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This model is similar to those considered earlier. We show that the probability of mutant fixation in a population of size <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"graphic\/sapm12373-math-0001.png\" xlink:title=\"urn:x-wiley:00222526:media:sapm12373:sapm12373-math-0001\" \/>, starting from a single mutant, is greater than <jats:inline-graphic xmlns:xlink=\"http:\/\/www.w3.org\/1999\/xlink\" xlink:href=\"graphic\/sapm12373-math-0002.png\" xlink:title=\"urn:x-wiley:00222526:media:sapm12373:sapm12373-math-0002\" \/>, which would be the case if there were no variation in fitness whatsoever. In the small variation regime, we recover precise asymptotics for the success probability of the mutant. This demonstrates that the introduction of randomness provides an advantage to minority mutations in this model, and shows that the advantage increases with the system size. 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We have monitored over 6000 sources with i-band between 13 and 23 mag within a 26 \u00d7 26 arcmin2 field of view. For each star, we collected \u223c1500 photometric points covering a temporal window of 23\u00a0d. Based on these data, we have measured rotation-modulated of 136 stars and identified around 90 additional variables, including 14 eclipsing binary candidates. Moreover, we found 298 other variables with photometric high-scatter. In addition, we have obtained r-band and H\u03b1 narrow-band photometry of the cluster with LCOGT and low-resolution optical spectroscopy of 229 stars with GMOS-Gemini. We used the Gaia data from the periodic stars and objects with H\u03b1 or IR-excesses, which are mostly low-mass pre-main sequence stars (&amp;lt;1\u00a0M\u2299) in the cluster to estimate the distance (825\u00a0\u00b1\u00a051\u00a0pc) and the mean proper motions (\u03bc\u03b1cos(\u03b4)\u00a0= \u22122.75 mas yr\u22121 and \u03bc\u03b4\u00a0= 1.15 mas yr\u22121) of its members. This allows us to use the Gaia data to identify additional Mon R2 member candidates. We also used Pan-STARRS photometry from our LCOGT sources to construct a more precise H-R diagram, from which we estimate the mean age of the cluster and identify other possible members including eleven spectroscopy brown dwarf with M7 to M9 GMOS spectral types. Finally, we combined our membership lists with Spitzer infrared photometry to investigate the incidence of stars with discs and the effect these have on stellar rotation.<\/jats:p>","DOI":"10.1093\/mnras\/stad1891","type":"journal-article","created":{"date-parts":[[2023,6,24]],"date-time":"2023-06-24T16:04:49Z","timestamp":1687622689000},"page":"1826-1854","source":"Crossref","is-referenced-by-count":1,"title":["Time-series photometry and multiwavelength characterization of the young stellar cluster Mon R2"],"prefix":"10.1093","volume":"524","author":[{"ORCID":"https:\/\/orcid.org\/0000-0002-7625-1768","authenticated-orcid":false,"given":"Santiago","family":"Orcajo","sequence":"first","affiliation":[{"name":"Facultad de Ciencias Astron\u00f3micas y Geof\u00edsicas, Universidad Nacional de La Plata , Paseo del Bosque S\/N, B1900 La Plata , Argentina"},{"name":"Instituto de Astrof\u00edsica de La Plata , CCT La Plata, CONICET\u2013UNLP, B1900 La Plata , Argentina"}]},{"given":"Lucas A","family":"Cieza","sequence":"additional","affiliation":[{"name":"N\u00facleo de Astronom\u00eda, Facultad de Ingenier\u00eda y Ciencias, Universidad Diego Portales , Av Ej\u00e9rcito 441, 8320000 Santiago , Chile"}]},{"ORCID":"https:\/\/orcid.org\/0000-0002-5227-9627","authenticated-orcid":false,"given":"Roberto","family":"Gamen","sequence":"additional","affiliation":[{"name":"Facultad de Ciencias Astron\u00f3micas y Geof\u00edsicas, Universidad Nacional de La Plata , Paseo del Bosque S\/N, B1900 La Plata , Argentina"},{"name":"Instituto de Astrof\u00edsica de La Plata , CCT La Plata, CONICET\u2013UNLP, B1900 La Plata , Argentina"}]}],"member":"286","published-online":{"date-parts":[[2023,6,24]]},"reference":[{"key":"2024062400065960700_bib1","doi-asserted-by":"publisher","first-page":"11","DOI":"10.1111\/j.1365-2966.2012.20802.x","volume":"424","author":"Affer","year":"2012","journal-title":"MNRAS"},{"key":"2024062400065960700_bib2","first-page":"223","volume-title":"SF2A-2016: Proc. 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Although rare, these ISOs can be captured into bound orbits around the Sun. In this study, we investigate the novel idea of capture of ISOs into near-Earth orbits and find that a steady population of ISOs exists among the current population of near-Earth objects (NEOs). Using numerical simulations, we find that the capture of ISOs into near-Earth orbits is dominated by Jupiter that is 104 times more efficient in capturing ISOs compared to Earth. Captured ISOs are more likely to be in orbits with high eccentricities and low inclinations. We also investigate the stability of captured ISOs and find that they are generally unstable and have an average survival lifetime of \u223c1\u00a0Myr, consistent with lifetime of NEOs originating from outer asteroid belt, and are ejected from the Solar system due to interactions with other planets or the Sun. Our results have important implications for understanding the population of ISOs in the Solar system and possible future detection. 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advances of the current generation of telescopes has been the detection of galaxies during the epoch of reionization, using deep fields that have pushed these instruments to their limits. It is essential to optimize our analyses of these fields in order to extract as much information as possible from them. In particular, standard methods of measuring the galaxy luminosity function discard information on large-scale dark matter density fluctuations, even though this large-scale structure drives galaxy formation and reionization during the Cosmic Dawn. Measuring these densities would provide a bedrock observable, connecting galaxy surveys to theoretical models of the reionization process and structure formation. Here, we use existing Hubble deep field data to simultaneously fit the universal luminosity function and measure large-scale densities for each Hubble deep field at z\u00a0= 6\u20138 by directly incorporating priors on the large-scale density field and galaxy bias. Our fit of the universal luminosity function is consistent with previous methods but differs in the details. For the first time, we measure the underlying densities of the survey fields, including the most over\/underdense Hubble fields. We show that the distribution of densities is consistent with current predictions for cosmic variance. This analysis on just 17 fields is a small sample of what will be possible with the James Webb Space Telescope, which will measure hundreds of fields at comparable (or better) depths and at higher redshifts.<\/jats:p>","DOI":"10.1093\/mnras\/stac2320","type":"journal-article","created":{"date-parts":[[2022,8,19]],"date-time":"2022-08-19T01:27:17Z","timestamp":1660872437000},"page":"4556-4567","source":"Crossref","is-referenced-by-count":0,"title":["A joint measurement of galaxy luminosity functions and large-scale field densities during the Epoch of Reionization"],"prefix":"10.1093","volume":"523","author":[{"ORCID":"https:\/\/orcid.org\/0000-0003-4650-9358","authenticated-orcid":false,"given":"A C","family":"Trapp","sequence":"first","affiliation":[{"name":"Department of Physics and Astronomy, University of California Los Angeles , Los Angeles, CA 90095-1562, USA"}]},{"ORCID":"https:\/\/orcid.org\/0000-0002-0658-1243","authenticated-orcid":false,"given":"Steven R","family":"Furlanetto","sequence":"additional","affiliation":[{"name":"Department of Physics and Astronomy, University of California Los Angeles , Los Angeles, CA 90095-1562, USA"}]}],"member":"286","published-online":{"date-parts":[[2022,8,18]]},"reference":[{"key":"2023081800543980300_bib1","doi-asserted-by":"publisher","first-page":"1853","DOI":"10.1093\/mnras\/stab2696","volume":"508","author":"Becker","year":"2021","journal-title":"MNRAS"},{"key":"2023081800543980300_bib2","doi-asserted-by":"publisher","first-page":"32","DOI":"10.1088\/0004-637X\/799\/1\/32","volume":"799","author":"Behroozi","year":"2015","journal-title":"ApJ"},{"key":"2023081800543980300_bib3","doi-asserted-by":"publisher","first-page":"754","DOI":"10.1093\/mnras\/staa1605","volume":"496","author":"Bhowmick","year":"2020","journal-title":"MNRAS"},{"key":"2023081800543980300_bib4","doi-asserted-by":"publisher","first-page":"440","DOI":"10.1086\/170520","volume":"379","author":"Bond","year":"1991","journal-title":"ApJ"},{"key":"2023081800543980300_bib5","doi-asserted-by":"publisher","first-page":"34","DOI":"10.1088\/0004-637X\/803\/1\/34","volume":"803","author":"Bouwens","year":"2015","journal-title":"ApJ"},{"key":"2023081800543980300_bib7","doi-asserted-by":"publisher","first-page":"25","DOI":"10.3847\/1538-4357\/ab24c5","volume":"880","author":"Bouwens","year":"2019","journal-title":"ApJ"},{"key":"2023081800543980300_bib6","doi-asserted-by":"publisher","first-page":"47","DOI":"10.3847\/1538-3881\/abf83e","volume":"162","author":"Bouwens","year":"2021","journal-title":"AJ"},{"key":"2023081800543980300_bib8","doi-asserted-by":"publisher","first-page":"2810","DOI":"10.1093\/mnras\/stu449","volume":"440","author":"Bowler","year":"2014","journal-title":"MNRAS"},{"key":"2023081800543980300_bib9","doi-asserted-by":"publisher","first-page":"1817","DOI":"10.1093\/mnras\/stv1403","volume":"452","author":"Bowler","year":"2015","journal-title":"MNRAS"},{"key":"2023081800543980300_bib10","doi-asserted-by":"publisher","first-page":"2059","DOI":"10.1093\/mnras\/staa313","volume":"493","author":"Bowler","year":"2020","journal-title":"MNRAS"},{"key":"2023081800543980300_bib11","doi-asserted-by":"publisher","first-page":"L23","DOI":"10.3847\/2041-8213\/aa7e7b","volume":"844","author":"Chiang","year":"2017","journal-title":"ApJ"},{"key":"2023081800543980300_bib12","doi-asserted-by":"publisher","first-page":"87","DOI":"10.3847\/1538-4357\/ac2a34","volume":"923","author":"Christenson","year":"2021","journal-title":"ApJ"},{"key":"2023081800543980300_bib13","doi-asserted-by":"publisher","first-page":"155","DOI":"10.3847\/1538-4357\/aac2d6","volume":"860","author":"Davies","year":"2018","journal-title":"ApJ"},{"key":"2023081800543980300_bib14","doi-asserted-by":"publisher","first-page":"605","DOI":"10.1086\/305424","volume":"496","author":"Eisenstein","year":"1998","journal-title":"ApJ"},{"key":"2023081800543980300_bib15","doi-asserted-by":"publisher","first-page":"6044","DOI":"10.1093\/mnras\/stab432","volume":"502","author":"Endsley","year":"2021","journal-title":"MNRAS"},{"key":"2023081800543980300_bib16","doi-asserted-by":"publisher","first-page":"71","DOI":"10.1088\/0004-637X\/810\/1\/71","volume":"810","author":"Finkelstein","year":"2015","journal-title":"ApJ"},{"key":"2023081800543980300_bib17","doi-asserted-by":"publisher","first-page":"52","DOI":"10.3847\/1538-4357\/ac3aed","volume":"928","author":"Finkelstein","year":"2022","journal-title":"ApJ"},{"key":"2023081800543980300_bib18","doi-asserted-by":"publisher","first-page":"1576","DOI":"10.1093\/mnras\/stx2132","volume":"472","author":"Furlanetto","year":"2017","journal-title":"MNRAS"},{"key":"2023081800543980300_bib19","doi-asserted-by":"publisher","first-page":"485","DOI":"10.1038\/s41550-020-01291-y","volume":"5","author":"Hu","year":"2021","journal-title":"Nat. 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In this method, optical variations of AGNs are monitored and CL-AGNs may appear to have a pattern of being bluer when in brightening flare-like events. Applying this method, previously classified type 2 AGNs that show the bluer-when-brighter (BWB) pattern are selected. Among more than ten thousands type 2 AGNs classified in the Sloan Digital Sky Survey (SDSS), we find 73 candidates with possibly the strongest BWB pattern. We note that 13 of them have previously been reported as CL-AGNs. We have observed nine candidates, and found that five among them showed the CL transition from type 2 to type 1. In addition, we also test extending the selection to previously classified type 1 AGNs in the SDSS by finding sources with a possible redder-when-brighter pattern, but none of the three sources observed by us is found to show the transition from type 1 to type 2. 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We generalize the analysis of Chandrasekhar, who determined that the threshold for instability of a self-gravitating hydrostatic body lies at \u03b3 = 4\/3, to account for the presence of a planetary core, which we model as an incompressible fluid. We show that the dominant effect of the core is to stabilize the envelope to radial perturbations, in some cases completely (i.e. for all \u03b3 &amp;gt; 1). When instability is possible, unstable planetary configurations occupy a strip of \u03b3 values whose upper boundary falls below \u03b3 = 4\/3. 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