorial mass-loss from the rapidly rotating O9 companion star, whose axis of rotation is aligned with that of the orbit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.15948v2-abstract-full').style.display = 'none'; document.getElementById('2311.15948v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 8 figures, Accepted for publication in ApJ. Updated plotting error in Fig. 2</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.02462">arXiv:2311.02462</a> <span> [<a href="https://arxiv.org/pdf/2311.02462">pdf</a>, <a href="https://arxiv.org/ps/2311.02462">ps</a>, <a href="https://arxiv.org/format/2311.02462">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Artificial Intelligence">cs.AI</span> </div> </div> <p class="title is-5 mathjax"> Levels of AGI for Operationalizing Progress on the Path to AGI </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Morris%2C+M+R">Meredith Ringel Morris</a>, <a href="/search/?searchtype=author&query=Sohl-dickstein%2C+J">Jascha Sohl-dickstein</a>, <a href="/search/?searchtype=author&query=Fiedel%2C+N">Noah Fiedel</a>, <a href="/search/?searchtype=author&query=Warkentin%2C+T">Tris Warkentin</a>, <a href="/search/?searchtype=author&query=Dafoe%2C+A">Allan Dafoe</a>, <a href="/search/?searchtype=author&query=Faust%2C+A">Aleksandra Faust</a>, <a href="/search/?searchtype=author&query=Farabet%2C+C">Clement Farabet</a>, <a href="/search/?searchtype=author&query=Legg%2C+S">Shane Legg</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.02462v4-abstract-short" style="display: inline;"> We propose a framework for classifying the capabilities and behavior of Artificial General Intelligence (AGI) models and their precursors. This framework introduces levels of AGI performance, generality, and autonomy, providing a common language to compare models, assess risks, and measure progress along the path to AGI. To develop our framework, we analyze existing definitions of AGI, and distill… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.02462v4-abstract-full').style.display = 'inline'; document.getElementById('2311.02462v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.02462v4-abstract-full" style="display: none;"> We propose a framework for classifying the capabilities and behavior of Artificial General Intelligence (AGI) models and their precursors. This framework introduces levels of AGI performance, generality, and autonomy, providing a common language to compare models, assess risks, and measure progress along the path to AGI. To develop our framework, we analyze existing definitions of AGI, and distill six principles that a useful ontology for AGI should satisfy. With these principles in mind, we propose "Levels of AGI" based on depth (performance) and breadth (generality) of capabilities, and reflect on how current systems fit into this ontology. We discuss the challenging requirements for future benchmarks that quantify the behavior and capabilities of AGI models against these levels. Finally, we discuss how these levels of AGI interact with deployment considerations such as autonomy and risk, and emphasize the importance of carefully selecting Human-AI Interaction paradigms for responsible and safe deployment of highly capable AI systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.02462v4-abstract-full').style.display = 'none'; document.getElementById('2311.02462v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">version 4 - Position Paper accepted to ICML 2024. Note that due to ICML position paper titling format requirements, the title has changed slightly from that of the original arXiv pre-print. The original pre-print title was "Levels of AGI: Operationalizing Progress on the Path to AGI" but the official published title for ICML 2024 is "Levels of AGI for Operationalizing Progress on the Path to AGI"</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proceedings of ICML 2024 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.00710">arXiv:2311.00710</a> <span> [<a href="https://arxiv.org/pdf/2311.00710">pdf</a>, <a href="https://arxiv.org/format/2311.00710">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Human-Computer Interaction">cs.HC</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Artificial Intelligence">cs.AI</span> </div> </div> <p class="title is-5 mathjax"> Interactive AI Alignment: Specification, Process, and Evaluation Alignment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Terry%2C+M">Michael Terry</a>, <a href="/search/?searchtype=author&query=Kulkarni%2C+C">Chinmay Kulkarni</a>, <a href="/search/?searchtype=author&query=Wattenberg%2C+M">Martin Wattenberg</a>, <a href="/search/?searchtype=author&query=Dixon%2C+L">Lucas Dixon</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Meredith Ringel Morris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.00710v2-abstract-short" style="display: inline;"> Modern AI enables a high-level, declarative form of interaction: Users describe the intended outcome they wish an AI to produce, but do not actually create the outcome themselves. In contrast, in traditional user interfaces, users invoke specific operations to create the desired outcome. This paper revisits the basic input-output interaction cycle in light of this declarative style of interaction,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00710v2-abstract-full').style.display = 'inline'; document.getElementById('2311.00710v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.00710v2-abstract-full" style="display: none;"> Modern AI enables a high-level, declarative form of interaction: Users describe the intended outcome they wish an AI to produce, but do not actually create the outcome themselves. In contrast, in traditional user interfaces, users invoke specific operations to create the desired outcome. This paper revisits the basic input-output interaction cycle in light of this declarative style of interaction, and connects concepts in AI alignment to define three objectives for interactive alignment of AI: specification alignment (aligning on what to do), process alignment (aligning on how to do it), and evaluation alignment (assisting users in verifying and understanding what was produced). Using existing systems as examples, we show how these user-centered views of AI alignment can be used descriptively, prescriptively, and as an evaluative aid. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00710v2-abstract-full').style.display = 'none'; document.getElementById('2311.00710v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.02892">arXiv:2310.02892</a> <span> [<a href="https://arxiv.org/pdf/2310.02892">pdf</a>, <a href="https://arxiv.org/format/2310.02892">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ad3248">10.3847/2041-8213/ad3248 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-rays from a Central "Exhaust Vent" of the Galactic Center Chimney </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mackey%2C+S+C">Scott C. Mackey</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Ponti%2C+G">Gabriele Ponti</a>, <a href="/search/?searchtype=author&query=Anastasopoulou%2C+K">Konstantina Anastasopoulou</a>, <a href="/search/?searchtype=author&query=Mondal%2C+S">Samaresh Mondal</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.02892v1-abstract-short" style="display: inline;"> Using deep archival observations from the Chandra X-ray Observatory, we present an analysis of linear X-ray-emitting features located within the southern portion of the Galactic center chimney, and oriented orthogonal to the Galactic plane, centered at coordinates l = 0.08 deg, b = -1.42 deg. The surface brightness and hardness ratio patterns are suggestive of a cylindrical morphology which may ha… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.02892v1-abstract-full').style.display = 'inline'; document.getElementById('2310.02892v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.02892v1-abstract-full" style="display: none;"> Using deep archival observations from the Chandra X-ray Observatory, we present an analysis of linear X-ray-emitting features located within the southern portion of the Galactic center chimney, and oriented orthogonal to the Galactic plane, centered at coordinates l = 0.08 deg, b = -1.42 deg. The surface brightness and hardness ratio patterns are suggestive of a cylindrical morphology which may have been produced by a plasma outflow channel extending from the Galactic center. Our fits of the feature's spectra favor a complex two-component model consisting of thermal and recombining plasma components, possibly a sign of shock compression or heating of the interstellar medium by outflowing material. Assuming a recombining plasma scenario, we further estimate the cooling timescale of this plasma to be on the order of a few hundred to thousands of years, leading us to speculate that a sequence of accretion events onto the Galactic Black Hole may be a plausible quasi-continuous energy source to sustain the observed morphology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.02892v1-abstract-full').style.display = 'none'; document.getElementById('2310.02892v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 6 figures. Submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.05265">arXiv:2309.05265</a> <span> [<a href="https://arxiv.org/pdf/2309.05265">pdf</a>, <a href="https://arxiv.org/format/2309.05265">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347227">10.1051/0004-6361/202347227 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ionized regions in the central arcsecond of NGC 1068. YJHK spatially resolved spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Vermot%2C+P">P. Vermot</a>, <a href="/search/?searchtype=author&query=Barna%2C+B">B. Barna</a>, <a href="/search/?searchtype=author&query=Ehlerov%C3%A1%2C+S">S. Ehlerov谩</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">M. R. Morris</a>, <a href="/search/?searchtype=author&query=Palous%2C+J">J. Palous</a>, <a href="/search/?searchtype=author&query=W%C3%BCnsch%2C+R">R. W眉nsch</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.05265v1-abstract-short" style="display: inline;"> Context. Several bright emission line regions have been observed in the central 100 parsecs of the active galaxy NGC 1068. Aims. We aim to determine the properties and ionization mechanism of three regions of NGC 1068: the nucleus (B) and two clouds located at 0.3" and 0.7" north of it (C and D). Methods. We combined SPHERE (0.95 - 1.65 um) and SINFONI (1.5 - 2.45 um) spectra for the three regions… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.05265v1-abstract-full').style.display = 'inline'; document.getElementById('2309.05265v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.05265v1-abstract-full" style="display: none;"> Context. Several bright emission line regions have been observed in the central 100 parsecs of the active galaxy NGC 1068. Aims. We aim to determine the properties and ionization mechanism of three regions of NGC 1068: the nucleus (B) and two clouds located at 0.3" and 0.7" north of it (C and D). Methods. We combined SPHERE (0.95 - 1.65 um) and SINFONI (1.5 - 2.45 um) spectra for the three regions B, C, and D. We compared these spectra to several CLOUDY photoionization models and to the MAPPINGS III Library of Fast Radiative Shock Models. Results. The emission line spectra of the three regions are almost identical to each other and contribute to most of the emission line flux in the nuclear region. The emitting media contain multiple phases, the most luminous of which have temperatures ranging from 104.8 K to 106 K. Central photoionization models can reproduce some features of the spectra, but the fast radiative shock model provides the best fit to the data. Conclusions. The similarity between the three regions indicates that they belong to the same class of objects. Based on our comparisons, we conclude that they are shock regions located where the jet of the active galactic nucleus impacts massive molecular clouds. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.05265v1-abstract-full').style.display = 'none'; document.getElementById('2309.05265v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">A&A, Forthcoming article, accepted for publication</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.09749">arXiv:2308.09749</a> <span> [<a href="https://arxiv.org/pdf/2308.09749">pdf</a>, <a href="https://arxiv.org/format/2308.09749">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Near-Infrared Flux Distribution of Sgr A* from 2005-2022: Evidence for an Enhanced Accretion Episode in 2019 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Weldon%2C+G+C">Grant C. Weldon</a>, <a href="/search/?searchtype=author&query=Do%2C+T">Tuan Do</a>, <a href="/search/?searchtype=author&query=Witzel%2C+G">Gunther Witzel</a>, <a href="/search/?searchtype=author&query=Ghez%2C+A+M">Andrea M. Ghez</a>, <a href="/search/?searchtype=author&query=Gautam%2C+A+K">Abhimat K. Gautam</a>, <a href="/search/?searchtype=author&query=Becklin%2C+E+E">Eric E. Becklin</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Martinez%2C+G+D">Gregory D. Martinez</a>, <a href="/search/?searchtype=author&query=Sakai%2C+S">Shoko Sakai</a>, <a href="/search/?searchtype=author&query=Lu%2C+J+R">Jessica R. Lu</a>, <a href="/search/?searchtype=author&query=Matthews%2C+K">Keith Matthews</a>, <a href="/search/?searchtype=author&query=Hosek%2C+M+W">Matthew W. Hosek Jr.</a>, <a href="/search/?searchtype=author&query=Haggard%2C+Z">Zo毛 Haggard</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.09749v1-abstract-short" style="display: inline;"> Sgr A* is the variable electromagnetic source associated with accretion onto the Galactic center supermassive black hole. While the near-infrared (NIR) variability of Sgr A* was shown to be consistent over two decades, unprecedented activity in 2019 challenges existing statistical models. We investigate the origin of this activity by re-calibrating and re-analyzing all of our Keck Observatory Sgr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.09749v1-abstract-full').style.display = 'inline'; document.getElementById('2308.09749v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.09749v1-abstract-full" style="display: none;"> Sgr A* is the variable electromagnetic source associated with accretion onto the Galactic center supermassive black hole. While the near-infrared (NIR) variability of Sgr A* was shown to be consistent over two decades, unprecedented activity in 2019 challenges existing statistical models. We investigate the origin of this activity by re-calibrating and re-analyzing all of our Keck Observatory Sgr A* imaging observations from 2005-2022. We present light curves from 69 observation epochs using the NIRC2 imager at 2.12 $渭$m with laser guide star adaptive optics. These observations reveal that the mean luminosity of Sgr A* increased by a factor of $\sim$3 in 2019, and the 2019 light curves had higher variance than in all time periods we examined. We find that the 2020-2022 flux distribution is statistically consistent with the historical sample and model predictions, but with fewer bright measurements above 0.6 mJy at the $\sim$2$蟽$ level. Since 2019, we have observed a maximum $K_s$ (2.2 $渭$m) flux of 0.9 mJy, compared to the highest pre-2019 flux of 2.0 mJy and highest 2019 flux of 5.6 mJy. Our results suggest that the 2019 activity was caused by a temporary accretion increase onto Sgr A*, possibly due to delayed accretion of tidally-stripped gas from the gaseous object G2 in 2014. We also examine faint Sgr A* fluxes over a long time baseline to search for a quasi-steady quiescent state. We find that Sgr A* displays flux variations over a factor of $\sim$500, with no evidence for a quiescent state in the NIR. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.09749v1-abstract-full').style.display = 'none'; document.getElementById('2308.09749v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted to ApJ Letters, 26 pages, 15 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.01681">arXiv:2306.01681</a> <span> [<a href="https://arxiv.org/pdf/2306.01681">pdf</a>, <a href="https://arxiv.org/format/2306.01681">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad12b9">10.3847/1538-4357/ad12b9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SOFIA/HAWC+ Far-InfraRed Polarimetric Large Area CMZ Exploration (FIREPLACE) Survey I: General Results from the Pilot Program </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Butterfield%2C+N+O">Natalie O. Butterfield</a>, <a href="/search/?searchtype=author&query=Chuss%2C+D+T">David T. Chuss</a>, <a href="/search/?searchtype=author&query=Guerra%2C+J+A">Jordan A. Guerra</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Pare%2C+D">Dylan Pare</a>, <a href="/search/?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</a>, <a href="/search/?searchtype=author&query=Dowell%2C+C+D">C. Darren Dowell</a>, <a href="/search/?searchtype=author&query=Hankins%2C+M+J">Matthew J. Hankins</a>, <a href="/search/?searchtype=author&query=Karpovich%2C+K">Kaitlyn Karpovich</a>, <a href="/search/?searchtype=author&query=Siah%2C+J">Javad Siah</a>, <a href="/search/?searchtype=author&query=Staguhn%2C+J">Johannes Staguhn</a>, <a href="/search/?searchtype=author&query=Zweibel%2C+E">Ellen Zweibel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.01681v2-abstract-short" style="display: inline;"> We present the first data release (DR1) of the Far-Infrared Polarimetric Large Area CMZ Exploration (FIREPLACE) survey. The survey was taken using the 214-micron band of the HAWC+ instrument with the SOFIA telescope (19.6$'$ resolution; 0.7 pc). In this first data release we present dust polarization observations covering a ~0.5$掳$ region of the Galactic Center's Central Molecular Zone (CMZ), appr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.01681v2-abstract-full').style.display = 'inline'; document.getElementById('2306.01681v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.01681v2-abstract-full" style="display: none;"> We present the first data release (DR1) of the Far-Infrared Polarimetric Large Area CMZ Exploration (FIREPLACE) survey. The survey was taken using the 214-micron band of the HAWC+ instrument with the SOFIA telescope (19.6$'$ resolution; 0.7 pc). In this first data release we present dust polarization observations covering a ~0.5$掳$ region of the Galactic Center's Central Molecular Zone (CMZ), approximately centered on the Sgr B2 complex. We detect ~25,000 Nyquist-sampled polarization pseudovectors, after applying the standard SOFIA cuts for minimum signal-to-noise in fractional polarization and total intensity of 3 and 200, respectively. Analysis of the magnetic field orientation suggests a bimodal distribution in the field direction. This bimodal distribution shows enhancements in the distribution of field directions for orientations parallel and perpendicular to the Galactic plane, which is suggestive of a CMZ magnetic field configuration with polodial and torodial components. Furthermore, a detailed analysis of individual clouds included in our survey (i.e., Sgr B2, Sgr B2-NW, Sgr B2-Halo, Sgr B1, and Clouds-E/F) shows these clouds have fractional polarization values of 1--10% at 214-micron, with most of the emission having values $<$5%. A few of these clouds (i.e., Sgr B2, Clouds-E/F) show relatively low fractional polarization values toward the cores of the cloud, with higher fractional polarization values toward the less dense periphery. We also observe higher fractional polarization towards compact HII regions which could indicate an enhancement in the grain alignment in the dust surrounding these sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.01681v2-abstract-full').style.display = 'none'; document.getElementById('2306.01681v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.19032">arXiv:2305.19032</a> <span> [<a href="https://arxiv.org/pdf/2305.19032">pdf</a>, <a href="https://arxiv.org/format/2305.19032">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245627">10.1051/0004-6361/202245627 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A 3D model for the stellar populations in the nuclei of NGC 1433,NGC 1566, and NGC 1808 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Vermot%2C+P">P. Vermot</a>, <a href="/search/?searchtype=author&query=Palou%C5%A1%2C+J">J. Palou拧</a>, <a href="/search/?searchtype=author&query=Barna%2C+B">B. Barna</a>, <a href="/search/?searchtype=author&query=Ehlerov%C3%A1%2C+S">S. Ehlerov谩</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">M. R. Morris</a>, <a href="/search/?searchtype=author&query=W%C3%BCnsch%2C+R">R. W眉nsch</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.19032v1-abstract-short" style="display: inline;"> Aims. We aim to characterize the properties of the stellar populations in the central few hundred parsecs of nearby galactic nuclei; specifically their age, mass, and 3D geometry. Methods. We use spatially resolved spectroscopic observations of NGC 1433, NGC 1566, and NGC 1808 obtained with SINFONI to constrain a 3D model composed of a spherically symmetric nuclear star cluster (NSC) and an extend… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.19032v1-abstract-full').style.display = 'inline'; document.getElementById('2305.19032v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.19032v1-abstract-full" style="display: none;"> Aims. We aim to characterize the properties of the stellar populations in the central few hundred parsecs of nearby galactic nuclei; specifically their age, mass, and 3D geometry. Methods. We use spatially resolved spectroscopic observations of NGC 1433, NGC 1566, and NGC 1808 obtained with SINFONI to constrain a 3D model composed of a spherically symmetric nuclear star cluster (NSC) and an extended thick stellar disk. We computed UV to mid-infrared single stellar population (UMISSP) spectra to determine the age of the stellar populations and construct synthetic observations for our model. To overcome degeneracies between key parameters, we simultaneously fit the spatially resolved line-of-sight velocity, line-of-sight-velocity-dispersion, low-spectral-resolution NIR continuum, and high-spectral-resolution CO absorption features for each pixel. Results. For the three objects, we derive the age and mass of the young and old stellar populations in the NSC and surrounding disk, as well as their 3D geometry: radius for the NSC; thickness, inclination, and position angle for the disk. These results are consistent with published independent measurements when available. Conclusions. The proposed method allows us to derive a consistent 3D model of the stellar populations in nearby galactic centers solely based on a near-infrared IFU observation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.19032v1-abstract-full').style.display = 'none'; document.getElementById('2305.19032v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, A135 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.09038">arXiv:2305.09038</a> <span> [<a href="https://arxiv.org/pdf/2305.09038">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Human-Computer Interaction">cs.HC</span> </div> </div> <p class="title is-5 mathjax"> Characterizing Image Accessibility on Wikipedia across Languages </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kreiss%2C+E">Elisa Kreiss</a>, <a href="/search/?searchtype=author&query=Srinivasan%2C+K">Krishna Srinivasan</a>, <a href="/search/?searchtype=author&query=Piccardi%2C+T">Tiziano Piccardi</a>, <a href="/search/?searchtype=author&query=Hermosillo%2C+J+A">Jesus Adolfo Hermosillo</a>, <a href="/search/?searchtype=author&query=Bennett%2C+C">Cynthia Bennett</a>, <a href="/search/?searchtype=author&query=Bernstein%2C+M+S">Michael S. Bernstein</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Meredith Ringel Morris</a>, <a href="/search/?searchtype=author&query=Potts%2C+C">Christopher Potts</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.09038v1-abstract-short" style="display: inline;"> We make a first attempt to characterize image accessibility on Wikipedia across languages, present new experimental results that can inform efforts to assess description quality, and offer some strategies to improve Wikipedia's image accessibility. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.09038v1-abstract-full" style="display: none;"> We make a first attempt to characterize image accessibility on Wikipedia across languages, present new experimental results that can inform efforts to assess description quality, and offer some strategies to improve Wikipedia's image accessibility. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.09038v1-abstract-full').style.display = 'none'; document.getElementById('2305.09038v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Presented at Wiki Workshop 2023</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.11296">arXiv:2304.11296</a> <span> [<a href="https://arxiv.org/pdf/2304.11296">pdf</a>, <a href="https://arxiv.org/format/2304.11296">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad1215">10.1093/mnras/stad1215 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hydrodynamic Evolution of Sgr A East: The Imprint of A Supernova Remnant in the Galactic Center </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Zhang%2C+M">Mengfei Zhang</a>, <a href="/search/?searchtype=author&query=Li%2C+Z">Zhiyuan Li</a>, <a href="/search/?searchtype=author&query=Morris%2C+Z+H+M+R">Ziqian Hua Mark R. Morris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.11296v1-abstract-short" style="display: inline;"> We perform three-dimensional numerical simulations to study the hydrodynamic evolution of Sgr A East, the only known supernova remnant (SNR) in the center of our Galaxy, to infer its debated progenitor SN type and its potential impact on the Galactic center environment. Three sets of simulations are performed, each of which represents a represent a certain type of SN explosion (SN Iax, SN Ia or co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.11296v1-abstract-full').style.display = 'inline'; document.getElementById('2304.11296v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.11296v1-abstract-full" style="display: none;"> We perform three-dimensional numerical simulations to study the hydrodynamic evolution of Sgr A East, the only known supernova remnant (SNR) in the center of our Galaxy, to infer its debated progenitor SN type and its potential impact on the Galactic center environment. Three sets of simulations are performed, each of which represents a represent a certain type of SN explosion (SN Iax, SN Ia or core-collapse SN) expanding against a nuclear outflow of hot gas driven by massive stars, whose thermodynamical properties have been well established by previous work and fixed in the simulations. All three simulations can simultaneously roughly reproduce the extent of Sgr A East and the position and morphology of an arc-shaped thermal X-ray feature, known as the "ridge". Confirming previous work, our simulations show that the ridge is the manifestation of a strong collision between the expanding SN ejecta and the nuclear outflow. The simulation of the core-collapse SN, with an assumed explosion energy of 5x10^50 erg and an ejecta mass of 10 M_sun, can well match the X-ray flux of the ridge, whereas the simulations of the SN Iax and SN Ia explosions underpredict its X-ray emission, due to a smaller ejecta mass. All three simulations constrain the age of Sgr A East to be <1500 yr and predict that the ridge should fade out over the next few hundred years. We address the implications of these results for our understanding of the Galactic center environment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.11296v1-abstract-full').style.display = 'none'; document.getElementById('2304.11296v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 18 figures. Accepted for publication on MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.10547">arXiv:2304.10547</a> <span> [<a href="https://arxiv.org/pdf/2304.10547">pdf</a>, <a href="https://arxiv.org/ps/2304.10547">ps</a>, <a href="https://arxiv.org/format/2304.10547">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Artificial Intelligence">cs.AI</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Human-Computer Interaction">cs.HC</span> </div> </div> <p class="title is-5 mathjax"> The Design Space of Generative Models </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Morris%2C+M+R">Meredith Ringel Morris</a>, <a href="/search/?searchtype=author&query=Cai%2C+C+J">Carrie J. Cai</a>, <a href="/search/?searchtype=author&query=Holbrook%2C+J">Jess Holbrook</a>, <a href="/search/?searchtype=author&query=Kulkarni%2C+C">Chinmay Kulkarni</a>, <a href="/search/?searchtype=author&query=Terry%2C+M">Michael Terry</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.10547v1-abstract-short" style="display: inline;"> Card et al.'s classic paper "The Design Space of Input Devices" established the value of design spaces as a tool for HCI analysis and invention. We posit that developing design spaces for emerging pre-trained, generative AI models is necessary for supporting their integration into human-centered systems and practices. We explore what it means to develop an AI model design space by proposing two de… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.10547v1-abstract-full').style.display = 'inline'; document.getElementById('2304.10547v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.10547v1-abstract-full" style="display: none;"> Card et al.'s classic paper "The Design Space of Input Devices" established the value of design spaces as a tool for HCI analysis and invention. We posit that developing design spaces for emerging pre-trained, generative AI models is necessary for supporting their integration into human-centered systems and practices. We explore what it means to develop an AI model design space by proposing two design spaces relating to generative AI models: the first considers how HCI can impact generative models (i.e., interfaces for models) and the second considers how generative models can impact HCI (i.e., models as an HCI prototyping material). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.10547v1-abstract-full').style.display = 'none'; document.getElementById('2304.10547v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> NeurIps 2022 Human-Centered AI Workshop </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.03442">arXiv:2304.03442</a> <span> [<a href="https://arxiv.org/pdf/2304.03442">pdf</a>, <a href="https://arxiv.org/format/2304.03442">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Human-Computer Interaction">cs.HC</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Artificial Intelligence">cs.AI</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> </div> </div> <p class="title is-5 mathjax"> Generative Agents: Interactive Simulacra of Human Behavior </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Park%2C+J+S">Joon Sung Park</a>, <a href="/search/?searchtype=author&query=O%27Brien%2C+J+C">Joseph C. O'Brien</a>, <a href="/search/?searchtype=author&query=Cai%2C+C+J">Carrie J. Cai</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Meredith Ringel Morris</a>, <a href="/search/?searchtype=author&query=Liang%2C+P">Percy Liang</a>, <a href="/search/?searchtype=author&query=Bernstein%2C+M+S">Michael S. Bernstein</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.03442v2-abstract-short" style="display: inline;"> Believable proxies of human behavior can empower interactive applications ranging from immersive environments to rehearsal spaces for interpersonal communication to prototyping tools. In this paper, we introduce generative agents--computational software agents that simulate believable human behavior. Generative agents wake up, cook breakfast, and head to work; artists paint, while authors write; t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.03442v2-abstract-full').style.display = 'inline'; document.getElementById('2304.03442v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.03442v2-abstract-full" style="display: none;"> Believable proxies of human behavior can empower interactive applications ranging from immersive environments to rehearsal spaces for interpersonal communication to prototyping tools. In this paper, we introduce generative agents--computational software agents that simulate believable human behavior. Generative agents wake up, cook breakfast, and head to work; artists paint, while authors write; they form opinions, notice each other, and initiate conversations; they remember and reflect on days past as they plan the next day. To enable generative agents, we describe an architecture that extends a large language model to store a complete record of the agent's experiences using natural language, synthesize those memories over time into higher-level reflections, and retrieve them dynamically to plan behavior. We instantiate generative agents to populate an interactive sandbox environment inspired by The Sims, where end users can interact with a small town of twenty five agents using natural language. In an evaluation, these generative agents produce believable individual and emergent social behaviors: for example, starting with only a single user-specified notion that one agent wants to throw a Valentine's Day party, the agents autonomously spread invitations to the party over the next two days, make new acquaintances, ask each other out on dates to the party, and coordinate to show up for the party together at the right time. We demonstrate through ablation that the components of our agent architecture--observation, planning, and reflection--each contribute critically to the believability of agent behavior. By fusing large language models with computational, interactive agents, this work introduces architectural and interaction patterns for enabling believable simulations of human behavior. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.03442v2-abstract-full').style.display = 'none'; document.getElementById('2304.03442v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.01420">arXiv:2304.01420</a> <span> [<a href="https://arxiv.org/pdf/2304.01420">pdf</a>, <a href="https://arxiv.org/ps/2304.01420">ps</a>, <a href="https://arxiv.org/format/2304.01420">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computers and Society">cs.CY</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Artificial Intelligence">cs.AI</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Human-Computer Interaction">cs.HC</span> </div> </div> <p class="title is-5 mathjax"> Scientists' Perspectives on the Potential for Generative AI in their Fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Morris%2C+M+R">Meredith Ringel Morris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.01420v1-abstract-short" style="display: inline;"> Generative AI models, including large language models and multimodal models that include text and other media, are on the cusp of transforming many aspects of modern life, including entertainment, education, civic life, the arts, and a range of professions. There is potential for Generative AI to have a substantive impact on the methods and pace of discovery for a range of scientific disciplines.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.01420v1-abstract-full').style.display = 'inline'; document.getElementById('2304.01420v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.01420v1-abstract-full" style="display: none;"> Generative AI models, including large language models and multimodal models that include text and other media, are on the cusp of transforming many aspects of modern life, including entertainment, education, civic life, the arts, and a range of professions. There is potential for Generative AI to have a substantive impact on the methods and pace of discovery for a range of scientific disciplines. We interviewed twenty scientists from a range of fields (including the physical, life, and social sciences) to gain insight into whether or how Generative AI technologies might add value to the practice of their respective disciplines, including not only ways in which AI might accelerate scientific discovery (i.e., research), but also other aspects of their profession, including the education of future scholars and the communication of scientific findings. In addition to identifying opportunities for Generative AI to augment scientists' current practices, we also asked participants to reflect on concerns about AI. These findings can help guide the responsible development of models and interfaces for scientific education, inquiry, and communication. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.01420v1-abstract-full').style.display = 'none'; document.getElementById('2304.01420v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.00920">arXiv:2304.00920</a> <span> [<a href="https://arxiv.org/pdf/2304.00920">pdf</a>, <a href="https://arxiv.org/format/2304.00920">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad1025">10.1093/mnras/stad1025 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Chandra X-ray Measurement of Gas-phase Heavy Element Abundances in the Central Parsec of the Galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Hua%2C+Z">Ziqian Hua</a>, <a href="/search/?searchtype=author&query=Li%2C+Z">Zhiyuan Li</a>, <a href="/search/?searchtype=author&query=Zhang%2C+M">Mengfei Zhang</a>, <a href="/search/?searchtype=author&query=Chen%2C+Z">Zhuo Chen</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.00920v1-abstract-short" style="display: inline;"> Elemental abundances are key to our understanding of star formation and evolution in the Galactic center. Previous work on this topic has been based on infrared (IR) observations, but X-ray observations have the potential of constraining the abundance of heavy elements, mainly through their K-shell emission lines. Using 5.7 Ms Chandra observations, we provide the first abundance measurement of Si,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.00920v1-abstract-full').style.display = 'inline'; document.getElementById('2304.00920v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.00920v1-abstract-full" style="display: none;"> Elemental abundances are key to our understanding of star formation and evolution in the Galactic center. Previous work on this topic has been based on infrared (IR) observations, but X-ray observations have the potential of constraining the abundance of heavy elements, mainly through their K-shell emission lines. Using 5.7 Ms Chandra observations, we provide the first abundance measurement of Si, S, Ar, Ca and Fe, in four prominent diffuse X-ray features located in the central parsec of the Galaxy, which are the manifestation of shock-heated hot gas. A two-temperature, non-equilibrium ionization spectral model is employed to derive the abundances of these five elements. In this procedure, a degeneracy is introduced due to uncertainties in the composition of light elements, in particular, H, C and N. Assuming that the hot gas is H-depleted but C- and N-enriched, as would be expected for a standard scenario in which the hot gas is dominated by Wolf-Rayet star winds, the spectral fit finds a generally subsolar abundance for the heavy elements. If, instead, the light elements had a solar-like abundance, the heavy elements have a fitted abundance of $\sim$1--2 solar. The $伪$/Fe abundance ratio, on the other hand, is mostly supersolar and insensitive to the exact composition of the light elements. These results are robust against potential biases due to either a moderate spectral S/N or the presence of non-thermal components. Implications of the measured abundances for the Galactic center environment are addressed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.00920v1-abstract-full').style.display = 'none'; document.getElementById('2304.00920v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 6 figures, Accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.02431">arXiv:2302.02431</a> <span> [<a href="https://arxiv.org/pdf/2302.02431">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1002/9781394163724">10.1002/9781394163724 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Galactic Black Hole </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.02431v2-abstract-short" style="display: inline;"> The black hole at the center of our Milky Way Galaxy -- the Galactic Black Hole, or GBH -- is a rather modest representative of its class. With a mass of 4 x 10^6 solar masses, it is well over a thousand times less massive than the most extreme supermassive black holes known to be powering the most luminous quasars. Furthermore, the Galactic Black Hole has a remarkably dim accretion flow, and its… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.02431v2-abstract-full').style.display = 'inline'; document.getElementById('2302.02431v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.02431v2-abstract-full" style="display: none;"> The black hole at the center of our Milky Way Galaxy -- the Galactic Black Hole, or GBH -- is a rather modest representative of its class. With a mass of 4 x 10^6 solar masses, it is well over a thousand times less massive than the most extreme supermassive black holes known to be powering the most luminous quasars. Furthermore, the Galactic Black Hole has a remarkably dim accretion flow, and its luminous energy output is overwhelmed by the dense cluster of bright stars and red giants that surround it, except at radio wavelengths. However, the proximity of the GBH compensates for its restrained activity; being over 100 times closer than the next nearest supermassive black hole in a galactic nucleus, it offers us an unparalleled opportunity to observe its behavior in detail. Consequently, far more observational attention has been paid to the GBH and its entourage of stars and gas than to any other single object outside the solar system. This review covers the history of our recognition of the GBH, its presently known physical characteristics, the manifestations of its current and past activity, and the prospects for refining our knowledge with future research. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.02431v2-abstract-full').style.display = 'none'; document.getElementById('2302.02431v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 12 figures, 210 references. Slightly revised and updated version of Chapter 2 of the volume, "Active Galactic Nuclei", 2022, coordinated by Fran莽oise Combes, ISTE/Wiley,</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.02040">arXiv:2302.02040</a> <span> [<a href="https://arxiv.org/pdf/2302.02040">pdf</a>, <a href="https://arxiv.org/format/2302.02040">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acb939">10.3847/1538-4357/acb939 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Stellar Populations in the Central 0.5 pc of Our Galaxy III: The Dynamical Sub-structures </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Jia%2C+S">Siyao Jia</a>, <a href="/search/?searchtype=author&query=Xu%2C+N">Ningyuan Xu</a>, <a href="/search/?searchtype=author&query=Lu%2C+J+R">Jessica R. Lu</a>, <a href="/search/?searchtype=author&query=Chu%2C+D+S">D. S Chu</a>, <a href="/search/?searchtype=author&query=O%27Neil%2C+K+K">K. Kosmo O'Neil</a>, <a href="/search/?searchtype=author&query=Drechsler%2C+W+B">W. B. Drechsler</a>, <a href="/search/?searchtype=author&query=Hosek%2C+M+W">M. W. Hosek Jr.</a>, <a href="/search/?searchtype=author&query=Sakai%2C+S">S. Sakai</a>, <a href="/search/?searchtype=author&query=Do%2C+T">T. Do</a>, <a href="/search/?searchtype=author&query=Ciurlo%2C+A">A. Ciurlo</a>, <a href="/search/?searchtype=author&query=Gautam%2C+A+K">A. K. Gautam</a>, <a href="/search/?searchtype=author&query=Ghez%2C+A+M">A. M. Ghez</a>, <a href="/search/?searchtype=author&query=Becklin%2C+E">E. Becklin</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">M. R. Morris</a>, <a href="/search/?searchtype=author&query=Bentley%2C+R+O">R. O. Bentley</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.02040v1-abstract-short" style="display: inline;"> We measure the 3D kinematic structures of the young stars within the central 0.5 parsec of our Galactic Center using the 10 m telescopes of the W.~M.~Keck Observatory over a time span of 25 years. Using high-precision measurements of positions on the sky, and proper motions and radial velocities from new observations and the literature, we constrain the orbital parameters for each young star. Our… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.02040v1-abstract-full').style.display = 'inline'; document.getElementById('2302.02040v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.02040v1-abstract-full" style="display: none;"> We measure the 3D kinematic structures of the young stars within the central 0.5 parsec of our Galactic Center using the 10 m telescopes of the W.~M.~Keck Observatory over a time span of 25 years. Using high-precision measurements of positions on the sky, and proper motions and radial velocities from new observations and the literature, we constrain the orbital parameters for each young star. Our results show two statistically significant sub-structures: a clockwise stellar disk with 18 candidate stars, as has been proposed before, but with an improved disk membership; a second, almost edge-on plane of 10 candidate stars oriented East-West on the sky that includes at least one IRS 13 star. We estimate the eccentricity distribution of each sub-structure and find that the clockwise disk has <$e$> = 0.39 and the edge-on plane has <$e$> = 0.68. We also perform simulations of each disk/plane with incompleteness and spatially-variable extinction to search for asymmetry. Our results show that the clockwise stellar disk is consistent with a uniform azimuthal distribution within the disk. The edge-on plane has an asymmetry that cannot be explained by variable extinction or incompleteness in the field. The orientation, asymmetric stellar distribution, and high eccentricity of the edge-on plane members suggest that this structure may be a stream associated with the IRS 13 group. The complex dynamical structure of the young nuclear cluster indicates that the star formation process involved complex gas structures and dynamics and is inconsistent with a single massive gaseous disk. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.02040v1-abstract-full').style.display = 'none'; document.getElementById('2302.02040v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">41 pages, 26 figures, 13 tables, 2 appendices. Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.13469">arXiv:2301.13469</a> <span> [<a href="https://arxiv.org/pdf/2301.13469">pdf</a>, <a href="https://arxiv.org/ps/2301.13469">ps</a>, <a href="https://arxiv.org/format/2301.13469">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.18716/kups/64624">10.18716/kups/64624 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Star Formation in the Extreme Galactic Center Environment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.13469v1-abstract-short" style="display: inline;"> Copious star formation occurs in the dense Central Molecular Zone (CMZ) of our Galaxy, but at a much smaller rate than occurs in a comparable mass of molecular gas in the Galactic disk. The combination of large turbulent velocity dispersions, a relatively strong magnetic field, and a strong tidal field all contribute to inhibiting star formation (SF) in different ways in different CMZ locations. N… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.13469v1-abstract-full').style.display = 'inline'; document.getElementById('2301.13469v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.13469v1-abstract-full" style="display: none;"> Copious star formation occurs in the dense Central Molecular Zone (CMZ) of our Galaxy, but at a much smaller rate than occurs in a comparable mass of molecular gas in the Galactic disk. The combination of large turbulent velocity dispersions, a relatively strong magnetic field, and a strong tidal field all contribute to inhibiting star formation (SF) in different ways in different CMZ locations. Nonetheless, there are spectacular displays of recent and ongoing SF in the CMZ, including massive young stellar clusters, sites of abundant SF in progress, and numerous spots of protostellar or YSO activity. The presence of giant molecular clouds in the CMZ that are almost entirely devoid of SF indicates that SF requires a trigger that is not present everywhere. The dominant provocation of SF is likely to be cloud compression, either by large-scale shocks or by orbital motion of clouds into a region of enhanced tidal compression and/or enhanced external pressure. Recent hypotheses for where and how SF takes place in the CMZ are constrained by the recent orbital determinations of the massive Arches and Quintuplet clusters. Star formation in the central parsec is subject to a very different set of physical conditions, and is less well understood, but is important for the co-evolution of the central black hole and the nuclear star cluster. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.13469v1-abstract-full').style.display = 'none'; document.getElementById('2301.13469v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, Proceedings of the 7th Chile-Cologne-Bonn-Symposium: Physics and Chemistry of Star Formation</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.11001">arXiv:2301.11001</a> <span> [<a href="https://arxiv.org/pdf/2301.11001">pdf</a>, <a href="https://arxiv.org/format/2301.11001">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245553">10.1051/0004-6361/202245553 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of periodicities in two highly variable intermediate polars towards the Galactic Center </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mondal%2C+S">Samaresh Mondal</a>, <a href="/search/?searchtype=author&query=Ponti%2C+G">Gabriele Ponti</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">Frank Haberl</a>, <a href="/search/?searchtype=author&query=Mori%2C+K">Kaya Mori</a>, <a href="/search/?searchtype=author&query=Rea%2C+N">Nanda Rea</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Campana%2C+S">Sergio Campana</a>, <a href="/search/?searchtype=author&query=Anastasopoulou%2C+K">Konstantina Anastasopoulou</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.11001v1-abstract-short" style="display: inline;"> We discovered Fe $K_伪$ complex emission and pulsation in two highly variable sources (4XMM J174917.7--283329, 4XMM J174954.6--294336). The equivalent widths of 6.4 and 6.7 keV lines of 4XMM J174917.7--283329 are $99^{+84}_{-72}$ and $220^{+160}_{-140}$ eV, respectively. The continuum is fitted by a partially absorbed apec model with plasma temperature of $kT=13^{+10}_{-2}$ keV. The inferred mass o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.11001v1-abstract-full').style.display = 'inline'; document.getElementById('2301.11001v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.11001v1-abstract-full" style="display: none;"> We discovered Fe $K_伪$ complex emission and pulsation in two highly variable sources (4XMM J174917.7--283329, 4XMM J174954.6--294336). The equivalent widths of 6.4 and 6.7 keV lines of 4XMM J174917.7--283329 are $99^{+84}_{-72}$ and $220^{+160}_{-140}$ eV, respectively. The continuum is fitted by a partially absorbed apec model with plasma temperature of $kT=13^{+10}_{-2}$ keV. The inferred mass of the white dwarf (WD) is $0.9^{+0.3}_{-0.2}\ M_{\odot}$. We detected pulsations with a period of $1212\pm3$ s and a pulsed fraction of $26\pm6\%$. The light curves of 4XMM J174954.6--294336 display asymmetric eclipse and dipping behaviour. To date, this is only the second intermediate polar (IP) that shows a total eclipse in X-rays. The spectrum of the sources is characterized by a power-law model with photon index $螕=0.4\pm0.2$. The equivalent widths of the 6.4 keV and 6.7 keV iron lines are $171^{+99}_{-79}$ and $136^{+89}_{-81}$ eV, respectively. The continuum is described by emission from optically thin plasma with a temperature of $kT\sim35$ keV. The inferred mass of the WD is $1.1^{+0.2}_{-0.3}\ M_{\odot}$. We discovered coherent pulsations from the source with a period of $1002\pm2$ s. The pulsed fraction is $66\pm15\%$. The measured spin period, hard photon index, and equivalent width of the fluorescent Fe $K_伪$ line in both sources are consistent with the values found in IP. While 4XMM J174954.6--294336 was already previously classified as an IP, we also suggest 4XMM J174917.7--283329 as a new IP. The X-ray eclipses in 4XMM J174954.6--294336 are most likely caused by a low-mass companion star obscuring the central X-ray source. The asymmetry in the eclipse is likely caused by a thick bulge that intercepts the line of sight during the ingress phase but not during the egress phase located behind the WD along the line of sight. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.11001v1-abstract-full').style.display = 'none'; document.getElementById('2301.11001v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, six figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 671, A120 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.07735">arXiv:2301.07735</a> <span> [<a href="https://arxiv.org/pdf/2301.07735">pdf</a>, <a href="https://arxiv.org/format/2301.07735">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acdb6f">10.3847/1538-4357/acdb6f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Inner 2 pc of Sagittarius A*: Simulations of the Circumnuclear Disk and Multiphase Gas Accretion in the Galactic Center </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Solanki%2C+S">Siddhant Solanki</a>, <a href="/search/?searchtype=author&query=Ressler%2C+S+M">Sean M. Ressler</a>, <a href="/search/?searchtype=author&query=Murchikova%2C+L">Lena Murchikova</a>, <a href="/search/?searchtype=author&query=Stone%2C+J+M">James M. Stone</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.07735v1-abstract-short" style="display: inline;"> We present hydrodynamic simulations of the inner few parsecs of the Milky Way's Galactic Center that, for the first time, combine a realistic treatment of stellar winds and the circumnuclear disk as they interact with the gravitational potential of the nuclear star cluster and Sagittarius~A*. We observe a complex interaction of the stellar winds with the inner edge of the circumnuclear disk, which… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07735v1-abstract-full').style.display = 'inline'; document.getElementById('2301.07735v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.07735v1-abstract-full" style="display: none;"> We present hydrodynamic simulations of the inner few parsecs of the Milky Way's Galactic Center that, for the first time, combine a realistic treatment of stellar winds and the circumnuclear disk as they interact with the gravitational potential of the nuclear star cluster and Sagittarius~A*. We observe a complex interaction of the stellar winds with the inner edge of the circumnuclear disk, which leads to the growth of instabilities, induced accretion of cool gas from the inner edge of the disk, and the eventual formation of a small accretion disk of $\sim 10^4-10^5$ K within $r \sim 0.1$ pc. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.07735v1-abstract-full').style.display = 'none'; document.getElementById('2301.07735v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 16 figures, (Submitted to ApJ)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.06562">arXiv:2301.06562</a> <span> [<a href="https://arxiv.org/pdf/2301.06562">pdf</a>, <a href="https://arxiv.org/format/2301.06562">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acb344">10.3847/1538-4357/acb344 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Swansong of the Galactic Center Source X7: An Extreme Example of Tidal Evolution near the Supermassive Black Hole </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ciurlo%2C+A">Anna Ciurlo</a>, <a href="/search/?searchtype=author&query=Campbell%2C+R+D">Randall D. Campbell</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Do%2C+T">Tuan Do</a>, <a href="/search/?searchtype=author&query=Ghez%2C+A+M">Andrea M. Ghez</a>, <a href="/search/?searchtype=author&query=Becklin%2C+E+E">Eric E. Becklin</a>, <a href="/search/?searchtype=author&query=Bentley%2C+R+O">Rory O. Bentley</a>, <a href="/search/?searchtype=author&query=Chu%2C+D+S">Devin S. Chu</a>, <a href="/search/?searchtype=author&query=Gautam%2C+A+K">Abhimat K. Gautam</a>, <a href="/search/?searchtype=author&query=Gursahani%2C+Y+A">Yash A. Gursahani</a>, <a href="/search/?searchtype=author&query=Hees%2C+A">Aurelien Hees</a>, <a href="/search/?searchtype=author&query=O%27Neil%2C+K+K">Kelly Kosmo O'Neil</a>, <a href="/search/?searchtype=author&query=Lu%2C+J+R">Jessica R. Lu</a>, <a href="/search/?searchtype=author&query=Martinez%2C+G+D">Gregory D. Martinez</a>, <a href="/search/?searchtype=author&query=Naoz%2C+S">Smadar Naoz</a>, <a href="/search/?searchtype=author&query=Sakai%2C+S">Shoko Sakai</a>, <a href="/search/?searchtype=author&query=Schoedel%2C+R">Rainer Schoedel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.06562v1-abstract-short" style="display: inline;"> We present two decades of new high-angular-resolution near-infrared data from the W. M. Keck Observatory that reveal extreme evolution in X7, an elongated dust and gas feature, presently located half an arcsecond from the Galactic Center supermassive black hole. With both spectro-imaging observations of Br-纬 line-emission and Lp (3.8 渭m) imaging data, we provide the first estimate of its orbital p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.06562v1-abstract-full').style.display = 'inline'; document.getElementById('2301.06562v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.06562v1-abstract-full" style="display: none;"> We present two decades of new high-angular-resolution near-infrared data from the W. M. Keck Observatory that reveal extreme evolution in X7, an elongated dust and gas feature, presently located half an arcsecond from the Galactic Center supermassive black hole. With both spectro-imaging observations of Br-纬 line-emission and Lp (3.8 渭m) imaging data, we provide the first estimate of its orbital parameters and quantitative characterization of the evolution of its morphology and mass. We find that the leading edge of X7 appears to be on a mildly eccentric (e~0.3), relatively short-period (170 years) orbit and is headed towards periapse passage, estimated to occur in ~2036. Furthermore, our kinematic measurements rule out the earlier suggestion that X7 is associated with the stellar source S0-73 or with any other point source that has overlapped with X7 during our monitoring period. Over the course of our observations, X7 has (1) become more elongated, with a current length-to-width ratio of 9, (2) maintained a very consistent long-axis orientation (position angle of 50 deg), (3) inverted its radial velocity differential from tip to tail from -50 to +80 km/sec, and (4) sustained its total brightness (12.8 Lp magnitudes at the leading edge) and color temperature (425 K), which suggest a constant mass of ~50 MEarth. We present a simple model showing that these results are compatible with the expected effect of tidal forces exerted on it by the central black hole and we propose that X7 is the gas and dust recently ejected from a grazing collision in a binary system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.06562v1-abstract-full').style.display = 'none'; document.getElementById('2301.06562v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted by ApJ, 20 pages, 16 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.04164">arXiv:2301.04164</a> <span> [<a href="https://arxiv.org/pdf/2301.04164">pdf</a>, <a href="https://arxiv.org/format/2301.04164">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202245001">10.1051/0004-6361/202245001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Study of the excess Fe XXV line emission in the central degrees of the Galactic centre using XMM-Newton data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Anastasopoulou%2C+K">K. Anastasopoulou</a>, <a href="/search/?searchtype=author&query=Ponti%2C+G">G. Ponti</a>, <a href="/search/?searchtype=author&query=Sormani%2C+M+C">M. C. Sormani</a>, <a href="/search/?searchtype=author&query=Locatelli%2C+N">N. Locatelli</a>, <a href="/search/?searchtype=author&query=Haberl%2C+F">F. Haberl</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">M. R. Morris</a>, <a href="/search/?searchtype=author&query=Churazov%2C+E+M">E. M. Churazov</a>, <a href="/search/?searchtype=author&query=Sch%C3%B6del%2C+R">R. Sch枚del</a>, <a href="/search/?searchtype=author&query=Maitra%2C+C">C. Maitra</a>, <a href="/search/?searchtype=author&query=Campana%2C+S">S. Campana</a>, <a href="/search/?searchtype=author&query=Di+Teodoro%2C+E+M">E. M. Di Teodoro</a>, <a href="/search/?searchtype=author&query=Jin%2C+C">C. Jin</a>, <a href="/search/?searchtype=author&query=Khabibullin%2C+I">I. Khabibullin</a>, <a href="/search/?searchtype=author&query=Mondal%2C+S">S. Mondal</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Zhang%2C+Y">Y. Zhang</a>, <a href="/search/?searchtype=author&query=Zheng%2C+X">X. Zheng</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.04164v1-abstract-short" style="display: inline;"> The diffuse Fe XXV (6.7 keV) line emission observed in the Galactic ridge is widely accepted to be produced by a superposition of a large number of unresolved X-ray point sources. In the very central degrees of our Galaxy, however, the existence of an extremely hot ($\sim$7 keV) diffuse plasma is still under debate. In this work we measure the Fe XXV line emission using all available XMM-Newton ob… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04164v1-abstract-full').style.display = 'inline'; document.getElementById('2301.04164v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.04164v1-abstract-full" style="display: none;"> The diffuse Fe XXV (6.7 keV) line emission observed in the Galactic ridge is widely accepted to be produced by a superposition of a large number of unresolved X-ray point sources. In the very central degrees of our Galaxy, however, the existence of an extremely hot ($\sim$7 keV) diffuse plasma is still under debate. In this work we measure the Fe XXV line emission using all available XMM-Newton observations of the Galactic centre (GC) and inner disc ($-10^{\circ}$$<\ell<10^{\circ}$, $-2^{\circ}<b<2^{\circ}$). We use recent stellar mass distribution models to estimate the amount of X-ray emission originating from unresolved point sources, and find that within a region of $\ell=\pm1^{\circ}$ and $b=\pm0.25^\circ$ the 6.7 keV emission is 1.3 to 1.5 times in excess of what is expected from unresolved point sources. The excess emission is enhanced towards regions where known supernova remnants are located, suggesting that at least a part of this emission is due to genuine diffuse very hot plasma. If the entire excess is due to very hot plasma, an energy injection rate of at least $\sim6\times10^{40}$ erg s$^{-1}$ is required, which cannot be provided by the measured supernova explosion rate or past Sgr A$^{*}$ activity alone. However, we find that almost the entire excess we observe can be explained by assuming GC stellar populations with iron abundances $\sim$1.9 times higher than those in the bar/bulge, a value that can be reproduced by fitting diffuse X-ray spectra from the corresponding regions. Even in this case, a leftover X-ray excess is concentrated within $\ell=\pm0.3^{\circ}$ and $b=\pm0.15^\circ$, corresponding to a thermal energy of $\sim2\times10^{52}$ erg, which can be reproduced by the estimated supernova explosion rate in the GC. Finally we discuss a possible connection to the observed GC Fermi-LAT excess. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.04164v1-abstract-full').style.display = 'none'; document.getElementById('2301.04164v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 11 figures, 7 tables, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 671, A55 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.01397">arXiv:2212.01397</a> <span> [<a href="https://arxiv.org/pdf/2212.01397">pdf</a>, <a href="https://arxiv.org/format/2212.01397">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aca8ad">10.3847/1538-4357/aca8ad <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Star Formation History of the Milky Way's Nuclear Star Cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Chen%2C+Z">Zhuo Chen</a>, <a href="/search/?searchtype=author&query=Do%2C+T">Tuan Do</a>, <a href="/search/?searchtype=author&query=Ghez%2C+A+M">Andrea M. Ghez</a>, <a href="/search/?searchtype=author&query=Hosek%2C+M">Matthew Hosek Jr.</a>, <a href="/search/?searchtype=author&query=Feldmeier-Krause%2C+A">Anja Feldmeier-Krause</a>, <a href="/search/?searchtype=author&query=Chu%2C+D">Devin Chu</a>, <a href="/search/?searchtype=author&query=Bentley%2C+R">Rory Bentley</a>, <a href="/search/?searchtype=author&query=Lu%2C+J+R">Jessica R. Lu</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2212.01397v1-abstract-short" style="display: inline;"> We report the first star formation history study of the Milky Way's nuclear star cluster (NSC) that includes observational constraints from a large sample of stellar metallicity measurements. These metallicity measurements were obtained from recent surveys from Gemini and VLT of 770 late-type stars within the central 1.5 pc. These metallicity measurements, along with photometry and spectroscopical… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.01397v1-abstract-full').style.display = 'inline'; document.getElementById('2212.01397v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.01397v1-abstract-full" style="display: none;"> We report the first star formation history study of the Milky Way's nuclear star cluster (NSC) that includes observational constraints from a large sample of stellar metallicity measurements. These metallicity measurements were obtained from recent surveys from Gemini and VLT of 770 late-type stars within the central 1.5 pc. These metallicity measurements, along with photometry and spectroscopically derived temperatures, are forward modeled with a Bayesian inference approach. Including metallicity measurements improves the overall fit quality, as the low-temperature red giants that were previously difficult to constrain are now accounted for, and the best fit favors a two-component model. The dominant component contains 93%$\pm$3% of the mass, is metal-rich ($\overline{[M/H]}\sim$0.45), and has an age of 5$^{+3}_{-2}$ Gyr, which is $\sim$3 Gyr younger than earlier studies with fixed (solar) metallicity; this younger age challenges co-evolutionary models in which the NSC and supermassive black holes formed simultaneously at early times. The minor population component has low metallicity ($\overline{[M/H]}\sim$ -1.1) and contains $\sim$7% of the stellar mass. The age of the minor component is uncertain (0.1 - 5 Gyr old). Using the estimated parameters, we infer the following NSC stellar remnant population (with $\sim$18% uncertainty): 1.5$\times$10$^5$ neutron stars, 2.5$\times$10$^5$ stellar mass black holes (BHs) and 2.2$\times$10$^4$ BH-BH binaries. These predictions result in 2-4 times fewer neutron stars compared to earlier predictions that assume solar metallicity, introducing a possible new path to understand the so-called "missing pulsar problem". Finally, we present updated predictions for the BH-BH merger rates (0.01-3 Gpc$^{-3}$yr$^{-1}$). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.01397v1-abstract-full').style.display = 'none'; document.getElementById('2212.01397v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">37 pages, 23 figures, Accepted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.04232">arXiv:2211.04232</a> <span> [<a href="https://arxiv.org/pdf/2211.04232">pdf</a>, <a href="https://arxiv.org/format/2211.04232">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202244682">10.1051/0004-6361/202244682 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> How to create Sgr A East: Where did the supernova explode? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ehlerov%C3%A1%2C+S">S. Ehlerov谩</a>, <a href="/search/?searchtype=author&query=Palou%C5%A1%2C+J">J. Palou拧</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">M. R. Morris</a>, <a href="/search/?searchtype=author&query=unsch%2C+R+W">R. W\" unsch</a>, <a href="/search/?searchtype=author&query=Barna%2C+B">B. Barna</a>, <a href="/search/?searchtype=author&query=Vermot%2C+P">P. Vermot</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.04232v1-abstract-short" style="display: inline;"> Sgr A East is the supernova remnant closest to the centre of the Milky Way. Its age has been estimated to be either very young, around 1-2 kyr, or about 10 kyr, and its exact origin remains unclear. We aspire to create a simple model of a supernova explosion that reproduces the shape, size, and location of Sgr A East. Using a simplified hydrodynamical code, we simulated the evolution of a supernov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.04232v1-abstract-full').style.display = 'inline'; document.getElementById('2211.04232v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.04232v1-abstract-full" style="display: none;"> Sgr A East is the supernova remnant closest to the centre of the Milky Way. Its age has been estimated to be either very young, around 1-2 kyr, or about 10 kyr, and its exact origin remains unclear. We aspire to create a simple model of a supernova explosion that reproduces the shape, size, and location of Sgr A East. Using a simplified hydrodynamical code, we simulated the evolution of a supernova remnant in the medium around the Galactic centre. The latter consists of a nearby massive molecular cloud with which Sgr A East is known to be interacting and a wind from the nuclear star cluster. Our preferred models of the Sgr A East remnant are compatible with an age of around 10 kyr. We also find suitable solutions for older ages, but not for ages younger than 5 kyr. Our simulations predict that the supernova exploded at a distance of about 3.5 pc from the Galactic centre, below the Galactic plane, slightly eastwards from the centre and 3 pc behind it. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.04232v1-abstract-full').style.display = 'none'; document.getElementById('2211.04232v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 15 figures, accepted by A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 668, A124 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.06452">arXiv:2210.06452</a> <span> [<a href="https://arxiv.org/pdf/2210.06452">pdf</a>, <a href="https://arxiv.org/format/2210.06452">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41550-022-01812-x">10.1038/s41550-022-01812-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Nested Dust Shells around the Wolf-Rayet Binary WR 140 observed with JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lau%2C+R+M">Ryan M. Lau</a>, <a href="/search/?searchtype=author&query=Hankins%2C+M+J">Matthew J. Hankins</a>, <a href="/search/?searchtype=author&query=Han%2C+Y">Yinuo Han</a>, <a href="/search/?searchtype=author&query=Argyriou%2C+I">Ioannis Argyriou</a>, <a href="/search/?searchtype=author&query=Corcoran%2C+M+F">Michael F. Corcoran</a>, <a href="/search/?searchtype=author&query=Eldridge%2C+J+J">Jan J. Eldridge</a>, <a href="/search/?searchtype=author&query=Endo%2C+I">Izumi Endo</a>, <a href="/search/?searchtype=author&query=Fox%2C+O+D">Ori D. Fox</a>, <a href="/search/?searchtype=author&query=Marin%2C+M+G">Macarena Garcia Marin</a>, <a href="/search/?searchtype=author&query=Gull%2C+T+R">Theodore R. Gull</a>, <a href="/search/?searchtype=author&query=Jones%2C+O+C">Olivia C. Jones</a>, <a href="/search/?searchtype=author&query=Hamaguchi%2C+K">Kenji Hamaguchi</a>, <a href="/search/?searchtype=author&query=Lamberts%2C+A">Astrid Lamberts</a>, <a href="/search/?searchtype=author&query=Law%2C+D+R">David R. Law</a>, <a href="/search/?searchtype=author&query=Madura%2C+T">Thomas Madura</a>, <a href="/search/?searchtype=author&query=Marchenko%2C+S+V">Sergey V. Marchenko</a>, <a href="/search/?searchtype=author&query=Matsuhara%2C+H">Hideo Matsuhara</a>, <a href="/search/?searchtype=author&query=Moffat%2C+A+F+J">Anthony F. J. Moffat</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Morris%2C+P+W">Patrick W. Morris</a>, <a href="/search/?searchtype=author&query=Onaka%2C+T">Takashi Onaka</a>, <a href="/search/?searchtype=author&query=Ressler%2C+M+E">Michael E. Ressler</a>, <a href="/search/?searchtype=author&query=Richardson%2C+N+D">Noel D. Richardson</a>, <a href="/search/?searchtype=author&query=Russell%2C+C+M+P">Christopher M. P. Russell</a>, <a href="/search/?searchtype=author&query=Sanchez-Bermudez%2C+J">Joel Sanchez-Bermudez</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.06452v1-abstract-short" style="display: inline;"> Massive colliding-wind binaries that host a Wolf-Rayet (WR) star present a potentially important source of dust and chemical enrichment in the interstellar medium (ISM). However, the chemical composition and survival of dust formed from such systems is not well understood. The carbon-rich WR (WC) binary WR~140 presents an ideal astrophysical laboratory for investigating these questions given its w… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.06452v1-abstract-full').style.display = 'inline'; document.getElementById('2210.06452v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.06452v1-abstract-full" style="display: none;"> Massive colliding-wind binaries that host a Wolf-Rayet (WR) star present a potentially important source of dust and chemical enrichment in the interstellar medium (ISM). However, the chemical composition and survival of dust formed from such systems is not well understood. The carbon-rich WR (WC) binary WR~140 presents an ideal astrophysical laboratory for investigating these questions given its well-defined orbital period and predictable dust-formation episodes every 7.93 years around periastron passage. We present observations from our Early Release Science program (ERS1349) with the James Webb Space Telescope (JWST) Mid-Infrared Instrument (MIRI) Medium-Resolution Spectrometer (MRS) and Imager that reveal the spectral and spatial signatures of nested circumstellar dust shells around WR~140. MIRI MRS spectroscopy of the second dust shell and Imager detections of over 17 shells formed throughout the past $\gtrsim130$ years confirm the survival of carbonaceous dust grains from WR~140 that are likely carriers of "unidentified infrared" (UIR)-band features at 6.4 and 7.7 $渭$m. The observations indicate that dust-forming WC binaries can enrich the ISM with organic compounds and carbonaceous dust. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.06452v1-abstract-full').style.display = 'none'; document.getElementById('2210.06452v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in Nature Astronomy on Oct 12, 2022; 21 pages, 5 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Lau, R.M., Hankins, M.J., Han, Y. et al. Nested dust shells around the Wolf-Rayet binary WR 140 observed with JWST. Nat Astron (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.08153">arXiv:2209.08153</a> <span> [<a href="https://arxiv.org/pdf/2209.08153">pdf</a>, <a href="https://arxiv.org/format/2209.08153">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aca40a">10.3847/1538-4357/aca40a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A VLA Study of Newly-Discovered Southern Latitude Non-Thermal Filaments in the Galactic Center: Radio Continuum Total-intensity and Spectral Index Properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Par%C3%A9%2C+D+M">Dylan M. Par茅</a>, <a href="/search/?searchtype=author&query=Lang%2C+C+C">Cornelia C. Lang</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.08153v1-abstract-short" style="display: inline;"> The non-thermal filament (NTF) radio structures clustered within a few hundred parsecs of the Galactic Center (GC) are apparently unique to this region of the Galaxy. Recent radio images of the GC using MeerKAT at 1 GHz have revealed a multitude of faint, previously unknown NTF bundles (NTFBs), some of which are comprised of as many as 10 or more individual filaments. In this work we present Very… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.08153v1-abstract-full').style.display = 'inline'; document.getElementById('2209.08153v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.08153v1-abstract-full" style="display: none;"> The non-thermal filament (NTF) radio structures clustered within a few hundred parsecs of the Galactic Center (GC) are apparently unique to this region of the Galaxy. Recent radio images of the GC using MeerKAT at 1 GHz have revealed a multitude of faint, previously unknown NTF bundles (NTFBs), some of which are comprised of as many as 10 or more individual filaments. In this work we present Very Large Array (VLA) observations at C- and X-bands (4 - 12 GHz) at arcsecond-scale resolutions of three of these newly-discovered NTFBs, all located at southern Galactic latitudes. These observations allow us to compare their total-intensity properties with those of the larger NTF population. We find that these targets generally possess properties similar to what is observed in the larger NTF population. However, the larger NTF population generally has steeper spectral index values than what we observe for our chosen targets. The results presented here based on the total-intensity properties of these structures indicate that the NTFs are likely all formed from Cosmic Rays (CRs). These CRs are either generated by a nearby compact source and then diffuse along the NTF lengths or are generated by extended, magnetized structures whose magnetic field undergoes reconnection with the NTF magnetic field. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.08153v1-abstract-full').style.display = 'none'; document.getElementById('2209.08153v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 13 figures, 2 tables. Submitted to ApJ for peer-review</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.12679">arXiv:2208.12679</a> <span> [<a href="https://arxiv.org/pdf/2208.12679">pdf</a>, <a href="https://arxiv.org/format/2208.12679">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac887c">10.3847/1538-4357/ac887c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence for an interaction between the Galactic Center clouds M0.10-0.08 and M0.11-0.11 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Butterfield%2C+N+O">Natalie O. Butterfield</a>, <a href="/search/?searchtype=author&query=Lang%2C+C+C">Cornelia C. Lang</a>, <a href="/search/?searchtype=author&query=Ginsburg%2C+A">Adam Ginsburg</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Ott%2C+J">Juergen Ott</a>, <a href="/search/?searchtype=author&query=Ludovici%2C+D+A">Dominic A. Ludovici</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.12679v1-abstract-short" style="display: inline;"> We present high-resolution (~2-3"; ~0.1 pc) radio observations of the Galactic center cloud M0.10-0.08 using the Very Large Array at K and Ka band (~25 and 36 GHz). The M0.10-0.08 cloud is located in a complex environment near the Galactic center Radio Arc and the adjacent M0.11-0.11 molecular cloud. From our data, M0.10-0.08 appears to be a compact molecular cloud (~3 pc) that contains multiple c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.12679v1-abstract-full').style.display = 'inline'; document.getElementById('2208.12679v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.12679v1-abstract-full" style="display: none;"> We present high-resolution (~2-3"; ~0.1 pc) radio observations of the Galactic center cloud M0.10-0.08 using the Very Large Array at K and Ka band (~25 and 36 GHz). The M0.10-0.08 cloud is located in a complex environment near the Galactic center Radio Arc and the adjacent M0.11-0.11 molecular cloud. From our data, M0.10-0.08 appears to be a compact molecular cloud (~3 pc) that contains multiple compact molecular cores (5+; <0.4 pc). In this study we detect a total of 15 molecular transitions in M0.10-0.08 from the following molecules: NH3, HC3N, CH3OH, HC5N, CH3CN, and OCS. We have identified more than sixty 36 GHz CH3OH masers in M0.10-0.08 with brightness temperatures above 400 K and 31 maser candidates with temperatures between 100-400 K. We conduct a kinematic analysis of the gas using NH3 and detect multiple velocity components towards this region of the Galactic center. The bulk of the gas in this region has a velocity of 51.5 km/s (M0.10-0.08) with a lower velocity wing at 37.6 km/s. We also detect a relatively faint velocity component at 10.6 km/s that we attribute to being an extension of the M0.11-0.11 cloud. Analysis of the gas kinematics, combined with past X-ray fluorescence observations, suggests M0.10-0.08 and M0.11-0.11 are located in the same vicinity of the Galactic center and could be physically interacting. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.12679v1-abstract-full').style.display = 'none'; document.getElementById('2208.12679v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in the Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.08508">arXiv:2208.08508</a> <span> [<a href="https://arxiv.org/pdf/2208.08508">pdf</a>, <a href="https://arxiv.org/format/2208.08508">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac8bd6">10.3847/1538-4357/ac8bd6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measuring the Orbits of the Arches and Quintuplet Clusters using HST and Gaia: Exploring Scenarios for Star Formation Near the Galactic Center </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Hosek%2C+M+W">Matthew W. Hosek Jr.</a>, <a href="/search/?searchtype=author&query=Do%2C+T">Tuan Do</a>, <a href="/search/?searchtype=author&query=Lu%2C+J+R">Jessica R. Lu</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/?searchtype=author&query=Ghez%2C+A+M">Andrea M. Ghez</a>, <a href="/search/?searchtype=author&query=Martinez%2C+G+D">Gregory D. Martinez</a>, <a href="/search/?searchtype=author&query=Anderson%2C+J">Jay Anderson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.08508v1-abstract-short" style="display: inline;"> We present new absolute proper motion measurements for the Arches and Quintuplet clusters, two young massive star clusters near the Galactic center. Using multi-epoch HST observations, we construct proper motion catalogs for the Arches ($\sim$35,000 stars) and Quintuplet ($\sim$40,000 stars) fields in ICRF coordinates established using stars in common with the Gaia EDR3 catalog. The bulk proper mo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.08508v1-abstract-full').style.display = 'inline'; document.getElementById('2208.08508v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.08508v1-abstract-full" style="display: none;"> We present new absolute proper motion measurements for the Arches and Quintuplet clusters, two young massive star clusters near the Galactic center. Using multi-epoch HST observations, we construct proper motion catalogs for the Arches ($\sim$35,000 stars) and Quintuplet ($\sim$40,000 stars) fields in ICRF coordinates established using stars in common with the Gaia EDR3 catalog. The bulk proper motions of the clusters are measured to be ($渭_{伪*}$, $渭_未$) = (-0.80 $\pm$ 0.032, -1.89 $\pm$ 0.021) mas/yr for the Arches and ($渭_{伪*}$, $渭_未$) = (-0.96 $\pm$ 0.032, -2.29 $\pm$ 0.023) mas/yr for the Quintuplet, achieving $\sim$5x higher precision than past measurements. We place the first constraints on the properties of the cluster orbits that incorporate the uncertainty in their current line-of-sight distances. The clusters will not approach closer than $\sim$25 pc to SgrA*, making it unlikely that they will inspiral into the Nuclear Star Cluster within their lifetime. Further, the cluster orbits are not consistent with being circular; the average value of r$_{apo}$ / r$_{peri}$ is $\sim$1.9 (equivalent to eccentricity of $\sim$0.31) for both clusters. Lastly, we find that the clusters do not share a common orbit, challenging one proposed formation scenario in which the clusters formed from molecular clouds on the open stream orbit derived by Kruijssen et al. (2015). Meanwhile, our constraints on the birth location and velocity of the clusters offer mild support for a scenario in which the clusters formed via collisions between gas clouds on the x1 and x2 bar orbit families. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.08508v1-abstract-full').style.display = 'none'; document.getElementById('2208.08508v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ. 38 pages, 25 figures. Proper motion catalogs included in ancillary materials</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.04024">arXiv:2208.04024</a> <span> [<a href="https://arxiv.org/pdf/2208.04024">pdf</a>, <a href="https://arxiv.org/format/2208.04024">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Human-Computer Interaction">cs.HC</span> </div> </div> <p class="title is-5 mathjax"> Social Simulacra: Creating Populated Prototypes for Social Computing Systems </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Park%2C+J+S">Joon Sung Park</a>, <a href="/search/?searchtype=author&query=Popowski%2C+L">Lindsay Popowski</a>, <a href="/search/?searchtype=author&query=Cai%2C+C+J">Carrie J. Cai</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Meredith Ringel Morris</a>, <a href="/search/?searchtype=author&query=Liang%2C+P">Percy Liang</a>, <a href="/search/?searchtype=author&query=Bernstein%2C+M+S">Michael S. Bernstein</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.04024v1-abstract-short" style="display: inline;"> Social computing prototypes probe the social behaviors that may arise in an envisioned system design. This prototyping practice is currently limited to recruiting small groups of people. Unfortunately, many challenges do not arise until a system is populated at a larger scale. Can a designer understand how a social system might behave when populated, and make adjustments to the design before the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.04024v1-abstract-full').style.display = 'inline'; document.getElementById('2208.04024v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.04024v1-abstract-full" style="display: none;"> Social computing prototypes probe the social behaviors that may arise in an envisioned system design. This prototyping practice is currently limited to recruiting small groups of people. Unfortunately, many challenges do not arise until a system is populated at a larger scale. Can a designer understand how a social system might behave when populated, and make adjustments to the design before the system falls prey to such challenges? We introduce social simulacra, a prototyping technique that generates a breadth of realistic social interactions that may emerge when a social computing system is populated. Social simulacra take as input the designer's description of a community's design -- goal, rules, and member personas -- and produce as output an instance of that design with simulated behavior, including posts, replies, and anti-social behaviors. We demonstrate that social simulacra shift the behaviors that they generate appropriately in response to design changes, and that they enable exploration of "what if?" scenarios where community members or moderators intervene. To power social simulacra, we contribute techniques for prompting a large language model to generate thousands of distinct community members and their social interactions with each other; these techniques are enabled by the observation that large language models' training data already includes a wide variety of positive and negative behavior on social media platforms. In evaluations, we show that participants are often unable to distinguish social simulacra from actual community behavior and that social computing designers successfully refine their social computing designs when using social simulacra. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.04024v1-abstract-full').style.display = 'none'; document.getElementById('2208.04024v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">This work will appear in the 35th Annual ACM Symposium on User Interface Software and Technology (UIST '22)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.02308">arXiv:2207.02308</a> <span> [<a href="https://arxiv.org/pdf/2207.02308">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Human-Computer Interaction">cs.HC</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1145/3517428.3544819">10.1145/3517428.3544819 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LaMPost: Design and Evaluation of an AI-assisted Email Writing Prototype for Adults with Dyslexia </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Goodman%2C+S+M">Steven M. Goodman</a>, <a href="/search/?searchtype=author&query=Buehler%2C+E">Erin Buehler</a>, <a href="/search/?searchtype=author&query=Clary%2C+P">Patrick Clary</a>, <a href="/search/?searchtype=author&query=Coenen%2C+A">Andy Coenen</a>, <a href="/search/?searchtype=author&query=Donsbach%2C+A">Aaron Donsbach</a>, <a href="/search/?searchtype=author&query=Horne%2C+T+N">Tiffanie N. Horne</a>, <a href="/search/?searchtype=author&query=Lahav%2C+M">Michal Lahav</a>, <a href="/search/?searchtype=author&query=Macdonald%2C+R">Robert Macdonald</a>, <a href="/search/?searchtype=author&query=Michaels%2C+R+B">Rain Breaw Michaels</a>, <a href="/search/?searchtype=author&query=Narayanan%2C+A">Ajit Narayanan</a>, <a href="/search/?searchtype=author&query=Pushkarna%2C+M">Mahima Pushkarna</a>, <a href="/search/?searchtype=author&query=Riley%2C+J">Joel Riley</a>, <a href="/search/?searchtype=author&query=Santana%2C+A">Alex Santana</a>, <a href="/search/?searchtype=author&query=Shi%2C+L">Lei Shi</a>, <a href="/search/?searchtype=author&query=Sweeney%2C+R">Rachel Sweeney</a>, <a href="/search/?searchtype=author&query=Weaver%2C+P">Phil Weaver</a>, <a href="/search/?searchtype=author&query=Yuan%2C+A">Ann Yuan</a>, <a href="/search/?searchtype=author&query=Morris%2C+M+R">Meredith Ringel Morris</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.02308v1-abstract-short" style="display: inline;"> Prior work has explored the writing challenges experienced by people with dyslexia, and the potential for new spelling, grammar, and word retrieval technologies to address these challenges. However, the capabilities for natural language generation demonstrated by the latest class of large language models (LLMs) highlight an opportunity to explore new forms of human-AI writing support tools. In thi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.02308v1-abstract-full').style.display = 'inline'; document.getElementById('2207.02308v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.02308v1-abstract-full" style="display: none;"> Prior work has explored the writing challenges experienced by people with dyslexia, and the potential for new spelling, grammar, and word retrieval technologies to address these challenges. However, the capabilities for natural language generation demonstrated by the latest class of large language models (LLMs) highlight an opportunity to explore new forms of human-AI writing support tools. In this paper, we introduce LaMPost, a prototype email-writing interface that explores the potential for LLMs to power writing support tools that address the varied needs of people with dyslexia. LaMPost draws from our understanding of these needs and introduces novel AI-powered features for email-writing, including: outlining main ideas, generating a subject line, suggesting changes, rewriting a selection. We evaluated LaMPost with 19 adults with dyslexia, identifying many promising routes for further exploration (including the popularity of the "rewrite" and "subject line" features), but also finding that the current generation of LLMs may not surpass the accuracy and quality thresholds required to meet the needs of writers with dyslexia. Surprisingly, we found that participants' awareness of the AI had no effect on their perception of the system, nor on their feelings of autonomy, expression, and self-efficacy when writing emails. Our findings yield further insight into the benefits and drawbacks of using LLMs as writing support for adults with dyslexia and provide a foundation to build upon in future research. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.02308v1-abstract-full').style.display = 'none'; document.getElementById('2207.02308v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To appear at The 24th International ACM SIGACCESS Conference on Computers and Accessibility (ASSETS '22), October 23-26, 2022, Athens, Greece. 26 pages</span> </p> </li> </ol> <nav class="pagination is-small 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