@article{17734, abstract = {Electromagnetic (EM) counterparts to supermassive black hole binary mergers observed by LISA can be localized to within the field of view of astronomical instruments ~10 deg^2 hours to weeks prior to coalescence. The temporal coincidence of any prompt EM counterpart with a gravitationally-timed merger may offer the best chance of identifying a unique host galaxy. We discuss the challenges posed by searches for prompt EM counterparts and propose novel observational strategies to address them. In particular, we discuss the size and shape evolution of the LISA localization error ellipses on the sky, and quantify the requirements for dedicated EM surveys of the area prior to coalescence. A triggered EM counterpart search campaign will require monitoring a several-square degree area. It could aim for variability at the 24-27 mag level in optical bands, for example, which corresponds to 1-10% of the Eddington luminosity of the prime LISA sources of 10^6-10^7 Msun BHs at z=1-2, on time-scales of minutes to hours, the orbital time-scale of the binary in the last 2-4 weeks. A cross-correlation of the period of any variable EM signal with the quasi-periodic gravitational waveform over 10-1000 cycles may aid the detection. Alternatively, EM searches can detect a transient signal accompanying the coalescence. We highlight the measurement of differences in the arrival times of photons and gravitons from the same cosmological source as a valuable independent test of the massive character of gravity, and of possible violations of Lorentz invariance in the gravity sector.}, author = {Kocsis, Bence and Haiman, Zoltán and Menou, Kristen}, issn = {0004-637X}, journal = {The Astrophysical Journal}, number = {2}, pages = {870--887}, publisher = {American Astronomical Society}, title = {{Premerger localization of gravitational wave standard sirens with LISA: Triggered search for an electromagnetic counterpart}}, doi = {10.1086/590230}, volume = {684}, year = {2008}, } @inproceedings{17751, abstract = {With the help of numerical simulations, we examine two aspects of feedback from the first generation of stars on later star formation. First, we investigate the impact of relic HII regions on forming halos. We find that the positive and negative effects of such feedback nearly cancel because the increase in entropy due to heating is balanced by the increase in the H 2 fraction due to the free electrons. However, these halos can be delayed more easily by a background Lyman-Werner flux. Second, we show that HD cooling is important in halos which have been ionized and allowed to recombine. Gas is allowed to cool to the CMB temperature at densities around n∼10 4cm-3, reducing the accreted mass by a factor of a few. However, as the collapse proceeds, the central gas density exceeds the critical density of HD and heats until HD cooling is no longer important. Therefore the behaviour of the (smaller mass) core is relatively unaffected by HD cooling.}, author = {Bryan, Greg L. and McGreer, Ian D. and Mesinger, Andrei and Haiman, Zoltán}, booktitle = {AIP Conference Proceedings}, issn = {0094-243X}, location = {Santa Fe, NM, United States}, publisher = {American Institute of Physics}, title = {{Feedback effects on population III star formation}}, doi = {10.1063/1.2905582}, year = {2008}, } @article{17752, abstract = {Supermassive black hole binaries (BHBs) produced in galaxy mergers recoil at the time of their coalescence due to the emission of gravitational waves (GWs). We simulate the response of a thin, 2D disk of collisionless particles, initially on circular orbits around a 10^6 M_sun BHB, to kicks that are either parallel or perpendicular to the initial orbital plane. Typical kick velocities (v_k) can exceed the sound speed in a circumbinary gas disk. While the inner disk is strongly bound to the recoiling binary, the outer disk is only weakly bound or unbound. This leads to differential motions in the disturbed disk that increase with radius and can become supersonic at ~700 Schwarzschild radii for v_k ~500 km/s, implying that shocks form beyond this radius. We indeed find that kicks in the disk plane lead to immediate strong density enhancements (within weeks) in a tightly wound spiral caustic, propagating outward at the speed v_k. Concentric density enhancements are also observed for kicks perpendicular to the disk, but are weaker and develop into caustics only after a long delay (>1 year). Unless both BH spins are low or precisely aligned with the orbital angular momentum, a significant fraction (> several %) of kicks are sufficiently large and well aligned with the orbital plane for strong shocks to be produced. The shocks could result in an afterglow whose characteristic photon energy increases with time, from the UV (~10eV) to the soft X-ray (~100eV) range, between one month and one year after the merger. This could help identify EM counterparts to GW sources discovered by LISA.}, author = {Lippai, Zoltán and Frei, Zsolt and Haiman, Zoltán}, issn = {0004-637X}, journal = {The Astrophysical Journal}, number = {1}, pages = {L5--L8}, publisher = {American Astronomical Society}, title = {{Prompt shocks in the gas disk around a recoiling supermassive black hole binary}}, doi = {10.1086/587034}, volume = {676}, year = {2008}, } @article{17756, abstract = {At the epoch of reionization, when the high-redshift inter-galactic medium (IGM) is being enriched with metals, the 63.2 micron fine structure line of OI is pumped by the ~ 1300 AA soft UV background and introduces a spectral distortion in the Cosmic Microwave Background (CMB). Here we use a toy model for the spatial distribution of neutral oxygen, assuming metal bubbles surround dark matter halos, and compute the fluctuations of this distortion, and the angular power spectrum it imprints on the CMB. We discuss the dependence of the power spectrum on the velocity of the winds polluting the IGM with metals, the minimum mass of the halos producing these winds, and on the cosmic epoch when the OI pumping occurs. We find that, although the clustering signal of the CMB distortion is weak \delta y_{rms} ~ 10^{-7} (roughly corresponding to a temperature anisotropy of few nK), it may be reachable in deep integrations with high-sensitivity infrared detectors. Even without a detection, these instruments should be able to useful constraints on the heavy element enrichment history of the IGM.}, author = {Hernandez‐Monteagudo, Carlos and Haiman, Zoltán and Verde, Licia and Jimenez, Raul}, issn = {0004-637X}, journal = {The Astrophysical Journal}, number = {1}, pages = {33--39}, publisher = {American Astronomical Society}, title = {{Oxygen pumping. II. Probing the inhomogeneous metal enrichment at the epoch of reionization with high‐frequency CMB observations}}, doi = {10.1086/523872}, volume = {672}, year = {2008}, } @article{17762, abstract = {We conduct a Markov Chain Monte Carlo study of the Dvali-Gabadadze-Porrati self-accelerating braneworld scenario given the cosmic microwave background (CMB) anisotropy, supernovae and Hubble constant data by implementing an effective dark energy prescription for modified gravity into a standard Einstein-Boltzmann code. We find no way to alleviate the tension between distance measures and horizon-scale growth in this model. Growth alterations due to perturbations propagating into the bulk appear as excess CMB anisotropy at the lowest multipoles. In a flat cosmology, the maximum likelihood Dvali-Gabadadze-Porrati model is nominally a 5.3⁢𝜎 poorer fit than 𝛬⁢CDM. Curvature can reduce the tension between distance measures but only at the expense of exacerbating the problem with growth leading to a 4.8⁢𝜎 result that is dominated by the low multipole CMB temperature spectrum. While changing the initial conditions to reduce large-scale power can flatten the temperature spectrum, this also suppresses the large angle polarization spectrum in violation of recent results from the five-year Wilkinson Microwave Anisotropy Probe. The failure of this model highlights the power of combining growth and distance measures in cosmology as a test of gravity on the largest scales.}, author = {Fang, Wenjuan and Wang, Sheng and Hu, Wayne and Haiman, Zoltán and Hui, Lam and May, Morgan}, issn = {1550-7998}, journal = {Physical Review D}, number = {10}, publisher = {American Physical Society}, title = {{Challenges to the DGP model from horizon-scale growth and geometry}}, doi = {10.1103/physrevd.78.103509}, volume = {78}, year = {2008}, } @article{17773, abstract = {The notion that microparsec-scale black holes can be used to probe gigaparsec-scale physics may seem counterintuitive, at first. Yet, the gravitational observatory LISA will detect cosmologically-distant coalescing pairs of massive black holes, accurately measure their luminosity distance and help identify an electromagnetic counterpart or a host galaxy. A wide variety of new black hole studies and a gravitational version of Hubble’s diagram become possible, if host galaxies are successfully identified. Furthermore, if dark energy is a manifestation of large-scale modified gravity, deviations from general relativistic expectations could become apparent in a gravitational signal propagated over cosmological scales, especially when compared to the electromagnetic signal from a same source. Finally, since inspirals of white dwarfs into massive black holes at cosmological distances may permit pre-merger localizations, we suggest that careful monitoring of these events and any associated electromagnetic counterpart could lead to high-precision cosmological measurements with LISA.}, author = {Menou, Kristen and Haiman, Zoltán and Kocsis, Bence}, issn = {1387-6473}, journal = {New Astronomy Reviews}, number = {10-12}, pages = {884--890}, publisher = {Elsevier BV}, title = {{Cosmological physics with black holes (and possibly white dwarfs)}}, doi = {10.1016/j.newar.2008.03.020}, volume = {51}, year = {2008}, } @article{17778, abstract = {The earliest generation of stars and black holes must have established an early ‘Lyman–Werner’ background (LWB) at high redshift, prior to the epoch of reionization. Because of the long mean free path of photons with energies hν < 13.6 eV, the LWB was nearly uniform. However, some variation in the LWB is expected due to the discrete nature of the sources, and their highly clustered spatial distribution. In this paper, we compute the probability distribution function (PDF) of the LW flux that irradiates dark matter (DM) haloes collapsing at high redshift (z≈ 10). Our model accounts for (i) the clustering of DM haloes, (ii) Poisson fluctuations in the number of corresponding star-forming galaxies and (iii) scatter in the LW luminosity produced by haloes of a given mass (calibrated using local observations). We find that >99 per cent of the DM haloes are illuminated by an LW flux within a factor of 2 of the global mean value. However, a small fraction, ∼10^−8 to 10^−6, of DM haloes with virial temperatures Tvir≳ 10^4 K have a close luminous neighbour within ≲10 kpc, and are exposed to an LW flux exceeding the global mean by a factor of >20, or to J21,LW > 10^3 (in units of 10^−21 erg s^−1 Hz^−1 sr^−1 cm^−2). This large LW flux can photodissociate H2 molecules in the gas collapsing due to atomic cooling in these haloes, and prevent its further cooling and fragmentation. Such close halo pairs therefore provide possible sites in which primordial gas clouds collapse directly into massive black holes (MBH≈ 10^4−6M⊙), and subsequently grow into supermassive (MBH≳ 10^9M⊙) black holes by z≈ 6.}, author = {Dijkstra, Mark and Haiman, Zoltán and Mesinger, Andrei and Wyithe, J. Stuart B.}, issn = {0035-8711}, journal = {Monthly Notices of the Royal Astronomical Society}, number = {4}, pages = {1961--1972}, publisher = {Oxford University Press}, title = {{Fluctuations in the high-redshift Lyman-Werner background: Close halo pairs as the origin of supermassive black holes}}, doi = {10.1111/j.1365-2966.2008.14031.x}, volume = {391}, year = {2008}, } @article{17787, abstract = {One of the most dramatic signatures of the reionization era may be the enormous ionized bubbles around luminous quasars (with radii reaching ~40 comoving Mpc), which may survive as "fossil" ionized regions long after their source shuts off. Here we study how the inhomogeneous intergalactic medium (IGM) evolves inside such fossils. The average recombination rate declines rapidly with time, and the brief quasar episode significantly increases the mean free path inside the fossil bubbles. As a result, even a weak ionizing background generated by galaxies inside the fossil can maintain it in a relatively highly and uniformly ionized state. For example, galaxies that would ionize 20%-30% of hydrogen in a random patch of the IGM can maintain 80%-90% ionization inside the fossil for a duration much longer than the average recombination time in the IGM. Quasar fossils at z≲ 10 thus retain their identity for nearly a Hubble time and appear "gray," distinct from both the average IGM (which has a "Swiss cheese" ionization topology and a lower mean ionized fraction) and the fully ionized bubbles around active quasars. More distant fossils, at z≳ 10, have a weaker galaxy-generated ionizing background and a higher gas density, so they can attain a Swiss cheese topology similar to the rest of the IGM, but with a smaller contrast between the ionized bubbles and the partially neutral regions separating them. Analogous He III fossils should exist around the epoch of He II/He III reionization at z ∼ 3, although rapid recombination inside the He III fossils is more common. Our model of inhomogeneous recombination also applies to "double-reionization" models and shows that a nonmonotonic reionization history is even more unlikely than previously thought.}, author = {Furlanetto, Steven R. and Haiman, Zoltán and Oh, S. Peng}, issn = {0004-637X}, journal = {The Astrophysical Journal}, number = {1}, pages = {25--40}, publisher = {American Astronomical Society}, title = {{Fossil Ionized bubbles around dead quasars during reionization}}, doi = {10.1086/591047}, volume = {686}, year = {2008}, } @article{17788, abstract = {Nongravitational processes, such as feedback from galaxies and their active nuclei, are believed to have injected excess entropy into the intracluster gas, and therefore to have modified the density profiles in galaxy clusters during their formation. Here we study a simple model for this so-called preheating scenario, and ask (1) whether it can simultaneously explain both global X-ray scaling relations and number counts of galaxy clusters, and (2) whether the amount of entropy required evolves with redshift. We adopt a baseline entropy profile that fits recent hydrodynamic simulations, modify the hydrostatic equilibrium condition for the gas by including ≈20% nonthermal pressure support, and add an entropy floor K0 that is allowed to vary with redshift. We find that the observed luminosity-temperature (L − T) relations of low-redshift (⟨ z⟩ = 0.05) HIFLUGCS clusters and high-redshift (⟨ z⟩ = 0.80) WARPS clusters are best simultaneously reproduced with an entropy floor that evolves from ≈200 h^−1/3 keV cm^ 2 at z ≈ 0.8 to ≳300 h^−1/3 keV cm^ 2 at z < 0.05. This evolution may take place predominantly at low redshift (z≲ 0.2). If we restrict our analysis to the subset of bright (kT≳ 3 keV) clusters, we find that the evolving entropy floor can mimic a self-similar evolution in the L − T scaling relation. This degeneracy with self-similar evolution is, however, lifted when 0.5 keV ≲ kT≲ 3 keV clusters are included. Using the cosmological parameters from the WMAP 3 yr data, but treating σ8 as a free parameter, our model can reproduce the number counts of the X-ray galaxy clusters in the 158 deg2 ROSAT PSPC survey, with a best-fit value of σ8 = 0.80 ± 0.05.}, author = {Fang, Wenjuan and Haiman, Zoltán}, issn = {0004-637X}, journal = {The Astrophysical Journal}, number = {1}, pages = {200--213}, publisher = {American Astronomical Society}, title = {{An evolving entropy floor in the intracluster gas?}}, doi = {10.1086/587780}, volume = {680}, year = {2008}, } @article{17789, abstract = {Light-travel time delays distort the apparent shapes of H II regions surrounding bright quasars during early stages of cosmic reionization. Individual H II regions may remain undetectable in forthcoming redshifted 21 cm experiments. However, the systematic deformation along the line of sight may be detectable statistically, either by stacking tomographic 21 cm images of quasars identified, for example, by the James Webb Space Telescope, or as small-scale anisotropy in the three-dimensional 21 cm power spectrum. Here we consider the detectability of this effect. The anisotropy is largest when H II regions are large and expand rapidly, and we find that if bright quasars contributed to the early stages of reionization, then they can produce significant anisotropy, on scales comparable to the typical sizes of H II regions of the bright quasars (≲30 Mpc). The effect therefore cannot be ignored when analyzing future 21 cm power spectra on small scales. If 10% of the volume of the intergalactic medium at z≃ 10 is ionized by quasars with typical ionizing luminosity of S≳ 5 × 10^56 s^−1, the distortions cause an ≳10 percent enhancement of the 21 cm power spectrum in the radial (redshift) direction, relative to the transverse directions. The level of this anisotropy exceeds that due to redshift-space distortion and has the opposite sign. We show that ongoing experiments such as Murchison Widefield Array (MWA, formerly known as the Mileura Widefield Array) should be able to detect this effect. A detection would reveal the presence of bright quasars and shed light on the ionizing yield and age of the ionizing sources and the distribution and small-scale clumping of neutral intergalactic gas in their vicinity.}, author = {Sethi, Shiv and Haiman, Zoltán}, issn = {0004-637X}, journal = {The Astrophysical Journal}, number = {1}, pages = {1--13}, publisher = {American Astronomical Society}, title = {{Can we detect the anisotropic shapes of quasar H ii regions during reionization through the small‐scale redshifted 21 cm power spectrum?}}, doi = {10.1086/523787}, volume = {673}, year = {2008}, } @article{17804, abstract = {Primordial gas in protogalactic DM halos with virial temperatures Tvir≳ 104 K begins to cool and condense via atomic hydrogen. Provided that this gas is irradiated by a strong UV flux and remains free of H2 and other molecules, it has been proposed that the halo with Tvir ∼ 104 K may avoid fragmentation and lead to the rapid formation of an SMBH as massive as M ≈ 105–106 M☉. This "head start" would help explain the presence of SMBHs with inferred masses of several times 109 M☉, powering the bright quasars discovered in the SDSS at redshift z≳ 6. However, high-redshift DM halos with Tvir ∼ 104 K are likely already enriched with at least trace amounts of metals and dust produced by prior star formation in their progenitors. Here we study the thermal and chemical evolution of low-metallicity gas exposed to extremely strong UV radiation fields. Our results, obtained in one-zone models, suggest that gas fragmentation is inevitable above a critical metallicity, whose value is between Zcr ≈ 3 × 10−4 Z☉ (in the absence of dust) and as low as Zcr ≈ 5 × 10−6 Z☉ (with a dust-to-gas mass ratio of about 0.01Z/Z☉). We propose that when the metallicity exceeds these critical values, dense clusters of low-mass stars may form at the halo nucleus. Relatively massive stars in such a cluster can then rapidly coalesce into a single more massive object, which may produce an intermediate-mass BH remnant with a mass up to M≲ 102–103 M☉.}, author = {Omukai, K. and Schneider, R. and Haiman, Zoltán}, issn = {1538-4357}, journal = {The Astrophysical Journal}, number = {2}, pages = {801--814}, publisher = {American Astronomical Society}, title = {{Can supermassive black holes form in metal‐enriched high‐redshift protogalaxies?}}, doi = {10.1086/591636}, volume = {686}, year = {2008}, } @article{18032, abstract = {A comprehensive review is presented of single-molecule junction conductance measurements across families of molecules measured while breaking a gold point contact in a solution of molecules with amine end groups. A theoretical framework unifies the picture for the amine–gold link bonding and the tunnel coupling through the junction using density functional theory based calculations. The reproducible electrical characteristics and utility for many molecules is shown to result from the selective binding between the gold electrodes and amine link groups through a donor–acceptor bond to undercoordinated gold atoms. While the bond energy is modest, the maximum force sustained by the junction is comparable to, but less than, that required to break gold point contacts. The calculated tunnel coupling provides conductance trends for all 41 molecule measurements presented here, as well as insight into the variability of conductance due to the conformational changes within molecules with torsional degrees of freedom. The calculated trends agree to within a factor of 2 with the measured values for conductance ranging from 10−7G0 to 10−2G0, where G0 is the quantum of conductance (2e2/h).}, author = {Hybertsen, Mark S and Venkataraman, Latha and Klare, Jennifer E and Whalley, Adam C and Steigerwald, Michael L and Nuckolls, Colin}, issn = {1361-648X}, journal = {Journal of Physics: Condensed Matter}, number = {37}, publisher = {IOP Publishing}, title = {{Amine-linked single-molecule circuits: Systematic trends across molecular families}}, doi = {10.1088/0953-8984/20/37/374115}, volume = {20}, year = {2008}, } @inproceedings{18033, abstract = {We measure the conductance of over 30 amine terminated molecules by breaking Au point-contacts in a molecular solution at room temperature. We find that the variability of the observed conductance for the diamine molecule-Au junctions is much less than the variability for diisonitrile and dithiol-Au junctions. This narrow distribution enables unambiguous conductance measurements of single molecules. For an alkane diamine series with 2-8 carbon atoms in the hydrocarbon chain and for polyphenyl diamine with 1-3 benzene rings, our results show that conductance decreases exponentially with length. For biphenyl diamines with different substituents that alter the phenyl-phenyl dihedral angle, we find that the conductance decreases with increasing twist angle, following a cosine squared dependence. Finally, for a series of substituted benzene diamines, we find that electron donating substituents on the ring, which drive the occupied molecular orbitals up, increase the junction conductance while electron withdrawing substituents have the opposite effect. Thus for this measured series, conductance varies inversely with the calculated ionization potential of the molecules. These results reveal that the occupied states are closest to the gold Fermi energy, indicating that the tunneling transport through these molecules is analogous to hole tunneling through an insulating film.}, author = {Venkataraman, Latha}, booktitle = {2008 International Symposium on VLSI Technology, Systems and Applications}, issn = {1930-885X}, location = {Hsinchu, Taiwan}, pages = {64--65}, publisher = {IEEE}, title = {{Molecule Nanoelectronics}}, doi = {10.1109/vtsa.2008.4530800}, year = {2008}, } @article{18034, abstract = {The ability to perform optical measurements on a single molecule placed between two electrodes while also measuring the current flowing through it could herald a new generation of experiments on molecular junctions.}, author = {Venkataraman, Latha}, issn = {1748-3395}, journal = {Nature Nanotechnology}, number = {4}, pages = {187--188}, publisher = {Springer Nature}, title = {{Seeing is believing}}, doi = {10.1038/nnano.2008.81}, volume = {3}, year = {2008}, } @article{1826, abstract = {Proliferating cell populations at steady-state growth often exhibit broad protein distributions with exponential tails. The sources of this variation and its universality are of much theoretical interest. Here we address the problem by asymptotic analysis of the population balance equation. We show that the steady-state distribution tail is determined by a combination of protein production and cell division and is insensitive to other model details. Under general conditions this tail is exponential with a dependence on parameters consistent with experiment. We discuss the conditions for this effect to be dominant over other sources of variation and the relation to experiments.}, author = {Tamar Friedlander and Brenner, Naama}, journal = {Physical Review Letters}, number = {1}, publisher = {American Physical Society}, title = {{Cellular properties and population asymptotics in the population balance equation}}, doi = {10.1103/PhysRevLett.101.018104}, volume = {101}, year = {2008}, } @inproceedings{18337, abstract = {Matching of rigid shapes is an important problem in numerous applications across the boundary of computer vision, pattern recognition and computer graphics communities. A particularly challenging setting of this problem is partial matching, where the two shapes are dissimilar in general, but have significant similar parts. In this paper, we show a rigorous approach allowing to find matching parts of rigid shapes with controllable size and regularity. The regularity term we use is similar to the spirit of the Mumford-Shah functional, extended to non-Euclidean spaces. Numerical experiments show that the regularized partial matching produces better results compared to the non-regularized one.}, author = {Bronstein, Alexander and Bronstein, Michael M.}, booktitle = {10th European Conference on Computer Vision}, isbn = {9783540886853}, issn = {0302-9743}, location = {Marseille, France}, pages = {143--154}, publisher = {Springer Berlin Heidelberg}, title = {{Regularized partial matching of rigid shapes}}, doi = {10.1007/978-3-540-88688-4_11}, volume = {5303}, year = {2008}, } @article{18355, abstract = {Analysis of deformable two-dimensional shapes is an important problem, encountered in numerous pattern recognition, computer vision and computer graphics applications. In this paper, we address three major problems in the analysis of non-rigid shapes: similarity, partial similarity, and correspondence. We present an axiomatic construction of similarity criteria for deformation-invariant shape comparison, based on intrinsic geometric properties of the shapes, and show that such criteria are related to the Gromov-Hausdorff distance. Next, we extend the problem of similarity computation to shapes which have similar parts but are dissimilar when considered as a whole, and present a construction of set-valued distances, based on the notion of Pareto optimality. Finally, we show that the correspondence between non-rigid shapes can be obtained as a byproduct of the non-rigid similarity problem. As a numerical framework, we use the generalized multidimensional scaling (GMDS) method, which is the numerical core of the three problems addressed in this paper.}, author = {Bronstein, Alexander and Bronstein, Michael M. and Bruckstein, Alfred M. and Kimmel, Ron}, issn = {0920-5691}, journal = {International Journal of Computer Vision}, pages = {67--88}, publisher = {Springer Nature}, title = {{Analysis of two-dimensional non-rigid shapes}}, doi = {10.1007/s11263-007-0078-4}, volume = {78}, year = {2008}, } @inproceedings{18381, abstract = {Partial matching is probably one of the most challenging problems in nonrigid shape analysis. The problem consists of matching similar parts of shapes that are dissimilar on the whole and can assume different forms by undergoing nonrigid deformations. Conceptually, two shapes can be considered partially matching if they have significant similar parts, with the simplest definition of significance being the size of the parts. Thus, partial matching can be defined as a multicriterion optimization problem trying to simultaneously maximize the similarity and the size of these parts. In this paper, we propose a different definition of significance, taking into account the regularity of parts besides their size. The regularity term proposed here is similar to the spirit of the Mumford-Shah functional. Numerical experiments show that the regularized partial matching produces semantically better results compared to the non-regularized one.}, author = {Bronstein, Alexander and Bronstein, Michael M.}, booktitle = {2008 IEEE Computer Society Conference on Computer Vision and Pattern Recognition Workshops}, isbn = {9781424423392}, issn = {2160-7508}, location = {Anchorage, AK, United States}, publisher = {IEEE}, title = {{Not only size matters: Regularized partial matching of nonrigid shapes}}, doi = {10.1109/cvprw.2008.4563077}, year = {2008}, } @article{18431, abstract = {We present an efficient O(n) numerical algorithm for first-order approximation of geodesic distances on geometry images, where n is the number of points on the surface. The structure of our algorithm allows efficient implementation on parallel architectures. Two implementations on a SIMD processor and on a GPU are discussed. Numerical results demonstrate up to four orders of magnitude improvement in execution time compared to the state-of-the-art algorithms.}, author = {Weber, Ofir and Devir, Yohai S. and Bronstein, Alexander and Bronstein, Michael M. and Kimmel, Ron}, issn = {1557-7368}, journal = {ACM Transactions on Graphics}, number = {4}, publisher = {Association for Computing Machinery}, title = {{Parallel algorithms for approximation of distance maps on parametric surfaces}}, doi = {10.1145/1409625.1409626}, volume = {27}, year = {2008}, } @article{7752, author = {Robinson, Matthew Richard and Pilkington, Jill G. and Clutton-Brock, Tim H. and Pemberton, Josephine M. and Kruuk, Loeske. E.B.}, issn = {0960-9822}, journal = {Current Biology}, number = {10}, pages = {751--757}, publisher = {Elsevier}, title = {{Environmental heterogeneity generates fluctuating selection on a secondary sexual trait}}, doi = {10.1016/j.cub.2008.04.059}, volume = {18}, year = {2008}, }