2015MNRAS.446.2456D


Query : 2015MNRAS.446.2456D

2015MNRAS.446.2456D - Mon. Not. R. Astron. Soc., 446, 2456-2467 (2015/January-3)

The most powerful flaring activity from the NLSy1 PMN J0948+0022.

D'AMMANDO F., ORIENTI M., FINKE J., RAITERI C.M., HOVATTA T., LARSSON J., MAX-MOERBECK W., PERKINS J., READHEAD A.C.S., RICHARDS J.L., BEILICKE M., BENBOW W., BERGER K., BIRD R., BUGAEV V., CARDENZANA J.V., CERRUTI M., CHEN X., CIUPIK L., DICKINSON H.J., EISCH J.D., ERRANDO M., FALCONE A., FINLEY J.P., FLEISCHHACK H., FORTIN P., FORTSON L., FURNISS A., GERARD L., GILLANDERS G.H., GRIFFITHS S.T., GRUBE J., GYUK G., HAKANSSON N., HOLDER J., HUMENSKY T.B., KAR P., KERTZMAN M., KHASSEN Y., KIEDA D., KRENNRICH F., KUMAR S., LANG M.J., MAIER G., McCANN A., MEAGHER K., MORIARTY P., MUKHERJEE R., NIETO D., O'FAOLAIN DE BHROITHE A., ONG R.A., OTTE A.N., POHL M., POPKOW A., PROKOPH H., PUESCHEL E., QUINN J., RAGAN K., REYNOLDS P.T., RICHARDS G.T., ROACHE E., ROUSSELLE J., SANTANDER M., SEMBROSKI G.H., SMITH A.W., STASZAK D., TELEZHINSKY I., TUCCI J.V., TYLER J., VARLOTTA A., VASSILIEV V.V., WAKELY S.P., WEINSTEIN A., WELSING R., WILLIAMS D.A. and ZITZER B.

Abstract (from CDS):

We report on multifrequency observations performed during 2012 December-2013 August of the first narrow-line Seyfert 1 galaxy detected in γ-rays, PMN J0948+0022 (z = 0.5846). A γ-ray flare was observed by the Large Area Telescope on board Fermi during 2012 December-2013 January, reaching a daily peak flux in the 0.1-100 GeV energy range of (155±31)x10–8 ph/cm2/s1 on 2013 January 1, corresponding to an apparent isotropic luminosity of ∼ 1.5x1048erg/s. The γ-ray flaring period triggered Swift and Very Energetic Radiation Imaging Telescope Array System (VERITAS) observations in addition to radio and optical monitoring by Owens Valley Radio Observatory, Monitoring Of Jets in Active galactic nuclei with VLBA Experiments, and Catalina Real-time Transient Survey. A strong flare was observed in optical, UV, and X-rays on 2012 December 30, quasi-simultaneously to the γ-ray flare, reaching a record flux for this source from optical to γ-rays. VERITAS observations at very high energy (E > 100 GeV) during 2013 January 6-17 resulted in an upper limit of F>0.2TeV < 4.0x10–12ph/cm2/s1. We compared the spectral energy distribution (SED) of the flaring state in 2013 January with that of an intermediate state observed in 2011. The two SEDs, modelled as synchrotron emission and an external Compton scattering of seed photons from a dust torus, can be modelled by changing both the electron distribution parameters and the magnetic field.

Abstract Copyright: © 2014 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society (2014)

Journal keyword(s): galaxies: active - galaxies: individual: PMN J0948+0022 - galaxies: nuclei - galaxies: Seyfert - gamma-rays: general

Simbad objects: 13

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Number of rows : 13
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026
#notes
1 6C 032130+340016 BLL 03 24 41.1612813408 +34 10 45.857918460     15.72 13.1   ~ 314 1
2 M 1 SNR 05 34 31.8 +22 01 03           ~ 6516 1
3 QSO B0537-441 BLL 05 38 50.36155950 -44 05 08.9390233   15.77 16.48 16   ~ 924 2
4 QSO J0849+5108 BLL 08 49 57.97685916 +51 08 29.0238146   19.37 18.78 17.79   ~ 270 2
5 4C 01.24B Bla 09 09 10.09159883 +01 21 35.6176206   17.63 17.29 17.04   ~ 454 2
6 QSO J0948+0022 Bla 09 48 57.32005819 +00 22 25.5596984   18.85 18.61 18.17   ~ 350 2
7 PSR J1023+0038 Psr 10 23 47.6841824712 +00 38 41.005893516     17.31     GV 470 0
8 7C 122223.5+213929 Bla 12 24 54.4583146056 +21 22 46.385507388   17.56 17.50 18.2   ~ 770 2
9 3C 279 Bla 12 56 11.16657958 -05 47 21.5251510   18.01 17.75 15.87   ~ 3205 2
10 3C 286 Sy1 13 31 08.2883506368 +30 30 32.960091564   17.51 17.25     ~ 4558 2
11 QSO J1512-0906 Bla 15 12 50.53293048 -09 05 59.8297908   16.74 16.54     ~ 1409 1
12 QSO J2147-7536 Bla 21 47 12.73063669 -75 36 13.2249063   17.79 17.30     ~ 167 1
13 3C 454.3 Bla 22 53 57.7480438728 +16 08 53.561508864   16.57 16.10 15.22   ~ 3004 2

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