Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; quantum space; expansion of the universe; dark energy; thermodynamics; dark matter; plasma; recombination; vacuum energy; Cosmological Constant; Quintessence; spaceons
Online: 18 August 2017 (04:51:40 CEST)
|
|
|
Share this article with
×
We present a model of space that considers it to be a quantized dynamical entity which is a component of the universe along with matter and radiation. The theory is used together with thermodynamic data to provide a new view of cosmic evolution and an insight into the nature of dark energy and dark matter.
Space is made up of energy quanta. The universe started from an atomic size volume at very high temperature and pressure near the Planck epoch. Upon expansion and cooling, phase transitions occurred resulting in the formation of radiation, fundamental particles, and matter. These nucleate and grow into stars, galaxies, and clusters. From a phase diagram of cosmic composition, we obtained a correlation between dark energy and the energy of space. Using the Friedmann equations, data from WMAP studies of the composition of the universe at 3.0 x 105 (a=5.25 x 10-2) years and at present (a=1), are well fitted by our model with an equation of state parameter, w= -0.7. The accelerated expansion of the universe, starting at about 7 billion years, determined by BOSS measurements, also correlates well with the dominance of dark energy at 7.25 x 109 years ( a= 0.65). The expansion can be attributed to Quintessence with a space force arising from a quantum space field. From our phase diagram, we also find a correlation suggesting that dark matter is a plasma form of matter similar to that which existed during the photon epoch immediately prior to recombination.
Our Quantum Space Model leads to a universe which is homogeneous and isotropic without the need for inflation. The thermodynamics of expansion is consistent with BOSS data that show the process to be adiabatic and the rate of expansion decelerating during the first 6 billion years after the Big Bang. However, it became non-adiabatic and accelerating thereafter. This implies an influx of energy from a source outside the universe; it warrants consideration as a possible factor in the accelerated expansion of the universe.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; gravitational waves; cosmology; dark energy; inflation
Online: 16 August 2017 (18:46:56 CEST)
|
|
Share this article with
×
In this three-part paper, we show that gravitational waves (classical and quantum) produce the accelerated de Sitter expansion at the start and by the end of the cosmological evolution of the Universe. In these periods of time, the Universe contains no matter fields but contains classical and quantum metric fluctuations, i.e. it is filled with classical gravitational waves and gravitons. In such gravitational wave and graviton dominated eras of evolution of the Universe, the de Sitter state is the exact solution to the self-consistent equations for gravitational waves and gravitons and background geometry for the empty (with no matter fields) space-time with FLRW metric. In both classical and quantum cases, this solution is of the instanton origin since it is obtained by Wick rotation with the subsequent analytic continuation to real time. The cosmological acceleration from gravitational waves and gravitons provides a transparent physical explanation to the coincidence and threshold paradoxes of dark energy avoiding recourse to the anthropic principle. The cosmological acceleration from gravitons/gravitational waves at the start of the Universe evolution produces inflation which is consistent with the observational data on CMB anisotropy.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; entropic gravity; Cosmological Constant; quantum gravity; dark matter
Online: 11 August 2017 (08:06:06 CEST)
|
|
Share this article with
×
It is shown that Verlinde’s hypothetical concepts of entropic gravity can be successfully applied to the author’s previous work on the modification of the Newtonian gravity by Einstein’s Cosmological Constant. It allows an assessment by theory for Milgrom’s empirical acceleration constant, thereby revealing some fundamental differences with Verlinde’s conclusions.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; Cosmological Constant; MOND; dark matter; antigravity
Online: 9 August 2017 (06:18:26 CEST)
|
|
Share this article with
×
By solving the weak field limit of Einstein’s Field Equation including the Cosmological Constant, under the constraint of spherical isotropy, it is shown that, at large cosmological distance, the gravitational force exceeds the one that is predicted by Newton’s gravity law, such that it corresponds with Milgrom’s MOND hypothesis. However, the resulting prediction that, at extremely large distances, gravity with some spatial periodicity turns on-and-off into antigravity marks a decisive difference.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; cosmology; dark energy; dark matter; cosmological constant problem
Online: 12 June 2017 (06:16:52 CEST)
|
|
Share this article with
×
We are encouraged to look beyond ɅCDM as there are no satisfactory explanations for either dark energy or dark matter. A data centred phenomenological approach supports an explanation where dark energy is Holographic Dark Information Energy, HDIE. HDIE explains many effects attributed separately to Ʌ and CDM. HDIE mimics Ʌ with sufficient energy and an equation of state parameter, w= -1.03±0.05 at redshifts z<1.35 to account for accelerating expansion. HDIE is clumped around galaxies at densities that distort space-time, explaining many CDM attributed effects. The present ratio of HDIE/baryons ~2.15, required for the observed expansion history, is equivalent to a dark matter fraction ~68%, consistent with many galaxies. The HDIE/baryon model is based largely on proven physics, provides a common explanation for dark energy and dark matter, and solves the cosmological coincidence problem. At earlier times, z > ~1.35, HDIE was phantom, w = -1.82±0.08, enabling the model to be falsified. HDIE fits Planck dark energy wo-wa plots at least as well as Ʌ, and is consistent with other results that suggest dark energy was phantom at earlier times. A new w-parameterisation is proposed, as the usual CPL parameterisation is biased and unsuitable for distinguishing between HDIE/baryon and ɅCDM models.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; entropic gravity; Lagrange formalism; phase-field models; gradient-entropy; constraints; maximum entropy principle; curvature of space; conservation laws; Modified Newtonian Dynamics; MOND
Online: 17 March 2017 (05:16:12 CET)
|
|
Share this article with
×
Terms related to gradients of scalar fields are introduced as scalar products into the formulation of entropy. A Lagrange density is then formulated by adding constraints based on known conservation laws. Applying the Lagrange formalism to the resulting Lagrange density leads to the Poisson equation of gravitation and also includes terms being related to curvature of space. The formalism further leads to terms possibly explaining nonlinear extensions known from modified Newtonian dynamics approaches. The article concludes with a short discussion of the presented methodology and provides an outlook on other phenomena, which might be tackled using this new approach.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; foundations of science; cosmology: observations; cosmology: theory; galaxies: kinematics and dynamics; inertia; MoND
Online: 16 March 2017 (09:31:27 CET)
|
|
Share this article with
×
First, this paper broaches the epistemological status of scientific tenets and approaches: phenomenological (descriptive only), well-founded (solid first principles, conducive to deep understanding), provisional (can be falsified if universal and verified if existential), and imaginary (fictitious entities or processes, conducive to empirically unsupported beliefs). The ΛCDM “concordance model” involves such beliefs: the emanation of the universe out of a non-physical stage, cosmic inflation (invented ad hoc), Λ (fictitious energy), and exotic dark matter. Big Bang cosmology further faces conceptual and pragmatic problems in delimiting what expands from what does not. The problems dissolve after untying inertia from space. The cosmology that emerges appears immediately compatible with the considered observations and the ‘perfect cosmological principle’. Waves and field perturbations that propagate at c expand exponentially with distance (a gravitational effect). The cosmic web of galaxies does not. Potential -Φ varies as H/(cz) instead of 1/r. Inertial forces arise from the gravitational action of the rest of the universe. Due to dilatation, they are reduced disproportionately at low accelerations. A cut-off value a0 = 0.168 cH is deduced. This explains the successful description of galaxy rotation curves by MoND. A fully elaborated physical theory is still pending. Wider implications are briefly discussed.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; active galaxies; blazars; jets; radio continuum; gamma-rays; time-series analysis; Bayesian modelling; Gaussian processes
Online: 1 March 2017 (12:56:13 CET)
|
|
Share this article with
×
This article shortly introduces Gaussian processes as a new approach for modelling time series in the field of blazar physics. In the second part of the paper, recent results from an application of GP modelling to the multi-wavelength light curves of the blazar PKS 1502+106 are discussed.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; Cosmology; Observational cosmology; Origin, formation, and abundances of the elements; dark matter; dark energy; superclusters; large-scale structure of the Universe
Online: 1 February 2017 (16:06:52 CET)
|
|
|
Share this article with
×
The main foundations of the standard $\Lambda $CDM model of cosmology are that: 1) The redshifts of the galaxies are due to the expansion of the Universe plus peculiar motions; 2) The cosmic microwave background radiation and its anisotropies derive from the high energy primordial Universe when matter and radiation became decoupled; 3) The abundance pattern of the light elements is explained in terms of primordial nucleosynthesis; and 4) The formation and evolution of galaxies can be explained only in terms of gravitation within a inflation+dark matter+dark energy scenario. Numerous tests have been carried out on these ideas and, although the standard model works pretty well in fitting many observations, there are also many data that present apparent caveats to be understood with it. In this paper, I offer a review of these tests and problems, as well as some examples of alternative models.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; galaxies; clusters; general; methods N-body simulations; cosmology; theory
Online: 9 December 2016 (16:38:17 CET)
|
|
Share this article with
×
We explore the possibility of using the external regions of galaxy clusters to measure their mass accretion rate (MAR). The main goal is to provide a method to observationally investigate the growth of structures on the nonlinear scales of galaxy clusters. We derive the MAR by using the mass profile beyond the splashback radius, evaluating the mass of a spherical shell and the time it takes to fall in. The infall velocity of the shell is extracted from N-body simulations. The average MAR returned by our prescription in the redshift range z=[0, 2] is within 20-40% of the average MAR derived from the merger trees of dark matter haloes in the reference N-body simulations. Our result suggests that the external regions of galaxy clusters can be used to measure the mean MAR of a sample of clusters.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; dark matter; THINGS; MOND; metric skew-tensor gravity; scalar-tensor-vector gravity; CMB angular power spectrum
Online: 16 November 2016 (09:39:24 CET)
|
|
Share this article with
×
Since general relativity (GR) has already established that matter can simultaneously have two different values of mass depending on its context, we argue that the missing mass attributed to non-baryonic dark matter (DM) actually obtains because there are two different values of mass for the baryonic matter involved. The globally obtained "dynamical mass'' of baryonic matter can be understood as a small perturbation to a background spacetime metric even though it's much larger than the locally obtained "proper mass". Having successfully fit the SCP Union2.1 SN Ia data without accelerating expansion or a cosmological constant, we employ the same ansatz to compute dynamical mass from proper mass and explain galactic rotation curves (THINGS data), the mass profiles of X-ray clusters (ROSAT and ASCA data) and the angular power spectrum of the cosmic microwave background (Planck 2015 data) without DM. We compare our fits to modified Newtonian dynamics (MOND), metric skew-tensor gravity (MSTG) and scalar-tensor-vector gravity (STVG) for each data set, respectively, since these modified gravity programs are known to generate good fits to these data. Overall, we find our fits to be comparable to those of MOND, MSTG and STVG. While this favorable comparison does not establish the validity of our proposition, it does provide confidence in using the fits to pursue an underlying action. Indeed, the functional form of our ansatz reveals an interesting structure in these fits.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; big bang; planck scale Hubble parameter; quantum cosmology; Mach’s principle; holographic principle; observational cosmology; super luminal expansion speed; super luminal rotation speed; dark energy; cosmic rotational kinetic energy; cosmic microwave back
Online: 8 October 2016 (10:26:06 CEST)
|
|
Share this article with
×
With reference to Planck scale Hubble parameter, super luminal expansion speeds, super luminal rotation speeds, Mach’s principle and Holographic principle, we review the current cosmological observations with eight simple assumptions. By understanding Yuri N. Obukhov and V.A. Korotky proposed cosmic rotational effects of polarization of radiation due to massive bodies, to some extent cosmic rotation can be deep-rooted in an observational approach and the ratio of current angular velocity and Hubble parameter can be estimated. It is possible to show that, at H0 =70 km/sec/Mpc, current cosmic temperature, age, radius, mass, mass density are 2.721 K, 4.41x1017 sec, 90 billion light years, 1.14654x1054 kg, 0.0482 times the current critical density respectively. Clearly speaking, current universe seems to constitute 267 Hubble spheres. Important point to be noted is that, current rotational kinetic energy is 0.6667 times the current critical energy. Based on the estimated current mass density and current rotational kinetic energy, current cosmic dark matter density can be shown to be 0.2851 times the current critical density. These numerical coincidences cast serious doubt on the on the real existence of currently believed ‘dark energy’. Initial and current expansion speeds are 3x108 m/sec and 3.56x109 m/sec respectively. With increasing cosmic age and increasing cosmic expansion speed, current universe is expanding with a speed of 11.885c. By knowing the time to time future cosmic temperatures, future Hubble parameters and corresponding future cosmic expansion speeds can be estimated and thus future expansion speed can be understood. Starting from ‘speed of light’, our model assumes a continuous increase in expansion speed and attains a current radius of 90 billion light years (without inflationary concepts) and casts a serious doubt on the actuality of currently believed ‘inflation’.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; Galaxy clusters; cosmic rays; magnetic fields; turbulence
Online: 30 August 2016 (08:53:32 CEST)
|
|
Share this article with
×
1) Background: the budget of non-thermal energy in galaxy clusters is not well constrained, owing to the observational and theoretical difficulties in studying these diluted plasmas on large scales. 2) Method: we use recent cosmological simulations with complex physics in order to connect the emergence of non-thermal energy to the underlying evolution of gas and dark matter. 3) Results: the impact of non-thermal energy (e.g. cosmic rays, magnetic fields and turbulent motions) is found to increase in the outer region of galaxy clusters. Within numerical and theoretical uncertainties, turbulent motions dominate the budget of non-thermal energy in most of the cosmic volume. 4) Conclusion: assessing the distribution non-thermal energy in galaxy clusters is crucial to perform high-precision cosmology in the future. Constraining the level of non-thermal energy in cluster outskirts will improve our understanding of the acceleration of relativistic particles by cosmic shocks and of the origin of extragalactic magnetic fields.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; Distant Retrograde Orbit; DRO; orbits–stability; radiation pressure; orbits–resonance; dynamics
Online: 1 August 2016 (09:00:06 CEST)
|
|
Share this article with
×
Distant Retrograde Orbits in the Earth-Moon system are gaining in popularity as stable `parking' orbits for various conceptual missions. To investigate the stability of potential Distant Retrograde Orbits, simulations were executed, with propagation running over a thirty-year period. Initial conditions for the vehicle state were limited such that the position and velocity vectors were in the Earth-Moon orbital plane, with the velocity oriented such that it would produce retrograde motion about Moon. The resulting trajectories were investigated for stability against the eccentric relative orbits of Earth and Moon in an environment that also included gravitational perturbations from Sun, Jupiter, and Venus, and the effects of radiation pressure. The results appear to indicate that stability is enhanced for certain resonant states within the Earth-Moon system.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; VLBI; Space-VLBI; Correlation; RadioAstron; AGN
Online: 19 July 2016 (04:54:57 CEST)
|
|
Share this article with
×
DiFX is a software VLBI correlator currently adopted by several main correlation sites around the globe. After the launch of the RadioAstron Space-VLBI mission in 2011, an extension was necessary to handle processing of an orbiting antenna, to be correlated with supporting ground arrays. We present here a branch of the main DiFX distribution (2.4), recently uploaded on the publicly available repository, that MPIfR developed to process data of the three AGN-imaging RadioAstron key science projects. It can account for general relativistic correction of an orbiting antenna with variable position/velocity, providing a routine to covert the native RDF format to the more common M5B one. Also, a fringe-finding algorithm able to manage arbitrary large fringe-search window is included, allowing one to increase the search space normally adopted by common software packages like HOPS.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; Gravitational collapse; Oppenheimer-Snyder; horizonless solutions; neutron stars
Online: 19 July 2016 (04:53:26 CEST)
|
|
Share this article with
×
This article argues that there is a consistent description of gravitationally collapsed bodies, including neutron stars above the Tolman-Oppenheimer-Volkoff mass and also supermassive galactic centres, according to which collapse stops before the object reaches its gravitational radius, the density reaching a maximum close to the surface and then decreasing towards the centre. Models for such shell-like objects have been constructed using classic formulations found in the 1939 articles of Oppenheimer-Volkoff and Oppenheimer-Snyder. It was possible to modify the conclusions of the first article by changing the authors’ boundary conditions at r = 0. In the second case we find that the authors’ solution of the field equations needs no changes, but that the choice of their article’s title led many of their successors to believe that it supports the black-hole hypothesis. However, it is easily demonstrated that their final density distribution accords with the shell models found in our articles. Because black holes, according to many formulations, "have no hair", their thermodynamics is rather simple. The kind of collapsar which our models describe are more like main-sequence stars; they have spatiotemporal distributions of pressure, density and temperature, that is they have hair. In this article we shall concentrate on the dynamics of the Oppenheimer-Snyder collapsar; both pressure and temperature are everywhere zero, so there can be no thermodynamics. Only in the time independent case of Oppenheimer-Volkoff type models is it currently feasible to consider some thermodynamic implications; here some valuable new insights are obtained through the incorporation of the Oppenheimer-Snyder dynamics.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; AGN; polarimetry
Online: 18 July 2016 (10:54:35 CEST)
|
|
Share this article with
×
We present preliminary results of JVLA wideband full polarization observations of a sample of Active Galactic Nuclei (AGN) with very high Rotation Measure (RM) values, sign of extreme environment. The polarization properties show a complex behaviour with the polarization angle (PA) and the fractional polarization (fp) that dramatically change within the wideband. The measured RM is not constant within the wide band. Its complex behaviour reflects the complexity of the medium with the presence of several Faraday components. The depolarization have been studied, modeling the Stokes parameters Q and U together with the polarization parameters (PA and fp) with wavelength by applying combinations of the simplest existing depolarisation models. With this JVLA study we could spectrally resolve multiple polarized components of unresolved AGN. These preliminary results reveal the complexity of these objects, still improvements have to be done on the depolairzation modeling to better understand the polarization structure of these sources.
Preprint
|
|
|
S. Zola,
M. Valtonen,
G. Bhatta,
A. Goyal,
B. Debski,
A. Baran,
J. Krzesinski,
M. Siwak,
S. Ciprini,
A. Gopakumar,
H. Jermak,
K. Nilsson,
D. Reichart,
K. Matsumoto,
K. Sadakane,
K. Gazeas,
M. Kidger,
V. Piirola,
F. Alicavus,
K.S. Baliyan,
A. Berdyugin,
D. Boyd,
M. Campas Torrent,
F. Campos,
J. Carrillo Gomez,
D.B. Caton,
V. Chavushyan,
J. Dalessio,
D. Dimitrov,
M. Drozdz,
A. Erdem,
A. Escartin Perez,
V. Fallah Ramazani,
A.V. Filippenko,
F. Garcia,
F. Gomez Pinilla,
M. Gopinathan,
J.B. Haislip,
J. Harmanen,
G. Hurst,
K.M. Ivarsen,
M. Jelinek,
A. Joshi,
M. Kagitani,
N. Kaur,
N. Karaman,
W.C. Keel,
A.P. LaCluyze,
B.C. Lee,
E. Lindfors,
J. Lozano De Haro,
J.P. Moore,
R. Naves Nogues,
A.W. Neely,
R.H. Nelson,
W. Ogloza,
S. Okano,
J.C. Pandey,
M. Perri,
P. Pihajoki,
G. Poyner,
J. Provencal,
T. Pursimo,
A. Raj,
R. Reinthal,
S. Sadegi,
T. Sakanoi,
J.-L. Salto Gonzales,
T. Schweyer,
F.C. Soldan Alfaro,
E. Sonbas,
I. Steele,
J.T. Stocke,
J. Strobl,
L.O. Takalo,
T. Tomov,
L. Tremosa Espasa,
J.R. Valdes,
J. Valero Perez,
F. Verrecchia,
J.R. Webb,
M. Yoneda,
M. Zejmo,
W. Zheng,
J. Telting,
J. Saario,
T. Reynolds,
A. Kvammen,
E. Gafton,
R. Karjalainen,
P. Blay
Physical Sciences, Astronomy & Astrophysics; galaxies: active; BL Lacertae objects: individual (OJ 287); super massive black holes
Online: 18 July 2016 (10:46:26 CEST)
|
|
Share this article with
×
We analyse the light curve in the R-band gathered during the 2015/16 observing season of OJ287. We did a search for QPOs using several methods in wide time domain. No statistically significant periods were found in the high frequency domain both in the ground data and also in K2 observations. In the longer periods domain the Lomb-Scargle periodogram revealed several peaks above the 99\% significance level. The longest one, about 95-day, corresponds to the ISCO period of the more massive SMBH. The 43-day period could be an alias or can be attributed to accretion in the form of two armed spiral wave.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; galaxies:blazar; light curve; simulation
Online: 18 July 2016 (10:39:32 CEST)
|
|
Share this article with
×
Blazars show rapid and high amplitude variability. In this work , Fermi daily light curve of 130 sources are analyzed, distribution of daily variability are compared with each other by using Kolmogorov-Smirnov (K-S) test. results show: 1)Some pairs of the distributions are similar; 2) In most cases, the distributions are not Gaussian.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; galaxies:blazar; light curve; simulation
Online: 18 July 2016 (10:36:38 CEST)
|
|
Share this article with
×
In this work, we'll present the power spectra density, auto-correlation function, dentrended fluctuation analysis and multifractal spectrum are performed to the daily light curves of Blazars monitored by Fermi LAT. Some signs of power law are found.
Preprint
|
|
|
Marina Manganaro,
Giovanna Pedaletti,
Marlene Doert,
Denis Bastieri,
Vandad Fallah Ramazani,
Dario Gasparrini,
Elina Lindfors,
Benoit Lott,
Mireia Nievas,
Bindu Rani,
Emmanouil Angelakis,
George Borman,
Mark Gurwell,
Talvikki Hovatta,
Ryosuke Itoh,
Svetlana Jorstad,
Alex Kraus,
Thomas P Krichbaum,
Paul Kuin,
Anne Lahteenmaki,
Valeri Larionov,
Amy Yarleen Lien,
Ioannis Myserlis,
David J Thompson,
Merja Tornikoski,
J Anton Zensus
Physical Sciences, Astronomy & Astrophysics; BL-Lacertae objects: individual: S5 0716+714; Galaxies:active; gamma-rays: galaxies
Online: 18 July 2016 (06:02:42 CEST)
|
|
Share this article with
×
S5 0716+714 is a well known BL-Lac object, one of the brightest and most active blazars. The discovery in the Very High Energy band (VHE, E > 100 GeV) by MAGIC happened in 2008. In January 2015 the source went through the brightest optical state ever observed, triggering MAGIC follow-up and a VHE detection with ~ sigma significance (ATel #6999). Rich multi-wavelength coverage of the flare allowed us to construct the broad-band spectral energy distribution of S5 0716+714 during its brightest outburst. In this work we will present the preliminary analysis of MAGIC and Fermi-LAT data of the flaring activity in January and February 2015 for the HE and VHE band, together with radio (Metsahovi, OVRO, VLBA, Effelsberg), sub-millimeter (SMA), optical (Tuorla, Perkins, Steward, AZT-8+ST7, LX-200, Kanata), X-ray and UV (Swift-XRT and UVOT), in the same time-window and discuss the time variability of the MWL light curves during this impressive outburst.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; galaxies: nuclei; galaxies: jets; galaxies: Seyfert; gamma-rays: general
Online: 15 July 2016 (11:29:08 CEST)
|
|
Share this article with
×
The discovery by the Large Area Telescope on board Fermi of variable gamma-ray emission from radio-loud narrow-line Seyfert 1 (NLSy1) galaxies revealed the presence of a possible third class of AGN with relativistic jets in addition to blazars and radio galaxies. Considering that NLSy1 are usually hosted in spiral galaxies, this finding poses intriguing questions about the nature of these objects and the formation of relativistic jets. We report on a systematic investigation of the gamma-ray properties of a sample of radio-loud NLSy1, including the detection of new objects, using 7 years of Fermi-LAT data with the new Pass 8 event-level analysis. In addition we discuss the radio-to-very-high-energy properties of the gamma-ray emitting NLSy1, their host galaxy, and black hole mass in the context of the blazar scenario and the unification of relativistic jets at different scales.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; active galaxies; BL Lacertae object: BL Lac; jets; GMVA: high-resolution VLBI; magnetic field; polarization
Online: 15 July 2016 (10:06:48 CEST)
|
|
Share this article with
×
The high radio frequency polarization imaging of non-thermal emission from active galactic nuclei (AGN) is a direct way to probe the magnetic field strength and structure in the immediate vicinity of supermassive black holes (SMBHs) and is crucial in testing the jet-launching scenario. To explore the the magnetic field configuration at the base of jets in blazars, we took advantage of the full polarization capabilities of the GMVA (Global Millimeter VLBI Array). With an angular resolution of ~50 micro-arcseconds at 86 GHz, one could reach scales down to ~900 Schwarzschild radii (for a 10^9 solar mass black hole). We present here the preliminary results of our study on the blazar BL Lac. Our results imply that on sub-mas scales the core and central jet of BL Lac is significantly polarized with two distinct regions of polarized intensity. We also noted a great morphological similarity between the 7mm/3mm VLBI images at very similar angular resolution.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; galaxies: active; galaxies: jets; galaxies: nuclei
Online: 15 July 2016 (09:37:39 CEST)
|
|
Share this article with
×
In a recent paper, we calculate spectral energy distributions (SEDs) for 1425 Fermi blazars, classifications of low synchrotron peak sources (LSPs) if log $\nu_{\rm p} (\rm Hz) \leq $ 14.0, intermediate synchrotron peak sources (ISPs) if $14.0 < \,\log\, \nu_{\rm p} (\rm Hz) \leq 15.3 $, and high synchrotron peak sources (HSPs) if $ \log\, \nu_{\rm p} (\rm Hz) > 15.3$ are made based on 999 logarithms of synchrotron peak frequencies with known redshift, and we obtain an empirical relation to estimate the synchrotron peak frequency, $\nu_{\rm p}^{\rm Eq.}$ from effective spectral indexes $\alpha_{ox}\, {\rm and}\, \alpha_{ro}$ as $\log \nu_{\rm p}^{\rm Eq.} = 16+4.238X $ if $X < 0$, and $\log \nu_{\rm p}^{\rm Eq.} = 16+4.005Y $ if $X > 0$, where $X = 1.0 - 1.262 \alpha_{ro} - 0.623 \alpha_{ox}$, and $Y = 1.0 + 0.034 \alpha_{ro} - 0.978 \alpha_{ox}$ \cite{Fan16}. In the present work, we investigate the correlation between the peak frequency and the radio to X-ray spectral index, that between peak luminosity (integrated luminosity) and $\gamma$-ray/optical luminosity, and that between peak luminosity and integrated luminosity. Some discussions are presented.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; galaxies: active; gamma-rays: general; radiation mechanisms: non-thermal
Online: 15 July 2016 (04:40:29 CEST)
|
|
Share this article with
×
High redshift blazars are among the most powerful objects in the Universe. Although they represent a significant fraction of the extragalactic hard X-ray sky, they are not commonly detected in gamma-rays. High redshift (z>2) objects represent <10 per cent of the AGN population observed by Fermi so far, and gamma-ray flaring activity from these sources is even more uncommon. The characterization of the radio-to-gamma-ray properties of high redshift blazars represents a powerful tool for the study of the energetics of such extreme objects and the Extragalactic Background Light. This contribution will present results of multi-band campaigns, from radio to gamma-rays, on PKS 0836+710, PKS 2149-306, and TXS 0536+145. The latter is the highest redshift detection of a flaring gamma-ray blazar so far. At the peaks of their respective flares these sources reached an apparent isotropic gamma-ray luminosity of about 10^50 erg/s, which is comparable with the luminosity observed from the most powerful blazars. The physical properties derived from the multi-wavelength observations of these sources are then compared with those shown by the high redshift population.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; BL Lacertae objects: general, catalogues, gamma rays: galaxies, quasars: general, radiation mechanisms: non-thermal, radio continuum: galaxies
Online: 14 July 2016 (12:11:50 CEST)
|
|
Share this article with
×
Radio loud active galactic nuclei are composed of different spatial features, each one characterized by different spectral properties in the radio band. Among them, blazars are the most common class of sources detected at gamma-rays by \fermi, and their radio emission is dominated by the flat spectrum compact core. In this contribution, we explore the connection between emission at high energy revealed by \fermi\ and at radio frequency. Taking as a reference the strong and very highly significant correlation found between gamma rays and cm-$\lambda$ radio emission, we explore different behaviours found as we change the energy range in gamma rays and in radio, therefore changing the physical parameters of the zones involved in the radiation emission. We find that the correlation weakens when we consider (1) gamma rays of energy above 10 GeV (except for high synchrotron peaked blazars) or (2) low frequency radio data taken by the Murchison Widefield Array; on the other hand, the correlation strengthens when we consider mm-$\lambda$ data taken by ALMA.
Preprint
|
|
|
Kenichi Nishikawa,
Yosuke Mizuno,
Jacek Niemiec,
Oleh Kobzar,
Martin Pohl,
Jose Gomez,
Ioana Dutan,
Asaf Pe’er,
Jacob Frederiksen,
Aake Nordlund,
Athina Meli,
Helene Sol,
Phil Hardee,
Dieter Hartmann
Physical Sciences, Astronomy & Astrophysics; relativistic jets; particle-in-cell simulations; global jets; helical magnetic fields; kinetic instabilities; kink instability
Online: 13 July 2016 (05:37:49 CEST)
|
|
Share this article with
×
In the study of relativistic jets one of the key open questions is their interaction with the
environment on the microscopic level. Here, we study the initial evolution of both electron–proton
(e- - p+) and electron–positron (e±) relativistic jets containing helical magnetic fields, focusing on
their interaction with an ambient plasma. We have performed simulations of "global" jets containing
helical magnetic fields in order to examine how helical magnetic fields affect kinetic instabilities
such as the Weibel instability, the kinetic Kelvin-Helmholtz instability (kKHI) and the Mushroom
instability (MI). In our initial simulation study these kinetic instabilities are suppressed and new
types of instabilities can grow. In the e- - p+ jet simulation recollimation-like instability occurs and
jet electrons are strongly perturbed. In the e± jet simulation a recollimation-like instability occurs
at early times followed by a kinetic instability and the general structure is similar to a simulation
without helical magnetic field. Simulations using much larger systems are required in order to
thoroughly follow the evolution of global jets containing helical magnetic fields.
Preprint
|
|
|
Julian Sitarek,
Josefa Becerra González,
Sara Buson,
Dijana Dominis Prester,
Marina Manganaro,
Daniel Mazin,
Kari Nilsson,
Mireia Nievas,
Antonio Stamerra,
Fabrizio Tavecchio,
Ievgen Vovk
Physical Sciences, Astronomy & Astrophysics; Gamma rays: galaxies; Gravitational lensing: strong; Galaxies: jets; Radiation mechanisms: non-thermal; Galaxies: individual: QSO B0218+357
Online: 13 July 2016 (05:36:15 CEST)
|
|
Share this article with
×
QSO B0218+357 is a blazar located at a cosmological redshift of 0.944. The source is gravitationally lensed by a spiral galaxy located at the redshift of 0.68. Strong gravitational lensing splits the signals emitted by the source into two components separated by 10-12 days, as observed in radio and gamma-ray bands. In July 2014 a GeV flare was observed by Fermi-LAT, triggering follow-up observations with the MAGIC telescopes at energies above 100 GeV. The expected time delay between the components allowed us to plan broad band MWL observations before, during and after the trailing component of the emission. The MAGIC observations at the expected time of arrival of the trailing component resulted in the first detection of QSO B0218+357 in Very-High-Energy (VHE, >100 GeV) gamma rays. It is both the farthest known VHE object and one of only a few Flat Spectrum Radio Quasars detected in this energy range. We report here the observed multiwavelength spectral and temporal properties of the emission during the 2014 flare.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; galaxies: jets---Galaxy: center---techniques: high angular resolution---techniques: image processing---techniques: interferometric
Online: 12 July 2016 (09:41:39 CEST)
|
|
Share this article with
×
Originally developed to image the shadow region of the central black hole in Sagittarius A* and in the nearby galaxy M87, the Event Horizon Telescope (EHT) provides deep, very high angular resolution data on other AGN sources too. The challenges of working with EHT data have spurred the development of new image reconstruction algorithms. This work briefly reviews the status of the EHT and its utility for observing AGN sources, with emphasis on novel imaging techniques that offer the promise of better reconstructions at 1.3 mm and other wavelengths.
Preprint
|
|
|
Physical Sciences, Astronomy & Astrophysics; active galaxies; blazars; jets; polarization; shock acceleration
Online: 8 July 2016 (03:03:04 CEST)
|
|
Share this article with
×
Relativistic shocks are one of the most plausible sites of the emission of strongly variable, polarized multi-wavelength emission from relativistic jet sources such as blazars, via diffusive shock acceleration (DSA) of relativistic particles. This paper summarizes recent results on a self-consistent coupling of diffusive shock acceleration and radiation transfer in blazar jets. We demonstrate that the observed spectral energy distributions (SEDs) of blazars strongly constrain the nature of hydromagnetic turbulence responsible for pitch-angle scattering by requiring a strongly energy-dependent pitch-angle mean free path. The prominent soft X-ray excess (``Big Blue Bump'') in the SED of the BL Lac object AO 0235+164 can be modelled as the signature of bulk Compton scattering of external radiation fields by the thermal electron population, which places additional constraints on the level of hydromagnetic turbulence. It has further been demonstrated that internal shocks propagating in a jet pervaded by a helical magnetic field naturally produce polarization-angle swings by 180$^o$, in tandem with multi-wavelength flaring activity, without requiring any helical motion paths or other asymmetric jet structures. The specific application of this model to 3C279 presents the first consistent, simultaneous modeling of snap-shot SEDs, multi-wavelength light curves and time-dependent polarization signatures of a blazar during a polarization-angle (PA) rotation. This model has recently been generalized to a lepto-hadronic model, in which the high-energy emission is dominated by proton synchrotron radiation. It is shown that in this case, the high-energy (X-ray and $\gamma$-ray) polarization signatures are expected to be significantly more stable (not showing PA rotations) than the low-energy (electron-synchrotron) signatures.