[{"_id":"17611","issue":"1","language":[{"iso":"eng"}],"intvolume":"       522","oa":1,"doi":"10.1093/mnrasl/slad016","extern":"1","abstract":[{"text":"The project MOMO (Multiwavelength Observations and Modelling of OJ 287) was set up to test predictions of binary supermassive black hole (SMBH) scenarios and to understand disc–jet physics of the blazar OJ 287. After a correction, the precessing binary (PB) SMBH model predicted the next main outburst of OJ 287 in 2022 October, making the outburst well observable and the model testable. We have densely covered this period in our ongoing multifrequency radio, optical, ultraviolet (UV), and X-ray monitoring. The predicted outburst was not detected. Instead, OJ 287 was at low optical–UV emission levels, declining further into November. The predicted thermal bremsstrahlung spectrum was not observed either, at any epoch. Further, applying scaling relations, we estimate an SMBH mass of OJ 287 of 108 M⊙. The latest in a sequence of deep low states that recur every 1–2 yr is used to determine an upper limit on the Eddington ratio and on the accretion-disc luminosity. This limit is at least a factor of 10 lower than required by the PB model with its massive primary SMBH of &amp;gt;1010 M⊙. All these results favour alternative binary SMBH models of OJ 287 that require neither strong orbital precession nor a very large mass of the primary SMBH.","lang":"eng"}],"article_processing_charge":"No","page":"L84-L88","author":[{"first_name":"S","last_name":"Komossa","full_name":"Komossa, S"},{"last_name":"Grupe","first_name":"D","full_name":"Grupe, D"},{"full_name":"Kraus, A","first_name":"A","last_name":"Kraus"},{"full_name":"Gurwell, M A","first_name":"M A","last_name":"Gurwell"},{"first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","full_name":"Haiman, Zoltán"},{"full_name":"Liu, F K","first_name":"F K","last_name":"Liu"},{"first_name":"A","last_name":"Tchekhovskoy","full_name":"Tchekhovskoy, A"},{"full_name":"Gallo, L C","last_name":"Gallo","first_name":"L C"},{"full_name":"Berton, M","first_name":"M","last_name":"Berton"},{"full_name":"Blandford, R","first_name":"R","last_name":"Blandford"},{"first_name":"J L","last_name":"Gómez","full_name":"Gómez, J L"},{"first_name":"A G","last_name":"Gonzalez","full_name":"Gonzalez, A G"}],"main_file_link":[{"url":"https://doi.org/10.1093/mnrasl/slad016","open_access":"1"}],"volume":522,"month":"02","publisher":"Oxford University Press","year":"2023","fulldoi":"https://doi.org/10.1093/mnrasl/slad016","date_updated":"2024-09-24T07:22:28Z","publication_identifier":{"issn":["1745-3925","1745-3933"]},"status":"public","publication_status":"published","publication":"Monthly Notices of the Royal Astronomical Society: Letters","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","title":"Absence of the predicted 2022 October outburst of OJ 287 and implications for binary SMBH scenarios","oa_version":"Published Version","date_published":"2023-02-23T00:00:00Z","quality_controlled":"1","type":"journal_article","article_type":"original","day":"23","scopus_import":"1","date_created":"2024-09-05T13:23:29Z","citation":{"ama":"Komossa S, Grupe D, Kraus A, et al. Absence of the predicted 2022 October outburst of OJ 287 and implications for binary SMBH scenarios. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2023;522(1):L84-L88. doi:<a href=\"https://doi.org/10.1093/mnrasl/slad016\">10.1093/mnrasl/slad016</a>","chicago":"Komossa, S, D Grupe, A Kraus, M A Gurwell, Zoltán Haiman, F K Liu, A Tchekhovskoy, et al. “Absence of the Predicted 2022 October Outburst of OJ 287 and Implications for Binary SMBH Scenarios.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2023. <a href=\"https://doi.org/10.1093/mnrasl/slad016\">https://doi.org/10.1093/mnrasl/slad016</a>.","mla":"Komossa, S., et al. “Absence of the Predicted 2022 October Outburst of OJ 287 and Implications for Binary SMBH Scenarios.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 522, no. 1, Oxford University Press, 2023, pp. L84–88, doi:<a href=\"https://doi.org/10.1093/mnrasl/slad016\">10.1093/mnrasl/slad016</a>.","short":"S. Komossa, D. Grupe, A. Kraus, M.A. Gurwell, Z. Haiman, F.K. Liu, A. Tchekhovskoy, L.C. Gallo, M. Berton, R. Blandford, J.L. Gómez, A.G. Gonzalez, Monthly Notices of the Royal Astronomical Society: Letters 522 (2023) L84–L88.","apa":"Komossa, S., Grupe, D., Kraus, A., Gurwell, M. A., Haiman, Z., Liu, F. K., … Gonzalez, A. G. (2023). Absence of the predicted 2022 October outburst of OJ 287 and implications for binary SMBH scenarios. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnrasl/slad016\">https://doi.org/10.1093/mnrasl/slad016</a>","ieee":"S. Komossa <i>et al.</i>, “Absence of the predicted 2022 October outburst of OJ 287 and implications for binary SMBH scenarios,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 522, no. 1. Oxford University Press, pp. L84–L88, 2023.","ista":"Komossa S, Grupe D, Kraus A, Gurwell MA, Haiman Z, Liu FK, Tchekhovskoy A, Gallo LC, Berton M, Blandford R, Gómez JL, Gonzalez AG. 2023. Absence of the predicted 2022 October outburst of OJ 287 and implications for binary SMBH scenarios. Monthly Notices of the Royal Astronomical Society: Letters. 522(1), L84–L88."}},{"status":"public","publication":"Monthly Notices of the Royal Astronomical Society: Letters","publication_status":"published","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1745-3933"],"issn":["1745-3925"]},"quality_controlled":"1","date_published":"2018-09-01T00:00:00Z","oa_version":"Preprint","title":"Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement","article_type":"original","arxiv":1,"day":"01","date_created":"2022-07-14T12:49:47Z","scopus_import":"1","type":"journal_article","acknowledgement":"We thank the anonymous referee for their constructive comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Jarle Brinchmann, Rob Crain and David Sobral for discussions. We acknowledge the use of the TOPCAT software (Taylor 2013) for assisting in rapid exploration of multidimensional data sets and the use of PYTHON and its NUMPY, MATPLOTLIB, and PANDAS packages.","citation":{"ama":"Matthee JJ, Schaye J. Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2018;479(1):L34-L39. doi:<a href=\"https://doi.org/10.1093/mnrasl/sly093\">10.1093/mnrasl/sly093</a>","mla":"Matthee, Jorryt J., and Joop Schaye. “Star-Forming Galaxies Are Predicted to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 479, no. 1, Oxford University Press, 2018, pp. L34–39, doi:<a href=\"https://doi.org/10.1093/mnrasl/sly093\">10.1093/mnrasl/sly093</a>.","chicago":"Matthee, Jorryt J, and Joop Schaye. “Star-Forming Galaxies Are Predicted to Lie on a Fundamental Plane of Mass, Star Formation Rate, and α-Enhancement.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnrasl/sly093\">https://doi.org/10.1093/mnrasl/sly093</a>.","apa":"Matthee, J. J., &#38; Schaye, J. (2018). Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnrasl/sly093\">https://doi.org/10.1093/mnrasl/sly093</a>","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society: Letters 479 (2018) L34–L39.","ista":"Matthee JJ, Schaye J. 2018. Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement. Monthly Notices of the Royal Astronomical Society: Letters. 479(1), L34–L39.","ieee":"J. J. Matthee and J. Schaye, “Star-forming galaxies are predicted to lie on a fundamental plane of mass, star formation rate, and α-enhancement,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 479, no. 1. Oxford University Press, pp. L34–L39, 2018."},"intvolume":"       479","oa":1,"external_id":{"arxiv":["1802.06786"]},"language":[{"iso":"eng"}],"_id":"11584","issue":"1","page":"L34 - L39","author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"last_name":"Schaye","first_name":"Joop","full_name":"Schaye, Joop"}],"abstract":[{"lang":"eng","text":"Observations show that star-forming galaxies reside on a tight 3D plane between mass, gas-phase metallicity, and star formation rate (SFR), which can be explained by the interplay between metal-poor gas inflows, SFR and outflows. However, different metals are released on different time-scales, which may affect the slope of this relation. Here, we use central, star-forming galaxies with Mstar = 109.0–10.5 M⊙ from the EAGLE hydrodynamical simulation to examine 3D relations between mass, SFR, and chemical enrichment using absolute and relative C, N, O, and Fe abundances. We show that the scatter is smaller when gas-phase α-enhancement is used rather than metallicity. A similar plane also exists for stellar α-enhancement, implying that present-day specific SFRs are correlated with long time-scale star formation histories. Between z = 0 and 1, the α-enhancement plane is even more insensitive to redshift than the plane using metallicity. However, it evolves at z > 1 due to lagging iron yields. At fixed mass, galaxies with higher SFRs have star formation histories shifted towards late times, are more α-enhanced, and this α-enhancement increases with redshift as observed. These findings suggest that relations between physical properties inferred from observations may be affected by systematic variations in α-enhancements."}],"article_processing_charge":"No","extern":"1","doi":"10.1093/mnrasl/sly093","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: abundances","galaxies: evolution","galaxies: formation","galaxies: star formation"],"fulldoi":"https://doi.org/10.1093/mnrasl/sly093","volume":479,"publisher":"Oxford University Press","year":"2018","month":"09","main_file_link":[{"url":"https://arxiv.org/abs/1802.06786","open_access":"1"}],"date_updated":"2024-10-14T11:37:53Z"},{"quality_controlled":"1","date_published":"2016-04-14T00:00:00Z","title":"Formation of massive Population III galaxies through photoionization feedback: A possible explanation for CR 7","oa_version":"Published Version","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication":"Monthly Notices of the Royal Astronomical Society: Letters","publication_status":"published","status":"public","publication_identifier":{"issn":["1745-3925","1745-3933"]},"citation":{"mla":"Visbal, Eli, et al. “Formation of Massive Population III Galaxies through Photoionization Feedback: A Possible Explanation for CR 7.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 460, no. 1, Oxford University Press, 2016, pp. L59–63, doi:<a href=\"https://doi.org/10.1093/mnrasl/slw071\">10.1093/mnrasl/slw071</a>.","chicago":"Visbal, Eli, Zoltán Haiman, and Greg L. Bryan. “Formation of Massive Population III Galaxies through Photoionization Feedback: A Possible Explanation for CR 7.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2016. <a href=\"https://doi.org/10.1093/mnrasl/slw071\">https://doi.org/10.1093/mnrasl/slw071</a>.","ama":"Visbal E, Haiman Z, Bryan GL. Formation of massive Population III galaxies through photoionization feedback: A possible explanation for CR 7. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2016;460(1):L59-L63. doi:<a href=\"https://doi.org/10.1093/mnrasl/slw071\">10.1093/mnrasl/slw071</a>","ista":"Visbal E, Haiman Z, Bryan GL. 2016. Formation of massive Population III galaxies through photoionization feedback: A possible explanation for CR 7. Monthly Notices of the Royal Astronomical Society: Letters. 460(1), L59–L63.","ieee":"E. Visbal, Z. Haiman, and G. L. Bryan, “Formation of massive Population III galaxies through photoionization feedback: A possible explanation for CR 7,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 460, no. 1. Oxford University Press, pp. L59–L63, 2016.","apa":"Visbal, E., Haiman, Z., &#38; Bryan, G. L. (2016). Formation of massive Population III galaxies through photoionization feedback: A possible explanation for CR 7. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnrasl/slw071\">https://doi.org/10.1093/mnrasl/slw071</a>","short":"E. Visbal, Z. Haiman, G.L. Bryan, Monthly Notices of the Royal Astronomical Society: Letters 460 (2016) L59–L63."},"date_created":"2024-09-06T07:32:23Z","day":"14","scopus_import":"1","article_type":"original","type":"journal_article","author":[{"first_name":"Eli","last_name":"Visbal","full_name":"Visbal, Eli"},{"full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"},{"full_name":"Bryan, Greg L.","first_name":"Greg L.","last_name":"Bryan"}],"page":"L59-L63","article_processing_charge":"No","abstract":[{"lang":"eng","text":"We explore the formation of massive high-redshift Population III (Pop III) galaxies through photoionization feedback. We consider dark matter haloes formed from progenitors that have undergone no star formation as a result of early reionization and photoevaporation caused by a nearby galaxy. Once such a halo reaches ≈109 M⊙, corresponding to the Jeans mass of the photoheated intergalactic medium at z ≈ 7, pristine gas is able to collapse into the halo, potentially producing a massive Pop III starburst. We suggest that this scenario may explain the recent observation of strong He ii 1640 Å line emission in CR 7, which is consistent with ∼107 M⊙ of young Pop III stars. Such a large mass of Pop III stars is unlikely without the photoionization feedback scenario, because star formation is expected to inject metals into haloes above the atomic cooling threshold (∼108 M⊙ at z ≈ 7). We use merger trees to analytically estimate the abundance of observable Pop III galaxies formed through this channel, and find a number density of ≈10−7 Mpc−3 at z = 6.6 (the redshift of CR 7). This is approximately a factor of 10 lower than the density of Ly α emitters as bright as CR 7."}],"extern":"1","doi":"10.1093/mnrasl/slw071","intvolume":"       460","oa":1,"language":[{"iso":"eng"}],"_id":"17654","issue":"1","date_updated":"2024-09-24T14:19:51Z","fulldoi":"https://doi.org/10.1093/mnrasl/slw071","year":"2016","month":"04","publisher":"Oxford University Press","volume":460,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnrasl/slw071"}]},{"author":[{"full_name":"Charisi, M.","last_name":"Charisi","first_name":"M."},{"full_name":"Bartos, I.","last_name":"Bartos","first_name":"I."},{"first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","full_name":"Haiman, Zoltán"},{"first_name":"A. M.","last_name":"Price-Whelan","full_name":"Price-Whelan, A. M."},{"first_name":"S.","last_name":"Márka","full_name":"Márka, S."}],"page":"L21-L25","extern":"1","doi":"10.1093/mnrasl/slv111","article_processing_charge":"No","abstract":[{"lang":"eng","text":"Graham et al. discovered a supermassive black hole binary (SMBHB) candidate and identified the detected 5.2 yr period of the optical variability as the orbital period of the binary. Hydrodynamical simulations predict multiple periodic components for the variability of SMBHBs, thus raising the possibility that the true period of the binary is different from 5.2 yr. We analyse the periodogram of PG1302 and find no compelling evidence for additional peaks. We also point out that, despite the 5.2 yr peak being significant if a single source is considered, further analysis is required to account for the fact that PG1302 was selected among a large sample of 247 000 quasars. We derive upper limits on any additional periodic modulations in the available data, by modelling the light curve as the sum of stochastic noise and the known 5.2 yr periodic component, and injecting additional sinusoidal signals. We find that, with the current data, we would be able to detect with high significance (false alarm probability <1 per cent) secondary periodic terms, with periods in the range predicted by the simulations, if the amplitude of the variability was at least ∼0.06 mag (compared to 0.14 mag for the main sinusoid). A three-year follow-up monitoring campaign with weekly observations can increase the sensitivity for detecting secondary peaks by ≈50 per cent, and would allow a more robust test of predictions from hydrodynamical simulations."}],"language":[{"iso":"eng"}],"intvolume":"       454","oa":1,"_id":"17622","issue":"1","date_updated":"2024-09-24T08:34:12Z","year":"2015","publisher":"Oxford University Press","month":"09","volume":454,"fulldoi":"https://doi.org/10.1093/mnrasl/slv111","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnrasl/slv111"}],"quality_controlled":"1","oa_version":"Published Version","title":"Multiple periods in the variability of the supermassive black hole binary candidate quasar PG1302-102?","date_published":"2015-09-11T00:00:00Z","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication_status":"published","publication":"Monthly Notices of the Royal Astronomical Society: Letters","status":"public","publication_identifier":{"issn":["1745-3933","1745-3925"]},"citation":{"mla":"Charisi, M., et al. “Multiple Periods in the Variability of the Supermassive Black Hole Binary Candidate Quasar PG1302-102?” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 454, no. 1, Oxford University Press, 2015, pp. L21–25, doi:<a href=\"https://doi.org/10.1093/mnrasl/slv111\">10.1093/mnrasl/slv111</a>.","chicago":"Charisi, M., I. Bartos, Zoltán Haiman, A. M. Price-Whelan, and S. Márka. “Multiple Periods in the Variability of the Supermassive Black Hole Binary Candidate Quasar PG1302-102?” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2015. <a href=\"https://doi.org/10.1093/mnrasl/slv111\">https://doi.org/10.1093/mnrasl/slv111</a>.","ama":"Charisi M, Bartos I, Haiman Z, Price-Whelan AM, Márka S. Multiple periods in the variability of the supermassive black hole binary candidate quasar PG1302-102? <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2015;454(1):L21-L25. doi:<a href=\"https://doi.org/10.1093/mnrasl/slv111\">10.1093/mnrasl/slv111</a>","ista":"Charisi M, Bartos I, Haiman Z, Price-Whelan AM, Márka S. 2015. Multiple periods in the variability of the supermassive black hole binary candidate quasar PG1302-102? Monthly Notices of the Royal Astronomical Society: Letters. 454(1), L21–L25.","ieee":"M. Charisi, I. Bartos, Z. Haiman, A. M. Price-Whelan, and S. Márka, “Multiple periods in the variability of the supermassive black hole binary candidate quasar PG1302-102?,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 454, no. 1. Oxford University Press, pp. L21–L25, 2015.","apa":"Charisi, M., Bartos, I., Haiman, Z., Price-Whelan, A. M., &#38; Márka, S. (2015). Multiple periods in the variability of the supermassive black hole binary candidate quasar PG1302-102? <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnrasl/slv111\">https://doi.org/10.1093/mnrasl/slv111</a>","short":"M. Charisi, I. Bartos, Z. Haiman, A.M. Price-Whelan, S. Márka, Monthly Notices of the Royal Astronomical Society: Letters 454 (2015) L21–L25."},"date_created":"2024-09-05T13:51:39Z","day":"11","scopus_import":"1","article_type":"original","type":"journal_article"},{"page":"L80-L84","author":[{"full_name":"Farris, Brian D.","first_name":"Brian D.","last_name":"Farris"},{"full_name":"Duffell, Paul","first_name":"Paul","last_name":"Duffell"},{"last_name":"MacFadyen","first_name":"Andrew I.","full_name":"MacFadyen, Andrew I."},{"full_name":"Haiman, Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán"}],"extern":"1","doi":"10.1093/mnrasl/slu184","abstract":[{"lang":"eng","text":"We present the results of 2D, moving mesh, viscous hydrodynamical simulations of accretion on to merging supermassive black hole (SMBH) binaries. We include viscous heating, shock heating, and radiative cooling, and simulate the transition from the ‘pre-decoupling’ epoch, where the inspiral time-scale is longer than the viscous time-scale, to the ‘post-decoupling’ epoch, where the inspiral time-scale is shorter than the viscous time-scale. We find that there is no abrupt halt to the accretion at decoupling, but rather the accretion shows a slow decay, with significant accretion well after the expected decoupling. Moreover, we find that the luminosity in X-rays is significantly higher prior to the merger, as orbital energy from the SMBH binary is converted to heat via strong shocks inside the cavity, and radiated away. Following the merger, the cavity refills viscously and the accretion rate relaxes to the Shakura–Sunyaev value, while the X-ray luminosity drops as the shocks quickly dissipate."}],"article_processing_charge":"No","external_id":{"arxiv":["1409.5124"]},"language":[{"iso":"eng"}],"intvolume":"       447","oa":1,"_id":"17625","issue":"1","date_updated":"2024-09-24T08:50:47Z","volume":447,"year":"2014","month":"12","publisher":"Oxford University Press","fulldoi":"https://doi.org/10.1093/mnrasl/slu184","main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.1409.5124"}],"quality_controlled":"1","title":"Binary black hole accretion during inspiral and merger","oa_version":"Preprint","date_published":"2014-12-19T00:00:00Z","status":"public","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication":"Monthly Notices of the Royal Astronomical Society: Letters","publication_status":"published","publication_identifier":{"issn":["1745-3933","1745-3925"]},"citation":{"apa":"Farris, B. D., Duffell, P., MacFadyen, A. I., &#38; Haiman, Z. (2014). Binary black hole accretion during inspiral and merger. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnrasl/slu184\">https://doi.org/10.1093/mnrasl/slu184</a>","short":"B.D. Farris, P. Duffell, A.I. MacFadyen, Z. Haiman, Monthly Notices of the Royal Astronomical Society: Letters 447 (2014) L80–L84.","ista":"Farris BD, Duffell P, MacFadyen AI, Haiman Z. 2014. Binary black hole accretion during inspiral and merger. Monthly Notices of the Royal Astronomical Society: Letters. 447(1), L80–L84.","ieee":"B. D. Farris, P. Duffell, A. I. MacFadyen, and Z. Haiman, “Binary black hole accretion during inspiral and merger,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 447, no. 1. Oxford University Press, pp. L80–L84, 2014.","ama":"Farris BD, Duffell P, MacFadyen AI, Haiman Z. Binary black hole accretion during inspiral and merger. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2014;447(1):L80-L84. doi:<a href=\"https://doi.org/10.1093/mnrasl/slu184\">10.1093/mnrasl/slu184</a>","mla":"Farris, Brian D., et al. “Binary Black Hole Accretion during Inspiral and Merger.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 447, no. 1, Oxford University Press, 2014, pp. L80–84, doi:<a href=\"https://doi.org/10.1093/mnrasl/slu184\">10.1093/mnrasl/slu184</a>.","chicago":"Farris, Brian D., Paul Duffell, Andrew I. MacFadyen, and Zoltán Haiman. “Binary Black Hole Accretion during Inspiral and Merger.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnrasl/slu184\">https://doi.org/10.1093/mnrasl/slu184</a>."},"article_type":"original","arxiv":1,"scopus_import":"1","day":"19","date_created":"2024-09-05T13:54:34Z","type":"journal_article"},{"status":"public","publication_status":"published","publication":"Monthly Notices of the Royal Astronomical Society: Letters","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication_identifier":{"issn":["1745-3933","1745-3925"]},"quality_controlled":"1","date_published":"2014-06-10T00:00:00Z","title":"A no-go theorem for direct collapse black holes without a strong ultraviolet background","oa_version":"Published Version","article_type":"original","scopus_import":"1","date_created":"2024-09-06T07:22:36Z","day":"10","type":"journal_article","citation":{"ieee":"E. Visbal, Z. Haiman, and G. L. Bryan, “A no-go theorem for direct collapse black holes without a strong ultraviolet background,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 442, no. 1. Oxford University Press, pp. L100–L104, 2014.","ista":"Visbal E, Haiman Z, Bryan GL. 2014. A no-go theorem for direct collapse black holes without a strong ultraviolet background. Monthly Notices of the Royal Astronomical Society: Letters. 442(1), L100–L104.","short":"E. Visbal, Z. Haiman, G.L. Bryan, Monthly Notices of the Royal Astronomical Society: Letters 442 (2014) L100–L104.","apa":"Visbal, E., Haiman, Z., &#38; Bryan, G. L. (2014). A no-go theorem for direct collapse black holes without a strong ultraviolet background. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnrasl/slu063\">https://doi.org/10.1093/mnrasl/slu063</a>","chicago":"Visbal, Eli, Zoltán Haiman, and Greg L. Bryan. “A No-Go Theorem for Direct Collapse Black Holes without a Strong Ultraviolet Background.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnrasl/slu063\">https://doi.org/10.1093/mnrasl/slu063</a>.","mla":"Visbal, Eli, et al. “A No-Go Theorem for Direct Collapse Black Holes without a Strong Ultraviolet Background.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 442, no. 1, Oxford University Press, 2014, pp. L100–04, doi:<a href=\"https://doi.org/10.1093/mnrasl/slu063\">10.1093/mnrasl/slu063</a>.","ama":"Visbal E, Haiman Z, Bryan GL. A no-go theorem for direct collapse black holes without a strong ultraviolet background. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2014;442(1):L100-L104. doi:<a href=\"https://doi.org/10.1093/mnrasl/slu063\">10.1093/mnrasl/slu063</a>"},"intvolume":"       442","oa":1,"language":[{"iso":"eng"}],"_id":"17643","issue":"1","page":"L100-L104","author":[{"full_name":"Visbal, Eli","first_name":"Eli","last_name":"Visbal"},{"last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","full_name":"Haiman, Zoltán"},{"full_name":"Bryan, Greg L.","last_name":"Bryan","first_name":"Greg L."}],"abstract":[{"text":"Explaining the existence of supermassive black holes (SMBHs) larger than ∼10^9M⊙ at redshifts z>∼6 remains an open theoretical question. One possibility is that gas collapsing rapidly in pristine atomic cooling halos (Tvir>∼10^4K) produces 10^4−10^6M⊙ black holes. Previous studies have shown that the formation of such a black hole requires a strong UV background to prevent molecular hydrogen cooling and gas fragmentation. Recently it has been proposed that a high UV background may not be required for halos that accrete material extremely rapidly or for halos where gas cooling is delayed due to a high baryon-dark matter streaming velocity. In this work, we point out that building up a halo with Tvir>∼104K before molecular cooling becomes efficient is not sufficient for forming a direct collapse black hole (DCBH). Though molecular hydrogen formation may be delayed, it will eventually form at high densities leading to efficient cooling and fragmentation. The only obvious way that molecular cooling could be avoided in the absence of strong UV radiation, is for gas to reach high enough density to cause collisional dissociation of molecular hydrogen (∼10^4 cm^−3) before cooling occurs. However, we argue that the minimum core entropy, set by the entropy of the intergalactic medium (IGM) when it decouples from the CMB, prevents this from occurring for realistic halo masses. This is confirmed by hydrodynamical cosmological simulations without radiative cooling. We explain the maximum density versus halo mass in these simulations with simple entropy arguments. The low densities found suggest that DCBH formation indeed requires a strong UV background.","lang":"eng"}],"article_processing_charge":"No","extern":"1","doi":"10.1093/mnrasl/slu063","fulldoi":"https://doi.org/10.1093/mnrasl/slu063","volume":442,"year":"2014","month":"06","publisher":"Oxford University Press","main_file_link":[{"url":"https://doi.org/10.1093/mnrasl/slu063","open_access":"1"}],"date_updated":"2024-09-24T12:04:03Z"},{"quality_controlled":"1","title":"Characteristic signatures in the thermal emission from accreting binary black holes","oa_version":"Published Version","date_published":"2014-11-10T00:00:00Z","publication":"Monthly Notices of the Royal Astronomical Society: Letters","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication_status":"published","status":"public","publication_identifier":{"issn":["1745-3933","1745-3925"]},"citation":{"ama":"Farris BD, Duffell P, MacFadyen AI, Haiman Z. Characteristic signatures in the thermal emission from accreting binary black holes. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2014;446(1):L36-L40. doi:<a href=\"https://doi.org/10.1093/mnrasl/slu160\">10.1093/mnrasl/slu160</a>","mla":"Farris, Brian D., et al. “Characteristic Signatures in the Thermal Emission from Accreting Binary Black Holes.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 446, no. 1, Oxford University Press, 2014, pp. L36–40, doi:<a href=\"https://doi.org/10.1093/mnrasl/slu160\">10.1093/mnrasl/slu160</a>.","chicago":"Farris, Brian D., Paul Duffell, Andrew I. MacFadyen, and Zoltán Haiman. “Characteristic Signatures in the Thermal Emission from Accreting Binary Black Holes.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnrasl/slu160\">https://doi.org/10.1093/mnrasl/slu160</a>.","apa":"Farris, B. D., Duffell, P., MacFadyen, A. I., &#38; Haiman, Z. (2014). Characteristic signatures in the thermal emission from accreting binary black holes. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnrasl/slu160\">https://doi.org/10.1093/mnrasl/slu160</a>","short":"B.D. Farris, P. Duffell, A.I. MacFadyen, Z. Haiman, Monthly Notices of the Royal Astronomical Society: Letters 446 (2014) L36–L40.","ista":"Farris BD, Duffell P, MacFadyen AI, Haiman Z. 2014. Characteristic signatures in the thermal emission from accreting binary black holes. Monthly Notices of the Royal Astronomical Society: Letters. 446(1), L36–L40.","ieee":"B. D. Farris, P. Duffell, A. I. MacFadyen, and Z. Haiman, “Characteristic signatures in the thermal emission from accreting binary black holes,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 446, no. 1. Oxford University Press, pp. L36–L40, 2014."},"date_created":"2024-09-06T07:23:36Z","day":"10","scopus_import":"1","article_type":"original","type":"journal_article","author":[{"first_name":"Brian D.","last_name":"Farris","full_name":"Farris, Brian D."},{"first_name":"Paul","last_name":"Duffell","full_name":"Duffell, Paul"},{"last_name":"MacFadyen","first_name":"Andrew I.","full_name":"MacFadyen, Andrew I."},{"full_name":"Haiman, Zoltán","last_name":"Haiman","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"}],"page":"L36-L40","doi":"10.1093/mnrasl/slu160","extern":"1","article_processing_charge":"No","abstract":[{"lang":"eng","text":"We present the results of a calculation of the thermal spectrum from a 2D, moving mesh, high-accuracy, viscous hydrodynamical simulation of an accreting supermassive black hole (SMBHs) binary. We include viscous heating, shock heating, and radiative cooling, evolving for longer than a viscous time so that we reach a quasi-steady accretion state. In agreement with previous work, we find that gas is efficiently stripped from the inner edge of the circumbinary disc and enters the cavity along accretion streams, which feed persistent ‘minidiscs’ surrounding each black hole. We also find that emission from the shock-heated minidiscs and accretion streams prevents any deficit in high-energy emission that may be expected inside the circumbinary cavity, and instead leads to a characteristic brightening of the spectrum beginning in soft X-rays."}],"language":[{"iso":"eng"}],"oa":1,"intvolume":"       446","_id":"17644","issue":"1","date_updated":"2024-09-24T12:07:00Z","year":"2014","publisher":"Oxford University Press","month":"11","volume":446,"fulldoi":"https://doi.org/10.1093/mnrasl/slu160","main_file_link":[{"url":"https://doi.org/10.1093/mnrasl/slu160","open_access":"1"}]},{"date_created":"2024-09-06T08:15:56Z","day":"02","scopus_import":"1","article_type":"original","type":"journal_article","citation":{"chicago":"Generozov, Aleksey, and Zoltán Haiman. “Lyman Edges in Supermassive Black Hole Binaries.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnrasl/slu075\">https://doi.org/10.1093/mnrasl/slu075</a>.","mla":"Generozov, Aleksey, and Zoltán Haiman. “Lyman Edges in Supermassive Black Hole Binaries.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 443, no. 1, Oxford University Press, 2014, pp. L64–68, doi:<a href=\"https://doi.org/10.1093/mnrasl/slu075\">10.1093/mnrasl/slu075</a>.","ama":"Generozov A, Haiman Z. Lyman edges in supermassive black hole binaries. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2014;443(1):L64-L68. doi:<a href=\"https://doi.org/10.1093/mnrasl/slu075\">10.1093/mnrasl/slu075</a>","ieee":"A. Generozov and Z. Haiman, “Lyman edges in supermassive black hole binaries,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 443, no. 1. Oxford University Press, pp. L64–L68, 2014.","ista":"Generozov A, Haiman Z. 2014. Lyman edges in supermassive black hole binaries. Monthly Notices of the Royal Astronomical Society: Letters. 443(1), L64–L68.","short":"A. Generozov, Z. Haiman, Monthly Notices of the Royal Astronomical Society: Letters 443 (2014) L64–L68.","apa":"Generozov, A., &#38; Haiman, Z. (2014). Lyman edges in supermassive black hole binaries. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnrasl/slu075\">https://doi.org/10.1093/mnrasl/slu075</a>"},"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication_status":"published","publication":"Monthly Notices of the Royal Astronomical Society: Letters","status":"public","publication_identifier":{"issn":["1745-3933","1745-3925"]},"quality_controlled":"1","date_published":"2014-07-02T00:00:00Z","title":"Lyman edges in supermassive black hole binaries","oa_version":"Published Version","fulldoi":"https://doi.org/10.1093/mnrasl/slu075","year":"2014","month":"07","publisher":"Oxford University Press","volume":443,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnrasl/slu075"}],"date_updated":"2024-09-25T09:10:05Z","oa":1,"intvolume":"       443","language":[{"iso":"eng"}],"_id":"17682","issue":"1","author":[{"last_name":"Generozov","first_name":"Aleksey","full_name":"Generozov, Aleksey"},{"first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","full_name":"Haiman, Zoltán"}],"page":"L64-L68","article_processing_charge":"No","abstract":[{"lang":"eng","text":"We propose a new spectral signature for supermassive black hole binaries (SMBHBs) with circumbinary gas discs: a sharp drop in flux bluewards of the Lyman limit. A prominent edge is produced if the gas dominating the emission in the Lyman continuum region of the spectrum is sufficiently cold (T ≲ 20 000 K) to contain significant neutral hydrogen. Circumbinary discs may be in this regime if the binary torques open a central cavity in the disc and clear most of the hot gas from the inner region, and if any residual UV emission from the individual BHs is either dim or intermittent. We model the vertical structure and spectra of circumbinary discs using the radiative transfer code tlusty, and identify the range of BH masses and binary separations producing a Lyman edge. We find that compact supermassive (M ≳ 108 M⊙) binaries with orbital periods of ∼0.1–10 yr, whose gravitational waves are expected to be detectable by pulsar timing arrays, could have prominent Lyman edges. Such strong spectral edge features are not typically present in AGN spectra and could serve as corroborating evidence for the presence of an SMBHB."}],"doi":"10.1093/mnrasl/slu075","extern":"1"},{"_id":"17692","issue":"1","oa":1,"intvolume":"       445","language":[{"iso":"eng"}],"abstract":[{"lang":"eng","text":"Quadrupole oscillation modes in stars can resonate with incident gravitational waves (GWs), and grow non-linear at the expense of GW energy. Stars near massive black hole binaries (MBHBs) can act as GW-charged batteries, discharging radiatively. Mass-loss from these stars can prompt MBHB accretion at near-Eddington rates. GW opacity is independent of amplitude, so distant resonating stars can eclipse GW sources. Absorption by the Sun of GWs from Galactic white dwarf binaries may be detectable with second-generation space-based GW detectors as a shadow within a complex diffraction pattern."}],"article_processing_charge":"No","extern":"1","doi":"10.1093/mnrasl/slu136","page":"L74-L78","author":[{"full_name":"McKernan, B.","first_name":"B.","last_name":"McKernan"},{"full_name":"Ford, K. E. S.","first_name":"K. E. S.","last_name":"Ford"},{"full_name":"Kocsis, B.","first_name":"B.","last_name":"Kocsis"},{"full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"}],"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnrasl/slu136"}],"fulldoi":"https://doi.org/10.1093/mnrasl/slu136","volume":445,"year":"2014","publisher":"Oxford University Press","month":"09","date_updated":"2024-09-25T09:58:34Z","publication_identifier":{"issn":["1745-3933","1745-3925"]},"status":"public","publication_status":"published","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication":"Monthly Notices of the Royal Astronomical Society: Letters","date_published":"2014-09-18T00:00:00Z","title":"Stars as resonant absorbers of gravitational waves","oa_version":"Published Version","quality_controlled":"1","type":"journal_article","article_type":"original","scopus_import":"1","day":"18","date_created":"2024-09-06T08:38:54Z","citation":{"ama":"McKernan B, Ford KES, Kocsis B, Haiman Z. Stars as resonant absorbers of gravitational waves. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2014;445(1):L74-L78. doi:<a href=\"https://doi.org/10.1093/mnrasl/slu136\">10.1093/mnrasl/slu136</a>","chicago":"McKernan, B., K. E. S. Ford, B. Kocsis, and Zoltán Haiman. “Stars as Resonant Absorbers of Gravitational Waves.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2014. <a href=\"https://doi.org/10.1093/mnrasl/slu136\">https://doi.org/10.1093/mnrasl/slu136</a>.","mla":"McKernan, B., et al. “Stars as Resonant Absorbers of Gravitational Waves.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 445, no. 1, Oxford University Press, 2014, pp. L74–78, doi:<a href=\"https://doi.org/10.1093/mnrasl/slu136\">10.1093/mnrasl/slu136</a>.","short":"B. McKernan, K.E.S. Ford, B. Kocsis, Z. Haiman, Monthly Notices of the Royal Astronomical Society: Letters 445 (2014) L74–L78.","apa":"McKernan, B., Ford, K. E. S., Kocsis, B., &#38; Haiman, Z. (2014). Stars as resonant absorbers of gravitational waves. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnrasl/slu136\">https://doi.org/10.1093/mnrasl/slu136</a>","ieee":"B. McKernan, K. E. S. Ford, B. Kocsis, and Z. Haiman, “Stars as resonant absorbers of gravitational waves,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 445, no. 1. Oxford University Press, pp. L74–L78, 2014.","ista":"McKernan B, Ford KES, Kocsis B, Haiman Z. 2014. Stars as resonant absorbers of gravitational waves. Monthly Notices of the Royal Astronomical Society: Letters. 445(1), L74–L78."}},{"citation":{"ista":"Pacucci F, Mesinger A, Haiman Z. 2013. Focusing on warm dark matter with lensed high-redshift galaxies. Monthly Notices of the Royal Astronomical Society: Letters. 435(1), L53–L57.","ieee":"F. Pacucci, A. Mesinger, and Z. Haiman, “Focusing on warm dark matter with lensed high-redshift galaxies,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 435, no. 1. Oxford University Press, pp. L53–L57, 2013.","apa":"Pacucci, F., Mesinger, A., &#38; Haiman, Z. (2013). Focusing on warm dark matter with lensed high-redshift galaxies. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnrasl/slt093\">https://doi.org/10.1093/mnrasl/slt093</a>","short":"F. Pacucci, A. Mesinger, Z. Haiman, Monthly Notices of the Royal Astronomical Society: Letters 435 (2013) L53–L57.","mla":"Pacucci, Fabio, et al. “Focusing on Warm Dark Matter with Lensed High-Redshift Galaxies.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 435, no. 1, Oxford University Press, 2013, pp. L53–57, doi:<a href=\"https://doi.org/10.1093/mnrasl/slt093\">10.1093/mnrasl/slt093</a>.","chicago":"Pacucci, Fabio, Andrei Mesinger, and Zoltán Haiman. “Focusing on Warm Dark Matter with Lensed High-Redshift Galaxies.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2013. <a href=\"https://doi.org/10.1093/mnrasl/slt093\">https://doi.org/10.1093/mnrasl/slt093</a>.","ama":"Pacucci F, Mesinger A, Haiman Z. Focusing on warm dark matter with lensed high-redshift galaxies. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2013;435(1):L53-L57. doi:<a href=\"https://doi.org/10.1093/mnrasl/slt093\">10.1093/mnrasl/slt093</a>"},"type":"journal_article","scopus_import":"1","date_created":"2024-09-05T14:00:29Z","day":"09","arxiv":1,"article_type":"original","oa_version":"Preprint","title":"Focusing on warm dark matter with lensed high-redshift galaxies","date_published":"2013-08-09T00:00:00Z","quality_controlled":"1","publication_identifier":{"issn":["1745-3933","1745-3925"]},"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication_status":"published","publication":"Monthly Notices of the Royal Astronomical Society: Letters","status":"public","date_updated":"2024-09-24T09:59:26Z","main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.1306.0009"}],"year":"2013","publisher":"Oxford University Press","month":"08","volume":435,"fulldoi":"https://doi.org/10.1093/mnrasl/slt093","extern":"1","doi":"10.1093/mnrasl/slt093","article_processing_charge":"No","abstract":[{"text":"We propose a novel use of high-redshift galaxies, discovered in deep Hubble Space Telescope (HST) fields around strong lensing clusters. These fields probe small comoving volumes (∼103 Mpc3) at high magnification (μ ≳ 10) and can detect otherwise inaccessible ultra-faint galaxies. Even a few galaxies found in such small volumes require a very high number density of collapsed dark matter (DM) haloes. This implies significant primordial power on small scales, allowing these observations to rule out popular alternatives to standard cold dark matter (CDM) models, such as warm dark matter (WDM). In this work, we analytically compute WDM halo mass functions at z = 10, including the effects of both particle free-streaming and residual velocity dispersion. We show that the two z ≈ 10 galaxies already detected by the Cluster Lensing And Supernova survey with Hubble (CLASH) survey are sufficient to constrain the WDM particle mass to mx > 1 (0.9) keV at 68 per cent (95 per cent) confidence limit (for a thermal relic relativistic at decoupling). This limit depends only on the WDM halo mass function and, unlike previous constraints on mx, is independent of any astrophysical modelling. The forthcoming HST Frontier Fields can significantly tighten these constraints.","lang":"eng"}],"author":[{"full_name":"Pacucci, Fabio","first_name":"Fabio","last_name":"Pacucci"},{"first_name":"Andrei","last_name":"Mesinger","full_name":"Mesinger, Andrei"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán"}],"page":"L53-L57","_id":"17631","issue":"1","language":[{"iso":"eng"}],"external_id":{"arxiv":["1306.0009"]},"intvolume":"       435","oa":1},{"language":[{"iso":"eng"}],"intvolume":"       425","oa":1,"_id":"17636","issue":"1","author":[{"last_name":"Wolcott-Green","first_name":"J.","full_name":"Wolcott-Green, J."},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán"}],"page":"L51-L55","extern":"1","doi":"10.1111/j.1745-3933.2012.01298.x","article_processing_charge":"No","abstract":[{"lang":"eng","text":"It is commonly believed that the earliest stages of star formation in the Universe were self-regulated by global radiation backgrounds - either by the ultraviolet (UV) Lyman-Werner (LW) photons emitted by the first stars (directly photodissociating H2), or by the X-rays produced by accretion on to the black hole (BH) remnants of these stars (heating the gas but catalysing H2 formation). Recent studies have suggested that a significant fraction of the first stars may have had low masses (a few M⊙). Such stars do not leave BH remnants and they have softer spectra, with copious infrared (IR) radiation at photon energies ∼1 eV. Similar to LW and X-ray photons, these photons have a mean-free path comparable to the Hubble distance, building up an early IR background. Here we show that if soft-spectrum stars, with masses of a few M⊙, contributed ≳0.3 per cent of the UV background (or their mass fraction exceeded ∼80 per cent), then their IR radiation dominated radiative feedback in the early Universe. The feedback is different from the UV feedback from high-mass stars, and occurs through the photodetachment of H− ions, necessary for efficient H2 formation. Nevertheless, we find that the baryon fraction which must be incorporated into low-mass stars in order to suppress H2 cooling is only a factor of a few higher than for high-mass stars."}],"publisher":"Oxford University Press","year":"2012","month":"09","volume":425,"fulldoi":"https://doi.org/10.1111/j.1745-3933.2012.01298.x","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1111/j.1745-3933.2012.01298.x"}],"date_updated":"2024-09-24T11:29:36Z","publication":"Monthly Notices of the Royal Astronomical Society: Letters","publication_status":"published","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","status":"public","publication_identifier":{"issn":["1745-3925","1745-3933"]},"quality_controlled":"1","title":"Feedback from the infrared background in the early universe","oa_version":"Published Version","date_published":"2012-09-01T00:00:00Z","day":"01","date_created":"2024-09-06T07:07:07Z","scopus_import":"1","article_type":"original","type":"journal_article","citation":{"short":"J. Wolcott-Green, Z. Haiman, Monthly Notices of the Royal Astronomical Society: Letters 425 (2012) L51–L55.","apa":"Wolcott-Green, J., &#38; Haiman, Z. (2012). Feedback from the infrared background in the early universe. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press. <a href=\"https://doi.org/10.1111/j.1745-3933.2012.01298.x\">https://doi.org/10.1111/j.1745-3933.2012.01298.x</a>","ieee":"J. Wolcott-Green and Z. Haiman, “Feedback from the infrared background in the early universe,” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 425, no. 1. Oxford University Press, pp. L51–L55, 2012.","ista":"Wolcott-Green J, Haiman Z. 2012. Feedback from the infrared background in the early universe. Monthly Notices of the Royal Astronomical Society: Letters. 425(1), L51–L55.","ama":"Wolcott-Green J, Haiman Z. Feedback from the infrared background in the early universe. <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. 2012;425(1):L51-L55. doi:<a href=\"https://doi.org/10.1111/j.1745-3933.2012.01298.x\">10.1111/j.1745-3933.2012.01298.x</a>","chicago":"Wolcott-Green, J., and Zoltán Haiman. “Feedback from the Infrared Background in the Early Universe.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>. Oxford University Press, 2012. <a href=\"https://doi.org/10.1111/j.1745-3933.2012.01298.x\">https://doi.org/10.1111/j.1745-3933.2012.01298.x</a>.","mla":"Wolcott-Green, J., and Zoltán Haiman. “Feedback from the Infrared Background in the Early Universe.” <i>Monthly Notices of the Royal Astronomical Society: Letters</i>, vol. 425, no. 1, Oxford University Press, 2012, pp. L51–55, doi:<a href=\"https://doi.org/10.1111/j.1745-3933.2012.01298.x\">10.1111/j.1745-3933.2012.01298.x</a>."}}]