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UHECRs: AGNs or Spiral galaxies?... or Ellipticals?

UHECRs: AGNs or Spiral galaxies?... or Ellipticals?. with Ghirlanda, Tavecchio, Fraternali, Pareschi MNRAS, 390, L88. 27 Auger Events >57 EeV. 1 EeV=10 18 eV. Auger events. The Auger collaboration, 2007, Science. If the Galactic plane is excluded, 19 out of 21 events do correlate. Virgo.

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UHECRs: AGNs or Spiral galaxies?... or Ellipticals?

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  1. UHECRs: AGNs or Spiral galaxies?... or Ellipticals? with Ghirlanda, Tavecchio, Fraternali, Pareschi MNRAS, 390, L88

  2. 27 Auger Events >57 EeV 1 EeV=1018 eV Auger events The Auger collaboration, 2007, Science

  3. If the Galactic plane is excluded, 19 out of 21 events do correlate Virgo AGNs from VC-V catalogue CenA Auger events The Auger collaboration, 2007, Science

  4. George, Fabian, Baumgartner, Mushotzky,Teueller 2008: Swift/BAT AGNs AGNs Supergalactic coordinates UHECRs

  5. 98% weighted by flux 84% not weighted by flux 138 AGNs; 19 UHECRs with |b|<15o, d <25o 57 AGNs within 100 Mpc GZK effect

  6. HIPASS: ~5000 HI emitting galaxies (21 cm) Weight for flux and Auger exposure GG+, 2008

  7. Completeness limit ~72%

  8. Cut in distance

  9. Cut in luminosity

  10. Virgo Centaurus

  11. It is not Cen A, it is the Centaurus cluster (>40 Mpc)

  12. 100 Mpc

  13. Can we discriminate between AGN and spirals?

  14. 2777 HI-galaxies (North+South 95% completeness)

  15. Swift 22 months = 242 AGN with z 2777 HI-galaxies (North+South 95% completeness)

  16. Swift 22 months = 242 AGN 93 AGN (dec<25; |b|<15: D < 164 Mpc) 2134 HI-galaxies (dec<25; |b|<15; D < 164 Mpc; 95% completeness) Pw=95.2%

  17. 2pt cross correlation function 2.6s 93 AGN (dec<25; |b|<15: D < 164 Mpc) 2134 HI-galaxies(dec<25; |b|<15; D < 164 Mpc; 95% completeness)

  18. AGN D n1/2 HI Gal N (extracted from HI galaxies) n=n1*n2/(n1+n2)

  19. What about Ellipticals? • If what is important is the local distribution of matter, then also ellipticals should correlate. Will they correlate better than spirals?

  20. 14677 IRAS Galaxies with z 4281: all types with dec<25;|b|<10 D<100 Mpc Pn=46.6% Pw=53.5% Preliminary!

  21. Ellipticals IRAS 549E0-S0 dec<25; |b|<10 d<100 Mpc Pn=58.2% Pw=99.4% Preliminary!

  22. Progenitors • AGNs • Spirals • Ellipticals

  23. Progenitors FAuger ~ 10-11 erg cm2 s-1Flux for E>57 EeV • Easy for AGNs (but they are radio-quiet… no g) In Spirals we can have GRBs and Magnetars, both should be related to the number of massive stars.

  24. Integrated HI flux Apparent magnitude

  25. Progenitors FAuger ~ 10-11 erg cm2 s-1Flux for E>57 EeV • Easy for AGNs (but they are radio-quiet… no g) • Short `BATSE’ GRBs: 150 yr-1; <Fluence>~10-7; 1/10 nearby  flux not enough (if Fem = FCR)

  26. Progenitors FAuger ~ 10-11 erg cm2 s-1Flux for E>57 EeV • Easy for AGNs (but they are radio-quiet… no g) • Short `BATSE’ GRBs: 150 yr-1; <Fluence>~10-7; 1/10 nearby  flux not enough (if Fem = FCR) • Long `BATSE’ GRBs: 450 yr-1; <Fluence>~10-6; very few nearby  (too distant)

  27. Progenitors FAuger ~ 10-11 erg cm2 s-1Flux for E>57 EeV • Easy for AGNs (but they are radio-quiet… no g) • Short `BATSE’ GRBs: 150 yr-1; <Fluence>~10-7; 1/10 nearby  flux not enough (if Fem = FCR) • Long `BATSE’ GRBs: 450 yr-1; <Fluence>~10-6; very few nearby  (too distant) • Giant Flares of Magnetars (flux not enough)

  28. Progenitors FAuger ~ 10-11 erg cm2 s-1Flux for E>57 EeV • Easy for AGNs (but they are radio-quiet… no g) • Short `BATSE’ GRBs: 150 yr-1; <Fluence>~10-7; 1/10 nearby  flux not enough (if Fem = FCR) • Long `BATSE’ GRBs: 450 yr-1; <Fluence>~10-6; very few nearby  (too distant) • Giant Flares of Magnetars (flux not enough) • Newly born, fastly spinning Magnetars (!!!, but went unobserved by BATSE)

  29. GRB 060218 ??? BAT [15-150 keV] F [erg/cm2/s] Toma et al. 2006 Epeak

  30. GRB 060218 ??? Campana et al. 2006 Opt-UV

  31. GRB 060218 ??? • Very long, soft, underluminous, nearby (145 Mpc) • It could not have triggered BATSE • Proposed to be a newborn magnetar (Soderberg+ 2007; Toma+ 2007) • Right rate

  32. 4p<R2> FAuger L ~ ~ 1040-1042 erg/s N Progenitors: Ellipticals 2002, ApJ, 571, 226

  33. Conclusions - I • UHECRs correlate with spirals • newly born magnetars? • ECR ~ 1050 erg. Rate: 1 every 104 years per galaxy • New class of GRBs (2 per yr all sky): similar to GRB 060218: soft, very long, underluminous+SN

  34. Conclusions - II • UHECRs correlate with ellipticals • Unconspicuos jets? • Very low power jets, small density, unscreened E-field • NOT CenA: its jet is powerful (~1045 erg/s), we see less because it is misaligned

  35. GRBs estimates assuming FUHECRs=Fg Short GRBs: 490 BATSE in 9 years Tot fluence = 5.5e-4 cgs. If a fraction 10% is nearby: <F>=3.9e-13 cgs (assumes BATSE saw half of the sky) Long GRBs: 1490 BATSE in 9 years Tot fluence = 0.024 cgs. <F>=1.7e-10 cgs. They can if 10% is very nearby (but it is not).

  36. Swift 22 months = 242 AGN 93 AGN (dec<25; |b|<15: D < 164 Mpc)

  37. Pn = Prob with number; Pw = Prob weighted for galaxies’ flux Different numbers of galaxies correspond to different cuts: |b|<10° and δ<24.8° when considering CR (for IRAS completeness and PAO FOV; |b|<15° and z<0.5 when considering AGN (for AGN completeness and IRAS extension in z, respectively)

  38. AGN D n1/2 Ellipt. Gal N (extracted from elliptical (<S0) galaxies) Extract N galaxies (<S0) and correlate with galaxies <S0 and AGN (note that 1.7 is the saturation value of AGN vs all IRAS galaxies)

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