1. 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 MWL team
1Institut für Theoretische Physik und Astrophysik, Lehrstuhl für Astronomie, Universität Würzburg

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

3. Mrk 180 and 1ES

4. 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 , 1ES

5. 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

6. Sources - 1ES
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
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

7. Instruments and Campaigns

8. 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

9. 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/ /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

10. 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

11. Results

12. 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’

13. 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

14. 1ES 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

15. 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)

16. 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
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

17. Image References
[1]
blazar header:
Effelsberg: public/cvh/seite7.html
IRAM:
Metsähovi:
RATAN-600:
VLBA:
KVA:
Swift:
AGILE: Caraveo, P., Moriond 2009
Fermi: