BRIGHT ACTIVE GALACTIC NUCLEI SOURCE LIST FROM THE FIRST THREE MONTHS OF THE<i>FERMI</i>LARGE AREA TELESCOPE ALL-SKY SURVEY

Abdo, A. A.; Ackermann, M.; Ajello, M.; Atwood, W. B.; Axelsson, M.; Baldini, Luca; Ballet, J.; Barbiellini, G.; Bastieri, D.; Baughman, B. M.; Bechtol, K.; Bellazzini, R.; Blandford, R. D.; Bloom, E. D.; Bonamente, E.; Borgland, A. W.; Bouvier, A.; Bregeon, J.; Brez, A.; Brigida, M.; Bruel, Pascal; Burnett, T. H.; Caliandro, G. A.; Cameron, R. A.; Caraveo, P. A.; Casandjian, J. M.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Chekhtman, A.; Chen, Andrew; Cheung, C. C.; Chiang, J.; Ciprini, S.; Claus, R.; Cohen-Tanugi, J.; Colafrancesco, S.; Collmar, W.; Cominsky, L.; Conrad, J.; Costamante, L.; Cutini, S.; Dermer, C. D.; Angelis, A. De; Palma, F. de; Digel, S. W.; Silva, E. do Couto e; Drell, P. S.; Dubois, R.; Dumora, D.; Farnier, C.; Favuzzi, C.; Fegan, S. J.; Ferrara, E. C.; Finke, J.; Focke, W. B.; Foschini, L.; Frailis, M.; Fuhrmann, L.; Fukazawa, Yasushi; Funk, S.; Fusco, P.; Gargano, F.; Gasparrini, D.; Gehrels, N.; Germani, S.; Giebels, B.; Giglietto, N.; Giommi, P.; Giordano, F.; Giroletti, M.; Glanzman, T.; Godfrey, G.; Grenier, I. A.; Grondin, M.‐H.; Grove, J. E.; Guillemot, L.; Guiriec, S.; Hanabata, Y.; Harding, A. K.; Hartman, R. C.; Hayashida, M.; Hays, E.; Healey, S. E.; Horan, D.; Hughes, R. E.; Jóhannesson, G.; Johnson, A. S.; Johnson, R. P.; Johnson, T. J.; Johnson, W. N.; Kadler, M.; Kamae, T.; Katagiri, H.; Kataoka, J.; Kerr, M.; Knödlseder, J.; Kocian, M.; Kuehn, F.; Kuss, M.; Landé, J.; Latronico, L.; Lemoine‐Goumard, M.; Longo, F.; Loparco, F.; Lott, B.; Lovellette, M. N.; Lubrano, P.; Madejski, G.; Makeev, A.; Massaro, E.; Mazziotta, M. N.; McConville, W.; McEnery, J. E.; McGlynn, S.; Meurer, C.; Michelson, P. F.; Mitthumsiri, W.; Mizuno, T.; Моисеев, А. А.; Monte, C.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.; Murgia, S.; Nolan, P. L.; Norris, J. P.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orlando, E.; Ormes, J. F.; Ozaki, Masanori; Paneque, D.; Panetta, J.; Parent, D.; Pelassa, V.; Pepé, M.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer, O.; Reposeur, T.; Reyes, Luis; Ritz, S.; Rochester, Lynn; Rodriguez, A. Y.; Romani, Roger W.; Ryde, F.; Sadrozinski, H. F-W.; Sánchez, David; Sander, A.; Parkinson, P. M. Saz; Scargle, Jeffrey D.; Schalk, T.; Sellerholm, A.; Sgrò, C.; Shaw, M. S.; Smith, David A.; Smith, P. D.; Spandre, G.; Spinelli, P.; Starck, Jean-Luc; Strickman, M. S.; Suson, D. J.; Tajima, H.; Takahashi, H.; Takahashi, Tadayuki; Tanaka, Takaaki; Taylor, G. B.; Thayer, J. B.; Thayer, J. G.; Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Tosti, G.; Tramacere, A.; Uchiyama, Y.; Usher, T.; Vilchez, N.; Villata, M.; Vitale, V.; Waite, A. P.; Winer, B. L.; Wood, K. S.; Ylinen, T.; Ziegler, M.

doi:10.1088/0004-637x/700/1/597

Cited by 395 publications

(340 citation statements)

References 69 publications

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“…Furthermore, these objects are hard γ-ray spectrum sources and we do not find any exception when placed in the γ-ray photon index versus then sy pk diagram ( Figure 5). Ghisellini et al (2009) utilized ∼100 blazars from the first three-month survey of Fermi-LAT data (Abdo et al 2009) and noticed a division between FSRQs and BL Lacs by comparing their γ-ray spectral indices (G g ) to the γ-ray luminosities ( g L ). These observations revealed that BL Lacs exhibited harder spectra (  G g 2.2) and were less luminous (  g L 10 47 erg s −1 ) than FSRQs.…”

Section: Blazar Sequencementioning

confidence: 99%

NEW HIGH-z FERMI BL LACS WITH THE PHOTOMETRIC DROPOUT TECHNIQUE

Kaur

Rau

Ajello

et al. 2016

ApJ

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Determining redshifts for BL Lacertae (BL Lac) objects using the traditional spectroscopic method is challenging due to the absence of strong emission lines in their optical spectra. We employ the photometric dropout technique to determine redshifts for this class of blazars using the combined 13 broadband filters from Swift-UVOT and the multi-channel imager GROND at the MPG 2.2 m telescope at ESOʼs La Silla Observatory. The wavelength range covered by these 13 filters extends from far-ultraviolet to the near-infrared. We report results on 40 new Fermidetected BL Lacs with the photometric redshiftdeterminations for fivesources, with 3FGL J1918.2-4110 being the most distant in our sample at z=2.16. Reliable upper limits are provided for 20 sources in this sample. Using the highest energy photons for these Fermi-LAT sources, we evaluate the consistency with the gamma-ray horizon due to the extragalactic background light.

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Section: Blazar Sequencementioning

confidence: 99%

NEW HIGH-z FERMI BL LACS WITH THE PHOTOMETRIC DROPOUT TECHNIQUE

Kaur

Rau

Ajello

et al. 2016

ApJ

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“…Relativistic beaming of radiation is generally invoked to explain the extreme properties (Madau, Ghisellini & Persic 1987). Since the launch of the Fermi satellite, we have entered in a new era of blazars research (Abdo et al 2009a(Abdo et al , 2010a(Abdo et al , 2012. Up to now, the Large Area Telescope (LAT) has detected hundreds of blazars because it has about 20 fold better sensitivity than its predecessor EGRET in the 0.1−100 GeV energy rang.…”

Section: Introductionmentioning

confidence: 99%

Basic properties of Fermi blazars and the ‘blazar sequence’

Xiong

Zhang

Bai

et al. 2015

Monthly Notices of the Royal Astronomical Society

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By statistically analyzing a large sample which includes blazars of Fermi detection (FBs) and non-Fermi detection (NFBs), we find that there are significant differences between FBs and NFBs for redshift, black hole mass, jet kinetic power from "cavity" power, broad-line luminosity, and ratio of core luminosity to absolute V-band magnitude (R v ), but not for ratio of radio core to extended flux (R c ) and Eddington ratio. Compared with NFBs, FBs have larger mean jet power, R c and R v while smaller mean redshift, black hole mass, broad-line luminosity. These results support that the beaming effect is main reason for differences between FBs and NFBs, and that FBs are likely to have a more powerful jet. For both Fermi and non-Fermi blazars, there are significant correlations between jet power and the accretion rate (traced by the broad-emission-lines luminosity), between jet power and black hole mass; for Fermi blazars, the black hole mass does not have significant influence on jet power while for non-Fermi blazars, both accretion rate and black hole mass have contributions to the jet power. Our results support the "blazar sequence" and show that synchrotron peak frequency (ν peak ) is associated with accretion rate but not with black hole mass.

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“…The variability at high radio frequencies is outstanding: the quiescent flux density is less than 1 Jy and during the outbursts the source reached up to more than 10 Jy with the fractional variability index, defined as Var ΔS = (S max − S min )/S min , about 13 and 18 at 37 and 90 GHz, respectively (Torniainen et al 2005). In gamma-ray band, it was recently detected with Fermi (Abdo et al 2009) though no counterpart was found by EGRET according to Mattox et al (2001).…”

Section: Introductionmentioning

confidence: 99%

The parsec-scale jet of PKS 1749+096

Shen

Krichbaum

et al. 2012

A&A

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Context. PKS 1749+096 is a BL Lac object showing weak extended jet emission to the northeast of the compact VLBI core on parsec scales. Aims. We aim at better understanding the jet kinematics and variability of this source and finding clues that may applicable to other BL Lac objects. Methods. The jet was studied with multi-epoch multi-frequency high-resolution VLBI observations. Results. The jet is characterized by a one-sided curved morphology at all epochs and all frequencies. The VLBI core, located at the southern end of the jet, was identified based on its spectral properties. The equipartition magnetic field of the core was investigated, through which we derived a Doppler factor of 5, largely consistent with that derived from kinematics (component C5). The study of the detailed jet kinematics at 22 and 15 GHz, spanning a period of more than 10 years, indicates the possible existence of a bimodal distribution of the jet apparent speed. Ballistic and non-ballistic components are found to coexist in the jet. Superluminal motions in the range of 5-21 c were measured in 11 distinct components. We estimated the physical jet parameters with the minimum Lorentz factor of 10.2 and Doppler factors in the range of 10.2-20.4 (component C5). The coincidence in time of the component's ejection and flares supports the idea that, at least in PKS 1749+096, ejection of new jet components is connected with major outbursts in flux density. For the best-traced component (C5) we found that the flux density decays rapidly as it travels downstream the jet, accompanied by a steepening of its spectra, which argues in favor of a contribution of inverse Compton cooling. These properties make PKS 1749+096 a suitable target for an intensive monitoring to decipher the variability phenomenon of BL Lac objects.

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BRIGHT ACTIVE GALACTIC NUCLEI SOURCE LIST FROM THE FIRST THREE MONTHS OF THEFERMILARGE AREA TELESCOPE ALL-SKY SURVEY

Cited by 395 publications

References 69 publications

NEW HIGH-z FERMI BL LACS WITH THE PHOTOMETRIC DROPOUT TECHNIQUE

NEW HIGH-z FERMI BL LACS WITH THE PHOTOMETRIC DROPOUT TECHNIQUE

Basic properties of Fermi blazars and the ‘blazar sequence’

The parsec-scale jet of PKS 1749+096

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