1 / 15

Luminosity Monitoring Issues

Luminosity Monitoring Issues. ZDC what’s the advantage? problems BBC can they do it?. A. Drees QCD critical point workshop, Mar 10 2006. What do we want/need?.

russery
Download Presentation

Luminosity Monitoring Issues

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. Luminosity Monitoring Issues ZDC what’s the advantage? problems BBC can they do it? A. Drees QCD critical point workshop, Mar 10 2006

  2. What do we want/need? • a reliable detector for online monitoring and steering • a reasonable signal/noise ratio • calibration (cross section measurement) for book-keeping • comparison between the different IRs • small integration times • independent from vertex distribution and location • redundancy

  3. ZDC overview • The ZDCs are sampling hadronic calorimeters with tungsten/fiber layers (27 per module) • common to all IRs • Since they are located at +/- 18 m, behind the DX magnets, they ‘see’ only neutrons • the mutual forward neutron cross-section is much smaller than the single neutron cross section (about x10 @100 GeV) • if used as a collision monitor in coincidence mode the signal/noise ratio is very good (typically very low background) • they see all collisions, regardless of the vertex position and distribution

  4. BBC ZDC Location • Peripheral Interactions have very low pt, so you need to put the detectors very forward • In a collider, you need to have a DX magnet to steer bunches so they collide • Spatial Distribution of Charged Particles shown below figure: courtesy S. White

  5. Fiber response vs. angle  (deg)  (deg) e, beam  ZDC Design NIM A 470:488-499,2001, nucl-ex/0008005 • ZDC Calorimeter construction: • Tungsten absorber/ fiber (C)sampling • 2 Lint/module, 3 modules total • C sampling filters shower secondaries • Uniform response vs. impact point figure: courtesy S. White

  6. South North ⊿η = 3.1 ~ 4.0 ⊿φ = 2π 144.35 cm The PHENIX BBC slide from T. Nakamura

  7. STAR Beam-Beam Counters 1-cm thick scintillator hexagons with fiber-optic light collection tiling an annulus (2.1<|h|<5). East/west annuli separated by 7.5 m. slide from L. Bland

  8. red triangles: STAR blue circles: PHENIX Luminosity from collision rates in the ZDC (calibration from 2002) divided by the luminosity calculated from beam parameters (size & bunch current). Beam parameters are derived from vernier scans. This ratio should be constant and about 1. Should not depend on luminosity. jump?

  9. Why does it help to have redundant measurements? Luminosity from collision rates measured by the STAR (triangles) and PHENIX (circles) BBCs divided by the luminosity from the ZDCs. This ratio should not depend on the luminosity but should be constant and about 1. Calibration used is from 2002. Luminosity from collision rates (calibration from 2002) as measured by the BBC divided by the luminosity from beam parameters (calculated). Beam parameters are derived from vernier scans. This ratio should be constant and about 1.

  10. The ZDCs are less affected by background BBC ZDC Vernier Scan in 2005 in PHENIX. ZDC data is “clean” while the BBC data exhibits significant background contribution for negative x.

  11. Shortcomings of the ZDCs Data from the 10 GeV run in 2001. Statistically the ZDCs are already at their limits, less than 10 Hz is difficult to use for steering and monitoring. The BBC seem to be still ok (2 tubes on either side only), full BBC would enhance rate. STAR BBC was not available in 2001. BBC ZDC

  12. PHENIX and STAR luminosity signals from ZDC and BBC during a pp store in 2005 The existing difference of ~20% could not be explained by beta* differences (STARs was actually smaller!). The gaps were aligned in IR4 & 10. BBC: PHENIX/STAR = 0.48 ZDC: PHENIX/STAR = 1.2

  13. PHENIX and STAR luminosity signals from ZDC and BBC during a pp store in 2006. No deliberate changes were made. While the ratio of the BBC basically didn’t change by more than about 10% between the two years (for whatever reason), it changed by approx. 40% for the ZDCs. BBC: PHENIX/STAR = 0.42 ZDC: PHENIX/STAR = 0.75

  14. Calorimeter limitations • limit of production of cherenkov light in the fibers: b > 1/n • n for the fibers = 1.4 => 1/n = 0.7 • for b = p/E = 2.3/3.5 = 0.65 • assume coulomb dissociation of the neutrons: Eneutron ~ Ebeam~Eshow.prod. • depending on the beam energy we are just at the limit • increase tube voltage, decrease discriminator voltage => new calibration … • acceptance drop due to fermi motion 1/p2beam

  15. Conclusion • ZDCs seem statistically, acceptance and light limited at low energies • they can most likely not be used reliably for monitoring or steering (and not for triggering) • we will have to give up the idea of two independent measurement systems • can we use the exp. BBCs and calibrate them?

More Related