Simultaneous multifrequency observations of blazars

Among active galactic nuclei, blazars have the most highly and rapidly variable spectral continua at all the wavelengths. Their repeated observation at different energies allows therefore to investigate the geometry and the physics of the emitting regions, provided the multifrequency data are monitored simultaneously and with complete and frequent sampling, to allow a reliable correlation analysis of the light curves at different wavelengths. The coordinated efforts of several international astronomical groups toward multifrequency monitoring implementation allowed to obtain unprecedentedly high quality data and to achieve substantial improvement in the theoretical understanding of the blazars PKS 2155–304 and 3C 279

Simultaneous multifrequency observations of blazars

Among active galactic nuclei, blazars have the most highly and rapidly variable spectral continua at all the wavelengths. Their repeated observation at different energies allows therefore to investigate the geometry and the physics of the emitting regions, provided the multifrequency data are monitored simultaneously and with complete and frequent sampling, to allow a reliable correlation analysis of the light curves at different wavelengths. The coordinated efforts of several international astronomical groups toward multifrequency monitoring implementation allowed to obtain unprecedentedly high quality data and to achieve substantial improvement in the theoretical understanding of the blazars PKS 2155–304 and 3C 279

On the July 2007 flare of the blazar 3C 454.3

In July 2007, the blazar 3C 454.3 underwent a flare in the optical, reaching R~13 on July 19. Then the optical flux decreased by one magnitude, being R~14 when the source was detected by the gamma-ray satellite AGILE, that observed the source on July 24-30. At the same time, the Swift satellite performed a series of snapshots. We can construct the simultaneous spectral energy distribution using optical, UV, X-ray and gamma-ray data. These shows that an increased gamma-ray flux is accompanied by a weaker optical/X-ray flux with respect to the flare observed in the Spring 2005 by INTEGRAL and Swift. This confirms earlier suggestions about the behaviour of the jet of 3C 454.3.Comment: 5 pages, 3 figures, MNRAS (Letters) in press (minor revision

The Near-IR-Optical-UV Emission of BL Lacertae Objects

Near--infrared, optical and ultraviolet quasi--simultaneous observations of 11 BL Lacertae objects are reported. For all but one source the dereddened spectral flux distribution in the $8\cdot10^{13}-2\cdot10^{15}$ Hz frequency range can be described by a single power law f$_\nu \propto \nu^{-\alpha}$ with average spectral index $$ = 0.88 $\pm$ 0.42 (standard deviation) plus, where relevant, the contribution of the host galaxy. In most cases the non simultaneous soft X--ray fluxes obtained by the {\it Einstein Observatory} lie on or below the extrapolation of the power law. The results are compared with the average spectral properties of other samples of BL Lacs studied separately in the IR--optical and in the UV bands. The implications for existing models of the objects are shortly discussed.Comment: 23 pages, latex file, 2 figures available as postscript files appended at the end of the latex text file, Ref. S.I.S.S.A. 31/94/

Abundance stratification in Type Ia supernovae - V. SN 1986G bridging the gap between normal and subluminous SNe Ia

A detailed spectroscopic analysis of SN 1986G has been performed. SN 1986G `bridges the gap' between normal and sub luminous type Ia supernova (SNe Ia). The abundance tomography technique is used to determine the abundance distribution of the elements in the ejecta. SN 1986G was found to be a low energy Chandrasekhar mass explosion. Its kinetic energy was 70% of the standard W7 model (0.9x10$^{51}$erg). Oxygen dominates the ejecta from the outermost layers down to $\sim$9000kms$^{-1}$ , intermediate mass elements (IME) dominate from $\sim$ 9000kms$^{-1}$ to $\sim$ 3500kms$^{-1}$ with Ni and Fe dominating the inner layers $<\sim$ 3500kms$^{-1}$. The final masses of the main elements in the ejecta were found to be, O=0.33M, IME=0.69M, stable NSE=0.21M, $^{56}$Ni=0.14M. An upper limit of the carbon mass is set at C=0.02M. The spectra of SN1986G consist of almost exclusively singly ionised species. SN1986G can be thought of as a low luminosity extension of the main population of SN Ia, with a large deflagration phase that produced more IMEs than a standard SN Ia.Comment: Accepted for publication in MNRAS, update