Radio-to-Gamma Ray Monitoring of Mkn 421 and Mkn 501: Source - PowerPoint PPT Presentation

Radio-to-Gamma Ray Monitoring of Mkn 421 and Mkn 501: Source Variability N. Nowak, D. Paneque, U. Barres de Almeida, N. Strah, D. Tescaro On behalf of the Fermi-LAT, MAGIC, VERITAS and other collaborations and groups involved in the multiwavelength campaigns

Outline • Introduction • 2009 MWL campaigns on Mrk 421 and Mrk 501: - SEDs - Lightcurves - Variability - Correlations • Conclusions & Outlook

Motivation Blazars: - AGN with relativistic jet pointing directly towards us - highly variable at all wavelengths - SEDs dominated by jet emission, two non-thermal bumps at low (radio- optical-Xray) and high (X/ γ -rays) energies respectively. Origin of high-energy bump not yet identified unambiguously. ➡ simultaneous observations of blazars over the whole wavelength range (Radio - TeV) over a long time period needed (mostly in low state). Mrk 421 and Mrk 501: - luminous gamma ray sources - nearby blazars ( z ~0.03) which implies a low EBL absorption ➡ ideal candidates for multiwavelength studies

2009 MWL campaigns on Mrk421 and Mrk501 4.5 months long multiwavelength campaigns in 2009 (PI: David Paneque): • Mrk421: Jan 19, 2009 (MJD 54850) - June 1st, 2009 (MJD 54983) • Mrk501: Mar 15, 2009 (MJD 54905) - Aug 1st, 2009 (MJD 55044) • monitored regardless of activity. However, both sources were in a relatively low state throughout the campaigns • participating collaborations/telescopes/instruments: MAGIC, Whipple, VERITAS, Fermi -LAT, Swift /BAT, RXTE /PCA, Swift /XRT, Swift /UVOT, GASP-WEBT, GRT, ROVOR, New Mexico Skies, MITSuME, OAGH, WIRO, SMA, VLBA, Noto, Metsähovi, OVRO, Medicina, UMRAO, RATAN-600, Effelsberg

2009 MWL campaigns on Mrk421 and Mrk501 Mrk501 Radio IR O-UV X-rays HE -rays VHE -rays 55050 � � Abdo et al., 2011, ApJ, 727, 129 Time [MJD] 55000 54950 Mrk421 Abdo et al., 2011, ApJ, 736, 131 55000 54900 Radio IR O-UV X-rays HE � -rays VHE � -rays 10 15 20 25 log10( [Hz]) � 54950 Time [MJD] Excellent time and energy coverage for both sources 54900 54850 10 15 20 25 log10( [Hz]) �

Spectral Energy Distribution of Mrk 421 -9 10 ] -1 SMA s -2 VLBA_core(BP143) [erg cm VLBA(BP143) -10 VLBA(BK150) 10 high-energy bump Metsahovi � Noto F of the SED well � VLBA_core(MOJAVE) -11 VLBA(MOJAVE) 10 covered by Fermi- OVRO RATAN LAT + MAGIC MAGIC Swift/UVOT Medicina ROVOR -12 Effelsberg Fermi 10 NewMexicoSkies Swift/BAT MITSuME RXTE/PCA GRT Swift/XRT -13 10 GASP WIRO OAGH Abdo et al., 2011, ApJ, 736, 131 -14 10 10 16 18 20 26 28 12 14 22 24 10 10 10 10 10 10 10 10 10 10 [Hz] �

Spectral Energy Distribution of Mrk 501 -9 10 ] -1 s SMA host galaxy Swift/BAT -2 VLBA(BP143) [erg cm RXTE/PCA VLBA_core(BP143) VLBA_core_ellipsefit(BP143) Swift/XRT 3-day spectrum -10 VLBA(BK150) 10 of a flare seen by VLBA_core(BK150) Noto � VERITAS F Metsahovi � Medicina low-state spectrum VLBA(MOJAVE) -11 10 VLBA_Core(MOJAVE) (flare excluded) OVRO RATAN UMRAO high-energy bump Effelsberg -12 10 of the SED well MAGIC Swift/UVOT VERITAS BradfordRoboticTelescope covered by Fermi- GASP VERITAS_flare GRT Fermi -13 MITSuME LAT + MAGIC + 10 ROVOR WIRO VERITAS OAGH Abdo et al., 2011, ApJ, 727, 129 CampoImperatore -14 10 10 12 14 16 18 20 22 24 26 28 10 10 10 10 10 10 10 10 10 10 [Hz] �

Modelling the Mrk 421 and Mrk 501 SEDs • can be well described by standard one-zone synchrotron self-Compton model with 2 breaks in the electron spectrum • model parameters (e.g. Doppler factor, size of emitting blob, magnetic field, properties of the electron population, ...) are very similar for both objects common properties of jets and acceleration mechanisms in blazars ➡ 10 � 9 -8 10 Mrk 421 SED with SSC model fits Mrk 501 SED with SSC model fits -9 10 10 � 10 10 � 10 � � � � � � Ν F Ν � erg cm � 2 s � 1 � � � � � ��� � � � � � � � � � �� � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � � -2 ] � � -10 � � � � � ������ � � 10 � � � � -1 cm � � 10 � 11 10 � 11 � � � � -11 � F � [erg s 10 10 � 12 10 � 12 � -12 � 10 � � � � � � � host galaxy � � � � � � � � � 10 � 13 10 � 13 � � � � � � � � � � � -13 � � � �� 10 � � � Abdo et al., 2011, ApJ, 736, 131 Abdo et al., 2011, ApJ, 727, 129 � 10 � 14 10 � 14 -14 10 8 11 14 17 20 23 26 29 10 10 10 10 10 12 10 12 10 14 10 14 10 16 10 16 10 18 10 18 10 20 10 20 10 22 10 22 10 24 10 24 10 26 10 26 10 28 10 10 10 10 10 10 10 10 � [Hz] Ν � Hz �

Lightcurves for Mrk 421 − Radio Metsähovi 37GHz 0.7 Effelsberg 9mm Effelsberg 13mm 0.6 Noto 22GHz Metsähovi Y OVRO 15GHz R Effelsberg 20mm 0.5 A Effelsberg 28mm Effelsberg N Effelsberg 36mm Noto Medicina 8GHz I 0.4 Flux [Jy] M Noto 8GHz I Effelsberg 60mm L 0.3 Effelsberg 110mm E OVRO Medicina R P 0.2 • Radio observations at different frequencies 0.1 • single-dish instruments • flux ~const., no strong variability 0 54800 54840 54880 54920 54960 55000 MJD

Lightcurves for Mrk 421 − NIR and Optical 50 45 ROVOR B OAGH H MITSuME Ic OAGH J Y R 45 OAGH K MITSuME Rc A Flux [mJy] Wiro J MITSuME g N 40 Wiro K 40 GRT B I Y M GRT I I R L 35 GRT R E 35 GRT V A R GASP 30 P N Steward V I Flux [mJy] 25 30 M 54800 54840 54880 54920 54960 55000 I I MJD L 25 E R • good coverage of optical-NIR P R 20 wavelengths provided by many telescopes around the world V 15 • flux increases with time • significant variability B 10 54800 54840 54880 54920 54960 55000 MJD

Lightcurves for Mrk 421 − UV and X-rays -9 10 × Y UVOT M2 R 14 Y 0.8 A UVOT W1 R N Flux [mJy] A UVOT W2 0.7 12 I N M ] -1 0.6 I s I M 10 -2 L Flux [ergs cm E I 0.5 L R 8 E P 0.4 R P 6 0.3 RXTE/PCA (2 - 10 keV) 0.2 54800 54840 54880 54920 54960 55000 Swift/XRT (0.3 - 2 keV) Swift/XRT (2 - 10 keV) MJD 0.1 2 Swift 0.0025 Y RXTE/ASM 1.8 R Swift/BAT 1.6 A 0.002 N 1.4 • UV: flux increases I ] ] M Flux [counts/s Flux [counts/s 0.0015 1.2 with time, significant I L 1 E 0.001 variability R 0.8 P • X-rays: large 0.6 0.0005 0.4 variability amplitudes 0 0.2 of ~factor 2 54800 54840 54880 54920 54960 55000 MJD RXTE

Lightcurves for Mrk 421 − γ -rays and VHE -6 -9 10 10 × × Y 0.14 E>300MeV, 2 day bins E>300GeV Fermi-LAT MAGIC R Y 0.16 A R 0.12 N ] A ] -1 -1 I s s N M -2 -2 0.12 0.1 I Flux [photons cm Flux [photons cm I M L E I 0.08 L R 0.08 E P R 0.06 P 0.04 0.04 0 54800 54840 54880 54920 54960 55000 E>400GeV 1.2 Whipple MJD Y ] R -1 1 • γ -rays and VHE: some level of Flux [photons minute A N variability 0.8 I M • no significant flaring activity 0.6 I L E R 0.4 P 0.2 0 54800 54840 54880 54920 54960 55000 MJD Fermi MAGIC Whipple

Lightcurves for Mrk 501 − Radio Effelsberg 110mm Effelsberg 60mm 2 GASP 5GHz GASP 8GHz Metsähovi 1.8 Y Noto 8GHz R Medicina 8GHz 1.6 A Effelsberg 36mm Effelsberg Effelsberg 28mm N Noto Effelsberg 20mm 1.4 I Flux [Jy] M GASP 14GHz I OVRO 1.2 L Medicina 22GHz E OVRO Effelsberg 13mm Medicina R 1 Effelsberg 9mm P Metsähovi 37GHz Effelsberg 7mm 0.8 Noto 43GHz • Radio observations at SMA 225GHz 0.6 many different frequencies 0.4 • no strong variability 54900 54940 54980 55020 55060 MJD

Lightcurves for Mrk 501 − NIR and Optical ROVOR B 30 GRT B ROVOR V • good coverage of optical-NIR Y MITSuME g wavelengths provided by I R GRT V 25 A many telescopes around the Steward V N GRT R world I ROVOR R • flux ~const. with time M GASP R Flux [mJy] 20 • little variability I MITSuME Rc L ROVOR I E R MITSuME Ic R P 15 65 GASP H Y GASP J R 60 A GASP K N OAGH H 55 Flux [mJy] V I OAGH J M 50 10 OAGH Ks I L Wiro J 45 E Wiro K R B 40 P 35 5 30 54900 54940 54980 55020 55060 54900 54940 54980 55020 55060 MJD MJD

Lightcurves for Mrk 501 − UV and X-rays -9 10 × 2.8 Y R RXTE/PCA (2 - 10 keV) 0.2 Y 2.6 A Swift/XRT (0.3 - 2 keV) R 0.18 N Swift/XRT (2 - 10 keV) 2.4 A Swift/XRT PC mode (0.3 - 2 keV) I Flux [mJy] N M ] 0.16 2.2 -1 Swift/XRT PC mode (2 - 10 keV) s I I M -2 0.14 L 2 Flux [ergs cm E I 0.12 L R 1.8 E P 0.1 R 1.6 UVOT M2 P 0.08 UVOT W1 1.4 UVOT W2 0.06 54900 54940 54980 55020 55060 0.04 MJD 0.02 Swift 0.0012 0.4 Y R 0.001 A 0.0008 N 0.3 ] ] Flux [counts/s Flux [counts/s I M 0.0006 I L 0.0004 0.2 E R 0.0002 P • UV and X-rays: 0 0.1 RXTE/ASM significant variability -0.0002 Swift/BAT 0 54900 54940 54980 55020 55060 MJD RXTE