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 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:
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FileName Lrecl Records Explanations
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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
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See also:
J/ApJS/123/79 : Third EGRET catalog (3EG) (Hartman+, 1999)
Byte-by-byte Description of file: tableb1.dat
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Bytes Format Units Label Explanations
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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
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Note (1): The IR data has been taken in the 1980s.
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Byte-by-byte Description of file: tableb2.dat
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Bytes Format Units Label Explanations
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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
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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
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Byte-by-byte Description of file: tableb3.dat
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Bytes Format Units Label Explanations
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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
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Byte-by-byte Description of file: tableb4.dat
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Bytes Format Units Label Explanations
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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
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Byte-by-byte Description of file: tableb5.dat
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Bytes Format Units Label Explanations
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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.
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Byte-by-byte Description of file: tableb6.dat
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Bytes Format Units Label Explanations
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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
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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)
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Byte-by-byte Description of file: tableb7.dat
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Bytes Format Units Label Explanations
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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
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Byte-by-byte Description of file: tableb[8-9].dat
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Bytes Format Units Label Explanations
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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
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Note (1): In the original 3CRR catalog (Laing et al., 1983MNRAS.204..151L 1983MNRAS.204..151L),
the spectral index is defined with an opposite sign.
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Byte-by-byte Description of file: tableb10.dat
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Bytes Format Units Label Explanations
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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)
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Note (1): Bright Quasar Survey (BQS, Schmidt and Green, 1983ApJ...269..352S 1983ApJ...269..352S)
data were taken until 1983.
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Byte-by-byte Description of file: tableb11.dat
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Bytes Format Units Label Explanations
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1- 12 A12 ---- RName Radio source (1)
14- 21 A8 ---- OName Other name
23- 76 A54 ---- Sample Samples (classes)
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Note (1): Due to their proximity they nevertheless may contribute
significantly to the neutrino flux. We propose to analyze them
as individual sources.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 01-Feb-2007