[ *.pdf format<\/a>\u00a0]<\/strong> [ *.pdf format<\/a>\u00a0] \u00a0[ *.pptx\u00a0format<\/a> ] \u00a0[ *.key\u00a0format<\/a> ] [ *.m4v format<\/a> ]<\/strong> [ *.pdf format<\/a>\u00a0] \u00a0[ *.pptx\u00a0format<\/a> ] \u00a0[ *.key\u00a0format<\/a> ] \u00a0[ *.tar.gz\u00a0format<\/a> ] \u00a0[ *.zip format<\/a> ]<\/strong> AAr UAr Spectra Null Field [ Plot (pdf)<\/a>\u00a0] AAr UAr Null Field Fits [ Plot (pdf)<\/a>\u00a0] [1]\u00a0P. Agnes, et al. (The DarkSide Collaboration), Phys. Lett. B, 743<\/strong>, 456 (2015)<\/a>. UAr Paper Submitted to arXiv: [ *.pdf format\u00a0] Public Summary Slides: [ *.pdf format\u00a0] \u00a0[ *.pptx\u00a0format ] \u00a0[ *.key\u00a0format […]<\/p>\n","protected":false},"author":4,"featured_media":0,"comment_status":"closed","ping_status":"closed","sticky":false,"template":"","format":"standard","meta":{"footnotes":""},"categories":[1],"tags":[],"class_list":["post-653","post","type-post","status-publish","format-standard","hentry","category-uncategorized"],"_links":{"self":[{"href":"https:\/\/darkside.lngs.infn.it\/index.php?rest_route=\/wp\/v2\/posts\/653","targetHints":{"allow":["GET"]}}],"collection":[{"href":"https:\/\/darkside.lngs.infn.it\/index.php?rest_route=\/wp\/v2\/posts"}],"about":[{"href":"https:\/\/darkside.lngs.infn.it\/index.php?rest_route=\/wp\/v2\/types\/post"}],"author":[{"embeddable":true,"href":"https:\/\/darkside.lngs.infn.it\/index.php?rest_route=\/wp\/v2\/users\/4"}],"replies":[{"embeddable":true,"href":"https:\/\/darkside.lngs.infn.it\/index.php?rest_route=%2Fwp%2Fv2%2Fcomments&post=653"}],"version-history":[{"count":0,"href":"https:\/\/darkside.lngs.infn.it\/index.php?rest_route=\/wp\/v2\/posts\/653\/revisions"}],"wp:attachment":[{"href":"https:\/\/darkside.lngs.infn.it\/index.php?rest_route=%2Fwp%2Fv2%2Fmedia&parent=653"}],"wp:term":[{"taxonomy":"category","embeddable":true,"href":"https:\/\/darkside.lngs.infn.it\/index.php?rest_route=%2Fwp%2Fv2%2Fcategories&post=653"},{"taxonomy":"post_tag","embeddable":true,"href":"https:\/\/darkside.lngs.infn.it\/index.php?rest_route=%2Fwp%2Fv2%2Ftags&post=653"}],"curies":[{"name":"wp","href":"https:\/\/api.w.org\/{rel}","templated":true}]}}
\n <\/p>\nPublic Summary Slides:<\/h1>\n
\n <\/p>\nAll Plots & Captions**:<\/h1>\n
\n** Captions for [ *.pptx ] and [ *.key ] formats only.
\n <\/p>\nIndividual Paper Plots:<\/h1>\n
\n<\/strong>Live-time-normalized S1-late pulse integral spectra obtained at zero drift field, with an AAr fill (black) and a UAr fill (blue).\u00a0 <\/span>Also shown are the GEANT4 MC fit to the UAr data (red) and individual components of <\/span>85<\/sup><\/span>Kr (green) and <\/span>39<\/sup><\/span>Ar (orange) extracted from the fit.<\/span>
\nAAr UAr Spectra Drift Field [ Plot (pdf)<\/a>\u00a0]<\/strong>
\nLive-time normalized S1 pulse integral spectra from single-scatter events in AAr (black) and UAr (blue) taken with 200 V\/cm drift field.\u00a0 <\/span>Also shown are the <\/span>85<\/sup><\/span>Kr (green) and <\/span>39<\/sup><\/span>Ar (orange) levels as inferred from a MC fit.\u00a0 <\/span>Note the peak in the lowest bin of the UAr spectrum, which is due to <\/span>37<\/sup><\/span>Ar from cosmic-ray activation.\u00a0 <\/span>The peak at \u223c600 PE is due to \u03b3-ray Compton scatters.<\/span>
\nUAr AmBe DMS St Cut [ Plot (pdf)<\/a>\u00a0]
\n<\/strong><\/strong>f<\/span>90<\/sub><\/span> NR median vs. S1 from a high-rate in situ AmBe calibration (blue) and scaled from SCENE measurements (red points).\u00a0 <\/span>Events in the region between the NR and ER bands are due to inelastic scattering of high energy neutrons, accidentals, and correlated neutron and \u03b3-ray emission by the AmBe source.<\/span>
\nUAr Efficiency St Cut [ Plot (pdf)<\/a>\u00a0]
\n<\/strong><\/strong>Combined acceptance of the physics cuts (red), acceptance of the f<\/span>90<\/sub><\/span> NR cut (green) and the final cumulative NR acceptance in UAr data (black).<\/span>
\nUAr 2015 DMS Std Cut [ Plot (pdf)<\/a>\u00a0]
\n<\/strong>Distribution of events in the f<\/span>90<\/sub><\/span> vs S1 plane which survive all quality and physics cuts (including veto cuts).\u00a0 <\/span>Shaded blue with solid blue outline: WIMP search region.\u00a0 <\/span>Percentages label the f<\/span>90<\/sub><\/span> acceptance contours for NRs, drawn by connecting points (shown with uncertainties) at which the acceptance was determined from the corresponding SCENE measurements.\u00a0 <\/span>Lighter shaded blue with dashed blue line show that extending the WIMP search region to 90% f<\/span>90<\/sub><\/span> NR acceptance is still far away from ER backgrounds.<\/span>
\nUAr 2015 DMS Stwo Cut [ Plot (pdf)<\/a>\u00a0]
\n<\/strong><\/strong>Distribution of events in the f<\/span>90<\/sub><\/span> vs S1 plane which survive all quality and physics cuts, and which in addition survive a radial cut and a S2\/S1 cut (see text).<\/span>
\nUAr 2015 Exclusion [ Plot (pdf)<\/a>\u00a0]
\n<\/strong><\/strong>Comparison of spin-independent WIMP-nucleon cross section 90% C.L. exclusion plot for the DarkSide-50 AAr (dotted red) and UAr campaign (dashed red), and combination of the UAr and AAr [1] campaigns (solid red). \u00a0Also shown are results from LUX [21] (solid black), XENON100 [22] (dashed black), CDMS [23] (solid green), PandaX-I [24] (dotted black), WARP [25] (solid magenta) and PICO [26] (solid cyan).
\n <\/p>\nSupporting Analysis Plots:<\/h1>\n
\n<\/strong><\/strong>Live-time-normalized S1-late pulse integral spectra obtained at zero drift field, with an AAr fill (black) and a UAr fill (blue).\u00a0 <\/span>Also shown are the GEANT4 MC fit to the UAr data (red) and individual components extracted from the fit.<\/span>
\nUAr 85Kr 85mRb Spectrum [ Plot (pdf)<\/a>\u00a0]
\n<\/strong><\/strong>Spectrum of <\/span>85<\/sup><\/span>Kr beta decay to the metastable state of <\/span>85<\/sup><\/span>Rb, occurring in 0.4% of <\/span>85<\/sup><\/span>Kr decays, shown after the removal of events with the associated <\/span>85<\/sup><\/span>Rb decay \u03b3-ray escaping the inner detector.<\/span>
\nUAr 85mKr Decay Time [ Plot (pdf)<\/a>\u00a0]
\n<\/strong><\/strong>Decay time of the metastable state of <\/span>85<\/sup><\/span>Rb, resulting from 0.4% of <\/span>85<\/sup><\/span>Kr beta decays, along with an exponential fit to the data that agrees with the expected value, within uncertainties.<\/span>
\nUAr AmBe S2\/S1 [ Plot (pdf)<\/a>\u00a0]
\n<\/strong><\/strong>Distribution of Log(S2\/S1) for AAr data (black) and AmBe calibration (blue) data, after the application of a radial fiducial volume cut placed 10 cm from the wall, for events with S1 in the range 300-400 PE.\u00a0 <\/span>Alphas emitted from <\/span>241<\/sup><\/span>Am capture on <\/span>9<\/sup><\/span>Be, producing a neutron and <\/span>12<\/sup><\/span>C<\/span>*<\/sup><\/span>.\u00a0 <\/span>The left peak of the AmBe data comes from the neutrons, while the right peak comes from the 4.43 MeV <\/span>12<\/sup><\/span>C<\/span>*<\/sup><\/span> deexcitation \u03b3-rays.<\/span>
\nUAr AmBe F90 S2\/S1 [ Plot (pdf)<\/a>\u00a0]
\n<\/strong><\/strong>Log(S2\/S1) versus f<\/span>90<\/sub><\/span> of AmBe calibration data, for events with S1 in the range 200-400 PE and an applied veto cut. The cluster with larger f<\/span>90<\/sub><\/span> results from the neutrons coming from the <\/span>241<\/sup><\/span>Am decay-alpha captures on <\/span>9<\/sup><\/span>Be, while the cluster with smaller f<\/span>90<\/sub><\/span> results from the <\/span>12<\/sup><\/span>C<\/span>*<\/sup><\/span> deexcitation \u03b3-rays.<\/span>
\nAAr UAr F90 [ Plot (pdf)<\/a>\u00a0]
\n<\/strong><\/strong>Comparison of the f<\/span>90<\/sub><\/span> distributions for AAr data (black), UAr data (blue) data and UAr core data (red), in the range of 60 to 150 PE.\u00a0 <\/span>All data are restricted to drift times between 40 and 334.6 us.\u00a0 <\/span>In addition, UAr core data restricts radius to be within 14.14 cm of the TPC center.\u00a0 <\/span>Each distribution is normalized by their respective number of events, to make the comparison of their shapes.\u00a0<\/span>
\nDAr 2014 St Cut DMS [ Plot (pdf)<\/a>\u00a0]
\n<\/strong><\/strong>AAr distribution of events in the S1 vs. f<\/span>90<\/sub><\/span> plane, after all quality and physics cuts.\u00a0 <\/span>Shaded blue with solid blue outline: dark matter search box in the f<\/span>90<\/sub><\/span> vs. S1 plane.\u00a0 <\/span>Percentages label the f<\/span>90<\/sub><\/span> acceptance contours for nuclear recoils drawn connecting points (shown with error bars) determined from the corresponding SCENE measurements.<\/span>
\nUAr 3yr Exclusion [ Plot (pdf)<\/a>\u00a0]
\n<\/strong><\/strong>Expected spin-independent WIMP-nucleon cross section sensitivity (90% C.L.) of DarkSide-50 after 3 years running with UAr (solid blue). \u00a0Also shown are the 90% C.L. exclusion plots for the DarkSide-50 AAr (dotted red) and UAr campaign (dashed red), and combination of the UAr and AAr [1] campaigns (solid red), LUX [21] (solid black), XENON100 [22] (dashed black), CDMS [23] (solid green), PandaX-I [24] (dotted black), WARP [25] (solid magenta) and PICO [26] (solid cyan).
\nArgo Projected Exclusion [ Plot (pdf)<\/a>\u00a0]
\n<\/strong><\/strong>Expected spin-independent WIMP-nucleon cross section sensitivity (90% C.L.) of DarkSide-50 after three years of UAr running (solid blue), DarkSide-20k (dashed blue) and Argo (dotted blue). \u00a0Also shown are the 90% C.L. exclusion plots for DarkSide-50 [1] (solid red), LUX [21] (solid black), XENON100 [22] (dashed black), CDMS [23] (solid green), PandaX-I [24] (dotted black), WARP [25] (solid magenta) and PICO [26] (solid cyan).
\n <\/p>\nReferences:<\/h1>\n
\n[21]\u00a0D. S. Akerib, et al. (The LUX Collaboration), Phys. Rev. Lett., 112<\/strong>, 091303 (2014)<\/a>.
\n[22]\u00a0E. Aprile, et al. (The XENON100 Collaboration), Phys. Rev. Lett., 109<\/strong>, 181301 (2012)<\/a>.
\n[23] R. Agnese, et al. (The SuperCDMS Collaboration), Phys. Rev. D, 92, 072003 (2015)<\/a>.
\n[24]\u00a0M. Xiao, et al. (The PandaX Collaboration), Sci. China Phys. Mech. Astron., 57<\/strong>, 2024 (2014)<\/a>.
\n[25]\u00a0P. Benetti, et al. (The WArP Collaboration), Astropart. Phys., 28<\/strong>, 495 (2008)<\/a>.
\n[26] C. Amole, et al. (The PICO\u00a0Collaboration), ArXiV 1510:07754 (2015)<\/a>.
\n <\/p>\n","protected":false},"excerpt":{"rendered":"