OUTLINE: Ø Introduction. Ø Problems. Ø Scope. Ø Why contemplate this at all? Ø What complicates the matter? Ø What will be covered in this class?

Transcription

1 PHOTON MASTERCLASS

2 OUTLINE: Ø Introduction Ø Why contemplate this at all? Ø Problems Ø What complicates the matter? Ø Scope Ø What will be covered in this class? 2

3 WHY CONTEMPLATE THIS AT ALL? Ø What drives us to even attempt to measure/identify photons at a hadron collider? Ø I mean, isn t it only Hà γγ? 3

4 JUST A FEW PHYSICS TOPICS: dσ/dmγ γ (pb/gev) Events/ GeV 3 Data Total Background Total Uncertainties MC Signal (250/700/225) 2 CMS Preliminary Events/ 42 GeV CMS preliminary CMS Preliminary, L = 4.7fb-, s = 7 TeV, γ, 3jets s = 7 TeV - s = 8 TeV jets γ bkg multijet Zγ +Jets top Wγ +jets WV γ -2 2 / Λ = 50 TeV 2-2 2γ NNLO CMS preliminary, 35 pb-, s=7 TeV eγ data Wγ e jet e γ ee eγ 8 data/2γ NNLO JETPHOX 6 SHERPA γ η < 0.9 (X8000) 5 γ 0.9 < η <.4442 (X400) γ.566 < η < 2. (X20) γ 2. < η < ETmiss [GeV] ETmiss [GeV] CMS 4.9 fb- - s = 7 TeV Drell-Yan/W (MC) DATA Total uncertainty γ + Jets (data) W/Z + Jets + γ (MC) QCD Multijet (data) t t + Jets (MC) Bkg. stat error GMSB (0, 2000) GMSB (0, 250) TCalib > 0.5 ns - η < pγ T 3 2 (GeV) PbPb 0 - % 4 PbPb - 30% 3 PbPb 30-0% 2 PbPb 0-0% pp Systematic Uncertainty JETPHOX (pp NLO) jet pγt (GeV) Photon ET (GeV) Higgs Mass Region Data Driven Background MC Signal: MStop=350 GeV, MHiggsino=35 GeV MC Signal: MStop=400 GeV, MHiggsino=300 GeV MC Signal: M =300 GeV, MHiggsino=290 GeV Stop CMS 2.2 fb- at 7 TeV 2 80 Observed Diphoton γ +jet Systematic Uncertainty ~ k = 0.05, M =.75 TeV n ED = 6, MS = 3 TeV ET [GeV] pγt γ (GeV) Dijet -2-3 Data/Bkg. Number of Events γ η <.44 Events per bin snn=2.76tev Lint (PbPb)= 6.8 µb- Lint (pp)= 23 nb- pp dσ/det (pb/gev) - CMS s = 7 TeV Events/20 GeV CMS Preliminary 2.4 fb PbPb dn/det/ <TAA > (pb/gev) γ Electroweak GGM γ γ (0_720_375) GGM γ γ (400_420_375) 7 T d3σ/dp dηγ dηjet QCD + Electroweak Error QCD (fake fake sample) 50 s = 7 TeV Data (b) SM W(µν)γ jets γ bkg e γ bkg Other bkg CMS Preliminary, s = 8 TeV, L dt = 9.5 fb- γ γ Candidate Sample Photon pt (GeV) 4 mγ γ (GeV) CMS, L = 5 fb >= Jet Requirement s = 8 TeV, Ldt = 4.04 fb CMS Preliminary T Photon p (GeV) background uncertainty JGB [GeV] 0 2 Events 50 data/diphox 0 50 Ratio Data/MC DIPHOX+GAMMA2MC -4-2 Events / GeV SM + aw 0 - data 20, L = 5.0 fb - Number of Events / GeV 3-3 Data/Prediction L dt = 9.2 fb Electron Data MC Uncertainty Mγ γ [GeV]

5 Ø Colorless tests of QCD, both in pp and HI Ø Diboson and now Triboson coupling measurements Ø Higgsà γγ sure, but also Hà Zγ, and Higgsino searches Ø Dark matter in monophotons Ø SUSY searches THERE S A LOT Ø New resonances (Gà γγ for instance) Ø χ c and some others Ø Exclusive diphoton production Ø There s a pretty long list 5

6 ALSO: Ø There are also accessory things one can learn from converted photons for instance, like material distribution and JES. We re not really going to cover that here, but it is something that we do. Ø There s also a lot of the commonality between photons and electrons, so learning about one can begin to inform the other. 6

7 THE CHALLENGE Ø There s a lot of nice things about photons, they form nice predictable electromagnetic showers (at least if they re not converted) that we can measure very precisely. Ø Unfortunately there are two real problems with photons: Ø Photons are non-redundant: you ONLY get the measurement of energy from the ECAL, and you typically have no indication of what vertex the photon came from. Ø Jets are EVERYWHERE: any jet which fragments to a significant electromagnetic portion is going to look photon-like to some extent. Ø Our photon reconstruction and Photon Identification are built to try to get the best estimate of the photon energy, and discriminate against as much of the jet background as possible. 7

8 WHAT WILL WE COVER? Ø The goal of this workshop is to introduce you to how we reconstruct photons, and the choices that have been made in the algorithms. Ø I want to make these quantities real to you, relate them to what the detector actually recorded. No more simply cutting on things from your ntuple! Ø Get real hands on experience, and further think critically about the choices that have been made. Ø We will mainly concentrate on the present reconstruction, that which is used in the 202 data, but we ll look into the future at various points as well. We ll also look into what past detectors have done, and what our distinguished competition does. 8

9 THREE PARTS: Ø There are three different exercises that have been prepared. Two out of the three are more fun if you have Microsoft Excel, but that s not strictly necessary. Ø We re not doing C++ coding, and we re not going to run CMSSW. Ø What we re going to do instead is look at what CMSSW is actually DOING. Ø Each exercise has a lecture that corresponds with it that details what the reconstruction is doing. Then you ll take the data, and try to put it to work. What I want to do with the rest of this talk is to try to put the other steps of photon reconstruction in context. 9

10 PRESENTLY: Ø We start making Photon objects out of superclusters, which have had energy corrections applied to them. Ø Exercise is all about how we form these clusters out of energy depositions in the ECAL. Ø The superclusters that we make Photons from, must be at least GeV in E T (calculated from the center of the detector). Ø That is almost ALL that is required. Thus why I put photon in quotation marks. Most of what lives in this collection is actually jets. Ø If you are above 0 GeV (in E T ), you enter the photon collection. Ø If you are below 0 GeV, you must pass a preselection cut.

11 Ø This is really pretty simple, it s a cut on the old version of H/E. Here: Ø H is the sum of Hcal towers in a cone of ΔR < 0.5 about the supercluster position. Ø E is the supercluster energy. PRESELECTION: Ø You are required to have this ratio be less than 0.5. This is a really weak preselection cut.

12 Ø The first somewhat weird quantity we ll meet is known as R9. R9 Ø R9 is a ratio between the energy in the 3x3 crystal array about the highest energy crystal in the cluster and the total supercluster energy. Ø This quantity is often used to classify photon candidates as being likely to be unconverted (large R9) or likely to be converted (smaller R9). Ø This quantity also controls what estimates of the photon energy and position are used. 2

13 R9 Ø The first somewhat weird quantity we ll meet is known as R9. η R9 = E 3x3 / E supercluster φ

14 BASED ON R9 Ø We assign the position of our photon to either: Ø The position of the seed basic cluster within the supercluster, if R9>0.94(0.95) in the barrel (endcap). Ø The position of the supercluster if not. Ø We then take the first vertex in the offlineprimaryvertex collection and calculate our physics rapidity. Ø The ENERGY of the photon is presently set to either: Ø The energy of the 5x5 array of crystals corrected for containment if R9 > 0.94 (0.95) in the barrel (endcap) Ø The corrected supercluster energy if not. Ø Either way there is an additional correction for cracks. 4

15 SO: Ø What the superclustering does is actually pretty darn relevant. Ultimately that s what will determine your value for R9: Ø and R9 will determine what you do for your position calculation Ø and R9 will determine what you do for your energy estimate. Ø Exercise is all about the clustering. 5

16 HERE S THE REST: Ex.2 Ex.3 Ø These are the cut based photon identification requirements. These take you, ostensibly, from the very low purity set of photons to something more pure. 6

17 H/E NEW: Ø Single tower H/E is supposed to be a more pileup safe version of the previous H/E. Ø Recall, the previous version, and the version still used in the preselection uses a cone of ΔR < 0.5 to pick the Hcal towers in proximity to the supercluster. Ø This time the DetId of the highest energy crystal (or the seed crystal) is used to look up the tower that this channel belongs to. Then only the corresponding Hcal energy is used. So in principle, you could have a large spread (as you ll see) across the Ecal, but only that one tower will be considered for H/E. 7

18 CONVERSION SAFE VETO: Ø This is an outgrowth of the older pixel seed veto that used to stand in for electron rejection. Ø The pixel seed in question was a combination of hits in the pixel detector found based on the E T, η, φ of the electron candidate, which originated from the same superclusters that seed photons. Ø Which is still used as an option for analyses that suffer from substantial electron backgrounds. Ø The conversion safe veto is in some sense a looser variant of this, see next slide. 8

19 CONVERSION SAFE VETO (2) Ø Take your photon. Find it s supercluster. Ø Check to see if this supercluster is shared by an electron candidate. Ø If it does, check if there are missing inner hits. If there are missing hits, you re still okay. Ø Otherwise, check if this electron matches a conversion. If it does, and this is a bona fide conversion (good vertex, distance from beamspot, and missing inner hits), you re still okay. Ø If you HAVE a matched conversion that isn t bona fide then you re an electron. (meaning you match an electron, which even if it is found as a conversion doesn t qualify as a displaced conversion). 9

20 Ø We ll now backtrack and look at the clustering, and then the shower shape from the identification requirements. Ø After we get through that, we ll look at photon ID at different detectors. Tomorrow we ll study isolation, and look to the future. Ø Let s get ready! SO THAT S WHERE WE ARE: 20