Properties of flat-spectrum radio-loud narrow-line Seyfert 1 galaxies

L. Foschini; M. Berton; A. Caccianiga; S. Ciroi; V. Cracco; B. M. Peterson; E. Angelakis; V. Braito; L. Fuhrmann; L. Gallo; D. Grupe; E. Järvelä; S. Kaufmann; S. Komossa; Y. Y. Kovalev; A. Lähteenmäki; M. M. Lisakov; M. L. Lister; S. Mathur; J. L. Richards; P. Romano; A. Sievers; G. Tagliaferri; J. Tammi; O. Tibolla; M. Tornikoski; S. Vercellone; G. La Mura; L. Maraschi; P. Rafanelli

doi:10.1051/0004-6361/201424972

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Volume 575 (March 2015)

A&A, 575 (2015) A13

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This article has an erratum: [erratum]

Issue		A&A Volume 575, March 2015


Article Number		A13
Number of page(s)		33
Section		Extragalactic astronomy
DOI		https://doi.org/10.1051/0004-6361/201424972
Published online		11 February 2015

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Table 4

Gamma-ray spectral characteristics.

Table 5

X-ray characteristics.

Table 6

Swift/UVOT observed average magnitudes (extracted from all the data integrated).

Table 7

Characteristics at radio frequencies (VLBI).

Table 8

Spectral indices (S_ν ∝ ν^{− α}) at different frequencies.

Table 9

Shortest variability at optical-to-γ ray frequencies.

	Fig. 8 Spectral energy distributions of the sources in the present sample. Data are corrected for the Galactic absorption. Points refer to detections; arrows are upper limits; the continuous lines are the optical spectra.
Open with DEXTER

	Fig. 9 Spectral energy distributions of the sources in the present sample. Data are corrected for the Galactic absorption. Points refer to detections; arrows are upper limits; the continuous lines are the optical spectra.
Open with DEXTER

	Fig. 10 Spectral energy distributions of the sources in the present sample. Data are corrected for the Galactic absorption. Points refer to detections; arrows are upper limits; the continuous lines are the optical spectra.
Open with DEXTER

	Fig. 11 Spectral energy distributions of the sources in the present sample. Data are corrected for the Galactic absorption. Points refer to detections; arrows are upper limits; the continuous lines are the optical spectra.
Open with DEXTER

	Fig. 12 Spectral energy distributions of the sources in the present sample. Data are corrected for the Galactic absorption. Points refer to detections; arrows are upper limits; the continuous lines are the optical spectra.
Open with DEXTER

	Fig. 13 Spectral energy distributions of the sources in the present sample. Data are corrected for the Galactic absorption. Points refer to detections; arrows are upper limits; the continuous lines are the optical spectra.
Open with DEXTER

© ESO, 2015

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