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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.14073">arXiv:2303.14073</a> <span> [<a href="https://arxiv.org/pdf/2303.14073">pdf</a>, <a href="https://arxiv.org/format/2303.14073">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346482">10.1051/0004-6361/202346482 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Blending from binarity in microlensing searches toward the Large Magellanic Cloud </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blaineau%2C+T">Tristan Blaineau</a>, <a href="/search/astro-ph?searchtype=author&query=Moniez%2C+M">Marc Moniez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.14073v3-abstract-short" style="display: inline;"> Studies of gravitational microlensing effects require the estimation of their detection efficiency as soon as one wants to quantify the massive compact objects along the line of sight of source targets. This is particularly important for setting limits on the contribution of massive compact objects to the Galactic halo. These estimates of detection efficiency must not only account for the blending… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.14073v3-abstract-full').style.display = 'inline'; document.getElementById('2303.14073v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.14073v3-abstract-full" style="display: none;"> Studies of gravitational microlensing effects require the estimation of their detection efficiency as soon as one wants to quantify the massive compact objects along the line of sight of source targets. This is particularly important for setting limits on the contribution of massive compact objects to the Galactic halo. These estimates of detection efficiency must not only account for the blending effects of accidentally superimposed sources in crowded fields, but also for possible mixing of light from stars belonging to multiple gravitationally bound stellar systems. Until now, only blending due to accidental alignment of stars had been studied, in particular as a result of high-resolution space images. In this paper, we address the impact of unresolved binary sources that are physically gravitationally bound and not accidentally aligned, in the case of microlensing detection efficiencies toward the Large Magellanic Cloud (LMC). We used the Gaia catalog of nearby stars to constrain the local binarity rate, which we extrapolated to the distance of the LMC. Then we estimated an upper limit to the impact of this binarity on the detection efficiency of microlensing effects, as a function of lens mass. We find that a maximum of 6.2\% of microlensing events on LMC sources due to halo lenses heavier than $30 M_{\odot}$ could be affected as a result of the sources belonging to unresolved binary systems. This number is the maximum fraction of events for which the source is a binary system separated by about one angular Einstein radius or more in a configuration where light-curve distortion could affect the efficiency of some detection algorithms. For events caused by lighter lenses on LMC sources, our study shows that the chances of blending effects by binary systems is likely to be higher and should be studied in more detail to improve the accuracy of efficiency calculations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.14073v3-abstract-full').style.display = 'none'; document.getElementById('2303.14073v3-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 11 figures, accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, A76 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.09450">arXiv:2205.09450</a> <span> [<a href="https://arxiv.org/pdf/2205.09450">pdf</a>, <a href="https://arxiv.org/format/2205.09450">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Search for Black Holes in the Galactic Halo by Gravitational Microlensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blaineau%2C+T">Tristan Blaineau</a>, <a href="/search/astro-ph?searchtype=author&query=Moniez%2C+M">Marc Moniez</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="2205.09450v2-abstract-short" style="display: inline;"> Black hole-like objects with mass greater than $10 M_{\odot}$, as discovered by gravitational antennas, can produce long time-scale (several years) gravitational microlensing effects. Considered separately, previous microlensing surveys were insensitive to such events because of their limited duration of 6-7 years. We combined light curves from the EROS-2 and MACHO surveys to the Large Magellanic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.09450v2-abstract-full').style.display = 'inline'; document.getElementById('2205.09450v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.09450v2-abstract-full" style="display: none;"> Black hole-like objects with mass greater than $10 M_{\odot}$, as discovered by gravitational antennas, can produce long time-scale (several years) gravitational microlensing effects. Considered separately, previous microlensing surveys were insensitive to such events because of their limited duration of 6-7 years. We combined light curves from the EROS-2 and MACHO surveys to the Large Magellanic Cloud (LMC) to create a joint database for 14.1 million stars, covering a total duration of 10.6 years, with fluxes measured through 4 wide passbands. We searched for multi-year microlensing events in this catalog of extended light curves, complemented by 24.1 million light curves observed by only one of the surveys. Our analysis, combined with previous analysis from EROS, shows that compact objects with mass between $10^{-7}$ and $200 M_{\odot}$ can not constitute more than $\sim 20\%$ of the total mass of a standard halo (at $95\%$ CL). We also exclude that $\sim 50\%$ of the halo is made of Black Holes (BH) lighter than $1000 M_{\odot}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.09450v2-abstract-full').style.display = 'none'; document.getElementById('2205.09450v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 6 figures. arXiv admin note: text overlap with arXiv:2202.13819</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> contribution to the 2022 QCD session of the 56th Rencontres de Moriond </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.13819">arXiv:2202.13819</a> <span> [<a href="https://arxiv.org/pdf/2202.13819">pdf</a>, <a href="https://arxiv.org/format/2202.13819">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202243430">10.1051/0004-6361/202243430 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New limits from microlensing on Galactic Black Holes in the mass range $10M_{\odot}<M<1000M_{\odot}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blaineau%2C+T">T. Blaineau</a>, <a href="/search/astro-ph?searchtype=author&query=Moniez%2C+M">M. Moniez</a>, <a href="/search/astro-ph?searchtype=author&query=Afonso%2C+C">C. Afonso</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+J+-">J. -N. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Ansari%2C+R">R. Ansari</a>, <a href="/search/astro-ph?searchtype=author&query=Aubourg%2C+E">E. Aubourg</a>, <a href="/search/astro-ph?searchtype=author&query=Coutures%2C+C">C. Coutures</a>, <a href="/search/astro-ph?searchtype=author&query=Glicenstein%2C+J+-">J. -F. Glicenstein</a>, <a href="/search/astro-ph?searchtype=author&query=Goldman%2C+B">B. Goldman</a>, <a href="/search/astro-ph?searchtype=author&query=Hamadache%2C+C">C. Hamadache</a>, <a href="/search/astro-ph?searchtype=author&query=Lasserre%2C+T">T. Lasserre</a>, <a href="/search/astro-ph?searchtype=author&query=LeGuillou%2C+L">L. LeGuillou</a>, <a href="/search/astro-ph?searchtype=author&query=Lesquoy%2C+E">E. Lesquoy</a>, <a href="/search/astro-ph?searchtype=author&query=Magneville%2C+C">C. Magneville</a>, <a href="/search/astro-ph?searchtype=author&query=Marquette%2C+J+-">J. -B. Marquette</a>, <a href="/search/astro-ph?searchtype=author&query=Palanque-Delabrouille%2C+N">N. Palanque-Delabrouille</a>, <a href="/search/astro-ph?searchtype=author&query=Perdereau%2C+O">O. Perdereau</a>, <a href="/search/astro-ph?searchtype=author&query=Rich%2C+J">J. Rich</a>, <a href="/search/astro-ph?searchtype=author&query=Spiro%2C+M">M. Spiro</a>, <a href="/search/astro-ph?searchtype=author&query=Tisserand%2C+P">P. Tisserand</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="2202.13819v3-abstract-short" style="display: inline;"> We have searched for long duration microlensing events originating from intermediate mass Black Holes (BH) in the halo of the Milky Way, using archival data from EROS-2 and MACHO photometric surveys towards the Large Magellanic Cloud. We combined data from these two surveys to create a common database of light curves for 14.1 million objects in LMC, covering a total duration of 10.6 years, with fl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.13819v3-abstract-full').style.display = 'inline'; document.getElementById('2202.13819v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.13819v3-abstract-full" style="display: none;"> We have searched for long duration microlensing events originating from intermediate mass Black Holes (BH) in the halo of the Milky Way, using archival data from EROS-2 and MACHO photometric surveys towards the Large Magellanic Cloud. We combined data from these two surveys to create a common database of light curves for 14.1 million objects in LMC, covering a total duration of 10.6 years, with flux series measured through four wide passbands. We have carried out a microlensing search on these light curves, complemented by the light curves of 22.7 million objects, observed by EROS-2 only or MACHO only over about 7 years, with flux series measured through only two passbands. A likelihood analysis, taking into account LMC self lensing and Milky Way disk contributions allows us to conclude that compact objects with masses in the range $10 - 100 M_{\odot}$ cannot make up more than $\sim 15\%$ of a standard halo total mass (at $95\%$ confidence level). Our analysis sensitivity weakens for heavier objects, although we still exclude that $\sim 50\%$ of the halo be made of $\sim 1000 M_{\odot}$ BHs. Combined with previous EROS results, an upper limit of $\sim 15\%$ of the total halo mass can be obtained for the contribution of compact halo objects in the mass range $10^{-6} - 10^2 M_{\odot}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.13819v3-abstract-full').style.display = 'none'; document.getElementById('2202.13819v3-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 5 figures, accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 664, A106 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.05676">arXiv:2104.05676</a> <span> [<a href="https://arxiv.org/pdf/2104.05676">pdf</a>, <a href="https://arxiv.org/format/2104.05676">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/10.3847/1538-4365/ac5033">10.3847/1538-4365/ac5033 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Impact of Observing Strategy on Cosmological Constraints with LSST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lochner%2C+M">Michelle Lochner</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">Dan Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Almoubayyed%2C+H">Husni Almoubayyed</a>, <a href="/search/astro-ph?searchtype=author&query=Anguita%2C+T">Timo Anguita</a>, <a href="/search/astro-ph?searchtype=author&query=Awan%2C+H">Humna Awan</a>, <a href="/search/astro-ph?searchtype=author&query=Gawiser%2C+E">Eric Gawiser</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">Satya Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Gris%2C+P">Philippe Gris</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+S">Simon Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Jha%2C+S+W">Saurabh W. Jha</a>, <a href="/search/astro-ph?searchtype=author&query=Jones%2C+R+L">R. Lynne Jones</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+A+G">Alex G. Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Mandelbaum%2C+R">Rachel Mandelbaum</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+P">Phil Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Petrushevska%2C+T">Tanja Petrushevska</a>, <a href="/search/astro-ph?searchtype=author&query=Regnault%2C+N">Nicolas Regnault</a>, <a href="/search/astro-ph?searchtype=author&query=Setzer%2C+C+N">Christian N. Setzer</a>, <a href="/search/astro-ph?searchtype=author&query=Suyu%2C+S+H">Sherry H. Suyu</a>, <a href="/search/astro-ph?searchtype=author&query=Yoachim%2C+P">Peter Yoachim</a>, <a href="/search/astro-ph?searchtype=author&query=Biswas%2C+R">Rahul Biswas</a>, <a href="/search/astro-ph?searchtype=author&query=Blaineau%2C+T">Tristan Blaineau</a>, <a href="/search/astro-ph?searchtype=author&query=Hook%2C+I">Isobel Hook</a>, <a href="/search/astro-ph?searchtype=author&query=Moniez%2C+M">Marc Moniez</a>, <a href="/search/astro-ph?searchtype=author&query=Neilsen%2C+E">Eric Neilsen</a>, <a href="/search/astro-ph?searchtype=author&query=Peiris%2C+H">Hiranya Peiris</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2104.05676v1-abstract-short" style="display: inline;"> The generation-defining Vera C. Rubin Observatory will make state-of-the-art measurements of both the static and transient universe through its Legacy Survey for Space and Time (LSST). With such capabilities, it is immensely challenging to optimize the LSST observing strategy across the survey's wide range of science drivers. Many aspects of the LSST observing strategy relevant to the LSST Dark En… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.05676v1-abstract-full').style.display = 'inline'; document.getElementById('2104.05676v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.05676v1-abstract-full" style="display: none;"> The generation-defining Vera C. Rubin Observatory will make state-of-the-art measurements of both the static and transient universe through its Legacy Survey for Space and Time (LSST). With such capabilities, it is immensely challenging to optimize the LSST observing strategy across the survey's wide range of science drivers. Many aspects of the LSST observing strategy relevant to the LSST Dark Energy Science Collaboration, such as survey footprint definition, single visit exposure time and the cadence of repeat visits in different filters, are yet to be finalized. Here, we present metrics used to assess the impact of observing strategy on the cosmological probes considered most sensitive to survey design; these are large-scale structure, weak lensing, type Ia supernovae, kilonovae and strong lens systems (as well as photometric redshifts, which enable many of these probes). We evaluate these metrics for over 100 different simulated potential survey designs. Our results show that multiple observing strategy decisions can profoundly impact cosmological constraints with LSST; these include adjusting the survey footprint, ensuring repeat nightly visits are taken in different filters and enforcing regular cadence. We provide public code for our metrics, which makes them readily available for evaluating further modifications to the survey design. We conclude with a set of recommendations and highlight observing strategy factors that require further research. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.05676v1-abstract-full').style.display = 'none'; document.getElementById('2104.05676v1-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 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">49 pages, 17 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJS 259 58, 2022 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2009.10185">arXiv:2009.10185</a> <span> [<a href="https://arxiv.org/pdf/2009.10185">pdf</a>, <a href="https://arxiv.org/format/2009.10185">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div 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/staa3602">10.1093/mnras/staa3602 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Fink, a new generation of broker for the LSST community </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">Anais M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Peloton%2C+J">Julien Peloton</a>, <a href="/search/astro-ph?searchtype=author&query=Ishida%2C+E+E+O">Emille E. O. Ishida</a>, <a href="/search/astro-ph?searchtype=author&query=Arnault%2C+C">Chris Arnault</a>, <a href="/search/astro-ph?searchtype=author&query=Bachelet%2C+E">Etienne Bachelet</a>, <a href="/search/astro-ph?searchtype=author&query=Blaineau%2C+T">Tristan Blaineau</a>, <a href="/search/astro-ph?searchtype=author&query=Boutigny%2C+D">Dominique Boutigny</a>, <a href="/search/astro-ph?searchtype=author&query=Chauhan%2C+A">Abhishek Chauhan</a>, <a href="/search/astro-ph?searchtype=author&query=Gangler%2C+E">Emmanuel Gangler</a>, <a href="/search/astro-ph?searchtype=author&query=Hernandez%2C+F">Fabio Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Hrivnac%2C+J">Julius Hrivnac</a>, <a href="/search/astro-ph?searchtype=author&query=Leoni%2C+M">Marco Leoni</a>, <a href="/search/astro-ph?searchtype=author&query=Leroy%2C+N">Nicolas Leroy</a>, <a href="/search/astro-ph?searchtype=author&query=Moniez%2C+M">Marc Moniez</a>, <a href="/search/astro-ph?searchtype=author&query=Pateyron%2C+S">Sacha Pateyron</a>, <a href="/search/astro-ph?searchtype=author&query=Ramparison%2C+A">Adrien Ramparison</a>, <a href="/search/astro-ph?searchtype=author&query=Turpin%2C+D">Damien Turpin</a>, <a href="/search/astro-ph?searchtype=author&query=Ansari%2C+R">R茅za Ansari</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+T">Tarek Allam Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Bajat%2C+A">Armelle Bajat</a>, <a href="/search/astro-ph?searchtype=author&query=Biswas%2C+B">Biswajit Biswas</a>, <a href="/search/astro-ph?searchtype=author&query=Boucaud%2C+A">Alexandre Boucaud</a>, <a href="/search/astro-ph?searchtype=author&query=Bregeon%2C+J">Johan Bregeon</a>, <a href="/search/astro-ph?searchtype=author&query=Campagne%2C+J">Jean-Eric Campagne</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen-Tanugi%2C+J">Johann Cohen-Tanugi</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2009.10185v3-abstract-short" style="display: inline;"> Fink is a broker designed to enable science with large time-domain alert streams such as the one from the upcoming Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST). It exhibits traditional astronomy broker features such as automatised ingestion, annotation, selection and redistribution of promising alerts for transient science. It is also designed to go beyond traditional broker fe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.10185v3-abstract-full').style.display = 'inline'; document.getElementById('2009.10185v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2009.10185v3-abstract-full" style="display: none;"> Fink is a broker designed to enable science with large time-domain alert streams such as the one from the upcoming Vera C. Rubin Observatory Legacy Survey of Space and Time (LSST). It exhibits traditional astronomy broker features such as automatised ingestion, annotation, selection and redistribution of promising alerts for transient science. It is also designed to go beyond traditional broker features by providing real-time transient classification which is continuously improved by using state-of-the-art Deep Learning and Adaptive Learning techniques. These evolving added values will enable more accurate scientific output from LSST photometric data for diverse science cases while also leading to a higher incidence of new discoveries which shall accompany the evolution of the survey. In this paper we introduce Fink, its science motivation, architecture and current status including first science verification cases using the Zwicky Transient Facility alert stream. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2009.10185v3-abstract-full').style.display = 'none'; document.getElementById('2009.10185v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted 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/2003.11308">arXiv:2003.11308</a> <span> [<a href="https://arxiv.org/pdf/2003.11308">pdf</a>, <a href="https://arxiv.org/format/2003.11308">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202038005">10.1051/0004-6361/202038005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Parallax in microlensing toward the Magellanic Clouds: effect on detection efficiency and detectability </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Blaineau%2C+T">T. Blaineau</a>, <a href="/search/astro-ph?searchtype=author&query=Moniez%2C+M">M. Moniez</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="2003.11308v2-abstract-short" style="display: inline;"> Aims. We study the impact of the parallax on the search for very long timescale microlensing events towards the Magellanic Clouds due to dark massive compact objects within the past MACHO and EROS, the ongoing MOA and OGLE, and the future LSST surveys. We quantify the impact of neglecting this effect on the classical event selection process and also quantify the parallax detectability without the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.11308v2-abstract-full').style.display = 'inline'; document.getElementById('2003.11308v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.11308v2-abstract-full" style="display: none;"> Aims. We study the impact of the parallax on the search for very long timescale microlensing events towards the Magellanic Clouds due to dark massive compact objects within the past MACHO and EROS, the ongoing MOA and OGLE, and the future LSST surveys. We quantify the impact of neglecting this effect on the classical event selection process and also quantify the parallax detectability without the help of follow-up observations.Methods. We define a distance between true events affected by parallax and the closest events without parallax. This distance is used to estimate the probability of missing the preselection of events because of parallax, for any survey characterised by its time sampling and photometric performance. We also define another distance to quantify the detectability of the parallax effect, in order to trigger complementary observations.Results. We find that the preselection of years long time scale events is marginally affected by parallax for all surveys, provided the criteria are reasonably tight. We also show that the parallax should be detectable in the majority of the events found by the LSST survey without follow-up observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.11308v2-abstract-full').style.display = 'none'; document.getElementById('2003.11308v2-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 June, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomy and Astrophysics - A\&A, EDP Sciences, 2020, 636, pp.L9 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a 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