@article{1759, abstract = {We report an electric-field-induced giant modulation of the hole g factor in SiGe nanocrystals. The observed effect is ascribed to a so-far overlooked contribution to the g factor that stems from the mixing between heavy- and light-hole wave functions. We show that the relative displacement between the confined heavy- and light-hole states, occurring upon application of the electric field, alters their mixing strength leading to a strong nonmonotonic modulation of the g factor.}, author = {Ares, Natalia and Golovach, Vitaly N and Georgios Katsaros and Stoffel, Mathieu and Fournel, Frank and Glazman, Leonid I and Schmidt, Oliver G and De Franceschi, Silvano}, journal = {Physical Review Letters}, number = {4}, publisher = {American Physical Society}, title = {{Nature of tunable hole g factors in quantum dots}}, doi = {10.1103/PhysRevLett.110.046602}, volume = {110}, year = {2013}, } @article{1760, abstract = {We report on hole g-factor measurements in three terminal SiGe self-assembled quantum dot devices with a top gate electrode positioned very close to the nanostructure. Measurements of both the perpendicular as well as the parallel g-factor reveal significant changes for a small modulation of the top gate voltage. From the observed modulations, we estimate that, for realistic experimental conditions, hole spins can be electrically manipulated with Rabi frequencies in the order of 100 MHz. This work emphasises the potential of hole-based nano-devices for efficient spin manipulation by means of the g-tensor modulation technique.}, author = {Ares, Natalia and Georgios Katsaros and Golovach, Vitaly N and Zhang, Jianjun and Prager, Aaron A and Glazman, Leonid I and Schmidt, Oliver G and De Franceschi, Silvano}, journal = {Applied Physics Letters}, number = {26}, publisher = {American Institute of Physics}, title = {{SiGe quantum dots for fast hole spin Rabi oscillations}}, doi = {10.1063/1.4858959}, volume = {103}, year = {2013}, } @article{17624, abstract = {A near-equal-mass binary black hole (BH) can clear a central cavity in a circumbinary accretion disc; however, previous works have revealed accretion streams entering this cavity. Here we use 2D hydrodynamical simulations to study the accretion streams and their periodic behaviour. In particular, we perform a suite of simulations, covering different binary mass ratios q = M2/M1 in the range 0.003 ≤ q ≤ 1. In each case, we follow the system for several thousand binary orbits, until it relaxes to a stable accretion pattern. We find the following results: (i) the binary is efficient in maintaining a low-density cavity. However, the time-averaged mass accretion rate into the cavity, through narrow coherent accretion streams, is suppressed by at most a factor of a few compared to a disc with a single BH with the same mass; (ii) for q ≳ 0.05, the accretion rate is strongly modulated by the binary, and depending on the precise value of q, the power spectrum of the accretion rate shows either one, two or three distinct periods; and (iii) for q ≲ 0.05, the accretion rate becomes steady, with no time variations. Most binaries produced in galactic mergers are expected to have q ≳ 0.05. If the luminosity of these binaries tracks their accretion rate, then a periodogram of their light curve could help in their identification, and to constrain their mass ratio and disc properties.}, author = {D'Orazio, Daniel J. and Haiman, Zoltán and MacFadyen, Andrew}, issn = {1365-2966}, journal = {Monthly Notices of the Royal Astronomical Society}, number = {4}, pages = {2997--3020}, publisher = {Oxford University Press}, title = {{Accretion into the central cavity of a circumbinary disc}}, doi = {10.1093/mnras/stt1787}, volume = {436}, year = {2013}, } @article{17631, abstract = {We propose a novel use of high-redshift galaxies, discovered in deep Hubble Space Telescope (HST) fields around strong lensing clusters. These fields probe small comoving volumes (∼103 Mpc3) at high magnification (μ ≳ 10) and can detect otherwise inaccessible ultra-faint galaxies. Even a few galaxies found in such small volumes require a very high number density of collapsed dark matter (DM) haloes. This implies significant primordial power on small scales, allowing these observations to rule out popular alternatives to standard cold dark matter (CDM) models, such as warm dark matter (WDM). In this work, we analytically compute WDM halo mass functions at z = 10, including the effects of both particle free-streaming and residual velocity dispersion. We show that the two z ≈ 10 galaxies already detected by the Cluster Lensing And Supernova survey with Hubble (CLASH) survey are sufficient to constrain the WDM particle mass to mx > 1 (0.9) keV at 68 per cent (95 per cent) confidence limit (for a thermal relic relativistic at decoupling). This limit depends only on the WDM halo mass function and, unlike previous constraints on mx, is independent of any astrophysical modelling. The forthcoming HST Frontier Fields can significantly tighten these constraints.}, author = {Pacucci, Fabio and Mesinger, Andrei and Haiman, Zoltán}, issn = {1745-3933}, journal = {Monthly Notices of the Royal Astronomical Society: Letters}, number = {1}, pages = {L53--L57}, publisher = {Oxford University Press}, title = {{Focusing on warm dark matter with lensed high-redshift galaxies}}, doi = {10.1093/mnrasl/slt093}, volume = {435}, year = {2013}, } @article{17638, abstract = {Pulsar timing arrays (PTAs) may eventually be able to detect not only the stochastic gravitational-wave (GW) background of SMBH binaries, but also individual, particularly massive binaries whose signals stick out above the background. In this contribution, we discuss the possibility of identifying and studying such 'resolved' binaries through their electromagnetic emission. The host galaxies of such binaries are themselves expected to be also very massive and rare, so that out to redshifts z ≈ 0.2 a unique massive galaxy may be identified as the host. At higher redshifts, the PTA error boxes are larger and may contain as many as several hundred massive-galaxy interlopers. In this case, the true counterpart may be identified, if it is accreting gas efficiently, as an active galactic nucleus (AGN) with a peculiar spectrum and variable emission features. Specifically, the binary's tidal torques expel the gas from the inner part of the accretion disc, making it unusually dim in x-ray and UV bands and in broad optical emission lines. The tails of the broad wings of any FeKα emission line may also be 'clipped' and missing. The binary's orbital motion, as well as the gas motions it induces, may trigger quasiperiodic variations. These include coherent flux variability, such as luminous, multi-wavelength flares, as well as Doppler shifts of broad emission lines and 'see-saw' oscillations in the FeKα line. Additional features, such as evidence for a recent major merger or dual collimated jets, could also corroborate the counterpart. These properties would make resolved PTA sources stand out among AGN with similar overall luminosities and allow their identification.}, author = {Tanaka, Takamitsu L and Haiman, Zoltán}, issn = {0264-9381}, journal = {Classical and Quantum Gravity}, number = {22}, publisher = {IOP Publishing}, title = {{Electromagnetic signatures of supermassive black hole binaries resolved by PTAs}}, doi = {10.1088/0264-9381/30/22/224012}, volume = {30}, year = {2013}, } @article{17646, abstract = {Structures in Warm Dark Matter (WDM) models are exponentially suppressed below a certain scale, characterized by the dark matter particle mass, mx. Since structures form hierarchically, the presence of collapsed objects at high-redshifts can set strong lower limits on mx. We place robust constraints on mx using recent results from the {\it Swift} database of high-redshift gamma-ray bursts (GRBs). We parameterize the redshift evolution of the ratio between the cosmic GRB rate and star formation rate (SFR) as ∝(1+z)α, thereby allowing astrophysical uncertainties to partially mimic the cosmological suppression of structures in WDM models. Using a maximum likelihood estimator on two different z>4 GRB subsamples (including two bursts at z>8), we constrain mx≳1.6-1.8 keV at 95% C.L., when marginalized over a flat prior in α. We further estimate that 5 years of a SVOM-like mission would tighten these constraints to mx≳2.3 keV. Our results show that GRBs are a powerful probe of high-redshift structures, providing robust and competitive constraints on mx.}, author = {de Souza, R. S. and Mesinger, A. and Ferrara, A. and Haiman, Zoltán and Perna, R. and Yoshida, N.}, issn = {0035-8711}, journal = {Monthly Notices of the Royal Astronomical Society}, number = {4}, pages = {3218--3227}, publisher = {Oxford University Press}, title = {{Constraints on warm dark matter models from high-redshift long gamma-ray bursts}}, doi = {10.1093/mnras/stt674}, volume = {432}, year = {2013}, } @article{17653, abstract = {Observations of quasars at redshifts z > 6 reveal that 10^9 Msol supermassive black holes (SMBHs) had already formed when the Universe was < 0.9 Gyr old. One hypothesis for the origins of these SMBHs is that they grew from the remnants of the first generation of massive stars, which formed in low-mass (~ 10^5 to 10^6 Msol) dark matter minihaloes at z > 20. This is the regime where baryonic streaming motions--the relative velocities of baryons with respect to dark matter in the early Universe--most strongly inhibit star formation by suppressing gas infall and cooling. We investigate the impact of this effect on the growth of the first SMBHs using a suite of high-fidelity, ellipsoidal-collapse Monte Carlo merger-tree simulations. We find that the suppression of seed BH formation by the streaming motions significantly reduces the number density of the most massive BHs at z > 15, but the residual effect at lower redshifts is essentially negligible. The streaming motions can reduce by a factor of few the number density of the most luminous quasars at z ~ 10-11, where such objects could be detected by the James Webb Space Telescope. We conclude, with minor theoretical caveats, that baryonic streaming motions are unlikely to pose a significant additional obstacle to the formation of the observed high-redshift quasar SMBHs. Nor do they appreciably affect the heating and reionization histories of the Universe or the merger rates of nuclear BHs in the mass and redshift ranges of interest for proposed gravitational-wave detectors.}, author = {Tanaka, Takamitsu L. and Li, Miao and Haiman, Zoltán}, issn = {1365-2966}, journal = {Monthly Notices of the Royal Astronomical Society}, number = {4}, pages = {3559--3567}, publisher = {Oxford University Press}, title = {{The effect of baryonic streaming motions on the formation of the first supermassive black holes}}, doi = {10.1093/mnras/stt1553}, volume = {435}, year = {2013}, } @article{17657, abstract = {We present observations of a luminous galaxy at z = 6.573—the end of the reionization epoch—which has been spectroscopically confirmed twice. The first spectroscopic confirmation comes from slitless Hubble Space Telescope Advanced Camera for Surveys grism spectra from the PEARS survey (Probing Evolution And Reionization Spectroscopically), which show a dramatic continuum break in the spectrum at rest frame 1216 Å. The second confirmation is done with Keck + DEIMOS. The continuum is not clearly detected with ground-based spectra, but high wavelength resolution enables the Lyα emission line profile to be determined. We compare the line profile to composite line profiles at z = 4.5. The Lyα line profile shows no signature of a damping wing attenuation, confirming that the intergalactic gas is ionized at z = 6.57. Spectra of Lyman breaks at yet higher redshifts will be possible using comparably deep observations with IR-sensitive grisms, even at redshifts where Lyα is too attenuated by the neutral intergalactic medium to be detectable using traditional spectroscopy from the ground.}, author = {Rhoads, James E. and Malhotra, Sangeeta and Stern, Daniel and Dickinson, Mark and Pirzkal, Norbert and Spinrad, Hyron and Reddy, Naveen and Hathi, Nimish and Grogin, Norman and Koekemoer, Anton and Peth, Michael A. and Cohen, Seth and Zheng, Zhenya and Budavari, Tamas and Ferreras, Ignacio and Gardner, Jonathan P. and Gronwall, Caryl and Haiman, Zoltán and Kümmel, Martin and Meurer, Gerhardt and Moustakas, Leonidas and Panagia, Nino and Pasquali, Anna and Sahu, Kailash and di Serego Alighieri, Sperello and Somerville, Rachel and Straughn, Amber and Walsh, Jeremy and Windhorst, Rogier and Xu, Chun and Yan, Haojing}, issn = {0004-637X}, journal = {The Astrophysical Journal}, number = {1}, publisher = {American Astronomical Society}, title = {{A Lyman break galaxy in the epoch of reionization from hubble space telescope grism spectroscopy}}, doi = {10.1088/0004-637x/773/1/32}, volume = {773}, year = {2013}, } @article{17670, abstract = {The statistics of peak counts in reconstructed shear maps contain information beyond the power spectrum, and can improve cosmological constraints from measurements of the power spectrum alone if systematic errors can be controlled. We study the effect of galaxy shape measurement errors on predicted cosmological constraints from the statistics of shear peak counts with the Large Synoptic Survey Telescope (LSST). We use the LSST image simulator in combination with cosmological N-body simulations to model realistic shear maps for different cosmological models. We include both galaxy shape noise and, for the first time, measurement errors on galaxy shapes. We find that the measurement errors considered have relatively little impact on the constraining power of shear peak counts for LSST.}, author = {Bard, D. and Kratochvil, J. M. and Chang, C. and May, M. and Kahn, S. M. and AlSayyad, Y. and Ahmad, Z. and Bankert, J. and Connolly, A. and Gibson, R. R. and Gilmore, K. and Grace, E. and Haiman, Zoltán and Hannel, M. and Huffenberger, K. M. and Jernigan, J. G. and Jones, L. and Krughoff, S. and Lorenz, S. and Marshall, S. and Meert, A. and Nagarajan, S. and Peng, E. and Peterson, J. and Rasmussen, A. P. and Shmakova, M. and Sylvestre, N. and Todd, N. and Young, M.}, issn = {0004-637X}, journal = {The Astrophysical Journal}, number = {1}, publisher = {American Astronomical Society}, title = {{Effect of measurement errors on predicted cosmological constraints from shear peak statistics with large synoptic survey telescope}}, doi = {10.1088/0004-637x/774/1/49}, volume = {774}, year = {2013}, } @article{17671, abstract = {Galactic nuclei are expected to be densely populated with stellar and intermediate mass black holes. Exploring this population will have important consequences for the observation prospects of gravitational waves as well as understanding galactic evolution. The gas cloud G2 currently approaching Sgr A* provides an unprecedented opportunity to probe the black hole and neutron star population of the Galactic nucleus. We examine the possibility of a G2-black hole encounter and its detectability with current X-ray satellites, such as Chandra and NuSTAR. We find that multiple encounters are likely to occur close to the pericenter, which may be detectable upon favorable circumstances. This opportunity provides an additional, important science case for leading X-ray observatories to closely follow G2 on its way to the nucleus.}, author = {Bartos, Imre and Haiman, Zoltán and Kocsis, Bence and Márka, Szabolcs}, issn = {0031-9007}, journal = {Physical Review Letters}, number = {22}, publisher = {American Physical Society}, title = {{Gas cloud G2 can illuminate the black hole population near the galactic center}}, doi = {10.1103/physrevlett.110.221102}, volume = {110}, year = {2013}, } @article{17677, abstract = {Peaks in two-dimensional weak lensing (WL) maps contain significant cosmological information, complementary to the WL power spectrum. This has recently been demonstrated using N-body simulations which neglect baryonic effects. Here we employ ray-tracing N-body simulations in which we manually steepen the density profile of each dark matter halo, mimicking the cooling and concentration of baryons into dark matter potential wells. We find, in agreement with previous works, that this causes a significant increase in the amplitude of the WL power spectrum on small scales (spherical harmonic index l>1,000). We then study the impact of the halo concentration increase on the peak counts, and find the following. (i) Low peaks (with convergence 0.02 < kappa_peak < 0.08), remain nearly unaffected. These peaks are created by a constellation of several halos with low masses (10^12-10^13 M_sun) and large angular offsets from the peak center (> 0.5 R_vir); as a result, they are insensitive to the central halo density profiles. These peaks contain most of the cosmological information, and thus provide an unusually sensitive and unbiased probe. (ii) The number of high peaks (with convergence kappa_peak > 0.08) is increased. However, when the baryon effects are neglected in cosmological parameter estimation, then the high peaks lead to a modest bias, comparable to that from the power spectrum on relatively large-scales (l<2000), and much smaller than the bias from the power spectrum on smaller scales (l>2,000). (iii) In the 3D parameter space (sigma_8, Omega_m, w), the biases from the high peaks and the power spectra are in different directions. This suggests the possibility of "self-calibration": the combination of peak counts and power spectrum can simultaneously constrain baryonic physics and cosmological parameters.}, author = {Yang, Xiuyuan and Kratochvil, Jan M. and Huffenberger, Kevin and Haiman, Zoltán and May, Morgan}, issn = {1550-7998}, journal = {Physical Review D}, number = {2}, publisher = {American Physical Society}, title = {{Baryon impact on weak lensing peaks and power spectrum: Low-bias statistics and self-calibration in future surveys}}, doi = {10.1103/physrevd.87.023511}, volume = {87}, year = {2013}, } @article{17683, abstract = {When a sufficiently massive satellite (or secondary) black hole is embedded in a gas disc around a (primary) supermassive black hole, it can open an empty gap in the disc. A gap-opening secondary close to the primary will leave an imprint in the broad component of the Fe Kα emission line, which varies in a unique and predictable manner. If the gap persists into the innermost disc, the effect consists of a pair of dips in the broad line which ripple blue-ward and red-ward from the line centroid energy, respectively, as the gap moves closer to the primary. This ripple effect could be unambiguously detectable and allow an electromagnetic monitoring of massive black hole mergers as they occur. As the mass ratio of the secondary to primary black hole increases to q ≳ 0.01, we expect the gap to widen, possibly clearing a central cavity in the inner disc, which shows up in the broad Fe Kα line component. If the secondary stalls at ≥ 102rg in its in-migration, due to low corotating gas mass, a detectable ripple effect occurs in the broad line component on the disc viscous time-scale as the inner disc drains and the outer disc is dammed. If the secondary maintains an accretion disc within a central cavity, due to dam bursting or leakage, a periodic ‘see-saw’ oscillation effect is exhibited in the observed line profile. Here, we demonstrate the range of ripple effect signatures potentially detectable with Astro-H and IXO/Athena, and oscillation effects potentially detectable with XMM–Newton or LOFT for a wide variety of merger and disc conditions, including gap width (or cavity size), disc inclination angle and emissivity profile, damming of the accretion flow by the secondary, and a minidisc around the satellite black hole. A systematic study of ripple effects would require a telescope effective area substantially larger than that planned for IXO/Athena. Future mission planning should take this into account. Observations of the ripple effect and periodic oscillations can be used to provide an early warning of gravitational radiation emission from the AGN. Once gravitational waves consistent with massive black hole mergers are detected, an archival search for the Fe Kα ripple effect or periodic oscillations will help in localizing their origin.}, author = {McKernan, B. and Ford, K. E. S. and Kocsis, B. and Haiman, Zoltán}, issn = {0035-8711}, journal = {Monthly Notices of the Royal Astronomical Society}, number = {2}, pages = {1468--1482}, publisher = {Oxford University Press}, title = {{Ripple effects and oscillations in the broad Fe Kα line as a probe of massive black hole mergers}}, doi = {10.1093/mnras/stt567}, volume = {432}, year = {2013}, } @article{17684, abstract = {We have performed cosmo-hydro simulations using the RAMSES code to study atomic cooling (ACHs) haloes at z=10 with masses 5E7Msun<~M<~2E9Msun. We assume primordial gas and H2-cooling and prior star-formation have been suppressed. We analysed 19 haloes (gas and DM) at a resolution of ~10 (proper) pc, selected from a total volume of ~2E3 (comoving) Mpc3. This is the largest statistical hydro-sim. study of ACHs at z>10 to date. We examine the morphology, angular momentum (AM), thermodynamic, and turbulence of these haloes, in order to assess the prevalence of disks and supermassive black holes (SMBHs). We find no correlation between either the magnitude or the direction of the AM of the gas and its parent DM halo. Only 3 haloes form rotationally supported cores. Two of the most massive haloes form massive, compact overdense blobs. These blobs have an accretion rate ~0.5 Msun/yr (at a distance of 100 pc), and are possible sites of SMBH formation. Our results suggest that the degree of rotational support and the fate of the gas in a halo is determined by its large-scale environment and merger history. In particular, the two haloes forming blobs are located at knots of the cosmic web, cooled early on, and experienced many mergers. The gas in these haloes is lumpy and highly turbulent, with Mach N. >~ 5. In contrast, the haloes forming rotationally supported cores are relatively more isolated, located midway along filaments, cooled more recently, and underwent fewer mergers. Thus, the gas in these haloes is less lumpy and less turbulent (Mach <~ 4), and could retain most of its AM. The remaining 14 haloes have intermediate properties. If verified in a larger sample of haloes and with additional physics, our results will have implications for observations of the highest-redshift galaxies and quasars with JWST.}, author = {Prieto, Joaquin and Jimenez, Raul and Haiman, Zoltán}, issn = {1365-2966}, journal = {Monthly Notices of the Royal Astronomical Society}, number = {3}, pages = {2301--2325}, publisher = {Oxford University Press}, title = {{Gas infall into atomic cooling haloes: On the formation of protogalactic discs and supermassive black holes at z > 10}}, doi = {10.1093/mnras/stt1730}, volume = {436}, year = {2013}, } @article{17704, abstract = {We compare the efficiency of moments and Minkowski functionals (MFs) in constraining the subset of cosmological parameters (Omega_m,w,sigma_8) using simulated weak lensing convergence maps. We study an analytic perturbative expansion of the MFs in terms of the moments of the convergence field and of its spatial derivatives. We show that this perturbation series breaks down on smoothing scales below 5', while it shows a good degree of convergence on larger scales (15'). Most of the cosmological distinguishing power is lost when the maps are smoothed on these larger scales. We also show that, on scales comparable to 1', where the perturbation series does not converge, cosmological constraints obtained from the MFs are approximately 1.5-2 times better than the ones obtained from the first few moments of the convergence distribution --- provided that the latter include spatial information, either from moments of gradients, or by combining multiple smoothing scales. Including either a set of these moments or the MFs can significantly tighten constraints on cosmological parameters, compared to the conventional method of using the power spectrum alone.}, author = {Petri, Andrea and Haiman, Zoltán and Hui, Lam and May, Morgan and Kratochvil, Jan M.}, issn = {1550-7998}, journal = {Physical Review D}, number = {12}, publisher = {American Physical Society}, title = {{Cosmology with Minkowski functionals and moments of the weak lensing convergence field}}, doi = {10.1103/physrevd.88.123002}, volume = {88}, year = {2013}, } @article{7745, abstract = {The underlying basis of genetic variation in quantitative traits, in terms of the number of causal variants and the size of their effects, is largely unknown in natural populations. The expectation is that complex quantitative trait variation is attributable to many, possibly interacting, causal variants, whose effects may depend upon the sex, age and the environment in which they are expressed. A recently developed methodology in animal breeding derives a value of relatedness among individuals from high‐density genomic marker data, to estimate additive genetic variance within livestock populations. Here, we adapt and test the effectiveness of these methods to partition genetic variation for complex traits across genomic regions within ecological study populations where individuals have varying degrees of relatedness. We then apply this approach for the first time to a natural population and demonstrate that genetic variation in wing length in the great tit (Parus major) reflects contributions from multiple genomic regions. We show that a polygenic additive mode of gene action best describes the patterns observed, and we find no evidence of dosage compensation for the sex chromosome. Our results suggest that most of the genomic regions that influence wing length have the same effects in both sexes. We found a limited amount of genetic variance in males that is attributed to regions that have no effects in females, which could facilitate the sexual dimorphism observed for this trait. Although this exploratory work focuses on one complex trait, the methodology is generally applicable to any trait for any laboratory or wild population, paving the way for investigating sex‐, age‐ and environment‐specific genetic effects and thus the underlying genetic architecture of phenotype in biological study systems.}, author = {Robinson, Matthew Richard and Santure, Anna W. and DeCauwer, Isabelle and Sheldon, Ben C. and Slate, Jon}, issn = {0962-1083}, journal = {Molecular Ecology}, number = {15}, pages = {3963--3980}, publisher = {Wiley}, title = {{Partitioning of genetic variation across the genome using multimarker methods in a wild bird population}}, doi = {10.1111/mec.12375}, volume = {22}, year = {2013}, } @article{7746, abstract = {Clutch size and egg mass are life history traits that have been extensively studied in wild bird populations, as life history theory predicts a negative trade‐off between them, either at the phenotypic or at the genetic level. Here, we analyse the genomic architecture of these heritable traits in a wild great tit (Parus major) population, using three marker‐based approaches – chromosome partitioning, quantitative trait locus (QTL) mapping and a genome‐wide association study (GWAS). The variance explained by each great tit chromosome scales with predicted chromosome size, no location in the genome contains genome‐wide significant QTL, and no individual SNPs are associated with a large proportion of phenotypic variation, all of which may suggest that variation in both traits is due to many loci of small effect, located across the genome. There is no evidence that any regions of the genome contribute significantly to both traits, which combined with a small, nonsignificant negative genetic covariance between the traits, suggests the absence of genetic constraints on the independent evolution of these traits. Our findings support the hypothesis that variation in life history traits in natural populations is likely to be determined by many loci of small effect spread throughout the genome, which are subject to continued input of variation by mutation and migration, although we cannot exclude the possibility of an additional input of major effect genes influencing either trait.}, author = {Santure, Anna W. and De Cauwer, Isabelle and Robinson, Matthew Richard and Poissant, Jocelyn and Sheldon, Ben C. and Slate, Jon}, issn = {0962-1083}, journal = {Molecular Ecology}, number = {15}, pages = {3949--3962}, publisher = {Wiley}, title = {{Genomic dissection of variation in clutch size and egg mass in a wild great tit (Parus major) population}}, doi = {10.1111/mec.12376}, volume = {22}, year = {2013}, } @article{7747, abstract = {Acquisition and allocation of resources are central to life‐history theory. However, empirical work typically focuses only on allocation despite the fact that relationships between fitness components may be governed by differences in the ability of individuals to acquire resources across environments. Here, we outline a statistical framework to partition the genetic basis of multivariate plasticity into independent axes of genetic variation, and quantify for the first time, the extent to which specific traits drive multitrait genotype–environment interactions. Our framework generalises to analyses of plasticity, growth and ageing. We apply this approach to a unique, large‐scale, multivariate study of acquisition, allocation and plasticity in the life history of the cricket, Gryllus firmus. We demonstrate that resource acquisition and allocation are genetically correlated, and that plasticity in trade‐offs between allocation to components of fitness is 90% dependent on genetic variance for total resource acquisition. These results suggest that genotype–environment effects for resource acquisition can maintain variation in life‐history components that are typically observed in the wild.}, author = {Robinson, Matthew Richard and Beckerman, Andrew P.}, issn = {1461-023X}, journal = {Ecology Letters}, number = {3}, pages = {281--290}, publisher = {Wiley}, title = {{Quantifying multivariate plasticity: Genetic variation in resource acquisition drives plasticity in resource allocation to components of life history}}, doi = {10.1111/ele.12047}, volume = {16}, year = {2013}, } @article{7774, abstract = {In 2005, Wyart et al. [Europhys. Lett., 2005, 72, 486] showed that the low frequency vibrational properties of jammed amorphous sphere packings can be understood in terms of a length scale, called l*, that diverges as the system becomes marginally unstable. Despite the tremendous success of this theory, it has been difficult to connect the counting argument that defines l* to other length scales that diverge near the jamming transition. We present an alternate derivation of l* based on the onset of rigidity. This phenomenological approach reveals the physical mechanism underlying the length scale and is relevant to a range of systems for which the original argument breaks down. It also allows us to present the first direct numerical measurement of l*.}, author = {Goodrich, Carl Peter and Ellenbroek, Wouter G. and Liu, Andrea J.}, issn = {1744-683X}, journal = {Soft Matter}, number = {46}, publisher = {Royal Society of Chemistry}, title = {{Stability of jammed packings I: The rigidity length scale}}, doi = {10.1039/c3sm51095f}, volume = {9}, year = {2013}, } @article{7775, abstract = {As a function of packing fraction at zero temperature and applied stress, an amorphous packing of spheres exhibits a jamming transition where the system is sensitive to boundary conditions even in the thermodynamic limit. Upon further compression, the system should become insensitive to boundary conditions provided it is sufficiently large. Here we explore the linear response to a large class of boundary perturbations in 2 and 3 dimensions. We consider each finite packing with periodic-boundary conditions as the basis of an infinite square or cubic lattice and study properties of vibrational modes at arbitrary wave vector. We find that the stability of such modes can be understood in terms of a competition between plane waves and the anomalous vibrational modes associated with the jamming transition; infinitesimal boundary perturbations become irrelevant for systems that are larger than a length scale that characterizes the transverse excitations. This previously identified length diverges at the jamming transition.}, author = {Schoenholz, Samuel S. and Goodrich, Carl Peter and Kogan, Oleg and Liu, Andrea J. and Nagel, Sidney R.}, issn = {1744-683X}, journal = {Soft Matter}, number = {46}, publisher = {Royal Society of Chemistry}, title = {{Stability of jammed packings II: The transverse length scale}}, doi = {10.1039/c3sm51096d}, volume = {9}, year = {2013}, } @article{7785, abstract = {Neural circuit assembly requires selection of specific cell fates, axonal trajectories, and synaptic targets. By analyzing the function of a secreted semaphorin, Sema-2b, in Drosophila olfactory receptor neuron (ORN) development, we identified multiple molecular and cellular mechanisms that link these events. Notch signaling limits Sema-2b expression to ventromedial ORN classes, within which Sema-2b cell-autonomously sensitizes ORN axons to external semaphorins. Central-brain-derived Sema-2a and Sema-2b attract Sema-2b-expressing axons to the ventromedial trajectory. In addition, Sema-2b/PlexB-mediated axon-axon interactions consolidate this trajectory choice and promote ventromedial axon-bundle formation. Selecting the correct developmental trajectory is ultimately essential for proper target choice. These findings demonstrate that Sema-2b couples ORN axon guidance to postsynaptic target neuron dendrite patterning well before the final target selection phase, and exemplify how a single guidance molecule can drive consecutive stages of neural circuit assembly with the help of sophisticated spatial and temporal regulation.}, author = {Joo, William J. and Sweeney, Lora Beatrice Jaeger and Liang, Liang and Luo, Liqun}, issn = {0896-6273}, journal = {Neuron}, number = {4}, pages = {673--686}, publisher = {Elsevier}, title = {{Linking cell fate, trajectory choice, and target selection: Genetic analysis of sema-2b in olfactory axon targeting}}, doi = {10.1016/j.neuron.2013.03.022}, volume = {78}, year = {2013}, }