MAGIC and Multi-Wavelength Observations of Mrk 180 and 1ES 2344+514 in 2008 Jan Storz1 (presenter), Stefan Rügamer1 on behalf of the MAGIC collaboration for the Mrk 180/1ES 2344+514 MWL team 1Institut für Theoretische Physik und Astrophysik, Lehrstuhl für Astronomie, Universität Würzburg

Outline The High-Frequency Peaked BL Lacertae Objects Mrk 180 and 1ES 2344+514 The MAGIC Telescope(s) The Multi-Wavelength (MWL) Campaigns Resulting Light Curves and Spectral Energy Distributions Summary & Conclusions

Mrk 180 and 1ES 2344+514

Blazars Blazar blazars classified according to position of their first SED peak dominating extra-galactic source species in the gamma regime still not well understood emission mechanism emitting particle species emission site variability drivers ... strong variability on various time scales at all energies simultaneous MWL campaigns (early 2008: only 4 sources studied in TeV MWL campaigns, mostly during flaring states) Jet Quasar Black Hole radio loud radio quiet Accretion Disc Obscuring Torus Radio Galaxy Seyfert II Quasar Seyfert I [1] log E [eV] VHE X-ray HE ‘optical’ radio log νFν 103 109 1012 100 ~ Fermi 2FGL: out of 1873 sources, 917 are AGN, of which 894 are blazars (~48%) (additional ~250 are candidate AGNs) VHE: out of 49 sources, 44 are AGN (~90%) MWL campaigns *with VHE detections* until 2008: Mrk 421, Mrk 501, PKS 2155-304, 1ES 1959+650

Sources - Mrk 180 nearby high-frequency peaked blazar (HBL) at z = 0.046 discovered by MAGIC in 2006 after an optical outburst flux ~11% of Crab Nebula flux no second VHE detection, yet no multi-wavelength campaign, yet Albert et al., 2006, ApJL 648, 105 SED models taken from Costamante & Ghisellini 2002, ApJ 384, 56 dashed line: phenomenological model Fossati 1998, modified by Donato 2001 (see Costamante & Ghisellini paper) solid line: Fossati 1998, modified by Costamante & Ghisellini 2002 phenomenological model: based on radio luminosity which determines the sync peak and relative IC power Albert et al., 2006, ApJL 648, 105

Sources - 1ES 2344+514 HBL at z = 0.044 3rd source discovered at VHE (Whipple 1995/6) nevertheless sparsely studied detected by MAGIC in 2005/6 in the lowest flux state up to now ‘extreme blazar’ first MWL campaign including VHE in 2007/8 Catanese et al. ’98, ApJ 501, 616 Acciari et al., arXiv 1106.4594 note: VERITAS and Swift high state data separated by 1 day ≈ flux doubling time scale at both energies back then low state VERITAS data are time averaged extreme blazars (Costamante 2001): blazars with peak >~ 1 keV; up to now: Mrk 501, 2344, 1426, 0548, 1943 SED modelling: Krawczynski 2004 Acciari, V. A., et al., 2011, arXiv 1106.4594

Instruments and Campaigns

The MAGIC Telescopes two 17 m Imaging Atmospheric Cherenkov Telescopes, La Palma MAGIC-I: fast repositioning: any sky position reachable within ~20 s reflective surface: 241 m2, parabolic trigger threshold: ~50 GeV (with special trigger ~25 GeV) energy resolution: 20% – 30% sensitivity: 1.6% Crab / 50 h stereo observations since summer 2009 improved energy & angular resolution, analysis threshold, sensitivity in the following only MAGIC-I results

Mrk 180 Campaign radio ‘optical’ X-rays HE VHE RATAN-600 FERMI-LAT log νFν radio ‘optical’ X-rays HE VHE RATAN-600 FERMI-LAT Swift UVOT Effelsberg KVA Suzaku and VLBA proposals rejected; VERITAS wanted to contribute but had no time left RATAN-600: end of 2008/09 – 10/03 Metsähovi: 2008/03/22; 04/23 – 24; 05/21 – 23 Effelsberg: 2008/02/18; 11/08 KVA (approx.): 2008/02/14; 02/27 – 03/19; 03/29 – 04/04; 04/13 – 05/29; 06/04; 11/18 – 19; 11/24; 11/30 - 12/12 Swift: 2008/04/29 – 05/10; 10/22; 26; 30; 11/22 – 12/10 AGILE: 2008/04/30 – 05/10; 10/31 – 11/30 Fermi: always since ~2008/08/02 MAGIC (approx.): 2008/04/29 – 05/03; 05/11; 10/23 – 28; 11/07; 11/23 – 12/08 Swift XRT AGILE MAGIC Metsähovi IRAM 2008/02 2008/04 2008/06 2008/08 2008/10 log E time

1ES 2344+514 Campaign radio ‘optical’ X-rays HE VHE RATAN-600 log νFν radio ‘optical’ X-rays HE VHE RATAN-600 FERMI-LAT Effelsberg Swift UVOT KVA VLBA RATAN-600: end of 2008/09 – 10/03 Effelsberg: 2008/10/17; 11/08; 12/06; 2009/01/24 VLBA: 2008/10/23 Metsähovi: 2008/09/21; 10/07; 12/24, 27, 30; 2009/01/05, 07 IRAM: 2008/09/16; 12/06; 2009/01/06; 02/16 KVA (approx.): 2008/10/14 – 2009/01/03 Swift (approx.): 2008/09/21; 10/06 – 11/14 AGILE: 2008/10/31 – 11/30 Fermi: 2008/10/20 – 11/30 MAGIC (approx.): 2008/10/20 – 11/30 Swift XRT AGILE MAGIC Metsähovi IRAM 2008/10 2008/11 2008/12 2009/01 log E time

Results

Mrk 180 MWL LCs preliminary ‘high’ ‘low’ variability present at radio, optical, X-rays and HE gamma-rays strongest X-ray flare and highest flux ever for this source no direct correlation between optical and X-rays on daily scales but: HE flare shortly before X-ray flare, higher flux in optical no detection by Metsähovi and AGILE preliminary ‘high’ Fermi flare ended ~0.5 days before Swift highest flux ‘low’

Mrk 180 MWL SED preliminary clear shift of first peak visible, in high state located > 5 keV low state model parameters in agreement with usual HBL values high state cannot be described satisfactorily by both models due to steep X-ray spectrum and high optical flux two separate emission regions? extreme blazars (Costamante 2001): blazars with peak >~ 1 keV; up to now: Mrk 501, 2344, 1426, 0548, 1943 UVOT data are not de-reddened! KVA data are host-galaxy corrected; MAGIC data are EBL corrected used models: 1 zone: Maraschi, L., & Tavecchio, F., 2003, ApJ 593, 667 2 zone: Weidinger, M., & Spanier, F., 2010, A&A 515, 18 VHE data corrected for EBL effects (Kneiske et al. 2004, A&A 413, 807) preliminary

1ES 2344+514 MWL LC significantly variable at radio and X-rays optical, HE1 and VHE flux consistent with being constant no detection by Metsähovi, AGILE and Fermi MAGIC < 5 sigma, but spectrum possible inter-band correlations cannot be investigated due to low sampling add optical and radio monitoring data 1from LAT 1-year public light curve sampling quite bad; during good optical sampling, no X-rays and the other way round; also not sufficient data at other wavelength to correlate radio observations with KVA fit: 99.5% (Chi^2/dof = 13/29) preliminary

1ES 2344+514 MWL SED preliminary fluxes among the lowest ever for this object in optical, X-rays and VHE gamma-rays SED can be described well by the applied models model parameters do not differ significantly from usual HBL values no ‘quiescent state’? preliminary KVA data are host-galaxy corrected; MAGIC data are EBL corrected “no quiescent state” is intentionally ambiguous, meaning on the one hand that no quiescent state was detected and on the other hand that there is maybe no such thing as an quiescent state 1 zone 2 zones B [G] 0.07 0.10 δ 20 23 R [cm] 3.7∙1015 6.0∙1015 e1 2.1 2.0 e2 3.1 3.0 γmin 1 7 γbreak 8.0∙104 3.5∙104 γmax 9.0∙105 1.2∙106 VHE data corrected for EBL effects (Kneiske & Dole 2010, A&A 515, 18)

Thank you for your attention Summary & Conclusions first MWL campaigns from radio to VHE for both sources Mrk 180 variability present in radio, optical, X-rays and HE hint of correlated variability highest X-ray flux and strongest flare ever seen from this object clear shift of first SED peak with increasing flux detected -> ‘extreme blazar’ candidate high state SED challenges current emission models 1ES 2344+514 significant variability present only in radio and X-rays historically low fluxes observed in all bands but radio nevertheless no peculiar quiescent state discernible more data to come, thorough SED modelling in production Thank you for your attention +OVRO (radio monitoring), +Perugia (optical monitoring), +UVOT, +MAGIC

Image References [1]http://www.nasa.gov/centers/goddard/news/topstory/2007/active_galaxy.html blazar header: http://integral.esa.int/integ_pictures.html Effelsberg: http://www.mpifr-bonn.mpg.de/ public/cvh/seite7.html IRAM: http://www.iram.es/IRAMES Metsähovi: http://www.metsahovi.fi/legacy-2008-04-25/gallery RATAN-600: http://www.sao.ru/ratan VLBA: http://images.nrao.edu/Telescopes/VLBA KVA: http://www.astro.utu.fi/research/telescopes Swift: http://heasarc.nasa.gov/docs/swift/swiftsc.html AGILE: Caraveo, P., Moriond 2009 Fermi: http://fermi.gsfc.nasa.gov/public/resources/images