المؤلفون: Sokolovsky, K. V., Schinzel, F. K., Tanaka, Y. T., Abolmasov, P. K., Angelakis, E., Bulgarelli, A., Carrasco, L., Cenko, S. B., Cheung, C. C., Clubb, K. I., D'Ammando, F., Escande, L., Fegan, S. J., Filippenko, A. V., Finke, J. D., Fuhrmann, L., Fukazawa, Y., Hays, E., Healey, S. E., Ikejiri, Y., Itoh, R., Kawabata, K. S., Komatsu, T., Kovalev, Yu. A., Kovalev, Y. Y., Krichbaum, T. P., Larsson, S., Lister, M. L., Lott, B., Max-Moerbeck, W., Nestoras, I., Pittori, C., Pursimo, T., Pushkarev, A. B., Readhead, A. C. S., Recillas, E., Richards, J. L., Riquelme, D., Romani, R. W., Sakimoto, K., Sasada, M., Schmidt, R., Shaw, M. S., Sievers, A., Thompson, D. J., Uemura, M., Ungerechts, H., Vercellone, S., Verrecchia, F., Yamanaka, M., Yoshida, M., Zensus, J. A.

المصدر: Astronomy & Astrophysics 565 (2014) A26

مصطلحات موضوعية: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics

الوصف: Previously unremarkable, the extragalactic radio source GB 1310+487 showed a gamma-ray flare on 2009 November 18, reaching a daily flux of ~10^-6 photons/cm^2/s at energies E>100 MeV and becoming one of the brightest GeV sources for about two weeks. Its optical spectrum is not typical for a blazar, instead, it resembles those of narrow emission-line galaxies. We investigate changes of the object's radio-to-GeV spectral energy distribution (SED) during and after the prominent GeV flare with the aim to determine the nature of the object and constrain the origin of the variable high-energy emission. The data collected by the Fermi and AGILE satellites at gamma-ray energies, Swift at X-ray and ultraviolet, Kanata, NOT, and Keck telescopes at optical, OAGH and WISE at infrared, and IRAM 30m, OVRO 40m, Effelsberg 100m, RATAN-600, and VLBA at radio, are analysed together to trace the SED evolution on timescales of months. The gamma-ray/radio-loud narrow-line active galactic nucleus (AGN) is located at redshift z=0.638. It is shining through an unrelated foreground galaxy at z=0.500. The AGN light is likely amplified by a factor of a few because of gravitational lensing. The AGN SED shows a two-humped structure typical of blazars and gamma-ray-loud NLSy1 galaxies, with the high-energy (inverse-Compton) emission dominating by more than an order of magnitude over the low-energy (synchrotron) emission during gamma-ray flares. The difference between the two SED humps is smaller during the low-activity state. Fermi observations reveal a strong correlation between the gamma-ray flux and spectral index, with the hardest spectrum observed during the brightest gamma-ray state. If the gamma-ray flux is a mixture of synchrotron self-Compton (SSC) and external Compton (EC) emission, the observed GeV spectral variability may result from varying relative contributions of these two emission components.
Comment: 18 pages, 10 figures, 6 tables; accepted to A&A

الوصول الحر: http://arxiv.org/abs/1401.2151Test

المؤلفون: Ajello, M., Romani, R. W., Gasparrini, D., Shaw, M. S., Bolmer, J., Cotter, G., Finke, J., Greiner, J., Healey, S. E., King, O., Max-Moerbeck, W., Michelson, P. F., Potter, W. J., Rau, A., Readhead, A. C. S., Richards, J. L., Schady, P.

مصطلحات موضوعية: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena

الوصف: Fermi has provided the largest sample of gamma-ray selected blazars to date. In this work we use a uniformly selected set of 211 BL Lacertae (BL Lac) objects detected by it Fermi during its first year of operation. We have obtained redshift constraints for 206 out of the 211 BL Lacs in our sample making it the largest and most complete sample of BL Lacs available in the literature. We use this sample to determine the luminosity function of BL Lacs and its evolution with cosmic time. We find that for most BL Lac classes, the evolution is positive with a space density peaking at modest redshift (z~1.2). The low-luminosity, high-synchrotron peaked (HSP) BL Lacs are an exception, showing strong negative evolution, with number density increasing for z$\lesssim$0.5. Since this rise corresponds to a drop-off in the density of flat-spectrum radio quasars (FSRQs), a possible interpretation is that these HSPs represent an accretion-starved end-state of an earlier merger-driven gas-rich phase. We additionally find that the known BL Lac correlation between luminosity and photon spectral index persists after correction for the substantial observational selection effects with implications for the so called `blazar sequence'. Finally, estimating the beaming corrections to the luminosity function, we find that BL Lacs have an average Lorentz factor of $\gamma=6.1^{+1.1}_{-0.8}$, and that most are seen within 10$^{\circ}$ of the jet axis.
Comment: accepted by ApJ

الوصول الحر: http://arxiv.org/abs/1310.0006Test

المؤلفون: Pavlidou, V., Richards, J. L., Max-Moerbeck, W., King, O. G., Pearson, T. J., Readhead, A. C. S., Reeves, R., Stevenson, M. A., Angelakis, E., Fuhrmann, L., Zensus, J. A., Giroletti, M., Reimer, A., Healey, S. E., Romani, R. W., Shaw, M. S.

مصطلحات موضوعية: Astrophysics - High Energy Astrophysical Phenomena

الوصف: Whether a correlation exists between the radio and gamma-ray flux densities of blazars is a long-standing question, and one that is difficult to answer confidently because of various observational biases which may either dilute or apparently enhance any intrinsic correlation between radio and gamma-ray luminosities. We introduce a novel method of data randomization to evaluate quantitatively the effect of these biases and to assess the intrinsic significance of an apparent correlation between radio and gamma-ray flux densities of blazars. The novelty of the method lies in a combination of data randomization in luminosity space (to ensure that the randomized data are intrinsically, and not just apparently, uncorrelated) and significance assessment in flux space (to explicitly avoid Malmquist bias and automatically account for the limited dynamical range in both frequencies). The method is applicable even to small samples that are not selected with strict statistical criteria. For larger samples we describe a variation of the method in which the sample is split in redshift bins, and the randomization is applied in each bin individually; this variation is designed to yield the equivalent to luminosity-function sampling of the underlying population in the limit of very large, statistically complete samples. We show that for a smaller number of redshift bins, the method yields a worse significance, and in this way it is conservative in that it does not assign a stronger, artificially enhanced significance. We demonstrate how our test performs as a function of number of sources, strength of correlation, and number of redshift bins used, and we show that while our test is robust against common-distance biases and associated false positives for uncorrelated data, it retains the power of other methods in rejecting the null hypothesis of no correlation for correlated data.
Comment: (corrected affiliations) 14 pages, 11 figures, accepted for publication in ApJ

الوصول الحر: http://arxiv.org/abs/1204.0790Test

المؤلفون: Ajello, M., Shaw, M. S., Romani, R. W., Dermer, C. D., Costamante, L., King, O. G., Max-Moerbeck, W., Readhead, A., Reimer, A., Richards, J. L., Stevenson, M.

مصطلحات موضوعية: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena

الوصف: Fermi has provided the largest sample of {\gamma}-ray selected blazars to date. In this work we use a complete sample of FSRQs detected during the first year of operation to determine the luminosity function (LF) and its evolution with cosmic time. The number density of FSRQs grows dramatically up to redshift \sim0.5-2.0 and declines thereafter. The redshift of the peak in the density is luminosity dependent, with more luminous sources peaking at earlier times; thus the LF of {\gamma}-ray FSRQs follows a luminosity-dependent density evolution similarly to that of radio-quiet AGN. Also using data from the Swift Burst Alert Telescope we derive the average spectral energy distribution of FSRQs in the 10 keV-100 GeV band and show that there is no correlation of the peak {\gamma}-ray luminosity with {\gamma}-ray peak frequency. The coupling of the SED and LF allows us to predict that the contribution of FSRQs to the Fermi isotropic {\gamma}-ray background is 9.3(+1.6/-1.0) (\pm3% systematic uncertainty) in the 0.1-100GeV band. Finally we determine the LF of unbeamed FSRQs, finding that FSRQs have an average Lorentz factor of {\gamma} = 11.7(+3.3/-2.2), that most are seen within 5\circ of the jet axis, and that they represent only ~0.1 % of the parent population.
Comment: Submitted to the Astrophysical Journal

الوصول الحر: http://arxiv.org/abs/1110.3787Test

المؤلفون: Lister, M. L., Aller, M., Aller, H., Hovatta, T., Kellermann, K. I., Kovalev, Y. Y., Meyer, E. T., Pushkarev, A. B., Ros, E., Ackermann, M., Antolini, E., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Blandford, R. D., Bloom, E. D., Boeck, M., Bonamente, E., Borgland, A. W., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cavazzuti, E., Cecchi, C., Chang, C. S., Charles, E., Chekhtman, A., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen-Tanugi, J., Conrad, J., Cutini, S., de Palma, F., Dermer, C. D., Silva, E. do Couto e, Drell, P. S., Drlica-Wagner, A., Favuzzi, C., Fegan, S. J., Ferrara, E. C., Finke, J., Focke, W. B., Fortin, P., Fukazawa, Y., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giglietto, N., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Grenier, I. A., Guiriec, S., Hadasch, D., Hayashida, M., Hays, E., Horan, D., Hughes, R. E., Jóhannesson, G., Johnson, A. S., Kadler, M., Katagiri, H., Kataoka, J., Knödlseder, J., Kuss, M., Lande, J., Longo, F., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Madejski, G. M., Mazziotta, M. N., McConville, W., McEnery, J. E., Mehault, J., Michelson, P. F., Mizuno, T., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Naumann-Godo, M., Nishino, S., Nolan, P. L., Norris, J. P., Nuss, E., Ohno, M., Ohsugi, T., Okumura, A., Omodei, N., Orlando, E., Ozaki, M., Paneque, D., Parent, D., Pesce-Rollins, M., Pierbattista, M., Piron, F., Pivato, G., Rainò, S., Readhead, A., Reimer, A., Reimer, O., Richards, J. L., Ritz, S., Sadrozinski, H. F. -W., Sgrò, C., Shaw, M. S., Siskind, E. J., Spandre, G., Spinelli, P., Takahashi, H., Tanaka, T., Thayer, J. G., Thayer, J. B., Thompson, D. J., Tosti, G., Tramacere, A., Troja, E., Usher, T. L., Vandenbroucke, J., Vasileiou, V., Vianello, G., Vitale, V., Waite, A. P., Wang, P., Winer, B. L., Wood, K. S., Zimmer, S.

المصدر: Astrophysical Journal 742 (2011) id. 27

مصطلحات موضوعية: Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena

الوصف: We investigate the Fermi LAT gamma-ray and 15 GHz VLBA radio properties of a joint gamma-ray- and radio-selected sample of AGNs obtained during the first 11 months of the Fermi mission (2008 Aug 4 - 2009 Jul 5). Our sample contains the brightest 173 AGNs in these bands above declination -30 deg. during this period, and thus probes the full range of gamma-ray loudness (gamma-ray to radio band luminosity ratio) in the bright blazar population. The latter quantity spans at least four orders of magnitude, reflecting a wide range of spectral energy distribution (SED) parameters in the bright blazar population. The BL Lac objects, however, display a linear correlation of increasing gamma-ray loudness with synchrotron SED peak frequency, suggesting a universal SED shape for objects of this class. The synchrotron self-Compton model is favored for the gamma-ray emission in these BL Lacs over external seed photon models, since the latter predict a dependence of Compton dominance on Doppler factor that would destroy any observed synchrotron SED peak - gamma-ray loudness correlation. The high-synchrotron peaked (HSP) BL Lac objects are distinguished by lower than average radio core brightness temperatures, and none display large radio modulation indices or high linear core polarization levels. No equivalent trends are seen for the flat-spectrum radio quasars (FSRQ) in our sample. Given the association of such properties with relativistic beaming, we suggest that the HSP BL Lacs have generally lower Doppler factors than the lower-synchrotron peaked BL Lacs or FSRQs in our sample.
Comment: 22 pages, 11 figures, 4 tables; accepted for publication in the Astrophysical Journal

الوصول الحر: http://arxiv.org/abs/1107.4977Test

المؤلفون: Vandenbroucke, J., Buehler, R., Ajello, M., Bechtol, K., Bellini, A., Bolte, M., Cheung, C. C., Civano, F., Donato, D., Fuhrmann, L., Funk, S., Healey, S. E., Hill, A. B., Knigge, C., Madejski, G. M., Romani, R. W., Santander-García, M., Shaw, M. S., Steeghs, D., Torres, M. A. P., Van Etten, A., Williams, K. A.

المصدر: Astrophysical Journal Letters 718 (2010) L166-L170

مصطلحات موضوعية: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Extragalactic Astrophysics

الوصف: The \emph{Fermi} Large Area Telescope (LAT) discovered a new gamma-ray source near the Galactic plane, \object{Fermi J0109+6134}, when it flared brightly in 2010 February. The low Galactic latitude (b =-1.2\degr) indicated that the source could be located within the Galaxy, which motivated rapid multi-wavelength follow-up including radio, optical, and X-ray observations. We report the results of analyzing all 19 months of LAT data for the source, and of X-ray observations with both \emph{Swift} and the \emph{Chandra X-ray Observatory}. We determined the source redshift, z =0.783, using a Keck LRIS observation. Finally, we compiled a broadband spectral energy distribution (SED) from both historical and new observations contemporaneous with the 2010 February flare. The redshift, SED, optical line width, X-ray absorption, and multi-band variability indicate that this new GeV source is a blazar seen through the Galactic plane. Because several of the optical emission lines have equivalent width >5\AA, this blazar belongs in the flat-spectrum radio quasar category.
Comment: 9 pages, 4 figures

الوصول الحر: http://arxiv.org/abs/1004.1413Test

المؤلفون: Richards, J. L., Max-Moerbeck, W., Pavlidou, V., Pearson, T. J., Readhead, A. C. S., Stevenson, M. A., Healey, S. E., Romani, R. W., Shaw, M. S., Fuhrmann, L., Angelakis, E., Zensus, J. A., Grainge, K., Taylor, G. B.

مصطلحات موضوعية: Astrophysics - Cosmology and Nongalactic Astrophysics

الوصف: We present results from the first two years of our fast-cadence 15 GHz gamma-ray blazar monitoring program, part of the F-GAMMA radio monitoring project. Our sample includes the 1158 blazars north of -20 degrees declination from the Candidate Gamma-Ray Blazar Survey (CGRaBS), which encompasses a significant fraction of the extragalactic sources detected by the Fermi Gamma-ray Space Telescope. We introduce a novel likelihood analysis for computing a time series variability amplitude statistic that separates intrinsic variability from measurement noise and produces a quantitative error estimate. We use this method to characterize our radio light curves. We also present results indicating a statistically significant correlation between simultaneous average 15 GHz radio flux density and gamma-ray photon flux.
Comment: 5 pages, 7 figures; 2009 Fermi Symposium; eConf Proceedings C091122

الوصول الحر: http://arxiv.org/abs/0912.3780Test

المؤلفون: Abdo, A. A., Ackermann, M., Ajello, M., Allafort, A., Antolini, E., Atwood, W. B., Axelsson, Magnus, Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Baughman, B. M., Bechtol, K., Bellazzini, R., Berenji, B., Blandford, R. D., Bloom, E. D., Bogart, J. R., Bonamente, E., Borgland, A. W., Bouvier, A., Bregeon, J., Brez, A., Brigida, M., Bruel, P., Buehler, R., Burnett, T. H., Buson, S., Caliandro, G. A., Cameron, R. A., Cannon, A., Caraveo, P. A., Carrigan, S., Casandjian, J. M., Cavazzuti, E., Cecchi, C., Celik, Oe., Celotti, A., Charles, E., Chekhtman, A., Chen, A. W., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen-Tanugi, J., Conrad, J., Costamante, L., Cotter, G., Cutini, S., D'Elia, V., Dermer, C. D., de Angelis, A., de Palma, F., De Rosa, A., Digel, S. W., do Couto e Silva, E., Drell, P. S., Dubois, R., Dumora, D., Escande, L., Farnier, C., Favuzzi, C., Fegan, S. J., Ferrara, E. C., Focke, W. B., Fortin, P., Frailis, M., Fukazawa, Y., 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., Grandi, P., Grenier, I. A., Grondin, M. -H, Grove, J. E., Guiriec, S., Hadasch, D., Harding, A. K., Hayashida, M., Hays, E., Healey, S. E., Hill, A. B., Horan, D., Hughes, R. E., Iafrate, G., Itoh, R., Johannesson, G., Johnson, A. S., Johnson, R. P., Johnson, T. J., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Kawai, N., Kerr, M., Knoedlseder, J., Kuss, M., Lande, J., Latronico, L., Lavalley, C., Lemoine-Goumard, M., Garde, M. Llena, Longo, F., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Madejski, G. M., Makeev, A., Malaguti, G., Massaro, E., Mazziotta, M. N., McConville, W., McEnery, J. E., McGlynn, Sinéad, Michelson, P. F., Mitthumsiri, W., Mizuno, T., Moiseev, A. A., Monte, C., Monzani, M. E., Morselli, A., Moskalenko, I. V., Murgia, S., Nolan, P. L., Norris, J. P., Nuss, E., Ohno, M., Ohsugi, T., Omodei, N., Orlando, E., Ormes, J. F., Ozaki, M., Paneque, D., Panetta, J. H., Parent, D., Pelassa, V., Pepe, M., Pesce-Rollins, M., Piranomonte, S., Piron, F., Porter, T. A., Raino, S., Rando, R., Razzano, M., Reimer, A., Reimer, O., Reposeur, T., Ripken, J., Ritz, S., Rodriguez, A. Y., Romani, R. W., Roth, M., Ryde, Felix, Sadrozinski, H. F. -W, Sanchez, D., Sander, A., Parkinson, P. M. Saz, Scargle, J. D., Sgro, C., Shaw, M. S., Siskind, E. J., Smith, P. D., Spandre, G., Spinelli, P., Starck, J. -L, Stawarz, L., Strickman, M. S., Suson, D. J., Tajima, H., Takahashi, H., Takahashi, T., Tanaka, T., Taylor, G. B., Thayer, J. B., Thayer, J. G., Thompson, D. J., Tibaldo, L., Torres, D. F., Tosti, G., Tramacere, A., Ubertini, P., Uchiyama, Y., Usher, T. L., Vasileiou, V., Vilchez, N., Villata, M., Vitale, V., Waite, A. P., Wallace, E., Wang, P., Winer, B. L., Wood, K. S., Yang, Z., Ylinen, Tomi, Ziegler, M.

المصدر: Astrophysical Journal. 715(1):429-457

مصطلحات موضوعية: BL Lacertae objects: general, catalogs, galaxies: active, gamma rays: galaxies, NATURAL SCIENCES, Physics, Astronomy and astrophysics, NATURVETENSKAP, Fysik, Astronomi och astrofysik

الوصف: We present the first catalog of active galactic nuclei (AGNs) detected by the Large Area Telescope (LAT), corresponding to 11 months of data collected in scientific operation mode. The First LAT AGN Catalog (1LAC) includes 671 gamma-ray sources located at high Galactic latitudes (|b| > 10 degrees) that are detected with a test statistic greater than 25 and associated statistically with AGNs. Some LAT sources are associated with multiple AGNs, and consequently, the catalog includes 709 AGNs, comprising 300 BL Lacertae objects, 296 flat-spectrum radio quasars, 41 AGNs of other types, and 72 AGNs of unknown type. We also classify the blazars based on their spectral energy distributions as archival radio, optical, and X-ray data permit. In addition to the formal 1LAC sample, we provide AGN associations for 51 low-latitude LAT sources and AGN "affiliations" (unquantified counterpart candidates) for 104 high-latitude LAT sources without AGN associations. The overlap of the 1LAC with existing gamma-ray AGN catalogs (LBAS, EGRET, AGILE, Swift, INTEGRAL, TeVCat) is briefly discussed. Various properties-such as gamma-ray fluxes and photon power-law spectral indices, redshifts, gamma-ray luminosities, variability, and archival radio luminosities-and their correlations are presented and discussed for the different blazar classes. We compare the 1LAC results with predictions regarding the gamma-ray AGN populations, and we comment on the power of the sample to address the question of the blazar sequence.

وصف الملف: print

الوصول الحر: https://urn.kb.se/resolve?urn=urn:nbn:se:kth:diva-28239Test
https://doi.org/10.1088/0004-637X/715/1/429Test

المؤلفون: Ackermann M., Ajello M., Allafort A., Antolini E., Atwood W. B., Axelsson M., Baldini L., Ballet J., Barbiellini G., Bastieri D., Bechtol K., Bellazzini R., Berenji B., Blandford R. D., Bloom E. D., Bonamente E., Borgland A. W., Bottacini E., Bouvier A., Bregeon J., Brigida M., Bruel P., Buehler R., Burnett T. H., Buson S., Caliandro G. A., Cameron R. A., Caraveo P. A., Casandjian J. M., Cavazzuti E., Cecchi C., Charles E., Cheung C. C., Chiang J., Ciprini S., Claus R., Cohen Tanugi J., Conrad J., Costamante L., Cutini S., De Angelis A., De Palma F., Dermer C. D., Digel S. W., Silva E. Do Couto E., Drell P. S., Dubois R., Escande L., Favuzzi C., Fegan S. J., Ferrara E. C., Finke J., Focke W. B., Fortin P., Frailis M., Fukazawa Y., Funk S., Fusco P., Gargano F., Gasparrini D., Gehrels N., Germani S., Giebels B., GIGLIETTO, Nicola, Giommi P., Giordano F., Giroletti M., Glanzman T., Godfrey G., Grenier I. A., Grove J. E., Guiriec S., Gustafsson M., Hadasch D., Hayashida M., Hays E., Healey S. E., Horan D., Hou X., Hughes R. E., Iafrate G., Johannesson G., Johnson A. S., Johnson W. N., Kamae T., Katagiri H., Kataoka J., Knodlseder J., Kuss M., Lande J., Larsson S., Latronico L., Longo F., Loparco F., Lott B., Lovellette M. N., Lubrano P., Madejski G. M., Mazziotta M. N., McConville W., McEnery J. E., Michelson P. F., Mitthumsiri W., Mizuno T., Moiseev A. A., Monte C., Monzani M. E., Moretti E., Morselli A., Moskalenko I. V., Murgia S., Nakamori T., Naumann Godo M., Nolan P. L., Norris P., Nuss E., Ohno M., Ohsugi T., Okumura A., Omodei N., Orienti M., Orlando E., Ormes J. F., Ozaki M., Paneque D., Parent D., Pesce Rollins M., Pierbattista M., Piranomonte S., Piron F., Pivato G., Porter T. A., Raino S., Rando R., Razzano M., Razzaque S., Reimer A., Reimer O., Ritz S., Rochester L. S., Romani R. W., Roth M., Sanchez D. A., Sbarra C., Scargle J. D., Schalk T. L., Sgro C., Shaw M. S., Siskind E. J., Spandre G., Spinelli P., Strong A. W., Suson D. J., Tajima H., Takahashi H., Takahashi T., Tanaka T., Thayer J. G., Thayer J. B., Thompson D. J., Tibaldo L., Tinivella M., Torres D. F., Tosti G., Troja E., Uchiyama Y., Vandenbroucke J., Vasileiou V., Vianello G., Vitale V., Waite A. P., Wallace E., Wang P., Winer B. L., Wood D. L., Wood K. S., Zimmer S.

المساهمون: Ackermann, M., Ajello, M., Allafort, A., Antolini, E., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Blandford, R. D., Bloom, E. D., Bonamente, E., Borgland, A. W., Bottacini, E., Bouvier, A., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Burnett, T. H., Buson, S., Caliandro, G. A., Cameron, R. A., Caraveo, P. A., Casandjian, J. M., Cavazzuti, E., Cecchi, C., Charles, E., Cheung, C. C., Chiang, J., Ciprini, S., Claus, R., Cohen Tanugi, J., Conrad, J., Costamante, L., Cutini, S., De Angelis, A., De Palma, F., Dermer, C. D., Digel, S. W., Silva, E. Do Couto E., Drell, P. S., Dubois, R., Escande, L., Favuzzi, C., Fegan, S. J., Ferrara, E. C., Finke, J., Focke, W. B., Fortin, P., Frailis, M., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Giebels, B., Giglietto, Nicola, Giommi, P., Giordano, F., Giroletti, M., Glanzman, T., Godfrey, G., Grenier, I. A., Grove, J. E., Guiriec, S., Gustafsson, M., Hadasch, D., Hayashida, M., Hays, E., Healey, S. E., Horan, D., Hou, X., Hughes, R. E., Iafrate, G., Johannesson, G., Johnson, A. S., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Knodlseder, J., Kuss, M., Lande, J., Larsson, S., Latronico, L., Longo, F., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Madejski, G. M., Mazziotta, M. N., Mcconville, W.

وصف الملف: ELETTRONICO

العلاقة: info:eu-repo/semantics/altIdentifier/wos/WOS:000356810300144; volume:806; issue:1; journal:THE ASTROPHYSICAL JOURNAL; http://hdl.handle.net/11589/7955Test; info:eu-repo/semantics/altIdentifier/scopus/2-s2.0-84934906120

الإتاحة: https://doi.org/10.1088/0004-637X/806/1/144Test
http://hdl.handle.net/11589/7955Test

المؤلفون: Ackermann, M., Ajello, M., Allafort, A., Antolini, E., Atwood, W. B., Axelsson, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bechtol, K., Ciprini, S., Claus, R., Cohen-Tanugi, J., Conrad, J., Costamante, L., Cutini, S., de Angelis, A., de Palma, F., Dermer, C. D., Michelson, P. F., Nakamori, T., Digel, S. W., Silva, E. do Couto e., Drell, P. S., Dubois, R., Escande, L., Favuzzi, C., Fegan, S. J., Ferrara, E. C., Finke, J., Focke, W. B., Naumann-Godo, M., Mitthumsiri, W., Fortin, P., FRAILIS, Marco, Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Gehrels, N., Germani, S., Nolan, P. L., Giebels, B., Mizuno, T., Giglietto, N., Giordano, F., GIROLETTI, MARCELLO, Glanzman, T., Godfrey, G., Grenier, I. A., Grove, J. E., Norris, J. P., Guiriec, S., Gustafsson, M., Moiseev, A. A., Hadasch, D., Hayashida, M., Hays, E., Healey, S. E., Horan, D., Hou, X., Hughes, R. E., Nuss, E., IAFRATE, Giulia, Jóhannesson, G., Johnson, A. S., Monte, C., Johnson, W. N., Kamae, T., Katagiri, H., Kataoka, J., Knödlseder, J., Kuss, M., Ohno, M., Lande, J., Larsson, S., Latronico, L., Longo, F., Monzani, M. E., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Madejski, G. M., Ohsugi, T., Mazziotta, M. N., McConville, W., Moretti, E., Morselli, A., Moskalenko, I. V., Bellazzini, R., Murgia, S., Okumura, A., Omodei, N., Berenji, B., Burnett, T. H., ORIENTI, Monica, Orlando, E., Ormes, J. F., Ozaki, M., Paneque, D., Parent, D., Pesce-Rollins, M., Pierbattista, M., PIRANOMONTE, Silvia, Piron, F., Buson, S., Blandford, R. D., Pivato, G., Porter, T. A., Rainò, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Ritz, S., Caliandro, G. A., Rochester, L. S., Bloom, E. D., Romani, R. W., Roth, M., Sanchez, D. A., Sbarra, C., Scargle, J. D., Schalk, T. L., SGRO, C., Shaw, M. S., Cameron, R. A., Siskind, E. J., Spandre, G., Bonamente, E., Spinelli, P., Strong, A. W., Suson, D. J., Tajima, H., Takahashi, H., Takahashi, T., Tanaka, T., CARAVEO, PATRIZIA, Thayer, J. G., Thayer, J. B., Thompson, D. J., Borgland, A. W., Tibaldo, L., Tinivella, M., Torres, D. F., Tosti, G., Troja, E., Uchiyama, Y., Casandjian, J. M., Vandenbroucke, J., Vasileiou, V., Vianello, G., Vitale, V., Bottacini, E., Waite, A. P., Wallace, E., Wang, P., Winer, B. L., Wood, D. L., Cavazzuti, E., Wood, K. S., Zimmer, S., Bouvier, A., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., Cecchi, C., Charles, E., Cheung, C. C., McEnery, J. E., Chiang, J.

المساهمون: ITA

العلاقة: THE ASTROPHYSICAL JOURNAL; http://hdl.handle.net/20.500.12386/24874Test; 2-s2.0-84934906120; 000356810300144; https://iopscience.iop.org/article/10.1088/0004-637X/806/1/144Test; 2015ApJ.806.144A

الإتاحة: https://doi.org/20.500.12386/24874Test
https://doi.org/10.1088/0004-637X/806/1/144Test
https://hdl.handle.net/20.500.12386/24874Test