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</div> <div class="control"> <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/2411.10874">arXiv:2411.10874</a> <span> [<a href="https://arxiv.org/pdf/2411.10874">pdf</a>, <a href="https://arxiv.org/format/2411.10874">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> A Wave Scattering Approach to Modelling Surface Roughness in Orbital Aerodynamics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S+V">Sabin Viorel Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+B+S">Bernardo Sousa Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Siemes%2C+C">Christian Siemes</a>, <a href="/search/astro-ph?searchtype=author&query=IJssel%2C+J+v+d">Jose van den IJssel</a>, <a href="/search/astro-ph?searchtype=author&query=Visser%2C+P+N+A+M">Pieter N. A. M. Visser</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.10874v1-abstract-short" style="display: inline;"> The increasing density of space objects in low-Earth orbit highlights the critical need for accurate orbit predictions to minimise operational disruptions. One significant challenge lies in accurately modelling the interaction of gas particles with the surfaces of these objects, as errors in aerodynamic coefficient modelling directly impact orbit prediction accuracy. Current approaches rely on emp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10874v1-abstract-full').style.display = 'inline'; document.getElementById('2411.10874v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.10874v1-abstract-full" style="display: none;"> The increasing density of space objects in low-Earth orbit highlights the critical need for accurate orbit predictions to minimise operational disruptions. One significant challenge lies in accurately modelling the interaction of gas particles with the surfaces of these objects, as errors in aerodynamic coefficient modelling directly impact orbit prediction accuracy. Current approaches rely on empirical models, such as those by Sentman and Cercignani-Lampis-Lord, incorporating one or two adjustable parameters typically calibrated with orbital acceleration data. However, these models fall short in capturing essential gas-solid interaction processes, including multiple reflections, shadowing, and backscattering caused by surface roughness. We present a novel, physics-based gas-surface interaction model that utilises electromagnetic wave theory to account for macroscopic effects of surface roughness on gas particle scattering distributions. This approach not only offers a more accurate representation of gas-surface interactions but also allows parameter determination through a combination of ground-based surface roughness measurements and molecular dynamics simulations at the atomic scale. The model validity is tested across the entire parameter space using a test-particle Monte Carlo method on a simulated rough surface. Furthermore, it successfully reproduces experimental results from the literature on the scattering of Argon and Helium from smooth and rough Kapton and Aluminium surfaces. Finally, we demonstrate the model's impact on aerodynamic coefficients for simple geometric shapes, comparing the results with those from the Sentman and Cercignani-Lampis-Lord models. This comparison reveals that inconsistencies previously observed between these models and tracking data for spherical satellites can be attributed to surface roughness effects, which our model effectively accounts for. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10874v1-abstract-full').style.display = 'none'; document.getElementById('2411.10874v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.17581">arXiv:2403.17581</a> <span> [<a href="https://arxiv.org/pdf/2403.17581">pdf</a>, <a href="https://arxiv.org/format/2403.17581">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> <p class="title is-5 mathjax"> The power of relativistic jets: a comparative study </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Foschini%2C+L">Luigi Foschini</a>, <a href="/search/astro-ph?searchtype=author&query=Barba%2C+B+D">Benedetta Dalla Barba</a>, <a href="/search/astro-ph?searchtype=author&query=Tornikoski%2C+M">Merja Tornikoski</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">Heinz Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=Marziani%2C+P">Paola Marziani</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=Jorstad%2C+S+G">Svetlana G. Jorstad</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%A4rvel%C3%A4%2C+E">Emilia J盲rvel盲</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">Sonia Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Bont%C3%A0%2C+E+D">Elena Dalla Bont脿</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.17581v1-abstract-short" style="display: inline;"> We present the results of a comparison between different methods to estimate the power of relativistic jets from active galactic nuclei (AGN). We selected a sample of 32 objects (21 flat-spectrum radio quasars, 7 BL Lacertae Objects, 2 misaligned AGN, and 2 changing-look AGN) from the Very Large Baseline Array (VLBA) observations at 43 GHz of the Boston University blazar program. We then calculate… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.17581v1-abstract-full').style.display = 'inline'; document.getElementById('2403.17581v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.17581v1-abstract-full" style="display: none;"> We present the results of a comparison between different methods to estimate the power of relativistic jets from active galactic nuclei (AGN). We selected a sample of 32 objects (21 flat-spectrum radio quasars, 7 BL Lacertae Objects, 2 misaligned AGN, and 2 changing-look AGN) from the Very Large Baseline Array (VLBA) observations at 43 GHz of the Boston University blazar program. We then calculated the total, radiative, and kinetic jet power from both radio and high-energy gamma-ray observations, and compare the values. We found an excellent agreement between the radiative power calculated by using the Blandford and K枚nigl model with 37 or 43 GHz data, and the values derived from the high-energy $纬-$ray luminosity. The agreement is still acceptable if 15 GHz data are used, although with a larger dispersion, but it improves if we use a constant fraction of the $纬-$ray luminosity. We found a good agreement also for the kinetic power calculated with Blandford and K枚nigl model with 15 GHz data, and the value from the extended radio emission. We also propose some easy-to-use equations to estimate the jet power. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.17581v1-abstract-full').style.display = 'none'; document.getElementById('2403.17581v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 12 figures, 6 tables. Accepted for publication on Universe, Special Issue: Recent Advances in Gamma Ray Astrophysics and Future Perspectives</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.01835">arXiv:2402.01835</a> <span> [<a href="https://arxiv.org/pdf/2402.01835">pdf</a>, <a href="https://arxiv.org/ps/2402.01835">ps</a>, <a href="https://arxiv.org/format/2402.01835">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"> Obscuration in high redshift jetted QSO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Caccianiga%2C+A">A. Caccianiga</a>, <a href="/search/astro-ph?searchtype=author&query=Ighina%2C+L">L. Ighina</a>, <a href="/search/astro-ph?searchtype=author&query=Moretti%2C+A">A. Moretti</a>, <a href="/search/astro-ph?searchtype=author&query=Brivio%2C+R">R. Brivio</a>, <a href="/search/astro-ph?searchtype=author&query=Belladitta%2C+S">S. Belladitta</a>, <a href="/search/astro-ph?searchtype=author&query=Dallacasa%2C+D">D. Dallacasa</a>, <a href="/search/astro-ph?searchtype=author&query=Spingola%2C+C">C. Spingola</a>, <a href="/search/astro-ph?searchtype=author&query=March%C3%A3%2C+M+J">M. J. March茫</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">S. Ant贸n</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.01835v1-abstract-short" style="display: inline;"> Obscuration in high-redshift quasi-stellar objects (QSO) has a profound impact on our understanding of the evolution of supermassive black holes across the cosmic time. An accurate quantification of its relevance is therefore mandatory. We present a study aimed at evaluating the importance of obscuration in high redshift jetted QSO, i.e. those active nuclei characterized by the presence of powerfu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.01835v1-abstract-full').style.display = 'inline'; document.getElementById('2402.01835v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.01835v1-abstract-full" style="display: none;"> Obscuration in high-redshift quasi-stellar objects (QSO) has a profound impact on our understanding of the evolution of supermassive black holes across the cosmic time. An accurate quantification of its relevance is therefore mandatory. We present a study aimed at evaluating the importance of obscuration in high redshift jetted QSO, i.e. those active nuclei characterized by the presence of powerful relativistic jets. We compare the observed number of radio detected QSO at different radio flux density limits with the value predicted by the beaming model on the basis of the number of oriented sources (blazars). Any significant deficit of radio-detected QSO compared to the predictions can be caused by the presence of obscuration along large angles from the jet direction. We apply this method to two sizable samples characterized by the same optical limit (mag=21) but significantly different radio density limits (30 mJy and 1 mJy respectively) and containing a total of 87 independent radio-loud 4<z<6.8 QSO, 31 of which classified as blazars. We find a general good agreement between the numbers predicted by the model and those actually observed, with only a marginal discrepancy at 0.5 mJy that could be caused by the lack of completeness of the sample. We conclude that we have no evidence of obscuration within angles 10-20deg from the relativistic jet direction. We also show how the ongoing deep wide-angle radio surveys will be instrumental to test the presence of obscuration at much larger angles, up to 30-35deg. We finally suggest that, depending on the actual fraction of obscured QSO, relativistic jets could be much more common at high redshifts compared to what is usually observed in the local Universe <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.01835v1-abstract-full').style.display = 'none'; document.getElementById('2402.01835v1-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 5 figures. Accepted for publication on A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.03400">arXiv:2211.03400</a> <span> [<a href="https://arxiv.org/pdf/2211.03400">pdf</a>, <a href="https://arxiv.org/ps/2211.03400">ps</a>, <a href="https://arxiv.org/format/2211.03400">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/10.3390/universe8110587">10.3390/universe8110587 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A New Sample of Gamma-Ray Emitting Jetted Active Galactic Nuclei </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Foschini%2C+L">Luigi Foschini</a>, <a href="/search/astro-ph?searchtype=author&query=Lister%2C+M+L">Matthew L. Lister</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">Heinz Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=Ciroi%2C+S">Stefano Ciroi</a>, <a href="/search/astro-ph?searchtype=author&query=Marziani%2C+P">Paola Marziani</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">Sonia Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Berton%2C+M">Marco Berton</a>, <a href="/search/astro-ph?searchtype=author&query=Bont%C3%A0%2C+E+D">Elena Dalla Bont脿</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%A4rvel%C3%A4%2C+E">Emilia J盲rvel盲</a>, <a href="/search/astro-ph?searchtype=author&query=March%C3%A3%2C+M+J+M">Maria J. M. March茫</a>, <a href="/search/astro-ph?searchtype=author&query=Romano%2C+P">Patrizia Romano</a>, <a href="/search/astro-ph?searchtype=author&query=Tornikoski%2C+M">Merja Tornikoski</a>, <a href="/search/astro-ph?searchtype=author&query=Vercellone%2C+S">Stefano Vercellone</a>, <a href="/search/astro-ph?searchtype=author&query=Vietri%2C+A">Amelia Vietri</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.03400v1-abstract-short" style="display: inline;"> We considered the fourth catalog of gamma-ray point sources produced by the Fermi Large Area Telescope (LAT) and selected only jetted active galactic nuclei (AGN) or sources with no specific classification, but with a low-frequency counterpart. Our final list is composed of 2980 gamma-ray point sources. We then searched for optical spectra in all the available literature and publicly available dat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.03400v1-abstract-full').style.display = 'inline'; document.getElementById('2211.03400v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.03400v1-abstract-full" style="display: none;"> We considered the fourth catalog of gamma-ray point sources produced by the Fermi Large Area Telescope (LAT) and selected only jetted active galactic nuclei (AGN) or sources with no specific classification, but with a low-frequency counterpart. Our final list is composed of 2980 gamma-ray point sources. We then searched for optical spectra in all the available literature and publicly available databases, to measure redshifts and to confirm or change the original LAT classification. Our final list of gamma-ray emitting jetted AGN is composed of BL Lac Objects (40%), flat-spectrum radio quasars (23%), misaligned AGN (2.8%), narrow-line Seyfert 1, Seyfert, and low-ionization nuclear emission-line region galaxies (1.9%). We also found a significant number of objects changing from one type to another, and vice versa (changing-look AGN, 1.1%). About 30% of gamma-ray sources still have an ambiguous classification or lack one altogether. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.03400v1-abstract-full').style.display = 'none'; document.getElementById('2211.03400v1-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 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">18 pages, 5 figures, 1 Table. Accepted for publication on Universe, Special Issue "Black Holes and Relativistic Jets", edited by I. Dutan and N. R. MacDonald. This preprint contains only the main text. The full tables A1 and A2 are available on the journal web site (https://www.mdpi.com/2218-1997/8/11/587)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Universe 2022, 8(11), 587 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.12301">arXiv:2207.12301</a> <span> [<a href="https://arxiv.org/pdf/2207.12301">pdf</a>, <a href="https://arxiv.org/format/2207.12301">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/10.1093/mnras/stac2096">10.1093/mnras/stac2096 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The VMC Survey -- XLIX. Discovery of a population of quasars dominated by nuclear dust emission behind the Magellanic Clouds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pennock%2C+C+M">Clara M. Pennock</a>, <a href="/search/astro-ph?searchtype=author&query=van+Loon%2C+J+T">Jacco Th. van Loon</a>, <a href="/search/astro-ph?searchtype=author&query=Anih%2C+J+O">Joy O. Anih</a>, <a href="/search/astro-ph?searchtype=author&query=Maitra%2C+C">Chandreyee Maitra</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">Frank Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Sansom%2C+A+E">Anne E. Sansom</a>, <a href="/search/astro-ph?searchtype=author&query=Ivanov%2C+V+D">Valentin D. Ivanov</a>, <a href="/search/astro-ph?searchtype=author&query=Cowley%2C+M+J">Michael J. Cowley</a>, <a href="/search/astro-ph?searchtype=author&query=Afonso%2C+J">Jos茅 Afonso</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">Sonia Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Cioni%2C+M+L">Maria-Rosa L. Cioni</a>, <a href="/search/astro-ph?searchtype=author&query=Craig%2C+J+E+M">Jessica E. M. Craig</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovi%C4%87%2C+M+D">Miroslav D. Filipovi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">Andrew M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Nanni%2C+A">Ambra Nanni</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">Isabella Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Vardoulaki%2C+E">Eleni Vardoulaki</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.12301v1-abstract-short" style="display: inline;"> Following the discovery of SAGE0536AGN ($z \sim$ 0.14), with the strongest 10-$渭$m silicate emission ever observed for an Active Galactic Nucleus (AGN), we discovered SAGE0534AGN ($z \sim$ 1.01), a similar AGN but with less extreme silicate emission. Both were originally mistaken as evolved stars in the Magellanic Clouds. Lack of far-infrared emission, and therefore star-formation, implies we are… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12301v1-abstract-full').style.display = 'inline'; document.getElementById('2207.12301v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.12301v1-abstract-full" style="display: none;"> Following the discovery of SAGE0536AGN ($z \sim$ 0.14), with the strongest 10-$渭$m silicate emission ever observed for an Active Galactic Nucleus (AGN), we discovered SAGE0534AGN ($z \sim$ 1.01), a similar AGN but with less extreme silicate emission. Both were originally mistaken as evolved stars in the Magellanic Clouds. Lack of far-infrared emission, and therefore star-formation, implies we are seeing the central engine of the AGN without contribution from the host galaxy. They could be a key link in galaxy evolution. We used a dimensionality reduction algorithm, t-SNE (t-distributed Stochastic Neighbourhood Embedding) with multi-wavelength data from Gaia EDR3, VISTA survey of the Magellanic Clouds, AllWISE and the Australian SKA Pathfinder to find these two unusual AGN are grouped with 16 other objects separated from the rest, suggesting a rare class. Our spectroscopy at SAAO/SALT and literature data confirm at least 14 of these objects are extragalactic ($0.13 < z < 1.23$), all hosting AGN. Using spectral energy distribution fitter CIGALE we find that the majority of dust emission ($> 70 \%$) in these sources is due to the AGN. Host galaxies appear to be either in or transitioning into the green valley. There is a trend of a thinning torus, increasing X-ray luminosity and decreasing Eddington ratio as the AGN transition through the green valley, implying that as the accretion supply depletes, the torus depletes and the column density reduces. Also, the near-infrared variability amplitude of these sources correlates with attenuation by the torus, implying the torus plays a role in the variability. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.12301v1-abstract-full').style.display = 'none'; document.getElementById('2207.12301v1-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">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/2110.01995">arXiv:2110.01995</a> <span> [<a href="https://arxiv.org/pdf/2110.01995">pdf</a>, <a href="https://arxiv.org/ps/2110.01995">ps</a>, <a href="https://arxiv.org/format/2110.01995">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> <p class="title is-5 mathjax"> A New Sample of Gamma-Ray Emitting Jetted Active Galactic Nuclei -- Preliminary Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Foschini%2C+L">L. Foschini</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=Ant%C3%B3n%2C+S">S. Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Berton%2C+M">M. Berton</a>, <a href="/search/astro-ph?searchtype=author&query=Ciroi%2C+S">S. Ciroi</a>, <a href="/search/astro-ph?searchtype=author&query=March%C3%A3%2C+M+J+M">M. J. M. March茫</a>, <a href="/search/astro-ph?searchtype=author&query=Tornikoski%2C+M">M. Tornikoski</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%A4rvel%C3%A4%2C+E">E. J盲rvel盲</a>, <a href="/search/astro-ph?searchtype=author&query=Romano%2C+P">P. Romano</a>, <a href="/search/astro-ph?searchtype=author&query=Vercellone%2C+S">S. Vercellone</a>, <a href="/search/astro-ph?searchtype=author&query=Bont%C3%A0%2C+E+D">E. Dalla Bont脿</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="2110.01995v1-abstract-short" style="display: inline;"> We are compiling a new list of gamma-ray jetted active galactic nuclei (AGN), starting from the fourth catalog of point sources of the Fermi Large Area Telescope (LAT). Our aim is to prepare a list of jetted AGN with known redshifts and classifications to be used to calibrate jet power. We searched in the available literature for all the published optical spectra and multiwavelength studies useful… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.01995v1-abstract-full').style.display = 'inline'; document.getElementById('2110.01995v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.01995v1-abstract-full" style="display: none;"> We are compiling a new list of gamma-ray jetted active galactic nuclei (AGN), starting from the fourth catalog of point sources of the Fermi Large Area Telescope (LAT). Our aim is to prepare a list of jetted AGN with known redshifts and classifications to be used to calibrate jet power. We searched in the available literature for all the published optical spectra and multiwavelength studies useful to characterize the sources. We found new, missed, or even forgotten information leading to a substantial change in the redshift values and classification of many sources. We present here the preliminary results of this analysis and some statistics based on the gamma-ray sources with right ascension within the interval $0^{\rm h}-12^{\rm h}$ (J2000). Although flat-spectrum radio quasars and BL Lac objects are still the dominant populations, there is a significant increase in the number of other objects, such as misaligned AGN, narrow-line Seyfert 1 galaxies, and Seyfert galaxies. We also introduced two new classes of objects: changing-look AGN and ambiguous sources. About one third of the sources remain unclassified. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.01995v1-abstract-full').style.display = 'none'; document.getElementById('2110.01995v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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, 2 figures, 1 table. Accepted for publication on Universe (MDPI). The full list is available on the published article</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.03437">arXiv:2107.03437</a> <span> [<a href="https://arxiv.org/pdf/2107.03437">pdf</a>, <a href="https://arxiv.org/format/2107.03437">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-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/10.1016/j.asr.2021.05.023">10.1016/j.asr.2021.05.023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Radio astronomy and Space science in Azores: enhancing the Atlantic VLBI infrastructure cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barbosa%2C+D">Domingos Barbosa</a>, <a href="/search/astro-ph?searchtype=author&query=Coelho%2C+B">Bruno Coelho</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">Sonia Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Bergano%2C+M">Miguel Bergano</a>, <a href="/search/astro-ph?searchtype=author&query=Boekholt%2C+T">Tjarda Boekholt</a>, <a href="/search/astro-ph?searchtype=author&query=Correia%2C+A+C+M">Alexandre C. M. Correia</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+D">Dalmiro Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Pandeirada%2C+J">Jo茫o Pandeirada</a>, <a href="/search/astro-ph?searchtype=author&query=Ribeiro%2C+V">Val茅rio Ribeiro</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">Jason Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Barraca%2C+J+P">Jo茫o Paulo Barraca</a>, <a href="/search/astro-ph?searchtype=author&query=Gomes%2C+D">Diogo Gomes</a>, <a href="/search/astro-ph?searchtype=author&query=Morgado%2C+B">Bruno Morgado</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="2107.03437v1-abstract-short" style="display: inline;"> Radio astronomy and Space Infrastructures in the Azores have a great scientific and industrial interest because they benefit from a unique geographical location in the middle of the North Atlantic allowing a vast improvement in the sky coverage. This fact obviously has a very high added value for: i) the establishment of space tracking and communications networks for the emergent global small sate… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.03437v1-abstract-full').style.display = 'inline'; document.getElementById('2107.03437v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.03437v1-abstract-full" style="display: none;"> Radio astronomy and Space Infrastructures in the Azores have a great scientific and industrial interest because they benefit from a unique geographical location in the middle of the North Atlantic allowing a vast improvement in the sky coverage. This fact obviously has a very high added value for: i) the establishment of space tracking and communications networks for the emergent global small satellite fleets ii) it is invaluable to connect the radio astronomy infrastructure networks in Africa, Europe and America continents using Very Large Baseline Interferometry (VLBI) techniques, iii) it allows excellent potential for monitoring space debris and Near Earth Objects (NEOs). There is in S. Miguel island a 32-metre SATCOM antenna that could be integrated in advanced VLBI networks and be capable of additional Deep Space Network ground support. This paper explores the space science opportunities offered by the upgrade of the S. Miguel 32-metre SATCOM antenna into a world-class infrastructure for radio astronomy and space exploration: it would enable a Deep Space Network mode and would constitute a key space facility for data production, promoting local digital infrastructure investments and the testing of cutting-edge information technologies. Its Atlantic location also enables improvements in angular resolution, provides many baseline in East-West and North-South directions connecting the emergent VLBI stations in America to Europe and Africa VLBI arrays therefore contributing for greater array imaging capabilities especially for sources or well studied fields close to or below the celestial equator, where ESO facilities, ALMA, SKA and its precursors do or will operate and observe in the coming decades. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.03437v1-abstract-full').style.display = 'none'; document.getElementById('2107.03437v1-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">14 pages, 7 figures, 3 tables. Accepted for Publication at Advances in Space Research, COSPAR, Elsevier</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.01633">arXiv:2107.01633</a> <span> [<a href="https://arxiv.org/pdf/2107.01633">pdf</a>, <a href="https://arxiv.org/format/2107.01633">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="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/10.1051/0004-6361/202140883">10.1051/0004-6361/202140883 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The BINGO Project I: Baryon Acoustic Oscillations from Integrated Neutral Gas Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+E">Elcio Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+E+G+M">Elisa G. M. Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Landim%2C+R+G">Ricardo G. Landim</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+A+A">Andre A. Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Fornazier%2C+K+S+F">Karin S. F. Fornazier</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+F+B">Filipe B. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Barosi%2C+L">Luciano Barosi</a>, <a href="/search/astro-ph?searchtype=author&query=Brito%2C+F+A">Francisco A. Brito</a>, <a href="/search/astro-ph?searchtype=author&query=Queiroz%2C+A+R">Amilcar R. Queiroz</a>, <a href="/search/astro-ph?searchtype=author&query=Villela%2C+T">Thyrso Villela</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+B">Bin Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wuensche%2C+C+A">Carlos A. Wuensche</a>, <a href="/search/astro-ph?searchtype=author&query=Marins%2C+A">Alessandro Marins</a>, <a href="/search/astro-ph?searchtype=author&query=Novaes%2C+C+P">Camila P. Novaes</a>, <a href="/search/astro-ph?searchtype=author&query=Liccardo%2C+V">Vincenzo Liccardo</a>, <a href="/search/astro-ph?searchtype=author&query=Shan%2C+C">Chenxi Shan</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+J">Jiajun Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z">Zhongli Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Zhu%2C+Z">Zhenghao Zhu</a>, <a href="/search/astro-ph?searchtype=author&query=Browne%2C+I">Ian Browne</a>, <a href="/search/astro-ph?searchtype=author&query=Delabrouille%2C+J">Jacques Delabrouille</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+L">Larissa Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+M+V+d">Marcelo V. dos Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+H">Haiguang Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">Sonia Anton</a> , et al. (21 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="2107.01633v2-abstract-short" style="display: inline;"> Observations of the redshifted 21-cm line of neutral hydrogen (HI) are a new and powerful window of observation that offers us the possibility to map the spatial distribution of cosmic HI and learn about cosmology. BINGO (Baryon Acoustic Oscillations [BAO] from Integrated Neutral Gas Observations) is a new unique radio telescope designed to be one of the first to probe BAO at radio frequencies. BI… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.01633v2-abstract-full').style.display = 'inline'; document.getElementById('2107.01633v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.01633v2-abstract-full" style="display: none;"> Observations of the redshifted 21-cm line of neutral hydrogen (HI) are a new and powerful window of observation that offers us the possibility to map the spatial distribution of cosmic HI and learn about cosmology. BINGO (Baryon Acoustic Oscillations [BAO] from Integrated Neutral Gas Observations) is a new unique radio telescope designed to be one of the first to probe BAO at radio frequencies. BINGO has two science goals: cosmology and astrophysics. Cosmology is the main science goal and the driver for BINGO's design and strategy. The key of BINGO is to detect the low redshift BAO to put strong constraints in the dark sector models. Given the versatility of the BINGO telescope, a secondary goal is astrophysics, where BINGO can help discover and study Fast Radio Bursts (FRB) and other transients, Galactic and extragalactic science. In this paper, we introduce the latest progress of the BINGO project, its science goals, describing the scientific potential of the project in each science and the new developments obtained by the collaboration. We introduce the BINGO project and its science goals and give a general summary of recent developments in construction, science potential and pipeline development obtained by the BINGO collaboration in the past few years. We show that BINGO will be able to obtain competitive constraints for the dark sector, and also that will allow for the discovery of several FRBs in the southern hemisphere. The capacity of BINGO in obtaining information from 21-cm is also tested in the pipeline introduced here. There is still no measurement of the BAO in radio, and studying cosmology in this new window of observations is one of the most promising advances in the field. The BINGO project is a radio telescope that has the goal to be one of the first to perform this measurement and it is currently being built in the northeast of Brazil. (Abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.01633v2-abstract-full').style.display = 'none'; document.getElementById('2107.01633v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">23 pages. To appear in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> TUM-HEP-1323/21 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 664, A14 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.12013">arXiv:2106.12013</a> <span> [<a href="https://arxiv.org/pdf/2106.12013">pdf</a>, <a href="https://arxiv.org/format/2106.12013">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/10.1093/mnras/stab1858">10.1093/mnras/stab1858 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ASKAP-EMU Early Science Project: 888 MHz Radio Continuum Survey of the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pennock%2C+C+M">Clara M. Pennock</a>, <a href="/search/astro-ph?searchtype=author&query=van+Loon%2C+J+T">Jacco Th. van Loon</a>, <a href="/search/astro-ph?searchtype=author&query=Filipovic%2C+M+D">Miroslav D. Filipovic</a>, <a href="/search/astro-ph?searchtype=author&query=Andernach%2C+H">Heinz Andernach</a>, <a href="/search/astro-ph?searchtype=author&query=Haberl%2C+F">Frank Haberl</a>, <a href="/search/astro-ph?searchtype=author&query=Kothes%2C+R">Roland Kothes</a>, <a href="/search/astro-ph?searchtype=author&query=Lenc%2C+E">Emil Lenc</a>, <a href="/search/astro-ph?searchtype=author&query=Rudnick%2C+L">Lawrence Rudnick</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+S+V">Sarah V. White</a>, <a href="/search/astro-ph?searchtype=author&query=Agliozzo%2C+C">Claudia Agliozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">Sonia Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Bojicic%2C+I">Ivan Bojicic</a>, <a href="/search/astro-ph?searchtype=author&query=Bomans%2C+D+J">Dominik J. Bomans</a>, <a href="/search/astro-ph?searchtype=author&query=Collier%2C+J+D">Jordan D. Collier</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+E+J">Evan J. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">Andrew M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Jeganathan%2C+K">Kanapathippillai Jeganathan</a>, <a href="/search/astro-ph?searchtype=author&query=Kavanagh%2C+P+J">Patrick J. Kavanagh</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B盲rbel S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Leahy%2C+D">Denis Leahy</a>, <a href="/search/astro-ph?searchtype=author&query=Maggi%2C+P">Pierre Maggi</a>, <a href="/search/astro-ph?searchtype=author&query=Maitra%2C+C">Chandreyee Maitra</a>, <a href="/search/astro-ph?searchtype=author&query=Marvil%2C+J">Josh Marvil</a>, <a href="/search/astro-ph?searchtype=author&query=Micha%C5%82owski%2C+M+J">Micha艂 J. Micha艂owski</a>, <a href="/search/astro-ph?searchtype=author&query=Norris%2C+R+P">Ray P. Norris</a> , et al. (6 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="2106.12013v1-abstract-short" style="display: inline;"> We present an analysis of a new 120 deg$^{2}$ radio continuum image of the Large Magellanic Cloud (LMC) at 888 MHz with a bandwidth of 288 MHz and beam size of $13\rlap{.}^{\prime\prime}9\times12\rlap{.}^{\prime\prime}1$, from the Australian Square Kilometre Array Pathfinder (ASKAP) processed as part of the Evolutionary Map of the Universe (EMU) survey. The median Root Mean Squared noise is 58… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.12013v1-abstract-full').style.display = 'inline'; document.getElementById('2106.12013v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.12013v1-abstract-full" style="display: none;"> We present an analysis of a new 120 deg$^{2}$ radio continuum image of the Large Magellanic Cloud (LMC) at 888 MHz with a bandwidth of 288 MHz and beam size of $13\rlap{.}^{\prime\prime}9\times12\rlap{.}^{\prime\prime}1$, from the Australian Square Kilometre Array Pathfinder (ASKAP) processed as part of the Evolutionary Map of the Universe (EMU) survey. The median Root Mean Squared noise is 58 $渭$Jy beam$^{-1}$. We present a catalogue of 54,612 sources, divided over a GOLD list (30,866 sources) complete down to 0.5 mJy uniformly across the field, a SILVER list (22,080 sources) reaching down to $<$ 0.2 mJy and a BRONZE list (1,666 sources) of visually inspected sources in areas of high noise and/or near bright complex emission. We discuss detections of planetary nebulae and their radio luminosity function, young stellar objects showing a correlation between radio luminosity and gas temperature, novae and X-ray binaries in the LMC, and active stars in the Galactic foreground that may become a significant population below this flux level. We present examples of diffuse emission in the LMC (H II regions, supernova remnants, bubbles) and distant galaxies showcasing spectacular interaction between jets and intracluster medium. Among 14,333 infrared counterparts of the predominantly background radio source population we find that star-forming galaxies become more prominent below 3 mJy compared to active galactic nuclei. We combine the new 888 MHz data with archival Australia Telescope Compact Array data at 1.4 GHz to determine spectral indices; the vast majority display synchrotron emission but flatter spectra occur too. We argue that the most extreme spectral index values are due to variability. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.12013v1-abstract-full').style.display = 'none'; document.getElementById('2106.12013v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">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/2105.09895">arXiv:2105.09895</a> <span> [<a href="https://arxiv.org/pdf/2105.09895">pdf</a>, <a href="https://arxiv.org/format/2105.09895">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </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/stab1462">10.1093/mnras/stab1462 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An ACA 1mm survey of HzRGs in the ELAIS-S1: survey description and first results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Messias%2C+H">Hugo Messias</a>, <a href="/search/astro-ph?searchtype=author&query=Hatziminaoglou%2C+E">Evanthia Hatziminaoglou</a>, <a href="/search/astro-ph?searchtype=author&query=Hibon%2C+P">Pascale Hibon</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">Tony Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Matute%2C+I">Israel Matute</a>, <a href="/search/astro-ph?searchtype=author&query=Lacy%2C+M">Mark Lacy</a>, <a href="/search/astro-ph?searchtype=author&query=Mason%2C+B">Brian Mason</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%ADn%2C+S">Sergio Mart铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Afonso%2C+J+M">Jos茅 M. Afonso</a>, <a href="/search/astro-ph?searchtype=author&query=Fomalont%2C+E">Edward Fomalont</a>, <a href="/search/astro-ph?searchtype=author&query=Amarantidis%2C+S">Stergios Amarantidis</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">Sonia Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Demarco%2C+R">Ricardo Demarco</a>, <a href="/search/astro-ph?searchtype=author&query=Gendron-Marsolais%2C+M">Marie-Lou Gendron-Marsolais</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+A+M">Andrew M. Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Kneissl%2C+R">R眉diger Kneissl</a>, <a href="/search/astro-ph?searchtype=author&query=Lopez%2C+C">Cristian Lopez</a>, <a href="/search/astro-ph?searchtype=author&query=Rebolledo%2C+D">David Rebolledo</a>, <a href="/search/astro-ph?searchtype=author&query=Yang%2C+C">Chentao Yang</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="2105.09895v1-abstract-short" style="display: inline;"> Radio-emitting jets might be one of the main ingredients shaping the evolution of massive galaxies in the Universe since early cosmic times. However, identifying early radio active galactic nuclei (AGN) and confirming this scenario has been hard to accomplish, with studies of samples of radio AGN hosts at z>2 becoming routinely possible only recently. With the above in mind, we have carried out a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.09895v1-abstract-full').style.display = 'inline'; document.getElementById('2105.09895v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.09895v1-abstract-full" style="display: none;"> Radio-emitting jets might be one of the main ingredients shaping the evolution of massive galaxies in the Universe since early cosmic times. However, identifying early radio active galactic nuclei (AGN) and confirming this scenario has been hard to accomplish, with studies of samples of radio AGN hosts at z>2 becoming routinely possible only recently. With the above in mind, we have carried out a survey with the Atacama Compact Array (ACA, or Morita Array) at 1.3 mm (rms=0.15 mJy) of 36 high-redshift radio AGN candidates found within 3.9deg2 in the ELAIS-S1 field. The work presented here describes the survey and showcases a preliminary set of results. The selection of the sample was based on three criteria making use of infrared (IR) and radio fluxes only. The criterion providing the highest selection rate of high-redshift sources (86% at z>0.8) is one combining an IR colour cut and radio flux cut (S(5.8um)/S(3.6um)>1.3 and S(1.4GHz)>1mJy). Among the sample of 36 sources, 16 show a millimetre (mm) detection. In eight of these cases, the emission has a non-thermal origin. A zsp=1.58 object, with a mm detection of non-thermal origin, shows a clear spatial offset between the jet-dominated mm continuum emission and that of the host's molecular gas, as traced by serendipitously detected CO(5-4) emission. Among the objects with serendipitous line detections there is a source with a narrow jet-like region, as revealed by CS(6-5) emission stretching 20kpc out of the host galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.09895v1-abstract-full').style.display = 'none'; document.getElementById('2105.09895v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">25 pages, 15 figures, accepted on MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.07413">arXiv:2011.07413</a> <span> [<a href="https://arxiv.org/pdf/2011.07413">pdf</a>, <a href="https://arxiv.org/format/2011.07413">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/10.1093/mnras/stab1046">10.1093/mnras/stab1046 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observations of the gamma-ray emitting narrow-line Seyfert 1, SBS 0846+513, and its host galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hamilton%2C+T+S">Timothy S. Hamilton</a>, <a href="/search/astro-ph?searchtype=author&query=Berton%2C+M">Marco Berton</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">Sonia Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Busoni%2C+L">Lorenzo Busoni</a>, <a href="/search/astro-ph?searchtype=author&query=Caccianiga%2C+A">Alessandro Caccianiga</a>, <a href="/search/astro-ph?searchtype=author&query=Ciroi%2C+S">Stefano Ciroi</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%A4ssler%2C+W">Wolfgang G盲ssler</a>, <a href="/search/astro-ph?searchtype=author&query=Georgiev%2C+I">Iskren Georgiev</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%A4rvel%C3%A4%2C+E">Emilia J盲rvel盲</a>, <a href="/search/astro-ph?searchtype=author&query=Komossa%2C+S">S. Komossa</a>, <a href="/search/astro-ph?searchtype=author&query=Mathur%2C+S">Smita Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Rabien%2C+S">Sebastian Rabien</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="2011.07413v1-abstract-short" style="display: inline;"> The gamma-ray emitting galaxy SBS 0846+513 has been classified as a Narrow-Line Seyfert 1 from its spectroscopy, and on that basis it was thought likely to have a small central black hole hosted in a spiral galaxy. But very few of the gamma-ray Narrow-Line Seyfert 1s have high-resolution imaging of their hosts, so it is unknown how those expectations hold up for the gamma-emitting class. We have o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.07413v1-abstract-full').style.display = 'inline'; document.getElementById('2011.07413v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.07413v1-abstract-full" style="display: none;"> The gamma-ray emitting galaxy SBS 0846+513 has been classified as a Narrow-Line Seyfert 1 from its spectroscopy, and on that basis it was thought likely to have a small central black hole hosted in a spiral galaxy. But very few of the gamma-ray Narrow-Line Seyfert 1s have high-resolution imaging of their hosts, so it is unknown how those expectations hold up for the gamma-emitting class. We have observed this galaxy in the J-band with the Large Binocular Telescope's LUCI1 camera and the ARGOS adaptive optics system. We estimate its black hole mass to lie between $7.70 \leq \log \frac{\text{M}}{\text{M}_\odot} \leq 8.19$, using the correlation with bulge luminosity, or $7.96 \leq \log \frac{\text{M}}{\text{M}_\odot} \leq 8.16$ using the correlation with S茅rsic index, putting its mass at the high end of the Narrow Line Seyfert 1 range. These estimates are independent of the Broad Line Region viewing geometry and avoid underestimates due to looking down the jet axis. Its host shows evidence of a bulge + disc structure, both from two-dimensional modeling and isophote shape, in keeping with the expectations. Mergers and interactions appear to be common among the gamma-ray Narrow-Line Seyfert 1s, and we see some circumstantial evidence for companion galaxies or disturbed features in the host. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.07413v1-abstract-full').style.display = 'none'; document.getElementById('2011.07413v1-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> 14 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">10 pages, 6 figures. Submitted to 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/2009.13346">arXiv:2009.13346</a> <span> [<a href="https://arxiv.org/pdf/2009.13346">pdf</a>, <a href="https://arxiv.org/format/2009.13346">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/staa3023">10.1093/mnras/staa3023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Square Kilometre Array Science Data Challenge 1: analysis and results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bonaldi%2C+A">A. Bonaldi</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+T">T. An</a>, <a href="/search/astro-ph?searchtype=author&query=Bruggen%2C+M">M. Bruggen</a>, <a href="/search/astro-ph?searchtype=author&query=Burkutean%2C+S">S. Burkutean</a>, <a href="/search/astro-ph?searchtype=author&query=Coelho%2C+B">B. Coelho</a>, <a href="/search/astro-ph?searchtype=author&query=Goodarzi%2C+H">H. Goodarzi</a>, <a href="/search/astro-ph?searchtype=author&query=Hartley%2C+P">P. Hartley</a>, <a href="/search/astro-ph?searchtype=author&query=Sandhu%2C+P+K">P. K. Sandhu</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+C">C. Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Yu%2C+L">L. Yu</a>, <a href="/search/astro-ph?searchtype=author&query=Haghighi%2C+M+H+Z">M. H. Zhoolideh Haghighi</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">S. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Bagheri%2C+Z">Z. Bagheri</a>, <a href="/search/astro-ph?searchtype=author&query=Barbosa%2C+D">D. Barbosa</a>, <a href="/search/astro-ph?searchtype=author&query=Barraca%2C+J+P">J. P. Barraca</a>, <a href="/search/astro-ph?searchtype=author&query=Bartashevich%2C+D">D. Bartashevich</a>, <a href="/search/astro-ph?searchtype=author&query=Bergano%2C+M">M. Bergano</a>, <a href="/search/astro-ph?searchtype=author&query=Bonato%2C+M">M. Bonato</a>, <a href="/search/astro-ph?searchtype=author&query=Brand%2C+J">J. Brand</a>, <a href="/search/astro-ph?searchtype=author&query=de+Gasperin%2C+F">F. de Gasperin</a>, <a href="/search/astro-ph?searchtype=author&query=Giannetti%2C+A">A. Giannetti</a>, <a href="/search/astro-ph?searchtype=author&query=Dodson%2C+R">R. Dodson</a>, <a href="/search/astro-ph?searchtype=author&query=Jain%2C+P">P. Jain</a>, <a href="/search/astro-ph?searchtype=author&query=Jaiswal%2C+S">S. Jaiswal</a>, <a href="/search/astro-ph?searchtype=author&query=Lao%2C+B">B. Lao</a> , et al. (20 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="2009.13346v1-abstract-short" style="display: inline;"> As the largest radio telescope in the world, the Square Kilometre Array (SKA) will lead the next generation of radio astronomy. The feats of engineering required to construct the telescope array will be matched only by the techniques developed to exploit the rich scientific value of the data. To drive forward the development of efficient and accurate analysis methods, we are designing a series of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.13346v1-abstract-full').style.display = 'inline'; document.getElementById('2009.13346v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.13346v1-abstract-full" style="display: none;"> As the largest radio telescope in the world, the Square Kilometre Array (SKA) will lead the next generation of radio astronomy. The feats of engineering required to construct the telescope array will be matched only by the techniques developed to exploit the rich scientific value of the data. To drive forward the development of efficient and accurate analysis methods, we are designing a series of data challenges that will provide the scientific community with high-quality datasets for testing and evaluating new techniques. In this paper we present a description and results from the first such Science Data Challenge (SDC1). Based on SKA MID continuum simulated observations and covering three frequencies (560 MHz, 1400MHz and 9200 MHz) at three depths (8 h, 100 h and 1000 h), SDC1 asked participants to apply source detection, characterization and classification methods to simulated data. The challenge opened in November 2018, with nine teams submitting results by the deadline of April 2019. In this work we analyse the results for 8 of those teams, showcasing the variety of approaches that can be successfully used to find, characterise and classify sources in a deep, crowded field. The results also demonstrate the importance of building domain knowledge and expertise on this kind of analysis to obtain the best performance. As high-resolution observations begin revealing the true complexity of the sky, one of the outstanding challenges emerging from this analysis is the ability to deal with highly resolved and complex sources as effectively as the unresolved source population. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.13346v1-abstract-full').style.display = 'none'; document.getElementById('2009.13346v1-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 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">18 pages, 11 figures, accepted by 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/2005.01140">arXiv:2005.01140</a> <span> [<a href="https://arxiv.org/pdf/2005.01140">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</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="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Popular Physics">physics.pop-ph</span> </div> </div> <p class="title is-5 mathjax"> Portuguese SKA White Book </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barbosa%2C+D">Domingos Barbosa</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">Sonia Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Barraca%2C+J+P">Jo茫o Paulo Barraca</a>, <a href="/search/astro-ph?searchtype=author&query=Bergano%2C+M">Miguel Bergano</a>, <a href="/search/astro-ph?searchtype=author&query=Correia%2C+A+C+M">Alexandre C. M. Correia</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+D">Dalmiro Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Ribeiro%2C+V+A+R+M">Val茅rio A. R. M. Ribeiro</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="2005.01140v1-abstract-short" style="display: inline;"> This white book stems from the contributions presented at the Portuguese SKA Days, held on the 6th and 7th February 2018 with the presence of the SKA Deputy Director General Alistair McPherson and the SKA Science Director Robert Braun. This initiative was held to promote the Square Kilometer Array (SKA) - the world's largest radio telescope - among the Portuguese scientific and business communitie… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.01140v1-abstract-full').style.display = 'inline'; document.getElementById('2005.01140v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2005.01140v1-abstract-full" style="display: none;"> This white book stems from the contributions presented at the Portuguese SKA Days, held on the 6th and 7th February 2018 with the presence of the SKA Deputy Director General Alistair McPherson and the SKA Science Director Robert Braun. This initiative was held to promote the Square Kilometer Array (SKA) - the world's largest radio telescope - among the Portuguese scientific and business communities with support from the Portuguese Science and Technology Foundation (FCT) with the contribution of Portuguese policy makers and researchers. The meeting was very successful in providing a detailed overview of the SKA status, vision and goals and describes most of the Portuguese contributions to science, technology and the related industry aspirations <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2005.01140v1-abstract-full').style.display = 'none'; document.getElementById('2005.01140v1-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 May, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">210 pages, UA Editora, Preface in Portuguese, contains arXiv:1607.02415, arXiv:1809.08663</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> UA Editora, April 2020, ISBN 978-972-789-637-0 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.07558">arXiv:1907.07558</a> <span> [<a href="https://arxiv.org/pdf/1907.07558">pdf</a>, <a href="https://arxiv.org/format/1907.07558">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</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"> All-sky Medium Energy Gamma-ray Observatory: Exploring the Extreme Multimessenger Universe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=McEnery%2C+J">Julie McEnery</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">Juan Abel Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">Ivan Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Ajello%2C+M">Marco Ajello</a>, <a href="/search/astro-ph?searchtype=author&query=%C3%81lvarez%2C+J">Jos茅-Manuel 脕lvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">Stefano Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">Sonia Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">Natalia Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Stephen%2C+J+B">John B. Stephen</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+L">Luca Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Bambi%2C+C">Cosimo Bambi</a>, <a href="/search/astro-ph?searchtype=author&query=Baring%2C+M">Matthew Baring</a>, <a href="/search/astro-ph?searchtype=author&query=Barres%2C+U">Ulisses Barres</a>, <a href="/search/astro-ph?searchtype=author&query=Bastieri%2C+D">Denis Bastieri</a>, <a href="/search/astro-ph?searchtype=author&query=Beacom%2C+J">John Beacom</a>, <a href="/search/astro-ph?searchtype=author&query=Beckmann%2C+V">Volker Beckmann</a>, <a href="/search/astro-ph?searchtype=author&query=Bednarek%2C+W">Wlodek Bednarek</a>, <a href="/search/astro-ph?searchtype=author&query=Bernard%2C+D">Denis Bernard</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">Elisabetta Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bloser%2C+P">Peter Bloser</a>, <a href="/search/astro-ph?searchtype=author&query=Blumer%2C+H">Harsha Blumer</a>, <a href="/search/astro-ph?searchtype=author&query=Boettcher%2C+M">Markus Boettcher</a>, <a href="/search/astro-ph?searchtype=author&query=Boggs%2C+S">Steven Boggs</a>, <a href="/search/astro-ph?searchtype=author&query=Bolotnikov%2C+A">Aleksey Bolotnikov</a>, <a href="/search/astro-ph?searchtype=author&query=Bottacini%2C+E">Eugenio Bottacini</a> , et al. (160 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="1907.07558v2-abstract-short" style="display: inline;"> The All-sky Medium Energy Gamma-ray Observatory (AMEGO) is a probe class mission concept that will provide essential contributions to multimessenger astrophysics in the late 2020s and beyond. AMEGO combines high sensitivity in the 200 keV to 10 GeV energy range with a wide field of view, good spectral resolution, and polarization sensitivity. Therefore, AMEGO is key in the study of multimessenger… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.07558v2-abstract-full').style.display = 'inline'; document.getElementById('1907.07558v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.07558v2-abstract-full" style="display: none;"> The All-sky Medium Energy Gamma-ray Observatory (AMEGO) is a probe class mission concept that will provide essential contributions to multimessenger astrophysics in the late 2020s and beyond. AMEGO combines high sensitivity in the 200 keV to 10 GeV energy range with a wide field of view, good spectral resolution, and polarization sensitivity. Therefore, AMEGO is key in the study of multimessenger astrophysical objects that have unique signatures in the gamma-ray regime, such as neutron star mergers, supernovae, and flaring active galactic nuclei. The order-of-magnitude improvement compared to previous MeV missions also enables discoveries of a wide range of phenomena whose energy output peaks in the relatively unexplored medium-energy gamma-ray band. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.07558v2-abstract-full').style.display = 'none'; document.getElementById('1907.07558v2-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, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 July, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2019. </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">Astro2020 APC White Paper Updated to make small change to author list in metadata</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.04607">arXiv:1903.04607</a> <span> [<a href="https://arxiv.org/pdf/1903.04607">pdf</a>, <a href="https://arxiv.org/format/1903.04607">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> <p class="title is-5 mathjax"> High-Energy Polarimetry - a new window to probe extreme physics in AGN jets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rani%2C+B">B. Rani</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">H. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Hunter%2C+S+D">S. D. Hunter</a>, <a href="/search/astro-ph?searchtype=author&query=Kislat%2C+F">F. Kislat</a>, <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ttcher%2C+M">M. B枚ttcher</a>, <a href="/search/astro-ph?searchtype=author&query=McEnery%2C+J+E">J. E. McEnery</a>, <a href="/search/astro-ph?searchtype=author&query=Thompson%2C+D+J">D. J. Thompson</a>, <a href="/search/astro-ph?searchtype=author&query=Giannios%2C+D">D. Giannios</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+F">F. Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+H">H. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Baring%2C+M">M. Baring</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Buson%2C+S">S. Buson</a>, <a href="/search/astro-ph?searchtype=author&query=Petropoulou%2C+M">M. Petropoulou</a>, <a href="/search/astro-ph?searchtype=author&query=Pavlidou%2C+V">V. Pavlidou</a>, <a href="/search/astro-ph?searchtype=author&query=Angelakis%2C+E">E. Angelakis</a>, <a href="/search/astro-ph?searchtype=author&query=Myserlis%2C+I">I. Myserlis</a>, <a href="/search/astro-ph?searchtype=author&query=Wadiasingh%2C+Z">Z. Wadiasingh</a>, <a href="/search/astro-ph?searchtype=author&query=da+Silva%2C+R+M+C">R. M. Curado da Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Kilian%2C+P">P. Kilian</a>, <a href="/search/astro-ph?searchtype=author&query=Guiriec%2C+S">S. Guiriec</a>, <a href="/search/astro-ph?searchtype=author&query=Bozhilov%2C+V+V">V. V. Bozhilov</a>, <a href="/search/astro-ph?searchtype=author&query=Hodgson%2C+J">J. Hodgson</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">S. Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Kazanas%2C+D">D. Kazanas</a> , et al. (9 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="1903.04607v1-abstract-short" style="display: inline;"> The constantly improving sensitivity of ground-based and space-borne observatories has made possible the detection of high-energy emission (X-rays and gamma-rays) from several thousands of extragalactic sources. Enormous progress has been made in measuring the continuum flux enabling us to perform imaging, spectral and timing studies. An important remaining challenge for high-energy astronomy is m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.04607v1-abstract-full').style.display = 'inline'; document.getElementById('1903.04607v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.04607v1-abstract-full" style="display: none;"> The constantly improving sensitivity of ground-based and space-borne observatories has made possible the detection of high-energy emission (X-rays and gamma-rays) from several thousands of extragalactic sources. Enormous progress has been made in measuring the continuum flux enabling us to perform imaging, spectral and timing studies. An important remaining challenge for high-energy astronomy is measuring polarization. The capability to measure polarization is being realized currently at X-ray energies (e.g. with IXPE), and sensitive gamma-ray telescopes capable of measuring polarization, such as AMEGO, AdEPT, e-ASTROGAM, etc., are being developed. These future gamma-ray telescopes will probe the radiation mechanisms and magnetic fields of relativistic jets from active galactic nuclei at spatial scales much smaller than the angular resolution achieved with continuum observations of the instrument. In this white paper, we discuss the scientific potentials of high-energy polarimetry, especially gamma-ray polarimetry, including the theoretical implications, and observational technology advances being made. In particular, we will explore the primary scientific opportunities and wealth of information expected from synergy of multi-wavelength polarimetry that will be brought to multi-messenger astronomy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.04607v1-abstract-full').style.display = 'none'; document.getElementById('1903.04607v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2019. </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">submitted to Astro2020 (Astronomy and Astrophysics Decadal Survey)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.02910">arXiv:1901.02910</a> <span> [<a href="https://arxiv.org/pdf/1901.02910">pdf</a>, <a href="https://arxiv.org/ps/1901.02910">ps</a>, <a href="https://arxiv.org/format/1901.02910">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/10.1093/mnras/sty3526">10.1093/mnras/sty3526 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The space density of z>4 blazars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Caccianiga%2C+A">Alessandro Caccianiga</a>, <a href="/search/astro-ph?searchtype=author&query=Moretti%2C+A">Alberto Moretti</a>, <a href="/search/astro-ph?searchtype=author&query=Belladitta%2C+S">Silvia Belladitta</a>, <a href="/search/astro-ph?searchtype=author&query=Della+Ceca%2C+R">Roberto Della Ceca</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">Sonia Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Ballo%2C+L">Lucia Ballo</a>, <a href="/search/astro-ph?searchtype=author&query=Cicone%2C+C">Claudia Cicone</a>, <a href="/search/astro-ph?searchtype=author&query=Dallacasa%2C+D">Daniele Dallacasa</a>, <a href="/search/astro-ph?searchtype=author&query=Gargiulo%2C+A">Adriana Gargiulo</a>, <a href="/search/astro-ph?searchtype=author&query=Ighina%2C+L">Luca Ighina</a>, <a href="/search/astro-ph?searchtype=author&query=March%C3%A3%2C+M+J">Maria J. March茫</a>, <a href="/search/astro-ph?searchtype=author&query=Severgnini%2C+P">Paola Severgnini</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="1901.02910v1-abstract-short" style="display: inline;"> High redshift blazars are an important class of Active Galactic Nuclei (AGN) that can provide an independent estimate of the supermassive black-hole mass function in high redshift radio-loud AGN without the bias due to absorption along the line-of-sight. Using the Cosmic Lens All Sky Survey (CLASS) we built a complete radio flux-limited sample of high redshift (z>4) blazars suitable for statistica… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.02910v1-abstract-full').style.display = 'inline'; document.getElementById('1901.02910v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.02910v1-abstract-full" style="display: none;"> High redshift blazars are an important class of Active Galactic Nuclei (AGN) that can provide an independent estimate of the supermassive black-hole mass function in high redshift radio-loud AGN without the bias due to absorption along the line-of-sight. Using the Cosmic Lens All Sky Survey (CLASS) we built a complete radio flux-limited sample of high redshift (z>4) blazars suitable for statistical studies. By combining dedicated optical observations and the SDSS spectroscopic database, we obtained a sample of 26 blazar candidates with a spectroscopic redshift above 4. On the basis of their radio spectrum we distinguish between blazars and QSO with a Gigahertz Peaked Spectrum (GPS) like spectrum. Out of the 18 confirmed blazars 14 constitute a completely identified, flux-limited sample down to a magnitude of 21 (AB). Using this complete sample we derive a space density of blazars with 4<z<5.5 of rho=0.13 (+0.05,-0.03) Gpc^-3. This is the first actual estimate of the blazar space density in this range of redshift. This value is in good agreement with the extrapolation of the luminosity function and cosmological evolution based on a sample of flat-spectrum radio quasars selected at lower redshifts and it is consistent with a cosmological evolution peaking at z$\sim$2 similar to radio-quiet QSO. We do not confirm, instead, the presence of a peak at z~4 in the space density evolution, recently suggested using an X-ray selected sample of blazars. It is possible that this extreme peak of the evolution is present only among the most luminous blazars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.02910v1-abstract-full').style.display = 'none'; document.getElementById('1901.02910v1-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 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2019. </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">14 pages, accepted for publication on MNRAS (https://doi.org/10.1093/mnras/sty3526)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.09464">arXiv:1811.09464</a> <span> [<a href="https://arxiv.org/pdf/1811.09464">pdf</a>, <a href="https://arxiv.org/format/1811.09464">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/10.1142/S2251171719400051">10.1142/S2251171719400051 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Baryon acoustic oscillations from Integrated Neutral Gas Observations: Radio frequency interference measurements and telescope site selection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Peel%2C+M+W">M. W. Peel</a>, <a href="/search/astro-ph?searchtype=author&query=Wuensche%2C+C+A">C. A. Wuensche</a>, <a href="/search/astro-ph?searchtype=author&query=Abdalla%2C+E">E. Abdalla</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">S. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Barosi%2C+L">L. Barosi</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=Caldas%2C+M">M. Caldas</a>, <a href="/search/astro-ph?searchtype=author&query=Dickinson%2C+C">C. Dickinson</a>, <a href="/search/astro-ph?searchtype=author&query=Fornazier%2C+K+S+F">K. S. F. Fornazier</a>, <a href="/search/astro-ph?searchtype=author&query=Monstein%2C+C">C. Monstein</a>, <a href="/search/astro-ph?searchtype=author&query=Strauss%2C+C">C. Strauss</a>, <a href="/search/astro-ph?searchtype=author&query=Tancredi%2C+G">G. Tancredi</a>, <a href="/search/astro-ph?searchtype=author&query=Villela%2C+T">T. Villela</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="1811.09464v1-abstract-short" style="display: inline;"> The Baryon acoustic oscillations from Integrated Neutral Gas Observations (BINGO) telescope is a new 40-m class radio telescope to measure the large-angular-scale intensity of Hi emission at 980-1260 MHz to constrain dark energy parameters. As it needs to measure faint cosmological signals at the milliKelvin level, it requires a site that has very low radio frequency interference (RFI) at frequenc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.09464v1-abstract-full').style.display = 'inline'; document.getElementById('1811.09464v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.09464v1-abstract-full" style="display: none;"> The Baryon acoustic oscillations from Integrated Neutral Gas Observations (BINGO) telescope is a new 40-m class radio telescope to measure the large-angular-scale intensity of Hi emission at 980-1260 MHz to constrain dark energy parameters. As it needs to measure faint cosmological signals at the milliKelvin level, it requires a site that has very low radio frequency interference (RFI) at frequencies around 1 GHz. We report on measurement campaigns across Uruguay and Brazil to find a suitable site, which looked at the strength of the mobile phone signals and other radio transmissions, the location of wind turbines, and also included mapping airplane flight paths. The site chosen for the BINGO telescope is a valley at Serra do Urubu, a remote part of Paraiba in North-East Brazil, which has sheltering terrain. During our measurements with a portable receiver we did not detect any RFI in or near the BINGO band, given the sensitivity of the equipment. A radio quiet zone around the selected site has been requested to the Brazilian authorities ahead of the telescope construction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.09464v1-abstract-full').style.display = 'none'; document.getElementById('1811.09464v1-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 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2018. </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">Preprint of an article accepted in the Journal of Astronomical Instrumentation, copyright 2018 World Scientific Publishing Company https://www.worldscientific.com/worldscinet/jai</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1809.01558">arXiv:1809.01558</a> <span> [<a href="https://arxiv.org/pdf/1809.01558">pdf</a>, <a href="https://arxiv.org/format/1809.01558">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> What is in a radio loud NLS1? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">Sonia Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Caccianiga%2C+A">Alessandro Caccianiga</a>, <a href="/search/astro-ph?searchtype=author&query=Bizzocchi%2C+L">Luca Bizzocchi</a>, <a href="/search/astro-ph?searchtype=author&query=Afonso%2C+J">Jose Afonso</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="1809.01558v1-abstract-short" style="display: inline;"> A fraction of Narrow Line Seyfert 1 galaxies (NLS1) are hosted by galaxies that present a disturbed morphology, in some cases hinting for merger processes, that are putative sources of gas replenishment. We have been investigating the poorly studied population of radio loud NLS1 (RL-NLS1) showing a flat radio spectrum, assumed to be the manifestation of the presence of a radio jet. In some of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.01558v1-abstract-full').style.display = 'inline'; document.getElementById('1809.01558v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1809.01558v1-abstract-full" style="display: none;"> A fraction of Narrow Line Seyfert 1 galaxies (NLS1) are hosted by galaxies that present a disturbed morphology, in some cases hinting for merger processes, that are putative sources of gas replenishment. We have been investigating the poorly studied population of radio loud NLS1 (RL-NLS1) showing a flat radio spectrum, assumed to be the manifestation of the presence of a radio jet. In some of the objects the infrared emission is well fitted by a combination of an AGN component and an "active" host galaxy component like M82, the estimate SFR being in the LIRG/ULIRG range (10-500 Msun/year). In order to better characterize that component, we have been investigating the sub-millimeter/millimeter emission of the sources using APEX. Here we present the results concerning a pilot sample of 2 representative objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1809.01558v1-abstract-full').style.display = 'none'; document.getElementById('1809.01558v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 September, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, published on Proceedings of Science - volume "Revisiting narrow-line Seyfert 1 galaxies and their place in the Universe"</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.08953">arXiv:1807.08953</a> <span> [<a href="https://arxiv.org/pdf/1807.08953">pdf</a>, <a href="https://arxiv.org/format/1807.08953">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-3881/aaf5ca">10.3847/1538-3881/aaf5ca <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The interacting late-type host galaxy of the radio-loud narrow-line Seyfert 1 IRAS 20181-2244 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Berton%2C+M">M. Berton</a>, <a href="/search/astro-ph?searchtype=author&query=Congiu%2C+E">E. Congiu</a>, <a href="/search/astro-ph?searchtype=author&query=Ciroi%2C+S">S. Ciroi</a>, <a href="/search/astro-ph?searchtype=author&query=Komossa%2C+S">S. Komossa</a>, <a href="/search/astro-ph?searchtype=author&query=Frezzato%2C+M">M. Frezzato</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Mille%2C+F">F. Di Mille</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">S. Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Antonucci%2C+R">R. Antonucci</a>, <a href="/search/astro-ph?searchtype=author&query=Caccianiga%2C+A">A. Caccianiga</a>, <a href="/search/astro-ph?searchtype=author&query=Coppi%2C+P">P. Coppi</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%A4rvel%C3%A4%2C+E">E. J盲rvel盲</a>, <a href="/search/astro-ph?searchtype=author&query=Kotilainen%2C+J">J. Kotilainen</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=Mathur%2C+S">S. Mathur</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">S. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cracco%2C+V">V. Cracco</a>, <a href="/search/astro-ph?searchtype=author&query=La+Mura%2C+G">G. La Mura</a>, <a href="/search/astro-ph?searchtype=author&query=Rafanelli%2C+P">P. Rafanelli</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="1807.08953v2-abstract-short" style="display: inline;"> Narrow-line Seyfert 1 galaxies (NLS1s) are a class of active galactic nuclei (AGN) which are known to be one of the few sources of $纬$ rays, which originate in a relativistic beamed jet. Becuase of their relatively large distance, a poorly investigated aspect of these jetted NLS1s is their environment, and in particular their host galaxy. In this work we present the results of a morphological anal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.08953v2-abstract-full').style.display = 'inline'; document.getElementById('1807.08953v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.08953v2-abstract-full" style="display: none;"> Narrow-line Seyfert 1 galaxies (NLS1s) are a class of active galactic nuclei (AGN) which are known to be one of the few sources of $纬$ rays, which originate in a relativistic beamed jet. Becuase of their relatively large distance, a poorly investigated aspect of these jetted NLS1s is their environment, and in particular their host galaxy. In this work we present the results of a morphological analysis of the host galaxy of the jetted NLS1 IRAS 20181-2244 observed with the 6.5m Baade Telescope of the Las Campanas Observatory. The GALFIT analysis ran on the Ks image, along with additional spectroscopic observations performed with the Nordic Optical Telescope, clearly revealed the presence of an interacting system of two galaxies. The data suggest that this NLS1 is hosted by a late-type galaxy, although the result is not conclusive. This analysis, along with other results in the literature, might suggest that two populations of jetted NLS1 exist. Further morphological studies are needed to confirm or disprove this hypothesis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.08953v2-abstract-full').style.display = 'none'; document.getElementById('1807.08953v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2018. </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">8 pages, 5 figures, 1 table, accepted for publication by AJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1711.01265">arXiv:1711.01265</a> <span> [<a href="https://arxiv.org/pdf/1711.01265">pdf</a>, <a href="https://arxiv.org/format/1711.01265">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</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/10.1016/j.jheap.2018.07.001">10.1016/j.jheap.2018.07.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Science with e-ASTROGAM (A space mission for MeV-GeV gamma-ray astrophysics) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=De+Angelis%2C+A">A. De Angelis</a>, <a href="/search/astro-ph?searchtype=author&query=Tatischeff%2C+V">V. Tatischeff</a>, <a href="/search/astro-ph?searchtype=author&query=Grenier%2C+I+A">I. A. Grenier</a>, <a href="/search/astro-ph?searchtype=author&query=McEnery%2C+J">J. McEnery</a>, <a href="/search/astro-ph?searchtype=author&query=Mallamaci%2C+M">M. Mallamaci</a>, <a href="/search/astro-ph?searchtype=author&query=Tavani%2C+M">M. Tavani</a>, <a href="/search/astro-ph?searchtype=author&query=Oberlack%2C+U">U. Oberlack</a>, <a href="/search/astro-ph?searchtype=author&query=Hanlon%2C+L">L. Hanlon</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+R">R. Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Argan%2C+A">A. Argan</a>, <a href="/search/astro-ph?searchtype=author&query=Von+Ballmoos%2C+P">P. Von Ballmoos</a>, <a href="/search/astro-ph?searchtype=author&query=Bulgarelli%2C+A">A. Bulgarelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bykov%2C+A">A. Bykov</a>, <a href="/search/astro-ph?searchtype=author&query=Hernanz%2C+M">M. Hernanz</a>, <a href="/search/astro-ph?searchtype=author&query=Kanbach%2C+G">G. Kanbach</a>, <a href="/search/astro-ph?searchtype=author&query=Kuvvetli%2C+I">I. Kuvvetli</a>, <a href="/search/astro-ph?searchtype=author&query=Pearce%2C+M">M. Pearce</a>, <a href="/search/astro-ph?searchtype=author&query=Zdziarski%2C+A">A. Zdziarski</a>, <a href="/search/astro-ph?searchtype=author&query=Conrad%2C+J">J. Conrad</a>, <a href="/search/astro-ph?searchtype=author&query=Ghisellini%2C+G">G. Ghisellini</a>, <a href="/search/astro-ph?searchtype=author&query=Harding%2C+A">A. Harding</a>, <a href="/search/astro-ph?searchtype=author&query=Isern%2C+J">J. Isern</a>, <a href="/search/astro-ph?searchtype=author&query=Leising%2C+M">M. Leising</a>, <a href="/search/astro-ph?searchtype=author&query=Longo%2C+F">F. Longo</a>, <a href="/search/astro-ph?searchtype=author&query=Madejski%2C+G">G. Madejski</a> , et al. (226 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="1711.01265v4-abstract-short" style="display: inline;"> e-ASTROGAM (enhanced ASTROGAM) is a breakthrough Observatory space mission, with a detector composed by a Silicon tracker, a calorimeter, and an anticoincidence system, dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV - the lower energy limit can be pushed to energies as low as 150 keV for the tracker, and to 30 keV for calorimetric detection. The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.01265v4-abstract-full').style.display = 'inline'; document.getElementById('1711.01265v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1711.01265v4-abstract-full" style="display: none;"> e-ASTROGAM (enhanced ASTROGAM) is a breakthrough Observatory space mission, with a detector composed by a Silicon tracker, a calorimeter, and an anticoincidence system, dedicated to the study of the non-thermal Universe in the photon energy range from 0.3 MeV to 3 GeV - the lower energy limit can be pushed to energies as low as 150 keV for the tracker, and to 30 keV for calorimetric detection. The mission is based on an advanced space-proven detector technology, with unprecedented sensitivity, angular and energy resolution, combined with polarimetric capability. Thanks to its performance in the MeV-GeV domain, substantially improving its predecessors, e-ASTROGAM will open a new window on the non-thermal Universe, making pioneering observations of the most powerful Galactic and extragalactic sources, elucidating the nature of their relativistic outflows and their effects on the surroundings. With a line sensitivity in the MeV energy range one to two orders of magnitude better than previous generation instruments, e-ASTROGAM will determine the origin of key isotopes fundamental for the understanding of supernova explosion and the chemical evolution of our Galaxy. The mission will provide unique data of significant interest to a broad astronomical community, complementary to powerful observatories such as LIGO-Virgo-GEO600-KAGRA, SKA, ALMA, E-ELT, TMT, LSST, JWST, Athena, CTA, IceCube, KM3NeT, and LISA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1711.01265v4-abstract-full').style.display = 'none'; document.getElementById('1711.01265v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published on Journal of High Energy Astrophysics (Elsevier)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of High Energy Astrophysics, 2018, 19, 1-106 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1705.00688">arXiv:1705.00688</a> <span> [<a href="https://arxiv.org/pdf/1705.00688">pdf</a>, <a href="https://arxiv.org/format/1705.00688">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201629925">10.1051/0004-6361/201629925 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 1. Testing the parallaxes with local Cepheids and RR Lyrae stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Clementini%2C+G">G. Clementini</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Ripepi%2C+V">V. Ripepi</a>, <a href="/search/astro-ph?searchtype=author&query=Marconi%2C+M">M. Marconi</a>, <a href="/search/astro-ph?searchtype=author&query=Muraveva%2C+T">T. Muraveva</a>, <a href="/search/astro-ph?searchtype=author&query=Garofalo%2C+A">A. Garofalo</a>, <a href="/search/astro-ph?searchtype=author&query=Sarro%2C+L+M">L. M. Sarro</a>, <a href="/search/astro-ph?searchtype=author&query=Palmer%2C+M">M. Palmer</a>, <a href="/search/astro-ph?searchtype=author&query=Luri%2C+X">X. Luri</a>, <a href="/search/astro-ph?searchtype=author&query=Molinaro%2C+R">R. Molinaro</a>, <a href="/search/astro-ph?searchtype=author&query=Rimoldini%2C+L">L. Rimoldini</a>, <a href="/search/astro-ph?searchtype=author&query=Szabados%2C+L">L. Szabados</a>, <a href="/search/astro-ph?searchtype=author&query=Musella%2C+I">I. Musella</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R+I">R. I. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Bailer-Jones%2C+C+A+L">C. A. L. Bailer-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+U">U. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+F">F. Jansen</a> , et al. (566 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="1705.00688v1-abstract-short" style="display: inline;"> Parallaxes for 331 classical Cepheids, 31 Type II Cepheids and 364 RR Lyrae stars in common between Gaia and the Hipparcos and Tycho-2 catalogues are published in Gaia Data Release 1 (DR1) as part of the Tycho-Gaia Astrometric Solution (TGAS). In order to test these first parallax measurements of the primary standard candles of the cosmological distance ladder, that involve astrometry collected by… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.00688v1-abstract-full').style.display = 'inline'; document.getElementById('1705.00688v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1705.00688v1-abstract-full" style="display: none;"> Parallaxes for 331 classical Cepheids, 31 Type II Cepheids and 364 RR Lyrae stars in common between Gaia and the Hipparcos and Tycho-2 catalogues are published in Gaia Data Release 1 (DR1) as part of the Tycho-Gaia Astrometric Solution (TGAS). In order to test these first parallax measurements of the primary standard candles of the cosmological distance ladder, that involve astrometry collected by Gaia during the initial 14 months of science operation, we compared them with literature estimates and derived new period-luminosity ($PL$), period-Wesenheit ($PW$) relations for classical and Type II Cepheids and infrared $PL$, $PL$-metallicity ($PLZ$) and optical luminosity-metallicity ($M_V$-[Fe/H]) relations for the RR Lyrae stars, with zero points based on TGAS. The new relations were computed using multi-band ($V,I,J,K_{\mathrm{s}},W_{1}$) photometry and spectroscopic metal abundances available in the literature, and applying three alternative approaches: (i) by linear least squares fitting the absolute magnitudes inferred from direct transformation of the TGAS parallaxes, (ii) by adopting astrometric-based luminosities, and (iii) using a Bayesian fitting approach. TGAS parallaxes bring a significant added value to the previous Hipparcos estimates. The relations presented in this paper represent first Gaia-calibrated relations and form a "work-in-progress" milestone report in the wait for Gaia-only parallaxes of which a first solution will become available with Gaia's Data Release 2 (DR2) in 2018. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.00688v1-abstract-full').style.display = 'none'; document.getElementById('1705.00688v1-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, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 25 figures. Accepted for publication by A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 605, A79 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.01131">arXiv:1703.01131</a> <span> [<a href="https://arxiv.org/pdf/1703.01131">pdf</a>, <a href="https://arxiv.org/format/1703.01131">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </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/10.1051/0004-6361/201730552">10.1051/0004-6361/201730552 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 1. Open cluster astrometry: performance, limitations, and future prospects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gaia+Collaboration"> Gaia Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+F">F. van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Vallenari%2C+A">A. Vallenari</a>, <a href="/search/astro-ph?searchtype=author&query=Jordi%2C+C">C. Jordi</a>, <a href="/search/astro-ph?searchtype=author&query=Lindegren%2C+L">L. Lindegren</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+U">U. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Prusti%2C+T">T. Prusti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bruijne%2C+J+H+J">J. H. J. de Bruijne</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+G+A">A. G. A. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Babusiaux%2C+C">C. Babusiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Bailer-Jones%2C+C+A+L">C. A. L. Bailer-Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+M">M. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Evans%2C+D+W">D. W. Evans</a>, <a href="/search/astro-ph?searchtype=author&query=Eyer%2C+L">L. Eyer</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+F">F. Jansen</a>, <a href="/search/astro-ph?searchtype=author&query=Klioner%2C+S+A">S. A. Klioner</a>, <a href="/search/astro-ph?searchtype=author&query=Lammers%2C+U">U. Lammers</a>, <a href="/search/astro-ph?searchtype=author&query=Luri%2C+X">X. Luri</a>, <a href="/search/astro-ph?searchtype=author&query=Mignard%2C+F">F. Mignard</a>, <a href="/search/astro-ph?searchtype=author&query=Panem%2C+C">C. Panem</a>, <a href="/search/astro-ph?searchtype=author&query=Pourbaix%2C+D">D. Pourbaix</a>, <a href="/search/astro-ph?searchtype=author&query=Randich%2C+S">S. Randich</a>, <a href="/search/astro-ph?searchtype=author&query=Sartoretti%2C+P">P. Sartoretti</a>, <a href="/search/astro-ph?searchtype=author&query=Siddiqui%2C+H+I">H. I. Siddiqui</a>, <a href="/search/astro-ph?searchtype=author&query=Soubiran%2C+C">C. Soubiran</a> , et al. (567 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="1703.01131v1-abstract-short" style="display: inline;"> Context. The first Gaia Data Release contains the Tycho-Gaia Astrometric Solution (TGAS). This is a subset of about 2 million stars for which, besides the position and photometry, the proper motion and parallax are calculated using Hipparcos and Tycho-2 positions in 1991.25 as prior information. Aims. We investigate the scientific potential and limitations of the TGAS component by means of the ast… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.01131v1-abstract-full').style.display = 'inline'; document.getElementById('1703.01131v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.01131v1-abstract-full" style="display: none;"> Context. The first Gaia Data Release contains the Tycho-Gaia Astrometric Solution (TGAS). This is a subset of about 2 million stars for which, besides the position and photometry, the proper motion and parallax are calculated using Hipparcos and Tycho-2 positions in 1991.25 as prior information. Aims. We investigate the scientific potential and limitations of the TGAS component by means of the astrometric data for open clusters. Methods. Mean cluster parallax and proper motion values are derived taking into account the error correlations within the astrometric solutions for individual stars, an estimate of the internal velocity dispersion in the cluster, and, where relevant, the effects of the depth of the cluster along the line of sight. Internal consistency of the TGAS data is assessed. Results. Values given for standard uncertainties are still inaccurate and may lead to unrealistic unit-weight standard deviations of least squares solutions for cluster parameters. Reconstructed mean cluster parallax and proper motion values are generally in very good agreement with earlier Hipparcos-based determination, although the Gaia mean parallax for the Pleiades is a significant exception. We have no current explanation for that discrepancy. Most clusters are observed to extend to nearly 15 pc from the cluster centre, and it will be up to future Gaia releases to establish whether those potential cluster-member stars are still dynamically bound to the clusters. Conclusions. The Gaia DR1 provides the means to examine open clusters far beyond their more easily visible cores, and can provide membership assessments based on proper motions and parallaxes. A combined HR diagram shows the same features as observed before using the Hipparcos data, with clearly increased luminosities for older A and F dwarfs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.01131v1-abstract-full').style.display = 'none'; document.getElementById('1703.01131v1-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 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </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 by A&A. 21 pages main text plus 46 pages appendices. 34 figures main text, 38 figures appendices. 8 table in main text, 19 tables in appendices</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 601, A19 (2017) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.09501">arXiv:1609.09501</a> <span> [<a href="https://arxiv.org/pdf/1609.09501">pdf</a>, <a href="https://arxiv.org/ps/1609.09501">ps</a>, <a href="https://arxiv.org/format/1609.09501">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/10.1093/mnras/stw2471">10.1093/mnras/stw2471 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SDSSJ143244.91+301435.3 at VLBI: a compact radio galaxy in a narrow-line Seyfert 1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Caccianiga%2C+A">A. Caccianiga</a>, <a href="/search/astro-ph?searchtype=author&query=Dallacasa%2C+D">D. Dallacasa</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">S. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Ballo%2C+L">L. Ballo</a>, <a href="/search/astro-ph?searchtype=author&query=Berton%2C+M">M. Berton</a>, <a href="/search/astro-ph?searchtype=author&query=Mack%2C+K+-">K. -H. Mack</a>, <a href="/search/astro-ph?searchtype=author&query=Paulino-Afonso%2C+A">A. Paulino-Afonso</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="1609.09501v1-abstract-short" style="display: inline;"> We present VLBI observations, carried out with the European Very Long Baseline Interferometry Network (EVN), of SDSSJ143244.91+301435.3, a radio-loud narrow-line Seyfert 1 (RLNLS1) characterized by a steep radio spectrum. The source, compact at Very Large Array (VLA) resolution, is resolved on the milliarcsec scale, showing a central region plus two extended structures. The relatively high brightn… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.09501v1-abstract-full').style.display = 'inline'; document.getElementById('1609.09501v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.09501v1-abstract-full" style="display: none;"> We present VLBI observations, carried out with the European Very Long Baseline Interferometry Network (EVN), of SDSSJ143244.91+301435.3, a radio-loud narrow-line Seyfert 1 (RLNLS1) characterized by a steep radio spectrum. The source, compact at Very Large Array (VLA) resolution, is resolved on the milliarcsec scale, showing a central region plus two extended structures. The relatively high brightness temperature of all components (5x10^6-1.3x10^8 K) supports the hypothesis that the radio emission is non-thermal and likely produced by a relativistic jet and/or small radio lobes. The observed radio morphology, the lack of a significant core and the presence of a low frequency (230 MHz) spectral turnover are reminiscent of the Compact Steep Spectrum sources (CSS). However, the linear size of the source (~0.5kpc) measured from the EVN map is lower than the value predicted using the turnover/size relation valid for CSS sources (~6kpc). This discrepancy can be explained by an additional component not detected in our observations, accounting for about a quarter of the total source flux density, combined to projection effects. The low core-dominance of the source (CD<0.29) confirms that SDSSJ143244.91+301435.3 is not a blazar, i.e. the relativistic jet is not pointing towards the observer. This supports the idea that SDSSJ143244.91+301435.3 may belong to the "parent population" of flat-spectrum RLNLS1 and favours the hypothesis of a direct link between RLNLS1 and compact, possibly young, radio galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.09501v1-abstract-full').style.display = 'none'; document.getElementById('1609.09501v1-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 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </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">8 pages, 3 figures, accepted for publication in MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.04303">arXiv:1609.04303</a> <span> [<a href="https://arxiv.org/pdf/1609.04303">pdf</a>, <a href="https://arxiv.org/format/1609.04303">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/10.1051/0004-6361/201628714">10.1051/0004-6361/201628714 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gaia Data Release 1: Astrometry - one billion positions, two million proper motions and parallaxes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lindegren%2C+L">L. Lindegren</a>, <a href="/search/astro-ph?searchtype=author&query=Lammers%2C+U">U. Lammers</a>, <a href="/search/astro-ph?searchtype=author&query=Bastian%2C+U">U. Bastian</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez%2C+J">J. Hern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Klioner%2C+S">S. Klioner</a>, <a href="/search/astro-ph?searchtype=author&query=Hobbs%2C+D">D. Hobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Bombrun%2C+A">A. Bombrun</a>, <a href="/search/astro-ph?searchtype=author&query=Michalik%2C+D">D. Michalik</a>, <a href="/search/astro-ph?searchtype=author&query=Ramos-Lerate%2C+M">M. Ramos-Lerate</a>, <a href="/search/astro-ph?searchtype=author&query=Butkevich%2C+A">A. Butkevich</a>, <a href="/search/astro-ph?searchtype=author&query=Comoretto%2C+G">G. Comoretto</a>, <a href="/search/astro-ph?searchtype=author&query=Joliet%2C+E">E. Joliet</a>, <a href="/search/astro-ph?searchtype=author&query=Holl%2C+B">B. Holl</a>, <a href="/search/astro-ph?searchtype=author&query=Hutton%2C+A">A. Hutton</a>, <a href="/search/astro-ph?searchtype=author&query=Parsons%2C+P">P. Parsons</a>, <a href="/search/astro-ph?searchtype=author&query=Steidelm%C3%BCller%2C+H">H. Steidelm眉ller</a>, <a href="/search/astro-ph?searchtype=author&query=Abbas%2C+U">U. Abbas</a>, <a href="/search/astro-ph?searchtype=author&query=Altmann%2C+M">M. Altmann</a>, <a href="/search/astro-ph?searchtype=author&query=Andrei%2C+A">A. Andrei</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">S. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Bach%2C+N">N. Bach</a>, <a href="/search/astro-ph?searchtype=author&query=Barache%2C+C">C. Barache</a>, <a href="/search/astro-ph?searchtype=author&query=Becciani%2C+U">U. Becciani</a>, <a href="/search/astro-ph?searchtype=author&query=Berthier%2C+J">J. Berthier</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+L">L. Bianchi</a> , et al. (58 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="1609.04303v1-abstract-short" style="display: inline;"> Gaia Data Release 1 (Gaia DR1) contains astrometric results for more than 1 billion stars brighter than magnitude 20.7 based on observations collected by the Gaia satellite during the first 14 months of its operational phase. We give a brief overview of the astrometric content of the data release and of the model assumptions, data processing, and validation of the results. For stars in common with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.04303v1-abstract-full').style.display = 'inline'; document.getElementById('1609.04303v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.04303v1-abstract-full" style="display: none;"> Gaia Data Release 1 (Gaia DR1) contains astrometric results for more than 1 billion stars brighter than magnitude 20.7 based on observations collected by the Gaia satellite during the first 14 months of its operational phase. We give a brief overview of the astrometric content of the data release and of the model assumptions, data processing, and validation of the results. For stars in common with the Hipparcos and Tycho-2 catalogues, complete astrometric single-star solutions are obtained by incorporating positional information from the earlier catalogues. For other stars only their positions are obtained by neglecting their proper motions and parallaxes. The results are validated by an analysis of the residuals, through special validation runs, and by comparison with external data. Results. For about two million of the brighter stars (down to magnitude ~11.5) we obtain positions, parallaxes, and proper motions to Hipparcos-type precision or better. For these stars, systematic errors depending e.g. on position and colour are at a level of 0.3 milliarcsecond (mas). For the remaining stars we obtain positions at epoch J2015.0 accurate to ~10 mas. Positions and proper motions are given in a reference frame that is aligned with the International Celestial Reference Frame (ICRF) to better than 0.1 mas at epoch J2015.0, and non-rotating with respect to ICRF to within 0.03 mas/yr. The Hipparcos reference frame is found to rotate with respect to the Gaia DR1 frame at a rate of 0.24 mas/yr. Based on less than a quarter of the nominal mission length and on very provisional and incomplete calibrations, the quality and completeness of the astrometric data in Gaia DR1 are far from what is expected for the final mission products. The results nevertheless represent a huge improvement in the available fundamental stellar data and practical definition of the optical reference frame. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.04303v1-abstract-full').style.display = 'none'; document.getElementById('1609.04303v1-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> 14 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </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 Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 595, A4 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1512.03072">arXiv:1512.03072</a> <span> [<a href="https://arxiv.org/pdf/1512.03072">pdf</a>, <a href="https://arxiv.org/format/1512.03072">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/10.1093/mnras/stv2872">10.1093/mnras/stv2872 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Red galaxies with pseudo-bulges in the SDSS: closer to disk galaxies or to classical bulges? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ribeiro%2C+B">B. Ribeiro</a>, <a href="/search/astro-ph?searchtype=author&query=Lobo%2C+C">C. Lobo</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">S. Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Gomes%2C+J+M">J. M. Gomes</a>, <a href="/search/astro-ph?searchtype=author&query=Papaderos%2C+P">P. Papaderos</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="1512.03072v1-abstract-short" style="display: inline;"> Pseudo-bulges are expected to markedly differ from classical, quasi-monolithically forming bulges in their star formation history (SFH) and chemical abundance patterns. To test this simple expectation, we carry out a comparative structural and spectral synthesis analysis of 106 red, massive galaxies issued from the SDSS, subdivided into bulgeless, pseudo-bulge and classical bulge galaxies accordin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.03072v1-abstract-full').style.display = 'inline'; document.getElementById('1512.03072v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.03072v1-abstract-full" style="display: none;"> Pseudo-bulges are expected to markedly differ from classical, quasi-monolithically forming bulges in their star formation history (SFH) and chemical abundance patterns. To test this simple expectation, we carry out a comparative structural and spectral synthesis analysis of 106 red, massive galaxies issued from the SDSS, subdivided into bulgeless, pseudo-bulge and classical bulge galaxies according to their photometric characteristics, and further obeying a specific selection to minimize uncertainties in the analysis and ensure an unbiased derivation and comparison of SFHs. Our 2D photometry analysis suggests that disks underlying pseudo-bulges typically have larger exponential scale lengths than bulgeless galaxies, despite similar integral disk luminosities. Spectral synthesis models of the stellar emission within the 3" SDSS fiber aperture reveal a clear segregation of bulgeless and pseudo-bulge galaxies from classical bulges on the luminosity-weighted planes of age-metallicity and mass-metallicity, though a large dispersion is observed within the two former classes. The secular growth of pseudo-bulges is also reflected upon their cumulative stellar mass as a function of time, which is shallower than that for classical bulges. Such results suggest that the centers of bulgeless and pseudo-bulge galaxies substantially differ from those of bulgy galaxies with respect to their SFH and chemical enrichment history, which likely points to different formation/assembly mechanisms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.03072v1-abstract-full').style.display = 'none'; document.getElementById('1512.03072v1-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2015. </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, 12 figure, accepted for MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2016, MNRAS, 456, 3899 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1504.07068">arXiv:1504.07068</a> <span> [<a href="https://arxiv.org/pdf/1504.07068">pdf</a>, <a href="https://arxiv.org/ps/1504.07068">ps</a>, <a href="https://arxiv.org/format/1504.07068">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> WISE colours and star-formation in the host galaxies of radio-loud narrow-line Seyfert 1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Caccianiga%2C+A">A. Caccianiga</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">S. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Ballo%2C+L">L. Ballo</a>, <a href="/search/astro-ph?searchtype=author&query=Foschini%2C+L">L. Foschini</a>, <a href="/search/astro-ph?searchtype=author&query=Maccacaro%2C+T">T. Maccacaro</a>, <a href="/search/astro-ph?searchtype=author&query=Della+Ceca%2C+R">R. Della Ceca</a>, <a href="/search/astro-ph?searchtype=author&query=Severgnini%2C+P">P. Severgnini</a>, <a href="/search/astro-ph?searchtype=author&query=Marcha%2C+M+J">M. J. Marcha</a>, <a href="/search/astro-ph?searchtype=author&query=Mateos%2C+S">S. Mateos</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</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="1504.07068v1-abstract-short" style="display: inline;"> We investigate the mid-infrared properties of the largest (42 objects) sample of radio-loud narrow-line Seyfert 1 (RL NLS1) collected to date, using data from the Wide-field Infrared Survey Explorer (WISE). We analyse the mid-IR colours of these objects and compare them to what is expected from different combinations of AGN and galaxy templates. We find that, in general, the host-galaxy emission g… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.07068v1-abstract-full').style.display = 'inline'; document.getElementById('1504.07068v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.07068v1-abstract-full" style="display: none;"> We investigate the mid-infrared properties of the largest (42 objects) sample of radio-loud narrow-line Seyfert 1 (RL NLS1) collected to date, using data from the Wide-field Infrared Survey Explorer (WISE). We analyse the mid-IR colours of these objects and compare them to what is expected from different combinations of AGN and galaxy templates. We find that, in general, the host-galaxy emission gives an importan contribution to the observed mid-IR flux in particular at the longest wavelengths (W3, at 12micron, and W4, at 22micron). In about half of the sources (22 objects) we observe a very red mid-IR colour (W4-W3>2.5) that can be explained only using a starburst galaxy template (M82). Using the 22micron luminosities, corrected for the AGN contribution, we have then estimated the star-formation rate for 20 of these "red" RL NLS1, finding values ranging from 10 to 500 Msun/y. For the RL NLS1 showing bluer colours, instead, we cannot exclude the presence of a star-forming host galaxy although, on average, we expect a lower star-formation rate. Studying the radio (1.4GHz) to mid-IR (22micron) flux ratios of the RL NLS1 in the sample we found that in ~10 objects the star-forming activity could represent the most important component also at radio frequencies, in addition (or in alternative) to the relativistic jet. We conclude that both the mid-IR and the radio emission of RL NLS1 are a mixture of different components, including the relativistic jet, the dusty torus and an intense star-forming activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.07068v1-abstract-full').style.display = 'none'; document.getElementById('1504.07068v1-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 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2015. </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 MNRAS, 11 pages, 7 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1409.2518">arXiv:1409.2518</a> <span> [<a href="https://arxiv.org/pdf/1409.2518">pdf</a>, <a href="https://arxiv.org/format/1409.2518">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/10.1088/0004-637X/795/1/58">10.1088/0004-637X/795/1/58 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The host-galaxy of the gamma-ray Narrow-line Seyfert 1 galaxy 1H~0323+342 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Le%C3%B3n-Tavares%2C+J">J. Le贸n-Tavares</a>, <a href="/search/astro-ph?searchtype=author&query=Kotilainen%2C+J">J. Kotilainen</a>, <a href="/search/astro-ph?searchtype=author&query=Chavushyan%2C+V">V. Chavushyan</a>, <a href="/search/astro-ph?searchtype=author&query=A%C3%B1orve%2C+C">C. A帽orve</a>, <a href="/search/astro-ph?searchtype=author&query=Puerari%2C+I">I. Puerari</a>, <a href="/search/astro-ph?searchtype=author&query=Cruz-Gonz%C3%A1lez%2C+I">I. Cruz-Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Pati%C3%B1o-%C3%81lvarez%2C+V">V. Pati帽o-脕lvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">S. Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Carrami%C3%B1ana%2C+A">A. Carrami帽ana</a>, <a href="/search/astro-ph?searchtype=author&query=Carrasco%2C+L">L. Carrasco</a>, <a href="/search/astro-ph?searchtype=author&query=Guichard%2C+J">J. Guichard</a>, <a href="/search/astro-ph?searchtype=author&query=Karhunen%2C+K">K. Karhunen</a>, <a href="/search/astro-ph?searchtype=author&query=Olgu%C3%ADn-Iglesias%2C+A">A. Olgu铆n-Iglesias</a>, <a href="/search/astro-ph?searchtype=author&query=Sanghvi%2C+J">J. Sanghvi</a>, <a href="/search/astro-ph?searchtype=author&query=Valdes%2C+J+R">J. R. Valdes</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="1409.2518v1-abstract-short" style="display: inline;"> We present optical and near infrared (NIR) imaging data of the radio-loud Narrow-line Seyfert 1 galaxy 1H 0323+342, which shows intense and variable gamma-ray activity discovered by the Fermi satellite with the Large Area Telescope. NIR and optical images are used to investigate the structural properties of the host galaxy of 1H 0323+342; this together with optical spectroscopy allowed us to exami… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.2518v1-abstract-full').style.display = 'inline'; document.getElementById('1409.2518v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.2518v1-abstract-full" style="display: none;"> We present optical and near infrared (NIR) imaging data of the radio-loud Narrow-line Seyfert 1 galaxy 1H 0323+342, which shows intense and variable gamma-ray activity discovered by the Fermi satellite with the Large Area Telescope. NIR and optical images are used to investigate the structural properties of the host galaxy of 1H 0323+342; this together with optical spectroscopy allowed us to examine its black hole mass. Based on the 2D multiwavelength surface brightness modeling, we find that, statistically, the best model fit is a combination of a nuclear component and a S茅rsic profile (n~2.8). However, the presence of a disc component (with a small bulge n~1.2) remains also a possibility and cannot be ruled out with the present data. Although at first glance a spiral-arm like structure is revealed in our images, a 2D Fourier analysis of the imagery suggests that such structure corresponds to an asymmetric ring, likely associated to a recent violent dynamical interaction. We discuss our results on the context of relativistic jets production and galaxy evolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.2518v1-abstract-full').style.display = 'none'; document.getElementById('1409.2518v1-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 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2014. </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">14 pages, 6 figures, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1403.3229">arXiv:1403.3229</a> <span> [<a href="https://arxiv.org/pdf/1403.3229">pdf</a>, <a href="https://arxiv.org/ps/1403.3229">ps</a>, <a href="https://arxiv.org/format/1403.3229">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </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/stu508">10.1093/mnras/stu508 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SDSSJ143244.91+301435.3: a link between radio-loud narrow-line Seyfert 1 galaxies and compact steep-spectrum radio sources? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Caccianiga%2C+A">A. Caccianiga</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">S. Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Ballo%2C+L">L. Ballo</a>, <a href="/search/astro-ph?searchtype=author&query=Dallacasa%2C+D">D. Dallacasa</a>, <a href="/search/astro-ph?searchtype=author&query=Della+Ceca%2C+R">R. Della Ceca</a>, <a href="/search/astro-ph?searchtype=author&query=Fanali%2C+R">R. Fanali</a>, <a href="/search/astro-ph?searchtype=author&query=Foschini%2C+L">L. Foschini</a>, <a href="/search/astro-ph?searchtype=author&query=Hamilton%2C+T">T. Hamilton</a>, <a href="/search/astro-ph?searchtype=author&query=Kraus%2C+A">A. Kraus</a>, <a href="/search/astro-ph?searchtype=author&query=Maccacaro%2C+T">T. Maccacaro</a>, <a href="/search/astro-ph?searchtype=author&query=Mack%2C+K+-">K. -H. Mack</a>, <a href="/search/astro-ph?searchtype=author&query=March%C3%A3%2C+M+J">M. J. March茫</a>, <a href="/search/astro-ph?searchtype=author&query=Paulino-Afonso%2C+A">A. Paulino-Afonso</a>, <a href="/search/astro-ph?searchtype=author&query=Sani%2C+E">E. Sani</a>, <a href="/search/astro-ph?searchtype=author&query=Severgnini%2C+P">P. Severgnini</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="1403.3229v1-abstract-short" style="display: inline;"> We present SDSSJ143244.91+301435.3, a new case of radio-loud narrow line Seyfert 1 (RL NLS1) with a relatively high radio power (P1.4GHz=2.1x10^25 W Hz^-1) and large radioloudness parameter (R1.4=600+/-100). The radio source is compact with a linear size below ~1.4 kpc but, contrary to most of the RL NLS1 discovered so far with such a high R1.4, its radio spectrum is very steep (alpha=0.93) and no… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1403.3229v1-abstract-full').style.display = 'inline'; document.getElementById('1403.3229v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1403.3229v1-abstract-full" style="display: none;"> We present SDSSJ143244.91+301435.3, a new case of radio-loud narrow line Seyfert 1 (RL NLS1) with a relatively high radio power (P1.4GHz=2.1x10^25 W Hz^-1) and large radioloudness parameter (R1.4=600+/-100). The radio source is compact with a linear size below ~1.4 kpc but, contrary to most of the RL NLS1 discovered so far with such a high R1.4, its radio spectrum is very steep (alpha=0.93) and not supporting a 'blazar-like' nature. Both the small mass of the central super-massive black-hole and the high accretion rate relative to the Eddington limit estimated for this object (3.2x10^7 Msun and 0.27, respectively, with a formal error of ~0.4 dex on both quantities) are typical of the class of NLS1. Through a modeling of the spectral energy distribution of the source we have found that the galaxy hosting SDSSJ143244.91+301435.3 is undergoing a quite intense star-formation (SFR=50 Msun y^-1) which, however, is expected to contribute only marginally (~1 per cent) to the observed radio emission. The radio properties of SDSSJ143244.91+301435.3 are remarkably similar to those of compact steep spectrum (CSS) radio sources, a class of AGN mostly composed by young radio galaxies. This may suggest a direct link between these two classes of AGN, with the CSS sources possibly representing the misaligned version (the so-called parent population) of RL NLS1 showing blazar characteristics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1403.3229v1-abstract-full').style.display = 'none'; document.getElementById('1403.3229v1-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 March, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2014. </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">14 pages, 7 figures, 4 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/1401.7767">arXiv:1401.7767</a> <span> [<a href="https://arxiv.org/pdf/1401.7767">pdf</a>, <a href="https://arxiv.org/ps/1401.7767">ps</a>, <a href="https://arxiv.org/format/1401.7767">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/782/1/22">10.1088/0004-637X/782/1/22 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Bulgeless Galaxies at Intermediate Redshift: Sample Selection, Colour Properties, and the Existence of Powerful AGN </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bizzocchi%2C+L">Luca Bizzocchi</a>, <a href="/search/astro-ph?searchtype=author&query=Filho%2C+M+E">Mercedes E. Filho</a>, <a href="/search/astro-ph?searchtype=author&query=Leonardo%2C+E">Elvira Leonardo</a>, <a href="/search/astro-ph?searchtype=author&query=Grossi%2C+M">Marco Grossi</a>, <a href="/search/astro-ph?searchtype=author&query=Griffith%2C+R+L">Roger L. Griffith</a>, <a href="/search/astro-ph?searchtype=author&query=Afonso%2C+J">Jos茅 Afonso</a>, <a href="/search/astro-ph?searchtype=author&query=Fernandes%2C+C">Cristina Fernandes</a>, <a href="/search/astro-ph?searchtype=author&query=Retr%C3%AA%2C+J">Jo茫o Retr锚</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">Sonia Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Bell%2C+E+F">Eric F. Bell</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">Jarle Brinchmann</a>, <a href="/search/astro-ph?searchtype=author&query=Henriques%2C+B">Bruno Henriques</a>, <a href="/search/astro-ph?searchtype=author&query=Lobo%2C+C">Catarina Lobo</a>, <a href="/search/astro-ph?searchtype=author&query=Messias%2C+H">Hugo Messias</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="1401.7767v1-abstract-short" style="display: inline;"> We present a catalogue of bulgeless galaxies, which includes 19225 objects selected in four of the deepest, largest multi-wavelength datasets available -- COSMOS, AEGIS, GEMS and GOODS -- at intermediate redshift ($0.4 \leq z \leq 1.0$). The morphological classification was provided by the Advanced Camera for Surveys General Catalogue (ACS-GC), which used publicly available data obtained with the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.7767v1-abstract-full').style.display = 'inline'; document.getElementById('1401.7767v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1401.7767v1-abstract-full" style="display: none;"> We present a catalogue of bulgeless galaxies, which includes 19225 objects selected in four of the deepest, largest multi-wavelength datasets available -- COSMOS, AEGIS, GEMS and GOODS -- at intermediate redshift ($0.4 \leq z \leq 1.0$). The morphological classification was provided by the Advanced Camera for Surveys General Catalogue (ACS-GC), which used publicly available data obtained with the ACS instrument on the Hubble Space Telescope. Rest-frame photometric quantities were derived using kcorrect. We analyse the properties of the sample and the evolution of pure-disc systems with redshift. Very massive [$\log (M_\star/M_{\odot}) > 10.5$] bulgeless galaxies contribute to ~30% of the total galaxy population number density at $z \geq 0.7$, but their number density drops substantially with decreasing redshift. We show that only a negligible fraction of pure discs appear to be quiescent systems, and red sequence bulgeless galaxies show indications of dust-obscured star formation. X-ray catalogues were used to search for X-ray emission within our sample. After visual inspection and detailed parametric morphological fitting we identify 30 AGN that reside in galaxies without a classical bulge. The finding of such peculiar objects at intermediate redshift shows that while AGN growth in merger-free systems is a rare event (0.2% AGN hosts in this sample of bulgeless galaxies), it can indeed happen relatively early in the Universe history. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.7767v1-abstract-full').style.display = 'none'; document.getElementById('1401.7767v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">49 pages, 13 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophysical Journal, 782, 22 (2013) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1309.4120">arXiv:1309.4120</a> <span> [<a href="https://arxiv.org/pdf/1309.4120">pdf</a>, <a href="https://arxiv.org/ps/1309.4120">ps</a>, <a href="https://arxiv.org/format/1309.4120">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> </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/stt1736">10.1093/mnras/stt1736 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Red bulgeless galaxies in SDSS DR7. Are there any AGN hosts? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Coelho%2C+B">Bruno Coelho</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">Sonia Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Lobo%2C+C">Catarina Lobo</a>, <a href="/search/astro-ph?searchtype=author&query=Ribeiro%2C+B">Bruno Ribeiro</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="1309.4120v1-abstract-short" style="display: inline;"> With the main goal of finding bulgeless galaxies harbouring super massive black holes and showing, at most, just residual star formation activity, we have selected a sample of massive bulgeless red sequence galaxies from the SDSS-DR7, based on the NYU-VAGC catalogue. Multivavelength data were retrieved using EURO-VO tools, and the objects are characterised in terms of degree of star formation and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.4120v1-abstract-full').style.display = 'inline'; document.getElementById('1309.4120v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1309.4120v1-abstract-full" style="display: none;"> With the main goal of finding bulgeless galaxies harbouring super massive black holes and showing, at most, just residual star formation activity, we have selected a sample of massive bulgeless red sequence galaxies from the SDSS-DR7, based on the NYU-VAGC catalogue. Multivavelength data were retrieved using EURO-VO tools, and the objects are characterised in terms of degree of star formation and the presence of an AGN. We have found seven objects that are quenched massive galaxies, that have no prominent bulge and that show signs of extra activity in their nuclei, five of them being central in their halo. These objects are rather robust candidates for rare systems that, though devoid of a significant bulge, harbor a supermassive black hole with an activity level likely capable of having halted the star formation through feedback. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.4120v1-abstract-full').style.display = 'none'; document.getElementById('1309.4120v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 September, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2013. </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 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/1210.4972">arXiv:1210.4972</a> <span> [<a href="https://arxiv.org/pdf/1210.4972">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Physics and Society">physics.soc-ph</span> </div> </div> <p class="title is-5 mathjax"> Power Challenges of Large Scale Research Infrastructures: the Square Kilometer Array and Solar Energy Integration; Towards a zero-carbon footprint next generation telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barbosa%2C+D">Domingos Barbosa</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%A1rquez%2C+G+L">Gonzalo Lobo M谩rquez</a>, <a href="/search/astro-ph?searchtype=author&query=Ruiz%2C+V">Valeriano Ruiz</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+M">Manuel Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Verdes-Montenegro%2C+L">Lourdes Verdes-Montenegro</a>, <a href="/search/astro-ph?searchtype=author&query=Santander-Vela%2C+J">Juande Santander-Vela</a>, <a href="/search/astro-ph?searchtype=author&query=Maia%2C+D">Dalmiro Maia</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">Sonia Ant贸n</a>, <a href="/search/astro-ph?searchtype=author&query=van+Ardenne%2C+A">Arnold van Ardenne</a>, <a href="/search/astro-ph?searchtype=author&query=Vetter%2C+M">Matthias Vetter</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+M">Michael Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Keller%2C+R">Reinhard Keller</a>, <a href="/search/astro-ph?searchtype=author&query=Pereira%2C+N">Nuno Pereira</a>, <a href="/search/astro-ph?searchtype=author&query=Silva%2C+V">Vitor Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+B">The BIOSTIRLING Consortium</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="1210.4972v1-abstract-short" style="display: inline;"> The Square Kilometer Array (SKA) will be the largest Global science project of the next two decades. It will encompass a sensor network dedicated to radioastronomy, covering two continents. It will be constructed in remote areas of South Africa and Australia, spreading over 3000Km, in high solar irradiance latitudes. Solar Power supply is therefore an option to power supply the SKA and contribute… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1210.4972v1-abstract-full').style.display = 'inline'; document.getElementById('1210.4972v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1210.4972v1-abstract-full" style="display: none;"> The Square Kilometer Array (SKA) will be the largest Global science project of the next two decades. It will encompass a sensor network dedicated to radioastronomy, covering two continents. It will be constructed in remote areas of South Africa and Australia, spreading over 3000Km, in high solar irradiance latitudes. Solar Power supply is therefore an option to power supply the SKA and contribute to a zero carbon footprint next generation telescope. Here we outline the major characteristics of the SKA and some innovation approaches on thermal solar energy Integration with SKA prototypes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1210.4972v1-abstract-full').style.display = 'none'; document.getElementById('1210.4972v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2012. </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">4 pages; 3 figures. Paper accepted for presentation at Proceedings of the 2nd International Workshop on Integration on Solar Power into Power Systems; 12th-13th November, 2012, Lisbon, Portugal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1110.0339">arXiv:1110.0339</a> <span> [<a href="https://arxiv.org/pdf/1110.0339">pdf</a>, <a href="https://arxiv.org/format/1110.0339">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> </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/10.1051/0004-6361/201117834">10.1051/0004-6361/201117834 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optically Faint Radio Sources: Reborn AGN? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Filho%2C+M+E">Mercedes E. Filho</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">Jarle Brinchmann</a>, <a href="/search/astro-ph?searchtype=author&query=Lobo%2C+C">Catarina Lobo</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">Sonia Ant贸n</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="1110.0339v1-abstract-short" style="display: inline;"> We have discovered a number of relatively strong radio sources in the field-of-view of SDSS galaxy clusters which present no optical counterparts down to the magnitude limits of the SDSS. The optically faint radio sources appear as double-lobed or core-jet objects on the FIRST radio images and have projected angular sizes ranging from 0.5 to 1.0 arcmin. We have followed-up these sources with near-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1110.0339v1-abstract-full').style.display = 'inline'; document.getElementById('1110.0339v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1110.0339v1-abstract-full" style="display: none;"> We have discovered a number of relatively strong radio sources in the field-of-view of SDSS galaxy clusters which present no optical counterparts down to the magnitude limits of the SDSS. The optically faint radio sources appear as double-lobed or core-jet objects on the FIRST radio images and have projected angular sizes ranging from 0.5 to 1.0 arcmin. We have followed-up these sources with near-infrared imaging using the wide-field imager HAWK-I on the VLT. K_s-band emitting regions, about 1.5 arcsec in size and coincident with the centers of the radio structures, were detected in all the sources, with magnitudes in the range 17-20 mag. We have used spectral modelling to characterize the sample sources. In general, the radio properties are similar to those observed in 3CRR sources but the optical-radio slopes are consistent with moderate to high redshift (z<4) gigahertz-peaked spectrum sources. Our results suggest that these unusual objects are galaxies whose black hole has been recently re-ignited but retain large-scale radio structures, signatures of previous AGN activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1110.0339v1-abstract-full').style.display = 'none'; document.getElementById('1110.0339v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 October, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2011. </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</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1109.3659">arXiv:1109.3659</a> <span> [<a href="https://arxiv.org/pdf/1109.3659">pdf</a>, <a href="https://arxiv.org/ps/1109.3659">ps</a>, <a href="https://arxiv.org/format/1109.3659">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201117245">10.1051/0004-6361/201117245 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Photo-centric variability of quasars caused by variations in their inner structure: Consequences on Gaia measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+L+C">Luka C. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Jovanovic%2C+P">Predrag Jovanovic</a>, <a href="/search/astro-ph?searchtype=author&query=Stalevski%2C+M">Marko Stalevski</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">Sonia Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Andrei%2C+A+H">Alexandre H. Andrei</a>, <a href="/search/astro-ph?searchtype=author&query=Kovacevic%2C+J">Jelena Kovacevic</a>, <a href="/search/astro-ph?searchtype=author&query=Baes%2C+M">Maarten Baes</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="1109.3659v3-abstract-short" style="display: inline;"> We study the photocenter position variability due to variations in the quasar inner structure. We consider variability in the accretion disk emissivity and torus structure variability due to different illumination by the central source. We discuss possible detection of these effects by Gaia. Observations of the photocenter variability in two AGNs, SDSS J121855+020002 and SDSS J162011+1724327 have… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1109.3659v3-abstract-full').style.display = 'inline'; document.getElementById('1109.3659v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1109.3659v3-abstract-full" style="display: none;"> We study the photocenter position variability due to variations in the quasar inner structure. We consider variability in the accretion disk emissivity and torus structure variability due to different illumination by the central source. We discuss possible detection of these effects by Gaia. Observations of the photocenter variability in two AGNs, SDSS J121855+020002 and SDSS J162011+1724327 have been reported and discussed. With investigation of the variations in the quasar inner structure we explore how much this effect can affect the position determination and whether it can be (or not) detected with Gaia mission. We used (a) a model of a relativistic disk, including the perturbation that can increase brightness of a part of the disk, and consequently offset the photocenter position, and (b) a model of a dusty torus which absorbs and re-emits the incoming radiation from accretion disk. We estimated the value of the photocenter offset due to these two effects. We found that perturbations in the inner structure can significantly offset the photocenter. It depends on the characteristics of perturbation and accretion disk and structure of the torus. In the case of two considered QSOs the observed photocenter offsets cannot be explained by variations in the accretion disk and other effects should be considered. We discussed possibility of exploding stars very close to the AGN source, and also possibility that there are two variable sources in the center of these two AGNs that may indicate a binary super-massive black hole system on a kpc (pc) scale. The Gaia mission seems to be very perspective, not only for astrometry, but also for exploring the inner structure of AGNs. We conclude that variations in the quasar inner structure can affect the observed photocenter (up to several mas). There is a chance to observe such effect in the case of bright and low-redshifted QSOs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1109.3659v3-abstract-full').style.display = 'none'; document.getElementById('1109.3659v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 October, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 September, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2011. </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, 8 figures, 3 tables. Accepted for publication in Astronomy and Astrophysics. Language improved, typos corrected</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0907.2400">arXiv:0907.2400</a> <span> [<a href="https://arxiv.org/pdf/0907.2400">pdf</a>, <a href="https://arxiv.org/ps/0907.2400">ps</a>, <a href="https://arxiv.org/format/0907.2400">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361:20078926">10.1051/0004-6361:20078926 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The colour of the narrow line Sy1-blazar 0324+3410 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">S. Anton</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=Marcha%2C+M+J">M. J. Marcha</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="0907.2400v1-abstract-short" style="display: inline;"> Aims. We investigate the properties of the host galaxy of the blazar J0324+3410 (B2 0321+33) by the analysis of B and R images obtained with the NOT under good photometric conditions. Methods: The galaxy was studied using different methods: Sersic model fitting, unsharp-masked images, B-R image and B-R profile analysis. Results: The images show that the host galaxy has a ring-like morphology. Th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.2400v1-abstract-full').style.display = 'inline'; document.getElementById('0907.2400v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0907.2400v1-abstract-full" style="display: none;"> Aims. We investigate the properties of the host galaxy of the blazar J0324+3410 (B2 0321+33) by the analysis of B and R images obtained with the NOT under good photometric conditions. Methods: The galaxy was studied using different methods: Sersic model fitting, unsharp-masked images, B-R image and B-R profile analysis. Results: The images show that the host galaxy has a ring-like morphology. The B-R colour image reveals two bluish zones: one that coincides with the nuclear region, interpreted as the signature of emission related to the active nucleus, the other zone is extended and is located in the host ring-structure. We discuss the hypothesis that the later is thermal emission from a burst of star formation triggered by an interacting/merging process. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0907.2400v1-abstract-full').style.display = 'none'; document.getElementById('0907.2400v1-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> 14 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">Journal ref:</span> Astron.Astrophys.583:490,2008 </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/0505170">arXiv:astro-ph/0505170</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0505170">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0505170">ps</a>, <a href="https://arxiv.org/format/astro-ph/0505170">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/10.1111/j.1365-2966.2005.09180.x">10.1111/j.1365-2966.2005.09180.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Unification in the low radio luminosity regime; evidence from optical line emission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=March%C3%A3%2C+M+J+M">M. J. M. March茫</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=Jethava%2C+N">N. Jethava</a>, <a href="/search/astro-ph?searchtype=author&query=Ant%C3%B3n%2C+S">S. Ant贸n</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/0505170v1-abstract-short" style="display: inline;"> We address the question of whether or not the properties of all low-luminosity flat spectrum radio sources, not just the obvious BL Lac objects, are consistent with them being the relativistically beamed counterparts of the low radio luminosity radio galaxies (the Fanaroff-Riley type 1 - FRI). We compare the emission-line luminosities of a well studied sample of core-dominated radio sources with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0505170v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0505170v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0505170v1-abstract-full" style="display: none;"> We address the question of whether or not the properties of all low-luminosity flat spectrum radio sources, not just the obvious BL Lac objects, are consistent with them being the relativistically beamed counterparts of the low radio luminosity radio galaxies (the Fanaroff-Riley type 1 - FRI). We compare the emission-line luminosities of a well studied sample of core-dominated radio sources with a matched sample of FR I radio galaxies. The emission lines in the core-dominated objects are on average significantly more luminous than those in the comparison sample, inconsistent with the simplest unified models in which there is no orientation dependence of the line emission. However, the results are equally consistent with a scenario in which, for the majority of objects, beaming has minimal effect on the observed core luminosities of a large fraction of the FRI population and that intrinsically stronger cores simply give rise to stronger emission lines. We conclude that FRI unification is much more complex than usually portrayed, and models combining beaming with an intrinsic relationship between core and emission line strengths need to be explored. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0505170v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0505170v1-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 May, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2005. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, accepted for publication in MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mon.Not.Roy.Astron.Soc. 361 (2005) 469-475 </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/0409643">arXiv:astro-ph/0409643</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0409643">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0409643">ps</a>, <a href="https://arxiv.org/format/astro-ph/0409643">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/10.1111/j.1365-2966.2004.08441.x">10.1111/j.1365-2966.2004.08441.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The recognition of blazars and the blazar spectral sequence </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">S. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Browne%2C+I+W+A">I. W. A. Browne</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/0409643v1-abstract-short" style="display: inline;"> We analyse a group of radio sources, a subset of the 200 mJy sample, all of which have core-jet radio structures measured with VLBI and have flat spectra stretching from the radio to the millimetre/sub-millimetre band. Thus the objects have most of the properties expected of blazars. However, they display varied optical properties ranging from ``Seyfert-like'' objects, through BL Lac objects, to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0409643v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0409643v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0409643v1-abstract-full" style="display: none;"> We analyse a group of radio sources, a subset of the 200 mJy sample, all of which have core-jet radio structures measured with VLBI and have flat spectra stretching from the radio to the millimetre/sub-millimetre band. Thus the objects have most of the properties expected of blazars. However, they display varied optical properties ranging from ``Seyfert-like'' objects, through BL Lac objects, to ``normal'' elliptical galaxies. We investigate the distribution of synchrotron peak frequencies in their Spectral Energy Distributions (SEDs) and find a broad distribution between 10^12 and 10^16 Hz. Our conclusion is that we should consider virtually all objects in the sample as blazars since much of the diversity in their classification based on traditional optical criteria arises from differences in the frequency at which the non-thermal emission begins to decline. Specifically, an object is only classified as BL Lac when its peak frequency falls in the near IR/optical range. We determine peak frequencies using the same method for objects from other blazar samples. An important result is that our objects do not follow the blazar spectral sequence proposed by Fossati et al. and Ghisellini et al. in which, on average, peak frequencies increase as the radio luminosity decreases. Most of our low radio-luminosity sources have peaks in their SEDs at low frequencies, not at the expected high frequencies. We suggest that at least part of the systematic trend seen by Fossati et al. and Ghisellini et al. results from selection effects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0409643v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0409643v1-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 September, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2004. </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 MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mon.Not.Roy.Astron.Soc. 356 (2005) 225-231 </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/0404606">arXiv:astro-ph/0404606</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0404606">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0404606">ps</a>, <a href="https://arxiv.org/format/astro-ph/0404606">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/10.1111/j.1365-2966.2004.07961.x">10.1111/j.1365-2966.2004.07961.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The SEDs of the revised 200 mJy sample </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">S. Anton</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=Marcha%2C+M+J+M">M. J. M. Marcha</a>, <a href="/search/astro-ph?searchtype=author&query=Bondi%2C+M">M. Bondi</a>, <a href="/search/astro-ph?searchtype=author&query=Polatidis%2C+A">A. Polatidis</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/0404606v2-abstract-short" style="display: inline;"> We address the question of why low-luminosity radio sources with similar flat radio spectra show a range of optical activity. The investigation is based on the spectral energy distributions (SEDs) of objects from the 200 mJy sample. We gathered new data from the VLA at 43 GHz, from SCUBA in the JCMT at 2000, 1350 and 850 micron and from the ISOPHOT instrument on ISO at 170, 90, 60 and 25 micron.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0404606v2-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0404606v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0404606v2-abstract-full" style="display: none;"> We address the question of why low-luminosity radio sources with similar flat radio spectra show a range of optical activity. The investigation is based on the spectral energy distributions (SEDs) of objects from the 200 mJy sample. We gathered new data from the VLA at 43 GHz, from SCUBA in the JCMT at 2000, 1350 and 850 micron and from the ISOPHOT instrument on ISO at 170, 90, 60 and 25 micron. There is considerable diversity amongst the SEDs of the objects: there are objects with steep broadband spectra between centimetre and millimetre bands (14% of the sample), there are those with flat broadband spectra over most of the spectral range (48% of the sample) and there are those which show pronounced sub-mm/infrared excesses (27% of the sample). Some objects of the first group have two sided radio morphology indicating that their pc-scale emission is not dominated by beamed jet emission. Amongst the objects that have smooth broadband spectra from the radio to the infrared there are passive elliptical galaxies as well as the expected BL Lacs objects. The most pronounced sub-mm/infrared excesses are shown by the broad emission line objects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0404606v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0404606v2-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 May, 2004; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 April, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2004. </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 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/astro-ph/0207173">arXiv:astro-ph/0207173</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0207173">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0207173">ps</a>, <a href="https://arxiv.org/format/astro-ph/0207173">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/10.1046/j.1365-8711.2002.05763.x">10.1046/j.1365-8711.2002.05763.x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The orientation of the Seyfert nucleus in Markarian 348 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anton%2C+S">S. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Thean%2C+A">A. Thean</a>, <a href="/search/astro-ph?searchtype=author&query=Pedlar%2C+A">A. Pedlar</a>, <a href="/search/astro-ph?searchtype=author&query=Browne%2C+I+W+A">I. W. A. Browne</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/0207173v1-abstract-short" style="display: inline;"> Multi-frequency observations of Mrk 348 are presented consisting of 2 epochs of MERLIN data at 5 GHz, ISOPHOT data at 170, 90, 60 and 25 micron, NOT images at U, B, R and I bands and data at 1350 micron from the archive for SCUBA. The new optical images reveal a disrupted arm that ends towards the eastern companion of Mrk 348, consistent with the hypothesis that Mrk 348 and its companion form an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0207173v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0207173v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0207173v1-abstract-full" style="display: none;"> Multi-frequency observations of Mrk 348 are presented consisting of 2 epochs of MERLIN data at 5 GHz, ISOPHOT data at 170, 90, 60 and 25 micron, NOT images at U, B, R and I bands and data at 1350 micron from the archive for SCUBA. The new optical images reveal a disrupted arm that ends towards the eastern companion of Mrk 348, consistent with the hypothesis that Mrk 348 and its companion form an interacting system. 5 GHz MERLIN imaging shows that only one of the radio components of Mrk 348 is polarized (%P=5). The broadband spectrum of Mrk 348 is flat between the radio and millimetre bands, suggesting that synchrotron emission extends to high frequencies. Mrk 348 has many of the characteristics of a radio-loud object. We discuss the orientation of the radio axis of Mrk 348 with respect to the line of sight. We conclude that the evidence is conflicting, and the geometry in Mrk 348 is not well-described by a simple edge-on or face-on model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0207173v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0207173v1-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 July, 2002; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2002. </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 MNRAS; higher resolution images at http://www.oal.ul.pt/ftp-anon/Images</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mon.Not.Roy.Astron.Soc. 336 (2002) 319 </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 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