The Halo Occupation Distribution of Black Holes: Dependence on Mass

We investigate the halo occupation distribution (HOD) of black holes within a hydrodynamic cosmological simulation that directly follows black hole growth. Similar to the HOD of galaxies/subhalos, we find that the black hole occupation number can be described by the form N_BH proportional to 1+ (M_Host)^alpha where alpha evolves mildly with redshift indicating that a given mass halo (M_Host) at low redshift tends to host fewer BHs than at high redshift (as expected as a result of galaxy and BH mergers). We further divide the occupation number into contributions from black holes residing in central and satellite galaxies within a halo. The distribution of M_BH within halos tends to consist of a single massive BH (distributed about a peak mass strongly correlated with M_Host), and a collection of relatively low-mass secondary BHs, with weaker correlation with M_Host. We also examine the spatial distribution of BHs within their host halos, and find they typically follow a power-law radial distribution (i.e. much more centrally concentrated than the subhalo distribution). Finally, we characterize the host mass for which BH growth is feedback dominated (e.g. star formation quenched). We show that halos with M_Host > 3 * 10^12 M_sun have primary BHs that are feedback dominated by z~3 with lower mass halos becoming increasingly more affected at lower redshift.Comment: 10 pages, 7 figures, submitted to MNRA

Multimessenger astronomy with pulsar timing and X-ray observations of massive black hole binaries

We demonstrate that very massive (>10^8\msun), cosmologically nearby (z<1) black hole binaries (MBHBs), which are primary targets for ongoing and upcoming pulsar timing arrays (PTAs), are particularly appealing multimessenger carriers. According to current models for massive black hole formation and evolution, the planned Square Kilometer Array (SKA) will collect gravitational wave signals from thousands of such massive systems, being able to individually resolve and locate in the sky several of them (maybe up to a hundred). By employing a standard model for the evolution of MBHBs in circumbinary discs, with the aid of dedicated numerical simulations, we characterize the gas-binary interplay, identifying possible electromagnetic signatures of the PTA sources. We concentrate our investigation on two particularly promising scenarios in the high energy domain, namely, the detection of X-ray periodic variability and of double broad K\alpha iron lines. Up to several hundreds of periodic X-ray sources with a flux >10^-13 erg s^-1 cm^-2 will be in the reach of upcoming X-ray observatories. Double relativistic K\alpha lines may be observable in a handful of low redshift (z<0.3) sources by proposed deep X-ray probes, such as Athena. (Abridged)Comment: 19 pages, 11 figures, submitted to MNRAS, minor revision of the reference lis

Simple and More Efficient PRFs with Tight Security from LWE and Matrix-DDH

We construct efficient and tightly secure pseudorandom functions (PRFs) with only logarithmic security loss and short secret keys. This yields very simple and efficient variants of well-known constructions, including those of Naor-Reingold (FOCS 1997) and Lewko-Waters (ACM CCS 2009). Most importantly, in combination with the construction of Banerjee, Peikert and Rosen (EUROCRYPT 2012) we obtain the currently most efficient LWE-based PRF from a weak LWE-assumption with a much smaller modulus than the original construction. In comparison to the only previous construction with this property, which is due to Doettling and Schroeder (CRYPTO 2015), we use a modulus of similar size, but only a single instance of the underlying PRF, instead of $\lambda \cdot \omega(\log \lambda)$ parallel instances, where $\lambda$ is the security parameter. Like Doettling and Schroeder, our security proof is only almost back-box, due to the fact that the number of queries made by the adversary and its advantage must be known a-priori. Technically, we introduce all-prefix universal hash functions (APUHFs), which are hash functions that are (almost-)universal, even if any prefix of the output is considered. We give simple and very efficient constructions of APUHFs, and show how they can be combined with the augmented cascade of Boneh et al. (ACM CCS 2010) to obtain our results. Along the way, we develop a new and more direct way to prove security of PRFs based on the augmented cascade

The Luminosity Function of Fermi-detected Flat-Spectrum Radio Quasars

Fermi has provided the largest sample of {\gamma}-ray selected blazars to date. In this work we use a complete sample of FSRQs detected during the first year of operation to determine the luminosity function (LF) and its evolution with cosmic time. The number density of FSRQs grows dramatically up to redshift \sim0.5-2.0 and declines thereafter. The redshift of the peak in the density is luminosity dependent, with more luminous sources peaking at earlier times; thus the LF of {\gamma}-ray FSRQs follows a luminosity-dependent density evolution similarly to that of radio-quiet AGN. Also using data from the Swift Burst Alert Telescope we derive the average spectral energy distribution of FSRQs in the 10 keV-100 GeV band and show that there is no correlation of the peak {\gamma}-ray luminosity with {\gamma}-ray peak frequency. The coupling of the SED and LF allows us to predict that the contribution of FSRQs to the Fermi isotropic {\gamma}-ray background is 9.3(+1.6/-1.0) (\pm3% systematic uncertainty) in the 0.1-100GeV band. Finally we determine the LF of unbeamed FSRQs, finding that FSRQs have an average Lorentz factor of {\gamma} = 11.7(+3.3/-2.2), that most are seen within 5\circ of the jet axis, and that they represent only ~0.1 % of the parent population.Comment: Submitted to the Astrophysical Journa

The Origins of AGN Obscuration: The 'Torus' as a Dynamical, Unstable Driver of Accretion

Multi-scale simulations have made it possible to follow gas inflows onto massive black holes (BHs) from galactic scales to the accretion disk. When sufficient gas is driven towards the BH, gravitational instabilities generically form lopsided, eccentric disks that propagate inwards. The lopsided stellar disk exerts a strong torque on the gas disk, driving inflows that fuel rapid BH growth. Here, we investigate whether the same gas disk is the 'torus' invoked to explain obscured AGN. The disk is generically thick and has characteristic ~1-10 pc sizes and masses resembling those required of the torus. The scale heights and obscured fractions of the predicted torii are substantial even in the absence of strong stellar feedback providing the vertical support. Rather, they can be maintained by strong bending modes and warps excited by the inflow-generating instabilities. Other properties commonly attributed to feedback processes may be explained by dynamical effects: misalignment between torus and host galaxy, correlations between local SFR and turbulent gas velocities, and dependence of obscured fractions on AGN luminosity or SFR. We compare the predicted torus properties with observations of gas surface density profiles, kinematics, scale heights, and SFR densities in AGN nuclei, and find that they are consistent. We argue that it is not possible to reproduce these observations and the observed column density (N_H) distribution without a clumpy gas distribution, but allowing for clumping on small scales the predicted N_H distribution is in good agreement with observations from 10^20-27 cm^-2. We examine how N_H scales with galaxy and AGN properties, and find that AGN feedback may be necessary to explain some trends with luminosity and/or redshift. The torus is not merely a bystander or passive fuel source for accretion, but is itself the mechanism driving accretion.Comment: 20 pages, 10 figures, accepted to MNRAS (matches accepted version

Benzimidazole and aminoalcohol derivatives show in vitro anthelmintic activity against Trichuris muris and Heligmosomoides polygyrus

8 páginas, 4 tablas.Background: Infections by gastrointestinal nematodes cause significant economic losses and disease in both humans and animals worldwide. The discovery of novel anthelmintic drugs is crucial for maintaining control of these parasitic infections. Methods: For this purpose, the aim of the present study was to evaluate the potential anthelmintic activity of three series of compounds against the gastrointestinal nematodes Trichuris muris and Heligmosomoides polygyrus in vitro. The compounds tested were derivatives of benzimidazole, lipidic aminoalcohols and diamines. A primary screening was performed to select those compounds with an ability to inhibit T. muris L1 motility by > 90% at a single concentration of 100 µM; then, their respective IC50 values were calculated. Those compounds with IC50 < 10 µM were also tested against the adult stage of T. muris and H. polygyrus at a single concentration of 10 µM. Results: Of the 41 initial compounds screened, only compounds AO14, BZ6 and BZ12 had IC50 values < 10 µM on T. muris L1 assay, showing IC50 values of 3.30, 8.89 and 4.17 µM, respectively. However, only two of them displayed activity against the adult stage of the parasites: BZ12 killed 81% of adults of T. muris (IC50 of 8.1 µM) and 53% of H. polygyrus while BZ6 killed 100% of H. polygyrus adults (IC50 of 5.3 µM) but only 17% of T. muris. Conclusions: BZ6 and BZ12 could be considered as a starting point for the synthesis of further structurally related compounds. GraphicalFinancial support came from MINECO: RETOS (AGL2016‑79813‑C2‑1R/2R) and Junta de Castilla y León co‑financed by FEDER, UE [LE020P17]. EVG was funded by FPU17/00627; VCGA and MAB are recipients of Junta de Castilla y Leon (JCyL) (LE082‑18, LE051‑18, respectively) and MMV by the Spanish “Ramon y Cajal” Programme (Ministerio de Economía y competitividad; MMV, RYC‑2015‑18368).Peer reviewe