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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <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/2410.22319">arXiv:2410.22319</a> <span> [<a href="https://arxiv.org/pdf/2410.22319">pdf</a>, <a href="https://arxiv.org/format/2410.22319">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/10.1051/0004-6361/202452311">10.1051/0004-6361/202452311 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A wiggling filamentary jet at the origin of the blazar multi-wavelength behaviour </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Raiteri%2C+C+M">C. M. Raiteri</a>, <a href="/search/astro-ph?searchtype=author&query=Villata%2C+M">M. Villata</a>, <a href="/search/astro-ph?searchtype=author&query=Carnerero%2C+M+I">M. I. Carnerero</a>, <a href="/search/astro-ph?searchtype=author&query=Kurtanidze%2C+S+O">S. O. Kurtanidze</a>, <a href="/search/astro-ph?searchtype=author&query=Mirzaqulov%2C+D+O">D. O. Mirzaqulov</a>, <a href="/search/astro-ph?searchtype=author&query=Ben%C3%ADtez%2C+E">E. Ben铆tez</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnoli%2C+G">G. Bonnoli</a>, <a href="/search/astro-ph?searchtype=author&query=Carosati%2C+D">D. Carosati</a>, <a href="/search/astro-ph?searchtype=author&query=Acosta-Pulido%2C+J+A">J. A. Acosta-Pulido</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Andreeva%2C+T+S">T. S. Andreeva</a>, <a href="/search/astro-ph?searchtype=author&query=Apolonio%2C+G">G. Apolonio</a>, <a href="/search/astro-ph?searchtype=author&query=Bachev%2C+R">R. Bachev</a>, <a href="/search/astro-ph?searchtype=author&query=Borman%2C+G+A">G. A. Borman</a>, <a href="/search/astro-ph?searchtype=author&query=Bozhilov%2C+V">V. Bozhilov</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+L+F">L. F. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Carbonell%2C+W">W. Carbonell</a>, <a href="/search/astro-ph?searchtype=author&query=Casadio%2C+C">C. Casadio</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+W+P">W. P. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Damljanovic%2C+G">G. Damljanovic</a>, <a href="/search/astro-ph?searchtype=author&query=Ehgamberdiev%2C+S+A">S. A. Ehgamberdiev</a>, <a href="/search/astro-ph?searchtype=author&query=Elsaesser%2C+D">D. Elsaesser</a>, <a href="/search/astro-ph?searchtype=author&query=Escudero%2C+J">J. Escudero</a>, <a href="/search/astro-ph?searchtype=author&query=Feige%2C+M">M. Feige</a>, <a href="/search/astro-ph?searchtype=author&query=Fuentes%2C+A">A. Fuentes</a> , et al. (74 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="2410.22319v1-abstract-short" style="display: inline;"> Blazars are beamed active galactic nuclei known for their strong multi-wavelength variability on timescales from years down to minutes. We aim to investigate the suitability of the twisting jet model presented in previous works to explain the multi-wavelength behaviour of BL Lacertae, the prototype of one of the blazar classes. According to this model, the jet is inhomogeneous, curved, and twistin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.22319v1-abstract-full').style.display = 'inline'; document.getElementById('2410.22319v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.22319v1-abstract-full" style="display: none;"> Blazars are beamed active galactic nuclei known for their strong multi-wavelength variability on timescales from years down to minutes. We aim to investigate the suitability of the twisting jet model presented in previous works to explain the multi-wavelength behaviour of BL Lacertae, the prototype of one of the blazar classes. According to this model, the jet is inhomogeneous, curved, and twisting, and the long-term variability is due to changes in the Doppler factor due to variations in the orientation of the jet-emitting regions. We analysed optical data of the source obtained during monitoring campaigns organised by the Whole Earth Blazar Telescope (WEBT) in 2019-2022, together with radio data from the WEBT and other teams, and gamma-ray data from the Fermi satellite. In this period, BL Lacertae underwent an extraordinary activity phase, reaching its historical optical and gamma-ray brightness maxima. The application of the twisting jet model to the source light curves allows us to infer the wiggling motion of the optical, radio, and gamma-ray jet-emitting regions. The optical-radio correlation shows that the changes in the radio viewing angle follow those in the optical viewing angle by about 120 days, and it suggests that the jet is composed of plasma filaments, which is in agreement with some radio high-resolution observations of other sources. The gamma-ray emitting region is found to be co-spatial with the optical one, and the analysis of the gamma-optical correlation is consistent with both the geometric interpretation and a synchrotron self-Compton (SSC) origin of the high-energy photons. We propose a geometric scenario where the jet is made up of a pair of emitting plasma filaments in a sort of double-helix curved rotating structure, whose wiggling motion produces changes in the Doppler beaming and can thus explain the observed multi-wavelength long-term variability. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.22319v1-abstract-full').style.display = 'none'; document.getElementById('2410.22319v1-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 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">In press for 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 692 (2024) A48 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.16964">arXiv:2409.16964</a> <span> [<a href="https://arxiv.org/pdf/2409.16964">pdf</a>, <a href="https://arxiv.org/format/2409.16964">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> <p class="title is-5 mathjax"> Preferential Occurrence of Fast Radio Bursts in Massive Star-Forming Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+K">Kritti Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">Vikram Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+C">Casey Law</a>, <a href="/search/astro-ph?searchtype=author&query=Ocker%2C+S+K">Stella Koch Ocker</a>, <a href="/search/astro-ph?searchtype=author&query=Sherman%2C+M">Myles Sherman</a>, <a href="/search/astro-ph?searchtype=author&query=Kosogorov%2C+N">Nikita Kosogorov</a>, <a href="/search/astro-ph?searchtype=author&query=Faber%2C+J">Jakob Faber</a>, <a href="/search/astro-ph?searchtype=author&query=Hallinan%2C+G">Gregg Hallinan</a>, <a href="/search/astro-ph?searchtype=author&query=Harnach%2C+C">Charlie Harnach</a>, <a href="/search/astro-ph?searchtype=author&query=Hellbourg%2C+G">Greg Hellbourg</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Rick Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Hodge%2C+D">David Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">Mark Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J">James Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+P">Paul Rasmussen</a>, <a href="/search/astro-ph?searchtype=author&query=Somalwar%2C+J">Jean Somalwar</a>, <a href="/search/astro-ph?searchtype=author&query=Weinreb%2C+S">Sander Weinreb</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D">David Woody</a>, <a href="/search/astro-ph?searchtype=author&query=Leja%2C+J">Joel Leja</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+S">Shreya Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Das%2C+K+K">Kaustav Kashyap Das</a>, <a href="/search/astro-ph?searchtype=author&query=Qin%2C+Y">Yu-Jing Qin</a>, <a href="/search/astro-ph?searchtype=author&query=Rose%2C+S">Sam Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+D+Z">Dillon Z. Dong</a> , et al. (2 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="2409.16964v1-abstract-short" style="display: inline;"> Fast Radio Bursts (FRBs) are millisecond-duration events detected from beyond the Milky Way. FRB emission characteristics favor highly magnetized neutron stars, or magnetars, as the sources, as evidenced by FRB-like bursts from a galactic magnetar, and the star-forming nature of FRB host galaxies. However, the processes that produce FRB sources remain unknown. Although galactic magnetars are often… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16964v1-abstract-full').style.display = 'inline'; document.getElementById('2409.16964v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.16964v1-abstract-full" style="display: none;"> Fast Radio Bursts (FRBs) are millisecond-duration events detected from beyond the Milky Way. FRB emission characteristics favor highly magnetized neutron stars, or magnetars, as the sources, as evidenced by FRB-like bursts from a galactic magnetar, and the star-forming nature of FRB host galaxies. However, the processes that produce FRB sources remain unknown. Although galactic magnetars are often linked to core-collapse supernovae (CCSNe), it's uncertain what determines which supernovae result in magnetars. The galactic environments of FRB sources can be harnessed to probe their progenitors. Here, we present the stellar population properties of 30 FRB host galaxies discovered by the Deep Synoptic Array. Our analysis shows a significant deficit of low-mass FRB hosts compared to the occurrence of star-formation in the universe, implying that FRBs are a biased tracer of star-formation, preferentially selecting massive star-forming galaxies. This bias may be driven by galaxy metallicity, which is positively correlated with stellar mass. Metal-rich environments may favor the formation of magnetar progenitors through stellar mergers, as higher metallicity stars are less compact and more likely to fill their Roche lobes, leading to unstable mass transfer. Although massive stars do not have convective interiors to generate strong magnetic fields by dynamo, merger remnants are thought to have the requisite internal magnetic-field strengths to result in magnetars. The preferential occurrence of FRBs in massive star-forming galaxies suggests that CCSN of merger remnants preferentially forms magnetars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16964v1-abstract-full').style.display = 'none'; document.getElementById('2409.16964v1-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> 25 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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 Nature. The final version will be published by the 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/2409.16952">arXiv:2409.16952</a> <span> [<a href="https://arxiv.org/pdf/2409.16952">pdf</a>, <a href="https://arxiv.org/format/2409.16952">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="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"> A gas rich cosmic web revealed by partitioning the missing baryons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">Vikram Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+K">Kritti Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Ocker%2C+S+K">Stella Koch Ocker</a>, <a href="/search/astro-ph?searchtype=author&query=Faber%2C+J">Jakob Faber</a>, <a href="/search/astro-ph?searchtype=author&query=Hallinan%2C+G">Gregg Hallinan</a>, <a href="/search/astro-ph?searchtype=author&query=Harnach%2C+C">Charlie Harnach</a>, <a href="/search/astro-ph?searchtype=author&query=Hellbourg%2C+G">Greg Hellbourg</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Rick Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Hodge%2C+D">David Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">Mark Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Kosogorov%2C+N">Nikita Kosogorov</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J">James Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+C">Casey Law</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+P">Paul Rasmussen</a>, <a href="/search/astro-ph?searchtype=author&query=Sherman%2C+M">Myles Sherman</a>, <a href="/search/astro-ph?searchtype=author&query=Somalwar%2C+J">Jean Somalwar</a>, <a href="/search/astro-ph?searchtype=author&query=Weinreb%2C+S">Sander Weinreb</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D">David Woody</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="2409.16952v1-abstract-short" style="display: inline;"> Approximately half of the Universe's dark matter resides in collapsed halos; significantly less than half of the baryonic matter (protons and neutrons) remains confined to halos. A small fraction of baryons are in stars and the interstellar medium within galaxies. The lion's share are diffuse (less than $10^{-3}$ cm$^{-3}$) and ionized (neutral fraction less than $10^{-4}$), located in the interga… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16952v1-abstract-full').style.display = 'inline'; document.getElementById('2409.16952v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.16952v1-abstract-full" style="display: none;"> Approximately half of the Universe's dark matter resides in collapsed halos; significantly less than half of the baryonic matter (protons and neutrons) remains confined to halos. A small fraction of baryons are in stars and the interstellar medium within galaxies. The lion's share are diffuse (less than $10^{-3}$ cm$^{-3}$) and ionized (neutral fraction less than $10^{-4}$), located in the intergalactic medium (IGM) and in the halos of galaxy clusters, groups, and galaxies. The quantity and spatial distribution of this diffuse ionized gas is notoriously difficult to measure, but has wide implications for galaxy formation, astrophysical feedback, and precision cosmology. Recently, the dispersion of extragalactic Fast Radio Bursts (FRBs) has been used to measure the total content of cosmic baryons. However, past efforts had modest samples and methods that cannot discriminate between IGM and halo gas, which is critical for studying feedback and for observational cosmology. Here, we present a large cosmological sample of FRB sources localized to their host galaxies. We have robustly partitioned the missing baryons into the IGM, galaxy clusters, and galaxies, providing a late-Universe measurement of the total baryon density of $惟_b h_{70}$=0.049$\pm$0.003. Our results indicate efficient feedback processes that can expel gas from galaxy halos and into the intergalactic medium, agreeing with the enriched cosmic web scenario seen in cosmological simulations. The large diffuse baryon fraction that we have measured disfavours bottom-heavy stellar initial mass functions, which predict a large total stellar density, $惟_*$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16952v1-abstract-full').style.display = 'none'; document.getElementById('2409.16952v1-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> 25 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.14182">arXiv:2405.14182</a> <span> [<a href="https://arxiv.org/pdf/2405.14182">pdf</a>, <a href="https://arxiv.org/format/2405.14182">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> <p class="title is-5 mathjax"> A Heavily Scattered Fast Radio Burst Is Viewed Through Multiple Galaxy Halos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Faber%2C+J+T">Jakob T. Faber</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">Vikram Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Ocker%2C+S+K">Stella Koch Ocker</a>, <a href="/search/astro-ph?searchtype=author&query=Sherman%2C+M+B">Myles B. Sherman</a>, <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+K">Kritti Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+C">Casey Law</a>, <a href="/search/astro-ph?searchtype=author&query=Kosogorov%2C+N">Nikita Kosogorov</a>, <a href="/search/astro-ph?searchtype=author&query=Hallinan%2C+G">Gregg Hallinan</a>, <a href="/search/astro-ph?searchtype=author&query=Harnach%2C+C">Charlie Harnach</a>, <a href="/search/astro-ph?searchtype=author&query=Hellbourg%2C+G">Greg Hellbourg</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Rick Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Hodge%2C+D">David Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">Mark Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">James W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+P">Paul Rasmussen</a>, <a href="/search/astro-ph?searchtype=author&query=Somalwar%2C+J+J">Jean J. Somalwar</a>, <a href="/search/astro-ph?searchtype=author&query=Weinreb%2C+S">Sander Weinreb</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D+P">David P. Woody</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="2405.14182v1-abstract-short" style="display: inline;"> We present a multi-wavelength study of the apparently non-repeating, heavily scattered fast radio burst, FRB 20221219A, detected by the Deep Synoptic Array 110 (DSA-110). The burst exhibits a moderate dispersion measure (DM) of $706.7^{+0.6}_{-0.6}$ $\mathrm{pc}~\mathrm{cm}^{-3}$ and an unusually high scattering timescale of $蟿_{\mathrm{obs}} = 19.2_{-2.7}^{+2.7}$ ms at 1.4 GHz. We associate the F… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14182v1-abstract-full').style.display = 'inline'; document.getElementById('2405.14182v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.14182v1-abstract-full" style="display: none;"> We present a multi-wavelength study of the apparently non-repeating, heavily scattered fast radio burst, FRB 20221219A, detected by the Deep Synoptic Array 110 (DSA-110). The burst exhibits a moderate dispersion measure (DM) of $706.7^{+0.6}_{-0.6}$ $\mathrm{pc}~\mathrm{cm}^{-3}$ and an unusually high scattering timescale of $蟿_{\mathrm{obs}} = 19.2_{-2.7}^{+2.7}$ ms at 1.4 GHz. We associate the FRB with a Milky Way-like host galaxy at $z_{\mathrm{host}} = 0.554$ of stellar mass $\mathrm{log}_{10}(M_{\star, \mathrm{host}}) = 10.20^{+0.04}_{-0.03} ~M_\odot$. We identify two intervening galaxy halos at redshifts $z_{\mathrm{igh1}} = 0.492$ and $z_{\mathrm{igh2}} = 0.438$, with low impact parameters, $b_{\mathrm{igh1}} = 43.0_{-11.3}^{+11.3}$ kpc and $b_{\mathrm{igh2}} = 36.1_{-11.3}^{+11.3}$ kpc, and intermediate stellar masses, $\mathrm{log}_{10}(M_{\star, \mathrm{igh1}}) = 10.01^{+0.02}_{-0.02} ~M_\odot$ and $\mathrm{log}_{10}(M_{\star, \mathrm{igh2}}) = 10.60^{+0.02}_{-0.02} ~M_\odot$. The presence of two such galaxies suggests that the sightline is significantly overcrowded compared to the median sightline to this redshift, as inferred from the halo mass function. We perform a detailed analysis of the sightline toward FRB 20221219A, constructing both DM and scattering budgets. Our results suggest that, unlike most well-localized sources, the host galaxy does not dominate the observed scattering. Instead, we posit that an intersection with a single partially ionized cloudlet in the circumgalactic medium of an intervening galaxy could account for the substantial scattering in FRB 20221219A and remain in agreement with typical electron densities inferred for extra-planar dense cloud-like structures in the Galactic and extragalactic halos (e.g., high-velocity clouds). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14182v1-abstract-full').style.display = 'none'; document.getElementById('2405.14182v1-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> 23 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">18 pages, 6 figures, submitted to ApJ, comments appreciated</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.06816">arXiv:2308.06816</a> <span> [<a href="https://arxiv.org/pdf/2308.06816">pdf</a>, <a href="https://arxiv.org/format/2308.06816">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/10.3847/2041-8213/ad0380">10.3847/2041-8213/ad0380 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Deep Synoptic Array Science: Implications of Faraday Rotation Measures of Localized Fast Radio Bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sherman%2C+M+B">Myles B. Sherman</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">Vikram Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+C">Casey Law</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+G">Ge Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+K">Kritti Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Catha%2C+M">Morgan Catha</a>, <a href="/search/astro-ph?searchtype=author&query=Faber%2C+J+T">Jakob T. Faber</a>, <a href="/search/astro-ph?searchtype=author&query=Hallinan%2C+G">Gregg Hallinan</a>, <a href="/search/astro-ph?searchtype=author&query=Harnach%2C+C">Charlie Harnach</a>, <a href="/search/astro-ph?searchtype=author&query=Hellbourg%2C+G">Greg Hellbourg</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Rick Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Hodge%2C+D">David Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">Mark Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">James W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+P">Paul Rasmussen</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+J">Jun Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Simard%2C+D">Dana Simard</a>, <a href="/search/astro-ph?searchtype=author&query=Somalwar%2C+J">Jean Somalwar</a>, <a href="/search/astro-ph?searchtype=author&query=Squillace%2C+R">Reynier Squillace</a>, <a href="/search/astro-ph?searchtype=author&query=Weinreb%2C+S">Sander Weinreb</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D+P">David P. Woody</a>, <a href="/search/astro-ph?searchtype=author&query=Yadlapalli%2C+N">Nitika Yadlapalli</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="2308.06816v2-abstract-short" style="display: inline;"> Faraday rotation measures (RMs) of fast radio bursts (FRBs) offer the prospect of directly measuring extragalactic magnetic fields. We present an analysis of the RMs of ten as yet non-repeating FRBs detected and localized to host galaxies by the 110-antenna Deep Synoptic Array (DSA-110). We combine this sample with published RMs of 15 localized FRBs, nine of which are repeating sources. For each F… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.06816v2-abstract-full').style.display = 'inline'; document.getElementById('2308.06816v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.06816v2-abstract-full" style="display: none;"> Faraday rotation measures (RMs) of fast radio bursts (FRBs) offer the prospect of directly measuring extragalactic magnetic fields. We present an analysis of the RMs of ten as yet non-repeating FRBs detected and localized to host galaxies by the 110-antenna Deep Synoptic Array (DSA-110). We combine this sample with published RMs of 15 localized FRBs, nine of which are repeating sources. For each FRB in the combined sample, we estimate the host-galaxy dispersion measure (DM) contributions and extragalactic RM. We find compelling evidence that the extragalactic components of FRB RMs are often dominated by contributions from the host-galaxy interstellar medium (ISM). Specifically, we find that both repeating and as yet non-repeating FRBs show a correlation between the host-DM and host-RM in the rest frame, and we find an anti-correlation between extragalactic RM (in the observer frame) and redshift for non-repeaters, as expected if the magnetized plasma is in the host galaxy. Important exceptions to the ISM origin include a dense, magnetized circum-burst medium in some repeating FRBs, and the intra-cluster medium (ICM) of host or intervening galaxy clusters. We find that the estimated ISM magnetic-field strengths, $\bar{B}_{||}$, are characteristically larger than those inferred from Galactic radio pulsars. This suggests either increased ISM magnetization in FRB hosts in comparison with the Milky Way, or that FRBs preferentially reside in regions of increased magnetic-field strength within their hosts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.06816v2-abstract-full').style.display = 'none'; document.getElementById('2308.06816v2-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 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">13 pages, 4 figures, 1 table ; added references to section 1, 2, and 3; added a paragraph in Section 3 to discuss simulations addressing interplay of local and ISM magnetic field; added bar to B|| to indicate average over line of sight</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.06813">arXiv:2308.06813</a> <span> [<a href="https://arxiv.org/pdf/2308.06813">pdf</a>, <a href="https://arxiv.org/format/2308.06813">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/ad275e">10.3847/1538-4357/ad275e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Deep Synoptic Array Science: Polarimetry of 25 New Fast Radio Bursts Provides Insights into their Origins </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sherman%2C+M+B">Myles B. Sherman</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">Vikram Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+C">Casey Law</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+G">Ge Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Catha%2C+M">Morgan Catha</a>, <a href="/search/astro-ph?searchtype=author&query=Faber%2C+J+T">Jakob T. Faber</a>, <a href="/search/astro-ph?searchtype=author&query=Hallinan%2C+G">Gregg Hallinan</a>, <a href="/search/astro-ph?searchtype=author&query=Harnach%2C+C">Charlie Harnach</a>, <a href="/search/astro-ph?searchtype=author&query=Hellbourg%2C+G">Greg Hellbourg</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Rick Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Hodge%2C+D">David Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">Mark Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">James W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+P">Paul Rasmussen</a>, <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+K">Kritti Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+J">Jun Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Simard%2C+D">Dana Simard</a>, <a href="/search/astro-ph?searchtype=author&query=Somalwar%2C+J">Jean Somalwar</a>, <a href="/search/astro-ph?searchtype=author&query=Squillace%2C+R">Reynier Squillace</a>, <a href="/search/astro-ph?searchtype=author&query=Weinreb%2C+S">Sander Weinreb</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D+P">David P. Woody</a>, <a href="/search/astro-ph?searchtype=author&query=Yadlapalli%2C+N">Nitika Yadlapalli</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="2308.06813v3-abstract-short" style="display: inline;"> We report on a full-polarization analysis of the first 25 as yet non-repeating FRBs detected at 1.4 GHz by the 110-antenna Deep Synoptic Array (DSA-110) during commissioning observations. We present details of the data-reduction, calibration, and analysis procedures developed for this novel instrument. Faraday rotation measures (RMs) are searched between $\pm10^6$ rad m$^{-2}$ and detected for 20… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.06813v3-abstract-full').style.display = 'inline'; document.getElementById('2308.06813v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.06813v3-abstract-full" style="display: none;"> We report on a full-polarization analysis of the first 25 as yet non-repeating FRBs detected at 1.4 GHz by the 110-antenna Deep Synoptic Array (DSA-110) during commissioning observations. We present details of the data-reduction, calibration, and analysis procedures developed for this novel instrument. Faraday rotation measures (RMs) are searched between $\pm10^6$ rad m$^{-2}$ and detected for 20 FRBs with magnitudes ranging from $4-4670$ rad m$^{-2}$. $15/25$ FRBs are consistent with 100% polarization, 10 of which have high ($\ge70\%$) linear-polarization fractions and 2 of which have high ($\ge30\%$) circular-polarization fractions. Our results disfavor multipath RM scattering as a dominant depolarization mechanism. Polarization-state and possible RM variations are observed in the four FRBs with multiple sub-components. We combine the DSA-110 sample with polarimetry of previously published FRBs, and compare the polarization properties of FRB sub-populations and FRBs with Galactic pulsars. Although FRB polarization fractions are typically higher than those of Galactic pulsars, and cover a wider range than those of pulsar single pulses, they resemble those of the youngest (characteristic ages $<10^{5}$ yr) pulsars. Our results support a scenario wherein FRB emission is intrinsically highly linearly polarized, and propagation effects can result in conversion to circular polarization and depolarization. Young pulsar emission and magnetospheric-propagation geometries may form a useful analogy for the origin of FRB polarization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.06813v3-abstract-full').style.display = 'none'; document.getElementById('2308.06813v3-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 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">57 pages, 24 figures, 5 tables ; version accepted by ApJ ; revised classification to include polarized signal-to-noise; added appendices for PA error/variability, J1935 polarization ; corrected literature FRB sample and supplemented with omitted data; added discussion of biases, limitations, and selection criteria; revised sigmaRM analysis ; additional plots added ; revised FRB20220424E analysis</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.03344">arXiv:2307.03344</a> <span> [<a href="https://arxiv.org/pdf/2307.03344">pdf</a>, <a href="https://arxiv.org/format/2307.03344">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> <p class="title is-5 mathjax"> Deep Synoptic Array Science: First FRB and Host Galaxy Catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Law%2C+C+J">C. J. Law</a>, <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+K">K. Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">V. Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+G">G. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Catha%2C+M">M. Catha</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">L. Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Faber%2C+J+T">J. T. Faber</a>, <a href="/search/astro-ph?searchtype=author&query=Hallinan%2C+G">G. Hallinan</a>, <a href="/search/astro-ph?searchtype=author&query=Harnach%2C+C">C. Harnach</a>, <a href="/search/astro-ph?searchtype=author&query=Hellbourg%2C+G">G. Hellbourg</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">R. Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Hodge%2C+D">D. Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">M. Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">J. W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+P">P. Rasmussen</a>, <a href="/search/astro-ph?searchtype=author&query=Sherman%2C+M+B">M. B. Sherman</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+J">J. Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Simard%2C+D">D. Simard</a>, <a href="/search/astro-ph?searchtype=author&query=Squillace%2C+R">R. Squillace</a>, <a href="/search/astro-ph?searchtype=author&query=Weinreb%2C+S">S. Weinreb</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D+P">D. P. Woody</a>, <a href="/search/astro-ph?searchtype=author&query=Yadlapalli%2C+N">N. Yadlapalli</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="2307.03344v2-abstract-short" style="display: inline;"> Fast Radio Bursts (FRBs) are a powerful and mysterious new class of transient that are luminous enough to be detected at cosmological distances. By associating FRBs to host galaxies, we can measure intrinsic and environmental properties that test FRB origin models, in addition to using them as precise probes of distant cosmic gas. The Deep Synoptic Array (DSA-110) is a radio interferometer built t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.03344v2-abstract-full').style.display = 'inline'; document.getElementById('2307.03344v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.03344v2-abstract-full" style="display: none;"> Fast Radio Bursts (FRBs) are a powerful and mysterious new class of transient that are luminous enough to be detected at cosmological distances. By associating FRBs to host galaxies, we can measure intrinsic and environmental properties that test FRB origin models, in addition to using them as precise probes of distant cosmic gas. The Deep Synoptic Array (DSA-110) is a radio interferometer built to maximize the rate at which it can simultaneously detect and localize FRBs. Here, we present the first sample of FRBs and host galaxies discovered by the DSA-110. This sample of 11 FRBs is the largest, most uniform sample of localized FRBs to date, as it is selected based on association to host galaxies identified in optical imaging by Pan-STARRS1. These FRBs have not been observed to repeat and their radio properties (dispersion, temporal scattering, energy) are similar to that of the known non-repeating FRB population. Most host galaxies have ongoing star formation, as has been identified before for FRB hosts. Two hosts of the new sample are massive, quiescent galaxies. The distribution of star-formation history across this host-galaxy sample shows that the delay-time distribution is wide, with a powerlaw model that spans from $\sim100$\,Myr to $\gtrsim2$\,Gyr. This requires the existence of one or more progenitor formation channels associated with old stellar populations, such as the binary evolution of compact objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.03344v2-abstract-full').style.display = 'none'; document.getElementById('2307.03344v2-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> 24 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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. Submitted to AAS Journals. Includes changes based on referee comments and improved host galaxy analysis</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.14788">arXiv:2302.14788</a> <span> [<a href="https://arxiv.org/pdf/2302.14788">pdf</a>, <a href="https://arxiv.org/format/2302.14788">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/acd3ea">10.3847/2041-8213/acd3ea <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Deep Synoptic Array science: Two fast radio burst sources in massive galaxy clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">Vikram Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Catha%2C+M">Morgan Catha</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+G">Ge Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Faber%2C+J+T">Jakob T. Faber</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">James W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Hallinan%2C+G">Gregg Hallinan</a>, <a href="/search/astro-ph?searchtype=author&query=Harnach%2C+C">Charlie Harnach</a>, <a href="/search/astro-ph?searchtype=author&query=Hellbourg%2C+G">Greg Hellbourg</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Rick Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Hodge%2C+D">David Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">Mark Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+C">Casey Law</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+P">Paul Rasmussen</a>, <a href="/search/astro-ph?searchtype=author&query=Sayers%2C+J">Jack Sayers</a>, <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+K">Kritti Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Sherman%2C+M+B">Myles B. Sherman</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+J">Jun Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Simard%2C+D">Dana Simard</a>, <a href="/search/astro-ph?searchtype=author&query=Somalwar%2C+J">Jean Somalwar</a>, <a href="/search/astro-ph?searchtype=author&query=Squillace%2C+R">Reynier Squillace</a>, <a href="/search/astro-ph?searchtype=author&query=Weinreb%2C+S">Sander Weinreb</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D+P">David P. Woody</a>, <a href="/search/astro-ph?searchtype=author&query=Yadlapalli%2C+N">Nitika Yadlapalli</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="2302.14788v1-abstract-short" style="display: inline;"> The hot gas that constitutes the intracluster medium (ICM) has been studied at X-ray and millimeter/sub-millimeter wavelengths (Sunyaev-Zeldovich effect) for decades. Fast radio bursts (FRBs) offer an additional method of directly measuring the ICM and gas surrounding clusters, via observables such as dispersion measure (DM) and Faraday rotation measure (RM). We report the discovery of two FRB sou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.14788v1-abstract-full').style.display = 'inline'; document.getElementById('2302.14788v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.14788v1-abstract-full" style="display: none;"> The hot gas that constitutes the intracluster medium (ICM) has been studied at X-ray and millimeter/sub-millimeter wavelengths (Sunyaev-Zeldovich effect) for decades. Fast radio bursts (FRBs) offer an additional method of directly measuring the ICM and gas surrounding clusters, via observables such as dispersion measure (DM) and Faraday rotation measure (RM). We report the discovery of two FRB sources detected with the Deep Synoptic Array (DSA-110) whose host galaxies belong to massive galaxy clusters. In both cases, the FRBs exhibit excess extragalactic DM, some of which likely originates in the ICM of their respective clusters. FRB 20220914A resides in the galaxy cluster Abell 2310 at z=0.1125 with a projected offset from the cluster center of 520 kpc. The host of a second source, FRB 20220509G, is an elliptical galaxy at z=0.0894 that belongs to the galaxy cluster Abell 2311 at projected offset of 870 kpc. These sources represent the first time an FRB has been localized to a galaxy cluster. We combine our FRB data with archival X-ray, SZ, and optical observations of these clusters in order to infer properties of the ICM, including a measurement of gas temperature from DM and ySZ of 0.8-3.9 keV. We then compare our results to massive cluster halos from the IllustrisTNG simulation. Finally, we describe how large samples of localized FRBs from future surveys will constrain the ICM, particularly beyond the virial radius of clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.14788v1-abstract-full').style.display = 'none'; document.getElementById('2302.14788v1-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.14782">arXiv:2302.14782</a> <span> [<a href="https://arxiv.org/pdf/2302.14782">pdf</a>, <a href="https://arxiv.org/format/2302.14782">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/10.3847/1538-4357/accf1d">10.3847/1538-4357/accf1d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Deep Synoptic Array science: A massive elliptical host among two galaxy-cluster fast radio bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+K">Kritti Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Somalwar%2C+J">Jean Somalwar</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+C">Casey Law</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">Vikram Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Catha%2C+M">Morgan Catha</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+G">Ge Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Faber%2C+J+T">Jakob T. Faber</a>, <a href="/search/astro-ph?searchtype=author&query=Hallinan%2C+G">Gregg Hallinan</a>, <a href="/search/astro-ph?searchtype=author&query=Harnach%2C+C">Charlie Harnach</a>, <a href="/search/astro-ph?searchtype=author&query=Hellbourg%2C+G">Greg Hellbourg</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Rick Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Hodge%2C+D">David Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">Mark Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">James W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+P">Paul Rasmussen</a>, <a href="/search/astro-ph?searchtype=author&query=Sherman%2C+M+B">Myles B. Sherman</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+J">Jun Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Simard%2C+D">Dana Simard</a>, <a href="/search/astro-ph?searchtype=author&query=Squillace%2C+R">Reynier Squillace</a>, <a href="/search/astro-ph?searchtype=author&query=Weinreb%2C+S">Sander Weinreb</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D+P">David P. Woody</a>, <a href="/search/astro-ph?searchtype=author&query=Yadlapalli%2C+N">Nitika Yadlapalli</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="2302.14782v1-abstract-short" style="display: inline;"> The stellar population environments associated with fast radio burst (FRB) sources provide important insights for developing their progenitor theories. We expand the diversity of known FRB host environments by reporting two FRBs in massive galaxy clusters discovered by the Deep Synoptic Array (DSA-110) during its commissioning observations. FRB 20220914A has been localized to a star-forming, late-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.14782v1-abstract-full').style.display = 'inline'; document.getElementById('2302.14782v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.14782v1-abstract-full" style="display: none;"> The stellar population environments associated with fast radio burst (FRB) sources provide important insights for developing their progenitor theories. We expand the diversity of known FRB host environments by reporting two FRBs in massive galaxy clusters discovered by the Deep Synoptic Array (DSA-110) during its commissioning observations. FRB 20220914A has been localized to a star-forming, late-type galaxy at a redshift of 0.1139 with multiple starbursts at lookback times less than $\sim$3.5 Gyr in the Abell 2310 galaxy cluster. Although the host galaxy of FRB 20220914A is similar to typical FRB hosts, the FRB 20220509G host stands out as a quiescent, early-type galaxy at a redshift of 0.0894 in the Abell 2311 galaxy cluster. The discovery of FRBs in both late and early-type galaxies adds to the body of evidence that the FRB sources have multiple formation channels. Therefore, even though FRB hosts are typically star-forming, there must exist formation channels consistent with old stellar population in galaxies. The varied star formation histories of the two FRB hosts we report indicate a wide delay-time distribution of FRB progenitors. Future work in constraining the FRB delay-time distribution, using methods we develop herein, will prove crucial in determining the evolutionary histories of FRB sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.14782v1-abstract-full').style.display = 'none'; document.getElementById('2302.14782v1-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 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">18 pages, 9 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/2301.01000">arXiv:2301.01000</a> <span> [<a href="https://arxiv.org/pdf/2301.01000">pdf</a>, <a href="https://arxiv.org/format/2301.01000">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"> Deep Synoptic Array science: a 50 Mpc fast radio burst constrains the mass of the Milky Way circumgalactic medium </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">Vikram Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Catha%2C+M">Morgan Catha</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+G">Ge Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Cordes%2C+J+M">James M. Cordes</a>, <a href="/search/astro-ph?searchtype=author&query=Faber%2C+J+T">Jakob T. Faber</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">James W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Hallinan%2C+G">Gregg Hallinan</a>, <a href="/search/astro-ph?searchtype=author&query=Harnach%2C+C">Charlie Harnach</a>, <a href="/search/astro-ph?searchtype=author&query=Hellbourg%2C+G">Greg Hellbourg</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Rick Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Hodge%2C+D">David Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">Mark Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+C">Casey Law</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+P">Paul Rasmussen</a>, <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+K">Kritti Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Sherman%2C+M+B">Myles B. Sherman</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+J">Jun Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Simard%2C+D">Dana Simard</a>, <a href="/search/astro-ph?searchtype=author&query=Somalwar%2C+J+J">Jean J. Somalwar</a>, <a href="/search/astro-ph?searchtype=author&query=Squillace%2C+R">Reynier Squillace</a>, <a href="/search/astro-ph?searchtype=author&query=Weinreb%2C+S">Sander Weinreb</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D+P">David P. Woody</a>, <a href="/search/astro-ph?searchtype=author&query=Yadlapalli%2C+N">Nitika Yadlapalli</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="2301.01000v1-abstract-short" style="display: inline;"> We present the Deep Synoptic Array (DSA-110) discovery and interferometric localization of the so far non-repeating FRB 20220319D. The FRB originates in a young, rapidly star-forming barred spiral galaxy, IRAS 02044$+$7048, at just 50 Mpc. Although the NE2001 and YMW16 models for the Galactic interstellar-medium (ISM) contribution to the DM of FRB 20220319D exceed its total observed DM, we show th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.01000v1-abstract-full').style.display = 'inline'; document.getElementById('2301.01000v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.01000v1-abstract-full" style="display: none;"> We present the Deep Synoptic Array (DSA-110) discovery and interferometric localization of the so far non-repeating FRB 20220319D. The FRB originates in a young, rapidly star-forming barred spiral galaxy, IRAS 02044$+$7048, at just 50 Mpc. Although the NE2001 and YMW16 models for the Galactic interstellar-medium (ISM) contribution to the DM of FRB 20220319D exceed its total observed DM, we show that uncertainties in these models accommodate an extragalactic origin for the burst. We derive a conservative upper limit on the DM contributed by the circumgalactic medium (CGM) of the Milky Way: the limit is either 28.7 pc cm$^{-3}$ and 47.3 pc cm$^{-3}$, depending on which of two pulsars nearby on the sky to FRB 20220319D is used to estimate the ISM DM. These limits both imply that the total Galactic CGM mass is $<10^{11}M_{\odot}$, and that the baryonic mass of the Milky Way is $\lesssim60\%$ of the cosmological average given the total halo mass. More stringent albeit less conservative constraints are possible when the DMs of pulsars in the distant globular cluster M53 are additionally considered. Although our constraints are sensitive to possible anisotropy in the CGM and to the assumed form of the radial-density profile, they are not subject to uncertainties in the chemical and thermal properties of the CGM. Our results strongly support scenarios commonly predicted by galaxy-formation simulations wherein feedback processes expel baryonic matter from the halos of galaxies like the Milky Way. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.01000v1-abstract-full').style.display = 'none'; document.getElementById('2301.01000v1-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 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">17 pages, 8 figures, 3 tables, submitted to AAS Journals</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.09049">arXiv:2211.09049</a> <span> [<a href="https://arxiv.org/pdf/2211.09049">pdf</a>, <a href="https://arxiv.org/format/2211.09049">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/10.3847/2041-8213/acc4b6">10.3847/2041-8213/acc4b6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Deep Synoptic Array science I: discovery of the host galaxy of FRB 20220912A </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">Vikram Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Catha%2C+M">Morgan Catha</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+G">Ge Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Faber%2C+J+T">Jakob T. Faber</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">James W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Hallinan%2C+G">Gregg Hallinan</a>, <a href="/search/astro-ph?searchtype=author&query=Harnach%2C+C">Charlie Harnach</a>, <a href="/search/astro-ph?searchtype=author&query=Hellbourg%2C+G">Greg Hellbourg</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+R">Rick Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Hodge%2C+D">David Hodge</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">Mark Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Law%2C+C">Casey Law</a>, <a href="/search/astro-ph?searchtype=author&query=Rasmussen%2C+P">Paul Rasmussen</a>, <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+K">Kritti Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Sherman%2C+M+B">Myles B. Sherman</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+J">Jun Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Simard%2C+D">Dana Simard</a>, <a href="/search/astro-ph?searchtype=author&query=Squillace%2C+R">Reynier Squillace</a>, <a href="/search/astro-ph?searchtype=author&query=Weinreb%2C+S">Sander Weinreb</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D+P">David P. Woody</a>, <a href="/search/astro-ph?searchtype=author&query=Yadlapalli%2C+N">Nitika Yadlapalli</a>, <a href="/search/astro-ph?searchtype=author&query=Ahumada%2C+T">Tomas Ahumada</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+D">Dillon Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Fremling%2C+C">Christoffer Fremling</a> , et al. (3 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="2211.09049v1-abstract-short" style="display: inline;"> We report the detection and interferometric localization of the repeating fast radio burst (FRB) source FRB 20220912A during commissioning observations with the Deep Synoptic Array (DSA-110). Two bursts were detected from FRB 20220912A, one each on 2022 October 18 and 2022 October 25. The best-fit position is (R.A. J2000, decl. J2000) = (23:09:04.9, +48:42:25.4), with a 90% confidence error ellips… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.09049v1-abstract-full').style.display = 'inline'; document.getElementById('2211.09049v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.09049v1-abstract-full" style="display: none;"> We report the detection and interferometric localization of the repeating fast radio burst (FRB) source FRB 20220912A during commissioning observations with the Deep Synoptic Array (DSA-110). Two bursts were detected from FRB 20220912A, one each on 2022 October 18 and 2022 October 25. The best-fit position is (R.A. J2000, decl. J2000) = (23:09:04.9, +48:42:25.4), with a 90% confidence error ellipse of $\pm2$ arcsec and $\pm1$ arcsec in right ascension and declination respectively. The two bursts have disparate polarization properties and temporal profiles. We find a Faraday rotation measure that is consistent with the low value of $+0.6$ rad m$^{-2}$ reported by CHIME/FRB. The DSA-110 localization overlaps with the galaxy PSO J347.2702+48.7066 at a redshift $z=0.0771$, which we identify as the likely host. PSO J347.2702$+$48.7066 has a stellar mass of approximately $10^{10}M_{\odot}$, modest internal dust extinction, and a star-formation rate likely in excess of $0.1\,M_{\odot}$ yr$^{-1}$. The host-galaxy contribution to the dispersion measure is likely $\lesssim50$ pc cm$^{-3}$. The FRB 20220912A source is therefore likely viewed along a tenuous plasma column through the host galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.09049v1-abstract-full').style.display = 'none'; document.getElementById('2211.09049v1-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 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">10 pages, 7 figures, 2 tables, submitted to AAS Journals</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.02600">arXiv:2202.02600</a> <span> [<a href="https://arxiv.org/pdf/2202.02600">pdf</a>, <a href="https://arxiv.org/format/2202.02600">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/ac531d">10.3847/1538-4357/ac531d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigating the blazar TXS 0506+056 through sharp multi-wavelength eyes during 2017-2019 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=MAGIC+Collaboration"> MAGIC Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/astro-ph?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/astro-ph?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/astro-ph?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardos%2C+M">M. Bernardos</a>, <a href="/search/astro-ph?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/astro-ph?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+W">W. Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a>, <a href="/search/astro-ph?searchtype=author&query=Biland%2C+A">A. Biland</a>, <a href="/search/astro-ph?searchtype=author&query=Blanch%2C+O">O. Blanch</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6kenkamp%2C+H">H. B枚kenkamp</a> , et al. (192 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="2202.02600v2-abstract-short" style="display: inline;"> The blazar TXS 0506+056 got into the spotlight of the astrophysical community in September 2017, when a high-energy neutrino detected by IceCube (IceCube-170922A) was associated at the 3 $蟽$ level to a $纬$-ray flare from this source. This multi-messenger photon-neutrino association remains, as per today, the most significant one ever observed. TXS 0506+056 was a poorly studied object before the Ic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.02600v2-abstract-full').style.display = 'inline'; document.getElementById('2202.02600v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.02600v2-abstract-full" style="display: none;"> The blazar TXS 0506+056 got into the spotlight of the astrophysical community in September 2017, when a high-energy neutrino detected by IceCube (IceCube-170922A) was associated at the 3 $蟽$ level to a $纬$-ray flare from this source. This multi-messenger photon-neutrino association remains, as per today, the most significant one ever observed. TXS 0506+056 was a poorly studied object before the IceCube-170922A event. To better characterize its broad-band emission, we organized a multi-wavelength campaign lasting 16 months (November 2017 to February 2019), covering the radio-band (Mets盲hovi, OVRO), the optical/UV (ASAS-SN, KVA, REM, Swift/UVOT), the X-rays (Swift/XRT, NuSTAR), the high-energy $纬$ rays (Fermi/LAT) and the very-high-energy (VHE) $纬$ rays (MAGIC). In $纬$ rays, the behaviour of the source was significantly different from the 2017 one: MAGIC observations show the presence of flaring activity during December 2018, while the source only shows an excess at the 4$蟽$ level during the rest of the campaign (74 hours of accumulated exposure); Fermi/LAT observations show several short (days-to-week timescale) flares, different from the long-term brightening of 2017. No significant flares are detected at lower energies. The radio light curve shows an increasing flux trend, not seen in other wavelengths. We model the multi-wavelength spectral energy distributions in a lepto-hadronic scenario, in which the hadronic emission emerges as Bethe-Heitler and pion-decay cascade in the X-rays and VHE $纬$ rays. According to the model presented here, the December 2018 $纬$-ray flare was connected to a neutrino emission that was too brief and not bright enough to be detected by current neutrino instruments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.02600v2-abstract-full').style.display = 'none'; document.getElementById('2202.02600v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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, 6 figures; V2 to match published version, typo fixed</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.01110">arXiv:2201.01110</a> <span> [<a href="https://arxiv.org/pdf/2201.01110">pdf</a>, <a href="https://arxiv.org/format/2201.01110">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/10.3847/1538-4357/ac469e">10.3847/1538-4357/ac469e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New Tests of Millilensing in the Blazar PKS 1413+135 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Peirson%2C+A+L">A. L. Peirson</a>, <a href="/search/astro-ph?searchtype=author&query=Liodakis%2C+I">I. Liodakis</a>, <a href="/search/astro-ph?searchtype=author&query=Readhead%2C+A+C+S">A. C. S. Readhead</a>, <a href="/search/astro-ph?searchtype=author&query=Lister%2C+M+L">M. L. Lister</a>, <a href="/search/astro-ph?searchtype=author&query=Perlman%2C+E+S">E. S. Perlman</a>, <a href="/search/astro-ph?searchtype=author&query=Aller%2C+M+F">M. F. Aller</a>, <a href="/search/astro-ph?searchtype=author&query=Blandford%2C+R+D">R. D. Blandford</a>, <a href="/search/astro-ph?searchtype=author&query=Grainge%2C+K+J+B">K. J. B. Grainge</a>, <a href="/search/astro-ph?searchtype=author&query=Green%2C+D+A">D. A. Green</a>, <a href="/search/astro-ph?searchtype=author&query=Gurwell%2C+M+A">M. A. Gurwell</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M+W">M. W. Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Hovatta%2C+T">T. Hovatta</a>, <a href="/search/astro-ph?searchtype=author&query=Kiehlmann%2C+S">S. Kiehlmann</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%A4hteenm%C3%A4ki%2C+A">A. L盲hteenm盲ki</a>, <a href="/search/astro-ph?searchtype=author&query=Max-Moerbeck%2C+W">W. Max-Moerbeck</a>, <a href="/search/astro-ph?searchtype=author&query=Mcaloone%2C+T">T. Mcaloone</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Neill%2C+S">S. O'Neill</a>, <a href="/search/astro-ph?searchtype=author&query=Pavlidou%2C+V">V. Pavlidou</a>, <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+T+J">T. J. Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">V. Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Reeves%2C+R+A">R. A. Reeves</a>, <a href="/search/astro-ph?searchtype=author&query=Scott%2C+P+F">P. F. Scott</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+G+B">G. B. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Titterington%2C+D+J">D. J. Titterington</a>, <a href="/search/astro-ph?searchtype=author&query=Tornikoski%2C+M">M. Tornikoski</a> , et al. (4 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="2201.01110v2-abstract-short" style="display: inline;"> Symmetric Achromatic Variability (SAV) is a rare form of radio variability in blazars that has been attributed to gravitational millilensing by a ~$10^2 - 10^5$ $M_\odot$ mass condensate. Four SAVs have been identified between 1980 and 2020 in the long-term radio monitoring data of the blazar PKS 1413+135. We show that all four can be fitted with the same, unchanging, gravitational lens model. If… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.01110v2-abstract-full').style.display = 'inline'; document.getElementById('2201.01110v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.01110v2-abstract-full" style="display: none;"> Symmetric Achromatic Variability (SAV) is a rare form of radio variability in blazars that has been attributed to gravitational millilensing by a ~$10^2 - 10^5$ $M_\odot$ mass condensate. Four SAVs have been identified between 1980 and 2020 in the long-term radio monitoring data of the blazar PKS 1413+135. We show that all four can be fitted with the same, unchanging, gravitational lens model. If SAV is due to gravitational millilensing, PKS 1413+135 provides a unique system for studying active galactic nuclei with unprecedented microarcsecond resolution, as well as for studying the nature of the millilens itself. We discuss two possible candidates for the putative millilens: a giant molecular cloud hosted in the intervening edge-on spiral galaxy, and an undetected dwarf galaxy with a massive black hole. We find a significant dependence of SAV crossing time on frequency, which could indicate a fast shock moving in a slower underlying flow. We also find tentative evidence for a 989-day periodicity in the SAVs, which, if real, makes possible the prediction of future SAVs: the next three windows for possible SAVs begin in August 2022, May 2025, and February 2028. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.01110v2-abstract-full').style.display = 'none'; document.getElementById('2201.01110v2-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 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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 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/2112.04194">arXiv:2112.04194</a> <span> [<a href="https://arxiv.org/pdf/2112.04194">pdf</a>, <a href="https://arxiv.org/format/2112.04194">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/ac4d95">10.3847/1538-4357/ac4d95 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength variability power spectrum analysis of the blazars 3C 279 and PKS 1510-089 on multiple timescales </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Goyal%2C+A">Arti Goyal</a>, <a href="/search/astro-ph?searchtype=author&query=Soida%2C+M">Marian Soida</a>, <a href="/search/astro-ph?searchtype=author&query=Stawarz%2C+L">Lukasz Stawarz</a>, <a href="/search/astro-ph?searchtype=author&query=Wiita%2C+P+J">Paul J. Wiita</a>, <a href="/search/astro-ph?searchtype=author&query=Nilsson%2C+K">Kari Nilsson</a>, <a href="/search/astro-ph?searchtype=author&query=Jorstad%2C+S">Svetlana Jorstad</a>, <a href="/search/astro-ph?searchtype=author&query=Marscher%2C+A+P">Alan P. Marscher</a>, <a href="/search/astro-ph?searchtype=author&query=Aller%2C+M+F">Margo F. Aller</a>, <a href="/search/astro-ph?searchtype=author&query=Aller%2C+H+D">Hugh D. Aller</a>, <a href="/search/astro-ph?searchtype=author&query=Lahteenmaki%2C+A">Anne Lahteenmaki</a>, <a href="/search/astro-ph?searchtype=author&query=Hovatta%2C+T">Talvikki Hovatta</a>, <a href="/search/astro-ph?searchtype=author&query=Zola%2C+S">Staszek Zola</a>, <a href="/search/astro-ph?searchtype=author&query=Nalewajko%2C+K">Krzysztof Nalewajko</a>, <a href="/search/astro-ph?searchtype=author&query=Tornikoski%2C+M">Merja Tornikoski</a>, <a href="/search/astro-ph?searchtype=author&query=Tammi%2C+J">Joni Tammi</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">Mark Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Kiehlmann%2C+S">Sebastian Kiehlmann</a>, <a href="/search/astro-ph?searchtype=author&query=Readhead%2C+A+C+S">Anthony C. S. Readhead</a>, <a href="/search/astro-ph?searchtype=author&query=Max-Moerbeck%2C+W">Walter Max-Moerbeck</a>, <a href="/search/astro-ph?searchtype=author&query=Lindfors%2C+E">Elina Lindfors</a>, <a href="/search/astro-ph?searchtype=author&query=Ramazani%2C+V+F">Vandad Fallah Ramazani</a>, <a href="/search/astro-ph?searchtype=author&query=Reichart%2C+D+E">D. E. Reichart</a>, <a href="/search/astro-ph?searchtype=author&query=Caton%2C+D+B">D. B. Caton</a>, <a href="/search/astro-ph?searchtype=author&query=Valverde%2C+J">Janeth Valverde</a>, <a href="/search/astro-ph?searchtype=author&query=Horan%2C+D">Deirdre Horan</a> , et al. (2 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="2112.04194v2-abstract-short" style="display: inline;"> We present the results of variability power spectral density (PSD) analysis using multiwavelength radio to GeV\,$纬$-ray light curves covering decades/years to days/minutes timescales for the blazars 3C 279 and PKS 1510-089. The PSDs are modeled as single power-laws, and the best-fit spectral shape is derived using the `power spectral response' method. With more than ten years of data obtained with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.04194v2-abstract-full').style.display = 'inline'; document.getElementById('2112.04194v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.04194v2-abstract-full" style="display: none;"> We present the results of variability power spectral density (PSD) analysis using multiwavelength radio to GeV\,$纬$-ray light curves covering decades/years to days/minutes timescales for the blazars 3C 279 and PKS 1510-089. The PSDs are modeled as single power-laws, and the best-fit spectral shape is derived using the `power spectral response' method. With more than ten years of data obtained with weekly/daily sampling intervals, most of the PSDs cover ~2-4 decades in temporal frequency; moreover, in the optical band, the PSDs cover ~6 decades for 3C 279 due to the availability of intranight light curves. Our main results are the following: (1) on timescales ranging from decades to days, the synchrotron and the inverse Compton spectral components, in general, exhibit red-noise (slope ~2) and flicker-noise (slope ~1) type variability, respectively; (2) the slopes of $纬$-ray variability PSDs obtained using a 3-hr integration bin and a 3-weeks total duration exhibit a range between ~1.4 and ~2.0 (mean slope = 1.60$\pm$0.70), consistent within errors with the slope on longer timescales; (3) comparisons of fractional variability indicate more power on timescales $\leq$100\, days at $纬$-ray frequencies as compared to longer wavelengths, in general (except between $纬$-ray and optical frequencies for PKS 1510$-$089); (4) the normalization of intranight optical PSDs for 3C\,279 appears to be a simple extrapolation from longer timescales, indicating a continuous (single) process driving the variability at optical wavelengths; (5) the emission at optical/infrared wavelengths may involve a combination of disk and jet processes for PKS\,1510$-$089. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.04194v2-abstract-full').style.display = 'none'; document.getElementById('2112.04194v2-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> 20 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </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">ApJ accepted. Comments are welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.14025">arXiv:2111.14025</a> <span> [<a href="https://arxiv.org/pdf/2111.14025">pdf</a>, <a href="https://arxiv.org/format/2111.14025">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/stab3473">10.1093/mnras/stab3473 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Magnetic Field Strengths of the Synchrotron Self-Absorption Region in the Jet of CTA 102 During Radio Flares </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kim%2C+S">Sang-Hyun Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+S">Sang-Sung Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J+W">Jee Won Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Hodgson%2C+J+A">Jeffrey A. Hodgson</a>, <a href="/search/astro-ph?searchtype=author&query=Kang%2C+S">Sincheol Kang</a>, <a href="/search/astro-ph?searchtype=author&query=Algaba%2C+J">Juan-Carlos Algaba</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Jae-Young Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">Mark Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">Ivan Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Fuentes%2C+A">Antonio Fuentes</a>, <a href="/search/astro-ph?searchtype=author&query=Escudero%2C+J">Juan Escudero</a>, <a href="/search/astro-ph?searchtype=author&query=Myserlis%2C+I">Ioannis Myserlis</a>, <a href="/search/astro-ph?searchtype=author&query=Traianou%2C+E">Efthalia Traianou</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%A4hteenm%C3%A4ki%2C+A">Anne L盲hteenm盲ki</a>, <a href="/search/astro-ph?searchtype=author&query=Tornikoski%2C+M">Merja Tornikoski</a>, <a href="/search/astro-ph?searchtype=author&query=Tammi%2C+J">Joni Tammi</a>, <a href="/search/astro-ph?searchtype=author&query=Ramakrishnan%2C+V">Venkatessh Ramakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%A4rvel%C3%A4%2C+E">Emilia J盲rvel盲</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="2111.14025v1-abstract-short" style="display: inline;"> CTA 102 is a blazar implying that its relativistic jet points towards Earth and emits synchrotron radiation produced by energetic particles gyrating in the magnetic field. This study aims to figure out the physical origins of radio flares in the jet, including the connection between the magnetic field and the radio flares. The dataset in the range 2.6-343.5 GHz was collected over a period of 5.5 y… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14025v1-abstract-full').style.display = 'inline'; document.getElementById('2111.14025v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.14025v1-abstract-full" style="display: none;"> CTA 102 is a blazar implying that its relativistic jet points towards Earth and emits synchrotron radiation produced by energetic particles gyrating in the magnetic field. This study aims to figure out the physical origins of radio flares in the jet, including the connection between the magnetic field and the radio flares. The dataset in the range 2.6-343.5 GHz was collected over a period of 5.5 years (2012 November 20-2018 September 23). During the data collection period, seven flares at 15 GHz with a range of the variability time-scale of roughly 26-171 days were detected. The quasi-simultaneous radio data were used to investigate the synchrotron spectrum of the source. We found that the synchrotron radiation is self-absorbed. The turnover frequency and the peak flux density of the synchrotron self-absorption (SSA) spectra are in the ranges of 42-167 GHz and 0.9-10.2 Jy, respectively. From the SSA spectra, we derived the SSA magnetic field strengths to be 9.20 mG, 12.28 mG, and 50.97 mG on 2013 December 24, 2014 February 28, and 2018 January 13, respectively. We also derived the equipartition magnetic field strengths to be in the range 24-109 mG. The equipartition magnetic field strengths are larger than the SSA magnetic field strengths in most cases, which indicates that particle energy mainly dominates in the jet. Our results suggest that the flares in the jet of CTA 102 originated due to particle acceleration. We propose the possible mechanisms of particle acceleration. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14025v1-abstract-full').style.display = 'none'; document.getElementById('2111.14025v1-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </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, 8 figures, 6 tables, 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/2111.12926">arXiv:2111.12926</a> <span> [<a href="https://arxiv.org/pdf/2111.12926">pdf</a>, <a href="https://arxiv.org/ps/2111.12926">ps</a>, <a href="https://arxiv.org/format/2111.12926">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/stab3454">10.1093/mnras/stab3454 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multiwavelength study of the gravitationally lensed blazar QSO B0218+357 between 2016 and 2020 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=MAGIC+Collaboration"> MAGIC Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/astro-ph?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/astro-ph?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/astro-ph?searchtype=author&query=Bellizzi%2C+L">L. Bellizzi</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardos%2C+M">M. Bernardos</a>, <a href="/search/astro-ph?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/astro-ph?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+W">W. Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a>, <a href="/search/astro-ph?searchtype=author&query=Biland%2C+A">A. Biland</a>, <a href="/search/astro-ph?searchtype=author&query=Blanch%2C+O">O. Blanch</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnoli%2C+G">G. Bonnoli</a> , et al. (186 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="2111.12926v1-abstract-short" style="display: inline;"> We report multiwavelength observations of the gravitationally lensed blazar QSO B0218+357 in 2016-2020. Optical, X-ray and GeV flares were detected. The contemporaneous MAGIC observations do not show significant very-high-energy (VHE, >= 100 GeV) gamma-ray emission. The lack of enhancement in radio emission measured by OVRO indicates the multi-zone nature of the emission from this object. We const… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.12926v1-abstract-full').style.display = 'inline'; document.getElementById('2111.12926v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.12926v1-abstract-full" style="display: none;"> We report multiwavelength observations of the gravitationally lensed blazar QSO B0218+357 in 2016-2020. Optical, X-ray and GeV flares were detected. The contemporaneous MAGIC observations do not show significant very-high-energy (VHE, >= 100 GeV) gamma-ray emission. The lack of enhancement in radio emission measured by OVRO indicates the multi-zone nature of the emission from this object. We constrain the VHE duty cycle of the source to be < 16 2014-like flares per year (95% confidence). For the first time for this source, a broadband low-state SED is constructed with a deep exposure up to the VHE range. A flux upper limit on the low-state VHE gamma-ray emission of an order of magnitude below that of the 2014 flare is determined. The X-ray data are used to fit the column density of (8.10 +- 0.93 stat ) x 10^21 cm^-2 of the dust in the lensing galaxy. VLBI observations show a clear radio core and jet components in both lensed images, yet no significant movement of the components is seen. The radio measurements are used to model the source-lens-observer geometry and determine the magnifications and time delays for both components. The quiescent emission is modeled with the high-energy bump explained as a combination of synchrotron-self-Compton and external Compton emission from a region located outside of the broad line region. The bulk of the low-energy emission is explained as originating from a tens-of-parsecs scale jet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.12926v1-abstract-full').style.display = 'none'; document.getElementById('2111.12926v1-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> 25 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </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, 12 figures, 5 tables, 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/2111.02436">arXiv:2111.02436</a> <span> [<a href="https://arxiv.org/pdf/2111.02436">pdf</a>, <a href="https://arxiv.org/format/2111.02436">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/ac504b">10.3847/2041-8213/ac504b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Unanticipated Phenomenology of the Blazar PKS~2131$-$021: A Unique Super-Massive Black Hole Binary Candidate </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=O%27Neill%2C+S">S. O'Neill</a>, <a href="/search/astro-ph?searchtype=author&query=Kiehlmann%2C+S">S. Kiehlmann</a>, <a href="/search/astro-ph?searchtype=author&query=Readhead%2C+A+C+S">A. C. S. Readhead</a>, <a href="/search/astro-ph?searchtype=author&query=Aller%2C+M+F">M. F. Aller</a>, <a href="/search/astro-ph?searchtype=author&query=Blandford%2C+R+D">R. D. Blandford</a>, <a href="/search/astro-ph?searchtype=author&query=Liodakis%2C+I">I. Liodakis</a>, <a href="/search/astro-ph?searchtype=author&query=Lister%2C+M+L">M. L. Lister</a>, <a href="/search/astro-ph?searchtype=author&query=Mr%C3%B3z%2C+P">P. Mr贸z</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Dea%2C+C+P">C. P. O'Dea</a>, <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+T+J">T. J. Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">V. Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Vallisneri%2C+M">M. Vallisneri</a>, <a href="/search/astro-ph?searchtype=author&query=Cleary%2C+K+A">K. A. Cleary</a>, <a href="/search/astro-ph?searchtype=author&query=Graham%2C+M+J">M. J. Graham</a>, <a href="/search/astro-ph?searchtype=author&query=Grainge%2C+K+J+B">K. J. B. Grainge</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M+W">M. W. Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Hovatta%2C+T">T. Hovatta</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%A4hteenm%C3%A4ki%2C+A">A. L盲hteenm盲ki</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">J. W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Lazio%2C+T+J+W">T. J. W. Lazio</a>, <a href="/search/astro-ph?searchtype=author&query=Max-Moerbeck%2C+W">W. Max-Moerbeck</a>, <a href="/search/astro-ph?searchtype=author&query=Pavlidou%2C+V">V. Pavlidou</a>, <a href="/search/astro-ph?searchtype=author&query=Prince%2C+T+A">T. A. Prince</a>, <a href="/search/astro-ph?searchtype=author&query=Reeves%2C+R+A">R. A. Reeves</a>, <a href="/search/astro-ph?searchtype=author&query=Tornikoski%2C+M">M. Tornikoski</a> , et al. (2 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="2111.02436v2-abstract-short" style="display: inline;"> Most large galaxies host supermassive black holes in their nuclei and are subject to mergers, which can produce a supermassive black hole binary (SMBHB), and hence periodic signatures due to orbital motion. We report unique periodic radio flux density variations in the blazar PKS~2131$-$021, which strongly suggest an SMBHB with an orbital separation of $\sim 0.001-0.01$ pc. Our 45.1-year radio lig… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.02436v2-abstract-full').style.display = 'inline'; document.getElementById('2111.02436v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.02436v2-abstract-full" style="display: none;"> Most large galaxies host supermassive black holes in their nuclei and are subject to mergers, which can produce a supermassive black hole binary (SMBHB), and hence periodic signatures due to orbital motion. We report unique periodic radio flux density variations in the blazar PKS~2131$-$021, which strongly suggest an SMBHB with an orbital separation of $\sim 0.001-0.01$ pc. Our 45.1-year radio light curve shows two epochs of strong sinusoidal variation with the same period and phase to within $<2\%$ and $\sim 10\%$, respectively, straddling a 20-year period when this variation was absent. Our simulated light curves accurately reproduce the ``red noise'' of this object, and Lomb-Scargle, weighted wavelet Z-transform, and least-squares sine wave analyses demonstrate conclusively, at the $4.6蟽$ significance level, that the periodicity in this object is not due to random fluctuations in flux density. The observed period translates to $2.082\pm 0.003$ years in the rest frame at the $z=1.285$ redshift of PKS~2131$-$021. The periodic variation in PKS~2131$-$021 is remarkably sinusoidal. We present a model in which orbital motion, combined with the strong Doppler boosting of the approaching relativistic jet, produces a sine-wave modulation in the flux density which easily fits the observations. Given the rapidly-developing field of gravitational wave experiments with pulsar timing arrays, closer counterparts to PKS~2131$-$021 and searches using the techniques we have developed are strongly motivated. These results constitute a compelling demonstration that the phenomenology, not the theory, must provide the lead in this field. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.02436v2-abstract-full').style.display = 'none'; document.getElementById('2111.02436v2-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> 24 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </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">24 pages, 13 figure, 3 Tables, accepted for publication in 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/2012.11380">arXiv:2012.11380</a> <span> [<a href="https://arxiv.org/pdf/2012.11380">pdf</a>, <a href="https://arxiv.org/format/2012.11380">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/10.1051/0004-6361/202039687">10.1051/0004-6361/202039687 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> VHE gamma-ray detection of FSRQ QSO B1420+326 and modeling of its enhanced broadband state in 2020 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/astro-ph?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/astro-ph?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Baquero%2C+A">A. Baquero</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/astro-ph?searchtype=author&query=Bellizzi%2C+L">L. Bellizzi</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardos%2C+M">M. Bernardos</a>, <a href="/search/astro-ph?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/astro-ph?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+W">W. Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a>, <a href="/search/astro-ph?searchtype=author&query=Biland%2C+A">A. Biland</a>, <a href="/search/astro-ph?searchtype=author&query=Blanch%2C+O">O. Blanch</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnoli%2C+G">G. Bonnoli</a>, <a href="/search/astro-ph?searchtype=author&query=Bo%C5%A1njak%2C+%C5%BD">沤. Bo拧njak</a>, <a href="/search/astro-ph?searchtype=author&query=Busetto%2C+G">G. Busetto</a> , et al. (209 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="2012.11380v1-abstract-short" style="display: inline;"> Context. QSO B1420+326 is a blazar classified as a Flat Spectrum Radio Quasar (FSRQ). In the beginning of 2020 it underwent an enhanced flux state. An extensive multiwavelength campaign allowed us to trace the evolution of the flare. Aims. We search for VHE gamma-ray emission from QSO B1420+326 during this flaring state. We aim to characterize and model the broadband emission of the source over di… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.11380v1-abstract-full').style.display = 'inline'; document.getElementById('2012.11380v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.11380v1-abstract-full" style="display: none;"> Context. QSO B1420+326 is a blazar classified as a Flat Spectrum Radio Quasar (FSRQ). In the beginning of 2020 it underwent an enhanced flux state. An extensive multiwavelength campaign allowed us to trace the evolution of the flare. Aims. We search for VHE gamma-ray emission from QSO B1420+326 during this flaring state. We aim to characterize and model the broadband emission of the source over different phases of the flare. Methods. The source was observed with a number of instruments in radio, near infrared, optical (including polarimetry and spectroscopy), ultra-violet, X-ray and gamma-ray bands. We use dedicated optical spectroscopy results to estimate the accretion disk and the dust torus luminosity. We perform spectral energy distribution modeling in the framework of combined Synchrotron-Self-Compton and External Compton scenario in which the electron energy distribution is partially determined from acceleration and cooling processes. Results. During the enhanced state the flux of both SED components drastically increased and the peaks were shifted to higher energies. Follow up observations with the MAGIC telescopes led to the detection of very-high-energy gamma-ray emission from this source, making it one of only a handful of FSRQs known in this energy range. Modeling allows us to constrain the evolution of the magnetic field and electron energy distribution in the emission region. The gamma-ray flare was accompanied by a rotation of the optical polarization vector during a low polarization state. Also, a new, superluminal radio knot contemporaneously appeared in the radio image of the jet. The optical spectroscopy shows a prominent FeII bump with flux evolving together with the continuum emission and a MgII line with varying equivalent width. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.11380v1-abstract-full').style.display = 'none'; document.getElementById('2012.11380v1-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </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">20 pages, 15 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 647, A163 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.04045">arXiv:2012.04045</a> <span> [<a href="https://arxiv.org/pdf/2012.04045">pdf</a>, <a href="https://arxiv.org/format/2012.04045">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/10.3847/1538-4357/abd08c">10.3847/1538-4357/abd08c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Relativistic Jet Orientation and Host Galaxy of the Peculiar Blazar PKS 1413+135 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Readhead%2C+A+C+S">A. C. S. Readhead</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+V">V. Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Liodakis%2C+I">I. Liodakis</a>, <a href="/search/astro-ph?searchtype=author&query=Lister%2C+M+L">M. L. Lister</a>, <a href="/search/astro-ph?searchtype=author&query=Singh%2C+V">V. Singh</a>, <a href="/search/astro-ph?searchtype=author&query=Aller%2C+M+F">M. F. Aller</a>, <a href="/search/astro-ph?searchtype=author&query=Blandford%2C+R+D">R. D. Blandford</a>, <a href="/search/astro-ph?searchtype=author&query=Browne%2C+I+W+A">I. W. A. Browne</a>, <a href="/search/astro-ph?searchtype=author&query=Gorjian%2C+V">V. Gorjian</a>, <a href="/search/astro-ph?searchtype=author&query=Grainge%2C+K+J+B">K. J. B. Grainge</a>, <a href="/search/astro-ph?searchtype=author&query=Gurwell%2C+M+A">M. A. Gurwell</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M+W">M. W. Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Hovatta%2C+T">T. Hovatta</a>, <a href="/search/astro-ph?searchtype=author&query=Kiehlmann%2C+S">S. Kiehlmann</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%A4hteenm%C3%A4ki%2C+A">A. L盲hteenm盲ki</a>, <a href="/search/astro-ph?searchtype=author&query=McAloone%2C+T">T. McAloone</a>, <a href="/search/astro-ph?searchtype=author&query=Max-Moerbeck%2C+W">W. Max-Moerbeck</a>, <a href="/search/astro-ph?searchtype=author&query=Pavlidou%2C+V">V. Pavlidou</a>, <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+T+J">T. J. Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Peirson%2C+A+L">A. L. Peirson</a>, <a href="/search/astro-ph?searchtype=author&query=Perlman%2C+E+S">E. S. Perlman</a>, <a href="/search/astro-ph?searchtype=author&query=Reeves%2C+R+A">R. A. Reeves</a>, <a href="/search/astro-ph?searchtype=author&query=Soifer%2C+B+T">B. T. Soifer</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+G+B">G. B. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Tornikoski%2C+M">M. Tornikoski</a> , et al. (4 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="2012.04045v1-abstract-short" style="display: inline;"> PKS 1413+135 is one of the most peculiar blazars known. Its strange properties led to the hypothesis almost four decades ago that it is gravitationally lensed by a mass concentration associated with an intervening galaxy. It exhibits symmetric achromatic variability, a rare form of variability that has been attributed to gravitational milli-lensing. It has been classified as a BL Lac object, and i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.04045v1-abstract-full').style.display = 'inline'; document.getElementById('2012.04045v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.04045v1-abstract-full" style="display: none;"> PKS 1413+135 is one of the most peculiar blazars known. Its strange properties led to the hypothesis almost four decades ago that it is gravitationally lensed by a mass concentration associated with an intervening galaxy. It exhibits symmetric achromatic variability, a rare form of variability that has been attributed to gravitational milli-lensing. It has been classified as a BL Lac object, and is one of the rare objects in this class with a visible counterjet. BL Lac objects have jet axes aligned close to the line of sight. It has also been classified as a compact symmetric object, which have jet axes not aligned close to the line of sight. Intensive efforts to understand this blazar have hitherto failed to resolve even the questions of the orientation of the relativistic jet, and the host galaxy. Answering these two questions is important as they challenge our understanding of jets in active galactic nuclei and the classification schemes we use to describe them. We show that the jet axis is aligned close to the line of sight and PKS 1413+135 is almost certainly not located in the apparent host galaxy, but is a background object in the redshift range $0.247 < z < 0.5$. The intervening spiral galaxy at $z = 0.247$ provides a natural host for the putative lens responsible for symmetric achromatic variability and is shown to be a Seyfert 2 galaxy. We also show that, as for the radio emission, a "multizone" model is needed to account for the high-energy emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.04045v1-abstract-full').style.display = 'none'; document.getElementById('2012.04045v1-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </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. 28 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/2009.10523">arXiv:2009.10523</a> <span> [<a href="https://arxiv.org/pdf/2009.10523">pdf</a>, <a href="https://arxiv.org/format/2009.10523">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/10.1051/0004-6361/202039481">10.1051/0004-6361/202039481 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Association of IceCube neutrinos with radio sources observed at Owens Valley and Mets盲hovi Radio Observatories </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hovatta%2C+T">T. Hovatta</a>, <a href="/search/astro-ph?searchtype=author&query=Lindfors%2C+E">E. Lindfors</a>, <a href="/search/astro-ph?searchtype=author&query=Kiehlmann%2C+S">S. Kiehlmann</a>, <a href="/search/astro-ph?searchtype=author&query=Max-Moerbeck%2C+W">W. Max-Moerbeck</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">M. Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Liodakis%2C+I">I. Liodakis</a>, <a href="/search/astro-ph?searchtype=author&query=Lahteenmaki%2C+A">A. Lahteenmaki</a>, <a href="/search/astro-ph?searchtype=author&query=Pearson%2C+T+J">T. J. Pearson</a>, <a href="/search/astro-ph?searchtype=author&query=Readhead%2C+A+C+S">A. C. S. Readhead</a>, <a href="/search/astro-ph?searchtype=author&query=Reeves%2C+R+A">R. A. Reeves</a>, <a href="/search/astro-ph?searchtype=author&query=Suutarinen%2C+S">S. Suutarinen</a>, <a href="/search/astro-ph?searchtype=author&query=Tammi%2C+J">J. Tammi</a>, <a href="/search/astro-ph?searchtype=author&query=Tornikoski%2C+M">M. Tornikoski</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="2009.10523v3-abstract-short" style="display: inline;"> Identifying the most likely sources for high-energy neutrino emission has been one of the main topics in high-energy astrophysics ever since the first observation of high-energy neutrinos by the IceCube Neutrino Observatory. Active galactic nuclei with relativistic jets, also known as blazars, have been considered to be one of the main candidates because of their ability to accelerate particles to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.10523v3-abstract-full').style.display = 'inline'; document.getElementById('2009.10523v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.10523v3-abstract-full" style="display: none;"> Identifying the most likely sources for high-energy neutrino emission has been one of the main topics in high-energy astrophysics ever since the first observation of high-energy neutrinos by the IceCube Neutrino Observatory. Active galactic nuclei with relativistic jets, also known as blazars, have been considered to be one of the main candidates because of their ability to accelerate particles to high energies. We study the connection between radio emission and IceCube neutrino events using data from the Owens Valley Radio Observatory (OVRO) and Mets盲hovi Radio Observatory blazar monitoring programs. We identify sources in our radio monitoring sample that are positionally consistent with IceCube high-energy neutrino events. We estimate their mean flux density and variability amplitudes around the neutrino arrival time, and compare these with values from random samples to establish the significance of our results. We find radio source associations within our samples with 15 high-energy neutrino events detected by IceCube. Nearly half of the associated sources are not detected in the $纬$-ray energies, but their radio variability properties and Doppler boosting factors are similar to the $纬$-ray detected objects in our sample, meaning that they could still be potential neutrino emitters. We find that the number of strongly flaring objects in our statistically complete OVRO samples is unlikely to be a random coincidence (at $2蟽$ level). Based on our results, we conclude that although it is clear that not all neutrino events are associated with strong radio flaring blazars, observations of large-amplitude radio flares in a blazar at the same time as a neutrino event are unlikely to be a random coincidence. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.10523v3-abstract-full').style.display = 'none'; document.getElementById('2009.10523v3-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </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 A&A (18 pages, 6 figures). Accepted version (v2) includes changes to methodology and associations, but the main conclusions are unaffected. V3 minor fix to numbers in Sect. 3.3.1. and some language edits</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 650, A83 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2006.04493">arXiv:2006.04493</a> <span> [<a href="https://arxiv.org/pdf/2006.04493">pdf</a>, <a href="https://arxiv.org/format/2006.04493">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/10.1051/0004-6361/202037811">10.1051/0004-6361/202037811 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Testing two-component models on very-high-energy gamma-ray emitting BL Lac objects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=MAGIC+Collaboration"> MAGIC Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Engels%2C+A+A">A. Arbet Engels</a>, <a href="/search/astro-ph?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/astro-ph?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Banerjee%2C+B">B. Banerjee</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Bednarek%2C+W">W. Bednarek</a>, <a href="/search/astro-ph?searchtype=author&query=Bellizzi%2C+L">L. Bellizzi</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/astro-ph?searchtype=author&query=Besenrieder%2C+J">J. Besenrieder</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharyya%2C+W">W. Bhattacharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Bigongiari%2C+C">C. Bigongiari</a>, <a href="/search/astro-ph?searchtype=author&query=Biland%2C+A">A. Biland</a>, <a href="/search/astro-ph?searchtype=author&query=Blanch%2C+O">O. Blanch</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnoli%2C+G">G. Bonnoli</a>, <a href="/search/astro-ph?searchtype=author&query=Bo%C5%A1njak%2C+%C5%BD">沤. Bo拧njak</a>, <a href="/search/astro-ph?searchtype=author&query=Busetto%2C+G">G. Busetto</a>, <a href="/search/astro-ph?searchtype=author&query=Carosi%2C+R">R. Carosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ceribella%2C+G">G. Ceribella</a> , et al. (179 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="2006.04493v1-abstract-short" style="display: inline;"> Context. It has become evident that one-zone synchrotron self-Compton models are not always adequate for very-high-energy (VHE) gamma-ray emitting blazars. While two-component models are performing better, they are difficult to constrain due to the large number of free parameters. Aims. In this work, we make a first attempt to take into account the observational constraints from Very Long Baseline… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.04493v1-abstract-full').style.display = 'inline'; document.getElementById('2006.04493v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.04493v1-abstract-full" style="display: none;"> Context. It has become evident that one-zone synchrotron self-Compton models are not always adequate for very-high-energy (VHE) gamma-ray emitting blazars. While two-component models are performing better, they are difficult to constrain due to the large number of free parameters. Aims. In this work, we make a first attempt to take into account the observational constraints from Very Long Baseline Interferometry (VLBI) data, long-term light curves (radio, optical, and X-rays) and optical polarisation to limit the parameter space for a two-component model and test if it can still reproduce the observed spectral energy distribution (SED) of the blazars. Methods. We selected five TeV BL Lac objects based on the availability of VHE gamma-ray and optical polarisation data. We collected constraints for the jet parameters from VLBI observations. We evaluated the contributions of the two components to the optical flux by means of decomposition of long-term radio and optical light curves as well as modeling of the optical polarisation variability of the objects. We selected eight epochs for these five objects, based on the variability observed at VHE gamma rays, for which we constructed the SEDs that we then modeled with a two-component model. Results. We found parameter sets which can reproduce the broadband SED of the sources in the framework of two-component models considering all available observational constraints from VLBI observations. Moreover, the constraints obtained from the long-term behavior of the sources in the lower energy bands could be used to determine the region where the emission in each band originates. Finally, we attempted to use optical polarisation data to shed new light on the behavior of the two components in the optical band. Our observationally constrained two zone model allows explanation of the entire SED from radio to VHE with two co-located emission regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.04493v1-abstract-full').style.display = 'none'; document.getElementById('2006.04493v1-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 640, A132 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0907.1656">arXiv:0907.1656</a> <span> [<a href="https://arxiv.org/pdf/0907.1656">pdf</a>, <a href="https://arxiv.org/ps/0907.1656">ps</a>, <a href="https://arxiv.org/format/0907.1656">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="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/10.1088/0004-637X/700/2/L132">10.1088/0004-637X/700/2/L132 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dynamically Driven Evolution of the Interstellar Medium in M51 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Koda%2C+J">J. Koda</a>, <a href="/search/astro-ph?searchtype=author&query=Scoville%2C+N">N. Scoville</a>, <a href="/search/astro-ph?searchtype=author&query=Sawada%2C+T">T. Sawada</a>, <a href="/search/astro-ph?searchtype=author&query=La+Vigne%2C+M+A">M. A. La Vigne</a>, <a href="/search/astro-ph?searchtype=author&query=Vogel%2C+S+N">S. N. Vogel</a>, <a href="/search/astro-ph?searchtype=author&query=Potts%2C+A+E">A. E. Potts</a>, <a href="/search/astro-ph?searchtype=author&query=Carpenter%2C+J+M">J. M. Carpenter</a>, <a href="/search/astro-ph?searchtype=author&query=Corder%2C+S+A">S. A. Corder</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+M+C+H">M. C. H. Wright</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+S+M">S. M. White</a>, <a href="/search/astro-ph?searchtype=author&query=Zauderer%2C+B+A">B. A. Zauderer</a>, <a href="/search/astro-ph?searchtype=author&query=Patience%2C+J">J. Patience</a>, <a href="/search/astro-ph?searchtype=author&query=Sargent%2C+A+I">A. I. Sargent</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+D+C+-">D. C. -J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Hawkins%2C+D">D. Hawkins</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">M. Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Kemball%2C+A">A. Kemball</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">J. W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Plambeck%2C+R+L">R. L. Plambeck</a>, <a href="/search/astro-ph?searchtype=author&query=Pound%2C+M+W">M. W. Pound</a>, <a href="/search/astro-ph?searchtype=author&query=Scott%2C+S+L">S. L. Scott</a>, <a href="/search/astro-ph?searchtype=author&query=Teuben%2C+P">P. Teuben</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D+P">D. P. Woody</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="0907.1656v1-abstract-short" style="display: inline;"> We report the highest-fidelity observations of the spiral galaxy M51 in CO emission, revealing the evolution of giant molecular clouds (GMCs) vis-a-vis the large-scale galactic structure and dynamics. The most massive GMCs (so-called GMAs) are first assembled and then broken up as the gas flow through the spiral arms. The GMAs and their H2 molecules are not fully dissociated into atomic gas as p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.1656v1-abstract-full').style.display = 'inline'; document.getElementById('0907.1656v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0907.1656v1-abstract-full" style="display: none;"> We report the highest-fidelity observations of the spiral galaxy M51 in CO emission, revealing the evolution of giant molecular clouds (GMCs) vis-a-vis the large-scale galactic structure and dynamics. The most massive GMCs (so-called GMAs) are first assembled and then broken up as the gas flow through the spiral arms. The GMAs and their H2 molecules are not fully dissociated into atomic gas as predicted in stellar feedback scenarios, but are fragmented into smaller GMCs upon leaving the spiral arms. The remnants of GMAs are detected as the chains of GMCs that emerge from the spiral arms into interarm regions. The kinematic shear within the spiral arms is sufficient to unbind the GMAs against self-gravity. We conclude that the evolution of GMCs is driven by large-scale galactic dynamics --their coagulation into GMAs is due to spiral arm streaming motions upon entering the arms, followed by fragmentation due to shear as they leave the arms on the downstream side. In M51, the majority of the gas remains molecular from arm entry through the inter-arm region and into the next spiral arm passage. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.1656v1-abstract-full').style.display = 'none'; document.getElementById('0907.1656v1-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 July, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2009. </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">6 pages, including 3 figures. Accepted, ApJL</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.700:L132-L136,2009 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0902.2409">arXiv:0902.2409</a> <span> [<a href="https://arxiv.org/pdf/0902.2409">pdf</a>, <a href="https://arxiv.org/ps/0902.2409">ps</a>, <a href="https://arxiv.org/format/0902.2409">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/10.1088/0004-637X/696/2/1374">10.1088/0004-637X/696/2/1374 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dense, Parsec-Scale Clumps near the Great Annihilator </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hodges-Kluck%2C+E+J">E. J. Hodges-Kluck</a>, <a href="/search/astro-ph?searchtype=author&query=Pound%2C+M+W">M. W. Pound</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+A+I">A. I. Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">J. W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M+W">M. W. Hodges</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="0902.2409v1-abstract-short" style="display: inline;"> We report on Combined Array for Research in Millimeter-Wave Astronomy (CARMA) and James Clerk Maxwell Telescope (JCMT) observations toward the Einstein source 1E 1740.7-2942, a LMXB commonly known as the "Great Annihilator." The Great Annihilator is known to be near a small, bright molecular cloud on the sky in a region largely devoid of emission in 12-CO surveys of the Galactic Center. The regi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0902.2409v1-abstract-full').style.display = 'inline'; document.getElementById('0902.2409v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0902.2409v1-abstract-full" style="display: none;"> We report on Combined Array for Research in Millimeter-Wave Astronomy (CARMA) and James Clerk Maxwell Telescope (JCMT) observations toward the Einstein source 1E 1740.7-2942, a LMXB commonly known as the "Great Annihilator." The Great Annihilator is known to be near a small, bright molecular cloud on the sky in a region largely devoid of emission in 12-CO surveys of the Galactic Center. The region is of interest because it is interior to the dust lanes which may be the shock zones where atomic gas from HI nuclear disk is converted into molecular gas. We find that the region is populated with a number of dense (n ~ 10^5 cm^-3) regions of excited gas with small filling factors, and estimate that up to 1-3 x 10^5 solar masses of gas can be seen in our maps. The detection suggests that a significant amount of mass is transported from the shock zones to the GC star-forming regions in the form of small, dense bundles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0902.2409v1-abstract-full').style.display = 'none'; document.getElementById('0902.2409v1-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> 13 February, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2009. </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, 7 figures, accepted for publication by the Astrophysical Journal, abstract abridged</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.696:1374-1384,2009 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0811.2713">arXiv:0811.2713</a> <span> [<a href="https://arxiv.org/pdf/0811.2713">pdf</a>, <a href="https://arxiv.org/format/0811.2713">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1088/0004-637X/690/1/L65">10.1088/0004-637X/690/1/L65 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Resolved Ring of Debris Dust Around the Solar Analog HD 107146 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Corder%2C+S+A">S. A. Corder</a>, <a href="/search/astro-ph?searchtype=author&query=Carpenter%2C+J+M">J. M. Carpenter</a>, <a href="/search/astro-ph?searchtype=author&query=Sargent%2C+A+I">A. I. Sargent</a>, <a href="/search/astro-ph?searchtype=author&query=Zauderer%2C+B+A">B. A. Zauderer</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+M+C+H">M. C. H. Wright</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+S">S. White</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D+P">D. P. Woody</a>, <a href="/search/astro-ph?searchtype=author&query=Teuben%2C+P">P. Teuben</a>, <a href="/search/astro-ph?searchtype=author&query=Scott%2C+S+L">S. L. Scott</a>, <a href="/search/astro-ph?searchtype=author&query=Pound%2C+M+W">M. W. Pound</a>, <a href="/search/astro-ph?searchtype=author&query=Plambeck%2C+R+L">R. L. Plambeck</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">J. W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Koda%2C+J">J. Koda</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M+W">M. W. Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Hawkins%2C+D+W">D. W. Hawkins</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+D+C+-">D. C. -J. Bock</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="0811.2713v2-abstract-short" style="display: inline;"> We present resolved images of the dust continuum emission from the debris disk around the young (80-200 Myr) solar-type star HD 107146 with CARMA at $位$1.3 mm and the CSO at $位$350 $渭$m. Both images show that the dust emission extends over an $\sim$10\arcsec diameter region. The high resolution (3\arcsec) CARMA image further reveals that the dust is distributed in a partial ring with significant… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0811.2713v2-abstract-full').style.display = 'inline'; document.getElementById('0811.2713v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0811.2713v2-abstract-full" style="display: none;"> We present resolved images of the dust continuum emission from the debris disk around the young (80-200 Myr) solar-type star HD 107146 with CARMA at $位$1.3 mm and the CSO at $位$350 $渭$m. Both images show that the dust emission extends over an $\sim$10\arcsec diameter region. The high resolution (3\arcsec) CARMA image further reveals that the dust is distributed in a partial ring with significant decrease in flux inward of 97 AU. Two prominent emission peaks appear within the ring separated by $\sim$140 degrees in position angle. The morphology of the dust emission is suggestive of dust captured into a mean motion resonance, which would imply the presence of a planet at an orbital radius of $\sim$45-75 AU. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0811.2713v2-abstract-full').style.display = 'none'; document.getElementById('0811.2713v2-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 December, 2008; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 November, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2008. </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 page, 3 figures, published in Astrophysical Journal Letters, AASTEX Format, figure 3 has additional data which improved the signal to noise</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.Lett.690:L65-L68,2009 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0805.0321">arXiv:0805.0321</a> <span> [<a href="https://arxiv.org/pdf/0805.0321">pdf</a>, <a href="https://arxiv.org/ps/0805.0321">ps</a>, <a href="https://arxiv.org/format/0805.0321">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/10.1086/589830">10.1086/589830 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Molecular Gas in the z=1.2 Ultraluminous Merger GOODS J123634.53+621241.3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Frayer%2C+D+T">David T. Frayer</a>, <a href="/search/astro-ph?searchtype=author&query=Koda%2C+J">Jin Koda</a>, <a href="/search/astro-ph?searchtype=author&query=Pope%2C+A">Alexandra Pope</a>, <a href="/search/astro-ph?searchtype=author&query=Huynh%2C+M+T">Minh T. Huynh</a>, <a href="/search/astro-ph?searchtype=author&query=Chary%2C+R">Ranga-Ram Chary</a>, <a href="/search/astro-ph?searchtype=author&query=Scott%2C+D">Douglas Scott</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+M">Mark Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+D+C+-">Douglas C. -J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Carpenter%2C+J+M">John M. Carpenter</a>, <a href="/search/astro-ph?searchtype=author&query=Hawkins%2C+D">David Hawkins</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+M">Mark Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Lamb%2C+J+W">James W. Lamb</a>, <a href="/search/astro-ph?searchtype=author&query=Plambeck%2C+R+L">Richard L. Plambeck</a>, <a href="/search/astro-ph?searchtype=author&query=Pound%2C+M+W">Marc W. Pound</a>, <a href="/search/astro-ph?searchtype=author&query=Scott%2C+S+L">Stephen L. Scott</a>, <a href="/search/astro-ph?searchtype=author&query=Scoville%2C+N+Z">Nicholas Z. Scoville</a>, <a href="/search/astro-ph?searchtype=author&query=Woody%2C+D+P">David P. Woody</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="0805.0321v1-abstract-short" style="display: inline;"> We report the detection of CO(2-1) emission from the z=1.2 ultraluminous infrared galaxy (ULIRG) GOODS J123634.53+621241.3 (also known as the sub-millimeter galaxy GN26). These observations represent the first discovery of high-redshift CO emission using the new Combined Array for Research in Millimeter-Wave Astronomy (CARMA). Of all high-redshift (z>1) galaxies within the GOODS-North field, thi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0805.0321v1-abstract-full').style.display = 'inline'; document.getElementById('0805.0321v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0805.0321v1-abstract-full" style="display: none;"> We report the detection of CO(2-1) emission from the z=1.2 ultraluminous infrared galaxy (ULIRG) GOODS J123634.53+621241.3 (also known as the sub-millimeter galaxy GN26). These observations represent the first discovery of high-redshift CO emission using the new Combined Array for Research in Millimeter-Wave Astronomy (CARMA). Of all high-redshift (z>1) galaxies within the GOODS-North field, this source has the largest far-infrared (FIR) flux observed in the Spitzer 70um and 160um bands. The CO redshift confirms the optical identification of the source, and the bright CO(2-1) line suggests the presence of a large molecular gas reservoir of about 7x10^10 M(sun). The infrared-to-CO luminosity ratio of L(IR)/L'(CO) = 80+/-30 L(sun) (K Km/s pc^2)^-1 is slightly smaller than the average ratio found in local ULIRGs and high-redshift sub-millimeter galaxies. The short star-formation time scale of about 70 Myr is consistent with a starburst associated with the merger event and is much shorter than the time scales for spiral galaxies and estimates made for high-redshift galaxies selected on the basis of their B-z and z-K colors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0805.0321v1-abstract-full').style.display = 'none'; document.getElementById('0805.0321v1-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 May, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2008. </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 Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/9207001">arXiv:astro-ph/9207001</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/9207001">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/9207001">ps</a>, <a href="https://arxiv.org/format/astro-ph/9207001">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</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/10.1103/PhysRevLett.69.1856">10.1103/PhysRevLett.69.1856 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmic Microwave Background Probes Models of Inflation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Davis%2C+R+L">R. L. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Hodges%2C+H+M">H. M. Hodges</a>, <a href="/search/astro-ph?searchtype=author&query=Smoot%2C+G+F">G. F. Smoot</a>, <a href="/search/astro-ph?searchtype=author&query=Steinhardt%2C+P+J">P. J. Steinhardt</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+M+S">M. S. Turner</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="astro-ph/9207001v1-abstract-short" style="display: inline;"> Inflation creates both scalar (density) and tensor (gravity wave) metric perturbations. We find that the tensor mode contribution to the CMB anisotropy on large-angular scales can only exceed that of the scalar mode in models where the spectrum of perturbations deviates significantly from scale invariance (e.g., extended and power-law inflation models and extreme versions of chaotic inflation).… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9207001v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/9207001v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/9207001v1-abstract-full" style="display: none;"> Inflation creates both scalar (density) and tensor (gravity wave) metric perturbations. We find that the tensor mode contribution to the CMB anisotropy on large-angular scales can only exceed that of the scalar mode in models where the spectrum of perturbations deviates significantly from scale invariance (e.g., extended and power-law inflation models and extreme versions of chaotic inflation). If the tensor mode dominates at large-angular scales, then the value of $螖T/T$ predicted on $1^\circ$ is less than if the scalar mode dominates, and, for cold dark matter models, $b>1$ can be made consistent with the COBE DMR results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/9207001v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/9207001v1-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> 13 July, 1992; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 1992. </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, FERMILAB-Pub-92/168-A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett.69:1856-1859,1992; ERRATUM-ibid.70:1733,1993 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

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