2001ApJ...553..683H

Query : 2001ApJ...553..683H

2001ApJ...553..683H - Astrophys. J., 553, 683-694 (2001/June-1)

Multiepoch multiwavelength spectra and models for blazar 3C 279.

HARTMAN R.C., BOTTCHER M., ALDERING G., ALLER H., ALLER M., BACKMAN D.E., BALONEK T.J., BERTSCH D.L., BLOOM S.D., BOCK H., BOLTWOOD P., CARINI M.T., COLLMAR W., DE FRANCESCO G., FERRARA E.C., FREUDLING W., GEAR W.K., HALL P.B., HEIDT J., HUGHES P., HUNTER S.D., JOGEE S., JOHNSON W.N., KANBACH G., KATAJAINEN S., KIDGER M., KII T., KOSKIMIES M., KRAUS A., KUBO H., KURTANIDZE O., LANTERI L., LAWSON A., LIN Y.C., LISENFELD U., MADEJSKI G., MAKINO F., MARASCHI L., MARSCHER A.P., McFARLAND J.P., McHARDY I., MILLER H.R., NIKOLASHVILI M., NILSSON K., NOBLE J.C., NUCCIARELLI G., OSTORERO L., PIAN E., PURSIMO T., RAITERI C.M., REICH W., REKOLA R., RICHTER G.M., ROBSON E.I., SADUN A., SAVOLAINEN T., SILLANPAA A., SMALE A., SOBRITO G., SREEKUMAR P., STEVENS J.A., TAKALO L.O., TAVECCHIO F., TERASRANTA H., THOMPSON D.J., TORNIKOSKI M., TOSTI G., UNGERECHTS H., URRY C.M., VALTAOJA E., VILLATA M., WAGNER S.J., WEHRLE A.E. and WILSON J.W.

Abstract (from CDS):

Of the blazars detected by EGRET in GeV γ-rays, 3C 279 is not only the best observed by EGRET but also one of the best monitored at lower frequencies. We have assembled 11 spectra, from GHz radio through GeV γ-rays, from the time intervals of EGRET observations. Although some of the data have appeared in previous publications, most are new, including data taken during the high states in early 1999 and early 2000. All of the spectra show substantial γ-ray contribution to the total luminosity of the object; in a high state, the γ-ray luminosity dominates over that at all other frequencies by a factor of more than 10. There is no clear pattern of time correlation; different bands do not always rise and fall together, even in the optical, X-ray, and γ-ray bands. The spectra are modeled using a leptonic jet, with combined synchrotron self-Compton plus external Compton γ-ray production. Spectral variability of 3C 279 is consistent with variations of the bulk Lorentz factor of the jet, accompanied by changes in the spectral shape of the electron distribution. Our modeling results are consistent with the UV spectrum of 3C 279 being dominated by accretion disk radiation during times of low γ-ray intensity.

Abstract Copyright: ∼

Journal keyword(s): Gamma Rays: Observations - Galaxies: Quasars: Individual: Alphanumeric: 3C 279

Simbad objects: 11

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Number of rows : 11

N	Identifier	Otype	ICRS (J2000) RA	ICRS (J2000) DEC	Mag U	Mag B	Mag V	Mag R	Mag I	Sp type	#ref 1850 - 2026	#notes
1	NAME W 3 OH	HII	02 27 04.1	+61 52 22						~	1064	2
2	RAFGL 618	pA*	04 42 53.6242032600	+36 06 53.400902220		16.32		12.59		C-rich	1027	0
3	QSO J0530+13	Bla	05 30 56.41674741	+13 31 55.1494688			20.00	19.35		~	1004	1
4	3C 273	BLL	12 29 06.6998257176	+02 03 08.597629980		13.05	14.830	14.11		~	6022	1
5	M 87	AGN	12 30 49.42338414	+12 23 28.0436859	10.16	9.59	8.63		7.49	~	7815	3
6	3C 279	Bla	12 56 11.16657958	-05 47 21.5251510		18.01	17.75	15.87		~	3205	2
7	3C 286	Sy1	13 31 08.2883506368	+30 30 32.960091564		17.51	17.25			~	4558	2
8	W 58a	HII	20 01 45.8	+33 32 43						~	294	4
9	NGC 7027	PN	21 07 01.571952	+42 14 10.47120		10.358	8.831	10.157		~	2541	1
10	NGC 7538	OpC	23 13 37	+61 30.0						~	920	1
11	NAME Cas A	SNR	23 23 26.0	+58 48 41			14.30			~	3033	1

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