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| = ISC Meeting on 2018/1/15 14:00 - 15:00 = Participants: |
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| eZuce meeting: "KAGRA ISC Meeting" in the KEK community. === Next meeting === 2018/1/29 14:00 - 15:00 ?? [[LCGT/subgroup/ifo/ISC/Meetings|back to Meetings page]] == Agenda == * KAGRA configuration for early phase of bKAGRA [[https://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/private/DocDB/ShowDocument?docid=7334|JGW-T1707334]] {*} * SRM reflectivity * Mirror ordered * Black coating for metal mass? * ETM swap * timing depends on final ETMX arrival * ITM asymmetry [Enomoto] [[https://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/private/DocDB/ShowDocument?docid=7565|JGW-T1707565]] {*} * ITM asymmetry is OK for early stages, but asymmetric ITMs cannot be used for achieving design sensitivity * bKAGRA Phase 1 [Michimura] * no AS optics for Phase 1, instead use reflection REFL beam from PRM * we have to prepare REFL optics * height of the beam from PR/BS breadboard will be 380 mm instead of 400 mm * bKAGRA Phase 2 schedule [Michimura] [[https://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/private/DocDB/ShowDocument?docid=7079|JGW-T1707079]] * meeting with SEO on Sept 6 * Goal: 1 hour lock of cryogenic RSE with RF readout, probably with ASC, no sensitivity goal * input laser power not decided * when to swap ETM, SRM reflectivity, vacuum * schedule adjustment between AS WFS and OMC test necessary * bKAGRA cables [Michimura] [[https://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/private/DocDB/ShowDocument?docid=7586|JGW-T1707586]] {*} * cable lengths depend on the position of ISC racks * discussion in the week of Jan 22? * PSL EOM Layout re-consideration [Enomoto] ([[https://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/private/DocDB/ShowDocument?docid=6748|JGW-T1706748]]) * Delay-line length decided to be 2.66 m (instead of 8.88 m) * Modulation phase between f1 AM and PM is always aligned (we need this to be aligned) * Modulation index needed at each EOM is less than measured maximum index by Uehera ([[https://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/private/DocDB/ShowDocument?docid=5611|JGW-T1605611]]) * Optickle simulation by Kohei Yamamoto [[https://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/private/DocDB/ShowDocument?docid=7309|JGW-G1707309]] {*} * simulation on imperfections (MZ arm asymmetry, MZ lock, EOM phase difference control etc.) * start with hand calculation, simple setups, and then to full IFO simulation * Optickle model basically made, and checked with hand calculations * calculations for requirements on delay line lock displacement noise, parallel EOM MZ lock displacement noise, EOM modulation phase difference, EOM imbalance on-going * A/I: check phase noise calculations, requirements for f1 AM-PM mixed case [Kohei Yamamoto] * Requirement on carrier power loss? * Comment from Stefan Ballmer * Similar calculation was done in LIGO in the past. Displacement noise requirement for MZ was tough (~1e-14 m/rtHz). * Any in-air interferometer suffer from jitter and frequency noise which cannot be suppressed. ---- * IMMT1 and IMMT2 transmission [Michimura, Takeda] * IMMT2 transmission optics are too much squeezed * IR/green steering mirrors [Michimura] * mirrors arrived, mirror mounts and picomotor driver ordered, pedestals by Akutsu, vacuum cables by Aso * DC QPD holder [Michimura] * beam height should be 4inch to use similar mount, with small modification of spacer (instead of 3inch in [[https://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/private/DocDB/ShowDocument?docid=2607|JGW-D1402607]]) * RF PD, RF QPD boxes are designed for 4inch beam height * stages are not needed for ISC DC QPD * design new ones; they can be very simple [-> Michimura?] * calibration can be done in different ways * put strain relief and anchors for cables to protect QPD board * OMC and OFI [Somiya] * look for OFI with larger aperture [Somiya] * DC PD and DC QPD [Michimura] * DC PD not available. Look for product with similar specs * DC QPD available from RS * In-vacuum RF PD and RF QPD {*} * we need them within 1 year, considering OMC REFL and AS RF * In-vac beam-dumps {*} * required spec? * Actuator noise modeling [Michimura,Miyamoto] * Summarized in the paper [[https://gwdoc.icrr.u-tokyo.ac.jp/cgi-bin/private/DocDB/ShowDocument?docid=7051|JGW-P1707051]] * Needs to implement frequency noise, but FSS modeling with ALS is complicated [student!] * Discuss mirror vibration from heat link {*} * Meeting on July 14 [Yamada, Miyamoto, Ushiba, Michimura] See [[KAGRA/subgroup/ifo/MIF/Minutes20170410|this page]] for other agendas. |
[[KAGRA/subgroup/ifo/MIF/Minutes20180115]] |
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