1 / 18

Kenneth Wraight, Andrew Blue, Kate Doonan & Sam Crawley

Kenneth Wraight, Andrew Blue, Kate Doonan & Sam Crawley. SLAC. SLAC. End Station A. Remote control required. Parasites & Particles. ESTB is parasitic beam from Linac Coherent Light Source Secondary beam of electrons up to 13.6GeV of LCLS beam 5Hz standard bunch frequency

todd
Télécharger la présentation

Kenneth Wraight, Andrew Blue, Kate Doonan & Sam Crawley

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. Kenneth Wraight, Andrew Blue, Kate Doonan & Sam Crawley SLAC

  2. SLAC Andy Blue

  3. End Station A Remote control required. Andy Blue

  4. Parasites & Particles ESTB is parasitic beam from Linac Coherent Light Source Secondary beam of electrons up to 13.6GeV of LCLS beam 5Hz standard bunch frequency Variable particle number per bunch SLAC benefits Triggering available from beam Larger region of interest than previous scintillator limited area Reduced multiple scattering Possible to take data with more devices in beam Andy Blue

  5. Beam Conditions Data taken with various conditions 5 & 10Hz frequencies dependent on LCLS users Varying charge per bunch Dependent on LCLS users some control with beam slits Consistent beam energy of 12.5GeV Used multiple devices in beam 2 – 4 devices used --> 6 – 10 sensor planes Limited by available power, mounts and cooling for devices More made as testbeam developed Andy Blue

  6. Telescope and device setup Telescope visiting from DESY from April to July Far side (Mimosa 5) Beam side (Mimosa 0) Devices <-- mounted and cooled --> Andy Blue

  7. (Remote) Control of devices EUTelescope Config for runs (devices) (semi-)Online monitor (not full quad monitor) RCE Usd to read out pixel devices Setting configs and thresholds DCS Voltage settings (HV > 500V, low voltages were 1.2V & 1.5V) Humidity & temperature monitors Teamviewer Linked to laptop in beam hall Peltier control and additional temperature monitoring Andy Blue

  8. Itinerary Tue 28/4 arrived in Palo Alto Wed 29/4 arrived SLAC: training and registration Thu 30/4 access to ESA: basic tour Fri 1/5 set-up and tune devices, begin data taking with Q5 Found out customs holding irr. devices over weekend Sat 2/5 data taking: Q5 and singles 10Hz periods, variable beam conditions Sun 3/5 data taking: singles Mon 4/5 set-up for irr. devices, data-taking: singles Receive irr. devices around noon; irr. quad and 125x100 broken Tue 5/5 data-taking: singles + Igor's angled measurements Wed 5/6 dismantle set-up Andy Blue

  9. Data taken Unirradiated Quad – data taken: 3 regions @ 100V, THL=2500 & 3000e 250x50 – data taken: 50 & 100V, THL=2500e 500x25 – data taken: 50 & 100V, THL=1.5, 2, 2.5, 3 ke 125x167 – data taken: 50 & 100V, THL=2500 & 3000 ke irradiated Quad – no data: unable to tune, 8mA @ 15V (no analogue) 250x50 – data taken: 0V, THL=1.5, 2, 2.5, 3 ke (broken bonds?) 500x25 – data taken: 100V, THL=1.5, 2, 2.5, 3 ke 125x167 – data taken: 100V, THL=1.5, 2, 2.5, 3 ke Andy Blue

  10. Irr. 500x25 IV Limited bias of device due to large leakage current Andy Blue

  11. Initial cluster scans Used online monitor and initial clustered reconstruction to check data quality 2k triggers 2k triggers Andy Blue

  12. 125x167 structure Can see structure in 125x167 online monitor Unbonded pixels due to mismatch of geometry 14

  13. Experience Facility Very helpful local support: from equipment to personnel >21hrs beam/day (2hrs MD); always updated by MCC Presence of other users important i.e. 5->10Hz (+ beam energy) Telescope After ironing out a few bugs, everyone gained experience Important to have experts available: Martin, Igor, Jens Bonus of triggering from beam DCS system was simple and easy to use: Voltage, humidity, temp Detectors Despite customs trouble, managed good runs Multiple devices tested in beam (e.g. Q+2sc, 4sc) Andy Blue

  14. Conclusions Experience of facility very positive Most training could be done online prior to arrival Local support very helpful: Philippe Grenier, Max Swiatlowski Very helpful with equipment & requests: cabling, dry ice Great experience for testbeam team Running all aspects of data-taking from Peltier cooling to configuring telescope Excellent beam conditions Triggering: larger RoI Energy: more devices possible per run Potential for increased statistics in future Andy Blue

  15. Advice for Strips work Proposal needed Sergio will write 1 for FCF work Volunteered to help write the abc130nm proposal Being a registered SLAC user should hopefully help Contacts For telescope issues, Igor Rubinsky For SLAC/facility issues, Philippe Grenier & Carsten Hast Data taking Can tune beam spot to less than we had Can control no. electron per bunch from 1-3 to 100 (at 5Hz) Are we anywhere near max occupancy for some of these numbers? After alignment data taking time should not be too long Reconstruction Currently standard for pixels More than happy to use our experience to help adapt for Strips CMS already tested strip devices with this telescope. Access to recon?...

  16. Back up Back up Andy Blue

  17. Triggering Trigger is from a scintillator attached to 1st telescope plane Only a fraction of coverage of 1 CMOS chip Scintillator Quad Module Reference sensor 19 19

  18. Quad RoIs Use automated stage to change position of beam Beam size of ~2x2cm (Perfect!) Centred Beam up from Centre Beam Left of Centre

More Related