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J/other/APh/26.282      AGN neutrino source candidates       (Achterberg+, 2006)

On the selection of AGN neutrino source candidates for a source stacking analysis with neutrino telescopes. Achterberg A., Ackermann M., Adams J., Ahrens J., Atlee D.W., Bahcall J.N., Bair X., Baret B., Bartelt M., Barwick S.W., Bay R., Beattie K., Becka T., Becker J.K., Becker K.-H., Berghaus P., Berley D., Bernardini E., Bertrand D., Besson D.Z., Blaufuss E., Boersma D.J., Bohm C., Boeser S., Botner O., Bouchta A., Braun J., Burgess C., Burgess T., Castermans T., Chirkin D., Clem J., Collin B., Conrad J., Cooley J., Cowen D.F., D'agostino M.V., Davour A., Day C.T., De Clercq C., Desiati P., Deyoung T., Dreyer J., Duvoort M.R., Edwards W.R., Ehrlich R., Ellsworth R.W., Evenson P.A., Fazely A.R., Feser T., Filimonov K., Gaisser T.K., Gallagher J., Ganugapati R., Geenen H., Gerhardt L., Goldschmidt A., Goodman J.A., Greene M.G., Grullon S., Gross A., Gunasingha R.M., Hallgren A., Halzen F., Han K., Hanson K., Hardtke D., Hardtke R., Harenberg T., Hart J.E., Hauschildt T., Hays D., Heise J., Helbing K., Hellwig M., Herquet P., Hill G.C., Hodges J., Hoffman K.D., Hoshina K., Hubert D., Hughey B., Hulth P.O., Hultqvist K., Hundertmark S., Ishihara A., Jacobsen J., Japaridze G.S., Jones A., Joseph J.M., Kampert K.-H., Karle A., Kawai H., Kelley J.L., Kestel M., Kitamura N., Klein S.R., Klepser S., Kohnen G., Kolanoski H., Koepke L., Krasberg M., Kuehn K., Landsman H., Lang R., Leich H., Leuthold M., Liubarsky I., Lundbert J., Madsen J., Mase K., Matis H.S., McCauley T., McParland C.P., Meli A., Messarius T., Meszaros P., Minor R.H., Miocinovic P., Miyamoto H., Mokhtarani A., Montaruli T., Morey A., Morse R., Movit S.M., Munich K., Nahnhauer R., Nam J.W., Niessen P., Nygren D.R., Oegelman H., Olbrechts PH., Olivas A., Patton S., Pena-Garay C., Perez de los Heros C., Pieloth D., Pohl A.C., Porrata R., Pretz J., Price P.B., Przybylski G.T., Rawlins K., Razzaque S., Refflinghaus F., Resconi E., Rhode W., Ribordy M., Richter S., Rizzo A., Robbins S., Rott C., Rutledge D., Sander H.-G., Schlenstedt S., Schneider D., Seckel D., Seo S.H., Seunarine S., Silvestri A., Smith A.J., Solarz M., Song C., Sopher J.E., Spiczak G.M., Spiering C., Stamatikos M., Stanev T., Steffen P., Steele D., Stezelberger T., Stokstad R.G., Stoufer M.C., Stoyanov S., Sulanke K.-H., Sullivan G.W., Sumner T.J., Taboada I., Tarasova O., Tepe A., Thollander L., Tilav S., Toale P.A., Turcan D., Van Eijndhoven T.J., Vandenbroucke J., Voigt B., Wagner W., Walck C., Waldmann H., Walter M., Wang Y.-R., Wendt C., Wiesbusch C.H., Wikstroem G., Williams D.R., Wischnewski R., Wissing H., Woschnagg K., Xu X.W., Yodh G., Yoshida S., Zornoza J.D., Biermann P.L. <Astroparticle Phys., 26, 282-300 (2006)> =2006APh....26..282A
ADC_Keywords: Active gal. nuclei ; Radio sources ; X-ray sources ; Infrared sources Keywords: Neutrinos - AGN - Source stacking - Point sources - AMANDA - IceCube Abstract: The sensitivity of a search for sources of TeV neutrinos can be improved by grouping potential sources together into generic classes in a procedure that is known as source stacking. In this paper, we define catalogs of Active Galactic Nuclei (AGN) and use them to perform a source stacking analysis. The grouping of AGN into classes is done in two steps: first, AGN classes are defined, then, sources to be stacked are selected assuming that a potential neutrino flux is linearly correlated with the photon luminosity in a certain energy band (radio, IR, optical, keV, GeV, TeV). Lacking any secure detailed knowledge on neutrino production in AGN, this correlation is motivated by hadronic AGN models, as briefly reviewed in this paper. The source stacking search for neutrinos from generic AGN classes is illustrated using the data collected by the AMANDA-II high-energy neutrino detector during the year 2000. No significant excess for any of the suggested groups was found. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file tableb1.dat 80 11 Strongest IR sources in blazar catalog tableb2.dat 80 14 ROSAT sources identified with strong radio blazars tableb3.dat 52 3 HEAO-A sources identified with strong radio blazars tableb4.dat 56 22 3EG sources identified with strong radio blazars tableb5.dat 32 25 Unidentified and weakly identified extragalactic EGRET sources, possibly blazars tableb6.dat 43 5 TeV blazars with δ>10° tableb7.dat 59 25 GPS and CSS sources fulfilling our selection rules (data compiled from previous catalogs in 1998) tableb8.dat 46 24 FR-I radio galaxies tableb9.dat 46 25 FR-II radio galaxies tableb10.dat 29 26 Radio-weak quasars from the Bright Quasar Survey (BQS) sorted according to IRAS mean flux at 60µ tableb11.dat 76 5 Nearby intrinsically weak sources
See also: J/ApJS/123/79 : Third EGRET catalog (3EG) (Hartman+, 1999) Byte-by-byte Description of file: tableb1.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [1Jy] 5- 11 A7 --- 1Jy Radio source (B1950, Cat. VIII/5) 13- 16 A4 --- --- [IRAS] 18- 28 A11 --- IRAS IR source (B1950, Cat. II/156) 30- 34 F5.2 Jy F5GHz Radio flux at 5GHz 36- 40 F5.2 --- Sp+Index Spectral index between 2.7GHz and 5GHz 42- 47 F6.4 Jy F12um 12µm infrared flux (1) 49- 54 F6.4 Jy F25um 25µm infrared flux (1) 56- 61 F6.4 Jy F60um 60µm infrared flux (1) 63- 68 F6.4 Jy F100um 100µm infrared flux (1) 70- 74 F5.3 --- z Cosmological redshift 76- 80 F5.1 Jy F5GHz(z=0.1) Distance corrected radio flux at 5GHz
Note (1): The IR data has been taken in the 1980s.
Byte-by-byte Description of file: tableb2.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [1RXS] 6- 21 A16 --- 1RXS X-ray source (J2000, JHHMMSS.s+DDMMSS) 23- 34 A12 --- RName Radio source (based on B1950 coordinates) 36- 41 F6.4 ct/s FX X-ray flux as measured by ROSAT in 1990/1991 (6 month of observation time) 43- 47 F5.2 --- HRI Hardness ratio I (1) 49- 53 F5.2 --- HRII Hardness ratio II (1) 55- 60 F6.3 Jy F5GHz Flux at 5GHz 62- 66 F5.2 --- Sp+Index Spectral index between 2.7GHz and 5GHz 68- 72 F5.3 --- z Redshift 74- 80 F7.1 Jy F5GHZ(z=1) Distance corrected radio flux at 5GHz
Note (1): The hardness ratios HR I and HR II display the ratio between low and high energy X-rays: HR=(H-L)/(H+L). For HR I, L=0.1-0.4keV and H=0.5-2.0keV For HR II, L=0.5-0.9keV and H=0.9-2.0keV
Byte-by-byte Description of file: tableb3.dat
Bytes Format Units Label Explanations
1- 10 A10 --- HEAO-A X-ray source (J2000, JHHMMSS.s+DDMMSS) 12- 23 A12 --- RName Radio source (based on B1950 coordinates) 25- 30 F6.4 ct/s FX X-ray flux as measured by HEAO-A in 1977-1978 (6 month of observation time) 32- 35 F4.2 Jy F5GHz Flux at 5GHz 37- 41 F5.2 --- Sp+Index Spectral index between 2.7GHz and 5GHz 43- 46 F4.2 --- z Redshift 48- 52 F5.1 Jy F5GHZ(z=1) Distance corrected radio flux at 5GHz
Byte-by-byte Description of file: tableb4.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [3EG] 5- 14 A10 --- 3EG 3EG source (J2000, JHHMMSS+DDMM) 16- 27 A12 --- RName Radio source (based on B1950 coordinates) 29- 33 F5.2 Jy F5GHz Flux at 5GHz 35- 39 F5.2 --- Sp+Index Spectral index between 2.7GHz and 5GHz 41- 45 F5.1 10-8s-1/cm2 FGeVmax Maximum flux measured by EGRET in 1991-1995 47- 50 F4.1 10-8s-1/cm2 FGeVmean Mean flux measured by EGRET in 1991-1995 52- 56 F5.3 --- z Redshift
Byte-by-byte Description of file: tableb5.dat
Bytes Format Units Label Explanations
1- 3 A3 --- --- [3EG] 5- 14 A10 --- 3EG 3EG source (J2000, JHHMMSS+DDMM) 16- 19 F4.1 10-8s-1/cm2 FGeVmax Maximum flux measured by EGRET in 1991-1995 21- 24 F4.1 10-8s-1/cm2 FGeVmean Mean flux measured by EGRET in 1991-1995 26- 30 F5.2 deg |GLAT| Absolute value of Galactic latitude 32 A1 --- f_3EG [a] indicates a possible AGN.
Byte-by-byte Description of file: tableb6.dat
Bytes Format Units Label Explanations
1- 13 A13 --- XName X-ray source designation 15- 21 A7 --- OName Other name 23- 26 F4.2 --- FTeVl Lower limit of TeV flux [in crab flux] (1) 27 A1 --- --- [-] 28- 31 F4.2 --- FTeVu ? Upper limit of TeV flux [in crab flux] (1) 33- 36 F4.2 Jy F5GHz Radio flux at 5 GHz 38- 43 F6.4 --- z Cosmoligical redshift
Note (1): The TeV fluxes are listed in units of the flux of the Crab nebula, dJγ/dE=(2.79±0.02±0.5)*10-7(E/TeV)(-2.59±0.03±0.05)
Byte-by-byte Description of file: tableb7.dat
Bytes Format Units Label Explanations
1- 8 A8 --- BName Coordinate name (B1950) 10- 17 A8 --- OName Other name (n.a. for not analysed) 19- 20 A2 --- Sample [GC ] (G)Hz Peaked Source and/or (C)ompact Steel Spectrum sample 22- 25 F4.1 mag Vmag Optical magnitude 27- 31 F5.3 --- z Cosmoligical redshift 33- 36 F4.2 Jy F5GHz Radio flux at 5GHz 38- 42 F5.3 arcsec Theta Angular size of the source 44- 47 I4 MHz FreqT Turnover frequency 49- 52 F4.1 [W/Hz] logP5GHz Power at 5GHz (assuming isotropic emission) 54- 59 F6.3 kpc Size Linear size of the sources
Byte-by-byte Description of file: tableb[8-9].dat
Bytes Format Units Label Explanations
1- 2 A2 --- --- [3C] 4- 9 A6 --- 3C Source name 10- 15 F6.1 Jy F178MHz Mean radio flux at 178MHz 18- 22 F5.2 --- Sp+Index Spectral index between 178MHz and 750MHz (1) 24- 30 F7.4 deg DEdeg Declination (B1950) 32- 40 F9.6 deg RAdeg Right ascension (B1950) 42- 46 F5.3 ---- z Cosmological redshift
Note (1): In the original 3CRR catalog (Laing et al., 1983MNRAS.204..151L), the spectral index is defined with an opposite sign.
Byte-by-byte Description of file: tableb10.dat
Bytes Format Units Label Explanations
1- 11 A11 --- QSO Quasar name 13- 16 I4 mJy F60um IRAS flux at 60um (data taken in the 1980s) 18- 22 F5.3 --- z Redshift (1) 24- 29 F6.2 [W/m2] logF14.5 Energy flux log(νF) at 1014.5Hz (1)
Note (1): Bright Quasar Survey (BQS, Schmidt and Green, 1983ApJ...269..352S) data were taken until 1983.
Byte-by-byte Description of file: tableb11.dat
Bytes Format Units Label Explanations
1- 12 A12 ---- RName Radio source (1) 14- 21 A8 ---- OName Other name 23- 76 A54 ---- Sample Samples (classes)
Note (1): Due to their proximity they nevertheless may contribute significantly to the neutrino flux. We propose to analyze them as individual sources.
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 01-Feb-2007
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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