Study of the classical TeV blazars with Fermi: Mrk421, Mrk501, 1es

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Study of the classical TeV blazars with Fermi: Mrk, Mrk50, es959+50 Outline Introduc,on (mo,va,on to study classical TeV blazars) Mrk Mrk50 es959 5 Conclusions David Paneque (SLAC/Kipac)

1 Study of the classical TeV blazars with Fermi: Mrk, Mrk50, es Outline Introduc,on (mo,va,on to study classical TeV blazars) Mrk Mrk50 es959 5 Conclusions David Paneque (SLAC/Kipac) dpaneque@slac.stanford.edu On behalf of the Fermi collabora,on and the mul, frequency campaign par,cipants (MAGIC, VERITAS, GASP, OVRO ) Just a glimpse of some of the (preliminary) results 7//09 David Paneque

2 Fermi mission (brief overview) Launch: June th 008 Cape Canaveral Start of normal science operaton: Aug th m.8 m Large Area Telescope (LAT) GLAST Burst Monitor (GBM) 7//09 David Paneque

3 Deep studies of few individual sources c7 c5. PKS 5 PMN J098 c79, ca, BLLac es8, PG55 weak TeV blazars Rela,vely low significance detec,ons In the last years!! (thanks to beeer Cherenkov Teles.) PKS55 0, es Mrk, Mrk50 Very Bright TeV blazars High signficance detec,ons Detected >= ago Classical TeV sources Current experimental data allow for a big inter-model and intra-model degeneracy. More and higher quality data required to constrain models. Leptonic vs hadronic emission models Acceleration/cooling in single or multi-zone; close or far from BH Production of flares (which are the shortest timescales) Role of external photon fields Intrinsic spectra vs EBL-affected spectra Time-resolved emission models etc,etc, etc David Paneque

4 Short intro (motvaton to study classical TeV blazars) Culprits for the relatively poor knowledge of these objects - Time-evolving broad band spectra Coordination of instruments covering different energies needed - Poor sensitivity to study high-energy part (E>0. GeV) Large observation times (with EGRET and old IACTs) were required for signal detection Data NOT simultaneous, and most of our HBL knowledge relates to the high state Recently, we had two performance jumps with respect to the past: New Generation of IACTs online since ~ years (low E th, high sensitivity) LAT in operation since almost year (~0 times more sensitive than EGRET) ~0 Tmes more sensitve at E>~ GeV Enhanced observatonal capability can be used to improve our knowledge on HBLs David Paneque

5 - Motivation to observe (again) the classical TeV blazars Mrk, Mrk 50, ES and PKS55-0 Exquisite characterization of the high energy component, which can be detected with Fermi and Cherenkov Telescopes (0 MeV 0 TeV) Excellent laboratory for studying High Energy blazar emission Strong gamma ray sources && Nearby objects; z <~ 0.; low EBL absorpton, we see almost intrinsic features Knowledge acquired with those objects could (in principle) be applied to other objects (fainter and/or larger z) Things we know about those classical TeV sources (and HBLs in general) Dominant gamma ray emission mechanism is believed to have a leptonic origin (SSC), at least in high (flaring) state Fast variatons (down to hours and sub hours in VHE) X rays Gamma rays correlaton (in general) David Paneque 5

6 - Motivation to observe (again) the classical TeV blazars Mrk, Mrk 50, ES and PKS55-0 Preliminary results in this talk Exquisite characterization of the high energy component, which can be detected with Fermi and Cherenkov Telescopes (0 MeV 0 TeV) Excellent laboratory for studying High Energy blazar emission Strong gamma ray sources && Nearby objects; z <~ 0.; low EBL absorpton, we see almost intrinsic features Knowledge acquired with those objects could (in principle) be applied to other objects (fainter and/or larger z) Things we know about those classical TeV sources (and HBLs in general) Dominant gamma ray emission mechanism is believed to have a leptonic origin (SSC), at least in high (flaring) state Fast variatons (down to hours and sub hours in VHE) X rays Gamma rays correlaton (in general) Accepted in ApJ (090.9) Chiang etal, This conference (Tuesday) David Paneque

Mrk RA =. ; DEC=8.0 Z = 0.0 First extragalac,c TeV emieer (Punch et al, 99, Nature 58, 77) Known to be one of the fastest varying gamma ray sources (Gaidos, J.A. et al99, Nature 8, 9; and many other publicahons).

7 Mrk RA =. ; DEC=8.0 Z = 0.0 First extragalac,c TeV emieer (Punch et al, 99, Nature 58, 77) Known to be one of the fastest varying gamma ray sources (Gaidos, J.A. et al99, Nature 8, 9; and many other publicahons). RXTE/ASM Light Curve ( kev) LAT All detectons of EGRET (9 years of operaton) DetecTon significance (EGRET) <~ 5 sigma Source is rela,vely low at Xrays David Paneque 7

8 Mrk RA =. ; DEC=8.0 Z = 0.0 First extragalac,c TeV emieer (Punch et al, 99, Nature 58, 77) All detectons of EGRET (9 years of operaton) Known to be one of the fastest varying gamma ray sources (Gaidos, J.A. et al99, Nature 8, 9; and many other publicahons). RXTE/ASM Light Curve ( kev) LAT ] Flux [!8 ph cm! s! 8 Aug th, 008 Fermi LAT systematcally resolves Mrk on day Tme scales (regardless of actvity) day interval E>0. GeV Jan st, 009 Preliminary Source is rela,vely low at X rays, but very clearly detected with Fermi (on day Hme intervals, signal typically > sigma) Photon index...8. Preliminary David Paneque 8

Mrk Because of the brightness of this source, LAT can resolve it also on,me scales as short as days and much shorter when it flares Data from August th 008 Tll Jan 0 th 009 (5.

9 Mrk Because of the brightness of this source, LAT can resolve it also on,me scales as short as days and much shorter when it flares Data from August th 008 Tll Jan 0 th 009 (5.5 months) FracTonal Variability vs Energy Light curve in day Tme bins (using Vaughan et al 00) E> 0. GeV ICRC 009 D.Paneque etal Out of the 85 day,me intervals: Detected on 79 (9%) above sigmas Detected on (7%) above 5 sigmas 0. GeV 0. GeV.0 GeV 0 GeV Hint of increase of Fvar vs energy To be repeated with enhre data set Great potental to study SED variatons in short Tme scales with our MW partners 7//09 David Paneque 9

10 Mrk MW campaign organized (+ months long): hsps://confluence.slac.stanford.edu/display/glamcog/campaign+on+mrk+(jan+009+to+may+009) ] Flux [!8 ph cm! s! Photon index Flux/Photon index (E>0. GeV) day interval Preliminary Preliminary MW campaign 0/0 05/ Radio: OVRO, Effelsberg, Noto Infrared: WIRO, OpTcal: GASP, GRT, MITSuMe X ray: Swiu, RXTE Gamma ray: Fermi VHE: MAGIC, VERITAS Because of the high brightness of this source in gamma rays, we aimed at following the mul, frequency ac,vity of the source on short,me scales: One observaton every days Big effort from many groups! 7//09 David Paneque

ObservaTons performed/planned during the MW campaign available on the web hsp://www.slac.stanford.edu/~dpaneque/mw_mrk_009/obs.

11 ObservaTons performed/planned during the MW campaign available on the web hsp:// ObservaTons and preliminary fluxes updated once/twice a week Different instruments could plan ahead when to observe the source Request additonal observatons if source shows outstanding actvity This Tme, no big flux variatons during these ~.5 months 7//09 David Paneque

12 Normalized Flux Mrk: mult frequency actvity Preliminary (quick&dirty analysis) from various instruments Some of the fluxes are the result of automa,c procedures (no checks) Proper mult frequency data reducton will happen during the next months OVRO (5 GHz) OVRO Gamma ray, Fermi E> 0. GeV Normalized Flux Normalized Flux GASP GRT UVOT!w OpTcal (R and UV) RXTE/PCA X rays from RXTE ( kev) GASP GRT Swiu UVOT Host galaxy not subtracted!! Normalized Flux VHE MAGIC (E>0.5 TeV) Whipple(E>0. TeV) WHIPPLE Low actvity at VHE: ~ 0.5 Crab But variability clearly seen: Min/Max values: ~ 0. Crab // David Paneque

13 Normalized Flux Mrk: mult frequency actvity Preliminary (quick&dirty analysis) from various instruments Some of the fluxes are the result of automa,c procedures (no checks) Proper mult frequency data reducton will happen during the next months OVRO (5 GHz) OVRO Gamma ray, Fermi E> 0. GeV Normalized Flux Normalized Flux GASP GRT UVOT!w OpTcal (R and UV) RXTE/PCA X rays from RXTE ( kev) GASP GRT Swiu UVOT Host galaxy not subtracted!! Normalized Flux VHE MAGIC (E>0.5 TeV) Whipple(E>0. TeV) WHIPPLE Low actvity at VHE: ~ 0.5 Crab But variability clearly seen: Min/Max values: ~ 0. Crab // David Paneque

14 Mrk: Fermi spectra Preliminary Informa,on on MW campaign organized on this object: hsps://confluence.slac.stanford.edu/display/glamcog/campaign+on+mrk+(jan+009+to+may+009) s! ]! dn/de [ erg cm E s! ]! dn/de [ erg cm E!!!! Augth,008 Juneth, GeV Preliminary 00 GeV 5 Jan0,009 April0,009 7 E [MeV] Fermi Spectra up to 00 GeV ( evts in bin GeV) Spectrum is consistent with Power Law with photon index.79 +/ 0.0 Fit dominated by the lower energies Turn over at the highest energies might be hidden in low photon count Energy coverage over orders of magnitude (!!) Fermi Spectra up to 00 GeV ( evts in bin GeV)!! 0. GeV 00 GeV Preliminary 5 7 E [MeV] Spectrum is consistent with Power Law with photon index.7 +/ 0.0 7//09 David Paneque

First simultaneous GeV TeV spectrum of Mrk Good agreement between these different instruments. Energy coverage of 5 orders of magnitude without GAPS. Important for modeling of the source s! ]!

15 First simultaneous GeV TeV spectrum of Mrk Good agreement between these different instruments. Energy coverage of 5 orders of magnitude without GAPS. Important for modeling of the source s! ]! dn/de [ erg cm! Fermi ~0 days /5. (FoV~0%) = 0 effectve days caveat MAGIC ~7 hours of data not EBL corrected E!! Preliminary 80 GeV 00 GeV Overlapping region Jan0,009 April0,009 7//09 David Paneque E [MeV] 5 5 7

16 First simultaneous GeV TeV spectrum of Mrk One of the goals of Fermi: closing the gap between satellite and ground gamma ray instruments: Mission Accomplished!! s! ]! dn/de [ erg cm! Fermi ~0 days /5. (FoV~0%) = 0 effectve days caveat MAGIC ~7 hours of data not EBL corrected E!! Preliminary 80 GeV 00 GeV Overlapping region Jan0,009 April0,009 7//09 David Paneque E [MeV] 5 7

17 Mrk Informa,on on MW campaign organized on this object: hsps://confluence.slac.stanford.edu/display/glamcog/campaign+on+mrk+(jan+009+to+may+009) Overall SED during the campaign (Jan0th April0th) Various WIRO radio (IR) instruments Op,cal + Swis UV Data analysis ongoing RXTE PCA Fermi MAGIC Swiu XRT Swiu BAT Sync and IC peaks WILL BE fully characterized tight constrains to emission models 7//09 David Paneque 7

18 Mrk50 MAGIC ~0 min RA =5.7 ; DEC = 9.7 Z = 0.0 Discovery at VHE: Quinn et al., 99 Huge flare in 997 (many publica,ons) Short flux varia,ons detected in 005 MAGIC, Albert et al, 007 Not present in rd EGRET catalogue Only detecton (~5 sigma) with EGRET was during a flare in 99 (Kataoka etal 999) EGRET did not detect it during the big outburst in 97 min bins RXTE/ASM Light Curve ( kev) LAT 997 Source is rela,vely low at X rays, 7//09 David Paneque 8

19 Mrk50 MAGIC ~0 min RA =5.7 ; DEC = 9.7 Z = 0.0 Discovery at VHE: Quinn et al., 99 Huge flare in 997 (many publica,ons) Short flux varia,ons detected in 005 MAGIC, Albert et al, 007 Not present in rd EGRET catalogue Only detecton (~5 sigma) with EGRET was during a flare in 99 (Kataoka etal 999) EGRET did not detect it during the big outburst in 97 min bins RXTE/ASM Light Curve ( kev) LAT 997 LAT systematcally resolves Mrk50 on day Tme scales ] Flux [!8 ph cm! s! 5 0 Aug th, 008 day interval Preliminary Jan st, 009 Source is rela,vely low at X rays, but decently detected with Fermi on day,me interval Flux increase ( or ) by February 009 7//09 David Paneque 9

20 Mrk50 MW campaign organized (+ months long): hsps://confluence.slac.stanford.edu/display/glamcog/campaign+on+mrk50+(march+009+to+july+009) ] Flux [!8 ph cm! s! Instruments partcipatng Radio: OVRO, Effelsberg, Metsahovi, Noto Infrared: WIRO, OpTcal: GASP, GRT, MITSuMe, Kanata X ray: Swiu, RXTE Gamma ray: Fermi VHE: MAGIC, VERITAS 5 0 Flux/Photon index (E>0. gev) day interval Preliminary MW campaign 0/5 07/ Less bright than Mrk at gamma rays. One observaton every 5 days Sampling frequency increases when source is found high: We triggered observahons with various instruments in May when the source was relahvely high and variable at gamma rays during few days Big effort from many groups! 7//09 David Paneque 0

21 Normalized Flux Normalized Flux Normalized Flux Mrk50: mult frequency actvity //09 OVRO OpTcal (R and UV) GASP Preliminary (quick&dirty analysis) from various instruments Some of the fluxes are the result of automa,c procedures (no checks) Proper mult frequency data reducton will happen during the next months OVRO (5 GHz) Gamma ray, Fermi E> 0. GeV Flux_00MeV_TS GRT UVOT!w X rays from RXTE ( kev) RXTE ] Flux [!8 ph cm! s! GASP GRT Swiu UVOT Host galaxy not subtracted!! Photon index Normalized Flux 5 David Paneque MAGIC(E>0.5TeV) ; Whipple(E>0.TeV) PhotonIndex Low actvity at VHE: ~ 0. Crab But variability clearly seen: Min/Max values: ~ 0.05 Crab (+ night at Crab) MAGIC Whipple

22 Mrk50: Fermi spectrum Informa,on on MW campaign organized on this object: hsps://confluence.slac.stanford.edu/display/glamcog/campaign+on+mrk50+(march+009+to+july+009) s! ]! dn/de [ erg cm E! Augth,008 Juneth, GeV 00 GeV Fermi Spectra up to 00 GeV ( evts in bin GeV) Spectrum is consistent with Power Law with photon index.7 +/ 0.0! Work ongoing towards the Combined GeV TeV spectrum from Mrk50.! Preliminary 5 E [MeV] 7 Overlap GeV TeV is also granted for this data set Energy coverage over orders of magnitude (!!) 7//09 David Paneque

es959+50 RA = 00.0; DEC =5. z = 0.09 Discovery at gamma: Nishiyama et al, 999 RXTE/ASM Light Curve ( kev) LAT Orphan flare in 00 (Krawcynski et al 00) Never Detected with EGRET (!

23 es RA = 00.0; DEC =5. z = 0.09 Discovery at gamma: Nishiyama et al, 999 RXTE/ASM Light Curve ( kev) LAT Orphan flare in 00 (Krawcynski et al 00) Never Detected with EGRET (!!!) X ray flux is rela,vely high with respect to past observa,ons, although NOT in flare ] Flux [!8 ph cm! s! Aug th, 008 Flux/Photon index (E>0. GeV) 5 day interval Preliminary Jan st, 009 Source is rather weak, but it can be resolved in ~ day,me scale (low significance) 7//09 David Paneque

24 es Never Detected with EGRET (!!!) Informa,on on MW campaign organized on this object: hsps://confluence.slac.stanford.edu/pages/viewpage.acton?pageid=89775 ] Flux [!8 ph cm! s! Instruments par,cipa,ng Radio: OVRO, Effelsberg, Pico Veleta OpTcal: GASP, Flagstaff, MITSuMe, Kanata.. X ray: Swiu, RXTE Gamma ray: Fermi VHE: MAGIC, VERITAS Flux/Photon index (E>0. gev) 5 day interval Preliminary Because of the low brightness of this source at gamma rays, we aimed at producing essen,ally snapshots of the SED (Big difference with the Mrks) Short campaign (.5 months) Due to various reasons we could not get enough TeV observa,ons ( hours Veritas and hour MAGIC) But we could get 0 hours (moon) data with MAGIC in May/ June. MW campaign 09/0 /05 7//09 David Paneque

25 es959+50: Fermi spectrum Never Detected with EGRET (!!!) Informa,on on MW campaign organized on this object: hsps://confluence.slac.stanford.edu/pages/viewpage.acton?pageid=89775 s! ]! dn/de [ erg cm E! Augth,008 Juneth,009 Preliminary Fermi Spectra up to 50 GeV ( evts in bin 58GeV) Spectrum is consistent with Power Law with photon index.9 +/ 0.05 Combined GeV TeV data will probably have a GAP for this source:! From Fermi: months of data will reach <~0 GeV! 5 7 E [MeV] From MAGIC: Rela,vely large zenith angle (0 deg) Moon observa,ons Higher threshold energy (00 GeV??) 7//09 David Paneque 5

26 5 Conclusions Fermi in survey mode since beginning of August, boosting our current capabilities to study AGNs. Uniform exposure Coverage of 0% sky at any Tme Large effectve area, small PSF It brings data that was non existent before and thus it is expected to constrain the current theoretcal models predictng the gamma ray emission In depth study of individual sources is important to understand the physical processes occurring in those objects Study of the classical (bright) TeV sources has the advantage that, together with the IACTs, Fermi data constrain the high energy bump Fermi data opens a new window to study those objects Spectra reaching energies beyond 0. TeV; overlap with IACTs CollecTon of MW data is ESSENTIAL for understanding those complex objects. We are collectng an exquisite data set that will surely help us to understand these extreme objects, and the blazar phenomenon. Some of the results already out, many others to come. Stay tuned: we live excitng Tmes for gamma ray astronomy 7//09 David Paneque

MWL. A Brief Advertisement Before Your Regularly Scheduled Program

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