2012A&A...548A.106F


C.D.S. - SIMBAD4 rel 1.7 - 2020.05.29CEST02:58:41

2012A&A...548A.106F - Astronomy and Astrophysics, volume 548A, 106-106 (2012/12-1)

Radio-to-γ-ray monitoring of the narrow-line Seyfert 1 galaxy PMN J0948+0022 from 2008 to 2011.

FOSCHINI L., ANGELAKIS E., FUHRMANN L., GHISELLINI G., HOVATTA T., LAHTEENMAKI A., LISTER M.L., BRAITO V., GALLO L., HAMILTON T.S., KINO M., KOMOSSA S., PUSHKAREV A.B., THOMPSON D.J., TIBOLLA O., TRAMACERE A., CARRAMINANA A., CARRASCO L., FALCONE A., GIROLETTI M., GRUPE D., KOVALEV Y.Y., KRICHBAUM T.P., MAX-MOERBECK W., NESTORAS I., PEARSON T.J., PORRAS A., READHEAD A.C.S., RECILLAS E., RICHARDS J.L., RIQUELME D., SIEVERS A., TAMMI J., TORNIKOSKI M., UNGERECHTS H., ZENSUS J.A., CELOTTI A., BONNOLI G., DOI A., MARASCHI L., TAGLIAFERRI G. and TAVECCHIO F.

Abstract (from CDS):

We present more than three years of observations at different frequencies, from radio to high-energy γ-rays, of the Narrow-Line Seyfert 1 (NLS1) Galaxy PMN J0948+0022 (z=0.585). This source is the first NLS1 detected at energies above 100 MeV and therefore can be considered the prototype of this emerging new class of γ-ray emitting active galactic nuclei (AGN). The observations performed from 2008 August 1 to 2011 December 31 confirmed that PMN J0948+0022 generates a powerful relativistic jet, which is able to develop an isotropic luminosity at γ-rays of the order of 1048erg/s, at the level of powerful quasars. The evolution of the radiation emission of this source in 2009 and 2010 followed the canonical expectations of relativistic jets with correlated multiwavelength variability (γ-rays followed by radio emission after a few months), but it was difficult to retrieve a similar pattern in the light curves of 2011. The comparison of γ-ray spectra before and including 2011 data suggested that there was a softening of the high-energy spectral slope. We selected five specific epochs to be studied by modelling the broad-band spectrum, which are characterised by an outburst at γ-rays or very low/high flux at other wavelengths. The observed variability can largely be explained by changes in the injected power, the bulk Lorentz factor of the jet, or the electron spectrum. The characteristic time scale of doubling/halving flux ranges from a few days to a few months, depending on the frequency and the sampling rate. The shortest doubling time scale at γ-rays is 2.3±0.5days. These small values underline the need of highly sampled multiwavelength campaigns to better understand the physics of these sources.

Abstract Copyright:

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

VizieR on-line data: <Available at CDS (J/A+A/548/A106): fermi.dat xrt.dat uvot.dat inaoe.dat radio.dat>

Status at CDS:  

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 - 2020
#notes
1 NAME W 3 OH HII 02 27 04.1 +61 52 22           ~ 939 2
2 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3523 3
3 QSO J0324+3410 BLL 03 24 41.1612231119 +34 10 45.856728058     15.72 13.1   ~ 197 1
4 QSO B0426-380 BLL 04 28 40.4242766573 -37 56 19.583011524   18.96 19.0 17.21   ~ 248 1
5 ICRF J084957.9+510829 Sy1 08 49 57.97682961 +51 08 29.0234509   19.37 18.78 17.79   ~ 192 2
6 3FGL J0948.8+0021 Sy1 09 48 57.3204380262 +00 22 25.561362007   18.85 18.61 18.17   ~ 245 2
7 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6169 3
8 3C 286 Sy1 13 31 08.2885060664 +30 30 32.960825108   17.51 17.25     ~ 3699 1
9 ICRF J150506.4+032630 Sy1 15 05 06.47715917 +03 26 30.8126616   19.02 18.62 17.72   ~ 194 1
10 QSO B1959+650 BLL 19 59 59.8525497024 +65 08 54.651170114     12.8 11.21   ~ 500 2
11 NAME K 3-50A HII 20 01 45.6 +33 32 42           ~ 75 0
12 GRS G081.70 +00.50 SFR 20 39 01.6 +42 19 38           O4.5 941 0
13 NGC 7027 PN 21 07 01.8 +42 14 10   9.1 10.9     ~ 2318 1

    Equat.    Gal    SGal    Ecl

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2020.05.29-02:58:41

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