---
_id: '17678'
abstract:
- lang: eng
  text: 'The spectra of several high-redshift (z>6) quasars have shown evidence for
    a Gunn-Peterson (GP) damping wing, indicating a substantial mean neutral hydrogen
    fraction (x_HI > 0.03) in the z ~ 6 intergalactic medium (IGM). However, previous
    analyses assumed that the IGM was uniformly ionized outside of the quasar''s HII
    region. Here we relax this assumption and model patchy reionization scenarios
    for a range of IGM and quasar parameters. We quantify the impact of these differences
    on the inferred x_HI, by fitting the spectra of three quasars: SDSS J1148+5251
    (z=6.419), J1030+0524 (z=6.308), and J1623+3112 (z=6.247). We find that the best-fit
    values of x_HI in the patchy models agree well with the uniform case. More importantly,
    we confirm that the observed spectra favor the presence of a GP damping wing,
    with peak likelihoods decreasing by factors of > few - 10 when the spectra are
    modeled without a damping wing. We also find that the Ly alpha absorption spectra,
    by themselves, cannot distinguish the damping wing in a relatively neutral IGM
    from a damping wing in a highly ionized IGM, caused either by an isolated neutral
    patch, or by a damped Ly alpha absorber (DLA). However, neutral patches in a highly
    ionized universe (x_HI < 0.01), and DLAs with the large required column densities
    (N_HI > few x 10^{20} cm^{-2}) are both rare. As a result, when we include reasonable
    prior probabilities for the line of sight (LOS) to intercept either a neutral
    patch or a DLA at the required distance of ~ 40-60 comoving Mpc away from the
    quasar, we find strong lower limits on the neutral fraction in the IGM, x_HI >
    0.1 (at 95% confidence). This strengthens earlier claims that a substantial global
    fraction of hydrogen in the z~6 IGM is in neutral form.'
article_processing_charge: No
article_type: original
author:
- first_name: Joshua
  full_name: Schroeder, Joshua
  last_name: Schroeder
- first_name: Andrei
  full_name: Mesinger, Andrei
  last_name: Mesinger
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: 'Schroeder J, Mesinger A, Haiman Z. Evidence of Gunn–Peterson damping wings
    in high-z quasar spectra: Strengthening the case for incomplete reionization at
    z ∼ 6–7. <i>Monthly Notices of the Royal Astronomical Society</i>. 2012;428(4):3058-3071.
    doi:<a href="https://doi.org/10.1093/mnras/sts253">10.1093/mnras/sts253</a>'
  apa: 'Schroeder, J., Mesinger, A., &#38; Haiman, Z. (2012). Evidence of Gunn–Peterson
    damping wings in high-z quasar spectra: Strengthening the case for incomplete
    reionization at z ∼ 6–7. <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press. <a href="https://doi.org/10.1093/mnras/sts253">https://doi.org/10.1093/mnras/sts253</a>'
  chicago: 'Schroeder, Joshua, Andrei Mesinger, and Zoltán Haiman. “Evidence of Gunn–Peterson
    Damping Wings in High-z Quasar Spectra: Strengthening the Case for Incomplete
    Reionization at z ∼ 6–7.” <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press, 2012. <a href="https://doi.org/10.1093/mnras/sts253">https://doi.org/10.1093/mnras/sts253</a>.'
  ieee: 'J. Schroeder, A. Mesinger, and Z. Haiman, “Evidence of Gunn–Peterson damping
    wings in high-z quasar spectra: Strengthening the case for incomplete reionization
    at z ∼ 6–7,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 428,
    no. 4. Oxford University Press, pp. 3058–3071, 2012.'
  ista: 'Schroeder J, Mesinger A, Haiman Z. 2012. Evidence of Gunn–Peterson damping
    wings in high-z quasar spectra: Strengthening the case for incomplete reionization
    at z ∼ 6–7. Monthly Notices of the Royal Astronomical Society. 428(4), 3058–3071.'
  mla: 'Schroeder, Joshua, et al. “Evidence of Gunn–Peterson Damping Wings in High-z
    Quasar Spectra: Strengthening the Case for Incomplete Reionization at z ∼ 6–7.”
    <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 428, no. 4, Oxford
    University Press, 2012, pp. 3058–71, doi:<a href="https://doi.org/10.1093/mnras/sts253">10.1093/mnras/sts253</a>.'
  short: J. Schroeder, A. Mesinger, Z. Haiman, Monthly Notices of the Royal Astronomical
    Society 428 (2012) 3058–3071.
date_created: 2024-09-06T08:04:35Z
date_published: 2012-11-22T00:00:00Z
date_updated: 2024-09-25T08:53:21Z
day: '22'
doi: 10.1093/mnras/sts253
extern: '1'
intvolume: '       428'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1093/mnras/sts253
month: '11'
oa: 1
oa_version: Published Version
page: 3058-3071
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Evidence of Gunn–Peterson damping wings in high-z quasar spectra: Strengthening
  the case for incomplete reionization at z ∼ 6–7'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 428
year: '2012'
...
---
_id: '17688'
abstract:
- lang: eng
  text: Pulsar timing arrays (PTAs) are expected to detect gravitational waves (GWs)
    from individual low-redshift (z<1.5) compact supermassive (M>10^9 Msun) black
    hole (SMBH) binaries with orbital periods of approx. 0.1 - 10 yrs. Identifying
    the electromagnetic (EM) counterparts of these sources would provide confirmation
    of putative direct detections of GWs, present a rare opportunity to study the
    environments of compact SMBH binaries, and could enable the use of these sources
    as standard sirens for cosmology. Here we consider the feasibility of such an
    EM identification. We show that because the host galaxies of resolved PTA sources
    are expected to be exceptionally massive and rare, it should be possible to find
    unique hosts of resolved sources out to redshift z=0.2. At higher redshifts, the
    PTA error boxes are larger, and may contain as many as 100 massive-galaxy interlopers.
    The number of candidates, however, remains tractable for follow-up searches in
    upcoming wide-field EM surveys. We develop a toy model to characterize the dynamics
    and the thermal emission from a geometrically thin, gaseous disc accreting onto
    a PTA-source SMBH binary. Our model predicts that at optical and infrared frequencies,
    the source should appear similar to a typical luminous active galactic nucleus
    (AGN). However, owing to the evacuation of the accretion flow by the binary's
    tidal torques, the source might have an unusually low soft X-ray luminosity and
    weak UV and broad optical emission lines, as compared to an AGN powered by a single
    SMBH with the same total mass. For sources near z=1, the decrement in the rest-frame
    UV should be observable as an extremely red optical color. These properties would
    make the PTA sources stand out among optically luminous AGN, and could allow their
    unique identification.
alternative_title:
- Electromagnetic counterparts of PTA sources
article_processing_charge: No
article_type: original
author:
- first_name: Takamitsu
  full_name: Tanaka, Takamitsu
  last_name: Tanaka
- first_name: Kristen
  full_name: Menou, Kristen
  last_name: Menou
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: Tanaka T, Menou K, Haiman Z. Electromagnetic counterparts of supermassive black
    hole binaries resolved by pulsar timing arrays. <i>Monthly Notices of the Royal
    Astronomical Society</i>. 2012;420(1):705-719. doi:<a href="https://doi.org/10.1111/j.1365-2966.2011.20083.x">10.1111/j.1365-2966.2011.20083.x</a>
  apa: Tanaka, T., Menou, K., &#38; Haiman, Z. (2012). Electromagnetic counterparts
    of supermassive black hole binaries resolved by pulsar timing arrays. <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1111/j.1365-2966.2011.20083.x">https://doi.org/10.1111/j.1365-2966.2011.20083.x</a>
  chicago: Tanaka, Takamitsu, Kristen Menou, and Zoltán Haiman. “Electromagnetic Counterparts
    of Supermassive Black Hole Binaries Resolved by Pulsar Timing Arrays.” <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press, 2012.
    <a href="https://doi.org/10.1111/j.1365-2966.2011.20083.x">https://doi.org/10.1111/j.1365-2966.2011.20083.x</a>.
  ieee: T. Tanaka, K. Menou, and Z. Haiman, “Electromagnetic counterparts of supermassive
    black hole binaries resolved by pulsar timing arrays,” <i>Monthly Notices of the
    Royal Astronomical Society</i>, vol. 420, no. 1. Oxford University Press, pp.
    705–719, 2012.
  ista: Tanaka T, Menou K, Haiman Z. 2012. Electromagnetic counterparts of supermassive
    black hole binaries resolved by pulsar timing arrays. Monthly Notices of the Royal
    Astronomical Society. 420(1), 705–719.
  mla: Tanaka, Takamitsu, et al. “Electromagnetic Counterparts of Supermassive Black
    Hole Binaries Resolved by Pulsar Timing Arrays.” <i>Monthly Notices of the Royal
    Astronomical Society</i>, vol. 420, no. 1, Oxford University Press, 2012, pp.
    705–19, doi:<a href="https://doi.org/10.1111/j.1365-2966.2011.20083.x">10.1111/j.1365-2966.2011.20083.x</a>.
  short: T. Tanaka, K. Menou, Z. Haiman, Monthly Notices of the Royal Astronomical
    Society 420 (2012) 705–719.
date_created: 2024-09-06T08:23:06Z
date_published: 2012-01-23T00:00:00Z
date_updated: 2024-09-25T09:49:01Z
day: '23'
doi: 10.1111/j.1365-2966.2011.20083.x
extern: '1'
intvolume: '       420'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1111/j.1365-2966.2011.20083.x
month: '01'
oa: 1
oa_version: Published Version
page: 705-719
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Electromagnetic counterparts of supermassive black hole binaries resolved by
  pulsar timing arrays
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 420
year: '2012'
...
---
_id: '17705'
abstract:
- lang: eng
  text: Observations of high-redshift quasars at z>6 imply that supermassive black
    holes (SMBHs) with masses over a billion solar masses were in place less than
    1 Gyr after the Big Bang. If these SMBHs assembled from "seed" BHs left behind
    by the first stars, then they must have accreted gas at close to the Eddington
    limit during a large fraction (>50%) of the time. A generic problem with this
    scenario, however, is that the mass density in million-solar-mass SMBHs at z=6
    already exceeds the locally observed SMBH mass density by several orders of magnitude;
    in order to avoid this overproduction, BH seed formation and growth must become
    significantly less efficient in less massive protogalaxies, while proceeding uninterrupted
    in the most massive galaxies that formed first. Using Monte-Carlo realizations
    of the merger and growth history of BHs, we show that X-rays from the earliest
    accreting BHs can provide such a feedback mechanism. Our calculations paint a
    self-consistent picture of black-hole-made climate change, in which the first
    miniquasars---among them the ancestors of the z>6 quasar SMBHs---globally warm
    the IGM and suppress the formation and growth of subsequent generations of BHs.
    We present two specific models with global miniquasar feedback that provide excellent
    agreement with recent estimates of the z=6 SMBH mass function. For each of these
    models, we estimate the rate of BH mergers at z>6 that could be detected by the
    proposed gravitational-wave observatory eLISA/NGO.
alternative_title:
- IGM global warming by high-redshift miniquasars
article_processing_charge: No
article_type: original
author:
- first_name: Takamitsu
  full_name: Tanaka, Takamitsu
  last_name: Tanaka
- first_name: Rosalba
  full_name: Perna, Rosalba
  last_name: Perna
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: 'Tanaka T, Perna R, Haiman Z. X-ray emission from high-redshift miniquasars:
    Self-regulating the population of massive black holes through global warming.
    <i>Monthly Notices of the Royal Astronomical Society</i>. 2012;425(4):2974-2987.
    doi:<a href="https://doi.org/10.1111/j.1365-2966.2012.21539.x">10.1111/j.1365-2966.2012.21539.x</a>'
  apa: 'Tanaka, T., Perna, R., &#38; Haiman, Z. (2012). X-ray emission from high-redshift
    miniquasars: Self-regulating the population of massive black holes through global
    warming. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University
    Press. <a href="https://doi.org/10.1111/j.1365-2966.2012.21539.x">https://doi.org/10.1111/j.1365-2966.2012.21539.x</a>'
  chicago: 'Tanaka, Takamitsu, Rosalba Perna, and Zoltán Haiman. “X-Ray Emission from
    High-Redshift Miniquasars: Self-Regulating the Population of Massive Black Holes
    through Global Warming.” <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press, 2012. <a href="https://doi.org/10.1111/j.1365-2966.2012.21539.x">https://doi.org/10.1111/j.1365-2966.2012.21539.x</a>.'
  ieee: 'T. Tanaka, R. Perna, and Z. Haiman, “X-ray emission from high-redshift miniquasars:
    Self-regulating the population of massive black holes through global warming,”
    <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 425, no. 4. Oxford
    University Press, pp. 2974–2987, 2012.'
  ista: 'Tanaka T, Perna R, Haiman Z. 2012. X-ray emission from high-redshift miniquasars:
    Self-regulating the population of massive black holes through global warming.
    Monthly Notices of the Royal Astronomical Society. 425(4), 2974–2987.'
  mla: 'Tanaka, Takamitsu, et al. “X-Ray Emission from High-Redshift Miniquasars:
    Self-Regulating the Population of Massive Black Holes through Global Warming.”
    <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 425, no. 4, Oxford
    University Press, 2012, pp. 2974–87, doi:<a href="https://doi.org/10.1111/j.1365-2966.2012.21539.x">10.1111/j.1365-2966.2012.21539.x</a>.'
  short: T. Tanaka, R. Perna, Z. Haiman, Monthly Notices of the Royal Astronomical
    Society 425 (2012) 2974–2987.
date_created: 2024-09-06T08:50:56Z
date_published: 2012-10-01T00:00:00Z
date_updated: 2024-09-25T11:40:30Z
day: '01'
doi: 10.1111/j.1365-2966.2012.21539.x
extern: '1'
intvolume: '       425'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1111/j.1365-2966.2012.21539.x
month: '10'
oa: 1
oa_version: Published Version
page: 2974-2987
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'X-ray emission from high-redshift miniquasars: Self-regulating the population
  of massive black holes through global warming'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 425
year: '2012'
...
---
_id: '17676'
abstract:
- lang: eng
  text: It has been shown that HD molecules can form efficiently in metal-free gas
    collapsing into massive protogalactic halos at high redshift. The resulting radiative
    cooling by HD can lower the gas temperature to that of the cosmic microwave background,
    T_CMB=2.7(1+z)K, significantly below the temperature of a few 100 K achievable
    via H_2-cooling alone, and thus reduce the masses of the first generation of stars.
    Here we consider the suppression of HD-cooling by UV irradiation in the Lyman-Werner
    (LW) bands. We include photo-dissociation of both H_2 and HD, and explicitly compute
    the self-shielding and shielding of both molecules by neutral hydrogen as well
    as the shielding of HD by H_2. We use a simplified dynamical collapse model, and
    follow the chemical and thermal evolution of the gas, in the presence of a UV
    background. We find that a LW flux of J_crit = 1e-22 erg/cm^2/sr/s/Hz is able
    to suppress HD cooling and thus prevent collapsing primordial gas from reaching
    temperatures below 100 K. The main reason for the lack of HD cooling for J>J_crit
    is the partial photo-dissociation of H_2, which prevents the gas from reaching
    sufficiently low temperatures (T<150K) for HD to become the dominant coolant;
    direct HD photo-dissociation is unimportant except for a narrow range of fluxes
    and column densities. Since the prevention of HD-cooling requires only partial
    H_2 photo-dissociation, the critical flux J_crit is modest, and is below the UV
    background required to reionize the universe at redshift z=10-20. We conclude
    that HD-cooling can reduce the masses of typical stars only in rare halos forming
    well before the epoch of reionization.
alternative_title:
- Suppression of HD cooling in primordial gas
article_processing_charge: No
article_type: original
author:
- first_name: J.
  full_name: Wolcott-Green, J.
  last_name: Wolcott-Green
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: Wolcott-Green J, Haiman Z. Suppression of HD cooling in protogalactic gas clouds
    by Lyman-Werner radiation. <i>Monthly Notices of the Royal Astronomical Society</i>.
    2011;412(4):2603-2616. doi:<a href="https://doi.org/10.1111/j.1365-2966.2010.18080.x">10.1111/j.1365-2966.2010.18080.x</a>
  apa: Wolcott-Green, J., &#38; Haiman, Z. (2011). Suppression of HD cooling in protogalactic
    gas clouds by Lyman-Werner radiation. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1111/j.1365-2966.2010.18080.x">https://doi.org/10.1111/j.1365-2966.2010.18080.x</a>
  chicago: Wolcott-Green, J., and Zoltán Haiman. “Suppression of HD Cooling in Protogalactic
    Gas Clouds by Lyman-Werner Radiation.” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2011. <a href="https://doi.org/10.1111/j.1365-2966.2010.18080.x">https://doi.org/10.1111/j.1365-2966.2010.18080.x</a>.
  ieee: J. Wolcott-Green and Z. Haiman, “Suppression of HD cooling in protogalactic
    gas clouds by Lyman-Werner radiation,” <i>Monthly Notices of the Royal Astronomical
    Society</i>, vol. 412, no. 4. Oxford University Press, pp. 2603–2616, 2011.
  ista: Wolcott-Green J, Haiman Z. 2011. Suppression of HD cooling in protogalactic
    gas clouds by Lyman-Werner radiation. Monthly Notices of the Royal Astronomical
    Society. 412(4), 2603–2616.
  mla: Wolcott-Green, J., and Zoltán Haiman. “Suppression of HD Cooling in Protogalactic
    Gas Clouds by Lyman-Werner Radiation.” <i>Monthly Notices of the Royal Astronomical
    Society</i>, vol. 412, no. 4, Oxford University Press, 2011, pp. 2603–16, doi:<a
    href="https://doi.org/10.1111/j.1365-2966.2010.18080.x">10.1111/j.1365-2966.2010.18080.x</a>.
  short: J. Wolcott-Green, Z. Haiman, Monthly Notices of the Royal Astronomical Society
    412 (2011) 2603–2616.
date_created: 2024-09-06T07:52:22Z
date_published: 2011-04-08T00:00:00Z
date_updated: 2024-09-25T08:47:23Z
day: '08'
doi: 10.1111/j.1365-2966.2010.18080.x
extern: '1'
intvolume: '       412'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1111/j.1365-2966.2010.18080.x
month: '04'
oa: 1
oa_version: Published Version
page: 2603-2616
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Suppression of HD cooling in protogalactic gas clouds by Lyman-Werner radiation
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 412
year: '2011'
...
---
_id: '17681'
abstract:
- lang: eng
  text: The gravitational waves (GWs) emitted by inspiralling binary black holes,
    expected to be detected by the Laser Interferometer Space Antenna (LISA), could
    be used to determine the luminosity distance to these sources with the unprecedented
    precision of ≲1 per cent. We study cosmological parameter constraints from such
    standard sirens, in the presence of gravitational lensing by large-scale structure.
    Lensing introduces magnification with a probability distribution function (PDF)
    whose shape has significant skewness and kurtosis, and depends on cosmological
    parameters. We use Monte Carlo simulations to generate mock samples of standard
    sirens, including a small intrinsic scatter, as well as the additional, larger
    scatter from lensing, in their inferred distances. We derive constraints on cosmological
    parameters, by simultaneously fitting the mean and the distribution of the residuals
    on the distance versus redshift (dL–z) Hubble diagram. We find that for standard
    sirens at redshift z≈ 1, the sensitivity to a single cosmological parameter, such
    as the matter density Ωm, or the dark energy equation of state w, is ∼50–80 per
    cent tighter when the lensing PDF is used, compared to the sensitivity derived
    from a Gaussian PDF with the same variance. When these two parameters are constrained
    simultaneously, the non-Gaussian shape yields a further enhanced improvement (by
    ∼120 per cent), owing to the correlation between the parameters. The sensitivity
    to the amplitude of the matter power spectrum, σ8 from the cosmological dependence
    of the PDF alone, however, is ∼20 per cent worse than that from the Gaussian PDF.
    The improvements for Ωm and w arise purely from the non-Gaussian shape of the
    lensing PDF and can be attributed specifically to the sharpness of the peak of
    this PDF (i.e. to a finite kurtosis); the dependence of the PDF on these parameters
    does not improve constraints relative to those available from the mean dL–z relation.
    At higher redshifts, the PDF resembles a Gaussian more closely, and the effects
    of the non-Gaussianities become less prominent. These results highlight the importance
    of obtaining an accurate and reliable PDF of the lensing convergence, in order
    to realize the full potential of standard sirens as cosmological probes.
alternative_title:
- WL and GW standard sirens
article_processing_charge: No
article_type: original
author:
- first_name: Cien
  full_name: Shang, Cien
  last_name: Shang
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: 'Shang C, Haiman Z. Cosmology with standard sirens: The importance of the shape
    of the lensing magnification distribution. <i>Monthly Notices of the Royal Astronomical
    Society</i>. 2011;411(1):9-22. doi:<a href="https://doi.org/10.1111/j.1365-2966.2010.17607.x">10.1111/j.1365-2966.2010.17607.x</a>'
  apa: 'Shang, C., &#38; Haiman, Z. (2011). Cosmology with standard sirens: The importance
    of the shape of the lensing magnification distribution. <i>Monthly Notices of
    the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1111/j.1365-2966.2010.17607.x">https://doi.org/10.1111/j.1365-2966.2010.17607.x</a>'
  chicago: 'Shang, Cien, and Zoltán Haiman. “Cosmology with Standard Sirens: The Importance
    of the Shape of the Lensing Magnification Distribution.” <i>Monthly Notices of
    the Royal Astronomical Society</i>. Oxford University Press, 2011. <a href="https://doi.org/10.1111/j.1365-2966.2010.17607.x">https://doi.org/10.1111/j.1365-2966.2010.17607.x</a>.'
  ieee: 'C. Shang and Z. Haiman, “Cosmology with standard sirens: The importance of
    the shape of the lensing magnification distribution,” <i>Monthly Notices of the
    Royal Astronomical Society</i>, vol. 411, no. 1. Oxford University Press, pp.
    9–22, 2011.'
  ista: 'Shang C, Haiman Z. 2011. Cosmology with standard sirens: The importance of
    the shape of the lensing magnification distribution. Monthly Notices of the Royal
    Astronomical Society. 411(1), 9–22.'
  mla: 'Shang, Cien, and Zoltán Haiman. “Cosmology with Standard Sirens: The Importance
    of the Shape of the Lensing Magnification Distribution.” <i>Monthly Notices of
    the Royal Astronomical Society</i>, vol. 411, no. 1, Oxford University Press,
    2011, pp. 9–22, doi:<a href="https://doi.org/10.1111/j.1365-2966.2010.17607.x">10.1111/j.1365-2966.2010.17607.x</a>.'
  short: C. Shang, Z. Haiman, Monthly Notices of the Royal Astronomical Society 411
    (2011) 9–22.
date_created: 2024-09-06T08:07:44Z
date_published: 2011-01-21T00:00:00Z
date_updated: 2024-09-25T09:04:38Z
day: '21'
doi: 10.1111/j.1365-2966.2010.17607.x
extern: '1'
intvolume: '       411'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1111/j.1365-2966.2010.17607.x
month: '01'
oa: 1
oa_version: Published Version
page: 9-22
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Cosmology with standard sirens: The importance of the shape of the lensing
  magnification distribution'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 411
year: '2011'
...
---
_id: '17690'
abstract:
- lang: eng
  text: The ability of primordial gas to cool in proto-galactic haloes exposed to
    Lyman-Werner (LW) radiation is critically dependent on the self-shielding of H_2.
    We perform radiative transfer calculations of LW line photons, post-processing
    outputs from three-dimensional adaptive mesh refinement (AMR) simulations of haloes
    with T_vir > 10^4 K at redshifts around z=10. We calculate the optically thick
    photodissociation rate numerically, including the effects of density, temperature,
    and velocity gradients in the gas, as well as line overlap and shielding of H_2
    by HI, over a large number of sight-lines. In low-density regions (n<10^4 cm^-3)
    the dissociation rates exceed those obtained using most previous approximations
    by more than an order of magnitude; the correction is smaller at higher densities.
    We trace the origin of the deviations primarily to inaccuracies of (i) the most
    common fitting formula (Draine & Bertoldi 1996) for the suppression of the dissociation
    rate and (ii) estimates for the effective shielding column density from local
    properties of the gas. The combined effects of gas temperature and velocity gradients
    are comparatively less important, typically altering the spherically averaged
    rate only by a factor of less than two. We present a simple modification to the
    DB96 fitting formula for the optically thick rate which improves agreement with
    our numerical results to within approx. 15 per cent, and can be adopted in future
    simulations. We find that estimates for the effective shielding column can be
    improved by using the local Sobolev length. Our correction to the H_2 self-shielding
    reduces the critical LW flux to suppress H_2-cooling in T_vir>10^4 K haloes by
    an order of magnitude; this increases the number of such haloes in which supermassive
    (approx. M=10^5 M_sun) black holes may have formed.
alternative_title:
- H 2 self-shielding in 3D simulations
article_processing_charge: No
article_type: original
author:
- first_name: J.
  full_name: Wolcott-Green, J.
  last_name: Wolcott-Green
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
- first_name: G. L.
  full_name: Bryan, G. L.
  last_name: Bryan
citation:
  ama: 'Wolcott-Green J, Haiman Z, Bryan GL. Photodissociation of H2 in protogalaxies:
    Modelling self-shielding in three-dimensional simulations. <i>Monthly Notices
    of the Royal Astronomical Society</i>. 2011;418(2):838-852. doi:<a href="https://doi.org/10.1111/j.1365-2966.2011.19538.x">10.1111/j.1365-2966.2011.19538.x</a>'
  apa: 'Wolcott-Green, J., Haiman, Z., &#38; Bryan, G. L. (2011). Photodissociation
    of H2 in protogalaxies: Modelling self-shielding in three-dimensional simulations.
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press.
    <a href="https://doi.org/10.1111/j.1365-2966.2011.19538.x">https://doi.org/10.1111/j.1365-2966.2011.19538.x</a>'
  chicago: 'Wolcott-Green, J., Zoltán Haiman, and G. L. Bryan. “Photodissociation
    of H2 in Protogalaxies: Modelling Self-Shielding in Three-Dimensional Simulations.”
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press,
    2011. <a href="https://doi.org/10.1111/j.1365-2966.2011.19538.x">https://doi.org/10.1111/j.1365-2966.2011.19538.x</a>.'
  ieee: 'J. Wolcott-Green, Z. Haiman, and G. L. Bryan, “Photodissociation of H2 in
    protogalaxies: Modelling self-shielding in three-dimensional simulations,” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 418, no. 2. Oxford University
    Press, pp. 838–852, 2011.'
  ista: 'Wolcott-Green J, Haiman Z, Bryan GL. 2011. Photodissociation of H2 in protogalaxies:
    Modelling self-shielding in three-dimensional simulations. Monthly Notices of
    the Royal Astronomical Society. 418(2), 838–852.'
  mla: 'Wolcott-Green, J., et al. “Photodissociation of H2 in Protogalaxies: Modelling
    Self-Shielding in Three-Dimensional Simulations.” <i>Monthly Notices of the Royal
    Astronomical Society</i>, vol. 418, no. 2, Oxford University Press, 2011, pp.
    838–52, doi:<a href="https://doi.org/10.1111/j.1365-2966.2011.19538.x">10.1111/j.1365-2966.2011.19538.x</a>.'
  short: J. Wolcott-Green, Z. Haiman, G.L. Bryan, Monthly Notices of the Royal Astronomical
    Society 418 (2011) 838–852.
date_created: 2024-09-06T08:37:08Z
date_published: 2011-11-16T00:00:00Z
date_updated: 2024-09-25T09:53:37Z
day: '16'
doi: 10.1111/j.1365-2966.2011.19538.x
extern: '1'
intvolume: '       418'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1111/j.1365-2966.2011.19538.x
month: '11'
oa: 1
oa_version: Published Version
page: 838-852
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Photodissociation of H2 in protogalaxies: Modelling self-shielding in three-dimensional
  simulations'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 418
year: '2011'
...
---
_id: '17648'
abstract:
- lang: eng
  text: In the absence of H_2 molecules, the primordial gas in early dark matter halos
    with virial temperatures just above T_vir >~ 10^4 K cools by collisional excitation
    of atomic H. Although it cools efficiently, this gas remains relatively hot, at
    a temperature near T ~ 8000 K, and consequently might be able to avoid fragmentation
    and collapse directly into a supermassive black hole (SMBH). In order for H_2--formation
    and cooling to be strongly suppressed, the gas must be irradiated by a sufficiently
    intense ultraviolet (UV) flux. We performed a suite of three--dimensional hydrodynamical
    adaptive mesh refinement (AMR) simulations of gas collapse in three different
    protogalactic halos with T_vir >~ 10^4 K, irradiated by a UV flux with various
    intensities and spectra. We determined the critical specific intensity, Jcrit,
    required to suppress H_2 cooling in each of the three halos. For a hard spectrum
    representative of metal--free stars, we find (in units of 10^{-21} erg s^{-1}
    Hz^{-1} sr^{-1} cm^{-2}) 10^4<Jcrit<10^5, while for a softer spectrum, which is
    characteristic of a normal stellar population, and for which H^{-} --dissociation
    is important, we find 30<Jcrit<300. These values are a factor of 3--10 lower than
    previous estimates. We attribute the difference to the higher, more accurate H_2
    collisional dissociation rate we adopted. The reduction in Jcrit exponentially
    increases the number of rare halos exposed to super--critical radiation. When
    H_2 cooling is suppressed, gas collapse starts with a delay, but it ultimately
    proceeds more rapidly. The infall velocity is near the increased sound speed,
    and an object as massive as M ~ 10^5 solar mass may form at the center of these
    halos, compared to the M ~ 10^2 solar mass stars forming when H_2--cooling is
    efficient.
article_processing_charge: No
article_type: original
author:
- first_name: Cien
  full_name: Shang, Cien
  last_name: Shang
- first_name: Greg L.
  full_name: Bryan, Greg L.
  last_name: Bryan
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: 'Shang C, Bryan GL, Haiman Z. Supermassive black hole formation by direct collapse:
    keeping protogalactic gas H2 free in dark matter haloes with virial temperatures
    T_vir &#62; rsim10^4 K . <i>Monthly Notices of the Royal Astronomical Society</i>.
    2010;402(2):1249-1262. doi:<a href="https://doi.org/10.1111/j.1365-2966.2009.15960.x">10.1111/j.1365-2966.2009.15960.x</a>'
  apa: 'Shang, C., Bryan, G. L., &#38; Haiman, Z. (2010). Supermassive black hole
    formation by direct collapse: keeping protogalactic gas H2 free in dark matter
    haloes with virial temperatures T_vir &#62; rsim10^4 K . <i>Monthly Notices of
    the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1111/j.1365-2966.2009.15960.x">https://doi.org/10.1111/j.1365-2966.2009.15960.x</a>'
  chicago: 'Shang, Cien, Greg L. Bryan, and Zoltán Haiman. “Supermassive Black Hole
    Formation by Direct Collapse: Keeping Protogalactic Gas H2 Free in Dark Matter
    Haloes with Virial Temperatures T_vir &#62; Rsim10^4 K .” <i>Monthly Notices of
    the Royal Astronomical Society</i>. Oxford University Press, 2010. <a href="https://doi.org/10.1111/j.1365-2966.2009.15960.x">https://doi.org/10.1111/j.1365-2966.2009.15960.x</a>.'
  ieee: 'C. Shang, G. L. Bryan, and Z. Haiman, “Supermassive black hole formation
    by direct collapse: keeping protogalactic gas H2 free in dark matter haloes with
    virial temperatures T_vir &#62; rsim10^4 K ,” <i>Monthly Notices of the Royal
    Astronomical Society</i>, vol. 402, no. 2. Oxford University Press, pp. 1249–1262,
    2010.'
  ista: 'Shang C, Bryan GL, Haiman Z. 2010. Supermassive black hole formation by direct
    collapse: keeping protogalactic gas H2 free in dark matter haloes with virial
    temperatures T_vir &#62; rsim10^4 K . Monthly Notices of the Royal Astronomical
    Society. 402(2), 1249–1262.'
  mla: 'Shang, Cien, et al. “Supermassive Black Hole Formation by Direct Collapse:
    Keeping Protogalactic Gas H2 Free in Dark Matter Haloes with Virial Temperatures
    T_vir &#62; Rsim10^4 K .” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 402, no. 2, Oxford University Press, 2010, pp. 1249–62, doi:<a href="https://doi.org/10.1111/j.1365-2966.2009.15960.x">10.1111/j.1365-2966.2009.15960.x</a>.'
  short: C. Shang, G.L. Bryan, Z. Haiman, Monthly Notices of the Royal Astronomical
    Society 402 (2010) 1249–1262.
date_created: 2024-09-06T07:26:50Z
date_published: 2010-02-02T00:00:00Z
date_updated: 2024-09-24T12:49:06Z
day: '02'
doi: 10.1111/j.1365-2966.2009.15960.x
extern: '1'
intvolume: '       402'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1111/j.1365-2966.2009.15960.x
month: '02'
oa: 1
oa_version: Published Version
page: 1249-1262
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Supermassive black hole formation by direct collapse: keeping protogalactic
  gas H2 free in dark matter haloes with virial temperatures T_vir > rsim10^4 K '
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 402
year: '2010'
...
---
_id: '17665'
abstract:
- lang: eng
  text: Finding electromagnetic (EM) counterparts of future gravitational wave (GW)
    sources would bring rich scientific benefits. A promising possibility, in the
    case of the coalescence of a supermassive black hole binary (SMBHB), is that the
    prompt emission from merger-induced disturbances in a supersonic circumbinary
    disc may be detectable. We follow the post-merger evolution of a thin, zero-viscosity
    circumbinary gas disc with two-dimensional simulations, using the hydrodynamic
    code flash. We analyse perturbations arising from the 530 km s−1 recoil of a 106
    M⊙ binary, oriented in the plane of the disc, assuming either a non-radiative
    gamma-law or a pseudo-isothermal equation of state for the gas. We find that a
    single-armed spiral shock wave forms and propagates outwards, sweeping up ∼40
    per cent of the mass of the disc. The morphology and evolution of the perturbations
    agrees well with those of caustics predicted to occur in a collisionless disc.
    Assuming that the disc radiates nearly instantaneously to maintain a constant
    temperature, we estimate the amount of dissipation and corresponding post-merger
    light curve. The luminosity rises steadily on the time-scale of months, and reaches
    few ×1043 erg s−1, corresponding to ≈10 per cent of the Eddington luminosity of
    the central SMBHB. We also analyse the case in which gravitational wave emission
    results in a 5 per cent mass loss in the merger remnant. The mass loss reduces
    the shock overdensities and the overall luminosity of the disc by ≈15–20 per cent,
    without any other major effects on the spiral shock pattern.
alternative_title:
- Gas disc response to black hole merger
article_processing_charge: No
article_type: original
author:
- first_name: Lia R.
  full_name: Corrales, Lia R.
  last_name: Corrales
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
- first_name: Andrew
  full_name: MacFadyen, Andrew
  last_name: MacFadyen
citation:
  ama: Corrales LR, Haiman Z, MacFadyen A. Hydrodynamical response of a circumbinary
    gas disc to black hole recoil and mass loss. <i>Monthly Notices of the Royal Astronomical
    Society</i>. 2010;404(2):947-962. doi:<a href="https://doi.org/10.1111/j.1365-2966.2010.16324.x">10.1111/j.1365-2966.2010.16324.x</a>
  apa: Corrales, L. R., Haiman, Z., &#38; MacFadyen, A. (2010). Hydrodynamical response
    of a circumbinary gas disc to black hole recoil and mass loss. <i>Monthly Notices
    of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1111/j.1365-2966.2010.16324.x">https://doi.org/10.1111/j.1365-2966.2010.16324.x</a>
  chicago: Corrales, Lia R., Zoltán Haiman, and Andrew MacFadyen. “Hydrodynamical
    Response of a Circumbinary Gas Disc to Black Hole Recoil and Mass Loss.” <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press, 2010.
    <a href="https://doi.org/10.1111/j.1365-2966.2010.16324.x">https://doi.org/10.1111/j.1365-2966.2010.16324.x</a>.
  ieee: L. R. Corrales, Z. Haiman, and A. MacFadyen, “Hydrodynamical response of a
    circumbinary gas disc to black hole recoil and mass loss,” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 404, no. 2. Oxford University Press,
    pp. 947–962, 2010.
  ista: Corrales LR, Haiman Z, MacFadyen A. 2010. Hydrodynamical response of a circumbinary
    gas disc to black hole recoil and mass loss. Monthly Notices of the Royal Astronomical
    Society. 404(2), 947–962.
  mla: Corrales, Lia R., et al. “Hydrodynamical Response of a Circumbinary Gas Disc
    to Black Hole Recoil and Mass Loss.” <i>Monthly Notices of the Royal Astronomical
    Society</i>, vol. 404, no. 2, Oxford University Press, 2010, pp. 947–62, doi:<a
    href="https://doi.org/10.1111/j.1365-2966.2010.16324.x">10.1111/j.1365-2966.2010.16324.x</a>.
  short: L.R. Corrales, Z. Haiman, A. MacFadyen, Monthly Notices of the Royal Astronomical
    Society 404 (2010) 947–962.
date_created: 2024-09-06T07:43:45Z
date_published: 2010-05-04T00:00:00Z
date_updated: 2024-09-25T07:43:38Z
day: '04'
doi: 10.1111/j.1365-2966.2010.16324.x
extern: '1'
intvolume: '       404'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1111/j.1365-2966.2010.16324.x
month: '05'
oa: 1
oa_version: Published Version
page: 947-962
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Hydrodynamical response of a circumbinary gas disc to black hole recoil and
  mass loss
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 404
year: '2010'
...
---
_id: '17765'
abstract:
- lang: eng
  text: 'Scaling relations among galaxy cluster observables, which will become available
    in large future samples of galaxy clusters, could be used to constrain not only
    cluster structure, but also cosmology. We study the utility of this approach,
    employing a physically motivated parametric model to describe cluster structure
    and applying it to the expected relation between the Sunyaev–Zel''dovich decrement
    (Sν) and the emission-weighted X-ray temperature (Tew). The slope and normalization
    of the entropy profile, the concentration of the dark matter potential, the pressure
    at the virial radius and the level of non-thermal pressure support as well as
    the mass and redshift dependence of these quantities are described by free parameters.
    With a suitable choice of fiducial parameter values, the cluster model satisfies
    several existing observational constraints. We employ a Fisher matrix approach
    to estimate the joint errors on cosmological and cluster structure parameters
    from a measurement of Sν versus Tew in a future survey. We find that different
    cosmological parameters affect the scaling relation differently: predominantly
    through the baryon fraction (Ωm and Ωb), the virial overdensity (w0 and wa for
    low-z clusters) and the angular diameter distance (w0 and wa for high-z clusters;
    ΩDE and h). We find that the cosmology constraints from the scaling relation are
    comparable to those expected from the number counts (dN/dz) of the same clusters.
    The scaling-relation approach is relatively insensitive to selection effects and
    it offers a valuable consistency check; combining the information from the scaling
    relation and dN/dz is also useful to break parameter degeneracies and help disentangle
    cluster physics from cosmology. Our work suggests that scaling relations should
    be a useful component in extracting cosmological information from large future
    cluster surveys.'
article_processing_charge: No
article_type: original
author:
- first_name: Cien
  full_name: Shang, Cien
  last_name: Shang
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
- first_name: Licia
  full_name: Verde, Licia
  last_name: Verde
citation:
  ama: Shang C, Haiman Z, Verde L. Probing cosmology and galaxy cluster structure
    with the Sunyaev-Zel’dovich decrement versus X-ray temperature scaling relation.
    <i>Monthly Notices of the Royal Astronomical Society</i>. 2009;400(2):1085-1104.
    doi:<a href="https://doi.org/10.1111/j.1365-2966.2009.15527.x">10.1111/j.1365-2966.2009.15527.x</a>
  apa: Shang, C., Haiman, Z., &#38; Verde, L. (2009). Probing cosmology and galaxy
    cluster structure with the Sunyaev-Zel’dovich decrement versus X-ray temperature
    scaling relation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford
    University Press. <a href="https://doi.org/10.1111/j.1365-2966.2009.15527.x">https://doi.org/10.1111/j.1365-2966.2009.15527.x</a>
  chicago: Shang, Cien, Zoltán Haiman, and Licia Verde. “Probing Cosmology and Galaxy
    Cluster Structure with the Sunyaev-Zel’dovich Decrement versus X-Ray Temperature
    Scaling Relation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford
    University Press, 2009. <a href="https://doi.org/10.1111/j.1365-2966.2009.15527.x">https://doi.org/10.1111/j.1365-2966.2009.15527.x</a>.
  ieee: C. Shang, Z. Haiman, and L. Verde, “Probing cosmology and galaxy cluster structure
    with the Sunyaev-Zel’dovich decrement versus X-ray temperature scaling relation,”
    <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 400, no. 2. Oxford
    University Press, pp. 1085–1104, 2009.
  ista: Shang C, Haiman Z, Verde L. 2009. Probing cosmology and galaxy cluster structure
    with the Sunyaev-Zel’dovich decrement versus X-ray temperature scaling relation.
    Monthly Notices of the Royal Astronomical Society. 400(2), 1085–1104.
  mla: Shang, Cien, et al. “Probing Cosmology and Galaxy Cluster Structure with the
    Sunyaev-Zel’dovich Decrement versus X-Ray Temperature Scaling Relation.” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 400, no. 2, Oxford University
    Press, 2009, pp. 1085–104, doi:<a href="https://doi.org/10.1111/j.1365-2966.2009.15527.x">10.1111/j.1365-2966.2009.15527.x</a>.
  short: C. Shang, Z. Haiman, L. Verde, Monthly Notices of the Royal Astronomical
    Society 400 (2009) 1085–1104.
date_created: 2024-09-06T09:51:57Z
date_published: 2009-11-12T00:00:00Z
date_updated: 2024-09-30T09:24:18Z
day: '12'
doi: 10.1111/j.1365-2966.2009.15527.x
extern: '1'
intvolume: '       400'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1111/j.1365-2966.2009.15527.x
month: '11'
oa: 1
oa_version: Published Version
page: 1085-1104
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Probing cosmology and galaxy cluster structure with the Sunyaev-Zel'dovich
  decrement versus X-ray temperature scaling relation
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 400
year: '2009'
...
---
_id: '17769'
abstract:
- lang: eng
  text: Arguably the best hope of understanding the tail end of the re-ionization
    of the intergalactic medium (IGM) at redshift z > 6 is through the detection and
    characterization of the Gunn–Peterson damping wing absorption of the IGM in bright
    quasar spectra. However, the use of quasar spectra to measure the IGM damping
    wing requires a model of the quasar's intrinsic Lyman α emission line. Here we
    quantify the uncertainties in the intrinsic line shapes, and how those uncertainties
    affect the determination of the IGM neutral fraction. We have assembled a catalogue
    of high-resolution Hubble Space Telescope spectra of the emission lines of unobscured
    low-redshift quasars, and have characterized the variance in the shapes of their
    lines. We then add simulated absorption from the high-redshift IGM to these quasar
    spectra in order to determine the corresponding uncertainties in re-ionization
    constraints using current and future samples of z > 6 quasar spectra. We find
    that, if the redshift of the Lyman α emission line is presumed to coincide with
    the systemic redshift determined from metal lines, the inferred IGM neutral fraction
    is systematically biased to low values due to a systematic blueshift of the Lyman
    α line relative to the metal lines. If a similar blueshift persists in quasars
    at z > 6, this bias strengthens previous claims of a significant neutral hydrogen
    fraction at z≈ 6. The bias can be reduced by including a Lyman α blueshift in
    the modelling procedure, or by excising wavelengths near the Lyman α line centre
    from the modelling. Intrinsic Lyman α line shape variations still induce significant
    scatter in the inferred xIGM values. Nevertheless, this scatter still allows a
    robust distinction between a highly ionized (xIGM∼ 10−3) and a neutral (xIGM=
    1) IGM with even a few bright quasars. We conclude that if the variations of the
    intrinsic Lyman α emission line shapes in high-z quasars are similar to those
    at low-z, this variation will not limit the usefulness of quasar spectra in probing
    re-ionization.
article_processing_charge: No
article_type: original
author:
- first_name: R. H.
  full_name: Kramer, R. H.
  last_name: Kramer
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: 'Kramer RH, Haiman Z. Probing re-ionization with quasar spectra: The impact
    of the intrinsic Lyman α emission line shape uncertainty. <i>Monthly Notices of
    the Royal Astronomical Society</i>. 2009;400(3):1493-1511. doi:<a href="https://doi.org/10.1111/j.1365-2966.2009.15552.x">10.1111/j.1365-2966.2009.15552.x</a>'
  apa: 'Kramer, R. H., &#38; Haiman, Z. (2009). Probing re-ionization with quasar
    spectra: The impact of the intrinsic Lyman α emission line shape uncertainty.
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press.
    <a href="https://doi.org/10.1111/j.1365-2966.2009.15552.x">https://doi.org/10.1111/j.1365-2966.2009.15552.x</a>'
  chicago: 'Kramer, R. H., and Zoltán Haiman. “Probing Re-Ionization with Quasar Spectra:
    The Impact of the Intrinsic Lyman α Emission Line Shape Uncertainty.” <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press, 2009.
    <a href="https://doi.org/10.1111/j.1365-2966.2009.15552.x">https://doi.org/10.1111/j.1365-2966.2009.15552.x</a>.'
  ieee: 'R. H. Kramer and Z. Haiman, “Probing re-ionization with quasar spectra: The
    impact of the intrinsic Lyman α emission line shape uncertainty,” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 400, no. 3. Oxford University Press,
    pp. 1493–1511, 2009.'
  ista: 'Kramer RH, Haiman Z. 2009. Probing re-ionization with quasar spectra: The
    impact of the intrinsic Lyman α emission line shape uncertainty. Monthly Notices
    of the Royal Astronomical Society. 400(3), 1493–1511.'
  mla: 'Kramer, R. H., and Zoltán Haiman. “Probing Re-Ionization with Quasar Spectra:
    The Impact of the Intrinsic Lyman α Emission Line Shape Uncertainty.” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 400, no. 3, Oxford University
    Press, 2009, pp. 1493–511, doi:<a href="https://doi.org/10.1111/j.1365-2966.2009.15552.x">10.1111/j.1365-2966.2009.15552.x</a>.'
  short: R.H. Kramer, Z. Haiman, Monthly Notices of the Royal Astronomical Society
    400 (2009) 1493–1511.
date_created: 2024-09-06T09:58:12Z
date_published: 2009-12-02T00:00:00Z
date_updated: 2024-09-30T09:48:06Z
day: '02'
doi: 10.1111/j.1365-2966.2009.15552.x
extern: '1'
intvolume: '       400'
issue: '3'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1111/j.1365-2966.2009.15552.x
month: '12'
oa: 1
oa_version: Published Version
page: 1493-1511
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Probing re-ionization with quasar spectra: The impact of the intrinsic Lyman
  α emission line shape uncertainty'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 400
year: '2009'
...
---
_id: '17782'
abstract:
- lang: eng
  text: Ultraviolet (UV) radiation from early astrophysical sources could have a large
    impact on subsequent star formation in nearby protogalaxies, and in general on
    the progress of cosmological reionization. Theoretical arguments based on the
    absence of metals in the early Universe suggest that the first stars were likely
    massive, bright, yet short-lived, with lifetimes of a few million years. Here
    we study the radiative feedback arising from such stars using hydrodynamical simulations
    with transient UV backgrounds (UVBs) and persistent Lyman–Werner backgrounds (LWBs)
    of varying intensity. We extend our prior work in Mesinger et al., by studying
    a more typical region whose protogalaxies form at lower redshifts, z∼ 13–20, in
    the epoch likely preceding the bulk of reionization. We confirm our previous results
    that feedback in the relic H ii regions resulting from such transient radiation
    is itself transient. Feedback effects dwindle away after ∼30 per cent of the Hubble
    time, and the same critical specific intensity of JUV∼ 0.1 × 10^−21 erg s^−1 cm^−2
    Hz^−1 sr^−1 separates positive and negative feedback regimes. This suggests that
    overall feedback is fairly insensitive to the large-scale environment, overdensity
    and redshift-dependent halo parameters, and can accurately be modelled in this
    regime with just the intensity of the impinging UVB. Additionally, we discover
    a second episode of eventual positive feedback in haloes which have not yet collapsed
    when their progenitor regions were exposed to the transient UVB. When exposed
    to the transient UVB, this gas suffers relatively little density depletion but
    a significant enhancement of the molecular hydrogen abundance, thus resulting
    in net positive feedback. This eventual positive feedback appears in all runs,
    regardless of the strength of the UVB. However, this feedback regime is very sensitive
    to the presence of Lyman–Werner radiation, and notable effects disappear under
    fairly modest background intensities of JLW≳ 10^−3× 10^−21 erg s^−1 cm^−2 Hz^−1
    sr^−1, assuming the region is optically thin for LW photons. Nevertheless, when
    exposed to the same LWB, haloes inside relic H ii regions always have a higher
    H2 abundance and shorter cooling times than haloes outside relic H ii regions,
    allowing gas to cool faster once it finally begins to collapse on to the halo.
    We conclude that UV radiative feedback in relic H ii regions, although a complicated
    process, seems unlikely to have a major impact on the progress of cosmological
    reionization, provided that present estimates of the lifetime and luminosity of
    a Population III star are accurate. More likely is that the build-up of the LWB
    ultimately governs the feedback strength until a persistent UV background can
    be established.
article_processing_charge: No
article_type: original
author:
- first_name: Andrei
  full_name: Mesinger, Andrei
  last_name: Mesinger
- first_name: Greg L.
  full_name: Bryan, Greg L.
  last_name: Bryan
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: Mesinger A, Bryan GL, Haiman Z. Relic H ii regions and radiative feedback at
    high redshifts. <i>Monthly Notices of the Royal Astronomical Society</i>. 2009;399(3):1650-1662.
    doi:<a href="https://doi.org/10.1111/j.1365-2966.2009.15404.x">10.1111/j.1365-2966.2009.15404.x</a>
  apa: Mesinger, A., Bryan, G. L., &#38; Haiman, Z. (2009). Relic H ii regions and
    radiative feedback at high redshifts. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1111/j.1365-2966.2009.15404.x">https://doi.org/10.1111/j.1365-2966.2009.15404.x</a>
  chicago: Mesinger, Andrei, Greg L. Bryan, and Zoltán Haiman. “Relic H Ii Regions
    and Radiative Feedback at High Redshifts.” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2009. <a href="https://doi.org/10.1111/j.1365-2966.2009.15404.x">https://doi.org/10.1111/j.1365-2966.2009.15404.x</a>.
  ieee: A. Mesinger, G. L. Bryan, and Z. Haiman, “Relic H ii regions and radiative
    feedback at high redshifts,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 399, no. 3. Oxford University Press, pp. 1650–1662, 2009.
  ista: Mesinger A, Bryan GL, Haiman Z. 2009. Relic H ii regions and radiative feedback
    at high redshifts. Monthly Notices of the Royal Astronomical Society. 399(3),
    1650–1662.
  mla: Mesinger, Andrei, et al. “Relic H Ii Regions and Radiative Feedback at High
    Redshifts.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 399,
    no. 3, Oxford University Press, 2009, pp. 1650–62, doi:<a href="https://doi.org/10.1111/j.1365-2966.2009.15404.x">10.1111/j.1365-2966.2009.15404.x</a>.
  short: A. Mesinger, G.L. Bryan, Z. Haiman, Monthly Notices of the Royal Astronomical
    Society 399 (2009) 1650–1662.
date_created: 2024-09-06T10:16:16Z
date_published: 2009-10-15T00:00:00Z
date_updated: 2024-09-30T12:42:48Z
day: '15'
doi: 10.1111/j.1365-2966.2009.15404.x
extern: '1'
intvolume: '       399'
issue: '3'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1111/j.1365-2966.2009.15404.x
month: '10'
oa: 1
oa_version: Published Version
page: 1650-1662
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Relic H ii regions and radiative feedback at high redshifts
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 399
year: '2009'
...
---
_id: '17721'
abstract:
- lang: eng
  text: High-redshift quasars (z >~ 6) drive ionization fronts into the intergalactic
    medium (IGM). If the thickness of the front can be measured, it can provide a
    novel constraint on the ionizing spectral energy distribution (SED). Here we follow
    the propagation of an I-front into a uniform IGM, and compute its thickness for
    a range of possible quasar spectra and ages. We also explore the effects of uniform
    and non-uniform ionizing backgrounds. We find that even for hard spectra, the
    fronts are initially thin, with a thickness much smaller than the mean free path
    of ionizing photons, but the thickness increases as the front approaches equilibrium
    in 10^8 - 10^9 years, and can eventually significantly exceed simple estimates
    based on the mean free path. With a high intrinsic hydrogen column density obscuring
    the source (log(N_H/cm^-2) >~ 19.2) or a hard power-law spectrum combined with
    some obscuration (e.g. dlog(F_\nu)/dlog(\nu) >~ -1.2 at log(N_H/cm^-2) >~ 18.0),
    the thickness of the front exceeds ~1 physical Mpc and may be measurable from
    the morphology of its redshifted 21cm signal. We find that the highly ionized
    inner part of the front, which may be probed by Lyman line absorption spectra,
    remains sharp for bright quasars unless a large obscuring column (log(N_H/cm^-2)
    >~ 19.2) removes most of their ionizing photons up to ~40 eV. For obscured sources
    with log(N_H/cm^-2) >~ 19.8, embedded in a significantly neutral IGM, the black
    Lyman-alpha trough (where the neutral fraction is ~10^-3) underestimates the size
    of the HII region by a factor of >~4.
article_processing_charge: No
article_type: original
author:
- first_name: R. H.
  full_name: Kramer, R. H.
  last_name: Kramer
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: Kramer RH, Haiman Z. The thickness of high-redshift quasar ionization fronts
    as a constraint on the ionizing spectral energy distribution. <i>Monthly Notices
    of the Royal Astronomical Society</i>. 2008;385(3):1561-1575. doi:<a href="https://doi.org/10.1111/j.1365-2966.2008.12945.x">10.1111/j.1365-2966.2008.12945.x</a>
  apa: Kramer, R. H., &#38; Haiman, Z. (2008). The thickness of high-redshift quasar
    ionization fronts as a constraint on the ionizing spectral energy distribution.
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press.
    <a href="https://doi.org/10.1111/j.1365-2966.2008.12945.x">https://doi.org/10.1111/j.1365-2966.2008.12945.x</a>
  chicago: Kramer, R. H., and Zoltán Haiman. “The Thickness of High-Redshift Quasar
    Ionization Fronts as a Constraint on the Ionizing Spectral Energy Distribution.”
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press,
    2008. <a href="https://doi.org/10.1111/j.1365-2966.2008.12945.x">https://doi.org/10.1111/j.1365-2966.2008.12945.x</a>.
  ieee: R. H. Kramer and Z. Haiman, “The thickness of high-redshift quasar ionization
    fronts as a constraint on the ionizing spectral energy distribution,” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 385, no. 3. Oxford University
    Press, pp. 1561–1575, 2008.
  ista: Kramer RH, Haiman Z. 2008. The thickness of high-redshift quasar ionization
    fronts as a constraint on the ionizing spectral energy distribution. Monthly Notices
    of the Royal Astronomical Society. 385(3), 1561–1575.
  mla: Kramer, R. H., and Zoltán Haiman. “The Thickness of High-Redshift Quasar Ionization
    Fronts as a Constraint on the Ionizing Spectral Energy Distribution.” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 385, no. 3, Oxford University
    Press, 2008, pp. 1561–75, doi:<a href="https://doi.org/10.1111/j.1365-2966.2008.12945.x">10.1111/j.1365-2966.2008.12945.x</a>.
  short: R.H. Kramer, Z. Haiman, Monthly Notices of the Royal Astronomical Society
    385 (2008) 1561–1575.
date_created: 2024-09-06T09:09:01Z
date_published: 2008-03-13T00:00:00Z
date_updated: 2024-09-25T13:54:14Z
day: '13'
doi: 10.1111/j.1365-2966.2008.12945.x
extern: '1'
intvolume: '       385'
issue: '3'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1111/j.1365-2966.2008.12945.x
month: '03'
oa: 1
oa_version: Published Version
page: 1561-1575
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The thickness of high-redshift quasar ionization fronts as a constraint on
  the ionizing spectral energy distribution
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 385
year: '2008'
...
---
_id: '17778'
abstract:
- lang: eng
  text: The earliest generation of stars and black holes must have established an
    early ‘Lyman–Werner’ background (LWB) at high redshift, prior to the epoch of
    reionization. Because of the long mean free path of photons with energies hν <
    13.6 eV, the LWB was nearly uniform. However, some variation in the LWB is expected
    due to the discrete nature of the sources, and their highly clustered spatial
    distribution. In this paper, we compute the probability distribution function
    (PDF) of the LW flux that irradiates dark matter (DM) haloes collapsing at high
    redshift (z≈ 10). Our model accounts for (i) the clustering of DM haloes, (ii)
    Poisson fluctuations in the number of corresponding star-forming galaxies and
    (iii) scatter in the LW luminosity produced by haloes of a given mass (calibrated
    using local observations). We find that >99 per cent of the DM haloes are illuminated
    by an LW flux within a factor of 2 of the global mean value. However, a small
    fraction, ∼10^−8 to 10^−6, of DM haloes with virial temperatures Tvir≳ 10^4 K
    have a close luminous neighbour within ≲10 kpc, and are exposed to an LW flux
    exceeding the global mean by a factor of >20, or to J21,LW > 10^3 (in units of
    10^−21 erg s^−1 Hz^−1 sr^−1 cm^−2). This large LW flux can photodissociate H2
    molecules in the gas collapsing due to atomic cooling in these haloes, and prevent
    its further cooling and fragmentation. Such close halo pairs therefore provide
    possible sites in which primordial gas clouds collapse directly into massive black
    holes (MBH≈ 10^4−6M⊙), and subsequently grow into supermassive (MBH≳ 10^9M⊙) black
    holes by z≈ 6.
article_processing_charge: No
article_type: original
author:
- first_name: Mark
  full_name: Dijkstra, Mark
  last_name: Dijkstra
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
- first_name: Andrei
  full_name: Mesinger, Andrei
  last_name: Mesinger
- first_name: J. Stuart B.
  full_name: Wyithe, J. Stuart B.
  last_name: Wyithe
citation:
  ama: 'Dijkstra M, Haiman Z, Mesinger A, Wyithe JSB. Fluctuations in the high-redshift
    Lyman-Werner background: Close halo pairs as the origin of supermassive black
    holes. <i>Monthly Notices of the Royal Astronomical Society</i>. 2008;391(4):1961-1972.
    doi:<a href="https://doi.org/10.1111/j.1365-2966.2008.14031.x">10.1111/j.1365-2966.2008.14031.x</a>'
  apa: 'Dijkstra, M., Haiman, Z., Mesinger, A., &#38; Wyithe, J. S. B. (2008). Fluctuations
    in the high-redshift Lyman-Werner background: Close halo pairs as the origin of
    supermassive black holes. <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press. <a href="https://doi.org/10.1111/j.1365-2966.2008.14031.x">https://doi.org/10.1111/j.1365-2966.2008.14031.x</a>'
  chicago: 'Dijkstra, Mark, Zoltán Haiman, Andrei Mesinger, and J. Stuart B. Wyithe.
    “Fluctuations in the High-Redshift Lyman-Werner Background: Close Halo Pairs as
    the Origin of Supermassive Black Holes.” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2008. <a href="https://doi.org/10.1111/j.1365-2966.2008.14031.x">https://doi.org/10.1111/j.1365-2966.2008.14031.x</a>.'
  ieee: 'M. Dijkstra, Z. Haiman, A. Mesinger, and J. S. B. Wyithe, “Fluctuations in
    the high-redshift Lyman-Werner background: Close halo pairs as the origin of supermassive
    black holes,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 391,
    no. 4. Oxford University Press, pp. 1961–1972, 2008.'
  ista: 'Dijkstra M, Haiman Z, Mesinger A, Wyithe JSB. 2008. Fluctuations in the high-redshift
    Lyman-Werner background: Close halo pairs as the origin of supermassive black
    holes. Monthly Notices of the Royal Astronomical Society. 391(4), 1961–1972.'
  mla: 'Dijkstra, Mark, et al. “Fluctuations in the High-Redshift Lyman-Werner Background:
    Close Halo Pairs as the Origin of Supermassive Black Holes.” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 391, no. 4, Oxford University Press,
    2008, pp. 1961–72, doi:<a href="https://doi.org/10.1111/j.1365-2966.2008.14031.x">10.1111/j.1365-2966.2008.14031.x</a>.'
  short: M. Dijkstra, Z. Haiman, A. Mesinger, J.S.B. Wyithe, Monthly Notices of the
    Royal Astronomical Society 391 (2008) 1961–1972.
date_created: 2024-09-06T10:13:39Z
date_published: 2008-12-11T00:00:00Z
date_updated: 2024-09-30T11:57:59Z
day: '11'
doi: 10.1111/j.1365-2966.2008.14031.x
extern: '1'
intvolume: '       391'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1111/j.1365-2966.2008.14031.x
month: '12'
oa: 1
oa_version: Published Version
page: 1961-1972
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Fluctuations in the high-redshift Lyman-Werner background: Close halo pairs
  as the origin of supermassive black holes'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 391
year: '2008'
...
---
_id: '17716'
abstract:
- lang: eng
  text: Recent observations imply that the observed number counts of Lyα emitters
    (LAEs) evolved significantly between z= 5.7 and 6.5. It has been suggested that
    this was due to a rapid evolution in the ionization state, and hence transmission
    of the intergalactic medium (IGM) which caused Lyα flux from z= 6.5 galaxies to
    be more strongly suppressed. In this paper, we consider the joint evolution of
    the Lyα and the ultraviolet luminosity functions (LFs) and show that the IGM transmission
    evolved between z= 6.5 and 5.7 by a factor 1.1 < R < 1.8 (95 per cent confidence
    level). This result is insensitive to the underlying model of the Lyα LF (as well
    as cosmic variance). Using a model for IGM transmission, we find that the evolution
    of the mean IGM density through cosmic expansion alone may result in a value for
    the ratio of transmissions as high as R= 1.3. Thus, the existing LFs do not provide
    evidence for overlap. Furthermore, the constraint R < 1.8 suggests that the Universe
    at z= 6.5 was more than half-ionized by volume, that is, xi,V > 0.5.
article_processing_charge: No
article_type: original
author:
- first_name: M.
  full_name: Dijkstra, M.
  last_name: Dijkstra
- first_name: J. S. B.
  full_name: Wyithe, J. S. B.
  last_name: Wyithe
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: Dijkstra M, Wyithe JSB, Haiman Z. Luminosity functions of Lyα emitting galaxies
    and cosmic reionization of hydrogen. <i>Monthly Notices of the Royal Astronomical
    Society</i>. 2007;379(1):253-259. doi:<a href="https://doi.org/10.1111/j.1365-2966.2007.11936.x">10.1111/j.1365-2966.2007.11936.x</a>
  apa: Dijkstra, M., Wyithe, J. S. B., &#38; Haiman, Z. (2007). Luminosity functions
    of Lyα emitting galaxies and cosmic reionization of hydrogen. <i>Monthly Notices
    of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1111/j.1365-2966.2007.11936.x">https://doi.org/10.1111/j.1365-2966.2007.11936.x</a>
  chicago: Dijkstra, M., J. S. B. Wyithe, and Zoltán Haiman. “Luminosity Functions
    of Lyα Emitting Galaxies and Cosmic Reionization of Hydrogen.” <i>Monthly Notices
    of the Royal Astronomical Society</i>. Oxford University Press, 2007. <a href="https://doi.org/10.1111/j.1365-2966.2007.11936.x">https://doi.org/10.1111/j.1365-2966.2007.11936.x</a>.
  ieee: M. Dijkstra, J. S. B. Wyithe, and Z. Haiman, “Luminosity functions of Lyα
    emitting galaxies and cosmic reionization of hydrogen,” <i>Monthly Notices of
    the Royal Astronomical Society</i>, vol. 379, no. 1. Oxford University Press,
    pp. 253–259, 2007.
  ista: Dijkstra M, Wyithe JSB, Haiman Z. 2007. Luminosity functions of Lyα emitting
    galaxies and cosmic reionization of hydrogen. Monthly Notices of the Royal Astronomical
    Society. 379(1), 253–259.
  mla: Dijkstra, M., et al. “Luminosity Functions of Lyα Emitting Galaxies and Cosmic
    Reionization of Hydrogen.” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 379, no. 1, Oxford University Press, 2007, pp. 253–59, doi:<a href="https://doi.org/10.1111/j.1365-2966.2007.11936.x">10.1111/j.1365-2966.2007.11936.x</a>.
  short: M. Dijkstra, J.S.B. Wyithe, Z. Haiman, Monthly Notices of the Royal Astronomical
    Society 379 (2007) 253–259.
date_created: 2024-09-06T09:01:21Z
date_published: 2007-06-21T00:00:00Z
date_updated: 2024-09-25T13:02:42Z
day: '21'
doi: 10.1111/j.1365-2966.2007.11936.x
extern: '1'
intvolume: '       379'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1111/j.1365-2966.2007.11936.x
month: '06'
oa: 1
oa_version: Published Version
page: 253-259
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Luminosity functions of Lyα emitting galaxies and cosmic reionization of hydrogen
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 379
year: '2007'
...
---
_id: '17768'
abstract:
- lang: eng
  text: 'We develop an analytic approach to study inhomogeneous reionization on large
    scales by solving the equations of ionization balance and radiative transfer to
    first order in perturbations. Given the spatial distribution and spectrum of the
    ionizing sources, our formalism can be used to predict the large-scale power spectra
    of fluctuations in the abundances of H ii, H i and radiation. Our approach avoids
    common approximations/assumptions in existing analytic methods – for instance,
    we do not assume a specific ionization topology from the outset; nor do we make
    a step-function bubble-like approximation to the H ii distribution. Applying our
    formalism to sources biased according to the Press–Schechter prescription, we
    find: (1) reionization always proceeds ‘inside–out’, with dense regions more highly
    ionized, at least on large scales; (2) on sufficiently large scales, H ii, H i
    and radiation exhibit a scale-independent bias relative to dark matter; (3) the
    bias is suppressed on scales comparable to or smaller than the mean free path
    of the ionizing photons; (4) if the ionizing source spectrum is sufficiently soft,
    the H ii bias closely tracks the source bias for most of the reionization process
    but drops precipitously after percolation; and (5) if the ionizing source spectrum
    is sufficiently hard, the H ii bias drops in a more steady fashion throughout
    the reionization process. The tools developed here will be useful for interpreting
    future 21-cm, cosmic microwave background and Lyman α forest observations, both
    to learn about the reionization astrophysics (such as the hardness of the source
    spectrum and therefore the nature of the ionizing sources) and to possibly extract
    interesting cosmological information.'
article_processing_charge: No
article_type: original
author:
- first_name: J.
  full_name: Zhang, J.
  last_name: Zhang
- first_name: L.
  full_name: Hui, L.
  last_name: Hui
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: Zhang J, Hui L, Haiman Z. A linear perturbation theory of inhomogeneous reionization.
    <i>Monthly Notices of the Royal Astronomical Society</i>. 2007;375(1):324-336.
    doi:<a href="https://doi.org/10.1111/j.1365-2966.2006.11311.x">10.1111/j.1365-2966.2006.11311.x</a>
  apa: Zhang, J., Hui, L., &#38; Haiman, Z. (2007). A linear perturbation theory of
    inhomogeneous reionization. <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press. <a href="https://doi.org/10.1111/j.1365-2966.2006.11311.x">https://doi.org/10.1111/j.1365-2966.2006.11311.x</a>
  chicago: Zhang, J., L. Hui, and Zoltán Haiman. “A Linear Perturbation Theory of
    Inhomogeneous Reionization.” <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press, 2007. <a href="https://doi.org/10.1111/j.1365-2966.2006.11311.x">https://doi.org/10.1111/j.1365-2966.2006.11311.x</a>.
  ieee: J. Zhang, L. Hui, and Z. Haiman, “A linear perturbation theory of inhomogeneous
    reionization,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol.
    375, no. 1. Oxford University Press, pp. 324–336, 2007.
  ista: Zhang J, Hui L, Haiman Z. 2007. A linear perturbation theory of inhomogeneous
    reionization. Monthly Notices of the Royal Astronomical Society. 375(1), 324–336.
  mla: Zhang, J., et al. “A Linear Perturbation Theory of Inhomogeneous Reionization.”
    <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 375, no. 1, Oxford
    University Press, 2007, pp. 324–36, doi:<a href="https://doi.org/10.1111/j.1365-2966.2006.11311.x">10.1111/j.1365-2966.2006.11311.x</a>.
  short: J. Zhang, L. Hui, Z. Haiman, Monthly Notices of the Royal Astronomical Society
    375 (2007) 324–336.
date_created: 2024-09-06T09:55:13Z
date_published: 2007-01-15T00:00:00Z
date_updated: 2024-09-30T09:36:26Z
day: '15'
doi: 10.1111/j.1365-2966.2006.11311.x
extern: '1'
intvolume: '       375'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1111/j.1365-2966.2006.11311.x
month: '01'
oa: 1
oa_version: Published Version
page: 324-336
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: A linear perturbation theory of inhomogeneous reionization
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 375
year: '2007'
...
---
_id: '17748'
abstract:
- lang: eng
  text: 'Recent results by the WMAP satellite suggest that the intergalactic medium
    was significantly reionized at redshifts as high as z~17. At this early epoch,
    the first ionizing sources likely appeared in the shallow potential wells of mini-halos
    with virial temperatures T < 10^4 K. Once such an ionizing source turns off, its
    surrounding HII region Compton cools and recombines. Nonetheless, we show that
    the ``fossil'''' HII regions left behind remain at high adiabats, prohibiting
    gas accretion and cooling in subsequent generations of mini-halos. Thus, early
    star formation is self-limiting. We quantify this effect to show that star formation
    in mini-halos cannot account for the bulk of the electron scattering opacity measured
    by WMAP, which must be due to more massive objects. We argue that gas entropy,
    rather than IGM metallicity, regulates the evolution of the global ionizing emissivity,
    and impedes full reionization until lower redshifts. We discuss several important
    consequences of this early entropy floor for reionization. It reduces gas clumping,
    curtailing the required photon budget for reionization. An entropy floor also
    prevents H2 formation and cooling, due to reduced gas densities: it greatly enhances
    feedback from UV photodissociation of H2. An early X-ray background would also
    furnish an entropy floor to the entire IGM; thus, X-rays impede rather than enhance
    H2 formation. Future 21cm observations may probe the topology of fossil HII regions.'
alternative_title:
- Fossil H ii regions
article_processing_charge: No
article_type: original
author:
- first_name: S. Peng
  full_name: Oh, S. Peng
  last_name: Oh
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: 'Oh SP, Haiman Z. Fossil H ii regions: Self-limiting star formation at high
    redshift. <i>Monthly Notices of the Royal Astronomical Society</i>. 2003;346(2):456-472.
    doi:<a href="https://doi.org/10.1046/j.1365-2966.2003.07103.x">10.1046/j.1365-2966.2003.07103.x</a>'
  apa: 'Oh, S. P., &#38; Haiman, Z. (2003). Fossil H ii regions: Self-limiting star
    formation at high redshift. <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press. <a href="https://doi.org/10.1046/j.1365-2966.2003.07103.x">https://doi.org/10.1046/j.1365-2966.2003.07103.x</a>'
  chicago: 'Oh, S. Peng, and Zoltán Haiman. “Fossil H Ii Regions: Self-Limiting Star
    Formation at High Redshift.” <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press, 2003. <a href="https://doi.org/10.1046/j.1365-2966.2003.07103.x">https://doi.org/10.1046/j.1365-2966.2003.07103.x</a>.'
  ieee: 'S. P. Oh and Z. Haiman, “Fossil H ii regions: Self-limiting star formation
    at high redshift,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol.
    346, no. 2. Oxford University Press, pp. 456–472, 2003.'
  ista: 'Oh SP, Haiman Z. 2003. Fossil H ii regions: Self-limiting star formation
    at high redshift. Monthly Notices of the Royal Astronomical Society. 346(2), 456–472.'
  mla: 'Oh, S. Peng, and Zoltán Haiman. “Fossil H Ii Regions: Self-Limiting Star Formation
    at High Redshift.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol.
    346, no. 2, Oxford University Press, 2003, pp. 456–72, doi:<a href="https://doi.org/10.1046/j.1365-2966.2003.07103.x">10.1046/j.1365-2966.2003.07103.x</a>.'
  short: S.P. Oh, Z. Haiman, Monthly Notices of the Royal Astronomical Society 346
    (2003) 456–472.
date_created: 2024-09-06T09:36:17Z
date_published: 2003-12-01T00:00:00Z
date_updated: 2024-09-26T15:00:48Z
day: '01'
doi: 10.1046/j.1365-2966.2003.07103.x
extern: '1'
intvolume: '       346'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1046/j.1365-2966.2003.07103.x
month: '12'
oa: 1
oa_version: Published Version
page: 456-472
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Fossil H ii regions: Self-limiting star formation at high redshift'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 346
year: '2003'
...