[{"_id":"17663","issue":"4","extern":"1","external_id":{"arxiv":["1505.06359"]},"author":[{"first_name":"Eli","last_name":"Visbal","full_name":"Visbal, Eli"},{"first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"first_name":"Greg L.","last_name":"Bryan","full_name":"Bryan, Greg L."}],"intvolume":"       453","volume":453,"date_published":"2015-09-16T00:00:00Z","page":"4457-4467","article_processing_charge":"No","publisher":"Oxford University Press","year":"2015","title":"Limits on population III star formation in minihaloes implied by Planck","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_type":"original","oa":1,"publication_identifier":{"issn":["0035-8711","1365-2966"]},"date_created":"2024-09-06T07:40:38Z","publication":"Monthly Notices of the Royal Astronomical Society","abstract":[{"text":"Recently, Planck measured a value of the cosmic microwave background (CMB) optical depth due to electron scattering of τ=0.066±0.016. Here we show that this low value leaves essentially no room for an early partial reionisation of the intergalactic medium (IGM) by high-redshift Population III (Pop III) stars, expected to have formed in low-mass minihaloes. We perform semi-analytic calculations of reionisation which include the contribution from Pop II stars in atomic cooling haloes, calibrated with high-redshift galaxy observations, and Pop III stars in minihaloes with feedback due to Lyman-Werner (LW) radiation and metal enrichment. We find that without LW feedback or prompt metal enrichment (and assuming a minihalo escape fraction of 0.5) the Pop III star formation efficiency cannot exceed ∼a few×10−4, without violating the constraints set by Planck data. This excludes massive Pop III star formation in typical 106M⊙ minihaloes. Including LW feedback and metal enrichment alleviates this tension, allowing large Pop III stars to form early on before they are quenched by feedback. We find that the total density of Pop III stars formed across cosmic time is ≲104−5 M⊙ Mpc−3 and does not depend strongly on the feedback prescription adopted. Additionally, we perform a simple estimate of the possible impact on reionisation of X-rays produced by accretion onto black hole remnants of Pop III stars. We find that unless the accretion duty cycle is very low (≲0.01), this could lead to an optical depth inconsistent with Planck.","lang":"eng"}],"date_updated":"2024-09-25T07:32:20Z","type":"journal_article","day":"16","doi":"10.1093/mnras/stv1941","publication_status":"published","month":"09","quality_controlled":"1","language":[{"iso":"eng"}],"oa_version":"Preprint","arxiv":1,"citation":{"mla":"Visbal, Eli, et al. “Limits on Population III Star Formation in Minihaloes Implied by Planck.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 453, no. 4, Oxford University Press, 2015, pp. 4457–67, doi:<a href=\"https://doi.org/10.1093/mnras/stv1941\">10.1093/mnras/stv1941</a>.","short":"E. Visbal, Z. Haiman, G.L. Bryan, Monthly Notices of the Royal Astronomical Society 453 (2015) 4457–4467.","chicago":"Visbal, Eli, Zoltán Haiman, and Greg L. Bryan. “Limits on Population III Star Formation in Minihaloes Implied by Planck.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2015. <a href=\"https://doi.org/10.1093/mnras/stv1941\">https://doi.org/10.1093/mnras/stv1941</a>.","ista":"Visbal E, Haiman Z, Bryan GL. 2015. Limits on population III star formation in minihaloes implied by Planck. Monthly Notices of the Royal Astronomical Society. 453(4), 4457–4467.","ieee":"E. Visbal, Z. Haiman, and G. L. Bryan, “Limits on population III star formation in minihaloes implied by Planck,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 453, no. 4. Oxford University Press, pp. 4457–4467, 2015.","apa":"Visbal, E., Haiman, Z., &#38; Bryan, G. L. (2015). Limits on population III star formation in minihaloes implied by Planck. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stv1941\">https://doi.org/10.1093/mnras/stv1941</a>","ama":"Visbal E, Haiman Z, Bryan GL. Limits on population III star formation in minihaloes implied by Planck. <i>Monthly Notices of the Royal Astronomical Society</i>. 2015;453(4):4457-4467. doi:<a href=\"https://doi.org/10.1093/mnras/stv1941\">10.1093/mnras/stv1941</a>"},"status":"public","main_file_link":[{"url":" https://doi.org/10.48550/arXiv.1505.06359","open_access":"1"}],"scopus_import":"1"},{"oa":1,"title":"A statistical method to search for recoiling supermassive black holes in active galactic nuclei","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_type":"original","date_updated":"2024-09-25T09:18:47Z","type":"journal_article","publication_identifier":{"issn":["0035-8711","1365-2966"]},"date_created":"2024-09-06T08:20:30Z","publication":"Monthly Notices of the Royal Astronomical Society","abstract":[{"text":"We propose an observational test for gravitationally recoiling supermassive black holes (BHs) in active galactic nuclei, based on a correlation between the velocities of BHs relative to their host galaxies, |\\Delta v|, and their obscuring dust column densities, \\Sigma_{dust} (both measured along the line of sight). We use toy models for the distribution of recoil velocities, BH trajectories, and the geometry of obscuring dust tori in galactic centres, to simulate 2.5x10^5 random observations of recoiling quasars. BHs with recoil velocities comparable to the escape velocity from the galactic centre remain bound to the nucleus, and do not fully settle back to the centre of the torus due to dynamical friction in a typical quasar lifetime. We find that |\\Delta v| and \\Sigma_ {dust} for these BHs are positively correlated. For obscured (\\Sigma_{dust}>0) and for partially obscured (0<\\Sigma_{dust}<~2.3 g/m^2) quasars with |\\Delta v|>=45 km/s, the sample correlation coefficient between log10(|\\Delta v|) and \\Sigma_{dust} is r_{45} = 0.28+/-0.02 and r_{45} = 0.13+/-0.02, respectively. Allowing for random +/-100 km/s errors in |\\Delta v| unrelated to the recoil dilutes the correlation for the partially obscured quasars to r_{45} = 0.026+/-0.004 measured between |\\Delta v| and \\Sigma_{dust}. A random sample of >~3,500 obscured quasars with |\\Delta v|>=45 km/s would allow rejection of the no-correlation hypothesis with 3 sigma significance 95% of the time. Finally, we find that the fraction of obscured quasars, F_{obs}(|\\Delta v|), decreases with |\\Delta v| from F_{obs}(<10 km/s)>~0.8 to F_{obs}(>10^3 km/s)<~0.4. This predicted trend can be compared to the observed fraction of type II quasars, and can further test combinations of recoil, trajectory, and dust torus models.","lang":"eng"}],"language":[{"iso":"eng"}],"quality_controlled":"1","oa_version":"Published Version","day":"02","doi":"10.1093/mnras/stv2371","publication_status":"published","month":"11","scopus_import":"1","citation":{"ieee":"P. Raffai, Z. Haiman, and Z. Frei, “A statistical method to search for recoiling supermassive black holes in active galactic nuclei,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 455, no. 1. Oxford University Press, pp. 484–492, 2015.","ama":"Raffai P, Haiman Z, Frei Z. A statistical method to search for recoiling supermassive black holes in active galactic nuclei. <i>Monthly Notices of the Royal Astronomical Society</i>. 2015;455(1):484-492. doi:<a href=\"https://doi.org/10.1093/mnras/stv2371\">10.1093/mnras/stv2371</a>","apa":"Raffai, P., Haiman, Z., &#38; Frei, Z. (2015). A statistical method to search for recoiling supermassive black holes in active galactic nuclei. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stv2371\">https://doi.org/10.1093/mnras/stv2371</a>","mla":"Raffai, P., et al. “A Statistical Method to Search for Recoiling Supermassive Black Holes in Active Galactic Nuclei.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 455, no. 1, Oxford University Press, 2015, pp. 484–92, doi:<a href=\"https://doi.org/10.1093/mnras/stv2371\">10.1093/mnras/stv2371</a>.","chicago":"Raffai, P., Zoltán Haiman, and Z. Frei. “A Statistical Method to Search for Recoiling Supermassive Black Holes in Active Galactic Nuclei.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2015. <a href=\"https://doi.org/10.1093/mnras/stv2371\">https://doi.org/10.1093/mnras/stv2371</a>.","short":"P. Raffai, Z. Haiman, Z. Frei, Monthly Notices of the Royal Astronomical Society 455 (2015) 484–492.","ista":"Raffai P, Haiman Z, Frei Z. 2015. A statistical method to search for recoiling supermassive black holes in active galactic nuclei. Monthly Notices of the Royal Astronomical Society. 455(1), 484–492."},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stv2371"}],"status":"public","author":[{"last_name":"Raffai","full_name":"Raffai, P.","first_name":"P."},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán"},{"first_name":"Z.","full_name":"Frei, Z.","last_name":"Frei"}],"_id":"17685","extern":"1","issue":"1","volume":455,"intvolume":"       455","page":"484-492","article_processing_charge":"No","date_published":"2015-11-02T00:00:00Z","year":"2015","publisher":"Oxford University Press"},{"article_processing_charge":"No","page":"2506-2513","date_published":"2015-05-06T00:00:00Z","year":"2015","publisher":"Oxford University Press","author":[{"first_name":"Eli","last_name":"Visbal","full_name":"Visbal, Eli"},{"first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","last_name":"Haiman"},{"full_name":"Bryan, Greg L.","last_name":"Bryan","first_name":"Greg L."}],"issue":"3","_id":"17694","extern":"1","volume":450,"intvolume":"       450","language":[{"iso":"eng"}],"quality_controlled":"1","oa_version":"Published Version","month":"05","day":"06","doi":"10.1093/mnras/stv785","publication_status":"published","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stv785"}],"status":"public","citation":{"ama":"Visbal E, Haiman Z, Bryan GL. Looking for Population III stars with He ii line intensity mapping. <i>Monthly Notices of the Royal Astronomical Society</i>. 2015;450(3):2506-2513. doi:<a href=\"https://doi.org/10.1093/mnras/stv785\">10.1093/mnras/stv785</a>","apa":"Visbal, E., Haiman, Z., &#38; Bryan, G. L. (2015). Looking for Population III stars with He ii line intensity mapping. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stv785\">https://doi.org/10.1093/mnras/stv785</a>","ieee":"E. Visbal, Z. Haiman, and G. L. Bryan, “Looking for Population III stars with He ii line intensity mapping,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 450, no. 3. Oxford University Press, pp. 2506–2513, 2015.","ista":"Visbal E, Haiman Z, Bryan GL. 2015. Looking for Population III stars with He ii line intensity mapping. Monthly Notices of the Royal Astronomical Society. 450(3), 2506–2513.","short":"E. Visbal, Z. Haiman, G.L. Bryan, Monthly Notices of the Royal Astronomical Society 450 (2015) 2506–2513.","chicago":"Visbal, Eli, Zoltán Haiman, and Greg L. Bryan. “Looking for Population III Stars with He Ii Line Intensity Mapping.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2015. <a href=\"https://doi.org/10.1093/mnras/stv785\">https://doi.org/10.1093/mnras/stv785</a>.","mla":"Visbal, Eli, et al. “Looking for Population III Stars with He Ii Line Intensity Mapping.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 450, no. 3, Oxford University Press, 2015, pp. 2506–13, doi:<a href=\"https://doi.org/10.1093/mnras/stv785\">10.1093/mnras/stv785</a>."},"oa":1,"article_type":"original","title":"Looking for Population III stars with He ii line intensity mapping","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_updated":"2024-09-25T10:05:24Z","type":"journal_article","abstract":[{"text":"Constraining the properties of Population III (Pop III) stars will be very challenging because they reside in small galaxies at high redshift which will be difficult to directly detect. In this paper, we suggest that intensity mapping may be a promising method to study Pop III stars. Intensity mapping is a technique proposed to measure large-scale fluctuations of galaxy line emission in three dimensions without resolving individual sources. This technique is well suited for observing many faint galaxies because it can measure their cumulative emission even if they cannot be directly detected. We focus on intensity mapping of He ii recombination lines. These lines are much stronger in Pop III stars than Pop II stars because the harder spectra of Pop III stars are expected to produce many He ii ionizing photons. Measuring the He ii 1640 Å intensity mapping signal, along with the signals from other lines such as Lyα, Hα, and metal lines, could give constraints on the initial mass function (IMF) and star formation rate density of Pop III stars as a function of redshift. To demonstrate the feasibility of these observations, we estimate the strength of the Pop III He ii 1640 Å intensity mapping signal from z = 10–20. We show that at z ≈ 10, the signal could be measured accurately by two different hypothetical future instruments, one which cross-correlates He ii 1640 Å with CO(1–0) line emission from galaxies and the other with 21 cm emission from the intergalactic medium.","lang":"eng"}],"publication_identifier":{"issn":["0035-8711","1365-2966"]},"date_created":"2024-09-06T08:40:33Z","publication":"Monthly Notices of the Royal Astronomical Society"},{"_id":"11582","extern":"1","issue":"3","external_id":{"arxiv":["1407.1047"]},"author":[{"first_name":"John P.","full_name":"Stott, John P.","last_name":"Stott"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"last_name":"Swinbank","full_name":"Swinbank, A. M.","first_name":"A. M."},{"full_name":"Smail, Ian","last_name":"Smail","first_name":"Ian"},{"full_name":"Bower, Richard","last_name":"Bower","first_name":"Richard"},{"first_name":"Philip N.","last_name":"Best","full_name":"Best, Philip N."},{"first_name":"Ray M.","last_name":"Sharples","full_name":"Sharples, Ray M."},{"first_name":"James E.","last_name":"Geach","full_name":"Geach, James E."},{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"}],"intvolume":"       443","volume":443,"date_published":"2014-09-21T00:00:00Z","article_processing_charge":"No","page":"2695-2704","publisher":"Oxford University Press","year":"2014","article_type":"original","title":"A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: abundances","galaxies: evolution","galaxies: kinematics and dynamics"],"oa":1,"abstract":[{"text":"We have observed a sample of typical z ∼ 1 star-forming galaxies, selected from the HiZELS survey, with the new K-band Multi-Object Spectrograph (KMOS) near-infrared, multi-integral field unit instrument on the Very Large Telescope (VLT), in order to obtain their dynamics and metallicity gradients. The majority of our galaxies have a metallicity gradient consistent with being flat or negative (i.e. higher metallicity cores than outskirts). Intriguingly, we find a trend between metallicity gradient and specific star formation rate (sSFR), such that galaxies with a high sSFR tend to have relatively metal poor centres, a result which is strengthened when combined with data sets from the literature. This result appears to explain the discrepancies reported between different high-redshift studies and varying claims for evolution. From a galaxy evolution perspective, the trend we see would mean that a galaxy's sSFR is governed by the amount of metal-poor gas that can be funnelled into its core, triggered either by merging or through efficient accretion. In fact, merging may play a significant role as it is the starburst galaxies at all epochs, which have the more positive metallicity gradients. Our results may help to explain the origin of the fundamental metallicity relation, in which galaxies at a fixed mass are observed to have lower metallicities at higher star formation rates, especially if the metallicity is measured in an aperture encompassing only the central regions of the galaxy. Finally, we note that this study demonstrates the power of KMOS as an efficient instrument for large-scale resolved galaxy surveys.","lang":"eng"}],"date_created":"2022-07-14T12:16:10Z","publication":"Monthly Notices of the Royal Astronomical Society","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"type":"journal_article","date_updated":"2022-08-19T08:27:25Z","month":"09","publication_status":"published","day":"21","doi":"10.1093/mnras/stu1343","arxiv":1,"language":[{"iso":"eng"}],"oa_version":"Preprint","quality_controlled":"1","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1407.1047"}],"citation":{"apa":"Stott, J. P., Sobral, D., Swinbank, A. M., Smail, I., Bower, R., Best, P. N., … Matthee, J. J. (2014). A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stu1343\">https://doi.org/10.1093/mnras/stu1343</a>","ama":"Stott JP, Sobral D, Swinbank AM, et al. A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS. <i>Monthly Notices of the Royal Astronomical Society</i>. 2014;443(3):2695-2704. doi:<a href=\"https://doi.org/10.1093/mnras/stu1343\">10.1093/mnras/stu1343</a>","ieee":"J. P. Stott <i>et al.</i>, “A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 443, no. 3. Oxford University Press, pp. 2695–2704, 2014.","ista":"Stott JP, Sobral D, Swinbank AM, Smail I, Bower R, Best PN, Sharples RM, Geach JE, Matthee JJ. 2014. A relationship between specific star formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS. Monthly Notices of the Royal Astronomical Society. 443(3), 2695–2704.","short":"J.P. Stott, D. Sobral, A.M. Swinbank, I. Smail, R. Bower, P.N. Best, R.M. Sharples, J.E. Geach, J.J. Matthee, Monthly Notices of the Royal Astronomical Society 443 (2014) 2695–2704.","mla":"Stott, John P., et al. “A Relationship between Specific Star Formation Rate and Metallicity Gradient within z ∼ 1 Galaxies from KMOS-HiZELS.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 443, no. 3, Oxford University Press, 2014, pp. 2695–704, doi:<a href=\"https://doi.org/10.1093/mnras/stu1343\">10.1093/mnras/stu1343</a>.","chicago":"Stott, John P., David Sobral, A. M. Swinbank, Ian Smail, Richard Bower, Philip N. Best, Ray M. Sharples, James E. Geach, and Jorryt J Matthee. “A Relationship between Specific Star Formation Rate and Metallicity Gradient within z ∼ 1 Galaxies from KMOS-HiZELS.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnras/stu1343\">https://doi.org/10.1093/mnras/stu1343</a>."},"scopus_import":"1","acknowledgement":"First, we acknowledge the referee for their comments, which have improved the clarity of this paper. JPS and IRS acknowledge support from STFC (ST/I001573/1). IRS also acknowledges support from the ERC Advanced Investigator programme DUSTYGAL and a Royal Society/Wolfson Merit Award. DS acknowledges financial support from NWO through a Veni fellowship and from FCT through the award of an FCT-IF starting grant. PNB acknowledges STFC for financial support."},{"day":"21","doi":"10.1093/mnras/stu392","publication_status":"published","month":"05","oa_version":"Preprint","language":[{"iso":"eng"}],"quality_controlled":"1","arxiv":1,"citation":{"ista":"Matthee JJ, Sobral D, Swinbank AM, Smail I, Best PN, Kim J-W, Franx M, Milvang-Jensen B, Fynbo J. 2014. A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys. Monthly Notices of the Royal Astronomical Society. 440(3), 2375–2387.","mla":"Matthee, Jorryt J., et al. “A 10 Deg2 Lyman α Survey at Z=8.8 with Spectroscopic Follow-up: Strong Constraints on the Luminosity Function and Implications for Other Surveys.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 440, no. 3, Oxford University Press, 2014, pp. 2375–87, doi:<a href=\"https://doi.org/10.1093/mnras/stu392\">10.1093/mnras/stu392</a>.","chicago":"Matthee, Jorryt J, David Sobral, A. M. Swinbank, Ian Smail, P. N. Best, Jae-Woo Kim, Marijn Franx, Bo Milvang-Jensen, and Johan Fynbo. “A 10 Deg2 Lyman α Survey at Z=8.8 with Spectroscopic Follow-up: Strong Constraints on the Luminosity Function and Implications for Other Surveys.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnras/stu392\">https://doi.org/10.1093/mnras/stu392</a>.","short":"J.J. Matthee, D. Sobral, A.M. Swinbank, I. Smail, P.N. Best, J.-W. Kim, M. Franx, B. Milvang-Jensen, J. Fynbo, Monthly Notices of the Royal Astronomical Society 440 (2014) 2375–2387.","ama":"Matthee JJ, Sobral D, Swinbank AM, et al. A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys. <i>Monthly Notices of the Royal Astronomical Society</i>. 2014;440(3):2375-2387. doi:<a href=\"https://doi.org/10.1093/mnras/stu392\">10.1093/mnras/stu392</a>","apa":"Matthee, J. J., Sobral, D., Swinbank, A. M., Smail, I., Best, P. N., Kim, J.-W., … Fynbo, J. (2014). A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stu392\">https://doi.org/10.1093/mnras/stu392</a>","ieee":"J. J. Matthee <i>et al.</i>, “A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 440, no. 3. Oxford University Press, pp. 2375–2387, 2014."},"status":"public","main_file_link":[{"url":"https://arxiv.org/abs/1402.6697","open_access":"1"}],"scopus_import":"1","acknowledgement":"We thank the anonymous referee for the comments and suggestions which improved both the quality and clarity of this work. DS acknowledges financial support from the Netherlands Organisation for Scientific Research (NWO) through a Veni fellowship. IRS acknowledges support from STFC (ST/I001573/1), a Leverhulme Fellowship, the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson Merit Award. PNB acknowledges support from the Leverhulme Trust. JWK acknowledges the support from the Creative Research Initiative Program, no. 2008- 0060544, of the National Research Foundation of Korea (NRF) funded by the Korean government (MSIP). JPUF and BMJ acknowledge support from the ERC-StG grant EGGS-278202. The Dark Cosmology Centre is funded by the Danish National Research Foundation. This work is based in part on data obtained as part of the UKIRT Infrared Deep Sky Survey. 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. This work was only possible due to OPTICON/FP7 and the access that it granted to the CFHT telescope. The authors also wish to acknowledge the CFHTLS and UKIDSS surveys for their excellent legacy and complementary value – without such high-quality data sets, this research would not have been possible.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","title":"A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints on the luminosity function and implications for other surveys","article_type":"original","oa":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations","dark ages","reionization","first stars"],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2022-07-14T12:33:24Z","abstract":[{"text":"Candidate galaxies at redshifts of z ∼ 10 are now being found in extremely deep surveys, probing very small areas. As a consequence, candidates are very faint, making spectroscopic confirmation practically impossible. In order to overcome such limitations, we have undertaken the CF-HiZELS survey, which is a large-area, medium-depth near-infrared narrow-band survey targeted at z = 8.8 Lyman α (Lyα) emitters (LAEs) and covering 10 deg2 in part of the SSA22 field with the Canada–France–Hawaii Telescope (CFHT). We surveyed a comoving volume of 4.7 × 106 Mpc3 to a Lyα luminosity limit of 6.3 × 1043舁erg舁s−1. We look for Lyα candidates by applying the following criteria: (i) clear emission-line source, (ii) no optical detections (ugriz from CFHTLS), (iii) no visible detection in the optical stack (ugriz > 27), (iv) visually checked reliable NBJ and J detections and (v) J − K ≤ 0. We compute photometric redshifts and remove a significant amount of dusty lower redshift line-emitters at z ∼ 1.4 or 2.2. A total of 13 Lyα candidates were found, of which two are marked as strong candidates, but the majority have very weak constraints on their spectral energy distributions. Using follow-up observations with SINFONI/VLT, we are able to exclude the most robust candidates as LAEs. We put a strong constraint on the Lyα luminosity function at z ∼ 9 and make realistic predictions for ongoing and future surveys. Our results show that surveys for the highest redshift LAEs are susceptible of multiple contaminations and that spectroscopic follow-up is absolutely necessary.","lang":"eng"}],"date_updated":"2024-10-14T11:37:28Z","type":"journal_article","date_published":"2014-05-21T00:00:00Z","page":"2375-2387","article_processing_charge":"No","publisher":"Oxford University Press","year":"2014","_id":"11583","external_id":{"arxiv":["1402.6697"]},"extern":"1","issue":"3","author":[{"first_name":"Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"last_name":"Swinbank","full_name":"Swinbank, A. M.","first_name":"A. M."},{"first_name":"Ian","last_name":"Smail","full_name":"Smail, Ian"},{"first_name":"P. N.","full_name":"Best, P. N.","last_name":"Best"},{"first_name":"Jae-Woo","full_name":"Kim, Jae-Woo","last_name":"Kim"},{"full_name":"Franx, Marijn","last_name":"Franx","first_name":"Marijn"},{"first_name":"Bo","full_name":"Milvang-Jensen, Bo","last_name":"Milvang-Jensen"},{"last_name":"Fynbo","full_name":"Fynbo, Johan","first_name":"Johan"}],"intvolume":"       440","volume":440},{"date_published":"2014-09-22T00:00:00Z","article_processing_charge":"No","page":"107-114","publisher":"Oxford University Press","year":"2014","extern":"1","_id":"17614","issue":"1","author":[{"first_name":"Eli","last_name":"Visbal","full_name":"Visbal, Eli"},{"first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"first_name":"Bryan","full_name":"Terrazas, Bryan","last_name":"Terrazas"},{"last_name":"Bryan","full_name":"Bryan, Greg L.","first_name":"Greg L."},{"first_name":"Rennan","last_name":"Barkana","full_name":"Barkana, Rennan"}],"intvolume":"       445","volume":445,"month":"09","publication_status":"published","doi":"10.1093/mnras/stu1710","day":"22","oa_version":"Published Version","quality_controlled":"1","language":[{"iso":"eng"}],"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stu1710"}],"status":"public","citation":{"mla":"Visbal, Eli, et al. “High-Redshift Star Formation in a Time-Dependent Lyman–Werner Background.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 445, no. 1, Oxford University Press, 2014, pp. 107–14, doi:<a href=\"https://doi.org/10.1093/mnras/stu1710\">10.1093/mnras/stu1710</a>.","chicago":"Visbal, Eli, Zoltán Haiman, Bryan Terrazas, Greg L. Bryan, and Rennan Barkana. “High-Redshift Star Formation in a Time-Dependent Lyman–Werner Background.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnras/stu1710\">https://doi.org/10.1093/mnras/stu1710</a>.","short":"E. Visbal, Z. Haiman, B. Terrazas, G.L. Bryan, R. Barkana, Monthly Notices of the Royal Astronomical Society 445 (2014) 107–114.","ista":"Visbal E, Haiman Z, Terrazas B, Bryan GL, Barkana R. 2014. High-redshift star formation in a time-dependent Lyman–Werner background. Monthly Notices of the Royal Astronomical Society. 445(1), 107–114.","ieee":"E. Visbal, Z. Haiman, B. Terrazas, G. L. Bryan, and R. Barkana, “High-redshift star formation in a time-dependent Lyman–Werner background,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 445, no. 1. Oxford University Press, pp. 107–114, 2014.","ama":"Visbal E, Haiman Z, Terrazas B, Bryan GL, Barkana R. High-redshift star formation in a time-dependent Lyman–Werner background. <i>Monthly Notices of the Royal Astronomical Society</i>. 2014;445(1):107-114. doi:<a href=\"https://doi.org/10.1093/mnras/stu1710\">10.1093/mnras/stu1710</a>","apa":"Visbal, E., Haiman, Z., Terrazas, B., Bryan, G. L., &#38; Barkana, R. (2014). High-redshift star formation in a time-dependent Lyman–Werner background. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stu1710\">https://doi.org/10.1093/mnras/stu1710</a>"},"scopus_import":"1","article_type":"original","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","title":"High-redshift star formation in a time-dependent Lyman–Werner background","oa":1,"abstract":[{"lang":"eng","text":"The first generation of stars produces a background of Lyman–Werner (LW) radiation which can photodissociate molecular hydrogen, increasing the mass of dark matter haloes required to host star formation. Previous studies have determined the critical mass required for efficient molecular cooling with a constant LW background. However, the true background is expected to increase rapidly at early times. Neglecting this evolution could underestimate star formation in small haloes that may have started to cool in the past when the LW intensity was much lower. Background evolution is a large source of uncertainty in pre-reionization predictions of the cosmological 21cm signal, which can be observed with future radio telescopes. To address this, we perform zero-dimensional one-zone calculations that follow the density, chemical abundances, and temperature of gas in the central regions of dark matter haloes, including hierarchical growth and an evolving LW background. We begin by studying the physics of haloes subjected to a background that increases exponentially with redshift. We find that when the intensity increases more slowly than JLW(z)∝10−z/5, cooling in the past is a relatively small effect. We then self-consistently compute the cosmological LW background over z = 15–50 and find that cooling in the past due to an evolving background has a modest impact. Finally, we compare these results to three-dimensional hydrodynamical cosmological simulations with varying LW histories. While only a small number of haloes were simulated, the results are consistent with our one-zone calculations."}],"date_created":"2024-09-05T13:30:21Z","publication":"Monthly Notices of the Royal Astronomical Society","publication_identifier":{"issn":["0035-8711","1365-2966"]},"type":"journal_article","date_updated":"2024-09-24T07:43:44Z"},{"page":"1549-1557","article_processing_charge":"No","date_published":"2014-10-09T00:00:00Z","year":"2014","publisher":"Oxford University Press","author":[{"last_name":"Inayoshi","full_name":"Inayoshi, Kohei","first_name":"Kohei"},{"first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"}],"_id":"17637","issue":"2","extern":"1","volume":445,"intvolume":"       445","quality_controlled":"1","oa_version":"Published Version","language":[{"iso":"eng"}],"doi":"10.1093/mnras/stu1870","day":"09","publication_status":"published","month":"10","scopus_import":"1","citation":{"ama":"Inayoshi K, Haiman Z. Does disc fragmentation prevent the formation of supermassive stars in protogalaxies? <i>Monthly Notices of the Royal Astronomical Society</i>. 2014;445(2):1549-1557. doi:<a href=\"https://doi.org/10.1093/mnras/stu1870\">10.1093/mnras/stu1870</a>","apa":"Inayoshi, K., &#38; Haiman, Z. (2014). Does disc fragmentation prevent the formation of supermassive stars in protogalaxies? <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stu1870\">https://doi.org/10.1093/mnras/stu1870</a>","ieee":"K. Inayoshi and Z. Haiman, “Does disc fragmentation prevent the formation of supermassive stars in protogalaxies?,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 445, no. 2. Oxford University Press, pp. 1549–1557, 2014.","ista":"Inayoshi K, Haiman Z. 2014. Does disc fragmentation prevent the formation of supermassive stars in protogalaxies? Monthly Notices of the Royal Astronomical Society. 445(2), 1549–1557.","chicago":"Inayoshi, Kohei, and Zoltán Haiman. “Does Disc Fragmentation Prevent the Formation of Supermassive Stars in Protogalaxies?” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnras/stu1870\">https://doi.org/10.1093/mnras/stu1870</a>.","short":"K. Inayoshi, Z. Haiman, Monthly Notices of the Royal Astronomical Society 445 (2014) 1549–1557.","mla":"Inayoshi, Kohei, and Zoltán Haiman. “Does Disc Fragmentation Prevent the Formation of Supermassive Stars in Protogalaxies?” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 445, no. 2, Oxford University Press, 2014, pp. 1549–57, doi:<a href=\"https://doi.org/10.1093/mnras/stu1870\">10.1093/mnras/stu1870</a>."},"status":"public","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stu1870"}],"oa":1,"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","title":"Does disc fragmentation prevent the formation of supermassive stars in protogalaxies?","article_type":"original","date_updated":"2024-09-24T11:33:30Z","type":"journal_article","publication_identifier":{"issn":["1365-2966","0035-8711"]},"publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2024-09-06T07:15:08Z","abstract":[{"lang":"eng","text":"Supermassive stars (SMSs; >10^5 Msun) formed in the first protogalaxies with virial temperature T_vir>10^4 K are expected to collapse into seeds of supermassive black hole (SMBHs) in the high-redshift universe (z>7). Fragmentation of the primordial gas is, however, a possible obstacle to SMS formation. We discuss the expected properties of a compact, metal-free, marginally unstable nuclear protogalactic disk, and the fate of the clumps formed in the disk by gravitational instability. Interior to a characteristic radius R_f=few*10^{-2} pc, the disk fragments into massive clumps with M_c~30 Msun. The clumps grow via accretion and migrate inward rapidly on a timescale of ~10^4 yr, which is comparable or shorter than the Kelvin-Helmholz time >10^4 yr. Some clumps may evolve to zero-age main sequence stars and halt gas accretion by radiative feedback, but most of the clumps can migrate inward and merge with the central protostar before forming massive stars. Moreover, we found that dust-induced-fragmentation in metal-enriched gas does not modify these conclusions unless Z> 3*10^{-4} Zsun, because clump migration below this metallicity remains as rapid as in the primordial case. Our results suggest that fragmentation of a compact, metal--poor disk can not prevent the formation of a SMS."}]},{"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","title":"H2 suppression with shocking inflows: Testing a pathway for supermassive black hole formation","article_type":"original","oa":1,"date_created":"2024-09-06T07:21:52Z","publication":"Monthly Notices of the Royal Astronomical Society","publication_identifier":{"issn":["1365-2966","0035-8711"]},"abstract":[{"text":"The presence of quasars at redshifts z > 6 indicates the existence of supermassive black holes (SMBHs) as massive as a few times 10^9 Msun, challenging models for SMBH formation. One pathway is through the direct collapse of gas in T_{vir} > 10^4 K halos; however, this requires the suppression of H_2 cooling to prevent fragmentation. In this paper, we examine a proposed new mechanism for this suppression which relies on cold-mode accretion flows leading to shocks at high densities (n > 10^4 cm^{-3}) and temperatures (T > 10^4 K). In such gas, H_2 is efficiently collisionally dissociated. We use high-resolution numerical simulations to test this idea, demonstrating that such halos typically have lower temperature progenitors, in which cooling is efficient. Those halos do show filamentary flows; however, the gas shocks at or near the virial radius (at low densities), thus preventing the proposed collisional mechanism from operating. We do find that, if we artificially suppress H_2 formation with a high UV background, so as to allow gas in the halo center to enter the high-temperature, high-density \"zone of no return\", it will remain there even if the UV flux is turned off, collapsing to high density at high temperature. Due to computational limitations, we simulated only three halos. However, we demonstrate, using Monte Carlo calculations of 10^6 halo merger histories, that a few rare halos could assemble rapidly enough to avoid efficient H_2 cooling in all of their progenitor halos, provided that the UV background exceeds J_{21} ~ few at redshifts as high as z ~ 20","lang":"eng"}],"type":"journal_article","date_updated":"2024-09-24T11:56:43Z","publication_status":"published","doi":"10.1093/mnras/stu230","day":"26","month":"02","oa_version":"Published Version","language":[{"iso":"eng"}],"quality_controlled":"1","citation":{"ista":"Fernandez R, Bryan GL, Haiman Z, Li M. 2014. H2 suppression with shocking inflows: Testing a pathway for supermassive black hole formation. Monthly Notices of the Royal Astronomical Society. 439(4), 3798–3807.","chicago":"Fernandez, Ricardo, Greg L. Bryan, Zoltán Haiman, and Miao Li. “H2 Suppression with Shocking Inflows: Testing a Pathway for Supermassive Black Hole Formation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnras/stu230\">https://doi.org/10.1093/mnras/stu230</a>.","mla":"Fernandez, Ricardo, et al. “H2 Suppression with Shocking Inflows: Testing a Pathway for Supermassive Black Hole Formation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 439, no. 4, Oxford University Press, 2014, pp. 3798–807, doi:<a href=\"https://doi.org/10.1093/mnras/stu230\">10.1093/mnras/stu230</a>.","short":"R. Fernandez, G.L. Bryan, Z. Haiman, M. Li, Monthly Notices of the Royal Astronomical Society 439 (2014) 3798–3807.","apa":"Fernandez, R., Bryan, G. L., Haiman, Z., &#38; Li, M. (2014). H2 suppression with shocking inflows: Testing a pathway for supermassive black hole formation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stu230\">https://doi.org/10.1093/mnras/stu230</a>","ama":"Fernandez R, Bryan GL, Haiman Z, Li M. H2 suppression with shocking inflows: Testing a pathway for supermassive black hole formation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2014;439(4):3798-3807. doi:<a href=\"https://doi.org/10.1093/mnras/stu230\">10.1093/mnras/stu230</a>","ieee":"R. Fernandez, G. L. Bryan, Z. Haiman, and M. Li, “H2 suppression with shocking inflows: Testing a pathway for supermassive black hole formation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 439, no. 4. Oxford University Press, pp. 3798–3807, 2014."},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stu230"}],"status":"public","scopus_import":"1","extern":"1","_id":"17642","issue":"4","author":[{"first_name":"Ricardo","full_name":"Fernandez, Ricardo","last_name":"Fernandez"},{"first_name":"Greg L.","full_name":"Bryan, Greg L.","last_name":"Bryan"},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán"},{"first_name":"Miao","full_name":"Li, Miao","last_name":"Li"}],"intvolume":"       439","volume":439,"date_published":"2014-02-26T00:00:00Z","page":"3798-3807","article_processing_charge":"No","publisher":"Oxford University Press","year":"2014"},{"citation":{"ieee":"M. Dijkstra, S. Wyithe, Z. Haiman, A. Mesinger, and L. Pentericci, “Evolution in the escape fraction of ionizing photons and the decline in strong Lyα emission from z &#62; 6 galaxies,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 440, no. 4. Oxford University Press, pp. 3309–3316, 2014.","apa":"Dijkstra, M., Wyithe, S., Haiman, Z., Mesinger, A., &#38; Pentericci, L. (2014). Evolution in the escape fraction of ionizing photons and the decline in strong Lyα emission from z &#62; 6 galaxies. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stu531\">https://doi.org/10.1093/mnras/stu531</a>","ama":"Dijkstra M, Wyithe S, Haiman Z, Mesinger A, Pentericci L. Evolution in the escape fraction of ionizing photons and the decline in strong Lyα emission from z &#62; 6 galaxies. <i>Monthly Notices of the Royal Astronomical Society</i>. 2014;440(4):3309-3316. doi:<a href=\"https://doi.org/10.1093/mnras/stu531\">10.1093/mnras/stu531</a>","mla":"Dijkstra, Mark, et al. “Evolution in the Escape Fraction of Ionizing Photons and the Decline in Strong Lyα Emission from z &#62; 6 Galaxies.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 440, no. 4, Oxford University Press, 2014, pp. 3309–16, doi:<a href=\"https://doi.org/10.1093/mnras/stu531\">10.1093/mnras/stu531</a>.","chicago":"Dijkstra, Mark, Stuart Wyithe, Zoltán Haiman, Andrei Mesinger, and Laura Pentericci. “Evolution in the Escape Fraction of Ionizing Photons and the Decline in Strong Lyα Emission from z &#62; 6 Galaxies.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnras/stu531\">https://doi.org/10.1093/mnras/stu531</a>.","short":"M. Dijkstra, S. Wyithe, Z. Haiman, A. Mesinger, L. Pentericci, Monthly Notices of the Royal Astronomical Society 440 (2014) 3309–3316.","ista":"Dijkstra M, Wyithe S, Haiman Z, Mesinger A, Pentericci L. 2014. Evolution in the escape fraction of ionizing photons and the decline in strong Lyα emission from z &#62; 6 galaxies. Monthly Notices of the Royal Astronomical Society. 440(4), 3309–3316."},"status":"public","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stu531"}],"scopus_import":"1","doi":"10.1093/mnras/stu531","day":"17","publication_status":"published","month":"04","language":[{"iso":"eng"}],"quality_controlled":"1","oa_version":"Published Version","publication_identifier":{"issn":["1365-2966","0035-8711"]},"publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2024-09-06T07:24:26Z","abstract":[{"lang":"eng","text":"The rapid decline in the number of strong Lyman Alpha (Lya) emitting galaxies at z > 6 provides evidence for neutral hydrogen in the IGM, but is difficult to explain with plausible models for reionization. We demonstrate that the observed reduction in Lya flux from galaxies at z > 6 can be explained by evolution in the escape fraction of ionizing photons, f_esc. We find that the median observed drop in the fraction of galaxies showing strong Lya emission, as well as the observed evolution of the Lya luminosity function both follow from a small increase in f_esc of Delta f_esc ~ 0.1 from f_esc ~ 0.6 at z ~ 6. This high escape fraction may be at odds with current constraints on the ionising photon escape fraction, which favor smaller values of f_esc < 20%. However, models that invoke a redshift evolution of f_ esc that is consistent with these constraints can suppress the z~7 Lya flux to the observed level, if they also include a small evolution in global neutral fraction of Delta x_HI ~ 0.2. Thus, an evolving escape fraction of ionising photons can be a plausible part of the explanation for evolution in the Lya emission of high redshift galaxies. More generally, our analysis also shows that the drop in the Lya fraction is quantitatively consistent with the observed evolution in the Lya luminosity functions of Lya Emitters."}],"date_updated":"2024-09-24T12:10:12Z","type":"journal_article","title":"Evolution in the escape fraction of ionizing photons and the decline in strong Lyα emission from z > 6 galaxies","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_type":"original","oa":1,"publisher":"Oxford University Press","year":"2014","date_published":"2014-04-17T00:00:00Z","page":"3309-3316","article_processing_charge":"No","intvolume":"       440","volume":440,"issue":"4","_id":"17645","extern":"1","author":[{"first_name":"Mark","last_name":"Dijkstra","full_name":"Dijkstra, Mark"},{"full_name":"Wyithe, Stuart","last_name":"Wyithe","first_name":"Stuart"},{"first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","last_name":"Haiman"},{"last_name":"Mesinger","full_name":"Mesinger, Andrei","first_name":"Andrei"},{"first_name":"Laura","last_name":"Pentericci","full_name":"Pentericci, Laura"}]},{"author":[{"first_name":"Eli","full_name":"Visbal, Eli","last_name":"Visbal"},{"first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán"},{"first_name":"Greg L.","full_name":"Bryan, Greg L.","last_name":"Bryan"}],"_id":"17650","extern":"1","issue":"1","volume":445,"intvolume":"       445","article_processing_charge":"No","page":"1056-1063","date_published":"2014-10-08T00:00:00Z","year":"2014","publisher":"Oxford University Press","oa":1,"article_type":"original","title":"Direct collapse black hole formation from synchronized pairs of atomic cooling haloes","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_updated":"2024-09-24T13:02:31Z","type":"journal_article","abstract":[{"text":"High-redshift quasar observations imply that supermassive black holes (SMBHs) larger than ∼109 M⊙ formed before z=6. That such large SMBHs formed so early in the Universe remains an open theoretical problem. One possibility is that gas in atomic cooling halos exposed to strong Lyman-Werner (LW) radiation forms 104−106 M⊙ supermassive stars which quickly collapse into black holes. We propose a scenario for direct collapse black hole (DCBH) formation based on synchronized pairs of pristine atomic cooling halos. We consider halos at very small separation with one halo being a subhalo of the other. The first halo to surpass the atomic cooling threshold forms stars. Soon after these stars are formed, the other halo reaches the cooling threshold and due to its small distance from the newly formed galaxy, is exposed to the critical LW intensity required to form a DCBH. The main advantage of this scenario is that synchronization can potentially prevent photoevaporation and metal pollution in DCBH-forming halos. Since the halos reach the atomic cooling threshold at nearly the same time, the DCBH-forming halo is only exposed to ionizing radiation for a brief period. Tight synchronization could allow the DCBH to form before stars in the nearby galaxy reach the end of their lives and generate supernovae winds. We use N-body simulations to estimate the abundance of DCBHs formed in this way. The largest source of uncertainty in our estimate is the initial mass function (IMF) of metal free stars formed in atomic cooling halos. We find that even for tight synchronization, the density of DCBHs formed in this scenario could explain the SMBHs implied by z=6 quasar observations. Metal pollution and photoevaporation could potentially reduce the abundance of DCBHs below that required to explain the observations in other models that rely on a high LW flux.","lang":"eng"}],"publication_identifier":{"issn":["0035-8711","1365-2966"]},"date_created":"2024-09-06T07:28:59Z","publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Published Version","language":[{"iso":"eng"}],"quality_controlled":"1","month":"10","day":"08","doi":"10.1093/mnras/stu1794","publication_status":"published","scopus_import":"1","main_file_link":[{"url":"https://doi.org/10.1093/mnras/stu1794","open_access":"1"}],"status":"public","citation":{"mla":"Visbal, Eli, et al. “Direct Collapse Black Hole Formation from Synchronized Pairs of Atomic Cooling Haloes.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 445, no. 1, Oxford University Press, 2014, pp. 1056–63, doi:<a href=\"https://doi.org/10.1093/mnras/stu1794\">10.1093/mnras/stu1794</a>.","chicago":"Visbal, Eli, Zoltán Haiman, and Greg L. Bryan. “Direct Collapse Black Hole Formation from Synchronized Pairs of Atomic Cooling Haloes.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnras/stu1794\">https://doi.org/10.1093/mnras/stu1794</a>.","short":"E. Visbal, Z. Haiman, G.L. Bryan, Monthly Notices of the Royal Astronomical Society 445 (2014) 1056–1063.","ista":"Visbal E, Haiman Z, Bryan GL. 2014. Direct collapse black hole formation from synchronized pairs of atomic cooling haloes. Monthly Notices of the Royal Astronomical Society. 445(1), 1056–1063.","ieee":"E. Visbal, Z. Haiman, and G. L. Bryan, “Direct collapse black hole formation from synchronized pairs of atomic cooling haloes,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 445, no. 1. Oxford University Press, pp. 1056–1063, 2014.","ama":"Visbal E, Haiman Z, Bryan GL. Direct collapse black hole formation from synchronized pairs of atomic cooling haloes. <i>Monthly Notices of the Royal Astronomical Society</i>. 2014;445(1):1056-1063. doi:<a href=\"https://doi.org/10.1093/mnras/stu1794\">10.1093/mnras/stu1794</a>","apa":"Visbal, E., Haiman, Z., &#38; Bryan, G. L. (2014). Direct collapse black hole formation from synchronized pairs of atomic cooling haloes. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stu1794\">https://doi.org/10.1093/mnras/stu1794</a>"}},{"scopus_import":"1","citation":{"mla":"D’Orazio, Daniel J., et al. “Accretion into the Central Cavity of a Circumbinary Disc.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 436, no. 4, Oxford University Press, 2013, pp. 2997–3020, doi:<a href=\"https://doi.org/10.1093/mnras/stt1787\">10.1093/mnras/stt1787</a>.","short":"D.J. D’Orazio, Z. Haiman, A. MacFadyen, Monthly Notices of the Royal Astronomical Society 436 (2013) 2997–3020.","chicago":"D’Orazio, Daniel J., Zoltán Haiman, and Andrew MacFadyen. “Accretion into the Central Cavity of a Circumbinary Disc.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2013. <a href=\"https://doi.org/10.1093/mnras/stt1787\">https://doi.org/10.1093/mnras/stt1787</a>.","ista":"D’Orazio DJ, Haiman Z, MacFadyen A. 2013. Accretion into the central cavity of a circumbinary disc. Monthly Notices of the Royal Astronomical Society. 436(4), 2997–3020.","ieee":"D. J. D’Orazio, Z. Haiman, and A. MacFadyen, “Accretion into the central cavity of a circumbinary disc,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 436, no. 4. Oxford University Press, pp. 2997–3020, 2013.","ama":"D’Orazio DJ, Haiman Z, MacFadyen A. Accretion into the central cavity of a circumbinary disc. <i>Monthly Notices of the Royal Astronomical Society</i>. 2013;436(4):2997-3020. doi:<a href=\"https://doi.org/10.1093/mnras/stt1787\">10.1093/mnras/stt1787</a>","apa":"D’Orazio, D. J., Haiman, Z., &#38; MacFadyen, A. (2013). Accretion into the central cavity of a circumbinary disc. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stt1787\">https://doi.org/10.1093/mnras/stt1787</a>"},"main_file_link":[{"url":" https://doi.org/10.48550/arXiv.1210.0536","open_access":"1"}],"status":"public","language":[{"iso":"eng"}],"oa_version":"Preprint","quality_controlled":"1","arxiv":1,"doi":"10.1093/mnras/stt1787","day":"18","publication_status":"published","month":"10","date_updated":"2024-09-24T08:47:58Z","type":"journal_article","publication_identifier":{"issn":["1365-2966","0035-8711"]},"date_created":"2024-09-05T13:53:11Z","publication":"Monthly Notices of the Royal Astronomical Society","abstract":[{"text":"A near-equal-mass binary black hole (BH) can clear a central cavity in a circumbinary accretion disc; however, previous works have revealed accretion streams entering this cavity. Here we use 2D hydrodynamical simulations to study the accretion streams and their periodic behaviour. In particular, we perform a suite of simulations, covering different binary mass ratios q = M2/M1 in the range 0.003 ≤ q ≤ 1. In each case, we follow the system for several thousand binary orbits, until it relaxes to a stable accretion pattern. We find the following results: (i) the binary is efficient in maintaining a low-density cavity. However, the time-averaged mass accretion rate into the cavity, through narrow coherent accretion streams, is suppressed by at most a factor of a few compared to a disc with a single BH with the same mass; (ii) for q ≳ 0.05, the accretion rate is strongly modulated by the binary, and depending on the precise value of q, the power spectrum of the accretion rate shows either one, two or three distinct periods; and (iii) for q ≲ 0.05, the accretion rate becomes steady, with no time variations. Most binaries produced in galactic mergers are expected to have q ≳ 0.05. If the luminosity of these binaries tracks their accretion rate, then a periodogram of their light curve could help in their identification, and to constrain their mass ratio and disc properties.","lang":"eng"}],"oa":1,"title":"Accretion into the central cavity of a circumbinary disc","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_type":"original","year":"2013","publisher":"Oxford University Press","page":"2997-3020","article_processing_charge":"No","date_published":"2013-10-18T00:00:00Z","volume":436,"intvolume":"       436","author":[{"first_name":"Daniel J.","full_name":"D'Orazio, Daniel J.","last_name":"D'Orazio"},{"last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","first_name":"Zoltán"},{"first_name":"Andrew","full_name":"MacFadyen, Andrew","last_name":"MacFadyen"}],"issue":"4","_id":"17624","extern":"1","external_id":{"arxiv":["1210.0536"]}},{"_id":"17646","issue":"4","extern":"1","author":[{"first_name":"R. S.","full_name":"de Souza, R. S.","last_name":"de Souza"},{"first_name":"A.","last_name":"Mesinger","full_name":"Mesinger, A."},{"full_name":"Ferrara, A.","last_name":"Ferrara","first_name":"A."},{"last_name":"Haiman","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán"},{"first_name":"R.","last_name":"Perna","full_name":"Perna, R."},{"last_name":"Yoshida","full_name":"Yoshida, N.","first_name":"N."}],"intvolume":"       432","volume":432,"date_published":"2013-05-09T00:00:00Z","article_processing_charge":"No","page":"3218-3227","publisher":"Oxford University Press","year":"2013","article_type":"original","title":"Constraints on warm dark matter models from high-redshift long gamma-ray bursts","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","oa":1,"abstract":[{"text":"Structures in Warm Dark Matter (WDM) models are exponentially suppressed below a certain scale, characterized by the dark matter particle mass, mx. Since structures form hierarchically, the presence of collapsed objects at high-redshifts can set strong lower limits on mx. We place robust constraints on mx using recent results from the {\\it Swift} database of high-redshift gamma-ray bursts (GRBs). We parameterize the redshift evolution of the ratio between the cosmic GRB rate and star formation rate (SFR) as ∝(1+z)α, thereby allowing astrophysical uncertainties to partially mimic the cosmological suppression of structures in WDM models. Using a maximum likelihood estimator on two different z>4 GRB subsamples (including two bursts at z>8), we constrain mx≳1.6-1.8 keV at 95% C.L., when marginalized over a flat prior in α. We further estimate that 5 years of a SVOM-like mission would tighten these constraints to mx≳2.3 keV. Our results show that GRBs are a powerful probe of high-redshift structures, providing robust and competitive constraints on mx.","lang":"eng"}],"publication_identifier":{"issn":["0035-8711","1365-2966"]},"publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2024-09-06T07:25:13Z","date_updated":"2024-09-24T12:40:52Z","type":"journal_article","month":"05","doi":"10.1093/mnras/stt674","day":"09","publication_status":"published","quality_controlled":"1","oa_version":"Published Version","language":[{"iso":"eng"}],"status":"public","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stt674"}],"citation":{"ista":"de Souza RS, Mesinger A, Ferrara A, Haiman Z, Perna R, Yoshida N. 2013. Constraints on warm dark matter models from high-redshift long gamma-ray bursts. Monthly Notices of the Royal Astronomical Society. 432(4), 3218–3227.","mla":"de Souza, R. S., et al. “Constraints on Warm Dark Matter Models from High-Redshift Long Gamma-Ray Bursts.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 432, no. 4, Oxford University Press, 2013, pp. 3218–27, doi:<a href=\"https://doi.org/10.1093/mnras/stt674\">10.1093/mnras/stt674</a>.","short":"R.S. de Souza, A. Mesinger, A. Ferrara, Z. Haiman, R. Perna, N. Yoshida, Monthly Notices of the Royal Astronomical Society 432 (2013) 3218–3227.","chicago":"Souza, R. S. de, A. Mesinger, A. Ferrara, Zoltán Haiman, R. Perna, and N. Yoshida. “Constraints on Warm Dark Matter Models from High-Redshift Long Gamma-Ray Bursts.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2013. <a href=\"https://doi.org/10.1093/mnras/stt674\">https://doi.org/10.1093/mnras/stt674</a>.","ama":"de Souza RS, Mesinger A, Ferrara A, Haiman Z, Perna R, Yoshida N. Constraints on warm dark matter models from high-redshift long gamma-ray bursts. <i>Monthly Notices of the Royal Astronomical Society</i>. 2013;432(4):3218-3227. doi:<a href=\"https://doi.org/10.1093/mnras/stt674\">10.1093/mnras/stt674</a>","apa":"de Souza, R. S., Mesinger, A., Ferrara, A., Haiman, Z., Perna, R., &#38; Yoshida, N. (2013). Constraints on warm dark matter models from high-redshift long gamma-ray bursts. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stt674\">https://doi.org/10.1093/mnras/stt674</a>","ieee":"R. S. de Souza, A. Mesinger, A. Ferrara, Z. Haiman, R. Perna, and N. Yoshida, “Constraints on warm dark matter models from high-redshift long gamma-ray bursts,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 432, no. 4. Oxford University Press, pp. 3218–3227, 2013."},"scopus_import":"1"},{"date_published":"2013-09-10T00:00:00Z","article_processing_charge":"No","page":"3559-3567","publisher":"Oxford University Press","year":"2013","extern":"1","_id":"17653","issue":"4","author":[{"last_name":"Tanaka","full_name":"Tanaka, Takamitsu L.","first_name":"Takamitsu L."},{"full_name":"Li, Miao","last_name":"Li","first_name":"Miao"},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán"}],"intvolume":"       435","volume":435,"month":"09","day":"10","doi":"10.1093/mnras/stt1553","publication_status":"published","language":[{"iso":"eng"}],"oa_version":"Published Version","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stt1553"}],"status":"public","citation":{"apa":"Tanaka, T. L., Li, M., &#38; Haiman, Z. (2013). The effect of baryonic streaming motions on the formation of the first supermassive black holes. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stt1553\">https://doi.org/10.1093/mnras/stt1553</a>","ama":"Tanaka TL, Li M, Haiman Z. The effect of baryonic streaming motions on the formation of the first supermassive black holes. <i>Monthly Notices of the Royal Astronomical Society</i>. 2013;435(4):3559-3567. doi:<a href=\"https://doi.org/10.1093/mnras/stt1553\">10.1093/mnras/stt1553</a>","ieee":"T. L. Tanaka, M. Li, and Z. Haiman, “The effect of baryonic streaming motions on the formation of the first supermassive black holes,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 435, no. 4. Oxford University Press, pp. 3559–3567, 2013.","ista":"Tanaka TL, Li M, Haiman Z. 2013. The effect of baryonic streaming motions on the formation of the first supermassive black holes. Monthly Notices of the Royal Astronomical Society. 435(4), 3559–3567.","short":"T.L. Tanaka, M. Li, Z. Haiman, Monthly Notices of the Royal Astronomical Society 435 (2013) 3559–3567.","chicago":"Tanaka, Takamitsu L., Miao Li, and Zoltán Haiman. “The Effect of Baryonic Streaming Motions on the Formation of the First Supermassive Black Holes.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2013. <a href=\"https://doi.org/10.1093/mnras/stt1553\">https://doi.org/10.1093/mnras/stt1553</a>.","mla":"Tanaka, Takamitsu L., et al. “The Effect of Baryonic Streaming Motions on the Formation of the First Supermassive Black Holes.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 435, no. 4, Oxford University Press, 2013, pp. 3559–67, doi:<a href=\"https://doi.org/10.1093/mnras/stt1553\">10.1093/mnras/stt1553</a>."},"scopus_import":"1","article_type":"original","title":"The effect of baryonic streaming motions on the formation of the first supermassive black holes","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","oa":1,"abstract":[{"text":"Observations of quasars at redshifts z > 6 reveal that 10^9 Msol supermassive black holes (SMBHs) had already formed when the Universe was < 0.9 Gyr old. One hypothesis for the origins of these SMBHs is that they grew from the remnants of the first generation of massive stars, which formed in low-mass (~ 10^5 to 10^6 Msol) dark matter minihaloes at z > 20. This is the regime where baryonic streaming motions--the relative velocities of baryons with respect to dark matter in the early Universe--most strongly inhibit star formation by suppressing gas infall and cooling. We investigate the impact of this effect on the growth of the first SMBHs using a suite of high-fidelity, ellipsoidal-collapse Monte Carlo merger-tree simulations. We find that the suppression of seed BH formation by the streaming motions significantly reduces the number density of the most massive BHs at z > 15, but the residual effect at lower redshifts is essentially negligible. The streaming motions can reduce by a factor of few the number density of the most luminous quasars at z ~ 10-11, where such objects could be detected by the James Webb Space Telescope. We conclude, with minor theoretical caveats, that baryonic streaming motions are unlikely to pose a significant additional obstacle to the formation of the observed high-redshift quasar SMBHs. Nor do they appreciably affect the heating and reionization histories of the Universe or the merger rates of nuclear BHs in the mass and redshift ranges of interest for proposed gravitational-wave detectors.","lang":"eng"}],"publication_identifier":{"issn":["1365-2966","0035-8711"]},"publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2024-09-06T07:31:32Z","date_updated":"2024-09-24T13:26:36Z","type":"journal_article"},{"scopus_import":"1","citation":{"mla":"McKernan, B., et al. “Ripple Effects and Oscillations in the Broad Fe Kα Line as a Probe of Massive Black Hole Mergers.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 432, no. 2, Oxford University Press, 2013, pp. 1468–82, doi:<a href=\"https://doi.org/10.1093/mnras/stt567\">10.1093/mnras/stt567</a>.","chicago":"McKernan, B., K. E. S. Ford, B. Kocsis, and Zoltán Haiman. “Ripple Effects and Oscillations in the Broad Fe Kα Line as a Probe of Massive Black Hole Mergers.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2013. <a href=\"https://doi.org/10.1093/mnras/stt567\">https://doi.org/10.1093/mnras/stt567</a>.","short":"B. McKernan, K.E.S. Ford, B. Kocsis, Z. Haiman, Monthly Notices of the Royal Astronomical Society 432 (2013) 1468–1482.","ista":"McKernan B, Ford KES, Kocsis B, Haiman Z. 2013. Ripple effects and oscillations in the broad Fe Kα line as a probe of massive black hole mergers. Monthly Notices of the Royal Astronomical Society. 432(2), 1468–1482.","ieee":"B. McKernan, K. E. S. Ford, B. Kocsis, and Z. Haiman, “Ripple effects and oscillations in the broad Fe Kα line as a probe of massive black hole mergers,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 432, no. 2. Oxford University Press, pp. 1468–1482, 2013.","ama":"McKernan B, Ford KES, Kocsis B, Haiman Z. Ripple effects and oscillations in the broad Fe Kα line as a probe of massive black hole mergers. <i>Monthly Notices of the Royal Astronomical Society</i>. 2013;432(2):1468-1482. doi:<a href=\"https://doi.org/10.1093/mnras/stt567\">10.1093/mnras/stt567</a>","apa":"McKernan, B., Ford, K. E. S., Kocsis, B., &#38; Haiman, Z. (2013). Ripple effects and oscillations in the broad Fe Kα line as a probe of massive black hole mergers. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stt567\">https://doi.org/10.1093/mnras/stt567</a>"},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stt567"}],"status":"public","quality_controlled":"1","oa_version":"Published Version","language":[{"iso":"eng"}],"day":"02","doi":"10.1093/mnras/stt567","publication_status":"published","month":"05","date_updated":"2024-09-25T09:13:00Z","type":"journal_article","publication_identifier":{"issn":["0035-8711","1365-2966"]},"publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2024-09-06T08:18:32Z","abstract":[{"text":"When a sufficiently massive satellite (or secondary) black hole is embedded in a gas disc around a (primary) supermassive black hole, it can open an empty gap in the disc. A gap-opening secondary close to the primary will leave an imprint in the broad component of the Fe Kα emission line, which varies in a unique and predictable manner. If the gap persists into the innermost disc, the effect consists of a pair of dips in the broad line which ripple blue-ward and red-ward from the line centroid energy, respectively, as the gap moves closer to the primary. This ripple effect could be unambiguously detectable and allow an electromagnetic monitoring of massive black hole mergers as they occur. As the mass ratio of the secondary to primary black hole increases to q ≳ 0.01, we expect the gap to widen, possibly clearing a central cavity in the inner disc, which shows up in the broad Fe Kα line component. If the secondary stalls at ≥ 102rg in its in-migration, due to low corotating gas mass, a detectable ripple effect occurs in the broad line component on the disc viscous time-scale as the inner disc drains and the outer disc is dammed. If the secondary maintains an accretion disc within a central cavity, due to dam bursting or leakage, a periodic ‘see-saw’ oscillation effect is exhibited in the observed line profile. Here, we demonstrate the range of ripple effect signatures potentially detectable with Astro-H and IXO/Athena, and oscillation effects potentially detectable with XMM–Newton or LOFT for a wide variety of merger and disc conditions, including gap width (or cavity size), disc inclination angle and emissivity profile, damming of the accretion flow by the secondary, and a minidisc around the satellite black hole. A systematic study of ripple effects would require a telescope effective area substantially larger than that planned for IXO/Athena. Future mission planning should take this into account. Observations of the ripple effect and periodic oscillations can be used to provide an early warning of gravitational radiation emission from the AGN. Once gravitational waves consistent with massive black hole mergers are detected, an archival search for the Fe Kα ripple effect or periodic oscillations will help in localizing their origin.","lang":"eng"}],"oa":1,"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","title":"Ripple effects and oscillations in the broad Fe Kα line as a probe of massive black hole mergers","article_type":"original","year":"2013","publisher":"Oxford University Press","page":"1468-1482","article_processing_charge":"No","date_published":"2013-05-02T00:00:00Z","volume":432,"intvolume":"       432","author":[{"first_name":"B.","last_name":"McKernan","full_name":"McKernan, B."},{"first_name":"K. E. S.","last_name":"Ford","full_name":"Ford, K. E. S."},{"first_name":"B.","full_name":"Kocsis, B.","last_name":"Kocsis"},{"first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"}],"_id":"17683","extern":"1","issue":"2"},{"article_processing_charge":"No","page":"2301-2325","date_published":"2013-10-08T00:00:00Z","year":"2013","publisher":"Oxford University Press","author":[{"first_name":"Joaquin","full_name":"Prieto, Joaquin","last_name":"Prieto"},{"full_name":"Jimenez, Raul","last_name":"Jimenez","first_name":"Raul"},{"first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","last_name":"Haiman"}],"_id":"17684","extern":"1","issue":"3","volume":436,"intvolume":"       436","language":[{"iso":"eng"}],"oa_version":"Published Version","quality_controlled":"1","month":"10","doi":"10.1093/mnras/stt1730","day":"08","publication_status":"published","scopus_import":"1","status":"public","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stt1730"}],"citation":{"mla":"Prieto, Joaquin, et al. “Gas Infall into Atomic Cooling Haloes: On the Formation of Protogalactic Discs and Supermassive Black Holes at z &#62; 10.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 436, no. 3, Oxford University Press, 2013, pp. 2301–25, doi:<a href=\"https://doi.org/10.1093/mnras/stt1730\">10.1093/mnras/stt1730</a>.","chicago":"Prieto, Joaquin, Raul Jimenez, and Zoltán Haiman. “Gas Infall into Atomic Cooling Haloes: On the Formation of Protogalactic Discs and Supermassive Black Holes at z &#62; 10.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2013. <a href=\"https://doi.org/10.1093/mnras/stt1730\">https://doi.org/10.1093/mnras/stt1730</a>.","short":"J. Prieto, R. Jimenez, Z. Haiman, Monthly Notices of the Royal Astronomical Society 436 (2013) 2301–2325.","ista":"Prieto J, Jimenez R, Haiman Z. 2013. Gas infall into atomic cooling haloes: On the formation of protogalactic discs and supermassive black holes at z &#62; 10. Monthly Notices of the Royal Astronomical Society. 436(3), 2301–2325.","ieee":"J. Prieto, R. Jimenez, and Z. Haiman, “Gas infall into atomic cooling haloes: On the formation of protogalactic discs and supermassive black holes at z &#62; 10,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 436, no. 3. Oxford University Press, pp. 2301–2325, 2013.","ama":"Prieto J, Jimenez R, Haiman Z. Gas infall into atomic cooling haloes: On the formation of protogalactic discs and supermassive black holes at z &#62; 10. <i>Monthly Notices of the Royal Astronomical Society</i>. 2013;436(3):2301-2325. doi:<a href=\"https://doi.org/10.1093/mnras/stt1730\">10.1093/mnras/stt1730</a>","apa":"Prieto, J., Jimenez, R., &#38; Haiman, Z. (2013). Gas infall into atomic cooling haloes: On the formation of protogalactic discs and supermassive black holes at z &#62; 10. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stt1730\">https://doi.org/10.1093/mnras/stt1730</a>"},"oa":1,"article_type":"original","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","title":"Gas infall into atomic cooling haloes: On the formation of protogalactic discs and supermassive black holes at z > 10","date_updated":"2024-09-25T09:15:36Z","type":"journal_article","abstract":[{"text":"We have performed cosmo-hydro simulations using the RAMSES code to study atomic cooling (ACHs) haloes at z=10 with masses 5E7Msun<~M<~2E9Msun. We assume primordial gas and H2-cooling and prior star-formation have been suppressed. We analysed 19 haloes (gas and DM) at a resolution of ~10 (proper) pc, selected from a total volume of ~2E3 (comoving) Mpc3. This is the largest statistical hydro-sim. study of ACHs at z>10 to date. We examine the morphology, angular momentum (AM), thermodynamic, and turbulence of these haloes, in order to assess the prevalence of disks and supermassive black holes (SMBHs). We find no correlation between either the magnitude or the direction of the AM of the gas and its parent DM halo. Only 3 haloes form rotationally supported cores. Two of the most massive haloes form massive, compact overdense blobs. These blobs have an accretion rate ~0.5 Msun/yr (at a distance of 100 pc), and are possible sites of SMBH formation. Our results suggest that the degree of rotational support and the fate of the gas in a halo is determined by its large-scale environment and merger history. In particular, the two haloes forming blobs are located at knots of the cosmic web, cooled early on, and experienced many mergers. The gas in these haloes is lumpy and highly turbulent, with Mach N. >~ 5. In contrast, the haloes forming rotationally supported cores are relatively more isolated, located midway along filaments, cooled more recently, and underwent fewer mergers. Thus, the gas in these haloes is less lumpy and less turbulent (Mach <~ 4), and could retain most of its AM. The remaining 14 haloes have intermediate properties. If verified in a larger sample of haloes and with additional physics, our results will have implications for observations of the highest-redshift galaxies and quasars with JWST.","lang":"eng"}],"publication_identifier":{"issn":["1365-2966","0035-8711"]},"date_created":"2024-09-06T08:19:41Z","publication":"Monthly Notices of the Royal Astronomical Society"},{"date_published":"2012-12-11T00:00:00Z","page":"2680-2700","article_processing_charge":"No","publisher":"Oxford University Press","year":"2012","alternative_title":["Overflow and migration: SMBH binaries"],"issue":"3","_id":"17613","extern":"1","author":[{"first_name":"Bence","last_name":"Kocsis","full_name":"Kocsis, Bence"},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán"},{"full_name":"Loeb, Abraham","last_name":"Loeb","first_name":"Abraham"}],"intvolume":"       427","volume":427,"publication_status":"published","day":"11","doi":"10.1111/j.1365-2966.2012.22118.x","month":"12","language":[{"iso":"eng"}],"quality_controlled":"1","oa_version":"Published Version","citation":{"ista":"Kocsis B, Haiman Z, Loeb A. 2012. Gas pile-up, gap overflow and Type 1.5 migration in circumbinary discs: Application to supermassive black hole binaries. Monthly Notices of the Royal Astronomical Society. 427(3), 2680–2700.","chicago":"Kocsis, Bence, Zoltán Haiman, and Abraham Loeb. “Gas Pile-up, Gap Overflow and Type 1.5 Migration in Circumbinary Discs: Application to Supermassive Black Hole Binaries.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2012. <a href=\"https://doi.org/10.1111/j.1365-2966.2012.22118.x\">https://doi.org/10.1111/j.1365-2966.2012.22118.x</a>.","mla":"Kocsis, Bence, et al. “Gas Pile-up, Gap Overflow and Type 1.5 Migration in Circumbinary Discs: Application to Supermassive Black Hole Binaries.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 427, no. 3, Oxford University Press, 2012, pp. 2680–700, doi:<a href=\"https://doi.org/10.1111/j.1365-2966.2012.22118.x\">10.1111/j.1365-2966.2012.22118.x</a>.","short":"B. Kocsis, Z. Haiman, A. Loeb, Monthly Notices of the Royal Astronomical Society 427 (2012) 2680–2700.","ama":"Kocsis B, Haiman Z, Loeb A. Gas pile-up, gap overflow and Type 1.5 migration in circumbinary discs: Application to supermassive black hole binaries. <i>Monthly Notices of the Royal Astronomical Society</i>. 2012;427(3):2680-2700. doi:<a href=\"https://doi.org/10.1111/j.1365-2966.2012.22118.x\">10.1111/j.1365-2966.2012.22118.x</a>","apa":"Kocsis, B., Haiman, Z., &#38; Loeb, A. (2012). Gas pile-up, gap overflow and Type 1.5 migration in circumbinary discs: Application to supermassive black hole binaries. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1111/j.1365-2966.2012.22118.x\">https://doi.org/10.1111/j.1365-2966.2012.22118.x</a>","ieee":"B. Kocsis, Z. Haiman, and A. Loeb, “Gas pile-up, gap overflow and Type 1.5 migration in circumbinary discs: Application to supermassive black hole binaries,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 427, no. 3. Oxford University Press, pp. 2680–2700, 2012."},"main_file_link":[{"url":"https://doi.org/10.1111/j.1365-2966.2012.22118.x","open_access":"1"}],"status":"public","scopus_import":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","title":"Gas pile-up, gap overflow and Type 1.5 migration in circumbinary discs: Application to supermassive black hole binaries","article_type":"original","oa":1,"date_created":"2024-09-05T13:28:17Z","publication":"Monthly Notices of the Royal Astronomical Society","publication_identifier":{"issn":["0035-8711","1365-2966"]},"abstract":[{"lang":"eng","text":"We study the interaction of a supermassive black hole (SMBH) binary and a standard radiatively efficient thin accretion disk. We examine steady-state configurations of the disk and migrating SMBH system, self-consistently accounting for tidal and viscous torques and heating, radiative diffusion limited cooling, gas and radiation pressure, and the decay of the binary's orbit. We obtain a \"phase diagram\" of the system as a function of binary parameters, showing regimes in which both the disk structure and migration have a different character. Although massive binaries can create a central gap in the disk at large radii, the tidal barrier of the secondary causes a significant pile-up of gas outside of its orbit, which can lead to the closing of the gap. We find that this spillover occurs at an orbital separation as large as ~200 M_7^{-1/2} gravitational radii, where M = 10^7 M_7 Msun is the total binary mass. If the secondary is less massive than ~10^6 Msun, then the gap is closed before gravitational waves (GWs) start dominating the orbital decay. In this regime, the disk is still strongly perturbed, but the piled-up gas continuously overflows as in a porous dam, and crosses inside the secondary's orbit. The corresponding migration rate, which we label Type 1.5, is slower than the usual limiting cases known as Type I and II migration. Compared to an unperturbed disk, the steady-state disk in the overflowing regime is up to several hundred times brighter in the optical bands. Surveys such as PanSTARRS or LSST may discover the periodic variability of this population of binaries. Our results imply that the circumbinary disks around SMBHs can extend to small radii during the last stages of their merger, when they are detectable by LISA, and may produce coincident electromagnetic (EM) emission similar to active galactic nuclei (AGN)."}],"type":"journal_article","date_updated":"2024-09-24T07:40:02Z"},{"article_processing_charge":"No","page":"2660-2679","date_published":"2012-12-11T00:00:00Z","year":"2012","publisher":"Oxford University Press","author":[{"first_name":"Bence","last_name":"Kocsis","full_name":"Kocsis, Bence"},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán"},{"last_name":"Loeb","full_name":"Loeb, Abraham","first_name":"Abraham"}],"_id":"17660","issue":"3","extern":"1","alternative_title":["Overflow and migration: general theory"],"volume":427,"intvolume":"       427","oa_version":"Published Version","language":[{"iso":"eng"}],"quality_controlled":"1","month":"12","day":"11","doi":"10.1111/j.1365-2966.2012.22129.x","publication_status":"published","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1111/j.1365-2966.2012.22129.x"}],"status":"public","citation":{"mla":"Kocsis, Bence, et al. “Gas Pile-up, Gap Overflow and Type 1.5 Migration in Circumbinary Discs: General Theory.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 427, no. 3, Oxford University Press, 2012, pp. 2660–79, doi:<a href=\"https://doi.org/10.1111/j.1365-2966.2012.22129.x\">10.1111/j.1365-2966.2012.22129.x</a>.","chicago":"Kocsis, Bence, Zoltán Haiman, and Abraham Loeb. “Gas Pile-up, Gap Overflow and Type 1.5 Migration in Circumbinary Discs: General Theory.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2012. <a href=\"https://doi.org/10.1111/j.1365-2966.2012.22129.x\">https://doi.org/10.1111/j.1365-2966.2012.22129.x</a>.","short":"B. Kocsis, Z. Haiman, A. Loeb, Monthly Notices of the Royal Astronomical Society 427 (2012) 2660–2679.","ista":"Kocsis B, Haiman Z, Loeb A. 2012. Gas pile-up, gap overflow and Type 1.5 migration in circumbinary discs: General theory. Monthly Notices of the Royal Astronomical Society. 427(3), 2660–2679.","ieee":"B. Kocsis, Z. Haiman, and A. Loeb, “Gas pile-up, gap overflow and Type 1.5 migration in circumbinary discs: General theory,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 427, no. 3. Oxford University Press, pp. 2660–2679, 2012.","ama":"Kocsis B, Haiman Z, Loeb A. Gas pile-up, gap overflow and Type 1.5 migration in circumbinary discs: General theory. <i>Monthly Notices of the Royal Astronomical Society</i>. 2012;427(3):2660-2679. doi:<a href=\"https://doi.org/10.1111/j.1365-2966.2012.22129.x\">10.1111/j.1365-2966.2012.22129.x</a>","apa":"Kocsis, B., Haiman, Z., &#38; Loeb, A. (2012). Gas pile-up, gap overflow and Type 1.5 migration in circumbinary discs: General theory. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1111/j.1365-2966.2012.22129.x\">https://doi.org/10.1111/j.1365-2966.2012.22129.x</a>"},"oa":1,"article_type":"original","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","title":"Gas pile-up, gap overflow and Type 1.5 migration in circumbinary discs: General theory","date_updated":"2024-09-25T07:21:05Z","type":"journal_article","abstract":[{"text":"Many astrophysical binaries, from planets to black holes, exert strong torques on their circumbinary accretion discs, and are expected to significantly modify the disc structure. Despite the several decade long history of the subject, the joint evolution of the binary + disc system has not been modelled with self-consistent assumptions for arbitrary mass ratios and accretion rates. Here, we solve the coupled binary–disc evolution equations analytically in the strongly perturbed limit, treating the azimuthally averaged angular momentum exchange between the disc and the binary and the modifications to the density, scaleheight, and viscosity self-consistently, including viscous and tidal heating, diffusion limited cooling, radiation pressure and the orbital decay of the binary. We find a solution with a central cavity and a migration rate similar to those previously obtained for Type II migration, applicable for large masses and binary separations, and near-equal mass ratios. However, we identify a distinct new regime, applicable at smaller separations and masses, and mass ratio in the range 10−3 ≲ q ≲ 0.1. For these systems, gas piles up outside the binary's orbit, but rather than creating a cavity, it continuously overflows as in a porous dam. The disc profile is intermediate between a weakly perturbed disc (producing Type I migration) and a disc with a gap (with Type II migration). However, the migration rate of the secondary is typically slower than both Type I and Type II rates. We term this new regime ‘Type 1.5’ migration.","lang":"eng"}],"publication_identifier":{"issn":["0035-8711","1365-2966"]},"publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2024-09-06T07:38:16Z"},{"_id":"17674","extern":"1","issue":"4","alternative_title":["Improved models for CIB anisotropies"],"author":[{"full_name":"Shang, Cien","last_name":"Shang","first_name":"Cien"},{"first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán"},{"first_name":"Lloyd","full_name":"Knox, Lloyd","last_name":"Knox"},{"first_name":"S. Peng","full_name":"Oh, S. Peng","last_name":"Oh"}],"intvolume":"       421","volume":421,"date_published":"2012-04-10T00:00:00Z","page":"2832-2845","article_processing_charge":"No","publisher":"Oxford University Press","year":"2012","title":"Improved models for cosmic infrared background anisotropies: New constraints on the infrared galaxy population","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_type":"original","oa":1,"publication_identifier":{"issn":["0035-8711"]},"publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2024-09-06T07:50:37Z","abstract":[{"text":"The power spectrum of cosmic infrared background (CIB) anisotropies is sensitive to the connection between star formation and dark matter haloes over the entire cosmic star formation history. Here we develop a model that associates star‐forming galaxies with dark matter haloes and their subhaloes. The model is based on a parametrized relation between the dust‐processed infrared luminosity and (sub)halo mass. By adjusting three free parameters, we attempt to simultaneously fit the four frequency bands of the Planck measurement of the CIB anisotropy power spectrum. To fit the data, we find that the star formation efficiency must peak on a halo mass scale of ≈5 × 10^12 M⊙ and the infrared luminosity per unit mass must increase rapidly with redshift. By comparing our predictions with a well‐calibrated phenomenological model for shot noise, and with a direct observation of source counts, we show that the mean duty cycle of the underlying infrared sources must be near unity, indicating that the CIB is dominated by long‐lived quiescent star formation, rather than intermittent short ‘starbursts’. Despite the improved flexibility of our model, the best simultaneous fit to all four Planck channels remains relatively poor. We discuss possible further extensions to alleviate the remaining tension with the data. Our model presents a theoretical framework for a future joint analysis of both background anisotropy and source count measurements.","lang":"eng"}],"date_updated":"2024-09-25T08:36:17Z","type":"journal_article","day":"10","doi":"10.1111/j.1365-2966.2012.20510.x","publication_status":"published","month":"04","oa_version":"Published Version","language":[{"iso":"eng"}],"quality_controlled":"1","citation":{"ista":"Shang C, Haiman Z, Knox L, Oh SP. 2012. Improved models for cosmic infrared background anisotropies: New constraints on the infrared galaxy population. Monthly Notices of the Royal Astronomical Society. 421(4), 2832–2845.","mla":"Shang, Cien, et al. “Improved Models for Cosmic Infrared Background Anisotropies: New Constraints on the Infrared Galaxy Population.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 421, no. 4, Oxford University Press, 2012, pp. 2832–45, doi:<a href=\"https://doi.org/10.1111/j.1365-2966.2012.20510.x\">10.1111/j.1365-2966.2012.20510.x</a>.","chicago":"Shang, Cien, Zoltán Haiman, Lloyd Knox, and S. Peng Oh. “Improved Models for Cosmic Infrared Background Anisotropies: New Constraints on the Infrared Galaxy Population.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2012. <a href=\"https://doi.org/10.1111/j.1365-2966.2012.20510.x\">https://doi.org/10.1111/j.1365-2966.2012.20510.x</a>.","short":"C. Shang, Z. Haiman, L. Knox, S.P. Oh, Monthly Notices of the Royal Astronomical Society 421 (2012) 2832–2845.","apa":"Shang, C., Haiman, Z., Knox, L., &#38; Oh, S. P. (2012). Improved models for cosmic infrared background anisotropies: New constraints on the infrared galaxy population. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1111/j.1365-2966.2012.20510.x\">https://doi.org/10.1111/j.1365-2966.2012.20510.x</a>","ama":"Shang C, Haiman Z, Knox L, Oh SP. Improved models for cosmic infrared background anisotropies: New constraints on the infrared galaxy population. <i>Monthly Notices of the Royal Astronomical Society</i>. 2012;421(4):2832-2845. doi:<a href=\"https://doi.org/10.1111/j.1365-2966.2012.20510.x\">10.1111/j.1365-2966.2012.20510.x</a>","ieee":"C. Shang, Z. Haiman, L. Knox, and S. P. Oh, “Improved models for cosmic infrared background anisotropies: New constraints on the infrared galaxy population,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 421, no. 4. Oxford University Press, pp. 2832–2845, 2012."},"status":"public","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1111/j.1365-2966.2012.20510.x"}],"scopus_import":"1"},{"publisher":"Oxford University Press","year":"2012","date_published":"2012-11-22T00:00:00Z","article_processing_charge":"No","page":"3058-3071","intvolume":"       428","volume":428,"issue":"4","_id":"17678","extern":"1","author":[{"first_name":"Joshua","full_name":"Schroeder, Joshua","last_name":"Schroeder"},{"first_name":"Andrei","last_name":"Mesinger","full_name":"Mesinger, Andrei"},{"last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","first_name":"Zoltán"}],"status":"public","main_file_link":[{"url":"https://doi.org/10.1093/mnras/sts253","open_access":"1"}],"citation":{"mla":"Schroeder, Joshua, et al. “Evidence of Gunn–Peterson Damping Wings in High-z Quasar Spectra: Strengthening the Case for Incomplete Reionization at z ∼ 6–7.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 428, no. 4, Oxford University Press, 2012, pp. 3058–71, doi:<a href=\"https://doi.org/10.1093/mnras/sts253\">10.1093/mnras/sts253</a>.","chicago":"Schroeder, Joshua, Andrei Mesinger, and Zoltán Haiman. “Evidence of Gunn–Peterson Damping Wings in High-z Quasar Spectra: Strengthening the Case for Incomplete Reionization at z ∼ 6–7.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2012. <a href=\"https://doi.org/10.1093/mnras/sts253\">https://doi.org/10.1093/mnras/sts253</a>.","short":"J. Schroeder, A. Mesinger, Z. Haiman, Monthly Notices of the Royal Astronomical Society 428 (2012) 3058–3071.","ista":"Schroeder J, Mesinger A, Haiman Z. 2012. Evidence of Gunn–Peterson damping wings in high-z quasar spectra: Strengthening the case for incomplete reionization at z ∼ 6–7. Monthly Notices of the Royal Astronomical Society. 428(4), 3058–3071.","ieee":"J. Schroeder, A. Mesinger, and Z. Haiman, “Evidence of Gunn–Peterson damping wings in high-z quasar spectra: Strengthening the case for incomplete reionization at z ∼ 6–7,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 428, no. 4. Oxford University Press, pp. 3058–3071, 2012.","ama":"Schroeder J, Mesinger A, Haiman Z. Evidence of Gunn–Peterson damping wings in high-z quasar spectra: Strengthening the case for incomplete reionization at z ∼ 6–7. <i>Monthly Notices of the Royal Astronomical Society</i>. 2012;428(4):3058-3071. doi:<a href=\"https://doi.org/10.1093/mnras/sts253\">10.1093/mnras/sts253</a>","apa":"Schroeder, J., Mesinger, A., &#38; Haiman, Z. (2012). Evidence of Gunn–Peterson damping wings in high-z quasar spectra: Strengthening the case for incomplete reionization at z ∼ 6–7. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sts253\">https://doi.org/10.1093/mnras/sts253</a>"},"scopus_import":"1","month":"11","doi":"10.1093/mnras/sts253","day":"22","publication_status":"published","oa_version":"Published Version","language":[{"iso":"eng"}],"quality_controlled":"1","abstract":[{"lang":"eng","text":"The spectra of several high-redshift (z>6) quasars have shown evidence for a Gunn-Peterson (GP) damping wing, indicating a substantial mean neutral hydrogen fraction (x_HI > 0.03) in the z ~ 6 intergalactic medium (IGM). However, previous analyses assumed that the IGM was uniformly ionized outside of the quasar's HII region. Here we relax this assumption and model patchy reionization scenarios for a range of IGM and quasar parameters. We quantify the impact of these differences on the inferred x_HI, by fitting the spectra of three quasars: SDSS J1148+5251 (z=6.419), J1030+0524 (z=6.308), and J1623+3112 (z=6.247). We find that the best-fit values of x_HI in the patchy models agree well with the uniform case. More importantly, we confirm that the observed spectra favor the presence of a GP damping wing, with peak likelihoods decreasing by factors of > few - 10 when the spectra are modeled without a damping wing. We also find that the Ly alpha absorption spectra, by themselves, cannot distinguish the damping wing in a relatively neutral IGM from a damping wing in a highly ionized IGM, caused either by an isolated neutral patch, or by a damped Ly alpha absorber (DLA). However, neutral patches in a highly ionized universe (x_HI < 0.01), and DLAs with the large required column densities (N_HI > few x 10^{20} cm^{-2}) are both rare. As a result, when we include reasonable prior probabilities for the line of sight (LOS) to intercept either a neutral patch or a DLA at the required distance of ~ 40-60 comoving Mpc away from the quasar, we find strong lower limits on the neutral fraction in the IGM, x_HI > 0.1 (at 95% confidence). This strengthens earlier claims that a substantial global fraction of hydrogen in the z~6 IGM is in neutral form."}],"publication_identifier":{"issn":["0035-8711","1365-2966"]},"publication":"Monthly Notices of the Royal Astronomical Society","date_created":"2024-09-06T08:04:35Z","date_updated":"2024-09-25T08:53:21Z","type":"journal_article","article_type":"original","title":"Evidence of Gunn–Peterson damping wings in high-z quasar spectra: Strengthening the case for incomplete reionization at z ∼ 6–7","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","oa":1},{"page":"705-719","article_processing_charge":"No","date_published":"2012-01-23T00:00:00Z","year":"2012","publisher":"Oxford University Press","author":[{"full_name":"Tanaka, Takamitsu","last_name":"Tanaka","first_name":"Takamitsu"},{"first_name":"Kristen","last_name":"Menou","full_name":"Menou, Kristen"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"}],"alternative_title":["Electromagnetic counterparts of PTA sources"],"issue":"1","_id":"17688","extern":"1","volume":420,"intvolume":"       420","quality_controlled":"1","oa_version":"Published Version","language":[{"iso":"eng"}],"publication_status":"published","doi":"10.1111/j.1365-2966.2011.20083.x","day":"23","month":"01","scopus_import":"1","citation":{"ama":"Tanaka T, Menou K, Haiman Z. Electromagnetic counterparts of supermassive black hole binaries resolved by pulsar timing arrays. <i>Monthly Notices of the Royal Astronomical Society</i>. 2012;420(1):705-719. doi:<a href=\"https://doi.org/10.1111/j.1365-2966.2011.20083.x\">10.1111/j.1365-2966.2011.20083.x</a>","apa":"Tanaka, T., Menou, K., &#38; Haiman, Z. (2012). Electromagnetic counterparts of supermassive black hole binaries resolved by pulsar timing arrays. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1111/j.1365-2966.2011.20083.x\">https://doi.org/10.1111/j.1365-2966.2011.20083.x</a>","ieee":"T. Tanaka, K. Menou, and Z. Haiman, “Electromagnetic counterparts of supermassive black hole binaries resolved by pulsar timing arrays,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 420, no. 1. Oxford University Press, pp. 705–719, 2012.","ista":"Tanaka T, Menou K, Haiman Z. 2012. Electromagnetic counterparts of supermassive black hole binaries resolved by pulsar timing arrays. Monthly Notices of the Royal Astronomical Society. 420(1), 705–719.","mla":"Tanaka, Takamitsu, et al. “Electromagnetic Counterparts of Supermassive Black Hole Binaries Resolved by Pulsar Timing Arrays.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 420, no. 1, Oxford University Press, 2012, pp. 705–19, doi:<a href=\"https://doi.org/10.1111/j.1365-2966.2011.20083.x\">10.1111/j.1365-2966.2011.20083.x</a>.","short":"T. Tanaka, K. Menou, Z. Haiman, Monthly Notices of the Royal Astronomical Society 420 (2012) 705–719.","chicago":"Tanaka, Takamitsu, Kristen Menou, and Zoltán Haiman. “Electromagnetic Counterparts of Supermassive Black Hole Binaries Resolved by Pulsar Timing Arrays.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2012. <a href=\"https://doi.org/10.1111/j.1365-2966.2011.20083.x\">https://doi.org/10.1111/j.1365-2966.2011.20083.x</a>."},"main_file_link":[{"url":"https://doi.org/10.1111/j.1365-2966.2011.20083.x","open_access":"1"}],"status":"public","oa":1,"title":"Electromagnetic counterparts of supermassive black hole binaries resolved by pulsar timing arrays","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_type":"original","type":"journal_article","date_updated":"2024-09-25T09:49:01Z","date_created":"2024-09-06T08:23:06Z","publication":"Monthly Notices of the Royal Astronomical Society","publication_identifier":{"issn":["0035-8711"]},"abstract":[{"text":"Pulsar timing arrays (PTAs) are expected to detect gravitational waves (GWs) from individual low-redshift (z<1.5) compact supermassive (M>10^9 Msun) black hole (SMBH) binaries with orbital periods of approx. 0.1 - 10 yrs. Identifying the electromagnetic (EM) counterparts of these sources would provide confirmation of putative direct detections of GWs, present a rare opportunity to study the environments of compact SMBH binaries, and could enable the use of these sources as standard sirens for cosmology. Here we consider the feasibility of such an EM identification. We show that because the host galaxies of resolved PTA sources are expected to be exceptionally massive and rare, it should be possible to find unique hosts of resolved sources out to redshift z=0.2. At higher redshifts, the PTA error boxes are larger, and may contain as many as 100 massive-galaxy interlopers. The number of candidates, however, remains tractable for follow-up searches in upcoming wide-field EM surveys. We develop a toy model to characterize the dynamics and the thermal emission from a geometrically thin, gaseous disc accreting onto a PTA-source SMBH binary. Our model predicts that at optical and infrared frequencies, the source should appear similar to a typical luminous active galactic nucleus (AGN). However, owing to the evacuation of the accretion flow by the binary's tidal torques, the source might have an unusually low soft X-ray luminosity and weak UV and broad optical emission lines, as compared to an AGN powered by a single SMBH with the same total mass. For sources near z=1, the decrement in the rest-frame UV should be observable as an extremely red optical color. These properties would make the PTA sources stand out among optically luminous AGN, and could allow their unique identification.","lang":"eng"}]}]