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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=Farinelli%2C+R&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Farinelli%2C+R&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Farinelli%2C+R&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </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/2412.02977">arXiv:2412.02977</a> <span> [<a href="https://arxiv.org/pdf/2412.02977">pdf</a>, <a href="https://arxiv.org/format/2412.02977">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"> X-ray Spectral and Timing Properties of the Black Hole Binary XTE J1859+226 and their Relation to Jets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yamaoka%2C+K">Kazutaka Yamaoka</a>, <a href="/search/astro-ph?searchtype=author&query=Kawaguchi%2C+T">Toshihiro Kawaguchi</a>, <a href="/search/astro-ph?searchtype=author&query=McCollough%2C+M+L">Michael L. McCollough</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">Ruben Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Trushkin%2C+S">Sergei Trushkin</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="2412.02977v1-abstract-short" style="display: inline;"> We compiled the X-ray and soft gamma-ray observations of the Galactic black hole binary XTE J1859+226 in the 1999--2000 outburst from RXTE, ASCA, BeppoSAX and CGRO. Throughout systematic spectral analysis using a two-component model consisting of a multi-temperature accretion disk plus a fraction of its flux convolved with an empirical Comptonized powerlaw component, we found that the innermost ra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.02977v1-abstract-full').style.display = 'inline'; document.getElementById('2412.02977v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.02977v1-abstract-full" style="display: none;"> We compiled the X-ray and soft gamma-ray observations of the Galactic black hole binary XTE J1859+226 in the 1999--2000 outburst from RXTE, ASCA, BeppoSAX and CGRO. Throughout systematic spectral analysis using a two-component model consisting of a multi-temperature accretion disk plus a fraction of its flux convolved with an empirical Comptonized powerlaw component, we found that the innermost radius ($r_{\rm in}$) and temperature (Tin) of the disk are very variable with time in the rising phase of soft X-ray flux where Type-A/B/C low-frequency quasi-periodic oscillations (QPOs) were found. After this phase, $r_{\rm in}$ remains constant at around 60 km assuming a distance of 8 kpc and an inclination angle of 67$^{\circ}$, and Tin smoothly decays with time. The constant $r_{\rm in}$ suggests a presence of the innermost stable circular orbit (ISCO), with $r_{\rm in}$ repeatedly moving closer and farther away from the ISCO in the rising phase. Both disk parameters are remarkably correlated with independently analyzed timing properties such as QPO frequency and rms variability. Type-A/B QPOs are seen only when $r_{\rm in}$ is close to the ISCO, while Type-C are seen when $r_{\rm in}$ is truncated and the frequency changes with a relation of $r^{-1.0}_{\rm in}$, supporting that Type-C QPOs occur at the inner edge of the truncated disk. Accurate determinations of the frequency--$r_{\rm in}$ relation for various objects should be a powerful tool to discriminate plausible Type-C QPO models. Furthermore, we suggest that jet ejection events may occur when $r_{\rm in}$ rapidly approaches to the ISCO, along with rapid changes of the disk flux, the rms variability and the hardness ratio. A rapid shrinkage of $r_{\rm in}$ down to the ISCO can be a useful index as a precursor of radio flares for triggering Target-of-Opportunity observations and would provide constraints on jet launching mechanisms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.02977v1-abstract-full').style.display = 'none'; document.getElementById('2412.02977v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 16 figures, accepted for publication in PASJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.00191">arXiv:2412.00191</a> <span> [<a href="https://arxiv.org/pdf/2412.00191">pdf</a>, <a href="https://arxiv.org/format/2412.00191">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Euclid preparation: TBD. The impact of line-of-sight projections on the covariance between galaxy cluster multi-wavelength observable properties -- insights from hydrodynamic simulations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Ragagnin%2C+A">A. Ragagnin</a>, <a href="/search/astro-ph?searchtype=author&query=Saro%2C+A">A. Saro</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Biviano%2C+A">A. Biviano</a>, <a href="/search/astro-ph?searchtype=author&query=Dolag%2C+K">K. Dolag</a>, <a href="/search/astro-ph?searchtype=author&query=Ettori%2C+S">S. Ettori</a>, <a href="/search/astro-ph?searchtype=author&query=Giocoli%2C+C">C. Giocoli</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+A+M+C+L">A. M. C. Le Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Mamon%2C+G+A">G. A. Mamon</a>, <a href="/search/astro-ph?searchtype=author&query=Maughan%2C+B+J">B. J. Maughan</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Moscardini%2C+L">L. Moscardini</a>, <a href="/search/astro-ph?searchtype=author&query=Pacaud%2C+F">F. Pacaud</a>, <a href="/search/astro-ph?searchtype=author&query=Pratt%2C+G+W">G. W. Pratt</a>, <a href="/search/astro-ph?searchtype=author&query=Sereno%2C+M">M. Sereno</a>, <a href="/search/astro-ph?searchtype=author&query=Borgani%2C+S">S. Borgani</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Castignani%2C+G">G. Castignani</a>, <a href="/search/astro-ph?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/astro-ph?searchtype=author&query=Eckert%2C+D">D. Eckert</a>, <a href="/search/astro-ph?searchtype=author&query=Lesci%2C+G+F">G. F. Lesci</a>, <a href="/search/astro-ph?searchtype=author&query=Macias-Perez%2C+J">J. Macias-Perez</a>, <a href="/search/astro-ph?searchtype=author&query=Maturi%2C+M">M. Maturi</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a> , et al. (218 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="2412.00191v1-abstract-short" style="display: inline;"> Cluster cosmology can benefit from combining multi-wavelength studies, which can benefit from characterising the correlation coefficients between different mass-observable relations. In this work, we aim to provide information on the scatter, the skewness, and the covariance of various mass-observable relations in galaxy clusters in cosmological hydrodynamic simulations. This information will help… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.00191v1-abstract-full').style.display = 'inline'; document.getElementById('2412.00191v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.00191v1-abstract-full" style="display: none;"> Cluster cosmology can benefit from combining multi-wavelength studies, which can benefit from characterising the correlation coefficients between different mass-observable relations. In this work, we aim to provide information on the scatter, the skewness, and the covariance of various mass-observable relations in galaxy clusters in cosmological hydrodynamic simulations. This information will help future analyses to better tackle accretion histories and projection effects and model mass observable relations for cosmology studies.We identify galaxy clusters in Magneticum Box2b simulations with mass $M_{\rm 200c}>10^{14} {\rm M}_\odot$ at redshift $z=0.24$ and $z=0.90$. Our analysis includes \Euclid-derived properties such as richness, stellar mass, lensing mass, and concentration. Additionally, we investigate complementary multi-wavelength data, including X-ray luminosity, integrated Compton-$y$ parameter, gas mass, and temperature. The impact of projection effects on mass-observable residuals and correlations is then examined. At intermediate redshift ($z=0.24$), projection effects impact lensing concentration, richness, and gas mass the most in terms of scatter and skewness of log-residuals of scaling relations. The contribution of projection effects can be significant enough to boost a spurious hot- vs. cold-baryons correlation and consequently hide underlying correlations due to halo accretion histories. At high redshift ($z=0.9$), the richness has a much lower scatter (of log-residuals), and the quantity that is most impacted by projection effects is the lensing mass. Lensing concentration reconstruction, in particular, is affected by deviations of the reduced-shear profile shape from the one derived by an NFW profile rather than interlopers in the line of sight. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.00191v1-abstract-full').style.display = 'none'; document.getElementById('2412.00191v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">26 pages, 22 figures, submitted to A&A, replied to referee comments</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.10353">arXiv:2411.10353</a> <span> [<a href="https://arxiv.org/pdf/2411.10353">pdf</a>, <a href="https://arxiv.org/format/2411.10353">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"> First spectropolarimetric observation of the neutron star low-mass X-ray binary GX 3+1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gnarini%2C+A">Andrea Gnarini</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">Ruben Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Ursini%2C+F">Francesco Ursini</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">Stefano Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Capitanio%2C+F">Fiamma Capitanio</a>, <a href="/search/astro-ph?searchtype=author&query=Matt%2C+G">Giorgio Matt</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+M">Mason Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Tarana%2C+A">Antonella Tarana</a>, <a href="/search/astro-ph?searchtype=author&query=Bobrikova%2C+A">Anna Bobrikova</a>, <a href="/search/astro-ph?searchtype=author&query=Cocchi%2C+M">Massimo Cocchi</a>, <a href="/search/astro-ph?searchtype=author&query=Fabiani%2C+S">Sergio Fabiani</a>, <a href="/search/astro-ph?searchtype=author&query=Kaaret%2C+P">Philip Kaaret</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">Juri Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+S">Swati Ravi</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="2411.10353v1-abstract-short" style="display: inline;"> We report the first simultaneous X-ray spectropolarimetric observation of the bright atoll neutron star low-mass X-ray binary GX 3+1, performed by the Imaging X-ray Polarimetry Explorer (IXPE) joint with NICER and NuSTAR. The source does not exhibit significant polarization in the 2-8 keV energy band, with an upper limit of 1.3% at a 99% confidence level on the polarization degree. The observed sp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10353v1-abstract-full').style.display = 'inline'; document.getElementById('2411.10353v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.10353v1-abstract-full" style="display: none;"> We report the first simultaneous X-ray spectropolarimetric observation of the bright atoll neutron star low-mass X-ray binary GX 3+1, performed by the Imaging X-ray Polarimetry Explorer (IXPE) joint with NICER and NuSTAR. The source does not exhibit significant polarization in the 2-8 keV energy band, with an upper limit of 1.3% at a 99% confidence level on the polarization degree. The observed spectra can be well described by a combination of thermal disk emission, the hard Comptonization component, and reflected photons off the accretion disk. In particular, from the broad Fe K$伪$ line profile, we were able to determine the inclination of the system ($i \approx 36^\circ$), which is crucial for comparing the observed polarization with theoretical models. Both the spectral and polarization properties of GX 3+1 are consistent with those of other atoll sources observed by IXPE. Therefore, we may expect a similar geometrical configuration for the accreting system and the hot Comptonizing region. The low polarization is also consistent with the low inclination of the system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10353v1-abstract-full').style.display = 'none'; document.getElementById('2411.10353v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <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">7 pages, 6 figures, 4 tables. Accepted for publication in Astronomy & Astrophysics. arXiv admin note: text overlap with arXiv:2408.02309</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.00956">arXiv:2410.00956</a> <span> [<a href="https://arxiv.org/pdf/2410.00956">pdf</a>, <a href="https://arxiv.org/format/2410.00956">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> <p class="title is-5 mathjax"> Euclid preparation. The impact of relativistic redshift-space distortions on two-point clustering statistics from the Euclid wide spectroscopic survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Elkhashab%2C+M+Y">M. Y. Elkhashab</a>, <a href="/search/astro-ph?searchtype=author&query=Bertacca%2C+D">D. Bertacca</a>, <a href="/search/astro-ph?searchtype=author&query=Porciani%2C+C">C. Porciani</a>, <a href="/search/astro-ph?searchtype=author&query=Salvalaggio%2C+J">J. Salvalaggio</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+M">M. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bodendorf%2C+C">C. Bodendorf</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+D">D. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">J. Brinchmann</a>, <a href="/search/astro-ph?searchtype=author&query=Camera%2C+S">S. Camera</a>, <a href="/search/astro-ph?searchtype=author&query=Capobianco%2C+V">V. Capobianco</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+C">C. Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Cardone%2C+V+F">V. F. Cardone</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Casas%2C+R">R. Casas</a>, <a href="/search/astro-ph?searchtype=author&query=Casas%2C+S">S. Casas</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a> , et al. (230 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.00956v1-abstract-short" style="display: inline;"> Measurements of galaxy clustering are affected by RSD. Peculiar velocities, gravitational lensing, and other light-cone projection effects modify the observed redshifts, fluxes, and sky positions of distant light sources. We determine which of these effects leave a detectable imprint on several 2-point clustering statistics extracted from the EWSS on large scales. We generate 140 mock galaxy catal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.00956v1-abstract-full').style.display = 'inline'; document.getElementById('2410.00956v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.00956v1-abstract-full" style="display: none;"> Measurements of galaxy clustering are affected by RSD. Peculiar velocities, gravitational lensing, and other light-cone projection effects modify the observed redshifts, fluxes, and sky positions of distant light sources. We determine which of these effects leave a detectable imprint on several 2-point clustering statistics extracted from the EWSS on large scales. We generate 140 mock galaxy catalogues with the survey geometry and selection function of the EWSS and make use of the LIGER method to account for a variable number of relativistic RSD to linear order in the cosmological perturbations. We estimate different 2-point clustering statistics from the mocks and use the likelihood-ratio test to calculate the statistical significance with which the EWSS could reject the null hypothesis that certain relativistic projection effects can be neglected in the theoretical models. We find that the combined effects of lensing magnification and convergence imprint characteristic signatures on several clustering observables. Their S/N ranges between 2.5 and 6 (depending on the adopted summary statistic) for the highest-redshift galaxies in the EWSS. The corresponding feature due to the peculiar velocity of the Sun is measured with a S/N of order one or two. The $P_{\ell}(k)$ from the catalogues that include all relativistic effects reject the null hypothesis that RSD are only generated by the variation of the peculiar velocity along the line of sight with a significance of 2.9 standard deviations. As a byproduct of our study, we demonstrate that the mixing-matrix formalism to model finite-volume effects in the $P_{\ell}(k)$ can be robustly applied to surveys made of several disconnected patches. Our results indicate that relativistic RSD, the contribution from weak gravitational lensing in particular, cannot be disregarded when modelling 2-point clustering statistics extracted from the EWSS. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.00956v1-abstract-full').style.display = 'none'; document.getElementById('2410.00956v1-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 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">23 pages, 14 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.18882">arXiv:2409.18882</a> <span> [<a href="https://arxiv.org/pdf/2409.18882">pdf</a>, <a href="https://arxiv.org/format/2409.18882">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> <p class="title is-5 mathjax"> Euclid preparation: 6x2 pt analysis of Euclid's spectroscopic and photometric data sets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Paganin%2C+L">L. Paganin</a>, <a href="/search/astro-ph?searchtype=author&query=Bonici%2C+M">M. Bonici</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+C">C. Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Camera%2C+S">S. Camera</a>, <a href="/search/astro-ph?searchtype=author&query=Tutusaus%2C+I">I. Tutusaus</a>, <a href="/search/astro-ph?searchtype=author&query=Davini%2C+S">S. Davini</a>, <a href="/search/astro-ph?searchtype=author&query=Bel%2C+J">J. Bel</a>, <a href="/search/astro-ph?searchtype=author&query=Tosi%2C+S">S. Tosi</a>, <a href="/search/astro-ph?searchtype=author&query=Sciotti%2C+D">D. Sciotti</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Domizio%2C+S">S. Di Domizio</a>, <a href="/search/astro-ph?searchtype=author&query=Risso%2C+I">I. Risso</a>, <a href="/search/astro-ph?searchtype=author&query=Testera%2C+G">G. Testera</a>, <a href="/search/astro-ph?searchtype=author&query=Sapone%2C+D">D. Sapone</a>, <a href="/search/astro-ph?searchtype=author&query=Sakr%2C+Z">Z. Sakr</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+M">M. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+P">P. Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+R">R. Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardeau%2C+F">F. Bernardeau</a>, <a href="/search/astro-ph?searchtype=author&query=Bodendorf%2C+C">C. Bodendorf</a> , et al. (230 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.18882v1-abstract-short" style="display: inline;"> We present cosmological parameter forecasts for the Euclid 6x2pt statistics, which include the galaxy clustering and weak lensing main probes together with previously neglected cross-covariance and cross-correlation signals between imaging/photometric and spectroscopic data. The aim is understanding the impact of such terms on the Euclid performance. We produce 6x2pt cosmological forecasts, consid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.18882v1-abstract-full').style.display = 'inline'; document.getElementById('2409.18882v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.18882v1-abstract-full" style="display: none;"> We present cosmological parameter forecasts for the Euclid 6x2pt statistics, which include the galaxy clustering and weak lensing main probes together with previously neglected cross-covariance and cross-correlation signals between imaging/photometric and spectroscopic data. The aim is understanding the impact of such terms on the Euclid performance. We produce 6x2pt cosmological forecasts, considering two different techniques: the so-called harmonic and hybrid approaches, respectively. In the first, we treat all the different Euclid probes in the same way, i.e. we consider only angular 2pt-statistics for spectroscopic and photometric clustering, as well as for weak lensing, analysing all their possible cross-covariances and cross-correlations in the spherical harmonic domain. In the second, we do not account for negligible cross-covariances between the 3D and 2D data, but consider the combination of their cross-correlation with the auto-correlation signals. We find that both cross-covariances and cross-correlation signals, have a negligible impact on the cosmological parameter constraints and, therefore, on the Euclid performance. In the case of the hybrid approach, we attribute this result to the effect of the cross-correlation between weak lensing and photometric data, which is dominant with respect to other cross-correlation signals. In the case of the 2D harmonic approach, we attribute this result to two main theoretical limitations of the 2D projected statistics implemented in this work according to the analysis of official Euclid forecasts: the high shot noise and the limited redshift range of the spectroscopic sample, together with the loss of radial information from subleading terms such as redshift-space distortions and lensing magnification. Our analysis suggests that 2D and 3D Euclid data can be safely treated as independent, with a great saving in computational resources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.18882v1-abstract-full').style.display = 'none'; document.getElementById('2409.18882v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages, 20 figures. Comments are welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.07528">arXiv:2409.07528</a> <span> [<a href="https://arxiv.org/pdf/2409.07528">pdf</a>, <a href="https://arxiv.org/format/2409.07528">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Euclid preparation. Deep learning true galaxy morphologies for weak lensing shear bias calibration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Csizi%2C+B">B. Csizi</a>, <a href="/search/astro-ph?searchtype=author&query=Schrabback%2C+T">T. Schrabback</a>, <a href="/search/astro-ph?searchtype=author&query=Grandis%2C+S">S. Grandis</a>, <a href="/search/astro-ph?searchtype=author&query=Hoekstra%2C+H">H. Hoekstra</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+H">H. Jansen</a>, <a href="/search/astro-ph?searchtype=author&query=Linke%2C+L">L. Linke</a>, <a href="/search/astro-ph?searchtype=author&query=Congedo%2C+G">G. Congedo</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+A+N">A. N. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+M">M. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+P">P. Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+R">R. Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Bodendorf%2C+C">C. Bodendorf</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+D">D. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">J. Brinchmann</a>, <a href="/search/astro-ph?searchtype=author&query=Camera%2C+S">S. Camera</a>, <a href="/search/astro-ph?searchtype=author&query=Capobianco%2C+V">V. Capobianco</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+C">C. Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a> , et al. (237 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.07528v1-abstract-short" style="display: inline;"> To date, galaxy image simulations for weak lensing surveys usually approximate the light profiles of all galaxies as a single or double S茅rsic profile, neglecting the influence of galaxy substructures and morphologies deviating from such a simplified parametric characterization. While this approximation may be sufficient for previous data sets, the stringent cosmic shear calibration requirements a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.07528v1-abstract-full').style.display = 'inline'; document.getElementById('2409.07528v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.07528v1-abstract-full" style="display: none;"> To date, galaxy image simulations for weak lensing surveys usually approximate the light profiles of all galaxies as a single or double S茅rsic profile, neglecting the influence of galaxy substructures and morphologies deviating from such a simplified parametric characterization. While this approximation may be sufficient for previous data sets, the stringent cosmic shear calibration requirements and the high quality of the data in the upcoming Euclid survey demand a consideration of the effects that realistic galaxy substructures have on shear measurement biases. Here we present a novel deep learning-based method to create such simulated galaxies directly from HST data. We first build and validate a convolutional neural network based on the wavelet scattering transform to learn noise-free representations independent of the point-spread function of HST galaxy images that can be injected into simulations of images from Euclid's optical instrument VIS without introducing noise correlations during PSF convolution or shearing. Then, we demonstrate the generation of new galaxy images by sampling from the model randomly and conditionally. Next, we quantify the cosmic shear bias from complex galaxy shapes in Euclid-like simulations by comparing the shear measurement biases between a sample of model objects and their best-fit double-S茅rsic counterparts. Using the KSB shape measurement algorithm, we find a multiplicative bias difference between these branches with realistic morphologies and parametric profiles on the order of $6.9\times 10^{-3}$ for a realistic magnitude-S茅rsic index distribution. Moreover, we find clear detection bias differences between full image scenes simulated with parametric and realistic galaxies, leading to a bias difference of $4.0\times 10^{-3}$ independent of the shape measurement method. This makes it relevant for stage IV weak lensing surveys such as Euclid. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.07528v1-abstract-full').style.display = 'none'; document.getElementById('2409.07528v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to A&A. 29 pages, 20 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.07161">arXiv:2409.07161</a> <span> [<a href="https://arxiv.org/pdf/2409.07161">pdf</a>, <a href="https://arxiv.org/format/2409.07161">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The IXPE View of Neutron Star Low-Mass X-ray Binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ursini%2C+F">Francesco Ursini</a>, <a href="/search/astro-ph?searchtype=author&query=Gnarini%2C+A">Andrea Gnarini</a>, <a href="/search/astro-ph?searchtype=author&query=Capitanio%2C+F">Fiamma Capitanio</a>, <a href="/search/astro-ph?searchtype=author&query=Bobrikova%2C+A">Anna Bobrikova</a>, <a href="/search/astro-ph?searchtype=author&query=Cocchi%2C+M">Massimo Cocchi</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marco%2C+A">Alessandro Di Marco</a>, <a href="/search/astro-ph?searchtype=author&query=Fabiani%2C+S">Sergio Fabiani</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">Ruben Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=La+Monaca%2C+F">Fabio La Monaca</a>, <a href="/search/astro-ph?searchtype=author&query=Rankin%2C+J">John Rankin</a>, <a href="/search/astro-ph?searchtype=author&query=Saade%2C+M+L">Mary Lynne Saade</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">Juri Poutanen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.07161v1-abstract-short" style="display: inline;"> Low-mass X-ray binaries hosting weakly magnetized neutron stars (NS-LMXBs) are among the brightest sources in the X-ray sky. Since 2021, the Imaging X-ray Polarimetry Explorer (IXPE) has provided new measurements of the X-ray polarization of these sources. IXPE observations have revealed that most NS-LMXBs are significantly polarized in the X-rays, providing unprecedented insight into the geometry… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.07161v1-abstract-full').style.display = 'inline'; document.getElementById('2409.07161v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.07161v1-abstract-full" style="display: none;"> Low-mass X-ray binaries hosting weakly magnetized neutron stars (NS-LMXBs) are among the brightest sources in the X-ray sky. Since 2021, the Imaging X-ray Polarimetry Explorer (IXPE) has provided new measurements of the X-ray polarization of these sources. IXPE observations have revealed that most NS-LMXBs are significantly polarized in the X-rays, providing unprecedented insight into the geometry of their accretion flow. In this review paper, we summarize the first results obtained by IXPE on NS-LMXBs, the emerging trends within each class of sources (atoll/Z), and possible physical interpretations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.07161v1-abstract-full').style.display = 'none'; document.getElementById('2409.07161v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 3 figures, invited review for the Special Issue X-ray Polarization: A New Era Begins</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.03524">arXiv:2409.03524</a> <span> [<a href="https://arxiv.org/pdf/2409.03524">pdf</a>, <a href="https://arxiv.org/format/2409.03524">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> <p class="title is-5 mathjax"> Euclid preparation. Simulations and nonlinearities beyond $螞$CDM. 4. Constraints on $f(R)$ models from the photometric primary probes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Koyama%2C+K">K. Koyama</a>, <a href="/search/astro-ph?searchtype=author&query=Pamuk%2C+S">S. Pamuk</a>, <a href="/search/astro-ph?searchtype=author&query=Casas%2C+S">S. Casas</a>, <a href="/search/astro-ph?searchtype=author&query=Bose%2C+B">B. Bose</a>, <a href="/search/astro-ph?searchtype=author&query=Carrilho%2C+P">P. Carrilho</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1ez-Casares%2C+I">I. S谩ez-Casares</a>, <a href="/search/astro-ph?searchtype=author&query=Atayde%2C+L">L. Atayde</a>, <a href="/search/astro-ph?searchtype=author&query=Cataneo%2C+M">M. Cataneo</a>, <a href="/search/astro-ph?searchtype=author&query=Fiorini%2C+B">B. Fiorini</a>, <a href="/search/astro-ph?searchtype=author&query=Giocoli%2C+C">C. Giocoli</a>, <a href="/search/astro-ph?searchtype=author&query=Brun%2C+A+M+C+L">A. M. C. Le Brun</a>, <a href="/search/astro-ph?searchtype=author&query=Pace%2C+F">F. Pace</a>, <a href="/search/astro-ph?searchtype=author&query=Pourtsidou%2C+A">A. Pourtsidou</a>, <a href="/search/astro-ph?searchtype=author&query=Rasera%2C+Y">Y. Rasera</a>, <a href="/search/astro-ph?searchtype=author&query=Sakr%2C+Z">Z. Sakr</a>, <a href="/search/astro-ph?searchtype=author&query=Winther%2C+H+-">H. -A. Winther</a>, <a href="/search/astro-ph?searchtype=author&query=Altamura%2C+E">E. Altamura</a>, <a href="/search/astro-ph?searchtype=author&query=Adamek%2C+J">J. Adamek</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+M">M. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Breton%2C+M+-">M. -A. Breton</a>, <a href="/search/astro-ph?searchtype=author&query=R%C3%A1cz%2C+G">G. R谩cz</a>, <a href="/search/astro-ph?searchtype=author&query=Vernizzi%2C+F">F. Vernizzi</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a> , et al. (253 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.03524v1-abstract-short" style="display: inline;"> We study the constraint on $f(R)$ gravity that can be obtained by photometric primary probes of the Euclid mission. Our focus is the dependence of the constraint on the theoretical modelling of the nonlinear matter power spectrum. In the Hu-Sawicki $f(R)$ gravity model, we consider four different predictions for the ratio between the power spectrum in $f(R)$ and that in $螞$CDM: a fitting formula,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03524v1-abstract-full').style.display = 'inline'; document.getElementById('2409.03524v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.03524v1-abstract-full" style="display: none;"> We study the constraint on $f(R)$ gravity that can be obtained by photometric primary probes of the Euclid mission. Our focus is the dependence of the constraint on the theoretical modelling of the nonlinear matter power spectrum. In the Hu-Sawicki $f(R)$ gravity model, we consider four different predictions for the ratio between the power spectrum in $f(R)$ and that in $螞$CDM: a fitting formula, the halo model reaction approach, ReACT and two emulators based on dark matter only $N$-body simulations, FORGE and e-Mantis. These predictions are added to the MontePython implementation to predict the angular power spectra for weak lensing (WL), photometric galaxy clustering and their cross-correlation. By running Markov Chain Monte Carlo, we compare constraints on parameters and investigate the bias of the recovered $f(R)$ parameter if the data are created by a different model. For the pessimistic setting of WL, one dimensional bias for the $f(R)$ parameter, $\log_{10}|f_{R0}|$, is found to be $0.5 蟽$ when FORGE is used to create the synthetic data with $\log_{10}|f_{R0}| =-5.301$ and fitted by e-Mantis. The impact of baryonic physics on WL is studied by using a baryonification emulator BCemu. For the optimistic setting, the $f(R)$ parameter and two main baryon parameters are well constrained despite the degeneracies among these parameters. However, the difference in the nonlinear dark matter prediction can be compensated by the adjustment of baryon parameters, and the one-dimensional marginalised constraint on $\log_{10}|f_{R0}|$ is biased. This bias can be avoided in the pessimistic setting at the expense of weaker constraints. For the pessimistic setting, using the $螞$CDM synthetic data for WL, we obtain the prior-independent upper limit of $\log_{10}|f_{R0}|< -5.6$. Finally, we implement a method to include theoretical errors to avoid the bias. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03524v1-abstract-full').style.display = 'none'; document.getElementById('2409.03524v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 16 figures, submitted on behalf of the Euclid Collaboration</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.02783">arXiv:2409.02783</a> <span> [<a href="https://arxiv.org/pdf/2409.02783">pdf</a>, <a href="https://arxiv.org/format/2409.02783">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> <p class="title is-5 mathjax"> Euclid preparation: Determining the weak lensing mass accuracy and precision for galaxy clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Ingoglia%2C+L">L. Ingoglia</a>, <a href="/search/astro-ph?searchtype=author&query=Sereno%2C+M">M. Sereno</a>, <a href="/search/astro-ph?searchtype=author&query=Farrens%2C+S">S. Farrens</a>, <a href="/search/astro-ph?searchtype=author&query=Giocoli%2C+C">C. Giocoli</a>, <a href="/search/astro-ph?searchtype=author&query=Baumont%2C+L">L. Baumont</a>, <a href="/search/astro-ph?searchtype=author&query=Lesci%2C+G+F">G. F. Lesci</a>, <a href="/search/astro-ph?searchtype=author&query=Moscardini%2C+L">L. Moscardini</a>, <a href="/search/astro-ph?searchtype=author&query=Murray%2C+C">C. Murray</a>, <a href="/search/astro-ph?searchtype=author&query=Vannier%2C+M">M. Vannier</a>, <a href="/search/astro-ph?searchtype=author&query=Biviano%2C+A">A. Biviano</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+C">C. Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Covone%2C+G">G. Covone</a>, <a href="/search/astro-ph?searchtype=author&query=Despali%2C+G">G. Despali</a>, <a href="/search/astro-ph?searchtype=author&query=Maturi%2C+M">M. Maturi</a>, <a href="/search/astro-ph?searchtype=author&query=Maurogordato%2C+S">S. Maurogordato</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Radovich%2C+M">M. Radovich</a>, <a href="/search/astro-ph?searchtype=author&query=Altieri%2C+B">B. Altieri</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+M">M. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a> , et al. (257 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.02783v2-abstract-short" style="display: inline;"> We investigate the level of accuracy and precision of cluster weak-lensing (WL) masses measured with the \Euclid data processing pipeline. We use the DEMNUni-Cov $N$-body simulations to assess how well the WL mass probes the true halo mass, and, then, how well WL masses can be recovered in the presence of measurement uncertainties. We consider different halo mass density models, priors, and mass p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02783v2-abstract-full').style.display = 'inline'; document.getElementById('2409.02783v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.02783v2-abstract-full" style="display: none;"> We investigate the level of accuracy and precision of cluster weak-lensing (WL) masses measured with the \Euclid data processing pipeline. We use the DEMNUni-Cov $N$-body simulations to assess how well the WL mass probes the true halo mass, and, then, how well WL masses can be recovered in the presence of measurement uncertainties. We consider different halo mass density models, priors, and mass point estimates. WL mass differs from true mass due to, e.g., the intrinsic ellipticity of sources, correlated or uncorrelated matter and large-scale structure, halo triaxiality and orientation, and merging or irregular morphology. In an ideal scenario without observational or measurement errors, the maximum likelihood estimator is the most accurate, with WL masses biased low by $\langle b_M \rangle = -14.6 \pm 1.7 \, \%$ on average over the full range $M_\text{200c} > 5 \times 10^{13} \, M_\odot$ and $z < 1$. Due to the stabilising effect of the prior, the biweight, mean, and median estimates are more precise. The scatter decreases with increasing mass and informative priors significantly reduce the scatter. Halo mass density profiles with a truncation provide better fits to the lensing signal, while the accuracy and precision are not significantly affected. We further investigate the impact of additional sources of systematic uncertainty on the WL mass, namely the impact of photometric redshift uncertainties and source selection, the expected performance of \Euclid cluster detection algorithms, and the presence of masks. Taken in isolation, we find that the largest effect is induced by non-conservative source selection. This effect can be mostly removed with a robust selection. As a final \Euclid-like test, we combine systematic effects in a realistic observational setting and find results similar to the ideal case, $\langle b_M \rangle = - 15.5 \pm 2.4 \, \%$, under a robust selection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02783v2-abstract-full').style.display = 'none'; document.getElementById('2409.02783v2-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.16713">arXiv:2408.16713</a> <span> [<a href="https://arxiv.org/pdf/2408.16713">pdf</a>, <a href="https://arxiv.org/format/2408.16713">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> X-ray spectropolarimetry of the bright atoll Serpens X-1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ursini%2C+F">F. Ursini</a>, <a href="/search/astro-ph?searchtype=author&query=Gnarini%2C+A">A. Gnarini</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Bobrikova%2C+A">A. Bobrikova</a>, <a href="/search/astro-ph?searchtype=author&query=Capitanio%2C+F">F. Capitanio</a>, <a href="/search/astro-ph?searchtype=author&query=Cocchi%2C+M">M. Cocchi</a>, <a href="/search/astro-ph?searchtype=author&query=Fabiani%2C+S">S. Fabiani</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">R. Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Kaaret%2C+P">P. Kaaret</a>, <a href="/search/astro-ph?searchtype=author&query=Matt%2C+G">G. Matt</a>, <a href="/search/astro-ph?searchtype=author&query=Ng%2C+M">M. Ng</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">J. Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Ravi%2C+S">S. Ravi</a>, <a href="/search/astro-ph?searchtype=author&query=Tarana%2C+A">A. Tarana</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.16713v1-abstract-short" style="display: inline;"> We present simultaneous X-ray polarimetric and spectral observations of the bright atoll source Ser~X-1 carried out with the Imaging X-ray Polarimetry Explorer (IXPE), NICER, and NuSTAR. We obtain an upper limit of 2% (99% confidence level) on the polarization degree in the 2--8 keV energy band. We detect four type-I X-ray bursts, two of which during the IXPE observation. This is the first time th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.16713v1-abstract-full').style.display = 'inline'; document.getElementById('2408.16713v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.16713v1-abstract-full" style="display: none;"> We present simultaneous X-ray polarimetric and spectral observations of the bright atoll source Ser~X-1 carried out with the Imaging X-ray Polarimetry Explorer (IXPE), NICER, and NuSTAR. We obtain an upper limit of 2% (99% confidence level) on the polarization degree in the 2--8 keV energy band. We detect four type-I X-ray bursts, two of which during the IXPE observation. This is the first time that has IXPE observed type-I X-ray bursts, and it allows us to place an upper limit on their polarization degree; however, due to the limited total number of counts in each burst, we obtain a relatively high upper limit (80%). We confirm the presence of reflection features in the X-ray spectrum, notably a broad iron line. Fitting the data with a relativistic reflection model, we derive a disk inclination of 25 deg. The spectral and polarization properties are comparable with other atolls observed by IXPE, suggesting a similar accretion geometry, and the relatively low polarization is consistent with the low inclination. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.16713v1-abstract-full').style.display = 'none'; document.getElementById('2408.16713v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by 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/2408.05296">arXiv:2408.05296</a> <span> [<a href="https://arxiv.org/pdf/2408.05296">pdf</a>, <a href="https://arxiv.org/format/2408.05296">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Euclid Preparation. Cosmic Dawn Survey: Data release 1 multiwavelength catalogues for Euclid Deep Field North and Euclid Deep Field Fornax </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Zalesky%2C+L">L. Zalesky</a>, <a href="/search/astro-ph?searchtype=author&query=McPartland%2C+C+J+R">C. J. R. McPartland</a>, <a href="/search/astro-ph?searchtype=author&query=Weaver%2C+J+R">J. R. Weaver</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">S. Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+D+B">D. B. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Mobasher%2C+B">B. Mobasher</a>, <a href="/search/astro-ph?searchtype=author&query=Suzuki%2C+N">N. Suzuki</a>, <a href="/search/astro-ph?searchtype=author&query=Szapudi%2C+I">I. Szapudi</a>, <a href="/search/astro-ph?searchtype=author&query=Valdes%2C+I">I. Valdes</a>, <a href="/search/astro-ph?searchtype=author&query=Murphree%2C+G">G. Murphree</a>, <a href="/search/astro-ph?searchtype=author&query=Chartab%2C+N">N. Chartab</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+N">N. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Taamoli%2C+S">S. Taamoli</a>, <a href="/search/astro-ph?searchtype=author&query=Barrow%2C+S+W+J">S. W. J. Barrow</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+O+C">O. Ch谩vez Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">S. L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S">S. Gwyn</a>, <a href="/search/astro-ph?searchtype=author&query=Sawicki%2C+M">M. Sawicki</a>, <a href="/search/astro-ph?searchtype=author&query=McCracken%2C+H+J">H. J. McCracken</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Dannerbauer%2C+H">H. Dannerbauer</a>, <a href="/search/astro-ph?searchtype=author&query=Altieri%2C+B">B. Altieri</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a> , et al. (250 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="2408.05296v3-abstract-short" style="display: inline;"> The Cosmic Dawn Survey (DAWN survey) provides multiwavelength (UV/optical to mid-IR) data across the combined 59 deg$^{2}$ of the Euclid Deep and Auxiliary fields (EDFs and EAFs). Here, the first public data release (DR1) from the DAWN survey is presented. DR1 catalogues are made available for a subset of the full DAWN survey that consists of two Euclid Deep fields: Euclid Deep Field North (EDF-N)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.05296v3-abstract-full').style.display = 'inline'; document.getElementById('2408.05296v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.05296v3-abstract-full" style="display: none;"> The Cosmic Dawn Survey (DAWN survey) provides multiwavelength (UV/optical to mid-IR) data across the combined 59 deg$^{2}$ of the Euclid Deep and Auxiliary fields (EDFs and EAFs). Here, the first public data release (DR1) from the DAWN survey is presented. DR1 catalogues are made available for a subset of the full DAWN survey that consists of two Euclid Deep fields: Euclid Deep Field North (EDF-N) and Euclid Deep Field Fornax (EDF-F). The DAWN survey DR1 catalogues do not include $Euclid$ data as they are not yet public for these fields. Nonetheless, each field has been covered by the ongoing Hawaii Twenty Square Degree Survey (H20), which includes imaging from CFHT MegaCam in the new $u$ filter and from Subaru Hyper Suprime-Cam (HSC) in the $griz$ filters. Each field is further covered by $Spitzer$/IRAC 3.6-4.5$渭$m imaging spanning 10 deg$^{2}$ and reaching $\sim$25 mag AB (5$蟽$). All present H20 imaging and all publicly available imaging from the aforementioned facilities are combined with the deep $Spitzer$/IRAC data to create source catalogues spanning a total area of 16.87 deg$^{2}$ in EDF-N and 2.85 deg$^{2}$ in EDF-F for this first release. Photometry is measured using The Farmer, a well-validated model-based photometry code. Photometric redshifts and stellar masses are computed using two independent codes for modeling spectral energy distributions: EAZY and LePhare. Photometric redshifts show good agreement with spectroscopic redshifts ($蟽_{\rm NMAD} \sim 0.5, 畏< 8\%$ at $i < 25$). Number counts, photometric redshifts, and stellar masses are further validated in comparison to the COSMOS2020 catalogue. The DAWN survey DR1 catalogues are designed to be of immediate use in these two EDFs and will be continuously updated. Future data releases will provide catalogues of all EDFs and EAFs and include $Euclid$ data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.05296v3-abstract-full').style.display = 'none'; document.getElementById('2408.05296v3-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 9 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.05275">arXiv:2408.05275</a> <span> [<a href="https://arxiv.org/pdf/2408.05275">pdf</a>, <a href="https://arxiv.org/format/2408.05275">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"> Euclid preparation. The Cosmic Dawn Survey (DAWN) of the Euclid Deep and Auxiliary Fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=McPartland%2C+C+J+R">C. J. R. McPartland</a>, <a href="/search/astro-ph?searchtype=author&query=Zalesky%2C+L">L. Zalesky</a>, <a href="/search/astro-ph?searchtype=author&query=Weaver%2C+J+R">J. R. Weaver</a>, <a href="/search/astro-ph?searchtype=author&query=Toft%2C+S">S. Toft</a>, <a href="/search/astro-ph?searchtype=author&query=Sanders%2C+D+B">D. B. Sanders</a>, <a href="/search/astro-ph?searchtype=author&query=Mobasher%2C+B">B. Mobasher</a>, <a href="/search/astro-ph?searchtype=author&query=Suzuki%2C+N">N. Suzuki</a>, <a href="/search/astro-ph?searchtype=author&query=Szapudi%2C+I">I. Szapudi</a>, <a href="/search/astro-ph?searchtype=author&query=Valdes%2C+I">I. Valdes</a>, <a href="/search/astro-ph?searchtype=author&query=Murphree%2C+G">G. Murphree</a>, <a href="/search/astro-ph?searchtype=author&query=Chartab%2C+N">N. Chartab</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+N">N. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Taamoli%2C+S">S. Taamoli</a>, <a href="/search/astro-ph?searchtype=author&query=Eisenhardt%2C+P+R+M">P. R. M. Eisenhardt</a>, <a href="/search/astro-ph?searchtype=author&query=Arnouts%2C+S">S. Arnouts</a>, <a href="/search/astro-ph?searchtype=author&query=Atek%2C+H">H. Atek</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">J. Brinchmann</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Chary%2C+R">R. Chary</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+O+C">O. Ch谩vez Ortiz</a>, <a href="/search/astro-ph?searchtype=author&query=Cuby%2C+J+-">J. -G. Cuby</a>, <a href="/search/astro-ph?searchtype=author&query=Finkelstein%2C+S+L">S. L. Finkelstein</a>, <a href="/search/astro-ph?searchtype=author&query=Goto%2C+T">T. Goto</a>, <a href="/search/astro-ph?searchtype=author&query=Gwyn%2C+S">S. Gwyn</a> , et al. (266 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="2408.05275v3-abstract-short" style="display: inline;"> Euclid will provide deep NIR imaging to $\sim$26.5 AB magnitude over $\sim$59 deg$^2$ in its deep and auxiliary fields. The Cosmic DAWN survey complements the deep Euclid data with matched depth multiwavelength imaging and spectroscopy in the UV--IR to provide consistently processed Euclid selected photometric catalogs, accurate photometric redshifts, and measurements of galaxy properties to a red… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.05275v3-abstract-full').style.display = 'inline'; document.getElementById('2408.05275v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.05275v3-abstract-full" style="display: none;"> Euclid will provide deep NIR imaging to $\sim$26.5 AB magnitude over $\sim$59 deg$^2$ in its deep and auxiliary fields. The Cosmic DAWN survey complements the deep Euclid data with matched depth multiwavelength imaging and spectroscopy in the UV--IR to provide consistently processed Euclid selected photometric catalogs, accurate photometric redshifts, and measurements of galaxy properties to a redshift of $z\sim 10$. In this paper, we present an overview of the survey, including the footprints of the survey fields, the existing and planned observations, and the primary science goals for the combined data set. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.05275v3-abstract-full').style.display = 'none'; document.getElementById('2408.05275v3-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 10 figures, submitted to A&A; Updated references; Updated author list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.18274">arXiv:2406.18274</a> <span> [<a href="https://arxiv.org/pdf/2406.18274">pdf</a>, <a href="https://arxiv.org/format/2406.18274">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> <p class="title is-5 mathjax"> Euclid preparation. Sensitivity to non-standard particle dark matter model </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Lesgourgues%2C+J">J. Lesgourgues</a>, <a href="/search/astro-ph?searchtype=author&query=Schwagereit%2C+J">J. Schwagereit</a>, <a href="/search/astro-ph?searchtype=author&query=Bucko%2C+J">J. Bucko</a>, <a href="/search/astro-ph?searchtype=author&query=Parimbelli%2C+G">G. Parimbelli</a>, <a href="/search/astro-ph?searchtype=author&query=Giri%2C+S+K">S. K. Giri</a>, <a href="/search/astro-ph?searchtype=author&query=Hervas-Peters%2C+F">F. Hervas-Peters</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+A">A. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Archidiacono%2C+M">M. Archidiacono</a>, <a href="/search/astro-ph?searchtype=author&query=Pace%2C+F">F. Pace</a>, <a href="/search/astro-ph?searchtype=author&query=Sakr%2C+Z">Z. Sakr</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Amendola%2C+L">L. Amendola</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Aussel%2C+H">H. Aussel</a>, <a href="/search/astro-ph?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+M">M. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+R">R. Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Bodendorf%2C+C">C. Bodendorf</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+D">D. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">J. Brinchmann</a> , et al. (227 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="2406.18274v1-abstract-short" style="display: inline;"> The Euclid mission of the European Space Agency will provide weak gravitational lensing and galaxy clustering surveys that can be used to constrain the standard cosmological model and its extensions, with an opportunity to test the properties of dark matter beyond the minimal cold dark matter paradigm. We present forecasts from the combination of these surveys on the parameters describing four int… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18274v1-abstract-full').style.display = 'inline'; document.getElementById('2406.18274v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.18274v1-abstract-full" style="display: none;"> The Euclid mission of the European Space Agency will provide weak gravitational lensing and galaxy clustering surveys that can be used to constrain the standard cosmological model and its extensions, with an opportunity to test the properties of dark matter beyond the minimal cold dark matter paradigm. We present forecasts from the combination of these surveys on the parameters describing four interesting and representative non-minimal dark matter models: a mixture of cold and warm dark matter relics; unstable dark matter decaying either into massless or massive relics; and dark matter experiencing feeble interactions with relativistic relics. We model these scenarios at the level of the non-linear matter power spectrum using emulators trained on dedicated N-body simulations. We use a mock Euclid likelihood to fit mock data and infer error bars on dark matter parameters marginalised over other parameters. We find that the Euclid photometric probe (alone or in combination with CMB data from the Planck satellite) will be sensitive to the effect of each of the four dark matter models considered here. The improvement will be particularly spectacular for decaying and interacting dark matter models. With Euclid, the bounds on some dark matter parameters can improve by up to two orders of magnitude compared to current limits. We discuss the dependence of predicted uncertainties on different assumptions: inclusion of photometric galaxy clustering data, minimum angular scale taken into account, modelling of baryonic feedback effects. We conclude that the Euclid mission will be able to measure quantities related to the dark sector of particle physics with unprecedented sensitivity. This will provide important information for model building in high-energy physics. Any hint of a deviation from the minimal cold dark matter paradigm would have profound implications for cosmology and particle physics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18274v1-abstract-full').style.display = 'none'; document.getElementById('2406.18274v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 21 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> TTK-24-26 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.18126">arXiv:2405.18126</a> <span> [<a href="https://arxiv.org/pdf/2405.18126">pdf</a>, <a href="https://arxiv.org/format/2405.18126">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"> Euclid preparation. Observational expectations for redshift z<7 active galactic nuclei in the Euclid Wide and Deep surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Selwood%2C+M">M. Selwood</a>, <a href="/search/astro-ph?searchtype=author&query=Fotopoulou%2C+S">S. Fotopoulou</a>, <a href="/search/astro-ph?searchtype=author&query=Bremer%2C+M+N">M. N. Bremer</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">L. Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Landt%2C+H">H. Landt</a>, <a href="/search/astro-ph?searchtype=author&query=Ba%C3%B1ados%2C+E">E. Ba帽ados</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</a>, <a href="/search/astro-ph?searchtype=author&query=Shankar%2C+F">F. Shankar</a>, <a href="/search/astro-ph?searchtype=author&query=Stern%2C+D">D. Stern</a>, <a href="/search/astro-ph?searchtype=author&query=Lusso%2C+E">E. Lusso</a>, <a href="/search/astro-ph?searchtype=author&query=Spinoglio%2C+L">L. Spinoglio</a>, <a href="/search/astro-ph?searchtype=author&query=Allevato%2C+V">V. Allevato</a>, <a href="/search/astro-ph?searchtype=author&query=Ricci%2C+F">F. Ricci</a>, <a href="/search/astro-ph?searchtype=author&query=Feltre%2C+A">A. Feltre</a>, <a href="/search/astro-ph?searchtype=author&query=Mannucci%2C+F">F. Mannucci</a>, <a href="/search/astro-ph?searchtype=author&query=Salvato%2C+M">M. Salvato</a>, <a href="/search/astro-ph?searchtype=author&query=Bowler%2C+R+A+A">R. A. A. Bowler</a>, <a href="/search/astro-ph?searchtype=author&query=Mignoli%2C+M">M. Mignoli</a>, <a href="/search/astro-ph?searchtype=author&query=Vergani%2C+D">D. Vergani</a>, <a href="/search/astro-ph?searchtype=author&query=La+Franca%2C+F">F. La Franca</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+M">M. Baldi</a> , et al. (238 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="2405.18126v1-abstract-short" style="display: inline;"> We forecast the expected population of active galactic nuclei (AGN) observable in the Euclid Wide Survey (EWS) and Euclid Deep Survey (EDS). Starting from an X-ray luminosity function (XLF) we generate volume-limited samples of the AGN expected in the survey footprints. Each AGN is assigned an SED appropriate for its X-ray luminosity and redshift, with perturbations sampled from empirical distribu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.18126v1-abstract-full').style.display = 'inline'; document.getElementById('2405.18126v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.18126v1-abstract-full" style="display: none;"> We forecast the expected population of active galactic nuclei (AGN) observable in the Euclid Wide Survey (EWS) and Euclid Deep Survey (EDS). Starting from an X-ray luminosity function (XLF) we generate volume-limited samples of the AGN expected in the survey footprints. Each AGN is assigned an SED appropriate for its X-ray luminosity and redshift, with perturbations sampled from empirical distributions. The photometric detectability of each AGN is assessed via mock observation of the assigned SED. We estimate 40 million AGN will be detectable in at least one band in the EWS and 0.24 million in the EDS, corresponding to surface densities of 2.8$\times$10$^{3}$ deg$^{-2}$ and 4.7$\times$10$^{3}$ deg$^{-2}$. Employing colour selection criteria on our simulated data we select a sample of 4.8$\times$10$^{6}$ (331 deg$^{-2}$) AGN in the EWS and 1.7$\times$10$^{4}$ (346 deg$^{-2}$) in the EDS, amounting to 10% and 8% of the AGN detectable in the EWS and EDS. Including ancillary Rubin/LSST bands improves the completeness and purity of AGN selection. These data roughly double the total number of selected AGN to comprise 21% and 15% of the detectable AGN in the EWS and EDS. The total expected sample of colour-selected AGN contains 6.0$\times$10$^{6}$ (74%) unobscured AGN and 2.1$\times$10$^{6}$ (26%) obscured AGN, covering $0.02 \leq z \lesssim 5.2$ and $43 \leq \log_{10} (L_{bol} / erg s^{-1}) \leq 47$. With this simple colour selection, expected surface densities are already comparable to the yield of modern X-ray and mid-infrared surveys of similar area. The relative uncertainty on our expectation for detectable AGN is 6.7% for the EWS and 12.5% for the EDS, driven by the uncertainty of the XLF. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.18126v1-abstract-full').style.display = 'none'; document.getElementById('2405.18126v1-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 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">36 pages, 21 figures, submitted to 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/2405.14015">arXiv:2405.14015</a> <span> [<a href="https://arxiv.org/pdf/2405.14015">pdf</a>, <a href="https://arxiv.org/format/2405.14015">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"> Euclid preparation. LVIII. Detecting globular clusters in the Euclid survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Voggel%2C+K">K. Voggel</a>, <a href="/search/astro-ph?searchtype=author&query=Lan%C3%A7on%2C+A">A. Lan莽on</a>, <a href="/search/astro-ph?searchtype=author&query=Saifollahi%2C+T">T. Saifollahi</a>, <a href="/search/astro-ph?searchtype=author&query=Larsen%2C+S+S">S. S. Larsen</a>, <a href="/search/astro-ph?searchtype=author&query=Cantiello%2C+M">M. Cantiello</a>, <a href="/search/astro-ph?searchtype=author&query=Rejkuba%2C+M">M. Rejkuba</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J+-">J. -C. Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Hudelot%2C+P">P. Hudelot</a>, <a href="/search/astro-ph?searchtype=author&query=Nucita%2C+A+A">A. A. Nucita</a>, <a href="/search/astro-ph?searchtype=author&query=Urbano%2C+M">M. Urbano</a>, <a href="/search/astro-ph?searchtype=author&query=Romelli%2C+E">E. Romelli</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=Schirmer%2C+M">M. Schirmer</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Abdurro%27uf"> Abdurro'uf</a>, <a href="/search/astro-ph?searchtype=author&query=Annibali%2C+F">F. Annibali</a>, <a href="/search/astro-ph?searchtype=author&query=Baes%2C+M">M. Baes</a>, <a href="/search/astro-ph?searchtype=author&query=Boldrini%2C+P">P. Boldrini</a>, <a href="/search/astro-ph?searchtype=author&query=Cabanac%2C+R">R. Cabanac</a>, <a href="/search/astro-ph?searchtype=author&query=Carollo%2C+D">D. Carollo</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">C. J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P+-">P. -A. Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Ferguson%2C+A+M+N">A. M. N. Ferguson</a>, <a href="/search/astro-ph?searchtype=author&query=Hunt%2C+L+K">L. K. Hunt</a> , et al. (248 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="2405.14015v3-abstract-short" style="display: inline;"> Extragalactic globular clusters (EGCs) are an abundant and powerful tracer of galaxy dynamics and formation, and their own formation and evolution is also a matter of extensive debate. The compact nature of globular clusters means that they are hard to spatially resolve and thus study outside the Local Group. In this work we have examined how well EGCs will be detectable in images from the Euclid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14015v3-abstract-full').style.display = 'inline'; document.getElementById('2405.14015v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.14015v3-abstract-full" style="display: none;"> Extragalactic globular clusters (EGCs) are an abundant and powerful tracer of galaxy dynamics and formation, and their own formation and evolution is also a matter of extensive debate. The compact nature of globular clusters means that they are hard to spatially resolve and thus study outside the Local Group. In this work we have examined how well EGCs will be detectable in images from the Euclid telescope, using both simulated pre-launch images and the first early-release observations of the Fornax galaxy cluster. The Euclid Wide Survey will provide high-spatial resolution VIS imaging in the broad IE band as well as near-infrared photometry (YE, JE, and HE). We estimate that the galaxies within 100 Mpc in the footprint of the Euclid survey host around 830 000 EGCs of which about 350 000 are within the survey's detection limits. For about half of these EGCs, three infrared colours will be available as well. For any galaxy within 50Mpc the brighter half of its GC luminosity function will be detectable by the Euclid Wide Survey. The detectability of EGCs is mainly driven by the residual surface brightness of their host galaxy. We find that an automated machine-learning EGC-classification method based on real Euclid data of the Fornax galaxy cluster provides an efficient method to generate high purity and high completeness GC candidate catalogues. We confirm that EGCs are spatially resolved compared to pure point sources in VIS images of Fornax. Our analysis of both simulated and first on-sky data show that Euclid will increase the number of GCs accessible with high-resolution imaging substantially compared to previous surveys, and will permit the study of GCs in the outskirts of their hosts. Euclid is unique in enabling systematic studies of EGCs in a spatially unbiased and homogeneous manner and is primed to improve our understanding of many understudied aspects of GC astrophysics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14015v3-abstract-full').style.display = 'none'; document.getElementById('2405.14015v3-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">Accepted 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/2405.13494">arXiv:2405.13494</a> <span> [<a href="https://arxiv.org/pdf/2405.13494">pdf</a>, <a href="https://arxiv.org/format/2405.13494">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Euclid. IV. The NISP Calibration Unit </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Hormuth%2C+F">F. Hormuth</a>, <a href="/search/astro-ph?searchtype=author&query=Jahnke%2C+K">K. Jahnke</a>, <a href="/search/astro-ph?searchtype=author&query=Schirmer%2C+M">M. Schirmer</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+C+G+-">C. G. -Y. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Scott%2C+T">T. Scott</a>, <a href="/search/astro-ph?searchtype=author&query=Barbier%2C+R">R. Barbier</a>, <a href="/search/astro-ph?searchtype=author&query=Ferriol%2C+S">S. Ferriol</a>, <a href="/search/astro-ph?searchtype=author&query=Gillard%2C+W">W. Gillard</a>, <a href="/search/astro-ph?searchtype=author&query=Grupp%2C+F">F. Grupp</a>, <a href="/search/astro-ph?searchtype=author&query=Holmes%2C+R">R. Holmes</a>, <a href="/search/astro-ph?searchtype=author&query=Holmes%2C+W">W. Holmes</a>, <a href="/search/astro-ph?searchtype=author&query=Kubik%2C+B">B. Kubik</a>, <a href="/search/astro-ph?searchtype=author&query=Macias-Perez%2C+J">J. Macias-Perez</a>, <a href="/search/astro-ph?searchtype=author&query=Laurent%2C+M">M. Laurent</a>, <a href="/search/astro-ph?searchtype=author&query=Marpaud%2C+J">J. Marpaud</a>, <a href="/search/astro-ph?searchtype=author&query=Marton%2C+M">M. Marton</a>, <a href="/search/astro-ph?searchtype=author&query=Medinaceli%2C+E">E. Medinaceli</a>, <a href="/search/astro-ph?searchtype=author&query=Morgante%2C+G">G. Morgante</a>, <a href="/search/astro-ph?searchtype=author&query=Toledo-Moreo%2C+R">R. Toledo-Moreo</a>, <a href="/search/astro-ph?searchtype=author&query=Trifoglio%2C+M">M. Trifoglio</a>, <a href="/search/astro-ph?searchtype=author&query=Rix%2C+H">Hans-Walter Rix</a>, <a href="/search/astro-ph?searchtype=author&query=Secroun%2C+A">A. Secroun</a>, <a href="/search/astro-ph?searchtype=author&query=Seiffert%2C+M">M. Seiffert</a>, <a href="/search/astro-ph?searchtype=author&query=Stassi%2C+P">P. Stassi</a> , et al. (310 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="2405.13494v2-abstract-short" style="display: inline;"> The near-infrared calibration unit (NI-CU) on board Euclid's Near-Infrared Spectrometer and Photometer (NISP) is the first astronomical calibration lamp based on light-emitting diodes (LEDs) to be operated in space. Euclid is a mission in ESA's Cosmic Vision 2015-2025 framework, to explore the dark universe and provide a next-level characterisation of the nature of gravitation, dark matter, and da… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13494v2-abstract-full').style.display = 'inline'; document.getElementById('2405.13494v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13494v2-abstract-full" style="display: none;"> The near-infrared calibration unit (NI-CU) on board Euclid's Near-Infrared Spectrometer and Photometer (NISP) is the first astronomical calibration lamp based on light-emitting diodes (LEDs) to be operated in space. Euclid is a mission in ESA's Cosmic Vision 2015-2025 framework, to explore the dark universe and provide a next-level characterisation of the nature of gravitation, dark matter, and dark energy. Calibrating photometric and spectrometric measurements of galaxies to better than 1.5% accuracy in a survey homogeneously mapping ~14000 deg^2 of extragalactic sky requires a very detailed characterisation of near-infrared (NIR) detector properties, as well their constant monitoring in flight. To cover two of the main contributions - relative pixel-to-pixel sensitivity and non-linearity characteristics - as well as support other calibration activities, NI-CU was designed to provide spatially approximately homogeneous (<12% variations) and temporally stable illumination (0.1%-0.2% over 1200s) over the NISP detector plane, with minimal power consumption and energy dissipation. NI-CU is covers the spectral range ~[900,1900] nm - at cryo-operating temperature - at 5 fixed independent wavelengths to capture wavelength-dependent behaviour of the detectors, with fluence over a dynamic range of >=100 from ~15 ph s^-1 pixel^-1 to >1500 ph s^-1 pixel^-1. For this functionality, NI-CU is based on LEDs. We describe the rationale behind the decision and design process, describe the challenges in sourcing the right LEDs, as well as the qualification process and lessons learned. We also provide a description of the completed NI-CU, its capabilities and performance as well as its limits. NI-CU has been integrated into NISP and the Euclid satellite, and since Euclid's launch in July 2023 has started supporting survey operations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13494v2-abstract-full').style.display = 'none'; document.getElementById('2405.13494v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">Paper accepted for publication in A&A as part of the special issue 'Euclid on Sky', which contains Euclid key reference papers and first results from the Euclid Early Release Observations</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13493">arXiv:2405.13493</a> <span> [<a href="https://arxiv.org/pdf/2405.13493">pdf</a>, <a href="https://arxiv.org/format/2405.13493">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Euclid. III. The NISP Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Jahnke%2C+K">K. Jahnke</a>, <a href="/search/astro-ph?searchtype=author&query=Gillard%2C+W">W. Gillard</a>, <a href="/search/astro-ph?searchtype=author&query=Schirmer%2C+M">M. Schirmer</a>, <a href="/search/astro-ph?searchtype=author&query=Ealet%2C+A">A. Ealet</a>, <a href="/search/astro-ph?searchtype=author&query=Maciaszek%2C+T">T. Maciaszek</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+E">E. Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Barbier%2C+R">R. Barbier</a>, <a href="/search/astro-ph?searchtype=author&query=Bonoli%2C+C">C. Bonoli</a>, <a href="/search/astro-ph?searchtype=author&query=Corcione%2C+L">L. Corcione</a>, <a href="/search/astro-ph?searchtype=author&query=Dusini%2C+S">S. Dusini</a>, <a href="/search/astro-ph?searchtype=author&query=Grupp%2C+F">F. Grupp</a>, <a href="/search/astro-ph?searchtype=author&query=Hormuth%2C+F">F. Hormuth</a>, <a href="/search/astro-ph?searchtype=author&query=Ligori%2C+S">S. Ligori</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+L">L. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Morgante%2C+G">G. Morgante</a>, <a href="/search/astro-ph?searchtype=author&query=Padilla%2C+C">C. Padilla</a>, <a href="/search/astro-ph?searchtype=author&query=Toledo-Moreo%2C+R">R. Toledo-Moreo</a>, <a href="/search/astro-ph?searchtype=author&query=Trifoglio%2C+M">M. Trifoglio</a>, <a href="/search/astro-ph?searchtype=author&query=Valenziano%2C+L">L. Valenziano</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+R">R. Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Castander%2C+F+J">F. J. Castander</a>, <a href="/search/astro-ph?searchtype=author&query=Garilli%2C+B">B. Garilli</a>, <a href="/search/astro-ph?searchtype=author&query=Lilje%2C+P+B">P. B. Lilje</a>, <a href="/search/astro-ph?searchtype=author&query=Rix%2C+H+-">H. -W. Rix</a> , et al. (412 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="2405.13493v1-abstract-short" style="display: inline;"> The Near-Infrared Spectrometer and Photometer (NISP) on board the Euclid satellite provides multiband photometry and R>=450 slitless grism spectroscopy in the 950-2020nm wavelength range. In this reference article we illuminate the background of NISP's functional and calibration requirements, describe the instrument's integral components, and provide all its key properties. We also sketch the proc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13493v1-abstract-full').style.display = 'inline'; document.getElementById('2405.13493v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13493v1-abstract-full" style="display: none;"> The Near-Infrared Spectrometer and Photometer (NISP) on board the Euclid satellite provides multiband photometry and R>=450 slitless grism spectroscopy in the 950-2020nm wavelength range. In this reference article we illuminate the background of NISP's functional and calibration requirements, describe the instrument's integral components, and provide all its key properties. We also sketch the processes needed to understand how NISP operates and is calibrated, and its technical potentials and limitations. Links to articles providing more details and technical background are included. NISP's 16 HAWAII-2RG (H2RG) detectors with a plate scale of 0.3" pix^-1 deliver a field-of-view of 0.57deg^2. In photo mode, NISP reaches a limiting magnitude of ~24.5AB mag in three photometric exposures of about 100s exposure time, for point sources and with a signal-to-noise ratio (SNR) of 5. For spectroscopy, NISP's point-source sensitivity is a SNR = 3.5 detection of an emission line with flux ~2x10^-16erg/s/cm^2 integrated over two resolution elements of 13.4A, in 3x560s grism exposures at 1.6 mu (redshifted Ha). Our calibration includes on-ground and in-flight characterisation and monitoring of detector baseline, dark current, non-linearity, and sensitivity, to guarantee a relative photometric accuracy of better than 1.5%, and relative spectrophotometry to better than 0.7%. The wavelength calibration must be better than 5A. NISP is the state-of-the-art instrument in the NIR for all science beyond small areas available from HST and JWST - and an enormous advance due to its combination of field size and high throughput of telescope and instrument. During Euclid's 6-year survey covering 14000 deg^2 of extragalactic sky, NISP will be the backbone for determining distances of more than a billion galaxies. Its NIR data will become a rich reference imaging and spectroscopy data set for the coming decades. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13493v1-abstract-full').style.display = 'none'; document.getElementById('2405.13493v1-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 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">Paper submitted as part of the A&A special issue 'Euclid on Sky', which contains Euclid key reference papers and first results from the Euclid Early Release Observations</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13492">arXiv:2405.13492</a> <span> [<a href="https://arxiv.org/pdf/2405.13492">pdf</a>, <a href="https://arxiv.org/format/2405.13492">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </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/10.1051/0004-6361/202450996">10.1051/0004-6361/202450996 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid. II. The VIS Instrument </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Cropper%2C+M+S">M. S. Cropper</a>, <a href="/search/astro-ph?searchtype=author&query=Al-Bahlawan%2C+A">A. Al-Bahlawan</a>, <a href="/search/astro-ph?searchtype=author&query=Amiaux%2C+J">J. Amiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+S">S. Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Azzollini%2C+R">R. Azzollini</a>, <a href="/search/astro-ph?searchtype=author&query=Benson%2C+K">K. Benson</a>, <a href="/search/astro-ph?searchtype=author&query=Berthe%2C+M">M. Berthe</a>, <a href="/search/astro-ph?searchtype=author&query=Boucher%2C+J">J. Boucher</a>, <a href="/search/astro-ph?searchtype=author&query=Bozzo%2C+E">E. Bozzo</a>, <a href="/search/astro-ph?searchtype=author&query=Brockley-Blatt%2C+C">C. Brockley-Blatt</a>, <a href="/search/astro-ph?searchtype=author&query=Candini%2C+G+P">G. P. Candini</a>, <a href="/search/astro-ph?searchtype=author&query=Cara%2C+C">C. Cara</a>, <a href="/search/astro-ph?searchtype=author&query=Chaudery%2C+R+A">R. A. Chaudery</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+R+E">R. E. Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Danto%2C+P">P. Danto</a>, <a href="/search/astro-ph?searchtype=author&query=Denniston%2C+J">J. Denniston</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Giorgio%2C+A+M">A. M. Di Giorgio</a>, <a href="/search/astro-ph?searchtype=author&query=Dryer%2C+B">B. Dryer</a>, <a href="/search/astro-ph?searchtype=author&query=Dubois%2C+J+-">J. -P. Dubois</a>, <a href="/search/astro-ph?searchtype=author&query=Endicott%2C+J">J. Endicott</a>, <a href="/search/astro-ph?searchtype=author&query=Farina%2C+M">M. Farina</a>, <a href="/search/astro-ph?searchtype=author&query=Galli%2C+E">E. Galli</a>, <a href="/search/astro-ph?searchtype=author&query=Genolet%2C+L">L. Genolet</a>, <a href="/search/astro-ph?searchtype=author&query=Gow%2C+J+P+D">J. P. D. Gow</a> , et al. (410 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="2405.13492v2-abstract-short" style="display: inline;"> This paper presents the specification, design, and development of the Visible Camera (VIS) on the ESA Euclid mission. VIS is a large optical-band imager with a field of view of 0.54 deg^2 sampled at 0.1" with an array of 609 Megapixels and spatial resolution of 0.18". It will be used to survey approximately 14,000 deg^2 of extragalactic sky to measure the distortion of galaxies in the redshift ran… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13492v2-abstract-full').style.display = 'inline'; document.getElementById('2405.13492v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13492v2-abstract-full" style="display: none;"> This paper presents the specification, design, and development of the Visible Camera (VIS) on the ESA Euclid mission. VIS is a large optical-band imager with a field of view of 0.54 deg^2 sampled at 0.1" with an array of 609 Megapixels and spatial resolution of 0.18". It will be used to survey approximately 14,000 deg^2 of extragalactic sky to measure the distortion of galaxies in the redshift range z=0.1-1.5 resulting from weak gravitational lensing, one of the two principal cosmology probes of Euclid. With photometric redshifts, the distribution of dark matter can be mapped in three dimensions, and, from how this has changed with look-back time, the nature of dark energy and theories of gravity can be constrained. The entire VIS focal plane will be transmitted to provide the largest images of the Universe from space to date, reaching m_AB>24.5 with S/N >10 in a single broad I_E~(r+i+z) band over a six year survey. The particularly challenging aspects of the instrument are the control and calibration of observational biases, which lead to stringent performance requirements and calibration regimes. With its combination of spatial resolution, calibration knowledge, depth, and area covering most of the extra-Galactic sky, VIS will also provide a legacy data set for many other fields. This paper discusses the rationale behind the VIS concept and describes the instrument design and development before reporting the pre-launch performance derived from ground calibrations and brief results from the in-orbit commissioning. VIS should reach fainter than m_AB=25 with S/N>10 for galaxies of full-width half-maximum of 0.3" in a 1.3" diameter aperture over the Wide Survey, and m_AB>26.4 for a Deep Survey that will cover more than 50 deg^2. The paper also describes how VIS works with the other Euclid components of survey, telescope, and science data processing to extract the cosmological information. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13492v2-abstract-full').style.display = 'none'; document.getElementById('2405.13492v2-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">Paper submitted as part of the A&A special issue `Euclid on Sky', which contains Euclid key reference papers and first results from the Euclid Early Release Observations (A&A reference aa50996-24). This revision is the version accepted by A&A on 19 September 2024. Other than changes to the author list, changes are limited to editorial and journal style</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13491">arXiv:2405.13491</a> <span> [<a href="https://arxiv.org/pdf/2405.13491">pdf</a>, <a href="https://arxiv.org/format/2405.13491">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Euclid. I. Overview of the Euclid mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Mellier%2C+Y">Y. Mellier</a>, <a href="/search/astro-ph?searchtype=author&query=Abdurro%27uf"> Abdurro'uf</a>, <a href="/search/astro-ph?searchtype=author&query=Barroso%2C+J+A+A">J. A. Acevedo Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Ach%C3%BAcarro%2C+A">A. Ach煤carro</a>, <a href="/search/astro-ph?searchtype=author&query=Adamek%2C+J">J. Adamek</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Addison%2C+G+E">G. E. Addison</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Ajani%2C+V">V. Ajani</a>, <a href="/search/astro-ph?searchtype=author&query=Akrami%2C+Y">Y. Akrami</a>, <a href="/search/astro-ph?searchtype=author&query=Al-Bahlawan%2C+A">A. Al-Bahlawan</a>, <a href="/search/astro-ph?searchtype=author&query=Alavi%2C+A">A. Alavi</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+S">I. S. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Alestas%2C+G">G. Alestas</a>, <a href="/search/astro-ph?searchtype=author&query=Alguero%2C+G">G. Alguero</a>, <a href="/search/astro-ph?searchtype=author&query=Allaoui%2C+A">A. Allaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+S+W">S. W. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allevato%2C+V">V. Allevato</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Tetilla%2C+A+V">A. V. Alonso-Tetilla</a>, <a href="/search/astro-ph?searchtype=author&query=Altieri%2C+B">B. Altieri</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Candal%2C+A">A. Alvarez-Candal</a>, <a href="/search/astro-ph?searchtype=author&query=Alvi%2C+S">S. Alvi</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a> , et al. (1115 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="2405.13491v2-abstract-short" style="display: inline;"> The current standard model of cosmology successfully describes a variety of measurements, but the nature of its main ingredients, dark matter and dark energy, remains unknown. Euclid is a medium-class mission in the Cosmic Vision 2015-2025 programme of the European Space Agency (ESA) that will provide high-resolution optical imaging, as well as near-infrared imaging and spectroscopy, over about 14… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13491v2-abstract-full').style.display = 'inline'; document.getElementById('2405.13491v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13491v2-abstract-full" style="display: none;"> The current standard model of cosmology successfully describes a variety of measurements, but the nature of its main ingredients, dark matter and dark energy, remains unknown. Euclid is a medium-class mission in the Cosmic Vision 2015-2025 programme of the European Space Agency (ESA) that will provide high-resolution optical imaging, as well as near-infrared imaging and spectroscopy, over about 14,000 deg^2 of extragalactic sky. In addition to accurate weak lensing and clustering measurements that probe structure formation over half of the age of the Universe, its primary probes for cosmology, these exquisite data will enable a wide range of science. This paper provides a high-level overview of the mission, summarising the survey characteristics, the various data-processing steps, and data products. We also highlight the main science objectives and expected performance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13491v2-abstract-full').style.display = 'none'; document.getElementById('2405.13491v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">Accepted for publication in the A&A special issue`Euclid on Sky'</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.12157">arXiv:2404.12157</a> <span> [<a href="https://arxiv.org/pdf/2404.12157">pdf</a>, <a href="https://arxiv.org/format/2404.12157">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450368">10.1051/0004-6361/202450368 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid preparation. Improving cosmological constraints using a new multi-tracer method with the spectroscopic and photometric samples </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Dournac%2C+F">F. Dournac</a>, <a href="/search/astro-ph?searchtype=author&query=Blanchard%2C+A">A. Blanchard</a>, <a href="/search/astro-ph?searchtype=author&query=Ili%C4%87%2C+S">S. Ili膰</a>, <a href="/search/astro-ph?searchtype=author&query=Lamine%2C+B">B. Lamine</a>, <a href="/search/astro-ph?searchtype=author&query=Tutusaus%2C+I">I. Tutusaus</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Aussel%2C+H">H. Aussel</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+M">M. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bodendorf%2C+C">C. Bodendorf</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+D">D. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/astro-ph?searchtype=author&query=Brau-Nogue%2C+S">S. Brau-Nogue</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">J. Brinchmann</a>, <a href="/search/astro-ph?searchtype=author&query=Camera%2C+S">S. Camera</a>, <a href="/search/astro-ph?searchtype=author&query=Capobianco%2C+V">V. Capobianco</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Casas%2C+S">S. Casas</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cavuoti%2C+S">S. Cavuoti</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a> , et al. (218 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="2404.12157v1-abstract-short" style="display: inline;"> Future data provided by the Euclid mission will allow us to better understand the cosmic history of the Universe. A metric of its performance is the figure-of-merit (FoM) of dark energy, usually estimated with Fisher forecasts. The expected FoM has previously been estimated taking into account the two main probes of Euclid, namely the three-dimensional clustering of the spectroscopic galaxy sample… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.12157v1-abstract-full').style.display = 'inline'; document.getElementById('2404.12157v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.12157v1-abstract-full" style="display: none;"> Future data provided by the Euclid mission will allow us to better understand the cosmic history of the Universe. A metric of its performance is the figure-of-merit (FoM) of dark energy, usually estimated with Fisher forecasts. The expected FoM has previously been estimated taking into account the two main probes of Euclid, namely the three-dimensional clustering of the spectroscopic galaxy sample, and the so-called 3x2pt signal from the photometric sample (i.e., the weak lensing signal, the galaxy clustering, and their cross-correlation). So far, these two probes have been treated as independent. In this paper, we introduce a new observable given by the ratio of the (angular) two-point correlation function of galaxies from the two surveys. For identical (normalised) selection functions, this observable is unaffected by sampling noise, and its variance is solely controlled by Poisson noise. We present forecasts for Euclid where this multi-tracer method is applied and is particularly relevant because the two surveys will cover the same area of the sky. This method allows for the exploitation of the combination of the spectroscopic and photometric samples. When the correlation between this new observable and the other probes is not taken into account, a significant gain is obtained in the FoM, as well as in the constraints on other cosmological parameters. The benefit is more pronounced for a commonly investigated modified gravity model, namely the $纬$ parametrisation of the growth factor. However, the correlation between the different probes is found to be significant and hence the actual gain is uncertain. We present various strategies for circumventing this issue and still extract useful information from the new observable. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.12157v1-abstract-full').style.display = 'none'; document.getElementById('2404.12157v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 7 figures, 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 690, A30 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.08036">arXiv:2404.08036</a> <span> [<a href="https://arxiv.org/pdf/2404.08036">pdf</a>, <a href="https://arxiv.org/format/2404.08036">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> <p class="title is-5 mathjax"> Euclid preparation. XLII. A unified catalogue-level reanalysis of weak lensing by galaxy clusters in five imaging surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Sereno%2C+M">M. Sereno</a>, <a href="/search/astro-ph?searchtype=author&query=Farrens%2C+S">S. Farrens</a>, <a href="/search/astro-ph?searchtype=author&query=Ingoglia%2C+L">L. Ingoglia</a>, <a href="/search/astro-ph?searchtype=author&query=Lesci%2C+G+F">G. F. Lesci</a>, <a href="/search/astro-ph?searchtype=author&query=Baumont%2C+L">L. Baumont</a>, <a href="/search/astro-ph?searchtype=author&query=Covone%2C+G">G. Covone</a>, <a href="/search/astro-ph?searchtype=author&query=Giocoli%2C+C">C. Giocoli</a>, <a href="/search/astro-ph?searchtype=author&query=Marulli%2C+F">F. Marulli</a>, <a href="/search/astro-ph?searchtype=author&query=La+Hera%2C+S+M">S. Miranda La Hera</a>, <a href="/search/astro-ph?searchtype=author&query=Vannier%2C+M">M. Vannier</a>, <a href="/search/astro-ph?searchtype=author&query=Biviano%2C+A">A. Biviano</a>, <a href="/search/astro-ph?searchtype=author&query=Maurogordato%2C+S">S. Maurogordato</a>, <a href="/search/astro-ph?searchtype=author&query=Moscardini%2C+L">L. Moscardini</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+M">M. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bellagamba%2C+F">F. Bellagamba</a>, <a href="/search/astro-ph?searchtype=author&query=Bodendorf%2C+C">C. Bodendorf</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+D">D. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">J. Brinchmann</a> , et al. (199 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="2404.08036v1-abstract-short" style="display: inline;"> Precise and accurate mass calibration is required to exploit galaxy clusters as astrophysical and cosmological probes in the Euclid era. Systematic errors in lensing signals by galaxy clusters can be empirically estimated by comparing different surveys with independent and uncorrelated systematics. To assess the robustness of the lensing results to systematic errors, we carried out end-to-end test… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.08036v1-abstract-full').style.display = 'inline'; document.getElementById('2404.08036v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.08036v1-abstract-full" style="display: none;"> Precise and accurate mass calibration is required to exploit galaxy clusters as astrophysical and cosmological probes in the Euclid era. Systematic errors in lensing signals by galaxy clusters can be empirically estimated by comparing different surveys with independent and uncorrelated systematics. To assess the robustness of the lensing results to systematic errors, we carried out end-to-end tests across different data sets. We performed a unified analysis at the catalogue level by leveraging the Euclid combined cluster and weak-lensing pipeline (COMB-CL). COMB-CL will measure weak lensing cluster masses for the Euclid Survey. Heterogeneous data sets from five independent, recent, lensing surveys (CHFTLenS, DES~SV1, HSC-SSP~S16a, KiDS~DR4, and RCSLenS), which exploited different shear and photometric redshift estimation algorithms, were analysed with a consistent pipeline under the same model assumptions. We performed a comparison of the amplitude of the reduced excess surface density and of the mass estimates using lenses from the Planck PSZ2 and SDSS redMaPPer cluster samples. Mass estimates agree with literature results collected in the LC2 catalogues. Mass accuracy was further investigated considering the AMICO detected clusters in the HSC-SSP XXL North field. The consistency of the data sets was tested using our unified analysis framework. We found agreement between independent surveys, at the level of systematic noise in Stage-III surveys or precursors. This indicates successful control over systematics. If such control continues in Stage-IV, Euclid will be able to measure the weak lensing masses of around 13000 (considering shot noise only) or 3000 (noise from shape and large-scale-structure) massive clusters with a signal-to-noise ratio greater than 3. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.08036v1-abstract-full').style.display = 'none'; document.getElementById('2404.08036v1-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 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">25 pages; in press on A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.10187">arXiv:2402.10187</a> <span> [<a href="https://arxiv.org/pdf/2402.10187">pdf</a>, <a href="https://arxiv.org/format/2402.10187">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/10.1051/0004-6361/202449609">10.1051/0004-6361/202449609 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid preparation. XLIII. Measuring detailed galaxy morphologies for Euclid with machine learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aussel%2C+B">B. Aussel</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S">S. Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Walmsley%2C+M">M. Walmsley</a>, <a href="/search/astro-ph?searchtype=author&query=Huertas-Company%2C+M">M. Huertas-Company</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">C. J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Veneri%2C+M+D">M. Delli Veneri</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+H+D">H. Dom铆nguez S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P+-">P. -A. Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Kuchner%2C+U">U. Kuchner</a>, <a href="/search/astro-ph?searchtype=author&query=La+Marca%2C+A">A. La Marca</a>, <a href="/search/astro-ph?searchtype=author&query=Margalef-Bentabol%2C+B">B. Margalef-Bentabol</a>, <a href="/search/astro-ph?searchtype=author&query=Marleau%2C+F+R">F. R. Marleau</a>, <a href="/search/astro-ph?searchtype=author&query=Stevens%2C+G">G. Stevens</a>, <a href="/search/astro-ph?searchtype=author&query=Toba%2C+Y">Y. Toba</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">L. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Altieri%2C+B">B. Altieri</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+M">M. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a> , et al. (233 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="2402.10187v2-abstract-short" style="display: inline;"> The Euclid mission is expected to image millions of galaxies with high resolution, providing an extensive dataset to study galaxy evolution. We investigate the application of deep learning to predict the detailed morphologies of galaxies in Euclid using Zoobot a convolutional neural network pretrained with 450000 galaxies from the Galaxy Zoo project. We adapted Zoobot for emulated Euclid images, g… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.10187v2-abstract-full').style.display = 'inline'; document.getElementById('2402.10187v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.10187v2-abstract-full" style="display: none;"> The Euclid mission is expected to image millions of galaxies with high resolution, providing an extensive dataset to study galaxy evolution. We investigate the application of deep learning to predict the detailed morphologies of galaxies in Euclid using Zoobot a convolutional neural network pretrained with 450000 galaxies from the Galaxy Zoo project. We adapted Zoobot for emulated Euclid images, generated based on Hubble Space Telescope COSMOS images, and with labels provided by volunteers in the Galaxy Zoo: Hubble project. We demonstrate that the trained Zoobot model successfully measures detailed morphology for emulated Euclid images. It effectively predicts whether a galaxy has features and identifies and characterises various features such as spiral arms, clumps, bars, disks, and central bulges. When compared to volunteer classifications Zoobot achieves mean vote fraction deviations of less than 12% and an accuracy above 91% for the confident volunteer classifications across most morphology types. However, the performance varies depending on the specific morphological class. For the global classes such as disk or smooth galaxies, the mean deviations are less than 10%, with only 1000 training galaxies necessary to reach this performance. For more detailed structures and complex tasks like detecting and counting spiral arms or clumps, the deviations are slightly higher, around 12% with 60000 galaxies used for training. In order to enhance the performance on complex morphologies, we anticipate that a larger pool of labelled galaxies is needed, which could be obtained using crowdsourcing. Finally, our findings imply that the model can be effectively adapted to new morphological labels. We demonstrate this adaptability by applying Zoobot to peculiar galaxies. In summary, our trained Zoobot CNN can readily predict morphological catalogues for Euclid images. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.10187v2-abstract-full').style.display = 'none'; document.getElementById('2402.10187v2-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 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">27 pages, 26 figures, 5 tables, 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 689, A274 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.03436">arXiv:2402.03436</a> <span> [<a href="https://arxiv.org/pdf/2402.03436">pdf</a>, <a href="https://arxiv.org/format/2402.03436">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/10.1051/0004-6361/202449500">10.1051/0004-6361/202449500 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid preparation. Optical emission-line predictions of intermediate-z galaxy populations in GAEA for the Euclid Deep and Wide Surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Scharr%C3%A9%2C+L">L. Scharr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Hirschmann%2C+M">M. Hirschmann</a>, <a href="/search/astro-ph?searchtype=author&query=De+Lucia%2C+G">G. De Lucia</a>, <a href="/search/astro-ph?searchtype=author&query=Charlot%2C+S">S. Charlot</a>, <a href="/search/astro-ph?searchtype=author&query=Fontanot%2C+F">F. Fontanot</a>, <a href="/search/astro-ph?searchtype=author&query=Spinelli%2C+M">M. Spinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Xie%2C+L">L. Xie</a>, <a href="/search/astro-ph?searchtype=author&query=Feltre%2C+A">A. Feltre</a>, <a href="/search/astro-ph?searchtype=author&query=Allevato%2C+V">V. Allevato</a>, <a href="/search/astro-ph?searchtype=author&query=Plat%2C+A">A. Plat</a>, <a href="/search/astro-ph?searchtype=author&query=Bremer%2C+M+N">M. N. Bremer</a>, <a href="/search/astro-ph?searchtype=author&query=Fotopoulou%2C+S">S. Fotopoulou</a>, <a href="/search/astro-ph?searchtype=author&query=Gabarra%2C+L">L. Gabarra</a>, <a href="/search/astro-ph?searchtype=author&query=Granett%2C+B+R">B. R. Granett</a>, <a href="/search/astro-ph?searchtype=author&query=Moresco%2C+M">M. Moresco</a>, <a href="/search/astro-ph?searchtype=author&query=Scarlata%2C+C">C. Scarlata</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzetti%2C+L">L. Pozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Spinoglio%2C+L">L. Spinoglio</a>, <a href="/search/astro-ph?searchtype=author&query=Talia%2C+M">M. Talia</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</a>, <a href="/search/astro-ph?searchtype=author&query=Altieri%2C+B">B. Altieri</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a> , et al. (217 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="2402.03436v1-abstract-short" style="display: inline;"> In anticipation of the Euclid Wide and Deep Surveys, we present optical emission-line predictions at intermediate redshifts from 0.4 to 2.5. Our approach combines a mock light cone from the GAEA semi-analytic model to self-consistently model nebular emission from HII regions, narrow-line regions of active galactic nuclei (AGN), and evolved stellar populations. Our analysis focuses on seven optical… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.03436v1-abstract-full').style.display = 'inline'; document.getElementById('2402.03436v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.03436v1-abstract-full" style="display: none;"> In anticipation of the Euclid Wide and Deep Surveys, we present optical emission-line predictions at intermediate redshifts from 0.4 to 2.5. Our approach combines a mock light cone from the GAEA semi-analytic model to self-consistently model nebular emission from HII regions, narrow-line regions of active galactic nuclei (AGN), and evolved stellar populations. Our analysis focuses on seven optical emission lines: H$伪$, H$尾$, [SII]$位位6717, 6731$, [NII]$位6584$, [OI]$位6300$, [OIII]$位5007$, and [OII]$位位3727, 3729$. We find that Euclid will predominantly observe massive, star-forming, and metal-rich line-emitters. Interstellar dust, modelled using a Calzetti law with mass-dependent scaling, may decrease observable percentages by a further 20-30% with respect to our underlying emission-line populations from GAEA. We predict Euclid to observe around 30-70% of H$伪$-, [NII]-, [SII]-, and [OIII]-emitting galaxies at redshift below 1 and under 10% at higher redshift. Observability of H$尾$-, [OII]-, and [OI]- emission is limited to below 5%. For the Euclid-observable sample, we find that BPT diagrams can effectively distinguish between different galaxy types up to around redshift 1.8, attributed to the bias toward metal-rich systems. Moreover, we show that the relationships of H$伪$ and [OIII]+H$尾$ to the star-formation rate, and the [OIII]-AGN luminosity relation, exhibit minimal changes with increasing redshift. Based on line ratios [NII]/H$伪$, [NII]/[OII], and [NII]/[SII], we further propose novel z-invariant tracers for the black hole accretion rate-to-star formation rate ratio. Lastly, we find that commonly used metallicity estimators display gradual shifts in normalisations with increasing redshift, while maintaining the overall shape of local calibrations. This is in tentative agreement with recent JWST data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.03436v1-abstract-full').style.display = 'none'; document.getElementById('2402.03436v1-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 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">32 pages, 15 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 689, A276 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.17945">arXiv:2401.17945</a> <span> [<a href="https://arxiv.org/pdf/2401.17945">pdf</a>, <a href="https://arxiv.org/format/2401.17945">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> Euclid preparation XLVI. The Near-IR Background Dipole Experiment with Euclid </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Kashlinsky%2C+A">A. Kashlinsky</a>, <a href="/search/astro-ph?searchtype=author&query=Arendt%2C+R+G">R. G. Arendt</a>, <a href="/search/astro-ph?searchtype=author&query=Ashby%2C+M+L+N">M. L. N. Ashby</a>, <a href="/search/astro-ph?searchtype=author&query=Atrio-Barandela%2C+F">F. Atrio-Barandela</a>, <a href="/search/astro-ph?searchtype=author&query=Scaramella%2C+R">R. Scaramella</a>, <a href="/search/astro-ph?searchtype=author&query=Strauss%2C+M+A">M. A. Strauss</a>, <a href="/search/astro-ph?searchtype=author&query=Altieri%2C+B">B. Altieri</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+M">M. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+R">R. Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Bodendorf%2C+C">C. Bodendorf</a>, <a href="/search/astro-ph?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">J. Brinchmann</a>, <a href="/search/astro-ph?searchtype=author&query=Camera%2C+S">S. Camera</a>, <a href="/search/astro-ph?searchtype=author&query=Capobianco%2C+V">V. Capobianco</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+C">C. Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Casas%2C+S">S. Casas</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cavuoti%2C+S">S. Cavuoti</a> , et al. (195 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="2401.17945v2-abstract-short" style="display: inline;"> Verifying the fully kinematic nature of the cosmic microwave background (CMB) dipole is of fundamental importance in cosmology. In the standard cosmological model with the Friedman-Lemaitre-Robertson-Walker (FLRW) metric from the inflationary expansion the CMB dipole should be entirely kinematic. Any non-kinematic CMB dipole component would thus reflect the preinflationary structure of spacetime p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17945v2-abstract-full').style.display = 'inline'; document.getElementById('2401.17945v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.17945v2-abstract-full" style="display: none;"> Verifying the fully kinematic nature of the cosmic microwave background (CMB) dipole is of fundamental importance in cosmology. In the standard cosmological model with the Friedman-Lemaitre-Robertson-Walker (FLRW) metric from the inflationary expansion the CMB dipole should be entirely kinematic. Any non-kinematic CMB dipole component would thus reflect the preinflationary structure of spacetime probing the extent of the FLRW applicability. Cosmic backgrounds from galaxies after the matter-radiation decoupling, should have kinematic dipole component identical in velocity with the CMB kinematic dipole. Comparing the two can lead to isolating the CMB non-kinematic dipole. It was recently proposed that such measurement can be done using the near-IR cosmic infrared background (CIB) measured with the currently operating Euclid telescope, and later with Roman. The proposed method reconstructs the resolved CIB, the Integrated Galaxy Light (IGL), from Euclid's Wide Survey and probes its dipole, with a kinematic component amplified over that of the CMB by the Compton-Getting effect. The amplification coupled with the extensive galaxy samples forming the IGL would determine the CIB dipole with an overwhelming signal/noise, isolating its direction to sub-degree accuracy. We develop details of the method for Euclid's Wide Survey in 4 bands spanning 0.6 to 2 mic. We isolate the systematic and other uncertainties and present methodologies to minimize them, after confining the sample to the magnitude range with negligible IGL/CIB dipole from galaxy clustering. These include the required star-galaxy separation, accounting for the extinction correction dipole using the method newly developed here achieving total separation, accounting for the Earth's orbital motion and other systematic effects. (Abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.17945v2-abstract-full').style.display = 'none'; document.getElementById('2401.17945v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Euclid Key Project paper, A&A, in press</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.16239">arXiv:2401.16239</a> <span> [<a href="https://arxiv.org/pdf/2401.16239">pdf</a>, <a href="https://arxiv.org/format/2401.16239">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The polarization of the boundary layer around weakly magnetized neutron stars in X-ray binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">R. Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Waghmare%2C+A">A. Waghmare</a>, <a href="/search/astro-ph?searchtype=author&query=Ducci%2C+L">L. Ducci</a>, <a href="/search/astro-ph?searchtype=author&query=Santangelo%2C+A">A. Santangelo</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.16239v1-abstract-short" style="display: inline;"> X-ray binaries hosting a compact object have been among the main targets of the Imaging X-ray Polarimetry Explorer (IXPE) since its launch, due to their high brightness in the 2-8 keV energy band. The spectropolarimetric analysis performed so far has proved to be of great importance in providing constraints on the accretion geometry of these systems. However, the data statistics is not enough to u… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16239v1-abstract-full').style.display = 'inline'; document.getElementById('2401.16239v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.16239v1-abstract-full" style="display: none;"> X-ray binaries hosting a compact object have been among the main targets of the Imaging X-ray Polarimetry Explorer (IXPE) since its launch, due to their high brightness in the 2-8 keV energy band. The spectropolarimetric analysis performed so far has proved to be of great importance in providing constraints on the accretion geometry of these systems. However, the data statistics is not enough to unambiguously disentangle the contribution of the single components to the net observed polarimetric signal. In this work, we aim to present a model for computing the polarization degree and polarization angle of the boundary layer around weakly magnetized neutron stars in low-mass X-ray binaries in the soft state. The main motivation is to provide strong theoretical support to data interpretation of observations performed by IXPE or future satellites for X-ray polarimetry. The results were obtained by modeling the boundary layer as an equatorial belt around the compact object and locally approximating it as a plane-parallel scattering atmosphere, for which the associated radiative transfer equation for polarized radiation in the Thomson limit was solved. The polarimetric quantities were then transformed from the comoving frame to the observer frame using the numerical methods formerly developed for X-ray pulsars. For typical values of the optical depth and electron temperature of the boundary layer of these systems in a soft state, the polarization degree was less then 0.5\%, while the polarization angle was rotated by $\protect \la 5^{\circ}$ with respect to the neutron star spin axis due to special and general relativistic effects for fast rotation, the amount progressively decreasing for lower spin frequencies. The derived quantities can be used to remove degeneracy when multicomponent spectropolarimetry is performed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16239v1-abstract-full').style.display = 'none'; document.getElementById('2401.16239v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 8 figures, 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/2401.01452">arXiv:2401.01452</a> <span> [<a href="https://arxiv.org/pdf/2401.01452">pdf</a>, <a href="https://arxiv.org/format/2401.01452">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202349128">10.1051/0004-6361/202349128 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid preparation: XLVIII. The pre-launch Science Ground Segment simulation framework </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Serrano%2C+S">S. Serrano</a>, <a href="/search/astro-ph?searchtype=author&query=Hudelot%2C+P">P. Hudelot</a>, <a href="/search/astro-ph?searchtype=author&query=Seidel%2C+G">G. Seidel</a>, <a href="/search/astro-ph?searchtype=author&query=Pollack%2C+J+E">J. E. Pollack</a>, <a href="/search/astro-ph?searchtype=author&query=Jullo%2C+E">E. Jullo</a>, <a href="/search/astro-ph?searchtype=author&query=Torradeflot%2C+F">F. Torradeflot</a>, <a href="/search/astro-ph?searchtype=author&query=Benielli%2C+D">D. Benielli</a>, <a href="/search/astro-ph?searchtype=author&query=Fahed%2C+R">R. Fahed</a>, <a href="/search/astro-ph?searchtype=author&query=Auphan%2C+T">T. Auphan</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Aussel%2C+H">H. Aussel</a>, <a href="/search/astro-ph?searchtype=author&query=Casenove%2C+P">P. Casenove</a>, <a href="/search/astro-ph?searchtype=author&query=Castander%2C+F+J">F. J. Castander</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+J+E">J. E. Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Fourmanoit%2C+N">N. Fourmanoit</a>, <a href="/search/astro-ph?searchtype=author&query=Huot%2C+S">S. Huot</a>, <a href="/search/astro-ph?searchtype=author&query=Kara%2C+A">A. Kara</a>, <a href="/search/astro-ph?searchtype=author&query=Keih%C3%A4nen%2C+E">E. Keih盲nen</a>, <a href="/search/astro-ph?searchtype=author&query=Kermiche%2C+S">S. Kermiche</a>, <a href="/search/astro-ph?searchtype=author&query=Okumura%2C+K">K. Okumura</a>, <a href="/search/astro-ph?searchtype=author&query=Zoubian%2C+J">J. Zoubian</a>, <a href="/search/astro-ph?searchtype=author&query=Ealet%2C+A">A. Ealet</a>, <a href="/search/astro-ph?searchtype=author&query=Boucaud%2C+A">A. Boucaud</a>, <a href="/search/astro-ph?searchtype=author&query=Bretonni%C3%A8re%2C+H">H. Bretonni猫re</a> , et al. (252 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="2401.01452v2-abstract-short" style="display: inline;"> The European Space Agency's Euclid mission is one of the upcoming generation of large-scale cosmology surveys, which will map the large-scale structure in the Universe with unprecedented precision. The development and validation of the SGS pipeline requires state-of-the-art simulations with a high level of complexity and accuracy that include subtle instrumental features not accounted for previous… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.01452v2-abstract-full').style.display = 'inline'; document.getElementById('2401.01452v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.01452v2-abstract-full" style="display: none;"> The European Space Agency's Euclid mission is one of the upcoming generation of large-scale cosmology surveys, which will map the large-scale structure in the Universe with unprecedented precision. The development and validation of the SGS pipeline requires state-of-the-art simulations with a high level of complexity and accuracy that include subtle instrumental features not accounted for previously as well as faster algorithms for the large-scale production of the expected Euclid data products. In this paper, we present the Euclid SGS simulation framework as applied in a large-scale end-to-end simulation exercise named Science Challenge 8. Our simulation pipeline enables the swift production of detailed image simulations for the construction and validation of the Euclid mission during its qualification phase and will serve as a reference throughout operations. Our end-to-end simulation framework starts with the production of a large cosmological N-body & mock galaxy catalogue simulation. We perform a selection of galaxies down to I_E=26 and 28 mag, respectively, for a Euclid Wide Survey spanning 165 deg^2 and a 1 deg^2 Euclid Deep Survey. We build realistic stellar density catalogues containing Milky Way-like stars down to H<26. Using the latest instrumental models for both the Euclid instruments and spacecraft as well as Euclid-like observing sequences, we emulate with high fidelity Euclid satellite imaging throughout the mission's lifetime. We present the SC8 data set consisting of overlapping visible and near-infrared Euclid Wide Survey and Euclid Deep Survey imaging and low-resolution spectroscopy along with ground-based. This extensive data set enables end-to-end testing of the entire ground segment data reduction and science analysis pipeline as well as the Euclid mission infrastructure, paving the way to future scientific and technical developments and enhancements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.01452v2-abstract-full').style.display = 'none'; document.getElementById('2401.01452v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">39 pages, 25 figures, A&A submitted</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A103 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.14779">arXiv:2312.14779</a> <span> [<a href="https://arxiv.org/pdf/2312.14779">pdf</a>, <a href="https://arxiv.org/format/2312.14779">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"> Polarised light from accreting low mass X-ray binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Capitanio%2C+F">F. Capitanio</a>, <a href="/search/astro-ph?searchtype=author&query=Gnarini%2C+A">A. Gnarini</a>, <a href="/search/astro-ph?searchtype=author&query=Fabiani%2C+S">S. Fabiani</a>, <a href="/search/astro-ph?searchtype=author&query=Ursini%2C+F">F. Ursini</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">R. Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cocchi%2C+M">M. Cocchi</a>, <a href="/search/astro-ph?searchtype=author&query=Cavero%2C+N+R">N. Rodriguez Cavero</a>, <a href="/search/astro-ph?searchtype=author&query=Marra%2C+L">L. Marra</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.14779v1-abstract-short" style="display: inline;"> Thanks to IXPE , the X-ray spectro-polarimeter launched at the end of 2021, X-ray polarimetry has finally become an extraordinary tool in investigating the physics of accretion in low mass X-ray binaries. Similarly to what happened with gravitational waves, X-ray polarimetry would play a new complementary but at the same time fundamental role in the high-energy astrophysical domain. We summarize h… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.14779v1-abstract-full').style.display = 'inline'; document.getElementById('2312.14779v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.14779v1-abstract-full" style="display: none;"> Thanks to IXPE , the X-ray spectro-polarimeter launched at the end of 2021, X-ray polarimetry has finally become an extraordinary tool in investigating the physics of accretion in low mass X-ray binaries. Similarly to what happened with gravitational waves, X-ray polarimetry would play a new complementary but at the same time fundamental role in the high-energy astrophysical domain. We summarize here the first 1.5 year results on accreting low-mass X-ray binaries obtained by a huge IXPE observation campaign coordinated with the principal X-ray and Gamma-ray telescopes. Then we compare these results with the theoretical prediction highlighting the unexpected results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.14779v1-abstract-full').style.display = 'none'; document.getElementById('2312.14779v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">Proceeding presented at the Fifth Zeldovich meeting, an international conference held in Yerevan, Armenia on June 12-16, 2023. To be published in Astronomy Report</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.06359">arXiv:2311.06359</a> <span> [<a href="https://arxiv.org/pdf/2311.06359">pdf</a>, <a href="https://arxiv.org/format/2311.06359">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ad132d">10.3847/2041-8213/ad132d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Highly Significant Detection of X-Ray Polarization from the Brightest Accreting Neutron Star Sco X-1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=La+Monaca%2C+F">Fabio La Monaca</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marco%2C+A">Alessandro Di Marco</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">Juri Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Bachetti%2C+M">Matteo Bachetti</a>, <a href="/search/astro-ph?searchtype=author&query=Motta%2C+S+E">Sara E. Motta</a>, <a href="/search/astro-ph?searchtype=author&query=Papitto%2C+A">Alessandro Papitto</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">Maura Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Xie%2C+F">Fei Xie</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">Stefano Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Bobrikova%2C+A">Anna Bobrikova</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+E">Enrico Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+W">Wei Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Ge%2C+M">Mingyu Ge</a>, <a href="/search/astro-ph?searchtype=author&query=Illiano%2C+G">Giulia Illiano</a>, <a href="/search/astro-ph?searchtype=author&query=Jia%2C+S">Shu-Mei Jia</a>, <a href="/search/astro-ph?searchtype=author&query=Krawczynski%2C+H">Henric Krawczynski</a>, <a href="/search/astro-ph?searchtype=author&query=Lai%2C+E+V">Eleonora V. Lai</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+K">Kuan Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Mastroserio%2C+G">Guglielmo Mastroserio</a>, <a href="/search/astro-ph?searchtype=author&query=Muleri%2C+F">Fabio Muleri</a>, <a href="/search/astro-ph?searchtype=author&query=Rankin%2C+J">John Rankin</a>, <a href="/search/astro-ph?searchtype=author&query=Soffitta%2C+P">Paolo Soffitta</a>, <a href="/search/astro-ph?searchtype=author&query=Veledina%2C+A">Alexandra Veledina</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosino%2C+F">Filippo Ambrosino</a>, <a href="/search/astro-ph?searchtype=author&query=Del+Santo%2C+M">Melania Del Santo</a> , et al. (94 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="2311.06359v3-abstract-short" style="display: inline;"> The Imaging X-ray Polarimetry Explorer (IXPE) measured with high significance the X-ray polarization of the brightest Z-source Scorpius X-1, resulting in the nominal 2-8 keV energy band in a polarization degree of 1.0(0.2)% and a polarization angle of 8(6)掳 at 90% of confidence level. This observation was strictly simultaneous with observations performed by NICER, NuSTAR, and Insight-HXMT, which a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.06359v3-abstract-full').style.display = 'inline'; document.getElementById('2311.06359v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.06359v3-abstract-full" style="display: none;"> The Imaging X-ray Polarimetry Explorer (IXPE) measured with high significance the X-ray polarization of the brightest Z-source Scorpius X-1, resulting in the nominal 2-8 keV energy band in a polarization degree of 1.0(0.2)% and a polarization angle of 8(6)掳 at 90% of confidence level. This observation was strictly simultaneous with observations performed by NICER, NuSTAR, and Insight-HXMT, which allowed for a precise characterization of its broad-band spectrum from soft to hard X-rays. The source has been observed mainly in its soft state, with short periods of flaring. We also observed low-frequency quasi-periodic oscillations. From a spectro-polarimetric analysis, we associate a polarization to the accretion disk at <3.2% at 90% of confidence level, compatible with expectations for an electron-scattering dominated optically thick atmosphere at the Sco X-1 inclination of 44掳; for the higher-energy Comptonized component, we obtain a polarization of 1.3(0.4)%, in agreement with expectations for a slab of Thomson optical depth of ~7 and an electron temperature of ~3 keV. A polarization rotation with respect to previous observations by OSO-8 and PolarLight, and also with respect to the radio-jet position angle, is observed. This result may indicate a variation of the polarization with the source state that can be related to relativistic precession or to a change in the corona geometry with the accretion flow. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.06359v3-abstract-full').style.display = 'none'; document.getElementById('2311.06359v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL 960 L11 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.04632">arXiv:2311.04632</a> <span> [<a href="https://arxiv.org/pdf/2311.04632">pdf</a>, <a href="https://arxiv.org/format/2311.04632">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/ad1832">10.3847/2041-8213/ad1832 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-Ray Polarized View on the Accretion Geometry in the X-Ray Binary Circinus X-1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rankin%2C+J">John Rankin</a>, <a href="/search/astro-ph?searchtype=author&query=La+Monaca%2C+F">Fabio La Monaca</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marco%2C+A">Alessandro Di Marco</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">Juri Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Bobrikova%2C+A">Anna Bobrikova</a>, <a href="/search/astro-ph?searchtype=author&query=Kravtsov%2C+V">Vadim Kravtsov</a>, <a href="/search/astro-ph?searchtype=author&query=Muleri%2C+F">Fabio Muleri</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">Maura Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Veledina%2C+A">Alexandra Veledina</a>, <a href="/search/astro-ph?searchtype=author&query=Fender%2C+R">Rob Fender</a>, <a href="/search/astro-ph?searchtype=author&query=Kaaret%2C+P">Philip Kaaret</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D+E">Dawoon E. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Marinucci%2C+A">Andrea Marinucci</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+H+L">Herman L. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Papitto%2C+A">Alessandro Papitto</a>, <a href="/search/astro-ph?searchtype=author&query=Tennant%2C+A+F">Allyn F. Tennant</a>, <a href="/search/astro-ph?searchtype=author&query=Tsygankov%2C+S+S">Sergey S. Tsygankov</a>, <a href="/search/astro-ph?searchtype=author&query=Weisskopf%2C+M+C">Martin C. Weisskopf</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+K">Kinwah Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Zane%2C+S">Silvia Zane</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosino%2C+F">Filippo Ambrosino</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">Ruben Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Gnarini%2C+A">Andrea Gnarini</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">Iv谩n Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">Lucio A. Antonelli</a> , et al. (79 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="2311.04632v2-abstract-short" style="display: inline;"> Cir X-1 is a neutron star X-ray binary characterized by strong variations in flux during its eccentric $\sim$16.6 days orbit. There are also strong variations in the spectral state, and historically it has shown both atoll and Z state properties. We observed the source with the Imaging X-ray Polarimetry Explorer during two orbital segments, 6 days apart, for a total of 263~ks. We find an X-ray pol… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04632v2-abstract-full').style.display = 'inline'; document.getElementById('2311.04632v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.04632v2-abstract-full" style="display: none;"> Cir X-1 is a neutron star X-ray binary characterized by strong variations in flux during its eccentric $\sim$16.6 days orbit. There are also strong variations in the spectral state, and historically it has shown both atoll and Z state properties. We observed the source with the Imaging X-ray Polarimetry Explorer during two orbital segments, 6 days apart, for a total of 263~ks. We find an X-ray polarization degree in these segments of $1.6\%\pm0.3\%$ and $1.4\%\pm0.3\%$ at polarization angles of $37^\circ\pm5^\circ$ and $-12^\circ\pm7^\circ$, respectively. Thus we observed a rotation of the polarization angle by $49^\circ\pm8^\circ$ along the orbit. Because variations of accretion flow, and then of the hardness ratio, are expected during the orbit, we also studied the polarization binned in hardness ratio, and found the polarization angle differing by $67^\circ\pm11^\circ$ between the lowest and highest values of the hardness ratio. We discuss possible interpretations of this result that could indicate a possible misalignment between the symmetry axes of the accretion disk and the Comptonizing region caused by the misalignment of the neutron star's angular momentum with respect to the orbital one. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.04632v2-abstract-full').style.display = 'none'; document.getElementById('2311.04632v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 6 figures, Accepted for publication in ApJL</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJL 961 L8 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.03202">arXiv:2311.03202</a> <span> [<a href="https://arxiv.org/pdf/2311.03202">pdf</a>, <a href="https://arxiv.org/format/2311.03202">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/10.1117/12.2629843">10.1117/12.2629843 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid's Near-Infrared Spectrometer and Photometer ready for flight -- review of final performance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Medinaceli%2C+E">E. Medinaceli</a>, <a href="/search/astro-ph?searchtype=author&query=Valenziano%2C+L">L. Valenziano</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Franceschi%2C+E">E. Franceschi</a>, <a href="/search/astro-ph?searchtype=author&query=Gianotti%2C+F">F. Gianotti</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+P">P. Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">R. Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Balestra%2C+A">A. Balestra</a>, <a href="/search/astro-ph?searchtype=author&query=Dusini%2C+S">S. Dusini</a>, <a href="/search/astro-ph?searchtype=author&query=Sirignano%2C+C">C. Sirignano</a>, <a href="/search/astro-ph?searchtype=author&query=Borsato%2C+E">E. Borsato</a>, <a href="/search/astro-ph?searchtype=author&query=Stanco%2C+L">L. Stanco</a>, <a href="/search/astro-ph?searchtype=author&query=Renzi%2C+A">A. Renzi</a>, <a href="/search/astro-ph?searchtype=author&query=Troja%2C+A">A. Troja</a>, <a href="/search/astro-ph?searchtype=author&query=Gabarra%2C+L">L. Gabarra</a>, <a href="/search/astro-ph?searchtype=author&query=Ligori%2C+S">S. Ligori</a>, <a href="/search/astro-ph?searchtype=author&query=Capobianco%2C+V">V. Capobianco</a>, <a href="/search/astro-ph?searchtype=author&query=Corcione%2C+L">L. Corcione</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+D">D. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Sirri%2C+G">G. Sirri</a>, <a href="/search/astro-ph?searchtype=author&query=Patrizii%2C+L">L. Patrizii</a>, <a href="/search/astro-ph?searchtype=author&query=Tenti%2C+M">M. Tenti</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Ferdinando%2C+D">D. Di Ferdinando</a>, <a href="/search/astro-ph?searchtype=author&query=Valieri%2C+C">C. Valieri</a>, <a href="/search/astro-ph?searchtype=author&query=Mauri%2C+N">N. Mauri</a> , et al. (22 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="2311.03202v1-abstract-short" style="display: inline;"> ESA's mission Euclid, while undertaking its final integration stage, is fully qualified. Euclid will perform an extragalactic survey ($0<z<2$) by observing in the visible and near-infrared wavelength range. To detect infrared radiation, it is equipped with the Near Infrared Spectrometer and Photometer (NISP) instrument, operating in the 0.9--2 $渭$m range. In this paper, after introducing the surve… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03202v1-abstract-full').style.display = 'inline'; document.getElementById('2311.03202v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.03202v1-abstract-full" style="display: none;"> ESA's mission Euclid, while undertaking its final integration stage, is fully qualified. Euclid will perform an extragalactic survey ($0<z<2$) by observing in the visible and near-infrared wavelength range. To detect infrared radiation, it is equipped with the Near Infrared Spectrometer and Photometer (NISP) instrument, operating in the 0.9--2 $渭$m range. In this paper, after introducing the survey strategy, we focus our attention on the NISP Data Processing Unit's Application Software, highlighting the experimental process to obtain the final parametrization of the on-board processing of data produced by the array of 16 Teledyne HAWAII-2RG (HgCdTe) detectors. We report results from the latest ground test campaigns with the flight configuration hardware - complete optical system (Korsh anastigmat telescope), detectors array (0.56 deg$^2$ field of view), and readout systems (16 Digital Control Units and Sidecar ASICs). The performance of the on-board processing is then presented. We also describe a major issue found during the final test phase. We show how the problem was identified and solved thanks to an intensive coordinated effort of an independent review `Tiger' team, lead by ESA, and a team of NISP experts from the Euclid Consortium. An extended PLM level campaign at ambient temperature in Li猫ge and a dedicated test campaign conducted in Marseille on the NISP EQM model eventually confirmed the resolution of the problem. Finally, we report examples of the outstanding spectrometric (using a Blue and two Red Grisms) and photometric performance of the NISP instrument, as derived from the end-to-end payload module test campaign at FOCAL 5 -- CSL; these results include the photometric Point Spread Function (PSF) determination and the spectroscopic dispersion verification. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.03202v1-abstract-full').style.display = 'none'; document.getElementById('2311.03202v1-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proc. SPIE 12180, Space Telescopes and Instrumentation 2022: Optical, Infrared, and Millimeter Wave, 121801L (27 August 2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.15731">arXiv:2310.15731</a> <span> [<a href="https://arxiv.org/pdf/2310.15731">pdf</a>, <a href="https://arxiv.org/format/2310.15731">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202348389">10.1051/0004-6361/202348389 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid preparation. LII. Forecast impact of super-sample covariance on 3x2pt analysis with Euclid </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Sciotti%2C+D">D. Sciotti</a>, <a href="/search/astro-ph?searchtype=author&query=Beauchamps%2C+S+G">S. Gouyou Beauchamps</a>, <a href="/search/astro-ph?searchtype=author&query=Cardone%2C+V+F">V. F. Cardone</a>, <a href="/search/astro-ph?searchtype=author&query=Camera%2C+S">S. Camera</a>, <a href="/search/astro-ph?searchtype=author&query=Tutusaus%2C+I">I. Tutusaus</a>, <a href="/search/astro-ph?searchtype=author&query=Lacasa%2C+F">F. Lacasa</a>, <a href="/search/astro-ph?searchtype=author&query=Barreira%2C+A">A. Barreira</a>, <a href="/search/astro-ph?searchtype=author&query=Bonici%2C+M">M. Bonici</a>, <a href="/search/astro-ph?searchtype=author&query=Gorce%2C+A">A. Gorce</a>, <a href="/search/astro-ph?searchtype=author&query=Aubert%2C+M">M. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Baratta%2C+P">P. Baratta</a>, <a href="/search/astro-ph?searchtype=author&query=Upham%2C+R+E">R. E. Upham</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+C">C. Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Casas%2C+S">S. Casas</a>, <a href="/search/astro-ph?searchtype=author&query=Ili%C4%87%2C+S">S. Ili膰</a>, <a href="/search/astro-ph?searchtype=author&query=Martinelli%2C+M">M. Martinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Sakr%2C+Z">Z. Sakr</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+A">A. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Maoli%2C+R">R. Maoli</a>, <a href="/search/astro-ph?searchtype=author&query=Scaramella%2C+R">R. Scaramella</a>, <a href="/search/astro-ph?searchtype=author&query=Escoffier%2C+S">S. Escoffier</a>, <a href="/search/astro-ph?searchtype=author&query=Gillard%2C+W">W. Gillard</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a> , et al. (199 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="2310.15731v2-abstract-short" style="display: inline;"> Deviations from Gaussianity in the distribution of the fields probed by large-scale structure surveys generate additional terms in the data covariance matrix, increasing the uncertainties in the measurement of the cosmological parameters. Super-sample covariance (SSC) is among the largest of these non-Gaussian contributions, with the potential to significantly degrade constraints on some of the pa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.15731v2-abstract-full').style.display = 'inline'; document.getElementById('2310.15731v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.15731v2-abstract-full" style="display: none;"> Deviations from Gaussianity in the distribution of the fields probed by large-scale structure surveys generate additional terms in the data covariance matrix, increasing the uncertainties in the measurement of the cosmological parameters. Super-sample covariance (SSC) is among the largest of these non-Gaussian contributions, with the potential to significantly degrade constraints on some of the parameters of the cosmological model under study - especially for weak lensing cosmic shear. We compute and validate the impact of SSC on the forecast uncertainties on the cosmological parameters for the Euclid photometric survey, obtained with a Fisher matrix analysis, both considering the Gaussian covariance alone and adding the SSC term - computed through the public code $\tt{PySSC}$. The photometric probes are considered in isolation and combined in the '3$\times$2pt' analysis. We find the SSC impact to be non-negligible - halving the Figure of Merit of the dark energy parameters $(w_0, w_a)$ in the 3$\times$2pt case and substantially increasing the uncertainties on $惟_{{\rm m}, 0}, w_0$, and $蟽_8$ for cosmic shear; photometric galaxy clustering, on the other hand, is less affected due to the lower probe response. The relative impact of SSC does not show significant changes under variations of the redshift binning scheme, while it is smaller for weak lensing when marginalising over the multiplicative shear bias nuisance parameters, which also leads to poorer constraints on the cosmological parameters. Finally, we explore how the use of prior information on the shear and galaxy bias changes the SSC impact. Improving shear bias priors does not have a significant impact, while galaxy bias must be calibrated to sub-percent level to increase the Figure of Merit by the large amount needed to achieve the value when SSC is not included. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.15731v2-abstract-full').style.display = 'none'; document.getElementById('2310.15731v2-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 13 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A318 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.11125">arXiv:2310.11125</a> <span> [<a href="https://arxiv.org/pdf/2310.11125">pdf</a>, <a href="https://arxiv.org/format/2310.11125">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"> IXPE observation confirms a high spin in the accreting black hole 4U 1957+115 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marra%2C+L">L. Marra</a>, <a href="/search/astro-ph?searchtype=author&query=Brigitte%2C+M">M. Brigitte</a>, <a href="/search/astro-ph?searchtype=author&query=Cavero%2C+N+R">N. Rodriguez Cavero</a>, <a href="/search/astro-ph?searchtype=author&query=Chun%2C+S">S. Chun</a>, <a href="/search/astro-ph?searchtype=author&query=Steiner%2C+J+F">J. F. Steiner</a>, <a href="/search/astro-ph?searchtype=author&query=Dov%C4%8Diak%2C+M">M. Dov膷iak</a>, <a href="/search/astro-ph?searchtype=author&query=Nowak%2C+M">M. Nowak</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Capitanio%2C+F">F. Capitanio</a>, <a href="/search/astro-ph?searchtype=author&query=Ingram%2C+A">A. Ingram</a>, <a href="/search/astro-ph?searchtype=author&query=Matt%2C+G">G. Matt</a>, <a href="/search/astro-ph?searchtype=author&query=Muleri%2C+F">F. Muleri</a>, <a href="/search/astro-ph?searchtype=author&query=Podgorn%C3%BD%2C+J">J. Podgorn媒</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">J. Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Svoboda%2C+J">J. Svoboda</a>, <a href="/search/astro-ph?searchtype=author&query=Taverna%2C+R">R. Taverna</a>, <a href="/search/astro-ph?searchtype=author&query=Ursini%2C+F">F. Ursini</a>, <a href="/search/astro-ph?searchtype=author&query=Veledina%2C+A">A. Veledina</a>, <a href="/search/astro-ph?searchtype=author&query=De+Rosa%2C+A">A. De Rosa</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia%2C+J+A">J. A. Garcia</a>, <a href="/search/astro-ph?searchtype=author&query=Lutovinov%2C+A+A">A. A. Lutovinov</a>, <a href="/search/astro-ph?searchtype=author&query=Mereminskiy%2C+I+A">I. A. Mereminskiy</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">R. Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Gunji%2C+S">S. Gunji</a>, <a href="/search/astro-ph?searchtype=author&query=Kaaret%2C+P">P. Kaaret</a> , et al. (91 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="2310.11125v2-abstract-short" style="display: inline;"> We present the results of the first X-ray polarimetric observation of the low-mass X-ray binary 4U 1957+115, performed with the Imaging X-ray Polarimetry Explorer in May 2023. The binary system has been in a high-soft spectral state since its discovery and is thought to host a black hole. The $\sim$571 ks observation reveals a linear polarisation degree of $1.9\% \pm 0.6\%$ and a polarisation angl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.11125v2-abstract-full').style.display = 'inline'; document.getElementById('2310.11125v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.11125v2-abstract-full" style="display: none;"> We present the results of the first X-ray polarimetric observation of the low-mass X-ray binary 4U 1957+115, performed with the Imaging X-ray Polarimetry Explorer in May 2023. The binary system has been in a high-soft spectral state since its discovery and is thought to host a black hole. The $\sim$571 ks observation reveals a linear polarisation degree of $1.9\% \pm 0.6\%$ and a polarisation angle of $-41^\circ.8 \pm 7^\circ.9$ in the 2-8 keV energy range. Spectral modelling is consistent with the dominant contribution coming from the standard accretion disc, while polarimetric data suggest a significant role of returning radiation: photons that are bent by strong gravity effects and forced to return to the disc surface, where they can be reflected before eventually reaching the observer. In this setting, we find that models with a black hole spin lower than 0.96 and an inclination lower than $50^\circ$ are disfavoured. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.11125v2-abstract-full').style.display = 'none'; document.getElementById('2310.11125v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 10 figures, 2 tables, 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/2310.06788">arXiv:2310.06788</a> <span> [<a href="https://arxiv.org/pdf/2310.06788">pdf</a>, <a href="https://arxiv.org/ps/2310.06788">ps</a>, <a href="https://arxiv.org/format/2310.06788">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"> Discovery of a variable energy-dependent X-ray polarization in the accreting neutron star GX 5-1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fabiani%2C+S">Sergio Fabiani</a>, <a href="/search/astro-ph?searchtype=author&query=Capitanio%2C+F">Fiamma Capitanio</a>, <a href="/search/astro-ph?searchtype=author&query=Iaria%2C+R">Rosario Iaria</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">Juri Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Gnarini%2C+A">Andrea Gnarini</a>, <a href="/search/astro-ph?searchtype=author&query=Ursini%2C+F">Francesco Ursini</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">Ruben Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bobrikova%2C+A">Anna Bobrikova</a>, <a href="/search/astro-ph?searchtype=author&query=Steiner%2C+J+F">James F. Steiner</a>, <a href="/search/astro-ph?searchtype=author&query=Svoboda%2C+J">Jiri Svoboda</a>, <a href="/search/astro-ph?searchtype=author&query=Anitra%2C+A">Alessio Anitra</a>, <a href="/search/astro-ph?searchtype=author&query=Baglio%2C+M+C">Maria C. Baglio</a>, <a href="/search/astro-ph?searchtype=author&query=Carotenuto%2C+F">Francesco Carotenuto</a>, <a href="/search/astro-ph?searchtype=author&query=Del+Santo%2C+M">Melania Del Santo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrigno%2C+C">Carlo Ferrigno</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+F">Fraser Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Russell%2C+D+M">David M. Russell</a>, <a href="/search/astro-ph?searchtype=author&query=Russell%2C+T+D">Thomas D. Russell</a>, <a href="/search/astro-ph?searchtype=author&query=Eijnden%2C+J+v+d">Jakob van den Eijnden</a>, <a href="/search/astro-ph?searchtype=author&query=Cocchi%2C+M">Massimo Cocchi</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marco%2C+A">Alessandro Di Marco</a>, <a href="/search/astro-ph?searchtype=author&query=La+Monaca%2C+F">Fabio La Monaca</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+K">Kuan Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Rankin%2C+J">John Rankin</a>, <a href="/search/astro-ph?searchtype=author&query=Weisskopf%2C+M+C">Martin C. Weisskopf</a> , et al. (94 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="2310.06788v2-abstract-short" style="display: inline;"> We report on the coordinated observations of the neutron star low-mass X-ray binary (NS-LMXB) \gx in X-rays (IXPE, NICER, Nustar and INTEGRAL), optical (REM and LCO), near-infrared (REM), mid-infrared (VLT VISIR), and radio (ATCA). This Z-source was observed by \IXPE twice in March-April 2023 (Obs. 1 and 2). In the radio band, the source was detected, but only upper-limits to the linear polarizati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06788v2-abstract-full').style.display = 'inline'; document.getElementById('2310.06788v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.06788v2-abstract-full" style="display: none;"> We report on the coordinated observations of the neutron star low-mass X-ray binary (NS-LMXB) \gx in X-rays (IXPE, NICER, Nustar and INTEGRAL), optical (REM and LCO), near-infrared (REM), mid-infrared (VLT VISIR), and radio (ATCA). This Z-source was observed by \IXPE twice in March-April 2023 (Obs. 1 and 2). In the radio band, the source was detected, but only upper-limits to the linear polarization were obtained at a $3蟽$ level of $6.1\%$ at 5.5 GHz and $5.9\%$ at 9 GHz in Obs.~1 and $12.5\%$ at 5.5~GHz and $20\%$ at 9~GHz in Obs.~2. The mid-IR, near-IR and optical observations suggest the presence of a compact jet which peaks in the mid- or far-IR. The X-ray polarization degree was found to be $3.7\% \pm 0.4 \%$ (at $90\%$ confidence level) during Obs.~1 when the source was in the horizontal branch of the Z-track and $1.8\% \pm 0.4 \%$ during Obs.~2 when the source was in the normal-flaring branch. These results confirm the variation of polarization degree as a function of the position of the source in the color-color diagram as for previously observed Z-track sources (Cyg~X-2 and XTE~1701$-$462). Evidence for a variation of the polarization angle $\sim 20^\circ$ with energy is found in both observations, likely related to the different, non-orthogonal polarization angles of the disk and Comptonization components which peak at different energies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06788v2-abstract-full').style.display = 'none'; document.getElementById('2310.06788v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to Astronomy and Astrophysics on 06 July 2023. Accepted on 21 November 2023</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.00052">arXiv:2309.00052</a> <span> [<a href="https://arxiv.org/pdf/2309.00052">pdf</a>, <a href="https://arxiv.org/format/2309.00052">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347870">10.1051/0004-6361/202347870 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid preparation. XXXIV. The effect of linear redshift-space distortions in photometric galaxy clustering and its cross-correlation with cosmic shear </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Tanidis%2C+K">K. Tanidis</a>, <a href="/search/astro-ph?searchtype=author&query=Cardone%2C+V+F">V. F. Cardone</a>, <a href="/search/astro-ph?searchtype=author&query=Martinelli%2C+M">M. Martinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Tutusaus%2C+I">I. Tutusaus</a>, <a href="/search/astro-ph?searchtype=author&query=Camera%2C+S">S. Camera</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+M">M. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">J. Brinchmann</a>, <a href="/search/astro-ph?searchtype=author&query=Capobianco%2C+V">V. Capobianco</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+C">C. Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Casas%2C+S">S. Casas</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cavuoti%2C+S">S. Cavuoti</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Cledassou%2C+R">R. Cledassou</a>, <a href="/search/astro-ph?searchtype=author&query=Congedo%2C+G">G. Congedo</a>, <a href="/search/astro-ph?searchtype=author&query=Conversi%2C+L">L. Conversi</a> , et al. (185 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="2309.00052v3-abstract-short" style="display: inline;"> The cosmological surveys that are planned for the current decade will provide us with unparalleled observations of the distribution of galaxies on cosmic scales, by means of which we can probe the underlying large-scale structure (LSS) of the Universe. This will allow us to test the concordance cosmological model and its extensions. However, precision pushes us to high levels of accuracy in the th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.00052v3-abstract-full').style.display = 'inline'; document.getElementById('2309.00052v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.00052v3-abstract-full" style="display: none;"> The cosmological surveys that are planned for the current decade will provide us with unparalleled observations of the distribution of galaxies on cosmic scales, by means of which we can probe the underlying large-scale structure (LSS) of the Universe. This will allow us to test the concordance cosmological model and its extensions. However, precision pushes us to high levels of accuracy in the theoretical modelling of the LSS observables, so that no biases are introduced into the estimation of the cosmological parameters. In particular, effects such as redshift-space distortions (RSD) can become relevant in the computation of harmonic-space power spectra even for the clustering of the photometrically selected galaxies, as has previously been shown in literature. In this work, we investigate the contribution of linear RSD, as formulated in the Limber approximation by a previous work, in forecast cosmological analyses with the photometric galaxy sample of the Euclid survey. We aim to assess their impact and to quantify the bias on the measurement of cosmological parameters that would be caused if this effect were neglected. We performed this task by producing mock power spectra for photometric galaxy clustering and weak lensing, as is expected to be obtained from the Euclid survey. We then used a Markov chain Monte Carlo approach to obtain the posterior distributions of cosmological parameters from these simulated observations. When the linear RSD is neglected, significant biases are caused when galaxy correlations are used alone and when they are combined with cosmic shear in the so-called 3$\times$2pt approach. These biases can be equivalent to as much as $5\,蟽$ when an underlying $螞$CDM cosmology is assumed. When the cosmological model is extended to include the equation-of-state parameters of dark energy, the extension parameters can be shifted by more than $1\,蟽$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.00052v3-abstract-full').style.display = 'none'; document.getElementById('2309.00052v3-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 6 figures. Version matching publication at journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.08736">arXiv:2307.08736</a> <span> [<a href="https://arxiv.org/pdf/2307.08736">pdf</a>, <a href="https://arxiv.org/format/2307.08736">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/10.1051/0004-6361/202347244">10.1051/0004-6361/202347244 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid Preparation XXXIII. Characterization of convolutional neural networks for the identification of galaxy-galaxy strong lensing events </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Leuzzi%2C+L">L. Leuzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Meneghetti%2C+M">M. Meneghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Angora%2C+G">G. Angora</a>, <a href="/search/astro-ph?searchtype=author&query=Metcalf%2C+R+B">R. B. Metcalf</a>, <a href="/search/astro-ph?searchtype=author&query=Moscardini%2C+L">L. Moscardini</a>, <a href="/search/astro-ph?searchtype=author&query=Rosati%2C+P">P. Rosati</a>, <a href="/search/astro-ph?searchtype=author&query=Bergamini%2C+P">P. Bergamini</a>, <a href="/search/astro-ph?searchtype=author&query=Calura%2C+F">F. Calura</a>, <a href="/search/astro-ph?searchtype=author&query=Cl%C3%A9ment%2C+B">B. Cl茅ment</a>, <a href="/search/astro-ph?searchtype=author&query=Gavazzi%2C+R">R. Gavazzi</a>, <a href="/search/astro-ph?searchtype=author&query=Gentile%2C+F">F. Gentile</a>, <a href="/search/astro-ph?searchtype=author&query=Lochner%2C+M">M. Lochner</a>, <a href="/search/astro-ph?searchtype=author&query=Grillo%2C+C">C. Grillo</a>, <a href="/search/astro-ph?searchtype=author&query=Vernardos%2C+G">G. Vernardos</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Amendola%2C+L">L. Amendola</a>, <a href="/search/astro-ph?searchtype=author&query=Andreon%2C+S">S. Andreon</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Bardelli%2C+S">S. Bardelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bodendorf%2C+C">C. Bodendorf</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+D">D. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a> , et al. (194 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="2307.08736v2-abstract-short" style="display: inline;"> Forthcoming imaging surveys will potentially increase the number of known galaxy-scale strong lenses by several orders of magnitude. For this to happen, images of tens of millions of galaxies will have to be inspected to identify potential candidates. In this context, deep learning techniques are particularly suitable for the finding patterns in large data sets, and convolutional neural networks (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.08736v2-abstract-full').style.display = 'inline'; document.getElementById('2307.08736v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.08736v2-abstract-full" style="display: none;"> Forthcoming imaging surveys will potentially increase the number of known galaxy-scale strong lenses by several orders of magnitude. For this to happen, images of tens of millions of galaxies will have to be inspected to identify potential candidates. In this context, deep learning techniques are particularly suitable for the finding patterns in large data sets, and convolutional neural networks (CNNs) in particular can efficiently process large volumes of images. We assess and compare the performance of three network architectures in the classification of strong lensing systems on the basis of their morphological characteristics. We train and test our models on different subsamples of a data set of forty thousand mock images, having characteristics similar to those expected in the wide survey planned with the ESA mission \Euclid, gradually including larger fractions of faint lenses. We also evaluate the importance of adding information about the colour difference between the lens and source galaxies by repeating the same training on single-band and multi-band images. Our models find samples of clear lenses with $\gtrsim 90\%$ precision and completeness, without significant differences in the performance of the three architectures. Nevertheless, when including lenses with fainter arcs in the training set, the three models' performance deteriorates with accuracy values of $\sim 0.87$ to $\sim 0.75$ depending on the model. Our analysis confirms the potential of the application of CNNs to the identification of galaxy-scale strong lenses. We suggest that specific training with separate classes of lenses might be needed for detecting the faint lenses since the addition of the colour information does not yield a significant improvement in the current analysis, with the accuracy ranging from $\sim 0.89$ to $\sim 0.78$ for the different models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.08736v2-abstract-full').style.display = 'none'; document.getElementById('2307.08736v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages,12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomy & Astrophysics,2024, 681, A68 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.10965">arXiv:2306.10965</a> <span> [<a href="https://arxiv.org/pdf/2306.10965">pdf</a>, <a href="https://arxiv.org/format/2306.10965">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346275">10.1051/0004-6361/202346275 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of strongly variable X-ray polarization in the neutron star low-mass X-ray binary transient XTE J1701$-$462 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cocchi%2C+M">Massimo Cocchi</a>, <a href="/search/astro-ph?searchtype=author&query=Gnarini%2C+A">Andrea Gnarini</a>, <a href="/search/astro-ph?searchtype=author&query=Fabiani%2C+S">Sergio Fabiani</a>, <a href="/search/astro-ph?searchtype=author&query=Ursini%2C+F">Francesco Ursini</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">Juri Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Capitanio%2C+F">Fiamma Capitanio</a>, <a href="/search/astro-ph?searchtype=author&query=Bobrikova%2C+A">Anna Bobrikova</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">Ruben Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Paizis%2C+A">Adamantia Paizis</a>, <a href="/search/astro-ph?searchtype=author&query=Sidoli%2C+L">Lara Sidoli</a>, <a href="/search/astro-ph?searchtype=author&query=Veledina%2C+A">Alexandra Veledina</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">Stefano Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marco%2C+A">Alessandro Di Marco</a>, <a href="/search/astro-ph?searchtype=author&query=Ingram%2C+A">Adam Ingram</a>, <a href="/search/astro-ph?searchtype=author&query=Kajava%2C+J+J+E">Jari J. E. Kajava</a>, <a href="/search/astro-ph?searchtype=author&query=La+Monaca%2C+F">Fabio La Monaca</a>, <a href="/search/astro-ph?searchtype=author&query=Matt%2C+G">Giorgio Matt</a>, <a href="/search/astro-ph?searchtype=author&query=Malacaria%2C+C">Christian Malacaria</a>, <a href="/search/astro-ph?searchtype=author&query=Miku%C5%A1incov%C3%A1%2C+R">Romana Miku拧incov谩</a>, <a href="/search/astro-ph?searchtype=author&query=Rankin%2C+J">John Rankin</a>, <a href="/search/astro-ph?searchtype=author&query=Zane%2C+S">Silvia Zane</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">Iv谩n Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">Lucio A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bachetti%2C+M">Matteo Bachetti</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+L">Luca Baldini</a> , et al. (83 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="2306.10965v1-abstract-short" style="display: inline;"> After about 16 years since its first outburst, the transient neutron star low-mass X-ray binary XTE J1701$-$462 turned on again in September 2022, allowing for the first study of its X-ray polarimetric characteristics by a dedicated observing program with the Imaging X-ray Polarimeter Explorer (IXPE). Polarimetric studies of XTE J1701$-$462 have been expected to improve our understanding of accret… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.10965v1-abstract-full').style.display = 'inline'; document.getElementById('2306.10965v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.10965v1-abstract-full" style="display: none;"> After about 16 years since its first outburst, the transient neutron star low-mass X-ray binary XTE J1701$-$462 turned on again in September 2022, allowing for the first study of its X-ray polarimetric characteristics by a dedicated observing program with the Imaging X-ray Polarimeter Explorer (IXPE). Polarimetric studies of XTE J1701$-$462 have been expected to improve our understanding of accreting weakly magnetized neutron stars, in particular, the physics and the geometry of the hot inner regions close to the compact object. The IXPE data of two triggered observations were analyzed using time-resolved spectroscopic and polarimetric techniques, following the source along its Z-track of the color-color diagram. During the first pointing on 2022 September 29, an average 2-8 keV polarization degree of 4.6$\pm$ 0.4\% was measured, the highest value found up to now for this class of sources. Conversely, only a $\sim$0.6\% average degree was obtained during the second pointing ten days later. The polarimetric signal appears to be strictly related to the higher energy blackbody component associated with the boundary layer (BL) emission and its reflection from the inner accretion disk, and it is as strong as 6.1\% and 1.2\% ($>95\%$ significant) above 3-4 keV for the two measurements, respectively. The variable polarimetric signal is apparently related to the spectral characteristics of XTE J1701$-$462, which is the strongest when the source was in the horizontal branch of its Z-track and the weakest in the normal branch. These IXPE results provide new important observational constraints on the physical models and geometry of the Z-sources. Here, we discuss the possible reasons for the presence of strong and variable polarization among these sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.10965v1-abstract-full').style.display = 'none'; document.getElementById('2306.10965v1-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 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">7 pages, 8 figures; published in A&A 674, L10 (2023)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 674, L10 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.08476">arXiv:2306.08476</a> <span> [<a href="https://arxiv.org/pdf/2306.08476">pdf</a>, <a href="https://arxiv.org/format/2306.08476">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/acec6e">10.3847/2041-8213/acec6e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First detection of X-ray polarization from the accreting neutron star 4U 1820-303 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Di+Marco%2C+A">Alessandro Di Marco</a>, <a href="/search/astro-ph?searchtype=author&query=La+Monaca%2C+F">Fabio La Monaca</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">Juri Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Russell%2C+T+D">Thomas D. Russell</a>, <a href="/search/astro-ph?searchtype=author&query=Anitra%2C+A">Alessio Anitra</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">Ruben Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Mastroserio%2C+G">Guglielmo Mastroserio</a>, <a href="/search/astro-ph?searchtype=author&query=Muleri%2C+F">Fabio Muleri</a>, <a href="/search/astro-ph?searchtype=author&query=Xie%2C+F">Fei Xie</a>, <a href="/search/astro-ph?searchtype=author&query=Bachetti%2C+M">Matteo Bachetti</a>, <a href="/search/astro-ph?searchtype=author&query=Burderi%2C+L">Luciano Burderi</a>, <a href="/search/astro-ph?searchtype=author&query=Carotenuto%2C+F">Francesco Carotenuto</a>, <a href="/search/astro-ph?searchtype=author&query=Del+Santo%2C+M">Melania Del Santo</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Salvo%2C+T">Tiziana Di Salvo</a>, <a href="/search/astro-ph?searchtype=author&query=Dovciak%2C+M">Michal Dovciak</a>, <a href="/search/astro-ph?searchtype=author&query=Gnarini%2C+A">Andrea Gnarini</a>, <a href="/search/astro-ph?searchtype=author&query=Iaria%2C+R">Rosario Iaria</a>, <a href="/search/astro-ph?searchtype=author&query=Kajava%2C+J+J+E">Jari J. E. Kajava</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+K">Kuan Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Middei%2C+R">Riccardo Middei</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Dell%2C+S+L">Stephen L. O'Dell</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">Maura Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Rankin%2C+J">John Rankin</a>, <a href="/search/astro-ph?searchtype=author&query=Sanna%2C+A">Andrea Sanna</a>, <a href="/search/astro-ph?searchtype=author&query=Eijnden%2C+J+v+d">Jakob van den Eijnden</a> , et al. (94 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="2306.08476v4-abstract-short" style="display: inline;"> This paper reports the first detection of polarization in the X-rays for atoll-source 4U 1820-303, obtained with the Imaging X-ray Polarimetry Explorer (IXPE) at 99.999% confidence level (CL). Simultaneous polarimetric measurements were also performed in the radio with the Australia Telescope Compact Array (ATCA). The IXPE observations of 4U 1820-303 were coordinated with Swift-XRT, NICER, and NuS… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.08476v4-abstract-full').style.display = 'inline'; document.getElementById('2306.08476v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.08476v4-abstract-full" style="display: none;"> This paper reports the first detection of polarization in the X-rays for atoll-source 4U 1820-303, obtained with the Imaging X-ray Polarimetry Explorer (IXPE) at 99.999% confidence level (CL). Simultaneous polarimetric measurements were also performed in the radio with the Australia Telescope Compact Array (ATCA). The IXPE observations of 4U 1820-303 were coordinated with Swift-XRT, NICER, and NuSTAR aiming to obtain an accurate X-ray spectral model covering a broad energy interval. The source shows a significant polarization above 4 keV, with a polarization degree of 2.0(0.5)% and a polarization angle of -55(7) deg in the 4-7 keV energy range, and a polarization degree of 10(2)% and a polarization angle of -67(7) deg in the 7-8 keV energy bin. This polarization also shows a clear energy trend with polarization degree increasing with energy and a hint for a position-angle change of about 90 deg at 96% CL around 4 keV. The spectro-polarimetric fit indicates that the accretion disk is polarized orthogonally to the hard spectral component, which is presumably produced in the boundary/spreading layer. We do not detect linear polarization from the radio counterpart, with a 99.97% upper limit of 50% at 7.25 GHz. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.08476v4-abstract-full').style.display = 'none'; document.getElementById('2306.08476v4-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 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">Journal ref:</span> ApJL 953 L22 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.02740">arXiv:2306.02740</a> <span> [<a href="https://arxiv.org/pdf/2306.02740">pdf</a>, <a href="https://arxiv.org/format/2306.02740">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346541">10.1051/0004-6361/202346541 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> X-ray polarimetry and spectroscopy of the neutron star low-mass X-ray binary GX 9+9: an in-depth study with IXPE and NuSTAR </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ursini%2C+F">F. Ursini</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">R. Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Gnarini%2C+A">A. Gnarini</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">J. Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Capitanio%2C+F">F. Capitanio</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Marco%2C+A">A. Di Marco</a>, <a href="/search/astro-ph?searchtype=author&query=Fabiani%2C+S">S. Fabiani</a>, <a href="/search/astro-ph?searchtype=author&query=La+Monaca%2C+F">F. La Monaca</a>, <a href="/search/astro-ph?searchtype=author&query=Malacaria%2C+C">C. Malacaria</a>, <a href="/search/astro-ph?searchtype=author&query=Matt%2C+G">G. Matt</a>, <a href="/search/astro-ph?searchtype=author&query=Miku%C5%A1incov%C3%A1%2C+R">R. Miku拧incov谩</a>, <a href="/search/astro-ph?searchtype=author&query=Cocchi%2C+M">M. Cocchi</a>, <a href="/search/astro-ph?searchtype=author&query=Kaaret%2C+P">P. Kaaret</a>, <a href="/search/astro-ph?searchtype=author&query=Kajava%2C+J+J+E">J. J. E. Kajava</a>, <a href="/search/astro-ph?searchtype=author&query=Pilia%2C+M">M. Pilia</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+W">W. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bachetti%2C+M">M. Bachetti</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+L">L. Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Baumgartner%2C+W+H">W. H. Baumgartner</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+R">R. Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+S+D">S. D. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+R">R. Bonino</a> , et al. (80 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="2306.02740v1-abstract-short" style="display: inline;"> We report on a comprehensive analysis of simultaneous X-ray polarimetric and spectral data of the bright atoll source GX 9+9 with the Imaging X-ray Polarimetry Explorer (IXPE) and NuSTAR. The source is significantly polarized in the 4--8 keV band, with a degree of $2.2\% \pm 0.5\%$ (uncertainty at the 68% confidence level). The NuSTAR broad-band spectrum clearly shows an iron line, and is well des… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.02740v1-abstract-full').style.display = 'inline'; document.getElementById('2306.02740v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.02740v1-abstract-full" style="display: none;"> We report on a comprehensive analysis of simultaneous X-ray polarimetric and spectral data of the bright atoll source GX 9+9 with the Imaging X-ray Polarimetry Explorer (IXPE) and NuSTAR. The source is significantly polarized in the 4--8 keV band, with a degree of $2.2\% \pm 0.5\%$ (uncertainty at the 68% confidence level). The NuSTAR broad-band spectrum clearly shows an iron line, and is well described by a model including thermal disk emission, a Comptonized component, and reflection. From a spectro-polarimetric fit, we obtain an upper limit to the polarization degree of the disk of 4% (at 99% confidence level), while the contribution of Comptonized and reflected radiation cannot be conclusively separated. However, the polarization is consistent with resulting from a combination of Comptonization in a boundary or spreading layer, plus reflection off the disc, which gives a significant contribution in any realistic scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.02740v1-abstract-full').style.display = 'none'; document.getElementById('2306.02740v1-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, 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">10 pages, 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 676, A20 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2212.13119">arXiv:2212.13119</a> <span> [<a href="https://arxiv.org/pdf/2212.13119">pdf</a>, <a href="https://arxiv.org/format/2212.13119">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/stac3726">10.1093/mnras/stac3726 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Accretion geometry of the neutron star low mass X-ray binary Cyg X-2 from X-ray polarization measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">R. Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Fabiani%2C+S">S. Fabiani</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">J. Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Ursini%2C+F">F. Ursini</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrigno%2C+C">C. Ferrigno</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">S. Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Cocchi%2C+M">M. Cocchi</a>, <a href="/search/astro-ph?searchtype=author&query=Capitanio%2C+F">F. Capitanio</a>, <a href="/search/astro-ph?searchtype=author&query=De+Rosa%2C+A">A. De Rosa</a>, <a href="/search/astro-ph?searchtype=author&query=Gnarini%2C+A">A. Gnarini</a>, <a href="/search/astro-ph?searchtype=author&query=Kislat%2C+F">F. Kislat</a>, <a href="/search/astro-ph?searchtype=author&query=Matt%2C+G">G. Matt</a>, <a href="/search/astro-ph?searchtype=author&query=Mikusincova%2C+R">R. Mikusincova</a>, <a href="/search/astro-ph?searchtype=author&query=Muleri%2C+F">F. Muleri</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bachetti%2C+M">M. Bachetti</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+L">L. Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Baumgartner%2C+W+H">W. H. Baumgartner</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+R">R. Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+S+D">S. D. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+R">R. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Brez%2C+A">A. Brez</a>, <a href="/search/astro-ph?searchtype=author&query=Bucciantini%2C+N">N. Bucciantini</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+S">S. Castellano</a> , et al. (70 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="2212.13119v1-abstract-short" style="display: inline;"> We report spectro-polarimetric results of an observational campaign of the bright neutron star low-mass X-ray binary Cyg X-2 simultaneously observed by IXPE, NICER and INTEGRAL. Consistently with previous results, the broad-band spectrum is characterized by a lower-energy component, attributed to the accretion disc with $kT_{\rm in} \approx$ 1 keV, plus unsaturated Comptonization in thermal plasma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.13119v1-abstract-full').style.display = 'inline'; document.getElementById('2212.13119v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.13119v1-abstract-full" style="display: none;"> We report spectro-polarimetric results of an observational campaign of the bright neutron star low-mass X-ray binary Cyg X-2 simultaneously observed by IXPE, NICER and INTEGRAL. Consistently with previous results, the broad-band spectrum is characterized by a lower-energy component, attributed to the accretion disc with $kT_{\rm in} \approx$ 1 keV, plus unsaturated Comptonization in thermal plasma with temperature $kT_{\rm e} = 3$ keV and optical depth $蟿\approx 4$, assuming a slab geometry. We measure the polarization degree in the 2-8 keV band $P=1.8 \pm 0.3$ per cent and polarization angle $蠁= 140^{\circ} \pm 4^{\circ}$, consistent with the previous X-ray polarimetric measurements by OSO-8 as well as with the direction of the radio jet which was earlier observed from the source. While polarization of the disc spectral component is poorly constrained with the IXPE data, the Comptonized emission has a polarization degree $P =4.0 \pm 0.7$ per cent and a polarization angle aligned with the radio jet. Our results strongly favour a spreading layer at the neutron star surface as the main source of the polarization signal. However, we cannot exclude a significant contribution from reflection off the accretion disc, as indicated by the presence of the iron fluorescence line. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.13119v1-abstract-full').style.display = 'none'; document.getElementById('2212.13119v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 7 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/2212.12472">arXiv:2212.12472</a> <span> [<a href="https://arxiv.org/pdf/2212.12472">pdf</a>, <a href="https://arxiv.org/format/2212.12472">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acae88">10.3847/1538-4357/acae88 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Polarization properties of the weakly magnetized neutron star X-ray binary GS 1826-238 in the high soft state </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Capitanio%2C+F">Fiamma Capitanio</a>, <a href="/search/astro-ph?searchtype=author&query=Fabiani%2C+S">Sergio Fabiani</a>, <a href="/search/astro-ph?searchtype=author&query=Gnarini%2C+A">Andrea Gnarini</a>, <a href="/search/astro-ph?searchtype=author&query=Ursini%2C+F">Francesco Ursini</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrigno%2C+C">Carlo Ferrigno</a>, <a href="/search/astro-ph?searchtype=author&query=Matt%2C+G">Giorgio Matt</a>, <a href="/search/astro-ph?searchtype=author&query=Poutanen%2C+J">Juri Poutanen</a>, <a href="/search/astro-ph?searchtype=author&query=Cocchi%2C+M">Massimo Cocchi</a>, <a href="/search/astro-ph?searchtype=author&query=Mikusincova%2C+R">Romana Mikusincova</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">Ruben Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">Stefano Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Kajava%2C+J+J+E">Jari J. E. Kajava</a>, <a href="/search/astro-ph?searchtype=author&query=Muleri%2C+F">Fabio Muleri</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez-Fernandez%2C+C">Celia Sanchez-Fernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Soffitta%2C+P">Paolo Soffitta</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+K">Kinwah Wu</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">Ivan Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">Lucio A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bachetti%2C+M">Matteo Bachetti</a>, <a href="/search/astro-ph?searchtype=author&query=Baldini%2C+L">Luca Baldini</a>, <a href="/search/astro-ph?searchtype=author&query=Baumgartner%2C+W+H">Wayne H. Baumgartner</a>, <a href="/search/astro-ph?searchtype=author&query=Bellazzini%2C+R">Ronaldo Bellazzini</a>, <a href="/search/astro-ph?searchtype=author&query=Bongiorno%2C+S+D">Stephen D. Bongiorno</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+R">Raffaella Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Brez%2C+A">Alessandro Brez</a> , et al. (72 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="2212.12472v1-abstract-short" style="display: inline;"> The launch of the Imaging X-ray Polarimetry Explorer (IXPE) on 2021 December 9 has opened a new window in X-ray astronomy. We report here the results of the first IXPE observation of a weakly magnetized neutron star, GS 1826-238, performed on 2022 March 29-31 when the source was in a high soft state. An upper limit (99.73% confidence level) of 1.3% for the linear polarization degree is obtained ov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.12472v1-abstract-full').style.display = 'inline'; document.getElementById('2212.12472v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.12472v1-abstract-full" style="display: none;"> The launch of the Imaging X-ray Polarimetry Explorer (IXPE) on 2021 December 9 has opened a new window in X-ray astronomy. We report here the results of the first IXPE observation of a weakly magnetized neutron star, GS 1826-238, performed on 2022 March 29-31 when the source was in a high soft state. An upper limit (99.73% confidence level) of 1.3% for the linear polarization degree is obtained over the IXPE 2-8 keV energy range. Coordinated INTEGRAL and NICER observations were carried out simultaneously with IXPE. The spectral parameters obtained from the fits to the broad-band spectrum were used as inputs for Monte Carlo simulations considering different possible geometries of the X-ray emitting region. Comparing the IXPE upper limit with these simulations, we can put constraints on the geometry and inclination angle of GS 1826-238. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.12472v1-abstract-full').style.display = 'none'; document.getElementById('2212.12472v1-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accpted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.10112">arXiv:2210.10112</a> <span> [<a href="https://arxiv.org/pdf/2210.10112">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </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/10.1117/12.2630338">10.1117/12.2630338 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid Near Infrared Spectrometer and Photometer instrument flight model presentation, performance and ground calibration results summary </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Maciaszek%2C+T">T. Maciaszek</a>, <a href="/search/astro-ph?searchtype=author&query=Ealet%2C+A">A. Ealet</a>, <a href="/search/astro-ph?searchtype=author&query=Gillard%2C+W">W. Gillard</a>, <a href="/search/astro-ph?searchtype=author&query=Jahnke%2C+K">K. Jahnke</a>, <a href="/search/astro-ph?searchtype=author&query=Barbier%2C+R">R. Barbier</a>, <a href="/search/astro-ph?searchtype=author&query=Prieto%2C+E">E. Prieto</a>, <a href="/search/astro-ph?searchtype=author&query=Bon%2C+W">W. Bon</a>, <a href="/search/astro-ph?searchtype=author&query=Bonnefoi%2C+A">A. Bonnefoi</a>, <a href="/search/astro-ph?searchtype=author&query=Caillat%2C+A">A. Caillat</a>, <a href="/search/astro-ph?searchtype=author&query=Carle%2C+M">M. Carle</a>, <a href="/search/astro-ph?searchtype=author&query=Costille%2C+A">A. Costille</a>, <a href="/search/astro-ph?searchtype=author&query=Ducret%2C+F">F. Ducret</a>, <a href="/search/astro-ph?searchtype=author&query=Fabron%2C+C">C. Fabron</a>, <a href="/search/astro-ph?searchtype=author&query=Foulon%2C+B">B. Foulon</a>, <a href="/search/astro-ph?searchtype=author&query=Gimenez%2C+J+L">J. L. Gimenez</a>, <a href="/search/astro-ph?searchtype=author&query=Grassi%2C+E">E. Grassi</a>, <a href="/search/astro-ph?searchtype=author&query=Jaquet%2C+M">M. Jaquet</a>, <a href="/search/astro-ph?searchtype=author&query=Mignant%2C+D+L">D. Le Mignant</a>, <a href="/search/astro-ph?searchtype=author&query=Martin%2C+L">L. Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Pamplona%2C+T">T. Pamplona</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+P">P. Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Cl%C3%A9mens%2C+J+C">J. C. Cl茅mens</a>, <a href="/search/astro-ph?searchtype=author&query=Caillat%2C+L">L. Caillat</a>, <a href="/search/astro-ph?searchtype=author&query=Niclas%2C+M">M. Niclas</a>, <a href="/search/astro-ph?searchtype=author&query=Secroun%2C+A">A. Secroun</a> , et al. (73 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.10112v1-abstract-short" style="display: inline;"> The NISP (Near Infrared Spectrometer and Photometer) is one of the two Euclid instruments. It operates in the near-IR spectral region (950-2020nm) as a photometer and spectrometer. The instrument is composed of: a cold (135 K) optomechanical subsystem consisting of a Silicon carbide structure, an optical assembly, a filter wheel mechanism, a grism wheel mechanism, a calibration unit, and a thermal… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.10112v1-abstract-full').style.display = 'inline'; document.getElementById('2210.10112v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.10112v1-abstract-full" style="display: none;"> The NISP (Near Infrared Spectrometer and Photometer) is one of the two Euclid instruments. It operates in the near-IR spectral region (950-2020nm) as a photometer and spectrometer. The instrument is composed of: a cold (135 K) optomechanical subsystem consisting of a Silicon carbide structure, an optical assembly, a filter wheel mechanism, a grism wheel mechanism, a calibration unit, and a thermal control system, a detection system based on a mosaic of 16 H2RG with their front-end readout electronic, and a warm electronic system (290 K) composed of a data processing / detector control unit and of an instrument control unit that interfaces with the spacecraft via a 1553 bus for command and control and via Spacewire links for science data. This paper presents: the final architecture of the flight model instrument and subsystems, and the performance and the ground calibration measurement done at NISP level and at Euclid Payload Module level at operational cold temperature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.10112v1-abstract-full').style.display = 'none'; document.getElementById('2210.10112v1-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 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">18 pages, to appear in Proceedings of the SPIE</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proceedings of the SPIE, Volume 12180, id. 121801K 18 pp. (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.13074">arXiv:2209.13074</a> <span> [<a href="https://arxiv.org/pdf/2209.13074">pdf</a>, <a href="https://arxiv.org/format/2209.13074">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/10.1051/0004-6361/202244307">10.1051/0004-6361/202244307 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid preparation: XXII. Selection of Quiescent Galaxies from Mock Photometry using Machine Learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Humphrey%2C+A">A. Humphrey</a>, <a href="/search/astro-ph?searchtype=author&query=Bisigello%2C+L">L. Bisigello</a>, <a href="/search/astro-ph?searchtype=author&query=Cunha%2C+P+A+C">P. A. C. Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Fotopoulou%2C+S">S. Fotopoulou</a>, <a href="/search/astro-ph?searchtype=author&query=Caputi%2C+K">K. Caputi</a>, <a href="/search/astro-ph?searchtype=author&query=Tortora%2C+C">C. Tortora</a>, <a href="/search/astro-ph?searchtype=author&query=Zamorani%2C+G">G. Zamorani</a>, <a href="/search/astro-ph?searchtype=author&query=Papaderos%2C+P">P. Papaderos</a>, <a href="/search/astro-ph?searchtype=author&query=Vergani%2C+D">D. Vergani</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">J. Brinchmann</a>, <a href="/search/astro-ph?searchtype=author&query=Moresco%2C+M">M. Moresco</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Baldi%2C+M">M. Baldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+R">R. Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+D">D. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Camera%2C+S">S. Camera</a>, <a href="/search/astro-ph?searchtype=author&query=Capobianco%2C+V">V. Capobianco</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+C">C. Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Castander%2C+F+J">F. J. Castander</a> , et al. (184 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="2209.13074v2-abstract-short" style="display: inline;"> The Euclid Space Telescope will provide deep imaging at optical and near-infrared wavelengths, along with slitless near-infrared spectroscopy, across ~15,000 sq deg of the sky. Euclid is expected to detect ~12 billion astronomical sources, facilitating new insights into cosmology, galaxy evolution, and various other topics. To optimally exploit the expected very large data set, there is the need t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.13074v2-abstract-full').style.display = 'inline'; document.getElementById('2209.13074v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.13074v2-abstract-full" style="display: none;"> The Euclid Space Telescope will provide deep imaging at optical and near-infrared wavelengths, along with slitless near-infrared spectroscopy, across ~15,000 sq deg of the sky. Euclid is expected to detect ~12 billion astronomical sources, facilitating new insights into cosmology, galaxy evolution, and various other topics. To optimally exploit the expected very large data set, there is the need to develop appropriate methods and software. Here we present a novel machine-learning based methodology for selection of quiescent galaxies using broad-band Euclid I_E, Y_E, J_E, H_E photometry, in combination with multiwavelength photometry from other surveys. The ARIADNE pipeline uses meta-learning to fuse decision-tree ensembles, nearest-neighbours, and deep-learning methods into a single classifier that yields significantly higher accuracy than any of the individual learning methods separately. The pipeline has `sparsity-awareness', so that missing photometry values are still informative for the classification. Our pipeline derives photometric redshifts for galaxies selected as quiescent, aided by the `pseudo-labelling' semi-supervised method. After application of the outlier filter, our pipeline achieves a normalized mean absolute deviation of ~< 0.03 and a fraction of catastrophic outliers of ~< 0.02 when measured against the COSMOS2015 photometric redshifts. We apply our classification pipeline to mock galaxy photometry catalogues corresponding to three main scenarios: (i) Euclid Deep Survey with ancillary ugriz, WISE, and radio data; (ii) Euclid Wide Survey with ancillary ugriz, WISE, and radio data; (iii) Euclid Wide Survey only. Our classification pipeline outperforms UVJ selection, in addition to the Euclid I_E-Y_E, J_E-H_E and u-I_E,I_E-J_E colour-colour methods, with improvements in completeness and the F1-score of up to a factor of 2. (Abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.13074v2-abstract-full').style.display = 'none'; document.getElementById('2209.13074v2-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">37 pages (including appendices), 26 figures; 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 671, A99 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.00749">arXiv:2206.00749</a> <span> [<a href="https://arxiv.org/pdf/2206.00749">pdf</a>, <a href="https://arxiv.org/format/2206.00749">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/stac1523">10.1093/mnras/stac1523 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Polarization properties of weakly magnetized Neutron Stars in Low Mass X-ray Binaries </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gnarini%2C+A">Andrea Gnarini</a>, <a href="/search/astro-ph?searchtype=author&query=Ursini%2C+F">Francesco Ursini</a>, <a href="/search/astro-ph?searchtype=author&query=Matt%2C+G">Giorgio Matt</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+S">Stefano Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Capitanio%2C+F">Fiamma Capitanio</a>, <a href="/search/astro-ph?searchtype=author&query=Cocchi%2C+M">Massimo Cocchi</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">Ruben Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+W">Wenda Zhang</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="2206.00749v1-abstract-short" style="display: inline;"> X-ray polarimetry missions like IXPE will be able to measure for the first time the polarization properties of accreting, weakly magnetized neutron stars in Low Mass X-ray Binaries. In this work we present simulations of the expected X-ray polarized signal including the coronal emission for different geometries of the corona itself, i.e. a slab above the accretion disc and a spherical shell around… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.00749v1-abstract-full').style.display = 'inline'; document.getElementById('2206.00749v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.00749v1-abstract-full" style="display: none;"> X-ray polarimetry missions like IXPE will be able to measure for the first time the polarization properties of accreting, weakly magnetized neutron stars in Low Mass X-ray Binaries. In this work we present simulations of the expected X-ray polarized signal including the coronal emission for different geometries of the corona itself, i.e. a slab above the accretion disc and a spherical shell around the neutron star. The simulations are performed with the fully relativistic Monte Carlo code monk capable of computing the X-ray polarization degree and angle for various physical input parameters of the neutron star, disc and corona. Different coronal geometries result in significantly different X-ray polarization properties, which can therefore be used to constrain the geometry of the systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.00749v1-abstract-full').style.display = 'none'; document.getElementById('2206.00749v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.01650">arXiv:2203.01650</a> <span> [<a href="https://arxiv.org/pdf/2203.01650">pdf</a>, <a href="https://arxiv.org/format/2203.01650">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </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/10.1051/0004-6361/202142897">10.1051/0004-6361/202142897 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid preparation. XVIII. The NISP photometric system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Schirmer%2C+M">M. Schirmer</a>, <a href="/search/astro-ph?searchtype=author&query=Jahnke%2C+K">K. Jahnke</a>, <a href="/search/astro-ph?searchtype=author&query=Seidel%2C+G">G. Seidel</a>, <a href="/search/astro-ph?searchtype=author&query=Aussel%2C+H">H. Aussel</a>, <a href="/search/astro-ph?searchtype=author&query=Bodendorf%2C+C">C. Bodendorf</a>, <a href="/search/astro-ph?searchtype=author&query=Grupp%2C+F">F. Grupp</a>, <a href="/search/astro-ph?searchtype=author&query=Hormuth%2C+F">F. Hormuth</a>, <a href="/search/astro-ph?searchtype=author&query=Wachter%2C+S">S. Wachter</a>, <a href="/search/astro-ph?searchtype=author&query=Appleton%2C+P+N">P. N. Appleton</a>, <a href="/search/astro-ph?searchtype=author&query=Barbier%2C+R">R. Barbier</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">J. Brinchmann</a>, <a href="/search/astro-ph?searchtype=author&query=Carrasco%2C+J+M">J. M. Carrasco</a>, <a href="/search/astro-ph?searchtype=author&query=Castander%2C+F+J">F. J. Castander</a>, <a href="/search/astro-ph?searchtype=author&query=Coupon%2C+J">J. Coupon</a>, <a href="/search/astro-ph?searchtype=author&query=De+Paolis%2C+F">F. De Paolis</a>, <a href="/search/astro-ph?searchtype=author&query=Franco%2C+A">A. Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Ganga%2C+K">K. Ganga</a>, <a href="/search/astro-ph?searchtype=author&query=Hudelot%2C+P">P. Hudelot</a>, <a href="/search/astro-ph?searchtype=author&query=Jullo%2C+E">E. Jullo</a>, <a href="/search/astro-ph?searchtype=author&query=Lancon%2C+A">A. Lancon</a>, <a href="/search/astro-ph?searchtype=author&query=Nucita%2C+A+A">A. A. Nucita</a>, <a href="/search/astro-ph?searchtype=author&query=Paltani%2C+S">S. Paltani</a>, <a href="/search/astro-ph?searchtype=author&query=Smadja%2C+G">G. Smadja</a>, <a href="/search/astro-ph?searchtype=author&query=Venancio%2C+L+M+G">L. M. G. Venancio</a> , et al. (198 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="2203.01650v2-abstract-short" style="display: inline;"> Euclid will be the first space mission to survey most of the extragalactic sky in the 0.95-2.02 $渭$m range, to a 5$蟽$ point-source median depth of 24.4 AB mag. This unique photometric data set will find wide use beyond Euclid's core science. In this paper, we present accurate computations of the Euclid Y_E, J_E and H_E passbands used by the Near-Infrared Spectrometer and Photometer (NISP), and the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.01650v2-abstract-full').style.display = 'inline'; document.getElementById('2203.01650v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.01650v2-abstract-full" style="display: none;"> Euclid will be the first space mission to survey most of the extragalactic sky in the 0.95-2.02 $渭$m range, to a 5$蟽$ point-source median depth of 24.4 AB mag. This unique photometric data set will find wide use beyond Euclid's core science. In this paper, we present accurate computations of the Euclid Y_E, J_E and H_E passbands used by the Near-Infrared Spectrometer and Photometer (NISP), and the associated photometric system. We pay particular attention to passband variations in the field of view, accounting among others for spatially variable filter transmission, and variations of the angle of incidence on the filter substrate using optical ray tracing. The response curves' cut-on and cut-off wavelengths - and their variation in the field of view - are determined with 0.8 nm accuracy, essential for the photometric redshift accuracy required by Euclid. After computing the photometric zeropoints in the AB mag system, we present linear transformations from and to common ground-based near-infrared photometric systems, for normal stars, red and brown dwarfs, and galaxies separately. A Python tool to compute accurate magnitudes for arbitrary passbands and spectral energy distributions is provided. We discuss various factors from space weathering to material outgassing that may slowly alter Euclid's spectral response. At the absolute flux scale, the Euclid in-flight calibration program connects the NISP photometric system to Hubble Space Telescope spectrophotometric white dwarf standards; at the relative flux scale, the chromatic evolution of the response is tracked at the milli-mag level. In this way, we establish an accurate photometric system that is fully controlled throughout Euclid's lifetime. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.01650v2-abstract-full').style.display = 'none'; document.getElementById('2203.01650v2-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">v1</span> submitted 3 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">33 pages, 25 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 662, A92 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.06947">arXiv:2110.06947</a> <span> [<a href="https://arxiv.org/pdf/2110.06947">pdf</a>, <a href="https://arxiv.org/format/2110.06947">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202142481">10.1051/0004-6361/202142481 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KiDS & Euclid: Cosmological implications of a pseudo angular power spectrum analysis of KiDS-1000 cosmic shear tomography </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Loureiro%2C+A">A. Loureiro</a>, <a href="/search/astro-ph?searchtype=author&query=Whittaker%2C+L">L. Whittaker</a>, <a href="/search/astro-ph?searchtype=author&query=Mancini%2C+A+S">A. Spurio Mancini</a>, <a href="/search/astro-ph?searchtype=author&query=Joachimi%2C+B">B. Joachimi</a>, <a href="/search/astro-ph?searchtype=author&query=Cuceu%2C+A">A. Cuceu</a>, <a href="/search/astro-ph?searchtype=author&query=Asgari%2C+M">M. Asgari</a>, <a href="/search/astro-ph?searchtype=author&query=St%C3%B6lzner%2C+B">B. St枚lzner</a>, <a href="/search/astro-ph?searchtype=author&query=Tr%C3%B6ster%2C+T">T. Tr枚ster</a>, <a href="/search/astro-ph?searchtype=author&query=Wright%2C+A+H">A. H. Wright</a>, <a href="/search/astro-ph?searchtype=author&query=Bilicki%2C+M">M. Bilicki</a>, <a href="/search/astro-ph?searchtype=author&query=Dvornik%2C+A">A. Dvornik</a>, <a href="/search/astro-ph?searchtype=author&query=Giblin%2C+B">B. Giblin</a>, <a href="/search/astro-ph?searchtype=author&query=Heymans%2C+C">C. Heymans</a>, <a href="/search/astro-ph?searchtype=author&query=Hildebrandt%2C+H">H. Hildebrandt</a>, <a href="/search/astro-ph?searchtype=author&query=Shan%2C+H">H. Shan</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Bodendorf%2C+C">C. Bodendorf</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+D">D. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Capobianco%2C+V">V. Capobianco</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+C">C. Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a> , et al. (89 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="2110.06947v2-abstract-short" style="display: inline;"> We present a tomographic weak lensing analysis of the Kilo Degree Survey Data Release 4 (KiDS-1000), using a new pseudo angular power spectrum estimator (pseudo-$C_{\ell}$) under development for the ESA Euclid mission. Over 21 million galaxies with shape information are divided into five tomographic redshift bins, ranging from 0.1 to 1.2 in photometric redshift. We measured pseudo-$C_{\ell}$ using… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.06947v2-abstract-full').style.display = 'inline'; document.getElementById('2110.06947v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.06947v2-abstract-full" style="display: none;"> We present a tomographic weak lensing analysis of the Kilo Degree Survey Data Release 4 (KiDS-1000), using a new pseudo angular power spectrum estimator (pseudo-$C_{\ell}$) under development for the ESA Euclid mission. Over 21 million galaxies with shape information are divided into five tomographic redshift bins, ranging from 0.1 to 1.2 in photometric redshift. We measured pseudo-$C_{\ell}$ using eight bands in the multipole range $76<\ell<1500$ for auto- and cross-power spectra between the tomographic bins. A series of tests were carried out to check for systematic contamination from a variety of observational sources including stellar number density, variations in survey depth, and point spread function properties. While some marginal correlations with these systematic tracers were observed, there is no evidence of bias in the cosmological inference. B-mode power spectra are consistent with zero signal, with no significant residual contamination from E/B-mode leakage. We performed a Bayesian analysis of the pseudo-$C_{\ell}$ estimates by forward modelling the effects of the mask. Assuming a spatially flat $螞$CDM cosmology, we constrained the structure growth parameter $S_8 = 蟽_8(惟_{\rm m}/0.3)^{1/2} = 0.754_{-0.029}^{+0.027}$. When combining cosmic shear from KiDS-1000 with baryon acoustic oscillation and redshift space distortion data from recent Sloan Digital Sky Survey (SDSS) measurements of luminous red galaxies, as well as the Lyman-$伪$ forest and its cross-correlation with quasars, we tightened these constraints to $S_8 = 0.771^{+0.006}_{-0.032}$. These results are in very good agreement with previous KiDS-1000 and SDSS analyses and confirm a $\sim 3蟽$ tension with early-Universe constraints from cosmic microwave background experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.06947v2-abstract-full').style.display = 'none'; document.getElementById('2110.06947v2-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 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 17 figures, Accepted by A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 665, A56 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.07303">arXiv:2109.07303</a> <span> [<a href="https://arxiv.org/pdf/2109.07303">pdf</a>, <a href="https://arxiv.org/format/2109.07303">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202142224">10.1051/0004-6361/202142224 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid: Constraining ensemble photometric redshift distributions with stacked spectroscopy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cagliari%2C+M+S">M. S. Cagliari</a>, <a href="/search/astro-ph?searchtype=author&query=Granett%2C+B+R">B. R. Granett</a>, <a href="/search/astro-ph?searchtype=author&query=Guzzo%2C+L">L. Guzzo</a>, <a href="/search/astro-ph?searchtype=author&query=Bolzonella%2C+M">M. Bolzonella</a>, <a href="/search/astro-ph?searchtype=author&query=Pozzetti%2C+L">L. Pozzetti</a>, <a href="/search/astro-ph?searchtype=author&query=Tutusaus%2C+I">I. Tutusaus</a>, <a href="/search/astro-ph?searchtype=author&query=Camera%2C+S">S. Camera</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+R">R. Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Bodendorf%2C+C">C. Bodendorf</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+D">D. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/astro-ph?searchtype=author&query=Brescia%2C+M">M. Brescia</a>, <a href="/search/astro-ph?searchtype=author&query=Capobianco%2C+V">V. Capobianco</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+C">C. Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Castander%2C+F+J">F. J. Castander</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cavuoti%2C+S">S. Cavuoti</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Cledassou%2C+R">R. Cledassou</a>, <a href="/search/astro-ph?searchtype=author&query=Congedo%2C+G">G. Congedo</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">C. J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Conversi%2C+L">L. Conversi</a> , et al. (87 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="2109.07303v2-abstract-short" style="display: inline;"> The ESA Euclid mission will produce photometric galaxy samples over 15000 square degrees of the sky that will be rich for clustering and weak lensing statistics. The accuracy of the cosmological constraints derived from these measurements will depend on the knowledge of the underlying redshift distributions based on photometric redshift calibrations. A new approach is proposed to use the stacked s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.07303v2-abstract-full').style.display = 'inline'; document.getElementById('2109.07303v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.07303v2-abstract-full" style="display: none;"> The ESA Euclid mission will produce photometric galaxy samples over 15000 square degrees of the sky that will be rich for clustering and weak lensing statistics. The accuracy of the cosmological constraints derived from these measurements will depend on the knowledge of the underlying redshift distributions based on photometric redshift calibrations. A new approach is proposed to use the stacked spectra from Euclid slitless spectroscopy to augment broad-band photometric information to constrain the redshift distribution with spectral energy distribution fitting. The high spectral resolution available in the stacked spectra complements the photometry and helps to break the colour-redshift degeneracy and constrain the redshift distribution of galaxy samples. We modelled the stacked spectra as a linear mixture of spectral templates. The mixture may be inverted to infer the underlying redshift distribution using constrained regression algorithms. We demonstrate the method on simulated Vera C. Rubin Observatory and Euclid mock survey data sets based on the Euclid Flagship mock galaxy catalogue. We assess the accuracy of the reconstruction by considering the inference of the baryon acoustic scale from angular two-point correlation function measurements. We selected mock photometric galaxy samples at redshift z>1 using the self-organising map algorithm. Considering the idealised case without dust attenuation, we find that the redshift distributions of these samples can be recovered with 0.5% accuracy on the baryon acoustic scale. The estimates are not significantly degraded by the spectroscopic measurement noise due to the large sample size. However, the error degrades to 2% when the dust attenuation model is left free. We find that the colour degeneracies introduced by attenuation limit the accuracy considering the wavelength coverage of Euclid near-infrared spectroscopy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.07303v2-abstract-full').style.display = 'none'; document.getElementById('2109.07303v2-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 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 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">16 pages, 10 figures. Accepted by A&A (Jan. 18)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 660, A9 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.01201">arXiv:2108.01201</a> <span> [<a href="https://arxiv.org/pdf/2108.01201">pdf</a>, <a href="https://arxiv.org/format/2108.01201">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="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/10.1051/0004-6361/202141938">10.1051/0004-6361/202141938 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid preparation: I. The Euclid Wide Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Scaramella%2C+R">R. Scaramella</a>, <a href="/search/astro-ph?searchtype=author&query=Amiaux%2C+J">J. Amiaux</a>, <a href="/search/astro-ph?searchtype=author&query=Mellier%2C+Y">Y. Mellier</a>, <a href="/search/astro-ph?searchtype=author&query=Burigana%2C+C">C. Burigana</a>, <a href="/search/astro-ph?searchtype=author&query=Carvalho%2C+C+S">C. S. Carvalho</a>, <a href="/search/astro-ph?searchtype=author&query=Cuillandre%2C+J+-">J. -C. Cuillandre</a>, <a href="/search/astro-ph?searchtype=author&query=Da+Silva%2C+A">A. Da Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Derosa%2C+A">A. Derosa</a>, <a href="/search/astro-ph?searchtype=author&query=Dinis%2C+J">J. Dinis</a>, <a href="/search/astro-ph?searchtype=author&query=Maiorano%2C+E">E. Maiorano</a>, <a href="/search/astro-ph?searchtype=author&query=Maris%2C+M">M. Maris</a>, <a href="/search/astro-ph?searchtype=author&query=Tereno%2C+I">I. Tereno</a>, <a href="/search/astro-ph?searchtype=author&query=Laureijs%2C+R">R. Laureijs</a>, <a href="/search/astro-ph?searchtype=author&query=Boenke%2C+T">T. Boenke</a>, <a href="/search/astro-ph?searchtype=author&query=Buenadicha%2C+G">G. Buenadicha</a>, <a href="/search/astro-ph?searchtype=author&query=Dupac%2C+X">X. Dupac</a>, <a href="/search/astro-ph?searchtype=author&query=Venancio%2C+L+M+G">L. M. Gaspar Venancio</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%B3mez-%C3%81lvarez%2C+P">P. G贸mez-脕lvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Hoar%2C+J">J. Hoar</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+J+L">J. Lorenzo Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Racca%2C+G+D">G. D. Racca</a>, <a href="/search/astro-ph?searchtype=author&query=Saavedra-Criado%2C+G">G. Saavedra-Criado</a>, <a href="/search/astro-ph?searchtype=author&query=Schwartz%2C+J">J. Schwartz</a>, <a href="/search/astro-ph?searchtype=author&query=Vavrek%2C+R">R. Vavrek</a>, <a href="/search/astro-ph?searchtype=author&query=Schirmer%2C+M">M. Schirmer</a> , et al. (216 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="2108.01201v1-abstract-short" style="display: inline;"> Euclid is an ESA mission designed to constrain the properties of dark energy and gravity via weak gravitational lensing and galaxy clustering. It will carry out a wide area imaging and spectroscopy survey (EWS) in visible and near-infrared, covering roughly 15,000 square degrees of extragalactic sky on six years. The wide-field telescope and instruments are optimized for pristine PSF and reduced s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.01201v1-abstract-full').style.display = 'inline'; document.getElementById('2108.01201v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.01201v1-abstract-full" style="display: none;"> Euclid is an ESA mission designed to constrain the properties of dark energy and gravity via weak gravitational lensing and galaxy clustering. It will carry out a wide area imaging and spectroscopy survey (EWS) in visible and near-infrared, covering roughly 15,000 square degrees of extragalactic sky on six years. The wide-field telescope and instruments are optimized for pristine PSF and reduced straylight, producing very crisp images. This paper presents the building of the Euclid reference survey: the sequence of pointings of EWS, Deep fields, Auxiliary fields for calibrations, and spacecraft movements followed by Euclid as it operates in a step-and-stare mode from its orbit around the Lagrange point L2. Each EWS pointing has four dithered frames; we simulate the dither pattern at pixel level to analyse the effective coverage. We use up-to-date models for the sky background to define the Euclid region-of-interest (RoI). The building of the reference survey is highly constrained from calibration cadences, spacecraft constraints and background levels; synergies with ground-based coverage are also considered. Via purposely-built software optimized to prioritize best sky areas, produce a compact coverage, and ensure thermal stability, we generate a schedule for the Auxiliary and Deep fields observations and schedule the RoI with EWS transit observations. The resulting reference survey RSD_2021A fulfills all constraints and is a good proxy for the final solution. Its wide survey covers 14,500 square degrees. The limiting AB magnitudes ($5蟽$ point-like source) achieved in its footprint are estimated to be 26.2 (visible) and 24.5 (near-infrared); for spectroscopy, the H$_伪$ line flux limit is $2\times 10^{-16}$ erg cm$^{-2}$ s$^{-1}$ at 1600 nm; and for diffuse emission the surface brightness limits are 29.8 (visible) and 28.4 (near-infrared) mag arcsec$^{-2}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.01201v1-abstract-full').style.display = 'none'; document.getElementById('2108.01201v1-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">43 pages, 51 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 662, A112 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.12149">arXiv:2105.12149</a> <span> [<a href="https://arxiv.org/pdf/2105.12149">pdf</a>, <a href="https://arxiv.org/format/2105.12149">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/10.1051/0004-6361/202141393">10.1051/0004-6361/202141393 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid preparation: XIII. Forecasts for galaxy morphology with the Euclid Survey using Deep Generative Models </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Bretonni%C3%A8re%2C+H">H. Bretonni猫re</a>, <a href="/search/astro-ph?searchtype=author&query=Huertas-Company%2C+M">M. Huertas-Company</a>, <a href="/search/astro-ph?searchtype=author&query=Boucaud%2C+A">A. Boucaud</a>, <a href="/search/astro-ph?searchtype=author&query=Lanusse%2C+F">F. Lanusse</a>, <a href="/search/astro-ph?searchtype=author&query=Jullo%2C+E">E. Jullo</a>, <a href="/search/astro-ph?searchtype=author&query=Merlin%2C+E">E. Merlin</a>, <a href="/search/astro-ph?searchtype=author&query=Tuccillo%2C+D">D. Tuccillo</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Brinchmann%2C+J">J. Brinchmann</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">C. J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Dole%2C+H">H. Dole</a>, <a href="/search/astro-ph?searchtype=author&query=Cabanac%2C+R">R. Cabanac</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=Castander%2C+F+J">F. J. Castander</a>, <a href="/search/astro-ph?searchtype=author&query=Duc%2C+P+A">P. A. Duc</a>, <a href="/search/astro-ph?searchtype=author&query=Fosalba%2C+P">P. Fosalba</a>, <a href="/search/astro-ph?searchtype=author&query=Guinet%2C+D">D. Guinet</a>, <a href="/search/astro-ph?searchtype=author&query=Kruk%2C+S">S. Kruk</a>, <a href="/search/astro-ph?searchtype=author&query=Kuchner%2C+U">U. Kuchner</a>, <a href="/search/astro-ph?searchtype=author&query=Serrano%2C+S">S. Serrano</a>, <a href="/search/astro-ph?searchtype=author&query=Soubrie%2C+E">E. Soubrie</a>, <a href="/search/astro-ph?searchtype=author&query=Tramacere%2C+A">A. Tramacere</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+L">L. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a> , et al. (171 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="2105.12149v3-abstract-short" style="display: inline;"> We present a machine learning framework to simulate realistic galaxies for the Euclid Survey. The proposed method combines a control on galaxy shape parameters offered by analytic models with realistic surface brightness distributions learned from real Hubble Space Telescope observations by deep generative models. We simulate a galaxy field of $0.4\,\rm{deg}^2$ as it will be seen by the Euclid vis… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.12149v3-abstract-full').style.display = 'inline'; document.getElementById('2105.12149v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.12149v3-abstract-full" style="display: none;"> We present a machine learning framework to simulate realistic galaxies for the Euclid Survey. The proposed method combines a control on galaxy shape parameters offered by analytic models with realistic surface brightness distributions learned from real Hubble Space Telescope observations by deep generative models. We simulate a galaxy field of $0.4\,\rm{deg}^2$ as it will be seen by the Euclid visible imager VIS and show that galaxy structural parameters are recovered with similar accuracy as for pure analytic S茅rsic profiles. Based on these simulations, we estimate that the Euclid Wide Survey will be able to resolve the internal morphological structure of galaxies down to a surface brightness of $22.5\,\rm{mag}\,\rm{arcsec}^{-2}$, and $24.9\,\rm{mag}\,\rm{arcsec}^{-2}$ for the Euclid Deep Survey. This corresponds to approximately $250$ million galaxies at the end of the mission and a $50\,\%$ complete sample for stellar masses above $10^{10.6}\,\rm{M}_\odot$ (resp. $10^{9.6}\,\rm{M}_\odot$) at a redshift $z\sim0.5$ for the wide (resp. deep) survey. The approach presented in this work can contribute to improving the preparation of future high-precision cosmological imaging surveys by allowing simulations to incorporate more realistic galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.12149v3-abstract-full').style.display = 'none'; document.getElementById('2105.12149v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 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">22 pages, 21 figures (6 in appendinx). Accepted for publication to A&A. Change in the title for Euclid submission chronology coherence. Few changes for clarification</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.09746">arXiv:2105.09746</a> <span> [<a href="https://arxiv.org/pdf/2105.09746">pdf</a>, <a href="https://arxiv.org/format/2105.09746">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202141353">10.1051/0004-6361/202141353 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Euclid: constraining dark energy coupled to electromagnetism using astrophysical and laboratory data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Martinelli%2C+M">M. Martinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Martins%2C+C+J+A+P">C. J. A. P. Martins</a>, <a href="/search/astro-ph?searchtype=author&query=Nesseris%2C+S">S. Nesseris</a>, <a href="/search/astro-ph?searchtype=author&query=Tutusaus%2C+I">I. Tutusaus</a>, <a href="/search/astro-ph?searchtype=author&query=Blanchard%2C+A">A. Blanchard</a>, <a href="/search/astro-ph?searchtype=author&query=Camera%2C+S">S. Camera</a>, <a href="/search/astro-ph?searchtype=author&query=Carbone%2C+C">C. Carbone</a>, <a href="/search/astro-ph?searchtype=author&query=Casas%2C+S">S. Casas</a>, <a href="/search/astro-ph?searchtype=author&query=Pettorino%2C+V">V. Pettorino</a>, <a href="/search/astro-ph?searchtype=author&query=Sakr%2C+Z">Z. Sakr</a>, <a href="/search/astro-ph?searchtype=author&query=Yankelevich%2C+V">V. Yankelevich</a>, <a href="/search/astro-ph?searchtype=author&query=Sapone%2C+D">D. Sapone</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a>, <a href="/search/astro-ph?searchtype=author&query=Auricchio%2C+N">N. Auricchio</a>, <a href="/search/astro-ph?searchtype=author&query=Bodendorf%2C+C">C. Bodendorf</a>, <a href="/search/astro-ph?searchtype=author&query=Bonino%2C+D">D. Bonino</a>, <a href="/search/astro-ph?searchtype=author&query=Branchini%2C+E">E. Branchini</a>, <a href="/search/astro-ph?searchtype=author&query=Capobianco%2C+V">V. Capobianco</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Castellano%2C+M">M. Castellano</a>, <a href="/search/astro-ph?searchtype=author&query=Cavuoti%2C+S">S. Cavuoti</a>, <a href="/search/astro-ph?searchtype=author&query=Cimatti%2C+A">A. Cimatti</a>, <a href="/search/astro-ph?searchtype=author&query=Cledassou%2C+R">R. Cledassou</a>, <a href="/search/astro-ph?searchtype=author&query=Corcione%2C+L">L. Corcione</a>, <a href="/search/astro-ph?searchtype=author&query=Costille%2C+A">A. Costille</a> , et al. (70 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="2105.09746v1-abstract-short" style="display: inline;"> In physically realistic scalar-field based dynamical dark energy models (including, e.g., quintessence) one naturally expects the scalar field to couple to the rest of the model's degrees of freedom. In particular, a coupling to the electromagnetic sector leads to a time (redshift) dependence of the fine-structure constant and a violation of the Weak Equivalence Principle. Here we extend the previ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.09746v1-abstract-full').style.display = 'inline'; document.getElementById('2105.09746v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.09746v1-abstract-full" style="display: none;"> In physically realistic scalar-field based dynamical dark energy models (including, e.g., quintessence) one naturally expects the scalar field to couple to the rest of the model's degrees of freedom. In particular, a coupling to the electromagnetic sector leads to a time (redshift) dependence of the fine-structure constant and a violation of the Weak Equivalence Principle. Here we extend the previous Euclid forecast constraints on dark energy models to this enlarged (but physically more realistic) parameter space, and forecast how well Euclid, together with high-resolution spectroscopic data and local experiments, can constrain these models. Our analysis combines simulated Euclid data products with astrophysical measurements of the fine-structure constant, $伪$, and local experimental constraints, and includes both parametric and non-parametric methods. For the astrophysical measurements of $伪$ we consider both the currently available data and a simulated dataset representative of Extremely Large Telescope measurements and expected to be available in the 2030s. Our parametric analysis shows that in the latter case the inclusion of astrophysical and local data improves the Euclid dark energy figure of merit by between $8\%$ and $26\%$, depending on the correct fiducial model, with the improvements being larger in the null case where the fiducial coupling to the electromagnetic sector is vanishing. These improvements would be smaller with the current astrophysical data. Moreover, we illustrate how a genetic algorithms based reconstruction provides a null test for the presence of the coupling. Our results highlight the importance of complementing surveys like Euclid with external data products, in order to accurately test the wider parameter spaces of physically motivated paradigms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.09746v1-abstract-full').style.display = 'none'; document.getElementById('2105.09746v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 7 figures. Submitted to Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> IFT-UAM/CSIC-21-60 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 654, A148 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.08698">arXiv:2102.08698</a> <span> [<a href="https://arxiv.org/pdf/2102.08698">pdf</a>, <a href="https://arxiv.org/format/2102.08698">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"> Scientific simulations and optimization of the XGIS instrument on board THESEUS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mereghetti%2C+S">Sandro Mereghetti</a>, <a href="/search/astro-ph?searchtype=author&query=Ghirlanda%2C+G">Giancarlo Ghirlanda</a>, <a href="/search/astro-ph?searchtype=author&query=Salvaterra%2C+R">Ruben Salvaterra</a>, <a href="/search/astro-ph?searchtype=author&query=Campana%2C+R">Riccardo Campana</a>, <a href="/search/astro-ph?searchtype=author&query=Labanti%2C+C">Claudio Labanti</a>, <a href="/search/astro-ph?searchtype=author&query=Connell%2C+P+H">Paul H. Connell</a>, <a href="/search/astro-ph?searchtype=author&query=Farinelli%2C+R">Ruben Farinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Frontera%2C+F">Filippo Frontera</a>, <a href="/search/astro-ph?searchtype=author&query=Fuschino%2C+F">Fabio Fuschino</a>, <a href="/search/astro-ph?searchtype=author&query=Gasent-Blesa%2C+J+L">Jose L. Gasent-Blesa</a>, <a href="/search/astro-ph?searchtype=author&query=Guidorzi%2C+C">Cristiano Guidorzi</a>, <a href="/search/astro-ph?searchtype=author&query=Lissoni%2C+M">Michele Lissoni</a>, <a href="/search/astro-ph?searchtype=author&query=Rigoselli%2C+M">Michela Rigoselli</a>, <a href="/search/astro-ph?searchtype=author&query=Stephen%2C+J+B">John B. Stephen</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">Lorenzo Amati</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="2102.08698v1-abstract-short" style="display: inline;"> The XGIS (X and Gamma Imaging Spectrometer) is one of the three instruments onboard the THESEUS mission (ESA M5, currently in Phase-A). Thanks to its wide field of view and good imaging capabilities, it will efficiently detect and localize gamma-ray bursts and other transients in the 2-150 keV sky, and also provide spectroscopy up to 10 MeV. Its current design has been optimized by means of scient… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.08698v1-abstract-full').style.display = 'inline'; document.getElementById('2102.08698v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.08698v1-abstract-full" style="display: none;"> The XGIS (X and Gamma Imaging Spectrometer) is one of the three instruments onboard the THESEUS mission (ESA M5, currently in Phase-A). Thanks to its wide field of view and good imaging capabilities, it will efficiently detect and localize gamma-ray bursts and other transients in the 2-150 keV sky, and also provide spectroscopy up to 10 MeV. Its current design has been optimized by means of scientific simulations based on a Monte Carlo model of the instrument coupled to a state-of-the-art description of the populations of long and short GRBs extending to high redshifts. We describe the optimization process that led to the current design of the XGIS, based on two identical units with partially overlapping fields of view, and discuss the expected performance of the instrument. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.08698v1-abstract-full').style.display = 'none'; document.getElementById('2102.08698v1-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 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">Proceedings of the SPIE 2020, paper 11444-276</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a 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