[{"doi":"10.1086/322310","volume":558,"oa":1,"day":"10","month":"09","publisher":"American Astronomical Society","external_id":{"arxiv":["astro-ph/0101196"]},"article_processing_charge":"No","date_published":"2001-09-10T00:00:00Z","arxiv":1,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.astro-ph/0101196"}],"fulldoi":"https://doi.org/10.1086/322310","intvolume":"       558","year":"2001","quality_controlled":"1","publication_status":"published","OA_place":"repository","OA_type":"green","language":[{"iso":"eng"}],"issue":"2","scopus_import":"1","publication":"The Astrophysical Journal","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"citation":{"mla":"Menou, Kristen, et al. “The Merger History of Supermassive Black Holes in Galaxies.” <i>The Astrophysical Journal</i>, vol. 558, no. 2, American Astronomical Society, 2001, pp. 535–42, doi:<a href=\"https://doi.org/10.1086/322310\">10.1086/322310</a>.","ama":"Menou K, Haiman Z, Narayanan VK. The merger history of supermassive black holes in galaxies. <i>The Astrophysical Journal</i>. 2001;558(2):535-542. doi:<a href=\"https://doi.org/10.1086/322310\">10.1086/322310</a>","ista":"Menou K, Haiman Z, Narayanan VK. 2001. The merger history of supermassive black holes in galaxies. The Astrophysical Journal. 558(2), 535–542.","ieee":"K. Menou, Z. Haiman, and V. K. Narayanan, “The merger history of supermassive black holes in galaxies,” <i>The Astrophysical Journal</i>, vol. 558, no. 2. American Astronomical Society, pp. 535–542, 2001.","short":"K. Menou, Z. Haiman, V.K. Narayanan, The Astrophysical Journal 558 (2001) 535–542.","chicago":"Menou, Kristen, Zoltán Haiman, and Vijay K. Narayanan. “The Merger History of Supermassive Black Holes in Galaxies.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2001. <a href=\"https://doi.org/10.1086/322310\">https://doi.org/10.1086/322310</a>.","apa":"Menou, K., Haiman, Z., &#38; Narayanan, V. K. (2001). The merger history of supermassive black holes in galaxies. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/322310\">https://doi.org/10.1086/322310</a>"},"page":"535-542","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2024-11-12T12:47:14Z","status":"public","author":[{"last_name":"Menou","first_name":"Kristen","full_name":"Menou, Kristen"},{"last_name":"Haiman","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403"},{"last_name":"Narayanan","first_name":"Vijay K.","full_name":"Narayanan, Vijay K."}],"date_created":"2024-09-06T11:57:11Z","_id":"17824","title":"The merger history of supermassive black holes in galaxies","abstract":[{"text":"The ubiquity of supermassive black holes (SMBHs) at the centers of nearby luminous galaxies can arise from the multiple mergers experienced by dark matter halos in hierarchical structure formation models, even if only a small fraction of these galaxies harbor SMBHs at high redshifts. We illustrate this possibility using cosmological Monte Carlo simulations of the merger history of dark matter halos and their associated SMBHs. In our most extreme models, in order to populate nearly every bright galaxy with an SMBH at z = 0, only a few percent of the halos with virial temperatures above 104 K are required to harbor an SMBH at high redshift. This possibility must be included in studies of the luminosity function and the clustering properties of quasars. We predict the number of SMBH merger events that are detectable by the gravitational wave experiment Laser Interferometer Space Antenna (LISA), as a function of redshift, out to z = 5. Although the event rates can be significantly reduced in scenarios with rare SMBHs, a minimum of ~10 detectable merger events per year is predicted if SMBH binaries coalesce efficiently. The observed distribution of events with redshift could yield valuable information on the SMBH formation process. If SMBH binaries do not coalesce, we find that at least several SMBH slingshot ejections probably occurred from z = 5 to the present in each galaxy more massive than ~1011 M☉ at z = 0. Although our results are sensitive to the minimum cooling mass assumed for the formation of SMBHs, we expect the qualitative predictions of our models to be robust.","lang":"eng"}],"extern":"1","article_type":"original","type":"journal_article","oa_version":"Preprint"},{"publication_status":"published","quality_controlled":"1","year":"2001","intvolume":"       553","fulldoi":"https://doi.org/10.1086/320650","main_file_link":[{"url":"https://doi.org/10.48550/arXiv.astro-ph/0007351","open_access":"1"}],"arxiv":1,"date_published":"2001-05-20T00:00:00Z","article_processing_charge":"No","external_id":{"arxiv":["astro-ph/0007351"]},"publisher":"American Astronomical Society","month":"05","day":"20","oa":1,"volume":553,"doi":"10.1086/320650","oa_version":"Preprint","type":"journal_article","article_type":"original","extern":"1","abstract":[{"lang":"eng","text":"The hardness of the ionizing continuum from the first sources of UV radiation plays a crucial role in the reionization of the intergalactic medium (IGM). While usual stellar populations have soft spectra, miniquasars or metal-free stars with high effective temperatures may emit hard photons, capable of doubly ionizing helium and increasing the IGM temperature. Absorption within the source and in the intervening IGM will render the ionizing continuum of high-redshift sources inaccessible to direct observation. Here we show that He recombination lines from the first luminous objects are potentially detectable by the Next Generation Space Telescope. Together with measurements of the Hα emission line, this detection can be used to infer the ratio of He II to H I ionizing photons, [mathematical formula]. A measurement of this ratio would shed light on the nature and emission mechanism of the first luminous sources, with important astrophysical consequences for the reheating and reionization of the IGM."}],"title":"He II recombination lines from the first luminous objects","_id":"17826","author":[{"full_name":"Oh, S. Peng","first_name":"S. Peng","last_name":"Oh"},{"orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman"},{"full_name":"Rees, Martin J.","last_name":"Rees","first_name":"Martin J."}],"status":"public","date_created":"2024-09-06T11:58:39Z","date_updated":"2024-11-12T12:54:57Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"73-77","citation":{"apa":"Oh, S. P., Haiman, Z., &#38; Rees, M. J. (2001). He II recombination lines from the first luminous objects. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/320650\">https://doi.org/10.1086/320650</a>","chicago":"Oh, S. Peng, Zoltán Haiman, and Martin J. Rees. “He II Recombination Lines from the First Luminous Objects.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2001. <a href=\"https://doi.org/10.1086/320650\">https://doi.org/10.1086/320650</a>.","ista":"Oh SP, Haiman Z, Rees MJ. 2001. He II recombination lines from the first luminous objects. The Astrophysical Journal. 553(1), 73–77.","ieee":"S. P. Oh, Z. Haiman, and M. J. Rees, “He II recombination lines from the first luminous objects,” <i>The Astrophysical Journal</i>, vol. 553, no. 1. American Astronomical Society, pp. 73–77, 2001.","short":"S.P. Oh, Z. Haiman, M.J. Rees, The Astrophysical Journal 553 (2001) 73–77.","ama":"Oh SP, Haiman Z, Rees MJ. He II recombination lines from the first luminous objects. <i>The Astrophysical Journal</i>. 2001;553(1):73-77. doi:<a href=\"https://doi.org/10.1086/320650\">10.1086/320650</a>","mla":"Oh, S. Peng, et al. “He II Recombination Lines from the First Luminous Objects.” <i>The Astrophysical Journal</i>, vol. 553, no. 1, American Astronomical Society, 2001, pp. 73–77, doi:<a href=\"https://doi.org/10.1086/320650\">10.1086/320650</a>."},"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"publication":"The Astrophysical Journal","scopus_import":"1","issue":"1","language":[{"iso":"eng"}],"OA_type":"green","OA_place":"repository"},{"publisher":"American Astronomical Society","month":"07","external_id":{"arxiv":["astro-ph/0101174"]},"oa":1,"day":"01","doi":"10.1086/321567","volume":556,"intvolume":"       556","publication_status":"published","year":"2001","quality_controlled":"1","main_file_link":[{"url":"https://doi.org/10.48550/arXiv.astro-ph/0101174","open_access":"1"}],"arxiv":1,"fulldoi":"https://doi.org/10.1086/321567","article_processing_charge":"No","date_published":"2001-07-01T00:00:00Z","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"scopus_import":"1","issue":"1","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"OA_place":"repository","OA_type":"green","extern":"1","abstract":[{"text":"The early stage in the formation of a galaxy inevitably involves a spatially extended distribution of infalling, cold gas. If a central luminous quasar turned on during this phase, it would result in significant extended Lyα emission, possibly accompanied by other lines. For halos condensing at redshifts 3 ≲ z ≲ 8 and having virial temperatures 2 × 105 K ≲ Tvir ≲ 2 × 106 K, this emission results in a \"fuzz\" of characteristic angular diameter of a few arcseconds and surface brightness ~10-18 to 10-16 ergs s-1 cm-2 arcsec-2. The fuzz around bright, high-redshift quasars could be detected in deep narrowband imaging with current telescopes, providing a direct constraint on galaxy formation models. The absence of detectable fuzz might suggest that most of the protogalaxy's gas settles to a self-gravitating disk before a quasar turns on. However, continued gas infall from large radii, or an on-going merger spreading cold gas over a large solid angle, during the luminous quasar phase could also result in extended Lyα emission, and can be constrained by deep narrowband imaging.","lang":"eng"}],"type":"journal_article","oa_version":"Preprint","article_type":"original","date_created":"2024-09-06T12:09:20Z","author":[{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403"},{"full_name":"Rees, Martin J.","last_name":"Rees","first_name":"Martin J."}],"status":"public","title":"Extended Lyα emission around young quasars: A constraint on galaxy formation","_id":"17829","date_updated":"2024-11-13T07:17:10Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"chicago":"Haiman, Zoltán, and Martin J. Rees. “Extended Lyα Emission around Young Quasars: A Constraint on Galaxy Formation.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2001. <a href=\"https://doi.org/10.1086/321567\">https://doi.org/10.1086/321567</a>.","apa":"Haiman, Z., &#38; Rees, M. J. (2001). Extended Lyα emission around young quasars: A constraint on galaxy formation. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/321567\">https://doi.org/10.1086/321567</a>","mla":"Haiman, Zoltán, and Martin J. Rees. “Extended Lyα Emission around Young Quasars: A Constraint on Galaxy Formation.” <i>The Astrophysical Journal</i>, vol. 556, no. 1, American Astronomical Society, 2001, pp. 87–92, doi:<a href=\"https://doi.org/10.1086/321567\">10.1086/321567</a>.","ama":"Haiman Z, Rees MJ. Extended Lyα emission around young quasars: A constraint on galaxy formation. <i>The Astrophysical Journal</i>. 2001;556(1):87-92. doi:<a href=\"https://doi.org/10.1086/321567\">10.1086/321567</a>","short":"Z. Haiman, M.J. Rees, The Astrophysical Journal 556 (2001) 87–92.","ista":"Haiman Z, Rees MJ. 2001. Extended Lyα emission around young quasars: A constraint on galaxy formation. The Astrophysical Journal. 556(1), 87–92.","ieee":"Z. Haiman and M. J. Rees, “Extended Lyα emission around young quasars: A constraint on galaxy formation,” <i>The Astrophysical Journal</i>, vol. 556, no. 1. American Astronomical Society, pp. 87–92, 2001."},"page":"87-92"},{"citation":{"ieee":"Z. Haiman and A. Loeb, “What is the highest plausible redshift of luminous quasars?,” <i>The Astrophysical Journal</i>, vol. 552, no. 2. American Astronomical Society, pp. 459–463, 2001.","short":"Z. Haiman, A. Loeb, The Astrophysical Journal 552 (2001) 459–463.","ista":"Haiman Z, Loeb A. 2001. What is the highest plausible redshift of luminous quasars? The Astrophysical Journal. 552(2), 459–463.","mla":"Haiman, Zoltán, and Abraham Loeb. “What Is the Highest Plausible Redshift of Luminous Quasars?” <i>The Astrophysical Journal</i>, vol. 552, no. 2, American Astronomical Society, 2001, pp. 459–63, doi:<a href=\"https://doi.org/10.1086/320586\">10.1086/320586</a>.","ama":"Haiman Z, Loeb A. What is the highest plausible redshift of luminous quasars? <i>The Astrophysical Journal</i>. 2001;552(2):459-463. doi:<a href=\"https://doi.org/10.1086/320586\">10.1086/320586</a>","apa":"Haiman, Z., &#38; Loeb, A. (2001). What is the highest plausible redshift of luminous quasars? <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/320586\">https://doi.org/10.1086/320586</a>","chicago":"Haiman, Zoltán, and Abraham Loeb. “What Is the Highest Plausible Redshift of Luminous Quasars?” <i>The Astrophysical Journal</i>. American Astronomical Society, 2001. <a href=\"https://doi.org/10.1086/320586\">https://doi.org/10.1086/320586</a>."},"page":"459-463","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2024-11-13T07:21:28Z","_id":"17831","title":"What is the highest plausible redshift of luminous quasars?","author":[{"first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán"},{"first_name":"Abraham","last_name":"Loeb","full_name":"Loeb, Abraham"}],"date_created":"2024-09-06T12:10:38Z","status":"public","article_type":"original","oa_version":"Preprint","type":"journal_article","extern":"1","abstract":[{"text":"The recent discoveries of luminous quasars at high redshifts imply that black holes more massive than a few billion solar masses were already assembled when the universe was less than a billion years old. We show that the existence of these black holes is not surprising in popular hierarchical models of structure formation. For example, the black hole needed to power the quasar SDSS 1044-0125 at z = 5.8 could arise naturally from the growth of stellar-mass seeds forming at z > 10, when typical values are assumed for the radiative accretion efficiency (~0.1) and the bolometric accretion luminosity in Eddington units (~1). Nevertheless, SDSS 1044-0125 yields a nontrivial constraint on a combination of these parameters. Extrapolating our model to future surveys, we derive the highest plausible redshift for quasars that are not lensed or beamed, as a function of their apparent magnitude. We find that at a limiting magnitude of K ~ 20, quasar surveys can yield strong constraints on the growth of supermassive black holes out to z ~ 10.","lang":"eng"}],"OA_type":"green","OA_place":"repository","language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","issue":"2","scopus_import":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"date_published":"2001-05-10T00:00:00Z","article_processing_charge":"No","fulldoi":"https://doi.org/10.1086/320586","arxiv":1,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.astro-ph/0011529"}],"year":"2001","quality_controlled":"1","publication_status":"published","intvolume":"       552","volume":552,"doi":"10.1086/320586","day":"10","oa":1,"external_id":{"arxiv":["astro-ph/0011529"]},"month":"05","publisher":"American Astronomical Society"},{"volume":558,"doi":"10.1086/322393","external_id":{"arxiv":["astro-ph/0102304"]},"publisher":"American Astronomical Society","month":"09","day":"10","oa":1,"fulldoi":"https://doi.org/10.1086/322393","main_file_link":[{"url":"https://doi.org/10.48550/arXiv.astro-ph/0102304","open_access":"1"}],"arxiv":1,"date_published":"2001-09-10T00:00:00Z","article_processing_charge":"No","publication_status":"published","quality_controlled":"1","year":"2001","intvolume":"       558","language":[{"iso":"eng"}],"OA_place":"repository","OA_type":"green","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"publication":"The Astrophysical Journal","scopus_import":"1","issue":"2","date_updated":"2024-11-13T07:23:48Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","citation":{"ista":"Barkana R, Haiman Z, Ostriker JP. 2001. Constraints on warm dark matter from cosmological reionization. The Astrophysical Journal. 558(2), 482–496.","ieee":"R. Barkana, Z. Haiman, and J. P. Ostriker, “Constraints on warm dark matter from cosmological reionization,” <i>The Astrophysical Journal</i>, vol. 558, no. 2. American Astronomical Society, pp. 482–496, 2001.","short":"R. Barkana, Z. Haiman, J.P. Ostriker, The Astrophysical Journal 558 (2001) 482–496.","ama":"Barkana R, Haiman Z, Ostriker JP. Constraints on warm dark matter from cosmological reionization. <i>The Astrophysical Journal</i>. 2001;558(2):482-496. doi:<a href=\"https://doi.org/10.1086/322393\">10.1086/322393</a>","mla":"Barkana, Rennan, et al. “Constraints on Warm Dark Matter from Cosmological Reionization.” <i>The Astrophysical Journal</i>, vol. 558, no. 2, American Astronomical Society, 2001, pp. 482–96, doi:<a href=\"https://doi.org/10.1086/322393\">10.1086/322393</a>.","apa":"Barkana, R., Haiman, Z., &#38; Ostriker, J. P. (2001). Constraints on warm dark matter from cosmological reionization. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/322393\">https://doi.org/10.1086/322393</a>","chicago":"Barkana, Rennan, Zoltán Haiman, and Jeremiah P. Ostriker. “Constraints on Warm Dark Matter from Cosmological Reionization.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2001. <a href=\"https://doi.org/10.1086/322393\">https://doi.org/10.1086/322393</a>."},"page":"482-496","oa_version":"Preprint","type":"journal_article","article_type":"original","abstract":[{"lang":"eng","text":"We study the constraints that high-redshift structure formation in the universe places on warm dark matter (WDM) dominated cosmological models. We modify the extended Press-Schechter formalism to derive the halo mass function in WDM models. We show that our predictions agree with recent numerical simulations at low redshift over the halo masses of interest. Applying our model to galaxy formation at high redshift, we find that the loss of power on small scales, together with the delayed collapse of low-mass objects, results in strong limits on the root-mean-square velocity dispersion vrms,0 of the WDM particles at redshift zero. For fermions decoupling while relativistic, these limits are equivalent to constraints on the mass mX of the particles. The presence of a ≈4 × 109 M☉ supermassive black hole at redshift 5.8, believed to power the quasar SDSS 1044-1215, implies mX ≳ 0.5 keV (or vrms,0 ≲ 0.10 km s-1), assuming that the quasar is unlensed and radiating at or below the Eddington limit. Reionization by redshift 5.8 also implies a limit on mX. If high-redshift galaxies produce ionizing photons with an efficiency similar to their redshift-three counterparts, we find mX ≳ 1.2 keV (or vrms,0 ≲ 0.03 s-1). However, given the uncertainties in current measurements from the proximity effect of the ionizing background at redshift three, values of mX as low as 0.75 keV (or vrms,0 = 0.06 s-1) are not ruled out. The limit weakens further to mX ≳ 0.4 keV (or vrms,0 ≲ 0.14 s-1), if, instead, the ionizing-photon production efficiency is 10 times greater at high redshift, but this limit will tighten considerably if reionization is shown in the future to have occurred at higher redshifts. WDM models with mX ≲ 1 keV (or vrms,0 ≳ 0.04 s-1) produce a low-luminosity cutoff in the high-redshift galaxy luminosity function that is directly detectable with the Next Generation Space Telescope, and which serves as a direct constraint on mX."}],"extern":"1","title":"Constraints on warm dark matter from cosmological reionization","_id":"17832","author":[{"last_name":"Barkana","first_name":"Rennan","full_name":"Barkana, Rennan"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán","full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403"},{"first_name":"Jeremiah P.","last_name":"Ostriker","full_name":"Ostriker, Jeremiah P."}],"date_created":"2024-09-06T12:11:23Z","status":"public"},{"citation":{"ista":"Knox L, Cooray A, Eisenstein D, Haiman Z. 2001. Probing early structure formation with far‐infrared background correlations. The Astrophysical Journal. 550(1), 7–20.","short":"L. Knox, A. Cooray, D. Eisenstein, Z. Haiman, The Astrophysical Journal 550 (2001) 7–20.","ieee":"L. Knox, A. Cooray, D. Eisenstein, and Z. Haiman, “Probing early structure formation with far‐infrared background correlations,” <i>The Astrophysical Journal</i>, vol. 550, no. 1. American Astronomical Society, pp. 7–20, 2001.","ama":"Knox L, Cooray A, Eisenstein D, Haiman Z. Probing early structure formation with far‐infrared background correlations. <i>The Astrophysical Journal</i>. 2001;550(1):7-20. doi:<a href=\"https://doi.org/10.1086/319732\">10.1086/319732</a>","mla":"Knox, Lloyd, et al. “Probing Early Structure Formation with Far‐infrared Background Correlations.” <i>The Astrophysical Journal</i>, vol. 550, no. 1, American Astronomical Society, 2001, pp. 7–20, doi:<a href=\"https://doi.org/10.1086/319732\">10.1086/319732</a>.","apa":"Knox, L., Cooray, A., Eisenstein, D., &#38; Haiman, Z. (2001). Probing early structure formation with far‐infrared background correlations. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/319732\">https://doi.org/10.1086/319732</a>","chicago":"Knox, Lloyd, Asantha Cooray, Daniel Eisenstein, and Zoltán Haiman. “Probing Early Structure Formation with Far‐infrared Background Correlations.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2001. <a href=\"https://doi.org/10.1086/319732\">https://doi.org/10.1086/319732</a>."},"page":"7-20","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2024-11-13T07:46:11Z","_id":"17840","title":"Probing early structure formation with far‐infrared background correlations","author":[{"full_name":"Knox, Lloyd","last_name":"Knox","first_name":"Lloyd"},{"full_name":"Cooray, Asantha","first_name":"Asantha","last_name":"Cooray"},{"first_name":"Daniel","last_name":"Eisenstein","full_name":"Eisenstein, Daniel"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán","full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403"}],"status":"public","date_created":"2024-09-06T12:17:01Z","article_type":"original","type":"journal_article","oa_version":"Preprint","extern":"1","abstract":[{"lang":"eng","text":"The large-scale structure of high-redshift galaxies produces correlated anisotropy in the far-infrared background (FIRB). In regions of the sky where the thermal emission from Galactic dust is well below average, these high-redshift correlations may be the most significant source of angular fluctuation power over a wide range of angular scales, from ~7' to ~3°, and frequencies, from ~400 to ~1000 GHz. The strength of this signal should allow detailed studies of the statistics of the FIRB fluctuations, including the shape of the angular power spectrum at a given frequency and the degree of coherence between FIRB maps at different frequencies. The FIRB correlations depend on and hence constrain the redshift-dependent spectral energy distributions, number counts, and clustering bias of the galaxies and active nuclei that contribute to the background. We quantify the accuracy to which Planck and a newly proposed balloon-borne mission, Explorer of Diffuse Galactic Emissions, could constrain models of the high-redshift universe through the measurement of FIRB fluctuations. We conclude that the average bias of high-redshift galaxies could be measured to an accuracy of ≲1% or, for example, separated into four redshift bins with ~10% accuracy."}],"OA_place":"repository","OA_type":"green","language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","issue":"1","scopus_import":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"date_published":"2001-03-20T00:00:00Z","article_processing_charge":"No","fulldoi":"https://doi.org/10.1086/319732","arxiv":1,"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.astro-ph/0009151","open_access":"1"}],"year":"2001","quality_controlled":"1","publication_status":"published","intvolume":"       550","volume":550,"doi":"10.1086/319732","day":"20","oa":1,"external_id":{"arxiv":["astro-ph/0009151"]},"month":"03","publisher":"American Astronomical Society"},{"language":[{"iso":"eng"}],"OA_place":"repository","OA_type":"green","publication_identifier":{"issn":["0004-637X"]},"publication":"The Astrophysical Journal","scopus_import":"1","issue":"2","date_updated":"2024-11-13T07:48:32Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","page":"L111-L114","citation":{"short":"G. Holder, Z. Haiman, J.J. Mohr, The Astrophysical Journal 560 (2001) L111–L114.","ista":"Holder G, Haiman Z, Mohr JJ. 2001. Constraints on Ωm, ΩΛ, and σ8 from galaxy cluster redshift distributions. The Astrophysical Journal. 560(2), L111–L114.","ieee":"G. Holder, Z. Haiman, and J. J. Mohr, “Constraints on Ωm, ΩΛ, and σ8 from galaxy cluster redshift distributions,” <i>The Astrophysical Journal</i>, vol. 560, no. 2. American Astronomical Society, pp. L111–L114, 2001.","ama":"Holder G, Haiman Z, Mohr JJ. Constraints on Ωm, ΩΛ, and σ8 from galaxy cluster redshift distributions. <i>The Astrophysical Journal</i>. 2001;560(2):L111-L114. doi:<a href=\"https://doi.org/10.1086/324309\">10.1086/324309</a>","mla":"Holder, Gilbert, et al. “Constraints on Ωm, ΩΛ, and Σ8 from Galaxy Cluster Redshift Distributions.” <i>The Astrophysical Journal</i>, vol. 560, no. 2, American Astronomical Society, 2001, pp. L111–14, doi:<a href=\"https://doi.org/10.1086/324309\">10.1086/324309</a>.","apa":"Holder, G., Haiman, Z., &#38; Mohr, J. J. (2001). Constraints on Ωm, ΩΛ, and σ8 from galaxy cluster redshift distributions. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/324309\">https://doi.org/10.1086/324309</a>","chicago":"Holder, Gilbert, Zoltán Haiman, and Joseph J. Mohr. “Constraints on Ωm, ΩΛ, and Σ8 from Galaxy Cluster Redshift Distributions.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2001. <a href=\"https://doi.org/10.1086/324309\">https://doi.org/10.1086/324309</a>."},"oa_version":"Preprint","type":"journal_article","article_type":"original","abstract":[{"lang":"eng","text":"We show that the number and redshift distribution of galaxy clusters in future deep cluster surveys can place strong constraints on the matter density, Ωm, the vacuum energy density, ΩΛ, and the normalization of the matter power spectrum, σ8. Degeneracies between these parameters are different from those in studies of either high-redshift Type Ia supernovae or cosmic microwave background anisotropies. Using a mass threshold for cluster detection expected to be typical for upcoming Sunyaev-Zeldovich effect surveys, we find that constraints on Ωm and σ8 at the level of roughly 5% or better can be expected, assuming redshift information is known at least to z ~ 0.5 and in the absence of significant systematic errors. Without information past this redshift, ΩΛ is constrained to 25%. With complete redshift information, deep (Mlim ~ 1014 h-1 M☉), relatively small solid angle (~12 deg 2) surveys can further constrain ΩΛ to an accuracy of ~15%, while large solid angle surveys with ground-based, large-format bolometer arrays could measure ΩΛ to a precision of ~4% or better."}],"extern":"1","title":"Constraints on Ωm, ΩΛ, and σ8 from galaxy cluster redshift distributions","_id":"17846","status":"public","author":[{"full_name":"Holder, Gilbert","first_name":"Gilbert","last_name":"Holder"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403"},{"first_name":"Joseph J.","last_name":"Mohr","full_name":"Mohr, Joseph J."}],"date_created":"2024-09-06T12:23:31Z","volume":560,"doi":"10.1086/324309","external_id":{"arxiv":["astro-ph/0105396"]},"publisher":"American Astronomical Society","month":"09","day":"28","oa":1,"fulldoi":"https://doi.org/10.1086/324309","main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.astro-ph/0105396"}],"arxiv":1,"date_published":"2001-09-28T00:00:00Z","article_processing_charge":"No","publication_status":"published","year":"2001","quality_controlled":"1","intvolume":"       560"},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2024-11-13T07:51:12Z","citation":{"short":"Z. Haiman, T. Abel, P. Madau, The Astrophysical Journal 551 (2001) 599–607.","ieee":"Z. Haiman, T. Abel, and P. Madau, “Photon consumption in minihalos during cosmological reionization,” <i>The Astrophysical Journal</i>, vol. 551, no. 2. American Astronomical Society, pp. 599–607, 2001.","ista":"Haiman Z, Abel T, Madau P. 2001. Photon consumption in minihalos during cosmological reionization. The Astrophysical Journal. 551(2), 599–607.","mla":"Haiman, Zoltán, et al. “Photon Consumption in Minihalos during Cosmological Reionization.” <i>The Astrophysical Journal</i>, vol. 551, no. 2, American Astronomical Society, 2001, pp. 599–607, doi:<a href=\"https://doi.org/10.1086/320232\">10.1086/320232</a>.","ama":"Haiman Z, Abel T, Madau P. Photon consumption in minihalos during cosmological reionization. <i>The Astrophysical Journal</i>. 2001;551(2):599-607. doi:<a href=\"https://doi.org/10.1086/320232\">10.1086/320232</a>","apa":"Haiman, Z., Abel, T., &#38; Madau, P. (2001). Photon consumption in minihalos during cosmological reionization. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/320232\">https://doi.org/10.1086/320232</a>","chicago":"Haiman, Zoltán, Tom Abel, and Piero Madau. “Photon Consumption in Minihalos during Cosmological Reionization.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2001. <a href=\"https://doi.org/10.1086/320232\">https://doi.org/10.1086/320232</a>."},"page":"599-607","article_type":"original","type":"journal_article","oa_version":"Preprint","abstract":[{"lang":"eng","text":"At the earliest epochs of structure formation in cold dark matter (CDM) cosmologies, the smallest nonlinear objects are the numerous small halos that condense with virial temperatures below ~104 K. Such \"minihalos\" are not yet resolved in large-scale three-dimensional cosmological simulations. Here we employ a semianalytic method, combined with three-dimensional simulations of individual minihalos, to examine their importance during cosmological reionization. We show that, depending on when reionization takes place, they potentially play an important role as sinks of ionizing radiation. If reionization occurs at sufficiently high redshifts (zr ≳ 20), the intergalactic medium is heated to ~104 K and most minihalos never form. On the other hand, if zr ≲ 20, a significant fraction (≳10%) of all baryons have already collapsed into minihalos, and are subsequently removed from the halos by photoevaporation as the ionizing background flux builds up. We show that this process can require a significant budget of ionizing photons, exceeding the production by straightforward extrapolations back in time of known quasar and galaxy populations by a factor of up to ~10 and ~3, respectively."}],"extern":"1","_id":"17847","title":"Photon consumption in minihalos during cosmological reionization","status":"public","author":[{"full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403","last_name":"Haiman","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"full_name":"Abel, Tom","first_name":"Tom","last_name":"Abel"},{"first_name":"Piero","last_name":"Madau","full_name":"Madau, Piero"}],"date_created":"2024-09-06T12:25:03Z","language":[{"iso":"eng"}],"OA_place":"repository","OA_type":"green","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"publication":"The Astrophysical Journal","issue":"2","scopus_import":"1","fulldoi":"https://doi.org/10.1086/320232","arxiv":1,"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.astro-ph/0009125","open_access":"1"}],"date_published":"2001-04-20T00:00:00Z","article_processing_charge":"No","quality_controlled":"1","year":"2001","publication_status":"published","intvolume":"       551","volume":551,"doi":"10.1086/320232","external_id":{"arxiv":["astro-ph/0009125"]},"month":"04","publisher":"American Astronomical Society","day":"20","oa":1},{"page":"545-561","citation":{"mla":"Haiman, Zoltán, et al. “Constraints on Cosmological Parameters from Future Galaxy Cluster Surveys.” <i>The Astrophysical Journal</i>, vol. 553, no. 2, American Astronomical Society, 2001, pp. 545–61, doi:<a href=\"https://doi.org/10.1086/320939\">10.1086/320939</a>.","ama":"Haiman Z, Mohr JJ, Holder GP. Constraints on cosmological parameters from future galaxy cluster surveys. <i>The Astrophysical Journal</i>. 2001;553(2):545-561. doi:<a href=\"https://doi.org/10.1086/320939\">10.1086/320939</a>","short":"Z. Haiman, J.J. Mohr, G.P. Holder, The Astrophysical Journal 553 (2001) 545–561.","ista":"Haiman Z, Mohr JJ, Holder GP. 2001. Constraints on cosmological parameters from future galaxy cluster surveys. The Astrophysical Journal. 553(2), 545–561.","ieee":"Z. Haiman, J. J. Mohr, and G. P. Holder, “Constraints on cosmological parameters from future galaxy cluster surveys,” <i>The Astrophysical Journal</i>, vol. 553, no. 2. American Astronomical Society, pp. 545–561, 2001.","chicago":"Haiman, Zoltán, Joseph J. Mohr, and Gilbert P. Holder. “Constraints on Cosmological Parameters from Future Galaxy Cluster Surveys.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2001. <a href=\"https://doi.org/10.1086/320939\">https://doi.org/10.1086/320939</a>.","apa":"Haiman, Z., Mohr, J. J., &#38; Holder, G. P. (2001). Constraints on cosmological parameters from future galaxy cluster surveys. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/320939\">https://doi.org/10.1086/320939</a>"},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2024-11-13T07:58:34Z","status":"public","author":[{"orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman"},{"full_name":"Mohr, Joseph J.","last_name":"Mohr","first_name":"Joseph J."},{"last_name":"Holder","first_name":"Gilbert P.","full_name":"Holder, Gilbert P."}],"date_created":"2024-09-06T12:26:22Z","_id":"17849","title":"Constraints on cosmological parameters from future galaxy cluster surveys","extern":"1","abstract":[{"text":"We study the expected redshift evolution of galaxy cluster abundance between 0 ≲ z ≲ 3 in different cosmologies, including the effects of the cosmic equation of state parameter w ≡ p/ρ. Using the halo mass function obtained in recent large-scale numerical simulations, we model the expected cluster yields in a 12 deg2 Sunyaev-Zeldovich effect (SZE) survey and a deep 104 deg2 X-ray survey over a wide range of cosmological parameters. We quantify the statistical differences among cosmologies using both the total number and redshift distribution of clusters. Provided that the local cluster abundance is known to a few percent accuracy, we find only mild degeneracies between w and either Ωm or h. As a result, both surveys will provide improved constraints on Ωm and w. The Ωm-w degeneracy from both surveys is complementary to those found either in studies of cosmic microwave background (CMB) anisotropies or of high-redshift supernovae (SNe). As a result, combining these surveys together with either CMB or SNe studies can reduce the statistical uncertainty on both w and Ωm to levels below what could be obtained by combining only the latter two data sets. Our results indicate a formal statistical uncertainty of ≈3% (68% confidence) on both Ωm and w when the SZE survey is combined with either the CMB or SN data; the large number of clusters in the X-ray survey further suppresses the degeneracy between w and both Ωm and h. Systematics and internal evolution of cluster structure at the present pose uncertainties above these levels. We briefly discuss and quantify the relevant systematic errors. By focusing on clusters with measured temperatures in the X-ray survey, we reduce our sensitivity to systematics such as nonstandard evolution of internal cluster structure.","lang":"eng"}],"article_type":"original","type":"journal_article","oa_version":"Preprint","OA_type":"green","OA_place":"repository","language":[{"iso":"eng"}],"issue":"2","scopus_import":"1","publication":"The Astrophysical Journal","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"article_processing_charge":"No","date_published":"2001-06-01T00:00:00Z","arxiv":1,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.astro-ph/0002336"}],"fulldoi":"https://doi.org/10.1086/320939","intvolume":"       553","year":"2001","quality_controlled":"1","publication_status":"published","doi":"10.1086/320939","volume":553,"oa":1,"day":"01","month":"06","publisher":"American Astronomical Society","external_id":{"arxiv":["astro-ph/0002336"]}},{"extern":"1","abstract":[{"lang":"eng","text":"Ionizing sources embedded in the neutral intergalactic medium (IGM) before cosmological reionization generate discrete H II regions. We show that a sufficiently bright quasar (for example, 1/10 as luminous as that recently discovered by Fan et al.) can ionize a large volume, allowing the transmission of a substantial fraction of the flux of its intrinsic Lyα emission line on both sides of the Lyα wavelength. The observed line profile is richly informative. We show that a sufficiently accurate, high spectral resolution (R ≈ 104) measurement of the line profile of a bright quasar is feasible using the Next Generation Space Telescope as well as large ground-based telescopes. Such a measurement has two potentially important applications. First, the red side of the Lyα emission line provides a way to measure the quasar lifetime. Second, the blue side provides a direct measure of the density fluctuations of the IGM at the quasar redshift. The estimate of the absorption of the red side is limited by the accuracy to which the intrinsic profile of the Lyα emission line is known. The blue side, however, does not sensitively depend on the intrinsic profile because the former is much narrower than the latter."}],"article_type":"original","oa_version":"Preprint","type":"journal_article","status":"public","author":[{"full_name":"Cen, Renyue","first_name":"Renyue","last_name":"Cen"},{"full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403","first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"}],"date_created":"2024-09-06T11:42:33Z","_id":"17813","title":"Quasar Strömgren spheres before cosmological reionization","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2024-11-12T10:32:23Z","citation":{"apa":"Cen, R., &#38; Haiman, Z. (2000). Quasar Strömgren spheres before cosmological reionization. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/312937\">https://doi.org/10.1086/312937</a>","chicago":"Cen, Renyue, and Zoltán Haiman. “Quasar Strömgren Spheres before Cosmological Reionization.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2000. <a href=\"https://doi.org/10.1086/312937\">https://doi.org/10.1086/312937</a>.","ista":"Cen R, Haiman Z. 2000. Quasar Strömgren spheres before cosmological reionization. The Astrophysical Journal. 542(2), L75–L78.","short":"R. Cen, Z. Haiman, The Astrophysical Journal 542 (2000) L75–L78.","ieee":"R. Cen and Z. Haiman, “Quasar Strömgren spheres before cosmological reionization,” <i>The Astrophysical Journal</i>, vol. 542, no. 2. American Astronomical Society, pp. L75–L78, 2000.","ama":"Cen R, Haiman Z. Quasar Strömgren spheres before cosmological reionization. <i>The Astrophysical Journal</i>. 2000;542(2):L75-L78. doi:<a href=\"https://doi.org/10.1086/312937\">10.1086/312937</a>","mla":"Cen, Renyue, and Zoltán Haiman. “Quasar Strömgren Spheres before Cosmological Reionization.” <i>The Astrophysical Journal</i>, vol. 542, no. 2, American Astronomical Society, 2000, pp. L75–78, doi:<a href=\"https://doi.org/10.1086/312937\">10.1086/312937</a>."},"page":"L75-L78","publication_identifier":{"issn":["0004-637X"]},"issue":"2","scopus_import":"1","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"OA_type":"green","OA_place":"repository","intvolume":"       542","quality_controlled":"1","year":"2000","publication_status":"published","arxiv":1,"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.astro-ph/0006376","open_access":"1"}],"fulldoi":"https://doi.org/10.1086/312937","article_processing_charge":"No","date_published":"2000-10-20T00:00:00Z","month":"10","publisher":"American Astronomical Society","external_id":{"arxiv":["astro-ph/0006376"]},"oa":1,"day":"20","doi":"10.1086/312937","volume":542},{"month":"05","publisher":"American Astronomical Society","external_id":{"arxiv":["astro-ph/9903336"]},"oa":1,"day":"01","doi":"10.1086/308723","volume":534,"intvolume":"       534","year":"2000","quality_controlled":"1","publication_status":"published","arxiv":1,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.astro-ph/9903336"}],"fulldoi":"https://doi.org/10.1086/308723","article_processing_charge":"No","date_published":"2000-05-01T00:00:00Z","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"issue":"1","scopus_import":"1","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"OA_type":"green","OA_place":"repository","abstract":[{"text":"In hierarchical models of structure formation, an early cosmic UV background (UVB) is produced by the small (Tvir ≲ 10^4 K) halos that collapse before reionization. The UVB at energies below 13.6 eV suppresses the formation of stars or black holes inside small halos by photodissociating their only cooling agent, molecular H2. We self-consistently compute the buildup of the early UVB in Press-Schechter models, coupled with H2 photodissociation both in the intergalactic medium (IGM) and inside virialized halos. We find that the intergalactic H2 has a negligible effect on the UVB, both because its initial optical depth is small (≲0.1) and because it is photodissociated at an early stage. If the UV sources in the first collapsed halos are stars, then their UV flux suppresses further star formation inside small halos. This results in a pause in the buildup of the UVB, and reionization is delayed until larger halos (Tvir ≳ 10^4 K) collapse. If the small halos host miniquasars with hard spectra extending to ~1 keV, then their X-rays balance the effects of the UVB, the negative feedback does not occur, and reionization could be caused by the small halos.","lang":"eng"}],"extern":"1","article_type":"original","type":"journal_article","oa_version":"Preprint","author":[{"full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán"},{"last_name":"Abel","first_name":"Tom","full_name":"Abel, Tom"},{"full_name":"Rees, Martin J.","first_name":"Martin J.","last_name":"Rees"}],"date_created":"2024-09-06T11:43:22Z","status":"public","_id":"17814","title":"The radiative feedback of the first cosmological objects","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2024-11-12T12:17:03Z","page":"11-24","citation":{"ieee":"Z. Haiman, T. Abel, and M. J. Rees, “The radiative feedback of the first cosmological objects,” <i>The Astrophysical Journal</i>, vol. 534, no. 1. American Astronomical Society, pp. 11–24, 2000.","ista":"Haiman Z, Abel T, Rees MJ. 2000. The radiative feedback of the first cosmological objects. The Astrophysical Journal. 534(1), 11–24.","short":"Z. Haiman, T. Abel, M.J. Rees, The Astrophysical Journal 534 (2000) 11–24.","mla":"Haiman, Zoltán, et al. “The Radiative Feedback of the First Cosmological Objects.” <i>The Astrophysical Journal</i>, vol. 534, no. 1, American Astronomical Society, 2000, pp. 11–24, doi:<a href=\"https://doi.org/10.1086/308723\">10.1086/308723</a>.","ama":"Haiman Z, Abel T, Rees MJ. The radiative feedback of the first cosmological objects. <i>The Astrophysical Journal</i>. 2000;534(1):11-24. doi:<a href=\"https://doi.org/10.1086/308723\">10.1086/308723</a>","apa":"Haiman, Z., Abel, T., &#38; Rees, M. J. (2000). The radiative feedback of the first cosmological objects. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/308723\">https://doi.org/10.1086/308723</a>","chicago":"Haiman, Zoltán, Tom Abel, and Martin J. Rees. “The Radiative Feedback of the First Cosmological Objects.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2000. <a href=\"https://doi.org/10.1086/308723\">https://doi.org/10.1086/308723</a>."}},{"day":"20","oa":1,"external_id":{"arxiv":["astro-ph/9907039"]},"publisher":"American Astronomical Society","month":"03","volume":532,"doi":"10.1086/308557","publication_status":"published","quality_controlled":"1","year":"2000","intvolume":"       532","date_published":"2000-03-20T00:00:00Z","article_processing_charge":"No","fulldoi":"https://doi.org/10.1086/308557","main_file_link":[{"url":"https://doi.org/10.48550/arXiv.astro-ph/9907039","open_access":"1"}],"arxiv":1,"publication":"The Astrophysical Journal","scopus_import":"1","issue":"1","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"OA_place":"repository","OA_type":"green","language":[{"iso":"eng"}],"title":"Cosmological constant or intergalactic dust? Constraints from the cosmic far‐infrared background","_id":"17817","status":"public","author":[{"full_name":"Aguirre, Anthony","last_name":"Aguirre","first_name":"Anthony"},{"last_name":"Haiman","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán"}],"date_created":"2024-09-06T11:45:26Z","oa_version":"Preprint","type":"journal_article","article_type":"original","abstract":[{"text":"Recent observations of Type Ia supernovae (SNe) at redshifts 0 < z < 1 reveal a progressive dimming that has been interpreted as evidence for a cosmological constant of ΩΛ ~ 0.7. An alternative explanation of the SN results is an open universe with ΩΛ = 0 and the presence of ≳0.1 μm dust grains with a mass density of Ωdust ~ a few × 10-5 in the intergalactic (IG) medium. The same dust that dims the SNe absorbs the cosmic UV/optical background radiation around ~1 μm, and reemits it at far-infrared (FIR) wavelengths. Here we compare the FIR emission from IG dust with observations of the cosmic microwave (CMB) and cosmic far-infrared backgrounds (FIRB) by the DIRBE/FIRAS instruments. We find that the emission would not lead to measurable distortion of the CMB, but would represent a substantial fraction (≳75%) of the measured value of the FIRB in the 300-1000 μm range. This contribution would be marginally consistent with the present unresolved fraction of the observed FIRB in an open universe. However, we find that IG dust probably could not reconcile the standard Ω = 1 CDM model with the SN observations, even if the necessary quantity of dust existed. Future observations, capable of reliably resolving the FIRB to a flux limit of ~0.5 mJy, along with a more precise measure of the coarse-grained FIRB, will provide a definitive test of the IG dust hypothesis in all cosmologies.","lang":"eng"}],"extern":"1","citation":{"apa":"Aguirre, A., &#38; Haiman, Z. (2000). Cosmological constant or intergalactic dust? Constraints from the cosmic far‐infrared background. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/308557\">https://doi.org/10.1086/308557</a>","chicago":"Aguirre, Anthony, and Zoltán Haiman. “Cosmological Constant or Intergalactic Dust? Constraints from the Cosmic Far‐infrared Background.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2000. <a href=\"https://doi.org/10.1086/308557\">https://doi.org/10.1086/308557</a>.","ieee":"A. Aguirre and Z. Haiman, “Cosmological constant or intergalactic dust? Constraints from the cosmic far‐infrared background,” <i>The Astrophysical Journal</i>, vol. 532, no. 1. American Astronomical Society, pp. 28–36, 2000.","short":"A. Aguirre, Z. Haiman, The Astrophysical Journal 532 (2000) 28–36.","ista":"Aguirre A, Haiman Z. 2000. Cosmological constant or intergalactic dust? Constraints from the cosmic far‐infrared background. The Astrophysical Journal. 532(1), 28–36.","ama":"Aguirre A, Haiman Z. Cosmological constant or intergalactic dust? Constraints from the cosmic far‐infrared background. <i>The Astrophysical Journal</i>. 2000;532(1):28-36. doi:<a href=\"https://doi.org/10.1086/308557\">10.1086/308557</a>","mla":"Aguirre, Anthony, and Zoltán Haiman. “Cosmological Constant or Intergalactic Dust? Constraints from the Cosmic Far‐infrared Background.” <i>The Astrophysical Journal</i>, vol. 532, no. 1, American Astronomical Society, 2000, pp. 28–36, doi:<a href=\"https://doi.org/10.1086/308557\">10.1086/308557</a>."},"page":"28-36","date_updated":"2024-11-12T12:25:50Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"page":"124-132","citation":{"short":"Z. Haiman, L. Knox, The Astrophysical Journal 530 (2000) 124–132.","ista":"Haiman Z, Knox L. 2000. Correlations in the far‐infrared background. The Astrophysical Journal. 530(1), 124–132.","ieee":"Z. Haiman and L. Knox, “Correlations in the far‐infrared background,” <i>The Astrophysical Journal</i>, vol. 530, no. 1. American Astronomical Society, pp. 124–132, 2000.","mla":"Haiman, Zoltán, and Lloyd Knox. “Correlations in the Far‐infrared Background.” <i>The Astrophysical Journal</i>, vol. 530, no. 1, American Astronomical Society, 2000, pp. 124–32, doi:<a href=\"https://doi.org/10.1086/308374\">10.1086/308374</a>.","ama":"Haiman Z, Knox L. Correlations in the far‐infrared background. <i>The Astrophysical Journal</i>. 2000;530(1):124-132. doi:<a href=\"https://doi.org/10.1086/308374\">10.1086/308374</a>","apa":"Haiman, Z., &#38; Knox, L. (2000). Correlations in the far‐infrared background. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/308374\">https://doi.org/10.1086/308374</a>","chicago":"Haiman, Zoltán, and Lloyd Knox. “Correlations in the Far‐infrared Background.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2000. <a href=\"https://doi.org/10.1086/308374\">https://doi.org/10.1086/308374</a>."},"date_updated":"2024-11-13T07:19:17Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","status":"public","author":[{"full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán"},{"first_name":"Lloyd","last_name":"Knox","full_name":"Knox, Lloyd"}],"date_created":"2024-09-06T12:09:57Z","title":"Correlations in the far‐infrared background","_id":"17830","extern":"1","abstract":[{"lang":"eng","text":"We compute the expected angular power spectrum of the cosmic far infrared background (FIRB). We find that the signal due to source correlations dominates the shot noise for l ≲ 1000 and results in anisotropies with rms amplitudes [l(l + 1)Cl/2π]1/2 between 5% and 10% of the mean for l ≳ 150. The angular power spectrum depends on several unknown quantities, such as the UV flux density evolution, optical properties of the dust, biasing of the sources of the FIRB, and cosmological parameters. However, when we require our models to reproduce the observed direct current level of the FIRB, we find that the anisotropy is at least a few percent in all cases. This anisotropy is detectable with proposed instruments, and its measurement will provide strong constraints on models of galaxy evolution and large-scale structure at redshifts up to at least z ~ 5."}],"type":"journal_article","oa_version":"Preprint","article_type":"original","OA_place":"repository","OA_type":"green","language":[{"iso":"eng"}],"scopus_import":"1","issue":"1","publication":"The Astrophysical Journal","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"article_processing_charge":"No","date_published":"2000-02-10T00:00:00Z","main_file_link":[{"url":"https://doi.org/10.48550/arXiv.astro-ph/9906399","open_access":"1"}],"arxiv":1,"fulldoi":"https://doi.org/10.1086/308374","intvolume":"       530","publication_status":"published","quality_controlled":"1","year":"2000","doi":"10.1086/308374","volume":530,"oa":1,"day":"10","publisher":"American Astronomical Society","month":"02","external_id":{"arxiv":["astro-ph/9906399"]}},{"intvolume":"       531","quality_controlled":"1","year":"2000","publication_status":"published","arxiv":1,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.astro-ph/9810426"}],"fulldoi":"https://doi.org/10.1086/308468","article_processing_charge":"No","date_published":"2000-03-01T00:00:00Z","month":"03","publisher":"American Astronomical Society","external_id":{"arxiv":["astro-ph/9810426"]},"oa":1,"day":"01","doi":"10.1086/308468","volume":531,"extern":"1","abstract":[{"lang":"eng","text":"We consider a class of models for the redshift evolution (between 0 ≲ z ≲ 4) of the observed optical and X-ray quasar luminosity functions (LFs), with the following assumptions: (1) the mass function of dark matter halos follows the Press-Schechter theory, (2) the black hole (BH) mass scales linearly with the halo mass, (3) quasars have a constant universal lifetime, and (4) a thin accretion disk provides the optical luminosity of quasars, while the X-ray/optical flux ratio is calibrated from a sample of observed quasars. The mass accretion rate, , onto quasar BHs is a free parameter of the models, which we constrain using the observed LFs. The accretion rate inferred from either the optical or X-ray data under these assumptions generally decreases as a function of cosmic time from z ≃ 4 to z ≃ 0. We find that a comparable accretion rate is inferred from the X-ray and optical LF only if the X-ray/optical flux ratio decreases with BH mass. Near z ≃ 0, drops to substantially sub-Eddington values at which advection-dominated accretion flows (ADAFs) exist. Such a decline of M, possibly followed by a transition to radiatively inefficient ADAFs, could explain both the absence of bright quasars in the local universe and the faintness of accreting BHs at the centers of nearby galaxies. We argue that a decline of the accretion rate of the quasar population is indeed expected in cosmological structure formation models."}],"article_type":"original","oa_version":"Preprint","type":"journal_article","author":[{"orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán","first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"full_name":"Menou, Kristen","last_name":"Menou","first_name":"Kristen"}],"status":"public","date_created":"2024-09-06T12:12:11Z","_id":"17833","title":"On the cosmological evolution of the luminosity function and the accretion rate of quasars","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2024-11-13T07:27:11Z","citation":{"ama":"Haiman Z, Menou K. On the cosmological evolution of the luminosity function and the accretion rate of quasars. <i>The Astrophysical Journal</i>. 2000;531(1):42-51. doi:<a href=\"https://doi.org/10.1086/308468\">10.1086/308468</a>","mla":"Haiman, Zoltán, and Kristen Menou. “On the Cosmological Evolution of the Luminosity Function and the Accretion Rate of Quasars.” <i>The Astrophysical Journal</i>, vol. 531, no. 1, American Astronomical Society, 2000, pp. 42–51, doi:<a href=\"https://doi.org/10.1086/308468\">10.1086/308468</a>.","short":"Z. Haiman, K. Menou, The Astrophysical Journal 531 (2000) 42–51.","ista":"Haiman Z, Menou K. 2000. On the cosmological evolution of the luminosity function and the accretion rate of quasars. The Astrophysical Journal. 531(1), 42–51.","ieee":"Z. Haiman and K. Menou, “On the cosmological evolution of the luminosity function and the accretion rate of quasars,” <i>The Astrophysical Journal</i>, vol. 531, no. 1. American Astronomical Society, pp. 42–51, 2000.","chicago":"Haiman, Zoltán, and Kristen Menou. “On the Cosmological Evolution of the Luminosity Function and the Accretion Rate of Quasars.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2000. <a href=\"https://doi.org/10.1086/308468\">https://doi.org/10.1086/308468</a>.","apa":"Haiman, Z., &#38; Menou, K. (2000). On the cosmological evolution of the luminosity function and the accretion rate of quasars. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/308468\">https://doi.org/10.1086/308468</a>"},"page":"42-51","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"issue":"1","scopus_import":"1","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"OA_type":"green","OA_place":"repository"},{"OA_type":"green","OA_place":"repository","language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","issue":"1","scopus_import":"1","publication_identifier":{"issn":["0004-637X"]},"citation":{"chicago":"Haiman, Zoltán, Marco Spaans, and Eliot Quataert. “Lyα Cooling Radiation from High-Redshift Halos.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2000. <a href=\"https://doi.org/10.1086/312754\">https://doi.org/10.1086/312754</a>.","apa":"Haiman, Z., Spaans, M., &#38; Quataert, E. (2000). Lyα cooling radiation from high-redshift halos. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/312754\">https://doi.org/10.1086/312754</a>","mla":"Haiman, Zoltán, et al. “Lyα Cooling Radiation from High-Redshift Halos.” <i>The Astrophysical Journal</i>, vol. 537, no. 1, American Astronomical Society, 2000, pp. L5–8, doi:<a href=\"https://doi.org/10.1086/312754\">10.1086/312754</a>.","ama":"Haiman Z, Spaans M, Quataert E. Lyα cooling radiation from high-redshift halos. <i>The Astrophysical Journal</i>. 2000;537(1):L5-L8. doi:<a href=\"https://doi.org/10.1086/312754\">10.1086/312754</a>","short":"Z. Haiman, M. Spaans, E. Quataert, The Astrophysical Journal 537 (2000) L5–L8.","ista":"Haiman Z, Spaans M, Quataert E. 2000. Lyα cooling radiation from high-redshift halos. The Astrophysical Journal. 537(1), L5–L8.","ieee":"Z. Haiman, M. Spaans, and E. Quataert, “Lyα cooling radiation from high-redshift halos,” <i>The Astrophysical Journal</i>, vol. 537, no. 1. American Astronomical Society, pp. L5–L8, 2000."},"page":"L5-L8","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2024-11-13T07:41:20Z","_id":"17838","title":"Lyα cooling radiation from high-redshift halos","status":"public","date_created":"2024-09-06T12:15:30Z","author":[{"orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman"},{"last_name":"Spaans","first_name":"Marco","full_name":"Spaans, Marco"},{"full_name":"Quataert, Eliot","last_name":"Quataert","first_name":"Eliot"}],"article_type":"original","type":"journal_article","oa_version":"Preprint","extern":"1","abstract":[{"text":"The baryons inside high-redshift halos with virial temperatures T ≳ 10^4 K cool radiatively as they condense inside dark matter potential wells. We show that the release of the gravitational binding energy, over the halo assembly timescale, results in a significant and detectable Lyα flux. At the limiting line flux ≈10^-19 ergs s^-1 cm^-2 arcsec^-2 of the Next Generation Space Telescope, several sufficiently massive halos, with velocity dispersions σ ≳ 120 km s^-1, would be visible per 4' × 4' field. The halos would have characteristic angular sizes of ≈10'', would be detectable in a broadband survey out to z ≈ 6-8, and would provide a direct probe of galaxies in the process of forming. They may be accompanied by He+ Lyα emission at the ≈10% level, but remain undetectable at other wavelengths. Our predictions are in good agreement with the recent finding of two Lyα \"blobs\" at z = 3.1 by Steidel et al.","lang":"eng"}],"volume":537,"doi":"10.1086/312754","day":"01","oa":1,"external_id":{"arxiv":["astro-ph/0003366"]},"month":"07","publisher":"American Astronomical Society","date_published":"2000-07-01T00:00:00Z","article_processing_charge":"No","fulldoi":"https://doi.org/10.1086/312754","arxiv":1,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.astro-ph/0003366"}],"year":"2000","quality_controlled":"1","publication_status":"published","intvolume":"       537"},{"volume":519,"doi":"10.1086/307393","day":"10","oa":1,"external_id":{"arxiv":["astro-ph/9807070"]},"month":"07","publisher":"American Astronomical Society","date_published":"1999-07-10T00:00:00Z","article_processing_charge":"No","fulldoi":"https://doi.org/10.1086/307393","arxiv":1,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.astro-ph/9807070"}],"year":"1999","quality_controlled":"1","publication_status":"published","intvolume":"       519","OA_place":"repository","OA_type":"green","language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","issue":"2","scopus_import":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"page":"479-485","citation":{"chicago":"Haiman, Zoltán, and Abraham Loeb. “Determining the Redshift of Reionization from the Spectra of High‐redshift Sources.” <i>The Astrophysical Journal</i>. American Astronomical Society, 1999. <a href=\"https://doi.org/10.1086/307393\">https://doi.org/10.1086/307393</a>.","apa":"Haiman, Z., &#38; Loeb, A. (1999). Determining the redshift of reionization from the spectra of high‐redshift sources. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/307393\">https://doi.org/10.1086/307393</a>","ama":"Haiman Z, Loeb A. Determining the redshift of reionization from the spectra of high‐redshift sources. <i>The Astrophysical Journal</i>. 1999;519(2):479-485. doi:<a href=\"https://doi.org/10.1086/307393\">10.1086/307393</a>","mla":"Haiman, Zoltán, and Abraham Loeb. “Determining the Redshift of Reionization from the Spectra of High‐redshift Sources.” <i>The Astrophysical Journal</i>, vol. 519, no. 2, American Astronomical Society, 1999, pp. 479–85, doi:<a href=\"https://doi.org/10.1086/307393\">10.1086/307393</a>.","ista":"Haiman Z, Loeb A. 1999. Determining the redshift of reionization from the spectra of high‐redshift sources. The Astrophysical Journal. 519(2), 479–485.","short":"Z. Haiman, A. Loeb, The Astrophysical Journal 519 (1999) 479–485.","ieee":"Z. Haiman and A. Loeb, “Determining the redshift of reionization from the spectra of high‐redshift sources,” <i>The Astrophysical Journal</i>, vol. 519, no. 2. American Astronomical Society, pp. 479–485, 1999."},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2024-11-12T12:19:49Z","_id":"17815","title":"Determining the redshift of reionization from the spectra of high‐redshift sources","status":"public","date_created":"2024-09-06T11:44:04Z","author":[{"orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán","first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"full_name":"Loeb, Abraham","last_name":"Loeb","first_name":"Abraham"}],"article_type":"original","type":"journal_article","oa_version":"Preprint","extern":"1","abstract":[{"text":"The redshift at which the universe was reionized is currently unknown. We examine the optimal strategy for extracting this redshift, zreion, from the spectra of early sources. For a source located at a redshift zs beyond but close to the reionization redshift, (1 + zreion) < (1 + zs) < 32/27(1 + zreion), the Gunn-Peterson trough splits into disjoint Lyα, Lyβ, and possibly higher Lyman series troughs, with some transmitted flux between these troughs. We show that although the transmitted flux is suppressed considerably by the dense Lyα forest at high redshifts, it could still be detectable as long as zreion ≲ 8. If the ionizing sources are bright and have a short duty cycle (e.g., if they are miniquasars or starbursts with a lifetime ≲106 yr), then breakthrough occurs shortly after the H II regions around them overlap, and the transmitted flux provides a measurement of zreion. The Next Generation Space Telescope will reach the spectroscopic sensitivity required for such a measurement.","lang":"eng"}]},{"doi":"10.1086/312177","volume":521,"oa":1,"day":"10","publisher":"American Astronomical Society","month":"08","external_id":{"arxiv":["astro-ph/9904340"]},"article_processing_charge":"No","date_published":"1999-08-10T00:00:00Z","main_file_link":[{"url":"https://doi.org/10.48550/arXiv.astro-ph/9904340","open_access":"1"}],"arxiv":1,"fulldoi":"https://doi.org/10.1086/312177","intvolume":"       521","publication_status":"published","year":"1999","quality_controlled":"1","OA_place":"repository","OA_type":"green","language":[{"iso":"eng"}],"scopus_import":"1","issue":"1","publication":"The Astrophysical Journal","publication_identifier":{"issn":["0004-637X"]},"page":"L9-L12","citation":{"ama":"Haiman Z, Loeb A. X-ray emission from the first quasars. <i>The Astrophysical Journal</i>. 1999;521(1):L9-L12. doi:<a href=\"https://doi.org/10.1086/312177\">10.1086/312177</a>","mla":"Haiman, Zoltán, and Abraham Loeb. “X-Ray Emission from the First Quasars.” <i>The Astrophysical Journal</i>, vol. 521, no. 1, American Astronomical Society, 1999, pp. L9–12, doi:<a href=\"https://doi.org/10.1086/312177\">10.1086/312177</a>.","short":"Z. Haiman, A. Loeb, The Astrophysical Journal 521 (1999) L9–L12.","ieee":"Z. Haiman and A. Loeb, “X-ray emission from the first quasars,” <i>The Astrophysical Journal</i>, vol. 521, no. 1. American Astronomical Society, pp. L9–L12, 1999.","ista":"Haiman Z, Loeb A. 1999. X-ray emission from the first quasars. The Astrophysical Journal. 521(1), L9–L12.","chicago":"Haiman, Zoltán, and Abraham Loeb. “X-Ray Emission from the First Quasars.” <i>The Astrophysical Journal</i>. American Astronomical Society, 1999. <a href=\"https://doi.org/10.1086/312177\">https://doi.org/10.1086/312177</a>.","apa":"Haiman, Z., &#38; Loeb, A. (1999). X-ray emission from the first quasars. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/312177\">https://doi.org/10.1086/312177</a>"},"date_updated":"2024-11-12T13:00:30Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2024-09-06T12:06:45Z","status":"public","author":[{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403"},{"full_name":"Loeb, Abraham","last_name":"Loeb","first_name":"Abraham"}],"title":"X-ray emission from the first quasars","_id":"17827","extern":"1","abstract":[{"lang":"eng","text":"It is currently unknown whether the universe was reionized by quasars or stars at z ≳ 5. We point out that quasars can be best distinguished from stellar systems by their X-ray emission. Based on a simple hierarchical CDM model, we predict the number counts and X-ray fluxes of quasars at high redshifts. The model is consistent with available data on the luminosity function of high-redshift quasars in the optical and soft X-ray bands. The cumulative contribution of faint, undetected quasars in our model is consistent with the unresolved fraction of the X-ray background. We find that the Chandra X-ray Observatory might detect ~10^2 quasars from redshifts z ≳ 5 per its 17' × 17' field of view at the flux threshold of ~2 × 10^-16 ergs s^-1 cm^-2. The redshifts of these faint point sources could be identified by follow-up infrared observations from the ground or with the Next Generation Space Telescope."}],"oa_version":"Preprint","type":"journal_article","article_type":"original"},{"citation":{"apa":"Haiman, Z., &#38; Spaans, M. (1999). Models for dusty Lyα emitters at high redshift. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/307276\">https://doi.org/10.1086/307276</a>","chicago":"Haiman, Zoltán, and Marco Spaans. “Models for Dusty Lyα Emitters at High Redshift.” <i>The Astrophysical Journal</i>. American Astronomical Society, 1999. <a href=\"https://doi.org/10.1086/307276\">https://doi.org/10.1086/307276</a>.","ieee":"Z. Haiman and M. Spaans, “Models for dusty Lyα emitters at high redshift,” <i>The Astrophysical Journal</i>, vol. 518, no. 1. American Astronomical Society, pp. 138–144, 1999.","short":"Z. Haiman, M. Spaans, The Astrophysical Journal 518 (1999) 138–144.","ista":"Haiman Z, Spaans M. 1999. Models for dusty Lyα emitters at high redshift. The Astrophysical Journal. 518(1), 138–144.","mla":"Haiman, Zoltán, and Marco Spaans. “Models for Dusty Lyα Emitters at High Redshift.” <i>The Astrophysical Journal</i>, vol. 518, no. 1, American Astronomical Society, 1999, pp. 138–44, doi:<a href=\"https://doi.org/10.1086/307276\">10.1086/307276</a>.","ama":"Haiman Z, Spaans M. Models for dusty Lyα emitters at high redshift. <i>The Astrophysical Journal</i>. 1999;518(1):138-144. doi:<a href=\"https://doi.org/10.1086/307276\">10.1086/307276</a>"},"page":"138-144","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2024-11-13T07:30:03Z","_id":"17835","title":"Models for dusty Lyα emitters at high redshift","status":"public","author":[{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán","orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán"},{"last_name":"Spaans","first_name":"Marco","full_name":"Spaans, Marco"}],"date_created":"2024-09-06T12:13:30Z","article_type":"original","oa_version":"Preprint","type":"journal_article","extern":"1","abstract":[{"text":"Models are presented for the Lyα emission of dusty high-redshift galaxies by combining the Press-Schechter formalism with a treatment of the inhomogeneous dust distribution inside galaxies. It is found that the amount of Lyα radiation escaping from the galaxies strongly depends on the time over which the dust is produced through stellar activity and on the ambient inhomogeneity of the H II regions that surround the ionizing OB stars. Good agreement is found with recent observations, as well as with previous nondetections. Although a detailed determination of the individual model parameters is precluded by uncertainties, we find that (1) the dust content in primordial galaxies builds up in no more than ~5 × 108 yr, (2) the galactic H II regions are inhomogeneous with a cloud-covering factor of order unity, and (3) the overall star formation efficiency is at least ~5%. It is predicted that future observations can detect these Lyα galaxies up to redshifts of ~8. If the universe is reionized at zr ≲ 8, the corresponding decline in the number of Lyα emitters at z ≳ zr could prove to be a useful probe of the reionization epoch.","lang":"eng"}],"OA_place":"repository","OA_type":"green","language":[{"iso":"eng"}],"publication":"The Astrophysical Journal","issue":"1","scopus_import":"1","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"date_published":"1999-06-10T00:00:00Z","article_processing_charge":"No","fulldoi":"https://doi.org/10.1086/307276","arxiv":1,"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.astro-ph/9809223","open_access":"1"}],"year":"1999","quality_controlled":"1","publication_status":"published","intvolume":"       518","volume":518,"doi":"10.1086/307276","day":"10","oa":1,"external_id":{"arxiv":["astro-ph/9809223"]},"month":"06","publisher":"American Astronomical Society"},{"oa":1,"day":"01","publisher":"American Astronomical Society","month":"04","external_id":{"arxiv":["astro-ph/9805258"]},"doi":"10.1086/306969","volume":514,"intvolume":"       514","publication_status":"published","quality_controlled":"1","year":"1999","article_processing_charge":"No","date_published":"1999-04-01T00:00:00Z","main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.astro-ph/9805258"}],"arxiv":1,"fulldoi":"https://doi.org/10.1086/306969","scopus_import":"1","issue":"2","publication":"The Astrophysical Journal","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"OA_type":"green","OA_place":"repository","language":[{"iso":"eng"}],"date_created":"2024-09-06T12:14:48Z","author":[{"orcid":"0000-0003-3633-5403","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán"},{"full_name":"Madau, Piero","first_name":"Piero","last_name":"Madau"},{"full_name":"Loeb, Abraham","last_name":"Loeb","first_name":"Abraham"}],"status":"public","title":"Constraints from the Hubble deep field on high‐redshift quasar models","_id":"17837","abstract":[{"lang":"eng","text":"High-resolution, deep-imaging surveys are instrumental in setting constraints on semianalytical structure formation models in cold dark matter (CDM) cosmologies. We show here that the lack of unresolved B-band \"dropouts\" with V>25 mag in the Hubble Deep Field appears to be inconsistent with the number of \"miniquasars\" expected if massive black holes form with a constant universal efficiency in all CDM halos. To reconcile the models with the data, a mechanism is needed that suppresses the formation of active nuclei in halos with circular velocities vcirc≲50-75 km s-1. This feedback naturally arises because of the photoionization heating of the gas by the UV background. We consider several alternative effects that would help reducing the number of miniquasars and find that these cannot alone account for the observed lack of detections. If reddening by dust can be neglected at early epochs, consistency with the optical data also requires that the luminous extent of dwarf galaxies at high redshifts be larger than a few percent of the virial radii of their dark matter halos, in order not to overpredict the number of pointlike B-band dropouts. Future deep observations in the J and H bands with NICMOS might reveal several z≳5 objects per field or provide even stronger constraints on the models than existing B, V, and I data."}],"extern":"1","oa_version":"Preprint","type":"journal_article","article_type":"original","citation":{"chicago":"Haiman, Zoltán, Piero Madau, and Abraham Loeb. “Constraints from the Hubble Deep Field on High‐redshift Quasar Models.” <i>The Astrophysical Journal</i>. American Astronomical Society, 1999. <a href=\"https://doi.org/10.1086/306969\">https://doi.org/10.1086/306969</a>.","apa":"Haiman, Z., Madau, P., &#38; Loeb, A. (1999). Constraints from the Hubble deep field on high‐redshift quasar models. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/306969\">https://doi.org/10.1086/306969</a>","mla":"Haiman, Zoltán, et al. “Constraints from the Hubble Deep Field on High‐redshift Quasar Models.” <i>The Astrophysical Journal</i>, vol. 514, no. 2, American Astronomical Society, 1999, pp. 535–43, doi:<a href=\"https://doi.org/10.1086/306969\">10.1086/306969</a>.","ama":"Haiman Z, Madau P, Loeb A. Constraints from the Hubble deep field on high‐redshift quasar models. <i>The Astrophysical Journal</i>. 1999;514(2):535-543. doi:<a href=\"https://doi.org/10.1086/306969\">10.1086/306969</a>","short":"Z. Haiman, P. Madau, A. Loeb, The Astrophysical Journal 514 (1999) 535–543.","ista":"Haiman Z, Madau P, Loeb A. 1999. Constraints from the Hubble deep field on high‐redshift quasar models. The Astrophysical Journal. 514(2), 535–543.","ieee":"Z. Haiman, P. Madau, and A. Loeb, “Constraints from the Hubble deep field on high‐redshift quasar models,” <i>The Astrophysical Journal</i>, vol. 514, no. 2. American Astronomical Society, pp. 535–543, 1999."},"page":"535-543","date_updated":"2024-11-13T07:37:51Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"extern":"1","abstract":[{"lang":"eng","text":"We study the observational signatures of a potential population of low-luminosity quasars at high redshifts in a ΛCDM cosmology. We derive the evolution of the quasar luminosity function at fainter luminosities and higher redshifts than currently detected based on three assumptions: (1) the formation of dark matter halos follows the Press-Schechter theory, (2) the ratio of central black hole mass to halo mass is the same for all halos, and (3) the light curve of quasars, in Eddington units, is universal. We show that a universal light curve provides an excellent fit to the observed quasar luminosity function at redshifts 2.6 < z < 4.5. By extrapolating the evolution of this luminosity function to higher redshifts (4.5 < z < 20), we find that the associated early population of low-luminosity quasars reionizes the universe at a redshift z ~ 12. The reprocessing of the UV light of these quasars by dust from early Type II supernovae distorts the microwave background spectrum by a Compton y-parameter y ~ 10-5, comparable to the lower limit set by COBE. The Next Generation Space Telescope could detect tens of quasars per arcmin-2 from redshifts z > 10 with its proposed 1 nJy sensitivity at 1-3.5 μm. Absorption spectra of several such quasars would reveal the reionization history of the universe."}],"article_type":"original","type":"journal_article","oa_version":"Preprint","status":"public","author":[{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán","full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403"},{"full_name":"Loeb, Abraham","first_name":"Abraham","last_name":"Loeb"}],"date_created":"2024-09-06T12:16:27Z","_id":"17839","title":"Observational signatures of the first quasars","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2024-11-13T07:43:28Z","page":"505-517","citation":{"apa":"Haiman, Z., &#38; Loeb, A. (1998). Observational signatures of the first quasars. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/306017\">https://doi.org/10.1086/306017</a>","chicago":"Haiman, Zoltán, and Abraham Loeb. “Observational Signatures of the First Quasars.” <i>The Astrophysical Journal</i>. American Astronomical Society, 1998. <a href=\"https://doi.org/10.1086/306017\">https://doi.org/10.1086/306017</a>.","short":"Z. Haiman, A. Loeb, The Astrophysical Journal 503 (1998) 505–517.","ieee":"Z. Haiman and A. Loeb, “Observational signatures of the first quasars,” <i>The Astrophysical Journal</i>, vol. 503, no. 2. American Astronomical Society, pp. 505–517, 1998.","ista":"Haiman Z, Loeb A. 1998. Observational signatures of the first quasars. The Astrophysical Journal. 503(2), 505–517.","ama":"Haiman Z, Loeb A. Observational signatures of the first quasars. <i>The Astrophysical Journal</i>. 1998;503(2):505-517. doi:<a href=\"https://doi.org/10.1086/306017\">10.1086/306017</a>","mla":"Haiman, Zoltán, and Abraham Loeb. “Observational Signatures of the First Quasars.” <i>The Astrophysical Journal</i>, vol. 503, no. 2, American Astronomical Society, 1998, pp. 505–17, doi:<a href=\"https://doi.org/10.1086/306017\">10.1086/306017</a>."},"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"issue":"2","scopus_import":"1","publication":"The Astrophysical Journal","language":[{"iso":"eng"}],"OA_type":"green","OA_place":"repository","intvolume":"       503","quality_controlled":"1","year":"1998","publication_status":"published","arxiv":1,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.astro-ph/9710208"}],"fulldoi":"https://doi.org/10.1086/306017","article_processing_charge":"No","date_published":"1998-08-20T00:00:00Z","month":"08","publisher":"American Astronomical Society","external_id":{"arxiv":["astro-ph/9710208"]},"oa":1,"day":"20","doi":"10.1086/306017","volume":503}]