[{"extern":"1","date_created":"2024-09-05T08:56:14Z","_id":"17516","page":"5593-5602","title":"κTNG: effect of baryonic processes on weak lensing with IllustrisTNG simulations","quality_controlled":"1","article_type":"original","author":[{"full_name":"Osato, Ken","last_name":"Osato","first_name":"Ken"},{"last_name":"Liu","full_name":"Liu, Jia","first_name":"Jia"},{"first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán"}],"publication_identifier":{"issn":["0035-8711","1365-2966"]},"publisher":"Oxford University Press","scopus_import":"1","day":"11","publication":"Monthly Notices of the Royal Astronomical Society","volume":502,"oa":1,"intvolume":" 502","year":"2021","language":[{"iso":"eng"}],"status":"public","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stab395"}],"doi":"10.1093/mnras/stab395","date_published":"2021-02-11T00:00:00Z","citation":{"apa":"Osato, K., Liu, J., & Haiman, Z. (2021). κTNG: effect of baryonic processes on weak lensing with IllustrisTNG simulations. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab395","mla":"Osato, Ken, et al. “ΚTNG: Effect of Baryonic Processes on Weak Lensing with IllustrisTNG Simulations.” Monthly Notices of the Royal Astronomical Society, vol. 502, no. 4, Oxford University Press, 2021, pp. 5593–602, doi:10.1093/mnras/stab395.","ama":"Osato K, Liu J, Haiman Z. κTNG: effect of baryonic processes on weak lensing with IllustrisTNG simulations. Monthly Notices of the Royal Astronomical Society. 2021;502(4):5593-5602. doi:10.1093/mnras/stab395","chicago":"Osato, Ken, Jia Liu, and Zoltán Haiman. “ΚTNG: Effect of Baryonic Processes on Weak Lensing with IllustrisTNG Simulations.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab395.","ista":"Osato K, Liu J, Haiman Z. 2021. κTNG: effect of baryonic processes on weak lensing with IllustrisTNG simulations. Monthly Notices of the Royal Astronomical Society. 502(4), 5593–5602.","ieee":"K. Osato, J. Liu, and Z. Haiman, “κTNG: effect of baryonic processes on weak lensing with IllustrisTNG simulations,” Monthly Notices of the Royal Astronomical Society, vol. 502, no. 4. Oxford University Press, pp. 5593–5602, 2021.","short":"K. Osato, J. Liu, Z. Haiman, Monthly Notices of the Royal Astronomical Society 502 (2021) 5593–5602."},"oa_version":"Published Version","type":"journal_article","month":"02","abstract":[{"text":"We study the effect of baryonic processes on weak lensing (WL) observables with a suite of mock WL maps, the κTNG, based on the cosmological hydrodynamic simulations IllustrisTNG. We quantify the baryonic effects on the WL angular power spectrum, one-point probability distribution function (PDF), and number counts of peaks and minima. We also show the redshift evolution of the effects, which is a key to distinguish the effect of baryons from fundamental physics such as dark energy, dark matter, and massive neutrinos. We find that baryonic processes reduce the small-scale power, suppress the tails of the PDF, peak and minimum counts, and change the total number of peaks and minima. We compare our results to existing semi-analytical models and hydrodynamic simulations, and discuss the source of discrepancies. The κTNG suite includes 10 000 realizations of $5 \\times 5 \\, \\mathrm{deg}^2$ maps for 40 source redshifts up to zs = 2.6, well covering the range of interest for existing and upcoming WL surveys. We also produce the κTNG-Dark suite of maps, generated based on the corresponding dark matter-only IllustrisTNG simulations. Our mock maps are not only suitable for developing analytical models that incorporate the effect of baryons, but also particularly useful for studies that rely on mass maps, such as non-Gaussian statistics and machine learning with convolutional neural networks. The suite of mock maps is publicly available at Columbia Lensing (http://columbialensing.org).","lang":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication_status":"published","issue":"4","date_updated":"2024-09-10T13:53:06Z","fulldoi":"https://doi.org/10.1093/mnras/stab395","article_processing_charge":"No"},{"scopus_import":"1","publication_identifier":{"issn":["0035-8711","1365-2966"]},"publisher":"Oxford University Press","author":[{"full_name":"Lu, Tianhuan","last_name":"Lu","first_name":"Tianhuan"},{"full_name":"Haiman, Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán"}],"article_type":"original","title":"The impact of baryons on cosmological inference from weak lensing statistics","quality_controlled":"1","extern":"1","_id":"17574","date_created":"2024-09-05T12:17:24Z","page":"3406-3417","language":[{"iso":"eng"}],"year":"2021","intvolume":" 506","oa":1,"volume":506,"publication":"Monthly Notices of the Royal Astronomical Society","day":"10","abstract":[{"text":"As weak lensing surveys are becoming deeper and cover larger areas, information will be available on small angular scales down to the arcmin level. To extract this extra information, accurate modelling of baryonic effects is necessary. In this work, we adopt a baryonic correction model, which includes gas both bound inside and ejected from dark matter (DM) haloes, a central galaxy, and changes in the DM profile induced by baryons. We use this model to incorporate baryons into a large suite of DM-only N-body simulations, covering a grid of 75 cosmologies in the Ωm–σ8 parameter space. We investigate how baryons affect Gaussian and non-Gaussian weak lensing statistics and the cosmological parameter inferences from these statistics. Our results show that marginalizing over baryonic parameters degrades the constraints in Ωm–σ8 space by a factor of 2–5 compared to those with baryonic parameters fixed. We also find that combining the lensing power spectrum and peak counts can break the degeneracy between cosmological and baryonic parameters and mitigate the impact of the uncertainty in baryonic physics.","lang":"eng"}],"month":"07","type":"journal_article","oa_version":"Published Version","citation":{"ieee":"T. Lu and Z. Haiman, “The impact of baryons on cosmological inference from weak lensing statistics,” Monthly Notices of the Royal Astronomical Society, vol. 506, no. 3. Oxford University Press, pp. 3406–3417, 2021.","short":"T. Lu, Z. Haiman, Monthly Notices of the Royal Astronomical Society 506 (2021) 3406–3417.","ista":"Lu T, Haiman Z. 2021. The impact of baryons on cosmological inference from weak lensing statistics. Monthly Notices of the Royal Astronomical Society. 506(3), 3406–3417.","ama":"Lu T, Haiman Z. The impact of baryons on cosmological inference from weak lensing statistics. Monthly Notices of the Royal Astronomical Society. 2021;506(3):3406-3417. doi:10.1093/mnras/stab1978","chicago":"Lu, Tianhuan, and Zoltán Haiman. “The Impact of Baryons on Cosmological Inference from Weak Lensing Statistics.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab1978.","apa":"Lu, T., & Haiman, Z. (2021). The impact of baryons on cosmological inference from weak lensing statistics. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab1978","mla":"Lu, Tianhuan, and Zoltán Haiman. “The Impact of Baryons on Cosmological Inference from Weak Lensing Statistics.” Monthly Notices of the Royal Astronomical Society, vol. 506, no. 3, Oxford University Press, 2021, pp. 3406–17, doi:10.1093/mnras/stab1978."},"date_published":"2021-07-10T00:00:00Z","doi":"10.1093/mnras/stab1978","status":"public","main_file_link":[{"url":"https://doi.org/10.1093/mnras/stab1978","open_access":"1"}],"article_processing_charge":"No","publication_status":"published","issue":"3","fulldoi":"https://doi.org/10.1093/mnras/stab1978","date_updated":"2024-09-19T07:43:16Z","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345"},{"doi":"10.1093/mnras/stab1856","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stab1856"}],"status":"public","citation":{"chicago":"Xin, Chengcheng, and Zoltán Haiman. “Ultra-Short-Period Massive Black Hole Binary Candidates in LSST as LISA ‘Verification Binaries.’” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab1856.","ama":"Xin C, Haiman Z. Ultra-short-period massive black hole binary candidates in LSST as LISA ‘verification binaries.’ Monthly Notices of the Royal Astronomical Society. 2021;506(2):2408-2417. doi:10.1093/mnras/stab1856","ista":"Xin C, Haiman Z. 2021. Ultra-short-period massive black hole binary candidates in LSST as LISA ‘verification binaries’. Monthly Notices of the Royal Astronomical Society. 506(2), 2408–2417.","ieee":"C. Xin and Z. Haiman, “Ultra-short-period massive black hole binary candidates in LSST as LISA ‘verification binaries,’” Monthly Notices of the Royal Astronomical Society, vol. 506, no. 2. Oxford University Press, pp. 2408–2417, 2021.","short":"C. Xin, Z. Haiman, Monthly Notices of the Royal Astronomical Society 506 (2021) 2408–2417.","apa":"Xin, C., & Haiman, Z. (2021). Ultra-short-period massive black hole binary candidates in LSST as LISA ‘verification binaries.’ Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab1856","mla":"Xin, Chengcheng, and Zoltán Haiman. “Ultra-Short-Period Massive Black Hole Binary Candidates in LSST as LISA ‘Verification Binaries.’” Monthly Notices of the Royal Astronomical Society, vol. 506, no. 2, Oxford University Press, 2021, pp. 2408–17, doi:10.1093/mnras/stab1856."},"date_published":"2021-07-05T00:00:00Z","type":"journal_article","oa_version":"Published Version","abstract":[{"lang":"eng","text":"The Legacy Survey of Space and Time (LSST) by the Vera C. Rubin Observatory is expected to discover tens of millions of quasars. A significant fraction of these could be powered by coalescing massive black hole (MBH) binaries, since many quasars are believed to be triggered by mergers. We show that under plausible assumptions about the luminosity functions, lifetimes, and binary fractions of quasars, we expect the full LSST quasar catalogue to contain between 20 and 100 million compact MBH binaries with masses M = 105–9M⊙, redshifts z = 0–6, and orbital periods P = 1–70 d. Their light-curves are expected to be distinctly periodic, which can be confidently distinguished from stochastic red-noise variability, because LSST will cover dozens, or even hundreds of cycles. A very small subset of 10–150 ultracompact (P ≲ 1 d) binary quasars among these will, over ∼5–15 yr, evolve into the mHz gravitational-wave frequency band and can be detected by LISA. They can therefore be regarded as ‘LISA verification binaries’, analogous to short-period Galactic compact-object binaries. The practical question is how to find these handful of ‘needles in the haystack’ among the large number of quasars: this will likely require a tailored co-adding analysis optimized for this purpose."}],"month":"07","date_updated":"2024-09-19T08:07:41Z","fulldoi":"https://doi.org/10.1093/mnras/stab1856","publication_status":"published","issue":"2","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_processing_charge":"No","_id":"17577","date_created":"2024-09-05T12:19:58Z","page":"2408-2417","extern":"1","author":[{"first_name":"Chengcheng","last_name":"Xin","full_name":"Xin, Chengcheng"},{"first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán"}],"article_type":"original","quality_controlled":"1","title":"Ultra-short-period massive black hole binary candidates in LSST as LISA ‘verification binaries’","scopus_import":"1","publisher":"Oxford University Press","publication_identifier":{"issn":["0035-8711","1365-2966"]},"day":"05","publication":"Monthly Notices of the Royal Astronomical Society","volume":506,"intvolume":" 506","oa":1,"language":[{"iso":"eng"}],"year":"2021"},{"date_updated":"2024-09-19T11:50:46Z","fulldoi":"https://doi.org/10.1093/mnras/stab2315","issue":"3","publication_status":"published","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_processing_charge":"No","doi":"10.1093/mnras/stab2315","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stab2315"}],"status":"public","citation":{"ieee":"H. Tagawa, Z. Haiman, I. Bartos, B. Kocsis, and K. Omukai, “Signatures of hierarchical mergers in black hole spin and mass distribution,” Monthly Notices of the Royal Astronomical Society, vol. 507, no. 3. Oxford University Press, pp. 3362–3380, 2021.","short":"H. Tagawa, Z. Haiman, I. Bartos, B. Kocsis, K. Omukai, Monthly Notices of the Royal Astronomical Society 507 (2021) 3362–3380.","chicago":"Tagawa, Hiromichi, Zoltán Haiman, Imre Bartos, Bence Kocsis, and Kazuyuki Omukai. “Signatures of Hierarchical Mergers in Black Hole Spin and Mass Distribution.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab2315.","ama":"Tagawa H, Haiman Z, Bartos I, Kocsis B, Omukai K. Signatures of hierarchical mergers in black hole spin and mass distribution. Monthly Notices of the Royal Astronomical Society. 2021;507(3):3362-3380. doi:10.1093/mnras/stab2315","ista":"Tagawa H, Haiman Z, Bartos I, Kocsis B, Omukai K. 2021. Signatures of hierarchical mergers in black hole spin and mass distribution. Monthly Notices of the Royal Astronomical Society. 507(3), 3362–3380.","mla":"Tagawa, Hiromichi, et al. “Signatures of Hierarchical Mergers in Black Hole Spin and Mass Distribution.” Monthly Notices of the Royal Astronomical Society, vol. 507, no. 3, Oxford University Press, 2021, pp. 3362–80, doi:10.1093/mnras/stab2315.","apa":"Tagawa, H., Haiman, Z., Bartos, I., Kocsis, B., & Omukai, K. (2021). Signatures of hierarchical mergers in black hole spin and mass distribution. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab2315"},"date_published":"2021-08-13T00:00:00Z","type":"journal_article","oa_version":"Published Version","abstract":[{"lang":"eng","text":"Recent gravitational wave (GW) observations by LIGO/Virgo show evidence for hierarchical mergers, where the merging BHs are the remnants of previous BH merger events. These events may carry important clues about the astrophysical host environments of the GW sources. In this paper, we present the distributions of the effective spin parameter (χeff), the precession spin parameter (χp), and the chirp mass (mchirp) expected in hierarchical mergers. Under a wide range of assumptions, hierarchical mergers produce (i) a monotonic increase of the average of the typical total spin for merging binaries, which we characterize with χ¯typ≡(χ2eff+χ2p)1/2¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯¯, up to roughly the maximum mchirp among first-generation (1g) BHs, and (ii) a plateau at χ¯typ∼0.6 at higher mchirp. We suggest that the maximum mass and typical spin magnitudes for 1g BHs can be estimated from χ¯typ as a function of mchirp. The GW data observed in LIGO/Virgo O1--O3a prefers an increase in χ¯typ at low mchirp, which is consistent with the growth of the BH spin magnitude by hierarchical mergers, at ∼2σ confidence. A Bayesian analysis suggests that 1g BHs have the maximum mass of ∼15--30M⊙ if the majority of mergers are of high-generation BHs (not among 1g-1g BHs), which is consistent with mergers in active galactic nucleus disks and/or nuclear star clusters, while if mergers mainly originate from globular clusters, 1g BHs are favored to have non-zero spin magnitudes of ∼0.3. We also forecast that signatures for hierarchical mergers in the χ¯typ distribution can be confidently recovered once the number of GW events increases to ≳O(100)."}],"month":"08","day":"13","publication":"Monthly Notices of the Royal Astronomical Society","volume":507,"intvolume":" 507","oa":1,"language":[{"iso":"eng"}],"year":"2021","page":"3362-3380","_id":"17585","date_created":"2024-09-05T12:30:08Z","extern":"1","author":[{"last_name":"Tagawa","full_name":"Tagawa, Hiromichi","first_name":"Hiromichi"},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán"},{"first_name":"Imre","last_name":"Bartos","full_name":"Bartos, Imre"},{"first_name":"Bence","last_name":"Kocsis","full_name":"Kocsis, Bence"},{"last_name":"Omukai","full_name":"Omukai, Kazuyuki","first_name":"Kazuyuki"}],"article_type":"original","quality_controlled":"1","title":"Signatures of hierarchical mergers in black hole spin and mass distribution","scopus_import":"1","publisher":"Oxford University Press","publication_identifier":{"issn":["0035-8711","1365-2966"]}},{"citation":{"mla":"Dotti, Massimo, et al. “Binary Black Hole Signatures in Polarized Light Curves.” Monthly Notices of the Royal Astronomical Society, vol. 509, no. 1, Oxford University Press, 2021, pp. 212–23, doi:10.1093/mnras/stab2893.","apa":"Dotti, M., Bonetti, M., D’Orazio, D. J., Haiman, Z., & Ho, L. C. (2021). Binary black hole signatures in polarized light curves. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab2893","ista":"Dotti M, Bonetti M, D’Orazio DJ, Haiman Z, Ho LC. 2021. Binary black hole signatures in polarized light curves. Monthly Notices of the Royal Astronomical Society. 509(1), 212–223.","ama":"Dotti M, Bonetti M, D’Orazio DJ, Haiman Z, Ho LC. Binary black hole signatures in polarized light curves. Monthly Notices of the Royal Astronomical Society. 2021;509(1):212-223. doi:10.1093/mnras/stab2893","chicago":"Dotti, Massimo, Matteo Bonetti, Daniel J D’Orazio, Zoltán Haiman, and Luis C Ho. “Binary Black Hole Signatures in Polarized Light Curves.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab2893.","ieee":"M. Dotti, M. Bonetti, D. J. D’Orazio, Z. Haiman, and L. C. Ho, “Binary black hole signatures in polarized light curves,” Monthly Notices of the Royal Astronomical Society, vol. 509, no. 1. Oxford University Press, pp. 212–223, 2021.","short":"M. Dotti, M. Bonetti, D.J. D’Orazio, Z. Haiman, L.C. Ho, Monthly Notices of the Royal Astronomical Society 509 (2021) 212–223."},"date_published":"2021-10-07T00:00:00Z","doi":"10.1093/mnras/stab2893","main_file_link":[{"url":"https://doi.org/10.1093/mnras/stab2893","open_access":"1"}],"status":"public","abstract":[{"lang":"eng","text":"Variable active galactic nuclei showing periodic light curves have been proposed as massive black hole binary (MBHB) candidates. In such scenarios, the periodicity can be due to relativistic Doppler-boosting of the emitted light. This hypothesis can be tested through the timing of scattered polarized light. Following the results of polarization studies in type I nuclei and of dynamical studies of MBHBs with circumbinary discs, we assume a coplanar equatorial scattering ring, whose elements contribute differently to the total polarized flux, due to different scattering angles, levels of Doppler boost, and line-of-sight time delays. We find that in the presence of an MBHB, both the degree of polarization and the polarization position angle have periodic modulations. The polarization angle oscillates around the semiminor axis of the projected MBHB orbital ellipse, with a frequency equal either to the binary’s orbital frequency (for large scattering screen radii), or twice this value (for smaller scattering structures). These distinctive features can be used to probe the nature of periodic MBHB candidates and to compile catalogues of the most promising sub-pc MBHBs. The identification of such polarization features in gravitational-wave (GW) detected MBHBs would enormously increase the amount of physical information about the sources, allowing the measurement of the individual masses of the binary components, and the orientation of the line of nodes on the sky, even for monochromatic GW signals."}],"month":"10","type":"journal_article","oa_version":"Published Version","date_updated":"2024-09-19T11:55:01Z","fulldoi":"https://doi.org/10.1093/mnras/stab2893","issue":"1","publication_status":"published","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","article_processing_charge":"No","date_created":"2024-09-05T12:32:01Z","_id":"17586","page":"212-223","extern":"1","scopus_import":"1","publisher":"Oxford University Press","publication_identifier":{"issn":["0035-8711","1365-2966"]},"article_type":"original","author":[{"full_name":"Dotti, Massimo","last_name":"Dotti","first_name":"Massimo"},{"last_name":"Bonetti","full_name":"Bonetti, Matteo","first_name":"Matteo"},{"first_name":"Daniel J","full_name":"D’Orazio, Daniel J","last_name":"D’Orazio"},{"last_name":"Haiman","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán"},{"last_name":"Ho","full_name":"Ho, Luis C","first_name":"Luis C"}],"quality_controlled":"1","title":"Binary black hole signatures in polarized light curves","volume":509,"publication":"Monthly Notices of the Royal Astronomical Society","day":"07","language":[{"iso":"eng"}],"year":"2021","intvolume":" 509","oa":1},{"extern":"1","page":"5046-5060","_id":"17610","date_created":"2024-09-05T13:22:23Z","publication_identifier":{"issn":["0035-8711","1365-2966"]},"publisher":"Oxford University Press","scopus_import":"1","title":"Forming massive seed black holes in high-redshift quasar host progenitors","quality_controlled":"1","article_type":"original","author":[{"full_name":"Lupi, Alessandro","last_name":"Lupi","first_name":"Alessandro"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"},{"last_name":"Volonteri","full_name":"Volonteri, Marta","first_name":"Marta"}],"publication":"Monthly Notices of the Royal Astronomical Society","volume":503,"day":"24","arxiv":1,"year":"2021","language":[{"iso":"eng"}],"oa":1,"intvolume":" 503","date_published":"2021-03-24T00:00:00Z","citation":{"ista":"Lupi A, Haiman Z, Volonteri M. 2021. Forming massive seed black holes in high-redshift quasar host progenitors. Monthly Notices of the Royal Astronomical Society. 503(4), 5046–5060.","ama":"Lupi A, Haiman Z, Volonteri M. Forming massive seed black holes in high-redshift quasar host progenitors. Monthly Notices of the Royal Astronomical Society. 2021;503(4):5046-5060. doi:10.1093/mnras/stab692","chicago":"Lupi, Alessandro, Zoltán Haiman, and Marta Volonteri. “Forming Massive Seed Black Holes in High-Redshift Quasar Host Progenitors.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2021. https://doi.org/10.1093/mnras/stab692.","short":"A. Lupi, Z. Haiman, M. Volonteri, Monthly Notices of the Royal Astronomical Society 503 (2021) 5046–5060.","ieee":"A. Lupi, Z. Haiman, and M. Volonteri, “Forming massive seed black holes in high-redshift quasar host progenitors,” Monthly Notices of the Royal Astronomical Society, vol. 503, no. 4. Oxford University Press, pp. 5046–5060, 2021.","mla":"Lupi, Alessandro, et al. “Forming Massive Seed Black Holes in High-Redshift Quasar Host Progenitors.” Monthly Notices of the Royal Astronomical Society, vol. 503, no. 4, Oxford University Press, 2021, pp. 5046–60, doi:10.1093/mnras/stab692.","apa":"Lupi, A., Haiman, Z., & Volonteri, M. (2021). Forming massive seed black holes in high-redshift quasar host progenitors. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stab692"},"status":"public","main_file_link":[{"url":" https://doi.org/10.48550/arXiv.2102.05051","open_access":"1"}],"doi":"10.1093/mnras/stab692","month":"03","abstract":[{"lang":"eng","text":"The presence of massive black holes (BHs) with masses of order 109M⊙, powering bright quasars when the Universe was less than 1 Gyr old, poses strong constraints on their formation mechanism. Several scenarios have been proposed to date to explain massive BH formation, from the low-mass seed BH remnants of the first generation of stars to the massive seed BHs resulting from the rapid collapse of massive gas clouds. However, the plausibility of some of these scenarios to occur within the progenitors of high-z quasars has not yet been thoroughly explored. In this work, we investigate, by combining dark-matter only N-body simulations with a semi-analytic framework, whether the conditions for the formation of massive seed BHs from synchronised atomic-cooling halo pairs and/or dynamically-heated mini-haloes are fulfilled in the overdense regions where the progenitors of a typical high-redshift quasar host form and evolve. Our analysis shows that the peculiar conditions in such regions, i.e. strong halo clustering and high star formation rates, are crucial to produce a non-negligible number of massive seed BH host candidates: we find ≈1400 dynamically heated metal-free mini-haloes, including one of these which evolves to a synchronised pair and ends up in the massive quasar-host halo by z=6. This demonstrates that the progenitors of high-redshift quasar host haloes can harbour early massive seed BHs. Our results further suggest that multiple massive seed BHs may form in or near the quasar host's progenitors, potentially merging at lower redshifts and yielding gravitational wave events."}],"oa_version":"Preprint","external_id":{"arxiv":["2102.05051"]},"type":"journal_article","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","issue":"4","publication_status":"published","date_updated":"2024-09-23T14:49:49Z","fulldoi":"https://doi.org/10.1093/mnras/stab692","article_processing_charge":"No"},{"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: haloes","galaxies: high-redshift","quasars: absorption lines"],"publication_status":"published","issue":"2","date_updated":"2022-08-18T11:00:24Z","fulldoi":"https://doi.org/10.1093/mnras/staa1347","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_processing_charge":"No","doi":"10.1093/mnras/staa1347","status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1910.03593"}],"citation":{"mla":"Muzahid, Sowgat, et al. “MUSEQuBES: Calibrating the Redshifts of Lyα Emitters Using Stacked Circumgalactic Medium Absorption Profiles.” Monthly Notices of the Royal Astronomical Society, vol. 496, no. 2, Oxford University Press, 2020, pp. 1013–22, doi:10.1093/mnras/staa1347.","apa":"Muzahid, S., Schaye, J., Marino, R. A., Cantalupo, S., Brinchmann, J., Contini, T., … Verhamme, A. (2020). MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa1347","ieee":"S. Muzahid et al., “MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles,” Monthly Notices of the Royal Astronomical Society, vol. 496, no. 2. Oxford University Press, pp. 1013–1022, 2020.","short":"S. Muzahid, J. Schaye, R.A. Marino, S. Cantalupo, J. Brinchmann, T. Contini, M. Wendt, L. Wisotzki, J. Zabl, N. Bouché, M. Akhlaghi, H.-W. Chen, A. Claeyssens, S. Johnson, F. Leclercq, M. Maseda, J.J. Matthee, J. Richard, T. Urrutia, A. Verhamme, Monthly Notices of the Royal Astronomical Society 496 (2020) 1013–1022.","ama":"Muzahid S, Schaye J, Marino RA, et al. MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles. Monthly Notices of the Royal Astronomical Society. 2020;496(2):1013-1022. doi:10.1093/mnras/staa1347","ista":"Muzahid S, Schaye J, Marino RA, Cantalupo S, Brinchmann J, Contini T, Wendt M, Wisotzki L, Zabl J, Bouché N, Akhlaghi M, Chen H-W, Claeyssens A, Johnson S, Leclercq F, Maseda M, Matthee JJ, Richard J, Urrutia T, Verhamme A. 2020. MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles. Monthly Notices of the Royal Astronomical Society. 496(2), 1013–1022.","chicago":"Muzahid, Sowgat, Joop Schaye, Raffaella Anna Marino, Sebastiano Cantalupo, Jarle Brinchmann, Thierry Contini, Martin Wendt, et al. “MUSEQuBES: Calibrating the Redshifts of Lyα Emitters Using Stacked Circumgalactic Medium Absorption Profiles.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa1347."},"date_published":"2020-08-01T00:00:00Z","external_id":{"arxiv":["1910.03593"]},"type":"journal_article","oa_version":"Preprint","abstract":[{"lang":"eng","text":"Ly α emission lines are typically found to be redshifted with respect to the systemic redshifts of galaxies, likely due to resonant scattering of Ly α photons. Here, we measure the average velocity offset for a sample of 96 z ≈ 3.3 Ly α emitters (LAEs) with a median Ly α flux (luminosity) of ≈10−17 erg cm−2 s−1 (≈1042 erg s−1) and a median star formation rate (SFR) of ≈1.3 M⊙ yr−1 (not corrected for possible dust extinction), detected by the Multi-Unit Spectroscopic Explorer as part of our MUSEQuBES circumgalactic medium (CGM) survey. By postulating that the stacked CGM absorption profiles of these LAEs, probed by eight background quasars, must be centred on the systemic redshift, we measure an average velocity offset, Voffset = 171\\pm 8 km s−1, between the Ly α emission peak and the systemic redshift. The observed Voffset is lower by factors of ≈1.4 and ≈2.6 compared to the velocity offsets measured for narrow-band-selected LAEs and Lyman break galaxies, respectively, which probe galaxies with higher masses and SFRs. Consistent with earlier studies based on direct measurements for individual objects, we find that the Voffset is correlated with the full width at half-maximum of the red peak of the Ly α line, and anticorrelated with the rest-frame equivalent width. Moreover, we find that Voffset is correlated with SFR with a sub-linear scaling relation, Voffset∝SFR0.16±0.03. Adopting the mass scaling for main-sequence galaxies, such a relation suggests that Voffset scales with the circular velocity of the dark matter haloes hosting the LAEs."}],"related_material":{"link":[{"relation":"erratum","url":"https://doi.org/10.1093/mnras/staa2668"}]},"month":"08","acknowledgement":"We thank the anonymous referee for useful suggestions. This study is based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme(s): 094.A-0131(B), 095.A 0200(A), 096.A0222(A), 097.A-0089(A), and 099.A-0159(A). SM acknowledges support from the Alexander von Humboldt Foundation, Germany. SM thanks Christian Herenz for useful discussion. SC gratefully acknowledges support from Swiss National Science Foundation grant PP00P2 163824. JB acknowledges support by FCT/MCTES through national funds by grant UID/FIS/04434/2019 and through Investigador FCT Contract No. IF/01654/2014/CP1215/CT0003. NB and JZ acknowledge support from ANR grant ANR-17-CE31- 0017 (3DGasFlows). AC and JR acknowledge support from the ERC starting grant 336736-CALENDS. MA acknowledges support from European Union’s H2020 Marie Skłodowska-Curie Actions grant 721463 to the SUNDIAL ITN, and from the Spanish Ministry of Economy and Competitiveness (MINECO) under grant number AYA2016-76219-P. MA also acknowledges support from the Fundacion BBVA under its 2017 programme of assistance to ´scientific research groups, for the project ‘Using machine-learning techniques to drag galaxies from the noise in deep imaging’. FL and AV acknowledge support from the ERC starting grant ERC757258-TRIPLE.","day":"01","arxiv":1,"publication":"Monthly Notices of the Royal Astronomical Society","volume":496,"intvolume":" 496","oa":1,"language":[{"iso":"eng"}],"year":"2020","extern":"1","date_created":"2022-07-07T10:20:11Z","_id":"11528","page":"1013-1022","article_type":"original","author":[{"first_name":"Sowgat","last_name":"Muzahid","full_name":"Muzahid, Sowgat"},{"first_name":"Joop","last_name":"Schaye","full_name":"Schaye, Joop"},{"full_name":"Marino, Raffaella Anna","last_name":"Marino","first_name":"Raffaella Anna"},{"full_name":"Cantalupo, Sebastiano","last_name":"Cantalupo","first_name":"Sebastiano"},{"full_name":"Brinchmann, Jarle","last_name":"Brinchmann","first_name":"Jarle"},{"first_name":"Thierry","full_name":"Contini, Thierry","last_name":"Contini"},{"first_name":"Martin","last_name":"Wendt","full_name":"Wendt, Martin"},{"first_name":"Lutz","last_name":"Wisotzki","full_name":"Wisotzki, Lutz"},{"last_name":"Zabl","full_name":"Zabl, Johannes","first_name":"Johannes"},{"first_name":"Nicolas","full_name":"Bouché, Nicolas","last_name":"Bouché"},{"first_name":"Mohammad","last_name":"Akhlaghi","full_name":"Akhlaghi, Mohammad"},{"full_name":"Chen, Hsiao-Wen","last_name":"Chen","first_name":"Hsiao-Wen"},{"first_name":"Adélaîde","last_name":"Claeyssens","full_name":"Claeyssens, Adélaîde"},{"first_name":"Sean","last_name":"Johnson","full_name":"Johnson, Sean"},{"last_name":"Leclercq","full_name":"Leclercq, Floriane","first_name":"Floriane"},{"last_name":"Maseda","full_name":"Maseda, Michael","first_name":"Michael"},{"last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"first_name":"Johan","full_name":"Richard, Johan","last_name":"Richard"},{"full_name":"Urrutia, Tanya","last_name":"Urrutia","first_name":"Tanya"},{"first_name":"Anne","full_name":"Verhamme, Anne","last_name":"Verhamme"}],"title":"MUSEQuBES: Calibrating the redshifts of Lyα emitters using stacked circumgalactic medium absorption profiles","quality_controlled":"1","scopus_import":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publisher":"Oxford University Press"},{"volume":498,"publication":"Monthly Notices of the Royal Astronomical Society","day":"01","arxiv":1,"language":[{"iso":"eng"}],"year":"2020","intvolume":" 498","oa":1,"_id":"11529","page":"3043-3059","date_created":"2022-07-07T10:36:01Z","extern":"1","scopus_import":"1","publisher":"Oxford University Press","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"author":[{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"first_name":"Gabriele","full_name":"Pezzulli, Gabriele","last_name":"Pezzulli"},{"last_name":"Mackenzie","full_name":"Mackenzie, Ruari","first_name":"Ruari"},{"full_name":"Cantalupo, Sebastiano","last_name":"Cantalupo","first_name":"Sebastiano"},{"last_name":"Kusakabe","full_name":"Kusakabe, Haruka","first_name":"Haruka"},{"last_name":"Leclercq","full_name":"Leclercq, Floriane","first_name":"Floriane"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"first_name":"Johan","last_name":"Richard","full_name":"Richard, Johan"},{"first_name":"Lutz","last_name":"Wisotzki","full_name":"Wisotzki, Lutz"},{"first_name":"Simon","full_name":"Lilly, Simon","last_name":"Lilly"},{"full_name":"Boogaard, Leindert","last_name":"Boogaard","first_name":"Leindert"},{"last_name":"Marino","full_name":"Marino, Raffaella","first_name":"Raffaella"},{"last_name":"Maseda","full_name":"Maseda, Michael","first_name":"Michael"},{"first_name":"Themiya","last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya"}],"article_type":"original","quality_controlled":"1","title":"The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6","date_updated":"2024-10-14T11:33:21Z","fulldoi":"https://doi.org/10.1093/mnras/staa2550","issue":"2","publication_status":"published","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"article_processing_charge":"No","citation":{"chicago":"Matthee, Jorryt J, Gabriele Pezzulli, Ruari Mackenzie, Sebastiano Cantalupo, Haruka Kusakabe, Floriane Leclercq, David Sobral, et al. “The Nature of CR7 Revealed with MUSE: A Young Starburst Powering Extended Ly α Emission at z = 6.6.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa2550.","ama":"Matthee JJ, Pezzulli G, Mackenzie R, et al. The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. 2020;498(2):3043-3059. doi:10.1093/mnras/staa2550","ista":"Matthee JJ, Pezzulli G, Mackenzie R, Cantalupo S, Kusakabe H, Leclercq F, Sobral D, Richard J, Wisotzki L, Lilly S, Boogaard L, Marino R, Maseda M, Nanayakkara T. 2020. The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. 498(2), 3043–3059.","ieee":"J. J. Matthee et al., “The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6,” Monthly Notices of the Royal Astronomical Society, vol. 498, no. 2. Oxford University Press, pp. 3043–3059, 2020.","short":"J.J. Matthee, G. Pezzulli, R. Mackenzie, S. Cantalupo, H. Kusakabe, F. Leclercq, D. Sobral, J. Richard, L. Wisotzki, S. Lilly, L. Boogaard, R. Marino, M. Maseda, T. Nanayakkara, Monthly Notices of the Royal Astronomical Society 498 (2020) 3043–3059.","mla":"Matthee, Jorryt J., et al. “The Nature of CR7 Revealed with MUSE: A Young Starburst Powering Extended Ly α Emission at z = 6.6.” Monthly Notices of the Royal Astronomical Society, vol. 498, no. 2, Oxford University Press, 2020, pp. 3043–59, doi:10.1093/mnras/staa2550.","apa":"Matthee, J. J., Pezzulli, G., Mackenzie, R., Cantalupo, S., Kusakabe, H., Leclercq, F., … Nanayakkara, T. (2020). The nature of CR7 revealed with MUSE: A young starburst powering extended Ly α emission at z = 6.6. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa2550"},"date_published":"2020-10-01T00:00:00Z","doi":"10.1093/mnras/staa2550","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/2008.01731"}],"status":"public","abstract":[{"text":"CR7 is among the most luminous Ly α emitters (LAEs) known at z = 6.6 and consists of at least three UV components that are surrounded by Ly α emission. Previous studies have suggested that it may host an extreme ionizing source. Here, we present deep integral field spectroscopy of CR7 with VLT/Multi Unit Spectroscopic Explorer (MUSE). We measure extended emission with a similar halo scale length as typical LAEs at z ≈ 5. CR7’s Ly α halo is clearly elongated along the direction connecting the multiple components, likely tracing the underlying gas distribution. The Ly α emission originates almost exclusively from the brightest UV component, but we also identify a faint kinematically distinct Ly α emitting region nearby a fainter component. Combined with new near-infrared data, the MUSE data show that the rest-frame Ly α equivalent width (EW) is ≈100 Å. This is a factor 4 higher than the EW measured in low-redshift analogues with carefully matched Ly α profiles (and thus arguably H I column density), but this EW can plausibly be explained by star formation. Alternative scenarios requiring active galactic nucleus (AGN) powering are also disfavoured by the narrower and steeper Ly α spectrum and much smaller IR to UV ratio compared to obscured AGN in other Ly α blobs. CR7’s Ly α emission, while extremely luminous, resembles the emission in more common LAEs at lower redshifts very well and is likely powered by a young metal-poor starburst.","lang":"eng"}],"month":"10","external_id":{"arxiv":["2008.01731"]},"type":"journal_article","oa_version":"Preprint"},{"article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high-redshift","intergalactic medium","quasars: emission lines","quasars: general"],"issue":"2","publication_status":"published","fulldoi":"https://doi.org/10.1093/mnras/staa1269","date_updated":"2022-08-18T11:17:47Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","type":"journal_article","external_id":{"arxiv":["2005.01732"]},"oa_version":"Preprint","abstract":[{"lang":"eng","text":"A prediction of the classic active galactic nucleus (AGN) unification model is the presence of ionization cones with different orientations depending on the AGN type. Confirmations of this model exist for present times, but it is less clear in the early Universe. Here, we use the morphology of giant Ly α nebulae around AGNs at redshift z ∼ 3 to probe AGN emission and therefore the validity of the AGN unification model at this redshift. We compare the spatial morphology of 19 nebulae previously found around type I AGNs with a new sample of four Ly α nebulae detected around type II AGNs. Using two independent techniques, we find that nebulae around type II AGNs are more asymmetric than around type I, at least at radial distances r > 30 physical kpc (pkpc) from the ionizing source. We conclude that the type I and type II AGNs in our sample show evidence of different surrounding ionizing geometries. This suggests that the classical AGN unification model is also valid for high-redshift sources. Finally, we discuss how the lack of asymmetry in the inner parts (r ≲ 30 pkpc) and the associated high values of the He II to Ly α ratios in these regions could indicate additional sources of (hard) ionizing radiation originating within or in proximity of the AGN host galaxies. This work demonstrates that the morphologies of giant Ly α nebulae can be used to understand and study the geometry of high-redshift AGNs on circumnuclear scales and it lays the foundation for future studies using much larger statistical samples."}],"month":"06","doi":"10.1093/mnras/staa1269","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/2005.01732","open_access":"1"}],"citation":{"chicago":"den Brok, J S, S Cantalupo, R Mackenzie, R A Marino, G Pezzulli, Jorryt J Matthee, S D Johnson, M Krumpe, T Urrutia, and W Kollatschny. “Probing the AGN Unification Model at Redshift z ∼ 3 with MUSE Observations of Giant Lyα Nebulae.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa1269.","ista":"den Brok JS, Cantalupo S, Mackenzie R, Marino RA, Pezzulli G, Matthee JJ, Johnson SD, Krumpe M, Urrutia T, Kollatschny W. 2020. Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 495(2), 1874–1887.","ama":"den Brok JS, Cantalupo S, Mackenzie R, et al. Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. 2020;495(2):1874-1887. doi:10.1093/mnras/staa1269","short":"J.S. den Brok, S. Cantalupo, R. Mackenzie, R.A. Marino, G. Pezzulli, J.J. Matthee, S.D. Johnson, M. Krumpe, T. Urrutia, W. Kollatschny, Monthly Notices of the Royal Astronomical Society 495 (2020) 1874–1887.","ieee":"J. S. den Brok et al., “Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae,” Monthly Notices of the Royal Astronomical Society, vol. 495, no. 2. Oxford University Press, pp. 1874–1887, 2020.","mla":"den Brok, J. S., et al. “Probing the AGN Unification Model at Redshift z ∼ 3 with MUSE Observations of Giant Lyα Nebulae.” Monthly Notices of the Royal Astronomical Society, vol. 495, no. 2, Oxford University Press, 2020, pp. 1874–87, doi:10.1093/mnras/staa1269.","apa":"den Brok, J. S., Cantalupo, S., Mackenzie, R., Marino, R. A., Pezzulli, G., Matthee, J. J., … Kollatschny, W. (2020). Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa1269"},"date_published":"2020-06-01T00:00:00Z","intvolume":" 495","oa":1,"language":[{"iso":"eng"}],"year":"2020","acknowledgement":"SC and GP gratefully acknowledge support from Swiss National Science Foundation grant PP00P2 163824. MK acknowledges support by DLR500R1904.","arxiv":1,"day":"01","publication":"Monthly Notices of the Royal Astronomical Society","volume":495,"author":[{"first_name":"J S","full_name":"den Brok, J S","last_name":"den Brok"},{"first_name":"S","full_name":"Cantalupo, S","last_name":"Cantalupo"},{"first_name":"R","full_name":"Mackenzie, R","last_name":"Mackenzie"},{"first_name":"R A","last_name":"Marino","full_name":"Marino, R A"},{"full_name":"Pezzulli, G","last_name":"Pezzulli","first_name":"G"},{"last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Johnson","full_name":"Johnson, S D","first_name":"S D"},{"first_name":"M","full_name":"Krumpe, M","last_name":"Krumpe"},{"first_name":"T","last_name":"Urrutia","full_name":"Urrutia, T"},{"first_name":"W","last_name":"Kollatschny","full_name":"Kollatschny, W"}],"article_type":"original","title":"Probing the AGN unification model at redshift z ∼ 3 with MUSE observations of giant Lyα nebulae","quality_controlled":"1","scopus_import":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publisher":"Oxford University Press","extern":"1","date_created":"2022-07-07T10:40:17Z","_id":"11530","page":"1874-1887"},{"month":"04","abstract":[{"lang":"eng","text":"While low-luminosity galaxies dominate number counts at all redshifts, their contribution to cosmic reionization is poorly understood due to a lack of knowledge of their physical properties. We isolate a sample of 35 z ≈ 4–5 continuum-faint Lyman-α emitters from deep VLT/MUSE spectroscopy and directly measure their H α emission using stacked Spitzer/IRAC Ch. 1 photometry. Based on Hubble Space Telescope imaging, we determine that the average UV continuum magnitude is fainter than −16 (≈ 0.01 L⋆), implying a median Lyman-α equivalent width of 259 Å. By combining the H α measurement with the UV magnitude, we determine the ionizing photon production efficiency, ξion, a first for such faint galaxies. The measurement of log10 (ξion [Hz erg−1]) = 26.28 (+0.28−0.40) is in excess of literature measurements of both continuum- and emission line-selected samples, implying a more efficient production of ionizing photons in these lower luminosity, Lyman-α-selected systems. We conclude that this elevated efficiency can be explained by stellar populations with metallicities between 4 × 10−4 and 0.008, with light-weighted ages less than 3 Myr."}],"oa_version":"Published Version","external_id":{"arxiv":["2002.11117"]},"type":"journal_article","date_published":"2020-04-01T00:00:00Z","citation":{"chicago":"Maseda, Michael V, Roland Bacon, Daniel Lam, Jorryt J Matthee, Jarle Brinchmann, Joop Schaye, Ivo Labbe, et al. “Elevated Ionizing Photon Production Efficiency in Faint High-Equivalent-Width Lyman-α Emitters.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa622.","ama":"Maseda MV, Bacon R, Lam D, et al. Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. Monthly Notices of the Royal Astronomical Society. 2020;493(4):5120-5130. doi:10.1093/mnras/staa622","ista":"Maseda MV, Bacon R, Lam D, Matthee JJ, Brinchmann J, Schaye J, Labbe I, Schmidt KB, Boogaard L, Bouwens R, Cantalupo S, Franx M, Hashimoto T, Inami H, Kusakabe H, Mahler G, Nanayakkara T, Richard J, Wisotzki L. 2020. Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. Monthly Notices of the Royal Astronomical Society. 493(4), 5120–5130.","short":"M.V. Maseda, R. Bacon, D. Lam, J.J. Matthee, J. Brinchmann, J. Schaye, I. Labbe, K.B. Schmidt, L. Boogaard, R. Bouwens, S. Cantalupo, M. Franx, T. Hashimoto, H. Inami, H. Kusakabe, G. Mahler, T. Nanayakkara, J. Richard, L. Wisotzki, Monthly Notices of the Royal Astronomical Society 493 (2020) 5120–5130.","ieee":"M. V. Maseda et al., “Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters,” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 4. Oxford University Press, pp. 5120–5130, 2020.","apa":"Maseda, M. V., Bacon, R., Lam, D., Matthee, J. J., Brinchmann, J., Schaye, J., … Wisotzki, L. (2020). Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa622","mla":"Maseda, Michael V., et al. “Elevated Ionizing Photon Production Efficiency in Faint High-Equivalent-Width Lyman-α Emitters.” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 4, Oxford University Press, 2020, pp. 5120–30, doi:10.1093/mnras/staa622."},"status":"public","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/staa622"}],"doi":"10.1093/mnras/staa622","article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_status":"published","issue":"4","fulldoi":"https://doi.org/10.1093/mnras/staa622","date_updated":"2022-08-18T11:23:27Z","keyword":["Space and Planetary Science","Astronomy and Astrophysics","Galaxies: evolution","Galaxies: high-redshift","Galaxies: ISM"],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publisher":"Oxford University Press","scopus_import":"1","title":"Elevated ionizing photon production efficiency in faint high-equivalent-width Lyman-α emitters","quality_controlled":"1","article_type":"original","author":[{"first_name":"Michael V","full_name":"Maseda, Michael V","last_name":"Maseda"},{"last_name":"Bacon","full_name":"Bacon, Roland","first_name":"Roland"},{"first_name":"Daniel","full_name":"Lam, Daniel","last_name":"Lam"},{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"first_name":"Jarle","last_name":"Brinchmann","full_name":"Brinchmann, Jarle"},{"first_name":"Joop","full_name":"Schaye, Joop","last_name":"Schaye"},{"full_name":"Labbe, Ivo","last_name":"Labbe","first_name":"Ivo"},{"first_name":"Kasper B","full_name":"Schmidt, Kasper B","last_name":"Schmidt"},{"first_name":"Leindert","last_name":"Boogaard","full_name":"Boogaard, Leindert"},{"full_name":"Bouwens, Rychard","last_name":"Bouwens","first_name":"Rychard"},{"last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano","first_name":"Sebastiano"},{"first_name":"Marijn","full_name":"Franx, Marijn","last_name":"Franx"},{"full_name":"Hashimoto, Takuya","last_name":"Hashimoto","first_name":"Takuya"},{"first_name":"Hanae","last_name":"Inami","full_name":"Inami, Hanae"},{"full_name":"Kusakabe, Haruka","last_name":"Kusakabe","first_name":"Haruka"},{"last_name":"Mahler","full_name":"Mahler, Guillaume","first_name":"Guillaume"},{"first_name":"Themiya","last_name":"Nanayakkara","full_name":"Nanayakkara, Themiya"},{"first_name":"Johan","full_name":"Richard, Johan","last_name":"Richard"},{"full_name":"Wisotzki, Lutz","last_name":"Wisotzki","first_name":"Lutz"}],"extern":"1","_id":"11531","page":"5120-5130","date_created":"2022-07-07T10:46:41Z","year":"2020","language":[{"iso":"eng"}],"oa":1,"intvolume":" 493","publication":"Monthly Notices of the Royal Astronomical Society","volume":493,"acknowledgement":"We would like to thank the anonymous referee for a thoughtful report and suggestions that have improved this manuscript. We are also grateful to everyone involved in the Spitzer Space Telescope mission and everyone at the Spitzer Science Center: we are truly fortunate to have been able to use data from this facility. J. B. acknowledges support by FCT/MCTES through national funds by this grant UID/FIS/04434/2019 and through the Investigador FCT contract no. IF/01654/2014/CP1215/CT0003. S. C. gratefully acknowledges support from Swiss National Science Foundation grant PP00P2 163824. We would also like to thank Mauro Stefanon for his assistance with de-blending the IRAC photometry, Pieter van Dokkum for a number of useful suggestions, and Daniel Schaerer for information regarding the stellar population models. This study is based on observations made with ESO telescopes at the La Silla Paranal Observatory under programs IDs 094.A-2089(B), 095.A0010(A), 096.A-0045(A), and 096.A-0045(B).","day":"01","arxiv":1},{"acknowledgement":"We thank the anonymous referee for the valuable feedback that significantly improved the quality and clarity of this paper. SS and JC acknowledge studentships from Lancaster University. APA acknowledges support from Fundação para a Ciência e a Tecnologia through the project PTDC/FISAST/31546/2017. The authors would like to thank Ali Khostovan, Sara Perez Sanchez, Alex Bennett and Tom Rose for contributions and discussions in the early stages of this work. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme ID 179.A-2005 and on data products produced by CALET and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Finally, the authors acknowledge the unique value of the publicly available analysis software TOPCAT (Taylor 2005) and publicly available programming language Python, including the numpy, pyfits, matplotlib, scipy and astropy (Astropy Collaboration et al. 2013) packages. This work is based on the public SC4K sample of LAEs (Sobral et al. 2018a) and we release the full catalogue with all the photometry and properties derived in this paper, in electronic format, along with the relevant tables.","day":"01","arxiv":1,"publication":"Monthly Notices of the Royal Astronomical Society","volume":493,"oa":1,"intvolume":" 493","year":"2020","language":[{"iso":"eng"}],"extern":"1","page":"141-160","_id":"11533","date_created":"2022-07-07T12:05:23Z","title":"The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs","quality_controlled":"1","article_type":"original","author":[{"first_name":"S","full_name":"Santos, S","last_name":"Santos"},{"full_name":"Sobral, D","last_name":"Sobral","first_name":"D"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J"},{"last_name":"Calhau","full_name":"Calhau, J","first_name":"J"},{"first_name":"E","full_name":"da Cunha, E","last_name":"da Cunha"},{"full_name":"Ribeiro, B","last_name":"Ribeiro","first_name":"B"},{"first_name":"A","full_name":"Paulino-Afonso, A","last_name":"Paulino-Afonso"},{"first_name":"P","full_name":"Arrabal Haro, P","last_name":"Arrabal Haro"},{"first_name":"J","full_name":"Butterworth, J","last_name":"Butterworth"}],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publisher":"Oxford University Press","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: high-redshift","galaxies: star formation"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"1","publication_status":"published","date_updated":"2022-08-18T11:27:43Z","fulldoi":"https://doi.org/10.1093/mnras/staa093","article_processing_charge":"No","status":"public","main_file_link":[{"url":"https://arxiv.org/abs/1910.02959","open_access":"1"}],"doi":"10.1093/mnras/staa093","date_published":"2020-03-01T00:00:00Z","citation":{"ieee":"S. Santos et al., “The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs,” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 1. Oxford University Press, pp. 141–160, 2020.","short":"S. Santos, D. Sobral, J.J. Matthee, J. Calhau, E. da Cunha, B. Ribeiro, A. Paulino-Afonso, P. Arrabal Haro, J. Butterworth, Monthly Notices of the Royal Astronomical Society 493 (2020) 141–160.","chicago":"Santos, S, D Sobral, Jorryt J Matthee, J Calhau, E da Cunha, B Ribeiro, A Paulino-Afonso, P Arrabal Haro, and J Butterworth. “The Evolution of Rest-Frame UV Properties, Ly α EWs, and the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K LAEs.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa093.","ista":"Santos S, Sobral D, Matthee JJ, Calhau J, da Cunha E, Ribeiro B, Paulino-Afonso A, Arrabal Haro P, Butterworth J. 2020. The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly Notices of the Royal Astronomical Society. 493(1), 141–160.","ama":"Santos S, Sobral D, Matthee JJ, et al. The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly Notices of the Royal Astronomical Society. 2020;493(1):141-160. doi:10.1093/mnras/staa093","mla":"Santos, S., et al. “The Evolution of Rest-Frame UV Properties, Ly α EWs, and the SFR–Stellar Mass Relation at z ∼ 2–6 for SC4K LAEs.” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 1, Oxford University Press, 2020, pp. 141–60, doi:10.1093/mnras/staa093.","apa":"Santos, S., Sobral, D., Matthee, J. J., Calhau, J., da Cunha, E., Ribeiro, B., … Butterworth, J. (2020). The evolution of rest-frame UV properties, Ly α EWs, and the SFR–stellar mass relation at z ∼ 2–6 for SC4K LAEs. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa093"},"oa_version":"Preprint","external_id":{"arxiv":["1910.02959"]},"type":"journal_article","month":"03","abstract":[{"lang":"eng","text":"We explore deep rest-frame UV to FIR data in the COSMOS field to measure the individual spectral energy distributions (SED) of the ∼4000 SC4K (Sobral et al.) Lyman α (Ly α) emitters (LAEs) at z ∼ 2–6. We find typical stellar masses of 109.3 ± 0.6 M⊙ and star formation rates (SFR) of SFRSED=4.4+10.5−2.4 M⊙ yr−1 and SFRLyα=5.9+6.3−2.6 M⊙ yr−1, combined with very blue UV slopes of β=−2.1+0.5−0.4, but with significant variations within the population. MUV and β are correlated in a similar way to UV-selected sources, but LAEs are consistently bluer. This suggests that LAEs are the youngest and/or most dust-poor subset of the UV-selected population. We also study the Ly α rest-frame equivalent width (EW0) and find 45 ‘extreme’ LAEs with EW0 > 240 Å (3σ), implying a low number density of (7 ± 1) × 10−7 Mpc−3. Overall, we measure little to no evolution of the Ly α EW0 and scale length parameter (w0), which are consistently high (EW0=140+280−70 Å, w0=129+11−11 Å) from z ∼ 6 to z ∼ 2 and below. However, w0 is anticorrelated with MUV and stellar mass. Our results imply that sources selected as LAEs have a high Ly α escape fraction (fesc,Ly α) irrespective of cosmic time, but fesc,Ly α is still higher for UV-fainter and lower mass LAEs. The least massive LAEs (<109.5 M⊙) are typically located above the star formation ‘main sequence’ (MS), but the offset from the MS decreases towards z ∼ 6 and towards 1010 M⊙. Our results imply a lack of evolution in the properties of LAEs across time and reveals the increasing overlap in properties of LAEs and UV-continuum selected galaxies as typical star-forming galaxies at high redshift effectively become LAEs."}]},{"arxiv":1,"day":"01","acknowledgement":"We thank the referee for their suggestions and constructive comments that helped to improve the presentation of our results. Based on observations obtained with the Very Large Telescope, program 99.A-0462. Based on observations made with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program #14699. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2017.1.01451.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan) and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. MG acknowledges support from NASA grant NNX17AK58G. GP and SC gratefully acknowledge support from Swiss National Science Foundation grant PP00P2 163824. BD acknowledges financial support from the National Science Foundation, grant number 1716907. We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, SCIPY (Jones et al. 2001; Hunter 2007; van der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration 2013) packages, the astronomical imaging tools SEXTRACTOR, SWARP, and SCAMP (Bertin & Arnouts 1996; Bertin 2006, 2010) and the TOPCAT analysis tool (Taylor 2013).","volume":492,"publication":"Monthly Notices of the Royal Astronomical Society","oa":1,"intvolume":" 492","year":"2020","language":[{"iso":"eng"}],"date_created":"2022-07-07T12:21:36Z","_id":"11534","page":"1778-1790","extern":"1","quality_controlled":"1","title":"Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ","author":[{"full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"full_name":"Gronke, Max","last_name":"Gronke","first_name":"Max"},{"first_name":"Gabriele","last_name":"Pezzulli","full_name":"Pezzulli, Gabriele"},{"first_name":"Sebastiano","last_name":"Cantalupo","full_name":"Cantalupo, Sebastiano"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"},{"last_name":"Darvish","full_name":"Darvish, Behnam","first_name":"Behnam"},{"last_name":"Santos","full_name":"Santos, Sérgio","first_name":"Sérgio"}],"article_type":"original","publisher":"Oxford University Press","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","fulldoi":"https://doi.org/10.1093/mnras/stz3554","date_updated":"2024-10-14T11:33:34Z","publication_status":"published","issue":"2","article_processing_charge":"No","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1909.06376"}],"status":"public","doi":"10.1093/mnras/stz3554","date_published":"2020-02-01T00:00:00Z","citation":{"mla":"Matthee, Jorryt J., et al. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” Monthly Notices of the Royal Astronomical Society, vol. 492, no. 2, Oxford University Press, 2020, pp. 1778–90, doi:10.1093/mnras/stz3554.","apa":"Matthee, J. J., Sobral, D., Gronke, M., Pezzulli, G., Cantalupo, S., Röttgering, H., … Santos, S. (2020). Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz3554","ista":"Matthee JJ, Sobral D, Gronke M, Pezzulli G, Cantalupo S, Röttgering H, Darvish B, Santos S. 2020. Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. 492(2), 1778–1790.","chicago":"Matthee, Jorryt J, David Sobral, Max Gronke, Gabriele Pezzulli, Sebastiano Cantalupo, Huub Röttgering, Behnam Darvish, and Sérgio Santos. “Resolved Lyman-α Properties of a Luminous Lyman-Break Galaxy in a Large Ionized Bubble at z = 6.53 .” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/stz3554.","ama":"Matthee JJ, Sobral D, Gronke M, et al. Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 . Monthly Notices of the Royal Astronomical Society. 2020;492(2):1778-1790. doi:10.1093/mnras/stz3554","short":"J.J. Matthee, D. Sobral, M. Gronke, G. Pezzulli, S. Cantalupo, H. Röttgering, B. Darvish, S. Santos, Monthly Notices of the Royal Astronomical Society 492 (2020) 1778–1790.","ieee":"J. J. Matthee et al., “Resolved Lyman-α properties of a luminous Lyman-break galaxy in a large ionized bubble at z = 6.53 ,” Monthly Notices of the Royal Astronomical Society, vol. 492, no. 2. Oxford University Press, pp. 1778–1790, 2020."},"oa_version":"Preprint","type":"journal_article","external_id":{"arxiv":["1909.06376"]},"month":"02","abstract":[{"lang":"eng","text":"The observed properties of the Lyman-α (Ly α) emission line are a powerful probe of neutral gas in and around galaxies. We present spatially resolved Ly α spectroscopy with VLT/MUSE targeting VR7, a UV-luminous galaxy at z = 6.532 with moderate Ly α equivalent width (EW0 ≈ 38 Å). These data are combined with deep resolved [CII]158μm spectroscopy obtained with ALMA and UV imaging from HST and we also detect UV continuum with MUSE. Ly α emission is clearly detected with S/N ≈ 40 and FWHM of 374 km s−1. Ly α and [C II] are similarly extended beyond the UV, with effective radius reff = 2.1 ± 0.2 kpc for a single exponential model or reff,Lyα,halo=3.45+1.08−0.87 kpc when measured jointly with the UV continuum. The Ly α profile is broader and redshifted with respect to the [C II] line (by 213 km s−1), but there are spatial variations that are qualitatively similar in both lines and coincide with resolved UV components. This suggests that the emission originates from two components with plausibly different H I column densities. We place VR7 in the context of other galaxies at similar and lower redshift. The Ly α halo scale length is similar at different redshifts and velocity shifts with respect to the systemic are typically smaller. Overall, we find little indications of a more neutral vicinity at higher redshift. This means that the local (∼10 kpc) neutral gas conditions that determine the observed Ly α properties in VR7 resemble the conditions in post-reionization galaxies."}]},{"oa":1,"intvolume":" 493","year":"2020","language":[{"iso":"eng"}],"acknowledgement":"JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Camila Correa for help analysing snipshot merger trees. We thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann, Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and ideas. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT analysis tool (Taylor 2013).","arxiv":1,"day":"01","publication":"Monthly Notices of the Royal Astronomical Society","volume":493,"title":"The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population","quality_controlled":"1","article_type":"original","author":[{"first_name":"João","last_name":"Calhau","full_name":"Calhau, João"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"first_name":"Sérgio","last_name":"Santos","full_name":"Santos, Sérgio"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana","first_name":"Ana"},{"last_name":"Stroe","full_name":"Stroe, Andra","first_name":"Andra"},{"full_name":"Simmons, Brooke","last_name":"Simmons","first_name":"Brooke"},{"first_name":"Cassandra","last_name":"Barlow-Hall","full_name":"Barlow-Hall, Cassandra"},{"full_name":"Adams, Benjamin","last_name":"Adams","first_name":"Benjamin"}],"publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publisher":"Oxford University Press","scopus_import":"1","extern":"1","date_created":"2022-07-08T07:34:10Z","_id":"11539","page":"3341-3362","article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: evolution","galaxies: high-redshift","quasars: supermassive black holes","galaxies: star formation","cosmology: observations","X-rays: galaxies"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"3","publication_status":"published","fulldoi":"https://doi.org/10.1093/mnras/staa476","date_updated":"2022-08-18T11:25:31Z","oa_version":"Preprint","external_id":{"arxiv":["1909.11672"]},"type":"journal_article","month":"04","abstract":[{"text":"Despite recent progress in understanding Ly α emitters (LAEs), relatively little is known regarding their typical black hole activity across cosmic time. Here, we study the X-ray and radio properties of ∼4000 LAEs at 2.2 < z < 6 from the SC4K survey in the COSMOS field. We detect 254 (6.8per cent±0.4per cent) LAEs individually in the X-rays (S/N > 3) with an average luminosity of 1044.31±0.01ergs−1 and average black hole accretion rate (BHAR) of 0.72±0.01 M⊙ yr−1, consistent with moderate to high accreting active galactic neuclei (AGNs). We detect 120 sources in deep radio data (radio AGN fraction of 3.2per cent±0.3per cent). The global AGN fraction (8.6per cent±0.4per cent) rises with Ly α luminosity and declines with increasing redshift. For X-ray-detected LAEs, Ly α luminosities correlate with the BHARs, suggesting that Ly α luminosity becomes a BHAR indicator. Most LAEs (93.1per cent±0.6per cent) at 2 < z < 6 have no detectable X-ray emission (BHARs < 0.017 M⊙ yr−1). The median star formation rate (SFR) of star-forming LAEs from Ly α and radio luminosities is 7.6+6.6−2.8 M⊙ yr−1. The black hole to galaxy growth ratio (BHAR/SFR) for LAEs is <0.0022, consistent with typical star-forming galaxies and the local BHAR/SFR relation. We conclude that LAEs at 2 < z < 6 include two different populations: an AGN population, where Ly α luminosity traces BHAR, and another with low SFRs which remain undetected in even the deepest X-ray stacks but is detected in the radio stacks.","lang":"eng"}],"status":"public","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1909.11672"}],"doi":"10.1093/mnras/staa476","date_published":"2020-04-01T00:00:00Z","citation":{"ieee":"J. Calhau et al., “The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population,” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 3. Oxford University Press, pp. 3341–3362, 2020.","short":"J. Calhau, D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, A. Stroe, B. Simmons, C. Barlow-Hall, B. Adams, Monthly Notices of the Royal Astronomical Society 493 (2020) 3341–3362.","ista":"Calhau J, Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Stroe A, Simmons B, Barlow-Hall C, Adams B. 2020. The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. Monthly Notices of the Royal Astronomical Society. 493(3), 3341–3362.","chicago":"Calhau, João, David Sobral, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Andra Stroe, Brooke Simmons, Cassandra Barlow-Hall, and Benjamin Adams. “The X-Ray and Radio Activity of Typical and Luminous Ly α Emitters from z ∼ 2 to z ∼ 6: Evidence for a Diverse, Evolving Population.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa476.","ama":"Calhau J, Sobral D, Santos S, et al. The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. Monthly Notices of the Royal Astronomical Society. 2020;493(3):3341-3362. doi:10.1093/mnras/staa476","mla":"Calhau, João, et al. “The X-Ray and Radio Activity of Typical and Luminous Ly α Emitters from z ∼ 2 to z ∼ 6: Evidence for a Diverse, Evolving Population.” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 3, Oxford University Press, 2020, pp. 3341–62, doi:10.1093/mnras/staa476.","apa":"Calhau, J., Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Stroe, A., … Adams, B. (2020). The X-ray and radio activity of typical and luminous Ly α emitters from z ∼ 2 to z ∼ 6: Evidence for a diverse, evolving population. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa476"}},{"publication":"Monthly Notices of the Royal Astronomical Society","volume":493,"day":"04","arxiv":1,"language":[{"iso":"eng"}],"year":"2020","intvolume":" 493","oa":1,"extern":"1","page":"4333-4341","_id":"13465","date_created":"2023-08-03T10:13:20Z","scopus_import":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"publisher":"Oxford University Press","author":[{"last_name":"Renzo","full_name":"Renzo, M","first_name":"M"},{"first_name":"R J","full_name":"Farmer, R J","last_name":"Farmer"},{"first_name":"S","full_name":"Justham, S","last_name":"Justham"},{"first_name":"S E","full_name":"de Mink, S E","last_name":"de Mink"},{"first_name":"Ylva Louise Linsdotter","orcid":"0000-0002-6960-6911","last_name":"Götberg","full_name":"Götberg, Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d"},{"full_name":"Marchant, P","last_name":"Marchant","first_name":"P"}],"article_type":"original","title":"Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection","quality_controlled":"1","issue":"3","publication_status":"published","fulldoi":"https://doi.org/10.1093/mnras/staa549","date_updated":"2023-08-09T12:53:37Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"article_processing_charge":"No","citation":{"mla":"Renzo, M., et al. “Sensitivity of the Lower Edge of the Pair-Instability Black Hole Mass Gap to the Treatment of Time-Dependent Convection.” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 3, Oxford University Press, 2020, pp. 4333–41, doi:10.1093/mnras/staa549.","apa":"Renzo, M., Farmer, R. J., Justham, S., de Mink, S. E., Götberg, Y. L. L., & Marchant, P. (2020). Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa549","short":"M. Renzo, R.J. Farmer, S. Justham, S.E. de Mink, Y.L.L. Götberg, P. Marchant, Monthly Notices of the Royal Astronomical Society 493 (2020) 4333–4341.","ieee":"M. Renzo, R. J. Farmer, S. Justham, S. E. de Mink, Y. L. L. Götberg, and P. Marchant, “Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection,” Monthly Notices of the Royal Astronomical Society, vol. 493, no. 3. Oxford University Press, pp. 4333–4341, 2020.","ista":"Renzo M, Farmer RJ, Justham S, de Mink SE, Götberg YLL, Marchant P. 2020. Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection. Monthly Notices of the Royal Astronomical Society. 493(3), 4333–4341.","chicago":"Renzo, M, R J Farmer, S Justham, S E de Mink, Ylva Louise Linsdotter Götberg, and P Marchant. “Sensitivity of the Lower Edge of the Pair-Instability Black Hole Mass Gap to the Treatment of Time-Dependent Convection.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa549.","ama":"Renzo M, Farmer RJ, Justham S, de Mink SE, Götberg YLL, Marchant P. Sensitivity of the lower edge of the pair-instability black hole mass gap to the treatment of time-dependent convection. Monthly Notices of the Royal Astronomical Society. 2020;493(3):4333-4341. doi:10.1093/mnras/staa549"},"date_published":"2020-04-04T00:00:00Z","doi":"10.1093/mnras/staa549","status":"public","main_file_link":[{"url":"https://doi.org/10.1093/mnras/staa549","open_access":"1"}],"abstract":[{"lang":"eng","text":"Gravitational-wave detections are now probing the black hole (BH) mass distribution, including the predicted pair-instability mass gap. These data require robust quantitative predictions, which are challenging to obtain. The most massive BH progenitors experience episodic mass ejections on time-scales shorter than the convective turnover time-scale. This invalidates the steady-state assumption on which the classic mixing length theory relies. We compare the final BH masses computed with two different versions of the stellar evolutionary code MESA\r\n: (i) using the default implementation of Paxton et al. (2018) and (ii) solving an additional equation accounting for the time-scale for convective deceleration. In the second grid, where stronger convection develops during the pulses and carries part of the energy, we find weaker pulses. This leads to lower amounts of mass being ejected and thus higher final BH masses of up to ∼5M⊙\r\n. The differences are much smaller for the progenitors that determine the maximum mass of BHs below the gap. This prediction is robust at MBH,max≃48M⊙\r\n, at least within the idealized context of this study. This is an encouraging indication that current models are robust enough for comparison with the present-day gravitational-wave detections. However, the large differences between individual models emphasize the importance of improving the treatment of convection in stellar models, especially in the light of the data anticipated from the third generation of gravitational-wave detectors."}],"month":"04","external_id":{"arxiv":["2002.08200"]},"type":"journal_article","oa_version":"Published Version"},{"article_processing_charge":"No","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2024-10-14T12:32:49Z","fulldoi":"https://doi.org/10.1093/mnras/staa3428","issue":"1","publication_status":"published","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"month":"11","abstract":[{"lang":"eng","text":"A new window is opening in high-energy astronomy: X-ray polarimetry. With many missions currently under development and scheduled to launch as early as 2021, observations of the X-ray polarization of accreting X-ray pulsars will soon be available. As polarization is particularly sensitive to the geometry of the emission region, the upcoming polarimeters will shed new light on the emission mechanism of these objects, provided that we have sound theoretical models that agree with current spectroscopic and timing observation and that can make predictions of the polarization parameters of the emission. We here present a new model for the polarized emission of accreting X-ray pulsars in the accretion column scenario that for the first time takes into account the macroscopic structure and dynamics of the accretion region and the propagation of the radiation towards the observer, including relativistic beaming, gravitational lensing, and quantum electrodynamics. In this paper, we present all the details of the model, while in a companion paper, we apply our model to predict the polarization parameters of the bright X-ray pulsar Hercules X-1."}],"oa_version":"Preprint","type":"journal_article","external_id":{"arxiv":["2009.00631"]},"date_published":"2020-11-05T00:00:00Z","citation":{"ieee":"I. Caiazzo and J. Heyl, “Polarization of accreting X-ray pulsars. I. A new model,” Monthly Notices of the Royal Astronomical Society, vol. 501, no. 1. Oxford University Press, pp. 109–128, 2020.","short":"I. Caiazzo, J. Heyl, Monthly Notices of the Royal Astronomical Society 501 (2020) 109–128.","ista":"Caiazzo I, Heyl J. 2020. Polarization of accreting X-ray pulsars. I. A new model. Monthly Notices of the Royal Astronomical Society. 501(1), 109–128.","ama":"Caiazzo I, Heyl J. Polarization of accreting X-ray pulsars. I. A new model. Monthly Notices of the Royal Astronomical Society. 2020;501(1):109-128. doi:10.1093/mnras/staa3428","chicago":"Caiazzo, Ilaria, and Jeremy Heyl. “Polarization of Accreting X-Ray Pulsars. I. A New Model.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa3428.","mla":"Caiazzo, Ilaria, and Jeremy Heyl. “Polarization of Accreting X-Ray Pulsars. I. A New Model.” Monthly Notices of the Royal Astronomical Society, vol. 501, no. 1, Oxford University Press, 2020, pp. 109–28, doi:10.1093/mnras/staa3428.","apa":"Caiazzo, I., & Heyl, J. (2020). Polarization of accreting X-ray pulsars. I. A new model. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa3428"},"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.2009.00631","open_access":"1"}],"status":"public","doi":"10.1093/mnras/staa3428","year":"2020","language":[{"iso":"eng"}],"oa":1,"intvolume":" 501","volume":501,"publication":"Monthly Notices of the Royal Astronomical Society","day":"05","arxiv":1,"publisher":"Oxford University Press","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"scopus_import":"1","quality_controlled":"1","title":"Polarization of accreting X-ray pulsars. I. A new model","author":[{"first_name":"Ilaria","orcid":"0000-0002-4770-5388","full_name":"Caiazzo, Ilaria","last_name":"Caiazzo","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d"},{"full_name":"Heyl, Jeremy","last_name":"Heyl","first_name":"Jeremy"}],"article_type":"original","date_created":"2024-03-26T10:33:43Z","_id":"15220","page":"109-128","extern":"1"},{"intvolume":" 501","oa":1,"language":[{"iso":"eng"}],"year":"2020","arxiv":1,"day":"05","volume":501,"publication":"Monthly Notices of the Royal Astronomical Society","article_type":"original","author":[{"last_name":"Caiazzo","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","first_name":"Ilaria"},{"first_name":"Jeremy","full_name":"Heyl, Jeremy","last_name":"Heyl"}],"title":"Polarization of accreting X-ray pulsars – II. Hercules X-1","quality_controlled":"1","scopus_import":"1","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"publisher":"Oxford University Press","extern":"1","_id":"15221","page":"129-136","date_created":"2024-03-26T10:34:03Z","article_processing_charge":"No","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"publication_status":"published","issue":"1","date_updated":"2024-10-14T12:32:58Z","fulldoi":"https://doi.org/10.1093/mnras/staa3429","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","external_id":{"arxiv":["2009.00634"]},"type":"journal_article","oa_version":"Preprint","abstract":[{"lang":"eng","text":"We employ our new model for the polarized emission of accreting X-ray pulsars to describe the emission from the luminous X-ray pulsar Hercules X-1. In contrast with previous works, our model predicts the polarization parameters independently of spectral formation, and considers the structure and dynamics of the accretion column, as well as the additional effects on propagation due to general relativity and quantum electrodynamics. We find that our model can describe the observed pulse fraction and the pulse shape of the main peak, as well as the modulation of the cyclotron line with phase. We pick two geometries, assuming a single accretion column or two columns at the magnetic poles, that can describe current observations of pulse shape and cyclotron modulation with phase. Both models predict a high polarization fraction, between 60 and 80 per cent in the 1–10 keV range, that is phase and energy dependent, and that peaks at the same phase as the intensity. The phase and energy dependence of the polarization fraction and of the polarization angle can help discern between the different geometries."}],"month":"11","doi":"10.1093/mnras/staa3429","status":"public","main_file_link":[{"url":"https://doi.org/10.48550/arXiv.2009.00634","open_access":"1"}],"citation":{"mla":"Caiazzo, Ilaria, and Jeremy Heyl. “Polarization of Accreting X-Ray Pulsars – II. Hercules X-1.” Monthly Notices of the Royal Astronomical Society, vol. 501, no. 1, Oxford University Press, 2020, pp. 129–36, doi:10.1093/mnras/staa3429.","apa":"Caiazzo, I., & Heyl, J. (2020). Polarization of accreting X-ray pulsars – II. Hercules X-1. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa3429","ama":"Caiazzo I, Heyl J. Polarization of accreting X-ray pulsars – II. Hercules X-1. Monthly Notices of the Royal Astronomical Society. 2020;501(1):129-136. doi:10.1093/mnras/staa3429","chicago":"Caiazzo, Ilaria, and Jeremy Heyl. “Polarization of Accreting X-Ray Pulsars – II. Hercules X-1.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa3429.","ista":"Caiazzo I, Heyl J. 2020. Polarization of accreting X-ray pulsars – II. Hercules X-1. Monthly Notices of the Royal Astronomical Society. 501(1), 129–136.","ieee":"I. Caiazzo and J. Heyl, “Polarization of accreting X-ray pulsars – II. Hercules X-1,” Monthly Notices of the Royal Astronomical Society, vol. 501, no. 1. Oxford University Press, pp. 129–136, 2020.","short":"I. Caiazzo, J. Heyl, Monthly Notices of the Royal Astronomical Society 501 (2020) 129–136."},"date_published":"2020-11-05T00:00:00Z"},{"abstract":[{"text":"The variability of quasars across multiple wavelengths is a useful probe of physical conditions in active galactic nuclei. In particular, variable accretion rates, instabilities, and reverberation effects in the accretion disc of a supermassive black hole are expected to produce correlated flux variations in ultraviolet (UV) and optical bands. Recent work has further argued that binary quasars should exhibit strongly correlated UV and optical periodicities. Strong UV–optical correlations have indeed been established in small samples of (N ≲ 30) quasars with well-sampled light curves, and have extended the ‘bluer-when-brighter’ trend previously found within the optical bands. Here, we further test the nature of quasar variability by examining the observed-frame UV–optical correlations among bright quasars extracted from the Half Million Quasars (HMQ) catalogue. We identified a large sample of 1315 quasars in HMQ with overlapping UV and optical light curves from the Galaxy Evolution Explorer and the Catalina Real-time Transient Survey, respectively. We find that strong correlations exist in this much larger sample, but we rule out, at ∼95 per cent confidence, the simple hypothesis that the intrinsic UV and optical variations of all quasars are fully correlated. Our results therefore imply the existence of physical mechanism(s) that can generate uncorrelated optical and UV flux variations.","lang":"eng"}],"month":"05","type":"journal_article","oa_version":"Published Version","citation":{"apa":"Xin, C., Charisi, M., Haiman, Z., & Schiminovich, D. (2020). Correlation between optical and UV variability of a large sample of quasars. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa1258","mla":"Xin, Chengcheng, et al. “Correlation between Optical and UV Variability of a Large Sample of Quasars.” Monthly Notices of the Royal Astronomical Society, vol. 495, no. 1, Oxford University Press, 2020, pp. 1403–13, doi:10.1093/mnras/staa1258.","ieee":"C. Xin, M. Charisi, Z. Haiman, and D. Schiminovich, “Correlation between optical and UV variability of a large sample of quasars,” Monthly Notices of the Royal Astronomical Society, vol. 495, no. 1. Oxford University Press, pp. 1403–1413, 2020.","short":"C. Xin, M. Charisi, Z. Haiman, D. Schiminovich, Monthly Notices of the Royal Astronomical Society 495 (2020) 1403–1413.","chicago":"Xin, Chengcheng, Maria Charisi, Zoltán Haiman, and David Schiminovich. “Correlation between Optical and UV Variability of a Large Sample of Quasars.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa1258.","ista":"Xin C, Charisi M, Haiman Z, Schiminovich D. 2020. Correlation between optical and UV variability of a large sample of quasars. Monthly Notices of the Royal Astronomical Society. 495(1), 1403–1413.","ama":"Xin C, Charisi M, Haiman Z, Schiminovich D. Correlation between optical and UV variability of a large sample of quasars. Monthly Notices of the Royal Astronomical Society. 2020;495(1):1403-1413. doi:10.1093/mnras/staa1258"},"date_published":"2020-05-07T00:00:00Z","doi":"10.1093/mnras/staa1258","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/staa1258"}],"status":"public","article_processing_charge":"No","date_updated":"2024-09-11T08:08:21Z","fulldoi":"https://doi.org/10.1093/mnras/staa1258","issue":"1","publication_status":"published","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","scopus_import":"1","publisher":"Oxford University Press","publication_identifier":{"issn":["0035-8711","1365-2966"]},"author":[{"first_name":"Chengcheng","last_name":"Xin","full_name":"Xin, Chengcheng"},{"first_name":"Maria","last_name":"Charisi","full_name":"Charisi, Maria"},{"last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","first_name":"Zoltán"},{"full_name":"Schiminovich, David","last_name":"Schiminovich","first_name":"David"}],"article_type":"original","quality_controlled":"1","title":"Correlation between optical and UV variability of a large sample of quasars","_id":"17524","date_created":"2024-09-05T09:27:32Z","page":"1403-1413","extern":"1","language":[{"iso":"eng"}],"year":"2020","intvolume":" 495","oa":1,"volume":495,"publication":"Monthly Notices of the Royal Astronomical Society","day":"07"},{"date_published":"2020-10-17T00:00:00Z","citation":{"mla":"Sakurai, Yuya, et al. “Radiative Feedback for Supermassive Star Formation in a Massive Cloud with H2 Molecules in an Atomic-Cooling Halo.” Monthly Notices of the Royal Astronomical Society, vol. 499, no. 4, Oxford University Press, 2020, pp. 5960–71, doi:10.1093/mnras/staa3227.","apa":"Sakurai, Y., Haiman, Z., & Inayoshi, K. (2020). Radiative feedback for supermassive star formation in a massive cloud with H2 molecules in an atomic-cooling halo. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa3227","ista":"Sakurai Y, Haiman Z, Inayoshi K. 2020. Radiative feedback for supermassive star formation in a massive cloud with H2 molecules in an atomic-cooling halo. Monthly Notices of the Royal Astronomical Society. 499(4), 5960–5971.","chicago":"Sakurai, Yuya, Zoltán Haiman, and Kohei Inayoshi. “Radiative Feedback for Supermassive Star Formation in a Massive Cloud with H2 Molecules in an Atomic-Cooling Halo.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa3227.","ama":"Sakurai Y, Haiman Z, Inayoshi K. Radiative feedback for supermassive star formation in a massive cloud with H2 molecules in an atomic-cooling halo. Monthly Notices of the Royal Astronomical Society. 2020;499(4):5960-5971. doi:10.1093/mnras/staa3227","ieee":"Y. Sakurai, Z. Haiman, and K. Inayoshi, “Radiative feedback for supermassive star formation in a massive cloud with H2 molecules in an atomic-cooling halo,” Monthly Notices of the Royal Astronomical Society, vol. 499, no. 4. Oxford University Press, pp. 5960–5971, 2020.","short":"Y. Sakurai, Z. Haiman, K. Inayoshi, Monthly Notices of the Royal Astronomical Society 499 (2020) 5960–5971."},"main_file_link":[{"url":"https://doi.org/10.1093/mnras/staa3227","open_access":"1"}],"status":"public","doi":"10.1093/mnras/staa3227","month":"10","abstract":[{"lang":"eng","text":"Recent three-dimensional cosmological simulations of protogalaxy formation have suggested that supermassive stars (SMSs) can form in gas clouds in which H2 cooling is suppressed by dynamical heating prior to the activation of atomic cooling (Wise et al. 2019), but they stopped short of the following growth of a central protostar. Here we examine whether accretion on the protostellar core in this cloud is sufficiently rapid, in the face of the radiation feedback, to produce a SMS. We perform one-dimensional radiation-hydrodynamical simulations of the hot collapsing cloud with non-equilibrium chemical reactions directly adopting the cloud properties from Wise et al. (2019) as an initial condition. We find that the stellar Lyman-Werner (LW) radiation from the SMS dissociates H2 in the inner regions of the gas flow, increasing gas temperature and thermal pressure, and temporarily stopping the accretion. However, this negative feedback ceases when the self-gravity and inward ram pressure force on larger scales push the gas inward. The central protostar is unable to expand an HII region due to the high density, and grows to a mass of ≳105M⊙. Our results suggests the successful formation of SMSs, and resulting massive (∼105M⊙) remnant black holes in the clouds, but need to be confirmed in two- or three-dimensional simulations."}],"oa_version":"Published Version","type":"journal_article","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_updated":"2024-09-12T09:39:27Z","fulldoi":"https://doi.org/10.1093/mnras/staa3227","publication_status":"published","issue":"4","article_processing_charge":"No","_id":"17538","date_created":"2024-09-05T09:51:17Z","page":"5960-5971","extern":"1","publisher":"Oxford University Press","publication_identifier":{"issn":["0035-8711","1365-2966"]},"scopus_import":"1","quality_controlled":"1","title":"Radiative feedback for supermassive star formation in a massive cloud with H2 molecules in an atomic-cooling halo","article_type":"original","author":[{"last_name":"Sakurai","full_name":"Sakurai, Yuya","first_name":"Yuya"},{"first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","last_name":"Haiman"},{"last_name":"Inayoshi","full_name":"Inayoshi, Kohei","first_name":"Kohei"}],"volume":499,"publication":"Monthly Notices of the Royal Astronomical Society","day":"17","year":"2020","language":[{"iso":"eng"}],"oa":1,"intvolume":" 499"},{"_id":"17540","date_created":"2024-09-05T09:55:24Z","page":"3540-3557","extern":"1","quality_controlled":"1","title":"Evolution of gas disc–embedded intermediate mass ratio inspirals in the LISA band","article_type":"original","author":[{"last_name":"Derdzinski","full_name":"Derdzinski, A","first_name":"A"},{"first_name":"D","last_name":"D’Orazio","full_name":"D’Orazio, D"},{"last_name":"Duffell","full_name":"Duffell, P","first_name":"P"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"},{"last_name":"MacFadyen","full_name":"MacFadyen, A","first_name":"A"}],"publisher":"Oxford University Press","publication_identifier":{"issn":["0035-8711","1365-2966"]},"scopus_import":"1","day":"29","publication":"Monthly Notices of the Royal Astronomical Society","volume":501,"oa":1,"intvolume":" 501","year":"2020","language":[{"iso":"eng"}],"main_file_link":[{"url":"https://doi.org/10.1093/mnras/staa3976","open_access":"1"}],"status":"public","doi":"10.1093/mnras/staa3976","date_published":"2020-12-29T00:00:00Z","citation":{"mla":"Derdzinski, A., et al. “Evolution of Gas Disc–Embedded Intermediate Mass Ratio Inspirals in the LISA Band.” Monthly Notices of the Royal Astronomical Society, vol. 501, no. 3, Oxford University Press, 2020, pp. 3540–57, doi:10.1093/mnras/staa3976.","apa":"Derdzinski, A., D’Orazio, D., Duffell, P., Haiman, Z., & MacFadyen, A. (2020). Evolution of gas disc–embedded intermediate mass ratio inspirals in the LISA band. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa3976","ama":"Derdzinski A, D’Orazio D, Duffell P, Haiman Z, MacFadyen A. Evolution of gas disc–embedded intermediate mass ratio inspirals in the LISA band. Monthly Notices of the Royal Astronomical Society. 2020;501(3):3540-3557. doi:10.1093/mnras/staa3976","ista":"Derdzinski A, D’Orazio D, Duffell P, Haiman Z, MacFadyen A. 2020. Evolution of gas disc–embedded intermediate mass ratio inspirals in the LISA band. Monthly Notices of the Royal Astronomical Society. 501(3), 3540–3557.","chicago":"Derdzinski, A, D D’Orazio, P Duffell, Zoltán Haiman, and A MacFadyen. “Evolution of Gas Disc–Embedded Intermediate Mass Ratio Inspirals in the LISA Band.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa3976.","ieee":"A. Derdzinski, D. D’Orazio, P. Duffell, Z. Haiman, and A. MacFadyen, “Evolution of gas disc–embedded intermediate mass ratio inspirals in the LISA band,” Monthly Notices of the Royal Astronomical Society, vol. 501, no. 3. Oxford University Press, pp. 3540–3557, 2020.","short":"A. Derdzinski, D. D’Orazio, P. Duffell, Z. Haiman, A. MacFadyen, Monthly Notices of the Royal Astronomical Society 501 (2020) 3540–3557."},"oa_version":"Published Version","type":"journal_article","month":"12","abstract":[{"lang":"eng","text":"Among the potential milliHz gravitational wave (GW) sources for the upcoming space-based interferometer LISA are extreme- or intermediate-mass ratio inspirals (EMRI/IMRIs). These events involve the coalescence of supermassive black holes in the mass range 105M⊙≲M≲107M⊙ with companion BHs of much lower masses. A subset of E/IMRIs are expected to occur in the accretion discs of active galactic nuclei (AGN), where torques exerted by the disc can interfere with the inspiral and cause a phase shift in the GW waveform. Here we use a suite of two-dimensional hydrodynamical simulations with the moving-mesh code DISCO to present a systematic study of disc torques. We measure torques on an inspiraling BH and compute the corresponding waveform deviations as a function of the binary mass ratio q≡M2/M1, the disc viscosity (α), and gas temperature (or equivalently Mach number; M). We find that the absolute value of the gas torques is within an order of magnitude of previously determined planetary migration torques, but their precise value and sign depends non-trivially on the combination of these parameters. The gas imprint is detectable by LISA for binaries embedded in AGN discs with surface densities above Σ0≥104−6gcm−2, depending on q, α and M. Deviations are most pronounced in discs with higher viscosities, and for E/IMRIs detected at frequencies where LISA is most sensitive. Torques in colder discs exhibit a noticeable dependence on the GW-driven inspiral rate as well as strong fluctuations at late stages of the inspiral. Our results further suggest that LISA may be able to place constraints on AGN disc parameters and the physics of disc-satellite interaction."}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_updated":"2024-09-12T09:54:26Z","fulldoi":"https://doi.org/10.1093/mnras/staa3976","publication_status":"published","issue":"3","article_processing_charge":"No"},{"article_processing_charge":"No","fulldoi":"https://doi.org/10.1093/mnras/staa1312","date_updated":"2024-09-18T10:14:15Z","issue":"4","publication_status":"published","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","type":"journal_article","oa_version":"Published Version","abstract":[{"lang":"eng","text":"We examine the light curves of two quasars, motivated by recent suggestions that a supermassive black hole binary (SMBHB) can exhibit sharp lensing spikes. We model the variability of each light curve as due to a combination of two relativistic effects: the orbital relativistic Doppler boost and gravitational binary self-lensing. In order to model each system we extend previous Doppler plus self-lensing models to include eccentricity. The first quasar is identified in optical data as a binary candidate with a 20-yr period (Ark 120), and shows a prominent spike. For this source, we rule out the lensing hypothesis and disfavor the Doppler-boost hypothesis due to discrepancies in the measured vs. recovered values of the binary mass and optical spectral slope. The second source, which we nickname Spikey, is the rare case of an active galactic nucleus (AGN) identified in Kepler's high-quality, high-cadence photometric data. For this source, we find a model, consisting of a combination of a Doppler modulation and a narrow symmetric lensing spike, consistent with an eccentric SMBHB with a total mass of approximately 30 million solar masses, rest-frame orbital period T=418 days, eccentricity e=0.5, and seen at an inclination of 8 degrees from edge-on. This interpretation can be tested by monitoring Spikey for periodic behavior and recurring flares in the next few years. In preparation for such monitoring we present the first X-ray observations of this object taken by the Neil Gehrels Swift observatory."}],"month":"05","doi":"10.1093/mnras/staa1312","main_file_link":[{"url":"https://doi.org/10.1093/mnras/staa1312","open_access":"1"}],"status":"public","citation":{"apa":"Hu, B. X., D’Orazio, D. J., Haiman, Z., Smith, K. L., Snios, B., Charisi, M., & Di Stefano, R. (2020). Spikey: self-lensing flares from eccentric SMBH binaries. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/staa1312","mla":"Hu, Betty X., et al. “Spikey: Self-Lensing Flares from Eccentric SMBH Binaries.” Monthly Notices of the Royal Astronomical Society, vol. 495, no. 4, Oxford University Press, 2020, pp. 4061–70, doi:10.1093/mnras/staa1312.","short":"B.X. Hu, D.J. D’Orazio, Z. Haiman, K.L. Smith, B. Snios, M. Charisi, R. Di Stefano, Monthly Notices of the Royal Astronomical Society 495 (2020) 4061–4070.","ieee":"B. X. Hu et al., “Spikey: self-lensing flares from eccentric SMBH binaries,” Monthly Notices of the Royal Astronomical Society, vol. 495, no. 4. Oxford University Press, pp. 4061–4070, 2020.","ista":"Hu BX, D’Orazio DJ, Haiman Z, Smith KL, Snios B, Charisi M, Di Stefano R. 2020. Spikey: self-lensing flares from eccentric SMBH binaries. Monthly Notices of the Royal Astronomical Society. 495(4), 4061–4070.","chicago":"Hu, Betty X, Daniel J D’Orazio, Zoltán Haiman, Krista Lynne Smith, Bradford Snios, Maria Charisi, and Rosanne Di Stefano. “Spikey: Self-Lensing Flares from Eccentric SMBH Binaries.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2020. https://doi.org/10.1093/mnras/staa1312.","ama":"Hu BX, D’Orazio DJ, Haiman Z, et al. Spikey: self-lensing flares from eccentric SMBH binaries. Monthly Notices of the Royal Astronomical Society. 2020;495(4):4061-4070. doi:10.1093/mnras/staa1312"},"date_published":"2020-05-11T00:00:00Z","intvolume":" 495","oa":1,"language":[{"iso":"eng"}],"year":"2020","day":"11","publication":"Monthly Notices of the Royal Astronomical Society","volume":495,"author":[{"last_name":"Hu","full_name":"Hu, Betty X","first_name":"Betty X"},{"full_name":"D’Orazio, Daniel J","last_name":"D’Orazio","first_name":"Daniel J"},{"first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","full_name":"Haiman, Zoltán"},{"first_name":"Krista Lynne","last_name":"Smith","full_name":"Smith, Krista Lynne"},{"first_name":"Bradford","full_name":"Snios, Bradford","last_name":"Snios"},{"last_name":"Charisi","full_name":"Charisi, Maria","first_name":"Maria"},{"last_name":"Di Stefano","full_name":"Di Stefano, Rosanne","first_name":"Rosanne"}],"article_type":"original","quality_controlled":"1","title":"Spikey: self-lensing flares from eccentric SMBH binaries","scopus_import":"1","publisher":"Oxford University Press","publication_identifier":{"issn":["0035-8711","1365-2966"]},"_id":"17552","page":"4061-4070","date_created":"2024-09-05T10:16:03Z","extern":"1"}]