238 research outputs found
Facilitated diffusion on confined DNA
In living cells, proteins combine 3D bulk diffusion and 1D sliding along the
DNA to reach a target faster. This process is known as facilitated diffusion,
and we investigate its dynamics in the physiologically relevant case of
confined DNA. The confining geometry and DNA elasticity are key parameters: we
find that facilitated diffusion is most efficient inside an isotropic volume,
and on a flexible polymer. By considering the typical copy numbers of proteins
in vivo, we show that the speedup due to sliding becomes insensitive to fine
tuning of parameters, rendering facilitated diffusion a robust mechanism to
speed up intracellular diffusion-limited reactions. The parameter range we
focus on is relevant for in vitro systems and for facilitated diffusion on
yeast chromatin
Colloids in active fluids: Anomalous micro-rheology and negative drag
We simulate an experiment in which a colloidal probe is pulled through an
active nematic fluid. We find that the drag on the particle is non-Stokesian
(not proportional to its radius). Strikingly, a large enough particle in
contractile fluid (such as an actomyosin gel) can show negative viscous drag in
steady state: the particle moves in the opposite direction to the externally
applied force. We explain this, and the qualitative trends seen in our
simulations, in terms of the disruption of orientational order around the probe
particle and the resulting modifications to the active stress.Comment: 5 pages, 3 figure
You Can't See Me: Anonymizing Graphs Using the Szemerédi Regularity Lemma.
Complex networks gathered from our online interactions provide a rich source of information that can be used to try to model and predict our behavior. While this has very tangible benefits that we have all grown accustomed to, there is a concrete privacy risk in sharing potentially sensitive data about ourselves and the people we interact with, especially when this data is publicly available online and unprotected from malicious attacks. k-anonymity is a technique aimed at reducing this risk by obfuscating the topological information of a graph that can be used to infer the nodes' identity. In this paper we propose a novel algorithm to enforce k-anonymity based on a well-known result in extremal graph theory, the Szemerédi regularity lemma. Given a graph, we start by computing a regular partition of its nodes. The Szemerédi regularity lemma ensures that such a partition exists and that the edges between the sets of nodes behave almost randomly. With this partition, we anonymize the graph by randomizing the edges within each set, obtaining a graph that is structurally similar to the original one yet the nodes within each set are structurally indistinguishable. We test the proposed approach on real-world networks extracted from Facebook. Our experimental results show that the proposed approach is able to anonymize a graph while retaining most of its structural information
Bulk rheology and microrheology of active fluids
We simulate macroscopic shear experiments in active nematics and compare them
with microrheology simulations where a spherical probe particle is dragged
through an active fluid. In both cases we define an effective viscosity: in the
case of bulk shear simulations this is the ratio between shear stress and shear
rate, whereas in the microrheology case it involves the ratio between the
friction coefficient and the particle size. We show that this effective
viscosity, rather than being solely a property of the active fluid, is affected
by the way chosen to measure it, and strongly depends on details such as the
anchoring conditions at the probe surface and on both the system size and the
size of the probe particle.Comment: 12 pages, 10 figure
MAGIC eyes to the extreme: testing the blazar emission models on EHBLs
Extreme high-energy peaked BL Lac objects (EHBLs) are blazars whose
synchrotron emission peaks at exceptionally high energies, above few keV, in
the hard X-ray regime. So far, only a handful of those objects has been
detected at very high energy (VHE, E > 100 GeV) gamma rays by Imaging
Atmospheric Cherenkov Telescopes. Very remarkably, VHE observations of some of
these blazars (like 1ES 0229+200) have provided evidence of a VHE gamma-ray
emission extending to several TeV, which is difficult to explain with standard,
one-zone synchrotron self-Compton models usually applied to BL Lac objects. The
MAGIC collaboration coordinated a multi-year, multi-wavelength observational
campaign on ten targets. The MAGIC telescopes detected VHE gamma rays from four
EHBLs. In this paper we focus on the source 1ES 1426+426 and its X-ray and VHE
gamma-ray properties. The results of different models (synchrotron
self-Compton, spine-layer, hadronic) reproducing the broadband spectral energy
distribution are also presented.Comment: Proceedings of the 36th International Cosmic Ray Conference
(ICRC2019), July 24th-August 1st, 2019. Madison, WI, U.S.
New Hard-TeV Extreme Blazars Detected with the MAGIC Telescopes
Extreme high-frequency-peaked BL Lac objects (EHBLs) are blazars that exhibit extremely energetic synchrotron emission. They also feature nonthermal gamma-ray emission whose peak lies in the very high-energy (VHE, E > 100 GeV) range, and in some sources exceeds 1 TeV: this is the case for hard-TeV EHBLs such as 1ES 0229+200. With the aim of increasing the EHBL population, 10 targets were observed with the MAGIC telescopes from 2010 to 2017, for a total of 265 hr of good-quality data. The data were complemented by coordinated Swift observations. The X-ray data analysis confirms that all but two sources are EHBLs. The sources show only a modest variability and a harder-when-brighter behavior, typical for this class of objects. At VHE gamma-rays, three new sources were detected and a hint of a signal was found for another new source. In each case, the intrinsic spectrum is compatible with the hypothesis of a hard-TeV nature of these EHBLs. The broadband spectral energy distributions (SEDs) of all sources are built and modeled in the framework of a single-zone, purely leptonic model. The VHE gamma-ray-detected sources were also interpreted with a spine-layer model and a proton synchrotron model. The three models provide a good description of the SEDs. However, the resulting parameters differ substantially in the three scenarios, in particular the magnetization parameter. This work presents the first mini catalog of VHE gamma-ray and multiwavelength observations of EHBLs
Measurement of the Extragalactic Background Light using MAGIC and Fermi-LAT gamma-ray observations of blazars up to z = 1
We present a measurement of the extragalactic background light (EBL) based on
a joint likelihood analysis of 32 gamma-ray spectra for 12 blazars in the
redshift range z = 0.03 to 0.944, obtained by the MAGIC telescopes and
Fermi-LAT. The EBL is the part of the diffuse extragalactic radiation spanning
the ultraviolet, visible and infrared bands. Major contributors to the EBL are
the light emitted by stars through the history of the universe, and the
fraction of it which was absorbed by dust in galaxies and re-emitted at longer
wavelengths. The EBL can be studied indirectly through its effect on very-high
energy photons that are emitted by cosmic sources and absorbed via
photon-photon interactions during their propagation across cosmological
distances. We obtain estimates of the EBL density in good agreement with
state-of-the-art models of the EBL production and evolution. The 1-sigma upper
bounds, including systematic uncertainties, are between 13% and 23% above the
nominal EBL density in the models. No anomaly in the expected transparency of
the universe to gamma rays is observed in any range of optical depth.We also
perform a wavelength-resolved EBL determination, which results in a hint of an
excess of EBL in the 0.18 - 0.62 m range relative to the studied models,
yet compatible with them within systematics.Comment: Accepted by MNRA
Discovery of TeV γ-ray emission from the neighbourhood of the supernova remnant G24.7+0.6 by MAGIC
SNR G24.7+0.6 is a 9.5 kyrs radio and gamma-ray supernova remnant evolving in a dense medium. In the GeV regime, SNR G24.7+0.6 (3FHL J1834.1– 0706e/FGES J1834.1–0706) shows a hard spectral index (Γ∼2) up to 200 GeV, which makes it a good candidate to be observed with Cherenkov telescopes such as MAGIC. We observed the field of view of SNR G24.7+0.6 with the MAGIC telescopes for a total of 31 hours. We detect very high energy γ-ray emission from an extended source located 0.34 degree away from the center of the radio SNR. The new source, named MAGIC J1835–069 is detected up to 5 TeV, and its spectrum is well-represented by a power-law function with spectral index of 2.74 ± 0.08. The complexity of the region makes the identification of the origin of the very-high energy emission difficult, however the spectral agreement with the LAT source and overlapping position at less than 1.5 sigma point to a common origin. We analysed 8 years of Fermi-LAT data to extend the spectrum of the source down to 60 MeV. Fermi-LAT and MAGIC spectra overlap within errors and the global broad band spectrum is described by a power-law with exponential cutoff at 1.9 ± 0.5 TeV. The detected γ-ray emission can be interpreted as the results of proton-proton interaction between the supernova and the CO-rich surrounding
A fast, very-high-energy γ -ray flare from BL Lacertae during a period of multi-wavelength activity in June 2015
The mechanisms producing fast variability of the γ-ray emission in active galactic nuclei (AGNs) are under debate. The MAGIC telescopes detected a fast, very-high-energy (VHE, E > 100 GeV) γ-ray flare from BL Lacertae on 2015 June 15. The flare had a maximum flux of (1.5 ± 0.3) × 10-10 photons cm-2 s-1 and halving time of 26 ± 8 min. The MAGIC observations were triggered by a high state in the optical and high-energy (HE, E > 100 MeV) γ-ray bands. In this paper we present the MAGIC VHE γ-ray data together with multi-wavelength data from radio, optical, X-rays, and HE γ rays from 2015 May 1 to July 31. Well-sampled multi-wavelength data allow us to study the variability in detail and compare it to the other epochs when fast, VHE γ-ray flares have been detected from this source. Interestingly, we find that the behaviour in radio, optical, X-rays, and HE γ-rays is very similar to two other observed VHE γ-ray flares. In particular, also during this flare there was an indication of rotation of the optical polarization angle and of activity at the 43 GHz core. These repeating patterns indicate a connection between the three events. We also test modelling of the spectral energy distribution based on constraints from the light curves and VLBA observations, with two different geometrical setups of two-zone inverse Compton models. In addition we model the γ-ray data with the star-jet interaction model. We find that all of the tested emission models are compatible with the fast VHE γ-ray flare, but all have some tension with the multi-wavelength observations
The Blazar TXS 0506+056 Associated with a High-energy Neutrino: Insights into Extragalactic Jets and Cosmic-Ray Acceleration
A neutrino with energy ∼290 TeV, IceCube-170922A, was detected in coincidence with the BL Lac object TXS 0506+056 during enhanced gamma-ray activity, with chance coincidence being rejected at ∼3σ level. We monitored the object in the very-high-energy (VHE) band with the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes for ∼41 hr from 1.3 to 40.4 days after the neutrino detection. Day-timescale variability is clearly resolved. We interpret the quasi-simultaneous neutrino and broadband electromagnetic observations with a novel one-zone lepto-hadronic model, based on interactions of electrons and protons co-accelerated in the jet with external photons originating from a slow-moving plasma sheath surrounding the faster jet spine. We can reproduce the multiwavelength spectra of TXS 0506+056 with neutrino rate and energy compatible with IceCube-170922A, and with plausible values for the jet power of
. The steep spectrum observed by MAGIC is concordant with internal γγ absorption above ∼100 GeV entailed by photohadronic production of a ∼290 TeV neutrino, corroborating a genuine connection between the multi-messenger signals. In contrast to previous predictions of predominantly hadronic emission from neutrino sources, the gamma-rays can be mostly ascribed to inverse Compton upscattering of external photons by accelerated electrons. The X-ray and VHE bands provide crucial constraints on the emission from both accelerated electrons and protons. We infer that the maximum energy of protons in the jet comoving frame can be in the range ∼1014 – 1018 eV.Peer Reviewe
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