Analysis report of SN1006 D.Nishida( Kyoto-Univ.) JPS meeting Autumn 2005 Osaka.

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Presentation transcript:

Analysis report of SN1006 D.Nishida( Kyoto-Univ.) JPS meeting Autumn 2005 Osaka

Status of SN1006(G ) Age ~1000 years Right ascension deg Declination deg  NE rim( , ) Bamba et al.(2003,2004) Chandra image

Observation Long On/Off mode Data set  SN /14 – 5/ 26 (T2 & T3 & T4)  Elevation 65 – 80 deg observation time T2T3T4 ON39h40.8h43h OFF36.3h35.1h33.4h

SN1006 (Long ON/OFF) NE rim Track point 3.4Mag 2.8Mag T2 & T3 & T4 Field of view Track point , (deg) NE rim , (deg) 3.4Mag , (deg) 2.8Mag , (deg) HV off (crab 3 Mag)

Analysis with T2 & T3 Cut parameters  -30 ns<TDC start < 30ns  5 p.e x T5a  Distance from camera center < 1.6 deg  Likelihood ratio > 0.6 (Used image parameters : length, width) Observation time  2003 min ( 33.4h)

Theta square distribution from SN1006 from NE rim Effective time 1725min(28.7h) Black line: on, Red line : off Significance -0.7

Upper limit (T2 &T3) Upper limit (integral flux)  F(E>640GeV) = 2.1 x ph cm -2 s -1 H.E.S.S (A.Aharonian et al A&A 2005) HEGRA (Vitale et al ICRC 2003)

Cut parameters -30 ns < TDC start < 30 ns 5 p.e x T5a Distance from camera center < 1.6 deg Likelihood ratio > 0.7 (Used image parameters : length, width) Analyzed 3fold (telescope 2,3,4) data

Intersection Points (IPs) Maximum IPs is equals to n(n-1)/2. (n is number of telescopes)

Calculating intersection point (1) HEGRA method x’ = (xa*sinA + xb*sinB + xc*sinC)/(sinA+sinB+sinC) y’ = (ya*sinA + yb*sinB + yc*sinC)/(sinA+sinB+sinC) A B C (xa, ya) (xb, yb) (xc, yc) W.Hofmann et al. Astroparticle Physics (1999)

Theta square distribution (1) lratio > 0.5 cross line: On data red line: Off data Significance -0.9 Effective time  ~27h

Fitting method    width(x,y)/  wid   Calculating intersection point (2)

Theta square distribution (2) lratio > 0.5 Cross line : On data Red line : Off data Significance -1.1

Summary We observed SN1006 on May 2004 with telescope 2,3,4. Stereoscopic observation time ~30h Analyzed data (T2 & T3), but there is no signal of TeV gamma ray from SN1006 NE rim Upper limit is F(E>630GeV) = 2.1 x ph cm -2 s -1 Analyzed data (T2 & T3 & T4), used 2 method. I will check RX J and feedback to SN1006 analysis.

Appendix F.Aharonian A&A (2005)

Threshold energy

Upper limit Use calculating method No.2 F(E>630GeV) = 1.7 x photon/cm 2 /sec( ~4% Crab flux)

Likelihood parameters Length, Opening Angle, Arm length Length Arm length Opening angle Gamma (simulation) Proton (real)

Theta square ( Θ x, Θ y ) Θ ２＝ Θ x ２ + Θ y ２   distribution simulation Target 00.5 （ deg 2 ） 0.25 IP

HEGRA method Lratio > 0.6 Theta square distribution (3)

Fitting method Lratio > 0.6 Theta square distribution (4)