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Multiwavelength observations of Fermi-LAT monitored blazars with SMARTS

Multiwavelength observations of Fermi-LAT monitored blazars with SMARTS. Erin Wells Bonning Yale University. Collaborators. Yale Charles Bailyn (Fermi GI Grant 011283) Paolo Coppi Meg Urry Michelle Buxton (Postdoc) Ritaban Chatterjee (Postdoc) Jedidah Isler (Grad student)

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Multiwavelength observations of Fermi-LAT monitored blazars with SMARTS

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  1. Multiwavelength observations of Fermi-LAT monitored blazars with SMARTS Erin Wells Bonning Yale University

  2. Collaborators Yale Charles Bailyn (Fermi GI Grant 011283) Paolo Coppi Meg Urry Michelle Buxton (Postdoc) Ritaban Chatterjee (Postdoc) Jedidah Isler (Grad student) Nathan Loughton (Undergrad) Laura Maraschi (INAF-Brera) Giovanni Fossati (Rice U)

  3. Sources LAT monitored blazars visible from CTIO (Chile) + other sources of interest (e.g. 0948+0022) FSRQ 0208-512 0528+134 3C 273 3C 279 1406-076 1510-089 1622-297 1730-130 2155-304 3C 454.3 BL Lac 0235+164 OJ 287 2155-304

  4. Optical/IR observations • Bright blazars observed near-daily with the Small and Moderate Aperture Telescope System (SMARTS) at Cerro Tololo, Chile • SMARTS 1.3m + ANDICAM. Can obtain simultaneous data from 0.4 to 2.2 microns (BVRJK). Photometry taken with 1-3 day cadence. • Spectra of brighter blazars taken about once per month. • Data through 31 July 2009 released at http://www.astro.yale.edu/smarts/glast Fermi GI grant 011283

  5. 0208-512

  6. 0528+134

  7. 0235+164

  8. 3C 279

  9. 3C 273

  10. OJ 287

  11. 1510-089

  12. 1510-089 Blue Red

  13. 3C 454.3

  14. 3C 454.3

  15. 3C 454.3

  16. 3C 454.3

  17. 3C 454.3

  18. 3C 454.3: underlying optical emission

  19. 3C 454.3 Fractional variability amplitude

  20. 3C 454.3: color-magnitude Blue Red

  21. 3C 454.3: color-magnitude Blue Red

  22. 3C 454.3: Spectra From J. Isler

  23. 2155-304

  24. 2155-304

  25. 2155-304: colors v R-band

  26. Future directions • SMARTS monitoring of bright blazars is ongoing. • Favorite source? Let us know glast@panlists.yale.edu • Can the time-dependent SED be modeled self-consistently? • Do optical emission line properties correlate with jet power? • Short v. long term variability studies • How is jet powered? • What particle populations?

  27. Challenges to SED modeling • Single-epoch SED can be fit with leptonic or hadronic models. • Variable sources require simultaneous data • Broad-band SED measurements require multiple observatories • Long term, simultaneous, multi-wavelength monitoring programs required Boettcher et al. 2009

  28. MW light curve • NIR, Optical, UV, and Gamma-ray fluxes vary together with lag of less than one day. • Variability amplitude in IR comparable to that in Gamma rays; decreases towards the UV • Colors redder at higher fluxes. • X-rays uncorrelated with other wavelengths. Bonning et al., ApJL, 697, L81 (2009)

  29. Historical comparison Summer 08 Fall 08 Raiteri et al. 2007

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