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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2503.00194">arXiv:2503.00194</a> <span> [<a href="https://arxiv.org/pdf/2503.00194">pdf</a>, <a href="https://arxiv.org/format/2503.00194">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The multi-wavelength Tully-Fisher relation in the TNG50 cosmological simulation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Baes%2C+M">Maarten Baes</a>, <a href="/search/astro-ph?searchtype=author&query=Gebek%2C+A">Andrea Gebek</a>, <a href="/search/astro-ph?searchtype=author&query=Kunene%2C+S">Sabelo Kunene</a>, <a href="/search/astro-ph?searchtype=author&query=Leeuw%2C+L">Lerothodi Leeuw</a>, <a href="/search/astro-ph?searchtype=author&query=Nelson%2C+D">Dylan Nelson</a>, <a href="/search/astro-ph?searchtype=author&query=Ponomareva%2C+A+A">Anastasia A. Ponomareva</a>, <a href="/search/astro-ph?searchtype=author&query=Andreadis%2C+N">Nick Andreadis</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchetti%2C+A">Alessandro Bianchetti</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Rajohnson%2C+S+H+A">Sambatriniaina H. A. Rajohnson</a>, <a href="/search/astro-ph?searchtype=author&query=Sorgho%2C+A">Amidou Sorgho</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="2503.00194v1-abstract-short" style="display: inline;"> The Tully-Fisher relation (TFR) is one of the most important and widely used empirical correlations in extragalactic astronomy. Apart from its importance as a secondary distance indicator, the TFR relation serves as a test for galaxy evolution models, because it connects the baryonic and dark matter components of galaxies. We aim at simulating the multi-wavelength TFR relation from UV to mid-infra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2503.00194v1-abstract-full').style.display = 'inline'; document.getElementById('2503.00194v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2503.00194v1-abstract-full" style="display: none;"> The Tully-Fisher relation (TFR) is one of the most important and widely used empirical correlations in extragalactic astronomy. Apart from its importance as a secondary distance indicator, the TFR relation serves as a test for galaxy evolution models, because it connects the baryonic and dark matter components of galaxies. We aim at simulating the multi-wavelength TFR relation from UV to mid-infrared wavelengths for the TNG50 cosmological simulation at $z = 0$, and at comparing the results with observational TFR studies. We want to compare the wavelength dependence of the slope and scatter with the observed values, and search for secondary parameters that reduce the scatter in the TFR. We select a large sample of simulated late-type, disc-dominated galaxies from the TNG50 simulation. For each galaxy, we use the SKIRT radiative transfer code to generate realistic synthetic global fluxes in 12 UV to mid-infrared broadbands and synthetic integrated HI line profiles. We use bivariate linear regression to determine the TFR in each band, and we search for a second TFR parameter by correlating the residuals with different physical parameters. Our TNG50 TFR reproduces the characteristic behaviour of the observed TFR in many studies: the TFR becomes steeper and tighter as we move from UV/optical to infrared wavelengths. The slope changes from $-7.46 \pm 0.14~{\text{mag}}~{\text{dex}}^{-1}$ in the NUV band to $-9.66 \pm 0.09~{\text{mag}}~{\text{dex}}^{-1}$ in the IRAC [4.5] band. Quantitatively, our slopes are well within the spread of different observational results. The ${\textit{u}} - {\textit{r}}$ colour or the sSFR can significantly reduce the scatter in the UV and optical bands. Using ${\textit{u}} - {\textit{r}}$ colour as second parameter, the modified TFR has a roughly constant intrinsic tightness of over the entire UV to MIR range. The combination of the TNG50... <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2503.00194v1-abstract-full').style.display = 'none'; document.getElementById('2503.00194v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 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/2411.11584">arXiv:2411.11584</a> <span> [<a href="https://arxiv.org/pdf/2411.11584">pdf</a>, <a href="https://arxiv.org/format/2411.11584">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/10.1051/0004-6361/202452085">10.1051/0004-6361/202452085 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for HI around MHONGOOSE Galaxies via Spectral Stacking </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Veronese%2C+S">S. Veronese</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Healy%2C+J">J. Healy</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Marasco%2C+A">A. Marasco</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Brinks%2C+E">E. Brinks</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Zabel%2C+N">N. Zabel</a>, <a href="/search/astro-ph?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Kurapati%2C+S">S. Kurapati</a>, <a href="/search/astro-ph?searchtype=author&query=Sorgho%2C+A">A. Sorgho</a>, <a href="/search/astro-ph?searchtype=author&query=Spekkens%2C+K">K. Spekkens</a>, <a href="/search/astro-ph?searchtype=author&query=Combes%2C+F">F. Combes</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">F. Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Amram%2C+P">P. Amram</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+O+I">O. I. Wong</a>, <a href="/search/astro-ph?searchtype=author&query=Athanassoula%2C+E">E. Athanassoula</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="2411.11584v2-abstract-short" style="display: inline;"> The observed star formation rates of galaxies in the Local Universe suggests that they are replenishing their gas reservoir across cosmic time. Cosmological simulations predict that this accretion of fresh gas can occur in a hot or a cold mode, yet the existence of low column density ($\sim10^{17}$ cm$^{-2}$) neutral atomic hydrogen (HI) tracing the cold mode has not been unambiguously confirmed b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.11584v2-abstract-full').style.display = 'inline'; document.getElementById('2411.11584v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.11584v2-abstract-full" style="display: none;"> The observed star formation rates of galaxies in the Local Universe suggests that they are replenishing their gas reservoir across cosmic time. Cosmological simulations predict that this accretion of fresh gas can occur in a hot or a cold mode, yet the existence of low column density ($\sim10^{17}$ cm$^{-2}$) neutral atomic hydrogen (HI) tracing the cold mode has not been unambiguously confirmed by observations. We present the application of unconstrained spectral stacking to attempt to detect the emission from this HI in the Circum-Galactic Medium (CGM) and Inter-Galactic Medium (IGM) of 6 nearby star forming galaxies from the MHONGOOSE sample for which full-depth observations are available. Our stacking procedure consists of a standard spectral stacking algorithm coupled with a one-dimensional spectral line finder designed to extract reliable signal close to the noise level. In agreement with previous studies, we found that the amount of signal detected outside the HI disk is much smaller than implied by simulations. Furthermore, the column density limit that we achieve via stacking ($\sim10^{17}$ cm$^{-2}$) suggests that direct detection of the neutral CGM/IGM component might be challenging in the future, even with the next generation of radio telescopes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.11584v2-abstract-full').style.display = 'none'; document.getElementById('2411.11584v2-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in 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 693, A97 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.02222">arXiv:2410.02222</a> <span> [<a href="https://arxiv.org/pdf/2410.02222">pdf</a>, <a href="https://arxiv.org/format/2410.02222">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> The spatially resolved relation between dust, gas, and metal abundance with the TYPHOON survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Park%2C+H">Hye-Jin Park</a>, <a href="/search/astro-ph?searchtype=author&query=Battisti%2C+A+J">Andrew J. Battisti</a>, <a href="/search/astro-ph?searchtype=author&query=Wisnioski%2C+E">Emily Wisnioski</a>, <a href="/search/astro-ph?searchtype=author&query=Cortese%2C+L">Luca Cortese</a>, <a href="/search/astro-ph?searchtype=author&query=Seibert%2C+M">Mark Seibert</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Madore%2C+B+F">Barry F. Madore</a>, <a href="/search/astro-ph?searchtype=author&query=Groves%2C+B">Brent Groves</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J+A">Jeff A. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Beaton%2C+R+L">Rachael L. Beaton</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Q">Qian-Hui Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Mun%2C+M">Marcie Mun</a>, <a href="/search/astro-ph?searchtype=author&query=McClure-Griffiths%2C+N+M">Naomi M. McClure-Griffiths</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Kewley%2C+L+J">Lisa J. Kewley</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.02222v1-abstract-short" style="display: inline;"> We present the spatially resolved relationship between the dust-to-gas mass ratio (DGR) and gas-phase metallicity (Zgas or 12+log(O/H)) (i.e., DGR-Zgas relation) of 11 nearby galaxies with a large metallicity range (1.5 dex of 12+log(O/H)) at (sub-)kpc scales. We used the large field-of-view (> 3') optical pseudo-Integral Field Spectroscopy data taken by the TYPHOON/PrISM survey, covering the opti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.02222v1-abstract-full').style.display = 'inline'; document.getElementById('2410.02222v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.02222v1-abstract-full" style="display: none;"> We present the spatially resolved relationship between the dust-to-gas mass ratio (DGR) and gas-phase metallicity (Zgas or 12+log(O/H)) (i.e., DGR-Zgas relation) of 11 nearby galaxies with a large metallicity range (1.5 dex of 12+log(O/H)) at (sub-)kpc scales. We used the large field-of-view (> 3') optical pseudo-Integral Field Spectroscopy data taken by the TYPHOON/PrISM survey, covering the optical size of galaxies, combining them with multi-wavelength data (far-UV to far-IR, CO, and HI 21 cm radio). A large scatter of DGR in the intermediate metallicity galaxies (8.0 < 12+log(O/H) < 8.3) is found, which is in line with dust evolution models, where grain growth begins to dominate the mechanism of dust mass accumulation. In the lowest metallicity galaxy of our sample, Sextans A (12+log(O/H) < 7.6), the star-forming regions have significantly higher DGR values (by 0.5-2 dex) than the global estimates from literature at the same metallicity but aligns with the DGR values from metal depletion method from Damped Lyman Alpha systems and high hydrogen gas density regions of Sextans A. Using dust evolution models with a Bayesian MCMC approach suggests: 1) a high SN dust yield and 2) a negligible amount of photofragmentation by UV radiation, although we note that our sample in the low-metallicity regime is limited to Sextans A. On the other hand, it is also possible that while metallicity influences DGR, gas density also plays a role, indicating an early onset of dust grain growth in the dust mass build-up process despite its low metallicity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.02222v1-abstract-full').style.display = 'none'; document.getElementById('2410.02222v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 10 figures, 7 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/2407.09082">arXiv:2407.09082</a> <span> [<a href="https://arxiv.org/pdf/2407.09082">pdf</a>, <a href="https://arxiv.org/format/2407.09082">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/10.1051/0004-6361/202450114">10.1051/0004-6361/202450114 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MeerKAT Fornax Survey. III. Ram-pressure stripping of the tidally interacting galaxy NGC 1427A in the Fornax cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">P. Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Jozsa%2C+G+I+G">G. I. G. Jozsa</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+G+L">G. L. Bryan</a>, <a href="/search/astro-ph?searchtype=author&query=van+Gorkom%2C+J+H">J. H. van Gorkom</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Loni%2C+A">A. Loni</a>, <a href="/search/astro-ph?searchtype=author&query=Loubser%2C+S+I">S. I. Loubser</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Molnar%2C+D">D. Molnar</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R">R. Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Ramatsoku%2C+M">M. Ramatsoku</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M+W+L">M. W. L. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Verheijen%2C+M+A+W">M. A. W. Verheijen</a>, <a href="/search/astro-ph?searchtype=author&query=Zabel%2C+N">N. Zabel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.09082v1-abstract-short" style="display: inline;"> We present MeerKAT Fornax Survey HI observations of NGC 1427A, a blue irregular galaxy with a stellar mass of 2e+9 Msun located near the centre of the Fornax galaxy cluster. Thanks to the excellent resolution (1 to 6 kpc spatially, 1.4 km/s in velocity) and HI column density sensitivity (4e+19/cm^2 to 1e+18/cm^2 depending on resolution), our data deliver new insights on the long-debated interactio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.09082v1-abstract-full').style.display = 'inline'; document.getElementById('2407.09082v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.09082v1-abstract-full" style="display: none;"> We present MeerKAT Fornax Survey HI observations of NGC 1427A, a blue irregular galaxy with a stellar mass of 2e+9 Msun located near the centre of the Fornax galaxy cluster. Thanks to the excellent resolution (1 to 6 kpc spatially, 1.4 km/s in velocity) and HI column density sensitivity (4e+19/cm^2 to 1e+18/cm^2 depending on resolution), our data deliver new insights on the long-debated interaction of this galaxy with the cluster environment. We confirm the presence of a broad, one-sided, starless HI tail stretching from the outer regions of the stellar body and pointing away from the cluster centre. We find the tail to have 50% more HI (4e+8 Msun) and to be 3 times longer (70 kpc) than in previous observations. In fact, we detect scattered HI clouds out to 300 kpc from the galaxy in the direction of the tail -- possibly the most ancient remnant of the passage of NGC 1427A through the intracluster medium of Fornax. Both the velocity gradient along the HI tail and the peculiar kinematics of HI in the outer region of the stellar body are consistent with the effect of ram pressure given the line-of-sight motion of the galaxy within the cluster. However, several properties cannot be explained solely by ram pressure and suggest an ongoing tidal interaction. This includes: the close match between dense HI and stars within the disturbed stellar body; the abundant kinematically-anomalous HI; and the inversion of the HI velocity gradient near the base of the HI tail. We rule out an interaction with the cluster tidal field, and conclude that NGC 1427A is the result of a high-speed galaxy encounter or of a merger started at least 300 Myr ago, where ram pressure shapes the distribution and kinematics of the HI in the perturbed outer stellar body and in the tidal tails. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.09082v1-abstract-full').style.display = 'none'; document.getElementById('2407.09082v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Astronomy & Astrophysics, accepted. Data available at the MeerKAT Fornax Survey website, https://sites.google.com/inaf.it/meerkatfornaxsurvey</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A4 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.04531">arXiv:2407.04531</a> <span> [<a href="https://arxiv.org/pdf/2407.04531">pdf</a>, <a href="https://arxiv.org/format/2407.04531">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/10.1051/0004-6361/202450265">10.1051/0004-6361/202450265 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutral atomic and molecular gas dynamics in the nearby spiral galaxies NGC 1512, NGC 4535, and NGC 7496 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Laudage%2C+S">Sebastian Laudage</a>, <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Meidt%2C+S">Sharon Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguele Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Stuber%2C+S">Sophia Stuber</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">Dario Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Utomo%2C+D">Dyas Utomo</a>, <a href="/search/astro-ph?searchtype=author&query=Levy%2C+R+C">Rebecca C. Levy</a>, <a href="/search/astro-ph?searchtype=author&query=Klessen%2C+R">Ralf Klessen</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Koch%2C+E+W">Eric W. Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Kurapati%2C+S">Sushma Kurapati</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Blazquez%2C+P">Patricia Sanchez-Blazquez</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+J">Justus Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+L">Lukas Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+H">Hsi-An Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Williams%2C+T+G">Thomas G. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.04531v1-abstract-short" style="display: inline;"> Neutral atomic gas (HI) effectively traces galactic dynamics across mid to large galactocentric radii. However, its limitations in observing small-scale changes within the central few kiloparsecs, coupled with the often observed HI deficit in galactic centers, necessitates using molecular gas emission as a preferred tracer in these regions. Understanding the dynamics of both neutral atomic and mol… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04531v1-abstract-full').style.display = 'inline'; document.getElementById('2407.04531v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.04531v1-abstract-full" style="display: none;"> Neutral atomic gas (HI) effectively traces galactic dynamics across mid to large galactocentric radii. However, its limitations in observing small-scale changes within the central few kiloparsecs, coupled with the often observed HI deficit in galactic centers, necessitates using molecular gas emission as a preferred tracer in these regions. Understanding the dynamics of both neutral atomic and molecular gas is crucial for a more complete understanding of how galaxies evolve, funnel gas from the outer disk into their central parts, and eventually form stars. In this work we aim to quantify the dynamics of both, the neutral atomic and molecular gas, in the nearby spiral galaxies NGC 1512, NGC 4535, and NGC 7496 using new MeerKAT-HI observations together with ALMA CO (2-1) observations from the PHANGS collaboration. We use the analysis tool 3D-Barolo to fit tilted ring models to the HI and CO observations. A combined approach of using the HI to constrain the true disk orientation parameters before applying these to the CO datasets is tested. This paper sets expectations for the results of the upcoming high-resolution HI coverage of many galaxies in the PHANGS-ALMA sample using MeerKAT or VLA, to establish a robust methodology for characterizing galaxy orientations and deriving dynamics from combining new HI with existing CO data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04531v1-abstract-full').style.display = 'none'; document.getElementById('2407.04531v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in A&A; 13 pages, 9 Figures (+2 appendix pages)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A169 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.03166">arXiv:2407.03166</a> <span> [<a href="https://arxiv.org/pdf/2407.03166">pdf</a>, <a href="https://arxiv.org/format/2407.03166">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/10.46620/URSIATRASC24/UXQP4342">10.46620/URSIATRASC24/UXQP4342 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutral Atomic Hydrogen Surveys: past, present and future </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.03166v2-abstract-short" style="display: inline;"> Neutral atomic hydrogen (HI) observations are fundamental to understand the dynamics of galaxies, their assembly, the fuelling of their star formation and environmental interactions. HI studies have so far been limited by the capabilities of single-dish radio telescopes or synthesis arrays to either small samples or low resolution and sensitivities. Now, the Square Kilometer Array precursors and p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.03166v2-abstract-full').style.display = 'inline'; document.getElementById('2407.03166v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.03166v2-abstract-full" style="display: none;"> Neutral atomic hydrogen (HI) observations are fundamental to understand the dynamics of galaxies, their assembly, the fuelling of their star formation and environmental interactions. HI studies have so far been limited by the capabilities of single-dish radio telescopes or synthesis arrays to either small samples or low resolution and sensitivities. Now, the Square Kilometer Array precursors and pathfinders are providing a novel view of the HI in and around galaxies allowing wide-field high resolution deep surveys in nearby galaxies. We give an overview of past, current and future HI surveys consistently comparing their HI column density and spatial resolutions highlighting their main scientific key goals and results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.03166v2-abstract-full').style.display = 'none'; document.getElementById('2407.03166v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 3 figures, 1 table originally presented at 2024 URSI Atlantic Radio Science Meeting (AT-RASC), Gran Canaria, Spain</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.01716">arXiv:2407.01716</a> <span> [<a href="https://arxiv.org/pdf/2407.01716">pdf</a>, <a href="https://arxiv.org/format/2407.01716">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/10.1051/0004-6361/202449944">10.1051/0004-6361/202449944 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PHANGS-MeerKAT and MHONGOOSE HI observations of nearby spiral galaxies: physical drivers of the molecular gas fraction, $R_{\mathrm{mol}}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+J">Jiayi Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Kurapati%2C+S">Sushma Kurapati</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A+T">Ashley T. Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Thorp%2C+M">Mallory Thorp</a>, <a href="/search/astro-ph?searchtype=author&query=Colombo%2C+D">Dario Colombo</a>, <a href="/search/astro-ph?searchtype=author&query=Koch%2C+E+W">Eric W. Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+I">I-Da Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Ostriker%2C+E+C">Eve C. Ostriker</a>, <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+E+J">Eric J. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Zabel%2C+N">Nikki Zabel</a>, <a href="/search/astro-ph?searchtype=author&query=Laudage%2C+S">Sebstian Laudage</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">Filippo M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Healy%2C+J">Julia Healy</a>, <a href="/search/astro-ph?searchtype=author&query=Sekhar%2C+S">Srikrishna Sekhar</a>, <a href="/search/astro-ph?searchtype=author&query=Utomo%2C+D">Dyas Utomo</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+d">Jakob den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Cao%2C+Y">Yixian Cao</a>, <a href="/search/astro-ph?searchtype=author&query=Chevance%2C+M">M茅lanie Chevance</a> , et al. (14 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="2407.01716v1-abstract-short" style="display: inline;"> The molecular-to-atomic gas ratio is crucial to the evolution of the interstellar medium in galaxies. We investigate the balance between the atomic ($危_{\rm HI}$) and molecular gas ($危_{\rm H2}$) surface densities in eight nearby star-forming galaxies using new high-quality observations from MeerKAT and ALMA (for HI and CO, respectively). We define the molecular gas ratio as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.01716v1-abstract-full').style.display = 'inline'; document.getElementById('2407.01716v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.01716v1-abstract-full" style="display: none;"> The molecular-to-atomic gas ratio is crucial to the evolution of the interstellar medium in galaxies. We investigate the balance between the atomic ($危_{\rm HI}$) and molecular gas ($危_{\rm H2}$) surface densities in eight nearby star-forming galaxies using new high-quality observations from MeerKAT and ALMA (for HI and CO, respectively). We define the molecular gas ratio as $R_{\rm mol} = 危_{\rm H2} / 危_{\rm HI}$ and measure how it depends on local conditions in the galaxy disks using multi-wavelength observations. We find that, depending on the galaxy, HI is detected at $>3蟽$ out to 20-120 kpc in galactocentric radius ($r_{\rm gal}$). The typical radius at which $危_{\rm HI}$ reaches 1~$\rm M_\odot~pc^{-2}$ is $r_{\rm HI}\approx22$~kpc, which corresponds to 1-3 times the optical radius ($r_{25}$). $R_{\rm mol}$ correlates best with the dynamical equilibrium pressure, P$_{\rm DE}$, among potential drivers studied, with a median correlation coefficient of $<蟻>=0.89$. Correlations between $R_{\rm mol}$ and star formation rate, total gas and stellar surface density, metallicity, and $危_{\rm SFR}$/P$_{\rm DE}$ are present but somewhat weaker. Our results also show a direct correlation between P$_{\rm DE}$ and $危_{\rm SFR}$, supporting self-regulation models. Quantitatively, we measure similar scalings as previous works and attribute the modest differences that we find to the effect of varying resolution and sensitivity. At $r_{\rm gal} {\gtrsim}0.4~r_{25}$, atomic gas dominates over molecular gas, and at the balance of these two gas phases, we find that the baryon mass is dominated by stars, with $危_{*} > 5~危_{\rm gas}$. Our study constitutes an important step in the statistical investigation of how local galaxy properties impact the conversion from atomic to molecular gas in nearby galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.01716v1-abstract-full').style.display = 'none'; document.getElementById('2407.01716v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in A&A; 20 pages, 12 Figures (+4 appendix pages)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A163 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.17000">arXiv:2405.17000</a> <span> [<a href="https://arxiv.org/pdf/2405.17000">pdf</a>, <a href="https://arxiv.org/format/2405.17000">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/10.1051/0004-6361/202449441">10.1051/0004-6361/202449441 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MHONGOOSE discovery of a gas-rich low-surface brightness galaxy in the Dorado Group </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Pi%C3%B1a%2C+P+E+M">P. E. Mancera Pi帽a</a>, <a href="/search/astro-ph?searchtype=author&query=Ragusa%2C+R">R. Ragusa</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=McGaugh%2C+S">S. McGaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Oman%2C+K+A">K. A. Oman</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+M">M. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Amram%2C+P">P. Amram</a>, <a href="/search/astro-ph?searchtype=author&query=Bosma%2C+A">A. Bosma</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Brinks%2C+E">E. Brinks</a>, <a href="/search/astro-ph?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/astro-ph?searchtype=author&query=Combes%2C+F">F. Combes</a>, <a href="/search/astro-ph?searchtype=author&query=Gibson%2C+B">B. Gibson</a>, <a href="/search/astro-ph?searchtype=author&query=Healy%2C+J">J. Healy</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">G. I. G. J贸zsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Kurapati%2C+S">S. Kurapati</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="2405.17000v1-abstract-short" style="display: inline;"> We present the discovery of a low-mass gas-rich low-surface brightness galaxy in the Dorado Group, at a distance of 17.7 Mpc. Combining deep MeerKAT 21-cm observations from the MeerKAT HI Observations of Nearby Galactic Objects: Observing Southern Emitters (MHONGOOSE) survey with deep photometric images from the VST Early-type Galaxy Survey (VEGAS) we find a stellar and neutral atomic hydrogen (HI… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17000v1-abstract-full').style.display = 'inline'; document.getElementById('2405.17000v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.17000v1-abstract-full" style="display: none;"> We present the discovery of a low-mass gas-rich low-surface brightness galaxy in the Dorado Group, at a distance of 17.7 Mpc. Combining deep MeerKAT 21-cm observations from the MeerKAT HI Observations of Nearby Galactic Objects: Observing Southern Emitters (MHONGOOSE) survey with deep photometric images from the VST Early-type Galaxy Survey (VEGAS) we find a stellar and neutral atomic hydrogen (HI) gas mass of $M_\star = 2.23\times10^6$ M$_\odot$ and $M_{\rm HI}=1.68\times10^6$ M$_\odot$, respectively. This low-surface brightness galaxy is the lowest mass HI detection found in a group beyond the Local Universe ($D\gtrsim 10$ Mpc). The dwarf galaxy has the typical overall properties of gas-rich low surface brightness galaxies in the Local group, but with some striking differences. Namely, the MHONGOOSE observations reveal a very low column density ($\sim 10^{18-19}$ cm$^{-2}$) HI disk with asymmetrical morphology possibly supported by rotation and higher velocity dispersion in the centre. There, deep optical photometry and UV-observations suggest a recent enhancement of the star formation. Found at galactocentric distances where in the Local Group dwarf galaxies are depleted of cold gas (at $390$ projected-kpc distance from the group centre), this galaxy is likely on its first orbit within the Dorado group. We discuss the possible environmental effects that may have caused the formation of the HI disk and the enhancement of star formation, highlighting the short-lived phase (a few hundreds of Myr) of the gaseous disk, before either SF or hydrodynamical forces will deplete the gas of the galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17000v1-abstract-full').style.display = 'none'; document.getElementById('2405.17000v1-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 14 figures, 5 tables; accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A69 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.01774">arXiv:2404.01774</a> <span> [<a href="https://arxiv.org/pdf/2404.01774">pdf</a>, <a href="https://arxiv.org/format/2404.01774">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/10.1051/0004-6361/202348297">10.1051/0004-6361/202348297 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MHONGOOSE -- A MeerKAT Nearby Galaxy HI Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Healy%2C+J">J. Healy</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Bosma%2C+A">A. Bosma</a>, <a href="/search/astro-ph?searchtype=author&query=English%2C+J">J. English</a>, <a href="/search/astro-ph?searchtype=author&query=Jarrett%2C+T">T. Jarrett</a>, <a href="/search/astro-ph?searchtype=author&query=Marasco%2C+A">A. Marasco</a>, <a href="/search/astro-ph?searchtype=author&query=Meurer%2C+G+R">G. R. Meurer</a>, <a href="/search/astro-ph?searchtype=author&query=Veronese%2C+S">S. Veronese</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/astro-ph?searchtype=author&query=Fraternali%2C+F">F. Fraternali</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Kl%C3%B6ckner%2C+H+R">H. R. Kl枚ckner</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">A. K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Mogotsi%2C+M">M. Mogotsi</a>, <a href="/search/astro-ph?searchtype=author&query=Oman%2C+K+A">K. A. Oman</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">E. Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Verdes-Montenegro%2C+L">L. Verdes-Montenegro</a>, <a href="/search/astro-ph?searchtype=author&query=Westmeier%2C+T">T. Westmeier</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+O+I">O. I. Wong</a>, <a href="/search/astro-ph?searchtype=author&query=Zabel%2C+N">N. Zabel</a> , et al. (35 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.01774v2-abstract-short" style="display: inline;"> The MHONGOOSE (MeerKAT HI Observations of Nearby Galactic Objects: Observing Southern Emitters) survey maps the distribution and kinematics of the neutral atomic hydrogen (HI) gas in and around 30 nearby star-forming spiral and dwarf galaxies to extremely low HI column densities. The HI column density sensitivity (3 sigma over 16 km/s) ranges from ~ 5 x 10^{17} cm^{-2} at 90'' resolution to ~4 x 1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.01774v2-abstract-full').style.display = 'inline'; document.getElementById('2404.01774v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.01774v2-abstract-full" style="display: none;"> The MHONGOOSE (MeerKAT HI Observations of Nearby Galactic Objects: Observing Southern Emitters) survey maps the distribution and kinematics of the neutral atomic hydrogen (HI) gas in and around 30 nearby star-forming spiral and dwarf galaxies to extremely low HI column densities. The HI column density sensitivity (3 sigma over 16 km/s) ranges from ~ 5 x 10^{17} cm^{-2} at 90'' resolution to ~4 x 10^{19} cm^{-2} at the highest resolution of 7''. The HI mass sensitivity (3 sigma over 50 km/s) is ~5.5 X 10^5 M_sun at a distance of 10 Mpc (the median distance of the sample galaxies). The velocity resolution of the data is 1.4 km/s. One of the main science goals of the survey is the detection of cold, accreting gas in the outskirts of the sample galaxies. The sample was selected to cover a range in HI masses, from 10^7 M_sun to almost 10^{11} M_sun, to optimally sample possible accretion scenarios and environments. The distance to the sample galaxies ranges from 3 to 23 Mpc. In this paper, we present the sample selection, survey design, and observation and reduction procedures. We compare the integrated HI fluxes based on the MeerKAT data with those derived from single-dish measurement and find good agreement, indicating that our MeerKAT observations are recovering all flux. We present HI moment maps of the entire sample based on the first ten percent of the survey data, and find that a comparison of the zeroth- and second-moment values shows a clear separation between the physical properties of the HI in areas with star formation and areas without, related to the formation of a cold neutral medium. Finally, we give an overview of the HI-detected companion and satellite galaxies in the 30 fields, five of which have not previously been catalogued. We find a clear relation between the number of companion galaxies and the mass of the main target galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.01774v2-abstract-full').style.display = 'none'; document.getElementById('2404.01774v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted 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 688, A109 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.13749">arXiv:2402.13749</a> <span> [<a href="https://arxiv.org/pdf/2402.13749">pdf</a>, <a href="https://arxiv.org/format/2402.13749">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/10.1051/0004-6361/202347475">10.1051/0004-6361/202347475 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Possible origins of anomalous H$\,$I gas around MHONGOOSE galaxy, NGC 5068 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Healy%2C+J">J. Healy</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Amram%2C+P">P. Amram</a>, <a href="/search/astro-ph?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/astro-ph?searchtype=author&query=Combes%2C+F">F. Combes</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">B. W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">E. Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Spekkens%2C+K">K. Spekkens</a>, <a href="/search/astro-ph?searchtype=author&query=Verdes-Montenegro%2C+L">L. Verdes-Montenegro</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">F. Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Gibson%2C+B+K">B. K. Gibson</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Veronese%2C+S">S. Veronese</a>, <a href="/search/astro-ph?searchtype=author&query=Zabel%2C+N">N. Zabel</a>, <a href="/search/astro-ph?searchtype=author&query=English%2C+J">J. English</a>, <a href="/search/astro-ph?searchtype=author&query=Carignan%2C+C">C. Carignan</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="2402.13749v1-abstract-short" style="display: inline;"> The existing reservoirs of neutral atomic hydrogen gas (H$\,$I) in galaxies are insufficient to have maintained the observed levels of star formation without some kind of replenishment. {This refuelling of the H$\,$I reservoirs} is likely to occur at column densities an order of magnitude lower than previous observational limits (N$_{\rm{H\,I}\, limit} \sim 10^{19}\,$cm$^{-2}$ at 30$''$ resolution… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.13749v1-abstract-full').style.display = 'inline'; document.getElementById('2402.13749v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.13749v1-abstract-full" style="display: none;"> The existing reservoirs of neutral atomic hydrogen gas (H$\,$I) in galaxies are insufficient to have maintained the observed levels of star formation without some kind of replenishment. {This refuelling of the H$\,$I reservoirs} is likely to occur at column densities an order of magnitude lower than previous observational limits (N$_{\rm{H\,I}\, limit} \sim 10^{19}\,$cm$^{-2}$ at 30$''$ resolution over a linewidth of $20\,$km/s). In this paper, we present recent deep H$\,$I observations of NGC 5068, a nearby isolated star-forming galaxy observed by MeerKAT as part of the MHONGOOSE survey. With these new data, we are able to detect low column density H$\,$I around NGC 5068 with a $3蟽$ detection limit of N$_{\rm{H\,I}} = 6.4 \times 10^{17}\,$cm$^{-2}$ at 90$''$ resolution over a $20\,$km/s linewidth. The high sensitivity and resolution of the MeerKAT data reveal a complex morphology of the H$\,$I in this galaxy -- a regularly rotating inner disk coincident with the main star-forming disk of the galaxy, a warped outer disk of low column density gas (N$_{\rm{H\,I}} < 9 \times 10^{19}\,$cm$^{-2}$), in addition to clumps of gas on the north west side of the galaxy. We employ a simple two disk model that describe the inner and outer disks, and are able to identify anomalous gas that deviates from the rotation of the main galaxy. The morphology and the kinematics of the anomalous gas suggest a possible extra-galactic origin. We explore a number of possible origin scenarios that may explain the anomalous gas, and conclude that fresh accretion is the most likely scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.13749v1-abstract-full').style.display = 'none'; document.getElementById('2402.13749v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 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">17 pages, 13 figures, 5 tables. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 687, A254 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.16383">arXiv:2306.16383</a> <span> [<a href="https://arxiv.org/pdf/2306.16383">pdf</a>, <a href="https://arxiv.org/format/2306.16383">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 method for short duration transient detection in radio images: Searching for transient sources in MeerKAT data of NGC 5068 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fijma%2C+S">S. Fijma</a>, <a href="/search/astro-ph?searchtype=author&query=Rowlinson%2C+A">A. Rowlinson</a>, <a href="/search/astro-ph?searchtype=author&query=Wijers%2C+R+A+M+J">R. A. M. J. Wijers</a>, <a href="/search/astro-ph?searchtype=author&query=de+Ruiter%2C+I">I. de Ruiter</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Chastain%2C+S">S. Chastain</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Horst%2C+A+J">A. J. van der Horst</a>, <a href="/search/astro-ph?searchtype=author&query=Meyers%2C+Z+S">Z. S. Meyers</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Meulen%2C+K">K. van der Meulen</a>, <a href="/search/astro-ph?searchtype=author&query=Fender%2C+R">R. Fender</a>, <a href="/search/astro-ph?searchtype=author&query=Woudt%2C+P+A">P. A. Woudt</a>, <a href="/search/astro-ph?searchtype=author&query=Andersson%2C+A">A. Andersson</a>, <a href="/search/astro-ph?searchtype=author&query=Zijlstra%2C+A">A. Zijlstra</a>, <a href="/search/astro-ph?searchtype=author&query=Healy%2C+J">J. Healy</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.16383v1-abstract-short" style="display: inline;"> Transient surveys are a vital tool in exploring the dynamic universe, with radio transients acting as beacons for explosive and highly energetic astrophysical phenomena. However, performing commensal transient surveys using radio imaging can require a significant amount of computing power, data storage and time. With the instrumentation available to us, and with new and exciting radio interferomet… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16383v1-abstract-full').style.display = 'inline'; document.getElementById('2306.16383v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.16383v1-abstract-full" style="display: none;"> Transient surveys are a vital tool in exploring the dynamic universe, with radio transients acting as beacons for explosive and highly energetic astrophysical phenomena. However, performing commensal transient surveys using radio imaging can require a significant amount of computing power, data storage and time. With the instrumentation available to us, and with new and exciting radio interferometers in development, it is essential that we develop efficient methods to probe the radio transient sky. In this paper, we present results from an commensal short duration transient survey, on time scales of 8 seconds, 128 seconds and 1 hour, using data from the MeerKAT radio telescope. The dataset used was obtained as part of a galaxy observing campaign, and we focus on the field of NGC 5068. We present a quick, wide field imaging strategy to enable fast imaging of large datasets, and develop methods to efficiently filter detected transient candidates. No transient candidates were identified on the time scales of 8 seconds, 128 seconds and 1 hour, leading to competitive limits on the transient surface densities of $6.7{\times}10^{-5}$ deg$^{-1}$, $1.1{\times}10^{-3}$ deg$^{-1}$, and $3.2{\times}10^{-2}$ deg$^{-1}$ at sensitivities of 56.4 mJy, 19.2 mJy, and 3.9 mJy for the respective time scales. We find one possible candidate that could be associated with a stellar flare, that was rejected due to strict image quality control. Further short time-scale radio observations of this candidate could give definite results to its origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.16383v1-abstract-full').style.display = 'none'; document.getElementById('2306.16383v1-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages (9 main, 2 appendix), 8 figures, 2 tables. 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/2306.03710">arXiv:2306.03710</a> <span> [<a href="https://arxiv.org/pdf/2306.03710">pdf</a>, <a href="https://arxiv.org/format/2306.03710">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/10.1051/0004-6361/202346618">10.1051/0004-6361/202346618 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Apertif 1.4 GHz continuum observations of the Bo枚tes field and their combined view with LOFAR </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kutkin%2C+A+M">A. M. Kutkin</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Morganti%2C+R">R. Morganti</a>, <a href="/search/astro-ph?searchtype=author&query=Offringa%2C+A+R">A. R. Offringa</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">K. M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Bozkurt%2C+A">A. Bozkurt</a>, <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">W. A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=Gunst%2C+A+W">A. W. Gunst</a>, <a href="/search/astro-ph?searchtype=author&query=Holties%2C+H+A">H. A. Holties</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">J. van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Loose%2C+G+M">G. M. Loose</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L+C">L. C. Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Vohl%2C+D">D. Vohl</a>, <a href="/search/astro-ph?searchtype=author&query=Wijnholds%2C+S+J">S. J. Wijnholds</a>, <a href="/search/astro-ph?searchtype=author&query=Ziemke%2C+J">J. Ziemke</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.03710v1-abstract-short" style="display: inline;"> We present a new image of a 26.5 square degree region in the Bo枚tes constellation obtained at 1.4 GHz using the Aperture Tile in Focus (Apertif) system on the Westerbork Synthesis Radio Telescope. We use a newly developed processing pipeline which includes direction-dependent self-calibration which provides a significant improvement of the quality of the images compared to those released as part o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.03710v1-abstract-full').style.display = 'inline'; document.getElementById('2306.03710v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.03710v1-abstract-full" style="display: none;"> We present a new image of a 26.5 square degree region in the Bo枚tes constellation obtained at 1.4 GHz using the Aperture Tile in Focus (Apertif) system on the Westerbork Synthesis Radio Telescope. We use a newly developed processing pipeline which includes direction-dependent self-calibration which provides a significant improvement of the quality of the images compared to those released as part of the Apertif first data release. For the Bo枚tes region, we mosaic 187 Apertif images and extract a source catalog. The mosaic image has an angular resolution of 27${\times}$11.5 arcseconds and a median background noise of 40 $渭$Jy/beam. The catalog has 8994 sources and is complete down to the 0.3 mJy level. We combine the Apertif image with LOFAR images of the Bo枚tes field at 54 and 150 MHz to study spectral properties of the sources. We find a spectral flattening towards low flux density sources. Using the spectral index limits from Apertif non-detections we derive that up to 9 percent of the sources have ultra-steep spectra with a slope steeper than -1.2. Steepening of the spectral index with increasing redshift is also seen in the data showing a different dependency for the low-frequency spectral index and the high frequency one. This can be explained by a population of sources having concave radio spectra with a turnover frequency around the LOFAR band. Additionally, we discuss cases of individual extended sources with an interesting resolved spectral structure. With the improved pipeline, we aim to continue processing data from the Apertif wide-area surveys and release the improved 1.4 GHz images of several famous fields. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.03710v1-abstract-full').style.display = 'none'; document.getElementById('2306.03710v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 9 figures; to be published in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 676, A37 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.13163">arXiv:2305.13163</a> <span> [<a href="https://arxiv.org/pdf/2305.13163">pdf</a>, <a href="https://arxiv.org/format/2305.13163">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/10.1051/0004-6361/202346461">10.1051/0004-6361/202346461 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MeerKAT Fornax Survey II. The rapid removal of HI from dwarf galaxies in the Fornax cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">P. Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Raj%2C+M+A">M. A. Raj</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">G. I. G. J贸zsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Kraan-Korteweg%2C+R">R. Kraan-Korteweg</a>, <a href="/search/astro-ph?searchtype=author&query=Loi%2C+F">F. Loi</a>, <a href="/search/astro-ph?searchtype=author&query=Loni%2C+A">A. Loni</a>, <a href="/search/astro-ph?searchtype=author&query=Loubser%2C+S+I">S. I. Loubser</a>, <a href="/search/astro-ph?searchtype=author&query=Moln%C3%A1r%2C+D+C">D. Cs. Moln谩r</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R">R. Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.13163v2-abstract-short" style="display: inline;"> We present MeerKAT Fornax Survey atomic hydrogen (HI) observations of the dwarf galaxies located in the central ~2.5 x 4 deg$^2$ of the Fornax galaxy cluster. The HI images presented in this work have a $3蟽$ column density sensitivity between 2.7 and 50 x 10$^{18}$ cm$^{-2}$ over 25 km s$^{-1}$ for spatial resolution between 4 and 1 kpc. We are able to detect an impressive MHI = 5 x 10$^{5}$ Msun… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.13163v2-abstract-full').style.display = 'inline'; document.getElementById('2305.13163v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.13163v2-abstract-full" style="display: none;"> We present MeerKAT Fornax Survey atomic hydrogen (HI) observations of the dwarf galaxies located in the central ~2.5 x 4 deg$^2$ of the Fornax galaxy cluster. The HI images presented in this work have a $3蟽$ column density sensitivity between 2.7 and 50 x 10$^{18}$ cm$^{-2}$ over 25 km s$^{-1}$ for spatial resolution between 4 and 1 kpc. We are able to detect an impressive MHI = 5 x 10$^{5}$ Msun 3$蟽$ point source with a line width of 50 km s$^{-1}$ at a distance of 20 Mpc. We detect HI in 17 out of the 304 dwarfs in our field -- 14 out of the 36 late type dwarfs (LTDs), and 3 of the 268 early type dwarfs (ETDs). The HI-detected LTDs have likely just joined the cluster and are on their first infall as they are located at large clustocentric radii, with comparable MHI and mean stellar surface brightness at fixed luminosity as blue, star-forming LTDs in the field. The HI-detected ETDs have likely been in the cluster longer than the LTDs and acquired their HI through a recent merger or accretion from nearby HI. Eight of the HI-detected LTDs host irregular or asymmetric HI emission and disturbed or lopsided stellar emission. There are two clear cases of ram-pressure shaping the HI, with the LTDs displaying compressed HI on the side closest to the cluster centre and a one-sided, starless tail pointing away from the cluster centre. The HI-detected dwarfs avoid the most massive potentials, consistent with massive galaxies playing an active role in the removal of HI. We create a simple toy model to quantify the timescale of HI stripping in the cluster. We find that a MHI = 10$^{8}$ Msun dwarf will be stripped in ~ 240 Myr. The model is consistent with our observations, where low mass LTDs are directly stripped of their HI from a single encounter and more massive LTDs can harbour a disturbed HI morphology due to longer times or multiple encounters being required to fully strip their HI. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.13163v2-abstract-full').style.display = 'none'; document.getElementById('2305.13163v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in Astronomy & Astrophysics. 21 pages, 10 figures. Data available at the MeerKAT Fornax Survey website https://sites.google.com/inaf.it/meerkatfornaxsurvey</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 675, A108 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.05709">arXiv:2305.05709</a> <span> [<a href="https://arxiv.org/pdf/2305.05709">pdf</a>, <a href="https://arxiv.org/format/2305.05709">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/stad1422">10.1093/mnras/stad1422 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NGC 1436: the making of a lenticular galaxy in the Fornax cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Loni%2C+A">Alessandro Loni</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">Paolo Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Sarzi%2C+M">Marc Sarzi</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">Gyula I. G. J贸zsa</a>, <a href="/search/astro-ph?searchtype=author&query=Anta%2C+P+M+G">Pablo M. Gal谩n-de Anta</a>, <a href="/search/astro-ph?searchtype=author&query=Zabel%2C+N">Nikki Zabel</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">Dane Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">Filippo M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Moln%C3%A1r%2C+D">Daniel Moln谩r</a>, <a href="/search/astro-ph?searchtype=author&query=Ramatsoku%2C+M">Mpati Ramatsoku</a>, <a href="/search/astro-ph?searchtype=author&query=Loi%2C+F">Francesca Loi</a>, <a href="/search/astro-ph?searchtype=author&query=Corsini%2C+E+M">Enrico M. Corsini</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">Peter Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+A">Timothy A. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Dettmar%2C+R+J">Ralf J. Dettmar</a>, <a href="/search/astro-ph?searchtype=author&query=Falcon-Barroso%2C+J">Jesus Falcon-Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">Enrichetta Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Lara-L%C3%B3pez%2C+M+A">Maritza A. Lara-L贸pez</a>, <a href="/search/astro-ph?searchtype=author&query=Loubser%2C+S+I">S. Ilani Loubser</a>, <a href="/search/astro-ph?searchtype=author&query=Morokuma-Matsui%2C+K">Kana Morokuma-Matsui</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R">Reynier Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Pinna%2C+F">Francesca Pinna</a>, <a href="/search/astro-ph?searchtype=author&query=Poci%2C+A">Adriano Poci</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.05709v2-abstract-short" style="display: inline;"> We study the evolutionary path of the Fornax cluster galaxy NGC$~$1436, which is known to be currently transitioning from a spiral into a lenticular morphology. This galaxy hosts an inner star-forming disc and an outer quiescent disc, and we analyse data from the MeerKAT Fornax Survey, ALMA, and the Fornax3D survey to study the interstellar medium and the stellar populations of both disc component… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.05709v2-abstract-full').style.display = 'inline'; document.getElementById('2305.05709v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.05709v2-abstract-full" style="display: none;"> We study the evolutionary path of the Fornax cluster galaxy NGC$~$1436, which is known to be currently transitioning from a spiral into a lenticular morphology. This galaxy hosts an inner star-forming disc and an outer quiescent disc, and we analyse data from the MeerKAT Fornax Survey, ALMA, and the Fornax3D survey to study the interstellar medium and the stellar populations of both disc components. Thanks to the combination of high resolution and sensitivity of the MeerKAT data, we find that the $\textrm{H}\scriptstyle\mathrm{I}$ is entirely confined within the inner star-forming disc, and that its kinematics is coincident with that of the CO. The cold gas disc is now well settled, which suggests that the galaxy has not been affected by any environmental interactions in the last $\sim1~$Gyr. The star formation history derived from the Fornax3D data shows that both the inner and outer disc experienced a burst of star formation $\sim5$ Gyr ago, followed by rapid quenching in the outer disc and by slow quenching in the inner disc, which continues forming stars to this day. We claim that NGC$~$1436 has begun to effectively interact with the cluster environment 5$~$Gyr ago, when a combination of gravitational and hydrodynamical interactions caused the temporary enhancement of the star-formation rate. Furthermore, due to the weaker gravitational binding $\textrm{H}\scriptstyle\mathrm{I}$ was stripped from the outer disc, causing its rapid quenching. At the same time, accretion of gas onto the inner disc stopped, causing slow quenching in this region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.05709v2-abstract-full').style.display = 'none'; document.getElementById('2305.05709v2-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Monthly Notices of the Royal Astronomical Society (MNRAS), accepted for publication. Data available at the MeerKAT Fornax Survey website https://sites.google.com/inaf.it/meerkatfornaxsurvey</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.02037">arXiv:2304.02037</a> <span> [<a href="https://arxiv.org/pdf/2304.02037">pdf</a>, <a href="https://arxiv.org/format/2304.02037">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/10.1051/0004-6361/202245290">10.1051/0004-6361/202245290 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Kinematic analysis of the super-extended HI disk of the nearby spiral galaxy M83 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Eibensteiner%2C+C">Cosima Eibensteiner</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">Frank Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Koch%2C+E+W">Eric W. Koch</a>, <a href="/search/astro-ph?searchtype=author&query=Rosolowsky%2C+E">Erik Rosolowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Schinnerer%2C+E">Eva Schinnerer</a>, <a href="/search/astro-ph?searchtype=author&query=Sardone%2C+A">Amy Sardone</a>, <a href="/search/astro-ph?searchtype=author&query=Meidt%2C+S">Sharon Meidt</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Thilker%2C+D">David Thilker</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Ott%2C+J">J眉rgen Ott</a>, <a href="/search/astro-ph?searchtype=author&query=Barnes%2C+A">Ashley Barnes</a>, <a href="/search/astro-ph?searchtype=author&query=Querejeta%2C+M">Miguel Querejeta</a>, <a href="/search/astro-ph?searchtype=author&query=Emsellem%2C+E">Eric Emsellem</a>, <a href="/search/astro-ph?searchtype=author&query=Puschnig%2C+J">Johannes Puschnig</a>, <a href="/search/astro-ph?searchtype=author&query=Utomo%2C+D">Dyas Utomo</a>, <a href="/search/astro-ph?searchtype=author&query=Be%C5%A1lic%2C+I">Ivana Be拧lic</a>, <a href="/search/astro-ph?searchtype=author&query=Brok%2C+J+d">Jakob den Brok</a>, <a href="/search/astro-ph?searchtype=author&query=Faridani%2C+S">Shahram Faridani</a>, <a href="/search/astro-ph?searchtype=author&query=Glover%2C+S+C+O">Simon C. O. Glover</a>, <a href="/search/astro-ph?searchtype=author&query=Grasha%2C+K">Kathryn Grasha</a>, <a href="/search/astro-ph?searchtype=author&query=Hassani%2C+H">Hamid Hassani</a>, <a href="/search/astro-ph?searchtype=author&query=Henshaw%2C+J+D">Jonathan D. Henshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez-Donaire%2C+M+J">Maria J. Jim茅nez-Donaire</a> , et al. (11 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="2304.02037v1-abstract-short" style="display: inline;"> We present new HI observations of the nearby massive spiral galaxy M83, taken with the VLA at $21^{\prime\prime}$ angular resolution ($\approx500$ pc) of an extended ($\sim$1.5 deg$^2$) 10-point mosaic combined with GBT single dish data. We study the super-extended HI disk of M83 (${\sim}$50 kpc in radius), in particular disc kinematics, rotation and the turbulent nature of the atomic interstellar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02037v1-abstract-full').style.display = 'inline'; document.getElementById('2304.02037v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.02037v1-abstract-full" style="display: none;"> We present new HI observations of the nearby massive spiral galaxy M83, taken with the VLA at $21^{\prime\prime}$ angular resolution ($\approx500$ pc) of an extended ($\sim$1.5 deg$^2$) 10-point mosaic combined with GBT single dish data. We study the super-extended HI disk of M83 (${\sim}$50 kpc in radius), in particular disc kinematics, rotation and the turbulent nature of the atomic interstellar medium. We define distinct regions in the outer disk ($r_{\rm gal}>$central optical disk), including ring, southern area, and southern and northern arm. We examine HI gas surface density, velocity dispersion and non-circular motions in the outskirts, which we compare to the inner optical disk. We find an increase of velocity dispersion ($蟽_v$) towards the pronounced HI ring, indicative of more turbulent HI gas. Additionally, we report over a large galactocentric radius range (until $r_{\rm gal}{\sim}$50 kpc) that $蟽_v$ is slightly larger than thermal (i.e. $>8$km s$^{-1}$ ). We find that a higher star formation rate (as traced by FUV emission) is not always necessarily associated with a higher HI velocity dispersion, suggesting that radial transport could be a dominant driver for the enhanced velocity dispersion. We further find a possible branch that connects the extended HI disk to the dwarf irregular galaxy UGCA365, that deviates from the general direction of the northern arm. Lastly, we compare mass flow rate profiles (based on 2D and 3D tilted ring models) and find evidence for outflowing gas at r$_{\rm gal}$ $\sim$2 kpc, inflowing gas at r$_{\rm gal}$ $\sim$5.5 kpc and outflowing gas at r$_{\rm gal}$ $\sim$14 kpc. We caution that mass flow rates are highly sensitive to the assumed kinematic disk parameters, in particular, to the inclination. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02037v1-abstract-full').style.display = 'none'; document.getElementById('2304.02037v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in A&A; 16 pages, 12 figures (+8 pages appendix)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 675, A37 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.07237">arXiv:2303.07237</a> <span> [<a href="https://arxiv.org/pdf/2303.07237">pdf</a>, <a href="https://arxiv.org/format/2303.07237">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/stad792">10.1093/mnras/stad792 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The atomic-to-molecular hydrogen transition in the TNG50 simulation: Using realistic UV fields to create spatially resolved HI maps </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gebek%2C+A">Andrea Gebek</a>, <a href="/search/astro-ph?searchtype=author&query=Baes%2C+M">Maarten Baes</a>, <a href="/search/astro-ph?searchtype=author&query=Diemer%2C+B">Benedikt Diemer</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Nelson%2C+D">Dylan Nelson</a>, <a href="/search/astro-ph?searchtype=author&query=Kapoor%2C+A+U">Anand Utsav Kapoor</a>, <a href="/search/astro-ph?searchtype=author&query=Camps%2C+P">Peter Camps</a>, <a href="/search/astro-ph?searchtype=author&query=Rabyang%2C+O">Omphile Rabyang</a>, <a href="/search/astro-ph?searchtype=author&query=Leeuw%2C+L">Lerothodi Leeuw</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="2303.07237v1-abstract-short" style="display: inline;"> Cold gas in galaxies provides a crucial test to evaluate the realism of cosmological hydrodynamical simulations. To extract the atomic and molecular hydrogen properties of the simulated galaxy population, postprocessing methods taking the local UV field into account are required. We improve upon previous studies by calculating realistic UV fields with the dust radiative transfer code SKIRT to mode… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.07237v1-abstract-full').style.display = 'inline'; document.getElementById('2303.07237v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.07237v1-abstract-full" style="display: none;"> Cold gas in galaxies provides a crucial test to evaluate the realism of cosmological hydrodynamical simulations. To extract the atomic and molecular hydrogen properties of the simulated galaxy population, postprocessing methods taking the local UV field into account are required. We improve upon previous studies by calculating realistic UV fields with the dust radiative transfer code SKIRT to model the atomic-to-molecular transition in TNG50, the highest-resolution run of the IllustrisTNG suite. Comparing integrated quantities such as the HI mass function, we study to what detail the UV field needs to be modelled in order to calculate realistic cold gas properties. We then evaluate new, spatially resolved comparisons for cold gas in galaxies by exploring synthetic maps of atomic hydrogen at redshift zero and compare them to 21-cm observations of local galaxies from the WHISP survey. In terms of non-parametric morphologies, we find that TNG50 HI maps are less concentrated than their WHISP counterparts (median $螖C\approx0.3$), due in part to central HI deficits related to the ejective character of supermassive black hole feedback in TNG. In terms of the HI column density distribution function, we find discrepancies between WHISP and IllustrisTNG that depend on the total HI abundance in these datasets as well as the postprocessing method. To fully exploit the synergy between cosmological simulations and upcoming deep HI/H2 data, we advocate the use of accurate methods to estimate the UV radiation field and to generate mock maps. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.07237v1-abstract-full').style.display = 'none'; document.getElementById('2303.07237v1-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 10 figures (main text). Accepted 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/2302.11895">arXiv:2302.11895</a> <span> [<a href="https://arxiv.org/pdf/2302.11895">pdf</a>, <a href="https://arxiv.org/format/2302.11895">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/10.1051/0004-6361/202346071">10.1051/0004-6361/202346071 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The MeerKAT Fornax Survey -- I. Survey description and first evidence of ram pressure in the Fornax galaxy cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">P. Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Molnar%2C+D">D. Molnar</a>, <a href="/search/astro-ph?searchtype=author&query=Ramatsoku%2C+M">M. Ramatsoku</a>, <a href="/search/astro-ph?searchtype=author&query=Loni%2C+A">A. Loni</a>, <a href="/search/astro-ph?searchtype=author&query=Loi%2C+F">F. Loi</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+G+L">G. L. Bryan</a>, <a href="/search/astro-ph?searchtype=author&query=Dettmar%2C+R+J">R. J. Dettmar</a>, <a href="/search/astro-ph?searchtype=author&query=Frank%2C+B+S">B. S. Frank</a>, <a href="/search/astro-ph?searchtype=author&query=van+Gorkom%2C+J+H">J. H. van Gorkom</a>, <a href="/search/astro-ph?searchtype=author&query=Govoni%2C+F">F. Govoni</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Jozsa%2C+G+I+G">G. I. G. Jozsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Kraan-Korteweg%2C+R">R. Kraan-Korteweg</a>, <a href="/search/astro-ph?searchtype=author&query=Loubser%2C+S+I">S. I. Loubser</a>, <a href="/search/astro-ph?searchtype=author&query=Murgia%2C+M">M. Murgia</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R">R. Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M+W+L">M. W. L. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Trager%2C+S+C">S. C. Trager</a>, <a href="/search/astro-ph?searchtype=author&query=Verheijen%2C+M+A+W">M. A. W. Verheijen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.11895v1-abstract-short" style="display: inline;"> The MeerKAT Fornax Survey maps the distribution and kinematics of atomic neutral hydrogen gas (HI) in the nearby Fornax galaxy cluster using the MeerKAT telescope. The 12 deg^2 survey footprint covers the central region of the cluster out to ~ Rvir and stretches out to ~ 2 Rvir towards south west to include the NGC 1316 galaxy group. The HI column density sensitivity (3 sigma over 25 km/s) ranges… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.11895v1-abstract-full').style.display = 'inline'; document.getElementById('2302.11895v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.11895v1-abstract-full" style="display: none;"> The MeerKAT Fornax Survey maps the distribution and kinematics of atomic neutral hydrogen gas (HI) in the nearby Fornax galaxy cluster using the MeerKAT telescope. The 12 deg^2 survey footprint covers the central region of the cluster out to ~ Rvir and stretches out to ~ 2 Rvir towards south west to include the NGC 1316 galaxy group. The HI column density sensitivity (3 sigma over 25 km/s) ranges from 5e+19/cm^2 at a resolution of ~ 10" (~ 1 kpc at the 20 Mpc distance of Fornax) down to ~ 1e+18/cm^2 at ~ 1' (~ 6 kpc), and slightly below this level at the lowest resolution of ~ 100" (~ 10 kpc). The HI mass sensitivity (3 sigma over 50 km/s) is 6e+5 Msun. The HI velocity resolution is 1.4 km/s. In this paper we describe the survey design and HI data processing, and we present a sample of six galaxies with long, one-sided, star-less HI tails (of which only one was previously known) radially oriented within the cluster and with measurable internal velocity gradients. We argue that the joint properties of the HI tails represent the first unambiguous evidence of ram pressure shaping the distribution of HI in the Fornax cluster. The disturbed optical morphology of all host galaxies supports the idea that the tails consist of HI initially pulled out of the galaxies' stellar body by tidal forces. Ram pressure was then able to further displace the weakly bound HI and give the tails their present direction, length and velocity gradient. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.11895v1-abstract-full').style.display = 'none'; document.getElementById('2302.11895v1-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Astronomy & Astrophysics, accepted. Data available at the MeerKAT Fornax Survey website https://sites.google.com/inaf.it/meerkatfornaxsurvey</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 673, A146 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2301.13526">arXiv:2301.13526</a> <span> [<a href="https://arxiv.org/pdf/2301.13526">pdf</a>, <a href="https://arxiv.org/format/2301.13526">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/10.1051/0004-6361/202245423">10.1051/0004-6361/202245423 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extended neutral hydrogen filamentary network in NGC 2403 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Veronese%2C+S">S. Veronese</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">F. Walter</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2301.13526v1-abstract-short" style="display: inline;"> We present new neutral hydrogen (HI) observations of the nearby galaxy NGC 2403 to determine the nature of a low-column density cloud that was detected earlier by the Green Bank Telescope. We find that this cloud is the tip of a complex of filaments of extraplanar gas that is coincident with the thin disk. The total HI mass of the complex is $2\times10^{7}\text{ M}_\odot$ or 0.6% of the total HI m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.13526v1-abstract-full').style.display = 'inline'; document.getElementById('2301.13526v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2301.13526v1-abstract-full" style="display: none;"> We present new neutral hydrogen (HI) observations of the nearby galaxy NGC 2403 to determine the nature of a low-column density cloud that was detected earlier by the Green Bank Telescope. We find that this cloud is the tip of a complex of filaments of extraplanar gas that is coincident with the thin disk. The total HI mass of the complex is $2\times10^{7}\text{ M}_\odot$ or 0.6% of the total HI mass of the galaxy. The main structure, previously referred to as the 8-kpc filament, is now seen to be even more extended, along a 20 kpc stream. The kinematics and morphological properties of the filaments are unlikely to be the result of outflows related to galactic fountains. It is more likely that the 20 kpc filament is related to a recent galaxy interaction. In this context, a $\sim$ 50 kpc long stellar stream has been recently detected connecting NGC 2403 with the nearby dwarf satellite DDO 44. Intriguingly, the southern tip of this stream overlaps with that of 20 kpc HI filament. We conclude that the HII anomalies in NGC 2403 are the result of a recent ($\sim2\text{ Gyr}$) interaction with DDO 44 leading to the observed filamentary complex. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2301.13526v1-abstract-full').style.display = 'none'; document.getElementById('2301.13526v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A55 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.07333">arXiv:2211.07333</a> <span> [<a href="https://arxiv.org/pdf/2211.07333">pdf</a>, <a href="https://arxiv.org/format/2211.07333">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/10.1017/pasa.2022.43">10.1017/pasa.2022.43 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> WALLABY Pilot Survey: Public release of HI kinematic models for more than 100 galaxies from phase 1 of ASKAP pilot observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Deg%2C+N">N. Deg</a>, <a href="/search/astro-ph?searchtype=author&query=Spekkens%2C+K">K. Spekkens</a>, <a href="/search/astro-ph?searchtype=author&query=Westmeier%2C+T">T. Westmeier</a>, <a href="/search/astro-ph?searchtype=author&query=Reynolds%2C+T+N">T. N. Reynolds</a>, <a href="/search/astro-ph?searchtype=author&query=Venkataraman%2C+P">P. Venkataraman</a>, <a href="/search/astro-ph?searchtype=author&query=Goliath%2C+S">S. Goliath</a>, <a href="/search/astro-ph?searchtype=author&query=Shen%2C+A+X">A. X. Shen</a>, <a href="/search/astro-ph?searchtype=author&query=Halloran%2C+R">R. Halloran</a>, <a href="/search/astro-ph?searchtype=author&query=Bosma%2C+A">A. Bosma</a>, <a href="/search/astro-ph?searchtype=author&query=Catinella%2C+B">B. Catinella</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Teodoro%2C+E+M">E. M. Di Teodoro</a>, <a href="/search/astro-ph?searchtype=author&query=Elagali%2C+A">A. Elagali</a>, <a href="/search/astro-ph?searchtype=author&query=For%2C+B+-">B. -Q. For</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">C. Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">G. I. G. J贸zsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B">B. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Lee-Waddell%2C+K">K. Lee-Waddell</a>, <a href="/search/astro-ph?searchtype=author&query=Lelli%2C+F">F. Lelli</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+X">X. Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Murugeshan%2C+C">C. Murugeshan</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+S">S. Oh</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2211.07333v1-abstract-short" style="display: inline;"> We present the Widefield ASKAP L-band Legacy All-sky Blind surveY (WALLABY) Pilot Phase I HI kinematic models. This first data release consists of HI observations of three fields in the direction of the Hydra and Norma clusters, and the NGC 4636 galaxy group. In this paper, we describe how we generate and publicly release flat-disk tilted-ring kinematic models for 109/592 unique HI detections in t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.07333v1-abstract-full').style.display = 'inline'; document.getElementById('2211.07333v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.07333v1-abstract-full" style="display: none;"> We present the Widefield ASKAP L-band Legacy All-sky Blind surveY (WALLABY) Pilot Phase I HI kinematic models. This first data release consists of HI observations of three fields in the direction of the Hydra and Norma clusters, and the NGC 4636 galaxy group. In this paper, we describe how we generate and publicly release flat-disk tilted-ring kinematic models for 109/592 unique HI detections in these fields. The modelling method adopted here - which we call the WALLABY Kinematic Analysis Proto-Pipeline (WKAPP) and for which the corresponding scripts are also publicly available - consists of combining results from the homogeneous application of the FAT and 3DBAROLO algorithms to the subset of 209 detections with sufficient resolution and S/N in order to generate optimized model parameters and uncertainties. The 109 models presented here tend to be gas rich detections resolved by at least 3-4 synthesized beams across their major axes, but there is no obvious environmental bias in the modelling. The data release described here is the first step towards the derivation of similar products for thousands of spatially-resolved WALLABY detections via a dedicated kinematic pipeline. Such a large publicly available and homogeneously analyzed dataset will be a powerful legacy product that that will enable a wide range of scientific studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.07333v1-abstract-full').style.display = 'none'; document.getElementById('2211.07333v1-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, 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">Accepted to PASA</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.09383">arXiv:2210.09383</a> <span> [<a href="https://arxiv.org/pdf/2210.09383">pdf</a>, <a href="https://arxiv.org/format/2210.09383">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/10.1051/0004-6361/202140704">10.1051/0004-6361/202140704 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HALOGAS: Strong Constraints on the Neutral Gas Reservoir and Accretion Rate in Nearby Spiral Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%BCtte%2C+E">E. J眉tte</a>, <a href="/search/astro-ph?searchtype=author&query=Heald%2C+G+H">G. H. Heald</a>, <a href="/search/astro-ph?searchtype=author&query=Ruiz%2C+N+H">N. Herrera Ruiz</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">G. I. G. J贸zsa</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">P. Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Marasco%2C+A">A. Marasco</a>, <a href="/search/astro-ph?searchtype=author&query=Dettmar%2C+R+-">R. -J. Dettmar</a>, <a href="/search/astro-ph?searchtype=author&query=Pingel%2C+N+M">N. M. Pingel</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T">T. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Rand%2C+R+J">R. J. Rand</a>, <a href="/search/astro-ph?searchtype=author&query=Walterbos%2C+R+A+M">R. A. M. Walterbos</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</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="2210.09383v1-abstract-short" style="display: inline;"> Galaxies in the local Universe are thought to require ongoing replenishment of their gas reservoir in order to maintain the observed star formation rates. Cosmological simulations predict that such accretion can occur in both a dynamically hot and cold mode. However, until now observational evidence of the accretion required to match the observed star formation histories is lacking. This paper att… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.09383v1-abstract-full').style.display = 'inline'; document.getElementById('2210.09383v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.09383v1-abstract-full" style="display: none;"> Galaxies in the local Universe are thought to require ongoing replenishment of their gas reservoir in order to maintain the observed star formation rates. Cosmological simulations predict that such accretion can occur in both a dynamically hot and cold mode. However, until now observational evidence of the accretion required to match the observed star formation histories is lacking. This paper attempts to determine whether galaxies in the local Universe possess a significant reservoir of HI and what would be the accretion rates derived from such reservoirs. We search the vicinity of 22 nearby galaxies for isolated HI clouds or distinct streams in a systematic and automated manner. The HALOGAS observations represent one of the most sensitive and detailed HI surveys to date. These observations typically reach column density sensitivities of 10^19 cm^-2 over a 20 km/s width. We find 14 secure HI cloud candidates without an observed optical counterpart. These cloud candidates appear to be analogues to the most massive clouds detected around the Milky Way and M31. However, on average their numbers seem significantly reduced. We constrain upper limits for HI accretion in the local Universe. The average HI mass currently observed amounts to a rate of 0.05 Msun/yr with a stringent upper limit of 0.22 Msun/yr, confirming previous estimates. This is much lower than the average star formation rate in this sample. Our best estimate, based on GBT detection limits of several galaxies, suggests that another 0.04 Msun/yr could be accreted from undetected clouds and streams. These results show that in nearby galaxies HI is not being accreted at the same rate as stars are currently being formed. Our study can not exclude that other forms of gas accretion are at work. However, these observations also do not reveal extended neutral gas reservoirs around most nearby spiral galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.09383v1-abstract-full').style.display = 'none'; document.getElementById('2210.09383v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy & Astrophysics section 4. Extragalactic astronomy. Data available at https://www.astron.nl/halogas/data.php</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 668, A182 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.05348">arXiv:2208.05348</a> <span> [<a href="https://arxiv.org/pdf/2208.05348">pdf</a>, <a href="https://arxiv.org/format/2208.05348">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="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/10.1051/0004-6361/202244007">10.1051/0004-6361/202244007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First release of Apertif imaging survey data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">Elizabeth A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Denes%2C+H">H. Denes</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">K. M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=Kutkin%2C+A">A. Kutkin</a>, <a href="/search/astro-ph?searchtype=author&query=Lucero%2C+D+M">D. M. Lucero</a>, <a href="/search/astro-ph?searchtype=author&query=Morganti%2C+R">R. Morganti</a>, <a href="/search/astro-ph?searchtype=author&query=Moss%2C+V+A">V. A. Moss</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Orru%2C+E">E. Orru</a>, <a href="/search/astro-ph?searchtype=author&query=Schulz%2C+R">R. Schulz</a>, <a href="/search/astro-ph?searchtype=author&query=van+Amesfoort%2C+A+S">A. S. van Amesfoort</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+A">A. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Boersma%2C+O+M">O. M. Boersma</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M">M. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+R+v+d">R. van den Brink</a>, <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">W. A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">L. Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">A. H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=van+Diepen%2C+G+N+J">G. N. J. van Diepen</a>, <a href="/search/astro-ph?searchtype=author&query=Dijkema%2C+T+J">T. J. Dijkema</a>, <a href="/search/astro-ph?searchtype=author&query=Ebbendorf%2C+N">N. Ebbendorf</a> , et al. (34 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="2208.05348v2-abstract-short" style="display: inline;"> (Abridged) Apertif is a phased-array feed system for WSRT, providing forty instantaneous beams over 300 MHz of bandwidth. A dedicated survey program started on 1 July 2019, with the last observations taken on 28 February 2022. We describe the release of data products from the first year of survey operations, through 30 June 2020. We focus on defining quality control metrics for the processed data… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.05348v2-abstract-full').style.display = 'inline'; document.getElementById('2208.05348v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.05348v2-abstract-full" style="display: none;"> (Abridged) Apertif is a phased-array feed system for WSRT, providing forty instantaneous beams over 300 MHz of bandwidth. A dedicated survey program started on 1 July 2019, with the last observations taken on 28 February 2022. We describe the release of data products from the first year of survey operations, through 30 June 2020. We focus on defining quality control metrics for the processed data products. The Apertif imaging pipeline, Apercal, automatically produces non-primary beam corrected continuum images, polarization images and cubes, and uncleaned spectral line and dirty beam cubes for each beam of an Apertif imaging observation. For this release, processed data products are considered on a beam-by-beam basis within an observation. We validate the continuum images by using metrics that identify deviations from Gaussian noise in the residual images. If the continuum image passes validation, we release all processed data products for a given beam. We apply further validation to the polarization and line data products. We release all raw observational data from the first year of survey observations, for a total of 221 observations of 160 independent target fields, covering approximately one thousand square degrees of sky. Images and cubes are released on a per beam basis, and 3374 beams are released. The median noise in the continuum images is 41.4 uJy/bm, with a slightly lower median noise of 36.9 uJy/bm in the Stokes V polarization image. The median angular resolution is 11.6"/sin(Dec). The median noise for all line cubes, with a spectral resolution of 36.6 kHz, is 1.6 mJy/bm, corresponding to a 3-sigma HI column density sensitivity of 1.8 x 10^20 atoms cm^-2 over 20 km/s (for a median angular resolution of 24" x 15"). We also provide primary beam images for each individual Apertif compound beam. The data are made accessible using a Virtual Observatory interface. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.05348v2-abstract-full').style.display = 'none'; document.getElementById('2208.05348v2-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 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, updated Figure 1</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 667, A38 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.05342">arXiv:2208.05342</a> <span> [<a href="https://arxiv.org/pdf/2208.05342">pdf</a>, <a href="https://arxiv.org/format/2208.05342">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="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/10.1051/0004-6361/202244008">10.1051/0004-6361/202244008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Continuum source catalog for the first APERTIF data release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kutkin%2C+A+M">A. M. Kutkin</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Morganti%2C+R">R. Morganti</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Mancini%2C+M">M. Mancini</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">K. M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=Lucero%2C+D+M">D. M. Lucero</a>, <a href="/search/astro-ph?searchtype=author&query=Moss%2C+V+A">V. A. Moss</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+A">A. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+R+v+d">R. van den Brink</a>, <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">W. A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">L. Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=Loose%2C+G+M">G. M. Loose</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">J. van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Y. Maan</a>, <a href="/search/astro-ph?searchtype=author&query=Mika%2C+A">A'. Mika</a>, <a href="/search/astro-ph?searchtype=author&query=Norden%2C+M+J">M. J. Norden</a>, <a href="/search/astro-ph?searchtype=author&query=Offringa%2C+A+R">A. R. Offringa</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L+C">L. C. Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Schuur%2C+D">D. van der Schuur</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2208.05342v1-abstract-short" style="display: inline;"> The first data release of Apertif survey contains 3074 radio continuum images covering a thousand square degrees of the sky. The observations were performed during August 2019 to July 2020. The continuum images were produced at a central frequency 1355 MHz with the bandwidth of $\sim$150 MHz and angular resolution reaching 10". In this work we introduce and apply a new method to obtain a primary b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.05342v1-abstract-full').style.display = 'inline'; document.getElementById('2208.05342v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.05342v1-abstract-full" style="display: none;"> The first data release of Apertif survey contains 3074 radio continuum images covering a thousand square degrees of the sky. The observations were performed during August 2019 to July 2020. The continuum images were produced at a central frequency 1355 MHz with the bandwidth of $\sim$150 MHz and angular resolution reaching 10". In this work we introduce and apply a new method to obtain a primary beam model using a machine learning approach, Gaussian process regression. The primary beam models obtained with this method are published along with the data products for the first Apertif data release. We apply the method to the continuum images, mosaic them and extract the source catalog. The catalog contains 249672 radio sources many of which are detected for the first time at these frequencies. We cross-match the coordinates with the NVSS, LOFAR/DR1/value-added and LOFAR/DR2 catalogs resulting in 44523, 22825 and 152824 common sources respectively. The first sample provides a unique opportunity to detect long term transient sources which have significantly changed their flux density for the last 25 years. The second and the third ones combined together provide information about spectral properties of the sources as well as the redshift estimates. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.05342v1-abstract-full').style.display = 'none'; document.getElementById('2208.05342v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 9 figures; accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 667, A39 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.06698">arXiv:2207.06698</a> <span> [<a href="https://arxiv.org/pdf/2207.06698">pdf</a>, <a href="https://arxiv.org/format/2207.06698">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/ac7c1b">10.3847/1538-3881/ac7c1b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gas dynamics and star formation in NGC 6822 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Park%2C+H">Hye-Jin Park</a>, <a href="/search/astro-ph?searchtype=author&query=Oh%2C+S">Se-Heon Oh</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J">Jing Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Zheng%2C+Y">Yun Zheng</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+H">Hong-Xin Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</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="2207.06698v1-abstract-short" style="display: inline;"> We present H I gas kinematics and star formation activities of NGC 6822, a dwarf galaxy located in the Local Group at a distance of ~ 490 kpc. We perform profile decomposition of line-of-sight velocity profiles of the H I data cube (42.4" x 12.0" spatial, corresponding to ~ 100 pc; 1.6 km s$^{-1}$ spectral) taken with the Australia Telescope Compact Array (ATCA). For this, we use a new tool, the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.06698v1-abstract-full').style.display = 'inline'; document.getElementById('2207.06698v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.06698v1-abstract-full" style="display: none;"> We present H I gas kinematics and star formation activities of NGC 6822, a dwarf galaxy located in the Local Group at a distance of ~ 490 kpc. We perform profile decomposition of line-of-sight velocity profiles of the H I data cube (42.4" x 12.0" spatial, corresponding to ~ 100 pc; 1.6 km s$^{-1}$ spectral) taken with the Australia Telescope Compact Array (ATCA). For this, we use a new tool, the so-called BAYGAUD which is based on Bayesian analysis techniques, allowing us to decompose a line-of-sight velocity profile into an optimal number of Gaussian components in a quantitative manner. We classify the decomposed H I gas components of NGC 6822 into cool-bulk, warm-bulk, cool-non-bulk and warm-non-bulk motions with respect to their centroid velocities and velocity dispersions. We correlate their gas surface densities with corresponding star formation rate densities derived using both the GALEX far-ultraviolet and WISE 22 $渭$m data to examine the resolved Kennicutt-Schmidt (K-S) law for NGC 6822. Of the decomposed H I gas components, the cool-bulk component is likely to better follow the linear extension of the K-S law for molecular hydrogen (H$_2$) at low gas surface densities where H I is not saturated. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.06698v1-abstract-full').style.display = 'none'; document.getElementById('2207.06698v1-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, 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">20 pages, 11 figures, 4 tables, accepted for publication in 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/2206.02847">arXiv:2206.02847</a> <span> [<a href="https://arxiv.org/pdf/2206.02847">pdf</a>, <a href="https://arxiv.org/format/2206.02847">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/10.1051/0004-6361/202243174">10.1051/0004-6361/202243174 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Seeing the forest and the trees: a radio investigation of the ULIRG Mrk 273 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kukreti%2C+P">Pranav Kukreti</a>, <a href="/search/astro-ph?searchtype=author&query=Morganti%2C+R">Raffaella Morganti</a>, <a href="/search/astro-ph?searchtype=author&query=Bondi%2C+M">Marco Bondi</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T">Tom Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Tadhunter%2C+C">Clive Tadhunter</a>, <a href="/search/astro-ph?searchtype=author&query=Morabito%2C+L+K">Leah K. Morabito</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</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=Drabent%2C+A">A. Drabent</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">K. M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=Ivashina%2C+M+V">M. V. Ivashina</a>, <a href="/search/astro-ph?searchtype=author&query=Kutkin%2C+A">A. Kutkin</a>, <a href="/search/astro-ph?searchtype=author&query=Mika%2C+%C3%81+M">脕. M. Mika</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L">Leon Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Shimwell%2C+T+W">T. W. Shimwell</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">Joeri van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=van+Weeren%2C+R+J">R. J. van Weeren</a>, <a href="/search/astro-ph?searchtype=author&query=Vohl%2C+D">Dany Vohl</a>, <a href="/search/astro-ph?searchtype=author&query=Ziemke%2C+J">J. Ziemke</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="2206.02847v1-abstract-short" style="display: inline;"> Galaxy mergers have been observed to trigger nuclear activity by feeding gas to the central supermassive black hole. One such class of objects are Ultra Luminous InfraRed Galaxies (ULIRGs), which are mostly late stage major mergers of gas-rich galaxies. Recently, large-scale ($\sim$100 kpc) radio continuum emission has been detected in a select number of ULIRGs, all of which also harbour powerful… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.02847v1-abstract-full').style.display = 'inline'; document.getElementById('2206.02847v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.02847v1-abstract-full" style="display: none;"> Galaxy mergers have been observed to trigger nuclear activity by feeding gas to the central supermassive black hole. One such class of objects are Ultra Luminous InfraRed Galaxies (ULIRGs), which are mostly late stage major mergers of gas-rich galaxies. Recently, large-scale ($\sim$100 kpc) radio continuum emission has been detected in a select number of ULIRGs, all of which also harbour powerful Active Galactic Nuclei (AGN). This hints at the presence of large-scale radio emission being evidence for nuclear activity. Exploring the origin of this radio emission and its link to nuclear activity requires high sensitivity multi-frequency data. We present such an analysis of the ULIRG Mrk 273. Using the International LOFAR telescope (ILT), we detected spectacular large-scale arcs in this system. This detection includes, for the first time, a giant $\sim$190 kpc arc in the north. We propose these arcs are fuelled by a low power radio AGN triggered by the merger. We also identified a bright $\sim$45 kpc radio ridge, which is likely related to the ionised gas nebula in that region. We combined this with high sensitivity data from APERture Tile In Focus (Apertif) and archival data from the Very Large Array (VLA) to explore the spectral properties. The ILT simultaneously allowed us to probe the nucleus at a resolution of $\sim$0.3 arcsec, where we detected three components, and, for the first time, diffuse emission around these components. Combining this with archival high frequency VLA images of the nucleus allowed us to detect absorption in one component, and a steep spectrum radio AGN in another. We then extrapolate from this case study to the importance of investigating the presence of radio emission in more ULIRGs and what it can tell us about the link between mergers and the presence of radio activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.02847v1-abstract-full').style.display = 'none'; document.getElementById('2206.02847v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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 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 664, A25 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.12362">arXiv:2205.12362</a> <span> [<a href="https://arxiv.org/pdf/2205.12362">pdf</a>, <a href="https://arxiv.org/format/2205.12362">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> </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/10.1051/0004-6361/202244107">10.1051/0004-6361/202244107 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Apertif Radio Transient System (ARTS): Design, Commissioning, Data Release, and Detection of the first 5 Fast Radio Bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">Joeri van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Kooistra%2C+E">Eric Kooistra</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L">Leon Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Hargreaves%2C+J+E">J. E. Hargreaves</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Yogesh Maan</a>, <a href="/search/astro-ph?searchtype=author&query=Pastor-Marazuela%2C+I">In茅s Pastor-Marazuela</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Schuur%2C+D">Daniel van der Schuur</a>, <a href="/search/astro-ph?searchtype=author&query=Sclocco%2C+A">Alessio Sclocco</a>, <a href="/search/astro-ph?searchtype=author&query=Straal%2C+S+M">Samayra M. Straal</a>, <a href="/search/astro-ph?searchtype=author&query=Vohl%2C+D">Dany Vohl</a>, <a href="/search/astro-ph?searchtype=author&query=Wijnholds%2C+S+J">Stefan J. Wijnholds</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">Elizabeth A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">Bj枚rn Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=Attema%2C+J">Jisk Attema</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C">Cees Bassa</a>, <a href="/search/astro-ph?searchtype=author&query=Bast%2C+J+E">Jeanette E. Bast</a>, <a href="/search/astro-ph?searchtype=author&query=Bilous%2C+A">Anna Bilous</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Boersma%2C+O+M">Oliver M. Boersma</a>, <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">Wim A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">Arthur H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">Sieds Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">Helga D茅nes</a> , et al. (27 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="2205.12362v2-abstract-short" style="display: inline;"> Fast Radio Bursts must be powered by uniquely energetic emission mechanisms. This requirement has eliminated a number of possible source types, but several remain. Identifying the physical nature of Fast Radio Burst (FRB) emitters arguably requires good localisation of more detections, and broadband studies enabled by real-time alerting. We here present the Apertif Radio Transient System (ARTS), a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.12362v2-abstract-full').style.display = 'inline'; document.getElementById('2205.12362v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.12362v2-abstract-full" style="display: none;"> Fast Radio Bursts must be powered by uniquely energetic emission mechanisms. This requirement has eliminated a number of possible source types, but several remain. Identifying the physical nature of Fast Radio Burst (FRB) emitters arguably requires good localisation of more detections, and broadband studies enabled by real-time alerting. We here present the Apertif Radio Transient System (ARTS), a supercomputing radio-telescope instrument that performs real-time FRB detection and localisation on the Westerbork Synthesis Radio Telescope (WSRT) interferometer. It reaches coherent-addition sensitivity over the entire field of the view of the primary dish beam. After commissioning results verified the system performed as planned, we initiated the Apertif FRB survey (ALERT). Over the first 5 weeks we observed at design sensitivity in 2019, we detected 5 new FRBs, and interferometrically localised each of these to 0.4--10 sq. arcmin. All detections are broad band and very narrow, of order 1 ms duration, and unscattered. Dispersion measures are generally high. Only through the very high time and frequency resolution of ARTS are these hard-to-find FRBs detected, producing an unbiased view of the intrinsic population properties. Most localisation regions are small enough to rule out the presence of associated persistent radio sources. Three FRBs cut through the halos of M31 and M33. We demonstrate that Apertif can localise one-off FRBs with an accuracy that maps magneto-ionic material along well-defined lines of sight. The rate of 1 every ~7 days next ensures a considerable number of new sources are detected for such study. The combination of detection rate and localisation accuracy exemplified by the 5 first ARTS FRBs thus marks a new phase in which a growing number of bursts can be used to probe our Universe. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.12362v2-abstract-full').style.display = 'none'; document.getElementById('2205.12362v2-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 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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 version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 672, A117 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.09662">arXiv:2205.09662</a> <span> [<a href="https://arxiv.org/pdf/2205.09662">pdf</a>, <a href="https://arxiv.org/format/2205.09662">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/10.1051/0004-6361/202244045">10.1051/0004-6361/202244045 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterising the Apertif primary beam response </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">K. M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Kutkin%2C+A">A. Kutkin</a>, <a href="/search/astro-ph?searchtype=author&query=Morganti%2C+R">R. Morganti</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Moss%2C+V+A">V. A. Moss</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Ivashina%2C+M+V">M. V. Ivashina</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">A. H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=Hut%2C+B">B. Hut</a>, <a href="/search/astro-ph?searchtype=author&query=Loose%2C+G+M">G. M. Loose</a>, <a href="/search/astro-ph?searchtype=author&query=Lucero%2C+D+M">D. M. Lucero</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Y. Maan</a>, <a href="/search/astro-ph?searchtype=author&query=Mika%2C+%C3%81">脕. Mika</a>, <a href="/search/astro-ph?searchtype=author&query=Norden%2C+M+J">M. J. Norden</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L+C">L. C. Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Smits%2C+R">R. Smits</a>, <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">W. A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+R+v+d">R. van den Brink</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Schuur%2C+D">D. van der Schuur</a> , et al. (5 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="2205.09662v2-abstract-short" style="display: inline;"> Context. Phased Array Feeds (PAFs) are multi element receivers in the focal plane of a telescope that make it possible to form simultaneously multiple beams on the sky by combining the complex gains of the individual antenna elements. Recently the Westerbork Synthesis Radio Telescope (WSRT) was upgraded with PAF receivers and carried out several observing programs including two imaging surveys and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.09662v2-abstract-full').style.display = 'inline'; document.getElementById('2205.09662v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.09662v2-abstract-full" style="display: none;"> Context. Phased Array Feeds (PAFs) are multi element receivers in the focal plane of a telescope that make it possible to form simultaneously multiple beams on the sky by combining the complex gains of the individual antenna elements. Recently the Westerbork Synthesis Radio Telescope (WSRT) was upgraded with PAF receivers and carried out several observing programs including two imaging surveys and a time domain survey. The Apertif imaging surveys use a configuration, where 40 partially overlapping compound beams (CBs) are simultaneously formed on the sky and arranged in an approximately rectangular shape. Aims. This manuscript aims to characterise the response of the 40 Apertif CBs to create frequency-resolved, I, XX and YY polarization empirical beam shapes. The measured CB maps can be used for image deconvolution, primary beam correction and mosaicing of Apertif imaging data. Methods. We use drift scan measurements to measure the response of each of the 40 CBs of Apertif. We derive beam maps for all individual beams in I, XX and YY polarisation in 10 or 18 frequency bins over the same bandwidth as the Apertif imaging surveys. We sample the main lobe of the beams and the side lobes up to a radius of 0.6 degrees from the beam centres. In addition, we derive beam maps for each individual WSRT dish as well. Results. We present the frequency and time dependence of the beam shapes and sizes. We compare the compound beam shapes derived with the drift scan method to beam shapes derived with an independent method using a Gaussian Process Regression comparison between the Apertif continuum images and the NRAO VLA Sky Survey (NVSS) catalogue. We find a good agreement between the beam shapes derived with the two independent methods. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.09662v2-abstract-full').style.display = 'none'; document.getElementById('2205.09662v2-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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 by A&A, 14 pages, 15 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 667, A40 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.00637">arXiv:2204.00637</a> <span> [<a href="https://arxiv.org/pdf/2204.00637">pdf</a>, <a href="https://arxiv.org/format/2204.00637">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/stac936">10.1093/mnras/stac936 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The extended HI halo of NGC 4945 as seen by MeerKAT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ianjamasimanana%2C+R">Roger Ianjamasimanana</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">Gyula I. G. J贸zsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">Peter Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">Dane Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Namumba%2C+B">Brenda Namumba</a>, <a href="/search/astro-ph?searchtype=author&query=Carignan%2C+C">Claude Carignan</a>, <a href="/search/astro-ph?searchtype=author&query=Dettmar%2C+R">Ralf-J眉rgen Dettmar</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">Paolo Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Smirnov%2C+O+M">Oleg M. Smirnov</a>, <a href="/search/astro-ph?searchtype=author&query=Thorat%2C+K">Kshitij Thorat</a>, <a href="/search/astro-ph?searchtype=author&query=Hugo%2C+B+V">Benjamin V. Hugo</a>, <a href="/search/astro-ph?searchtype=author&query=Ramaila%2C+A+J+T">Athanaseus J. T. Ramaila</a>, <a href="/search/astro-ph?searchtype=author&query=Maina%2C+E">Eric Maina</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">Filippo M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Makhathini%2C+S">Sphesihle Makhathini</a>, <a href="/search/astro-ph?searchtype=author&query=Andati%2C+L+A+L">Lexy A. L. Andati</a>, <a href="/search/astro-ph?searchtype=author&query=Moln%C3%A1r%2C+D+C">D谩niel Cs. Moln谩r</a>, <a href="/search/astro-ph?searchtype=author&query=Perkins%2C+S">Simon Perkins</a>, <a href="/search/astro-ph?searchtype=author&query=Loi%2C+F">Francesca Loi</a>, <a href="/search/astro-ph?searchtype=author&query=Ramatsoku%2C+M">Mpati Ramatsoku</a>, <a href="/search/astro-ph?searchtype=author&query=Atemkeng%2C+M">Marcellin Atemkeng</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="2204.00637v1-abstract-short" style="display: inline;"> Observations of the neutral atomic hydrogen (HI) in the nuclear starburst galaxy NGC 4945 with MeerKAT are presented. We find a large amount of halo gas, previously missed by HI observations, accounting for 6.8% of the total HI mass. This is most likely gas blown into the halo by star formation. Our maps go down to a $3蟽$ column density level of $5\times10^{18} cm^{-2}$ . We model the HI distribut… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.00637v1-abstract-full').style.display = 'inline'; document.getElementById('2204.00637v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.00637v1-abstract-full" style="display: none;"> Observations of the neutral atomic hydrogen (HI) in the nuclear starburst galaxy NGC 4945 with MeerKAT are presented. We find a large amount of halo gas, previously missed by HI observations, accounting for 6.8% of the total HI mass. This is most likely gas blown into the halo by star formation. Our maps go down to a $3蟽$ column density level of $5\times10^{18} cm^{-2}$ . We model the HI distribution using tilted-ring fitting techniques and find a warp on the galaxy's approaching and receding sides. The HI in the northern side of the galaxy appears to be suppressed. This may be the result of ionisation by the starburst activity in the galaxy, as suggested by a previous study. The origin of the warp is unclear but could be due to past interactions or ram pressure stripping. Broad, asymmetric HI absorption lines extending beyond the HI emission velocity channels are present towards the nuclear region of NGC 4945. Such broad lines suggest the existence of a nuclear ring moving at a high circular velocity. This is supported by the clear rotation patterns in the HI absorption velocity field. The asymmetry of the absorption spectra can be caused by outflows or inflows of gas in the nuclear region of NGC 4945. The continuum map shows small extensions on both sides of the galaxy's major axis that might be signs of outflows resulting from the starburst activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.00637v1-abstract-full').style.display = 'none'; document.getElementById('2204.00637v1-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">20 pages, 15 figures, 3 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/2203.16925">arXiv:2203.16925</a> <span> [<a href="https://arxiv.org/pdf/2203.16925">pdf</a>, <a href="https://arxiv.org/format/2203.16925">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202243201">10.1051/0004-6361/202243201 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Apertif science verification campaign - Characteristics of polarised radio sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+A">A. Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">K. M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Moss%2C+V+A">V. A. Moss</a>, <a href="/search/astro-ph?searchtype=author&query=Schulz%2C+R">R. Schulz</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">L. Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=Hut%2C+B">B. Hut</a>, <a href="/search/astro-ph?searchtype=author&query=Ivashina%2C+M+V">M. V. Ivashina</a>, <a href="/search/astro-ph?searchtype=author&query=Loose%2C+G+M">G. M. Loose</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Y. Maan</a>, <a href="/search/astro-ph?searchtype=author&query=Mika%2C+A">A. Mika</a>, <a href="/search/astro-ph?searchtype=author&query=Mulder%2C+H">H. Mulder</a>, <a href="/search/astro-ph?searchtype=author&query=Norden%2C+M+J">M. J. Norden</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L+C">L. C. Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Orr%C3%BA%2C+E">E. Orr煤</a>, <a href="/search/astro-ph?searchtype=author&query=Ruiter%2C+M">M. Ruiter</a>, <a href="/search/astro-ph?searchtype=author&query=Smits%2C+R">R. Smits</a>, <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">W. A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">J. van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Vermaas%2C+N+J">N. J. Vermaas</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.16925v1-abstract-short" style="display: inline;"> We analyse five early science datasets from the APERture Tile in Focus (Apertif) phased array feed system to verify the polarisation capabilities of Apertif in view of future larger data releases. We aim to characterise the source population of the polarised sky in the L-Band using polarised source information in combination with IR and optical data. We use automatic routines to generate full fiel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.16925v1-abstract-full').style.display = 'inline'; document.getElementById('2203.16925v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.16925v1-abstract-full" style="display: none;"> We analyse five early science datasets from the APERture Tile in Focus (Apertif) phased array feed system to verify the polarisation capabilities of Apertif in view of future larger data releases. We aim to characterise the source population of the polarised sky in the L-Band using polarised source information in combination with IR and optical data. We use automatic routines to generate full field-of-view Q- and U-cubes and perform RM-Synthesis, source finding, and cross-matching with published radio, optical, and IR data to generate polarised source catalogues. SED-fitting routines were used to determine photometric redshifts, star-formation rates, and galaxy masses. IR colour information was used to classify sources as AGN or star-forming-dominated and early- or late-type. We surveyed an area of 56deg$^2$ and detected 1357 polarised source components in 1170 sources. The fraction of polarised sources is 10.57% with a median fractional polarisation of 4.70$\pm$0.14%. We confirmed the reliability of the Apertif measurements by comparing them with polarised cross-identified NVSS sources. Average RMs of the individual fields lie within the error of the best Milky Way foreground measurements. All of our polarised sources were found to be dominated by AGN activity in the radio regime with most of them being radio-loud (79%) and of the FRII class (87%). The host galaxies of our polarised source sample are dominated by intermediate disc and star-forming disc galaxies. The contribution of star formation to the radio emission is on the order of a few percent for $\approx$10% of the polarised sources while for $\approx$90% it is completely dominated by the AGN. We do not see any change in fractional polarisation for different star-formation rates of the AGN host galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.16925v1-abstract-full').style.display = 'none'; document.getElementById('2203.16925v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">24 pages, 21 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 663, A103 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.03722">arXiv:2112.03722</a> <span> [<a href="https://arxiv.org/pdf/2112.03722">pdf</a>, <a href="https://arxiv.org/format/2112.03722">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/10.1016/j.ascom.2021.100514">10.1016/j.ascom.2021.100514 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Apercal -- The Apertif Calibration Pipeline </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=Schulz%2C+R">R. Schulz</a>, <a href="/search/astro-ph?searchtype=author&query=Dijkema%2C+T+J">T. J. Dijkema</a>, <a href="/search/astro-ph?searchtype=author&query=Moss%2C+V+A">V. A. Moss</a>, <a href="/search/astro-ph?searchtype=author&query=Offringa%2C+A+R">A. R. Offringa</a>, <a href="/search/astro-ph?searchtype=author&query=Kutkin%2C+A">A. Kutkin</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=Frank%2C+B+S">B. S. Frank</a>, <a href="/search/astro-ph?searchtype=author&query=Vilchez%2C+N+P+E">N. P. E. Vilchez</a>, <a href="/search/astro-ph?searchtype=author&query=Verstappen%2C+J">J. Verstappen</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+K">E. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Denes%2C+H">H. Denes</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">K. M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=Lucero%2C+D">D. Lucero</a>, <a href="/search/astro-ph?searchtype=author&query=Morganti%2C+R">R. Morganti</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T">T. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+-">D. -J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Ivashina%2C+M+V">M. V. Ivashina</a>, <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">W. A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L+D">L. D. Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">A. H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=Loose%2C+G+M">G. M. Loose</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Y. Maan</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.03722v1-abstract-short" style="display: inline;"> Apertif (APERture Tile In Focus) is one of the Square Kilometre Array (SKA) pathfinder facilities. The Apertif project is an upgrade to the 50-year-old Westerbork Synthesis Radio Telescope (WSRT) using phased-array feed technology. The new receivers create 40 individual beams on the sky, achieving an instantaneous sky coverage of 6.5 square degrees. The primary goal of the Apertif Imaging Survey i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.03722v1-abstract-full').style.display = 'inline'; document.getElementById('2112.03722v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.03722v1-abstract-full" style="display: none;"> Apertif (APERture Tile In Focus) is one of the Square Kilometre Array (SKA) pathfinder facilities. The Apertif project is an upgrade to the 50-year-old Westerbork Synthesis Radio Telescope (WSRT) using phased-array feed technology. The new receivers create 40 individual beams on the sky, achieving an instantaneous sky coverage of 6.5 square degrees. The primary goal of the Apertif Imaging Survey is to perform a wide survey of 3500 square degrees (AWES) and a medium deep survey of 350 square degrees (AMES) of neutral atomic hydrogen (up to a redshift of 0.26), radio continuum emission and polarisation. Each survey pointing yields 4.6 TB of correlated data. The goal of Apercal is to process this data and fully automatically generate science ready data products for the astronomical community while keeping up with the survey observations. We make use of common astronomical software packages in combination with Python based routines and parallelisation. We use an object oriented module-based approach to ensure easy adaptation of the pipeline. A Jupyter notebook based framework allows user interaction and execution of individual modules as well as a full automatic processing of a complete survey observation. If nothing interrupts processing, we are able to reduce a single pointing survey observation on our five node cluster with 24 physical cores and 256 GB of memory each within 24h keeping up with the speed of the surveys. The quality of the generated images is sufficient for scientific usage for 44 % of the recorded data products with single images reaching dynamic ranges of several thousands. Future improvements will increase this percentage to over 80 %. Our design allowed development of the pipeline in parallel to the commissioning of the Apertif system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.03722v1-abstract-full').style.display = 'none'; document.getElementById('2112.03722v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomy and Computing 38 (2022) 100514 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.14234">arXiv:2109.14234</a> <span> [<a href="https://arxiv.org/pdf/2109.14234">pdf</a>, <a href="https://arxiv.org/format/2109.14234">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/10.1051/0004-6361/202141739">10.1051/0004-6361/202141739 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Apertif, Phased Array Feeds for the Westerbork Synthesis Radio Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">W. A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Verheijen%2C+M+A+W">M. A. W. Verheijen</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=Braun%2C+R">R. Braun</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">K. M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=Holties%2C+H">H. Holties</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=Hut%2C+B">B. Hut</a>, <a href="/search/astro-ph?searchtype=author&query=Kooistra%2C+E">E. Kooistra</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">J. van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Loose%2C+G+M">G. M. Loose</a>, <a href="/search/astro-ph?searchtype=author&query=Morganti%2C+R">R. Morganti</a>, <a href="/search/astro-ph?searchtype=author&query=Moss%2C+V+A">V. A. Moss</a>, <a href="/search/astro-ph?searchtype=author&query=Orr%C3%BA%2C+E">E. Orr煤</a>, <a href="/search/astro-ph?searchtype=author&query=Ruiter%2C+M">M. Ruiter</a>, <a href="/search/astro-ph?searchtype=author&query=Schoenmakers%2C+A+P">A. P. Schoenmakers</a>, <a href="/search/astro-ph?searchtype=author&query=Vermaas%2C+N+J">N. J. Vermaas</a>, <a href="/search/astro-ph?searchtype=author&query=Wijnholds%2C+S+J">S. J. Wijnholds</a>, <a href="/search/astro-ph?searchtype=author&query=van+Amesfoort%2C+A+S">A. S. van Amesfoort</a>, <a href="/search/astro-ph?searchtype=author&query=Arts%2C+M+J">M. J. Arts</a>, <a href="/search/astro-ph?searchtype=author&query=Attema%2C+J+J">J. J. Attema</a>, <a href="/search/astro-ph?searchtype=author&query=Bakker%2C+L">L. Bakker</a>, <a href="/search/astro-ph?searchtype=author&query=Bassa%2C+C+G">C. G. Bassa</a> , et al. (65 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="2109.14234v2-abstract-short" style="display: inline;"> We describe the APERture Tile In Focus (Apertif) system, a phased array feed (PAF) upgrade of the Westerbork Synthesis Radio Telescope which has transformed this telescope into a high-sensitivity, wide field-of-view L-band imaging and transient survey instrument. Using novel PAF technology, up to 40 partially overlapping beams can be formed on the sky simultaneously, significantly increasing the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.14234v2-abstract-full').style.display = 'inline'; document.getElementById('2109.14234v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.14234v2-abstract-full" style="display: none;"> We describe the APERture Tile In Focus (Apertif) system, a phased array feed (PAF) upgrade of the Westerbork Synthesis Radio Telescope which has transformed this telescope into a high-sensitivity, wide field-of-view L-band imaging and transient survey instrument. Using novel PAF technology, up to 40 partially overlapping beams can be formed on the sky simultaneously, significantly increasing the survey speed of the telescope. With this upgraded instrument, an imaging survey covering an area of 2300 deg2 is being performed which will deliver both continuum and spectral line data sets, of which the first data has been publicly released. In addition, a time domain transient and pulsar survey covering 15,000 deg2 is in progress. An overview of the Apertif science drivers, hardware and software of the upgraded telescope is presented, along with its key performance characteristics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.14234v2-abstract-full').style.display = 'none'; document.getElementById('2109.14234v2-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">29 pages, 42 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 658, A146 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.10428">arXiv:2105.10428</a> <span> [<a href="https://arxiv.org/pdf/2105.10428">pdf</a>, <a href="https://arxiv.org/format/2105.10428">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/stab1524">10.1093/mnras/stab1524 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MeerKAT-64 discovers wide-spread tidal debris in the nearby NGC 7232 galaxy group </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Namumba%2C+B">Brenda Namumba</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">Baerbel Silvia Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">Gyula I. G. J贸zsa</a>, <a href="/search/astro-ph?searchtype=author&query=Lee-Waddell%2C+K">Karen Lee-Waddell</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+M+G">Michael Gordon Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Carignan%2C+C">Claude Carignan</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=Ianjamasimanana%2C+R">Roger Ianjamasimanana</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+E+W+J+G">Erwin W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Cluver%2C+M">Michelle Cluver</a>, <a href="/search/astro-ph?searchtype=author&query=Garrido%2C+J">Julian Garrido</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Exposito%2C+S">Susana Sanchez-Exposito</a>, <a href="/search/astro-ph?searchtype=author&query=Ramaila%2C+A">Athanaseus Ramaila</a>, <a href="/search/astro-ph?searchtype=author&query=Thorat%2C+K">Kshitij Thorat</a>, <a href="/search/astro-ph?searchtype=author&query=Andanti%2C+L+A+L">Lexy A. L. Andanti</a>, <a href="/search/astro-ph?searchtype=author&query=Hugo%2C+B">Benjamin Hugo</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">Dane Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">Peter Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">Paolo Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Smirnov%2C+O">Oleg Smirnov</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F">Filippo Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Makhathini%2C+S">Sphesihle Makhathini</a>, <a href="/search/astro-ph?searchtype=author&query=Molnar%2C+D+C+C">Daniel Csaba Csaba Molnar</a>, <a href="/search/astro-ph?searchtype=author&query=Perkins%2C+S">Simon Perkins</a>, <a href="/search/astro-ph?searchtype=author&query=Ramatsoku%2C+M">Mpati Ramatsoku</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2105.10428v1-abstract-short" style="display: inline;"> We report the discovery of large amounts of previously undetected cold neutral atomic hydrogen (\HI) around the core triplet galaxies in the nearby NGC~7232 galaxy group with MeerKAT. With a physical resolution of $\sim$1 kpc, we detect a complex web of low surface brightness \HI\ emission down to a 4$蟽$ column density level of $\sim$1 $\times$ 10$^{19}$ cm$^{-2}$ (over 44 \kms ). The newly discov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.10428v1-abstract-full').style.display = 'inline'; document.getElementById('2105.10428v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.10428v1-abstract-full" style="display: none;"> We report the discovery of large amounts of previously undetected cold neutral atomic hydrogen (\HI) around the core triplet galaxies in the nearby NGC~7232 galaxy group with MeerKAT. With a physical resolution of $\sim$1 kpc, we detect a complex web of low surface brightness \HI\ emission down to a 4$蟽$ column density level of $\sim$1 $\times$ 10$^{19}$ cm$^{-2}$ (over 44 \kms ). The newly discovered H\,{\sc i} streams extend over $\sim$20 arcmin corresponding to 140~kpc in projection. This is $\sim$3 times the \HI\ extent of the galaxy triplet (52 kpc). The \HI\ debris has an \HI\ mass of $\sim$6.6 $\times 10^9$~M$_{\odot}$, more than 50\% of the total \HI\ mass of the triplet. Within the galaxy triplet, NGC~7233 and NGC~7232 have lost a significant amount of \HI\ while NGC~7232B appears to have an excess of \HI. The \HI\ deficiency in NGC~7232 and NGC~7233 indicates that galaxy-galaxy interaction in the group concentrates on this galaxy pair while the other disc galaxies have visited them over time. In comparison to the AMIGA sample of isolated galaxies we find that with regards to its total \HI\ mass the NGC~7232/3 galaxy triplet is not \HI\ deficient. Despite the many interactions associated to the triplet galaxies, no \HI\ seems to have been lost from the group (yet). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.10428v1-abstract-full').style.display = 'none'; document.getElementById('2105.10428v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 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">17 pages, 11 figures, accepted for publication in MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 85A04 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.04280">arXiv:2104.04280</a> <span> [<a href="https://arxiv.org/pdf/2104.04280">pdf</a>, <a href="https://arxiv.org/format/2104.04280">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202140578">10.1051/0004-6361/202140578 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for radio emission from double-neutron star merger GW190425 using Apertif </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Boersma%2C+O">Oliv茅r Boersma</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">Joeri van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">Elizabeth A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">Bj枚rn Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=Kutkin%2C+A">Alexander Kutkin</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T">Tom Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+R+v+d">R. van den Brink</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">A. H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">L. Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">K. M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=Hut%2C+B">B. Hut</a>, <a href="/search/astro-ph?searchtype=author&query=Ivashina%2C+M">M. Ivashina</a>, <a href="/search/astro-ph?searchtype=author&query=Loose%2C+G+M">G. M. Loose</a>, <a href="/search/astro-ph?searchtype=author&query=Lucero%2C+D+M">D. M. Lucero</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Y. Maan</a>, <a href="/search/astro-ph?searchtype=author&query=Mika%2C+%C3%81">脕. Mika</a>, <a href="/search/astro-ph?searchtype=author&query=Moss%2C+V+A">V. A. Moss</a>, <a href="/search/astro-ph?searchtype=author&query=Mulder%2C+H">H. Mulder</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L+C">L. C. Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Ruiter%2C+M">M. Ruiter</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Schuur%2C+D">D. van der Schuur</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2104.04280v1-abstract-short" style="display: inline;"> Detection of the electromagnetic emission from coalescing binary neutron stars (BNS) is important for understanding the merger and afterglow. We present a search for a radio counterpart to the gravitational-wave source GW190425, a BNS merger, using Apertif on the Westerbork Synthesis Radio Telescope (WSRT). We observe a field of high probability in the associated localisation region for 3 epochs a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.04280v1-abstract-full').style.display = 'inline'; document.getElementById('2104.04280v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.04280v1-abstract-full" style="display: none;"> Detection of the electromagnetic emission from coalescing binary neutron stars (BNS) is important for understanding the merger and afterglow. We present a search for a radio counterpart to the gravitational-wave source GW190425, a BNS merger, using Apertif on the Westerbork Synthesis Radio Telescope (WSRT). We observe a field of high probability in the associated localisation region for 3 epochs at 68, 90 and 109 days post merger. We identify all sources that exhibit flux variations consistent with the expected afterglow emission of GW190425. We also look for possible transients. These are sources which are only present in one epoch. In addition, we quantify our ability to search for radio afterglows in fourth and future observing runs of the gravitational-wave detector network using Monte Carlo simulations. We found 25 afterglow candidates based on their variability. None of these could be associated with a possible host galaxy at the luminosity distance of GW190425. We also found 55 transient afterglow candidates that were only detected in one epoch. All turned out to be image artefacts. In the fourth observing run, we predict that up to three afterglows will be detectable by Apertif. While we did not find a source related to the afterglow emission of GW190425, the search validates our methods for future searches of radio afterglows. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.04280v1-abstract-full').style.display = 'none'; document.getElementById('2104.04280v1-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 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">11 pages, 7 figures, accepted for publication</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 650, A131 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.10347">arXiv:2101.10347</a> <span> [<a href="https://arxiv.org/pdf/2101.10347">pdf</a>, <a href="https://arxiv.org/format/2101.10347">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/10.1051/0004-6361/202039898">10.1051/0004-6361/202039898 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A MeerKAT view of pre-processing in the Fornax A group </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">P. Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Venhola%2C+A">A. Venhola</a>, <a href="/search/astro-ph?searchtype=author&query=Morokuma-Matsui%2C+K">K. Morokuma-Matsui</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R">R. Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Raj%2C+M+A">M. A. Raj</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Comrie%2C+A">A. Comrie</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">G. I. G. J贸zsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Loni%2C+A">A. Loni</a>, <a href="/search/astro-ph?searchtype=author&query=Loubser%2C+S+I">S. I. Loubser</a>, <a href="/search/astro-ph?searchtype=author&query=Moln%C3%A1r%2C+D+C">D. Cs. Moln谩r</a>, <a href="/search/astro-ph?searchtype=author&query=Passmoor%2C+S+S">S. S. Passmoor</a>, <a href="/search/astro-ph?searchtype=author&query=Ramatsoku%2C+M">M. Ramatsoku</a>, <a href="/search/astro-ph?searchtype=author&query=Sivitilli%2C+A">A. Sivitilli</a>, <a href="/search/astro-ph?searchtype=author&query=Smirnov%2C+O">O. Smirnov</a>, <a href="/search/astro-ph?searchtype=author&query=Thorat%2C+K">K. Thorat</a>, <a href="/search/astro-ph?searchtype=author&query=Vitello%2C+F">F. Vitello</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="2101.10347v2-abstract-short" style="display: inline;"> We present MeerKAT neutral hydrogen (HI) observations of the Fornax A group, that is likely falling into the Fornax cluster for the first time. Our HI image is sensitive to 1.4 x 10$^{19}$ cm$^{-2}$ over 44.1 km s$^{-1}$, where we detect HI in 10 galaxies and a total of 1.12 x 10$^{9}$ Msol of HI in the intra-group medium (IGM). We search for signs of pre-processing in the 12 group galaxies with c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.10347v2-abstract-full').style.display = 'inline'; document.getElementById('2101.10347v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.10347v2-abstract-full" style="display: none;"> We present MeerKAT neutral hydrogen (HI) observations of the Fornax A group, that is likely falling into the Fornax cluster for the first time. Our HI image is sensitive to 1.4 x 10$^{19}$ cm$^{-2}$ over 44.1 km s$^{-1}$, where we detect HI in 10 galaxies and a total of 1.12 x 10$^{9}$ Msol of HI in the intra-group medium (IGM). We search for signs of pre-processing in the 12 group galaxies with confirmed optical redshifts that reside within our HI image. There are 9 galaxies that show evidence of pre-processing and we classify the pre-processing status of each galaxy, according to their HI morphology and gas (atomic and molecular) scaling relations. Galaxies yet to experience pre-processing have extended HI disks, a high HI content with a H$_2$-to-HI ratio an order of magnitude lower than the median for their stellar mass. Galaxies currently being pre-processed display HI tails, truncated HI disks with typical gas ratios. Galaxies in the advanced stages of pre-processing are HI deficient. If there is any HI, they have lost their outer HI disk and efficiently converted their HI to H$_2$, resulting in H$_2$-to-HI ratios an order of magnitude higher than the median for their stellar mass. The central, massive galaxy in our group underwent a 10:1 merger 2 Gyr ago, and ejected 6.6 - 11.2 x 10$^{8}$ Msol of HI that we detect as clouds and streams in the IGM, some forming coherent structures up to 220 kpc in length. We also detect giant (100 kpc) ionised hydrogen (H$伪$) filaments in the IGM, likely from cool gas being removed (and ionised) from an infalling satellite. The H$伪$ filaments are situated within the hot halo of NGC 1316 and some regions contain HI. We speculate that the H$伪$ and multiphase gas is supported by magnetic pressure (possibly assisted by the AGN), such that the hot gas can condense and form HI that survives in the hot halo for cosmological timescales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.10347v2-abstract-full').style.display = 'none'; document.getElementById('2101.10347v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">18 pages, 9 figured. Accepted for publication in Astronomy and Astrophysics (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 648, A32 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.07822">arXiv:2101.07822</a> <span> [<a href="https://arxiv.org/pdf/2101.07822">pdf</a>, <a href="https://arxiv.org/format/2101.07822">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abde45">10.3847/1538-4357/abde45 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Census of the Extended Neutral Hydrogen Around 18 MHONGOOSE Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sardone%2C+A">Amy Sardone</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Pingel%2C+N+M">N. M. Pingel</a>, <a href="/search/astro-ph?searchtype=author&query=Sorgho%2C+A">Amidou Sorgho</a>, <a href="/search/astro-ph?searchtype=author&query=Carignan%2C+C">Claude Carignan</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</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="2101.07822v1-abstract-short" style="display: inline;"> We present the analysis of the diffuse, low column density HI environment of 18 MHONGOOSE galaxies. We obtained deep observations with the Robert C. Byrd Green Bank Telescope, and reached down to a 3sigma column density detection limit of NHI=6.3x10^{17} cm^{-2} over a 20 km/s linewidth. We analyze the environment around these galaxies, with a focus on HI gas that reaches column densities below NH… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.07822v1-abstract-full').style.display = 'inline'; document.getElementById('2101.07822v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.07822v1-abstract-full" style="display: none;"> We present the analysis of the diffuse, low column density HI environment of 18 MHONGOOSE galaxies. We obtained deep observations with the Robert C. Byrd Green Bank Telescope, and reached down to a 3sigma column density detection limit of NHI=6.3x10^{17} cm^{-2} over a 20 km/s linewidth. We analyze the environment around these galaxies, with a focus on HI gas that reaches column densities below NHI=10^{19} cm^{-2}. We calculate the total amount of HI gas in and around the galaxies revealing that nearly all of these galaxies contained excess HI outside of their disks. We quantify the amount of diffuse gas in the maps of each galaxy, defined by HI gas with column densities below 10^{19} cm^{-2}, and find a large spread in percentages of diffuse gas. However, by binning the percentage of diffuse HI into quarters, we find that the bin with the largest number of galaxies is the lowest quartile (0-25\% diffuse HI). We identified several galaxies which may be undergoing gas accretion onto the galaxy disk using multiple methods of analysis, including azimuthally averaging column densities beyond the disk, and identifying structure within our integrated intensity (Moment 0) maps. We measured HI mass outside the disks of most of our galaxies, with rising cumulative flux even at large radii. We also find a strong correlation between the fraction of diffuse gas in a galaxy and its baryonic mass, and test this correlation using both Spearman and Pearson correlation coefficients. We see evidence of a dark matter halo mass threshold of M_{halo}~10^{11.1} \msun{} in which galaxies with high fractions of diffuse HI all reside below. It is in this regime in which cold-mode accretion should dominate. Finally, we suggest a rotation velocity of v_{rot}~80 km\s as an upper threshold to find diffuse gas-dominated galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.07822v1-abstract-full').style.display = 'none'; document.getElementById('2101.07822v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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, ApJ, Jan. 1, 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.05818">arXiv:2101.05818</a> <span> [<a href="https://arxiv.org/pdf/2101.05818">pdf</a>, <a href="https://arxiv.org/ps/2101.05818">ps</a>, <a href="https://arxiv.org/format/2101.05818">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/10.1051/0004-6361/202040019">10.1051/0004-6361/202040019 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Apertif view of the OH Megamaser IRAS 10597+5926: OH 18 cm satellite lines in wide-area HI surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">Kelley M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=Roberts%2C+H">H. Roberts</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=Darling%2C+J">J. Darling</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Kutkin%2C+A">A. Kutkin</a>, <a href="/search/astro-ph?searchtype=author&query=Lucero%2C+D+M">D. M. Lucero</a>, <a href="/search/astro-ph?searchtype=author&query=Morganti%2C+R">Raffaella Morganti</a>, <a href="/search/astro-ph?searchtype=author&query=Moss%2C+V+A">V. A. Moss</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Schulz%2C+R">R. Schulz</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">A. H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=Ivashina%2C+M">M. Ivashina</a>, <a href="/search/astro-ph?searchtype=author&query=Loose%2C+G+M">G. Marcel Loose</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Yogesh Maan</a>, <a href="/search/astro-ph?searchtype=author&query=Mika%2C+%C3%81">脕. Mika</a>, <a href="/search/astro-ph?searchtype=author&query=Mulder%2C+H">H. Mulder</a>, <a href="/search/astro-ph?searchtype=author&query=Norden%2C+M+J">M. J. Norden</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L+C">L. C. Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Ruiter%2C+M">M. Ruiter</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">Joeri van Leeuwen</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2101.05818v1-abstract-short" style="display: inline;"> We present the serendipitous detection of the two main OH maser lines at 1667 and 1665 MHz associated with IRAS 10597+5926 at z = 0.19612 in the untargeted Apertif Wide-area Extragalactic Survey (AWES), and the subsequent measurement of the OH 1612 MHz satellite line in the same source. With a total OH luminosity of log(L/L_Sun) = 3.90 +/- 0.03, IRAS 10597+5926 is the fourth brightest OH megamaser… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05818v1-abstract-full').style.display = 'inline'; document.getElementById('2101.05818v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.05818v1-abstract-full" style="display: none;"> We present the serendipitous detection of the two main OH maser lines at 1667 and 1665 MHz associated with IRAS 10597+5926 at z = 0.19612 in the untargeted Apertif Wide-area Extragalactic Survey (AWES), and the subsequent measurement of the OH 1612 MHz satellite line in the same source. With a total OH luminosity of log(L/L_Sun) = 3.90 +/- 0.03, IRAS 10597+5926 is the fourth brightest OH megamaser (OHM) known. We measure a lower limit for the 1667/1612 ratio of R_1612 > 45.9 which is the highest limiting ratio measured for the 1612 MHz OH satellite line to date. OH satellite line measurements provide a potentially valuable constraint by which to compare detailed models of OH maser pumping mechanisms. Optical imaging shows the galaxy is likely a late-stage merger. Based on published infrared and far ultraviolet fluxes, we find that the galaxy is an ultra luminous infrared galaxy (ULIRG) with log(L_TIR/L_Sun) = 12.24, undergoing a star burst with an estimated star formation rate of 179 +/- 40 M_Sun/yr. These host galaxy properties are consistent with the physical conditions responsible for very bright OHM emission. Finally, we provide an update on the predicted number of OH masers that may be found in AWES, and estimate the total number of OH masers that will be detected in each of the individual main and satellite OH 18 cm lines. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05818v1-abstract-full').style.display = 'none'; document.getElementById('2101.05818v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">9 pages, 4 figures. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 647, A193 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.08348">arXiv:2012.08348</a> <span> [<a href="https://arxiv.org/pdf/2012.08348">pdf</a>, <a href="https://arxiv.org/format/2012.08348">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/10.1038/s41586-021-03724-8">10.1038/s41586-021-03724-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Chromatic periodic activity down to 120 MHz in a Fast Radio Burst </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pastor-Marazuela%2C+I">In茅s Pastor-Marazuela</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">Joeri van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Yogesh Maan</a>, <a href="/search/astro-ph?searchtype=author&query=ter+Veen%2C+S">Sander ter Veen</a>, <a href="/search/astro-ph?searchtype=author&query=Bilous%2C+A">Anna Bilous</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L">Leon Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">Emily Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Straal%2C+S">Samayra Straal</a>, <a href="/search/astro-ph?searchtype=author&query=Vohl%2C+D">Dany Vohl</a>, <a href="/search/astro-ph?searchtype=author&query=Attema%2C+J">Jisk Attema</a>, <a href="/search/astro-ph?searchtype=author&query=Boersma%2C+O+M">Oliver M. Boersma</a>, <a href="/search/astro-ph?searchtype=author&query=Kooistra%2C+E">Eric Kooistra</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Schuur%2C+D">Daniel van der Schuur</a>, <a href="/search/astro-ph?searchtype=author&query=Sclocco%2C+A">Alessio Sclocco</a>, <a href="/search/astro-ph?searchtype=author&query=Smits%2C+R">Roy Smits</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">Elizabeth A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">Bj枚rn Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">Willem J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">Arthur H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">Sieds Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">Helga D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">Kelley M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+T">Thijs van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=Hut%2C+B">Boudewijn Hut</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.08348v1-abstract-short" style="display: inline;"> Fast radio bursts (FRBs) are extragalactic astrophysical transients whose brightness requires emitters that are highly energetic, yet compact enough to produce the short, millisecond-duration bursts. FRBs have thus far been detected between 300 MHz and 8 GHz, but lower-frequency emission has remained elusive. A subset of FRBs is known to repeat, and one of those sources, FRB 20180916B, does so wit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.08348v1-abstract-full').style.display = 'inline'; document.getElementById('2012.08348v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.08348v1-abstract-full" style="display: none;"> Fast radio bursts (FRBs) are extragalactic astrophysical transients whose brightness requires emitters that are highly energetic, yet compact enough to produce the short, millisecond-duration bursts. FRBs have thus far been detected between 300 MHz and 8 GHz, but lower-frequency emission has remained elusive. A subset of FRBs is known to repeat, and one of those sources, FRB 20180916B, does so with a 16.3 day activity period. Using simultaneous Apertif and LOFAR data, we show that FRB 20180916B emits down to 120 MHz, and that its activity window is both narrower and earlier at higher frequencies. Binary wind interaction models predict a narrower periodic activity window at lower frequencies, which is the opposite of our observations. Our detections establish that low-frequency FRB emission can escape the local medium. For bursts of the same fluence, FRB 20180916B is more active below 200 MHz than at 1.4 GHz. Combining our results with previous upper-limits on the all-sky FRB rate at 150 MHz, we find that there are 3-450 FRBs/sky/day above 50 Jy ms at 90% confidence. We are able to rule out the scenario in which companion winds cause FRB periodicity. We also demonstrate that some FRBs live in clean environments that do not absorb or scatter low-frequency radiation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.08348v1-abstract-full').style.display = 'none'; document.getElementById('2012.08348v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">50 pages, 14 figures, 3 tables, submitted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.01751">arXiv:2012.01751</a> <span> [<a href="https://arxiv.org/pdf/2012.01751">pdf</a>, <a href="https://arxiv.org/format/2012.01751">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/staa3770">10.1093/mnras/staa3770 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Anomalous gas in ESO 149-G003: A MeerKAT-16 View </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">Gyula I. G. J贸zsa</a>, <a href="/search/astro-ph?searchtype=author&query=Thorat%2C+K">Kshitij Thorat</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">Peter Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Sebokolodi%2C+L">Lerato Sebokolodi</a>, <a href="/search/astro-ph?searchtype=author&query=Maina%2C+E+K">Eric K. Maina</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+J">Jing Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Pieterse%2C+D+L+A">Dani毛lle L. A. Pieterse</a>, <a href="/search/astro-ph?searchtype=author&query=Groot%2C+P">Paul Groot</a>, <a href="/search/astro-ph?searchtype=author&query=Ramaila%2C+A+J+T">Athanaseus J. T. Ramaila</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">Paolo Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Andati%2C+L+A+L">Lexy A. L. Andati</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Hugo%2C+B+V">Benjamin V. Hugo</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">Dane Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">Filippo M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Makhathini%2C+S">Sphesihle Makhathini</a>, <a href="/search/astro-ph?searchtype=author&query=Moln%C3%A1r%2C+D+C">D谩niel Cs. Moln谩r</a>, <a href="/search/astro-ph?searchtype=author&query=Ramatsoku%2C+M">Mpati Ramatsoku</a>, <a href="/search/astro-ph?searchtype=author&query=Smirnov%2C+O+M">Oleg M. Smirnov</a>, <a href="/search/astro-ph?searchtype=author&query=Bloemen%2C+S">Steven Bloemen</a>, <a href="/search/astro-ph?searchtype=author&query=Paterson%2C+K">Kerry Paterson</a>, <a href="/search/astro-ph?searchtype=author&query=Vreeswijk%2C+P">Paul Vreeswijk</a>, <a href="/search/astro-ph?searchtype=author&query=McBride%2C+V">Vanessa McBride</a>, <a href="/search/astro-ph?searchtype=author&query=Klein-Wolt%2C+M">Marc Klein-Wolt</a>, <a href="/search/astro-ph?searchtype=author&query=Woudt%2C+P">Patrick Woudt</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="2012.01751v2-abstract-short" style="display: inline;"> ESO 149-G003 is a close-by, isolated dwarf irregular galaxy. Previous observations with the ATCA indicated the presence of anomalous neutral hydrogen (HI) deviating from the kinematics of a regularly rotating disc. We conducted follow-up observations with the MeerKAT radio telescope during the 16-dish Early Science programme as well as with the MeerLICHT optical telescope. Our more sensitive radio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.01751v2-abstract-full').style.display = 'inline'; document.getElementById('2012.01751v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.01751v2-abstract-full" style="display: none;"> ESO 149-G003 is a close-by, isolated dwarf irregular galaxy. Previous observations with the ATCA indicated the presence of anomalous neutral hydrogen (HI) deviating from the kinematics of a regularly rotating disc. We conducted follow-up observations with the MeerKAT radio telescope during the 16-dish Early Science programme as well as with the MeerLICHT optical telescope. Our more sensitive radio observations confirm the presence of anomalous gas in ESO 149-G003, and further confirm the formerly tentative detection of an extraplanar HI component in the galaxy. Employing a simple tilted-ring model, in which the kinematics is determined with only four parameters but including morphological asymmetries, we reproduce the galaxy's morphology, which shows a high degree of asymmetry. By comparing our model with the observed HI, we find that in our model we cannot account for a significant (but not dominant) fraction of the gas. From the differences between our model and the observed data cube we estimate that at least 7%-8% of the HI in the galaxy exhibits anomalous kinematics, while we estimate a minimum mass fraction of less than 1% for the morphologically confirmed extraplanar component. We investigate a number of global scaling relations and find that, besides being gas-dominated with a neutral gas-to-stellar mass ratio of 1.7, the galaxy does not show any obvious global peculiarities. Given its isolation, as confirmed by optical observations, we conclude that the galaxy is likely currently acquiring neutral gas. It is either re-accreting gas expelled from the galaxy or accreting pristine intergalactic material. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.01751v2-abstract-full').style.display = 'none'; document.getElementById('2012.01751v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 14 figures, MNRAS, Accepted 2020 December 2, in original form 2019 September 18</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.08239">arXiv:2011.08239</a> <span> [<a href="https://arxiv.org/pdf/2011.08239">pdf</a>, <a href="https://arxiv.org/format/2011.08239">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/10.1051/0004-6361/202039102">10.1051/0004-6361/202039102 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The best of both worlds: Combining LOFAR and Apertif to derive resolved radio spectral index images </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morganti%2C+R">R. Morganti</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Brienza%2C+M">M. Brienza</a>, <a href="/search/astro-ph?searchtype=author&query=Jurlin%2C+N">N. Jurlin</a>, <a href="/search/astro-ph?searchtype=author&query=Prandoni%2C+I">I. Prandoni</a>, <a href="/search/astro-ph?searchtype=author&query=Orru%27%2C+E">E. Orru'</a>, <a href="/search/astro-ph?searchtype=author&query=Shabala%2C+S+S">S. S. Shabala</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=Best%2C+P+N">P. N. Best</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">A. H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</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=Denes%2C+H">H. Denes</a>, <a href="/search/astro-ph?searchtype=author&query=Hardcastle%2C+M">M. Hardcastle</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">K. M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=Hut%2C+B">B. Hut</a>, <a href="/search/astro-ph?searchtype=author&query=Kondapally%2C+R">R. Kondapally</a>, <a href="/search/astro-ph?searchtype=author&query=Kutkin%2C+A+M">A. M. Kutkin</a>, <a href="/search/astro-ph?searchtype=author&query=Loose%2C+G+M">G. M. Loose</a>, <a href="/search/astro-ph?searchtype=author&query=Lucero%2C+D+M">D. M. Lucero</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Y. Maan</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Mingo%2C+B">B. Mingo</a> , et al. (14 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="2011.08239v1-abstract-short" style="display: inline;"> Supermassive black holes at the centres of galaxies can cycle through periods of activity and quiescence. Characterising the duty cycle of active galactic nuclei is crucial for understanding the impact of the energy they release on the host galaxy. For radio AGN, this can be done by identifying dying (remnant) and restarted radio galaxies from their radio spectral properties. Using the combination… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.08239v1-abstract-full').style.display = 'inline'; document.getElementById('2011.08239v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.08239v1-abstract-full" style="display: none;"> Supermassive black holes at the centres of galaxies can cycle through periods of activity and quiescence. Characterising the duty cycle of active galactic nuclei is crucial for understanding the impact of the energy they release on the host galaxy. For radio AGN, this can be done by identifying dying (remnant) and restarted radio galaxies from their radio spectral properties. Using the combination of images at 1400 MHz produced by Apertif, the new phased-array feed receiver installed on the Westerbork Synthesis Radio Telescope, and images at 150 MHz provided by LOFAR, we have derived resolved spectral index images (at a resolution of ~15 arcsec) for all the sources within ~6 deg^2 area of the Lockman Hole region. We were able to select 15 extended radio sources with emission (partly or entirely) characterised by extremely steep spectral indices (steeper than 1.2). These objects represent radio sources in the remnant or the restarted phases of their life cycle. Our findings suggest this cycle to be relatively fast. They also show a variety of properties relevant for modelling the evolution of radio galaxies. For example, the restarted activity can occur while the remnant structure from a previous phase of activity is still visible. This provides constraints on the duration of the 'off' (dying) phase. In extended remnants with ultra-steep spectra at low frequencies, the activity likely stopped a few hundred megayears ago, and they correspond to the older tail of the age distribution of radio galaxies, in agreement with simulations of radio source evolution. We find remnant radio sources with a variety of structures (from double-lobed to amorphous), suggesting different types of progenitors. The present work sets the stage for exploiting low-frequency spectral index studies of extended sources by taking advantage of the large areas common to the LOFAR and the Apertif surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.08239v1-abstract-full').style.display = 'none'; document.getElementById('2011.08239v1-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, 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">Accepted for publication in A&A. This paper is part of the 1st data release of the LoTSS Deep Fields. 17 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.09766">arXiv:2009.09766</a> <span> [<a href="https://arxiv.org/pdf/2009.09766">pdf</a>, <a href="https://arxiv.org/format/2009.09766">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/10.1051/0004-6361/202038894">10.1051/0004-6361/202038894 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MeerKAT HI commissioning observations of MHONGOOSE galaxy ESO 302-G014 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Athanassoula%2C+E">E. Athanassoula</a>, <a href="/search/astro-ph?searchtype=author&query=Bosma%2C+A">A. Bosma</a>, <a href="/search/astro-ph?searchtype=author&query=Combes%2C+F">F. Combes</a>, <a href="/search/astro-ph?searchtype=author&query=English%2C+J">J. English</a>, <a href="/search/astro-ph?searchtype=author&query=Heald%2C+G+H">G. H. Heald</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Meurer%2C+G+R">G. R. Meurer</a>, <a href="/search/astro-ph?searchtype=author&query=Rom%C3%A1n%2C+J">J. Rom谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Sardone%2C+A">A. Sardone</a>, <a href="/search/astro-ph?searchtype=author&query=Verdes-Montenegro%2C+L">L. Verdes-Montenegro</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Brinks%2C+E">E. Brinks</a>, <a href="/search/astro-ph?searchtype=author&query=Chemin%2C+L">L. Chemin</a>, <a href="/search/astro-ph?searchtype=author&query=Fraternali%2C+F">F. Fraternali</a>, <a href="/search/astro-ph?searchtype=author&query=Jarrett%2C+T">T. Jarrett</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">P. Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Spekkens%2C+K">K. Spekkens</a>, <a href="/search/astro-ph?searchtype=author&query=Amram%2C+P">P. Amram</a>, <a href="/search/astro-ph?searchtype=author&query=Carignan%2C+C">C. Carignan</a>, <a href="/search/astro-ph?searchtype=author&query=Dettmar%2C+R">R-J. Dettmar</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="2009.09766v1-abstract-short" style="display: inline;"> We present the results of three commissioning HI observations obtained with the MeerKAT radio telescope. These observations make up part of the preparation for the forthcoming MHONGOOSE nearby galaxy survey, which is a MeerKAT large survey project that will study the accretion of gas in galaxies and the link between gas and star formation. We used the available HI data sets, along with ancillary d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.09766v1-abstract-full').style.display = 'inline'; document.getElementById('2009.09766v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.09766v1-abstract-full" style="display: none;"> We present the results of three commissioning HI observations obtained with the MeerKAT radio telescope. These observations make up part of the preparation for the forthcoming MHONGOOSE nearby galaxy survey, which is a MeerKAT large survey project that will study the accretion of gas in galaxies and the link between gas and star formation. We used the available HI data sets, along with ancillary data at other wavelengths, to study the morphology of the MHONGOOSE sample galaxy, ESO 302-G014, which is a nearby gas-rich dwarf galaxy. We find that ESO 302-G014 has a lopsided, asymmetric outer disc with a low column density. In addition, we find a tail or filament of HI clouds extending away from the galaxy, as well as an isolated HI cloud some 20 kpc to the south of the galaxy. We suggest that these features indicate a minor interaction with a low-mass galaxy. Optical imaging shows a possible dwarf galaxy near the tail, but based on the current data, we cannot confirm any association with ESO 302-G014. Nonetheless, an interaction scenario with some kind of low-mass companion is still supported by the presence of a significant amount of molecular gas, which is almost equal to the stellar mass, and a number of prominent stellar clusters, which suggest recently triggered star formation. These data show that MeerKAT produces exquisite imaging data. The forthcoming full-depth survey observations of ESO 302-G014 and other sample galaxies will, therefore, offer insights into the fate of neutral gas as it moves from the intergalactic medium onto galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.09766v1-abstract-full').style.display = 'none'; document.getElementById('2009.09766v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 643, A147 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.07945">arXiv:2008.07945</a> <span> [<a href="https://arxiv.org/pdf/2008.07945">pdf</a>, <a href="https://arxiv.org/format/2008.07945">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202038378">10.1051/0004-6361/202038378 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extreme intra-hour variability of the radio source J1402+5347 discovered with Apertif </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T+A">T. A. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Vedantham%2C+H+K">H. K. Vedantham</a>, <a href="/search/astro-ph?searchtype=author&query=Kutkin%2C+A+M">A. M. Kutkin</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">A. H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=De%27nes%2C+H">H. De'nes</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+K+M">K. M. Hess</a>, <a href="/search/astro-ph?searchtype=author&query=Hut%2C+B">B. Hut</a>, <a href="/search/astro-ph?searchtype=author&query=Loose%2C+G+M">G. M. Loose</a>, <a href="/search/astro-ph?searchtype=author&query=Lucero%2C+D+M">D. M. Lucero</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Y. Maan</a>, <a href="/search/astro-ph?searchtype=author&query=Morganti%2C+R">R. Morganti</a>, <a href="/search/astro-ph?searchtype=author&query=Moss%2C+V+A">V. A. Moss</a>, <a href="/search/astro-ph?searchtype=author&query=Mulder%2C+H">H. Mulder</a>, <a href="/search/astro-ph?searchtype=author&query=Norden%2C+M+J">M. J. Norden</a>, <a href="/search/astro-ph?searchtype=author&query=Offringa%2C+A+R">A. R. Offringa</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L+C">L. C. Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Orru%60%2C+E">E. Orru`</a>, <a href="/search/astro-ph?searchtype=author&query=Ruiter%2C+M">M. Ruiter</a>, <a href="/search/astro-ph?searchtype=author&query=Schulz%2C+R">R. Schulz</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+R+H+v+d">R. H. van den Brink</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a> , et al. (5 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="2008.07945v1-abstract-short" style="display: inline;"> The propagation of radio waves from distant compact radio sources through turbulent interstellar plasma in our Galaxy causes these sources to twinkle, a phenomenon called interstellar scintillation. Such scintillations are a unique probe of the micro-arcsecond structure of radio sources as well as of the sub-AU-scale structure of the Galactic interstellar medium. Weak scintillations (i.e. an inten… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.07945v1-abstract-full').style.display = 'inline'; document.getElementById('2008.07945v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.07945v1-abstract-full" style="display: none;"> The propagation of radio waves from distant compact radio sources through turbulent interstellar plasma in our Galaxy causes these sources to twinkle, a phenomenon called interstellar scintillation. Such scintillations are a unique probe of the micro-arcsecond structure of radio sources as well as of the sub-AU-scale structure of the Galactic interstellar medium. Weak scintillations (i.e. an intensity modulation of a few percent) on timescales of a few days or longer are commonly seen at centimetre wavelengths and are thought to result from the line-of-sight integrated turbulence in the interstellar plasma of the Milky Way. So far, only three sources were known that show more extreme variations, with modulations at the level of some dozen percent on timescales shorter than an hour. This requires propagation through nearby (d <~10 pc) anomalously dense (n_e ~10^2 cm^-3) plasma clouds. Here we report the discovery with Apertif of a source (J1402+5347) showing extreme (~50%) and rapid variations on a timescale of just 6.5 minutes in the decimetre band (1.4 GHz). The spatial scintillation pattern is highly anisotropic, with a semi-minor axis of about 20,000 km. The canonical theory of refractive scintillation constrains the scattering plasma to be within the Oort cloud. The sightline to J1402+5347, however, passes unusually close to the B3 star Alkaid (eta UMa) at a distance of 32 pc. If the scintillations are associated with Alkaid, then the angular size of J1402+5347 along the minor axis of the scintels must be smaller than ~10 micro arcsec yielding an apparent brightness temperature for an isotropic source of >~ 10^ 14K. } <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.07945v1-abstract-full').style.display = 'none'; document.getElementById('2008.07945v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for Astronomy and Astrophysics Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.01292">arXiv:2007.01292</a> <span> [<a href="https://arxiv.org/pdf/2007.01292">pdf</a>, <a href="https://arxiv.org/format/2007.01292">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/staa1967">10.1093/mnras/staa1967 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> MeerKAT-16 HI observation of the dIrr galaxy WLM </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ianjamasimanana%2C+R">Roger Ianjamasimanana</a>, <a href="/search/astro-ph?searchtype=author&query=Namumba%2C+B">Brenda Namumba</a>, <a href="/search/astro-ph?searchtype=author&query=Ramaila%2C+A+J+T">Athanaseus J. T. Ramaila</a>, <a href="/search/astro-ph?searchtype=author&query=Saburova%2C+A+S">Anna S. Saburova</a>, <a href="/search/astro-ph?searchtype=author&query=Jozsa%2C+G+I+G">Gyula I. G. Jozsa</a>, <a href="/search/astro-ph?searchtype=author&query=Myburgh%2C+T">Talon Myburgh</a>, <a href="/search/astro-ph?searchtype=author&query=Thorat%2C+K">Kshitij Thorat</a>, <a href="/search/astro-ph?searchtype=author&query=Carignan%2C+C">Claude Carignan</a>, <a href="/search/astro-ph?searchtype=author&query=Maina%2C+E">Eric Maina</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Andati%2C+L+A+L">Lexy A. L. Andati</a>, <a href="/search/astro-ph?searchtype=author&query=Hugo%2C+B+V">Benjamin V. Hugo</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">Dane Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">Peter Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">Paolo Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Smirnov%2C+O+M">Oleg M. Smirnov</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">Filippo M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Makhathini%2C+S">Sphesihle Makhathini</a>, <a href="/search/astro-ph?searchtype=author&query=Molnar%2C+D+C">Daniel Cs. Molnar</a>, <a href="/search/astro-ph?searchtype=author&query=Perkins%2C+S">Simon Perkins</a>, <a href="/search/astro-ph?searchtype=author&query=Ramatsoku%2C+M">Mpati Ramatsoku</a>, <a href="/search/astro-ph?searchtype=author&query=White%2C+S+V">Sarah V. White</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="2007.01292v1-abstract-short" style="display: inline;"> We present observations and models of the kinematics and the distribution of the neutral hydrogen (HI) in the isolated dwarf irregular galaxy, Wolf-Lundmark-Melotte (WLM). We observed WLM with the Green Bank Telescope (GBT) and as part of the MeerKAT Early Science Programme, where 16 dishes were available. The HI disc of WLM extends out to a major axis diameter of 30 arcmin (8.5 kpc), and a minor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.01292v1-abstract-full').style.display = 'inline'; document.getElementById('2007.01292v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.01292v1-abstract-full" style="display: none;"> We present observations and models of the kinematics and the distribution of the neutral hydrogen (HI) in the isolated dwarf irregular galaxy, Wolf-Lundmark-Melotte (WLM). We observed WLM with the Green Bank Telescope (GBT) and as part of the MeerKAT Early Science Programme, where 16 dishes were available. The HI disc of WLM extends out to a major axis diameter of 30 arcmin (8.5 kpc), and a minor axis diameter of 20 arcmin (5.6 kpc) as measured by the GBT. We use the MeerKAT data to model WLM using the TiRiFiC software suite, allowing us to fit different tilted-ring models and select the one that best matches the observation. Our final best-fitting model is a flat disc with a vertical thickness, a constant inclination and dispersion, and a radially-varying surface brightness with harmonic distortions. To simulate bar-like motions, we include second-order harmonic distortions in velocity in the tangential and the vertical directions. We present a model with only circular motions included and a model with non-circular motions. The latter describes the data better. Overall, the models reproduce the global distribution and the kinematics of the gas, except for some faint emission at the 2-sigma level. We model the mass distribution of WLM with a pseudo-isothermal (ISO) and a Navarro-Frenk-White (NFW) dark matter halo models. The NFW and the ISO models fit the derived rotation curves within the formal errors, but with the ISO model giving better reduced chi-square values. The mass distribution in WLM is dominated by dark matter at all radii. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.01292v1-abstract-full').style.display = 'none'; document.getElementById('2007.01292v1-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 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS, 25 pages, 21 figures, 5 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/2006.02955">arXiv:2006.02955</a> <span> [<a href="https://arxiv.org/pdf/2006.02955">pdf</a>, <a href="https://arxiv.org/ps/2006.02955">ps</a>, <a href="https://arxiv.org/format/2006.02955">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> <p class="title is-5 mathjax"> MeerKATHI -- an end-to-end data reduction pipeline for MeerKAT and other radio telescopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">Gyula I. G. J贸zsa</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=Thorat%2C+K">Kshitij Thorat</a>, <a href="/search/astro-ph?searchtype=author&query=Smirnov%2C+O+M">Oleg M. Smirnov</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">Paolo Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Ramatsoku%2C+M">Mpati Ramatsoku</a>, <a href="/search/astro-ph?searchtype=author&query=Ramaila%2C+A+J+T">Athanaseus J. T. Ramaila</a>, <a href="/search/astro-ph?searchtype=author&query=Perkins%2C+S+J">Simon J. Perkins</a>, <a href="/search/astro-ph?searchtype=author&query=Moln%C3%A1r%2C+D+C">D谩niel Cs. Moln谩r</a>, <a href="/search/astro-ph?searchtype=author&query=Makhathini%2C+S">Sphesihle Makhathini</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">Filippo M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">Dane Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">Peter Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Hugo%2C+B+V">Benjamin V. Hugo</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Andati%2C+L+A+L">Lexy A. L. Andati</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="2006.02955v2-abstract-short" style="display: inline;"> MeerKATHI is the current development name for a radio-interferometric data reduction pipeline, assembled by an international collaboration. We create a publicly available end-to-end continuum- and line imaging pipeline for MeerKAT and other radio telescopes. We implement advanced techniques that are suitable for producing high-dynamic-range continuum images and spectroscopic data cubes. Using cont… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.02955v2-abstract-full').style.display = 'inline'; document.getElementById('2006.02955v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2006.02955v2-abstract-full" style="display: none;"> MeerKATHI is the current development name for a radio-interferometric data reduction pipeline, assembled by an international collaboration. We create a publicly available end-to-end continuum- and line imaging pipeline for MeerKAT and other radio telescopes. We implement advanced techniques that are suitable for producing high-dynamic-range continuum images and spectroscopic data cubes. Using containerization, our pipeline is platform-independent. Furthermore, we are applying a standardized approach for using a number of different of advanced software suites, partly developed within our group. We aim to use distributed computing approaches throughout our pipeline to enable the user to reduce larger data sets like those provided by radio telescopes such as MeerKAT. The pipeline also delivers a set of imaging quality metrics that give the user the opportunity to efficiently assess the data quality. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2006.02955v2-abstract-full').style.display = 'none'; document.getElementById('2006.02955v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 1 figure, in conference proceedings of the ADASS XXIX, to appear in ASPC. CARACal (formerly MeerKATHI) can be accessed at: https://caracal.readthedocs.io</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.07311">arXiv:2002.07311</a> <span> [<a href="https://arxiv.org/pdf/2002.07311">pdf</a>, <a href="https://arxiv.org/format/2002.07311">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1007/s10509-020-03831-4">10.1007/s10509-020-03831-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> WALLABY -- An SKA Pathfinder HI Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Koribalski%2C+B+S">B. S. Koribalski</a>, <a href="/search/astro-ph?searchtype=author&query=Staveley-Smith%2C+L">L. Staveley-Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Westmeier%2C+T">T. Westmeier</a>, <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">P. Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Spekkens%2C+K">K. Spekkens</a>, <a href="/search/astro-ph?searchtype=author&query=Wong%2C+O+I">O. I. Wong</a>, <a href="/search/astro-ph?searchtype=author&query=Lagos%2C+C+D+P">C. D. P. Lagos</a>, <a href="/search/astro-ph?searchtype=author&query=Obreschkow%2C+D">D. Obreschkow</a>, <a href="/search/astro-ph?searchtype=author&query=Ryan-Weber%2C+E+V">E. V. Ryan-Weber</a>, <a href="/search/astro-ph?searchtype=author&query=Zwaan%2C+M">M. Zwaan</a>, <a href="/search/astro-ph?searchtype=author&query=Kilborn%2C+V">V. Kilborn</a>, <a href="/search/astro-ph?searchtype=author&query=Bekiaris%2C+G">G. Bekiaris</a>, <a href="/search/astro-ph?searchtype=author&query=Bekki%2C+K">K. Bekki</a>, <a href="/search/astro-ph?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/astro-ph?searchtype=author&query=Boselli%2C+A">A. Boselli</a>, <a href="/search/astro-ph?searchtype=author&query=Bosma%2C+A">A. Bosma</a>, <a href="/search/astro-ph?searchtype=author&query=Catinella%2C+B">B. Catinella</a>, <a href="/search/astro-ph?searchtype=author&query=Chauhan%2C+G">G. Chauhan</a>, <a href="/search/astro-ph?searchtype=author&query=Cluver%2C+M+E">M. E. Cluver</a>, <a href="/search/astro-ph?searchtype=author&query=Colless%2C+M">M. Colless</a>, <a href="/search/astro-ph?searchtype=author&query=Courtois%2C+H+M">H. M. Courtois</a>, <a href="/search/astro-ph?searchtype=author&query=Crain%2C+R+A">R. A. Crain</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Duffy%2C+A+R">A. R. Duffy</a> , et al. (45 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="2002.07311v2-abstract-short" style="display: inline;"> The Widefield ASKAP L-band Legacy All-sky Blind surveY (WALLABY) is a next-generation survey of neutral hydrogen (HI) in the Local Universe. It uses the widefield, high-resolution capability of the Australian Square Kilometer Array Pathfinder (ASKAP), a radio interferometer consisting of 36 x 12-m dishes equipped with Phased-Array Feeds (PAFs), located in an extremely radio-quiet zone in Western A… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.07311v2-abstract-full').style.display = 'inline'; document.getElementById('2002.07311v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.07311v2-abstract-full" style="display: none;"> The Widefield ASKAP L-band Legacy All-sky Blind surveY (WALLABY) is a next-generation survey of neutral hydrogen (HI) in the Local Universe. It uses the widefield, high-resolution capability of the Australian Square Kilometer Array Pathfinder (ASKAP), a radio interferometer consisting of 36 x 12-m dishes equipped with Phased-Array Feeds (PAFs), located in an extremely radio-quiet zone in Western Australia. WALLABY aims to survey three-quarters of the sky (-90 degr < Dec < +30 degr) to a redshift of z < 0.26, and generate spectral line image cubes at ~30 arcsec resolution and ~1.6 mJy/beam per 4 km/s channel sensitivity. ASKAP's instantaneous field of view at 1.4 GHz, delivered by the PAF's 36 beams, is about 30 sq deg. At an integrated signal-to-noise ratio of five, WALLABY is expected to detect over half a million galaxies with a mean redshift of z ~ 0.05 (~200 Mpc). The scientific goals of WALLABY include: (a) a census of gas-rich galaxies in the vicinity of the Local Group; (b) a study of the HI properties of galaxies, groups and clusters, in particular the influence of the environment on galaxy evolution; and (c) the refinement of cosmological parameters using the spatial and redshift distribution of low-bias gas-rich galaxies. For context we provide an overview of previous large-scale HI surveys. Combined with existing and new multi-wavelength sky surveys, WALLABY will enable an exciting new generation of panchromatic studies of the Local Universe. - First results from the WALLABY pilot survey are revealed, with initial data products publicly available in the CSIRO ASKAP Science Data Archive (CASDA). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.07311v2-abstract-full').style.display = 'none'; document.getElementById('2002.07311v2-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApSS (38 pages, 14 figures), see also https://www.atnf.csiro.au/research/WALLABY/ - Contact email: Baerbel.Koribalski@csiro.au</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Ap&SS 365, 118 (2020) - https://rdcu.be/b5Bfg </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.01399">arXiv:2002.01399</a> <span> [<a href="https://arxiv.org/pdf/2002.01399">pdf</a>, <a href="https://arxiv.org/format/2002.01399">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/staa3009">10.1093/mnras/staa3009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A bright, high rotation-measure FRB that skewers the M33 halo </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">Liam Connor</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">Joeri van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L+C">L. C. Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Yogesh Maan</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Attema%2C+J+J">J. J. Attema</a>, <a href="/search/astro-ph?searchtype=author&query=Bast%2C+J+E">J. E. Bast</a>, <a href="/search/astro-ph?searchtype=author&query=Boersma%2C+O+M">O. M. Boersma</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%A9nes%2C+H">H. D茅nes</a>, <a href="/search/astro-ph?searchtype=author&query=Gardenier%2C+D+W">D. W. Gardenier</a>, <a href="/search/astro-ph?searchtype=author&query=Hargreaves%2C+J+E">J. E. Hargreaves</a>, <a href="/search/astro-ph?searchtype=author&query=Kooistra%2C+E">E. Kooistra</a>, <a href="/search/astro-ph?searchtype=author&query=Pastor-Marazuela%2C+I">I. Pastor-Marazuela</a>, <a href="/search/astro-ph?searchtype=author&query=Schulz%2C+R">R. Schulz</a>, <a href="/search/astro-ph?searchtype=author&query=Sclocco%2C+A">A. Sclocco</a>, <a href="/search/astro-ph?searchtype=author&query=Smits%2C+R">R. Smits</a>, <a href="/search/astro-ph?searchtype=author&query=Straal%2C+S+M">S. M. Straal</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Schuur%2C+D">D. van der Schuur</a>, <a href="/search/astro-ph?searchtype=author&query=Vohl%2C+D">Dany Vohl</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">W. A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">A. H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a> , et al. (15 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2002.01399v2-abstract-short" style="display: inline;"> We report the detection of a bright fast radio burst, FRB\,191108, with Apertif on the Westerbork Synthesis Radio Telescope (WSRT). The interferometer allows us to localise the FRB to a narrow $5\arcsec\times7\arcmin$ ellipse by employing both multibeam information within the Apertif phased-array feed (PAF) beam pattern, and across different tied-array beams. The resulting sight line passes close… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.01399v2-abstract-full').style.display = 'inline'; document.getElementById('2002.01399v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.01399v2-abstract-full" style="display: none;"> We report the detection of a bright fast radio burst, FRB\,191108, with Apertif on the Westerbork Synthesis Radio Telescope (WSRT). The interferometer allows us to localise the FRB to a narrow $5\arcsec\times7\arcmin$ ellipse by employing both multibeam information within the Apertif phased-array feed (PAF) beam pattern, and across different tied-array beams. The resulting sight line passes close to Local Group galaxy M33, with an impact parameter of only 18\,kpc with respect to the core. It also traverses the much larger circumgalactic medium of M31, the Andromeda Galaxy. We find that the shared plasma of the Local Group galaxies could contribute $\sim$10\% of its dispersion measure of 588\,pc\,cm$^{-3}$. FRB\,191108 has a Faraday rotation measure of +474\,$\pm\,3$\,rad\,m$^{-2}$, which is too large to be explained by either the Milky Way or the intergalactic medium. Based on the more moderate RMs of other extragalactic sources that traverse the halo of M33, we conclude that the dense magnetised plasma resides in the host galaxy. The FRB exhibits frequency structure on two scales, one that is consistent with quenched Galactic scintillation and broader spectral structure with $螖谓\approx40$\,MHz. If the latter is due to scattering in the shared M33/M31 CGM, our results constrain the Local Group plasma environment. We found no accompanying persistent radio sources in the Apertif imaging survey data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.01399v2-abstract-full').style.display = 'none'; document.getElementById('2002.01399v2-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 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.12217">arXiv:1912.12217</a> <span> [<a href="https://arxiv.org/pdf/1912.12217">pdf</a>, <a href="https://arxiv.org/format/1912.12217">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201937422">10.1051/0004-6361/201937422 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Repeating fast radio bursts with WSRT/Apertif </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Oostrum%2C+L+C">L. C. Oostrum</a>, <a href="/search/astro-ph?searchtype=author&query=Maan%2C+Y">Y. Maan</a>, <a href="/search/astro-ph?searchtype=author&query=van+Leeuwen%2C+J">J. van Leeuwen</a>, <a href="/search/astro-ph?searchtype=author&query=Connor%2C+L">L. Connor</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+E">E. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Attema%2C+J+J">J. J. Attema</a>, <a href="/search/astro-ph?searchtype=author&query=Bast%2C+J+E">J. E. Bast</a>, <a href="/search/astro-ph?searchtype=author&query=Gardenier%2C+D+W">D. W. Gardenier</a>, <a href="/search/astro-ph?searchtype=author&query=Hargreaves%2C+J+E">J. E. Hargreaves</a>, <a href="/search/astro-ph?searchtype=author&query=Kooistra%2C+E">E. Kooistra</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Schuur%2C+D">D. van der Schuur</a>, <a href="/search/astro-ph?searchtype=author&query=Sclocco%2C+A">A. Sclocco</a>, <a href="/search/astro-ph?searchtype=author&query=Smits%2C+R">R. Smits</a>, <a href="/search/astro-ph?searchtype=author&query=Straal%2C+S+M">S. M. Straal</a>, <a href="/search/astro-ph?searchtype=author&query=ter+Veen%2C+S">S. ter Veen</a>, <a href="/search/astro-ph?searchtype=author&query=Vohl%2C+D">D. Vohl</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+E+A+K">E. A. K. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Adebahr%2C+B">B. Adebahr</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Brink%2C+R+H+v+d">R. H. van den Brink</a>, <a href="/search/astro-ph?searchtype=author&query=van+Cappellen%2C+W+A">W. A. van Cappellen</a>, <a href="/search/astro-ph?searchtype=author&query=Coolen%2C+A+H+W+M">A. H. W. M. Coolen</a>, <a href="/search/astro-ph?searchtype=author&query=Damstra%2C+S">S. Damstra</a>, <a href="/search/astro-ph?searchtype=author&query=van+Diepen%2C+G+N+J">G. N. J. van Diepen</a>, <a href="/search/astro-ph?searchtype=author&query=Frank%2C+B+S">B. S. Frank</a> , et al. (18 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="1912.12217v2-abstract-short" style="display: inline;"> Repeating fast radio bursts (FRBs) present excellent opportunities to identify FRB progenitors and host environments, as well as decipher the underlying emission mechanism. Detailed studies of repeating FRBs might also hold clues to the origin of FRBs as a population. We aim to detect the first two repeating FRBs: FRB 121102 (R1) and FRB 180814.J0422+73 (R2), and characterise their repeat statisti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.12217v2-abstract-full').style.display = 'inline'; document.getElementById('1912.12217v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.12217v2-abstract-full" style="display: none;"> Repeating fast radio bursts (FRBs) present excellent opportunities to identify FRB progenitors and host environments, as well as decipher the underlying emission mechanism. Detailed studies of repeating FRBs might also hold clues to the origin of FRBs as a population. We aim to detect the first two repeating FRBs: FRB 121102 (R1) and FRB 180814.J0422+73 (R2), and characterise their repeat statistics. We also want to significantly improve the sky localisation of R2. We use the Westerbork Synthesis Radio Telescope to conduct extensive follow-up of these two repeating FRBs. The new phased-array feed system, Apertif, allows covering the entire sky position uncertainty of R2 with fine spatial resolution in one pointing. We characterise the energy distribution and the clustering of detected R1 bursts. We detected 30 bursts from R1. Our measurements indicate a dispersion measure of 563.5(2) pc cm$^{-3}$, suggesting a significant increase in DM over the past few years. We place an upper limit of 8% on the linear polarisation fraction of the brightest burst. We did not detect any bursts from R2. A single power-law might not fit the R1 burst energy distribution across the full energy range or widely separated detections. Our observations provide improved constraints on the clustering of R1 bursts. Our stringent upper limits on the linear polarisation fraction imply a significant depolarisation, either intrinsic to the emission mechanism or caused by the intervening medium, at 1400 MHz that is not observed at higher frequencies. The non-detection of any bursts from R2 implies either a highly clustered nature of the bursts, a steep spectral index, or a combination of both. Alternatively, R2 has turned off completely, either permanently or for an extended period of time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.12217v2-abstract-full').style.display = 'none'; document.getElementById('1912.12217v2-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 January, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">11 pages, 7 figures, submitted to 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 635, A61 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.04048">arXiv:1909.04048</a> <span> [<a href="https://arxiv.org/pdf/1909.04048">pdf</a>, <a href="https://arxiv.org/format/1909.04048">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/10.1051/0004-6361/201936338">10.1051/0004-6361/201936338 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> HALOGAS: the properties of extraplanar HI in disc galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marasco%2C+A">A. Marasco</a>, <a href="/search/astro-ph?searchtype=author&query=Fraternali%2C+F">F. Fraternali</a>, <a href="/search/astro-ph?searchtype=author&query=Heald%2C+G">G. Heald</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T">T. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Jozsa%2C+G+I+G">G. I. G. Jozsa</a>, <a href="/search/astro-ph?searchtype=author&query=Vargas%2C+C+J">C. J. Vargas</a>, <a href="/search/astro-ph?searchtype=author&query=Winkel%2C+B">B. Winkel</a>, <a href="/search/astro-ph?searchtype=author&query=Walterbos%2C+R+A+M">R. A. M. Walterbos</a>, <a href="/search/astro-ph?searchtype=author&query=Dettmar%2C+R+J">R. J. Dettmar</a>, <a href="/search/astro-ph?searchtype=author&query=Jutte%2C+E">E. Jutte</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="1909.04048v1-abstract-short" style="display: inline;"> We present a systematic study of the extraplanar gas (EPG) in a sample of 15 nearby late-type galaxies at intermediate inclinations using publicly available, deep interferometric HI data from the HALOGAS survey. For each system we mask the HI emission coming from the regularly rotating disc and use synthetic datacubes to model the leftover "anomalous" HI flux. Our model consists of a smooth, axisy… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.04048v1-abstract-full').style.display = 'inline'; document.getElementById('1909.04048v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.04048v1-abstract-full" style="display: none;"> We present a systematic study of the extraplanar gas (EPG) in a sample of 15 nearby late-type galaxies at intermediate inclinations using publicly available, deep interferometric HI data from the HALOGAS survey. For each system we mask the HI emission coming from the regularly rotating disc and use synthetic datacubes to model the leftover "anomalous" HI flux. Our model consists of a smooth, axisymmetric thick component described by 3 structural and 4 kinematical parameters, which are fit to the data via a Bayesian MCMC approach. We find that extraplanar HI is nearly ubiquitous in disc galaxies, as we fail to detect it in only two of the systems with the poorest spatial resolution. The EPG component encloses ~5-25% of the total HI mass, with a mean value of 14%, and has a typical thickness of a few kpc, incompatible with expectations based on hydrostatic equilibrium models. The EPG kinematics is remarkably similar throughout the sample, and consists of a lagging rotation with typical vertical gradients of about -10 km/s/kpc, a velocity dispersion of 15-30 km/s and, for most galaxies, a global inflow in both the vertical and radial directions with speeds of 20-30 km/s. The EPG HI masses are in excellent agreement with predictions from simple models of the galactic fountain powered by stellar feedback. The combined effect of photo-ionisation and interaction of the fountain material with the circumgalactic medium can qualitatively explain the kinematics of the EPG, but dynamical models of the galactic fountain are required to fully test this framework. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.04048v1-abstract-full').style.display = 'none'; document.getElementById('1909.04048v1-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 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">27 pages, 14 figures, 4 tables. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 631, A50 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1907.08265">arXiv:1907.08265</a> <span> [<a href="https://arxiv.org/pdf/1907.08265">pdf</a>, <a href="https://arxiv.org/format/1907.08265">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/10.1051/0004-6361/201936114">10.1051/0004-6361/201936114 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutral hydrogen gas within and around NGC 1316 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Serra%2C+P">P. Serra</a>, <a href="/search/astro-ph?searchtype=author&query=Maccagni%2C+F+M">F. M. Maccagni</a>, <a href="/search/astro-ph?searchtype=author&query=Kleiner%2C+D">D. Kleiner</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=van+Gorkom%2C+J+H">J. H. van Gorkom</a>, <a href="/search/astro-ph?searchtype=author&query=Hugo%2C+B">B. Hugo</a>, <a href="/search/astro-ph?searchtype=author&query=Iodice%2C+E">E. Iodice</a>, <a href="/search/astro-ph?searchtype=author&query=Jozsa%2C+G+I+G">G. I. G. Jozsa</a>, <a href="/search/astro-ph?searchtype=author&query=Kamphuis%2C+P">P. Kamphuis</a>, <a href="/search/astro-ph?searchtype=author&query=Kraan-Korteweg%2C+R">R. Kraan-Korteweg</a>, <a href="/search/astro-ph?searchtype=author&query=Loni%2C+A">A. Loni</a>, <a href="/search/astro-ph?searchtype=author&query=Makhathini%2C+S">S. Makhathini</a>, <a href="/search/astro-ph?searchtype=author&query=Molnar%2C+D">D. Molnar</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T">T. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Peletier%2C+R">R. Peletier</a>, <a href="/search/astro-ph?searchtype=author&query=Ramaila%2C+A">A. Ramaila</a>, <a href="/search/astro-ph?searchtype=author&query=Ramatsoku%2C+M">M. Ramatsoku</a>, <a href="/search/astro-ph?searchtype=author&query=Smirnov%2C+O">O. Smirnov</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Spavone%2C+M">M. Spavone</a>, <a href="/search/astro-ph?searchtype=author&query=Thorat%2C+K">K. Thorat</a>, <a href="/search/astro-ph?searchtype=author&query=Trager%2C+S+C">S. C. Trager</a>, <a href="/search/astro-ph?searchtype=author&query=Venhola%2C+A">A. Venhola</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="1907.08265v1-abstract-short" style="display: inline;"> We present MeerKAT observations of neutral hydrogen gas (HI) in the nearby merger remnant NGC 1316 (Fornax A), the brightest member of a galaxy group which is falling into the Fornax cluster. We find HI on a variety of scales, from the galaxy centre to its large-scale environment. For the first time we detect HI at large radii (70 - 150 kpc in projection), mostly distributed on two long tails asso… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.08265v1-abstract-full').style.display = 'inline'; document.getElementById('1907.08265v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1907.08265v1-abstract-full" style="display: none;"> We present MeerKAT observations of neutral hydrogen gas (HI) in the nearby merger remnant NGC 1316 (Fornax A), the brightest member of a galaxy group which is falling into the Fornax cluster. We find HI on a variety of scales, from the galaxy centre to its large-scale environment. For the first time we detect HI at large radii (70 - 150 kpc in projection), mostly distributed on two long tails associated with the galaxy. Gas in the tails dominates the HI mass of NGC 1316: 7e+8 Msun -- 14 times more than in previous observations. The total HI mass is comparable to the amount of neutral gas found inside the stellar body, mostly in molecular form. The HI tails are associated with faint optical tidal features thought to be the remnant of a galaxy merger occurred a few billion years ago. They demonstrate that the merger was gas-rich. During the merger, tidal forces pulled some gas and stars out to large radii, where we now detect them in the form of optical tails and, thanks to our new data, HI tails; while torques caused the remaining gas to flow towards the centre of the remnant, where it was converted into molecular gas and fuelled the starburst revealed by the galaxy's stellar populations. Several of the observed properties of NGC 1316 can be reproduced by a ~ 10:1 merger between a dominant, gas-poor early-type galaxy and a smaller, gas-rich spiral occurred 1 - 3 Gyr ago, likely followed by subsequent accretion of satellite galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1907.08265v1-abstract-full').style.display = 'none'; document.getElementById('1907.08265v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 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">Astronomy & Astrophysics, accepted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 628, A122 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1810.05467">arXiv:1810.05467</a> <span> [<a href="https://arxiv.org/pdf/1810.05467">pdf</a>, <a href="https://arxiv.org/format/1810.05467">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/sty2785">10.1093/mnras/sty2785 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Early Observations of the MHONGOOSE Galaxies: Getting Ready for MeerKAT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sorgho%2C+A">A. Sorgho</a>, <a href="/search/astro-ph?searchtype=author&query=Carignan%2C+C">C. Carignan</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T">T. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Korsaga%2C+M">M. Korsaga</a>, <a href="/search/astro-ph?searchtype=author&query=Pingel%2C+N+M">N. M. Pingel</a>, <a href="/search/astro-ph?searchtype=author&query=Sardone%2C+A">Amy Sardone</a>, <a href="/search/astro-ph?searchtype=author&query=Goedhart%2C+S">S. Goedhart</a>, <a href="/search/astro-ph?searchtype=author&query=Passmoor%2C+S">S. Passmoor</a>, <a href="/search/astro-ph?searchtype=author&query=Dikgale%2C+A">A. Dikgale</a>, <a href="/search/astro-ph?searchtype=author&query=Sirothia%2C+S+K">S. K. Sirothia</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="1810.05467v1-abstract-short" style="display: inline;"> We present early observations of 20 galaxies in the MHONGOOSE survey galaxies using KAT-7, the GBT, and MeerKAT. We present the best calibrators for five of the MHONGOOSE galaxies observed with the KAT-7, and search for signs of gas accretion in the GBT data, down to $3蟽$ column density levels of $\rm 2.2\times10^{18}\, cm^{-2}$ over a $\rm 20\, km\, s^{-1}$ linewidth, but identify none. Using the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.05467v1-abstract-full').style.display = 'inline'; document.getElementById('1810.05467v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1810.05467v1-abstract-full" style="display: none;"> We present early observations of 20 galaxies in the MHONGOOSE survey galaxies using KAT-7, the GBT, and MeerKAT. We present the best calibrators for five of the MHONGOOSE galaxies observed with the KAT-7, and search for signs of gas accretion in the GBT data, down to $3蟽$ column density levels of $\rm 2.2\times10^{18}\, cm^{-2}$ over a $\rm 20\, km\, s^{-1}$ linewidth, but identify none. Using the KAT-7 and MeerKAT data, we have derived rotation curves and mass models for NGC 3621 and NGC 7424 out to an unprecedented extent. As a precursor to the SKA, the MeerKAT telescope combines both a high spatial resolution and a large field of view, necessary to map the extended neutral hydrogen in local galaxies. The mass models of the two galaxies were constructed for both the Dark Matter (DM) models (the pseudo-isothermal model and the Navarro-Frenk-White model) and MOND. Overall, we find that the DM models provide a better fit than MOND to the galaxies' rotation curves. Furthermore, the pseudo-isothermal model is found to be the most consistent with the observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1810.05467v1-abstract-full').style.display = 'none'; document.getElementById('1810.05467v1-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">16 pages (+ 9 pages appendix), 16 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/1808.02840">arXiv:1808.02840</a> <span> [<a href="https://arxiv.org/pdf/1808.02840">pdf</a>, <a href="https://arxiv.org/format/1808.02840">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aad557">10.3847/1538-4357/aad557 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A high-resolution mosaic of the neutral hydrogen in the M81 triplet </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=Walter%2C+F">Fabian Walter</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+A+M+N">Annette M. N. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Bernard%2C+E+J">Edouard J. Bernard</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+J+M">J. M. van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=Neeleman%2C+M">Marcel Neeleman</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+A+K">Adam K. Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Ott%2C+J">Juergen Ott</a>, <a href="/search/astro-ph?searchtype=author&query=Zschaechner%2C+L+K">Laura K. Zschaechner</a>, <a href="/search/astro-ph?searchtype=author&query=Zwaan%2C+M+A">Martin A. Zwaan</a>, <a href="/search/astro-ph?searchtype=author&query=Yun%2C+M+S">Min S. Yun</a>, <a href="/search/astro-ph?searchtype=author&query=Langston%2C+G">Glen Langston</a>, <a href="/search/astro-ph?searchtype=author&query=Keating%2C+K+M">Katie M. Keating</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="1808.02840v1-abstract-short" style="display: inline;"> We present a 3x3 degrees, 105-pointing, high-resolution neutral hydrogen (HI) mosaic of the M81 galaxy triplet (including the galaxies M81, M82 and NGC 3077, as well as dwarf galaxy NGC 2976) obtained with the Very Large Array (VLA) C and D arrays. This uniformly covers the entire area and velocity range of the triplet with a resolution of ~20'' or ~420 pc. The data reveal many small-scale anomalo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.02840v1-abstract-full').style.display = 'inline'; document.getElementById('1808.02840v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.02840v1-abstract-full" style="display: none;"> We present a 3x3 degrees, 105-pointing, high-resolution neutral hydrogen (HI) mosaic of the M81 galaxy triplet (including the galaxies M81, M82 and NGC 3077, as well as dwarf galaxy NGC 2976) obtained with the Very Large Array (VLA) C and D arrays. This uniformly covers the entire area and velocity range of the triplet with a resolution of ~20'' or ~420 pc. The data reveal many small-scale anomalous velocity features highlighting the complexity of the interacting M81 triplet. We compare our data with Green Bank Telescope (GBT) observations of the same area. This provides evidence for a substantial reservoir of low-column density gas in the northern part of the triplet, probably associated with M82. Such a reservoir is not found in the southern part. We report a number of kpc-sized low-mass HI clouds with HI masses of a few times 10^6 Msun. Their dynamical masses are much larger than their baryonic masses, which could indicate the presence of dark matter if the clouds are rotationally supported. However, due to their spatial and kinematical association with HI tidal features, it is more likely that the velocity widths indicate tidal effects or streaming motions. We do not find any clouds not associated with tidal features down to an HI mass limit of a few times 10^4 Msun. We compare the HI column densities with resolved stellar density maps and find a star formation threshold around 3-6 10^20 cm-2$. We find that extreme velocity dispersions can be explained by a superposition of multiple components along the line of sight near M81 as well as winds or outflows around M82. The velocity dispersions found are high enough that these processes could explain the linewidths of Damped-Lyman-alpha absorbers observed at high redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.02840v1-abstract-full').style.display = 'none'; document.getElementById('1808.02840v1-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">originally announced</span> August 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">Accepted for publication in The Astronomical Journal. Full-resolution PDF available at http://www.astron.nl/~blok/M81data/m81data.pdf. Data can be downloaded from http://www.astron.nl/~blok/M81data</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.02041">arXiv:1808.02041</a> <span> [<a href="https://arxiv.org/pdf/1808.02041">pdf</a>, <a href="https://arxiv.org/format/1808.02041">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/aad816">10.3847/1538-4357/aad816 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A GBT Survey of the HALOGAS Galaxies and Their Environments I: Revealing the full extent of HI around NGC891, NGC925, NGC4414 & NGC4565 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pingel%2C+N+M">N. M. Pingel</a>, <a href="/search/astro-ph?searchtype=author&query=Pisano%2C+D+J">D. J. Pisano</a>, <a href="/search/astro-ph?searchtype=author&query=Heald%2C+G">G. Heald</a>, <a href="/search/astro-ph?searchtype=author&query=Jarrett%2C+T+H">T. H. Jarrett</a>, <a href="/search/astro-ph?searchtype=author&query=de+Blok%2C+W+J+G">W. J. G. de Blok</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%B3zsa%2C+G+I+G">G. I. G. J贸zsa</a>, <a href="/search/astro-ph?searchtype=author&query=J%C3%BCtte%2C+E">E. J眉tte</a>, <a href="/search/astro-ph?searchtype=author&query=Rand%2C+R+J">R. J. Rand</a>, <a href="/search/astro-ph?searchtype=author&query=Oosterloo%2C+T">T. Oosterloo</a>, <a href="/search/astro-ph?searchtype=author&query=Winkel%2C+B">B. Winkel</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="1808.02041v1-abstract-short" style="display: inline;"> We present initial results from a deep neutral hydrogen (HI) survey of the HALOGAS galaxy sample, which includes the spiral galaxies NGC891, NGC925, NGC4414, and NGC4565, performed with the Robert C. Byrd Green Bank Telescope (GBT). The resulting observations cover at least four deg$^2$ around these galaxies with an average 5$蟽$ detection limit of 1.2$\times$10$^{18}$ cm$^{-2}$ over a velocity ran… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.02041v1-abstract-full').style.display = 'inline'; document.getElementById('1808.02041v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.02041v1-abstract-full" style="display: none;"> We present initial results from a deep neutral hydrogen (HI) survey of the HALOGAS galaxy sample, which includes the spiral galaxies NGC891, NGC925, NGC4414, and NGC4565, performed with the Robert C. Byrd Green Bank Telescope (GBT). The resulting observations cover at least four deg$^2$ around these galaxies with an average 5$蟽$ detection limit of 1.2$\times$10$^{18}$ cm$^{-2}$ over a velocity range of 20 km s$^{-1}$ and angular scale of 9.1$'$. In addition to detecting the same total flux as the GBT data, the spatial distribution of the GBT and original Westerbork Synthesis Radio Telescope (WSRT) data match well at equal spatial resolutions. The HI mass fraction below HI column densities of 10$^{19}$ cm$^{-2}$ is, on average, 2\%. We discuss the possible origins of low column density HI of nearby spiral galaxies. The absence of a considerable amount of newly detected HI by the GBT indicates these galaxies do not have significant extended diffuse HI structures, and suggests future surveys planned with the SKA and its precursors must go \textit{at least} as deep as 10$^{17}$ cm$^{-2}$ in column density to significantly increase the probability of detecting HI associated with the cosmic web and/or cold mode accretion. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.02041v1-abstract-full').style.display = 'none'; document.getElementById('1808.02041v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Accepted for publication in The Astrophysical Journal; 28 pages, 15 figures</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=de+Blok%2C+W+J+G&start=150" class="pagination-link " 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