[{"fulldoi":"https://doi.org/10.1088/0004-637x/694/2/867","publication_status":"published","publication":"The Astrophysical Journal","date_created":"2024-09-06T10:02:08Z","date_published":"2009-03-20T00:00:00Z","extern":"1","year":"2009","status":"public","intvolume":"       694","type":"journal_article","issue":"2","author":[{"full_name":"Shankar, Francesco","first_name":"Francesco","last_name":"Shankar"},{"last_name":"Bernardi","full_name":"Bernardi, Mariangela","first_name":"Mariangela"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","full_name":"Haiman, Zoltán","first_name":"Zoltán"}],"day":"20","page":"867-878","volume":694,"article_type":"original","quality_controlled":"1","article_processing_charge":"No","abstract":[{"text":"We utilize the local velocity dispersion function (VDF) of spheroids, together with their inferred age distributions, to predict the VDF at higher redshifts (0 < z lsim 6), under the assumption that (1) most of the stars in each nearby spheroid formed in a single episode and, (2) the velocity dispersion σ remained nearly constant afterward. We assume further that a supermassive BH forms concurrently with the stars, and within ±1 Gyr of the formation of the potential well of the spheroid, and that the relation between the mass of the BH and host velocity dispersion maintains the form M BH vprop σβ with β ≈ 4, but with the normalization allowed to evolve with redshift as vprop(1 + z)α. We compute the BH mass function associated with the VDF at each redshift, and compare the accumulated total BH mass density with that inferred from the integrated quasar luminosity function (LF; the so-called Sołtan argument). This comparison is insensitive to the assumed duty cycle or Eddington ratio of quasar activity, and we find that the match between the two BH mass densities favors a relatively mild redshift evolution, with α ~ 0.33, with a positive evolution as strong as α gsim 1.3 excluded at more than 99% confidence level. A direct match between the characteristic BH mass in the VDF-based and quasar LF-based BH mass functions also yields a mean Eddington ratio of λ ~ 0.5-1 that is roughly constant within 0 lsim z lsim 3. A strong positive evolution in the M BH-σ relation is still allowed by the data if galaxies increase, on average, their velocity dispersions since the moment of formation due to dissipative processes. If we assume that the mean velocity dispersion of the host galaxies evolves as σ(z) = σ(0) × (1 + z)-γ, we find a lower limit of γ gsim 0.23 for α gsim 1.5. The latter estimate represents an interesting constraint for galaxy evolution models and can be tested through hydro simulations. This dissipative model, however, also implies a decreasing λ at higher z, at variance with several independent studies.","lang":"eng"}],"publication_identifier":{"issn":["0004-637X","1538-4357"]},"citation":{"mla":"Shankar, Francesco, et al. “The Evolution of the Mbh-σ Relation Inferred from the Age Distribution of Local Early-Type Galaxies and Active Galactic Nuclei Evolution.” <i>The Astrophysical Journal</i>, vol. 694, no. 2, American Astronomical Society, 2009, pp. 867–78, doi:<a href=\"https://doi.org/10.1088/0004-637x/694/2/867\">10.1088/0004-637x/694/2/867</a>.","apa":"Shankar, F., Bernardi, M., &#38; Haiman, Z. (2009). The evolution of the mbh-σ relation inferred from the age distribution of local early-type galaxies and active galactic nuclei evolution. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1088/0004-637x/694/2/867\">https://doi.org/10.1088/0004-637x/694/2/867</a>","ieee":"F. Shankar, M. Bernardi, and Z. Haiman, “The evolution of the mbh-σ relation inferred from the age distribution of local early-type galaxies and active galactic nuclei evolution,” <i>The Astrophysical Journal</i>, vol. 694, no. 2. American Astronomical Society, pp. 867–878, 2009.","ista":"Shankar F, Bernardi M, Haiman Z. 2009. The evolution of the mbh-σ relation inferred from the age distribution of local early-type galaxies and active galactic nuclei evolution. The Astrophysical Journal. 694(2), 867–878.","chicago":"Shankar, Francesco, Mariangela Bernardi, and Zoltán Haiman. “The Evolution of the Mbh-σ Relation Inferred from the Age Distribution of Local Early-Type Galaxies and Active Galactic Nuclei Evolution.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2009. <a href=\"https://doi.org/10.1088/0004-637x/694/2/867\">https://doi.org/10.1088/0004-637x/694/2/867</a>.","short":"F. Shankar, M. Bernardi, Z. Haiman, The Astrophysical Journal 694 (2009) 867–878.","ama":"Shankar F, Bernardi M, Haiman Z. The evolution of the mbh-σ relation inferred from the age distribution of local early-type galaxies and active galactic nuclei evolution. <i>The Astrophysical Journal</i>. 2009;694(2):867-878. doi:<a href=\"https://doi.org/10.1088/0004-637x/694/2/867\">10.1088/0004-637x/694/2/867</a>"},"doi":"10.1088/0004-637x/694/2/867","title":"The evolution of the mbh-σ relation inferred from the age distribution of local early-type galaxies and active galactic nuclei evolution","date_updated":"2024-09-30T10:55:28Z","publisher":"American Astronomical Society","_id":"17772","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","month":"03","language":[{"iso":"eng"}],"scopus_import":"1","main_file_link":[{"url":"https://doi.org/10.1088/0004-637x/694/2/867"}],"oa_version":"Published Version"},{"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1088/0004-637X/701/1/360"}],"oa_version":"Published Version","month":"07","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","date_updated":"2024-10-02T07:26:28Z","_id":"17797","publisher":"American Astronomical Society","title":"On the occupation fraction of seed black holes in high-redshift dark matter halos","article_processing_charge":"No","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"abstract":[{"lang":"eng","text":"It is well known that an initial population of seed black holes (BHs), formed in the nuclei of low-mass galaxies at high redshift, can simultaneously explain, through their subsequent growth by mergers and accretion, both the observed evolution of the quasar luminosity function (LF) and the distribution of remnant supermassive black hole (SMBH) masses measured in local galactic nuclei. Here we consider three very different initial conditions for this scenario: models in which initial seed BHs form in either all, or only a small fraction (fbh = 0.1 or 0.01) of high-redshift dark matter halos (with Mhalo = 5 × 109 M☉ at z = 6–10). We show that with a suitable and relatively minor adjustment of two global physical parameters (the radiative efficiency and mass accretion time-scale of quasar episodes), models with fbh ≈ 0.1 and 1 can accurately reproduce the observed quasar LF at redshifts 0 < z ≲ 6, as well as the remnant SMBH mass function at z = 0. However, SMBHs remain rare, and the normalization of the high-z quasar LF and the local SMBH mass function are both significantly underpredicted, if fbh ≲ 0.01. We also show that the merger history of SMBHs, in the mass range detectable by the future Laser Interferometer Space Antenna (LISA) instrument, generically looks different as fbh is varied; this should allow LISA to deliver useful constraints on otherwise degenerate models."}],"citation":{"ama":"Lippai Z, Frei Z, Haiman Z. On the occupation fraction of seed black holes in high-redshift dark matter halos. <i>The Astrophysical Journal</i>. 2009;701(1):360-368. doi:<a href=\"https://doi.org/10.1088/0004-637x/701/1/360\">10.1088/0004-637x/701/1/360</a>","chicago":"Lippai, Zoltán, Zsolt Frei, and Zoltán Haiman. “On the Occupation Fraction of Seed Black Holes in High-Redshift Dark Matter Halos.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2009. <a href=\"https://doi.org/10.1088/0004-637x/701/1/360\">https://doi.org/10.1088/0004-637x/701/1/360</a>.","short":"Z. Lippai, Z. Frei, Z. Haiman, The Astrophysical Journal 701 (2009) 360–368.","ista":"Lippai Z, Frei Z, Haiman Z. 2009. On the occupation fraction of seed black holes in high-redshift dark matter halos. The Astrophysical Journal. 701(1), 360–368.","ieee":"Z. Lippai, Z. Frei, and Z. Haiman, “On the occupation fraction of seed black holes in high-redshift dark matter halos,” <i>The Astrophysical Journal</i>, vol. 701, no. 1. American Astronomical Society, pp. 360–368, 2009.","apa":"Lippai, Z., Frei, Z., &#38; Haiman, Z. (2009). On the occupation fraction of seed black holes in high-redshift dark matter halos. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1088/0004-637x/701/1/360\">https://doi.org/10.1088/0004-637x/701/1/360</a>","mla":"Lippai, Zoltán, et al. “On the Occupation Fraction of Seed Black Holes in High-Redshift Dark Matter Halos.” <i>The Astrophysical Journal</i>, vol. 701, no. 1, American Astronomical Society, 2009, pp. 360–68, doi:<a href=\"https://doi.org/10.1088/0004-637x/701/1/360\">10.1088/0004-637x/701/1/360</a>."},"doi":"10.1088/0004-637x/701/1/360","article_type":"original","quality_controlled":"1","volume":701,"page":"360-368","author":[{"first_name":"Zoltán","full_name":"Lippai, Zoltán","last_name":"Lippai"},{"last_name":"Frei","full_name":"Frei, Zsolt","first_name":"Zsolt"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","orcid":"0000-0003-3633-5403","first_name":"Zoltán","full_name":"Haiman, Zoltán"}],"day":"22","status":"public","extern":"1","year":"2009","intvolume":"       701","type":"journal_article","issue":"1","date_created":"2024-09-06T10:29:07Z","date_published":"2009-07-22T00:00:00Z","oa":1,"fulldoi":"https://doi.org/10.1088/0004-637x/701/1/360","publication_status":"published","publication":"The Astrophysical Journal"},{"title":"GRB 080913 at redshift 6.7","publisher":"American Astronomical Society","_id":"17805","date_updated":"2024-11-12T10:14:41Z","external_id":{"arxiv":["0810.2314"]},"article_processing_charge":"No","citation":{"mla":"Greiner, J., et al. “GRB 080913 at Redshift 6.7.” <i>The Astrophysical Journal</i>, vol. 693, no. 2, American Astronomical Society, 2009, pp. 1610–20, doi:<a href=\"https://doi.org/10.1088/0004-637x/693/2/1610\">10.1088/0004-637x/693/2/1610</a>.","apa":"Greiner, J., Krühler, T., Fynbo, J. P. U., Rossi, A., Schwarz, R., Klose, S., … Wiersema, K. (2009). GRB 080913 at redshift 6.7. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1088/0004-637x/693/2/1610\">https://doi.org/10.1088/0004-637x/693/2/1610</a>","ieee":"J. Greiner <i>et al.</i>, “GRB 080913 at redshift 6.7,” <i>The Astrophysical Journal</i>, vol. 693, no. 2. American Astronomical Society, pp. 1610–1620, 2009.","ista":"Greiner J, Krühler T, Fynbo JPU, Rossi A, Schwarz R, Klose S, Savaglio S, Tanvir NR, McBreen S, Totani T, Zhang BB, Wu XF, Watson D, Barthelmy SD, Beardmore AP, Ferrero P, Gehrels N, Kann DA, Kawai N, Yoldaş AK, Mészáros P, Milvang-Jensen B, Oates SR, Pierini D, Schady P, Toma K, Vreeswijk PM, Yoldaş A, Zhang B, Afonso P, Aoki K, Burrows DN, Clemens C, Filgas R, Haiman Z, Hartmann DH, Hasinger G, Hjorth J, Jehin E, Levan AJ, Liang EW, Malesani D, Pyo T-S, Schulze S, Szokoly G, Terada K, Wiersema K. 2009. GRB 080913 at redshift 6.7. The Astrophysical Journal. 693(2), 1610–1620.","chicago":"Greiner, J., T. Krühler, J. P. U. Fynbo, A. Rossi, R. Schwarz, S. Klose, S. Savaglio, et al. “GRB 080913 at Redshift 6.7.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2009. <a href=\"https://doi.org/10.1088/0004-637x/693/2/1610\">https://doi.org/10.1088/0004-637x/693/2/1610</a>.","short":"J. Greiner, T. Krühler, J.P.U. Fynbo, A. Rossi, R. Schwarz, S. Klose, S. Savaglio, N.R. Tanvir, S. McBreen, T. Totani, B.B. Zhang, X.F. Wu, D. Watson, S.D. Barthelmy, A.P. Beardmore, P. Ferrero, N. Gehrels, D.A. Kann, N. Kawai, A.K. Yoldaş, P. Mészáros, B. Milvang-Jensen, S.R. Oates, D. Pierini, P. Schady, K. Toma, P.M. Vreeswijk, A. Yoldaş, B. Zhang, P. Afonso, K. Aoki, D.N. Burrows, C. Clemens, R. Filgas, Z. Haiman, D.H. Hartmann, G. Hasinger, J. Hjorth, E. Jehin, A.J. Levan, E.W. Liang, D. Malesani, T.-S. Pyo, S. Schulze, G. Szokoly, K. Terada, K. Wiersema, The Astrophysical Journal 693 (2009) 1610–1620.","ama":"Greiner J, Krühler T, Fynbo JPU, et al. GRB 080913 at redshift 6.7. <i>The Astrophysical Journal</i>. 2009;693(2):1610-1620. doi:<a href=\"https://doi.org/10.1088/0004-637x/693/2/1610\">10.1088/0004-637x/693/2/1610</a>"},"doi":"10.1088/0004-637x/693/2/1610","publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"abstract":[{"text":"We report on the detection by Swift of GRB 080913, and subsequent optical/near-infrared follow-up observations by GROND, which led to the discovery of its optical/NIR afterglow and the recognition of its high-z nature via the detection of a spectral break between the i' and z' bands. Spectroscopy obtained at the ESO-VLT revealed a continuum extending down to λ = 9400 Å, and zero flux for 7500 Å<λ < 9400 Å, which we interpret as the onset of a Gunn–Peterson trough at z = 6.695± 0.025 (95.5% confidence level), making GRB 080913 the highest-redshift gamma-ray burst (GRB) to date, and more distant than the highest-redshift QSO. We note that many redshift indicators that are based on promptly available burst or afterglow properties have failed for GRB 080913. We report on our follow-up campaign and compare the properties of GRB 080913 with bursts at lower redshift. In particular, since the afterglow of this burst is fainter than typical for GRBs, we show that 2 m class telescopes can identify most high-redshift GRBs.","lang":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"month":"03","scopus_import":"1","main_file_link":[{"url":"https://doi.org/10.48550/arXiv.0810.2314","open_access":"1"}],"oa_version":"Preprint","date_created":"2024-09-06T11:33:49Z","oa":1,"date_published":"2009-03-10T00:00:00Z","intvolume":"       693","extern":"1","status":"public","year":"2009","issue":"2","type":"journal_article","arxiv":1,"publication_status":"published","fulldoi":"https://doi.org/10.1088/0004-637x/693/2/1610","publication":"The Astrophysical Journal","volume":693,"OA_type":"free access","article_type":"original","quality_controlled":"1","author":[{"last_name":"Greiner","first_name":"J.","full_name":"Greiner, J."},{"last_name":"Krühler","full_name":"Krühler, T.","first_name":"T."},{"last_name":"Fynbo","first_name":"J. P. U.","full_name":"Fynbo, J. P. U."},{"last_name":"Rossi","first_name":"A.","full_name":"Rossi, A."},{"last_name":"Schwarz","first_name":"R.","full_name":"Schwarz, R."},{"last_name":"Klose","first_name":"S.","full_name":"Klose, S."},{"last_name":"Savaglio","full_name":"Savaglio, S.","first_name":"S."},{"last_name":"Tanvir","full_name":"Tanvir, N. R.","first_name":"N. R."},{"full_name":"McBreen, S.","first_name":"S.","last_name":"McBreen"},{"full_name":"Totani, T.","first_name":"T.","last_name":"Totani"},{"first_name":"B. B.","full_name":"Zhang, B. B.","last_name":"Zhang"},{"last_name":"Wu","full_name":"Wu, X. F.","first_name":"X. F."},{"first_name":"D.","full_name":"Watson, D.","last_name":"Watson"},{"first_name":"S. D.","full_name":"Barthelmy, S. D.","last_name":"Barthelmy"},{"last_name":"Beardmore","first_name":"A. P.","full_name":"Beardmore, A. P."},{"last_name":"Ferrero","first_name":"P.","full_name":"Ferrero, P."},{"full_name":"Gehrels, N.","first_name":"N.","last_name":"Gehrels"},{"full_name":"Kann, D. A.","first_name":"D. A.","last_name":"Kann"},{"first_name":"N.","full_name":"Kawai, N.","last_name":"Kawai"},{"full_name":"Yoldaş, A. Küpcü","first_name":"A. Küpcü","last_name":"Yoldaş"},{"last_name":"Mészáros","first_name":"P.","full_name":"Mészáros, P."},{"last_name":"Milvang-Jensen","full_name":"Milvang-Jensen, B.","first_name":"B."},{"first_name":"S. R.","full_name":"Oates, S. R.","last_name":"Oates"},{"first_name":"D.","full_name":"Pierini, D.","last_name":"Pierini"},{"full_name":"Schady, P.","first_name":"P.","last_name":"Schady"},{"last_name":"Toma","first_name":"K.","full_name":"Toma, K."},{"first_name":"P. M.","full_name":"Vreeswijk, P. M.","last_name":"Vreeswijk"},{"last_name":"Yoldaş","full_name":"Yoldaş, A.","first_name":"A."},{"last_name":"Zhang","first_name":"B.","full_name":"Zhang, B."},{"full_name":"Afonso, P.","first_name":"P.","last_name":"Afonso"},{"last_name":"Aoki","first_name":"K.","full_name":"Aoki, K."},{"last_name":"Burrows","full_name":"Burrows, D. N.","first_name":"D. N."},{"last_name":"Clemens","first_name":"C.","full_name":"Clemens, C."},{"first_name":"R.","full_name":"Filgas, R.","last_name":"Filgas"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","orcid":"0000-0003-3633-5403","last_name":"Haiman"},{"first_name":"D. H.","full_name":"Hartmann, D. H.","last_name":"Hartmann"},{"full_name":"Hasinger, G.","first_name":"G.","last_name":"Hasinger"},{"last_name":"Hjorth","full_name":"Hjorth, J.","first_name":"J."},{"last_name":"Jehin","first_name":"E.","full_name":"Jehin, E."},{"last_name":"Levan","full_name":"Levan, A. J.","first_name":"A. J."},{"last_name":"Liang","first_name":"E. W.","full_name":"Liang, E. W."},{"last_name":"Malesani","full_name":"Malesani, D.","first_name":"D."},{"first_name":"T.-S.","full_name":"Pyo, T.-S.","last_name":"Pyo"},{"full_name":"Schulze, S.","first_name":"S.","last_name":"Schulze"},{"first_name":"G.","full_name":"Szokoly, G.","last_name":"Szokoly"},{"first_name":"K.","full_name":"Terada, K.","last_name":"Terada"},{"last_name":"Wiersema","first_name":"K.","full_name":"Wiersema, K."}],"day":"10","OA_place":"repository","page":"1610-1620"},{"intvolume":"       700","related_material":{"link":[{"url":"https://doi.org/10.3847/1538-4357/ac93f7","relation":"erratum"}]},"extern":"1","status":"public","year":"2009","issue":"2","type":"journal_article","date_created":"2024-09-06T11:38:01Z","oa":1,"date_published":"2009-07-17T00:00:00Z","publication_status":"published","fulldoi":"https://doi.org/10.1088/0004-637x/700/2/1952","publication":"The Astrophysical Journal","article_type":"original","quality_controlled":"1","volume":700,"page":"1952-1969","author":[{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","full_name":"Haiman, Zoltán","first_name":"Zoltán"},{"full_name":"Kocsis, Bence","first_name":"Bence","last_name":"Kocsis"},{"last_name":"Menou","first_name":"Kristen","full_name":"Menou, Kristen"}],"day":"17","_id":"17809","publisher":"American Astronomical Society","date_updated":"2024-09-18T12:26:50Z","title":"The population of viscosity- and gravitational wave-driven supermassive black hole binaries among luminous active galactic nuclei","article_processing_charge":"No","citation":{"ama":"Haiman Z, Kocsis B, Menou K. The population of viscosity- and gravitational wave-driven supermassive black hole binaries among luminous active galactic nuclei. <i>The Astrophysical Journal</i>. 2009;700(2):1952-1969. doi:<a href=\"https://doi.org/10.1088/0004-637x/700/2/1952\">10.1088/0004-637x/700/2/1952</a>","short":"Z. Haiman, B. Kocsis, K. Menou, The Astrophysical Journal 700 (2009) 1952–1969.","chicago":"Haiman, Zoltán, Bence Kocsis, and Kristen Menou. “The Population of Viscosity- and Gravitational Wave-Driven Supermassive Black Hole Binaries among Luminous Active Galactic Nuclei.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2009. <a href=\"https://doi.org/10.1088/0004-637x/700/2/1952\">https://doi.org/10.1088/0004-637x/700/2/1952</a>.","ista":"Haiman Z, Kocsis B, Menou K. 2009. The population of viscosity- and gravitational wave-driven supermassive black hole binaries among luminous active galactic nuclei. The Astrophysical Journal. 700(2), 1952–1969.","ieee":"Z. Haiman, B. Kocsis, and K. Menou, “The population of viscosity- and gravitational wave-driven supermassive black hole binaries among luminous active galactic nuclei,” <i>The Astrophysical Journal</i>, vol. 700, no. 2. American Astronomical Society, pp. 1952–1969, 2009.","apa":"Haiman, Z., Kocsis, B., &#38; Menou, K. (2009). The population of viscosity- and gravitational wave-driven supermassive black hole binaries among luminous active galactic nuclei. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1088/0004-637x/700/2/1952\">https://doi.org/10.1088/0004-637x/700/2/1952</a>","mla":"Haiman, Zoltán, et al. “The Population of Viscosity- and Gravitational Wave-Driven Supermassive Black Hole Binaries among Luminous Active Galactic Nuclei.” <i>The Astrophysical Journal</i>, vol. 700, no. 2, American Astronomical Society, 2009, pp. 1952–69, doi:<a href=\"https://doi.org/10.1088/0004-637x/700/2/1952\">10.1088/0004-637x/700/2/1952</a>."},"doi":"10.1088/0004-637x/700/2/1952","publication_identifier":{"issn":["0004-637X","1538-4357"]},"abstract":[{"text":"Supermassive black hole binaries (SMBHBs) in galactic nuclei are thought to be a common by-product of major galaxy mergers. We use simple disk models for the circumbinary gas and for the binary–disk interaction to follow the orbital decay of SMBHBs with a range of total masses (M) and mass ratios (q), through physically distinct regions of the disk, until gravitational waves (GWs) take over their evolution. Prior to the GW-driven phase, the viscous decay is generically in the stalled \"secondary-dominated\" regime. SMBHBs spend a non-negligible fraction of a fiducial time of 107 yr at orbital periods between days ≲torb≲ yr, and we argue that they may be sufficiently common to be detectable, provided they are luminous during these stages. A dedicated optical or X-ray survey could identify coalescing SMBHBs statistically, as a population of periodically variable quasars, whose abundance obeys the scaling Nvar ∝ tαvar within a range of periods around tvar∼ tens of weeks. SMBHBs with M ≲ 107 M☉, with 0.5 ≲ α ≲ 1.5, would probe the physics of viscous orbital decay, whereas the detection of a population of higher-mass binaries, with α = 8/3, would confirm that their decay is driven by GWs. The lowest-mass SMBHBs (M ≲ 105–6 M☉) enter the GW-driven regime at short orbital periods, when they are already in the frequency band of the Laser Interferometric Space Antenna (LISA). While viscous processes are negligible in the last few years of coalescence, they could reduce the amplitude of any unresolved background due to near-stationary LISA sources. We discuss modest constraints on the SMBHB population already available from existing data, and the sensitivity and sky coverage requirements for a detection in future surveys. SMBHBs may also be identified from velocity shifts in their spectra; we discuss the expected abundance of SMBHBs as a function of their orbital velocity.","lang":"eng"}],"main_file_link":[{"url":"https://doi.org/10.1088/0004-637X/700/2/1952","open_access":"1"}],"oa_version":"Published Version","month":"07","language":[{"iso":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","scopus_import":"1"},{"title":"Premerger localization of gravitational wave standard sirens with LISA: Triggered search for an electromagnetic counterpart","_id":"17734","publisher":"American Astronomical Society","date_updated":"2024-09-26T07:56:49Z","citation":{"mla":"Kocsis, Bence, et al. “Premerger Localization of Gravitational Wave Standard Sirens with LISA: Triggered Search for an Electromagnetic Counterpart.” <i>The Astrophysical Journal</i>, vol. 684, no. 2, American Astronomical Society, 2008, pp. 870–87, doi:<a href=\"https://doi.org/10.1086/590230\">10.1086/590230</a>.","apa":"Kocsis, B., Haiman, Z., &#38; Menou, K. (2008). Premerger localization of gravitational wave standard sirens with LISA: Triggered search for an electromagnetic counterpart. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/590230\">https://doi.org/10.1086/590230</a>","short":"B. Kocsis, Z. Haiman, K. Menou, The Astrophysical Journal 684 (2008) 870–887.","chicago":"Kocsis, Bence, Zoltán Haiman, and Kristen Menou. “Premerger Localization of Gravitational Wave Standard Sirens with LISA: Triggered Search for an Electromagnetic Counterpart.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2008. <a href=\"https://doi.org/10.1086/590230\">https://doi.org/10.1086/590230</a>.","ama":"Kocsis B, Haiman Z, Menou K. Premerger localization of gravitational wave standard sirens with LISA: Triggered search for an electromagnetic counterpart. <i>The Astrophysical Journal</i>. 2008;684(2):870-887. doi:<a href=\"https://doi.org/10.1086/590230\">10.1086/590230</a>","ieee":"B. Kocsis, Z. Haiman, and K. Menou, “Premerger localization of gravitational wave standard sirens with LISA: Triggered search for an electromagnetic counterpart,” <i>The Astrophysical Journal</i>, vol. 684, no. 2. American Astronomical Society, pp. 870–887, 2008.","ista":"Kocsis B, Haiman Z, Menou K. 2008. Premerger localization of gravitational wave standard sirens with LISA: Triggered search for an electromagnetic counterpart. The Astrophysical Journal. 684(2), 870–887."},"doi":"10.1086/590230","abstract":[{"lang":"eng","text":"Electromagnetic (EM) counterparts to supermassive black hole binary mergers observed by LISA can be localized to within the field of view of astronomical instruments ~10 deg^2 hours to weeks prior to coalescence. The temporal coincidence of any prompt EM counterpart with a gravitationally-timed merger may offer the best chance of identifying a unique host galaxy. We discuss the challenges posed by searches for prompt EM counterparts and propose novel observational strategies to address them. In particular, we discuss the size and shape evolution of the LISA localization error ellipses on the sky, and quantify the requirements for dedicated EM surveys of the area prior to coalescence. A triggered EM counterpart search campaign will require monitoring a several-square degree area. It could aim for variability at the 24-27 mag level in optical bands, for example, which corresponds to 1-10% of the Eddington luminosity of the prime LISA sources of 10^6-10^7 Msun BHs at z=1-2, on time-scales of minutes to hours, the orbital time-scale of the binary in the last 2-4 weeks. A cross-correlation of the period of any variable EM signal with the quasi-periodic gravitational waveform over 10-1000 cycles may aid the detection. Alternatively, EM searches can detect a transient signal accompanying the coalescence. We highlight the measurement of differences in the arrival times of photons and gravitons from the same cosmological source as a valuable independent test of the massive character of gravity, and of possible violations of Lorentz invariance in the gravity sector."}],"publication_identifier":{"issn":["0004-637X","1538-4357"]},"article_processing_charge":"No","scopus_import":"1","language":[{"iso":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","month":"09","oa_version":"Published Version","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1086/590230"}],"oa":1,"date_published":"2008-09-10T00:00:00Z","date_created":"2024-09-06T09:18:47Z","issue":"2","type":"journal_article","intvolume":"       684","extern":"1","year":"2008","status":"public","publication":"The Astrophysical Journal","publication_status":"published","fulldoi":"https://doi.org/10.1086/590230","volume":684,"quality_controlled":"1","article_type":"original","day":"10","author":[{"first_name":"Bence","full_name":"Kocsis, Bence","last_name":"Kocsis"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"},{"full_name":"Menou, Kristen","first_name":"Kristen","last_name":"Menou"}],"page":"870-887"},{"doi":"10.1086/587034","citation":{"mla":"Lippai, Zoltán, et al. “Prompt Shocks in the Gas Disk around a Recoiling Supermassive Black Hole Binary.” <i>The Astrophysical Journal</i>, vol. 676, no. 1, American Astronomical Society, 2008, pp. L5–8, doi:<a href=\"https://doi.org/10.1086/587034\">10.1086/587034</a>.","apa":"Lippai, Z., Frei, Z., &#38; Haiman, Z. (2008). Prompt shocks in the gas disk around a recoiling supermassive black hole binary. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/587034\">https://doi.org/10.1086/587034</a>","ieee":"Z. Lippai, Z. Frei, and Z. Haiman, “Prompt shocks in the gas disk around a recoiling supermassive black hole binary,” <i>The Astrophysical Journal</i>, vol. 676, no. 1. American Astronomical Society, pp. L5–L8, 2008.","ista":"Lippai Z, Frei Z, Haiman Z. 2008. Prompt shocks in the gas disk around a recoiling supermassive black hole binary. The Astrophysical Journal. 676(1), L5–L8.","short":"Z. Lippai, Z. Frei, Z. Haiman, The Astrophysical Journal 676 (2008) L5–L8.","chicago":"Lippai, Zoltán, Zsolt Frei, and Zoltán Haiman. “Prompt Shocks in the Gas Disk around a Recoiling Supermassive Black Hole Binary.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2008. <a href=\"https://doi.org/10.1086/587034\">https://doi.org/10.1086/587034</a>.","ama":"Lippai Z, Frei Z, Haiman Z. Prompt shocks in the gas disk around a recoiling supermassive black hole binary. <i>The Astrophysical Journal</i>. 2008;676(1):L5-L8. doi:<a href=\"https://doi.org/10.1086/587034\">10.1086/587034</a>"},"publication_identifier":{"issn":["0004-637X","1538-4357"]},"abstract":[{"text":"Supermassive black hole binaries (BHBs) produced in galaxy mergers recoil at the time of their coalescence due to the emission of gravitational waves (GWs). We simulate the response of a thin, 2D disk of collisionless particles, initially on circular orbits around a 10^6 M_sun BHB, to kicks that are either parallel or perpendicular to the initial orbital plane. Typical kick velocities (v_k) can exceed the sound speed in a circumbinary gas disk. While the inner disk is strongly bound to the recoiling binary, the outer disk is only weakly bound or unbound. This leads to differential motions in the disturbed disk that increase with radius and can become supersonic at ~700 Schwarzschild radii for v_k ~500 km/s, implying that shocks form beyond this radius. We indeed find that kicks in the disk plane lead to immediate strong density enhancements (within weeks) in a tightly wound spiral caustic, propagating outward at the speed v_k. Concentric density enhancements are also observed for kicks perpendicular to the disk, but are weaker and develop into caustics only after a long delay (>1 year). Unless both BH spins are low or precisely aligned with the orbital angular momentum, a significant fraction (> several %) of kicks are sufficiently large and well aligned with the orbital plane for strong shocks to be produced. The shocks could result in an afterglow whose characteristic photon energy increases with time, from the UV (~10eV) to the soft X-ray (~100eV) range, between one month and one year after the merger. This could help identify EM counterparts to GW sources discovered by LISA.","lang":"eng"}],"article_processing_charge":"No","title":"Prompt shocks in the gas disk around a recoiling supermassive black hole binary","_id":"17752","publisher":"American Astronomical Society","date_updated":"2024-09-30T07:50:45Z","scopus_import":"1","month":"03","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"oa_version":"Published Version","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1086/587034"}],"publication":"The Astrophysical Journal","publication_status":"published","fulldoi":"https://doi.org/10.1086/587034","oa":1,"date_published":"2008-03-20T00:00:00Z","date_created":"2024-09-06T09:40:05Z","issue":"1","type":"journal_article","intvolume":"       676","extern":"1","status":"public","year":"2008","day":"20","author":[{"full_name":"Lippai, Zoltán","first_name":"Zoltán","last_name":"Lippai"},{"first_name":"Zsolt","full_name":"Frei, Zsolt","last_name":"Frei"},{"full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"}],"page":"L5-L8","volume":676,"quality_controlled":"1","article_type":"original"},{"publisher":"American Astronomical Society","_id":"17756","date_updated":"2024-09-30T08:39:17Z","title":"Oxygen pumping. II. Probing the inhomogeneous metal enrichment at the epoch of reionization with high‐frequency CMB observations","citation":{"ama":"Hernandez‐Monteagudo C, Haiman Z, Verde L, Jimenez R. Oxygen pumping. II. Probing the inhomogeneous metal enrichment at the epoch of reionization with high‐frequency CMB observations. <i>The Astrophysical Journal</i>. 2008;672(1):33-39. doi:<a href=\"https://doi.org/10.1086/523872\">10.1086/523872</a>","chicago":"Hernandez‐Monteagudo, Carlos, Zoltán Haiman, Licia Verde, and Raul Jimenez. “Oxygen Pumping. II. Probing the Inhomogeneous Metal Enrichment at the Epoch of Reionization with High‐frequency CMB Observations.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2008. <a href=\"https://doi.org/10.1086/523872\">https://doi.org/10.1086/523872</a>.","short":"C. Hernandez‐Monteagudo, Z. Haiman, L. Verde, R. Jimenez, The Astrophysical Journal 672 (2008) 33–39.","ista":"Hernandez‐Monteagudo C, Haiman Z, Verde L, Jimenez R. 2008. Oxygen pumping. II. Probing the inhomogeneous metal enrichment at the epoch of reionization with high‐frequency CMB observations. The Astrophysical Journal. 672(1), 33–39.","ieee":"C. Hernandez‐Monteagudo, Z. Haiman, L. Verde, and R. Jimenez, “Oxygen pumping. II. Probing the inhomogeneous metal enrichment at the epoch of reionization with high‐frequency CMB observations,” <i>The Astrophysical Journal</i>, vol. 672, no. 1. American Astronomical Society, pp. 33–39, 2008.","apa":"Hernandez‐Monteagudo, C., Haiman, Z., Verde, L., &#38; Jimenez, R. (2008). Oxygen pumping. II. Probing the inhomogeneous metal enrichment at the epoch of reionization with high‐frequency CMB observations. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/523872\">https://doi.org/10.1086/523872</a>","mla":"Hernandez‐Monteagudo, Carlos, et al. “Oxygen Pumping. II. Probing the Inhomogeneous Metal Enrichment at the Epoch of Reionization with High‐frequency CMB Observations.” <i>The Astrophysical Journal</i>, vol. 672, no. 1, American Astronomical Society, 2008, pp. 33–39, doi:<a href=\"https://doi.org/10.1086/523872\">10.1086/523872</a>."},"doi":"10.1086/523872","abstract":[{"text":"At the epoch of reionization, when the high-redshift inter-galactic medium (IGM) is being enriched with metals, the 63.2 micron fine structure line of OI is pumped by the ~ 1300 AA soft UV background and introduces a spectral distortion in the Cosmic Microwave Background (CMB). Here we use a toy model for the spatial distribution of neutral oxygen, assuming metal bubbles surround dark matter halos, and compute the fluctuations of this distortion, and the angular power spectrum it imprints on the CMB. We discuss the dependence of the power spectrum on the velocity of the winds polluting the IGM with metals, the minimum mass of the halos producing these winds, and on the cosmic epoch when the OI pumping occurs. We find that, although the clustering signal of the CMB distortion is weak \\delta y_{rms} ~ 10^{-7} (roughly corresponding to a temperature anisotropy of few nK), it may be reachable in deep integrations with high-sensitivity infrared detectors. Even without a detection, these instruments should be able to useful constraints on the heavy element enrichment history of the IGM.","lang":"eng"}],"publication_identifier":{"issn":["0004-637X","1538-4357"]},"article_processing_charge":"No","oa_version":"Published Version","main_file_link":[{"url":"https://doi.org/10.1086/523872","open_access":"1"}],"scopus_import":"1","month":"01","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"issue":"1","type":"journal_article","intvolume":"       672","status":"public","extern":"1","year":"2008","oa":1,"date_published":"2008-01-01T00:00:00Z","date_created":"2024-09-06T09:44:50Z","publication":"The Astrophysical Journal","publication_status":"published","fulldoi":"https://doi.org/10.1086/523872","quality_controlled":"1","article_type":"original","volume":672,"page":"33-39","day":"01","author":[{"first_name":"Carlos","full_name":"Hernandez‐Monteagudo, Carlos","last_name":"Hernandez‐Monteagudo"},{"last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","first_name":"Zoltán"},{"first_name":"Licia","full_name":"Verde, Licia","last_name":"Verde"},{"last_name":"Jimenez","first_name":"Raul","full_name":"Jimenez, Raul"}]},{"publication":"The Astrophysical Journal","fulldoi":"https://doi.org/10.1086/591047","publication_status":"published","date_published":"2008-10-10T00:00:00Z","oa":1,"date_created":"2024-09-06T10:19:49Z","type":"journal_article","issue":"1","extern":"1","year":"2008","status":"public","intvolume":"       686","day":"10","author":[{"first_name":"Steven R.","full_name":"Furlanetto, Steven R.","last_name":"Furlanetto"},{"last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","full_name":"Haiman, Zoltán"},{"last_name":"Oh","first_name":"S. Peng","full_name":"Oh, S. Peng"}],"page":"25-40","volume":686,"quality_controlled":"1","article_type":"original","publication_identifier":{"issn":["0004-637X","1538-4357"]},"abstract":[{"text":"One of the most dramatic signatures of the reionization era may be the enormous ionized bubbles around luminous quasars (with radii reaching ~40 comoving Mpc), which may survive as \"fossil\" ionized regions long after their source shuts off. Here we study how the inhomogeneous intergalactic medium (IGM) evolves inside such fossils. The average recombination rate declines rapidly with time, and the brief quasar episode significantly increases the mean free path inside the fossil bubbles. As a result, even a weak ionizing background generated by galaxies inside the fossil can maintain it in a relatively highly and uniformly ionized state. For example, galaxies that would ionize 20%-30% of hydrogen in a random patch of the IGM can maintain 80%-90% ionization inside the fossil for a duration much longer than the average recombination time in the IGM. Quasar fossils at z≲ 10 thus retain their identity for nearly a Hubble time and appear \"gray,\" distinct from both the average IGM (which has a \"Swiss cheese\" ionization topology and a lower mean ionized fraction) and the fully ionized bubbles around active quasars. More distant fossils, at z≳ 10, have a weaker galaxy-generated ionizing background and a higher gas density, so they can attain a Swiss cheese topology similar to the rest of the IGM, but with a smaller contrast between the ionized bubbles and the partially neutral regions separating them. Analogous He III fossils should exist around the epoch of He II/He III reionization at z ∼ 3, although rapid recombination inside the He III fossils is more common. Our model of inhomogeneous recombination also applies to \"double-reionization\" models and shows that a nonmonotonic reionization history is even more unlikely than previously thought.","lang":"eng"}],"citation":{"ama":"Furlanetto SR, Haiman Z, Oh SP. Fossil Ionized bubbles around dead quasars during reionization. <i>The Astrophysical Journal</i>. 2008;686(1):25-40. doi:<a href=\"https://doi.org/10.1086/591047\">10.1086/591047</a>","short":"S.R. Furlanetto, Z. Haiman, S.P. Oh, The Astrophysical Journal 686 (2008) 25–40.","chicago":"Furlanetto, Steven R., Zoltán Haiman, and S. Peng Oh. “Fossil Ionized Bubbles around Dead Quasars during Reionization.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2008. <a href=\"https://doi.org/10.1086/591047\">https://doi.org/10.1086/591047</a>.","ista":"Furlanetto SR, Haiman Z, Oh SP. 2008. Fossil Ionized bubbles around dead quasars during reionization. The Astrophysical Journal. 686(1), 25–40.","ieee":"S. R. Furlanetto, Z. Haiman, and S. P. Oh, “Fossil Ionized bubbles around dead quasars during reionization,” <i>The Astrophysical Journal</i>, vol. 686, no. 1. American Astronomical Society, pp. 25–40, 2008.","apa":"Furlanetto, S. R., Haiman, Z., &#38; Oh, S. P. (2008). Fossil Ionized bubbles around dead quasars during reionization. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/591047\">https://doi.org/10.1086/591047</a>","mla":"Furlanetto, Steven R., et al. “Fossil Ionized Bubbles around Dead Quasars during Reionization.” <i>The Astrophysical Journal</i>, vol. 686, no. 1, American Astronomical Society, 2008, pp. 25–40, doi:<a href=\"https://doi.org/10.1086/591047\">10.1086/591047</a>."},"doi":"10.1086/591047","article_processing_charge":"No","title":"Fossil Ionized bubbles around dead quasars during reionization","date_updated":"2024-09-30T13:04:56Z","publisher":"American Astronomical Society","_id":"17787","scopus_import":"1","language":[{"iso":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","month":"10","oa_version":"Preprint","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1086/591047"}]},{"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1086/587780"}],"oa_version":"Published Version","month":"06","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"scopus_import":"1","_id":"17788","publisher":"American Astronomical Society","date_updated":"2024-09-30T13:33:11Z","title":"An evolving entropy floor in the intracluster gas?","article_processing_charge":"No","citation":{"chicago":"Fang, Wenjuan, and Zoltán Haiman. “An Evolving Entropy Floor in the Intracluster Gas?” <i>The Astrophysical Journal</i>. American Astronomical Society, 2008. <a href=\"https://doi.org/10.1086/587780\">https://doi.org/10.1086/587780</a>.","short":"W. Fang, Z. Haiman, The Astrophysical Journal 680 (2008) 200–213.","ama":"Fang W, Haiman Z. An evolving entropy floor in the intracluster gas? <i>The Astrophysical Journal</i>. 2008;680(1):200-213. doi:<a href=\"https://doi.org/10.1086/587780\">10.1086/587780</a>","ieee":"W. Fang and Z. Haiman, “An evolving entropy floor in the intracluster gas?,” <i>The Astrophysical Journal</i>, vol. 680, no. 1. American Astronomical Society, pp. 200–213, 2008.","ista":"Fang W, Haiman Z. 2008. An evolving entropy floor in the intracluster gas? The Astrophysical Journal. 680(1), 200–213.","mla":"Fang, Wenjuan, and Zoltán Haiman. “An Evolving Entropy Floor in the Intracluster Gas?” <i>The Astrophysical Journal</i>, vol. 680, no. 1, American Astronomical Society, 2008, pp. 200–13, doi:<a href=\"https://doi.org/10.1086/587780\">10.1086/587780</a>.","apa":"Fang, W., &#38; Haiman, Z. (2008). An evolving entropy floor in the intracluster gas? <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/587780\">https://doi.org/10.1086/587780</a>"},"doi":"10.1086/587780","abstract":[{"text":"Nongravitational processes, such as feedback from galaxies and their active nuclei, are believed to have injected excess entropy into the intracluster gas, and therefore to have modified the density profiles in galaxy clusters during their formation. Here we study a simple model for this so-called preheating scenario, and ask (1) whether it can simultaneously explain both global X-ray scaling relations and number counts of galaxy clusters, and (2) whether the amount of entropy required evolves with redshift. We adopt a baseline entropy profile that fits recent hydrodynamic simulations, modify the hydrostatic equilibrium condition for the gas by including ≈20% nonthermal pressure support, and add an entropy floor K0 that is allowed to vary with redshift. We find that the observed luminosity-temperature (L − T) relations of low-redshift (⟨ z⟩ = 0.05) HIFLUGCS clusters and high-redshift (⟨ z⟩ = 0.80) WARPS clusters are best simultaneously reproduced with an entropy floor that evolves from ≈200 h^−1/3 keV cm^ 2 at z ≈ 0.8 to ≳300 h^−1/3 keV cm^ 2 at z < 0.05. This evolution may take place predominantly at low redshift (z≲ 0.2). If we restrict our analysis to the subset of bright (kT≳ 3 keV) clusters, we find that the evolving entropy floor can mimic a self-similar evolution in the L − T scaling relation. This degeneracy with self-similar evolution is, however, lifted when 0.5 keV ≲ kT≲ 3 keV clusters are included. Using the cosmological parameters from the WMAP 3 yr data, but treating σ8 as a free parameter, our model can reproduce the number counts of the X-ray galaxy clusters in the 158 deg2 ROSAT PSPC survey, with a best-fit value of σ8 = 0.80 ± 0.05.","lang":"eng"}],"publication_identifier":{"issn":["0004-637X","1538-4357"]},"article_type":"original","quality_controlled":"1","volume":680,"page":"200-213","author":[{"last_name":"Fang","first_name":"Wenjuan","full_name":"Fang, Wenjuan"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"}],"day":"10","intvolume":"       680","extern":"1","status":"public","year":"2008","issue":"1","type":"journal_article","date_created":"2024-09-06T10:20:50Z","oa":1,"date_published":"2008-06-10T00:00:00Z","publication_status":"published","fulldoi":"https://doi.org/10.1086/587780","publication":"The Astrophysical Journal"},{"oa_version":"Published Version","main_file_link":[{"url":"https://doi.org/10.1086/523787","open_access":"1"}],"scopus_import":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","month":"01","language":[{"iso":"eng"}],"_id":"17789","publisher":"American Astronomical Society","date_updated":"2024-09-30T13:47:04Z","title":"Can we detect the anisotropic shapes of quasar H ii regions during reionization through the small‐scale redshifted 21 cm power spectrum?","citation":{"chicago":"Sethi, Shiv, and Zoltán Haiman. “Can We Detect the Anisotropic Shapes of Quasar H Ii Regions during Reionization through the Small‐scale Redshifted 21 Cm Power Spectrum?” <i>The Astrophysical Journal</i>. American Astronomical Society, 2008. <a href=\"https://doi.org/10.1086/523787\">https://doi.org/10.1086/523787</a>.","short":"S. Sethi, Z. Haiman, The Astrophysical Journal 673 (2008) 1–13.","ama":"Sethi S, Haiman Z. Can we detect the anisotropic shapes of quasar H ii regions during reionization through the small‐scale redshifted 21 cm power spectrum? <i>The Astrophysical Journal</i>. 2008;673(1):1-13. doi:<a href=\"https://doi.org/10.1086/523787\">10.1086/523787</a>","ieee":"S. Sethi and Z. Haiman, “Can we detect the anisotropic shapes of quasar H ii regions during reionization through the small‐scale redshifted 21 cm power spectrum?,” <i>The Astrophysical Journal</i>, vol. 673, no. 1. American Astronomical Society, pp. 1–13, 2008.","ista":"Sethi S, Haiman Z. 2008. Can we detect the anisotropic shapes of quasar H ii regions during reionization through the small‐scale redshifted 21 cm power spectrum? The Astrophysical Journal. 673(1), 1–13.","mla":"Sethi, Shiv, and Zoltán Haiman. “Can We Detect the Anisotropic Shapes of Quasar H Ii Regions during Reionization through the Small‐scale Redshifted 21 Cm Power Spectrum?” <i>The Astrophysical Journal</i>, vol. 673, no. 1, American Astronomical Society, 2008, pp. 1–13, doi:<a href=\"https://doi.org/10.1086/523787\">10.1086/523787</a>.","apa":"Sethi, S., &#38; Haiman, Z. (2008). Can we detect the anisotropic shapes of quasar H ii regions during reionization through the small‐scale redshifted 21 cm power spectrum? <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/523787\">https://doi.org/10.1086/523787</a>"},"doi":"10.1086/523787","publication_identifier":{"issn":["0004-637X","1538-4357"]},"abstract":[{"lang":"eng","text":"Light-travel time delays distort the apparent shapes of H II regions surrounding bright quasars during early stages of cosmic reionization. Individual H II regions may remain undetectable in forthcoming redshifted 21 cm experiments. However, the systematic deformation along the line of sight may be detectable statistically, either by stacking tomographic 21 cm images of quasars identified, for example, by the James Webb Space Telescope, or as small-scale anisotropy in the three-dimensional 21 cm power spectrum. Here we consider the detectability of this effect. The anisotropy is largest when H II regions are large and expand rapidly, and we find that if bright quasars contributed to the early stages of reionization, then they can produce significant anisotropy, on scales comparable to the typical sizes of H II regions of the bright quasars (≲30 Mpc). The effect therefore cannot be ignored when analyzing future 21 cm power spectra on small scales. If 10% of the volume of the intergalactic medium at z≃ 10 is ionized by quasars with typical ionizing luminosity of S≳ 5 × 10^56 s^−1, the distortions cause an ≳10 percent enhancement of the 21 cm power spectrum in the radial (redshift) direction, relative to the transverse directions. The level of this anisotropy exceeds that due to redshift-space distortion and has the opposite sign. We show that ongoing experiments such as Murchison Widefield Array (MWA, formerly known as the Mileura Widefield Array) should be able to detect this effect. A detection would reveal the presence of bright quasars and shed light on the ionizing yield and age of the ionizing sources and the distribution and small-scale clumping of neutral intergalactic gas in their vicinity."}],"article_processing_charge":"No","quality_controlled":"1","article_type":"original","volume":673,"page":"1-13","day":"20","author":[{"full_name":"Sethi, Shiv","first_name":"Shiv","last_name":"Sethi"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"}],"issue":"1","type":"journal_article","intvolume":"       673","extern":"1","year":"2008","status":"public","oa":1,"date_published":"2008-01-20T00:00:00Z","date_created":"2024-09-06T10:21:39Z","publication":"The Astrophysical Journal","publication_status":"published","fulldoi":"https://doi.org/10.1086/523787"},{"title":"Can supermassive black holes form in metal‐enriched high‐redshift protogalaxies?","date_updated":"2024-11-12T10:11:29Z","_id":"17804","publisher":"American Astronomical Society","external_id":{"arxiv":["0804.3141"]},"article_processing_charge":"No","publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"abstract":[{"lang":"eng","text":"Primordial gas in protogalactic DM halos with virial temperatures Tvir≳ 104 K begins to cool and condense via atomic hydrogen. Provided that this gas is irradiated by a strong UV flux and remains free of H2 and other molecules, it has been proposed that the halo with Tvir ∼ 104 K may avoid fragmentation and lead to the rapid formation of an SMBH as massive as M ≈ 105–106 M☉. This \"head start\" would help explain the presence of SMBHs with inferred masses of several times 109 M☉, powering the bright quasars discovered in the SDSS at redshift z≳ 6. However, high-redshift DM halos with Tvir ∼ 104 K are likely already enriched with at least trace amounts of metals and dust produced by prior star formation in their progenitors. Here we study the thermal and chemical evolution of low-metallicity gas exposed to extremely strong UV radiation fields. Our results, obtained in one-zone models, suggest that gas fragmentation is inevitable above a critical metallicity, whose value is between Zcr ≈ 3 × 10−4 Z☉ (in the absence of dust) and as low as Zcr ≈ 5 × 10−6 Z☉ (with a dust-to-gas mass ratio of about 0.01Z/Z☉). We propose that when the metallicity exceeds these critical values, dense clusters of low-mass stars may form at the halo nucleus. Relatively massive stars in such a cluster can then rapidly coalesce into a single more massive object, which may produce an intermediate-mass BH remnant with a mass up to M≲ 102–103 M☉."}],"doi":"10.1086/591636","citation":{"mla":"Omukai, K., et al. “Can Supermassive Black Holes Form in Metal‐enriched High‐redshift Protogalaxies?” <i>The Astrophysical Journal</i>, vol. 686, no. 2, American Astronomical Society, 2008, pp. 801–14, doi:<a href=\"https://doi.org/10.1086/591636\">10.1086/591636</a>.","apa":"Omukai, K., Schneider, R., &#38; Haiman, Z. (2008). Can supermassive black holes form in metal‐enriched high‐redshift protogalaxies? <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/591636\">https://doi.org/10.1086/591636</a>","ieee":"K. Omukai, R. Schneider, and Z. Haiman, “Can supermassive black holes form in metal‐enriched high‐redshift protogalaxies?,” <i>The Astrophysical Journal</i>, vol. 686, no. 2. American Astronomical Society, pp. 801–814, 2008.","ista":"Omukai K, Schneider R, Haiman Z. 2008. Can supermassive black holes form in metal‐enriched high‐redshift protogalaxies? The Astrophysical Journal. 686(2), 801–814.","chicago":"Omukai, K., R. Schneider, and Zoltán Haiman. “Can Supermassive Black Holes Form in Metal‐enriched High‐redshift Protogalaxies?” <i>The Astrophysical Journal</i>. American Astronomical Society, 2008. <a href=\"https://doi.org/10.1086/591636\">https://doi.org/10.1086/591636</a>.","short":"K. Omukai, R. Schneider, Z. Haiman, The Astrophysical Journal 686 (2008) 801–814.","ama":"Omukai K, Schneider R, Haiman Z. Can supermassive black holes form in metal‐enriched high‐redshift protogalaxies? <i>The Astrophysical Journal</i>. 2008;686(2):801-814. doi:<a href=\"https://doi.org/10.1086/591636\">10.1086/591636</a>"},"language":[{"iso":"eng"}],"month":"08","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.0804.3141"}],"oa_version":"Preprint","date_created":"2024-09-06T11:33:03Z","date_published":"2008-08-20T00:00:00Z","oa":1,"status":"public","extern":"1","year":"2008","intvolume":"       686","type":"journal_article","issue":"2","fulldoi":"https://doi.org/10.1086/591636","arxiv":1,"publication_status":"published","publication":"The Astrophysical Journal","volume":686,"article_type":"original","OA_type":"free access","quality_controlled":"1","author":[{"last_name":"Omukai","first_name":"K.","full_name":"Omukai, K."},{"full_name":"Schneider, R.","first_name":"R.","last_name":"Schneider"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","orcid":"0000-0003-3633-5403","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"}],"day":"20","OA_place":"repository","page":"801-814"},{"oa":1,"date_published":"2007-11-10T00:00:00Z","date_created":"2024-09-06T08:58:16Z","issue":"2","type":"journal_article","intvolume":"       669","extern":"1","year":"2007","status":"public","publication":"The Astrophysical Journal","publication_status":"published","fulldoi":"https://doi.org/10.1086/521921","volume":669,"quality_controlled":"1","article_type":"original","day":"10","author":[{"last_name":"Spiegel","first_name":"David S.","full_name":"Spiegel, David S."},{"full_name":"Haiman, Zoltán","first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"first_name":"B. Scott","full_name":"Gaudi, B. Scott","last_name":"Gaudi"}],"page":"1324-1335","title":"On constraining a transiting exoplanet’s rotation rate with its transit spectrum","_id":"17714","publisher":"American Astronomical Society","date_updated":"2024-09-25T12:42:28Z","doi":"10.1086/521921","citation":{"mla":"Spiegel, David S., et al. “On Constraining a Transiting Exoplanet’s Rotation Rate with Its Transit Spectrum.” <i>The Astrophysical Journal</i>, vol. 669, no. 2, American Astronomical Society, 2007, pp. 1324–35, doi:<a href=\"https://doi.org/10.1086/521921\">10.1086/521921</a>.","apa":"Spiegel, D. S., Haiman, Z., &#38; Gaudi, B. S. (2007). On constraining a transiting exoplanet’s rotation rate with its transit spectrum. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/521921\">https://doi.org/10.1086/521921</a>","chicago":"Spiegel, David S., Zoltán Haiman, and B. Scott Gaudi. “On Constraining a Transiting Exoplanet’s Rotation Rate with Its Transit Spectrum.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2007. <a href=\"https://doi.org/10.1086/521921\">https://doi.org/10.1086/521921</a>.","short":"D.S. Spiegel, Z. Haiman, B.S. Gaudi, The Astrophysical Journal 669 (2007) 1324–1335.","ama":"Spiegel DS, Haiman Z, Gaudi BS. On constraining a transiting exoplanet’s rotation rate with its transit spectrum. <i>The Astrophysical Journal</i>. 2007;669(2):1324-1335. doi:<a href=\"https://doi.org/10.1086/521921\">10.1086/521921</a>","ieee":"D. S. Spiegel, Z. Haiman, and B. S. Gaudi, “On constraining a transiting exoplanet’s rotation rate with its transit spectrum,” <i>The Astrophysical Journal</i>, vol. 669, no. 2. American Astronomical Society, pp. 1324–1335, 2007.","ista":"Spiegel DS, Haiman Z, Gaudi BS. 2007. On constraining a transiting exoplanet’s rotation rate with its transit spectrum. The Astrophysical Journal. 669(2), 1324–1335."},"abstract":[{"text":"We investigate the effect of planetary rotation on the transit spectrum of an extrasolar giant planet. During ingress and egress, absorption features arising from the planet's atmosphere are Doppler shifted by of order the planet's rotational velocity (~1-2 km/s) relative to where they would be if the planet were not rotating. We focus in particular on the case of HD209458b, which ought to be at least as good a target as any other known transiting planet. For HD209458b, this shift should give rise to a small net centroid shift of ~60 cm/s on the stellar absorption lines. Using a detailed model of the transmission spectrum due to a rotating star transited by a rotating planet with an isothermal atmosphere, we simulate the effect of the planet's rotation on the shape of the spectral lines, and in particular on the magnitude of their width and centroid shift. We then use this simulation to determine the expected signal-to-noise ratio for distinguishing a rotating from a non-rotating planet, and assess how this S/N scales with various parameters of HD209458b. We find that with a 6 m telescope, an equatorial rotational velocity of ~2 km/s could be detected with a S/N~5 by accumulating the signal over many transits over the course of several years. With a 30 m telescope, the time required to make such a detection reduces to less than 2 months.","lang":"eng"}],"publication_identifier":{"issn":["0004-637X","1538-4357"]},"article_processing_charge":"No","scopus_import":"1","language":[{"iso":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","month":"11","oa_version":"Published Version","main_file_link":[{"url":"https://doi.org/10.1086/521921","open_access":"1"}]},{"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","month":"05","language":[{"iso":"eng"}],"scopus_import":"1","main_file_link":[{"url":"https://doi.org/10.1086/513688","open_access":"1"}],"oa_version":"Published Version","article_processing_charge":"No","citation":{"short":"A. Mesinger, Z. Haiman, The Astrophysical Journal 660 (2007) 923–932.","chicago":"Mesinger, Andrei, and Zoltán Haiman. “Constraints on Reionization and Source Properties from the Absorption Spectra of z &#62; 6.2 Quasars.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2007. <a href=\"https://doi.org/10.1086/513688\">https://doi.org/10.1086/513688</a>.","ama":"Mesinger A, Haiman Z. Constraints on reionization and Source Properties from the Absorption Spectra of z &#62; 6.2 quasars. <i>The Astrophysical Journal</i>. 2007;660(2):923-932. doi:<a href=\"https://doi.org/10.1086/513688\">10.1086/513688</a>","ieee":"A. Mesinger and Z. Haiman, “Constraints on reionization and Source Properties from the Absorption Spectra of z &#62; 6.2 quasars,” <i>The Astrophysical Journal</i>, vol. 660, no. 2. American Astronomical Society, pp. 923–932, 2007.","ista":"Mesinger A, Haiman Z. 2007. Constraints on reionization and Source Properties from the Absorption Spectra of z &#62; 6.2 quasars. The Astrophysical Journal. 660(2), 923–932.","mla":"Mesinger, Andrei, and Zoltán Haiman. “Constraints on Reionization and Source Properties from the Absorption Spectra of z &#62; 6.2 Quasars.” <i>The Astrophysical Journal</i>, vol. 660, no. 2, American Astronomical Society, 2007, pp. 923–32, doi:<a href=\"https://doi.org/10.1086/513688\">10.1086/513688</a>.","apa":"Mesinger, A., &#38; Haiman, Z. (2007). Constraints on reionization and Source Properties from the Absorption Spectra of z &#62; 6.2 quasars. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/513688\">https://doi.org/10.1086/513688</a>"},"doi":"10.1086/513688","publication_identifier":{"issn":["0004-637X","1538-4357"]},"abstract":[{"text":"We make use of hydrodynamical simulations of the intergalactic medium (IGM) to create model quasar absorption spectra. We compare these model spectra with the observed Keck spectra of three z>6.2 quasars with full Gunn-Peterson troughs: SDSS J1148+5251 (z=6.42), SDSS J1030+0524 (z=6.28), and SDSS J1623+3112 (z=6.22). We fit the probability density distributions (PDFs) of the observed Ly alpha optical depths with those generated from the simulation, by exploring a range of values for the size of the quasar's surrounding HII region, R_S, the volume-weighted mean neutral hydrogen fraction in the ambient IGM, x_H, and the quasar's ionizing photon emissivity, N_Q. In order to avoid averaging over possibly large sightline-to-sightline fluctuations in IGM properties, we analyze each observed quasar independently. We find the following results for J1148+5251, J1030+0524, and J1623+3112: The best-fit sizes R_S are 40, 41, and 29 (comoving) Mpc, respectively. These constraints are tight, with only ~ 10% uncertainties, comparable to those caused by redshift--determination errors. The best-fit values of N_Q are 2.1, 1.3, and 0.9 x 10^{57} s^{-1}, respectively, with a factor of ~ 2 uncertainty in each case. Finally, the best--fit values of x_H are 0.16, 1.0, and 1.0, respectively. The uncertainty in the case of J1148+5251 is large, and x_H is not well constrained. However, for both J1030+0524 and J1623+3112, we find a significant lower limit of x_H >~ 0.033. Our method is different from previous analyses of the GP absorption spectra of these quasars, and our results strengthen the evidence that the rapid end--stage of reionization is occurring near z ~ 6.","lang":"eng"}],"title":"Constraints on reionization and Source Properties from the Absorption Spectra of z > 6.2 quasars","_id":"17729","publisher":"American Astronomical Society","date_updated":"2024-09-26T07:30:51Z","author":[{"first_name":"Andrei","full_name":"Mesinger, Andrei","last_name":"Mesinger"},{"last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","first_name":"Zoltán"}],"day":"10","page":"923-932","volume":660,"article_type":"original","quality_controlled":"1","publication_status":"published","fulldoi":"https://doi.org/10.1086/513688","publication":"The Astrophysical Journal","date_created":"2024-09-06T09:15:25Z","oa":1,"date_published":"2007-05-10T00:00:00Z","intvolume":"       660","year":"2007","extern":"1","status":"public","issue":"2","type":"journal_article"},{"abstract":[{"text":"Energetic feedback processes during the formation of galaxy clusters may have heated and ionized a large fraction of the intergalactic gas in proto-cluster regions. When such a highly ionized hot ``super-bubble'' falls along the sightline to a background quasar, it would be seen as a large void, with little or no absorption, in the Lyman alpha forest. We examine the spectra of 137 quasars in the Sloan Digital Sky Survey, to search for such voids, and find no clear evidence of their existence. The size distribution of voids in the range 5-70 Angstrom (corresponding to physical sizes of approximately 3-35 comoving Mpc/h) is consistent with the standard model for the Lyman alpha forest without additional hot bubbles. We adapt a physical model for HII bubble growth during cosmological reionization (Furlanetto, Zaldarriaga and Hernquist 2004), to describe the expected size-distribution of hot super-bubbles at redshift around z = 3. This model incorporates the conjoining of bubbles around individual neighboring galaxies. Using the non-detection of voids, we find that models in which the volume filling factor of hot bubbles exceeds approximately 20 percent at z=3 can be ruled out, primarily because they overproduce the number of large (40-50 Angstrom) voids. We conclude that any pre-heating mechanism that explains galaxy cluster observations must avoid heating the low-density gas in the proto-cluster regions, either by operating relatively recently (z<3) or by depositing entropy in the high-density regions.","lang":"eng"}],"publication_identifier":{"issn":["0004-637X","1538-4357"]},"doi":"10.1086/522331","citation":{"ama":"Shang C, Crotts A, Haiman Z. Constraints on the abundance of highly ionized protocluster regions from the absence of large voids in the Lyα forest. <i>The Astrophysical Journal</i>. 2007;671(1):136-145. doi:<a href=\"https://doi.org/10.1086/522331\">10.1086/522331</a>","chicago":"Shang, Cien, Arlin Crotts, and Zoltán Haiman. “Constraints on the Abundance of Highly Ionized Protocluster Regions from the Absence of Large Voids in the Lyα Forest.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2007. <a href=\"https://doi.org/10.1086/522331\">https://doi.org/10.1086/522331</a>.","short":"C. Shang, A. Crotts, Z. Haiman, The Astrophysical Journal 671 (2007) 136–145.","ista":"Shang C, Crotts A, Haiman Z. 2007. Constraints on the abundance of highly ionized protocluster regions from the absence of large voids in the Lyα forest. The Astrophysical Journal. 671(1), 136–145.","ieee":"C. Shang, A. Crotts, and Z. Haiman, “Constraints on the abundance of highly ionized protocluster regions from the absence of large voids in the Lyα forest,” <i>The Astrophysical Journal</i>, vol. 671, no. 1. American Astronomical Society, pp. 136–145, 2007.","apa":"Shang, C., Crotts, A., &#38; Haiman, Z. (2007). Constraints on the abundance of highly ionized protocluster regions from the absence of large voids in the Lyα forest. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/522331\">https://doi.org/10.1086/522331</a>","mla":"Shang, Cien, et al. “Constraints on the Abundance of Highly Ionized Protocluster Regions from the Absence of Large Voids in the Lyα Forest.” <i>The Astrophysical Journal</i>, vol. 671, no. 1, American Astronomical Society, 2007, pp. 136–45, doi:<a href=\"https://doi.org/10.1086/522331\">10.1086/522331</a>."},"article_processing_charge":"No","title":"Constraints on the abundance of highly ionized protocluster regions from the absence of large voids in the Lyα forest","date_updated":"2024-09-26T07:42:13Z","publisher":"American Astronomical Society","_id":"17732","scopus_import":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"month":"12","oa_version":"Published Version","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1086/522331"}],"publication":"The Astrophysical Journal","fulldoi":"https://doi.org/10.1086/522331","publication_status":"published","date_published":"2007-12-10T00:00:00Z","oa":1,"date_created":"2024-09-06T09:17:23Z","type":"journal_article","issue":"1","status":"public","extern":"1","year":"2007","intvolume":"       671","day":"10","author":[{"last_name":"Shang","full_name":"Shang, Cien","first_name":"Cien"},{"last_name":"Crotts","first_name":"Arlin","full_name":"Crotts, Arlin"},{"last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","first_name":"Zoltán"}],"page":"136-145","volume":671,"quality_controlled":"1","article_type":"original"},{"article_processing_charge":"No","publication_identifier":{"issn":["0004-637X","1538-4357"]},"abstract":[{"text":"Recent observations reveal that a majority of galaxies contain a central massive object (CMO), either a supermassive black hole (SMBH) or a compact stellar nucleus, regardless of the galaxy mass or morphological type. The masses of these CMOs correlate tightly with those of the host galaxies, MCMO ≈ 0.002Mgal. Several recent studies argue that feedback from black holes can successfully explain the MBH-σ correlation in massive elliptical galaxies that contain SMBHs. However, puzzles remain in spirals or dwarf spheroids that do not appear to have black holes but instead harbor a compact central stellar cluster. Here we use three-dimensional, smoothed particle hydrodynamics simulations of both isolated and merging galaxies to study the formation and evolution of CMOs in bulgeless disk galaxies, and the transition of the CMO-host relations from late-type bulgeless spirals to early-type ellipticals. Our simulations show that the mass of the CMO correlates with that of the host galaxy in both isolated bulgeless spirals and in ellipticals formed through mergers, and that MCMO correlates with the global star formation efficiency in the galaxy. We find that the final mass of the CMO is dominated by the accreted mass, rather than the initial fragment mass, and that both the final accreted CMO mass and the recently formed stellar mass increase monotonically with the total mass of the galaxy. Our results suggest that the observed correlations may be established primarily by the depletion of gas in the central region by accretion and star formation, and may hold for all galaxy types. A systematic search for CMOs in the nuclei of bulgeless disk galaxies would offer a test of this conclusion.","lang":"eng"}],"citation":{"apa":"Li, Y., Haiman, Z., &#38; Mac Low, M. (2007). Correlations between central massive objects and their host galaxies: From bulgeless spirals to ellipticals. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/518398\">https://doi.org/10.1086/518398</a>","mla":"Li, Yuexing, et al. “Correlations between Central Massive Objects and Their Host Galaxies: From Bulgeless Spirals to Ellipticals.” <i>The Astrophysical Journal</i>, vol. 663, no. 1, American Astronomical Society, 2007, pp. 61–70, doi:<a href=\"https://doi.org/10.1086/518398\">10.1086/518398</a>.","ista":"Li Y, Haiman Z, Mac Low M. 2007. Correlations between central massive objects and their host galaxies: From bulgeless spirals to ellipticals. The Astrophysical Journal. 663(1), 61–70.","ieee":"Y. Li, Z. Haiman, and M. Mac Low, “Correlations between central massive objects and their host galaxies: From bulgeless spirals to ellipticals,” <i>The Astrophysical Journal</i>, vol. 663, no. 1. American Astronomical Society, pp. 61–70, 2007.","ama":"Li Y, Haiman Z, Mac Low M. Correlations between central massive objects and their host galaxies: From bulgeless spirals to ellipticals. <i>The Astrophysical Journal</i>. 2007;663(1):61-70. doi:<a href=\"https://doi.org/10.1086/518398\">10.1086/518398</a>","chicago":"Li, Yuexing, Zoltán Haiman, and Mordecai‐Mark Mac Low. “Correlations between Central Massive Objects and Their Host Galaxies: From Bulgeless Spirals to Ellipticals.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2007. <a href=\"https://doi.org/10.1086/518398\">https://doi.org/10.1086/518398</a>.","short":"Y. Li, Z. Haiman, M. Mac Low, The Astrophysical Journal 663 (2007) 61–70."},"doi":"10.1086/518398","title":"Correlations between central massive objects and their host galaxies: From bulgeless spirals to ellipticals","date_updated":"2024-09-26T14:06:48Z","publisher":"American Astronomical Society","_id":"17738","month":"07","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"scopus_import":"1","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1086/518398"}],"oa_version":"Published Version","fulldoi":"https://doi.org/10.1086/518398","publication_status":"published","publication":"The Astrophysical Journal","date_created":"2024-09-06T09:21:21Z","date_published":"2007-07-01T00:00:00Z","oa":1,"year":"2007","status":"public","extern":"1","intvolume":"       663","type":"journal_article","issue":"1","author":[{"last_name":"Li","first_name":"Yuexing","full_name":"Li, Yuexing"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","full_name":"Haiman, Zoltán","first_name":"Zoltán"},{"last_name":"Mac Low","first_name":"Mordecai‐Mark","full_name":"Mac Low, Mordecai‐Mark"}],"day":"01","page":"61-70","volume":663,"article_type":"original","quality_controlled":"1"},{"title":"Reconstructing the cosmic evolution of quasars from the age distribution of local early‐type galaxies","date_updated":"2024-09-30T07:55:40Z","_id":"17753","publisher":"American Astronomical Society","publication_identifier":{"issn":["0004-637X","1538-4357"]},"abstract":[{"lang":"eng","text":"We use the spectra of 22,000 nearby early-type galaxies from the Sloan Digital Sky Survey (SDSS) to determine the age distribution of these galaxies as a function of their velocity dispersion sigma_v in the range 100 km/s < sigma_v < 280 km/s. We then combine the inferred age-distributions with the local abundance of spheroids, including early-type galaxies and late-type bulges, to predict the evolution of the quasar luminosity function (LF) in the redshift range 0<z<6. We make the following simple assumptions: (i) the formation of stars in each galaxy, at the epoch identified with the mean mass-weighted stellar age, is accompanied by the prompt assembly of the nuclear supermassive black hole (SMBH); (ii) the mass of the SMBH obeys the M_bh-sigma_v correlation observed in nearby galaxies; (iii) the SMBH radiates at a fraction f_Edd of the Eddington limit for a fixed duration t_Q, and is identified as a luminous quasar during this epoch, (iv) the intrinsic dispersions in the Eddington ratio and the M_bh-sigma_v relation produce a combined scatter of Delta(log L_Q) around the mean logarithmic quasar luminosity <log L_Q> at fixed sigma_v. These assumptions require that the SMBH remnants of quasars with bolometric luminosity below L_bol=10^{12.5} f_Edd L_sun reside predominantly in bulges of late type galaxies. We find that evolution of the observed quasar LF can be fit over the entire redshift range in this simple model, 0<z<6 with the choices of Delta(log L_Q)=0.6-0.9, t_Q= (6-8)x10^7 yr, and <f_Edd>=0.3-0.5. We find no evidence that any of the model parameters evolves with redshift, supporting the strong connection between the formation of stars and nuclear SMBHs in spheroids."}],"doi":"10.1086/510840","citation":{"apa":"Haiman, Z., Jimenez, R., &#38; Bernardi, M. (2007). Reconstructing the cosmic evolution of quasars from the age distribution of local early‐type galaxies. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/510840\">https://doi.org/10.1086/510840</a>","mla":"Haiman, Zoltán, et al. “Reconstructing the Cosmic Evolution of Quasars from the Age Distribution of Local Early‐type Galaxies.” <i>The Astrophysical Journal</i>, vol. 658, no. 2, American Astronomical Society, 2007, pp. 721–30, doi:<a href=\"https://doi.org/10.1086/510840\">10.1086/510840</a>.","ama":"Haiman Z, Jimenez R, Bernardi M. Reconstructing the cosmic evolution of quasars from the age distribution of local early‐type galaxies. <i>The Astrophysical Journal</i>. 2007;658(2):721-730. doi:<a href=\"https://doi.org/10.1086/510840\">10.1086/510840</a>","short":"Z. Haiman, R. Jimenez, M. Bernardi, The Astrophysical Journal 658 (2007) 721–730.","chicago":"Haiman, Zoltán, Raul Jimenez, and Mariangela Bernardi. “Reconstructing the Cosmic Evolution of Quasars from the Age Distribution of Local Early‐type Galaxies.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2007. <a href=\"https://doi.org/10.1086/510840\">https://doi.org/10.1086/510840</a>.","ista":"Haiman Z, Jimenez R, Bernardi M. 2007. Reconstructing the cosmic evolution of quasars from the age distribution of local early‐type galaxies. The Astrophysical Journal. 658(2), 721–730.","ieee":"Z. Haiman, R. Jimenez, and M. Bernardi, “Reconstructing the cosmic evolution of quasars from the age distribution of local early‐type galaxies,” <i>The Astrophysical Journal</i>, vol. 658, no. 2. American Astronomical Society, pp. 721–730, 2007."},"article_processing_charge":"No","scopus_import":"1","language":[{"iso":"eng"}],"month":"04","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","oa_version":"Published Version","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1086/510840"}],"date_published":"2007-04-01T00:00:00Z","oa":1,"date_created":"2024-09-06T09:40:51Z","type":"journal_article","issue":"2","status":"public","extern":"1","year":"2007","intvolume":"       658","publication":"The Astrophysical Journal","fulldoi":"https://doi.org/10.1086/510840","publication_status":"published","volume":658,"quality_controlled":"1","article_type":"original","day":"01","author":[{"full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"},{"full_name":"Jimenez, Raul","first_name":"Raul","last_name":"Jimenez"},{"last_name":"Bernardi","full_name":"Bernardi, Mariangela","first_name":"Mariangela"}],"page":"721-730"},{"doi":"10.1086/518090","citation":{"ista":"Hernández-Monteagudo C, Haiman Z, Jimenez R, Verde L. 2007. Oxygen pumping: Probing intergalactic metals at the epoch of reionization. The Astrophysical Journal. 660(2), L85–L88.","ieee":"C. Hernández-Monteagudo, Z. Haiman, R. Jimenez, and L. Verde, “Oxygen pumping: Probing intergalactic metals at the epoch of reionization,” <i>The Astrophysical Journal</i>, vol. 660, no. 2. American Astronomical Society, pp. L85–L88, 2007.","ama":"Hernández-Monteagudo C, Haiman Z, Jimenez R, Verde L. Oxygen pumping: Probing intergalactic metals at the epoch of reionization. <i>The Astrophysical Journal</i>. 2007;660(2):L85-L88. doi:<a href=\"https://doi.org/10.1086/518090\">10.1086/518090</a>","chicago":"Hernández-Monteagudo, Carlos, Zoltán Haiman, Raul Jimenez, and Licia Verde. “Oxygen Pumping: Probing Intergalactic Metals at the Epoch of Reionization.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2007. <a href=\"https://doi.org/10.1086/518090\">https://doi.org/10.1086/518090</a>.","short":"C. Hernández-Monteagudo, Z. Haiman, R. Jimenez, L. Verde, The Astrophysical Journal 660 (2007) L85–L88.","apa":"Hernández-Monteagudo, C., Haiman, Z., Jimenez, R., &#38; Verde, L. (2007). Oxygen pumping: Probing intergalactic metals at the epoch of reionization. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/518090\">https://doi.org/10.1086/518090</a>","mla":"Hernández-Monteagudo, Carlos, et al. “Oxygen Pumping: Probing Intergalactic Metals at the Epoch of Reionization.” <i>The Astrophysical Journal</i>, vol. 660, no. 2, American Astronomical Society, 2007, pp. L85–88, doi:<a href=\"https://doi.org/10.1086/518090\">10.1086/518090</a>."},"publication_identifier":{"issn":["0004-637X","1538-4357"]},"abstract":[{"text":"We consider the pumping of the 63.2 μm fine-structure line of neutral O I in the high-redshift intergalactic medium (IGM), in analogy with the Wouthuysen-Field effect for the 21 cm line of cosmic H I. We show that the soft UV background at ~1300 Å can affect the population levels, and if a significant fraction of the IGM volume is filled with \"fossil H II regions\" containing neutral O I, then this can produce a nonnegligible spectral distortion in the cosmic microwave background (CMB). O I from redshift z is seen in emission at (1 + z)63.2 μm, and in the range 7 < z < 10 produces a mean spectral distortion of the CMB with y = (10^-9 to 3 × 10^-8)(Z/10^-3 Z☉)(IUV), where Z is the mean metallicity of the IGM and IUV is the UV background at 1300 Å in units of 10^-20 ergs s-1 Hz^-1 cm-2 sr^-1. A measurement of this signature can trace the metallicity at the end of the dark ages, prior to the completion of cosmic reionization, and is complementary to cosmological 21 cm studies. While future CMB experiments such as Planck could constrain the metallicity to the 10^-2 Z☉ level, specifically designed experiments could potentially achieve a detection.","lang":"eng"}],"article_processing_charge":"No","_id":"17791","publisher":"American Astronomical Society","date_updated":"2024-09-30T13:59:15Z","title":"Oxygen pumping: Probing intergalactic metals at the epoch of reionization","oa_version":"Published Version","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1086/518090"}],"scopus_import":"1","language":[{"iso":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","month":"04","publication":"The Astrophysical Journal","publication_status":"published","fulldoi":"https://doi.org/10.1086/518090","issue":"2","type":"journal_article","intvolume":"       660","year":"2007","status":"public","extern":"1","oa":1,"date_published":"2007-04-11T00:00:00Z","date_created":"2024-09-06T10:23:23Z","page":"L85-L88","day":"11","author":[{"first_name":"Carlos","full_name":"Hernández-Monteagudo, Carlos","last_name":"Hernández-Monteagudo"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"},{"last_name":"Jimenez","first_name":"Raul","full_name":"Jimenez, Raul"},{"last_name":"Verde","first_name":"Licia","full_name":"Verde, Licia"}],"quality_controlled":"1","article_type":"original","volume":660},{"oa_version":"Published Version","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1086/521323"}],"scopus_import":"1","month":"11","language":[{"iso":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_updated":"2024-09-30T14:09:15Z","publisher":"American Astronomical Society","_id":"17793","title":"The ages, metallicities, and star formation histories of early‐type galaxies in the SDSS","abstract":[{"lang":"eng","text":"We use the spectra of ~22,000 early-type galaxies, selected from the Sloan Digital Sky Survey, to infer the ages, metallicities, and star formation histories of these galaxies. We find clear evidence of \"downsizing,\" i.e., that galaxies with larger velocity dispersion have older stellar populations. In particular, we find that most early-type galaxies with velocity dispersion exceeding 200 km s-1 formed more than 90% of their current stellar mass at redshift z > 2.5. Therefore, star formation was suppressed around this redshift. We also show that chemical enrichment was rapid, lasting 1-2 Gyr, and find evidence that [Fe/H] is subsolar. We study the robustness of these results by comparing three different approaches: (1) using Lick absorption line indices, (2) fitting a single-burst stellar population model to the whole spectrum (lines and continuum), and (3) reconstructing the star formation and metallicity histories in multiple age bins, providing a method to measure mass-weighted ages and metallicities. We find good agreement between the luminosity-weighted ages and metallicities computed with these three methods."}],"publication_identifier":{"issn":["0004-637X","1538-4357"]},"doi":"10.1086/521323","citation":{"mla":"Jimenez, Raul, et al. “The Ages, Metallicities, and Star Formation Histories of Early‐type Galaxies in the SDSS.” <i>The Astrophysical Journal</i>, vol. 669, no. 2, American Astronomical Society, 2007, pp. 947–51, doi:<a href=\"https://doi.org/10.1086/521323\">10.1086/521323</a>.","apa":"Jimenez, R., Bernardi, M., Haiman, Z., Panter, B., &#38; Heavens, A. F. (2007). The ages, metallicities, and star formation histories of early‐type galaxies in the SDSS. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/521323\">https://doi.org/10.1086/521323</a>","short":"R. Jimenez, M. Bernardi, Z. Haiman, B. Panter, A.F. Heavens, The Astrophysical Journal 669 (2007) 947–951.","chicago":"Jimenez, Raul, Mariangela Bernardi, Zoltán Haiman, Ben Panter, and Alan F. Heavens. “The Ages, Metallicities, and Star Formation Histories of Early‐type Galaxies in the SDSS.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2007. <a href=\"https://doi.org/10.1086/521323\">https://doi.org/10.1086/521323</a>.","ama":"Jimenez R, Bernardi M, Haiman Z, Panter B, Heavens AF. The ages, metallicities, and star formation histories of early‐type galaxies in the SDSS. <i>The Astrophysical Journal</i>. 2007;669(2):947-951. doi:<a href=\"https://doi.org/10.1086/521323\">10.1086/521323</a>","ieee":"R. Jimenez, M. Bernardi, Z. Haiman, B. Panter, and A. F. Heavens, “The ages, metallicities, and star formation histories of early‐type galaxies in the SDSS,” <i>The Astrophysical Journal</i>, vol. 669, no. 2. American Astronomical Society, pp. 947–951, 2007.","ista":"Jimenez R, Bernardi M, Haiman Z, Panter B, Heavens AF. 2007. The ages, metallicities, and star formation histories of early‐type galaxies in the SDSS. The Astrophysical Journal. 669(2), 947–951."},"article_processing_charge":"No","quality_controlled":"1","article_type":"original","volume":669,"page":"947-951","day":"10","author":[{"last_name":"Jimenez","full_name":"Jimenez, Raul","first_name":"Raul"},{"first_name":"Mariangela","full_name":"Bernardi, Mariangela","last_name":"Bernardi"},{"full_name":"Haiman, Zoltán","first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"first_name":"Ben","full_name":"Panter, Ben","last_name":"Panter"},{"last_name":"Heavens","first_name":"Alan F.","full_name":"Heavens, Alan F."}],"type":"journal_article","issue":"2","extern":"1","year":"2007","status":"public","intvolume":"       669","date_published":"2007-11-10T00:00:00Z","oa":1,"date_created":"2024-09-06T10:25:21Z","publication":"The Astrophysical Journal","fulldoi":"https://doi.org/10.1086/521323","publication_status":"published"},{"publisher":"American Astronomical Society","_id":"17718","date_updated":"2024-09-25T13:27:16Z","title":"Feedback from clustered sources during reionization","article_processing_charge":"No","doi":"10.1086/506906","citation":{"chicago":"Kramer, Roban Hultman, Zoltán Haiman, and S. Peng Oh. “Feedback from Clustered Sources during Reionization.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2006. <a href=\"https://doi.org/10.1086/506906\">https://doi.org/10.1086/506906</a>.","short":"R.H. Kramer, Z. Haiman, S.P. Oh, The Astrophysical Journal 649 (2006) 570–578.","ama":"Kramer RH, Haiman Z, Oh SP. Feedback from clustered sources during reionization. <i>The Astrophysical Journal</i>. 2006;649(2):570-578. doi:<a href=\"https://doi.org/10.1086/506906\">10.1086/506906</a>","ieee":"R. H. Kramer, Z. Haiman, and S. P. Oh, “Feedback from clustered sources during reionization,” <i>The Astrophysical Journal</i>, vol. 649, no. 2. American Astronomical Society, pp. 570–578, 2006.","ista":"Kramer RH, Haiman Z, Oh SP. 2006. Feedback from clustered sources during reionization. The Astrophysical Journal. 649(2), 570–578.","mla":"Kramer, Roban Hultman, et al. “Feedback from Clustered Sources during Reionization.” <i>The Astrophysical Journal</i>, vol. 649, no. 2, American Astronomical Society, 2006, pp. 570–78, doi:<a href=\"https://doi.org/10.1086/506906\">10.1086/506906</a>.","apa":"Kramer, R. H., Haiman, Z., &#38; Oh, S. P. (2006). Feedback from clustered sources during reionization. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/506906\">https://doi.org/10.1086/506906</a>"},"abstract":[{"lang":"eng","text":"The reionization history of the intergalactic medium at high redshift (z ≳ 6) was likely strongly shaped by several global feedback processes. Because the earliest ionizing sources formed at the locations of the rare density peaks, their spatial distribution was strongly clustered. Here we demonstrate that this clustering significantly boosts the impact of feedback processes operating at high redshift. We build a semianalytical model to include feedback and clustering simultaneously and apply this model to the suppression of star formation in minihalos due to photoionization. The model is built on the excursion-set-based formalism of Furlanetto, Zaldarriaga, and Hernquist, which incorporates the clustering of ionizing sources and which we here extend to include the suppression of star formation in minihalos. We find that clustering increases the mean H II bubble size by a factor of several, and it dramatically increases the fraction of minihalos that are suppressed by a factor of up to ~60 relative to a randomly distributed population. This enhanced suppression can significantly reduce the electron-scattering optical depth τ, as required by the 3 year data from the Wilkinson Microwave Anisotropy Probe. We argue that source clustering is likely to similarly boost the importance of a variety of other feedback mechanisms."}],"publication_identifier":{"issn":["0004-637X","1538-4357"]},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1086/506906"}],"oa_version":"Published Version","month":"10","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"scopus_import":"1","intvolume":"       649","year":"2006","status":"public","extern":"1","issue":"2","type":"journal_article","date_created":"2024-09-06T09:02:52Z","oa":1,"date_published":"2006-10-01T00:00:00Z","publication_status":"published","fulldoi":"https://doi.org/10.1086/506906","publication":"The Astrophysical Journal","article_type":"original","quality_controlled":"1","volume":649,"page":"570-578","author":[{"last_name":"Kramer","full_name":"Kramer, Roban Hultman","first_name":"Roban Hultman"},{"first_name":"Zoltán","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"},{"last_name":"Oh","full_name":"Oh, S. Peng","first_name":"S. Peng"}],"day":"01"},{"page":"37-47","author":[{"full_name":"Dijkstra, Mark","first_name":"Mark","last_name":"Dijkstra"},{"full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman"},{"last_name":"Spaans","first_name":"Marco","full_name":"Spaans, Marco"}],"day":"20","article_type":"original","quality_controlled":"1","volume":649,"fulldoi":"https://doi.org/10.1086/506244","publication_status":"published","publication":"The Astrophysical Journal","year":"2006","extern":"1","status":"public","intvolume":"       649","type":"journal_article","issue":"1","date_created":"2024-09-06T09:16:08Z","date_published":"2006-09-20T00:00:00Z","oa":1,"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1086/506244"}],"oa_version":"Published Version","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","month":"09","language":[{"iso":"eng"}],"scopus_import":"1","article_processing_charge":"No","publication_identifier":{"issn":["0004-637X","1538-4357"]},"abstract":[{"lang":"eng","text":"We model the spectra and surface brightness distributions for the Lyα radiation expected from protogalaxies that are caught in the early stages of their assembly. We use the results of a companion paper to characterize the radiation emerging from spherically collapsing gas clouds. We then modify these spectra to incorporate the effect of subsequent resonant scattering in the IGM. Using these models, we interpret a number of recent observations of extended Lyα blobs (LABs) at high redshift. We suggest, based on the angular size, energetics, relatively shallow surface brightness profiles, and double-peaked spectra, that several of these LABs may be associated with collapsing protogalaxies. We suggest two follow-up observations to diagnose the presence of gas infall. High-S/N spectra of LABs should reveal a preferential flattening of the surface brightness profile at the red side of the line. Complementary imaging of the blobs at redshifted Hα wavelengths should reveal the intrinsic Lyα emissivity and allow its separation from radiative transfer effects. We show that Lyα scattering by infalling gas can reproduce the observed spectrum of the Steidel et al. LAB2 as accurately as a recently proposed outflow model. Finally, we find similar evidence for infall in the spectra of pointlike Lyα emitters. The presence of scattering by the infalling gas implies that the intrinsic Lyα luminosities and derived quantities, such as the star formation rate, in these objects may have been underestimated by about an order of magnitude."}],"citation":{"mla":"Dijkstra, Mark, et al. “Lyα Radiation from Collapsing Protogalaxies. II. Observational Evidence for Gas Infall.” <i>The Astrophysical Journal</i>, vol. 649, no. 1, American Astronomical Society, 2006, pp. 37–47, doi:<a href=\"https://doi.org/10.1086/506244\">10.1086/506244</a>.","apa":"Dijkstra, M., Haiman, Z., &#38; Spaans, M. (2006). Lyα radiation from collapsing protogalaxies. II. Observational evidence for gas infall. <i>The Astrophysical Journal</i>. American Astronomical Society. <a href=\"https://doi.org/10.1086/506244\">https://doi.org/10.1086/506244</a>","ieee":"M. Dijkstra, Z. Haiman, and M. Spaans, “Lyα radiation from collapsing protogalaxies. II. Observational evidence for gas infall,” <i>The Astrophysical Journal</i>, vol. 649, no. 1. American Astronomical Society, pp. 37–47, 2006.","ista":"Dijkstra M, Haiman Z, Spaans M. 2006. Lyα radiation from collapsing protogalaxies. II. Observational evidence for gas infall. The Astrophysical Journal. 649(1), 37–47.","chicago":"Dijkstra, Mark, Zoltán Haiman, and Marco Spaans. “Lyα Radiation from Collapsing Protogalaxies. II. Observational Evidence for Gas Infall.” <i>The Astrophysical Journal</i>. American Astronomical Society, 2006. <a href=\"https://doi.org/10.1086/506244\">https://doi.org/10.1086/506244</a>.","short":"M. Dijkstra, Z. Haiman, M. Spaans, The Astrophysical Journal 649 (2006) 37–47.","ama":"Dijkstra M, Haiman Z, Spaans M. Lyα radiation from collapsing protogalaxies. II. Observational evidence for gas infall. <i>The Astrophysical Journal</i>. 2006;649(1):37-47. doi:<a href=\"https://doi.org/10.1086/506244\">10.1086/506244</a>"},"doi":"10.1086/506244","date_updated":"2024-09-26T07:34:55Z","publisher":"American Astronomical Society","_id":"17730","title":"Lyα radiation from collapsing protogalaxies. II. Observational evidence for gas infall"}]