---
_id: '17655'
abstract:
- lang: eng
  text: We have developed a semi-analytic framework to model the large-scale evolution
    of the first Population III (Pop III) stars and the transition to metal-enriched
    star formation. Our model follows dark matter haloes from cosmological N-body
    simulations, utilizing their individual merger histories and three-dimensional
    positions, and applies physically motivated prescriptions for star formation and
    feedback from Lyman–Werner (LW) radiation, hydrogen ionizing radiation, and external
    metal enrichment due to supernovae winds. This method is intended to complement
    analytic studies, which do not include clustering or individual merger histories,
    and hydrodynamical cosmological simulations, which include detailed physics, but
    are computationally expensive and have limited dynamic range. Utilizing this technique,
    we compute the cumulative Pop III and metal-enriched star formation rate density
    (SFRD) as a function of redshift at z ≥ 20. We find that varying the model parameters
    leads to significant qualitative changes in the global star formation history.
    The Pop III star formation efficiency and the delay time between Pop III and subsequent
    metal-enriched star formation are found to have the largest impact. The effect
    of clustering (i.e. including the three-dimensional positions of individual haloes)
    on various feedback mechanisms is also investigated. The impact of clustering
    on LW and ionization feedback is found to be relatively mild in our fiducial model,
    but can be larger if external metal enrichment can promote metal-enriched star
    formation over large distances.
article_processing_charge: No
article_type: original
author:
- first_name: Eli
  full_name: Visbal, Eli
  last_name: Visbal
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
- first_name: Greg L
  full_name: Bryan, Greg L
  last_name: Bryan
citation:
  ama: Visbal E, Haiman Z, Bryan GL. Self-consistent semi-analytic models of the first
    stars. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;475(4):5246-5256.
    doi:<a href="https://doi.org/10.1093/mnras/sty142">10.1093/mnras/sty142</a>
  apa: Visbal, E., Haiman, Z., &#38; Bryan, G. L. (2018). Self-consistent semi-analytic
    models of the first stars. <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press. <a href="https://doi.org/10.1093/mnras/sty142">https://doi.org/10.1093/mnras/sty142</a>
  chicago: Visbal, Eli, Zoltán Haiman, and Greg L Bryan. “Self-Consistent Semi-Analytic
    Models of the First Stars.” <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press, 2018. <a href="https://doi.org/10.1093/mnras/sty142">https://doi.org/10.1093/mnras/sty142</a>.
  ieee: E. Visbal, Z. Haiman, and G. L. Bryan, “Self-consistent semi-analytic models
    of the first stars,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 475, no. 4. Oxford University Press, pp. 5246–5256, 2018.
  ista: Visbal E, Haiman Z, Bryan GL. 2018. Self-consistent semi-analytic models of
    the first stars. Monthly Notices of the Royal Astronomical Society. 475(4), 5246–5256.
  mla: Visbal, Eli, et al. “Self-Consistent Semi-Analytic Models of the First Stars.”
    <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 475, no. 4, Oxford
    University Press, 2018, pp. 5246–56, doi:<a href="https://doi.org/10.1093/mnras/sty142">10.1093/mnras/sty142</a>.
  short: E. Visbal, Z. Haiman, G.L. Bryan, Monthly Notices of the Royal Astronomical
    Society 475 (2018) 5246–5256.
date_created: 2024-09-06T07:33:13Z
date_published: 2018-01-17T00:00:00Z
date_updated: 2024-09-24T14:23:23Z
day: '17'
doi: 10.1093/mnras/sty142
extern: '1'
intvolume: '       475'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1093/mnras/sty142
month: '01'
oa: 1
oa_version: Published Version
page: 5246-5256
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Self-consistent semi-analytic models of the first stars
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 475
year: '2018'
...
---
_id: '17679'
abstract:
- lang: eng
  text: We study low-density axisymmetric accretion flows onto black holes (BHs) with
    two-dimensional hydrodynamical simulations, adopting the α-viscosity prescription.
    When the gas angular momentum is low enough to form a rotationally supported disk
    within the Bondi radius (RB), we find a global steady accretion solution. The
    solution consists of a rotational equilibrium distribution at r∼RB, where the
    density follows ρ∝(1+RB/r)^3/2, surrounding a geometrically thick and optically
    thin accretion disk at the centrifugal radius, where thermal energy generated
    by viscosity is transported via strong convection. Physical properties of the
    inner solution agree with those expected in convection-dominated accretion flows
    (CDAF; ρ∝r^−1/2). In the inner CDAF solution, the gas inflow rate decreases towards
    the center due to convection (M˙∝r), and the net accretion rate (including both
    inflows and outflows) is strongly suppressed by several orders of magnitude from
    the Bondi accretion rate M˙B The net accretion rate depends on the viscous strength,
    following M˙/M˙B∝(α/0.01)^0.6. This solution holds for low accretion rates of
    M˙B/M˙Edd<10^−3 having minimal radiation cooling, where M˙Edd is the Eddington
    rate. In a hot plasma at the bottom (r<10^−3 RB), thermal conduction would dominate
    the convective energy flux. Since suppression of the accretion by convection ceases,
    the final BH feeding rate is found to be M˙/M˙B∼10^−3−10^−2. This rate is as low
    as M˙/M˙Edd∼10^−7−10^−6 inferred for SgrA∗ and the nuclear BHs in M31 and M87,
    and can explain the low luminosities in these sources, without invoking any feedback
    mechanism.
article_processing_charge: No
article_type: original
author:
- first_name: Kohei
  full_name: Inayoshi, Kohei
  last_name: Inayoshi
- first_name: Jeremiah P
  full_name: Ostriker, Jeremiah P
  last_name: Ostriker
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
- first_name: Rolf
  full_name: Kuiper, Rolf
  last_name: Kuiper
citation:
  ama: Inayoshi K, Ostriker JP, Haiman Z, Kuiper R. Low-density, radiatively inefficient
    rotating-accretion flow on to a black hole. <i>Monthly Notices of the Royal Astronomical
    Society</i>. 2018;476(1):1412-1426. doi:<a href="https://doi.org/10.1093/mnras/sty276">10.1093/mnras/sty276</a>
  apa: Inayoshi, K., Ostriker, J. P., Haiman, Z., &#38; Kuiper, R. (2018). Low-density,
    radiatively inefficient rotating-accretion flow on to a black hole. <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/sty276">https://doi.org/10.1093/mnras/sty276</a>
  chicago: Inayoshi, Kohei, Jeremiah P Ostriker, Zoltán Haiman, and Rolf Kuiper. “Low-Density,
    Radiatively Inefficient Rotating-Accretion Flow on to a Black Hole.” <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018.
    <a href="https://doi.org/10.1093/mnras/sty276">https://doi.org/10.1093/mnras/sty276</a>.
  ieee: K. Inayoshi, J. P. Ostriker, Z. Haiman, and R. Kuiper, “Low-density, radiatively
    inefficient rotating-accretion flow on to a black hole,” <i>Monthly Notices of
    the Royal Astronomical Society</i>, vol. 476, no. 1. Oxford University Press,
    pp. 1412–1426, 2018.
  ista: Inayoshi K, Ostriker JP, Haiman Z, Kuiper R. 2018. Low-density, radiatively
    inefficient rotating-accretion flow on to a black hole. Monthly Notices of the
    Royal Astronomical Society. 476(1), 1412–1426.
  mla: Inayoshi, Kohei, et al. “Low-Density, Radiatively Inefficient Rotating-Accretion
    Flow on to a Black Hole.” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 476, no. 1, Oxford University Press, 2018, pp. 1412–26, doi:<a href="https://doi.org/10.1093/mnras/sty276">10.1093/mnras/sty276</a>.
  short: K. Inayoshi, J.P. Ostriker, Z. Haiman, R. Kuiper, Monthly Notices of the
    Royal Astronomical Society 476 (2018) 1412–1426.
date_created: 2024-09-06T08:05:18Z
date_published: 2018-02-01T00:00:00Z
date_updated: 2024-09-25T08:57:35Z
day: '01'
doi: 10.1093/mnras/sty276
extern: '1'
intvolume: '       476'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1093/mnras/sty276
month: '02'
oa: 1
oa_version: Published Version
page: 1412-1426
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Low-density, radiatively inefficient rotating-accretion flow on to a black
  hole
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 476
year: '2018'
...
---
_id: '17687'
abstract:
- lang: eng
  text: We propose the formation of massive pristine dark-matter (DM) halos with masses
    of ∼10^8 M⊙, due to the dynamical effects of frequent mergers in rare regions
    of the Universe with high baryonic streaming velocity relative to DM. Since the
    streaming motion prevents gas collapse into DM halos and delays prior star formation
    episodes, the gas remains metal-free until the halo virial temperatures ≳2×10^4
    K. The minimum cooling mass of DM halos is boosted by a factor of ∼10−30 because
    frequent major mergers of halos further inhibit gas collapse. We use Monte Carlo
    merger trees to simulate the DM assembly history under a streaming velocity of
    twice the root-mean-square value, and estimate the number density of massive DM
    halos containing pristine gas as ≃10^−4 cMpc^−3. When the gas infall begins, efficient
    Lyα cooling drives cold streams penetrating inside the halo and feeding a central
    galactic disk. When one stream collides with the disk, strong shock forms a dense
    and hot gas cloud, where the gas never forms H2 molecules due to effective collisional
    dissociation. As a result, a massive gas cloud forms by gravitational instability
    and collapses directly into a massive black hole (BH) with M∙∼10^5 M⊙. Almost
    simultaneously, a galaxy with M⋆,tot∼10^6 M⊙ composed of Population III stars
    forms in the nuclear region. If the typical stellar mass is as high as ∼100 M⊙,
    the galaxy could be detected with the James Webb Space Telescope even at z≳15.
    These massive seed BHs would be fed by continuous gas accretion from the host
    galaxy, and grow to be bright quasars observed at z≳6.
article_processing_charge: No
article_type: original
author:
- first_name: Kohei
  full_name: Inayoshi, Kohei
  last_name: Inayoshi
- first_name: Miao
  full_name: Li, Miao
  last_name: Li
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: Inayoshi K, Li M, Haiman Z. Massive black hole and Population III galaxy formation
    in overmassive dark-matter haloes with violent merger histories. <i>Monthly Notices
    of the Royal Astronomical Society</i>. 2018;479(3):4017-4027. doi:<a href="https://doi.org/10.1093/mnras/sty1720">10.1093/mnras/sty1720</a>
  apa: Inayoshi, K., Li, M., &#38; Haiman, Z. (2018). Massive black hole and Population
    III galaxy formation in overmassive dark-matter haloes with violent merger histories.
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press.
    <a href="https://doi.org/10.1093/mnras/sty1720">https://doi.org/10.1093/mnras/sty1720</a>
  chicago: Inayoshi, Kohei, Miao Li, and Zoltán Haiman. “Massive Black Hole and Population
    III Galaxy Formation in Overmassive Dark-Matter Haloes with Violent Merger Histories.”
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press,
    2018. <a href="https://doi.org/10.1093/mnras/sty1720">https://doi.org/10.1093/mnras/sty1720</a>.
  ieee: K. Inayoshi, M. Li, and Z. Haiman, “Massive black hole and Population III
    galaxy formation in overmassive dark-matter haloes with violent merger histories,”
    <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 479, no. 3. Oxford
    University Press, pp. 4017–4027, 2018.
  ista: Inayoshi K, Li M, Haiman Z. 2018. Massive black hole and Population III galaxy
    formation in overmassive dark-matter haloes with violent merger histories. Monthly
    Notices of the Royal Astronomical Society. 479(3), 4017–4027.
  mla: Inayoshi, Kohei, et al. “Massive Black Hole and Population III Galaxy Formation
    in Overmassive Dark-Matter Haloes with Violent Merger Histories.” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 479, no. 3, Oxford University Press,
    2018, pp. 4017–27, doi:<a href="https://doi.org/10.1093/mnras/sty1720">10.1093/mnras/sty1720</a>.
  short: K. Inayoshi, M. Li, Z. Haiman, Monthly Notices of the Royal Astronomical
    Society 479 (2018) 4017–4027.
date_created: 2024-09-06T08:22:23Z
date_published: 2018-06-30T00:00:00Z
date_updated: 2024-09-25T09:46:30Z
day: '30'
doi: 10.1093/mnras/sty1720
extern: '1'
intvolume: '       479'
issue: '3'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1093/mnras/sty1720
month: '06'
oa: 1
oa_version: Published Version
page: 4017-4027
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Massive black hole and Population III galaxy formation in overmassive dark-matter
  haloes with violent merger histories
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 479
year: '2018'
...
---
_id: '17691'
abstract:
- lang: eng
  text: Supermassive black hole binaries (SMBHBs) should be common in galactic nuclei
    as a result of frequent galaxy mergers. Recently, a large sample of sub-parsec
    SMBHB candidates was identified as bright periodically variable quasars in optical
    surveys. If the observed periodicity corresponds to the redshifted binary orbital
    period, the inferred orbital velocities are relativistic (v/c ≈ 0.1). The optical
    and ultraviolet (UV) luminosities are expected to arise from gas bound to the
    individual BHs, and would be modulated by the relativistic Doppler effect. The
    optical and UV light curves should vary in tandem with relative amplitudes which
    depend on the respective spectral slopes. We constructed a control sample of 42
    quasars with aperiodic variability, to test whether this Doppler colour signature
    can be distinguished from intrinsic chromatic variability. We found that the Doppler
    signature can arise by chance in ∼20 per cent (∼37 per cent) of quasars in the
    nUV (fUV) band. These probabilities reflect the limited quality of the control
    sample and represent upper limits on how frequently quasars mimic the Doppler
    brightness+colour variations. We performed separate tests on the periodic quasar
    candidates, and found that for the majority, the Doppler boost hypothesis requires
    an unusually steep UV spectrum or an unexpectedly large BH mass and orbital velocity.
    We conclude that at most approximately one-third of these periodic candidates
    can harbor Doppler-modulated SMBHBs.
article_processing_charge: No
article_type: original
author:
- first_name: Maria
  full_name: Charisi, Maria
  last_name: Charisi
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
- first_name: David
  full_name: Schiminovich, David
  last_name: Schiminovich
- first_name: Daniel J
  full_name: D'Orazio, Daniel J
  last_name: D'Orazio
citation:
  ama: Charisi M, Haiman Z, Schiminovich D, D’Orazio DJ. Testing the relativistic
    Doppler boost hypothesis for supermassive black hole binary candidates. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2018;476(4):4617-4628. doi:<a href="https://doi.org/10.1093/mnras/sty516">10.1093/mnras/sty516</a>
  apa: Charisi, M., Haiman, Z., Schiminovich, D., &#38; D’Orazio, D. J. (2018). Testing
    the relativistic Doppler boost hypothesis for supermassive black hole binary candidates.
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press.
    <a href="https://doi.org/10.1093/mnras/sty516">https://doi.org/10.1093/mnras/sty516</a>
  chicago: Charisi, Maria, Zoltán Haiman, David Schiminovich, and Daniel J D’Orazio.
    “Testing the Relativistic Doppler Boost Hypothesis for Supermassive Black Hole
    Binary Candidates.” <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press, 2018. <a href="https://doi.org/10.1093/mnras/sty516">https://doi.org/10.1093/mnras/sty516</a>.
  ieee: M. Charisi, Z. Haiman, D. Schiminovich, and D. J. D’Orazio, “Testing the relativistic
    Doppler boost hypothesis for supermassive black hole binary candidates,” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 476, no. 4. Oxford University
    Press, pp. 4617–4628, 2018.
  ista: Charisi M, Haiman Z, Schiminovich D, D’Orazio DJ. 2018. Testing the relativistic
    Doppler boost hypothesis for supermassive black hole binary candidates. Monthly
    Notices of the Royal Astronomical Society. 476(4), 4617–4628.
  mla: Charisi, Maria, et al. “Testing the Relativistic Doppler Boost Hypothesis for
    Supermassive Black Hole Binary Candidates.” <i>Monthly Notices of the Royal Astronomical
    Society</i>, vol. 476, no. 4, Oxford University Press, 2018, pp. 4617–28, doi:<a
    href="https://doi.org/10.1093/mnras/sty516">10.1093/mnras/sty516</a>.
  short: M. Charisi, Z. Haiman, D. Schiminovich, D.J. D’Orazio, Monthly Notices of
    the Royal Astronomical Society 476 (2018) 4617–4628.
date_created: 2024-09-06T08:38:11Z
date_published: 2018-02-28T00:00:00Z
date_updated: 2024-09-25T09:56:16Z
day: '28'
doi: 10.1093/mnras/sty516
extern: '1'
intvolume: '       476'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1093/mnras/sty516
month: '02'
oa: 1
oa_version: Published Version
page: 4617-4628
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Testing the relativistic Doppler boost hypothesis for supermassive black hole
  binary candidates
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 476
year: '2018'
...
---
_id: '11561'
abstract:
- lang: eng
  text: We present a sample of ∼1000 emission-line galaxies at z = 0.4–4.7 from the
    ∼0.7deg2 High-z Emission-Line Survey in the Boötes field identified with a suite
    of six narrow-band filters at ≈0.4–2.1 μm. These galaxies have been selected on
    their Ly α (73), [O II] (285), H β/[O III] (387) or H α (362) emission line, and
    have been classified with optical to near-infrared colours. A subsample of 98
    sources have reliable redshifts from multiple narrow-band (e.g. [O II]–H α) detections
    and/or spectroscopy. In this survey paper, we present the observations, selection
    and catalogues of emitters. We measure number densities of Ly α, [O II], H β/[O III]
    and H α and confirm strong luminosity evolution in star-forming galaxies from
    z ∼ 0.4 to ∼5, in agreement with previous results. To demonstrate the usefulness
    of dual-line emitters, we use the sample of dual [O II]–H α emitters to measure
    the observed [O II]/H α ratio at z = 1.47. The observed [O II]/H α ratio increases
    significantly from 0.40 ± 0.01 at z = 0.1 to 0.52 ± 0.05 at z = 1.47, which we
    attribute to either decreasing dust attenuation with redshift, or due to a bias
    in the (typically) fibre measurements in the local Universe that only measure
    the central kpc regions. At the bright end, we find that both the H α and Ly α
    number densities at z ≈ 2.2 deviate significantly from a Schechter form, following
    a power law. We show that this is driven entirely by an increasing X-ray/active
    galactic nucleus fraction with line luminosity, which reaches ≈100 per cent at
    line luminosities L ≳ 3 × 1044 erg s−1.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Philip
  full_name: Best, Philip
  last_name: Best
- first_name: Ian
  full_name: Smail, Ian
  last_name: Smail
- first_name: Fuyan
  full_name: Bian, Fuyan
  last_name: Bian
- first_name: Behnam
  full_name: Darvish, Behnam
  last_name: Darvish
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
- first_name: Xiaohui
  full_name: Fan, Xiaohui
  last_name: Fan
citation:
  ama: 'Matthee JJ, Sobral D, Best P, et al. Boötes-HiZELS: An optical to near-infrared
    survey of emission-line galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal
    Astronomical Society</i>. 2017;471(1):629-649. doi:<a href="https://doi.org/10.1093/mnras/stx1569">10.1093/mnras/stx1569</a>'
  apa: 'Matthee, J. J., Sobral, D., Best, P., Smail, I., Bian, F., Darvish, B., …
    Fan, X. (2017). Boötes-HiZELS: An optical to near-infrared survey of emission-line
    galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx1569">https://doi.org/10.1093/mnras/stx1569</a>'
  chicago: 'Matthee, Jorryt J, David Sobral, Philip Best, Ian Smail, Fuyan Bian, Behnam
    Darvish, Huub Röttgering, and Xiaohui Fan. “Boötes-HiZELS: An Optical to near-Infrared
    Survey of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal
    Astronomical Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx1569">https://doi.org/10.1093/mnras/stx1569</a>.'
  ieee: 'J. J. Matthee <i>et al.</i>, “Boötes-HiZELS: An optical to near-infrared
    survey of emission-line galaxies at z = 0.4–4.7,” <i>Monthly Notices of the Royal
    Astronomical Society</i>, vol. 471, no. 1. Oxford University Press, pp. 629–649,
    2017.'
  ista: 'Matthee JJ, Sobral D, Best P, Smail I, Bian F, Darvish B, Röttgering H, Fan
    X. 2017. Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies
    at z = 0.4–4.7. Monthly Notices of the Royal Astronomical Society. 471(1), 629–649.'
  mla: 'Matthee, Jorryt J., et al. “Boötes-HiZELS: An Optical to near-Infrared Survey
    of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal Astronomical
    Society</i>, vol. 471, no. 1, Oxford University Press, 2017, pp. 629–49, doi:<a
    href="https://doi.org/10.1093/mnras/stx1569">10.1093/mnras/stx1569</a>.'
  short: J.J. Matthee, D. Sobral, P. Best, I. Smail, F. Bian, B. Darvish, H. Röttgering,
    X. Fan, Monthly Notices of the Royal Astronomical Society 471 (2017) 629–649.
date_created: 2022-07-12T11:01:35Z
date_published: 2017-10-01T00:00:00Z
date_updated: 2024-10-14T11:34:07Z
day: '01'
doi: 10.1093/mnras/stx1569
extern: '1'
external_id:
  arxiv:
  - '1702.04721'
intvolume: '       471'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics galaxies
- active
- galaxies
- evolution
- galaxies
- high-redshift
- galaxies
- luminosity function
- mass function
- 'galaxies: star formation'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1702.04721
month: '10'
oa: 1
oa_version: Preprint
page: 629-649
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies
  at z = 0.4–4.7'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_id: '11562'
abstract:
- lang: eng
  text: We present the CAlibrating LYMan-α with Hα (CALYMHA) pilot survey and new
    results on Lyman α (Lyα) selected galaxies at z ∼ 2. We use a custom-built Lyα
    narrow-band filter at the Isaac Newton Telescope, designed to provide a matched
    volume coverage to the z = 2.23 Hα HiZELS survey. Here, we present the first results
    for the COSMOS and UDS fields. Our survey currently reaches a 3σ line flux limit
    of ∼4 × 10−17 erg s−1 cm−2, and a Lyα luminosity limit of ∼1042.3 erg s−1. We
    find 188 Lyα emitters over 7.3 × 105 Mpc3, but also find significant numbers of
    other line-emitting sources corresponding to He II, C III] and C IV emission lines.
    These sources are important contaminants, and we carefully remove them, unlike
    most previous studies. We find that the Lyα luminosity function at z = 2.23 is
    very well described by a Schechter function up to LLy α ≈ 1043 erg s−1 with L∗=1042.59+0.16−0.08
    erg s−1, ϕ∗=10−3.09+0.14−0.34 Mpc−3 and α = −1.75 ± 0.25. Above LLy α ≈ 1043 erg
    s−1, the Lyα luminosity function becomes power-law like, driven by X-ray AGN.
    We find that Lyα-selected emitters have a high escape fraction of 37 ± 7 per cent,
    anticorrelated with Lyα luminosity and correlated with Lyα equivalent width. Lyα
    emitters have ubiquitous large (≈40 kpc) Lyα haloes, ∼2 times larger than their
    Hα extents. By directly comparing our Lyα and Hα luminosity functions, we find
    that the global/overall escape fraction of Lyα photons (within a 13 kpc radius)
    from the full population of star-forming galaxies is 5.1 ± 0.2 per cent at the
    peak of the star formation history. An extra 3.3 ± 0.3 per cent of Lyα photons
    likely still escape, but at larger radii.
acknowledgement: 'We thank the reviewer for his/her helpful comments and suggestions
  that have greatly improved this work. DS and JM acknowledge financial support from
  the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship.
  DS also acknowledges funding from FCT through an FCT Investigator Starting Grant
  and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from
  the UK STFC via grant ST/M001229/1. IRS acknowledges support from STFC (ST/L00075X/1),
  the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson
  merit award. We thank Matthew Hayes, Ryan Trainor, Kimihiko Nakajima and Anne Verhamme
  for many helpful discussions and Ana Sobral, Carolina Duarte and Miguel Domingos
  for taking part in observations with the NB392 filter. We also thank Sergio Santos
  for helpful comments. This research is based on observations obtained on the Isaac
  Newton Telescope (INT), programs: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B
  & I15AN008. The authors acknowledge the award of time from programmes: I13AN002,
  I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008 on the INT. INT is operated
  on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio
  del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. Based on
  observations made with ESO Telescopes at the La Silla Paranal Observatory under
  programme ID 098.A 0819. We have benefited greatly from the publicly available programming
  language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages,
  the astronomical imaging tools SEXTRACTOR, SWARP (Bertin & Arnouts 1996; Bertin
  2010), SCAMP (Bertin 2006) and TOPCAT (Taylor 2005). Dedicated to the memory of
  M. L. Nicolau and M. C. Serrano.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: Philip
  full_name: Best, Philip
  last_name: Best
- first_name: Andra
  full_name: Stroe, Andra
  last_name: Stroe
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
- first_name: Iván
  full_name: Oteo, Iván
  last_name: Oteo
- first_name: Ian
  full_name: Smail, Ian
  last_name: Smail
- first_name: Leah
  full_name: Morabito, Leah
  last_name: Morabito
- first_name: Ana
  full_name: Paulino-Afonso, Ana
  last_name: Paulino-Afonso
citation:
  ama: 'Sobral D, Matthee JJ, Best P, et al. The CALYMHA survey: Lyα luminosity function
    and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the
    Royal Astronomical Society</i>. 2017;466(1):1242-1258. doi:<a href="https://doi.org/10.1093/mnras/stw3090">10.1093/mnras/stw3090</a>'
  apa: 'Sobral, D., Matthee, J. J., Best, P., Stroe, A., Röttgering, H., Oteo, I.,
    … Paulino-Afonso, A. (2017). The CALYMHA survey: Lyα luminosity function and global
    escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stw3090">https://doi.org/10.1093/mnras/stw3090</a>'
  chicago: 'Sobral, David, Jorryt J Matthee, Philip Best, Andra Stroe, Huub Röttgering,
    Iván Oteo, Ian Smail, Leah Morabito, and Ana Paulino-Afonso. “The CALYMHA Survey:
    Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.”
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press,
    2017. <a href="https://doi.org/10.1093/mnras/stw3090">https://doi.org/10.1093/mnras/stw3090</a>.'
  ieee: 'D. Sobral <i>et al.</i>, “The CALYMHA survey: Lyα luminosity function and
    global escape fraction of Lyα photons at z = 2.23,” <i>Monthly Notices of the
    Royal Astronomical Society</i>, vol. 466, no. 1. Oxford University Press, pp.
    1242–1258, 2017.'
  ista: 'Sobral D, Matthee JJ, Best P, Stroe A, Röttgering H, Oteo I, Smail I, Morabito
    L, Paulino-Afonso A. 2017. The CALYMHA survey: Lyα luminosity function and global
    escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical
    Society. 466(1), 1242–1258.'
  mla: 'Sobral, David, et al. “The CALYMHA Survey: Lyα Luminosity Function and Global
    Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical
    Society</i>, vol. 466, no. 1, Oxford University Press, 2017, pp. 1242–58, doi:<a
    href="https://doi.org/10.1093/mnras/stw3090">10.1093/mnras/stw3090</a>.'
  short: D. Sobral, J.J. Matthee, P. Best, A. Stroe, H. Röttgering, I. Oteo, I. Smail,
    L. Morabito, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society
    466 (2017) 1242–1258.
date_created: 2022-07-12T12:04:16Z
date_published: 2017-04-01T00:00:00Z
date_updated: 2024-10-14T11:35:37Z
day: '01'
doi: 10.1093/mnras/stw3090
extern: '1'
external_id:
  arxiv:
  - '1609.05897'
intvolume: '       466'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: haloes'
- 'galaxies: high-redshift'
- 'galaxies: luminosity function'
- mass function
- 'galaxies: statistics'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1609.05897
month: '04'
oa: 1
oa_version: Preprint
page: 1242-1258
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The CALYMHA survey: Lyα luminosity function and global escape fraction of
  Lyα photons at z = 2.23'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 466
year: '2017'
...
---
_id: '11564'
abstract:
- lang: eng
  text: We study the production rate of ionizing photons of a sample of 588 Hα emitters
    (HAEs) and 160 Lyman-α emitters (LAEs) at z = 2.2 in the COSMOS field in order
    to assess the implied emissivity from galaxies, based on their ultraviolet (UV)
    luminosity. By exploring the rest-frame Lyman Continuum (LyC) with GALEX/NUV data,
    we find fesc < 2.8 (6.4) per cent through median (mean) stacking. By combining
    the Hα luminosity density with intergalactic medium emissivity measurements from
    absorption studies, we find a globally averaged 〈fesc〉 of 5.9+14.5−4.2 per cent
    at z = 2.2 if we assume HAEs are the only source of ionizing photons. We find
    similarly low values of the global 〈fesc〉 at z ≈ 3–5, also ruling out a high 〈fesc〉
    at z < 5. These low escape fractions allow us to measure ξion, the number of produced
    ionizing photons per unit UV luminosity, and investigate how this depends on galaxy
    properties. We find a typical ξion ≈ 1024.77 ± 0.04 Hz erg−1 for HAEs and ξion
    ≈ 1025.14 ± 0.09 Hz erg−1 for LAEs. LAEs and low-mass HAEs at z = 2.2 show similar
    values of ξion as typically assumed in the reionization era, while the typical
    HAE is three times less ionizing. Due to an increasing ξion with increasing EW(Hα),
    ξion likely increases with redshift. This evolution alone is fully in line with
    the observed evolution of ξion between z ≈ 2 and 5, indicating a typical value
    of ξion ≈ 1025.4 Hz erg−1 in the reionization era.
acknowledgement: "We thank the referee for the many helpful and constructive comments
  which have significantly improved this paper. JM acknowledges the support of a Huygens
  PhD fellowship from Leiden University. DS acknowledges financial support from the
  Netherlands Organization for Scientific research (NWO) through a Veni fellowship
  and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010).
  PNB is grateful for support from the UK STFC via grant ST/M001229/1. IO acknowledges
  support from the European Research Council in the form of the Advanced Investigator
  Programme, 321302, COSMICISM. The authors thank Andreas Faisst, Michael Rutkowski
  and Andreas Sandberg for answering questions related to this work and Daniel Schaerer
  and Mark Dijkstra for discussions. We acknowledge the work that has been done by
  both the COSMOS team in assembling such large, state-of-the-art multi-wavelength
  data set, as this has been crucial for the results presented in this paper. We have
  benefited greatly from the public available programming language PYTHON, including
  the NUMPY, MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt,
  Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages,
  the astronomical imaging tools SEXTRACTOR and SWARP (Bertin & Arnouts 1996;\r\nBertin
  2010) and the TOPCAT analysis program (Taylor 2013)."
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Philip
  full_name: Best, Philip
  last_name: Best
- first_name: Ali Ahmad
  full_name: Khostovan, Ali Ahmad
  last_name: Khostovan
- first_name: Iván
  full_name: Oteo, Iván
  last_name: Oteo
- first_name: Rychard
  full_name: Bouwens, Rychard
  last_name: Bouwens
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
citation:
  ama: Matthee JJ, Sobral D, Best P, et al. The production and escape of Lyman-Continuum
    radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2017;465(3):3637-3655. doi:<a href="https://doi.org/10.1093/mnras/stw2973">10.1093/mnras/stw2973</a>
  apa: Matthee, J. J., Sobral, D., Best, P., Khostovan, A. A., Oteo, I., Bouwens,
    R., &#38; Röttgering, H. (2017). The production and escape of Lyman-Continuum
    radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stw2973">https://doi.org/10.1093/mnras/stw2973</a>
  chicago: Matthee, Jorryt J, David Sobral, Philip Best, Ali Ahmad Khostovan, Iván
    Oteo, Rychard Bouwens, and Huub Röttgering. “The Production and Escape of Lyman-Continuum
    Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017.
    <a href="https://doi.org/10.1093/mnras/stw2973">https://doi.org/10.1093/mnras/stw2973</a>.
  ieee: J. J. Matthee <i>et al.</i>, “The production and escape of Lyman-Continuum
    radiation from star-forming galaxies at z ∼ 2 and their redshift evolution,” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 465, no. 3. Oxford University
    Press, pp. 3637–3655, 2017.
  ista: Matthee JJ, Sobral D, Best P, Khostovan AA, Oteo I, Bouwens R, Röttgering
    H. 2017. The production and escape of Lyman-Continuum radiation from star-forming
    galaxies at z ∼ 2 and their redshift evolution. Monthly Notices of the Royal Astronomical
    Society. 465(3), 3637–3655.
  mla: Matthee, Jorryt J., et al. “The Production and Escape of Lyman-Continuum Radiation
    from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 465, no. 3, Oxford University
    Press, 2017, pp. 3637–55, doi:<a href="https://doi.org/10.1093/mnras/stw2973">10.1093/mnras/stw2973</a>.
  short: J.J. Matthee, D. Sobral, P. Best, A.A. Khostovan, I. Oteo, R. Bouwens, H.
    Röttgering, Monthly Notices of the Royal Astronomical Society 465 (2017) 3637–3655.
date_created: 2022-07-12T12:12:14Z
date_published: 2017-03-01T00:00:00Z
date_updated: 2024-10-14T11:35:49Z
day: '01'
doi: 10.1093/mnras/stw2973
extern: '1'
external_id:
  arxiv:
  - '1605.08782'
intvolume: '       465'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'cosmology: observations'
- dark ages
- reionization
- first stars
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1605.08782
month: '03'
oa: 1
oa_version: Preprint
page: 3637-3655
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The production and escape of Lyman-Continuum radiation from star-forming galaxies
  at z ∼ 2 and their redshift evolution
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 465
year: '2017'
...
---
_id: '11565'
abstract:
- lang: eng
  text: We use the hydrodynamical EAGLE simulation to study the magnitude and origin
    of the scatter in the stellar mass–halo mass relation for central galaxies. We
    separate cause and effect by correlating stellar masses in the baryonic simulation
    with halo properties in a matched dark matter only (DMO) simulation. The scatter
    in stellar mass increases with redshift and decreases with halo mass. At z = 0.1,
    it declines from 0.25 dex at M200, DMO ≈ 1011 M⊙ to 0.12 dex at M200, DMO ≈ 1013
    M⊙, but the trend is weak above 1012 M⊙. For M200, DMO < 1012.5 M⊙ up to 0.04
    dex of the scatter is due to scatter in the halo concentration. At fixed halo
    mass, a larger stellar mass corresponds to a more concentrated halo. This is likely
    because higher concentrations imply earlier formation times and hence more time
    for accretion and star formation, and/or because feedback is less efficient in
    haloes with higher binding energies. The maximum circular velocity, Vmax, DMO,
    and binding energy are therefore more fundamental properties than halo mass, meaning
    that they are more accurate predictors of stellar mass, and we provide fitting
    formulae for their relations with stellar mass. However, concentration alone cannot
    explain the total scatter in the Mstar−M200,DMO relation, and it does not explain
    the scatter in Mstar–Vmax, DMO. Halo spin, sphericity, triaxiality, substructure
    and environment are also not responsible for the remaining scatter, which thus
    could be due to more complex halo properties or non-linear/stochastic baryonic
    effects.
acknowledgement: We thank the anonymous referee for their comments. JM acknowledges
  the support of a Huygens PhD fellowship from Leiden University. JM thanks David
  Sobral for useful discussions and help with fitting routines and Jonas Chavez Montero
  and Ying Zu for providing data. We thank PRACE for the access to the Curie facility
  in France. We have used the DiRAC system which is a part of National E-Infrastructure
  at Durham University, operated by the Institute for Computational Cosmology on behalf
  of the STFC DiRAC HPC Facility (www.dirac.ac.uk); the equipment was funded by BIS
  National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1,
  STFC DiRAC Operations grant ST/K003267/1 and Durham University. The study was sponsored
  by the Dutch National Computing Facilities Foundation (NCF) for the use of supercomputer
  facilities, with financial support from the Netherlands Organisation for Scientific
  Research (NWO), through VICI grant 639.043.409, and the European Research Council
  under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC Grant
  agreement 278594- GasAroundGalaxies, and from the Belgian Science Policy Office
  ([AP P7/08 CHARM]). We have benefited greatly from the public available programming
  language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY, H5PY and RPY2 packages,
  and the TOPCAT analysis program (Taylor 2005).
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: Joop
  full_name: Schaye, Joop
  last_name: Schaye
- first_name: Robert A.
  full_name: Crain, Robert A.
  last_name: Crain
- first_name: Matthieu
  full_name: Schaller, Matthieu
  last_name: Schaller
- first_name: Richard
  full_name: Bower, Richard
  last_name: Bower
- first_name: Tom
  full_name: Theuns, Tom
  last_name: Theuns
citation:
  ama: Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. The origin of
    scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE
    simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;465(2):2381-2396.
    doi:<a href="https://doi.org/10.1093/mnras/stw2884">10.1093/mnras/stw2884</a>
  apa: Matthee, J. J., Schaye, J., Crain, R. A., Schaller, M., Bower, R., &#38; Theuns,
    T. (2017). The origin of scatter in the stellar mass–halo mass relation of central
    galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stw2884">https://doi.org/10.1093/mnras/stw2884</a>
  chicago: Matthee, Jorryt J, Joop Schaye, Robert A. Crain, Matthieu Schaller, Richard
    Bower, and Tom Theuns. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation
    of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal
    Astronomical Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stw2884">https://doi.org/10.1093/mnras/stw2884</a>.
  ieee: J. J. Matthee, J. Schaye, R. A. Crain, M. Schaller, R. Bower, and T. Theuns,
    “The origin of scatter in the stellar mass–halo mass relation of central galaxies
    in the EAGLE simulation,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 465, no. 2. Oxford University Press, pp. 2381–2396, 2017.
  ista: Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. 2017. The origin
    of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE
    simulation. Monthly Notices of the Royal Astronomical Society. 465(2), 2381–2396.
  mla: Matthee, Jorryt J., et al. “The Origin of Scatter in the Stellar Mass–Halo
    Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 465, no. 2, Oxford University Press,
    2017, pp. 2381–96, doi:<a href="https://doi.org/10.1093/mnras/stw2884">10.1093/mnras/stw2884</a>.
  short: J.J. Matthee, J. Schaye, R.A. Crain, M. Schaller, R. Bower, T. Theuns, Monthly
    Notices of the Royal Astronomical Society 465 (2017) 2381–2396.
date_created: 2022-07-12T12:25:08Z
date_published: 2017-02-01T00:00:00Z
date_updated: 2024-10-14T11:36:05Z
day: '01'
doi: 10.1093/mnras/stw2884
extern: '1'
external_id:
  arxiv:
  - '1608.08218'
intvolume: '       465'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: formation'
- 'galaxies: haloes'
- 'cosmology: theory'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1608.08218
month: '02'
oa: 1
oa_version: Preprint
page: 2381-2396
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The origin of scatter in the stellar mass–halo mass relation of central galaxies
  in the EAGLE simulation
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 465
year: '2017'
...
---
_id: '11566'
abstract:
- lang: eng
  text: While traditionally associated with active galactic nuclei (AGN), the properties
    of the C II] (λ = 2326 Å), C III] (λ, λ = 1907, 1909 Å) and C IV (λ, λ = 1549,
    1551 Å) emission lines are still uncertain as large, unbiased samples of sources
    are scarce. We present the first blind, statistical study of C II], C III] and
    C IV emitters at z ∼ 0.68, 1.05, 1.53, respectively, uniformly selected down to
    a flux limit of ∼4 × 10−17 erg s−1 cm−1 through a narrow-band survey covering
    an area of ∼1.4 deg2 over COSMOS and UDS. We detect 16 C II], 35 C III] and 17
    C IV emitters, whose nature we investigate using optical colours as well as Hubble
    Space Telescope (HST), X-ray, radio and far-infrared data. We find that z ∼ 0.7
    C II] emitters are consistent with a mixture of blue (UV slope β = −2.0 ± 0.4)
    star-forming (SF) galaxies with discy HST structure and AGN with Seyfert-like
    morphologies. Bright C II] emitters have individual X-ray detections as well as
    high average black hole accretion rates (BHARs) of ∼0.1 M⊙ yr−1. C III] emitters
    at z ∼ 1.05 trace a general population of SF galaxies, with β = −0.8 ± 1.1, a
    variety of optical morphologies, including isolated and interacting galaxies and
    low BHAR (<0.02 M⊙ yr−1). Our C IV emitters at z ∼ 1.5 are consistent with young,
    blue quasars (β ∼ −1.9) with point-like optical morphologies, bright X-ray counterparts
    and large BHAR (0.8  M⊙ yr−1). We also find some surprising C II], C III] and
    C IV emitters with rest-frame equivalent widths (EWs) that could be as large as
    50–100 Å. AGN or spatial offsets between the UV continuum stellar disc and the
    line-emitting regions may explain the large EW. These bright C II], C III] and
    C IV emitters are ideal candidates for spectroscopic follow-up to fully unveil
    their nature.
acknowledgement: 'We would like to thank the anonymous referee for her/his valuable
  input that helped improve the clarity and interpretation of our results. DS acknowledges
  financial support from the Netherlands Organisation for Scientific research (NWO),
  through a Veni fellowship. IO acknowledges support from the European Research Council
  in the form of the Advanced Investigator Programme, 321302, COSMICISM. CALYMHA data
  are based on observations made with the Isaac Newton Telescope (proposals 13AN002,
  I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008) operated on the island
  of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los
  Muchachos of the Instituto de Astrofísica de Canarias. Also based on data products
  from observations made with ESO Telescopes at the La Silla Paranal Observatory under
  ESO programme IDs 098.A-0819 and 179.A-2005. We are grateful to E. L. Wright and
  J. Schombert for their cosmology calculator. We would like to thank the authors
  of NUMPY (van der Walt et al. 2011), SCIPY (Jones et al. 2001), MATPLOTLIB (Hunter
  2007) and ASTROPY (Astropy Collaboration et al. 2013) for making these packages
  publicly available. This research has made use of the NASA/IPAC Extragalactic Database
  (NED), which is '
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Andra
  full_name: Stroe, Andra
  last_name: Stroe
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: João
  full_name: Calhau, João
  last_name: Calhau
- first_name: Ivan
  full_name: Oteo, Ivan
  last_name: Oteo
citation:
  ama: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for
    C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent
    widths . <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(3):2558-2574.
    doi:<a href="https://doi.org/10.1093/mnras/stx1712">10.1093/mnras/stx1712</a>
  apa: Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., &#38; Oteo, I. (2017). A
    1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies
    and equivalent widths . <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx1712">https://doi.org/10.1093/mnras/stx1712</a>
  chicago: Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo.
    “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature,
    Morphologies and Equivalent Widths .” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx1712">https://doi.org/10.1093/mnras/stx1712</a>.
  ieee: A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind
    survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and
    equivalent widths ,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 471, no. 3. Oxford University Press, pp. 2558–2574, 2017.
  ista: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey
    for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent
    widths . Monthly Notices of the Royal Astronomical Society. 471(3), 2558–2574.
  mla: Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at
    z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 471, no. 3, Oxford University Press,
    2017, pp. 2558–74, doi:<a href="https://doi.org/10.1093/mnras/stx1712">10.1093/mnras/stx1712</a>.
  short: A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of
    the Royal Astronomical Society 471 (2017) 2558–2574.
date_created: 2022-07-12T12:33:16Z
date_published: 2017-11-01T00:00:00Z
date_updated: 2022-08-19T07:59:57Z
day: '01'
doi: 10.1093/mnras/stx1712
extern: '1'
external_id:
  arxiv:
  - '1703.10169'
intvolume: '       471'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: high-redshift'
- 'quasars: emission lines'
- 'galaxies: star formation'
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1703.10169
month: '11'
oa: 1
oa_version: Preprint
page: 2558-2574
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature,
  morphologies and equivalent widths '
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_id: '11567'
abstract:
- lang: eng
  text: Recently, the C III] and C IV emission lines have been observed in galaxies
    in the early Universe (z > 5), providing new ways to measure their redshift and
    study their stellar populations and active galactic nuclei (AGN). We explore the
    first blind C II], C III] and C IV survey (z ∼ 0.68, 1.05, 1.53, respectively)
    presented in Stroe et al. (2017). We derive luminosity functions (LF) and study
    properties of C II], C III] and C IV line emitters through comparisons to the
    LFs of H α and Ly α emitters, UV selected star-forming (SF) galaxies and quasars
    at similar redshifts. The C II] LF at z ∼ 0.68 is equally well described by a
    Schechter or a power-law LF, characteristic of a mixture of SF and AGN activity.
    The C III] LF (z ∼ 1.05) is consistent to a scaled down version of the Schechter
    H α and Ly α LF at their redshift, indicating a SF origin. In stark contrast,
    the C IV LF at z ∼ 1.53 is well fit by a power-law, quasar-like LF. We find that
    the brightest UV sources (MUV < −22) will universally have C III] and C IV emission.
    However, on average, C III] and C IV are not as abundant as H α or Ly α emitters
    at the same redshift, with cosmic average ratios of ∼0.02–0.06 to H α and ∼0.01–0.1
    to intrinsic Ly α. We predict that the C III] and C IV lines can only be truly
    competitive in confirming high-redshift candidates when the hosts are intrinsically
    bright and the effective Ly α escape fraction is below 1 per cent. While C III]
    and C IV were proposed as good tracers of young, relatively low-metallicity galaxies
    typical of the early Universe, we find that, at least at z ∼ 1.5, C IV is exclusively
    hosted by AGN/quasars, especially at large line equivalent widths.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Andra
  full_name: Stroe, Andra
  last_name: Stroe
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: João
  full_name: Calhau, João
  last_name: Calhau
- first_name: Ivan
  full_name: Oteo, Ivan
  last_name: Oteo
citation:
  ama: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for
    C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average
    line ratios. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(3):2575-2586.
    doi:<a href="https://doi.org/10.1093/mnras/stx1713">10.1093/mnras/stx1713</a>
  apa: Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., &#38; Oteo, I. (2017). A
    1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity
    functions and cosmic average line ratios. <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx1713">https://doi.org/10.1093/mnras/stx1713</a>
  chicago: Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo.
    “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity
    Functions and Cosmic Average Line Ratios.” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx1713">https://doi.org/10.1093/mnras/stx1713</a>.
  ieee: A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind
    survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and
    cosmic average line ratios,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 471, no. 3. Oxford University Press, pp. 2575–2586, 2017.
  ista: Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey
    for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic
    average line ratios. Monthly Notices of the Royal Astronomical Society. 471(3),
    2575–2586.
  mla: Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at
    z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 471, no. 3, Oxford University
    Press, 2017, pp. 2575–86, doi:<a href="https://doi.org/10.1093/mnras/stx1713">10.1093/mnras/stx1713</a>.
  short: A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of
    the Royal Astronomical Society 471 (2017) 2575–2586.
date_created: 2022-07-12T12:54:57Z
date_published: 2017-11-01T00:00:00Z
date_updated: 2022-08-19T08:02:04Z
day: '01'
doi: 10.1093/mnras/stx1713
extern: '1'
external_id:
  arxiv:
  - '1703.10169'
intvolume: '       471'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: active'
- 'galaxies: high redshift'
- 'galaxies: luminosity function'
- mass function
- 'quasars: emission lines'
- star formation
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1703.10169
month: '11'
oa: 1
oa_version: Preprint
page: 2575-2586
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity
  functions and cosmic average line ratios
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_id: '11572'
abstract:
- lang: eng
  text: We present spectroscopic follow-up of candidate luminous Ly α emitters (LAEs)
    at z = 5.7–6.6 in the SA22 field with VLT/X-SHOOTER. We confirm two new luminous
    LAEs at z = 5.676 (SR6) and z = 6.532 (VR7), and also present HST follow-up of
    both sources. These sources have luminosities LLy α ≈ 3 × 1043 erg s−1, very high
    rest-frame equivalent widths of EW0 ≳ 200 Å and narrow Ly α lines (200–340 km s−1).
    VR7 is the most UV-luminous LAE at z > 6.5, with M1500 = −22.5, even brighter
    in the UV than CR7. Besides Ly α, we do not detect any other rest-frame UV lines
    in the spectra of SR6 and VR7, and argue that rest-frame UV lines are easier to
    observe in bright galaxies with low Ly α equivalent widths. We confirm that Ly α
    line widths increase with Ly α luminosity at z = 5.7, while there are indications
    that Ly α lines of faint LAEs become broader at z = 6.6, potentially due to reionization.
    We find a large spread of up to 3 dex in UV luminosity for >L⋆ LAEs, but find
    that the Ly α luminosity of the brightest LAEs is strongly related to UV luminosity
    at z = 6.6. Under basic assumptions, we find that several LAEs at z ≈ 6–7 have
    Ly α escape fractions ≳ 100  per cent, indicating bursty star formation histories,
    alternative Ly α production mechanisms, or dust attenuating Ly α emission differently
    than UV emission. Finally, we present a method to compute ξion, the production
    efficiency of ionizing photons, and find that LAEs at z ≈ 6–7 have high values
    of log10(ξion/Hz erg−1) ≈ 25.51 ± 0.09 that may alleviate the need for high Lyman-Continuum
    escape fractions required for reionization.
acknowledgement: 'We thank the referee for a constructive report that has improved
  the quality and clarity of this work. The authors thank Grecco Oyarzún for discussions.
  JM acknowledges the support of a Huygens PhD fellowship from Leiden University.
  DS acknowledges financial support from the Netherlands Organisation for Scientific
  research (NWO) through a Veni fellowship and from Lancaster University through an
  Early Career Internal Grant A100679. BD acknowledges financial support from NASA
  through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G.
  We thank Kasper Schmidt for providing measurements. Based on observations with the
  W.M. Keck Observatory through programme C267D. The W.M. Keck Observatory is operated
  as a scientific partnership amongst the California Institute of Technology, the
  University of California and the National Aeronautics and Space Administration.
  Based on observations made with ESO Telescopes at the La Silla Paranal Observatory
  under programme IDs 097.A-0943, 294.A 5018 and 098.A-0819 and on data products produced
  by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium.
  The authors acknowledge the award of observing time (W16AN004) and of service time
  (SW2014b20) on the William Herschel Telescope (WHT). WHT and its service programme
  are operated on the island of La Palma by the Isaac Newton Group in the Spanish
  Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias.
  Based on observations made with the NASA/ESA HST, obtained (from the Data Archive)
  at the Space Telescope Science Institute, which is operated by the Association of
  Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These
  observations are associated with programme #14699. We are grateful for the excellent
  data sets from the COSMOS, UltraVISTA, SXDS, UDS and CFHTLS survey teams; without
  these legacy surveys, this research would have been impossible. We have benefited
  from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB,
  PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP
  and SCAMP and the TOPCAT analysis tool (Taylor 2013).'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: David
  full_name: Sobral, David
  last_name: Sobral
- first_name: Behnam
  full_name: Darvish, Behnam
  last_name: Darvish
- first_name: Sérgio
  full_name: Santos, Sérgio
  last_name: Santos
- first_name: Bahram
  full_name: Mobasher, Bahram
  last_name: Mobasher
- first_name: Ana
  full_name: Paulino-Afonso, Ana
  last_name: Paulino-Afonso
- first_name: Huub
  full_name: Röttgering, Huub
  last_name: Röttgering
- first_name: Lara
  full_name: Alegre, Lara
  last_name: Alegre
citation:
  ama: Matthee JJ, Sobral D, Darvish B, et al. Spectroscopic properties of luminous
    Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2017;472(1):772-787. doi:<a href="https://doi.org/10.1093/mnras/stx2061">10.1093/mnras/stx2061</a>
  apa: Matthee, J. J., Sobral, D., Darvish, B., Santos, S., Mobasher, B., Paulino-Afonso,
    A., … Alegre, L. (2017). Spectroscopic properties of luminous Ly α emitters at
    z ≈ 6–7 and comparison to the Lyman-break population. <i>Monthly Notices of the
    Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx2061">https://doi.org/10.1093/mnras/stx2061</a>
  chicago: Matthee, Jorryt J, David Sobral, Behnam Darvish, Sérgio Santos, Bahram
    Mobasher, Ana Paulino-Afonso, Huub Röttgering, and Lara Alegre. “Spectroscopic
    Properties of Luminous Ly α Emitters at z ≈ 6–7 and Comparison to the Lyman-Break
    Population.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford
    University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx2061">https://doi.org/10.1093/mnras/stx2061</a>.
  ieee: J. J. Matthee <i>et al.</i>, “Spectroscopic properties of luminous Ly α emitters
    at z ≈ 6–7 and comparison to the Lyman-break population,” <i>Monthly Notices of
    the Royal Astronomical Society</i>, vol. 472, no. 1. Oxford University Press,
    pp. 772–787, 2017.
  ista: Matthee JJ, Sobral D, Darvish B, Santos S, Mobasher B, Paulino-Afonso A, Röttgering
    H, Alegre L. 2017. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7
    and comparison to the Lyman-break population. Monthly Notices of the Royal Astronomical
    Society. 472(1), 772–787.
  mla: Matthee, Jorryt J., et al. “Spectroscopic Properties of Luminous Ly α Emitters
    at z ≈ 6–7 and Comparison to the Lyman-Break Population.” <i>Monthly Notices of
    the Royal Astronomical Society</i>, vol. 472, no. 1, Oxford University Press,
    2017, pp. 772–87, doi:<a href="https://doi.org/10.1093/mnras/stx2061">10.1093/mnras/stx2061</a>.
  short: J.J. Matthee, D. Sobral, B. Darvish, S. Santos, B. Mobasher, A. Paulino-Afonso,
    H. Röttgering, L. Alegre, Monthly Notices of the Royal Astronomical Society 472
    (2017) 772–787.
date_created: 2022-07-13T09:47:39Z
date_published: 2017-11-01T00:00:00Z
date_updated: 2024-10-14T11:36:26Z
day: '01'
doi: 10.1093/mnras/stx2061
extern: '1'
external_id:
  arxiv:
  - '1706.06591'
intvolume: '       472'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution – galaxies: high-redshift'
- dark ages
- reionization
- first stars
- 'cosmology: observations'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1706.06591
month: '11'
oa: 1
oa_version: Preprint
page: 772-787
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison
  to the Lyman-break population
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 472
year: '2017'
...
---
_id: '11573'
abstract:
- lang: eng
  text: We present dynamical measurements from the KMOS (K-band multi-object spectrograph)
    Deep Survey (KDS), which comprises 77 typical star-forming galaxies at z ≃ 3.5
    in the mass range 9.0 < log (M⋆/M⊙) < 10.5. These measurements constrain the internal
    dynamics, the intrinsic velocity dispersions (σint) and rotation velocities (VC)
    of galaxies in the high-redshift Universe. The mean velocity dispersion of the
    galaxies in our sample is σint=70.8+3.3−3.1kms−1⁠, revealing that the increasing
    average σint with increasing redshift, reported for z ≲ 2, continues out to z
    ≃ 3.5. Only 36 ± 8 per cent of our galaxies are rotation-dominated (VC/σint >
    1), with the sample average VC/σint value much smaller than at lower redshift.
    After carefully selecting comparable star-forming samples at multiple epochs,
    we find that the rotation-dominated fraction evolves with redshift with a z−0.2
    dependence. The rotation-dominated KDS galaxies show no clear offset from the
    local rotation velocity–stellar mass (i.e. VC–M⋆) relation, although a smaller
    fraction of the galaxies are on the relation due to the increase in the dispersion-dominated
    fraction. These observations are consistent with a simple equilibrium model picture,
    in which random motions are boosted in high-redshift galaxies by a combination
    of the increasing gas fractions, accretion efficiency, specific star formation
    rate and stellar feedback and which may provide significant pressure support against
    gravity on the galactic disc scale.
acknowledgement: 'We wish to thank the anonymous referee for their comments, which
  have improved the quality and clarity of this work. OJT acknowledges the financial
  support of the Science and Technology Facilities Council through a studentship award.
  MC and OJT acknowledge the KMOS team and all the personnel of the European Southern
  Observatory Very Large Telescope for outstanding support during the KMOS GTO observations.
  CMH, AMS and RMS acknowledge the Science and Technology Facilities Council through
  grant code ST/L00075X/1. RJM acknowledges the support of the European Research Council
  via the award of a Consolidator Grant (PI: McLure). JSD acknowledges the support
  of the European Research Council via the award of an Advanced Grant (PI J. Dunlop),
  and the contribution of the EC FP7 SPACE project ASTRODEEP (Ref.No: 312725). AMS
  acknowledges the Leverhulme Foundation. JM acknowledges the support of a Huygens
  PhD fellowship from Leiden University. DS acknowledges financial support from the
  Netherlands Organization for Scientific research (NWO) through a Veni fellowship
  and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010).
  This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program
  with the NASA/ESA HST, which is operated by the Association of Universities for
  Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is based
  on observations taken by the 3D HST Treasury Program (GO 12177 and 12328) with the
  NASA/ESA HST, which is operated by the Association of Universities for Research
  in Astronomy, Inc., under NASA contract NAS5-26555. Based on data obtained with
  the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large
  Program 185.A-0791, and made available by the VUDS team at the CESAM data centre,
  Laboratoire d’Astrophysique de Marseille, France. Based on observations obtained
  at the Very Large Telescope of the European Southern Observatory. Programme IDs:
  092.A 0399(A), 093.A-0122(A,B), 094.A-0214(A,B),095.A0680(A,B),096.A-0315(A,B,C).'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: O. J.
  full_name: Turner, O. J.
  last_name: Turner
- first_name: M.
  full_name: Cirasuolo, M.
  last_name: Cirasuolo
- first_name: C. M.
  full_name: Harrison, C. M.
  last_name: Harrison
- first_name: R. J.
  full_name: McLure, R. J.
  last_name: McLure
- first_name: J. S.
  full_name: Dunlop, J. S.
  last_name: Dunlop
- first_name: A. M.
  full_name: Swinbank, A. M.
  last_name: Swinbank
- first_name: H. L.
  full_name: Johnson, H. L.
  last_name: Johnson
- first_name: D.
  full_name: Sobral, D.
  last_name: Sobral
- first_name: Jorryt J
  full_name: Matthee, Jorryt J
  id: 7439a258-f3c0-11ec-9501-9df22fe06720
  last_name: Matthee
  orcid: 0000-0003-2871-127X
- first_name: R. M.
  full_name: Sharples, R. M.
  last_name: Sharples
citation:
  ama: Turner OJ, Cirasuolo M, Harrison CM, et al. The KMOS Deep Survey (KDS) – I.
    Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2017;471(2):1280-1320. doi:<a href="https://doi.org/10.1093/mnras/stx1366">10.1093/mnras/stx1366</a>
  apa: Turner, O. J., Cirasuolo, M., Harrison, C. M., McLure, R. J., Dunlop, J. S.,
    Swinbank, A. M., … Sharples, R. M. (2017). The KMOS Deep Survey (KDS) – I. Dynamical
    measurements of typical star-forming galaxies at z ≃ 3.5. <i>Monthly Notices of
    the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx1366">https://doi.org/10.1093/mnras/stx1366</a>
  chicago: Turner, O. J., M. Cirasuolo, C. M. Harrison, R. J. McLure, J. S. Dunlop,
    A. M. Swinbank, H. L. Johnson, D. Sobral, Jorryt J Matthee, and R. M. Sharples.
    “The KMOS Deep Survey (KDS) – I. Dynamical Measurements of Typical Star-Forming
    Galaxies at z ≃ 3.5.” <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx1366">https://doi.org/10.1093/mnras/stx1366</a>.
  ieee: O. J. Turner <i>et al.</i>, “The KMOS Deep Survey (KDS) – I. Dynamical measurements
    of typical star-forming galaxies at z ≃ 3.5,” <i>Monthly Notices of the Royal
    Astronomical Society</i>, vol. 471, no. 2. Oxford University Press, pp. 1280–1320,
    2017.
  ista: Turner OJ, Cirasuolo M, Harrison CM, McLure RJ, Dunlop JS, Swinbank AM, Johnson
    HL, Sobral D, Matthee JJ, Sharples RM. 2017. The KMOS Deep Survey (KDS) – I. Dynamical
    measurements of typical star-forming galaxies at z ≃ 3.5. Monthly Notices of the
    Royal Astronomical Society. 471(2), 1280–1320.
  mla: Turner, O. J., et al. “The KMOS Deep Survey (KDS) – I. Dynamical Measurements
    of Typical Star-Forming Galaxies at z ≃ 3.5.” <i>Monthly Notices of the Royal
    Astronomical Society</i>, vol. 471, no. 2, Oxford University Press, 2017, pp.
    1280–320, doi:<a href="https://doi.org/10.1093/mnras/stx1366">10.1093/mnras/stx1366</a>.
  short: O.J. Turner, M. Cirasuolo, C.M. Harrison, R.J. McLure, J.S. Dunlop, A.M.
    Swinbank, H.L. Johnson, D. Sobral, J.J. Matthee, R.M. Sharples, Monthly Notices
    of the Royal Astronomical Society 471 (2017) 1280–1320.
date_created: 2022-07-13T10:03:01Z
date_published: 2017-10-01T00:00:00Z
date_updated: 2022-08-19T08:07:31Z
day: '01'
doi: 10.1093/mnras/stx1366
extern: '1'
external_id:
  arxiv:
  - '1704.06263'
intvolume: '       471'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: evolution'
- 'galaxies: high-redshift'
- 'galaxies: kinematics and dynamics'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1704.06263
month: '10'
oa: 1
oa_version: Preprint
page: 1280-1320
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming
  galaxies at z ≃ 3.5
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_id: '15239'
abstract:
- lang: eng
  text: Using images from the Hubble Space Telescope Advanced Camera for Surveys,
    we measure the rate of cooling of white dwarfs in the globular cluster 47 Tucanae
    and compare it to modelled cooling curves. We examine the effects of the outer
    convective envelope reaching the nearly isothermal degenerate core and the release
    of latent heat during core crystallization on the white dwarf cooling rates. For
    white dwarfs typical of 47 Tuc, the onset of these effects occur at similar times.
    The latent heat released during crystallization is a small heat source. In contrast,
    the heat reservoir of the degenerate core is substantially larger. When the convective
    envelope reaches the nearly isothermal interior of the white dwarf, the star becomes
    brighter than it would be in the absence of this effect. Our modelled cooling
    curves that include this convective coupling closely match the observed luminosity
    function of the white dwarfs in 47 Tuc.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Alysa
  full_name: Obertas, Alysa
  last_name: Obertas
- first_name: Ilaria
  full_name: Caiazzo, Ilaria
  id: 8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d
  last_name: Caiazzo
  orcid: 0000-0002-4770-5388
- first_name: Jeremy
  full_name: Heyl, Jeremy
  last_name: Heyl
- first_name: Harvey
  full_name: Richer, Harvey
  last_name: Richer
- first_name: Jason
  full_name: Kalirai, Jason
  last_name: Kalirai
- first_name: Pier-Emmanuel
  full_name: Tremblay, Pier-Emmanuel
  last_name: Tremblay
citation:
  ama: Obertas A, Caiazzo I, Heyl J, Richer H, Kalirai J, Tremblay P-E. The onset
    of convective coupling and freezing in the white dwarfs of 47 Tucanae. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2017;474(1):677-682. doi:<a href="https://doi.org/10.1093/mnras/stx2759">10.1093/mnras/stx2759</a>
  apa: Obertas, A., Caiazzo, I., Heyl, J., Richer, H., Kalirai, J., &#38; Tremblay,
    P.-E. (2017). The onset of convective coupling and freezing in the white dwarfs
    of 47 Tucanae. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford
    University Press. <a href="https://doi.org/10.1093/mnras/stx2759">https://doi.org/10.1093/mnras/stx2759</a>
  chicago: Obertas, Alysa, Ilaria Caiazzo, Jeremy Heyl, Harvey Richer, Jason Kalirai,
    and Pier-Emmanuel Tremblay. “The Onset of Convective Coupling and Freezing in
    the White Dwarfs of 47 Tucanae.” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx2759">https://doi.org/10.1093/mnras/stx2759</a>.
  ieee: A. Obertas, I. Caiazzo, J. Heyl, H. Richer, J. Kalirai, and P.-E. Tremblay,
    “The onset of convective coupling and freezing in the white dwarfs of 47 Tucanae,”
    <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 474, no. 1. Oxford
    University Press, pp. 677–682, 2017.
  ista: Obertas A, Caiazzo I, Heyl J, Richer H, Kalirai J, Tremblay P-E. 2017. The
    onset of convective coupling and freezing in the white dwarfs of 47 Tucanae. Monthly
    Notices of the Royal Astronomical Society. 474(1), 677–682.
  mla: Obertas, Alysa, et al. “The Onset of Convective Coupling and Freezing in the
    White Dwarfs of 47 Tucanae.” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 474, no. 1, Oxford University Press, 2017, pp. 677–82, doi:<a href="https://doi.org/10.1093/mnras/stx2759">10.1093/mnras/stx2759</a>.
  short: A. Obertas, I. Caiazzo, J. Heyl, H. Richer, J. Kalirai, P.-E. Tremblay, Monthly
    Notices of the Royal Astronomical Society 474 (2017) 677–682.
date_created: 2024-03-26T10:40:05Z
date_published: 2017-10-24T00:00:00Z
date_updated: 2024-04-08T07:04:10Z
day: '24'
doi: 10.1093/mnras/stx2759
extern: '1'
external_id:
  arxiv:
  - '1709.08097'
intvolume: '       474'
issue: '1'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.48550/arXiv.1709.08097
month: '10'
oa: 1
oa_version: Preprint
page: 677-682
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The onset of convective coupling and freezing in the white dwarfs of 47 Tucanae
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 474
year: '2017'
...
---
_id: '15241'
abstract:
- lang: eng
  text: We present a model to account for the observed debris discs around young white
    dwarfs and the presence of metal lines in their spectra. Stellar evolution models
    predict that the mass-loss on the AGB will be pulsed; furthermore, observations
    indicate that the bulk of the mass-loss occurs on the AGB. In this case, if the
    progenitors of the white dwarfs had remnants of planetary formation like the Sun’s
    Oort cloud or the Kuiper Belt and a planet lying within that cloud or nearby,
    we find that up to 2 per cent of the planetesimals will fall either into planet-crossing
    orbits or into chaotic regions after the mass-loss, depending on the location
    and mass of the planet (from Mars to Neptune). This yields a sufficient mass of
    comets that can be scattered towards the star, form a debris disc and pollute
    the atmosphere.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Ilaria
  full_name: Caiazzo, Ilaria
  id: 8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d
  last_name: Caiazzo
  orcid: 0000-0002-4770-5388
- first_name: Jeremy S.
  full_name: Heyl, Jeremy S.
  last_name: Heyl
citation:
  ama: Caiazzo I, Heyl JS. Polluting white dwarfs with perturbed exo-comets. <i>Monthly
    Notices of the Royal Astronomical Society</i>. 2017;469(3):2750-2759. doi:<a href="https://doi.org/10.1093/mnras/stx1036">10.1093/mnras/stx1036</a>
  apa: Caiazzo, I., &#38; Heyl, J. S. (2017). Polluting white dwarfs with perturbed
    exo-comets. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University
    Press. <a href="https://doi.org/10.1093/mnras/stx1036">https://doi.org/10.1093/mnras/stx1036</a>
  chicago: Caiazzo, Ilaria, and Jeremy S. Heyl. “Polluting White Dwarfs with Perturbed
    Exo-Comets.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford
    University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx1036">https://doi.org/10.1093/mnras/stx1036</a>.
  ieee: I. Caiazzo and J. S. Heyl, “Polluting white dwarfs with perturbed exo-comets,”
    <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 469, no. 3. Oxford
    University Press, pp. 2750–2759, 2017.
  ista: Caiazzo I, Heyl JS. 2017. Polluting white dwarfs with perturbed exo-comets.
    Monthly Notices of the Royal Astronomical Society. 469(3), 2750–2759.
  mla: Caiazzo, Ilaria, and Jeremy S. Heyl. “Polluting White Dwarfs with Perturbed
    Exo-Comets.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 469,
    no. 3, Oxford University Press, 2017, pp. 2750–59, doi:<a href="https://doi.org/10.1093/mnras/stx1036">10.1093/mnras/stx1036</a>.
  short: I. Caiazzo, J.S. Heyl, Monthly Notices of the Royal Astronomical Society
    469 (2017) 2750–2759.
date_created: 2024-03-26T10:40:45Z
date_published: 2017-05-01T00:00:00Z
date_updated: 2024-10-14T12:33:43Z
day: '01'
doi: 10.1093/mnras/stx1036
extern: '1'
external_id:
  arxiv:
  - '1702.07682'
intvolume: '       469'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.48550/arXiv.1702.07682
month: '05'
oa: 1
oa_version: Preprint
page: 2750-2759
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Polluting white dwarfs with perturbed exo-comets
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 469
year: '2017'
...
---
_id: '15243'
abstract:
- lang: eng
  text: High-energy (>250 keV) emission has been detected persisting for several tens
    of seconds after the initial spike of magnetar giant flares (GFs). It has been
    conjectured that this emission might arise via inverse Compton scattering in a
    highly extended corona generated by super-Eddington outflows high up in the magnetosphere.
    In this paper, we undertake a detailed examination of this model. We investigate
    the properties of the required scatterers, and whether the mechanism is consistent
    with the degree of pulsed emission observed in the tail of the GF. We conclude
    that the mechanism is consistent with current data, although the origin of the
    scattering population remains an open question. We propose an alternative picture
    in which the emission is closer to that star and is dominated by synchrotron radiation.
    The Reuven Ramaty High Energy Solar Spectroscopic Imager observations of the 2004
    December flare modestly favour this latter picture. We assess the prospects for
    the Fermi Gamma-ray Space Telescope to detect and characterize a similar high-energy
    component in a future GF. Such a detection should help to resolve some of the
    outstanding issues.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: C.
  full_name: Elenbaas, C.
  last_name: Elenbaas
- first_name: D.
  full_name: Huppenkothen, D.
  last_name: Huppenkothen
- first_name: C.
  full_name: Omand, C.
  last_name: Omand
- first_name: A. L.
  full_name: Watts, A. L.
  last_name: Watts
- first_name: E.
  full_name: Bissaldi, E.
  last_name: Bissaldi
- first_name: Ilaria
  full_name: Caiazzo, Ilaria
  id: 8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d
  last_name: Caiazzo
  orcid: 0000-0002-4770-5388
- first_name: J.
  full_name: Heyl, J.
  last_name: Heyl
citation:
  ama: Elenbaas C, Huppenkothen D, Omand C, et al. Magnetar giant flare high-energy
    emission. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(2):1856-1872.
    doi:<a href="https://doi.org/10.1093/mnras/stx1727">10.1093/mnras/stx1727</a>
  apa: Elenbaas, C., Huppenkothen, D., Omand, C., Watts, A. L., Bissaldi, E., Caiazzo,
    I., &#38; Heyl, J. (2017). Magnetar giant flare high-energy emission. <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx1727">https://doi.org/10.1093/mnras/stx1727</a>
  chicago: Elenbaas, C., D. Huppenkothen, C. Omand, A. L. Watts, E. Bissaldi, Ilaria
    Caiazzo, and J. Heyl. “Magnetar Giant Flare High-Energy Emission.” <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017.
    <a href="https://doi.org/10.1093/mnras/stx1727">https://doi.org/10.1093/mnras/stx1727</a>.
  ieee: C. Elenbaas <i>et al.</i>, “Magnetar giant flare high-energy emission,” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 471, no. 2. Oxford University
    Press, pp. 1856–1872, 2017.
  ista: Elenbaas C, Huppenkothen D, Omand C, Watts AL, Bissaldi E, Caiazzo I, Heyl
    J. 2017. Magnetar giant flare high-energy emission. Monthly Notices of the Royal
    Astronomical Society. 471(2), 1856–1872.
  mla: Elenbaas, C., et al. “Magnetar Giant Flare High-Energy Emission.” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 471, no. 2, Oxford University
    Press, 2017, pp. 1856–72, doi:<a href="https://doi.org/10.1093/mnras/stx1727">10.1093/mnras/stx1727</a>.
  short: C. Elenbaas, D. Huppenkothen, C. Omand, A.L. Watts, E. Bissaldi, I. Caiazzo,
    J. Heyl, Monthly Notices of the Royal Astronomical Society 471 (2017) 1856–1872.
date_created: 2024-03-26T10:41:24Z
date_published: 2017-07-13T00:00:00Z
date_updated: 2024-04-08T07:05:47Z
day: '13'
doi: 10.1093/mnras/stx1727
extern: '1'
external_id:
  arxiv:
  - '1707.02922'
intvolume: '       471'
issue: '2'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.48550/arXiv.1707.02922
month: '07'
oa: 1
oa_version: Preprint
page: 1856-1872
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  eissn:
  - 1365-2966
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Magnetar giant flare high-energy emission
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 471
year: '2017'
...
---
_id: '1022'
abstract:
- lang: eng
  text: We introduce a multiscale topological description of the Megaparsec web-like
    cosmic matter distribution. Betti numbers and topological persistence offer a
    powerful means of describing the rich connectivity structure of the cosmic web
    and of its multiscale arrangement of matter and galaxies. Emanating from algebraic
    topology and Morse theory, Betti numbers and persistence diagrams represent an
    extension and deepening of the cosmologically familiar topological genus measure
    and the related geometric Minkowski functionals. In addition to a description
    of the mathematical background, this study presents the computational procedure
    for computing Betti numbers and persistence diagrams for density field filtrations.
    The field may be computed starting from a discrete spatial distribution of galaxies
    or simulation particles. The main emphasis of this study concerns an extensive
    and systematic exploration of the imprint of different web-like morphologies and
    different levels of multiscale clustering in the corresponding computed Betti
    numbers and persistence diagrams. To this end, we use Voronoi clustering models
    as templates for a rich variety of web-like configurations and the fractal-like
    Soneira-Peebles models exemplify a range of multiscale configurations. We have
    identified the clear imprint of cluster nodes, filaments, walls, and voids in
    persistence diagrams, along with that of the nested hierarchy of structures in
    multiscale point distributions. We conclude by outlining the potential of persistent
    topology for understanding the connectivity structure of the cosmic web, in large
    simulations of cosmic structure formation and in the challenging context of the
    observed galaxy distribution in large galaxy surveys.
acknowledgement: Part of this work has been supported by the 7th Framework Programme
  for Research of the European Commission, under FETOpen grant number 255827 (CGL
  Computational Geometry Learning) and ERC advanced grant, URSAT (Understanding Random
  Systems via Algebraic Topology) number 320422.
article_processing_charge: No
arxiv: 1
author:
- first_name: Pratyush
  full_name: Pranav, Pratyush
  last_name: Pranav
- first_name: Herbert
  full_name: Edelsbrunner, Herbert
  id: 3FB178DA-F248-11E8-B48F-1D18A9856A87
  last_name: Edelsbrunner
  orcid: 0000-0002-9823-6833
- first_name: Rien
  full_name: Van De Weygaert, Rien
  last_name: Van De Weygaert
- first_name: Gert
  full_name: Vegter, Gert
  last_name: Vegter
- first_name: Michael
  full_name: Kerber, Michael
  last_name: Kerber
- first_name: Bernard
  full_name: Jones, Bernard
  last_name: Jones
- first_name: Mathijs
  full_name: Wintraecken, Mathijs
  id: 307CFBC8-F248-11E8-B48F-1D18A9856A87
  last_name: Wintraecken
  orcid: 0000-0002-7472-2220
citation:
  ama: Pranav P, Edelsbrunner H, Van De Weygaert R, et al. The topology of the cosmic
    web in terms of persistent Betti numbers. <i>Monthly Notices of the Royal Astronomical
    Society</i>. 2017;465(4):4281-4310. doi:<a href="https://doi.org/10.1093/mnras/stw2862">10.1093/mnras/stw2862</a>
  apa: Pranav, P., Edelsbrunner, H., Van De Weygaert, R., Vegter, G., Kerber, M.,
    Jones, B., &#38; Wintraecken, M. (2017). The topology of the cosmic web in terms
    of persistent Betti numbers. <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press. <a href="https://doi.org/10.1093/mnras/stw2862">https://doi.org/10.1093/mnras/stw2862</a>
  chicago: Pranav, Pratyush, Herbert Edelsbrunner, Rien Van De Weygaert, Gert Vegter,
    Michael Kerber, Bernard Jones, and Mathijs Wintraecken. “The Topology of the Cosmic
    Web in Terms of Persistent Betti Numbers.” <i>Monthly Notices of the Royal Astronomical
    Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stw2862">https://doi.org/10.1093/mnras/stw2862</a>.
  ieee: P. Pranav <i>et al.</i>, “The topology of the cosmic web in terms of persistent
    Betti numbers,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol.
    465, no. 4. Oxford University Press, pp. 4281–4310, 2017.
  ista: Pranav P, Edelsbrunner H, Van De Weygaert R, Vegter G, Kerber M, Jones B,
    Wintraecken M. 2017. The topology of the cosmic web in terms of persistent Betti
    numbers. Monthly Notices of the Royal Astronomical Society. 465(4), 4281–4310.
  mla: Pranav, Pratyush, et al. “The Topology of the Cosmic Web in Terms of Persistent
    Betti Numbers.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol.
    465, no. 4, Oxford University Press, 2017, pp. 4281–310, doi:<a href="https://doi.org/10.1093/mnras/stw2862">10.1093/mnras/stw2862</a>.
  short: P. Pranav, H. Edelsbrunner, R. Van De Weygaert, G. Vegter, M. Kerber, B.
    Jones, M. Wintraecken, Monthly Notices of the Royal Astronomical Society 465 (2017)
    4281–4310.
date_created: 2018-12-11T11:49:44Z
date_published: 2017-01-01T00:00:00Z
date_updated: 2025-06-04T08:10:31Z
day: '01'
department:
- _id: HeEd
doi: 10.1093/mnras/stw2862
external_id:
  arxiv:
  - '1608.04519'
  isi:
  - '000395170200039'
intvolume: '       465'
isi: 1
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://arxiv.org/abs/1608.04519
month: '01'
oa: 1
oa_version: Submitted Version
page: 4281 - 4310
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
publication_status: published
publisher: Oxford University Press
publist_id: '6373'
quality_controlled: '1'
scopus_import: '1'
status: public
title: The topology of the cosmic web in terms of persistent Betti numbers
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 465
year: '2017'
...
---
_id: '17616'
abstract:
- lang: eng
  text: The optical and UV emission from sub-parsec massive black hole binaries (MBHBs)
    in active galactic nuclei (AGNs) is believed to vary periodically, on time-scales
    comparable to the binary's orbital time. If driven by accretion rate fluctuations,
    the variability could be isotropic. If dominated by relativistic Doppler modulation,
    the variability should instead be anisotropic, resembling a rotating forward-beamed
    lighthouse. We consider the infrared (IR) reverberation of either type of periodic
    emission by pc-scale circumbinary dust tori. We predict the phase and amplitude
    of IR variability as a function of the ratio of dust light crossing time to the
    source variability period, and of the torus inclination and opening angle. We
    enumerate several differences between the isotropic and anisotropic cases. Interestingly,
    for a nearly face-on binary with an inclined dust torus, the Doppler boost can
    produce IR variability without any observable optical/UV variability. Such orphan-IR
    variability would have been missed in optical searches for periodic AGNs. We apply
    our models to time-domain WISE IR data from the MBHB candidate PG 1302−102 and
    find consistency with dust reverberation by both isotropically emitting and Doppler-boosted
    sources in the shorter wavelength W1–W2 (2.8 → 5.3 μm) bands. We constrain the
    dust torus to be thin (aspect ratio ∼ 0.1), with an inner radius at 1–5 pc. More
    generally, our dust-echo models will aid in identifying new MBHB candidates, determining
    their nature and constraining the physical properties of MBHBs and their dust
    tori.
article_processing_charge: No
article_type: original
author:
- first_name: Daniel J.
  full_name: D'Orazio, Daniel J.
  last_name: D'Orazio
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: 'D’Orazio DJ, Haiman Z. Lighthouse in the dust: infrared echoes of periodic
    emission from massive black hole binaries★. <i>Monthly Notices of the Royal Astronomical
    Society</i>. 2017;470(1):1198-1217. doi:<a href="https://doi.org/10.1093/mnras/stx1269">10.1093/mnras/stx1269</a>'
  apa: 'D’Orazio, D. J., &#38; Haiman, Z. (2017). Lighthouse in the dust: infrared
    echoes of periodic emission from massive black hole binaries★. <i>Monthly Notices
    of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx1269">https://doi.org/10.1093/mnras/stx1269</a>'
  chicago: 'D’Orazio, Daniel J., and Zoltán Haiman. “Lighthouse in the Dust: Infrared
    Echoes of Periodic Emission from Massive Black Hole Binaries★.” <i>Monthly Notices
    of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx1269">https://doi.org/10.1093/mnras/stx1269</a>.'
  ieee: 'D. J. D’Orazio and Z. Haiman, “Lighthouse in the dust: infrared echoes of
    periodic emission from massive black hole binaries★,” <i>Monthly Notices of the
    Royal Astronomical Society</i>, vol. 470, no. 1. Oxford University Press, pp.
    1198–1217, 2017.'
  ista: 'D’Orazio DJ, Haiman Z. 2017. Lighthouse in the dust: infrared echoes of periodic
    emission from massive black hole binaries★. Monthly Notices of the Royal Astronomical
    Society. 470(1), 1198–1217.'
  mla: 'D’Orazio, Daniel J., and Zoltán Haiman. “Lighthouse in the Dust: Infrared
    Echoes of Periodic Emission from Massive Black Hole Binaries★.” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 470, no. 1, Oxford University Press,
    2017, pp. 1198–217, doi:<a href="https://doi.org/10.1093/mnras/stx1269">10.1093/mnras/stx1269</a>.'
  short: D.J. D’Orazio, Z. Haiman, Monthly Notices of the Royal Astronomical Society
    470 (2017) 1198–1217.
date_created: 2024-09-05T13:32:36Z
date_published: 2017-05-23T00:00:00Z
date_updated: 2024-09-24T08:01:52Z
day: '23'
doi: 10.1093/mnras/stx1269
extern: '1'
intvolume: '       470'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: https://doi.org/10.1093/mnras/stx1269
month: '05'
oa: 1
oa_version: Published Version
page: 1198-1217
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Lighthouse in the dust: infrared echoes of periodic emission from massive
  black hole binaries★'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 470
year: '2017'
...
---
_id: '17630'
abstract:
- lang: eng
  text: In symmetric gravitating systems experiencing rapid mass-loss, particle orbits
    change almost instantaneously, which can lead to the development of a sharply
    contoured density profile, including singular caustics for collisionless systems.
    This framework can be used to model a variety of dynamical systems, such as accretion
    discs following a massive black hole merger and dwarf galaxies following violent
    early star formation feedback. Particle interactions in the high-density peaks
    seem a promising source of observable signatures of these mass-loss events (i.e.
    a possible EM counterpart for black hole mergers or strong gamma-ray emission
    from dark matter annihilation around young galaxies), because the interaction
    rate depends on the square of the density. We study post-mass-loss density profiles,
    both analytic and numerical, in idealized cases and present arguments and methods
    to extend to any general system. An analytic derivation is presented for particles
    on Keplerian orbits responding to a drop in the central mass. We argue that this
    case, with initially circular orbits, gives the most sharply contoured profile
    possible. We find that despite the presence of a set of singular caustics, the
    total particle interaction rate is reduced compared to the unperturbed system;
    this is a result of the overall expansion of the system dominating over the steep
    caustics. Finally, we argue that this result holds more generally, and the loss
    of central mass decreases the particle interaction rate in any physical system.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Zephyr
  full_name: Penoyre, Zephyr
  last_name: Penoyre
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
citation:
  ama: 'Penoyre Z, Haiman Z. A drop in the pond: The effect of rapid mass-loss on
    the dynamics and interaction rate of collisionless particles. <i>Monthly Notices
    of the Royal Astronomical Society</i>. 2017;473(1):498-512. doi:<a href="https://doi.org/10.1093/mnras/stx2469">10.1093/mnras/stx2469</a>'
  apa: 'Penoyre, Z., &#38; Haiman, Z. (2017). A drop in the pond: The effect of rapid
    mass-loss on the dynamics and interaction rate of collisionless particles. <i>Monthly
    Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx2469">https://doi.org/10.1093/mnras/stx2469</a>'
  chicago: 'Penoyre, Zephyr, and Zoltán Haiman. “A Drop in the Pond: The Effect of
    Rapid Mass-Loss on the Dynamics and Interaction Rate of Collisionless Particles.”
    <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press,
    2017. <a href="https://doi.org/10.1093/mnras/stx2469">https://doi.org/10.1093/mnras/stx2469</a>.'
  ieee: 'Z. Penoyre and Z. Haiman, “A drop in the pond: The effect of rapid mass-loss
    on the dynamics and interaction rate of collisionless particles,” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 473, no. 1. Oxford University Press,
    pp. 498–512, 2017.'
  ista: 'Penoyre Z, Haiman Z. 2017. A drop in the pond: The effect of rapid mass-loss
    on the dynamics and interaction rate of collisionless particles. Monthly Notices
    of the Royal Astronomical Society. 473(1), 498–512.'
  mla: 'Penoyre, Zephyr, and Zoltán Haiman. “A Drop in the Pond: The Effect of Rapid
    Mass-Loss on the Dynamics and Interaction Rate of Collisionless Particles.” <i>Monthly
    Notices of the Royal Astronomical Society</i>, vol. 473, no. 1, Oxford University
    Press, 2017, pp. 498–512, doi:<a href="https://doi.org/10.1093/mnras/stx2469">10.1093/mnras/stx2469</a>.'
  short: Z. Penoyre, Z. Haiman, Monthly Notices of the Royal Astronomical Society
    473 (2017) 498–512.
date_created: 2024-09-05T13:59:48Z
date_published: 2017-09-25T00:00:00Z
date_updated: 2024-09-24T09:48:08Z
day: '25'
doi: 10.1093/mnras/stx2469
extern: '1'
external_id:
  arxiv:
  - '1709.08640'
intvolume: '       473'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: ' https://doi.org/10.48550/arXiv.1709.08640'
month: '09'
oa: 1
oa_version: Preprint
page: 498-512
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'A drop in the pond: The effect of rapid mass-loss on the dynamics and interaction
  rate of collisionless particles'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 473
year: '2017'
...
---
_id: '17632'
abstract:
- lang: eng
  text: 'We assess the contribution of dynamical hardening by direct three-body scattering
    interactions to the rate of stellar-mass black hole binary (BHB) mergers in galactic
    nuclei. We derive an analytic model for the single-binary encounter rate in a
    nucleus with spherical and disc components hosting a super-massive black hole
    (SMBH). We determine the total number of encounters NGW needed to harden a BHB
    to the point that inspiral due to gravitational wave emission occurs before the
    next three-body scattering event. This is done independently for both the spherical
    and disc components. Using a Monte Carlo approach, we refine our calculations
    for NGW to include gravitational wave emission between scattering events. For
    astrophysically plausible models, we find that typically NGW ≲ 10. We find two
    separate regimes for the efficient dynamical hardening of BHBs: (1) spherical
    star clusters with high central densities, low-velocity dispersions, and no significant
    Keplerian component and (2) migration traps in discs around SMBHs lacking any
    significant spherical stellar component in the vicinity of the migration trap,
    which is expected due to effective orbital inclination reduction of any spherical
    population by the disc. We also find a weak correlation between the ratio of the
    second-order velocity moment to velocity dispersion in galactic nuclei and the
    rate of BHB mergers, where this ratio is a proxy for the ratio between the rotation-
    and dispersion-supported components. Because discs enforce planar interactions
    that are efficient in hardening BHBs, particularly in migration traps, they have
    high merger rates that can contribute significantly to the rate of BHB mergers
    detected by the advanced Laser Interferometer Gravitational-Wave Observatory.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: N W C
  full_name: Leigh, N W C
  last_name: Leigh
- first_name: A M
  full_name: Geller, A M
  last_name: Geller
- first_name: B
  full_name: McKernan, B
  last_name: McKernan
- first_name: K E S
  full_name: Ford, K E S
  last_name: Ford
- first_name: M-M
  full_name: Mac Low, M-M
  last_name: Mac Low
- first_name: J
  full_name: Bellovary, J
  last_name: Bellovary
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
- first_name: W
  full_name: Lyra, W
  last_name: Lyra
- first_name: J
  full_name: Samsing, J
  last_name: Samsing
- first_name: M
  full_name: O'Dowd, M
  last_name: O'Dowd
- first_name: B
  full_name: Kocsis, B
  last_name: Kocsis
- first_name: S
  full_name: Endlich, S
  last_name: Endlich
citation:
  ama: Leigh NWC, Geller AM, McKernan B, et al. On the rate of black hole binary mergers
    in galactic nuclei due to dynamical hardening. <i>Monthly Notices of the Royal
    Astronomical Society</i>. 2017;474(4):5672-5683. doi:<a href="https://doi.org/10.1093/mnras/stx3134">10.1093/mnras/stx3134</a>
  apa: Leigh, N. W. C., Geller, A. M., McKernan, B., Ford, K. E. S., Mac Low, M.-M.,
    Bellovary, J., … Endlich, S. (2017). On the rate of black hole binary mergers
    in galactic nuclei due to dynamical hardening. <i>Monthly Notices of the Royal
    Astronomical Society</i>. Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx3134">https://doi.org/10.1093/mnras/stx3134</a>
  chicago: Leigh, N W C, A M Geller, B McKernan, K E S Ford, M-M Mac Low, J Bellovary,
    Zoltán Haiman, et al. “On the Rate of Black Hole Binary Mergers in Galactic Nuclei
    Due to Dynamical Hardening.” <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx3134">https://doi.org/10.1093/mnras/stx3134</a>.
  ieee: N. W. C. Leigh <i>et al.</i>, “On the rate of black hole binary mergers in
    galactic nuclei due to dynamical hardening,” <i>Monthly Notices of the Royal Astronomical
    Society</i>, vol. 474, no. 4. Oxford University Press, pp. 5672–5683, 2017.
  ista: Leigh NWC, Geller AM, McKernan B, Ford KES, Mac Low M-M, Bellovary J, Haiman
    Z, Lyra W, Samsing J, O’Dowd M, Kocsis B, Endlich S. 2017. On the rate of black
    hole binary mergers in galactic nuclei due to dynamical hardening. Monthly Notices
    of the Royal Astronomical Society. 474(4), 5672–5683.
  mla: Leigh, N. W. C., et al. “On the Rate of Black Hole Binary Mergers in Galactic
    Nuclei Due to Dynamical Hardening.” <i>Monthly Notices of the Royal Astronomical
    Society</i>, vol. 474, no. 4, Oxford University Press, 2017, pp. 5672–83, doi:<a
    href="https://doi.org/10.1093/mnras/stx3134">10.1093/mnras/stx3134</a>.
  short: N.W.C. Leigh, A.M. Geller, B. McKernan, K.E.S. Ford, M.-M. Mac Low, J. Bellovary,
    Z. Haiman, W. Lyra, J. Samsing, M. O’Dowd, B. Kocsis, S. Endlich, Monthly Notices
    of the Royal Astronomical Society 474 (2017) 5672–5683.
date_created: 2024-09-05T14:16:03Z
date_published: 2017-12-05T00:00:00Z
date_updated: 2024-09-24T10:21:37Z
day: '05'
doi: 10.1093/mnras/stx3134
extern: '1'
external_id:
  arxiv:
  - '1711.10494'
intvolume: '       474'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: ' https://doi.org/10.48550/arXiv.1711.10494'
month: '12'
oa: 1
oa_version: Preprint
page: 5672-5683
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: On the rate of black hole binary mergers in galactic nuclei due to dynamical
  hardening
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 474
year: '2017'
...
---
_id: '17633'
abstract:
- lang: eng
  text: 'Using few-body simulations, we investigate the evolution of supermassive
    black holes (SMBHs) in galaxies (M* = 1010–1012 M⊙ at z = 0) at 0 < z < 4. Following
    galaxy merger trees from the Millennium simulation, we model BH mergers with two
    extreme binary decay scenarios for the ‘hard binary’ stage: a full or an empty
    loss cone. These two models should bracket the true evolution, and allow us to
    separately explore the role of dynamical friction and that of multibody BH interactions
    on BH mergers. Using the computed merger rates, we infer the stochastic gravitational
    wave background (GWB). Our dynamical approach is a first attempt to study the
    dynamical evolution of multiple SMBHs in the host galaxies undergoing mergers
    with various mass ratios (10−4 < q* < 1). Our main result demonstrates that SMBH
    binaries are able to merge in both scenarios. In the empty loss cone case, we
    find that BHs merge via multibody interactions, avoiding the ‘final parsec’ problem,
    and entering the pulsar timing arrays band with substantial orbital eccentricity.
    Our full loss cone treatment, albeit more approximate, suggests that the eccentricity
    becomes even higher when GWs become dominant, leading to rapid coalescences (binary
    lifetime ≲1 Gyr). Despite the lower merger rates in the empty loss cone case,
    due to their higher mass ratios and lower redshifts, the GWB in the full/empty
    loss cone models are comparable (0.70 × 10−15 and 0.53 × 10−15 at a frequency
    of 1 yr−1, respectively). Finally, we compute the effects of high eccentricities
    on the GWB spectrum.'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Taeho
  full_name: Ryu, Taeho
  last_name: Ryu
- first_name: Rosalba
  full_name: Perna, Rosalba
  last_name: Perna
- first_name: Zoltán
  full_name: Haiman, Zoltán
  id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
  last_name: Haiman
- first_name: Jeremiah P.
  full_name: Ostriker, Jeremiah P.
  last_name: Ostriker
- first_name: Nicholas C.
  full_name: Stone, Nicholas C.
  last_name: Stone
citation:
  ama: 'Ryu T, Perna R, Haiman Z, Ostriker JP, Stone NC. Interactions between multiple
    supermassive black holes in galactic nuclei: A solution to the final parsec problem.
    <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;473(3):3410-3433.
    doi:<a href="https://doi.org/10.1093/mnras/stx2524">10.1093/mnras/stx2524</a>'
  apa: 'Ryu, T., Perna, R., Haiman, Z., Ostriker, J. P., &#38; Stone, N. C. (2017).
    Interactions between multiple supermassive black holes in galactic nuclei: A solution
    to the final parsec problem. <i>Monthly Notices of the Royal Astronomical Society</i>.
    Oxford University Press. <a href="https://doi.org/10.1093/mnras/stx2524">https://doi.org/10.1093/mnras/stx2524</a>'
  chicago: 'Ryu, Taeho, Rosalba Perna, Zoltán Haiman, Jeremiah P. Ostriker, and Nicholas
    C. Stone. “Interactions between Multiple Supermassive Black Holes in Galactic
    Nuclei: A Solution to the Final Parsec Problem.” <i>Monthly Notices of the Royal
    Astronomical Society</i>. Oxford University Press, 2017. <a href="https://doi.org/10.1093/mnras/stx2524">https://doi.org/10.1093/mnras/stx2524</a>.'
  ieee: 'T. Ryu, R. Perna, Z. Haiman, J. P. Ostriker, and N. C. Stone, “Interactions
    between multiple supermassive black holes in galactic nuclei: A solution to the
    final parsec problem,” <i>Monthly Notices of the Royal Astronomical Society</i>,
    vol. 473, no. 3. Oxford University Press, pp. 3410–3433, 2017.'
  ista: 'Ryu T, Perna R, Haiman Z, Ostriker JP, Stone NC. 2017. Interactions between
    multiple supermassive black holes in galactic nuclei: A solution to the final
    parsec problem. Monthly Notices of the Royal Astronomical Society. 473(3), 3410–3433.'
  mla: 'Ryu, Taeho, et al. “Interactions between Multiple Supermassive Black Holes
    in Galactic Nuclei: A Solution to the Final Parsec Problem.” <i>Monthly Notices
    of the Royal Astronomical Society</i>, vol. 473, no. 3, Oxford University Press,
    2017, pp. 3410–33, doi:<a href="https://doi.org/10.1093/mnras/stx2524">10.1093/mnras/stx2524</a>.'
  short: T. Ryu, R. Perna, Z. Haiman, J.P. Ostriker, N.C. Stone, Monthly Notices of
    the Royal Astronomical Society 473 (2017) 3410–3433.
date_created: 2024-09-05T14:16:56Z
date_published: 2017-09-27T00:00:00Z
date_updated: 2024-09-24T11:14:57Z
day: '27'
doi: 10.1093/mnras/stx2524
extern: '1'
external_id:
  arxiv:
  - '1709.06501'
intvolume: '       473'
issue: '3'
language:
- iso: eng
main_file_link:
- open_access: '1'
  url: ' https://doi.org/10.48550/arXiv.1709.06501'
month: '09'
oa: 1
oa_version: Preprint
page: 3410-3433
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
  issn:
  - 0035-8711
  - 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Interactions between multiple supermassive black holes in galactic nuclei:
  A solution to the final parsec problem'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 473
year: '2017'
...