[{"quality_controlled":"1","publication_status":"published","arxiv":1,"title":"Square-free values of reducible polynomials","language":[{"iso":"eng"}],"page":"1 - 18","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","volume":8,"author":[{"first_name":"Timothy D","full_name":"Browning, Timothy D","orcid":"0000-0002-8314-0177","last_name":"Browning","id":"35827D50-F248-11E8-B48F-1D18A9856A87"},{"last_name":"Booker","full_name":"Booker, Andrew","first_name":"Andrew"}],"intvolume":" 8","status":"public","oa":1,"date_published":"2016-06-01T00:00:00Z","publication":"Discrete Analysis","day":"01","extern":"1","type":"journal_article","year":"2016","month":"06","date_updated":"2021-01-12T06:52:49Z","publist_id":"7748","abstract":[{"lang":"eng","text":"We calculate admissible values of r such that a square-free polynomial with integer coefficients, no fixed prime divisor and irreducible factors of degree at most 3 takes infinitely many values that are a product of at most r distinct primes."}],"article_processing_charge":"No","_id":"173","citation":{"apa":"Browning, T. D., & Booker, A. (2016). Square-free values of reducible polynomials. Discrete Analysis. https://doi.org/10.19086/da.732","short":"T.D. Browning, A. Booker, Discrete Analysis 8 (2016) 1–18.","ama":"Browning TD, Booker A. Square-free values of reducible polynomials. Discrete Analysis. 2016;8:1-18. doi:10.19086/da.732","chicago":"Browning, Timothy D, and Andrew Booker. “Square-Free Values of Reducible Polynomials.” Discrete Analysis, 2016. https://doi.org/10.19086/da.732.","ieee":"T. D. Browning and A. Booker, “Square-free values of reducible polynomials,” Discrete Analysis, vol. 8. pp. 1–18, 2016.","ista":"Browning TD, Booker A. 2016. Square-free values of reducible polynomials. Discrete Analysis. 8, 1–18.","mla":"Browning, Timothy D., and Andrew Booker. “Square-Free Values of Reducible Polynomials.” Discrete Analysis, vol. 8, 2016, pp. 1–18, doi:10.19086/da.732."},"main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1511.00601"}],"article_type":"original","external_id":{"arxiv":["1511.00601"]},"date_created":"2018-12-11T11:45:00Z","doi":"10.19086/da.732"},{"type":"journal_article","publication_identifier":{"issn":["0004-637X","1538-4357"]},"month":"09","year":"2016","article_number":"110","date_published":"2016-09-12T00:00:00Z","publisher":"American Astronomical Society","publication":"The Astrophysical Journal","day":"12","extern":"1","article_processing_charge":"No","citation":{"chicago":"Inayoshi, Kohei, and Zoltán Haiman. “Is There a Maximum Mass for Black Holes in Galactic Nuclei?” The Astrophysical Journal. American Astronomical Society, 2016. https://doi.org/10.3847/0004-637x/828/2/110.","short":"K. Inayoshi, Z. Haiman, The Astrophysical Journal 828 (2016).","ama":"Inayoshi K, Haiman Z. Is there a maximum mass for black holes in galactic nuclei? The Astrophysical Journal. 2016;828(2). doi:10.3847/0004-637x/828/2/110","ieee":"K. Inayoshi and Z. Haiman, “Is there a maximum mass for black holes in galactic nuclei?,” The Astrophysical Journal, vol. 828, no. 2. American Astronomical Society, 2016.","mla":"Inayoshi, Kohei, and Zoltán Haiman. “Is There a Maximum Mass for Black Holes in Galactic Nuclei?” The Astrophysical Journal, vol. 828, no. 2, 110, American Astronomical Society, 2016, doi:10.3847/0004-637x/828/2/110.","ista":"Inayoshi K, Haiman Z. 2016. Is there a maximum mass for black holes in galactic nuclei? The Astrophysical Journal. 828(2), 110.","apa":"Inayoshi, K., & Haiman, Z. (2016). Is there a maximum mass for black holes in galactic nuclei? The Astrophysical Journal. American Astronomical Society. https://doi.org/10.3847/0004-637x/828/2/110"},"main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.1601.02611"}],"_id":"17618","external_id":{"arxiv":["1601.02611"]},"date_created":"2024-09-05T13:44:44Z","article_type":"original","doi":"10.3847/0004-637x/828/2/110","date_updated":"2024-09-24T08:11:51Z","scopus_import":"1","abstract":[{"lang":"eng","text":"The largest observed supermassive black holes (SMBHs) have a mass of M_BH ~ 10^{10} M_sun, nearly independent of redshift, from the local (z~0) to the early (z>6) Universe. We suggest that the growth of SMBHs above a few 10^{10} M_sun is prevented by small-scale accretion physics, independent of the properties of their host galaxies or of cosmology. Growing more massive BHs requires a gas supply rate from galactic scales onto a nuclear region as high as >10^3 M_sun/yr. At such a high accretion rate, most of the gas converts to stars at large radii (~10-100 pc), well before reaching the BH. We adopt a simple model (Thompson et al. 2005) for a star-forming accretion disk, and find that the accretion rate in the sub-pc nuclear region is reduced to the smaller value of at most a few M_sun/yr. This prevents SMBHs from growing above ~10^{11} M_sun in the age of the Universe. Furthermore, once a SMBH reaches a sufficiently high mass, this rate falls below the critical value at which the accretion flow becomes advection dominated. Once this transition occurs, BH feeding can be suppressed by strong outflows and jets from hot gas near the BH. We find that the maximum SMBH mass, given by this transition, is between M_{BH,max} ~ (1-6) * 10^{10} M_sun, depending primarily on the efficiency of angular momentum transfer inside the galactic disk, and not on other properties of the host galaxy."}],"title":"Is there a maximum mass for black holes in galactic nuclei?","arxiv":1,"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"oa_version":"Preprint","volume":828,"quality_controlled":"1","publication_status":"published","status":"public","oa":1,"author":[{"last_name":"Inayoshi","first_name":"Kohei","full_name":"Inayoshi, Kohei"},{"full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"}],"issue":"2","intvolume":" 828"},{"quality_controlled":"1","publication_status":"published","title":"Lyα emission-line reconstruction for high-z QSOs","page":"1814-1838","language":[{"iso":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","oa_version":"Published Version","volume":466,"author":[{"last_name":"Greig","first_name":"Bradley","full_name":"Greig, Bradley"},{"last_name":"Mesinger","full_name":"Mesinger, Andrei","first_name":"Andrei"},{"last_name":"McGreer","first_name":"Ian D.","full_name":"McGreer, Ian D."},{"last_name":"Gallerani","full_name":"Gallerani, Simona","first_name":"Simona"},{"full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"}],"intvolume":" 466","issue":"2","status":"public","oa":1,"date_published":"2016-12-10T00:00:00Z","publication":"Monthly Notices of the Royal Astronomical Society","publisher":"Oxford University Press","day":"10","extern":"1","publication_identifier":{"issn":["0035-8711","1365-2966"]},"type":"journal_article","year":"2016","month":"12","date_updated":"2024-09-24T08:31:25Z","scopus_import":"1","abstract":[{"text":"We introduce an intrinsic Lyα emission-line profile reconstruction method for high-z quasars (QSOs). This approach utilises a covariance matrix of emission-line properties obtained from a large, moderate-z (2 ≤ z ≤ 2.5), high signal to noise (S/N > 15) sample of BOSS QSOs. For each QSO, we complete a Monte Carlo Markov Chain fitting of the continuum and emission-line properties and perform a visual quality assessment to construct a large data base of robustly fit spectra. With this data set, we construct a covariance matrix to describe the correlations between the high-ionization emission lines Lyα, C iv, Si iv +O iv] and C iii], and find it to be well approximated by an N-dimensional Gaussian distribution. This covariance matrix characterizes the correlations between the linewidth, peak height and velocity offset from systemic while also allowing for the existence of broad- and narrow-line components for Lyα and C iv. We illustrate how this covariance matrix allows us to statistically characterize the intrinsic Lyα line solely from the observed spectrum redward of 1275 Å. This procedure can be used to reconstruct the intrinsic Lyα line emission profile in cases where Lyα may otherwise be obscured. Applying this reconstruction method to our sample of QSOs, we recovered the Lyα line flux to within 15 per cent of the measured flux at 1205 Å (1220 Å) ∼85 (90) per cent of the time.","lang":"eng"}],"article_processing_charge":"No","_id":"17621","citation":{"apa":"Greig, B., Mesinger, A., McGreer, I. D., Gallerani, S., & Haiman, Z. (2016). Lyα emission-line reconstruction for high-z QSOs. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw3210","ama":"Greig B, Mesinger A, McGreer ID, Gallerani S, Haiman Z. Lyα emission-line reconstruction for high-z QSOs. Monthly Notices of the Royal Astronomical Society. 2016;466(2):1814-1838. doi:10.1093/mnras/stw3210","chicago":"Greig, Bradley, Andrei Mesinger, Ian D. McGreer, Simona Gallerani, and Zoltán Haiman. “Lyα Emission-Line Reconstruction for High-z QSOs.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw3210.","ieee":"B. Greig, A. Mesinger, I. D. McGreer, S. Gallerani, and Z. Haiman, “Lyα emission-line reconstruction for high-z QSOs,” Monthly Notices of the Royal Astronomical Society, vol. 466, no. 2. Oxford University Press, pp. 1814–1838, 2016.","short":"B. Greig, A. Mesinger, I.D. McGreer, S. Gallerani, Z. Haiman, Monthly Notices of the Royal Astronomical Society 466 (2016) 1814–1838.","mla":"Greig, Bradley, et al. “Lyα Emission-Line Reconstruction for High-z QSOs.” Monthly Notices of the Royal Astronomical Society, vol. 466, no. 2, Oxford University Press, 2016, pp. 1814–38, doi:10.1093/mnras/stw3210.","ista":"Greig B, Mesinger A, McGreer ID, Gallerani S, Haiman Z. 2016. Lyα emission-line reconstruction for high-z QSOs. Monthly Notices of the Royal Astronomical Society. 466(2), 1814–1838."},"main_file_link":[{"url":"https://doi.org/10.1093/mnras/stw3210","open_access":"1"}],"article_type":"original","date_created":"2024-09-05T13:49:52Z","doi":"10.1093/mnras/stw3210"},{"main_file_link":[{"url":" https://doi.org/10.48550/arXiv.1605.01100","open_access":"1"}],"citation":{"apa":"Petri, A., May, M., & Haiman, Z. (2016). Cosmology with photometric weak lensing surveys: Constraints with redshift tomography of convergence peaks and moments. Physical Review D. American Physical Society. https://doi.org/10.1103/physrevd.94.063534","ama":"Petri A, May M, Haiman Z. Cosmology with photometric weak lensing surveys: Constraints with redshift tomography of convergence peaks and moments. Physical Review D. 2016;94(6). doi:10.1103/physrevd.94.063534","chicago":"Petri, Andrea, Morgan May, and Zoltán Haiman. “Cosmology with Photometric Weak Lensing Surveys: Constraints with Redshift Tomography of Convergence Peaks and Moments.” Physical Review D. American Physical Society, 2016. https://doi.org/10.1103/physrevd.94.063534.","ieee":"A. Petri, M. May, and Z. Haiman, “Cosmology with photometric weak lensing surveys: Constraints with redshift tomography of convergence peaks and moments,” Physical Review D, vol. 94, no. 6. American Physical Society, 2016.","short":"A. Petri, M. May, Z. Haiman, Physical Review D 94 (2016).","mla":"Petri, Andrea, et al. “Cosmology with Photometric Weak Lensing Surveys: Constraints with Redshift Tomography of Convergence Peaks and Moments.” Physical Review D, vol. 94, no. 6, 063534, American Physical Society, 2016, doi:10.1103/physrevd.94.063534.","ista":"Petri A, May M, Haiman Z. 2016. Cosmology with photometric weak lensing surveys: Constraints with redshift tomography of convergence peaks and moments. Physical Review D. 94(6), 063534."},"_id":"17626","article_processing_charge":"No","doi":"10.1103/physrevd.94.063534","date_created":"2024-09-05T13:55:24Z","external_id":{"arxiv":["1605.01100"]},"article_type":"original","scopus_import":"1","date_updated":"2024-09-24T08:54:34Z","abstract":[{"text":"Weak gravitational lensing is becoming a mature technique for constraining cosmological parameters, and future surveys will be able to constrain the dark energy equation of state 𝑤. When analyzing galaxy surveys, redshift information has proven to be a valuable addition to angular shear correlations. We forecast parameter constraints on the triplet (Ω𝑚,𝑤,𝜎8) for a LSST-like photometric galaxy survey, using tomography of the shear-shear power spectrum, convergence peak counts and higher convergence moments. We find that redshift tomography with the power spectrum reduces the area of the 1𝜎 confidence interval in (Ω𝑚,𝑤) space by a factor of 8 with respect to the case of the single highest redshift bin. We also find that adding non-Gaussian information from the peak counts and higher-order moments of the convergence field and its spatial derivatives further reduces the constrained area in (Ω𝑚,𝑤) by factors of 3 and 4, respectively. When we add cosmic microwave background parameter priors from Planck to our analysis, tomography improves power spectrum constraints by a factor of 3. Adding moments yields an improvement by an additional factor of 2, and adding both moments and peaks improves by almost a factor of 3 over power spectrum tomography alone. We evaluate the effect of uncorrected systematic photometric redshift errors on the parameter constraints. We find that different statistics lead to different bias directions in parameter space, suggesting the possibility of eliminating this bias via self-calibration.","lang":"eng"}],"type":"journal_article","publication_identifier":{"issn":["2470-0010","2470-0029"]},"month":"09","year":"2016","publisher":"American Physical Society","publication":"Physical Review D","date_published":"2016-09-30T00:00:00Z","article_number":"063534","extern":"1","day":"30","status":"public","oa":1,"author":[{"first_name":"Andrea","full_name":"Petri, Andrea","last_name":"Petri"},{"last_name":"May","first_name":"Morgan","full_name":"May, Morgan"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"}],"intvolume":" 94","issue":"6","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"title":"Cosmology with photometric weak lensing surveys: Constraints with redshift tomography of convergence peaks and moments","arxiv":1,"volume":94,"oa_version":"Preprint","quality_controlled":"1","publication_status":"published"},{"title":"Sample variance in weak lensing: How many simulations are required?","arxiv":1,"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"oa_version":"Preprint","volume":93,"quality_controlled":"1","publication_status":"published","status":"public","oa":1,"author":[{"first_name":"Andrea","full_name":"Petri, Andrea","last_name":"Petri"},{"full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"},{"last_name":"May","full_name":"May, Morgan","first_name":"Morgan"}],"intvolume":" 93","issue":"6","type":"journal_article","publication_identifier":{"issn":["2470-0010","2470-0029"]},"month":"03","year":"2016","article_number":"063524","date_published":"2016-03-24T00:00:00Z","publisher":"American Physical Society","publication":"Physical Review D","day":"24","extern":"1","article_processing_charge":"No","main_file_link":[{"url":" https://doi.org/10.48550/arXiv.1601.06792","open_access":"1"}],"citation":{"ama":"Petri A, Haiman Z, May M. Sample variance in weak lensing: How many simulations are required? Physical Review D. 2016;93(6). doi:10.1103/physrevd.93.063524","ieee":"A. Petri, Z. Haiman, and M. May, “Sample variance in weak lensing: How many simulations are required?,” Physical Review D, vol. 93, no. 6. American Physical Society, 2016.","short":"A. Petri, Z. Haiman, M. May, Physical Review D 93 (2016).","chicago":"Petri, Andrea, Zoltán Haiman, and Morgan May. “Sample Variance in Weak Lensing: How Many Simulations Are Required?” Physical Review D. American Physical Society, 2016. https://doi.org/10.1103/physrevd.93.063524.","ista":"Petri A, Haiman Z, May M. 2016. Sample variance in weak lensing: How many simulations are required? Physical Review D. 93(6), 063524.","mla":"Petri, Andrea, et al. “Sample Variance in Weak Lensing: How Many Simulations Are Required?” Physical Review D, vol. 93, no. 6, 063524, American Physical Society, 2016, doi:10.1103/physrevd.93.063524.","apa":"Petri, A., Haiman, Z., & May, M. (2016). Sample variance in weak lensing: How many simulations are required? Physical Review D. American Physical Society. https://doi.org/10.1103/physrevd.93.063524"},"_id":"17628","date_created":"2024-09-05T13:57:57Z","external_id":{"arxiv":["1601.06792"]},"article_type":"original","doi":"10.1103/physrevd.93.063524","date_updated":"2024-09-24T09:17:03Z","scopus_import":"1","abstract":[{"lang":"eng","text":"Constraining cosmology using weak gravitational lensing consists of comparing a measured feature vector of dimension 𝑁𝑏 with its simulated counterpart. An accurate estimate of the 𝑁𝑏×𝑁𝑏 feature covariance matrix 𝐂 is essential to obtain accurate parameter confidence intervals. When 𝐂 is measured from a set of simulations, an important question is how large this set should be. To answer this question, we construct different ensembles of 𝑁𝑟 realizations of the shear field, using a common randomization procedure that recycles the outputs from a smaller number 𝑁𝑠≤𝑁𝑟 of independent ray-tracing 𝑁-body simulations. We study parameter confidence intervals as a function of (𝑁𝑠, 𝑁𝑟) in the range 1≤𝑁𝑠≤200 and 1≤𝑁𝑟≲105. Previous work [S. Dodelson and M. D. Schneider, Phys. Rev. D 88, 063537 (2013)] has shown that Gaussian noise in the feature vectors (from which the covariance is estimated) lead, at quadratic order, to an 𝑂(1/𝑁𝑟) degradation of the parameter confidence intervals. Using a variety of lensing features measured in our simulations, including shear-shear power spectra and peak counts, we show that cubic and quartic covariance fluctuations lead to additional 𝑂(1/𝑁2𝑟) error degradation that is not negligible when 𝑁𝑟 is only a factor of few larger than 𝑁𝑏. We study the large 𝑁𝑟 limit, and find that a single, 240 Mpc/ℎ sized 5123-particle 𝑁-body simulation (𝑁𝑠=1) can be repeatedly recycled to produce as many as 𝑁𝑟=few×104 shear maps whose power spectra and high-significance peak counts can be treated as statistically independent. As a result, a small number of simulations (𝑁𝑠=1 or 2) is sufficient to forecast parameter confidence intervals at percent accuracy."}]},{"external_id":{"arxiv":["1606.01318"]},"date_created":"2024-09-06T07:28:02Z","article_type":"original","doi":"10.1103/physrevd.94.043533","article_processing_charge":"No","main_file_link":[{"url":" https://doi.org/10.48550/arXiv.1606.01318","open_access":"1"}],"citation":{"short":"J. Liu, Z. Haiman, Physical Review D 94 (2016).","chicago":"Liu, Jia, and Zoltán Haiman. “Origin of Weak Lensing Convergence Peaks.” Physical Review D. American Physical Society, 2016. https://doi.org/10.1103/physrevd.94.043533.","ieee":"J. Liu and Z. Haiman, “Origin of weak lensing convergence peaks,” Physical Review D, vol. 94, no. 4. American Physical Society, 2016.","ama":"Liu J, Haiman Z. Origin of weak lensing convergence peaks. Physical Review D. 2016;94(4). doi:10.1103/physrevd.94.043533","mla":"Liu, Jia, and Zoltán Haiman. “Origin of Weak Lensing Convergence Peaks.” Physical Review D, vol. 94, no. 4, 043533, American Physical Society, 2016, doi:10.1103/physrevd.94.043533.","ista":"Liu J, Haiman Z. 2016. Origin of weak lensing convergence peaks. Physical Review D. 94(4), 043533.","apa":"Liu, J., & Haiman, Z. (2016). Origin of weak lensing convergence peaks. Physical Review D. American Physical Society. https://doi.org/10.1103/physrevd.94.043533"},"_id":"17649","abstract":[{"text":"Weak lensing convergence peaks are a promising tool to probe nonlinear structure evolution at late times, providing additional cosmological information beyond second-order statistics. Previous theoretical and observational studies have shown that the cosmological constraints on Ωm and σ8 are improved by a factor of up to ~ 2 when peak counts and second-order statistics are combined, compared to using the latter alone. We study the origin of lensing peaks using observational data from the 154 deg2 Canada-France-Hawaii Telescope Lensing Survey. We found that while high peaks (with height κ >3.5 σκ, where σκ is the r.m.s. of the convergence κ) are typically due to one single massive halo of ~1015M⊙, low peaks (κ <~ σκ) are associated with constellations of 2-8 smaller halos (<~1013M⊙). In addition, halos responsible for forming low peaks are found to be significantly offset from the line-of-sight towards the peak center (impact parameter >~ their virial radii), compared with ~0.25 virial radii for halos linked with high peaks, hinting that low peaks are more immune to baryonic processes whose impact is confined to the inner regions of the dark matter halos. Our findings are in good agreement with results from the simulation work by Yang el al. (2011).","lang":"eng"}],"date_updated":"2024-09-24T12:59:05Z","scopus_import":"1","month":"08","year":"2016","type":"journal_article","publication_identifier":{"issn":["2470-0010","2470-0029"]},"day":"26","extern":"1","date_published":"2016-08-26T00:00:00Z","article_number":"043533","publisher":"American Physical Society","publication":"Physical Review D","oa":1,"status":"public","issue":"4","intvolume":" 94","author":[{"last_name":"Liu","first_name":"Jia","full_name":"Liu, Jia"},{"last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","full_name":"Haiman, Zoltán"}],"oa_version":"Preprint","volume":94,"title":"Origin of weak lensing convergence peaks","arxiv":1,"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"publication_status":"published","quality_controlled":"1"},{"publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society: Letters","date_published":"2016-04-14T00:00:00Z","extern":"1","day":"14","type":"journal_article","publication_identifier":{"issn":["1745-3925","1745-3933"]},"month":"04","year":"2016","scopus_import":"1","date_updated":"2024-09-24T14:19:51Z","abstract":[{"text":"We explore the formation of massive high-redshift Population III (Pop III) galaxies through photoionization feedback. We consider dark matter haloes formed from progenitors that have undergone no star formation as a result of early reionization and photoevaporation caused by a nearby galaxy. Once such a halo reaches ≈109 M⊙, corresponding to the Jeans mass of the photoheated intergalactic medium at z ≈ 7, pristine gas is able to collapse into the halo, potentially producing a massive Pop III starburst. We suggest that this scenario may explain the recent observation of strong He ii 1640 Å line emission in CR 7, which is consistent with ∼107 M⊙ of young Pop III stars. Such a large mass of Pop III stars is unlikely without the photoionization feedback scenario, because star formation is expected to inject metals into haloes above the atomic cooling threshold (∼108 M⊙ at z ≈ 7). We use merger trees to analytically estimate the abundance of observable Pop III galaxies formed through this channel, and find a number density of ≈10−7 Mpc−3 at z = 6.6 (the redshift of CR 7). This is approximately a factor of 10 lower than the density of Ly α emitters as bright as CR 7.","lang":"eng"}],"main_file_link":[{"url":"https://doi.org/10.1093/mnrasl/slw071","open_access":"1"}],"citation":{"apa":"Visbal, E., Haiman, Z., & Bryan, G. L. (2016). Formation of massive Population III galaxies through photoionization feedback: A possible explanation for CR 7. Monthly Notices of the Royal Astronomical Society: Letters. Oxford University Press. https://doi.org/10.1093/mnrasl/slw071","ieee":"E. Visbal, Z. Haiman, and G. L. Bryan, “Formation of massive Population III galaxies through photoionization feedback: A possible explanation for CR 7,” Monthly Notices of the Royal Astronomical Society: Letters, vol. 460, no. 1. Oxford University Press, pp. L59–L63, 2016.","ama":"Visbal E, Haiman Z, Bryan GL. Formation of massive Population III galaxies through photoionization feedback: A possible explanation for CR 7. Monthly Notices of the Royal Astronomical Society: Letters. 2016;460(1):L59-L63. doi:10.1093/mnrasl/slw071","chicago":"Visbal, Eli, Zoltán Haiman, and Greg L. Bryan. “Formation of Massive Population III Galaxies through Photoionization Feedback: A Possible Explanation for CR 7.” Monthly Notices of the Royal Astronomical Society: Letters. Oxford University Press, 2016. https://doi.org/10.1093/mnrasl/slw071.","short":"E. Visbal, Z. Haiman, G.L. Bryan, Monthly Notices of the Royal Astronomical Society: Letters 460 (2016) L59–L63.","mla":"Visbal, Eli, et al. “Formation of Massive Population III Galaxies through Photoionization Feedback: A Possible Explanation for CR 7.” Monthly Notices of the Royal Astronomical Society: Letters, vol. 460, no. 1, Oxford University Press, 2016, pp. L59–63, doi:10.1093/mnrasl/slw071.","ista":"Visbal E, Haiman Z, Bryan GL. 2016. Formation of massive Population III galaxies through photoionization feedback: A possible explanation for CR 7. Monthly Notices of the Royal Astronomical Society: Letters. 460(1), L59–L63."},"_id":"17654","article_processing_charge":"No","doi":"10.1093/mnrasl/slw071","date_created":"2024-09-06T07:32:23Z","article_type":"original","quality_controlled":"1","publication_status":"published","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"page":"L59-L63","title":"Formation of massive Population III galaxies through photoionization feedback: A possible explanation for CR 7","volume":460,"oa_version":"Published Version","author":[{"last_name":"Visbal","full_name":"Visbal, Eli","first_name":"Eli"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"last_name":"Bryan","full_name":"Bryan, Greg L.","first_name":"Greg L."}],"intvolume":" 460","issue":"1","status":"public","oa":1},{"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stw2260"}],"citation":{"apa":"Stone, N. C., Metzger, B. D., & Haiman, Z. (2016). Assisted inspirals of stellar mass black holes embedded in AGN discs: Solving the ‘final au problem.’ Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw2260","ieee":"N. C. Stone, B. D. Metzger, and Z. Haiman, “Assisted inspirals of stellar mass black holes embedded in AGN discs: Solving the ‘final au problem,’” Monthly Notices of the Royal Astronomical Society, vol. 464, no. 1. Oxford University Press, pp. 946–954, 2016.","ama":"Stone NC, Metzger BD, Haiman Z. Assisted inspirals of stellar mass black holes embedded in AGN discs: Solving the ‘final au problem.’ Monthly Notices of the Royal Astronomical Society. 2016;464(1):946-954. doi:10.1093/mnras/stw2260","chicago":"Stone, Nicholas C., Brian D. Metzger, and Zoltán Haiman. “Assisted Inspirals of Stellar Mass Black Holes Embedded in AGN Discs: Solving the ‘Final Au Problem.’” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw2260.","short":"N.C. Stone, B.D. Metzger, Z. Haiman, Monthly Notices of the Royal Astronomical Society 464 (2016) 946–954.","mla":"Stone, Nicholas C., et al. “Assisted Inspirals of Stellar Mass Black Holes Embedded in AGN Discs: Solving the ‘Final Au Problem.’” Monthly Notices of the Royal Astronomical Society, vol. 464, no. 1, Oxford University Press, 2016, pp. 946–54, doi:10.1093/mnras/stw2260.","ista":"Stone NC, Metzger BD, Haiman Z. 2016. Assisted inspirals of stellar mass black holes embedded in AGN discs: Solving the ‘final au problem’. Monthly Notices of the Royal Astronomical Society. 464(1), 946–954."},"_id":"17656","article_processing_charge":"No","doi":"10.1093/mnras/stw2260","date_created":"2024-09-06T07:35:10Z","article_type":"original","scopus_import":"1","date_updated":"2024-09-25T07:05:41Z","abstract":[{"lang":"eng","text":"We explore the evolution of stellar mass black hole binaries (BHBs) which are formed in the self-gravitating discs of active galactic nuclei (AGN). Hardening due to three-body scattering and gaseous drag are effective mechanisms that reduce the semimajor axis of a BHB to radii where gravitational waves take over, on time-scales shorter than the typical lifetime of the AGN disc. Taking observationally motivated assumptions for the rate of star formation in AGN discs, we find a rate of disc-induced BHB mergers (| $\\mathcal {R} \\sim 3\\ {\\rm yr}^{-1}\\ {\\rm Gpc}^{-3}$ |, but with large uncertainties) that is comparable with existing estimates of the field rate of BHB mergers, and the approximate BHB merger rate implied by the recent Advanced LIGO detection of GW150914. BHBs formed thorough this channel will frequently be associated with luminous AGN, which are relatively rare within the sky error regions of future gravitational wave detector arrays. This channel could also possess a (potentially transient) electromagnetic counterpart due to super-Eddington accretion on to the stellar mass black hole following the merger."}],"type":"journal_article","publication_identifier":{"issn":["0035-8711","1365-2966"]},"month":"09","year":"2016","publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","date_published":"2016-09-08T00:00:00Z","extern":"1","day":"08","status":"public","oa":1,"author":[{"first_name":"Nicholas C.","full_name":"Stone, Nicholas C.","last_name":"Stone"},{"last_name":"Metzger","first_name":"Brian D.","full_name":"Metzger, Brian D."},{"full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"}],"intvolume":" 464","issue":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","page":"946-954","language":[{"iso":"eng"}],"title":"Assisted inspirals of stellar mass black holes embedded in AGN discs: Solving the ‘final au problem’","volume":464,"oa_version":"Published Version","quality_controlled":"1","publication_status":"published"},{"month":"04","year":"2016","type":"journal_article","publication_identifier":{"issn":["0035-8711","1365-2966"]},"day":"06","extern":"1","date_published":"2016-04-06T00:00:00Z","publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2024-09-06T07:36:39Z","article_type":"original","doi":"10.1093/mnras/stw792","article_processing_charge":"No","citation":{"apa":"D’Orazio, D. J., Haiman, Z., Duffell, P., MacFadyen, A., & Farris, B. (2016). A transition in circumbinary accretion discs at a binary mass ratio of 1:25. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw792","ieee":"D. J. D’Orazio, Z. Haiman, P. Duffell, A. MacFadyen, and B. Farris, “A transition in circumbinary accretion discs at a binary mass ratio of 1:25,” Monthly Notices of the Royal Astronomical Society, vol. 459, no. 3. Oxford University Press, pp. 2379–2393, 2016.","ama":"D’Orazio DJ, Haiman Z, Duffell P, MacFadyen A, Farris B. A transition in circumbinary accretion discs at a binary mass ratio of 1:25. Monthly Notices of the Royal Astronomical Society. 2016;459(3):2379-2393. doi:10.1093/mnras/stw792","chicago":"D’Orazio, Daniel J., Zoltán Haiman, Paul Duffell, Andrew MacFadyen, and Brian Farris. “A Transition in Circumbinary Accretion Discs at a Binary Mass Ratio of 1:25.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw792.","short":"D.J. D’Orazio, Z. Haiman, P. Duffell, A. MacFadyen, B. Farris, Monthly Notices of the Royal Astronomical Society 459 (2016) 2379–2393.","mla":"D’Orazio, Daniel J., et al. “A Transition in Circumbinary Accretion Discs at a Binary Mass Ratio of 1:25.” Monthly Notices of the Royal Astronomical Society, vol. 459, no. 3, Oxford University Press, 2016, pp. 2379–93, doi:10.1093/mnras/stw792.","ista":"D’Orazio DJ, Haiman Z, Duffell P, MacFadyen A, Farris B. 2016. A transition in circumbinary accretion discs at a binary mass ratio of 1:25. Monthly Notices of the Royal Astronomical Society. 459(3), 2379–2393."},"main_file_link":[{"url":"https://doi.org/10.1093/mnras/stw792","open_access":"1"}],"_id":"17658","abstract":[{"lang":"eng","text":"We study circumbinary accretion discs in the framework of the restricted three-body problem (R3Bp) and via numerically solving the height-integrated equations of viscous hydrodynamics. Varying the mass ratio of the binary, we find a pronounced change in the behaviour of the disc near mass ratio q ≡ Ms/Mp ∼ 0.04. For mass ratios above q = 0.04, solutions for the hydrodynamic flow transition from steady, to strongly fluctuating; a narrow annular gap in the surface density around the secondary's orbit changes to a hollow central cavity; and a spatial symmetry is lost, resulting in a lopsided disc. This phase transition is coincident with the mass ratio above which stable orbits do not exist around the L4 and L5 equilibrium points of the R3Bp. Using the disco code, we find that for thin discs, for which a gap or cavity can remain open, the mass ratio of the transition is relatively insensitive to disc viscosity and pressure. The q = 0.04 transition has relevance for the evolution of massive black hole binary+disc systems at the centres of galactic nuclei, as well as for young stellar binaries and possibly planets around brown dwarfs."}],"date_updated":"2024-09-25T07:14:30Z","scopus_import":"1","oa_version":"Published Version","volume":459,"title":"A transition in circumbinary accretion discs at a binary mass ratio of 1:25","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","page":"2379-2393","language":[{"iso":"eng"}],"publication_status":"published","quality_controlled":"1","oa":1,"status":"public","issue":"3","intvolume":" 459","author":[{"first_name":"Daniel J.","full_name":"D'Orazio, Daniel J.","last_name":"D'Orazio"},{"full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"},{"first_name":"Paul","full_name":"Duffell, Paul","last_name":"Duffell"},{"full_name":"MacFadyen, Andrew","first_name":"Andrew","last_name":"MacFadyen"},{"last_name":"Farris","first_name":"Brian","full_name":"Farris, Brian"}]},{"author":[{"full_name":"Inayoshi, Kohei","first_name":"Kohei","last_name":"Inayoshi"},{"last_name":"Kashiyama","full_name":"Kashiyama, Kazumi","first_name":"Kazumi"},{"last_name":"Visbal","first_name":"Eli","full_name":"Visbal, Eli"},{"full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"}],"issue":"3","intvolume":" 461","status":"public","oa":1,"quality_controlled":"1","publication_status":"published","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","page":"2722-2727","language":[{"iso":"eng"}],"title":"Gravitational wave background from Population III binary black holes consistent with cosmic reionization","volume":461,"oa_version":"Published Version","scopus_import":"1","date_updated":"2024-09-25T07:17:34Z","abstract":[{"lang":"eng","text":"The recent discovery of the gravitational wave source GW150914 has revealed a coalescing binary black hole (BBH) with masses of ∼30 M⊙. Previous proposals for the origin of such a massive binary include Population III (PopIII) stars. PopIII stars are efficient producers of BBHs and of a gravitational wave background (GWB) in the 10–100 Hz band, and also of ionizing radiation in the early Universe. We quantify the relation between the amplitude of the GWB (Ωgw) and the electron scattering optical depth (τe), produced by PopIII stars, assuming that fesc ≈ 10 per cent of their ionizing radiation escapes into the intergalactic medium. We find that PopIII stars would produce a GWB that is detectable by the future O5 LIGO/Virgo if τe ≳ 0.07, consistent with the recent Planck measurement of τe = 0.055 ± 0.09. Moreover, the spectral index of the background from PopIII BBHs becomes as small as dln Ωgw/dln f ≲ 0.3 at f ≳ 30 Hz, which is significantly flatter than the value ∼2/3 generically produced by lower redshift and less-massive BBHs. A detection of the unique flattening at such low frequencies by the O5 LIGO/Virgo will indicate the existence of a high-chirp mass, high-redshift BBH population, which is consistent with the PopIII origin. A precise characterization of the spectral shape near 30–50 Hz by the Einstein Telescope could also constrain the PopIII initial mass function and star formation rate."}],"citation":{"apa":"Inayoshi, K., Kashiyama, K., Visbal, E., & Haiman, Z. (2016). Gravitational wave background from Population III binary black holes consistent with cosmic reionization. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw1431","ama":"Inayoshi K, Kashiyama K, Visbal E, Haiman Z. Gravitational wave background from Population III binary black holes consistent with cosmic reionization. Monthly Notices of the Royal Astronomical Society. 2016;461(3):2722-2727. doi:10.1093/mnras/stw1431","chicago":"Inayoshi, Kohei, Kazumi Kashiyama, Eli Visbal, and Zoltán Haiman. “Gravitational Wave Background from Population III Binary Black Holes Consistent with Cosmic Reionization.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw1431.","short":"K. Inayoshi, K. Kashiyama, E. Visbal, Z. Haiman, Monthly Notices of the Royal Astronomical Society 461 (2016) 2722–2727.","ieee":"K. Inayoshi, K. Kashiyama, E. Visbal, and Z. Haiman, “Gravitational wave background from Population III binary black holes consistent with cosmic reionization,” Monthly Notices of the Royal Astronomical Society, vol. 461, no. 3. Oxford University Press, pp. 2722–2727, 2016.","ista":"Inayoshi K, Kashiyama K, Visbal E, Haiman Z. 2016. Gravitational wave background from Population III binary black holes consistent with cosmic reionization. Monthly Notices of the Royal Astronomical Society. 461(3), 2722–2727.","mla":"Inayoshi, Kohei, et al. “Gravitational Wave Background from Population III Binary Black Holes Consistent with Cosmic Reionization.” Monthly Notices of the Royal Astronomical Society, vol. 461, no. 3, Oxford University Press, 2016, pp. 2722–27, doi:10.1093/mnras/stw1431."},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stw1431"}],"_id":"17659","article_processing_charge":"No","doi":"10.1093/mnras/stw1431","date_created":"2024-09-06T07:37:31Z","article_type":"original","publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","date_published":"2016-06-21T00:00:00Z","extern":"1","day":"21","type":"journal_article","publication_identifier":{"issn":["0035-8711","1365-2966"]},"month":"06","year":"2016"},{"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"title":"Do dark matter halos explain lensing peaks?","arxiv":1,"volume":94,"oa_version":"Preprint","quality_controlled":"1","publication_status":"published","status":"public","oa":1,"author":[{"last_name":"Zorrilla Matilla","first_name":"José Manuel","full_name":"Zorrilla Matilla, José Manuel"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"full_name":"Hsu, Daniel","first_name":"Daniel","last_name":"Hsu"},{"last_name":"Gupta","full_name":"Gupta, Arushi","first_name":"Arushi"},{"first_name":"Andrea","full_name":"Petri, Andrea","last_name":"Petri"}],"intvolume":" 94","issue":"8","type":"journal_article","publication_identifier":{"issn":["2470-0010","2470-0029"]},"month":"10","year":"2016","publisher":"American Physical Society","publication":"Physical Review D","date_published":"2016-10-04T00:00:00Z","article_number":"083506","extern":"1","day":"04","citation":{"apa":"Zorrilla Matilla, J. M., Haiman, Z., Hsu, D., Gupta, A., & Petri, A. (2016). Do dark matter halos explain lensing peaks? Physical Review D. American Physical Society. https://doi.org/10.1103/physrevd.94.083506","mla":"Zorrilla Matilla, José Manuel, et al. “Do Dark Matter Halos Explain Lensing Peaks?” Physical Review D, vol. 94, no. 8, 083506, American Physical Society, 2016, doi:10.1103/physrevd.94.083506.","ista":"Zorrilla Matilla JM, Haiman Z, Hsu D, Gupta A, Petri A. 2016. Do dark matter halos explain lensing peaks? Physical Review D. 94(8), 083506.","ama":"Zorrilla Matilla JM, Haiman Z, Hsu D, Gupta A, Petri A. Do dark matter halos explain lensing peaks? Physical Review D. 2016;94(8). doi:10.1103/physrevd.94.083506","ieee":"J. M. Zorrilla Matilla, Z. Haiman, D. Hsu, A. Gupta, and A. Petri, “Do dark matter halos explain lensing peaks?,” Physical Review D, vol. 94, no. 8. American Physical Society, 2016.","chicago":"Zorrilla Matilla, José Manuel, Zoltán Haiman, Daniel Hsu, Arushi Gupta, and Andrea Petri. “Do Dark Matter Halos Explain Lensing Peaks?” Physical Review D. American Physical Society, 2016. https://doi.org/10.1103/physrevd.94.083506.","short":"J.M. Zorrilla Matilla, Z. Haiman, D. Hsu, A. Gupta, A. Petri, Physical Review D 94 (2016)."},"main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.1609.03973"}],"_id":"17666","article_processing_charge":"No","doi":"10.1103/physrevd.94.083506","external_id":{"arxiv":["1609.03973"]},"date_created":"2024-09-06T07:44:28Z","article_type":"original","scopus_import":"1","date_updated":"2024-09-25T07:49:17Z","abstract":[{"text":"We have investigated a recently proposed halo-based model, Camelus, for predicting weak-lensing peak counts, and compared its results over a collection of 162 cosmologies with those from N-body simulations. While counts from both models agree for peaks with S/N>1 (where S/N is the ratio of the peak height to the r.m.s. shape noise), we find ≈50% fewer counts for peaks near S/N=0 and significantly higher counts in the negative S/N tail. Adding shape noise reduces the differences to within 20% for all cosmologies. We also found larger covariances that are more sensitive to cosmological parameters. As a result, credibility regions in the {Ωm,σ8} are ≈30% larger. Even though the credible contours are commensurate, each model draws its predictive power from different types of peaks. Low peaks, especially those with 23). Our results confirm the importance of using a cosmology-dependent covariance with at least a 14\\% improvement in parameter constraints. We identified the covariance estimation as the main driver behind differences in inference, and suggest possible ways to make Camelus even more useful as a highly accurate peak count emulator.","lang":"eng"}]},{"_id":"17669","citation":{"apa":"Liu, J., Hill, J. C., Sherwin, B. D., Petri, A., Böhm, V., & Haiman, Z. (2016). CMB lensing beyond the power spectrum: Cosmological constraints from the one-point probability distribution function and peak counts. Physical Review D. American Physical Society. https://doi.org/10.1103/physrevd.94.103501","mla":"Liu, Jia, et al. “CMB Lensing beyond the Power Spectrum: Cosmological Constraints from the One-Point Probability Distribution Function and Peak Counts.” Physical Review D, vol. 94, no. 10, 103501, American Physical Society, 2016, doi:10.1103/physrevd.94.103501.","ista":"Liu J, Hill JC, Sherwin BD, Petri A, Böhm V, Haiman Z. 2016. CMB lensing beyond the power spectrum: Cosmological constraints from the one-point probability distribution function and peak counts. Physical Review D. 94(10), 103501.","ama":"Liu J, Hill JC, Sherwin BD, Petri A, Böhm V, Haiman Z. CMB lensing beyond the power spectrum: Cosmological constraints from the one-point probability distribution function and peak counts. Physical Review D. 2016;94(10). doi:10.1103/physrevd.94.103501","chicago":"Liu, Jia, J. Colin Hill, Blake D. Sherwin, Andrea Petri, Vanessa Böhm, and Zoltán Haiman. “CMB Lensing beyond the Power Spectrum: Cosmological Constraints from the One-Point Probability Distribution Function and Peak Counts.” Physical Review D. American Physical Society, 2016. https://doi.org/10.1103/physrevd.94.103501.","short":"J. Liu, J.C. Hill, B.D. Sherwin, A. Petri, V. Böhm, Z. Haiman, Physical Review D 94 (2016).","ieee":"J. Liu, J. C. Hill, B. D. Sherwin, A. Petri, V. Böhm, and Z. Haiman, “CMB lensing beyond the power spectrum: Cosmological constraints from the one-point probability distribution function and peak counts,” Physical Review D, vol. 94, no. 10. American Physical Society, 2016."},"main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.1608.03169"}],"article_processing_charge":"No","doi":"10.1103/physrevd.94.103501","article_type":"original","external_id":{"arxiv":["1608.03169"]},"date_created":"2024-09-06T07:47:04Z","scopus_import":"1","date_updated":"2024-09-25T08:01:19Z","abstract":[{"lang":"eng","text":"Unprecedentedly precise cosmic microwave background (CMB) data are expected from ongoing and near-future CMB Stage-III and IV surveys, which will yield reconstructed CMB lensing maps with effective resolution approaching several arcminutes. The small-scale CMB lensing fluctuations receive non-negligible contributions from nonlinear structure in the late-time density field. These fluctuations are not fully characterized by traditional two-point statistics, such as the power spectrum. Here, we use N-body ray-tracing simulations of CMB lensing maps to examine two higher-order statistics: the lensing convergence one-point probability distribution function (PDF) and peak counts. We show that these statistics contain significant information not captured by the two-point function, and provide specific forecasts for the ongoing Stage-III Advanced Atacama Cosmology Telescope (AdvACT) experiment. Considering only the temperature-based reconstruction estimator, we forecast 9σ (PDF) and 6σ (peaks) detections of these statistics with AdvACT. Our simulation pipeline fully accounts for the non-Gaussianity of the lensing reconstruction noise, which is significant and cannot be neglected. Combining the power spectrum, PDF, and peak counts for AdvACT will tighten cosmological constraints in the Ωm-σ8 plane by ≈30%, compared to using the power spectrum alone."}],"publication_identifier":{"issn":["2470-0010","2470-0029"]},"type":"journal_article","year":"2016","month":"11","publication":"Physical Review D","publisher":"American Physical Society","article_number":"103501","date_published":"2016-11-02T00:00:00Z","extern":"1","day":"02","status":"public","oa":1,"author":[{"last_name":"Liu","full_name":"Liu, Jia","first_name":"Jia"},{"last_name":"Hill","first_name":"J. Colin","full_name":"Hill, J. Colin"},{"first_name":"Blake D.","full_name":"Sherwin, Blake D.","last_name":"Sherwin"},{"last_name":"Petri","first_name":"Andrea","full_name":"Petri, Andrea"},{"first_name":"Vanessa","full_name":"Böhm, Vanessa","last_name":"Böhm"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","full_name":"Haiman, Zoltán","first_name":"Zoltán"}],"intvolume":" 94","issue":"10","language":[{"iso":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","arxiv":1,"title":"CMB lensing beyond the power spectrum: Cosmological constraints from the one-point probability distribution function and peak counts","volume":94,"oa_version":"Preprint","quality_controlled":"1","publication_status":"published"},{"month":"07","year":"2016","type":"journal_article","publication_identifier":{"issn":["0035-8711","1365-2966"]},"extern":"1","day":"28","publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","date_published":"2016-07-28T00:00:00Z","doi":"10.1093/mnras/stw1838","date_created":"2024-09-06T07:49:15Z","article_type":"original","citation":{"chicago":"Charisi, M., I. Bartos, Zoltán Haiman, A. M. Price-Whelan, M. J. Graham, E. C. Bellm, R. R. Laher, and S. Márka. “A Population of Short-Period Variable Quasars from PTF as Supermassive Black Hole Binary Candidates.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw1838.","short":"M. Charisi, I. Bartos, Z. Haiman, A.M. Price-Whelan, M.J. Graham, E.C. Bellm, R.R. Laher, S. Márka, Monthly Notices of the Royal Astronomical Society 463 (2016) 2145–2171.","ama":"Charisi M, Bartos I, Haiman Z, et al. A population of short-period variable quasars from PTF as supermassive black hole binary candidates. Monthly Notices of the Royal Astronomical Society. 2016;463(2):2145-2171. doi:10.1093/mnras/stw1838","ieee":"M. Charisi et al., “A population of short-period variable quasars from PTF as supermassive black hole binary candidates,” Monthly Notices of the Royal Astronomical Society, vol. 463, no. 2. Oxford University Press, pp. 2145–2171, 2016.","ista":"Charisi M, Bartos I, Haiman Z, Price-Whelan AM, Graham MJ, Bellm EC, Laher RR, Márka S. 2016. A population of short-period variable quasars from PTF as supermassive black hole binary candidates. Monthly Notices of the Royal Astronomical Society. 463(2), 2145–2171.","mla":"Charisi, M., et al. “A Population of Short-Period Variable Quasars from PTF as Supermassive Black Hole Binary Candidates.” Monthly Notices of the Royal Astronomical Society, vol. 463, no. 2, Oxford University Press, 2016, pp. 2145–71, doi:10.1093/mnras/stw1838.","apa":"Charisi, M., Bartos, I., Haiman, Z., Price-Whelan, A. M., Graham, M. J., Bellm, E. C., … Márka, S. (2016). A population of short-period variable quasars from PTF as supermassive black hole binary candidates. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw1838"},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stw1838"}],"_id":"17672","article_processing_charge":"No","abstract":[{"lang":"eng","text":"Supermassive black hole binaries (SMBHBs) at sub-parsec separations should be common in galactic nuclei, as a result of frequent galaxy mergers. Hydrodynamical simulations of circum-binary discs predict strong periodic modulation of the mass accretion rate on time-scales comparable to the orbital period of the binary. As a result, SMBHBs may be recognized by the periodic modulation of their brightness. We conducted a statistical search for periodic variability in a sample of 35 383 spectroscopically confirmed quasars in the photometric data base of the Palomar Transient Factory (PTF). We analysed Lomb–Scargle periodograms and assessed the significance of our findings by modelling each individual quasar's variability as a damped random walk (DRW). We identified 50 quasars with significant periodicity beyond the DRW model, typically with short periods of a few hundred days. We find 33 of these to remain significant after a re-analysis of their periodograms including additional optical data from the intermediate-PTF and the Catalina Real-Time Transient Survey. Assuming that the observed periods correspond to the redshifted orbital periods of SMBHBs, we conclude that our findings are consistent with a population of unequal-mass SMBHBs, with a typical mass ratio as low as q ≡ M2/M1 ≈ 0.01."}],"scopus_import":"1","date_updated":"2024-09-25T08:28:42Z","volume":463,"oa_version":"Published Version","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"page":"2145-2171","title":"A population of short-period variable quasars from PTF as supermassive black hole binary candidates","publication_status":"published","quality_controlled":"1","oa":1,"status":"public","intvolume":" 463","issue":"2","author":[{"last_name":"Charisi","full_name":"Charisi, M.","first_name":"M."},{"first_name":"I.","full_name":"Bartos, I.","last_name":"Bartos"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","full_name":"Haiman, Zoltán","first_name":"Zoltán"},{"first_name":"A. M.","full_name":"Price-Whelan, A. M.","last_name":"Price-Whelan"},{"first_name":"M. J.","full_name":"Graham, M. J.","last_name":"Graham"},{"last_name":"Bellm","first_name":"E. C.","full_name":"Bellm, E. C."},{"last_name":"Laher","first_name":"R. R.","full_name":"Laher, R. R."},{"last_name":"Márka","first_name":"S.","full_name":"Márka, S."}]},{"publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","date_published":"2016-07-08T00:00:00Z","extern":"1","day":"08","type":"journal_article","publication_identifier":{"issn":["0035-8711","1365-2966"]},"month":"07","year":"2016","scopus_import":"1","date_updated":"2024-09-25T10:02:57Z","abstract":[{"lang":"eng","text":"We perform one-dimensional radiation hydrodynamical simulations to solve accretion flows onto massive black holes (BHs) with a very high rate. Assuming that photon trapping limits the luminosity emerging from the central region to L≲LEdd, Inayoshi, Haiman & Ostriker (2016) have shown that an accretion flow settles to a \"hyper-Eddington\" solution, with a steady and isothermal (T≃8000 K) Bondi profile reaching ≳5000 times the Eddington accretion rate M˙Edd≡LEdd/c2. Here we address the possibility that gas accreting with finite angular momentum forms a bright nuclear accretion disc, with a luminosity exceeding the Eddington limit (1≲L/LEdd≲100). Combining our simulations with an analytic model, we find that a transition to steady hyper-Eddington accretion still occurs, as long as the luminosity remains below L/LEdd≲35 (MBH/10^4 M⊙)^3/2(n∞/10^5 cm^−3)(T∞/10^4 K)^−3/2(r⋆/10^14 cm)^−1/2, where n∞ and T∞ are the density and temperature of the ambient gas, and r⋆ is the radius of the photosphere, at which radiation emerges. If the luminosity exceeds this value, accretion becomes episodic. Our results can be accurately recovered in a toy model of an optically thick spherical shell, driven by radiation force into a collapsing medium. When the central source is dimmer than the above critical value, the expansion of the shell is halted and reversed by ram pressure of the collapsing medium, and by shell's weight. Our results imply that rapid, unimpeded hyper-Eddington accretion is possible even if the luminosity of the central source far exceeds the Eddington limit, and can be either steady or strongly episodic."}],"citation":{"ista":"Sakurai Y, Inayoshi K, Haiman Z. 2016. Hyper-Eddington mass accretion on to a black hole with super-Eddington luminosity. Monthly Notices of the Royal Astronomical Society. 461(4), 4496–4504.","mla":"Sakurai, Yuya, et al. “Hyper-Eddington Mass Accretion on to a Black Hole with Super-Eddington Luminosity.” Monthly Notices of the Royal Astronomical Society, vol. 461, no. 4, Oxford University Press, 2016, pp. 4496–504, doi:10.1093/mnras/stw1652.","short":"Y. Sakurai, K. Inayoshi, Z. Haiman, Monthly Notices of the Royal Astronomical Society 461 (2016) 4496–4504.","ama":"Sakurai Y, Inayoshi K, Haiman Z. Hyper-Eddington mass accretion on to a black hole with super-Eddington luminosity. Monthly Notices of the Royal Astronomical Society. 2016;461(4):4496-4504. doi:10.1093/mnras/stw1652","chicago":"Sakurai, Yuya, Kohei Inayoshi, and Zoltán Haiman. “Hyper-Eddington Mass Accretion on to a Black Hole with Super-Eddington Luminosity.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw1652.","ieee":"Y. Sakurai, K. Inayoshi, and Z. Haiman, “Hyper-Eddington mass accretion on to a black hole with super-Eddington luminosity,” Monthly Notices of the Royal Astronomical Society, vol. 461, no. 4. Oxford University Press, pp. 4496–4504, 2016.","apa":"Sakurai, Y., Inayoshi, K., & Haiman, Z. (2016). Hyper-Eddington mass accretion on to a black hole with super-Eddington luminosity. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw1652"},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stw1652"}],"_id":"17693","article_processing_charge":"No","doi":"10.1093/mnras/stw1652","date_created":"2024-09-06T08:39:53Z","article_type":"original","quality_controlled":"1","publication_status":"published","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"page":"4496-4504","title":"Hyper-Eddington mass accretion on to a black hole with super-Eddington luminosity","volume":461,"oa_version":"Published Version","author":[{"first_name":"Yuya","full_name":"Sakurai, Yuya","last_name":"Sakurai"},{"last_name":"Inayoshi","full_name":"Inayoshi, Kohei","first_name":"Kohei"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"}],"issue":"4","intvolume":" 461","status":"public","oa":1},{"oa":1,"doi":"10.1093/mnras/stw3351","date_created":"2024-09-06T08:45:10Z","article_type":"original","citation":{"ieee":"B. Greig, A. Mesinger, Z. Haiman, and R. A. Simcoe, “Are we witnessing the epoch of reionization at z=7.1 from the spectrum of J1120+0641?,” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016.","chicago":"Greig, Bradley, Andrei Mesinger, Zoltán Haiman, and Robert A. Simcoe. “Are We Witnessing the Epoch of Reionization at Z=7.1 from the Spectrum of J1120+0641?” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw3351.","ama":"Greig B, Mesinger A, Haiman Z, Simcoe RA. Are we witnessing the epoch of reionization at z=7.1 from the spectrum of J1120+0641? Monthly Notices of the Royal Astronomical Society. 2016. doi:10.1093/mnras/stw3351","short":"B. Greig, A. Mesinger, Z. Haiman, R.A. Simcoe, Monthly Notices of the Royal Astronomical Society (2016).","mla":"Greig, Bradley, et al. “Are We Witnessing the Epoch of Reionization at Z=7.1 from the Spectrum of J1120+0641?” Monthly Notices of the Royal Astronomical Society, stw3351, Oxford University Press, 2016, doi:10.1093/mnras/stw3351.","ista":"Greig B, Mesinger A, Haiman Z, Simcoe RA. 2016. Are we witnessing the epoch of reionization at z=7.1 from the spectrum of J1120+0641? Monthly Notices of the Royal Astronomical Society., stw3351.","apa":"Greig, B., Mesinger, A., Haiman, Z., & Simcoe, R. A. (2016). Are we witnessing the epoch of reionization at z=7.1 from the spectrum of J1120+0641? Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw3351"},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stw3351"}],"_id":"17699","status":"public","article_processing_charge":"No","abstract":[{"lang":"eng","text":"We quantify the presence of Ly\\alpha\\ damping wing absorption from a partially-neutral intergalactic medium (IGM) in the spectrum of the z=7.08 QSO, ULASJ1120+0641. Using a Bayesian framework, we simultaneously account for uncertainties in: (i) the intrinsic QSO emission spectrum; and (ii) the distribution of cosmic HI patches during the epoch of reionisation (EoR). For (i) we use a new intrinsic Ly\\alpha\\ emission line reconstruction method (Greig et al.), sampling a covariance matrix of emission line properties built from a large database of moderate-z QSOs. For (ii), we use the Evolution of 21-cm Structure (EOS; Mesinger et al.) simulations, which span a range of physically-motivated EoR models. We find strong evidence for the presence of damping wing absorption redward of Ly\\alpha\\ (where there is no contamination from the Ly\\alpha\\ forest). Our analysis implies that the EoR is not yet complete by z=7.1, with the volume-weighted IGM neutral fraction constrained to x¯HI=0.40+0.21−0.19 at 1σ (x¯HI=0.40+0.41−0.32 at 2σ). This result is insensitive to the EoR morphology. Our detection of significant neutral HI in the IGM at z=7.1 is consistent with the latest Planck 2016 measurements of the CMB Thompson scattering optical depth (Planck Collaboration XLVII)."}],"scopus_import":"1","author":[{"last_name":"Greig","first_name":"Bradley","full_name":"Greig, Bradley"},{"full_name":"Mesinger, Andrei","first_name":"Andrei","last_name":"Mesinger"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","full_name":"Haiman, Zoltán","first_name":"Zoltán"},{"first_name":"Robert A.","full_name":"Simcoe, Robert A.","last_name":"Simcoe"}],"date_updated":"2024-09-25T11:19:08Z","month":"12","year":"2016","oa_version":"Published Version","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","type":"journal_article","publication_identifier":{"issn":["0035-8711","1365-2966"]},"language":[{"iso":"eng"}],"title":"Are we witnessing the epoch of reionization at z=7.1 from the spectrum of J1120+0641?","extern":"1","publication_status":"published","day":"24","publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","article_number":"stw3351","quality_controlled":"1","date_published":"2016-12-24T00:00:00Z"},{"type":"journal_article","publication_identifier":{"issn":["0035-8711","1365-2966"]},"month":"05","year":"2016","publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","date_published":"2016-05-24T00:00:00Z","extern":"1","day":"24","citation":{"mla":"Ryu, Taeho, et al. “Intermediate-Mass Black Holes from Population III Remnants in the First Galactic Nuclei.” Monthly Notices of the Royal Astronomical Society, vol. 460, no. 4, Oxford University Press, 2016, pp. 4122–34, doi:10.1093/mnras/stw1241.","ista":"Ryu T, Tanaka TL, Perna R, Haiman Z. 2016. Intermediate-mass black holes from Population III remnants in the first galactic nuclei. Monthly Notices of the Royal Astronomical Society. 460(4), 4122–4134.","ieee":"T. Ryu, T. L. Tanaka, R. Perna, and Z. Haiman, “Intermediate-mass black holes from Population III remnants in the first galactic nuclei,” Monthly Notices of the Royal Astronomical Society, vol. 460, no. 4. Oxford University Press, pp. 4122–4134, 2016.","ama":"Ryu T, Tanaka TL, Perna R, Haiman Z. Intermediate-mass black holes from Population III remnants in the first galactic nuclei. Monthly Notices of the Royal Astronomical Society. 2016;460(4):4122-4134. doi:10.1093/mnras/stw1241","short":"T. Ryu, T.L. Tanaka, R. Perna, Z. Haiman, Monthly Notices of the Royal Astronomical Society 460 (2016) 4122–4134.","chicago":"Ryu, Taeho, Takamitsu L. Tanaka, Rosalba Perna, and Zoltán Haiman. “Intermediate-Mass Black Holes from Population III Remnants in the First Galactic Nuclei.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw1241.","apa":"Ryu, T., Tanaka, T. L., Perna, R., & Haiman, Z. (2016). Intermediate-mass black holes from Population III remnants in the first galactic nuclei. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw1241"},"main_file_link":[{"url":"https://doi.org/10.1093/mnras/stw1241","open_access":"1"}],"_id":"17700","article_processing_charge":"No","doi":"10.1093/mnras/stw1241","date_created":"2024-09-06T08:46:28Z","article_type":"original","scopus_import":"1","date_updated":"2024-09-25T11:22:16Z","abstract":[{"text":"We report the formation of intermediate-mass black holes (IMBHs) in suites of numerical N-body simulations of Population III remnant black holes (BHs) embedded in gas-rich protogalaxies at redshifts z≳10. We model the effects of gas drag on the BHs' orbits, and allow BHs to grow via gas accretion, including a mode of hyper-Eddington accretion in which photon trapping and rapid gas inflow suppress any negative radiative feedback. Most initial BH configurations lead to the formation of one (but never more than one) IMBH in the center of the protogalaxy, reaching a mass of 10^3−5M⊙ through hyper-Eddington growth. Our results suggest a viable pathway to forming the earliest massive BHs in the centers of early galaxies. We also find that the nuclear IMBH typically captures a stellar-mass BH companion, making these systems observable in gravitational waves as extreme mass-ratio inspirals (EMRIs) with eLISA.","lang":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"page":"4122-4134","title":"Intermediate-mass black holes from Population III remnants in the first galactic nuclei","volume":460,"oa_version":"Published Version","quality_controlled":"1","publication_status":"published","status":"public","oa":1,"author":[{"last_name":"Ryu","full_name":"Ryu, Taeho","first_name":"Taeho"},{"last_name":"Tanaka","first_name":"Takamitsu L.","full_name":"Tanaka, Takamitsu L."},{"first_name":"Rosalba","full_name":"Perna, Rosalba","last_name":"Perna"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"}],"issue":"4","intvolume":" 460"},{"month":"04","year":"2016","type":"journal_article","publication_identifier":{"issn":["0035-8711","1365-2966"]},"extern":"1","day":"12","publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","date_published":"2016-04-12T00:00:00Z","doi":"10.1093/mnras/stw836","date_created":"2024-09-06T08:54:12Z","article_type":"original","citation":{"apa":"Inayoshi, K., Haiman, Z., & Ostriker, J. P. (2016). Hyper-Eddington accretion flows on to massive black holes. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw836","short":"K. Inayoshi, Z. Haiman, J.P. Ostriker, Monthly Notices of the Royal Astronomical Society 459 (2016) 3738–3755.","chicago":"Inayoshi, Kohei, Zoltán Haiman, and Jeremiah P. Ostriker. “Hyper-Eddington Accretion Flows on to Massive Black Holes.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw836.","ieee":"K. Inayoshi, Z. Haiman, and J. P. Ostriker, “Hyper-Eddington accretion flows on to massive black holes,” Monthly Notices of the Royal Astronomical Society, vol. 459, no. 4. Oxford University Press, pp. 3738–3755, 2016.","ama":"Inayoshi K, Haiman Z, Ostriker JP. Hyper-Eddington accretion flows on to massive black holes. Monthly Notices of the Royal Astronomical Society. 2016;459(4):3738-3755. doi:10.1093/mnras/stw836","mla":"Inayoshi, Kohei, et al. “Hyper-Eddington Accretion Flows on to Massive Black Holes.” Monthly Notices of the Royal Astronomical Society, vol. 459, no. 4, Oxford University Press, 2016, pp. 3738–55, doi:10.1093/mnras/stw836.","ista":"Inayoshi K, Haiman Z, Ostriker JP. 2016. Hyper-Eddington accretion flows on to massive black holes. Monthly Notices of the Royal Astronomical Society. 459(4), 3738–3755."},"main_file_link":[{"url":"https://doi.org/10.1093/mnras/stw836","open_access":"1"}],"_id":"17709","article_processing_charge":"No","abstract":[{"lang":"eng","text":"We study very-high rate spherically symmetric accretion flows onto a massive black hole (BH; 10^2 < M_BH < 10^6 Msun) embedded in a dense gas cloud with a low abundance of metals, performing one-dimensional hydrodynamical simulations which include multi-frequency radiation transfer and non-equilibrium primordial chemistry. We find that rapid gas supply from the Bondi radius at a hyper-Eddington rate can occur without being impeded by radiation feedback when (n/10^5 cm^-3) > (M_BH/10^4Msun)^{-1}(T/10^4 K)^{3/2}, where n and T are the density and temperature of ambient gas outside of the Bondi radius. The resulting accretion rate in this regime is steady, and larger than 3000 times the Eddington rate. At lower Bondi rates, the accretion is episodic due to radiative feedback and the average rate is limited below the Eddington rate. For the hyper-Eddington case, the steady solution consists of two parts: a radiation-dominated central core, where photon trapping due to electron scattering is important, and an accreting envelope which follows a Bondi profile with T~8000 K. When the emergent luminosity is limited below the Eddington luminosity because of photon trapping, radiation from the central region does not affect the gas dynamics at larger scales. We apply our result to the rapid formation of massive BHs in protogalaxies with a virial temperature of T_vir> 10^4 K. Once a seed BH forms at the center of the galaxy, it can grow up to a maximum ~10^5 (T_vir/10^4 K) Msun via gas accretion independent of the initial BH mass. Finally, we discuss possible observational signatures of rapidly accreting BHs with/without allowance for dust. We suggest that these systems could explain Lya emitters without X-rays and luminous infrared sources with hot dust emission, respectively."}],"scopus_import":"1","date_updated":"2024-09-25T12:00:22Z","volume":459,"oa_version":"Published Version","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"page":"3738-3755","title":"Hyper-Eddington accretion flows on to massive black holes","publication_status":"published","quality_controlled":"1","oa":1,"status":"public","issue":"4","intvolume":" 459","author":[{"last_name":"Inayoshi","first_name":"Kohei","full_name":"Inayoshi, Kohei"},{"last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","full_name":"Haiman, Zoltán"},{"full_name":"Ostriker, Jeremiah P.","first_name":"Jeremiah P.","last_name":"Ostriker"}]},{"quality_controlled":"1","publication_status":"published","language":[{"iso":"eng"}],"page":"17 - 46","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","arxiv":1,"title":"Inference algorithms for pattern-based CRFs on sequence data","corr_author":"1","volume":76,"oa_version":"Preprint","author":[{"id":"3D50B0BA-F248-11E8-B48F-1D18A9856A87","last_name":"Kolmogorov","full_name":"Kolmogorov, Vladimir","first_name":"Vladimir"},{"last_name":"Takhanov","id":"2CCAC26C-F248-11E8-B48F-1D18A9856A87","first_name":"Rustem","full_name":"Takhanov, Rustem"}],"issue":"1","intvolume":" 76","status":"public","isi":1,"oa":1,"publication":"Algorithmica","publisher":"Springer","date_published":"2016-09-01T00:00:00Z","project":[{"name":"Discrete Optimization in Computer Vision: Theory and Practice","call_identifier":"FP7","_id":"25FBA906-B435-11E9-9278-68D0E5697425","grant_number":"616160"}],"day":"01","type":"journal_article","year":"2016","month":"09","department":[{"_id":"VlKo"}],"scopus_import":"1","related_material":{"record":[{"id":"2272","relation":"earlier_version","status":"public"}]},"date_updated":"2025-09-29T14:28:47Z","abstract":[{"lang":"eng","text":"We consider Conditional random fields (CRFs) with pattern-based potentials defined on a chain. In this model the energy of a string (labeling) (Formula presented.) is the sum of terms over intervals [i, j] where each term is non-zero only if the substring (Formula presented.) equals a prespecified pattern w. Such CRFs can be naturally applied to many sequence tagging problems. We present efficient algorithms for the three standard inference tasks in a CRF, namely computing (i) the partition function, (ii) marginals, and (iii) computing the MAP. Their complexities are respectively (Formula presented.), (Formula presented.) and (Formula presented.) where L is the combined length of input patterns, (Formula presented.) is the maximum length of a pattern, and D is the input alphabet. This improves on the previous algorithms of Ye et al. (NIPS, 2009) whose complexities are respectively (Formula presented.), (Formula presented.) and (Formula presented.), where (Formula presented.) is the number of input patterns. In addition, we give an efficient algorithm for sampling, and revisit the case of MAP with non-positive weights."}],"publist_id":"5316","_id":"1794","citation":{"mla":"Kolmogorov, Vladimir, and Rustem Takhanov. “Inference Algorithms for Pattern-Based CRFs on Sequence Data.” Algorithmica, vol. 76, no. 1, Springer, 2016, pp. 17–46, doi:10.1007/s00453-015-0017-7.","ista":"Kolmogorov V, Takhanov R. 2016. Inference algorithms for pattern-based CRFs on sequence data. Algorithmica. 76(1), 17–46.","ama":"Kolmogorov V, Takhanov R. Inference algorithms for pattern-based CRFs on sequence data. Algorithmica. 2016;76(1):17-46. doi:10.1007/s00453-015-0017-7","chicago":"Kolmogorov, Vladimir, and Rustem Takhanov. “Inference Algorithms for Pattern-Based CRFs on Sequence Data.” Algorithmica. Springer, 2016. https://doi.org/10.1007/s00453-015-0017-7.","short":"V. Kolmogorov, R. Takhanov, Algorithmica 76 (2016) 17–46.","ieee":"V. Kolmogorov and R. Takhanov, “Inference algorithms for pattern-based CRFs on sequence data,” Algorithmica, vol. 76, no. 1. Springer, pp. 17–46, 2016.","apa":"Kolmogorov, V., & Takhanov, R. (2016). Inference algorithms for pattern-based CRFs on sequence data. Algorithmica. Springer. https://doi.org/10.1007/s00453-015-0017-7"},"main_file_link":[{"open_access":"1","url":"http://arxiv.org/abs/1210.0508"}],"article_processing_charge":"No","doi":"10.1007/s00453-015-0017-7","ec_funded":1,"external_id":{"arxiv":["1210.0508"],"isi":["000381149500002"]},"acknowledgement":"This work has been partially supported by the European Research Council under the European Unions Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement no. 616160.","date_created":"2018-12-11T11:54:02Z"},{"publication_status":"published","quality_controlled":"1","oa_version":"None","volume":138,"title":"Mechanism for Si–Si bond rupture in single molecule junctions","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"page":"16159-16164","issue":"49","intvolume":" 138","author":[{"full_name":"Li, Haixing","first_name":"Haixing","last_name":"Li"},{"last_name":"Kim","first_name":"Nathaniel T.","full_name":"Kim, Nathaniel T."},{"full_name":"Su, Timothy A.","first_name":"Timothy A.","last_name":"Su"},{"last_name":"Steigerwald","full_name":"Steigerwald, Michael L.","first_name":"Michael L."},{"first_name":"Colin","full_name":"Nuckolls, Colin","last_name":"Nuckolls"},{"last_name":"Darancet","full_name":"Darancet, Pierre","first_name":"Pierre"},{"full_name":"Leighton, James L.","first_name":"James L.","last_name":"Leighton"},{"id":"9ebb78a5-cc0d-11ee-8322-fae086a32caf","orcid":"0000-0002-6957-6089","last_name":"Venkataraman","full_name":"Venkataraman, Latha","first_name":"Latha"}],"pmid":1,"status":"public","day":"18","extern":"1","date_published":"2016-11-18T00:00:00Z","publisher":"American Chemical Society","publication":"Journal of the American Chemical Society","month":"11","year":"2016","type":"journal_article","OA_type":"closed access","publication_identifier":{"eissn":["1520-5126"],"issn":["0002-7863"]},"abstract":[{"lang":"eng","text":"The stability of chemical bonds can be studied experimentally by rupturing single molecule junctions under applied voltage. Here, we compare voltage-induced bond rupture in two Si–Si backbones: one has no alternate conductive pathway whereas the other contains an additional naphthyl pathway in parallel to the Si–Si bond. We show that in contrast to the first system, the second can conduct through the naphthyl group when the Si–Si bond is ruptured using an applied voltage. We investigate this voltage induced Si–Si bond rupture by ab initio density functional theory calculations and molecular dynamics simulations that ultimately demonstrate that the excitation of molecular vibrational modes by tunneling electrons leads to homolytic Si–Si bond rupture."}],"date_updated":"2024-12-18T08:36:48Z","scopus_import":"1","date_created":"2024-09-09T09:19:46Z","external_id":{"pmid":["27960303"]},"article_type":"original","doi":"10.1021/jacs.6b10700","article_processing_charge":"No","citation":{"apa":"Li, H., Kim, N. T., Su, T. A., Steigerwald, M. L., Nuckolls, C., Darancet, P., … Venkataraman, L. (2016). Mechanism for Si–Si bond rupture in single molecule junctions. Journal of the American Chemical Society. American Chemical Society. https://doi.org/10.1021/jacs.6b10700","short":"H. Li, N.T. Kim, T.A. Su, M.L. Steigerwald, C. Nuckolls, P. Darancet, J.L. Leighton, L. Venkataraman, Journal of the American Chemical Society 138 (2016) 16159–16164.","chicago":"Li, Haixing, Nathaniel T. Kim, Timothy A. Su, Michael L. Steigerwald, Colin Nuckolls, Pierre Darancet, James L. Leighton, and Latha Venkataraman. “Mechanism for Si–Si Bond Rupture in Single Molecule Junctions.” Journal of the American Chemical Society. American Chemical Society, 2016. https://doi.org/10.1021/jacs.6b10700.","ama":"Li H, Kim NT, Su TA, et al. Mechanism for Si–Si bond rupture in single molecule junctions. Journal of the American Chemical Society. 2016;138(49):16159-16164. doi:10.1021/jacs.6b10700","ieee":"H. Li et al., “Mechanism for Si–Si bond rupture in single molecule junctions,” Journal of the American Chemical Society, vol. 138, no. 49. American Chemical Society, pp. 16159–16164, 2016.","ista":"Li H, Kim NT, Su TA, Steigerwald ML, Nuckolls C, Darancet P, Leighton JL, Venkataraman L. 2016. Mechanism for Si–Si bond rupture in single molecule junctions. Journal of the American Chemical Society. 138(49), 16159–16164.","mla":"Li, Haixing, et al. “Mechanism for Si–Si Bond Rupture in Single Molecule Junctions.” Journal of the American Chemical Society, vol. 138, no. 49, American Chemical Society, 2016, pp. 16159–64, doi:10.1021/jacs.6b10700."},"_id":"17952"},{"_id":"17954","citation":{"chicago":"Borges, Anders, E-Dean Fung, Fay Ng, Latha Venkataraman, and Gemma C. Solomon. “Probing the Conductance of the σ-System of Bipyridine Using Destructive Interference.” The Journal of Physical Chemistry Letters. American Chemical Society, 2016. https://doi.org/10.1021/acs.jpclett.6b02494.","short":"A. Borges, E.-D. Fung, F. Ng, L. Venkataraman, G.C. Solomon, The Journal of Physical Chemistry Letters 7 (2016) 4825–4829.","ieee":"A. Borges, E.-D. Fung, F. Ng, L. Venkataraman, and G. C. Solomon, “Probing the conductance of the σ-system of bipyridine using destructive interference,” The Journal of Physical Chemistry Letters, vol. 7, no. 23. American Chemical Society, pp. 4825–4829, 2016.","ama":"Borges A, Fung E-D, Ng F, Venkataraman L, Solomon GC. Probing the conductance of the σ-system of bipyridine using destructive interference. The Journal of Physical Chemistry Letters. 2016;7(23):4825-4829. doi:10.1021/acs.jpclett.6b02494","ista":"Borges A, Fung E-D, Ng F, Venkataraman L, Solomon GC. 2016. Probing the conductance of the σ-system of bipyridine using destructive interference. The Journal of Physical Chemistry Letters. 7(23), 4825–4829.","mla":"Borges, Anders, et al. “Probing the Conductance of the σ-System of Bipyridine Using Destructive Interference.” The Journal of Physical Chemistry Letters, vol. 7, no. 23, American Chemical Society, 2016, pp. 4825–29, doi:10.1021/acs.jpclett.6b02494.","apa":"Borges, A., Fung, E.-D., Ng, F., Venkataraman, L., & Solomon, G. C. (2016). Probing the conductance of the σ-system of bipyridine using destructive interference. The Journal of Physical Chemistry Letters. American Chemical Society. https://doi.org/10.1021/acs.jpclett.6b02494"},"article_processing_charge":"No","doi":"10.1021/acs.jpclett.6b02494","article_type":"letter_note","date_created":"2024-09-09T09:22:48Z","external_id":{"pmid":["27934052"]},"scopus_import":"1","date_updated":"2024-12-18T08:47:29Z","abstract":[{"lang":"eng","text":"Guidelines to predict trends in the electrical conductance of molecules have been developed for the π-system of conjugated systems. Little is known, however, about the conductance of the underlying σ-systems because the π-system usually dominates the transport. Here we study a family of bipyridine-based molecules using STM-break junction experiments and density functional theory transport calculations. We use different lengths and substitution patterns to probe the role of both the σ-system and the π-system in controlling conductance. By exploiting the destructive interference feature found in the π-system of the meta-coupled six-membered aromatic rings, we show that the conductance of the σ-system of a meta-coupled molecule can be probed directly and can even exceed that of its para-coupled analog. These results add to the understanding of the conductance through the chemically hidden σ-electrons."}],"publication_identifier":{"eissn":["1948-7185"]},"type":"journal_article","OA_type":"closed access","year":"2016","month":"11","publication":"The Journal of Physical Chemistry Letters","publisher":"American Chemical Society","date_published":"2016-11-10T00:00:00Z","extern":"1","day":"10","status":"public","pmid":1,"author":[{"first_name":"Anders","full_name":"Borges, Anders","last_name":"Borges"},{"first_name":"E-Dean","full_name":"Fung, E-Dean","last_name":"Fung"},{"last_name":"Ng","first_name":"Fay","full_name":"Ng, Fay"},{"full_name":"Venkataraman, Latha","first_name":"Latha","id":"9ebb78a5-cc0d-11ee-8322-fae086a32caf","orcid":"0000-0002-6957-6089","last_name":"Venkataraman"},{"first_name":"Gemma C.","full_name":"Solomon, Gemma C.","last_name":"Solomon"}],"issue":"23","intvolume":" 7","page":"4825-4829","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"Probing the conductance of the σ-system of bipyridine using destructive interference","volume":7,"oa_version":"None","quality_controlled":"1","publication_status":"published"}]