20 Abr 2004Udine bootcamp1 First Analysis Results of the Crab Nebula and Mrk421 M. López Moya U.C.M. 1.Analysis chain 2.Mrk421 Camera rotation study Light Curve 3.Crab Nebula

20 Abr 2004Udine bootcamp2 Analysis chain (1) Calibration and Pedestal substraction –Used the standard calibration classes –P,C runs selected by hand: needed a method to look autmotically for the closer P,C runs to a given D run. –Pedestal runs seem to work fine, but many problems using calibration runs: many pixels look after calibration.

20 Abr 2004Udine bootcamp3 Image cleaning –Lvl1 = 3.0, Lvl2 = 2.5 (one ring) –We started to investigate the dependence of cleaning cuts, but no conclusive results yet: just that 5:3 seems to work better for the Crab. –Forseen insland analysis and moun rings rejection, specially to analysis at low energies. Analysis chain (2)

20 Abr 2004Udine bootcamp4 Signal Extraction –We use: MExtractSignal2 Hillas Paramter cuts –for the time being, only use SIZE, LENGTH, WIDTH & DIST. –we used static cuts: no dependence with zenith angle took into accout Analysis chain (3)

20 Abr 2004Udine bootcamp5 Getting the telescope pointing postion –Poiting position stored only in CC reports at a fixed frecuency –For having it in an event by event base, we extrapolated it using the arrival time of the event. Analysis chain (4)

20 Abr 2004Udine bootcamp6 Analysis of Mkn 421

20 Abr 2004Udine bootcamp7 Data Set 15 Feb.2004 Mrk 421 (1) TypeRuns# EventsDuration [m] ON PCDPCD OFFD

20 Abr 2004Udine bootcamp8 Mrk 421 (2) Hillas cuts: SIZE > < LENGTH < < WIDTH < < DIST < 1.4

20 Abr 2004Udine bootcamp9 Mrk 421 (3) Correcting the mispointing: The False Source Plot –We consider as source position, the position at the maximum in the 2D alpha plot Fitting the Alpha Plot –Signal region < 10  –Backg. region: between 30  - 90  –Fit the Backg. region to a 2 nd order polinomial. From it extrapolate the bg. in the signal region –The significance is calculated according to LiMa

20 Abr 2004Udine bootcamp10 ON data OFF data

20 Abr 2004Udine bootcamp11 Alpha plot at Src position

20 Abr 2004Udine bootcamp12 Alpha plot for SIZE > 3000

20 Abr 2004Udine bootcamp13 We get nearly 20 , but a relative broad alpha plot. The significance is high enough to split this day into subsamples. This allows: –Study camera rotation: is really the rotation uniform? –Get the ligth curve for that day Mrk 421 (4)

20 Abr 2004Udine bootcamp14 We divide the whole night (  1:45 h) into 10 subsamples Now, we don´t apply the camera rotation algorithm. Mrk 421 : Camera rotation (1)

20 Abr 2004Udine bootcamp15 Mrk 421: Camera rotation (2)

20 Abr 2004Udine bootcamp16

20 Abr 2004Udine bootcamp17 For each of the subsamples, we get the source position and it corresponding alpha plot. From each alpha plot, we get the number of excess events, that we plot vs. Time, obtaining the light curve for that night. Mrk 421: Light curve (1)

20 Abr 2004Udine bootcamp18 Mrk 421: Light curve (2)

20 Abr 2004Udine bootcamp19 Mrk 421: Light curve (3)

20 Abr 2004Udine bootcamp20 BUT, this light curve depends strongly on: –the binning criterium (binning in RunNumber, RunTime,...) –the hillas cuts Also we check the time stamp Mrk 421: Light curve (3)

20 Abr 2004Udine bootcamp21 Mrk 421: Checking timestamp (1)

20 Abr 2004Udine bootcamp22 Mrk 421: Checking timestamp (2)

20 Abr 2004Udine bootcamp23 Analysis of the Crab Nebula

20 Abr 2004Udine bootcamp24 Data Set 15 Feb.2004 Crab Nebula (1) RunsDuration [m] ON OFF

20 Abr 2004Udine bootcamp25 Alpa plot

20 Abr 2004Udine bootcamp26 So far, only analyzed the night: 15 Feb For Mrk 421 seems easy to get a nice signal, without using a detailed calibration or cut optimization. We get around 20 . According the light curve, although we see some variation, it is difficult for the time being to relay on it. Mrk 421 also quite useful to understand telescope behaviour. For the Crab the situation is more complex. Seems that different cuts should be used. We get only about 6 . Conclusions