[{"oa":1,"language":[{"iso":"eng"}],"issue":"4","intvolume":" 469","article_type":"original","year":"2017","date_published":"2017-05-10T00:00:00Z","date_created":"2024-09-06T08:44:11Z","volume":469,"abstract":[{"text":"Gaseous circumbinary accretion discs provide a promising mechanism to facilitate the mergers of supermassive black holes (SMBHs) in galactic nuclei. We measure the torques exerted on accreting SMBH binaries, using 2D, isothermal, moving-mesh, viscous hydrodynamical simulations of circumbinary accretion discs. Our computational domain includes the entire inner region of the circumbinary disk with the individual black holes (BHs) included as point masses on the grid and a sink prescription to model accretion onto each BH. The BHs each acquire their own well-resolved accretion discs (\"minidiscs\"). We explore a range of mass removal rates for the sink prescription removing gas from the central regions of the minidiscs. We find that the torque exerted on the binary is primarily gravitational, and dominated by the gas orbiting close behind and ahead of the individual BHs. The torques from the distorted circumbinary disc farther out and from the direct accretion of angular momentum are subdominant. The torques are sensitive to the sink prescription: slower sinks result in more gas accumulating near the BHs and more negative torques, driving the binary to merger more rapidly. For faster sinks, the torques are less negative and eventually turn positive (for unphysically fast sinks). When the minidiscs are modeled as standard alpha discs, our results are insensitive to the choice of sink radius. Scaling the simulations to a binary orbital period tbin = 1yr and background disc accretion rate Mdot = 0.3MEdd in Eddington units, the binary inspirals on a timescale of 3X10^6 years, irrespective of the SMBH masses. For binaries with total mass <10^7Msun, this is shorter than the inspiral time due to gravitational wave (GW) emission alone, implying that gas discs will have a significant impact on the SMBH binary population and can affect the GW signal for Pulsar Timing Arrays.","lang":"eng"}],"month":"05","author":[{"first_name":"Yike","last_name":"Tang","full_name":"Tang, Yike"},{"first_name":"Andrew","last_name":"MacFadyen","full_name":"MacFadyen, Andrew"},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman"}],"publication_status":"published","citation":{"short":"Y. Tang, A. MacFadyen, Z. Haiman, Monthly Notices of the Royal Astronomical Society 469 (2017) 4258–4267.","ista":"Tang Y, MacFadyen A, Haiman Z. 2017. On the orbital evolution of supermassive black hole binaries with circumbinary accretion discs. Monthly Notices of the Royal Astronomical Society. 469(4), 4258–4267.","chicago":"Tang, Yike, Andrew MacFadyen, and Zoltán Haiman. “On the Orbital Evolution of Supermassive Black Hole Binaries with Circumbinary Accretion Discs.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2017. https://doi.org/10.1093/mnras/stx1130.","ama":"Tang Y, MacFadyen A, Haiman Z. On the orbital evolution of supermassive black hole binaries with circumbinary accretion discs. Monthly Notices of the Royal Astronomical Society. 2017;469(4):4258-4267. doi:10.1093/mnras/stx1130","mla":"Tang, Yike, et al. “On the Orbital Evolution of Supermassive Black Hole Binaries with Circumbinary Accretion Discs.” Monthly Notices of the Royal Astronomical Society, vol. 469, no. 4, Oxford University Press, 2017, pp. 4258–67, doi:10.1093/mnras/stx1130.","apa":"Tang, Y., MacFadyen, A., & Haiman, Z. (2017). On the orbital evolution of supermassive black hole binaries with circumbinary accretion discs. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stx1130","ieee":"Y. Tang, A. MacFadyen, and Z. Haiman, “On the orbital evolution of supermassive black hole binaries with circumbinary accretion discs,” Monthly Notices of the Royal Astronomical Society, vol. 469, no. 4. Oxford University Press, pp. 4258–4267, 2017."},"publication":"Monthly Notices of the Royal Astronomical Society","publisher":"Oxford University Press","main_file_link":[{"url":"https://doi.org/10.1093/mnras/stx1130","open_access":"1"}],"title":"On the orbital evolution of supermassive black hole binaries with circumbinary accretion discs","_id":"17698","date_updated":"2024-09-25T11:16:50Z","day":"10","quality_controlled":"1","publication_identifier":{"issn":["0035-8711","1365-2966"]},"doi":"10.1093/mnras/stx1130","status":"public","page":"4258-4267","scopus_import":"1","oa_version":"Published Version","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","type":"journal_article","extern":"1","article_processing_charge":"No"},{"year":"2016","article_type":"original","date_published":"2016-12-01T00:00:00Z","date_created":"2022-07-13T10:08:20Z","acknowledgement":"We thank the anonymous referee for useful and constructive comments and suggestions which greatly improved the quality and clarity of our work. The authors acknowledge financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship. SS and DS acknowledge funding from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). SS also acknowledges support from FCT through the research grants UID/FIS/04434/2013 and PTDC/FIS-AST/2194/2012. JM acknowledges a Huygens PhD fellowship from Leiden University. Based on observations with the Subaru Telescope (Program IDs: S05B-027, S06A-025, S06B-010, S07A-013, S07B-008, S08B-008, S09A-017, S14A-086). Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 294.A-5018. Based on observations obtained with MegaPrime/Megacam, a joint project of CFHT and CEA/IRFU, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. We are grateful to the CFHTLS, COSMOS-UltraVISTA, UKIDSS, SXDF and COSMOS survey teams. Without these legacy surveys, this research would have been impossible. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct and explore observations from this mountain. Finally, the authors acknowledge the unique value of the publicly available programming language PYTHON, including the NUMPY, PYFITS, MATPLOTLIB, SCIPY and ASTROPY (Astropy Collaboration et al.","issue":"2","language":[{"iso":"eng"}],"oa":1,"intvolume":" 463","abstract":[{"lang":"eng","text":"We present new results from the widest narrow-band survey search for Lyα emitters at z = 5.7, just after reionization. We survey a total of 7 deg2 spread over the COSMOS, UDS and SA22 fields. We find over 11 000 line emitters, out of which 514 are robust Lyα candidates at z = 5.7 within a volume of 6.3 × 106 Mpc3. Our Lyα emitters span a wide range in Lyα luminosities, from faint to bright (LLyα ∼ 1042.5–44 erg s−1) and rest-frame equivalent widths (EW0 ∼ 25–1000 Å) in a single, homogeneous data set. By combining all our fields, we find that the faint end slope of the z = 5.7 Lyα luminosity function is very steep, with α=−2.3+0.4−0.3. We also present an updated z = 6.6 Lyα luminosity function, based on comparable volumes and obtained with the same methods, which we directly compare with that at z = 5.7. We find a significant decline of the number density of faint Lyα emitters from z = 5.7 to 6.6 (by 0.5 ± 0.1 dex), but no evolution at the bright end/no evolution in L*. Faint Lyα emitters at z = 6.6 show much more extended haloes than those at z = 5.7, suggesting that neutral Hydrogen plays an important role, increasing the scattering and leading to observations missing faint Lyα emission within the epoch of reionization. Altogether, our results suggest that we are observing patchy reionization which happens first around the brightest Lyα emitters, allowing the number densities of those sources to remain unaffected by the increase of neutral Hydrogen fraction from z ∼ 5 to 7."}],"month":"12","volume":463,"external_id":{"arxiv":["1606.07435"]},"publication_status":"published","author":[{"full_name":"Santos, Sérgio","last_name":"Santos","first_name":"Sérgio"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"title":"The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization","_id":"11574","citation":{"chicago":"Santos, Sérgio, David Sobral, and Jorryt J Matthee. “The Lyα Luminosity Function at Z= 5.7–6.6 and the Steep Drop of the Faint End: Implications for Reionization.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw2076.","ista":"Santos S, Sobral D, Matthee JJ. 2016. The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization. Monthly Notices of the Royal Astronomical Society. 463(2), 1678–1691.","short":"S. Santos, D. Sobral, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 463 (2016) 1678–1691.","ieee":"S. Santos, D. Sobral, and J. J. Matthee, “The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization,” Monthly Notices of the Royal Astronomical Society, vol. 463, no. 2. Oxford University Press, pp. 1678–1691, 2016.","apa":"Santos, S., Sobral, D., & Matthee, J. J. (2016). The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw2076","mla":"Santos, Sérgio, et al. “The Lyα Luminosity Function at Z= 5.7–6.6 and the Steep Drop of the Faint End: Implications for Reionization.” Monthly Notices of the Royal Astronomical Society, vol. 463, no. 2, Oxford University Press, 2016, pp. 1678–91, doi:10.1093/mnras/stw2076.","ama":"Santos S, Sobral D, Matthee JJ. The Lyα luminosity function at z= 5.7–6.6 and the steep drop of the faint end: Implications for reionization. Monthly Notices of the Royal Astronomical Society. 2016;463(2):1678-1691. doi:10.1093/mnras/stw2076"},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: high-redshift","galaxies: luminosity function","mass function","cosmology: observations","dark ages","reionization","first stars"],"publication":"Monthly Notices of the Royal Astronomical Society","publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1606.07435"}],"day":"01","date_updated":"2022-08-19T08:09:54Z","page":"1678-1691","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","oa_version":"Preprint","quality_controlled":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"doi":"10.1093/mnras/stw2076","status":"public","type":"journal_article","extern":"1","article_processing_charge":"No","arxiv":1},{"day":"01","date_updated":"2022-08-19T08:12:07Z","_id":"11575","title":"The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations","publisher":"Oxford University Press","main_file_link":[{"url":"https://arxiv.org/abs/1510.08067","open_access":"1"}],"citation":{"ieee":"C. del P. Lagos et al., “The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations,” Monthly Notices of the Royal Astronomical Society, vol. 459, no. 3. Oxford University Press, pp. 2632–2650, 2016.","apa":"Lagos, C. del P., Theuns, T., Schaye, J., Furlong, M., Bower, R. G., Schaller, M., … Matthee, J. J. (2016). The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw717","mla":"Lagos, Claudia del P., et al. “The Fundamental Plane of Star Formation in Galaxies Revealed by the EAGLE Hydrodynamical Simulations.” Monthly Notices of the Royal Astronomical Society, vol. 459, no. 3, Oxford University Press, 2016, pp. 2632–50, doi:10.1093/mnras/stw717.","ama":"Lagos C del P, Theuns T, Schaye J, et al. The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices of the Royal Astronomical Society. 2016;459(3):2632-2650. doi:10.1093/mnras/stw717","chicago":"Lagos, Claudia del P., Tom Theuns, Joop Schaye, Michelle Furlong, Richard G. Bower, Matthieu Schaller, Robert A. Crain, James W. Trayford, and Jorryt J Matthee. “The Fundamental Plane of Star Formation in Galaxies Revealed by the EAGLE Hydrodynamical Simulations.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw717.","ista":"Lagos C del P, Theuns T, Schaye J, Furlong M, Bower RG, Schaller M, Crain RA, Trayford JW, Matthee JJ. 2016. The Fundamental Plane of star formation in galaxies revealed by the EAGLE hydrodynamical simulations. Monthly Notices of the Royal Astronomical Society. 459(3), 2632–2650.","short":"C. del P. Lagos, T. Theuns, J. Schaye, M. Furlong, R.G. Bower, M. Schaller, R.A. Crain, J.W. Trayford, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 459 (2016) 2632–2650."},"keyword":["Space and Planetary Science","Astronomy and Astrophysics stars: formation","ISM: evolution","galaxies: evolution","galaxies: formation","galaxies: ISM"],"publication":"Monthly Notices of the Royal Astronomical Society","article_processing_charge":"No","arxiv":1,"extern":"1","type":"journal_article","page":"2632-2650","scopus_import":"1","oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","quality_controlled":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"doi":"10.1093/mnras/stw717","month":"07","abstract":[{"text":"We investigate correlations between different physical properties of star-forming galaxies in the ‘Evolution and Assembly of GaLaxies and their Environments’ (EAGLE) cosmological hydrodynamical simulation suite over the redshift range 0 ≤ z ≤ 4.5. A principal component analysis reveals that neutral gas fraction (fgas,neutral), stellar mass (Mstellar) and star formation rate (SFR) account for most of the variance seen in the population, with galaxies tracing a two-dimensional, nearly flat, surface in the three-dimensional space of fgas, neutral–Mstellar–SFR with little scatter. The location of this plane varies little with redshift, whereas galaxies themselves move along the plane as their fgas, neutral and SFR drop with redshift. The positions of galaxies along the plane are highly correlated with gas metallicity. The metallicity can therefore be robustly predicted from fgas, neutral, or from the Mstellar and SFR. We argue that the appearance of this ‘Fundamental Plane of star formation’ is a consequence of self-regulation, with the plane's curvature set by the dependence of the SFR on gas density and metallicity. We analyse a large compilation of observations spanning the redshift range 0 ≲ z ≲ 3, and find that such a plane is also present in the data. The properties of the observed Fundamental Plane of star formation are in good agreement with EAGLE's predictions.","lang":"eng"}],"volume":459,"date_created":"2022-07-13T10:21:24Z","article_type":"original","year":"2016","date_published":"2016-07-01T00:00:00Z","intvolume":" 459","language":[{"iso":"eng"}],"acknowledgement":"We thank Luca Cortese, Matt Bothwell, Paola Santini and Tim Davis for providing observational data sets, and Aaron Robotham, Luca Cortese and Barbara Catinella for useful discussions. CdPL is funded by a Discovery Early Career Researcher Award (DE150100618). CdPL also thanks the MERAC Foundation for a Postdoctoral Research Award. This work used the DiRAC Data Centric system at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk). This equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, and STFC DiRAC Operations grant ST/K003267/1 and Durham University. DiRAC is part of the National E-Infrastructure. Support was also received via the Interuniversity Attraction Poles Programme initiated by the Belgian Science Policy Office ([AP P7/08 CHARM]), the National Science Foundation under grant no. NSF PHY11-25915, and the UK Science and Technology Facilities Council (grant numbers ST/F001166/1 and ST/I000976/1) via rolling and consolidating grants awarded to the ICC. The research was supported in part by the European Research Council under the European Union‘s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement 278594-GasAroundGalaxies.","oa":1,"issue":"3","publication_status":"published","external_id":{"arxiv":["1510.08067"]},"author":[{"first_name":"Claudia del P.","last_name":"Lagos","full_name":"Lagos, Claudia del P."},{"last_name":"Theuns","first_name":"Tom","full_name":"Theuns, Tom"},{"full_name":"Schaye, Joop","first_name":"Joop","last_name":"Schaye"},{"full_name":"Furlong, Michelle","first_name":"Michelle","last_name":"Furlong"},{"first_name":"Richard G.","last_name":"Bower","full_name":"Bower, Richard G."},{"last_name":"Schaller","first_name":"Matthieu","full_name":"Schaller, Matthieu"},{"full_name":"Crain, Robert A.","first_name":"Robert A.","last_name":"Crain"},{"full_name":"Trayford, James W.","last_name":"Trayford","first_name":"James W."},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"}]},{"page":"1739-1752","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","scopus_import":"1","status":"public","quality_controlled":"1","doi":"10.1093/mnras/stw022","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"article_processing_charge":"No","arxiv":1,"type":"journal_article","extern":"1","title":"The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies","_id":"11576","publisher":"Oxford University Press","main_file_link":[{"url":"https://arxiv.org/abs/1601.02266","open_access":"1"}],"citation":{"chicago":"Sobral, David, Saul A. Kohn, Philip N. Best, Ian Smail, Chris M. Harrison, John Stott, João Calhau, and Jorryt J Matthee. “The Most Luminous H α Emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and Star-Forming Galaxies.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw022.","ista":"Sobral D, Kohn SA, Best PN, Smail I, Harrison CM, Stott J, Calhau J, Matthee JJ. 2016. The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical Society. 457(2), 1739–1752.","short":"D. Sobral, S.A. Kohn, P.N. Best, I. Smail, C.M. Harrison, J. Stott, J. Calhau, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 457 (2016) 1739–1752.","ieee":"D. Sobral et al., “The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies,” Monthly Notices of the Royal Astronomical Society, vol. 457, no. 2. Oxford University Press, pp. 1739–1752, 2016.","apa":"Sobral, D., Kohn, S. A., Best, P. N., Smail, I., Harrison, C. M., Stott, J., … Matthee, J. J. (2016). The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw022","mla":"Sobral, David, et al. “The Most Luminous H α Emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and Star-Forming Galaxies.” Monthly Notices of the Royal Astronomical Society, vol. 457, no. 2, Oxford University Press, 2016, pp. 1739–52, doi:10.1093/mnras/stw022.","ama":"Sobral D, Kohn SA, Best PN, et al. The most luminous H α emitters at z ∼ 0.8–2.23 from HiZELS: Evolution of AGN and star-forming galaxies. Monthly Notices of the Royal Astronomical Society. 2016;457(2):1739-1752. doi:10.1093/mnras/stw022"},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations"],"publication":"Monthly Notices of the Royal Astronomical Society","day":"01","date_updated":"2022-08-19T08:15:21Z","publication_status":"published","external_id":{"arxiv":["1601.02266"]},"author":[{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"last_name":"Kohn","first_name":"Saul A.","full_name":"Kohn, Saul A."},{"full_name":"Best, Philip N.","last_name":"Best","first_name":"Philip N."},{"last_name":"Smail","first_name":"Ian","full_name":"Smail, Ian"},{"full_name":"Harrison, Chris M.","first_name":"Chris M.","last_name":"Harrison"},{"last_name":"Stott","first_name":"John","full_name":"Stott, John"},{"first_name":"João","last_name":"Calhau","full_name":"Calhau, João"},{"first_name":"Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"}],"date_created":"2022-07-13T12:50:36Z","article_type":"original","year":"2016","date_published":"2016-04-01T00:00:00Z","intvolume":" 457","oa":1,"issue":"2","language":[{"iso":"eng"}],"acknowledgement":"The authors would like to thank the anonymous reviewer for the many helpful comments and suggestions which greatly improved the clarity and quality of this work. DS and SAK acknowledge financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship. DS also acknowledges funding from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010) and from FCT grant PEst-OE/FIS/UI2751/2014. Part of this project was undertaken during the inaugural Leiden/ESA Astrophysics Program for Summer Students (LEAPS). IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson merit award. CH acknowledges support from STFC. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 087.A-0337 and ID 089.A-0965. Also based on data from the Telescopio Nazionale Galileo, with time awarded through OPTICON programmes 2011A/026 and 2012A020 and the William Herschel Telescope under programme W12BN007. The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group in the Spanish\r\nObservatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The authors wish to thank all the help given by the telescope staff from all the observatories used in this study: ESO staff in La Silla, and the TNG and WHT staff in La Palma. This publication makes use of data products from the Two Micron All-Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation.","month":"04","abstract":[{"lang":"eng","text":"We use new near-infrared spectroscopic observations to investigate the nature and evolution of the most luminous Hα emitters at z ∼ 0.8–2.23, which evolve strongly in number density over this period, and compare them to more typical Hα emitters. We study 59 luminous Hα emitters with LHα > L∗Hα, roughly equally split per redshift slice at z ∼ 0.8, 1.47 and 2.23 from the HiZELS and CF-HiZELS surveys. We find that, overall, 30 ± 8 per cent are active galactic nuclei [AGNs; 80 ± 30 per cent of these AGNs are broad-line AGNs, BL-AGNs], and we find little to no evolution in the AGN fraction with redshift, within the errors. However, the AGN fraction increases strongly with Hα luminosity and correlates best with LHα/L∗Hα(z). While LHα ≤ L∗Hα(z) Hα emitters are largely dominated by star-forming galaxies (>80 per cent), the most luminous Hα emitters (LHα>10L∗Hα(z)) at any cosmic time are essentially all BL-AGN. Using our AGN-decontaminated sample of luminous star-forming galaxies, and integrating down to a fixed Hα luminosity, we find a factor of ∼1300 evolution in the star formation rate density from z = 0 to 2.23. This is much stronger than the evolution from typical Hα star-forming galaxies and in line with the evolution seen for constant luminosity cuts used to select ‘ultraluminous’ infrared galaxies and/or sub-millimetre galaxies. By taking into account the evolution in the typical Hα luminosity, we show that the most strongly star-forming Hα-selected galaxies at any epoch (LHα>L∗Hα(z)) contribute the same fractional amount of ≈15 per cent to the total star formation rate density, at least up to z = 2.23."}],"volume":457},{"publication_status":"published","external_id":{"arxiv":["1602.02756"]},"author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"first_name":"Iván","last_name":"Oteo","full_name":"Oteo, Iván"},{"full_name":"Best, Philip","first_name":"Philip","last_name":"Best"},{"last_name":"Smail","first_name":"Ian","full_name":"Smail, Ian"},{"first_name":"Huub","last_name":"Röttgering","full_name":"Röttgering, Huub"},{"first_name":"Ana","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana"}],"date_created":"2022-07-14T08:51:37Z","year":"2016","article_type":"original","date_published":"2016-05-01T00:00:00Z","intvolume":" 458","acknowledgement":"We thank the anonymous referee for constructive comments and suggestions which have improved the quality of this work. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS and JM acknowledge financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship, and DS from FCT through a FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010) and from FCT grant PEst-OE/FIS/UI2751/2014. IO acknowledges support from the European Research Council (ERC) in the form of Advanced Investigator Programme, COSMICISM, 321302. HR acknowledges support from the ERC Advanced Investigator programme NewClusters 321271. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson Merit Award. APA acknowledges support from the Fundac¸ao para a Ciencia e para a Tecnologia (FCT) through the Fellowship SFRH/BD/52706/2014.\r\nBased on observations made with the Isaac Newton Telescope (proposals 2013AN002, 2013BN008, 2014AC88, 2014AN002, 2014BN006, 2014BC118) operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrof´ısica de Canarias. We acknowledge the tremendous work that has been done by both COSMOS and UKIDSS UDS/SXDF teams in assembling such large, state-ofthe-art multi-wavelength data sets over such wide areas, as those have been crucial for the results presented in this paper. The sample of HAEs is publicly available from Sobral et al. (2013).\r\nWe have benefited greatly from the publically available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages, the imaging tools SEXTRACTOR, SWARP and SCAMP (Bertin & Arnouts 1996; Bertin 2006, 2010) and the TOPCAT analysis program (Taylor 2005).","issue":"1","oa":1,"language":[{"iso":"eng"}],"month":"05","abstract":[{"lang":"eng","text":"We present the first results from our CAlibrating LYMan α with Hα (CALYMHA) pilot survey at the Isaac Newton Telescope. We measure Lyα emission for 488 Hα selected galaxies at z = 2.23 from High-z Emission Line Survey in the COSMOS and UDS fields with a specially designed narrow-band filter (λc = 3918 Å, Δλ = 52 Å). We find 17 dual Hα-Lyα emitters [fLyα > 5 × 10−17 erg s−1 cm−2, of which five are X-ray active galactic nuclei (AGN)]. For star-forming galaxies, we find a range of Lyα escape fractions (fesc, measured with 3 arcsec apertures) from 2 to 30 per cent. These galaxies have masses from 3 × 108 M⊙ to 1011 M⊙ and dust attenuations E(B − V) = 0–0.5. Using stacking, we measure a median escape fraction of 1.6 ± 0.5 per cent (4.0 ± 1.0 per cent without correcting Hα for dust), but show that this depends on galaxy properties. The stacked fesc tends to decrease with increasing star formation rate and dust attenuation. However, at the highest masses and dust attenuations, we detect individual galaxies with fesc much higher than the typical values from stacking, indicating significant scatter in the values of fesc. Relations between fesc and UV slope are bimodal, with high fesc for either the bluest or reddest galaxies. We speculate that this bimodality and large scatter in the values of fesc is due to additional physical mechanisms such as outflows facilitating fesc for dusty/massive systems. Lyα is significantly more extended than Hα and the UV. fesc continues to increase up to at least 20 kpc (3σ, 40 kpc [2σ]) for typical star-forming galaxies and thus the aperture is the most important predictor of fesc."}],"volume":458,"page":"449-467","oa_version":"Preprint","scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","quality_controlled":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"doi":"10.1093/mnras/stw322","article_processing_charge":"No","arxiv":1,"extern":"1","type":"journal_article","title":"The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23","_id":"11578","publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1602.02756"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM"],"citation":{"ama":"Matthee JJ, Sobral D, Oteo I, et al. The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23. Monthly Notices of the Royal Astronomical Society. 2016;458(1):449-467. doi:10.1093/mnras/stw322","mla":"Matthee, Jorryt J., et al. “The CALYMHA Survey: Lyα Escape Fraction and Its Dependence on Galaxy Properties at z = 2.23.” Monthly Notices of the Royal Astronomical Society, vol. 458, no. 1, Oxford University Press, 2016, pp. 449–67, doi:10.1093/mnras/stw322.","apa":"Matthee, J. J., Sobral, D., Oteo, I., Best, P., Smail, I., Röttgering, H., & Paulino-Afonso, A. (2016). The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw322","ieee":"J. J. Matthee et al., “The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23,” Monthly Notices of the Royal Astronomical Society, vol. 458, no. 1. Oxford University Press, pp. 449–467, 2016.","short":"J.J. Matthee, D. Sobral, I. Oteo, P. Best, I. Smail, H. Röttgering, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society 458 (2016) 449–467.","ista":"Matthee JJ, Sobral D, Oteo I, Best P, Smail I, Röttgering H, Paulino-Afonso A. 2016. The CALYMHA survey: Lyα escape fraction and its dependence on galaxy properties at z = 2.23. Monthly Notices of the Royal Astronomical Society. 458(1), 449–467.","chicago":"Matthee, Jorryt J, David Sobral, Iván Oteo, Philip Best, Ian Smail, Huub Röttgering, and Ana Paulino-Afonso. “The CALYMHA Survey: Lyα Escape Fraction and Its Dependence on Galaxy Properties at z = 2.23.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw322."},"publication":"Monthly Notices of the Royal Astronomical Society","day":"01","date_updated":"2024-10-14T11:36:40Z"},{"intvolume":" 466","issue":"2","oa":1,"language":[{"iso":"eng"}],"date_created":"2024-03-26T10:41:04Z","date_published":"2016-12-17T00:00:00Z","article_type":"original","year":"2016","volume":466,"month":"12","abstract":[{"lang":"eng","text":"The recent discovery of gravitational radiation from merging black holes poses a challenge of how to organize the electromagnetic follow-up of gravitational-wave events as well as observed bursts of neutrinos. We propose a technique to select the galaxies that are most likely to host the event given some assumptions of whether the particular event is associated with recent star formation, low-metallicity stars or simply proportional to the total stellar mass in the galaxy. We combine data from the 2-MASS Photometric Redshift Galaxy Catalogue with results from galaxy formation simulations to develop observing strategies that potentially reduce the area of sky to search by up to a factor of 2 relative to an unweighted search of galaxies, and a factor of 20 to a search over the entire LIGO localization region."}],"author":[{"first_name":"Elisa","last_name":"Antolini","full_name":"Antolini, Elisa"},{"orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","last_name":"Caiazzo"},{"first_name":"Romeel","last_name":"Davé","full_name":"Davé, Romeel"},{"full_name":"Heyl, Jeremy S.","first_name":"Jeremy S.","last_name":"Heyl"}],"publication_status":"published","external_id":{"arxiv":["1612.04412"]},"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.1612.04412","open_access":"1"}],"publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"ama":"Antolini E, Caiazzo I, Davé R, Heyl JS. Using galaxy formation simulations to optimize LIGO follow-up observations. Monthly Notices of the Royal Astronomical Society. 2016;466(2):2212-2216. doi:10.1093/mnras/stw3292","mla":"Antolini, Elisa, et al. “Using Galaxy Formation Simulations to Optimize LIGO Follow-up Observations.” Monthly Notices of the Royal Astronomical Society, vol. 466, no. 2, Oxford University Press, 2016, pp. 2212–16, doi:10.1093/mnras/stw3292.","apa":"Antolini, E., Caiazzo, I., Davé, R., & Heyl, J. S. (2016). Using galaxy formation simulations to optimize LIGO follow-up observations. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stw3292","ieee":"E. Antolini, I. Caiazzo, R. Davé, and J. S. Heyl, “Using galaxy formation simulations to optimize LIGO follow-up observations,” Monthly Notices of the Royal Astronomical Society, vol. 466, no. 2. Oxford University Press, pp. 2212–2216, 2016.","short":"E. Antolini, I. Caiazzo, R. Davé, J.S. Heyl, Monthly Notices of the Royal Astronomical Society 466 (2016) 2212–2216.","ista":"Antolini E, Caiazzo I, Davé R, Heyl JS. 2016. Using galaxy formation simulations to optimize LIGO follow-up observations. Monthly Notices of the Royal Astronomical Society. 466(2), 2212–2216.","chicago":"Antolini, Elisa, Ilaria Caiazzo, Romeel Davé, and Jeremy S. Heyl. “Using Galaxy Formation Simulations to Optimize LIGO Follow-up Observations.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2016. https://doi.org/10.1093/mnras/stw3292."},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"title":"Using galaxy formation simulations to optimize LIGO follow-up observations","_id":"15242","date_updated":"2024-04-08T07:05:23Z","day":"17","status":"public","doi":"10.1093/mnras/stw3292","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"quality_controlled":"1","scopus_import":"1","oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"2212-2216","arxiv":1,"article_processing_charge":"No","extern":"1","type":"journal_article"},{"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stw3210"}],"publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"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","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.","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.","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","short":"B. Greig, A. Mesinger, I.D. McGreer, S. Gallerani, Z. Haiman, Monthly Notices of the Royal Astronomical Society 466 (2016) 1814–1838.","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.","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."},"_id":"17621","title":"Lyα emission-line reconstruction for high-z QSOs","date_updated":"2024-09-24T08:31:25Z","day":"10","status":"public","publication_identifier":{"issn":["0035-8711","1365-2966"]},"doi":"10.1093/mnras/stw3210","quality_controlled":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","oa_version":"Published Version","scopus_import":"1","page":"1814-1838","article_processing_charge":"No","type":"journal_article","extern":"1","intvolume":" 466","issue":"2","oa":1,"language":[{"iso":"eng"}],"date_created":"2024-09-05T13:49:52Z","date_published":"2016-12-10T00:00:00Z","article_type":"original","year":"2016","volume":466,"month":"12","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"}],"author":[{"full_name":"Greig, Bradley","first_name":"Bradley","last_name":"Greig"},{"full_name":"Mesinger, Andrei","first_name":"Andrei","last_name":"Mesinger"},{"first_name":"Ian D.","last_name":"McGreer","full_name":"McGreer, Ian D."},{"last_name":"Gallerani","first_name":"Simona","full_name":"Gallerani, Simona"},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman"}],"publication_status":"published"},{"publication_status":"published","author":[{"first_name":"Nicholas C.","last_name":"Stone","full_name":"Stone, Nicholas C."},{"full_name":"Metzger, Brian D.","first_name":"Brian D.","last_name":"Metzger"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","last_name":"Haiman","first_name":"Zoltán"}],"article_type":"original","year":"2016","date_published":"2016-09-08T00:00:00Z","date_created":"2024-09-06T07:35:10Z","issue":"1","language":[{"iso":"eng"}],"oa":1,"intvolume":" 464","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."}],"month":"09","volume":464,"page":"946-954","oa_version":"Published Version","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","scopus_import":"1","quality_controlled":"1","publication_identifier":{"issn":["0035-8711","1365-2966"]},"doi":"10.1093/mnras/stw2260","status":"public","extern":"1","type":"journal_article","article_processing_charge":"No","title":"Assisted inspirals of stellar mass black holes embedded in AGN discs: Solving the ‘final au problem’","_id":"17656","citation":{"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.","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.","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","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.","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.","short":"N.C. Stone, B.D. Metzger, Z. Haiman, Monthly Notices of the Royal Astronomical Society 464 (2016) 946–954."},"publication":"Monthly Notices of the Royal Astronomical Society","publisher":"Oxford University Press","main_file_link":[{"url":"https://doi.org/10.1093/mnras/stw2260","open_access":"1"}],"day":"08","date_updated":"2024-09-25T07:05:41Z"},{"author":[{"full_name":"D'Orazio, Daniel J.","first_name":"Daniel J.","last_name":"D'Orazio"},{"last_name":"Haiman","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán"},{"first_name":"Paul","last_name":"Duffell","full_name":"Duffell, Paul"},{"full_name":"MacFadyen, Andrew","first_name":"Andrew","last_name":"MacFadyen"},{"full_name":"Farris, Brian","last_name":"Farris","first_name":"Brian"}],"publication_status":"published","volume":459,"month":"04","abstract":[{"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.","lang":"eng"}],"intvolume":" 459","language":[{"iso":"eng"}],"oa":1,"issue":"3","date_created":"2024-09-06T07:36:39Z","date_published":"2016-04-06T00:00:00Z","article_type":"original","year":"2016","article_processing_charge":"No","extern":"1","type":"journal_article","status":"public","publication_identifier":{"issn":["0035-8711","1365-2966"]},"doi":"10.1093/mnras/stw792","quality_controlled":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","oa_version":"Published Version","scopus_import":"1","page":"2379-2393","date_updated":"2024-09-25T07:14:30Z","day":"06","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stw792"}],"publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"short":"D.J. D’Orazio, Z. Haiman, P. Duffell, A. MacFadyen, B. Farris, Monthly Notices of the Royal Astronomical Society 459 (2016) 2379–2393.","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.","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.","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","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.","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.","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"},"title":"A transition in circumbinary accretion discs at a binary mass ratio of 1:25","_id":"17658"},{"author":[{"full_name":"Inayoshi, Kohei","last_name":"Inayoshi","first_name":"Kohei"},{"last_name":"Kashiyama","first_name":"Kazumi","full_name":"Kashiyama, Kazumi"},{"full_name":"Visbal, Eli","first_name":"Eli","last_name":"Visbal"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","last_name":"Haiman","first_name":"Zoltán"}],"publication_status":"published","intvolume":" 461","language":[{"iso":"eng"}],"oa":1,"issue":"3","date_created":"2024-09-06T07:37:31Z","date_published":"2016-06-21T00:00:00Z","article_type":"original","year":"2016","volume":461,"month":"06","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."}],"status":"public","doi":"10.1093/mnras/stw1431","publication_identifier":{"issn":["0035-8711","1365-2966"]},"quality_controlled":"1","scopus_import":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","oa_version":"Published Version","page":"2722-2727","article_processing_charge":"No","type":"journal_article","extern":"1","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stw1431"}],"publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"short":"K. Inayoshi, K. Kashiyama, E. Visbal, Z. Haiman, Monthly Notices of the Royal Astronomical Society 461 (2016) 2722–2727.","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.","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.","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","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.","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","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."},"_id":"17659","title":"Gravitational wave background from Population III binary black holes consistent with cosmic reionization","date_updated":"2024-09-25T07:17:34Z","day":"21"},{"date_updated":"2024-09-25T08:28:42Z","day":"28","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"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.","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.","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","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.","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"},"main_file_link":[{"url":"https://doi.org/10.1093/mnras/stw1838","open_access":"1"}],"publisher":"Oxford University Press","title":"A population of short-period variable quasars from PTF as supermassive black hole binary candidates","_id":"17672","type":"journal_article","extern":"1","article_processing_charge":"No","doi":"10.1093/mnras/stw1838","publication_identifier":{"issn":["0035-8711","1365-2966"]},"quality_controlled":"1","status":"public","scopus_import":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","oa_version":"Published Version","page":"2145-2171","volume":463,"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."}],"month":"07","language":[{"iso":"eng"}],"oa":1,"issue":"2","intvolume":" 463","date_published":"2016-07-28T00:00:00Z","year":"2016","article_type":"original","date_created":"2024-09-06T07:49:15Z","author":[{"full_name":"Charisi, M.","last_name":"Charisi","first_name":"M."},{"full_name":"Bartos, I.","last_name":"Bartos","first_name":"I."},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman"},{"last_name":"Price-Whelan","first_name":"A. M.","full_name":"Price-Whelan, A. M."},{"full_name":"Graham, M. J.","first_name":"M. J.","last_name":"Graham"},{"full_name":"Bellm, E. C.","first_name":"E. C.","last_name":"Bellm"},{"full_name":"Laher, R. R.","last_name":"Laher","first_name":"R. R."},{"first_name":"S.","last_name":"Márka","full_name":"Márka, S."}],"publication_status":"published"},{"intvolume":" 461","language":[{"iso":"eng"}],"oa":1,"issue":"4","date_created":"2024-09-06T08:39:53Z","date_published":"2016-07-08T00:00:00Z","article_type":"original","year":"2016","volume":461,"month":"07","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."}],"author":[{"full_name":"Sakurai, Yuya","last_name":"Sakurai","first_name":"Yuya"},{"first_name":"Kohei","last_name":"Inayoshi","full_name":"Inayoshi, Kohei"},{"first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"}],"publication_status":"published","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stw1652"}],"publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","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.","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.","short":"Y. Sakurai, K. Inayoshi, Z. Haiman, Monthly Notices of the Royal Astronomical Society 461 (2016) 4496–4504.","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","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.","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.","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"},"_id":"17693","title":"Hyper-Eddington mass accretion on to a black hole with super-Eddington luminosity","date_updated":"2024-09-25T10:02:57Z","day":"08","status":"public","doi":"10.1093/mnras/stw1652","publication_identifier":{"issn":["0035-8711","1365-2966"]},"quality_controlled":"1","oa_version":"Published Version","scopus_import":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","page":"4496-4504","article_processing_charge":"No","type":"journal_article","extern":"1"},{"scopus_import":"1","oa_version":"Published Version","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","quality_controlled":"1","publication_identifier":{"issn":["0035-8711","1365-2966"]},"doi":"10.1093/mnras/stw3351","status":"public","extern":"1","type":"journal_article","article_processing_charge":"No","article_number":"stw3351","publication_status":"published","author":[{"last_name":"Greig","first_name":"Bradley","full_name":"Greig, Bradley"},{"first_name":"Andrei","last_name":"Mesinger","full_name":"Mesinger, Andrei"},{"first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"full_name":"Simcoe, Robert A.","first_name":"Robert A.","last_name":"Simcoe"}],"year":"2016","article_type":"original","date_published":"2016-12-24T00:00:00Z","title":"Are we witnessing the epoch of reionization at z=7.1 from the spectrum of J1120+0641?","_id":"17699","date_created":"2024-09-06T08:45:10Z","oa":1,"citation":{"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","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.","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","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.","short":"B. Greig, A. Mesinger, Z. Haiman, R.A. Simcoe, Monthly Notices of the Royal Astronomical Society (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.","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."},"language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","publisher":"Oxford University Press","main_file_link":[{"url":"https://doi.org/10.1093/mnras/stw3351","open_access":"1"}],"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)."}],"day":"24","month":"12","date_updated":"2024-09-25T11:19:08Z"},{"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","oa_version":"Published Version","scopus_import":"1","page":"4122-4134","status":"public","doi":"10.1093/mnras/stw1241","publication_identifier":{"issn":["0035-8711","1365-2966"]},"quality_controlled":"1","article_processing_charge":"No","type":"journal_article","extern":"1","title":"Intermediate-mass black holes from Population III remnants in the first galactic nuclei","_id":"17700","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stw1241"}],"publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"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.","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.","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","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","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.","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.","short":"T. Ryu, T.L. Tanaka, R. Perna, Z. Haiman, Monthly Notices of the Royal Astronomical Society 460 (2016) 4122–4134."},"day":"24","date_updated":"2024-09-25T11:22:16Z","publication_status":"published","author":[{"full_name":"Ryu, Taeho","last_name":"Ryu","first_name":"Taeho"},{"full_name":"Tanaka, Takamitsu L.","first_name":"Takamitsu L.","last_name":"Tanaka"},{"full_name":"Perna, Rosalba","last_name":"Perna","first_name":"Rosalba"},{"last_name":"Haiman","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán"}],"date_created":"2024-09-06T08:46:28Z","date_published":"2016-05-24T00:00:00Z","year":"2016","article_type":"original","intvolume":" 460","language":[{"iso":"eng"}],"oa":1,"issue":"4","month":"05","abstract":[{"lang":"eng","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."}],"volume":460},{"author":[{"full_name":"Inayoshi, Kohei","last_name":"Inayoshi","first_name":"Kohei"},{"first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"first_name":"Jeremiah P.","last_name":"Ostriker","full_name":"Ostriker, Jeremiah P."}],"publication_status":"published","intvolume":" 459","issue":"4","language":[{"iso":"eng"}],"oa":1,"date_created":"2024-09-06T08:54:12Z","date_published":"2016-04-12T00:00:00Z","article_type":"original","year":"2016","volume":459,"month":"04","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."}],"status":"public","publication_identifier":{"issn":["0035-8711","1365-2966"]},"doi":"10.1093/mnras/stw836","quality_controlled":"1","oa_version":"Published Version","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","scopus_import":"1","page":"3738-3755","article_processing_charge":"No","extern":"1","type":"journal_article","main_file_link":[{"url":"https://doi.org/10.1093/mnras/stw836","open_access":"1"}],"publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"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.","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.","short":"K. Inayoshi, Z. Haiman, J.P. Ostriker, Monthly Notices of the Royal Astronomical Society 459 (2016) 3738–3755.","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.","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","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.","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"},"_id":"17709","title":"Hyper-Eddington accretion flows on to massive black holes","date_updated":"2024-09-25T12:00:22Z","day":"12"},{"volume":453,"month":"11","abstract":[{"lang":"eng","text":"CR7 is the brightest z = 6.6 Ly α emitter (LAE) known to date, and spectroscopic follow-up by Sobral et al. suggests that CR7 might host Population (Pop) III stars. We examine this interpretation using cosmological hydrodynamical simulations. Several simulated galaxies show the same ‘Pop III wave’ pattern observed in CR7. However, to reproduce the extreme CR7 Ly α/He II1640 line luminosities (Lα/HeII) a top-heavy initial mass function and a massive ( ≳ 107 M⊙) Pop III burst with age ≲ 2 Myr are required. Assuming that the observed properties of Ly α and He II emission are typical for Pop III, we predict that in the COSMOS/UDS/SA22 fields, 14 out of the 30 LAEs at z = 6.6 with Lα > 1043.3 erg s−1 should also host Pop III stars producing an observable LHeII≳1042.7ergs−1. As an alternate explanation, we explore the possibility that CR7 is instead powered by accretion on to a direct collapse black hole. Our model predicts Lα, LHeII, and X-ray luminosities that are in agreement with the observations. In any case, the observed properties of CR7 indicate that this galaxy is most likely powered by sources formed from pristine gas. We propose that further X-ray observations can distinguish between the two above scenarios."}],"intvolume":" 453","acknowledgement":"SS acknowledges support from the Netherlands Organization for Scientific research (NWO), VENI grant 639.041.233. RS acknowledges support from the European Research Council under the European Union (FP/2007-2013)/ERC grant agreement no. 306476. DS acknowledges (i) financial support from the NWO through a Veni fellowship and (ii) funding from FCT through a FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010) and from FCT grant PEstOE/FIS/UI2751/2014.","language":[{"iso":"eng"}],"oa":1,"issue":"3","date_created":"2022-07-14T08:58:36Z","article_type":"original","year":"2015","date_published":"2015-11-01T00:00:00Z","author":[{"first_name":"A.","last_name":"Pallottini","full_name":"Pallottini, A."},{"full_name":"Ferrara, A.","first_name":"A.","last_name":"Ferrara"},{"full_name":"Pacucci, F.","last_name":"Pacucci","first_name":"F."},{"first_name":"S.","last_name":"Gallerani","full_name":"Gallerani, S."},{"full_name":"Salvadori, S.","first_name":"S.","last_name":"Salvadori"},{"first_name":"R.","last_name":"Schneider","full_name":"Schneider, R."},{"last_name":"Schaerer","first_name":"D.","full_name":"Schaerer, D."},{"full_name":"Sobral, D.","first_name":"D.","last_name":"Sobral"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","first_name":"Jorryt J"}],"publication_status":"published","external_id":{"arxiv":["1506.07173"]},"date_updated":"2022-08-19T08:19:23Z","day":"01","publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1506.07173"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","black hole physics","stars: Population III","galaxies: high-redshift"],"citation":{"ama":"Pallottini A, Ferrara A, Pacucci F, et al. The brightest Lyα emitter: Pop III or black hole? Monthly Notices of the Royal Astronomical Society. 2015;453(3):2465-2470. doi:10.1093/mnras/stv1795","apa":"Pallottini, A., Ferrara, A., Pacucci, F., Gallerani, S., Salvadori, S., Schneider, R., … Matthee, J. J. (2015). The brightest Lyα emitter: Pop III or black hole? Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stv1795","mla":"Pallottini, A., et al. “The Brightest Lyα Emitter: Pop III or Black Hole?” Monthly Notices of the Royal Astronomical Society, vol. 453, no. 3, Oxford University Press, 2015, pp. 2465–70, doi:10.1093/mnras/stv1795.","ieee":"A. Pallottini et al., “The brightest Lyα emitter: Pop III or black hole?,” Monthly Notices of the Royal Astronomical Society, vol. 453, no. 3. Oxford University Press, pp. 2465–2470, 2015.","short":"A. Pallottini, A. Ferrara, F. Pacucci, S. Gallerani, S. Salvadori, R. Schneider, D. Schaerer, D. Sobral, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 453 (2015) 2465–2470.","ista":"Pallottini A, Ferrara A, Pacucci F, Gallerani S, Salvadori S, Schneider R, Schaerer D, Sobral D, Matthee JJ. 2015. The brightest Lyα emitter: Pop III or black hole? Monthly Notices of the Royal Astronomical Society. 453(3), 2465–2470.","chicago":"Pallottini, A., A. Ferrara, F. Pacucci, S. Gallerani, S. Salvadori, R. Schneider, D. Schaerer, D. Sobral, and Jorryt J Matthee. “The Brightest Lyα Emitter: Pop III or Black Hole?” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv1795."},"publication":"Monthly Notices of the Royal Astronomical Society","_id":"11579","title":"The brightest Lyα emitter: Pop III or black hole?","article_processing_charge":"No","arxiv":1,"extern":"1","type":"journal_article","status":"public","quality_controlled":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"doi":"10.1093/mnras/stv1795","page":"2465-2470","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","scopus_import":"1"},{"publication_status":"published","external_id":{"arxiv":["1502.06602"]},"author":[{"first_name":"D.","last_name":"Sobral","full_name":"Sobral, D."},{"first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"full_name":"Best, P. N.","first_name":"P. N.","last_name":"Best"},{"full_name":"Smail, I.","last_name":"Smail","first_name":"I."},{"first_name":"A. A.","last_name":"Khostovan","full_name":"Khostovan, A. A."},{"first_name":"B.","last_name":"Milvang-Jensen","full_name":"Milvang-Jensen, B."},{"full_name":"Kim, J.-W.","first_name":"J.-W.","last_name":"Kim"},{"full_name":"Stott, J.","last_name":"Stott","first_name":"J."},{"first_name":"J.","last_name":"Calhau","full_name":"Calhau, J."},{"last_name":"Nayyeri","first_name":"H.","full_name":"Nayyeri, H."},{"first_name":"B.","last_name":"Mobasher","full_name":"Mobasher, B."}],"month":"08","abstract":[{"lang":"eng","text":"We present results from the largest contiguous narrow-band survey in the near-infrared. We have used the wide-field infrared camera/Canada–France–Hawaii Telescope and the lowOH2 filter (1.187 ± 0.005 μm) to survey ≈10 deg2 of contiguous extragalactic sky in the SA22 field. A total of ∼6000 candidate emission-line galaxies are found. We use deep ugrizJK data to obtain robust photometric redshifts. We combine our data with the High-redshift(Z) Emission Line Survey (HiZELS), explore spectroscopic surveys (VVDS, VIPERS) and obtain our own spectroscopic follow-up with KMOS, FMOS and MOSFIRE to derive large samples of high-redshift emission-line selected galaxies: 3471 Hα emitters at z = 0.8, 1343 [O III] + Hβ emitters at z = 1.4 and 572 [O II] emitters at z = 2.2. We probe comoving volumes of >106 Mpc3 and find significant overdensities, including an 8.5σ (spectroscopically confirmed) overdensity of Hα emitters at z = 0.81. We derive Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4, 2.2, respectively, and present implications for future surveys such as Euclid. Our uniquely large volumes/areas allow us to subdivide the samples in thousands of randomized combinations of areas and provide a robust empirical measurement of sample/cosmic variance. We show that surveys for star-forming/emission-line galaxies at a depth similar to ours can only overcome cosmic-variance (errors <10 per cent) if they are based on volumes >5 × 105 Mpc3; errors on L* and ϕ* due to sample (cosmic) variance on surveys probing ∼104 and ∼105 Mpc3 are typically very high: ∼300 and ∼40–60 per cent, respectively."}],"volume":451,"date_created":"2022-07-14T09:02:22Z","date_published":"2015-08-11T00:00:00Z","article_type":"original","year":"2015","intvolume":" 451","language":[{"iso":"eng"}],"oa":1,"issue":"3","acknowledgement":"The authors wish to thank the anonymous reviewer for many helpful comments and suggestions which greatly improved the clarity and quality of this work. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship, from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010), from FCT grant PEst-OE/FIS/UI2751/2014, and from LSF and LKBF. JM acknowledges the award of a Huygens PhD fellowship. PNB is grateful for support from STFC. IRS acknowledges support from STFC, a Leverhulme Fellowship, the ERC Advanced Investigator programme DUSTYGAL and a Royal Society/Wolfson Merit Award. BMJ acknowledges support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the DNRF. The Dark Cosmology Centre is funded by the DNRF. JWK acknowledges support from the National Research Foundation of Korea (NRF) grant, no. 2008-0060544, funded by the Korea government (MSIP). JPS acknowledges support from STFC (ST/I001573/1). JC acknowledges support from the FCT-IF grant IF/01154/2012/CP0189/CT0010. The work was only possible due to OPTICON/FP7 and the invaluable access that it granted to the CFHT telescope. We would also like to acknowledge the excellent work done by CFHT staff in conducting the observations in service mode, and on delivering truly excellent data. We are also tremendously thankful to Kentaro Aoki for the incredible support while observing at Subaru with FMOS, and also to the Keck staff for the help with the observations with MOSFIRE. This work is based on observations obtained with WIRCam on the CFHT, OPTICON programme 2011B/029, 2012A019 and 2012B/016. Based on observations made with ESO telescopes at the La Silla Paranal Observatory under programmes IDs 60.A-9460 (data can be accessed through the ESO data archive), 087.A 0337 and 089.A-0965. Based on observations done with FMOS on Subaru under programme S14A-084, and on MOSFIRE/Keck observations under programme U066M. Part of the data on which this analysis is based are available from Sobral et al. (2013a). Dedicated to the memory of C. M. Sobral (1953-2014).","arxiv":1,"article_processing_charge":"No","extern":"1","type":"journal_article","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","oa_version":"Preprint","page":"2303-2323","status":"public","doi":"10.1093/mnras/stv1076","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"quality_controlled":"1","day":"11","date_updated":"2024-10-14T11:36:57Z","title":"CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 ","_id":"11580","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1502.06602"}],"publisher":"Oxford University Press","publication":"Monthly Notices of the Royal Astronomical Society","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: luminosity function","mass function","cosmology: observations","early Universe","large-scale structure of Universe"],"citation":{"short":"D. Sobral, J.J. Matthee, P.N. Best, I. Smail, A.A. Khostovan, B. Milvang-Jensen, J.-W. Kim, J. Stott, J. Calhau, H. Nayyeri, B. Mobasher, Monthly Notices of the Royal Astronomical Society 451 (2015) 2303–2323.","chicago":"Sobral, D., Jorryt J Matthee, P. N. Best, I. Smail, A. A. Khostovan, B. Milvang-Jensen, J.-W. Kim, et al. “CF-HiZELS, an ∼10 Deg2 Emission-Line Survey with Spectroscopic Follow-up: Hα, [O III] + Hβ and [O II] Luminosity Functions at z = 0.8, 1.4 and 2.2 .” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv1076.","ista":"Sobral D, Matthee JJ, Best PN, Smail I, Khostovan AA, Milvang-Jensen B, Kim J-W, Stott J, Calhau J, Nayyeri H, Mobasher B. 2015. CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society. 451(3), 2303–2323.","ama":"Sobral D, Matthee JJ, Best PN, et al. CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society. 2015;451(3):2303-2323. doi:10.1093/mnras/stv1076","ieee":"D. Sobral et al., “CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 ,” Monthly Notices of the Royal Astronomical Society, vol. 451, no. 3. Oxford University Press, pp. 2303–2323, 2015.","mla":"Sobral, D., et al. “CF-HiZELS, an ∼10 Deg2 Emission-Line Survey with Spectroscopic Follow-up: Hα, [O III] + Hβ and [O II] Luminosity Functions at z = 0.8, 1.4 and 2.2 .” Monthly Notices of the Royal Astronomical Society, vol. 451, no. 3, Oxford University Press, 2015, pp. 2303–23, doi:10.1093/mnras/stv1076.","apa":"Sobral, D., Matthee, J. J., Best, P. N., Smail, I., Khostovan, A. A., Milvang-Jensen, B., … Mobasher, B. (2015). CF-HiZELS, an ∼10 deg2 emission-line survey with spectroscopic follow-up: Hα, [O III] + Hβ and [O II] luminosity functions at z = 0.8, 1.4 and 2.2 . Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stv1076"}},{"day":"21","date_updated":"2024-10-14T11:37:15Z","_id":"11581","title":"Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"citation":{"short":"J.J. Matthee, D. Sobral, S. Santos, H. Röttgering, B. Darvish, B. Mobasher, Monthly Notices of the Royal Astronomical Society 451 (2015) 400–417.","ista":"Matthee JJ, Sobral D, Santos S, Röttgering H, Darvish B, Mobasher B. 2015. Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era. Monthly Notices of the Royal Astronomical Society. 451(1), 400–417.","chicago":"Matthee, Jorryt J, David Sobral, Sérgio Santos, Huub Röttgering, Behnam Darvish, and Bahram Mobasher. “Identification of the Brightest Lyα Emitters at z = 6.6: Implications for the Evolution of the Luminosity Function in the Reionization Era.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv947.","ama":"Matthee JJ, Sobral D, Santos S, Röttgering H, Darvish B, Mobasher B. Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era. Monthly Notices of the Royal Astronomical Society. 2015;451(1):400-417. doi:10.1093/mnras/stv947","mla":"Matthee, Jorryt J., et al. “Identification of the Brightest Lyα Emitters at z = 6.6: Implications for the Evolution of the Luminosity Function in the Reionization Era.” Monthly Notices of the Royal Astronomical Society, vol. 451, no. 1, Oxford University Press, 2015, pp. 400–17, doi:10.1093/mnras/stv947.","apa":"Matthee, J. J., Sobral, D., Santos, S., Röttgering, H., Darvish, B., & Mobasher, B. (2015). Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stv947","ieee":"J. J. Matthee, D. Sobral, S. Santos, H. Röttgering, B. Darvish, and B. Mobasher, “Identification of the brightest Lyα emitters at z = 6.6: implications for the evolution of the luminosity function in the reionization era,” Monthly Notices of the Royal Astronomical Society, vol. 451, no. 1. Oxford University Press, pp. 400–417, 2015."},"publication":"Monthly Notices of the Royal Astronomical Society","publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1502.07355"}],"extern":"1","type":"journal_article","arxiv":1,"article_processing_charge":"No","page":"400-417","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","scopus_import":"1","quality_controlled":"1","doi":"10.1093/mnras/stv947","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"status":"public","abstract":[{"text":"Using wide-field narrow-band surveys, we provide a new measurement of the z = 6.6 Lymanα emitter (LAE) luminosity function (LF), which constraints the bright end for the first time. We use a combination of archival narrow-band NB921 data in UDS and new NB921 measurements in SA22 and COSMOS/UltraVISTA, all observed with the Subaru telescope, with a total area of ∼5 deg2. We exclude lower redshift interlopers by using broad-band optical and near-infrared photometry and also exclude three supernovae with data split over multiple epochs. Combining the UDS and COSMOS samples, we find no evolution of the bright end of the Lyα LF between z = 5.7 and 6.6, which is supported by spectroscopic follow-up, and conclude that sources with Himiko-like luminosity are not as rare as previously thought, with number densities of ∼1.5 × 10−5 Mpc−3. Combined with our wide-field SA22 measurements, our results indicate a non-Schechter-like bright end of the LF at z = 6.6 and a different evolution of observed faint and bright LAEs, overcoming cosmic variance. This differential evolution is also seen in the spectroscopic follow-up of UV-selected galaxies and is now also confirmed for LAEs, and we argue that it may be an effect of reionization. Using a toy model, we show that such differential evolution of the LF is expected, since brighter sources are able to ionize their surroundings earlier, such that Lyα photons are able to escape. Our targets are excellent candidates for detailed follow-up studies and provide the possibility to give a unique view on the earliest stages in the formation of galaxies and reionization process.","lang":"eng"}],"month":"07","volume":451,"article_type":"original","year":"2015","date_published":"2015-07-21T00:00:00Z","date_created":"2022-07-14T11:57:03Z","language":[{"iso":"eng"}],"acknowledgement":"We thank the anonymous referee for the comments and suggestions which have improved the quality of this work. We thank Masami Ouchi for his useful comments on an earlier version of this paper. JM acknowledges the support of a Huygens PhD fellowship from Leiden University and is thankful for the hospitality of the Center for Astronomy and Astrophysics of the University of Lisbon where part of this research has been done. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship, from FCT through a FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010) and from FCT grant PEstOE/FIS/UI2751/2014. HR acknowledges support from the ERC Advanced Investigator programme NewClusters 321271. We acknowledge the award of ESO DDT time (294.A-5018) for providing the possibility of a timely publication of this work.\r\nBased on observations with the Subaru Telescope (Programme IDs: our observations: S14A-086; archival: S05B-027, S06A-025, S06B-010, S07A-013, S07B-008, S08B-008 and S09A-017) and the W.M. Keck Observatory. The Subaru telescope is operated by the National Astronomical Observatory of Japan. The W.M. Keck Observatory is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 294.A-5018. Based on observations obtained with MegaPrime/Megacam, a joint project of CFHT and CEA/IRFU, at the Canada–France-Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at Terapix available at the Canadian Astronomy Data Centre as part of the CFHT Legacy Survey, a collaborative project of NRC and CNRS. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.\r\nIn addition to the CFHT-LS and COSMOS-UltraVISTA surveys, we are grateful for the excellent data sets from the UKIRT-DXS, SXDF and S-COSMOS survey teams, without these legacy surveys, this research would have been impossible. We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP and SCAMP and the indispensable TOPCAT analysis tool (Taylor 2013)","issue":"1","oa":1,"intvolume":" 451","external_id":{"arxiv":["1502.07355"]},"publication_status":"published","author":[{"orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee"},{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"last_name":"Santos","first_name":"Sérgio","full_name":"Santos, Sérgio"},{"full_name":"Röttgering, Huub","first_name":"Huub","last_name":"Röttgering"},{"first_name":"Behnam","last_name":"Darvish","full_name":"Darvish, Behnam"},{"full_name":"Mobasher, Bahram","last_name":"Mobasher","first_name":"Bahram"}]},{"title":"A reduced orbital period for the supermassive black hole binary candidate in the quasar PG 1302-102?","_id":"17615","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"ieee":"D. J. D’Orazio, Z. Haiman, P. Duffell, B. D. Farris, and A. I. MacFadyen, “A reduced orbital period for the supermassive black hole binary candidate in the quasar PG 1302-102?,” Monthly Notices of the Royal Astronomical Society, vol. 452, no. 3. Oxford University Press, pp. 2540–2545, 2015.","apa":"D’Orazio, D. J., Haiman, Z., Duffell, P., Farris, B. D., & MacFadyen, A. I. (2015). A reduced orbital period for the supermassive black hole binary candidate in the quasar PG 1302-102? Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stv1457","mla":"D’Orazio, D. J., et al. “A Reduced Orbital Period for the Supermassive Black Hole Binary Candidate in the Quasar PG 1302-102?” Monthly Notices of the Royal Astronomical Society, vol. 452, no. 3, Oxford University Press, 2015, pp. 2540–45, doi:10.1093/mnras/stv1457.","ama":"D’Orazio DJ, Haiman Z, Duffell P, Farris BD, MacFadyen AI. A reduced orbital period for the supermassive black hole binary candidate in the quasar PG 1302-102? Monthly Notices of the Royal Astronomical Society. 2015;452(3):2540-2545. doi:10.1093/mnras/stv1457","chicago":"D’Orazio, D. J., Zoltán Haiman, P. Duffell, B. D. Farris, and A. I. MacFadyen. “A Reduced Orbital Period for the Supermassive Black Hole Binary Candidate in the Quasar PG 1302-102?” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv1457.","ista":"D’Orazio DJ, Haiman Z, Duffell P, Farris BD, MacFadyen AI. 2015. A reduced orbital period for the supermassive black hole binary candidate in the quasar PG 1302-102? Monthly Notices of the Royal Astronomical Society. 452(3), 2540–2545.","short":"D.J. D’Orazio, Z. Haiman, P. Duffell, B.D. Farris, A.I. MacFadyen, Monthly Notices of the Royal Astronomical Society 452 (2015) 2540–2545."},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stv1457"}],"publisher":"Oxford University Press","day":"24","date_updated":"2024-09-24T07:58:52Z","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","scopus_import":"1","oa_version":"Published Version","page":"2540-2545","publication_identifier":{"issn":["0035-8711","1365-2966"]},"doi":"10.1093/mnras/stv1457","quality_controlled":"1","status":"public","extern":"1","type":"journal_article","article_processing_charge":"No","date_published":"2015-07-24T00:00:00Z","year":"2015","article_type":"original","date_created":"2024-09-05T13:31:30Z","oa":1,"issue":"3","language":[{"iso":"eng"}],"intvolume":" 452","abstract":[{"text":"Graham et al. have detected a 5.2 yr periodic optical variability of the quasar PG 1302-102 at redshift z = 0.3, which they interpret as the redshifted orbital period (1 + z)tbin of a putative supermassive black hole binary (SMBHB). Here, we consider the implications of a 3–8 times shorter orbital period, suggested by hydrodynamical simulations of circumbinary discs (CBDs) with nearly equal-mass SMBHBs (q ≡ M2/M1 ≳ 0.3). With the corresponding 2–4 times tighter binary separation, PG 1302 would be undergoing gravitational wave dominated inspiral, and serve as a proof that the BHs can be fuelled and produce bright emission even in this late stage of the merger. The expected fraction of binaries with the shorter tbin, among bright quasars, would be reduced by one to two orders of magnitude, compared to the 5.2 yr period, in better agreement with the rarity of candidates reported by Graham et al. Finally, shorter periods would imply higher binary speeds, possibly imprinting periodicity on the light curves from relativistic beaming, as well as measurable relativistic effects on the Fe K α line. The CBD model predicts additional periodic variability on time-scales of tbin and ≈0.5tbin, as well as periodic variation of broad line widths and offsets relative to the narrow lines, which are consistent with the observations. Future observations will be able to test these predictions and hence the binary+CBD hypothesis for PG 1302.","lang":"eng"}],"month":"07","volume":452,"publication_status":"published","author":[{"full_name":"D'Orazio, D. J.","last_name":"D'Orazio","first_name":"D. J."},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","last_name":"Haiman","first_name":"Zoltán"},{"first_name":"P.","last_name":"Duffell","full_name":"Duffell, P."},{"full_name":"Farris, B. D.","last_name":"Farris","first_name":"B. D."},{"full_name":"MacFadyen, A. I.","first_name":"A. I.","last_name":"MacFadyen"}]},{"publication_status":"published","author":[{"full_name":"Prieto, Joaquin","first_name":"Joaquin","last_name":"Prieto"},{"full_name":"Jimenez, Raul","first_name":"Raul","last_name":"Jimenez"},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman"},{"first_name":"Roberto E.","last_name":"González","full_name":"González, Roberto E."}],"date_published":"2015-07-08T00:00:00Z","year":"2015","article_type":"original","date_created":"2024-09-06T07:18:53Z","oa":1,"issue":"1","language":[{"iso":"eng"}],"intvolume":" 452","abstract":[{"text":"In order to elucidate the origin of spin in both dark matter and baryons in galaxies, we have performed hydrodynamical simulations from cosmological initial conditions. We study atomic cooling haloes in the redshift range 100>z>9 with masses of order 109M⊙ at redshift z=10. We assume that the gas has primordial composition and that H2-cooling and prior star-formation in the haloes have been suppressed. We present a comprehensive analysis of the gas and dark matter properties of four halos with very low (λ≈0.01), low (λ≈0.04), high (λ≈0.06) and very high (λ≈0.1) spin parameter. Our main conclusion is that the spin orientation and magnitude is initially well described by tidal torque linear theory, but later on is determined by the merging and accretion history of each halo. We provide evidence that the topology of the merging region, i.e. the number of colliding filaments, gives an accurate prediction for the spin of dark matter and gas: halos at the center of knots will have low spin while those in the center of filaments will have high spin. The spin of a halo is given by λ≈0.05×(7.6/numberoffilaments)^5.1","lang":"eng"}],"month":"07","volume":452,"oa_version":"Published Version","scopus_import":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","page":"784-802","publication_identifier":{"issn":["0035-8711","1365-2966"]},"doi":"10.1093/mnras/stv1234","quality_controlled":"1","status":"public","type":"journal_article","extern":"1","article_processing_charge":"No","title":"The origin of spin in galaxies: Clues from simulations of atomic cooling haloes","_id":"17641","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"ama":"Prieto J, Jimenez R, Haiman Z, González RE. The origin of spin in galaxies: Clues from simulations of atomic cooling haloes. Monthly Notices of the Royal Astronomical Society. 2015;452(1):784-802. doi:10.1093/mnras/stv1234","apa":"Prieto, J., Jimenez, R., Haiman, Z., & González, R. E. (2015). The origin of spin in galaxies: Clues from simulations of atomic cooling haloes. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stv1234","mla":"Prieto, Joaquin, et al. “The Origin of Spin in Galaxies: Clues from Simulations of Atomic Cooling Haloes.” Monthly Notices of the Royal Astronomical Society, vol. 452, no. 1, Oxford University Press, 2015, pp. 784–802, doi:10.1093/mnras/stv1234.","ieee":"J. Prieto, R. Jimenez, Z. Haiman, and R. E. González, “The origin of spin in galaxies: Clues from simulations of atomic cooling haloes,” Monthly Notices of the Royal Astronomical Society, vol. 452, no. 1. Oxford University Press, pp. 784–802, 2015.","short":"J. Prieto, R. Jimenez, Z. Haiman, R.E. González, Monthly Notices of the Royal Astronomical Society 452 (2015) 784–802.","ista":"Prieto J, Jimenez R, Haiman Z, González RE. 2015. The origin of spin in galaxies: Clues from simulations of atomic cooling haloes. Monthly Notices of the Royal Astronomical Society. 452(1), 784–802.","chicago":"Prieto, Joaquin, Raul Jimenez, Zoltán Haiman, and Roberto E. González. “The Origin of Spin in Galaxies: Clues from Simulations of Atomic Cooling Haloes.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv1234."},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stv1234"}],"publisher":"Oxford University Press","day":"08","date_updated":"2024-09-24T11:52:00Z"}]