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