---
_id: '17615'
abstract:
- lang: eng
text: Graham et al. have detected a 5.2 yr periodic optical variability of the quasar
PG 1302-102 at redshift z = 0.3, which they interpret as the redshifted orbital
period (1 + z)tbin of a putative supermassive black hole binary (SMBHB). Here,
we consider the implications of a 3–8 times shorter orbital period, suggested
by hydrodynamical simulations of circumbinary discs (CBDs) with nearly equal-mass
SMBHBs (q ≡ M2/M1 ≳ 0.3). With the corresponding 2–4 times tighter binary separation,
PG 1302 would be undergoing gravitational wave dominated inspiral, and serve as
a proof that the BHs can be fuelled and produce bright emission even in this late
stage of the merger. The expected fraction of binaries with the shorter tbin,
among bright quasars, would be reduced by one to two orders of magnitude, compared
to the 5.2 yr period, in better agreement with the rarity of candidates reported
by Graham et al. Finally, shorter periods would imply higher binary speeds, possibly
imprinting periodicity on the light curves from relativistic beaming, as well
as measurable relativistic effects on the Fe K α line. The CBD model predicts
additional periodic variability on time-scales of tbin and ≈0.5tbin, as well as
periodic variation of broad line widths and offsets relative to the narrow lines,
which are consistent with the observations. Future observations will be able to
test these predictions and hence the binary+CBD hypothesis for PG 1302.
article_processing_charge: No
article_type: original
author:
- first_name: D. J.
full_name: D'Orazio, D. J.
last_name: D'Orazio
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: P.
full_name: Duffell, P.
last_name: Duffell
- first_name: B. D.
full_name: Farris, B. D.
last_name: Farris
- first_name: A. I.
full_name: MacFadyen, A. I.
last_name: MacFadyen
citation:
ama: D’Orazio DJ, Haiman Z, Duffell P, Farris BD, MacFadyen AI. A reduced orbital
period for the supermassive black hole binary candidate in the quasar PG 1302-102?
Monthly Notices of the Royal Astronomical Society. 2015;452(3):2540-2545.
doi:10.1093/mnras/stv1457
apa: D’Orazio, D. J., Haiman, Z., Duffell, P., Farris, B. D., & MacFadyen, A.
I. (2015). A reduced orbital period for the supermassive black hole binary candidate
in the quasar PG 1302-102? Monthly Notices of the Royal Astronomical Society.
Oxford University Press. https://doi.org/10.1093/mnras/stv1457
chicago: D’Orazio, D. J., Zoltán Haiman, P. Duffell, B. D. Farris, and A. I. MacFadyen.
“A Reduced Orbital Period for the Supermassive Black Hole Binary Candidate in
the Quasar PG 1302-102?” Monthly Notices of the Royal Astronomical Society.
Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv1457.
ieee: D. J. D’Orazio, Z. Haiman, P. Duffell, B. D. Farris, and A. I. MacFadyen,
“A reduced orbital period for the supermassive black hole binary candidate in
the quasar PG 1302-102?,” Monthly Notices of the Royal Astronomical Society,
vol. 452, no. 3. Oxford University Press, pp. 2540–2545, 2015.
ista: D’Orazio DJ, Haiman Z, Duffell P, Farris BD, MacFadyen AI. 2015. A reduced
orbital period for the supermassive black hole binary candidate in the quasar
PG 1302-102? Monthly Notices of the Royal Astronomical Society. 452(3), 2540–2545.
mla: D’Orazio, D. J., et al. “A Reduced Orbital Period for the Supermassive Black
Hole Binary Candidate in the Quasar PG 1302-102?” Monthly Notices of the Royal
Astronomical Society, vol. 452, no. 3, Oxford University Press, 2015, pp.
2540–45, doi:10.1093/mnras/stv1457.
short: D.J. D’Orazio, Z. Haiman, P. Duffell, B.D. Farris, A.I. MacFadyen, Monthly
Notices of the Royal Astronomical Society 452 (2015) 2540–2545.
date_created: 2024-09-05T13:31:30Z
date_published: 2015-07-24T00:00:00Z
date_updated: 2024-09-24T07:58:52Z
day: '24'
doi: 10.1093/mnras/stv1457
extern: '1'
fulldoi: https://doi.org/10.1093/mnras/stv1457
intvolume: ' 452'
issue: '3'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stv1457
month: '07'
oa: 1
oa_version: Published Version
page: 2540-2545
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 reduced orbital period for the supermassive black hole binary candidate in
the quasar PG 1302-102?
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 452
year: '2015'
...
---
_id: '17641'
abstract:
- lang: eng
text: 'In order to elucidate the origin of spin in both dark matter and baryons
in galaxies, we have performed hydrodynamical simulations from cosmological initial
conditions. We study atomic cooling haloes in the redshift range 100>z>9 with
masses of order 109M⊙ at redshift z=10. We assume that the gas has primordial
composition and that H2-cooling and prior star-formation in the haloes have been
suppressed. We present a comprehensive analysis of the gas and dark matter properties
of four halos with very low (λ≈0.01), low (λ≈0.04), high (λ≈0.06) and very high
(λ≈0.1) spin parameter. Our main conclusion is that the spin orientation and magnitude
is initially well described by tidal torque linear theory, but later on is determined
by the merging and accretion history of each halo. We provide evidence that the
topology of the merging region, i.e. the number of colliding filaments, gives
an accurate prediction for the spin of dark matter and gas: halos at the center
of knots will have low spin while those in the center of filaments will have high
spin. The spin of a halo is given by λ≈0.05×(7.6/numberoffilaments)^5.1'
article_processing_charge: No
article_type: original
author:
- first_name: Joaquin
full_name: Prieto, Joaquin
last_name: Prieto
- first_name: Raul
full_name: Jimenez, Raul
last_name: Jimenez
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Roberto E.
full_name: González, Roberto E.
last_name: González
citation:
ama: 'Prieto J, Jimenez R, Haiman Z, González RE. The origin of spin in galaxies:
Clues from simulations of atomic cooling haloes. Monthly Notices of the Royal
Astronomical Society. 2015;452(1):784-802. doi:10.1093/mnras/stv1234'
apa: 'Prieto, J., Jimenez, R., Haiman, Z., & González, R. E. (2015). The origin
of spin in galaxies: Clues from simulations of atomic cooling haloes. Monthly
Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stv1234'
chicago: 'Prieto, Joaquin, Raul Jimenez, Zoltán Haiman, and Roberto E. González.
“The Origin of Spin in Galaxies: Clues from Simulations of Atomic Cooling Haloes.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2015. https://doi.org/10.1093/mnras/stv1234.'
ieee: 'J. Prieto, R. Jimenez, Z. Haiman, and R. E. González, “The origin of spin
in galaxies: Clues from simulations of atomic cooling haloes,” Monthly Notices
of the Royal Astronomical Society, vol. 452, no. 1. Oxford University Press,
pp. 784–802, 2015.'
ista: 'Prieto J, Jimenez R, Haiman Z, González RE. 2015. The origin of spin in galaxies:
Clues from simulations of atomic cooling haloes. Monthly Notices of the Royal
Astronomical Society. 452(1), 784–802.'
mla: 'Prieto, Joaquin, et al. “The Origin of Spin in Galaxies: Clues from Simulations
of Atomic Cooling Haloes.” Monthly Notices of the Royal Astronomical Society,
vol. 452, no. 1, Oxford University Press, 2015, pp. 784–802, doi:10.1093/mnras/stv1234.'
short: J. Prieto, R. Jimenez, Z. Haiman, R.E. González, Monthly Notices of the Royal
Astronomical Society 452 (2015) 784–802.
date_created: 2024-09-06T07:18:53Z
date_published: 2015-07-08T00:00:00Z
date_updated: 2024-09-24T11:52:00Z
day: '08'
doi: 10.1093/mnras/stv1234
extern: '1'
fulldoi: https://doi.org/10.1093/mnras/stv1234
intvolume: ' 452'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stv1234
month: '07'
oa: 1
oa_version: Published Version
page: 784-802
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
issn:
- 0035-8711
- 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'The origin of spin in galaxies: Clues from simulations of atomic cooling haloes'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 452
year: '2015'
...
---
_id: '17663'
abstract:
- lang: eng
text: Recently, Planck measured a value of the cosmic microwave background (CMB)
optical depth due to electron scattering of τ=0.066±0.016. Here we show that this
low value leaves essentially no room for an early partial reionisation of the
intergalactic medium (IGM) by high-redshift Population III (Pop III) stars, expected
to have formed in low-mass minihaloes. We perform semi-analytic calculations of
reionisation which include the contribution from Pop II stars in atomic cooling
haloes, calibrated with high-redshift galaxy observations, and Pop III stars in
minihaloes with feedback due to Lyman-Werner (LW) radiation and metal enrichment.
We find that without LW feedback or prompt metal enrichment (and assuming a minihalo
escape fraction of 0.5) the Pop III star formation efficiency cannot exceed ∼a
few×10−4, without violating the constraints set by Planck data. This excludes
massive Pop III star formation in typical 106M⊙ minihaloes. Including LW feedback
and metal enrichment alleviates this tension, allowing large Pop III stars to
form early on before they are quenched by feedback. We find that the total density
of Pop III stars formed across cosmic time is ≲104−5 M⊙ Mpc−3 and does not depend
strongly on the feedback prescription adopted. Additionally, we perform a simple
estimate of the possible impact on reionisation of X-rays produced by accretion
onto black hole remnants of Pop III stars. We find that unless the accretion duty
cycle is very low (≲0.01), this could lead to an optical depth inconsistent with
Planck.
article_processing_charge: No
article_type: original
arxiv: 1
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. Limits on population III star formation in minihaloes
implied by Planck. Monthly Notices of the Royal Astronomical Society. 2015;453(4):4457-4467.
doi:10.1093/mnras/stv1941
apa: Visbal, E., Haiman, Z., & Bryan, G. L. (2015). Limits on population III
star formation in minihaloes implied by Planck. Monthly Notices of the Royal
Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stv1941
chicago: Visbal, Eli, Zoltán Haiman, and Greg L. Bryan. “Limits on Population III
Star Formation in Minihaloes Implied by Planck.” Monthly Notices of the Royal
Astronomical Society. Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv1941.
ieee: E. Visbal, Z. Haiman, and G. L. Bryan, “Limits on population III star formation
in minihaloes implied by Planck,” Monthly Notices of the Royal Astronomical
Society, vol. 453, no. 4. Oxford University Press, pp. 4457–4467, 2015.
ista: Visbal E, Haiman Z, Bryan GL. 2015. Limits on population III star formation
in minihaloes implied by Planck. Monthly Notices of the Royal Astronomical Society.
453(4), 4457–4467.
mla: Visbal, Eli, et al. “Limits on Population III Star Formation in Minihaloes
Implied by Planck.” Monthly Notices of the Royal Astronomical Society,
vol. 453, no. 4, Oxford University Press, 2015, pp. 4457–67, doi:10.1093/mnras/stv1941.
short: E. Visbal, Z. Haiman, G.L. Bryan, Monthly Notices of the Royal Astronomical
Society 453 (2015) 4457–4467.
date_created: 2024-09-06T07:40:38Z
date_published: 2015-09-16T00:00:00Z
date_updated: 2024-09-25T07:32:20Z
day: '16'
doi: 10.1093/mnras/stv1941
extern: '1'
external_id:
arxiv:
- '1505.06359'
fulldoi: https://doi.org/10.1093/mnras/stv1941
intvolume: ' 453'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: ' https://doi.org/10.48550/arXiv.1505.06359'
month: '09'
oa: 1
oa_version: Preprint
page: 4457-4467
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: Limits on population III star formation in minihaloes implied by Planck
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 453
year: '2015'
...
---
_id: '17685'
abstract:
- lang: eng
text: We propose an observational test for gravitationally recoiling supermassive
black holes (BHs) in active galactic nuclei, based on a correlation between the
velocities of BHs relative to their host galaxies, |\Delta v|, and their obscuring
dust column densities, \Sigma_{dust} (both measured along the line of sight).
We use toy models for the distribution of recoil velocities, BH trajectories,
and the geometry of obscuring dust tori in galactic centres, to simulate 2.5x10^5
random observations of recoiling quasars. BHs with recoil velocities comparable
to the escape velocity from the galactic centre remain bound to the nucleus, and
do not fully settle back to the centre of the torus due to dynamical friction
in a typical quasar lifetime. We find that |\Delta v| and \Sigma_ {dust} for these
BHs are positively correlated. For obscured (\Sigma_{dust}>0) and for partially
obscured (0<\Sigma_{dust}<~2.3 g/m^2) quasars with |\Delta v|>=45 km/s, the sample
correlation coefficient between log10(|\Delta v|) and \Sigma_{dust} is r_{45}
= 0.28+/-0.02 and r_{45} = 0.13+/-0.02, respectively. Allowing for random +/-100
km/s errors in |\Delta v| unrelated to the recoil dilutes the correlation for
the partially obscured quasars to r_{45} = 0.026+/-0.004 measured between |\Delta
v| and \Sigma_{dust}. A random sample of >~3,500 obscured quasars with |\Delta
v|>=45 km/s would allow rejection of the no-correlation hypothesis with 3 sigma
significance 95% of the time. Finally, we find that the fraction of obscured quasars,
F_{obs}(|\Delta v|), decreases with |\Delta v| from F_{obs}(<10 km/s)>~0.8 to
F_{obs}(>10^3 km/s)<~0.4. This predicted trend can be compared to the observed
fraction of type II quasars, and can further test combinations of recoil, trajectory,
and dust torus models.
article_processing_charge: No
article_type: original
author:
- first_name: P.
full_name: Raffai, P.
last_name: Raffai
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Z.
full_name: Frei, Z.
last_name: Frei
citation:
ama: Raffai P, Haiman Z, Frei Z. A statistical method to search for recoiling supermassive
black holes in active galactic nuclei. Monthly Notices of the Royal Astronomical
Society. 2015;455(1):484-492. doi:10.1093/mnras/stv2371
apa: Raffai, P., Haiman, Z., & Frei, Z. (2015). A statistical method to search
for recoiling supermassive black holes in active galactic nuclei. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stv2371
chicago: Raffai, P., Zoltán Haiman, and Z. Frei. “A Statistical Method to Search
for Recoiling Supermassive Black Holes in Active Galactic Nuclei.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2015.
https://doi.org/10.1093/mnras/stv2371.
ieee: P. Raffai, Z. Haiman, and Z. Frei, “A statistical method to search for recoiling
supermassive black holes in active galactic nuclei,” Monthly Notices of the
Royal Astronomical Society, vol. 455, no. 1. Oxford University Press, pp.
484–492, 2015.
ista: Raffai P, Haiman Z, Frei Z. 2015. A statistical method to search for recoiling
supermassive black holes in active galactic nuclei. Monthly Notices of the Royal
Astronomical Society. 455(1), 484–492.
mla: Raffai, P., et al. “A Statistical Method to Search for Recoiling Supermassive
Black Holes in Active Galactic Nuclei.” Monthly Notices of the Royal Astronomical
Society, vol. 455, no. 1, Oxford University Press, 2015, pp. 484–92, doi:10.1093/mnras/stv2371.
short: P. Raffai, Z. Haiman, Z. Frei, Monthly Notices of the Royal Astronomical
Society 455 (2015) 484–492.
date_created: 2024-09-06T08:20:30Z
date_published: 2015-11-02T00:00:00Z
date_updated: 2024-09-25T09:18:47Z
day: '02'
doi: 10.1093/mnras/stv2371
extern: '1'
fulldoi: https://doi.org/10.1093/mnras/stv2371
intvolume: ' 455'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stv2371
month: '11'
oa: 1
oa_version: Published Version
page: 484-492
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 statistical method to search for recoiling supermassive black holes in active
galactic nuclei
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 455
year: '2015'
...
---
_id: '17694'
abstract:
- lang: eng
text: Constraining the properties of Population III (Pop III) stars will be very
challenging because they reside in small galaxies at high redshift which will
be difficult to directly detect. In this paper, we suggest that intensity mapping
may be a promising method to study Pop III stars. Intensity mapping is a technique
proposed to measure large-scale fluctuations of galaxy line emission in three
dimensions without resolving individual sources. This technique is well suited
for observing many faint galaxies because it can measure their cumulative emission
even if they cannot be directly detected. We focus on intensity mapping of He
ii recombination lines. These lines are much stronger in Pop III stars than Pop
II stars because the harder spectra of Pop III stars are expected to produce many
He ii ionizing photons. Measuring the He ii 1640 Å intensity mapping signal, along
with the signals from other lines such as Lyα, Hα, and metal lines, could give
constraints on the initial mass function (IMF) and star formation rate density
of Pop III stars as a function of redshift. To demonstrate the feasibility of
these observations, we estimate the strength of the Pop III He ii 1640 Å intensity
mapping signal from z = 10–20. We show that at z ≈ 10, the signal could be measured
accurately by two different hypothetical future instruments, one which cross-correlates
He ii 1640 Å with CO(1–0) line emission from galaxies and the other with 21 cm
emission from the intergalactic medium.
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. Looking for Population III stars with He ii line
intensity mapping. Monthly Notices of the Royal Astronomical Society. 2015;450(3):2506-2513.
doi:10.1093/mnras/stv785
apa: Visbal, E., Haiman, Z., & Bryan, G. L. (2015). Looking for Population III
stars with He ii line intensity mapping. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stv785
chicago: Visbal, Eli, Zoltán Haiman, and Greg L. Bryan. “Looking for Population
III Stars with He Ii Line Intensity Mapping.” Monthly Notices of the Royal
Astronomical Society. Oxford University Press, 2015. https://doi.org/10.1093/mnras/stv785.
ieee: E. Visbal, Z. Haiman, and G. L. Bryan, “Looking for Population III stars with
He ii line intensity mapping,” Monthly Notices of the Royal Astronomical Society,
vol. 450, no. 3. Oxford University Press, pp. 2506–2513, 2015.
ista: Visbal E, Haiman Z, Bryan GL. 2015. Looking for Population III stars with
He ii line intensity mapping. Monthly Notices of the Royal Astronomical Society.
450(3), 2506–2513.
mla: Visbal, Eli, et al. “Looking for Population III Stars with He Ii Line Intensity
Mapping.” Monthly Notices of the Royal Astronomical Society, vol. 450,
no. 3, Oxford University Press, 2015, pp. 2506–13, doi:10.1093/mnras/stv785.
short: E. Visbal, Z. Haiman, G.L. Bryan, Monthly Notices of the Royal Astronomical
Society 450 (2015) 2506–2513.
date_created: 2024-09-06T08:40:33Z
date_published: 2015-05-06T00:00:00Z
date_updated: 2024-09-25T10:05:24Z
day: '06'
doi: 10.1093/mnras/stv785
extern: '1'
fulldoi: https://doi.org/10.1093/mnras/stv785
intvolume: ' 450'
issue: '3'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stv785
month: '05'
oa: 1
oa_version: Published Version
page: 2506-2513
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: Looking for Population III stars with He ii line intensity mapping
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 450
year: '2015'
...
---
_id: '11582'
abstract:
- lang: eng
text: We have observed a sample of typical z ∼ 1 star-forming galaxies, selected
from the HiZELS survey, with the new K-band Multi-Object Spectrograph (KMOS) near-infrared,
multi-integral field unit instrument on the Very Large Telescope (VLT), in order
to obtain their dynamics and metallicity gradients. The majority of our galaxies
have a metallicity gradient consistent with being flat or negative (i.e. higher
metallicity cores than outskirts). Intriguingly, we find a trend between metallicity
gradient and specific star formation rate (sSFR), such that galaxies with a high
sSFR tend to have relatively metal poor centres, a result which is strengthened
when combined with data sets from the literature. This result appears to explain
the discrepancies reported between different high-redshift studies and varying
claims for evolution. From a galaxy evolution perspective, the trend we see would
mean that a galaxy's sSFR is governed by the amount of metal-poor gas that can
be funnelled into its core, triggered either by merging or through efficient accretion.
In fact, merging may play a significant role as it is the starburst galaxies at
all epochs, which have the more positive metallicity gradients. Our results may
help to explain the origin of the fundamental metallicity relation, in which galaxies
at a fixed mass are observed to have lower metallicities at higher star formation
rates, especially if the metallicity is measured in an aperture encompassing only
the central regions of the galaxy. Finally, we note that this study demonstrates
the power of KMOS as an efficient instrument for large-scale resolved galaxy surveys.
acknowledgement: First, we acknowledge the referee for their comments, which have
improved the clarity of this paper. JPS and IRS acknowledge support from STFC (ST/I001573/1).
IRS also acknowledges support from the ERC Advanced Investigator programme DUSTYGAL
and a Royal Society/Wolfson Merit Award. DS acknowledges financial support from
NWO through a Veni fellowship and from FCT through the award of an FCT-IF starting
grant. PNB acknowledges STFC for financial support.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: John P.
full_name: Stott, John P.
last_name: Stott
- first_name: David
full_name: Sobral, David
last_name: Sobral
- first_name: A. M.
full_name: Swinbank, A. M.
last_name: Swinbank
- first_name: Ian
full_name: Smail, Ian
last_name: Smail
- first_name: Richard
full_name: Bower, Richard
last_name: Bower
- first_name: Philip N.
full_name: Best, Philip N.
last_name: Best
- first_name: Ray M.
full_name: Sharples, Ray M.
last_name: Sharples
- first_name: James E.
full_name: Geach, James E.
last_name: Geach
- first_name: Jorryt J
full_name: Matthee, Jorryt J
id: 7439a258-f3c0-11ec-9501-9df22fe06720
last_name: Matthee
orcid: 0000-0003-2871-127X
citation:
ama: Stott JP, Sobral D, Swinbank AM, et al. A relationship between specific star
formation rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS.
Monthly Notices of the Royal Astronomical Society. 2014;443(3):2695-2704.
doi:10.1093/mnras/stu1343
apa: Stott, J. P., Sobral, D., Swinbank, A. M., Smail, I., Bower, R., Best, P. N.,
… Matthee, J. J. (2014). A relationship between specific star formation rate and
metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stu1343
chicago: Stott, John P., David Sobral, A. M. Swinbank, Ian Smail, Richard Bower,
Philip N. Best, Ray M. Sharples, James E. Geach, and Jorryt J Matthee. “A Relationship
between Specific Star Formation Rate and Metallicity Gradient within z ∼ 1 Galaxies
from KMOS-HiZELS.” Monthly Notices of the Royal Astronomical Society. Oxford
University Press, 2014. https://doi.org/10.1093/mnras/stu1343.
ieee: J. P. Stott et al., “A relationship between specific star formation
rate and metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS,” Monthly
Notices of the Royal Astronomical Society, vol. 443, no. 3. Oxford University
Press, pp. 2695–2704, 2014.
ista: Stott JP, Sobral D, Swinbank AM, Smail I, Bower R, Best PN, Sharples RM, Geach
JE, Matthee JJ. 2014. A relationship between specific star formation rate and
metallicity gradient within z ∼ 1 galaxies from KMOS-HiZELS. Monthly Notices of
the Royal Astronomical Society. 443(3), 2695–2704.
mla: Stott, John P., et al. “A Relationship between Specific Star Formation Rate
and Metallicity Gradient within z ∼ 1 Galaxies from KMOS-HiZELS.” Monthly Notices
of the Royal Astronomical Society, vol. 443, no. 3, Oxford University Press,
2014, pp. 2695–704, doi:10.1093/mnras/stu1343.
short: J.P. Stott, D. Sobral, A.M. Swinbank, I. Smail, R. Bower, P.N. Best, R.M.
Sharples, J.E. Geach, J.J. Matthee, Monthly Notices of the Royal Astronomical
Society 443 (2014) 2695–2704.
date_created: 2022-07-14T12:16:10Z
date_published: 2014-09-21T00:00:00Z
date_updated: 2022-08-19T08:27:25Z
day: '21'
doi: 10.1093/mnras/stu1343
extern: '1'
external_id:
arxiv:
- '1407.1047'
fulldoi: https://doi.org/10.1093/mnras/stu1343
intvolume: ' 443'
issue: '3'
keyword:
- Space and Planetary Science
- Astronomy and Astrophysics
- 'galaxies: abundances'
- 'galaxies: evolution'
- 'galaxies: kinematics and dynamics'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://arxiv.org/abs/1407.1047
month: '09'
oa: 1
oa_version: Preprint
page: 2695-2704
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 relationship between specific star formation rate and metallicity gradient
within z ∼ 1 galaxies from KMOS-HiZELS
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 443
year: '2014'
...
---
_id: '11583'
abstract:
- lang: eng
text: 'Candidate galaxies at redshifts of z ∼ 10 are now being found in extremely
deep surveys, probing very small areas. As a consequence, candidates are very
faint, making spectroscopic confirmation practically impossible. In order to overcome
such limitations, we have undertaken the CF-HiZELS survey, which is a large-area,
medium-depth near-infrared narrow-band survey targeted at z = 8.8 Lyman α (Lyα)
emitters (LAEs) and covering 10 deg2 in part of the SSA22 field with the Canada–France–Hawaii
Telescope (CFHT). We surveyed a comoving volume of 4.7 × 106 Mpc3 to a Lyα luminosity
limit of 6.3 × 1043舁erg舁s−1. We look for Lyα candidates by applying the following
criteria: (i) clear emission-line source, (ii) no optical detections (ugriz from
CFHTLS), (iii) no visible detection in the optical stack (ugriz > 27), (iv) visually
checked reliable NBJ and J detections and (v) J − K ≤ 0. We compute photometric
redshifts and remove a significant amount of dusty lower redshift line-emitters
at z ∼ 1.4 or 2.2. A total of 13 Lyα candidates were found, of which two are marked
as strong candidates, but the majority have very weak constraints on their spectral
energy distributions. Using follow-up observations with SINFONI/VLT, we are able
to exclude the most robust candidates as LAEs. We put a strong constraint on the
Lyα luminosity function at z ∼ 9 and make realistic predictions for ongoing and
future surveys. Our results show that surveys for the highest redshift LAEs are
susceptible of multiple contaminations and that spectroscopic follow-up is absolutely
necessary.'
acknowledgement: We thank the anonymous referee for the comments and suggestions which
improved both the quality and clarity of this work. DS acknowledges financial support
from the Netherlands Organisation for Scientific Research (NWO) through a Veni fellowship.
IRS acknowledges support from STFC (ST/I001573/1), a Leverhulme Fellowship, the
ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson
Merit Award. PNB acknowledges support from the Leverhulme Trust. JWK acknowledges
the support from the Creative Research Initiative Program, no. 2008- 0060544, of
the National Research Foundation of Korea (NRF) funded by the Korean government
(MSIP). JPUF and BMJ acknowledge support from the ERC-StG grant EGGS-278202. The
Dark Cosmology Centre is funded by the Danish National Research Foundation. This
work is based in part on data obtained as part of the UKIRT Infrared Deep Sky Survey.
Based on observations obtained with MegaPrime/MegaCam, a joint project of CFHT and
CEA/IRFU, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the
National Research Council (NRC) of Canada, the Institut National des Science de
l’Univers of the Centre National de la Recherche Scientifique (CNRS) of France and
the University of Hawaii. This work is based in part on data products produced at
Terapix available at the Canadian Astronomy Data Centre as part of the Canada-France-Hawaii
Telescope Legacy Survey, a collaborative project of NRC and CNRS. This work was
only possible due to OPTICON/FP7 and the access that it granted to the CFHT telescope.
The authors also wish to acknowledge the CFHTLS and UKIDSS surveys for their excellent
legacy and complementary value – without such high-quality data sets, this research
would not have been possible.
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: A. M.
full_name: Swinbank, A. M.
last_name: Swinbank
- first_name: Ian
full_name: Smail, Ian
last_name: Smail
- first_name: P. N.
full_name: Best, P. N.
last_name: Best
- first_name: Jae-Woo
full_name: Kim, Jae-Woo
last_name: Kim
- first_name: Marijn
full_name: Franx, Marijn
last_name: Franx
- first_name: Bo
full_name: Milvang-Jensen, Bo
last_name: Milvang-Jensen
- first_name: Johan
full_name: Fynbo, Johan
last_name: Fynbo
citation:
ama: 'Matthee JJ, Sobral D, Swinbank AM, et al. A 10 deg2 Lyman α survey at z=8.8
with spectroscopic follow-up: Strong constraints on the luminosity function and
implications for other surveys. Monthly Notices of the Royal Astronomical Society.
2014;440(3):2375-2387. doi:10.1093/mnras/stu392'
apa: 'Matthee, J. J., Sobral, D., Swinbank, A. M., Smail, I., Best, P. N., Kim,
J.-W., … Fynbo, J. (2014). A 10 deg2 Lyman α survey at z=8.8 with spectroscopic
follow-up: Strong constraints on the luminosity function and implications for
other surveys. Monthly Notices of the Royal Astronomical Society. Oxford
University Press. https://doi.org/10.1093/mnras/stu392'
chicago: 'Matthee, Jorryt J, David Sobral, A. M. Swinbank, Ian Smail, P. N. Best,
Jae-Woo Kim, Marijn Franx, Bo Milvang-Jensen, and Johan Fynbo. “A 10 Deg2 Lyman
α Survey at Z=8.8 with Spectroscopic Follow-up: Strong Constraints on the Luminosity
Function and Implications for Other Surveys.” Monthly Notices of the Royal
Astronomical Society. Oxford University Press, 2014. https://doi.org/10.1093/mnras/stu392.'
ieee: 'J. J. Matthee et al., “A 10 deg2 Lyman α survey at z=8.8 with spectroscopic
follow-up: Strong constraints on the luminosity function and implications for
other surveys,” Monthly Notices of the Royal Astronomical Society, vol.
440, no. 3. Oxford University Press, pp. 2375–2387, 2014.'
ista: 'Matthee JJ, Sobral D, Swinbank AM, Smail I, Best PN, Kim J-W, Franx M, Milvang-Jensen
B, Fynbo J. 2014. A 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up:
Strong constraints on the luminosity function and implications for other surveys.
Monthly Notices of the Royal Astronomical Society. 440(3), 2375–2387.'
mla: 'Matthee, Jorryt J., et al. “A 10 Deg2 Lyman α Survey at Z=8.8 with Spectroscopic
Follow-up: Strong Constraints on the Luminosity Function and Implications for
Other Surveys.” Monthly Notices of the Royal Astronomical Society, vol.
440, no. 3, Oxford University Press, 2014, pp. 2375–87, doi:10.1093/mnras/stu392.'
short: J.J. Matthee, D. Sobral, A.M. Swinbank, I. Smail, P.N. Best, J.-W. Kim, M.
Franx, B. Milvang-Jensen, J. Fynbo, Monthly Notices of the Royal Astronomical
Society 440 (2014) 2375–2387.
date_created: 2022-07-14T12:33:24Z
date_published: 2014-05-21T00:00:00Z
date_updated: 2024-10-14T11:37:28Z
day: '21'
doi: 10.1093/mnras/stu392
extern: '1'
external_id:
arxiv:
- '1402.6697'
fulldoi: https://doi.org/10.1093/mnras/stu392
intvolume: ' 440'
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/1402.6697
month: '05'
oa: 1
oa_version: Preprint
page: 2375-2387
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 10 deg2 Lyman α survey at z=8.8 with spectroscopic follow-up: Strong constraints
on the luminosity function and implications for other surveys'
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 440
year: '2014'
...
---
_id: '17614'
abstract:
- lang: eng
text: The first generation of stars produces a background of Lyman–Werner (LW) radiation
which can photodissociate molecular hydrogen, increasing the mass of dark matter
haloes required to host star formation. Previous studies have determined the critical
mass required for efficient molecular cooling with a constant LW background. However,
the true background is expected to increase rapidly at early times. Neglecting
this evolution could underestimate star formation in small haloes that may have
started to cool in the past when the LW intensity was much lower. Background evolution
is a large source of uncertainty in pre-reionization predictions of the cosmological
21cm signal, which can be observed with future radio telescopes. To address this,
we perform zero-dimensional one-zone calculations that follow the density, chemical
abundances, and temperature of gas in the central regions of dark matter haloes,
including hierarchical growth and an evolving LW background. We begin by studying
the physics of haloes subjected to a background that increases exponentially with
redshift. We find that when the intensity increases more slowly than JLW(z)∝10−z/5,
cooling in the past is a relatively small effect. We then self-consistently compute
the cosmological LW background over z = 15–50 and find that cooling in the past
due to an evolving background has a modest impact. Finally, we compare these results
to three-dimensional hydrodynamical cosmological simulations with varying LW histories.
While only a small number of haloes were simulated, the results are consistent
with our one-zone calculations.
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: Bryan
full_name: Terrazas, Bryan
last_name: Terrazas
- first_name: Greg L.
full_name: Bryan, Greg L.
last_name: Bryan
- first_name: Rennan
full_name: Barkana, Rennan
last_name: Barkana
citation:
ama: Visbal E, Haiman Z, Terrazas B, Bryan GL, Barkana R. High-redshift star formation
in a time-dependent Lyman–Werner background. Monthly Notices of the Royal Astronomical
Society. 2014;445(1):107-114. doi:10.1093/mnras/stu1710
apa: Visbal, E., Haiman, Z., Terrazas, B., Bryan, G. L., & Barkana, R. (2014).
High-redshift star formation in a time-dependent Lyman–Werner background. Monthly
Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stu1710
chicago: Visbal, Eli, Zoltán Haiman, Bryan Terrazas, Greg L. Bryan, and Rennan Barkana.
“High-Redshift Star Formation in a Time-Dependent Lyman–Werner Background.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2014.
https://doi.org/10.1093/mnras/stu1710.
ieee: E. Visbal, Z. Haiman, B. Terrazas, G. L. Bryan, and R. Barkana, “High-redshift
star formation in a time-dependent Lyman–Werner background,” Monthly Notices
of the Royal Astronomical Society, vol. 445, no. 1. Oxford University Press,
pp. 107–114, 2014.
ista: Visbal E, Haiman Z, Terrazas B, Bryan GL, Barkana R. 2014. High-redshift star
formation in a time-dependent Lyman–Werner background. Monthly Notices of the
Royal Astronomical Society. 445(1), 107–114.
mla: Visbal, Eli, et al. “High-Redshift Star Formation in a Time-Dependent Lyman–Werner
Background.” Monthly Notices of the Royal Astronomical Society, vol. 445,
no. 1, Oxford University Press, 2014, pp. 107–14, doi:10.1093/mnras/stu1710.
short: E. Visbal, Z. Haiman, B. Terrazas, G.L. Bryan, R. Barkana, Monthly Notices
of the Royal Astronomical Society 445 (2014) 107–114.
date_created: 2024-09-05T13:30:21Z
date_published: 2014-09-22T00:00:00Z
date_updated: 2024-09-24T07:43:44Z
day: '22'
doi: 10.1093/mnras/stu1710
extern: '1'
fulldoi: https://doi.org/10.1093/mnras/stu1710
intvolume: ' 445'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stu1710
month: '09'
oa: 1
oa_version: Published Version
page: 107-114
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: High-redshift star formation in a time-dependent Lyman–Werner background
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 445
year: '2014'
...
---
_id: '17637'
abstract:
- lang: eng
text: Supermassive stars (SMSs; >10^5 Msun) formed in the first protogalaxies with
virial temperature T_vir>10^4 K are expected to collapse into seeds of supermassive
black hole (SMBHs) in the high-redshift universe (z>7). Fragmentation of the primordial
gas is, however, a possible obstacle to SMS formation. We discuss the expected
properties of a compact, metal-free, marginally unstable nuclear protogalactic
disk, and the fate of the clumps formed in the disk by gravitational instability.
Interior to a characteristic radius R_f=few*10^{-2} pc, the disk fragments into
massive clumps with M_c~30 Msun. The clumps grow via accretion and migrate inward
rapidly on a timescale of ~10^4 yr, which is comparable or shorter than the Kelvin-Helmholz
time >10^4 yr. Some clumps may evolve to zero-age main sequence stars and halt
gas accretion by radiative feedback, but most of the clumps can migrate inward
and merge with the central protostar before forming massive stars. Moreover, we
found that dust-induced-fragmentation in metal-enriched gas does not modify these
conclusions unless Z> 3*10^{-4} Zsun, because clump migration below this metallicity
remains as rapid as in the primordial case. Our results suggest that fragmentation
of a compact, metal--poor disk can not prevent the formation of a SMS.
article_processing_charge: No
article_type: original
author:
- first_name: Kohei
full_name: Inayoshi, Kohei
last_name: Inayoshi
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
citation:
ama: Inayoshi K, Haiman Z. Does disc fragmentation prevent the formation of supermassive
stars in protogalaxies? Monthly Notices of the Royal Astronomical Society.
2014;445(2):1549-1557. doi:10.1093/mnras/stu1870
apa: Inayoshi, K., & Haiman, Z. (2014). Does disc fragmentation prevent the
formation of supermassive stars in protogalaxies? Monthly Notices of the Royal
Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stu1870
chicago: Inayoshi, Kohei, and Zoltán Haiman. “Does Disc Fragmentation Prevent the
Formation of Supermassive Stars in Protogalaxies?” Monthly Notices of the Royal
Astronomical Society. Oxford University Press, 2014. https://doi.org/10.1093/mnras/stu1870.
ieee: K. Inayoshi and Z. Haiman, “Does disc fragmentation prevent the formation
of supermassive stars in protogalaxies?,” Monthly Notices of the Royal Astronomical
Society, vol. 445, no. 2. Oxford University Press, pp. 1549–1557, 2014.
ista: Inayoshi K, Haiman Z. 2014. Does disc fragmentation prevent the formation
of supermassive stars in protogalaxies? Monthly Notices of the Royal Astronomical
Society. 445(2), 1549–1557.
mla: Inayoshi, Kohei, and Zoltán Haiman. “Does Disc Fragmentation Prevent the Formation
of Supermassive Stars in Protogalaxies?” Monthly Notices of the Royal Astronomical
Society, vol. 445, no. 2, Oxford University Press, 2014, pp. 1549–57, doi:10.1093/mnras/stu1870.
short: K. Inayoshi, Z. Haiman, Monthly Notices of the Royal Astronomical Society
445 (2014) 1549–1557.
date_created: 2024-09-06T07:15:08Z
date_published: 2014-10-09T00:00:00Z
date_updated: 2024-09-24T11:33:30Z
day: '09'
doi: 10.1093/mnras/stu1870
extern: '1'
fulldoi: https://doi.org/10.1093/mnras/stu1870
intvolume: ' 445'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stu1870
month: '10'
oa: 1
oa_version: Published Version
page: 1549-1557
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
issn:
- 1365-2966
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Does disc fragmentation prevent the formation of supermassive stars in protogalaxies?
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 445
year: '2014'
...
---
_id: '17642'
abstract:
- lang: eng
text: The presence of quasars at redshifts z > 6 indicates the existence of supermassive
black holes (SMBHs) as massive as a few times 10^9 Msun, challenging models for
SMBH formation. One pathway is through the direct collapse of gas in T_{vir} >
10^4 K halos; however, this requires the suppression of H_2 cooling to prevent
fragmentation. In this paper, we examine a proposed new mechanism for this suppression
which relies on cold-mode accretion flows leading to shocks at high densities
(n > 10^4 cm^{-3}) and temperatures (T > 10^4 K). In such gas, H_2 is efficiently
collisionally dissociated. We use high-resolution numerical simulations to test
this idea, demonstrating that such halos typically have lower temperature progenitors,
in which cooling is efficient. Those halos do show filamentary flows; however,
the gas shocks at or near the virial radius (at low densities), thus preventing
the proposed collisional mechanism from operating. We do find that, if we artificially
suppress H_2 formation with a high UV background, so as to allow gas in the halo
center to enter the high-temperature, high-density "zone of no return", it will
remain there even if the UV flux is turned off, collapsing to high density at
high temperature. Due to computational limitations, we simulated only three halos.
However, we demonstrate, using Monte Carlo calculations of 10^6 halo merger histories,
that a few rare halos could assemble rapidly enough to avoid efficient H_2 cooling
in all of their progenitor halos, provided that the UV background exceeds J_{21}
~ few at redshifts as high as z ~ 20
article_processing_charge: No
article_type: original
author:
- first_name: Ricardo
full_name: Fernandez, Ricardo
last_name: Fernandez
- first_name: Greg L.
full_name: Bryan, Greg L.
last_name: Bryan
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Miao
full_name: Li, Miao
last_name: Li
citation:
ama: 'Fernandez R, Bryan GL, Haiman Z, Li M. H2 suppression with shocking inflows:
Testing a pathway for supermassive black hole formation. Monthly Notices of
the Royal Astronomical Society. 2014;439(4):3798-3807. doi:10.1093/mnras/stu230'
apa: 'Fernandez, R., Bryan, G. L., Haiman, Z., & Li, M. (2014). H2 suppression
with shocking inflows: Testing a pathway for supermassive black hole formation.
Monthly Notices of the Royal Astronomical Society. Oxford University Press.
https://doi.org/10.1093/mnras/stu230'
chicago: 'Fernandez, Ricardo, Greg L. Bryan, Zoltán Haiman, and Miao Li. “H2 Suppression
with Shocking Inflows: Testing a Pathway for Supermassive Black Hole Formation.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2014. https://doi.org/10.1093/mnras/stu230.'
ieee: 'R. Fernandez, G. L. Bryan, Z. Haiman, and M. Li, “H2 suppression with shocking
inflows: Testing a pathway for supermassive black hole formation,” Monthly
Notices of the Royal Astronomical Society, vol. 439, no. 4. Oxford University
Press, pp. 3798–3807, 2014.'
ista: 'Fernandez R, Bryan GL, Haiman Z, Li M. 2014. H2 suppression with shocking
inflows: Testing a pathway for supermassive black hole formation. Monthly Notices
of the Royal Astronomical Society. 439(4), 3798–3807.'
mla: 'Fernandez, Ricardo, et al. “H2 Suppression with Shocking Inflows: Testing
a Pathway for Supermassive Black Hole Formation.” Monthly Notices of the Royal
Astronomical Society, vol. 439, no. 4, Oxford University Press, 2014, pp.
3798–807, doi:10.1093/mnras/stu230.'
short: R. Fernandez, G.L. Bryan, Z. Haiman, M. Li, Monthly Notices of the Royal
Astronomical Society 439 (2014) 3798–3807.
date_created: 2024-09-06T07:21:52Z
date_published: 2014-02-26T00:00:00Z
date_updated: 2024-09-24T11:56:43Z
day: '26'
doi: 10.1093/mnras/stu230
extern: '1'
fulldoi: https://doi.org/10.1093/mnras/stu230
intvolume: ' 439'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stu230
month: '02'
oa: 1
oa_version: Published Version
page: 3798-3807
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
issn:
- 1365-2966
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'H2 suppression with shocking inflows: Testing a pathway for supermassive black
hole formation'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 439
year: '2014'
...
---
_id: '17645'
abstract:
- lang: eng
text: The rapid decline in the number of strong Lyman Alpha (Lya) emitting galaxies
at z > 6 provides evidence for neutral hydrogen in the IGM, but is difficult to
explain with plausible models for reionization. We demonstrate that the observed
reduction in Lya flux from galaxies at z > 6 can be explained by evolution in
the escape fraction of ionizing photons, f_esc. We find that the median observed
drop in the fraction of galaxies showing strong Lya emission, as well as the observed
evolution of the Lya luminosity function both follow from a small increase in
f_esc of Delta f_esc ~ 0.1 from f_esc ~ 0.6 at z ~ 6. This high escape fraction
may be at odds with current constraints on the ionising photon escape fraction,
which favor smaller values of f_esc < 20%. However, models that invoke a redshift
evolution of f_ esc that is consistent with these constraints can suppress the
z~7 Lya flux to the observed level, if they also include a small evolution in
global neutral fraction of Delta x_HI ~ 0.2. Thus, an evolving escape fraction
of ionising photons can be a plausible part of the explanation for evolution in
the Lya emission of high redshift galaxies. More generally, our analysis also
shows that the drop in the Lya fraction is quantitatively consistent with the
observed evolution in the Lya luminosity functions of Lya Emitters.
article_processing_charge: No
article_type: original
author:
- first_name: Mark
full_name: Dijkstra, Mark
last_name: Dijkstra
- first_name: Stuart
full_name: Wyithe, Stuart
last_name: Wyithe
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Andrei
full_name: Mesinger, Andrei
last_name: Mesinger
- first_name: Laura
full_name: Pentericci, Laura
last_name: Pentericci
citation:
ama: Dijkstra M, Wyithe S, Haiman Z, Mesinger A, Pentericci L. Evolution in the
escape fraction of ionizing photons and the decline in strong Lyα emission from
z > 6 galaxies. Monthly Notices of the Royal Astronomical Society.
2014;440(4):3309-3316. doi:10.1093/mnras/stu531
apa: Dijkstra, M., Wyithe, S., Haiman, Z., Mesinger, A., & Pentericci, L. (2014).
Evolution in the escape fraction of ionizing photons and the decline in strong
Lyα emission from z > 6 galaxies. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stu531
chicago: Dijkstra, Mark, Stuart Wyithe, Zoltán Haiman, Andrei Mesinger, and Laura
Pentericci. “Evolution in the Escape Fraction of Ionizing Photons and the Decline
in Strong Lyα Emission from z > 6 Galaxies.” Monthly Notices of the Royal
Astronomical Society. Oxford University Press, 2014. https://doi.org/10.1093/mnras/stu531.
ieee: M. Dijkstra, S. Wyithe, Z. Haiman, A. Mesinger, and L. Pentericci, “Evolution
in the escape fraction of ionizing photons and the decline in strong Lyα emission
from z > 6 galaxies,” Monthly Notices of the Royal Astronomical Society,
vol. 440, no. 4. Oxford University Press, pp. 3309–3316, 2014.
ista: Dijkstra M, Wyithe S, Haiman Z, Mesinger A, Pentericci L. 2014. Evolution
in the escape fraction of ionizing photons and the decline in strong Lyα emission
from z > 6 galaxies. Monthly Notices of the Royal Astronomical Society. 440(4),
3309–3316.
mla: Dijkstra, Mark, et al. “Evolution in the Escape Fraction of Ionizing Photons
and the Decline in Strong Lyα Emission from z > 6 Galaxies.” Monthly Notices
of the Royal Astronomical Society, vol. 440, no. 4, Oxford University Press,
2014, pp. 3309–16, doi:10.1093/mnras/stu531.
short: M. Dijkstra, S. Wyithe, Z. Haiman, A. Mesinger, L. Pentericci, Monthly Notices
of the Royal Astronomical Society 440 (2014) 3309–3316.
date_created: 2024-09-06T07:24:26Z
date_published: 2014-04-17T00:00:00Z
date_updated: 2024-09-24T12:10:12Z
day: '17'
doi: 10.1093/mnras/stu531
extern: '1'
fulldoi: https://doi.org/10.1093/mnras/stu531
intvolume: ' 440'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stu531
month: '04'
oa: 1
oa_version: Published Version
page: 3309-3316
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
issn:
- 1365-2966
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Evolution in the escape fraction of ionizing photons and the decline in strong
Lyα emission from z > 6 galaxies
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 440
year: '2014'
...
---
_id: '17650'
abstract:
- lang: eng
text: High-redshift quasar observations imply that supermassive black holes (SMBHs)
larger than ∼109 M⊙ formed before z=6. That such large SMBHs formed so early in
the Universe remains an open theoretical problem. One possibility is that gas
in atomic cooling halos exposed to strong Lyman-Werner (LW) radiation forms 104−106
M⊙ supermassive stars which quickly collapse into black holes. We propose a scenario
for direct collapse black hole (DCBH) formation based on synchronized pairs of
pristine atomic cooling halos. We consider halos at very small separation with
one halo being a subhalo of the other. The first halo to surpass the atomic cooling
threshold forms stars. Soon after these stars are formed, the other halo reaches
the cooling threshold and due to its small distance from the newly formed galaxy,
is exposed to the critical LW intensity required to form a DCBH. The main advantage
of this scenario is that synchronization can potentially prevent photoevaporation
and metal pollution in DCBH-forming halos. Since the halos reach the atomic cooling
threshold at nearly the same time, the DCBH-forming halo is only exposed to ionizing
radiation for a brief period. Tight synchronization could allow the DCBH to form
before stars in the nearby galaxy reach the end of their lives and generate supernovae
winds. We use N-body simulations to estimate the abundance of DCBHs formed in
this way. The largest source of uncertainty in our estimate is the initial mass
function (IMF) of metal free stars formed in atomic cooling halos. We find that
even for tight synchronization, the density of DCBHs formed in this scenario could
explain the SMBHs implied by z=6 quasar observations. Metal pollution and photoevaporation
could potentially reduce the abundance of DCBHs below that required to explain
the observations in other models that rely on a high LW flux.
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. Direct collapse black hole formation from synchronized
pairs of atomic cooling haloes. Monthly Notices of the Royal Astronomical Society.
2014;445(1):1056-1063. doi:10.1093/mnras/stu1794
apa: Visbal, E., Haiman, Z., & Bryan, G. L. (2014). Direct collapse black hole
formation from synchronized pairs of atomic cooling haloes. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stu1794
chicago: Visbal, Eli, Zoltán Haiman, and Greg L. Bryan. “Direct Collapse Black Hole
Formation from Synchronized Pairs of Atomic Cooling Haloes.” Monthly Notices
of the Royal Astronomical Society. Oxford University Press, 2014. https://doi.org/10.1093/mnras/stu1794.
ieee: E. Visbal, Z. Haiman, and G. L. Bryan, “Direct collapse black hole formation
from synchronized pairs of atomic cooling haloes,” Monthly Notices of the Royal
Astronomical Society, vol. 445, no. 1. Oxford University Press, pp. 1056–1063,
2014.
ista: Visbal E, Haiman Z, Bryan GL. 2014. Direct collapse black hole formation from
synchronized pairs of atomic cooling haloes. Monthly Notices of the Royal Astronomical
Society. 445(1), 1056–1063.
mla: Visbal, Eli, et al. “Direct Collapse Black Hole Formation from Synchronized
Pairs of Atomic Cooling Haloes.” Monthly Notices of the Royal Astronomical
Society, vol. 445, no. 1, Oxford University Press, 2014, pp. 1056–63, doi:10.1093/mnras/stu1794.
short: E. Visbal, Z. Haiman, G.L. Bryan, Monthly Notices of the Royal Astronomical
Society 445 (2014) 1056–1063.
date_created: 2024-09-06T07:28:59Z
date_published: 2014-10-08T00:00:00Z
date_updated: 2024-09-24T13:02:31Z
day: '08'
doi: 10.1093/mnras/stu1794
extern: '1'
fulldoi: https://doi.org/10.1093/mnras/stu1794
intvolume: ' 445'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stu1794
month: '10'
oa: 1
oa_version: Published Version
page: 1056-1063
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: Direct collapse black hole formation from synchronized pairs of atomic cooling
haloes
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 445
year: '2014'
...
---
_id: '17624'
abstract:
- lang: eng
text: 'A near-equal-mass binary black hole (BH) can clear a central cavity in a
circumbinary accretion disc; however, previous works have revealed accretion streams
entering this cavity. Here we use 2D hydrodynamical simulations to study the accretion
streams and their periodic behaviour. In particular, we perform a suite of simulations,
covering different binary mass ratios q = M2/M1 in the range 0.003 ≤ q ≤ 1. In
each case, we follow the system for several thousand binary orbits, until it relaxes
to a stable accretion pattern. We find the following results: (i) the binary is
efficient in maintaining a low-density cavity. However, the time-averaged mass
accretion rate into the cavity, through narrow coherent accretion streams, is
suppressed by at most a factor of a few compared to a disc with a single BH with
the same mass; (ii) for q ≳ 0.05, the accretion rate is strongly modulated by
the binary, and depending on the precise value of q, the power spectrum of the
accretion rate shows either one, two or three distinct periods; and (iii) for
q ≲ 0.05, the accretion rate becomes steady, with no time variations. Most binaries
produced in galactic mergers are expected to have q ≳ 0.05. If the luminosity
of these binaries tracks their accretion rate, then a periodogram of their light
curve could help in their identification, and to constrain their mass ratio and
disc properties.'
article_processing_charge: No
article_type: original
arxiv: 1
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
- first_name: Andrew
full_name: MacFadyen, Andrew
last_name: MacFadyen
citation:
ama: D’Orazio DJ, Haiman Z, MacFadyen A. Accretion into the central cavity of a
circumbinary disc. Monthly Notices of the Royal Astronomical Society. 2013;436(4):2997-3020.
doi:10.1093/mnras/stt1787
apa: D’Orazio, D. J., Haiman, Z., & MacFadyen, A. (2013). Accretion into the
central cavity of a circumbinary disc. Monthly Notices of the Royal Astronomical
Society. Oxford University Press. https://doi.org/10.1093/mnras/stt1787
chicago: D’Orazio, Daniel J., Zoltán Haiman, and Andrew MacFadyen. “Accretion into
the Central Cavity of a Circumbinary Disc.” Monthly Notices of the Royal Astronomical
Society. Oxford University Press, 2013. https://doi.org/10.1093/mnras/stt1787.
ieee: D. J. D’Orazio, Z. Haiman, and A. MacFadyen, “Accretion into the central cavity
of a circumbinary disc,” Monthly Notices of the Royal Astronomical Society,
vol. 436, no. 4. Oxford University Press, pp. 2997–3020, 2013.
ista: D’Orazio DJ, Haiman Z, MacFadyen A. 2013. Accretion into the central cavity
of a circumbinary disc. Monthly Notices of the Royal Astronomical Society. 436(4),
2997–3020.
mla: D’Orazio, Daniel J., et al. “Accretion into the Central Cavity of a Circumbinary
Disc.” Monthly Notices of the Royal Astronomical Society, vol. 436, no.
4, Oxford University Press, 2013, pp. 2997–3020, doi:10.1093/mnras/stt1787.
short: D.J. D’Orazio, Z. Haiman, A. MacFadyen, Monthly Notices of the Royal Astronomical
Society 436 (2013) 2997–3020.
date_created: 2024-09-05T13:53:11Z
date_published: 2013-10-18T00:00:00Z
date_updated: 2024-09-24T08:47:58Z
day: '18'
doi: 10.1093/mnras/stt1787
extern: '1'
external_id:
arxiv:
- '1210.0536'
fulldoi: https://doi.org/10.1093/mnras/stt1787
intvolume: ' 436'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: ' https://doi.org/10.48550/arXiv.1210.0536'
month: '10'
oa: 1
oa_version: Preprint
page: 2997-3020
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
issn:
- 1365-2966
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: Accretion into the central cavity of a circumbinary disc
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 436
year: '2013'
...
---
_id: '17646'
abstract:
- lang: eng
text: Structures in Warm Dark Matter (WDM) models are exponentially suppressed below
a certain scale, characterized by the dark matter particle mass, mx. Since structures
form hierarchically, the presence of collapsed objects at high-redshifts can set
strong lower limits on mx. We place robust constraints on mx using recent results
from the {\it Swift} database of high-redshift gamma-ray bursts (GRBs). We parameterize
the redshift evolution of the ratio between the cosmic GRB rate and star formation
rate (SFR) as ∝(1+z)α, thereby allowing astrophysical uncertainties to partially
mimic the cosmological suppression of structures in WDM models. Using a maximum
likelihood estimator on two different z>4 GRB subsamples (including two bursts
at z>8), we constrain mx≳1.6-1.8 keV at 95% C.L., when marginalized over a flat
prior in α. We further estimate that 5 years of a SVOM-like mission would tighten
these constraints to mx≳2.3 keV. Our results show that GRBs are a powerful probe
of high-redshift structures, providing robust and competitive constraints on mx.
article_processing_charge: No
article_type: original
author:
- first_name: R. S.
full_name: de Souza, R. S.
last_name: de Souza
- first_name: A.
full_name: Mesinger, A.
last_name: Mesinger
- first_name: A.
full_name: Ferrara, A.
last_name: Ferrara
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: R.
full_name: Perna, R.
last_name: Perna
- first_name: N.
full_name: Yoshida, N.
last_name: Yoshida
citation:
ama: de Souza RS, Mesinger A, Ferrara A, Haiman Z, Perna R, Yoshida N. Constraints
on warm dark matter models from high-redshift long gamma-ray bursts. Monthly
Notices of the Royal Astronomical Society. 2013;432(4):3218-3227. doi:10.1093/mnras/stt674
apa: de Souza, R. S., Mesinger, A., Ferrara, A., Haiman, Z., Perna, R., & Yoshida,
N. (2013). Constraints on warm dark matter models from high-redshift long gamma-ray
bursts. Monthly Notices of the Royal Astronomical Society. Oxford University
Press. https://doi.org/10.1093/mnras/stt674
chicago: Souza, R. S. de, A. Mesinger, A. Ferrara, Zoltán Haiman, R. Perna, and
N. Yoshida. “Constraints on Warm Dark Matter Models from High-Redshift Long Gamma-Ray
Bursts.” Monthly Notices of the Royal Astronomical Society. Oxford University
Press, 2013. https://doi.org/10.1093/mnras/stt674.
ieee: R. S. de Souza, A. Mesinger, A. Ferrara, Z. Haiman, R. Perna, and N. Yoshida,
“Constraints on warm dark matter models from high-redshift long gamma-ray bursts,”
Monthly Notices of the Royal Astronomical Society, vol. 432, no. 4. Oxford
University Press, pp. 3218–3227, 2013.
ista: de Souza RS, Mesinger A, Ferrara A, Haiman Z, Perna R, Yoshida N. 2013. Constraints
on warm dark matter models from high-redshift long gamma-ray bursts. Monthly Notices
of the Royal Astronomical Society. 432(4), 3218–3227.
mla: de Souza, R. S., et al. “Constraints on Warm Dark Matter Models from High-Redshift
Long Gamma-Ray Bursts.” Monthly Notices of the Royal Astronomical Society,
vol. 432, no. 4, Oxford University Press, 2013, pp. 3218–27, doi:10.1093/mnras/stt674.
short: R.S. de Souza, A. Mesinger, A. Ferrara, Z. Haiman, R. Perna, N. Yoshida,
Monthly Notices of the Royal Astronomical Society 432 (2013) 3218–3227.
date_created: 2024-09-06T07:25:13Z
date_published: 2013-05-09T00:00:00Z
date_updated: 2024-09-24T12:40:52Z
day: '09'
doi: 10.1093/mnras/stt674
extern: '1'
fulldoi: https://doi.org/10.1093/mnras/stt674
intvolume: ' 432'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stt674
month: '05'
oa: 1
oa_version: Published Version
page: 3218-3227
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: Constraints on warm dark matter models from high-redshift long gamma-ray bursts
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 432
year: '2013'
...
---
_id: '17653'
abstract:
- lang: eng
text: Observations of quasars at redshifts z > 6 reveal that 10^9 Msol supermassive
black holes (SMBHs) had already formed when the Universe was < 0.9 Gyr old. One
hypothesis for the origins of these SMBHs is that they grew from the remnants
of the first generation of massive stars, which formed in low-mass (~ 10^5 to
10^6 Msol) dark matter minihaloes at z > 20. This is the regime where baryonic
streaming motions--the relative velocities of baryons with respect to dark matter
in the early Universe--most strongly inhibit star formation by suppressing gas
infall and cooling. We investigate the impact of this effect on the growth of
the first SMBHs using a suite of high-fidelity, ellipsoidal-collapse Monte Carlo
merger-tree simulations. We find that the suppression of seed BH formation by
the streaming motions significantly reduces the number density of the most massive
BHs at z > 15, but the residual effect at lower redshifts is essentially negligible.
The streaming motions can reduce by a factor of few the number density of the
most luminous quasars at z ~ 10-11, where such objects could be detected by the
James Webb Space Telescope. We conclude, with minor theoretical caveats, that
baryonic streaming motions are unlikely to pose a significant additional obstacle
to the formation of the observed high-redshift quasar SMBHs. Nor do they appreciably
affect the heating and reionization histories of the Universe or the merger rates
of nuclear BHs in the mass and redshift ranges of interest for proposed gravitational-wave
detectors.
article_processing_charge: No
article_type: original
author:
- first_name: Takamitsu L.
full_name: Tanaka, Takamitsu L.
last_name: Tanaka
- 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: Tanaka TL, Li M, Haiman Z. The effect of baryonic streaming motions on the
formation of the first supermassive black holes. Monthly Notices of the Royal
Astronomical Society. 2013;435(4):3559-3567. doi:10.1093/mnras/stt1553
apa: Tanaka, T. L., Li, M., & Haiman, Z. (2013). The effect of baryonic streaming
motions on the formation of the first supermassive black holes. Monthly Notices
of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stt1553
chicago: Tanaka, Takamitsu L., Miao Li, and Zoltán Haiman. “The Effect of Baryonic
Streaming Motions on the Formation of the First Supermassive Black Holes.” Monthly
Notices of the Royal Astronomical Society. Oxford University Press, 2013.
https://doi.org/10.1093/mnras/stt1553.
ieee: T. L. Tanaka, M. Li, and Z. Haiman, “The effect of baryonic streaming motions
on the formation of the first supermassive black holes,” Monthly Notices of
the Royal Astronomical Society, vol. 435, no. 4. Oxford University Press,
pp. 3559–3567, 2013.
ista: Tanaka TL, Li M, Haiman Z. 2013. The effect of baryonic streaming motions
on the formation of the first supermassive black holes. Monthly Notices of the
Royal Astronomical Society. 435(4), 3559–3567.
mla: Tanaka, Takamitsu L., et al. “The Effect of Baryonic Streaming Motions on the
Formation of the First Supermassive Black Holes.” Monthly Notices of the Royal
Astronomical Society, vol. 435, no. 4, Oxford University Press, 2013, pp.
3559–67, doi:10.1093/mnras/stt1553.
short: T.L. Tanaka, M. Li, Z. Haiman, Monthly Notices of the Royal Astronomical
Society 435 (2013) 3559–3567.
date_created: 2024-09-06T07:31:32Z
date_published: 2013-09-10T00:00:00Z
date_updated: 2024-09-24T13:26:36Z
day: '10'
doi: 10.1093/mnras/stt1553
extern: '1'
fulldoi: https://doi.org/10.1093/mnras/stt1553
intvolume: ' 435'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stt1553
month: '09'
oa: 1
oa_version: Published Version
page: 3559-3567
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
issn:
- 1365-2966
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The effect of baryonic streaming motions on the formation of the first supermassive
black holes
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 435
year: '2013'
...
---
_id: '17683'
abstract:
- lang: eng
text: When a sufficiently massive satellite (or secondary) black hole is embedded
in a gas disc around a (primary) supermassive black hole, it can open an empty
gap in the disc. A gap-opening secondary close to the primary will leave an imprint
in the broad component of the Fe Kα emission line, which varies in a unique and
predictable manner. If the gap persists into the innermost disc, the effect consists
of a pair of dips in the broad line which ripple blue-ward and red-ward from the
line centroid energy, respectively, as the gap moves closer to the primary. This
ripple effect could be unambiguously detectable and allow an electromagnetic monitoring
of massive black hole mergers as they occur. As the mass ratio of the secondary
to primary black hole increases to q ≳ 0.01, we expect the gap to widen, possibly
clearing a central cavity in the inner disc, which shows up in the broad Fe Kα
line component. If the secondary stalls at ≥ 102rg in its in-migration, due to
low corotating gas mass, a detectable ripple effect occurs in the broad line component
on the disc viscous time-scale as the inner disc drains and the outer disc is
dammed. If the secondary maintains an accretion disc within a central cavity,
due to dam bursting or leakage, a periodic ‘see-saw’ oscillation effect is exhibited
in the observed line profile. Here, we demonstrate the range of ripple effect
signatures potentially detectable with Astro-H and IXO/Athena, and oscillation
effects potentially detectable with XMM–Newton or LOFT for a wide variety of merger
and disc conditions, including gap width (or cavity size), disc inclination angle
and emissivity profile, damming of the accretion flow by the secondary, and a
minidisc around the satellite black hole. A systematic study of ripple effects
would require a telescope effective area substantially larger than that planned
for IXO/Athena. Future mission planning should take this into account. Observations
of the ripple effect and periodic oscillations can be used to provide an early
warning of gravitational radiation emission from the AGN. Once gravitational waves
consistent with massive black hole mergers are detected, an archival search for
the Fe Kα ripple effect or periodic oscillations will help in localizing their
origin.
article_processing_charge: No
article_type: original
author:
- 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: B.
full_name: Kocsis, B.
last_name: Kocsis
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
citation:
ama: McKernan B, Ford KES, Kocsis B, Haiman Z. Ripple effects and oscillations in
the broad Fe Kα line as a probe of massive black hole mergers. Monthly Notices
of the Royal Astronomical Society. 2013;432(2):1468-1482. doi:10.1093/mnras/stt567
apa: McKernan, B., Ford, K. E. S., Kocsis, B., & Haiman, Z. (2013). Ripple effects
and oscillations in the broad Fe Kα line as a probe of massive black hole mergers.
Monthly Notices of the Royal Astronomical Society. Oxford University Press.
https://doi.org/10.1093/mnras/stt567
chicago: McKernan, B., K. E. S. Ford, B. Kocsis, and Zoltán Haiman. “Ripple Effects
and Oscillations in the Broad Fe Kα Line as a Probe of Massive Black Hole Mergers.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2013. https://doi.org/10.1093/mnras/stt567.
ieee: B. McKernan, K. E. S. Ford, B. Kocsis, and Z. Haiman, “Ripple effects and
oscillations in the broad Fe Kα line as a probe of massive black hole mergers,”
Monthly Notices of the Royal Astronomical Society, vol. 432, no. 2. Oxford
University Press, pp. 1468–1482, 2013.
ista: McKernan B, Ford KES, Kocsis B, Haiman Z. 2013. Ripple effects and oscillations
in the broad Fe Kα line as a probe of massive black hole mergers. Monthly Notices
of the Royal Astronomical Society. 432(2), 1468–1482.
mla: McKernan, B., et al. “Ripple Effects and Oscillations in the Broad Fe Kα Line
as a Probe of Massive Black Hole Mergers.” Monthly Notices of the Royal Astronomical
Society, vol. 432, no. 2, Oxford University Press, 2013, pp. 1468–82, doi:10.1093/mnras/stt567.
short: B. McKernan, K.E.S. Ford, B. Kocsis, Z. Haiman, Monthly Notices of the Royal
Astronomical Society 432 (2013) 1468–1482.
date_created: 2024-09-06T08:18:32Z
date_published: 2013-05-02T00:00:00Z
date_updated: 2024-09-25T09:13:00Z
day: '02'
doi: 10.1093/mnras/stt567
extern: '1'
fulldoi: https://doi.org/10.1093/mnras/stt567
intvolume: ' 432'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stt567
month: '05'
oa: 1
oa_version: Published Version
page: 1468-1482
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: Ripple effects and oscillations in the broad Fe Kα line as a probe of massive
black hole mergers
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 432
year: '2013'
...
---
_id: '17684'
abstract:
- lang: eng
text: We have performed cosmo-hydro simulations using the RAMSES code to study atomic
cooling (ACHs) haloes at z=10 with masses 5E7Msun<~M<~2E9Msun. We assume primordial
gas and H2-cooling and prior star-formation have been suppressed. We analysed
19 haloes (gas and DM) at a resolution of ~10 (proper) pc, selected from a total
volume of ~2E3 (comoving) Mpc3. This is the largest statistical hydro-sim. study
of ACHs at z>10 to date. We examine the morphology, angular momentum (AM), thermodynamic,
and turbulence of these haloes, in order to assess the prevalence of disks and
supermassive black holes (SMBHs). We find no correlation between either the magnitude
or the direction of the AM of the gas and its parent DM halo. Only 3 haloes form
rotationally supported cores. Two of the most massive haloes form massive, compact
overdense blobs. These blobs have an accretion rate ~0.5 Msun/yr (at a distance
of 100 pc), and are possible sites of SMBH formation. Our results suggest that
the degree of rotational support and the fate of the gas in a halo is determined
by its large-scale environment and merger history. In particular, the two haloes
forming blobs are located at knots of the cosmic web, cooled early on, and experienced
many mergers. The gas in these haloes is lumpy and highly turbulent, with Mach
N. >~ 5. In contrast, the haloes forming rotationally supported cores are relatively
more isolated, located midway along filaments, cooled more recently, and underwent
fewer mergers. Thus, the gas in these haloes is less lumpy and less turbulent
(Mach <~ 4), and could retain most of its AM. The remaining 14 haloes have intermediate
properties. If verified in a larger sample of haloes and with additional physics,
our results will have implications for observations of the highest-redshift galaxies
and quasars with JWST.
article_processing_charge: No
article_type: original
author:
- first_name: Joaquin
full_name: Prieto, Joaquin
last_name: Prieto
- first_name: Raul
full_name: Jimenez, Raul
last_name: Jimenez
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
citation:
ama: 'Prieto J, Jimenez R, Haiman Z. Gas infall into atomic cooling haloes: On the
formation of protogalactic discs and supermassive black holes at z > 10. Monthly
Notices of the Royal Astronomical Society. 2013;436(3):2301-2325. doi:10.1093/mnras/stt1730'
apa: 'Prieto, J., Jimenez, R., & Haiman, Z. (2013). Gas infall into atomic cooling
haloes: On the formation of protogalactic discs and supermassive black holes at
z > 10. Monthly Notices of the Royal Astronomical Society. Oxford University
Press. https://doi.org/10.1093/mnras/stt1730'
chicago: 'Prieto, Joaquin, Raul Jimenez, and Zoltán Haiman. “Gas Infall into Atomic
Cooling Haloes: On the Formation of Protogalactic Discs and Supermassive Black
Holes at z > 10.” Monthly Notices of the Royal Astronomical Society.
Oxford University Press, 2013. https://doi.org/10.1093/mnras/stt1730.'
ieee: 'J. Prieto, R. Jimenez, and Z. Haiman, “Gas infall into atomic cooling haloes:
On the formation of protogalactic discs and supermassive black holes at z >
10,” Monthly Notices of the Royal Astronomical Society, vol. 436, no. 3.
Oxford University Press, pp. 2301–2325, 2013.'
ista: 'Prieto J, Jimenez R, Haiman Z. 2013. Gas infall into atomic cooling haloes:
On the formation of protogalactic discs and supermassive black holes at z >
10. Monthly Notices of the Royal Astronomical Society. 436(3), 2301–2325.'
mla: 'Prieto, Joaquin, et al. “Gas Infall into Atomic Cooling Haloes: On the Formation
of Protogalactic Discs and Supermassive Black Holes at z > 10.” Monthly
Notices of the Royal Astronomical Society, vol. 436, no. 3, Oxford University
Press, 2013, pp. 2301–25, doi:10.1093/mnras/stt1730.'
short: J. Prieto, R. Jimenez, Z. Haiman, Monthly Notices of the Royal Astronomical
Society 436 (2013) 2301–2325.
date_created: 2024-09-06T08:19:41Z
date_published: 2013-10-08T00:00:00Z
date_updated: 2024-09-25T09:15:36Z
day: '08'
doi: 10.1093/mnras/stt1730
extern: '1'
fulldoi: https://doi.org/10.1093/mnras/stt1730
intvolume: ' 436'
issue: '3'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1093/mnras/stt1730
month: '10'
oa: 1
oa_version: Published Version
page: 2301-2325
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
issn:
- 1365-2966
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Gas infall into atomic cooling haloes: On the formation of protogalactic discs
and supermassive black holes at z > 10'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 436
year: '2013'
...
---
_id: '17613'
abstract:
- lang: eng
text: We study the interaction of a supermassive black hole (SMBH) binary and a
standard radiatively efficient thin accretion disk. We examine steady-state configurations
of the disk and migrating SMBH system, self-consistently accounting for tidal
and viscous torques and heating, radiative diffusion limited cooling, gas and
radiation pressure, and the decay of the binary's orbit. We obtain a "phase diagram"
of the system as a function of binary parameters, showing regimes in which both
the disk structure and migration have a different character. Although massive
binaries can create a central gap in the disk at large radii, the tidal barrier
of the secondary causes a significant pile-up of gas outside of its orbit, which
can lead to the closing of the gap. We find that this spillover occurs at an orbital
separation as large as ~200 M_7^{-1/2} gravitational radii, where M = 10^7 M_7
Msun is the total binary mass. If the secondary is less massive than ~10^6 Msun,
then the gap is closed before gravitational waves (GWs) start dominating the orbital
decay. In this regime, the disk is still strongly perturbed, but the piled-up
gas continuously overflows as in a porous dam, and crosses inside the secondary's
orbit. The corresponding migration rate, which we label Type 1.5, is slower than
the usual limiting cases known as Type I and II migration. Compared to an unperturbed
disk, the steady-state disk in the overflowing regime is up to several hundred
times brighter in the optical bands. Surveys such as PanSTARRS or LSST may discover
the periodic variability of this population of binaries. Our results imply that
the circumbinary disks around SMBHs can extend to small radii during the last
stages of their merger, when they are detectable by LISA, and may produce coincident
electromagnetic (EM) emission similar to active galactic nuclei (AGN).
alternative_title:
- 'Overflow and migration: SMBH binaries'
article_processing_charge: No
article_type: original
author:
- first_name: Bence
full_name: Kocsis, Bence
last_name: Kocsis
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Abraham
full_name: Loeb, Abraham
last_name: Loeb
citation:
ama: 'Kocsis B, Haiman Z, Loeb A. Gas pile-up, gap overflow and Type 1.5 migration
in circumbinary discs: Application to supermassive black hole binaries. Monthly
Notices of the Royal Astronomical Society. 2012;427(3):2680-2700. doi:10.1111/j.1365-2966.2012.22118.x'
apa: 'Kocsis, B., Haiman, Z., & Loeb, A. (2012). Gas pile-up, gap overflow and
Type 1.5 migration in circumbinary discs: Application to supermassive black hole
binaries. Monthly Notices of the Royal Astronomical Society. Oxford University
Press. https://doi.org/10.1111/j.1365-2966.2012.22118.x'
chicago: 'Kocsis, Bence, Zoltán Haiman, and Abraham Loeb. “Gas Pile-up, Gap Overflow
and Type 1.5 Migration in Circumbinary Discs: Application to Supermassive Black
Hole Binaries.” Monthly Notices of the Royal Astronomical Society. Oxford
University Press, 2012. https://doi.org/10.1111/j.1365-2966.2012.22118.x.'
ieee: 'B. Kocsis, Z. Haiman, and A. Loeb, “Gas pile-up, gap overflow and Type 1.5
migration in circumbinary discs: Application to supermassive black hole binaries,”
Monthly Notices of the Royal Astronomical Society, vol. 427, no. 3. Oxford
University Press, pp. 2680–2700, 2012.'
ista: 'Kocsis B, Haiman Z, Loeb A. 2012. Gas pile-up, gap overflow and Type 1.5
migration in circumbinary discs: Application to supermassive black hole binaries.
Monthly Notices of the Royal Astronomical Society. 427(3), 2680–2700.'
mla: 'Kocsis, Bence, et al. “Gas Pile-up, Gap Overflow and Type 1.5 Migration in
Circumbinary Discs: Application to Supermassive Black Hole Binaries.” Monthly
Notices of the Royal Astronomical Society, vol. 427, no. 3, Oxford University
Press, 2012, pp. 2680–700, doi:10.1111/j.1365-2966.2012.22118.x.'
short: B. Kocsis, Z. Haiman, A. Loeb, Monthly Notices of the Royal Astronomical
Society 427 (2012) 2680–2700.
date_created: 2024-09-05T13:28:17Z
date_published: 2012-12-11T00:00:00Z
date_updated: 2024-09-24T07:40:02Z
day: '11'
doi: 10.1111/j.1365-2966.2012.22118.x
extern: '1'
fulldoi: https://doi.org/10.1111/j.1365-2966.2012.22118.x
intvolume: ' 427'
issue: '3'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1111/j.1365-2966.2012.22118.x
month: '12'
oa: 1
oa_version: Published Version
page: 2680-2700
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: 'Gas pile-up, gap overflow and Type 1.5 migration in circumbinary discs: Application
to supermassive black hole binaries'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 427
year: '2012'
...
---
_id: '17660'
abstract:
- lang: eng
text: Many astrophysical binaries, from planets to black holes, exert strong torques
on their circumbinary accretion discs, and are expected to significantly modify
the disc structure. Despite the several decade long history of the subject, the
joint evolution of the binary + disc system has not been modelled with self-consistent
assumptions for arbitrary mass ratios and accretion rates. Here, we solve the
coupled binary–disc evolution equations analytically in the strongly perturbed
limit, treating the azimuthally averaged angular momentum exchange between the
disc and the binary and the modifications to the density, scaleheight, and viscosity
self-consistently, including viscous and tidal heating, diffusion limited cooling,
radiation pressure and the orbital decay of the binary. We find a solution with
a central cavity and a migration rate similar to those previously obtained for
Type II migration, applicable for large masses and binary separations, and near-equal
mass ratios. However, we identify a distinct new regime, applicable at smaller
separations and masses, and mass ratio in the range 10−3 ≲ q ≲ 0.1. For these
systems, gas piles up outside the binary's orbit, but rather than creating a cavity,
it continuously overflows as in a porous dam. The disc profile is intermediate
between a weakly perturbed disc (producing Type I migration) and a disc with a
gap (with Type II migration). However, the migration rate of the secondary is
typically slower than both Type I and Type II rates. We term this new regime ‘Type
1.5’ migration.
alternative_title:
- 'Overflow and migration: general theory'
article_processing_charge: No
article_type: original
author:
- first_name: Bence
full_name: Kocsis, Bence
last_name: Kocsis
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Abraham
full_name: Loeb, Abraham
last_name: Loeb
citation:
ama: 'Kocsis B, Haiman Z, Loeb A. Gas pile-up, gap overflow and Type 1.5 migration
in circumbinary discs: General theory. Monthly Notices of the Royal Astronomical
Society. 2012;427(3):2660-2679. doi:10.1111/j.1365-2966.2012.22129.x'
apa: 'Kocsis, B., Haiman, Z., & Loeb, A. (2012). Gas pile-up, gap overflow and
Type 1.5 migration in circumbinary discs: General theory. Monthly Notices of
the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1111/j.1365-2966.2012.22129.x'
chicago: 'Kocsis, Bence, Zoltán Haiman, and Abraham Loeb. “Gas Pile-up, Gap Overflow
and Type 1.5 Migration in Circumbinary Discs: General Theory.” Monthly Notices
of the Royal Astronomical Society. Oxford University Press, 2012. https://doi.org/10.1111/j.1365-2966.2012.22129.x.'
ieee: 'B. Kocsis, Z. Haiman, and A. Loeb, “Gas pile-up, gap overflow and Type 1.5
migration in circumbinary discs: General theory,” Monthly Notices of the Royal
Astronomical Society, vol. 427, no. 3. Oxford University Press, pp. 2660–2679,
2012.'
ista: 'Kocsis B, Haiman Z, Loeb A. 2012. Gas pile-up, gap overflow and Type 1.5
migration in circumbinary discs: General theory. Monthly Notices of the Royal
Astronomical Society. 427(3), 2660–2679.'
mla: 'Kocsis, Bence, et al. “Gas Pile-up, Gap Overflow and Type 1.5 Migration in
Circumbinary Discs: General Theory.” Monthly Notices of the Royal Astronomical
Society, vol. 427, no. 3, Oxford University Press, 2012, pp. 2660–79, doi:10.1111/j.1365-2966.2012.22129.x.'
short: B. Kocsis, Z. Haiman, A. Loeb, Monthly Notices of the Royal Astronomical
Society 427 (2012) 2660–2679.
date_created: 2024-09-06T07:38:16Z
date_published: 2012-12-11T00:00:00Z
date_updated: 2024-09-25T07:21:05Z
day: '11'
doi: 10.1111/j.1365-2966.2012.22129.x
extern: '1'
fulldoi: https://doi.org/10.1111/j.1365-2966.2012.22129.x
intvolume: ' 427'
issue: '3'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1111/j.1365-2966.2012.22129.x
month: '12'
oa: 1
oa_version: Published Version
page: 2660-2679
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: 'Gas pile-up, gap overflow and Type 1.5 migration in circumbinary discs: General
theory'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 427
year: '2012'
...
---
_id: '17674'
abstract:
- lang: eng
text: The power spectrum of cosmic infrared background (CIB) anisotropies is sensitive
to the connection between star formation and dark matter haloes over the entire
cosmic star formation history. Here we develop a model that associates star‐forming
galaxies with dark matter haloes and their subhaloes. The model is based on a
parametrized relation between the dust‐processed infrared luminosity and (sub)halo
mass. By adjusting three free parameters, we attempt to simultaneously fit the
four frequency bands of the Planck measurement of the CIB anisotropy power spectrum.
To fit the data, we find that the star formation efficiency must peak on a halo
mass scale of ≈5 × 10^12 M⊙ and the infrared luminosity per unit mass must increase
rapidly with redshift. By comparing our predictions with a well‐calibrated phenomenological
model for shot noise, and with a direct observation of source counts, we show
that the mean duty cycle of the underlying infrared sources must be near unity,
indicating that the CIB is dominated by long‐lived quiescent star formation, rather
than intermittent short ‘starbursts’. Despite the improved flexibility of our
model, the best simultaneous fit to all four Planck channels remains relatively
poor. We discuss possible further extensions to alleviate the remaining tension
with the data. Our model presents a theoretical framework for a future joint analysis
of both background anisotropy and source count measurements.
alternative_title:
- Improved models for CIB anisotropies
article_processing_charge: No
article_type: original
author:
- first_name: Cien
full_name: Shang, Cien
last_name: Shang
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Lloyd
full_name: Knox, Lloyd
last_name: Knox
- first_name: S. Peng
full_name: Oh, S. Peng
last_name: Oh
citation:
ama: 'Shang C, Haiman Z, Knox L, Oh SP. Improved models for cosmic infrared background
anisotropies: New constraints on the infrared galaxy population. Monthly Notices
of the Royal Astronomical Society. 2012;421(4):2832-2845. doi:10.1111/j.1365-2966.2012.20510.x'
apa: 'Shang, C., Haiman, Z., Knox, L., & Oh, S. P. (2012). Improved models for
cosmic infrared background anisotropies: New constraints on the infrared galaxy
population. Monthly Notices of the Royal Astronomical Society. Oxford University
Press. https://doi.org/10.1111/j.1365-2966.2012.20510.x'
chicago: 'Shang, Cien, Zoltán Haiman, Lloyd Knox, and S. Peng Oh. “Improved Models
for Cosmic Infrared Background Anisotropies: New Constraints on the Infrared Galaxy
Population.” Monthly Notices of the Royal Astronomical Society. Oxford
University Press, 2012. https://doi.org/10.1111/j.1365-2966.2012.20510.x.'
ieee: 'C. Shang, Z. Haiman, L. Knox, and S. P. Oh, “Improved models for cosmic infrared
background anisotropies: New constraints on the infrared galaxy population,” Monthly
Notices of the Royal Astronomical Society, vol. 421, no. 4. Oxford University
Press, pp. 2832–2845, 2012.'
ista: 'Shang C, Haiman Z, Knox L, Oh SP. 2012. Improved models for cosmic infrared
background anisotropies: New constraints on the infrared galaxy population. Monthly
Notices of the Royal Astronomical Society. 421(4), 2832–2845.'
mla: 'Shang, Cien, et al. “Improved Models for Cosmic Infrared Background Anisotropies:
New Constraints on the Infrared Galaxy Population.” Monthly Notices of the
Royal Astronomical Society, vol. 421, no. 4, Oxford University Press, 2012,
pp. 2832–45, doi:10.1111/j.1365-2966.2012.20510.x.'
short: C. Shang, Z. Haiman, L. Knox, S.P. Oh, Monthly Notices of the Royal Astronomical
Society 421 (2012) 2832–2845.
date_created: 2024-09-06T07:50:37Z
date_published: 2012-04-10T00:00:00Z
date_updated: 2024-09-25T08:36:17Z
day: '10'
doi: 10.1111/j.1365-2966.2012.20510.x
extern: '1'
fulldoi: https://doi.org/10.1111/j.1365-2966.2012.20510.x
intvolume: ' 421'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1111/j.1365-2966.2012.20510.x
month: '04'
oa: 1
oa_version: Published Version
page: 2832-2845
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
issn:
- 0035-8711
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Improved models for cosmic infrared background anisotropies: New constraints
on the infrared galaxy population'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 421
year: '2012'
...