BEGIN:VCALENDAR
VERSION:2.0
PRODID:-//LBNL Physics Division Research Progress Meetings - ECPv6.8.3//NONSGML v1.0//EN
CALSCALE:GREGORIAN
METHOD:PUBLISH
X-ORIGINAL-URL:https://rpm.physics.lbl.gov
X-WR-CALDESC:Events for LBNL Physics Division Research Progress Meetings
REFRESH-INTERVAL;VALUE=DURATION:PT1H
X-Robots-Tag:noindex
X-PUBLISHED-TTL:PT1H
BEGIN:VTIMEZONE
TZID:UTC
BEGIN:STANDARD
TZOFFSETFROM:+0000
TZOFFSETTO:+0000
TZNAME:UTC
DTSTART:20190101T000000
END:STANDARD
END:VTIMEZONE
BEGIN:VEVENT
DTSTART;TZID=UTC:20191203T160000
DTEND;TZID=UTC:20191203T170000
DTSTAMP:20260416T213217
CREATED:20191022T015919Z
LAST-MODIFIED:20191122T164308Z
UID:1262-1575388800-1575392400@rpm.physics.lbl.gov
SUMMARY:Tommaso Ghigna (Oxford U.)  "The quest for CMB B-modes and the challenge of controlling systematic effects"
DESCRIPTION:Abstract:  \nThe Cosmic Microwave Background has played a central role for cosmology in the past few decades. From the very first detection of its temperature more than 50 years ago to the measurement of the temperature anisotropy\, every step contributed to advancing our understanding of the fundamental laws that govern our Universe. One of the most ambitious targets of current and future experiments is the detection of the primordial polarized B-mode signal. This signal is a tracer of inflation and it is expected to be most visible at large angular scales.\nI will review the current status of the search for B-modes focusing on one of the main challenges: instrumental systematic effects and strategies to keep them under control. In particular I will discuss the impact of band-pass uncertainty in the presence of Galactic foregrounds. I will describe a simulation procedure developed to study the induced bias into CMB polarization maps\, and the recovered tensor-to-scalar ratio parameter. I will describe the connection between the simulation results and the instrumental parameters for a representative space mission\, and define requirements to minimize the effect. Furthermore\, I will introduce our current plan to develop a testbed\, which we can use to address multiple systematic effects without waiting for the fully assembled instrument. \nThe required sensitivity for a definitive measurement of the B-mode signal is extremely challenging\, and focal planes of experiments are growing in size to increase the optical throughput in order to meet the requirements. This will require extra efforts in designing\, fabricating\, and testing all telescope components; only through meticulous knowledge of the instrument and all its sub-systems\, as well as a careful calibration\, we will be able to reach this ambitious goal.
URL:https://rpm.physics.lbl.gov/event/reserved-74/
LOCATION:HYBRID 50A-5132 (Sessler Conference Room)\, https://lbnl.zoom.us/j/91782268585\, 50A-5132
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=UTC:20191205T160000
DTEND;TZID=UTC:20191205T170000
DTSTAMP:20260416T213217
CREATED:20191022T015940Z
LAST-MODIFIED:20191119T165434Z
UID:1264-1575561600-1575565200@rpm.physics.lbl.gov
SUMMARY:Peter Timbie (UW-Madison) "21cm Intensity Mapping: A New Cosmological Tool?"
DESCRIPTION:ABSTRACT: \nThe 21 cm line from neutral hydrogen gas has many useful properties for mapping large volumes of the cosmos. These maps will give us a view of the Universe when the first luminous objects formed through gravity – the Cosmic Dawn and the Epoch of Reionization\, and later\, the post-Reionization Universe. They may even allow us to map the epoch before these luminous objects\, the cosmic dark ages. The large volumes of these maps promise dramatic improvements in estimation of cosmological parameters. Data is flowing now from a new generation of radio telescopes optimized for this task. Unfortunately\, the main challenge for all of them is that the astrophysical radio foregrounds are ~10\,000 times brighter than the expected hydrogen signal. In this talk I will focus on current and planned efforts to use the new technique of` ‘hydrogen intensity mapping’ to make tomographic maps of the post-Reionization universe. In particular\, I will describe the first measurements from an instrument in China\, called the Tianlai (‘Cosmic Sound’) Pathfinder.
URL:https://rpm.physics.lbl.gov/event/reserved-75/
LOCATION:HYBRID 50A-5132 (Sessler Conference Room)\, https://lbnl.zoom.us/j/91782268585\, 50A-5132
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=UTC:20191210T160000
DTEND;TZID=UTC:20191210T170000
DTSTAMP:20260416T213217
CREATED:20191022T020012Z
LAST-MODIFIED:20191209T163920Z
UID:1266-1575993600-1575997200@rpm.physics.lbl.gov
SUMMARY:Jelle Aalbers (Stockholm U) "XENON1T: When All Other Lights Go Out"
DESCRIPTION:Abstract:\nDirect detection experiments create the most radioactively quiet spots on earth\, to reveal collisions between dark and ordinary matter. XENON1T\, the most sensitive such experiment currently\, will soon be succeeded by LZ and XENONnT. This talk highlights XENON1T’s recent light dark matter search results\, and modern analysis techniques — full online processing\, and tensorflow-based profile likelihoods — to boost the physics reach of future direct detection experiments and other rare-event searches.
URL:https://rpm.physics.lbl.gov/event/reserved-76/
LOCATION:50B-4205
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=UTC:20191212T160000
DTEND;TZID=UTC:20191212T170000
DTSTAMP:20260416T213217
CREATED:20191022T020036Z
LAST-MODIFIED:20191209T164108Z
UID:1268-1576166400-1576170000@rpm.physics.lbl.gov
SUMMARY:Qing Shilo Xia (Yale) "Hunting for neutrinoless double beta decay with liquid xenon detectors"
DESCRIPTION:Abstract:  \n\nLiquid xenon (LXe) is employed in a number of current and future detectors for rare event searches. In this talk\, I will present the latest results from EXO-200\, which searched for neutrinoless double beta decay (0υββ) in Xe-136 between 2011 and 2018. I will also present a measurement of the absolute scintillation and ionization response generated by MeV energy gamma sources over a range of electric fields in EXO-200. These measurements are useful for simulating the performance of future 0υββ detectors employing LXe\, such as nEXO\, which is a next generation 0υββ experiment using Xe-136 aiming to reach a half-life sensitivity ~10^28 years. nEXO will require ultra-low radioactivity\, high-speed cabling to carry digital signals from in-LXe electronics. I will describe the development of high-bandwidth digital cable prototypes with sufficiently low radioactivity for use in the experiment. While designed specifically for nEXO\, the demonstration of radiopure high-bandwidth cabling and interconnection techniques is relevant for many next-generation rare-event searches with large channel counts and high-speed digital electronics.
URL:https://rpm.physics.lbl.gov/event/reserved-77/
LOCATION:HYBRID 50A-5132 (Sessler Conference Room)\, https://lbnl.zoom.us/j/91782268585\, 50A-5132
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=UTC:20191217T160000
DTEND;TZID=UTC:20191217T170000
DTSTAMP:20260416T213217
CREATED:20191022T020055Z
LAST-MODIFIED:20191210T201048Z
UID:1270-1576598400-1576602000@rpm.physics.lbl.gov
SUMMARY:Sumit Dahal (Johns Hopkins U) "The Cosmology Large Angular Scale Surveyor: Detector Design and Performance"
DESCRIPTION:Abstract: \nThe Cosmology Large Angular Scale Surveyor (CLASS) aims to characterize the primordial gravitational waves at the level of tensor-to-scalar ratio of 0.01\, and make a cosmic-variance-limited measurement of the optical depth to reionization. CLASS is an array of four telescopes that surveys 70% of the microwave sky from the Atacama Desert at 40\, 90\, 150\, and 220 GHz frequency bands. A unique combination of large sky coverage\, rapid front-end polarization modulator\, broad frequency coverage\, and background-limited detectors enables CLASS to characterize the B-mode and E-mode power spectra on both the reionization and recombination scales. The detector arrays for all four CLASS telescopes contain smooth-walled feedhorns that couple to transition-edge sensor bolometers through planar orthomode transducers fabricated on mono-crystalline silicon. In this talk\, I will give an overview of the design and performance of the CLASS detectors and provide an update on the current status of CLASS telescopes.
URL:https://rpm.physics.lbl.gov/event/reserved-78/
LOCATION:HYBRID 50A-5132 (Sessler Conference Room)\, https://lbnl.zoom.us/j/91782268585\, 50A-5132
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=UTC:20191219T160000
DTEND;TZID=UTC:20191219T170000
DTSTAMP:20260416T213217
CREATED:20191022T020125Z
LAST-MODIFIED:20191022T020149Z
UID:1272-1576771200-1576774800@rpm.physics.lbl.gov
SUMMARY:Reserved
DESCRIPTION:
URL:https://rpm.physics.lbl.gov/event/reserved-79/
LOCATION:HYBRID 50A-5132 (Sessler Conference Room)\, https://lbnl.zoom.us/j/91782268585\, 50A-5132
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=UTC:20191224T160000
DTEND;TZID=UTC:20191224T170000
DTSTAMP:20260416T213217
CREATED:20191022T020220Z
LAST-MODIFIED:20191022T020220Z
UID:1274-1577203200-1577206800@rpm.physics.lbl.gov
SUMMARY:Reserved
DESCRIPTION:
URL:https://rpm.physics.lbl.gov/event/reserved-80/
LOCATION:HYBRID 50A-5132 (Sessler Conference Room)\, https://lbnl.zoom.us/j/91782268585\, 50A-5132
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=UTC:20191226T160000
DTEND;TZID=UTC:20191226T170000
DTSTAMP:20260416T213217
CREATED:20191022T020246Z
LAST-MODIFIED:20191022T020246Z
UID:1276-1577376000-1577379600@rpm.physics.lbl.gov
SUMMARY:Reserved
DESCRIPTION:
URL:https://rpm.physics.lbl.gov/event/reserved-81/
LOCATION:HYBRID 50A-5132 (Sessler Conference Room)\, https://lbnl.zoom.us/j/91782268585\, 50A-5132
END:VEVENT
BEGIN:VEVENT
DTSTART;TZID=UTC:20191231T160000
DTEND;TZID=UTC:20191231T170000
DTSTAMP:20260416T213217
CREATED:20191022T020313Z
LAST-MODIFIED:20191022T020313Z
UID:1278-1577808000-1577811600@rpm.physics.lbl.gov
SUMMARY:Reserved
DESCRIPTION:
URL:https://rpm.physics.lbl.gov/event/reserved-82/
LOCATION:HYBRID 50A-5132 (Sessler Conference Room)\, https://lbnl.zoom.us/j/91782268585\, 50A-5132
END:VEVENT
END:VCALENDAR