Narrow-line Seyfert 1 galaxies (NLS1s) are active galactic nuclei (AGN) recently identified as a new class of $\gamma$-ray sources. The high energy emission is explained by the presence of a relativistic jet observed at small angles, just like in the case of blazars. When the latter are observed at larger angles they appear as radio-galaxies, but an analogue parent population for beamed NLS1s has not yet been determined. In this work we analyze this problem by studying the physical properties of three different samples of parent sources candidates: steep-spectrum radio-loud NLS1s, radio-quiet NLS1s, and disk-hosted radio-galaxies, along with compact steep-spectrum sources. In our approach, we first derived black hole mass and Eddington ratio from the optical spectra, then we investigated the interaction between the jet and the narrow-line region from the [O III] $\lambda\lambda$4959,5007 lines. Finally, the radio luminosity function allowed us to compare their jet luminosity and hence determine the relations between the samples.

M. Berton L. Foschini S. Ciroi A. Caccianiga B. M. Peterson S. Mathur M. L. Lister J. L. Richards E. Congiu V. Cracco F. Di Mille M. Frezzato G. La Mura P. Rafanelli

In this paper we describe the global on-sky calibration strategy of the LSPE-Strip instrument. Strip is a microwave telescope operating in the Q- and W-bands (central frequencies of 43 and 95 GHz respectively) from the Observatorio del Teide in Tenerife, with the goal to observe and characterise the polarised Galactic foreground emission, and complement the observations of the polarisation of the cosmic microwave background to be performed by the LSPE-SWIPE instrument and other similar experiments operating at higher frequencies to target the detection of the B-mode signal from the inflationary epoch of the Universe. Starting from basic assumptions on some of the instrument parameters (NET, 1/f noise knee frequency, beam properties, observing efficiency) we perform realistic simulations to study the level of accuracy that can be achieved through observations of bright celestial calibrators in the Strip footprint (sky fraction of 30 %) on the determination and characterisation of the main instrument parameters: global and relative gain factors (in intensity and in polarisation), polarisation direction, polarisation efficiency, leakage from intensity to polarisation, beams, window functions and pointing model.

R. T. Génova-Santos M. Bersanelli C. Franceschet M. Gervasi C. López-Caraballo L. Mandelli M. Maris A. Mennella J. A. Rubiño-Martín F. Villa M. Zannoni C. Baccigalupi B. Caccianiga L. Colombo F. Cuttaia F. Farsian G. Morgante S. Paradiso G. Polenta S. Ricciardi M. Sandri A. Taylor L. Terenzi M. Tomasi

We detected the seasonal modulation of the $^7$Be neutrino interaction rate with the Borexino detector at the Laboratori Nazionali del Gran Sasso in Italy. The period, amplitude, and phase of the observed time evolution of the signal are consistent with its solar origin, and the absence of an annual modulation is rejected at 99.99\% C.L. The data are analyzed using three methods: the sinusoidal fit, the Lomb-Scargle and the Empirical Mode Decomposition techniques, which all yield results in excellent agreement.

M. Agostini K. Altenmuller S. Appel V. Atroshchenko D. Basilico G. Bellini J. Benziger D. Bick G. Bonfini L. Borodikhina D. Bravo B. Caccianiga F. Calaprice A. Caminata S. Caprioli M. Carlini P. Cavalcante A. Chepurnov K. Choi D. D'Angelo S. Davini A. Derbin X. F. Ding L. Di Noto I. Drachnev K. Fomenko D. Franco F. Froborg F. Gabriele C. Galbiati C. Ghiano M. Giammarchi M. Goeger-Neff A. Goretti M. Gromov C. Hagner T. Houdy E. Hungerford Aldo Ianni Andrea Ianni A. Jany D. Jeschke V. Kobychev D. Korablev G. Korga D. Kryn M. Laubenstein B. Lehnert E. Litvinovich F. Lombardi P. Lombardi L. Ludhova G. Lukyanchenko I. Machulin S. Manecki G. Manuzio S. Marcocci J. Martyn E. Meroni M. Meyer L. Miramonti M. Misiaszek M. Montuschi V. Muratova B. Neumair L. Oberauer B. Opitz F. Ortica M. Pallavicini L. Papp A. Pocar G. Ranucci A. Razeto A. Re A. Romani R. Roncin N. Rossi S. Schonert D. Semenov P. Shakina M. Skorokhvatov O. Smirnov A. Sotnikov L. F. F. Stokes Y. Suvorov R. Tartaglia G. Testera J. Thurn M. Toropova E. Unzhakov A. Vishneva R. B. Vogelaar F. von Feilitzsch H. Wang S. Weinz M. Wojcik M. Wurm Z. Yokley O. Zaimidoroga S. Zavatarelli K. Zuber G. Zuzel

The main physical results on the registration of solar neutrinos and the search for rare processes obtained by the Borexino collaboration to date are presented.

A. Derbin V. Muratova M. Agostini K. Altenmuller S. Appel G. Bellini J. Benziger D. Bick G. Bonfini D. Bravo B. Caccianiga F. Calaprice A. Caminata M. Carlini P. Cavalcante A. Chepurnov D. D'Angelo S. Davini L. Di Noto I. Drachnev A. Etenko K. Fomenko A. Formozov D. Franco F. Gabriele C. Galbiati C. Ghiano M. Giammarchi M. Goeger-Neff A. Goretti M. Gromov C. Hagner E. Hungerford Aldo Ianni Andrea Ianni K. Jedrzejczak D. Jeschke M. Kaiser V. Kobychev D. Korablev G. Korga D. Kryn M. Laubenstein B. Lehnert E. Litvinovich F. Lombardi P. Lombardi L. Ludhova G. Lukyanchenko I. Machulin S. Manecki W. Maneschg S. Marcocci E. Meroni M. Meyer L. Miramonti M. Misiaszek M. Montuschi P. Mosteiro B Neumair L. Oberauer M. Obolensky F. Ortica M. Pallavicini L. Papp L. Perasso A. Pocar G. Ranucci A. Razeto A. Re A. Romani R. Roncin N. Rossi S. Schonert D. Semenov H. Simgen M. Skorokhvatov O. Smirnov A. Sotnikov S. Sukhotin Y. Suvorov R. Tartaglia G. Testera J. Thurn M. Toropova E. Unzhakov A. Vishneva R. B. Vogelaar F. von Feilitzsch H. Wang S. Weinz J. Winter M. Wojcik M. Wurm Z. Yokley O. Zaimidoroga S. Zavatarelli K. Zuber G. Zuzel

Borexino is a liquid scintillation detector located deep underground at the Laboratori Nazionali del Gran Sasso (LNGS, Italy). Thanks to the unmatched radio-purity of the scintillator, and to the well understood detector response at low energy, a new limit on the stability of the electron for decay into a neutrino and a single mono-energetic photon was obtained. This new bound, tau > 6.6 10**28 yr at 90 % C.L., is two orders of magnitude better than the previous limit.

Borexino Collaboration M. Agostini S. Appel G. Bellini J. Benziger D. Bick G. Bonfini D. Bravo B. Caccianiga F. Calaprice A. Caminata P. Cavalcante A. Chepurnov D. D'Angelo S. Davini A. Derbin L. Di Noto I. Drachnev A. Empl A. Etenko K. Fomenko D. Franco F. Gabriele C. Galbiati C. Ghiano M. Giammarchi M. Goeger-Neff A. Goretti M. Gromov C. Hagner E. Hungerford Aldo Ianni Andrea Ianni K. Jedrzejczak M. Kaiser V. Kobychev D. Korablev G. Korga D. Kryn M. Laubenstein B. Lehnert E. Litvinovich F. Lombardi P. Lombardi L. Ludhova G. Lukyanchenko I. Machulin S. Manecki W. Maneschg S. Marcocci E. Meroni M. Meyer L. Miramonti M. Misiaszek M. Montuschi P. Mosteiro V. Muratova B. Neumair L. Oberauer M. Obolensky F. Ortica K. Otis M. Pallavicini L. Papp L. Perasso A. Pocar G. Ranucci A. Razeto A. Re A. Romani R. Roncin N. Rossi S. Schoenert D. Semenov H. Simgen M. Skorokhvatov O. Smirnov A. Sotnikov S. Sukhotin Y. Suvorov R. Tartaglia G. Testera J. Thurn M. Toropova E. Unzhakov A. Vishneva R. B. Vogelaar F. von Feilitzsch H. Wang S. Weinz J. Winter M. Wojcik M. Wurm Z. Yokley O. Zaimidoroga S. Zavatarelli K. Zuber G. Zuzel

If heavy neutrinos with mass $m_{\nu_{H}}\geq$2$ m_e $ are produced in the Sun via the decay ${^8\rm{B}} \rightarrow {^8\rm{Be}} + e^+ + \nu_H$ in a side branch of pp-chain, they would undergo the observable decay into an electron, a positron and a light neutrino $\nu_{H}\rightarrow\nu_{L}+e^++e^-$. In the present work Borexino data are used to set a bound on the existence of such decays. We constrain the mixing of a heavy neutrino with mass 1.5 MeV $\leq m_{\nu_{H}} \le$ 14 MeV to be $|U_{eH}|^2\leq (10^{-3}-4\times10^{-6})$ respectively. These are tighter limits on the mixing parameters than obtained in previous experiments at nuclear reactors and accelerators.

Borexino collaboration G. Bellini J. Benziger D. Bick G. Bonfini D. Bravo M. Buizza Avanzini B. Caccianiga L. Cadonati F. Calaprice P. Cavalcante A. Chavarria A. Chepurnov D. DAngelo S. Davini A. Derbin I. Drachnev A. Empl A. Etenko K. Fomenko D. Franco C. Galbiati S. Gazzana C. Ghiano M. Giammarchi M. Goger-Neff A. Goretti L. Grandi C. Hagner E. Hungerford Aldo Ianni Andrea Ianni V. Kobychev D. Korablev G. Korga D. Kryn M. Laubenstein T. Lewke E. Litvinovich B. Loer F. Lombardi P. Lombardi L. Ludhova G. Lukyanchenko I. Machulin S. Manecki W. Maneschg G. Manuzio Q. Meindl E. Meroni L. Miramonti M. Misiaszek P. Mosteiro V. Muratova L. Oberauer M. Obolensky F. Ortica K. Otis M. Pallavicini L. Papp L. Perasso S. Perasso A. Pocar G. Ranucci A. Razeto A. Re A. Romani N. Rossi R. Saldanha C. Salvo S. Schonert H. Simgen M. Skorokhvatov O. Smirnov A. Sotnikov S. Sukhotin Y. Suvorov R. Tartaglia G. Testera D. Vignaud R. B. Vogelaar F. von Feilitzsch J. Winter M. Wojcik A. Wright M. Wurm J. Xu O. Zaimidoroga S. Zavatarelli G. Zuzel

Nuclear reactors are a source of electron antineutrinos due to the presence of unstable fission products that undergo $\beta^-$ decay. They will be exploited by the JUNO experiment to determine the neutrino mass ordering and to get very precise measurements of the neutrino oscillation parameters. This requires the reactor antineutrino spectrum to be characterized as precisely as possible both through high resolution measurements, as foreseen by the TAO experiment, and detailed simulation models. In this paper we present a benchmark analysis utilizing Serpent Monte Carlo simulations in comparison with real pressurized water reactor spent fuel data. Our objective is to study the accuracy of fission fraction predictions as a function of different reactor simulation approximations. Then, utilizing the BetaShape software, we construct fissile antineutrino spectra using the summation method, thereby assessing the influence of simulation uncertainties on reactor antineutrino spectrum.

A. Barresi M. Borghesi A. Cammi D. Chiesa L. Loi M. Nastasi E. Previtali M. Sisti S. Aiello G. Andronico V. Antonelli D. Basilico M. Beretta A. Bergnoli A. Brigatti R. Brugnera R. Bruno A. Budano B. Caccianiga V. Cerrone R. Caruso C. Clementi S. Dusini A. Fabbri G. Felici F. Ferraro A. Garfagnini M. G. Giammarchi N. Giugice A. Gavrikov M. Grassi R. M. Guizzetti N. Guardone B. Jelmini C. Landini I. Lippi S. Loffredo P. Lombardi C. Lombardo F. Mantovani S. M. Mari A. Martini L. Miramonti M. Montuschi D. Orestano F. Ortica A. Paoloni E. Percalli F. Petrucci G. Ranucci A. C. Re M. Redchuck B. Ricci A. Romani P. Saggese G. Sava A. Serafini C. Sirignano L. Stanco E. Stanescu Farilla V. Strati M. D. C. Torri A. Triossi C. Tuvè C. Venettacci G. Verde L. Votano

This paper presents a new complete and well defined sample of Flat Spectrum Radio Sources (FSRS) selected from the CLASS survey with the further constraint of a bright (mag<17.5) optical counterpart. The sample has been designed to produce a large number of low-luminosity blazars in order to test the current unifying models in the low luminosity regime. In this first paper the new sample is presented and the radio properties of the 325 sources contained therein discussed.

M. J. M. Marcha A. Caccianiga I. W. A. Browne N. Jackson

We have studied the relationship between the AGN radio-loudness and the mass of the central black-hole by using the ~190 type 1 AGN selected in the XMM-Newton Bright Survey (XBS). We find that radio-loud AGNs are much more frequent at high black-hole masses being a factor ~10 times more common for masses >10^9 Msun when compared to masses between 10^7-10^9 Msun.

A. Caccianiga P. Severgnini R. Della Ceca A. Corral E. Marchese

In this paper we discuss the latest developments of the STRIP instrument of the "Large Scale Polarization Explorer" (LSPE) experiment. LSPE is a novel project that combines ground-based (STRIP) and balloon-borne (SWIPE) polarization measurements of the microwave sky on large angular scales to attempt a detection of the "B-modes" of the Cosmic Microwave Background polarization. STRIP will observe approximately 25% of the Northern sky from the "Observatorio del Teide" in Tenerife, using an array of forty-nine coherent polarimeters at 43 GHz, coupled to a 1.5 m fully rotating crossed-Dragone telescope. A second frequency channel with six-elements at 95 GHz will be exploited as an atmospheric monitor. At present, most of the hardware of the STRIP instrument has been developed and tested at sub-system level. System-level characterization, starting in July 2018, will lead STRIP to be shipped and installed at the observation site within the end of the year. The on-site verification and calibration of the whole instrument will prepare STRIP for a 2-years campaign for the observation of the CMB polarization.

C. Franceschet S. Realini A. Mennella G. Addamo A. Baù P. M. Battaglia M. Bersanelli B. Caccianiga S. Caprioli F. Cavaliere K. A. Cleary F. Cuttaia F. Del Torto V. Fafone Z. Farooqui R. T. Génova Santos T. C. Gaier M. Gervasi T. Ghigna F. Incardona S. Iovenitti M. Jones P. Kangaslahti R. Mainini D. Maino M. Maris P. Mena R. Molina G. Morgante A. Passerini M. Perez-de-Taoro O. A. Peverini F. Pezzotta C. Pincella N. Reyes A. Rocchi J. A. Rubiño-Martín M. Sandri S. Sartor M. Soria V. Tapia L. Terenzi M. Tomasi E. Tommasi D. M. Viganó F. Villa G. Virone A. Volpe B. Watkins A. Zacchei M. Zannoni