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Multiwavelength monitoring of the enigmatic narrow -line Seyfert1 PMN J0948+0022 in 2009 March-July


Abdo, AA and Ackermann, M and Ajello, M and Axelsson, M and Baldini, L and Ballet, J and Barbiellini, G and Bastieri, D and Baughman, BM and Bechtol, K and Bellazzini, R and Berenji, B and Bloom, ED and Bonamente, E and Borgland, AW and Bregeon, J and Brez, A and Brigida, M and Bruel, P and Burnett, TH and Caliandro, GA and Cameron, RA and Caraveo, PA and Casandjian, JM and Cavazzuti, E and Cecchi, C and Celik, O and Celotti, A and Chekhtman, A and Chiang, J and Ciprini, S and Claus, R and Cohen-Tanugi, J and Collmar, W and Conrad, J and Costamante, L and Cutini, S and de Angelis, A and de Palma, F and Do Couto e Silva, E and Drell, PS and Dumora, D and Farnier, C and Favuzzi, C and Fegan, SJ and Focke, WB and Fortin, P and Foschini, L and Frailis, M and Fuhrmann, L and Fukazawa, Y and Funk, S and Fusco, P and Gargano, F and Gehrels, N and Germani, S and Giglietto, N and Giordano, F and Giroletti, M and Glanzman, T and Godfrey, G and Grenier, IA and Grove, JE and Guillemot, L and Guiriec, S and Hanabata, Y and Hays, E and Hughes, RE and Jackson, MS and Johannesson, G and Johnson, AS and Kadler, M and Kamae, T and Katagiri, H and Kataoka, J and Kawai, N and Kerr, M and Knoedlseder, J and Kocian, ML and Kuss, M and Lande, J and Latronico, L and Longo, F and Loparco, F and Lott, B and Lovellette, MN and Lubrano, P and Madejski, GM and Makeev, A and Max-Moerbeck, W and Mazziotta, MN and McConville, W and McEnery, JE and McGlynn, S and Meurer, C and Michelson, PF and Mitthumsiri, W and Mizuno, T and Moiseev, AA and Monte, C and Monzani, ME and Morselli, A and Moskalenko, I and Nestoras, I and Nolan, PL and Norris, JP and Nuss, E and Ohsugi, T and Omodei, N and Orlando, E and Ormes, JF and Paneque, D and Parent, D and Pavildou, V and Pelassa, V and Pepe, M and Pesce-Rollins, M and Piron, F and Porter, TA and Raino, S and Rando, R and Razzano, M and Readhead, A and Reimer, O and Reposeur, T and Richards, JL and Rodriguez, AY and Roth, M and Ryde, F and Sadrozinski, HFW and Sanchez, D and Sander, A and Parkinson, PMS and Scargle, JD and Shaw, MS and Smith, PD and Spandre, G and Spinelli, P and Strickman, MS and Suson, DJ and Tagliaferri, G and Tajima, H and Takahashi, H and Tanaka, T and Thayer, JB and Thompson, DJ and Tibaldo, L and Tibolla, O and Torres, DF and Tosti, G and Tramacere, A and Uchiyama, Y and Usher, TL and Vasileiou, V and Vilchez, N and Vitale, V and Waite, AP and Wang, P and Wehrle, AE and Winer, BL and Wood, KS and Yilnen, T and Zensus, JA and Ziegler, M and Angelakis, E and Bailyn, C and Bignall, H and Blanchard, JM and Bonning, EW and Buxton, M and Canterna, R and Carraminana, A and Carrasco, L and Colomer, F and Doi, A and Ghisellini, G and Hauser, M and Hong, X and Isler, J and Kino, M and Kovalev, YY and Kovalev, YA and Krichbaum, TP and Kutyrev, A and Lahteenmaki, A and van Langevelde, HJ and Lister, ML and Macomb, D and Maraschi, L and Marchili, N and Nagai, H and Paragi, Z and Phillips, C and Pushkarev, AB and Recillas, E and Roming, P and Sekido, M and Stark, MA and Szomoru, A and Tammi, J and Tavecchio, F and Tornikoski, M and Tzioumis, A and Urry, CM and Wagner, S and Johnson, WW and Sgro, C and Thayer, JG, Multiwavelength monitoring of the enigmatic narrow -line Seyfert1 PMN J0948+0022 in 2009 March-July, The Astrophysical Journal, 707, (1) pp. 727-737. ISSN 0004-637X (2009) [Refereed Article]

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DOI: doi:10.1088/0004-637X/707/1/727


Following the recent discovery of γ rays from the radio-loud narrow-line Seyfert 1 galaxy PMN J0948+0022 (z = 0.5846), we started a multiwavelength campaign from radio to γ rays, which was carried out between the end of 2009 March and the beginning of July. The source displayed activity at all the observed wavelengths: a general decreasing trend from optical to γ -ray frequencies was followed by an increase of radio emission after less than two months from the peak of the γ -ray emission. The largest flux change, about a factor of about 4, occurred in the X-ray band. The smallest was at ultraviolet and near-infrared frequencies, where the rate of the detected photons dropped by a factor 1.6–1.9. At optical wavelengths, where the sampling rate was the highest, it was possible to observe day scale variability, with flux variations up to a factor of about 3. The behavior of PMN J0948+0022 observed in this campaign and the calculated power carried out by its jet in the form of protons, electrons, radiation, and magnetic field are quite similar to that of blazars, specifically of flat-spectrum radio quasars. These results confirm the idea that radio-loud narrow-line Seyfert 1 galaxies host relativistic jets with power similar to that of average blazars.

Item Details

Item Type:Refereed Article
Keywords:galaxies: active – gamma rays: observations – infrared: galaxies – quasars: individual (PMN
Research Division:Physical Sciences
Research Group:Astronomical sciences
Research Field:Cosmology and extragalactic astronomy
Objective Division:Expanding Knowledge
Objective Group:Expanding knowledge
Objective Field:Expanding knowledge in the physical sciences
UTAS Author:Blanchard, JM (Mr Jay Blanchard)
ID Code:68926
Year Published:2009
Web of Science® Times Cited:77
Deposited By:Mathematics and Physics
Deposited On:2011-04-04
Last Modified:2011-04-15

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