---
_id: '4338'
abstract:
- lang: eng
  text: 'Mosaic hybrid zones arise when ecologically differentiated taxa hybridize
    across a network of habitat patches. Frequent interbreeding across a small-scale
    patchwork can erode species differences that might have been preserved in a clinal
    hybrid zone. In particular, the rapid breakdown of neutral divergence sets an
    upper limit to the time for which differences at marker loci can persist. We present
    here a case study of a mosaic hybrid zone between the fire-bellied toads Bombina
    bombina and B. variegata (Anura: Discoglossidae) near Apahida in Romania. In our
    20 × 20 km study area, we detected no evidence of a clinal transition but found
    a strong association between aquatic habitat and mean allele frequencies at four
    molecular markers. In particular, pure populations of B. bombina in ponds appear
    to cause massive introgression into the surrounding B. variegata gene pool found
    in temporary aquatic sites. Nevertheless, the genetic structure of these hybrid
    populations was remarkably similar to those of a previously studied transect near
    Pescenica (Croatia), which had both clinal and mosaic features: estimates of heterozygote
    deficit and linkage disequilibrium in each country are similar. In Apahida, the
    observed strong linkage disequilibria should stem from an imperfect habitat preference
    that guides most (but not all) adults into the habitats to which they are adapted.
    In the absence of a clinal structure, the inferred migration rate between habitats
    implies that associations between selected loci and neutral markers should break
    down rapidly. Although plausible selection strengths can maintain differentiation
    at those loci adapting the toads to either permanent or temporary breeding sites,
    the divergence at neutral markers must be transient. The hybrid zone may be approaching
    a state in which the gene pools are homogenized at all but the selected loci,
    not dissimilar from an early stage of sympatric divergence.'
acknowledgement: "We thank G. Mara and T. Galbena for enthusiastic field\r\nassistance,
  A. Hofmann and R. Sieglstetter for access to their\r\nunpublished data, B. Fo¨rg-Brey
  and G. Praetzel for help in\r\nthe lab. Helpful comments on a previous version of
  the man-\r\nuscript were provided by R. Ennos, J. Szymura, F. Balloux,\r\nJ. Bridle,
  L. Kruuk, F. Bonhomme, M. Arnold, and two anon-\r\nymous reviewers. We also thank
  A. Pinggera for providing\r\nthe cover illustration. This work was supported by
  Natural\r\nEnvironment Research Council studentships to THV and TRS\r\nand Deutsche
  Forschungsgemeinschaft grant Nu 51/2-1 to BN."
article_processing_charge: No
article_type: original
author:
- first_name: Timothy
  full_name: Vines, Timothy
  last_name: Vines
- first_name: S C
  full_name: Kohler, S C
  last_name: Kohler
- first_name: M
  full_name: Thiel, M
  last_name: Thiel
- first_name: Ioan
  full_name: Ghira, Ioan
  last_name: Ghira
- first_name: T R
  full_name: Sands, T R
  last_name: Sands
- first_name: Catriona
  full_name: Maccallum, Catriona
  last_name: Maccallum
- first_name: Nicholas H
  full_name: Barton, Nicholas H
  id: 4880FE40-F248-11E8-B48F-1D18A9856A87
  last_name: Barton
  orcid: 0000-0002-8548-5240
- first_name: Beate
  full_name: Nürnberger, Beate
  last_name: Nürnberger
citation:
  ama: Vines T, Kohler SC, Thiel M, et al. On the maintenance of reproductive isolation
    in a mosaic hybrid zone between the toads Bombina bombina and B. variegata. <i>Evolution</i>.
    2003;57(8):1876-1888. doi:<a href="https://doi.org/10.1111/j.0014-3820.2003.tb00595.x">10.1111/j.0014-3820.2003.tb00595.x</a>
  apa: Vines, T., Kohler, S. C., Thiel, M., Ghira, I., Sands, T. R., Maccallum, C.,
    … Nürnberger, B. (2003). On the maintenance of reproductive isolation in a mosaic
    hybrid zone between the toads Bombina bombina and B. variegata. <i>Evolution</i>.
    Wiley-Blackwell. <a href="https://doi.org/10.1111/j.0014-3820.2003.tb00595.x">https://doi.org/10.1111/j.0014-3820.2003.tb00595.x</a>
  chicago: Vines, Timothy, S C Kohler, M Thiel, Ioan Ghira, T R Sands, Catriona Maccallum,
    Nicholas H Barton, and Beate Nürnberger. “On the Maintenance of Reproductive Isolation
    in a Mosaic Hybrid Zone between the Toads Bombina Bombina and B. Variegata.” <i>Evolution</i>.
    Wiley-Blackwell, 2003. <a href="https://doi.org/10.1111/j.0014-3820.2003.tb00595.x">https://doi.org/10.1111/j.0014-3820.2003.tb00595.x</a>.
  ieee: T. Vines <i>et al.</i>, “On the maintenance of reproductive isolation in a
    mosaic hybrid zone between the toads Bombina bombina and B. variegata,” <i>Evolution</i>,
    vol. 57, no. 8. Wiley-Blackwell, pp. 1876–1888, 2003.
  ista: Vines T, Kohler SC, Thiel M, Ghira I, Sands TR, Maccallum C, Barton NH, Nürnberger
    B. 2003. On the maintenance of reproductive isolation in a mosaic hybrid zone
    between the toads Bombina bombina and B. variegata. Evolution. 57(8), 1876–1888.
  mla: Vines, Timothy, et al. “On the Maintenance of Reproductive Isolation in a Mosaic
    Hybrid Zone between the Toads Bombina Bombina and B. Variegata.” <i>Evolution</i>,
    vol. 57, no. 8, Wiley-Blackwell, 2003, pp. 1876–88, doi:<a href="https://doi.org/10.1111/j.0014-3820.2003.tb00595.x">10.1111/j.0014-3820.2003.tb00595.x</a>.
  short: T. Vines, S.C. Kohler, M. Thiel, I. Ghira, T.R. Sands, C. Maccallum, N.H.
    Barton, B. Nürnberger, Evolution 57 (2003) 1876–1888.
date_created: 2018-12-11T12:08:20Z
date_published: 2003-08-01T00:00:00Z
date_updated: 2024-01-23T09:16:43Z
day: '01'
doi: 10.1111/j.0014-3820.2003.tb00595.x
extern: '1'
fulldoi: https://doi.org/10.1111/j.0014-3820.2003.tb00595.x
intvolume: '        57'
issue: '8'
language:
- iso: eng
month: '08'
oa_version: None
page: 1876 - 1888
publication: Evolution
publication_identifier:
  issn:
  - 0014-3820
publication_status: published
publisher: Wiley-Blackwell
publist_id: '1692'
quality_controlled: '1'
scopus_import: '1'
status: public
title: On the maintenance of reproductive isolation in a mosaic hybrid zone between
  the toads Bombina bombina and B. variegata
type: journal_article
user_id: ea97e931-d5af-11eb-85d4-e6957dddbf17
volume: 57
year: '2003'
...
---
_id: '17741'
abstract:
- lang: eng
  text: The recent discovery of a Gunn-Peterson (GP) trough in the spectrum of the
    redshift 6.28 SDSS quasar has raised the tantalizing possibility that we have
    detected the reionization of the universe. However, a neutral fraction (of hydrogen)
    as small as 0.1% is sufficient to cause the GP trough; hence, its detection alone
    cannot rule out reionization at a much earlier epoch. The cosmic microwave background
    (CMB) polarization anisotropy offers an alternative way to explore the dark age
    of the universe. We show that for most models constrained by the current CMB data
    and by the discovery of a GP trough (showing that reionization occurred at z >
    6.3), Microwave Anisotropy Probe (MAP) can detect the reionization signature in
    the polarization power spectrum. The expected 1 σ error on the measurement of
    the electron optical depth is around 0.03 with a weak dependence on the value
    of that optical depth. Such a constraint on the optical depth will allow MAP to
    achieve a 1 σ error on the amplitude of the primordial power spectrum of 6%. MAP
    with 2 yr (Planck with 1 yr) of observation can distinguish a model with 50% (6%)
    partial ionization between redshifts of 6.3 and 20 from a model in which hydrogen
    was completely neutral at redshifts greater than 6.3. Planck will be able to distinguish
    between different reionization histories even when they imply the same optical
    depth to electron scattering for the CMB photons.
article_processing_charge: No
article_type: original
author:
- first_name: Manoj
  full_name: Kaplinghat, Manoj
  last_name: Kaplinghat
- first_name: Mike
  full_name: Chu, Mike
  last_name: Chu
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
- first_name: Gilbert P.
  full_name: Holder, Gilbert P.
  last_name: Holder
- first_name: Lloyd
  full_name: Knox, Lloyd
  last_name: Knox
- first_name: Constantinos
  full_name: Skordis, Constantinos
  last_name: Skordis
citation:
  ama: Kaplinghat M, Chu M, Haiman Z, Holder GP, Knox L, Skordis C. Probing the reionization
    history of the universe using the cosmic microwave background polarization. <i>The
    Astrophysical Journal</i>. 2003;583(1):24-32. doi:<a href="https://doi.org/10.1086/344927">10.1086/344927</a>
  apa: Kaplinghat, M., Chu, M., Haiman, Z., Holder, G. P., Knox, L., &#38; Skordis,
    C. (2003). Probing the reionization history of the universe using the cosmic microwave
    background polarization. <i>The Astrophysical Journal</i>. American Astronomical
    Society. <a href="https://doi.org/10.1086/344927">https://doi.org/10.1086/344927</a>
  chicago: Kaplinghat, Manoj, Mike Chu, Zoltán Haiman, Gilbert P. Holder, Lloyd Knox,
    and Constantinos Skordis. “Probing the Reionization History of the Universe Using
    the Cosmic Microwave Background Polarization.” <i>The Astrophysical Journal</i>.
    American Astronomical Society, 2003. <a href="https://doi.org/10.1086/344927">https://doi.org/10.1086/344927</a>.
  ieee: M. Kaplinghat, M. Chu, Z. Haiman, G. P. Holder, L. Knox, and C. Skordis, “Probing
    the reionization history of the universe using the cosmic microwave background
    polarization,” <i>The Astrophysical Journal</i>, vol. 583, no. 1. American Astronomical
    Society, pp. 24–32, 2003.
  ista: Kaplinghat M, Chu M, Haiman Z, Holder GP, Knox L, Skordis C. 2003. Probing
    the reionization history of the universe using the cosmic microwave background
    polarization. The Astrophysical Journal. 583(1), 24–32.
  mla: Kaplinghat, Manoj, et al. “Probing the Reionization History of the Universe
    Using the Cosmic Microwave Background Polarization.” <i>The Astrophysical Journal</i>,
    vol. 583, no. 1, American Astronomical Society, 2003, pp. 24–32, doi:<a href="https://doi.org/10.1086/344927">10.1086/344927</a>.
  short: M. Kaplinghat, M. Chu, Z. Haiman, G.P. Holder, L. Knox, C. Skordis, The Astrophysical
    Journal 583 (2003) 24–32.
date_created: 2024-09-06T09:25:08Z
date_published: 2003-01-20T00:00:00Z
date_updated: 2024-09-26T14:15:21Z
day: '20'
doi: 10.1086/344927
extern: '1'
fulldoi: https://doi.org/10.1086/344927
intvolume: '       583'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1086/344927
month: '01'
oa: 1
oa_version: Published Version
page: 24-32
publication: The Astrophysical Journal
publication_identifier:
  issn:
  - 0004-637X
  - 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Probing the reionization history of the universe using the cosmic microwave
  background polarization
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 583
year: '2003'
...
---
_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'
fulldoi: https://doi.org/10.1046/j.1365-2966.2003.07103.x
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'
...
---
_id: '17750'
abstract:
- lang: eng
  text: We present the discovery of three new quasars at z>6 in 1300 deg^2 of SDSS
    imaging data, J114816.64+525150.3 (z=6.43), J104845.05+463718.3 (z=6.23) and J163033.90+401209.6
    (z=6.05). The first two objects have weak Ly alpha emission lines; their redshifts
    are determined from the positions of the Lyman break. They are only accurate to
    0.05 and could be affected by the presence of broad absorption line systems. The
    last object has a Ly alpha strength more typical of lower redshift quasars. Based
    on a sample of six quasars at z>5.7 that cover 2870 deg^2 presented in this paper
    and in Paper I, we estimate the comoving density of luminous quasars at z 6 and
    M_{1450} < -26.8 to be (8 +/- 3)x10^{-10} Mpc^{-3} (for H_0 = 50 km/s/Mpc, Omega
    = 1). HST imaging of two z>5.7 quasars and high-resolution ground-based images
    (seeing 0.4'') of three additional z>5.7 quasars show that none of them is gravitationally
    lensed. The luminosity distribution of the high-redshfit quasar sample suggests
    the bright end slope of the quasar luminosity function at z 6 is shallower than
    Psi L^{-3.5} (2-sigma), consistent with the absence of strongly lensed objects.
article_processing_charge: No
article_type: original
author:
- first_name: Xiaohui
  full_name: Fan, Xiaohui
  last_name: Fan
- first_name: Michael A.
  full_name: Strauss, Michael A.
  last_name: Strauss
- first_name: Donald P.
  full_name: Schneider, Donald P.
  last_name: Schneider
- first_name: Robert H.
  full_name: Becker, Robert H.
  last_name: Becker
- first_name: Richard L.
  full_name: White, Richard L.
  last_name: White
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
- first_name: Michael
  full_name: Gregg, Michael
  last_name: Gregg
- first_name: Laura
  full_name: Pentericci, Laura
  last_name: Pentericci
- first_name: Eva K.
  full_name: Grebel, Eva K.
  last_name: Grebel
- first_name: Vijay K.
  full_name: Narayanan, Vijay K.
  last_name: Narayanan
- first_name: Yeong-Shang
  full_name: Loh, Yeong-Shang
  last_name: Loh
- first_name: Gordon T.
  full_name: Richards, Gordon T.
  last_name: Richards
- first_name: James E.
  full_name: Gunn, James E.
  last_name: Gunn
- first_name: Robert H.
  full_name: Lupton, Robert H.
  last_name: Lupton
- first_name: Gillian R.
  full_name: Knapp, Gillian R.
  last_name: Knapp
- first_name: Željko
  full_name: Ivezić, Željko
  last_name: Ivezić
- first_name: W. N.
  full_name: Brandt, W. N.
  last_name: Brandt
- first_name: Matthew
  full_name: Collinge, Matthew
  last_name: Collinge
- first_name: Lei
  full_name: Hao, Lei
  last_name: Hao
- first_name: Daniel
  full_name: Harbeck, Daniel
  last_name: Harbeck
- first_name: Francisco
  full_name: Prada, Francisco
  last_name: Prada
- first_name: Joop
  full_name: Schaye, Joop
  last_name: Schaye
- first_name: Iskra
  full_name: Strateva, Iskra
  last_name: Strateva
- first_name: Nadia
  full_name: Zakamska, Nadia
  last_name: Zakamska
- first_name: Scott
  full_name: Anderson, Scott
  last_name: Anderson
- first_name: Jon
  full_name: Brinkmann, Jon
  last_name: Brinkmann
- first_name: Neta A.
  full_name: Bahcall, Neta A.
  last_name: Bahcall
- first_name: Don Q.
  full_name: Lamb, Don Q.
  last_name: Lamb
- first_name: Sadanori
  full_name: Okamura, Sadanori
  last_name: Okamura
- first_name: Alex
  full_name: Szalay, Alex
  last_name: Szalay
- first_name: Donald G.
  full_name: York, Donald G.
  last_name: York
citation:
  ama: Fan X, Strauss MA, Schneider DP, et al. A survey of z &#62; 5.7 quasars in
    the Sloan Digital Sky Survey. II. Discovery of three additional quasars at z &#62;
    6. <i>The Astronomical Journal</i>. 2003;125(4):1649-1659. doi:<a href="https://doi.org/10.1086/368246">10.1086/368246</a>
  apa: Fan, X., Strauss, M. A., Schneider, D. P., Becker, R. H., White, R. L., Haiman,
    Z., … York, D. G. (2003). A survey of z &#62; 5.7 quasars in the Sloan Digital
    Sky Survey. II. Discovery of three additional quasars at z &#62; 6. <i>The Astronomical
    Journal</i>. American Astronomical Society. <a href="https://doi.org/10.1086/368246">https://doi.org/10.1086/368246</a>
  chicago: Fan, Xiaohui, Michael A. Strauss, Donald P. Schneider, Robert H. Becker,
    Richard L. White, Zoltán Haiman, Michael Gregg, et al. “A Survey of z &#62; 5.7
    Quasars in the Sloan Digital Sky Survey. II. Discovery of Three Additional Quasars
    at z &#62; 6.” <i>The Astronomical Journal</i>. American Astronomical Society,
    2003. <a href="https://doi.org/10.1086/368246">https://doi.org/10.1086/368246</a>.
  ieee: X. Fan <i>et al.</i>, “A survey of z &#62; 5.7 quasars in the Sloan Digital
    Sky Survey. II. Discovery of three additional quasars at z &#62; 6,” <i>The Astronomical
    Journal</i>, vol. 125, no. 4. American Astronomical Society, pp. 1649–1659, 2003.
  ista: Fan X, Strauss MA, Schneider DP, Becker RH, White RL, Haiman Z, Gregg M, Pentericci
    L, Grebel EK, Narayanan VK, Loh Y-S, Richards GT, Gunn JE, Lupton RH, Knapp GR,
    Ivezić Ž, Brandt WN, Collinge M, Hao L, Harbeck D, Prada F, Schaye J, Strateva
    I, Zakamska N, Anderson S, Brinkmann J, Bahcall NA, Lamb DQ, Okamura S, Szalay
    A, York DG. 2003. A survey of z &#62; 5.7 quasars in the Sloan Digital Sky Survey.
    II. Discovery of three additional quasars at z &#62; 6. The Astronomical Journal.
    125(4), 1649–1659.
  mla: Fan, Xiaohui, et al. “A Survey of z &#62; 5.7 Quasars in the Sloan Digital
    Sky Survey. II. Discovery of Three Additional Quasars at z &#62; 6.” <i>The Astronomical
    Journal</i>, vol. 125, no. 4, American Astronomical Society, 2003, pp. 1649–59,
    doi:<a href="https://doi.org/10.1086/368246">10.1086/368246</a>.
  short: X. Fan, M.A. Strauss, D.P. Schneider, R.H. Becker, R.L. White, Z. Haiman,
    M. Gregg, L. Pentericci, E.K. Grebel, V.K. Narayanan, Y.-S. Loh, G.T. Richards,
    J.E. Gunn, R.H. Lupton, G.R. Knapp, Ž. Ivezić, W.N. Brandt, M. Collinge, L. Hao,
    D. Harbeck, F. Prada, J. Schaye, I. Strateva, N. Zakamska, S. Anderson, J. Brinkmann,
    N.A. Bahcall, D.Q. Lamb, S. Okamura, A. Szalay, D.G. York, The Astronomical Journal
    125 (2003) 1649–1659.
date_created: 2024-09-06T09:38:08Z
date_published: 2003-04-01T00:00:00Z
date_updated: 2024-09-30T07:33:02Z
day: '01'
doi: 10.1086/368246
extern: '1'
fulldoi: https://doi.org/10.1086/368246
intvolume: '       125'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1086/368246
month: '04'
oa: 1
oa_version: Published Version
page: 1649-1659
publication: The Astronomical Journal
publication_identifier:
  issn:
  - 0004-6256
  - 1538-3881
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: A survey of z > 5.7 quasars in the Sloan Digital Sky Survey. II. Discovery
  of three additional quasars at z > 6
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 125
year: '2003'
...
---
_id: '17754'
abstract:
- lang: eng
  text: 'The recent discovery of a high optical depth tau to Thomson scattering from
    the WMAP data implies that significant reionization took place at redshifts z~15.
    This discovery has important implications for the sources of reionization, and
    allows, for the first time, constraints to be placed on physical reionization
    scenarios out to redshift z~20. Using a new suite of semi-analytic reionization
    models, we show that the high value of tau requires a surprisingly high efficiency
    epsilon of the first generation of UV sources for injecting ionizing photons into
    the intergalactic medium. We find that no simple reionization model can be consistent
    with the combination of the WMAP result with data from the z<6.5 universe. Satisfying
    both constraints requires either of the following: (i) H_2 molecules form efficiently
    at z~20, survive feedback processes, and allow UV sources in halos with virial
    temperatures below Tvir=10^4 K to contribute substantially to reionization, or
    (ii) the efficiency epsilon in halos with Tvir>10^4K decreased by a factor of
    ~ 30 between (z~20) and (z~6). We discuss the relevant physical issues to produce
    either scenario, and argue that both options are viable, and allowed by current
    data. In detailed models of the reionization history, we find that the evolution
    of the ionized fractions in the two scenarios have distinctive features that Planck
    can distinguish at 3 sigma significance. At the high WMAP value for tau, Planck
    will also be able to provide tight statistical constraints on reionization model
    parameters, and elucidate much of the physics at the end of the Dark Ages. The
    sources responsible for the high optical depth discovered by WMAP should be directly
    detectable out to z~15 by the James Webb Space Telescope.'
article_processing_charge: No
article_type: original
author:
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
- first_name: Gilbert P.
  full_name: Holder, Gilbert P.
  last_name: Holder
citation:
  ama: Haiman Z, Holder GP. The reionization history at high redshifts. I. Physical
    models and new constraints from cosmic microwave background polarization. <i>The
    Astrophysical Journal</i>. 2003;595(1):1-12. doi:<a href="https://doi.org/10.1086/377337">10.1086/377337</a>
  apa: Haiman, Z., &#38; Holder, G. P. (2003). The reionization history at high redshifts.
    I. Physical models and new constraints from cosmic microwave background polarization.
    <i>The Astrophysical Journal</i>. American Astronomical Society. <a href="https://doi.org/10.1086/377337">https://doi.org/10.1086/377337</a>
  chicago: Haiman, Zoltán, and Gilbert P. Holder. “The Reionization History at High
    Redshifts. I. Physical Models and New Constraints from Cosmic Microwave Background
    Polarization.” <i>The Astrophysical Journal</i>. American Astronomical Society,
    2003. <a href="https://doi.org/10.1086/377337">https://doi.org/10.1086/377337</a>.
  ieee: Z. Haiman and G. P. Holder, “The reionization history at high redshifts. I.
    Physical models and new constraints from cosmic microwave background polarization,”
    <i>The Astrophysical Journal</i>, vol. 595, no. 1. American Astronomical Society,
    pp. 1–12, 2003.
  ista: Haiman Z, Holder GP. 2003. The reionization history at high redshifts. I.
    Physical models and new constraints from cosmic microwave background polarization.
    The Astrophysical Journal. 595(1), 1–12.
  mla: Haiman, Zoltán, and Gilbert P. Holder. “The Reionization History at High Redshifts.
    I. Physical Models and New Constraints from Cosmic Microwave Background Polarization.”
    <i>The Astrophysical Journal</i>, vol. 595, no. 1, American Astronomical Society,
    2003, pp. 1–12, doi:<a href="https://doi.org/10.1086/377337">10.1086/377337</a>.
  short: Z. Haiman, G.P. Holder, The Astrophysical Journal 595 (2003) 1–12.
date_created: 2024-09-06T09:42:24Z
date_published: 2003-09-20T00:00:00Z
date_updated: 2024-09-30T08:02:54Z
day: '20'
doi: 10.1086/377337
extern: '1'
fulldoi: https://doi.org/10.1086/377337
intvolume: '       595'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1086/377337
month: '09'
oa: 1
oa_version: Published Version
page: 1-12
publication: The Astrophysical Journal
publication_identifier:
  issn:
  - 0004-637X
  - 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: The reionization history at high redshifts. I. Physical models and new constraints
  from cosmic microwave background polarization
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 595
year: '2003'
...
---
_id: '17759'
abstract:
- lang: eng
  text: "The cosmic microwave background (CMB) has provided a precise template for
    features in the linear power spectrum: the matter-radiation turnover, sound horizon
    drop, and acoustic oscillations. In a two-dimensional power spectrum in redshift
    and angular space, the features appear as distorted rings, and yield simultaneous,
    purely geometric, measures of the Hubble parameter \U0001D43B⁡(\U0001D467) and
    angular diameter distance \U0001D437\U0001D434⁡(\U0001D467) via an absolute version
    of the Alcock-Paczynski test. Employing a simple Fisher matrix tool, we explore
    how future surveys can exploit these rings of power for dark energy studies. High-z
    CMB determinations of H and \U0001D437\U0001D434 are best complemented at moderate
    to low redshift (\U0001D467≲0.5) with a population of objects that are at least
    as abundant as clusters of galaxies. We find that a sample similar to that of
    the ongoing SDSS luminous red galaxy survey can achieve statistical errors at
    the ∼5% level for \U0001D437\U0001D434⁡(\U0001D467) and \U0001D43B⁡(\U0001D467)
    in several redshift bins. This, in turn, implies errors of \U0001D70E⁡(\U0001D464)=0.03–0.05
    for a constant dark energy equation of state in a flat universe. Deep galaxy cluster
    surveys such as the planned South Pole Telescope survey can extend this test out
    to \U0001D467∼1 or as far as redshift follow-up is available. We find that the
    expected constraints are at the \U0001D70E⁡(\U0001D464)=0.04–0.08 level, comparable
    to those of galaxies and complementary in redshift coverage."
article_number: '063004'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Wayne
  full_name: Hu, Wayne
  last_name: Hu
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: Hu W, Haiman Z. Redshifting rings of power. <i>Physical Review D</i>. 2003;68(6).
    doi:<a href="https://doi.org/10.1103/physrevd.68.063004">10.1103/physrevd.68.063004</a>
  apa: Hu, W., &#38; Haiman, Z. (2003). Redshifting rings of power. <i>Physical Review
    D</i>. American Physical Society. <a href="https://doi.org/10.1103/physrevd.68.063004">https://doi.org/10.1103/physrevd.68.063004</a>
  chicago: Hu, Wayne, and Zoltán Haiman. “Redshifting Rings of Power.” <i>Physical
    Review D</i>. American Physical Society, 2003. <a href="https://doi.org/10.1103/physrevd.68.063004">https://doi.org/10.1103/physrevd.68.063004</a>.
  ieee: W. Hu and Z. Haiman, “Redshifting rings of power,” <i>Physical Review D</i>,
    vol. 68, no. 6. American Physical Society, 2003.
  ista: Hu W, Haiman Z. 2003. Redshifting rings of power. Physical Review D. 68(6),
    063004.
  mla: Hu, Wayne, and Zoltán Haiman. “Redshifting Rings of Power.” <i>Physical Review
    D</i>, vol. 68, no. 6, 063004, American Physical Society, 2003, doi:<a href="https://doi.org/10.1103/physrevd.68.063004">10.1103/physrevd.68.063004</a>.
  short: W. Hu, Z. Haiman, Physical Review D 68 (2003).
date_created: 2024-09-06T09:46:11Z
date_published: 2003-09-29T00:00:00Z
date_updated: 2024-09-30T08:47:45Z
day: '29'
doi: 10.1103/physrevd.68.063004
extern: '1'
external_id:
  arxiv:
  - '0306053'
fulldoi: https://doi.org/10.1103/physrevd.68.063004
intvolume: '        68'
issue: '6'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: ' https://doi.org/10.48550/arXiv.astro-ph/0306053'
month: '09'
oa: 1
oa_version: Preprint
publication: Physical Review D
publication_identifier:
  issn:
  - 0556-2821
  - 1089-4918
publication_status: published
publisher: American Physical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Redshifting rings of power
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 68
year: '2003'
...
---
_id: '17760'
abstract:
- lang: eng
  text: In light of the recent inference of a high optical depth τ to Thomson scattering
    from the Wilkinson Microwave Anisotropy Probe (WMAP) data, we investigate the
    effects of extended periods of partial ionization and ask if the value of τ inferred
    by assuming a single sharp transition is an unbiased estimate. We construct and
    consider several representative ionization models and evaluate their signatures
    in the cosmic microwave background (CMB). If τ is estimated with a single sharp
    transition, we show that there can be a significant bias in the derived value
    (and, therefore, a bias in σ8 as well). For WMAP noise levels, the bias in τ is
    smaller than the statistical uncertainty, but for Planck or a cosmic variance
    limited experiment the τ bias could be much larger than the statistical uncertainties.
    This bias can be reduced in the ionization models we consider by fitting a slightly
    more complicated ionization history, such as a two-step ionization process. Assuming
    this two-step process, we find that the Planck satellite can simultaneously determine
    the initial redshift of reionization to ±2 and τ to ±0.01. Uncertainty about the
    ionization history appears to provide a limit of ~0.005 on how well τ can be estimated
    from CMB polarization data, much better than expected from WMAP but significantly
    worse than expected from cosmic variance limits.
article_processing_charge: No
article_type: original
author:
- first_name: Gilbert P.
  full_name: Holder, Gilbert P.
  last_name: Holder
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
- first_name: Manoj
  full_name: Kaplinghat, Manoj
  last_name: Kaplinghat
- first_name: Lloyd
  full_name: Knox, Lloyd
  last_name: Knox
citation:
  ama: Holder GP, Haiman Z, Kaplinghat M, Knox L. The reionization history at high
    redshifts. II. Estimating the optical depth to Thomson scattering from cosmic
    microwave background polarization. <i>The Astrophysical Journal</i>. 2003;595(1):13-18.
    doi:<a href="https://doi.org/10.1086/377338">10.1086/377338</a>
  apa: Holder, G. P., Haiman, Z., Kaplinghat, M., &#38; Knox, L. (2003). The reionization
    history at high redshifts. II. Estimating the optical depth to Thomson scattering
    from cosmic microwave background polarization. <i>The Astrophysical Journal</i>.
    American Astronomical Society. <a href="https://doi.org/10.1086/377338">https://doi.org/10.1086/377338</a>
  chicago: Holder, Gilbert P., Zoltán Haiman, Manoj Kaplinghat, and Lloyd Knox. “The
    Reionization History at High Redshifts. II. Estimating the Optical Depth to Thomson
    Scattering from Cosmic Microwave Background Polarization.” <i>The Astrophysical
    Journal</i>. American Astronomical Society, 2003. <a href="https://doi.org/10.1086/377338">https://doi.org/10.1086/377338</a>.
  ieee: G. P. Holder, Z. Haiman, M. Kaplinghat, and L. Knox, “The reionization history
    at high redshifts. II. Estimating the optical depth to Thomson scattering from
    cosmic microwave background polarization,” <i>The Astrophysical Journal</i>, vol.
    595, no. 1. American Astronomical Society, pp. 13–18, 2003.
  ista: Holder GP, Haiman Z, Kaplinghat M, Knox L. 2003. The reionization history
    at high redshifts. II. Estimating the optical depth to Thomson scattering from
    cosmic microwave background polarization. The Astrophysical Journal. 595(1), 13–18.
  mla: Holder, Gilbert P., et al. “The Reionization History at High Redshifts. II.
    Estimating the Optical Depth to Thomson Scattering from Cosmic Microwave Background
    Polarization.” <i>The Astrophysical Journal</i>, vol. 595, no. 1, American Astronomical
    Society, 2003, pp. 13–18, doi:<a href="https://doi.org/10.1086/377338">10.1086/377338</a>.
  short: G.P. Holder, Z. Haiman, M. Kaplinghat, L. Knox, The Astrophysical Journal
    595 (2003) 13–18.
date_created: 2024-09-06T09:47:55Z
date_published: 2003-09-20T00:00:00Z
date_updated: 2024-09-30T08:51:32Z
day: '20'
doi: 10.1086/377338
extern: '1'
fulldoi: https://doi.org/10.1086/377338
intvolume: '       595'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1086/377338
month: '09'
oa: 1
oa_version: Published Version
page: 13-18
publication: The Astrophysical Journal
publication_identifier:
  issn:
  - 0004-637X
  - 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: The reionization history at high redshifts. II. Estimating the optical depth
  to Thomson scattering from cosmic microwave background polarization
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 595
year: '2003'
...
---
_id: '17767'
abstract:
- lang: eng
  text: Galaxy cluster surveys provide a powerful means of studying the density and
    nature of the dark energy. The redshift distribution of detected clusters in a
    deep, large solid angle SZE or X-ray survey is highly sensitive to the dark energy
    equation of state. Accurate constraints at the 5% level on the dark energy equation
    of state require that systematic biases in the mass estimators must be controlled
    at better than the ∼10% level. Observed regularity in the cluster population and
    the availability of multiple, independent mass estimators suggests these precise
    measurements are possible. Using hydrodynamical simulations that include preheating,
    we show that the level of preheating required to explain local galaxy cluster
    structure has a dramatic effect on X-ray cluster surveys, but only a mild effect
    on SZE surveys. This suggests that SZE surveys may be optimal for cosmology while
    X-ray surveys are well suited for studies of the thermal history of the intracluster
    medium.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Joseph J
  full_name: Mohr, Joseph J
  last_name: Mohr
- first_name: Brian
  full_name: O'Shea, Brian
  last_name: O'Shea
- first_name: August E
  full_name: Evrard, August E
  last_name: Evrard
- first_name: John
  full_name: Bialek, John
  last_name: Bialek
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: Mohr JJ, O’Shea B, Evrard AE, Bialek J, Haiman Z. Studying dark energy with
    galaxy cluster surveys. <i>Nuclear Physics B - Proceedings Supplements</i>. 2003;124:63-67.
    doi:<a href="https://doi.org/10.1016/s0920-5632(03)02078-4">10.1016/s0920-5632(03)02078-4</a>
  apa: Mohr, J. J., O’Shea, B., Evrard, A. E., Bialek, J., &#38; Haiman, Z. (2003).
    Studying dark energy with galaxy cluster surveys. <i>Nuclear Physics B - Proceedings
    Supplements</i>. Elsevier BV. <a href="https://doi.org/10.1016/s0920-5632(03)02078-4">https://doi.org/10.1016/s0920-5632(03)02078-4</a>
  chicago: Mohr, Joseph J, Brian O’Shea, August E Evrard, John Bialek, and Zoltán
    Haiman. “Studying Dark Energy with Galaxy Cluster Surveys.” <i>Nuclear Physics
    B - Proceedings Supplements</i>. Elsevier BV, 2003. <a href="https://doi.org/10.1016/s0920-5632(03)02078-4">https://doi.org/10.1016/s0920-5632(03)02078-4</a>.
  ieee: J. J. Mohr, B. O’Shea, A. E. Evrard, J. Bialek, and Z. Haiman, “Studying dark
    energy with galaxy cluster surveys,” <i>Nuclear Physics B - Proceedings Supplements</i>,
    vol. 124. Elsevier BV, pp. 63–67, 2003.
  ista: Mohr JJ, O’Shea B, Evrard AE, Bialek J, Haiman Z. 2003. Studying dark energy
    with galaxy cluster surveys. Nuclear Physics B - Proceedings Supplements. 124,
    63–67.
  mla: Mohr, Joseph J., et al. “Studying Dark Energy with Galaxy Cluster Surveys.”
    <i>Nuclear Physics B - Proceedings Supplements</i>, vol. 124, Elsevier BV, 2003,
    pp. 63–67, doi:<a href="https://doi.org/10.1016/s0920-5632(03)02078-4">10.1016/s0920-5632(03)02078-4</a>.
  short: J.J. Mohr, B. O’Shea, A.E. Evrard, J. Bialek, Z. Haiman, Nuclear Physics
    B - Proceedings Supplements 124 (2003) 63–67.
date_created: 2024-09-06T09:54:30Z
date_published: 2003-07-01T00:00:00Z
date_updated: 2024-09-30T09:33:33Z
day: '01'
doi: 10.1016/s0920-5632(03)02078-4
extern: '1'
external_id:
  arxiv:
  - '0208102'
fulldoi: https://doi.org/10.1016/s0920-5632(03)02078-4
intvolume: '       124'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: ' https://doi.org/10.48550/arXiv.astro-ph/0208102'
month: '07'
oa: 1
oa_version: Preprint
page: 63-67
publication: Nuclear Physics B - Proceedings Supplements
publication_identifier:
  issn:
  - 0920-5632
publication_status: published
publisher: Elsevier BV
quality_controlled: '1'
scopus_import: '1'
status: public
title: Studying dark energy with galaxy cluster surveys
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 124
year: '2003'
...
---
_id: '17780'
abstract:
- lang: eng
  text: We study contributions from inhomogeneous (patchy) reionization to arcminute-scale
    (1000 < l < 10,000) cosmic microwave background (CMB) anisotropies. We show that
    inhomogeneities in the ionization fraction, rather than in the mean density, dominate
    both the temperature and the polarization power spectra. Depending on the ionization
    history and the clustering bias of the ionizing sources, we find that rms temperature
    fluctuations range from 2 to 8 μK and the corresponding values for polarization
    are over 2 orders of magnitude smaller. Reionization can significantly bias cosmological
    parameter estimates and degrade gravitational lensing potential reconstruction
    from temperature maps but not from polarization maps. We demonstrate that a simple
    modeling of the reionization temperature power spectrum may be sufficient to remove
    the parameter bias. The high-l temperature power spectrum will contain some limited
    information about the sources of reionization.
article_processing_charge: No
article_type: original
author:
- first_name: Mario G.
  full_name: Santos, Mario G.
  last_name: Santos
- first_name: Asantha
  full_name: Cooray, Asantha
  last_name: Cooray
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
- first_name: Lloyd
  full_name: Knox, Lloyd
  last_name: Knox
- first_name: Chung‐Pei
  full_name: Ma, Chung‐Pei
  last_name: Ma
citation:
  ama: Santos MG, Cooray A, Haiman Z, Knox L, Ma C. Small‐scale cosmic microwave background
    temperature and polarization anisotropies due to patchy reionization. <i>The Astrophysical
    Journal</i>. 2003;598(2):756-766. doi:<a href="https://doi.org/10.1086/378772">10.1086/378772</a>
  apa: Santos, M. G., Cooray, A., Haiman, Z., Knox, L., &#38; Ma, C. (2003). Small‐scale
    cosmic microwave background temperature and polarization anisotropies due to patchy
    reionization. <i>The Astrophysical Journal</i>. American Astronomical Society.
    <a href="https://doi.org/10.1086/378772">https://doi.org/10.1086/378772</a>
  chicago: Santos, Mario G., Asantha Cooray, Zoltán Haiman, Lloyd Knox, and Chung‐Pei
    Ma. “Small‐scale Cosmic Microwave Background Temperature and Polarization Anisotropies
    Due to Patchy Reionization.” <i>The Astrophysical Journal</i>. American Astronomical
    Society, 2003. <a href="https://doi.org/10.1086/378772">https://doi.org/10.1086/378772</a>.
  ieee: M. G. Santos, A. Cooray, Z. Haiman, L. Knox, and C. Ma, “Small‐scale cosmic
    microwave background temperature and polarization anisotropies due to patchy reionization,”
    <i>The Astrophysical Journal</i>, vol. 598, no. 2. American Astronomical Society,
    pp. 756–766, 2003.
  ista: Santos MG, Cooray A, Haiman Z, Knox L, Ma C. 2003. Small‐scale cosmic microwave
    background temperature and polarization anisotropies due to patchy reionization.
    The Astrophysical Journal. 598(2), 756–766.
  mla: Santos, Mario G., et al. “Small‐scale Cosmic Microwave Background Temperature
    and Polarization Anisotropies Due to Patchy Reionization.” <i>The Astrophysical
    Journal</i>, vol. 598, no. 2, American Astronomical Society, 2003, pp. 756–66,
    doi:<a href="https://doi.org/10.1086/378772">10.1086/378772</a>.
  short: M.G. Santos, A. Cooray, Z. Haiman, L. Knox, C. Ma, The Astrophysical Journal
    598 (2003) 756–766.
date_created: 2024-09-06T10:15:03Z
date_published: 2003-12-01T00:00:00Z
date_updated: 2024-09-30T12:07:47Z
day: '01'
doi: 10.1086/378772
extern: '1'
fulldoi: https://doi.org/10.1086/378772
intvolume: '       598'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1086/378772
month: '12'
oa: 1
oa_version: Published Version
page: 756-766
publication: The Astrophysical Journal
publication_identifier:
  issn:
  - 0004-637X
  - 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Small‐scale cosmic microwave background temperature and polarization anisotropies
  due to patchy reionization
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 598
year: '2003'
...
---
_id: '17796'
abstract:
- lang: eng
  text: 'The recent measurement by WMAP of a large electron-scattering optical depth
    τe = 0.17 ± 0.04 is consistent with a simple model of reionization in which the
    intergalactic medium (IGM) is ionized at redshift z ~ 15 and remains highly ionized
    thereafter. Here we show that existing measurements of the IGM temperature from
    the Lyα forest at z ~ 2-4 rule out this "vanilla" model. Under reasonable assumptions
    about the ionizing spectrum, as long as the universe is reionized before z = 10
    and remains highly ionized thereafter, the IGM reaches an asymptotic thermal state
    that is too cold compared to observations. To simultaneously satisfy the cosmic
    microwave background and Lyα forest constraints, the reionization history must
    be complex: reionization begins early at z ≳ 15, but there must have been significant
    (order-of-unity) changes in fractions of neutral hydrogen and/or helium at 6 <
    z < 10 and/or singly ionized helium at 4 < z < 10. We describe a physically motivated
    reionization model that satisfies all current observations. We also explore the
    impact of a stochastic reionization history and show that a late epoch of (He  →
    He ) reionization induces a significant scatter in the IGM temperature, but the
    scatter diminishes with time quickly. Finally, we provide an analytic formula
    for the thermal asymptote and discuss possible additional heating mechanisms that
    might evade our constraints.'
article_processing_charge: No
article_type: original
author:
- first_name: Lam
  full_name: Hui, Lam
  last_name: Hui
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
  orcid: 0000-0003-3633-5403
citation:
  ama: Hui L, Haiman Z. The thermal memory of reionization history. <i>The Astrophysical
    Journal</i>. 2003;596(1):9-18. doi:<a href="https://doi.org/10.1086/377229">10.1086/377229</a>
  apa: Hui, L., &#38; Haiman, Z. (2003). The thermal memory of reionization history.
    <i>The Astrophysical Journal</i>. American Astronomical Society. <a href="https://doi.org/10.1086/377229">https://doi.org/10.1086/377229</a>
  chicago: Hui, Lam, and Zoltán Haiman. “The Thermal Memory of Reionization History.”
    <i>The Astrophysical Journal</i>. American Astronomical Society, 2003. <a href="https://doi.org/10.1086/377229">https://doi.org/10.1086/377229</a>.
  ieee: L. Hui and Z. Haiman, “The thermal memory of reionization history,” <i>The
    Astrophysical Journal</i>, vol. 596, no. 1. American Astronomical Society, pp.
    9–18, 2003.
  ista: Hui L, Haiman Z. 2003. The thermal memory of reionization history. The Astrophysical
    Journal. 596(1), 9–18.
  mla: Hui, Lam, and Zoltán Haiman. “The Thermal Memory of Reionization History.”
    <i>The Astrophysical Journal</i>, vol. 596, no. 1, American Astronomical Society,
    2003, pp. 9–18, doi:<a href="https://doi.org/10.1086/377229">10.1086/377229</a>.
  short: L. Hui, Z. Haiman, The Astrophysical Journal 596 (2003) 9–18.
date_created: 2024-09-06T10:28:15Z
date_published: 2003-10-10T00:00:00Z
date_updated: 2024-10-02T06:44:28Z
day: '10'
doi: 10.1086/377229
extern: '1'
fulldoi: https://doi.org/10.1086/377229
intvolume: '       596'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1086/377229
month: '10'
oa: 1
oa_version: Published Version
page: 9-18
publication: The Astrophysical Journal
publication_identifier:
  eissn:
  - 1538-4357
  issn:
  - 0004-637X
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: The thermal memory of reionization history
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 596
year: '2003'
...
---
OA_place: repository
OA_type: free access
_id: '17800'
abstract:
- lang: eng
  text: 'Deep mid-infrared (MIR) observations could reveal a population of faint,
    high-redshift (z > 3), dusty starburst galaxies that are the progenitors of present-day
    spheroids or bulges and are beyond the reach of current instruments. We utilize
    a semianalytic galaxy formation scheme to find a range of models for the MIR galaxy
    counts, down to a flux level of a few nanojanskys. The models incorporate the
    formation of heavily dust-enshrouded stellar populations at high redshift and
    are consistent with existing observations, including faint counts at 1.6 μm in
    the NICMOS Hubble Deep Field, and the upper limit on the extragalactic MIR background
    from TeV gamma rays. Our models predict ~0.04-0.4 galaxies arcsec-2 at the threshold
    of 100 nJy at 6 μm, with a comparable or larger surface density at longer MIR
    wavelengths. We conclude that a significant new population of high-redshift galaxies
    could be detected by the James Webb Space Telescope. Such a population would constitute
    background noise for the Terrestrial Planet Finder (TPF) and could necessitate
    repeat observations: every TPF resolution element would have a chance of up to
    ~10% of being contaminated by a background galaxy.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
  orcid: 0000-0003-3633-5403
- first_name: David N.
  full_name: Spergel, David N.
  last_name: Spergel
- first_name: Edwin L.
  full_name: Turner, Edwin L.
  last_name: Turner
citation:
  ama: Haiman Z, Spergel DN, Turner EL. Predictions for the counts of faint, high‐redshift
    galaxies in the mid‐infrared. <i>The Astrophysical Journal</i>. 2003;585(2):630-637.
    doi:<a href="https://doi.org/10.1086/346201">10.1086/346201</a>
  apa: Haiman, Z., Spergel, D. N., &#38; Turner, E. L. (2003). Predictions for the
    counts of faint, high‐redshift galaxies in the mid‐infrared. <i>The Astrophysical
    Journal</i>. American Astronomical Society. <a href="https://doi.org/10.1086/346201">https://doi.org/10.1086/346201</a>
  chicago: Haiman, Zoltán, David N. Spergel, and Edwin L. Turner. “Predictions for
    the Counts of Faint, High‐redshift Galaxies in the Mid‐infrared.” <i>The Astrophysical
    Journal</i>. American Astronomical Society, 2003. <a href="https://doi.org/10.1086/346201">https://doi.org/10.1086/346201</a>.
  ieee: Z. Haiman, D. N. Spergel, and E. L. Turner, “Predictions for the counts of
    faint, high‐redshift galaxies in the mid‐infrared,” <i>The Astrophysical Journal</i>,
    vol. 585, no. 2. American Astronomical Society, pp. 630–637, 2003.
  ista: Haiman Z, Spergel DN, Turner EL. 2003. Predictions for the counts of faint,
    high‐redshift galaxies in the mid‐infrared. The Astrophysical Journal. 585(2),
    630–637.
  mla: Haiman, Zoltán, et al. “Predictions for the Counts of Faint, High‐redshift
    Galaxies in the Mid‐infrared.” <i>The Astrophysical Journal</i>, vol. 585, no.
    2, American Astronomical Society, 2003, pp. 630–37, doi:<a href="https://doi.org/10.1086/346201">10.1086/346201</a>.
  short: Z. Haiman, D.N. Spergel, E.L. Turner, The Astrophysical Journal 585 (2003)
    630–637.
date_created: 2024-09-06T10:40:05Z
date_published: 2003-03-10T00:00:00Z
date_updated: 2024-11-12T09:55:48Z
day: '10'
doi: 10.1086/346201
extern: '1'
external_id:
  arxiv:
  - astro-ph/0110226
fulldoi: https://doi.org/10.1086/346201
intvolume: '       585'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.48550/arXiv.astro-ph/0110226
month: '03'
oa: 1
oa_version: Preprint
page: 630-637
publication: The Astrophysical Journal
publication_identifier:
  eissn:
  - 1538-4357
  issn:
  - 0004-637X
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Predictions for the counts of faint, high‐redshift galaxies in the mid‐infrared
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 585
year: '2003'
...
---
OA_type: closed access
_id: '18324'
abstract:
- lang: eng
  text: We present a novel 3D face recognition approach based on geometric invariants
    introduced by Elad and Kimmel. The key idea of the proposed algorithm is a representation
    of the facial surface, invariant to isometric deformations, such as those resulting
    from different expressions and postures of the face. The obtained geometric invariants
    allow mapping 2D facial texture images into special images that incorporate the
    3D geometry of the face. These signature images are then decomposed into their
    principal components. The result is an efficient and accurate face recognition
    algorithm that is robust to facial expressions. We demonstrate the results of
    our method and compare it to existing 2D and 3D face recognition algorithms.
alternative_title:
- LNCS
article_processing_charge: No
author:
- first_name: Alexander
  full_name: Bronstein, Alexander
  id: 58f3726e-7cba-11ef-ad8b-e6e8cb3904e6
  last_name: Bronstein
  orcid: 0000-0001-9699-8730
- first_name: Michael M.
  full_name: Bronstein, Michael M.
  last_name: Bronstein
- first_name: Ron
  full_name: Kimmel, Ron
  last_name: Kimmel
citation:
  ama: 'Bronstein AM, Bronstein MM, Kimmel R. Expression-invariant 3D face recognition.
    In: <i>4th International Conference on Audio- and Video-Based Biometric Person
    Authentication</i>. Vol 2688. Springer Nature; 2003:62-70. doi:<a href="https://doi.org/10.1007/3-540-44887-x_8">10.1007/3-540-44887-x_8</a>'
  apa: 'Bronstein, A. M., Bronstein, M. M., &#38; Kimmel, R. (2003). Expression-invariant
    3D face recognition. In <i>4th International Conference on Audio- and Video-Based
    Biometric Person Authentication</i> (Vol. 2688, pp. 62–70). Guildford, United
    Kingdom: Springer Nature. <a href="https://doi.org/10.1007/3-540-44887-x_8">https://doi.org/10.1007/3-540-44887-x_8</a>'
  chicago: Bronstein, Alex M., Michael M. Bronstein, and Ron Kimmel. “Expression-Invariant
    3D Face Recognition.” In <i>4th International Conference on Audio- and Video-Based
    Biometric Person Authentication</i>, 2688:62–70. Springer Nature, 2003. <a href="https://doi.org/10.1007/3-540-44887-x_8">https://doi.org/10.1007/3-540-44887-x_8</a>.
  ieee: A. M. Bronstein, M. M. Bronstein, and R. Kimmel, “Expression-invariant 3D
    face recognition,” in <i>4th International Conference on Audio- and Video-Based
    Biometric Person Authentication</i>, Guildford, United Kingdom, 2003, vol. 2688,
    pp. 62–70.
  ista: 'Bronstein AM, Bronstein MM, Kimmel R. 2003. Expression-invariant 3D face
    recognition. 4th International Conference on Audio- and Video-Based Biometric
    Person Authentication. AVBPA: Conference on Audio- and Video-Based Biometric Person
    Authentication, LNCS, vol. 2688, 62–70.'
  mla: Bronstein, Alex M., et al. “Expression-Invariant 3D Face Recognition.” <i>4th
    International Conference on Audio- and Video-Based Biometric Person Authentication</i>,
    vol. 2688, Springer Nature, 2003, pp. 62–70, doi:<a href="https://doi.org/10.1007/3-540-44887-x_8">10.1007/3-540-44887-x_8</a>.
  short: A.M. Bronstein, M.M. Bronstein, R. Kimmel, in:, 4th International Conference
    on Audio- and Video-Based Biometric Person Authentication, Springer Nature, 2003,
    pp. 62–70.
conference:
  end_date: 2003-06-11
  location: Guildford, United Kingdom
  name: 'AVBPA: Conference on Audio- and Video-Based Biometric Person Authentication'
  start_date: 2003-06-09
date_created: 2024-10-15T11:20:53Z
date_published: 2003-01-01T00:00:00Z
date_updated: 2024-10-22T07:20:09Z
day: '01'
doi: 10.1007/3-540-44887-x_8
extern: '1'
fulldoi: https://doi.org/10.1007/3-540-44887-x_8
intvolume: '      2688'
language:
- iso: eng
month: '01'
oa_version: None
page: 62-70
publication: 4th International Conference on Audio- and Video-Based Biometric Person
  Authentication
publication_identifier:
  eisbn:
  - '9783540448877'
  eissn:
  - 1611-3349
  isbn:
  - '9783540403029'
  issn:
  - 0302-9743
publication_status: published
publisher: Springer Nature
quality_controlled: '1'
scopus_import: '1'
status: public
title: Expression-invariant 3D face recognition
type: conference
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 2688
year: '2003'
...
---
OA_type: closed access
_id: '18410'
abstract:
- lang: eng
  text: The authors consider detection of high-energy photons in positron emission
    tomography using thick scintillation crystals. Parallax effect and multiple Compton
    interactions in such crystals significantly reduce the accuracy of conventional
    detection methods. In order to estimate the photon line of flight based on photomultiplier
    responses, the authors use asymptotically optimal nonlinear techniques, implemented
    by feedforward and radial basis function neural networks. Incorporation of information
    about angles of incidence of photons significantly improves accuracy of estimation.
    The proposed estimators are fast enough to perform detection, using conventional
    computers. Monte Carlo simulation results show that their approach significantly
    outperforms the conventional Anger algorithm.
article_processing_charge: No
article_type: original
author:
- first_name: Alexander
  full_name: Bronstein, Alexander
  id: 58f3726e-7cba-11ef-ad8b-e6e8cb3904e6
  last_name: Bronstein
  orcid: 0000-0001-9699-8730
- first_name: M.M.
  full_name: Bronstein, M.M.
  last_name: Bronstein
- first_name: M.
  full_name: Zibulevsky, M.
  last_name: Zibulevsky
- first_name: Y.Y.
  full_name: Zeevi, Y.Y.
  last_name: Zeevi
citation:
  ama: Bronstein AM, Bronstein MM, Zibulevsky M, Zeevi YY. Optimal nonlinear line-of-flight
    estimation in positron emission tomography. <i>IEEE Transactions on Nuclear Science</i>.
    2003;50(3):421-426. doi:<a href="https://doi.org/10.1109/tns.2003.812434">10.1109/tns.2003.812434</a>
  apa: Bronstein, A. M., Bronstein, M. M., Zibulevsky, M., &#38; Zeevi, Y. Y. (2003).
    Optimal nonlinear line-of-flight estimation in positron emission tomography. <i>IEEE
    Transactions on Nuclear Science</i>. Institute of Electrical and Electronics Engineers.
    <a href="https://doi.org/10.1109/tns.2003.812434">https://doi.org/10.1109/tns.2003.812434</a>
  chicago: Bronstein, Alex M., M.M. Bronstein, M. Zibulevsky, and Y.Y. Zeevi. “Optimal
    Nonlinear Line-of-Flight Estimation in Positron Emission Tomography.” <i>IEEE
    Transactions on Nuclear Science</i>. Institute of Electrical and Electronics Engineers,
    2003. <a href="https://doi.org/10.1109/tns.2003.812434">https://doi.org/10.1109/tns.2003.812434</a>.
  ieee: A. M. Bronstein, M. M. Bronstein, M. Zibulevsky, and Y. Y. Zeevi, “Optimal
    nonlinear line-of-flight estimation in positron emission tomography,” <i>IEEE
    Transactions on Nuclear Science</i>, vol. 50, no. 3. Institute of Electrical and
    Electronics Engineers, pp. 421–426, 2003.
  ista: Bronstein AM, Bronstein MM, Zibulevsky M, Zeevi YY. 2003. Optimal nonlinear
    line-of-flight estimation in positron emission tomography. IEEE Transactions on
    Nuclear Science. 50(3), 421–426.
  mla: Bronstein, Alex M., et al. “Optimal Nonlinear Line-of-Flight Estimation in
    Positron Emission Tomography.” <i>IEEE Transactions on Nuclear Science</i>, vol.
    50, no. 3, Institute of Electrical and Electronics Engineers, 2003, pp. 421–26,
    doi:<a href="https://doi.org/10.1109/tns.2003.812434">10.1109/tns.2003.812434</a>.
  short: A.M. Bronstein, M.M. Bronstein, M. Zibulevsky, Y.Y. Zeevi, IEEE Transactions
    on Nuclear Science 50 (2003) 421–426.
date_created: 2024-10-15T11:20:54Z
date_published: 2003-06-30T00:00:00Z
date_updated: 2024-10-22T06:48:53Z
day: '30'
doi: 10.1109/tns.2003.812434
extern: '1'
fulldoi: https://doi.org/10.1109/tns.2003.812434
intvolume: '        50'
issue: '3'
language:
- iso: eng
month: '06'
oa_version: None
page: 421-426
publication: IEEE Transactions on Nuclear Science
publication_identifier:
  eissn:
  - 1558-1578
  issn:
  - 0018-9499
publication_status: published
publisher: Institute of Electrical and Electronics Engineers
quality_controlled: '1'
scopus_import: '1'
status: public
title: Optimal nonlinear line-of-flight estimation in positron emission tomography
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 50
year: '2003'
...
---
_id: '18428'
article_processing_charge: No
author:
- first_name: Alexander
  full_name: Bronstein, Alexander
  id: 58f3726e-7cba-11ef-ad8b-e6e8cb3904e6
  last_name: Bronstein
  orcid: 0000-0001-9699-8730
- first_name: Michael M.
  full_name: Bronstein, Michael M.
  last_name: Bronstein
- first_name: Michael
  full_name: Zibulevsky, Michael
  last_name: Zibulevsky
- first_name: Yehoshua Y.
  full_name: Zeevi, Yehoshua Y.
  last_name: Zeevi
citation:
  ama: 'Bronstein AM, Bronstein MM, Zibulevsky M, Zeevi YY. Separation of reflections
    via sparse ICA. In: Unser MA, Aldroubi A, Laine AF, eds. <i>SPIE Proceedings</i>.
    Vol 5207. SPIE; 2003:292-296. doi:<a href="https://doi.org/10.1117/12.505210">10.1117/12.505210</a>'
  apa: 'Bronstein, A. M., Bronstein, M. M., Zibulevsky, M., &#38; Zeevi, Y. Y. (2003).
    Separation of reflections via sparse ICA. In M. A. Unser, A. Aldroubi, &#38; A.
    F. Laine (Eds.), <i>SPIE Proceedings</i> (Vol. 5207, pp. 292–296). San Diego,
    CA, United States: SPIE. <a href="https://doi.org/10.1117/12.505210">https://doi.org/10.1117/12.505210</a>'
  chicago: Bronstein, Alex M., Michael M. Bronstein, Michael Zibulevsky, and Yehoshua
    Y. Zeevi. “Separation of Reflections via Sparse ICA.” In <i>SPIE Proceedings</i>,
    edited by Michael A. Unser, Akram Aldroubi, and Andrew F. Laine, 5207:292–96.
    SPIE, 2003. <a href="https://doi.org/10.1117/12.505210">https://doi.org/10.1117/12.505210</a>.
  ieee: A. M. Bronstein, M. M. Bronstein, M. Zibulevsky, and Y. Y. Zeevi, “Separation
    of reflections via sparse ICA,” in <i>SPIE Proceedings</i>, San Diego, CA, United
    States, 2003, vol. 5207, no. 1, pp. 292–296.
  ista: 'Bronstein AM, Bronstein MM, Zibulevsky M, Zeevi YY. 2003. Separation of reflections
    via sparse ICA. SPIE Proceedings. Wavelets: Applications in Signal and Image Processing
    X vol. 5207, 292–296.'
  mla: Bronstein, Alex M., et al. “Separation of Reflections via Sparse ICA.” <i>SPIE
    Proceedings</i>, edited by Michael A. Unser et al., vol. 5207, no. 1, SPIE, 2003,
    pp. 292–96, doi:<a href="https://doi.org/10.1117/12.505210">10.1117/12.505210</a>.
  short: A.M. Bronstein, M.M. Bronstein, M. Zibulevsky, Y.Y. Zeevi, in:, M.A. Unser,
    A. Aldroubi, A.F. Laine (Eds.), SPIE Proceedings, SPIE, 2003, pp. 292–296.
conference:
  end_date: 2003-08-08
  location: San Diego, CA, United States
  name: 'Wavelets: Applications in Signal and Image Processing X'
  start_date: 2003-08-04
date_created: 2024-10-15T11:20:55Z
date_published: 2003-11-13T00:00:00Z
date_updated: 2024-12-19T09:20:04Z
day: '13'
doi: 10.1117/12.505210
editor:
- first_name: Michael A.
  full_name: Unser, Michael A.
  last_name: Unser
- first_name: Akram
  full_name: Aldroubi, Akram
  last_name: Aldroubi
- first_name: Andrew F.
  full_name: Laine, Andrew F.
  last_name: Laine
extern: '1'
fulldoi: https://doi.org/10.1117/12.505210
intvolume: '      5207'
issue: '1'
language:
- iso: eng
month: '11'
oa_version: None
page: 292 - 296
publication: SPIE Proceedings
publication_identifier:
  eissn:
  - 1996-756X
  issn:
  - 0277-786X
publication_status: published
publisher: SPIE
quality_controlled: '1'
scopus_import: '1'
status: public
title: Separation of reflections via sparse ICA
type: conference
user_id: 3E5EF7F0-F248-11E8-B48F-1D18A9856A87
volume: 5207
year: '2003'
...