---
_id: '1717'
abstract:
- lang: eng
text: 'Two key processes are in the basis of morphogenesis: the spatial allocation
of cell types in fields of naïve cells and the regulation of growth. Both are
controlled by morphogens, which activate target genes in the growing tissue in
a concentration-dependent manner. Thus the morphogen model is an intrinsically
quantitative concept. However, quantitative studies were performed only in recent
years on two morphogens: Bicoid and Decapentaplegic. This review covers quantitative
aspects of the formation and precision of the Decapentaplegic morphogen gradient.
The morphogen gradient concept is transitioning from a soft definition to a precise
idea of what the gradient could really do.'
acknowledgement: This work was supported by the University of Geneva, Max Planck Society,
VW, EU, SNF, and HFSP
author:
- first_name: Anna
full_name: Anna Kicheva
id: 3959A2A0-F248-11E8-B48F-1D18A9856A87
last_name: Kicheva
orcid: 0000-0003-4509-4998
- first_name: Marcos
full_name: González-Gaitán, Marcos A
last_name: González Gaitán
citation:
ama: Kicheva A, González Gaitán M. The Decapentaplegic morphogen gradient a precise
definition. Current Opinion in Cell Biology. 2008;20(2):137-143. doi:10.1016/j.ceb.2008.01.008
apa: Kicheva, A., & González Gaitán, M. (2008). The Decapentaplegic morphogen
gradient a precise definition. Current Opinion in Cell Biology. Elsevier.
https://doi.org/10.1016/j.ceb.2008.01.008
chicago: Kicheva, Anna, and Marcos González Gaitán. “The Decapentaplegic Morphogen
Gradient a Precise Definition.” Current Opinion in Cell Biology. Elsevier,
2008. https://doi.org/10.1016/j.ceb.2008.01.008.
ieee: A. Kicheva and M. González Gaitán, “The Decapentaplegic morphogen gradient
a precise definition,” Current Opinion in Cell Biology, vol. 20, no. 2.
Elsevier, pp. 137–143, 2008.
ista: Kicheva A, González Gaitán M. 2008. The Decapentaplegic morphogen gradient
a precise definition. Current Opinion in Cell Biology. 20(2), 137–143.
mla: Kicheva, Anna, and Marcos González Gaitán. “The Decapentaplegic Morphogen Gradient
a Precise Definition.” Current Opinion in Cell Biology, vol. 20, no. 2,
Elsevier, 2008, pp. 137–43, doi:10.1016/j.ceb.2008.01.008.
short: A. Kicheva, M. González Gaitán, Current Opinion in Cell Biology 20 (2008)
137–143.
date_created: 2018-12-11T11:53:38Z
date_published: 2008-04-01T00:00:00Z
date_updated: 2021-01-12T06:52:44Z
day: '01'
doi: 10.1016/j.ceb.2008.01.008
extern: 1
intvolume: ' 20'
issue: '2'
month: '04'
page: 137 - 143
publication: Current Opinion in Cell Biology
publication_status: published
publisher: Elsevier
publist_id: '5412'
quality_controlled: 0
status: public
title: The Decapentaplegic morphogen gradient a precise definition
type: journal_article
volume: 20
year: '2008'
...
---
_id: '1719'
abstract:
- lang: eng
text: We study the mechanics of tissue growth via cell division and cell death (apoptosis).
The rearrangements of cells can on large scales and times be captured by a continuum
theory which describes the tissue as an effective viscous material with active
stresses generated by cell division. We study the effects of anisotropies of cell
division on cell rearrangements and show that average cellular trajectories exhibit
anisotropic scaling behaviors. If cell division and apoptosis balance, there is
no net growth, but for anisotropic cell division the tissue undergoes spontaneous
shear deformations. Our description is relevant for the study of developing tissues
such as the imaginal disks of the fruit fly Drosophila melanogaster, which grow
anisotropically.
author:
- first_name: Thomas
full_name: Bittig, Thomas
last_name: Bittig
- first_name: Ortrud
full_name: Wartlick, Ortrud
last_name: Wartlick
- first_name: Anna
full_name: Anna Kicheva
id: 3959A2A0-F248-11E8-B48F-1D18A9856A87
last_name: Kicheva
orcid: 0000-0003-4509-4998
- first_name: Marcos
full_name: González-Gaitárr, Marcos
last_name: González Gaitárr
- first_name: Frank
full_name: Julicher, Frank
last_name: Julicher
citation:
ama: Bittig T, Wartlick O, Kicheva A, González Gaitárr M, Julicher F. Dynamics of
anisotropic tissue growth. New Journal of Physics. 2008;10. doi:10.1088/1367-2630/10/6/063001
apa: Bittig, T., Wartlick, O., Kicheva, A., González Gaitárr, M., & Julicher,
F. (2008). Dynamics of anisotropic tissue growth. New Journal of Physics.
IOP Publishing Ltd. https://doi.org/10.1088/1367-2630/10/6/063001
chicago: Bittig, Thomas, Ortrud Wartlick, Anna Kicheva, Marcos González Gaitárr,
and Frank Julicher. “Dynamics of Anisotropic Tissue Growth.” New Journal of
Physics. IOP Publishing Ltd., 2008. https://doi.org/10.1088/1367-2630/10/6/063001.
ieee: T. Bittig, O. Wartlick, A. Kicheva, M. González Gaitárr, and F. Julicher,
“Dynamics of anisotropic tissue growth,” New Journal of Physics, vol. 10.
IOP Publishing Ltd., 2008.
ista: Bittig T, Wartlick O, Kicheva A, González Gaitárr M, Julicher F. 2008. Dynamics
of anisotropic tissue growth. New Journal of Physics. 10.
mla: Bittig, Thomas, et al. “Dynamics of Anisotropic Tissue Growth.” New Journal
of Physics, vol. 10, IOP Publishing Ltd., 2008, doi:10.1088/1367-2630/10/6/063001.
short: T. Bittig, O. Wartlick, A. Kicheva, M. González Gaitárr, F. Julicher, New
Journal of Physics 10 (2008).
date_created: 2018-12-11T11:53:39Z
date_published: 2008-06-03T00:00:00Z
date_updated: 2021-01-12T06:52:44Z
day: '03'
doi: 10.1088/1367-2630/10/6/063001
extern: 1
intvolume: ' 10'
month: '06'
publication: New Journal of Physics
publication_status: published
publisher: IOP Publishing Ltd.
publist_id: '5411'
quality_controlled: 0
status: public
title: Dynamics of anisotropic tissue growth
type: journal_article
volume: 10
year: '2008'
...
---
_id: '1749'
abstract:
- lang: eng
text: Scanning probe microscopy; Semiconductor quantum dots; Composition gradients;
Composition profiles; Nanotomography; Single quantum dots; Strained sige/si; Three-dimensional
(3D); Wet-chemical etchings; X-ray scattering measurements; quantum dot; methodology;
nanotechnology; optical tomography; scanning probe microscopy; three dimensional
imaging; Imaging, Three-Dimensional; Materials Testing; Microscopy, Scanning Probe;
Nanotechnology; Quantum Dots; Tomography,
acknowledgement: This work was supported by the BMBF (No. 03N8711) and the EU project
D-DotFET (No. 012150)
author:
- first_name: Armando
full_name: Rastelli, Armando
last_name: Rastelli
- first_name: Mathieu
full_name: Stoffel, Mathieu
last_name: Stoffel
- first_name: Ângelo
full_name: Malachias, Ângelo S
last_name: Malachias
- first_name: Tsvetelina
full_name: Merdzhanova, Tsvetelina
last_name: Merdzhanova
- first_name: Georgios
full_name: Georgios Katsaros
id: 38DB5788-F248-11E8-B48F-1D18A9856A87
last_name: Katsaros
- first_name: Klaus
full_name: Kern, Klaus
last_name: Kern
- first_name: Till
full_name: Metzger, Till H
last_name: Metzger
- first_name: Oliver
full_name: Schmidt, Oliver G
last_name: Schmidt
citation:
ama: Rastelli A, Stoffel M, Malachias Â, et al. Three-dimensional composition profiles
of single quantum dots determined by scanning-probe-microscopy-based nanotomography.
Nano Letters. 2008;8(5):1404-1409. doi:10.1021/nl080290y
apa: Rastelli, A., Stoffel, M., Malachias, Â., Merdzhanova, T., Katsaros, G., Kern,
K., … Schmidt, O. (2008). Three-dimensional composition profiles of single quantum
dots determined by scanning-probe-microscopy-based nanotomography. Nano Letters.
American Chemical Society. https://doi.org/10.1021/nl080290y
chicago: Rastelli, Armando, Mathieu Stoffel, Ângelo Malachias, Tsvetelina Merdzhanova,
Georgios Katsaros, Klaus Kern, Till Metzger, and Oliver Schmidt. “Three-Dimensional
Composition Profiles of Single Quantum Dots Determined by Scanning-Probe-Microscopy-Based
Nanotomography.” Nano Letters. American Chemical Society, 2008. https://doi.org/10.1021/nl080290y.
ieee: A. Rastelli et al., “Three-dimensional composition profiles of single
quantum dots determined by scanning-probe-microscopy-based nanotomography,” Nano
Letters, vol. 8, no. 5. American Chemical Society, pp. 1404–1409, 2008.
ista: Rastelli A, Stoffel M, Malachias Â, Merdzhanova T, Katsaros G, Kern K, Metzger
T, Schmidt O. 2008. Three-dimensional composition profiles of single quantum dots
determined by scanning-probe-microscopy-based nanotomography. Nano Letters. 8(5),
1404–1409.
mla: Rastelli, Armando, et al. “Three-Dimensional Composition Profiles of Single
Quantum Dots Determined by Scanning-Probe-Microscopy-Based Nanotomography.” Nano
Letters, vol. 8, no. 5, American Chemical Society, 2008, pp. 1404–09, doi:10.1021/nl080290y.
short: A. Rastelli, M. Stoffel, Â. Malachias, T. Merdzhanova, G. Katsaros, K. Kern,
T. Metzger, O. Schmidt, Nano Letters 8 (2008) 1404–1409.
date_created: 2018-12-11T11:53:48Z
date_published: 2008-05-01T00:00:00Z
date_updated: 2021-01-12T06:52:57Z
day: '01'
doi: 10.1021/nl080290y
extern: 1
intvolume: ' 8'
issue: '5'
month: '05'
page: 1404 - 1409
publication: Nano Letters
publication_status: published
publisher: American Chemical Society
publist_id: '5374'
quality_controlled: 0
status: public
title: Three-dimensional composition profiles of single quantum dots determined by
scanning-probe-microscopy-based nanotomography
type: journal_article
volume: 8
year: '2008'
...
---
_id: '1751'
abstract:
- lang: eng
text: When strained Stranski-Krastanow islands are used as "self-assembled
quantum dots," a key goal is to control the island position. Here we show
that nanoscale grooves can control the nucleation of epitaxial Ge islands on Si(001),
and can drive lateral motion of existing islands onto the grooves, even when the
grooves are very narrow and shallow compared to the islands. A position centered
on the groove minimizes energy. We use as prototype grooves the trenches which
form naturally around islands. During coarsening, the shrinking islands move laterally
to sit directly astride that trench. In subsequent growth, we demonstrate that
islands nucleate on the "empty trenches" which remain on the surface
after complete dissolution of the original islands.
author:
- first_name: Georgios
full_name: Georgios Katsaros
id: 38DB5788-F248-11E8-B48F-1D18A9856A87
last_name: Katsaros
- first_name: Jerry
full_name: Tersoff, Jerry
last_name: Tersoff
- first_name: Mathieu
full_name: Stoffel, Mathieu
last_name: Stoffel
- first_name: Armando
full_name: Rastelli, Armando
last_name: Rastelli
- first_name: P
full_name: Acosta-Diaz, P
last_name: Acosta Diaz
- first_name: Gouranga
full_name: Kar, Gouranga S
last_name: Kar
- first_name: Giovanni
full_name: Costantini, Giovanni
last_name: Costantini
- first_name: Oliver
full_name: Schmidt, Oliver G
last_name: Schmidt
- first_name: Klaus
full_name: Kern, Klaus
last_name: Kern
citation:
ama: Katsaros G, Tersoff J, Stoffel M, et al. Positioning of strained islands by
interaction with surface nanogrooves. Physical Review Letters. 2008;101(9).
doi:10.1103/PhysRevLett.101.096103
apa: Katsaros, G., Tersoff, J., Stoffel, M., Rastelli, A., Acosta Diaz, P., Kar,
G., … Kern, K. (2008). Positioning of strained islands by interaction with surface
nanogrooves. Physical Review Letters. American Physical Society. https://doi.org/10.1103/PhysRevLett.101.096103
chicago: Katsaros, Georgios, Jerry Tersoff, Mathieu Stoffel, Armando Rastelli, P
Acosta Diaz, Gouranga Kar, Giovanni Costantini, Oliver Schmidt, and Klaus Kern.
“Positioning of Strained Islands by Interaction with Surface Nanogrooves.” Physical
Review Letters. American Physical Society, 2008. https://doi.org/10.1103/PhysRevLett.101.096103.
ieee: G. Katsaros et al., “Positioning of strained islands by interaction
with surface nanogrooves,” Physical Review Letters, vol. 101, no. 9. American
Physical Society, 2008.
ista: Katsaros G, Tersoff J, Stoffel M, Rastelli A, Acosta Diaz P, Kar G, Costantini
G, Schmidt O, Kern K. 2008. Positioning of strained islands by interaction with
surface nanogrooves. Physical Review Letters. 101(9).
mla: Katsaros, Georgios, et al. “Positioning of Strained Islands by Interaction
with Surface Nanogrooves.” Physical Review Letters, vol. 101, no. 9, American
Physical Society, 2008, doi:10.1103/PhysRevLett.101.096103.
short: G. Katsaros, J. Tersoff, M. Stoffel, A. Rastelli, P. Acosta Diaz, G. Kar,
G. Costantini, O. Schmidt, K. Kern, Physical Review Letters 101 (2008).
date_created: 2018-12-11T11:53:49Z
date_published: 2008-08-29T00:00:00Z
date_updated: 2021-01-12T06:52:58Z
day: '29'
doi: 10.1103/PhysRevLett.101.096103
extern: 1
intvolume: ' 101'
issue: '9'
month: '08'
publication: Physical Review Letters
publication_status: published
publisher: American Physical Society
publist_id: '5373'
quality_controlled: 0
status: public
title: Positioning of strained islands by interaction with surface nanogrooves
type: journal_article
volume: 101
year: '2008'
...
---
_id: '1763'
abstract:
- lang: eng
text: The field of cavity quantum electrodynamics (QED), traditionally studied in
atomic systems, has gained new momentum by recent reports of quantum optical experiments
with solid-state semiconducting and superconducting systems. In cavity QED, the
observation of the vacuum Rabi mode splitting is used to investigate the nature
of matter-light interaction at a quantum-mechanical level. However, this effect
can, at least in principle, be explained classically as the normal mode splitting
of two coupled linear oscillators. It has been suggested that an observation of
the scaling of the resonant atom-photon coupling strength in the Jaynes-Cummings
energy ladder with the square root of photon number n is sufficient to prove that
the system is quantum mechanical in nature. Here we report a direct spectroscopic
observation of this characteristic quantum nonlinearity. Measuring the photonic
degree of freedom of the coupled system, our measurements provide unambiguous
spectroscopic evidence for the quantum nature of the resonant atom-field interaction
in cavity QED. We explore atom-photon superposition states involving up to two
photons, using a spectroscopic pump and probe technique. The experiments have
been performed in a circuit QED set-up, in which very strong coupling is realized
by the large dipole coupling strength and the long coherence time of a superconducting
qubit embedded in a high-quality on-chip microwave cavity. Circuit QED systems
also provide a natural quantum interface between flying qubits (photons) and stationary
qubits for applications in quantum information processing and communication.
acknowledgement: This work was supported by SNF and ETHZ. P.J.L. was supported by
the EU with an MC-EIF. A.B. was supported by NSERC, CIFAR and FQRNT
author:
- first_name: Johannes M
full_name: Johannes Fink
id: 4B591CBA-F248-11E8-B48F-1D18A9856A87
last_name: Fink
orcid: 0000-0001-8112-028X
- first_name: M
full_name: Göppl, M
last_name: Göppl
- first_name: Matthias
full_name: Baur, Matthias P
last_name: Baur
- first_name: R
full_name: Bianchetti, R
last_name: Bianchetti
- first_name: Peter
full_name: Leek, Peter J
last_name: Leek
- first_name: Alexandre
full_name: Blais, Alexandre
last_name: Blais
- first_name: Andreas
full_name: Wallraff, Andreas
last_name: Wallraff
citation:
ama: Fink JM, Göppl M, Baur M, et al. Climbing the Jaynes-Cummings ladder and observing
its √n nonlinearity in a cavity QED system. Nature. 2008;454(7202):315-318.
doi:10.1038/nature07112
apa: Fink, J. M., Göppl, M., Baur, M., Bianchetti, R., Leek, P., Blais, A., &
Wallraff, A. (2008). Climbing the Jaynes-Cummings ladder and observing its √n
nonlinearity in a cavity QED system. Nature. Nature Publishing Group. https://doi.org/10.1038/nature07112
chicago: Fink, Johannes M, M Göppl, Matthias Baur, R Bianchetti, Peter Leek, Alexandre
Blais, and Andreas Wallraff. “Climbing the Jaynes-Cummings Ladder and Observing
Its √n Nonlinearity in a Cavity QED System.” Nature. Nature Publishing
Group, 2008. https://doi.org/10.1038/nature07112.
ieee: J. M. Fink et al., “Climbing the Jaynes-Cummings ladder and observing
its √n nonlinearity in a cavity QED system,” Nature, vol. 454, no. 7202.
Nature Publishing Group, pp. 315–318, 2008.
ista: Fink JM, Göppl M, Baur M, Bianchetti R, Leek P, Blais A, Wallraff A. 2008.
Climbing the Jaynes-Cummings ladder and observing its √n nonlinearity in a cavity
QED system. Nature. 454(7202), 315–318.
mla: Fink, Johannes M., et al. “Climbing the Jaynes-Cummings Ladder and Observing
Its √n Nonlinearity in a Cavity QED System.” Nature, vol. 454, no. 7202,
Nature Publishing Group, 2008, pp. 315–18, doi:10.1038/nature07112.
short: J.M. Fink, M. Göppl, M. Baur, R. Bianchetti, P. Leek, A. Blais, A. Wallraff,
Nature 454 (2008) 315–318.
date_created: 2018-12-11T11:53:53Z
date_published: 2008-07-17T00:00:00Z
date_updated: 2021-01-12T06:53:03Z
day: '17'
doi: 10.1038/nature07112
extern: 1
intvolume: ' 454'
issue: '7202'
main_file_link:
- open_access: '1'
url: http://arxiv.org/abs/0902.1827
month: '07'
oa: 1
page: 315 - 318
publication: Nature
publication_status: published
publisher: Nature Publishing Group
publist_id: '5358'
quality_controlled: 0
status: public
title: Climbing the Jaynes-Cummings ladder and observing its √n nonlinearity in a
cavity QED system
type: journal_article
volume: 454
year: '2008'
...
---
_id: '1764'
abstract:
- lang: eng
text: Quantum theory predicts that empty space is not truly empty. Even in the absence
of any particles or radiation, in pure vacuum, virtual particles are constantly
created and annihilated. In an electromagnetic field, the presence of virtual
photons manifests itself as a small renormalization of the energy of a quantum
system, known as the Lamb shift. We present an experimental observation of the
Lamb shift in a solid-state system. The strong dispersive coupling of a superconducting
electronic circuit acting as a quantum bit (qubit) to the vacuum field in a transmission-line
resonator leads to measurable Lamb shifts of up to 1.4% of the qubit transition
frequency. The qubit is also observed to couple more strongly to the vacuum field
than to a single photon inside the cavity, an effect that is explained by taking
into account the limited anharmonicity of the higher excited qubit states.
acknowledgement: This work was supported by the Swiss National Science Foundation
and ETHZ. P.J.L. was supported by the European Commission with a Marie Curie Intra-European
Fellowship. A.B. was supported by the Natural Sciences and Engineering Research
Council of Canada, Canadian Institute for Advanced Research, and Fonds Québécois
de la Recherche sur la Nature et les Technologies
author:
- first_name: A
full_name: Fragner, A
last_name: Fragner
- first_name: M
full_name: Göppl, M
last_name: Göppl
- first_name: Johannes M
full_name: Johannes Fink
id: 4B591CBA-F248-11E8-B48F-1D18A9856A87
last_name: Fink
orcid: 0000-0001-8112-028X
- first_name: Matthias
full_name: Baur, Matthias P
last_name: Baur
- first_name: R
full_name: Bianchetti, R
last_name: Bianchetti
- first_name: Peter
full_name: Leek, Peter J
last_name: Leek
- first_name: Alexandre
full_name: Blais, Alexandre
last_name: Blais
- first_name: Andreas
full_name: Wallraff, Andreas
last_name: Wallraff
citation:
ama: Fragner A, Göppl M, Fink JM, et al. Resolving vacuum fluctuations in an electrical
circuit by measuring the lamb shift. Science. 2008;322(5906):1357-1360.
doi:10.1126/science.1164482
apa: Fragner, A., Göppl, M., Fink, J. M., Baur, M., Bianchetti, R., Leek, P., …
Wallraff, A. (2008). Resolving vacuum fluctuations in an electrical circuit by
measuring the lamb shift. Science. American Association for the Advancement
of Science. https://doi.org/10.1126/science.1164482
chicago: Fragner, A, M Göppl, Johannes M Fink, Matthias Baur, R Bianchetti, Peter
Leek, Alexandre Blais, and Andreas Wallraff. “Resolving Vacuum Fluctuations in
an Electrical Circuit by Measuring the Lamb Shift.” Science. American Association
for the Advancement of Science, 2008. https://doi.org/10.1126/science.1164482.
ieee: A. Fragner et al., “Resolving vacuum fluctuations in an electrical
circuit by measuring the lamb shift,” Science, vol. 322, no. 5906. American
Association for the Advancement of Science, pp. 1357–1360, 2008.
ista: Fragner A, Göppl M, Fink JM, Baur M, Bianchetti R, Leek P, Blais A, Wallraff
A. 2008. Resolving vacuum fluctuations in an electrical circuit by measuring the
lamb shift. Science. 322(5906), 1357–1360.
mla: Fragner, A., et al. “Resolving Vacuum Fluctuations in an Electrical Circuit
by Measuring the Lamb Shift.” Science, vol. 322, no. 5906, American Association
for the Advancement of Science, 2008, pp. 1357–60, doi:10.1126/science.1164482.
short: A. Fragner, M. Göppl, J.M. Fink, M. Baur, R. Bianchetti, P. Leek, A. Blais,
A. Wallraff, Science 322 (2008) 1357–1360.
date_created: 2018-12-11T11:53:53Z
date_published: 2008-11-28T00:00:00Z
date_updated: 2021-01-12T06:53:03Z
day: '28'
doi: 10.1126/science.1164482
extern: 1
intvolume: ' 322'
issue: '5906'
month: '11'
page: 1357 - 1360
publication: Science
publication_status: published
publisher: American Association for the Advancement of Science
publist_id: '5357'
quality_controlled: 0
status: public
title: Resolving vacuum fluctuations in an electrical circuit by measuring the lamb
shift
type: journal_article
volume: 322
year: '2008'
...
---
_id: '1765'
abstract:
- lang: eng
text: High quality on-chip microwave resonators have recently found prominent new
applications in quantum optics and quantum information processing experiments
with superconducting electronic circuits, a field now known as circuit quantum
electrodynamics (QED). They are also used as single photon detectors and parametric
amplifiers. Here we analyze the physical properties of coplanar waveguide resonators
and their relation to the materials properties for use in circuit QED. We have
designed and fabricated resonators with fundamental frequencies from 2 to 9 GHz
and quality factors ranging from a few hundreds to a several hundred thousands
controlled by appropriately designed input and output coupling capacitors. The
microwave transmission spectra measured at temperatures of 20 mK are shown to
be in good agreement with theoretical lumped element and distributed element transmission
matrix models. In particular, the experimentally determined resonance frequencies,
quality factors, and insertion losses are fully and consistently explained by
the two models for all measured devices. The high level of control and flexibility
in design renders these resonators ideal for storing and manipulating quantum
electromagnetic fields in integrated superconducting electronic circuits.
acknowledgement: This work was supported by Swiss National Fund (SNF) and ETH Zürich.
P.J.L. was supported by the EC with a MC-EIF
author:
- first_name: M
full_name: Göppl, M
last_name: Göppl
- first_name: A
full_name: Fragner, A
last_name: Fragner
- first_name: Matthias
full_name: Baur, Matthias P
last_name: Baur
- first_name: R
full_name: Bianchetti, R
last_name: Bianchetti
- first_name: Stefan
full_name: Filipp, Stefan
last_name: Filipp
- first_name: Johannes M
full_name: Johannes Fink
id: 4B591CBA-F248-11E8-B48F-1D18A9856A87
last_name: Fink
orcid: 0000-0001-8112-028X
- first_name: Peter
full_name: Leek, Peter J
last_name: Leek
- first_name: G
full_name: Puebla, G
last_name: Puebla
- first_name: L.
full_name: Steffen, L. Kraig
last_name: Steffen
- first_name: Andreas
full_name: Wallraff, Andreas
last_name: Wallraff
citation:
ama: Göppl M, Fragner A, Baur M, et al. Coplanar waveguide resonators for circuit
quantum electrodynamics. Journal of Applied Physics. 2008;104(11). doi:10.1063/1.3010859
apa: Göppl, M., Fragner, A., Baur, M., Bianchetti, R., Filipp, S., Fink, J. M.,
… Wallraff, A. (2008). Coplanar waveguide resonators for circuit quantum electrodynamics.
Journal of Applied Physics. American Institute of Physics. https://doi.org/10.1063/1.3010859
chicago: Göppl, M, A Fragner, Matthias Baur, R Bianchetti, Stefan Filipp, Johannes
M Fink, Peter Leek, G Puebla, L. Steffen, and Andreas Wallraff. “Coplanar Waveguide
Resonators for Circuit Quantum Electrodynamics.” Journal of Applied Physics.
American Institute of Physics, 2008. https://doi.org/10.1063/1.3010859.
ieee: M. Göppl et al., “Coplanar waveguide resonators for circuit quantum
electrodynamics,” Journal of Applied Physics, vol. 104, no. 11. American
Institute of Physics, 2008.
ista: Göppl M, Fragner A, Baur M, Bianchetti R, Filipp S, Fink JM, Leek P, Puebla
G, Steffen L, Wallraff A. 2008. Coplanar waveguide resonators for circuit quantum
electrodynamics. Journal of Applied Physics. 104(11).
mla: Göppl, M., et al. “Coplanar Waveguide Resonators for Circuit Quantum Electrodynamics.”
Journal of Applied Physics, vol. 104, no. 11, American Institute of Physics,
2008, doi:10.1063/1.3010859.
short: M. Göppl, A. Fragner, M. Baur, R. Bianchetti, S. Filipp, J.M. Fink, P. Leek,
G. Puebla, L. Steffen, A. Wallraff, Journal of Applied Physics 104 (2008).
date_created: 2018-12-11T11:53:53Z
date_published: 2008-01-01T00:00:00Z
date_updated: 2021-01-12T06:53:03Z
day: '01'
doi: 10.1063/1.3010859
extern: 1
intvolume: ' 104'
issue: '11'
main_file_link:
- open_access: '1'
url: http://arxiv.org/abs/0807.4094
month: '01'
oa: 1
publication: Journal of Applied Physics
publication_status: published
publisher: American Institute of Physics
publist_id: '5355'
quality_controlled: 0
status: public
title: Coplanar waveguide resonators for circuit quantum electrodynamics
type: journal_article
volume: 104
year: '2008'
...
---
_id: '17721'
abstract:
- lang: eng
text: High-redshift quasars (z >~ 6) drive ionization fronts into the intergalactic
medium (IGM). If the thickness of the front can be measured, it can provide a
novel constraint on the ionizing spectral energy distribution (SED). Here we follow
the propagation of an I-front into a uniform IGM, and compute its thickness for
a range of possible quasar spectra and ages. We also explore the effects of uniform
and non-uniform ionizing backgrounds. We find that even for hard spectra, the
fronts are initially thin, with a thickness much smaller than the mean free path
of ionizing photons, but the thickness increases as the front approaches equilibrium
in 10^8 - 10^9 years, and can eventually significantly exceed simple estimates
based on the mean free path. With a high intrinsic hydrogen column density obscuring
the source (log(N_H/cm^-2) >~ 19.2) or a hard power-law spectrum combined with
some obscuration (e.g. dlog(F_\nu)/dlog(\nu) >~ -1.2 at log(N_H/cm^-2) >~ 18.0),
the thickness of the front exceeds ~1 physical Mpc and may be measurable from
the morphology of its redshifted 21cm signal. We find that the highly ionized
inner part of the front, which may be probed by Lyman line absorption spectra,
remains sharp for bright quasars unless a large obscuring column (log(N_H/cm^-2)
>~ 19.2) removes most of their ionizing photons up to ~40 eV. For obscured sources
with log(N_H/cm^-2) >~ 19.8, embedded in a significantly neutral IGM, the black
Lyman-alpha trough (where the neutral fraction is ~10^-3) underestimates the size
of the HII region by a factor of >~4.
article_processing_charge: No
article_type: original
author:
- first_name: R. H.
full_name: Kramer, R. H.
last_name: Kramer
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
citation:
ama: Kramer RH, Haiman Z. The thickness of high-redshift quasar ionization fronts
as a constraint on the ionizing spectral energy distribution. Monthly Notices
of the Royal Astronomical Society. 2008;385(3):1561-1575. doi:10.1111/j.1365-2966.2008.12945.x
apa: Kramer, R. H., & Haiman, Z. (2008). The thickness of high-redshift quasar
ionization fronts as a constraint on the ionizing spectral energy distribution.
Monthly Notices of the Royal Astronomical Society. Oxford University Press.
https://doi.org/10.1111/j.1365-2966.2008.12945.x
chicago: Kramer, R. H., and Zoltán Haiman. “The Thickness of High-Redshift Quasar
Ionization Fronts as a Constraint on the Ionizing Spectral Energy Distribution.”
Monthly Notices of the Royal Astronomical Society. Oxford University Press,
2008. https://doi.org/10.1111/j.1365-2966.2008.12945.x.
ieee: R. H. Kramer and Z. Haiman, “The thickness of high-redshift quasar ionization
fronts as a constraint on the ionizing spectral energy distribution,” Monthly
Notices of the Royal Astronomical Society, vol. 385, no. 3. Oxford University
Press, pp. 1561–1575, 2008.
ista: Kramer RH, Haiman Z. 2008. The thickness of high-redshift quasar ionization
fronts as a constraint on the ionizing spectral energy distribution. Monthly Notices
of the Royal Astronomical Society. 385(3), 1561–1575.
mla: Kramer, R. H., and Zoltán Haiman. “The Thickness of High-Redshift Quasar Ionization
Fronts as a Constraint on the Ionizing Spectral Energy Distribution.” Monthly
Notices of the Royal Astronomical Society, vol. 385, no. 3, Oxford University
Press, 2008, pp. 1561–75, doi:10.1111/j.1365-2966.2008.12945.x.
short: R.H. Kramer, Z. Haiman, Monthly Notices of the Royal Astronomical Society
385 (2008) 1561–1575.
date_created: 2024-09-06T09:09:01Z
date_published: 2008-03-13T00:00:00Z
date_updated: 2024-09-25T13:54:14Z
day: '13'
doi: 10.1111/j.1365-2966.2008.12945.x
extern: '1'
intvolume: ' 385'
issue: '3'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1111/j.1365-2966.2008.12945.x
month: '03'
oa: 1
oa_version: Published Version
page: 1561-1575
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
issn:
- 0035-8711
- 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: The thickness of high-redshift quasar ionization fronts as a constraint on
the ionizing spectral energy distribution
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 385
year: '2008'
...
---
_id: '17734'
abstract:
- lang: eng
text: Electromagnetic (EM) counterparts to supermassive black hole binary mergers
observed by LISA can be localized to within the field of view of astronomical
instruments ~10 deg^2 hours to weeks prior to coalescence. The temporal coincidence
of any prompt EM counterpart with a gravitationally-timed merger may offer the
best chance of identifying a unique host galaxy. We discuss the challenges posed
by searches for prompt EM counterparts and propose novel observational strategies
to address them. In particular, we discuss the size and shape evolution of the
LISA localization error ellipses on the sky, and quantify the requirements for
dedicated EM surveys of the area prior to coalescence. A triggered EM counterpart
search campaign will require monitoring a several-square degree area. It could
aim for variability at the 24-27 mag level in optical bands, for example, which
corresponds to 1-10% of the Eddington luminosity of the prime LISA sources of
10^6-10^7 Msun BHs at z=1-2, on time-scales of minutes to hours, the orbital time-scale
of the binary in the last 2-4 weeks. A cross-correlation of the period of any
variable EM signal with the quasi-periodic gravitational waveform over 10-1000
cycles may aid the detection. Alternatively, EM searches can detect a transient
signal accompanying the coalescence. We highlight the measurement of differences
in the arrival times of photons and gravitons from the same cosmological source
as a valuable independent test of the massive character of gravity, and of possible
violations of Lorentz invariance in the gravity sector.
article_processing_charge: No
article_type: original
author:
- first_name: Bence
full_name: Kocsis, Bence
last_name: Kocsis
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Kristen
full_name: Menou, Kristen
last_name: Menou
citation:
ama: 'Kocsis B, Haiman Z, Menou K. Premerger localization of gravitational wave
standard sirens with LISA: Triggered search for an electromagnetic counterpart.
The Astrophysical Journal. 2008;684(2):870-887. doi:10.1086/590230'
apa: 'Kocsis, B., Haiman, Z., & Menou, K. (2008). Premerger localization of
gravitational wave standard sirens with LISA: Triggered search for an electromagnetic
counterpart. The Astrophysical Journal. American Astronomical Society.
https://doi.org/10.1086/590230'
chicago: 'Kocsis, Bence, Zoltán Haiman, and Kristen Menou. “Premerger Localization
of Gravitational Wave Standard Sirens with LISA: Triggered Search for an Electromagnetic
Counterpart.” The Astrophysical Journal. American Astronomical Society,
2008. https://doi.org/10.1086/590230.'
ieee: 'B. Kocsis, Z. Haiman, and K. Menou, “Premerger localization of gravitational
wave standard sirens with LISA: Triggered search for an electromagnetic counterpart,”
The Astrophysical Journal, vol. 684, no. 2. American Astronomical Society,
pp. 870–887, 2008.'
ista: 'Kocsis B, Haiman Z, Menou K. 2008. Premerger localization of gravitational
wave standard sirens with LISA: Triggered search for an electromagnetic counterpart.
The Astrophysical Journal. 684(2), 870–887.'
mla: 'Kocsis, Bence, et al. “Premerger Localization of Gravitational Wave Standard
Sirens with LISA: Triggered Search for an Electromagnetic Counterpart.” The
Astrophysical Journal, vol. 684, no. 2, American Astronomical Society, 2008,
pp. 870–87, doi:10.1086/590230.'
short: B. Kocsis, Z. Haiman, K. Menou, The Astrophysical Journal 684 (2008) 870–887.
date_created: 2024-09-06T09:18:47Z
date_published: 2008-09-10T00:00:00Z
date_updated: 2024-09-26T07:56:49Z
day: '10'
doi: 10.1086/590230
extern: '1'
intvolume: ' 684'
issue: '2'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1086/590230
month: '09'
oa: 1
oa_version: Published Version
page: 870-887
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Premerger localization of gravitational wave standard sirens with LISA: Triggered
search for an electromagnetic counterpart'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 684
year: '2008'
...
---
_id: '17751'
abstract:
- lang: eng
text: With the help of numerical simulations, we examine two aspects of feedback
from the first generation of stars on later star formation. First, we investigate
the impact of relic HII regions on forming halos. We find that the positive and
negative effects of such feedback nearly cancel because the increase in entropy
due to heating is balanced by the increase in the H 2 fraction due to the free
electrons. However, these halos can be delayed more easily by a background Lyman-Werner
flux. Second, we show that HD cooling is important in halos which have been ionized
and allowed to recombine. Gas is allowed to cool to the CMB temperature at densities
around n∼10 4cm-3, reducing the accreted mass by a factor of a few. However, as
the collapse proceeds, the central gas density exceeds the critical density of
HD and heats until HD cooling is no longer important. Therefore the behaviour
of the (smaller mass) core is relatively unaffected by HD cooling.
article_processing_charge: No
author:
- first_name: Greg L.
full_name: Bryan, Greg L.
last_name: Bryan
- first_name: Ian D.
full_name: McGreer, Ian D.
last_name: McGreer
- first_name: Andrei
full_name: Mesinger, Andrei
last_name: Mesinger
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
citation:
ama: 'Bryan GL, McGreer ID, Mesinger A, Haiman Z. Feedback effects on population
III star formation. In: AIP Conference Proceedings. American Institute
of Physics; 2008. doi:10.1063/1.2905582'
apa: 'Bryan, G. L., McGreer, I. D., Mesinger, A., & Haiman, Z. (2008). Feedback
effects on population III star formation. In AIP Conference Proceedings.
Santa Fe, NM, United States: American Institute of Physics. https://doi.org/10.1063/1.2905582'
chicago: Bryan, Greg L., Ian D. McGreer, Andrei Mesinger, and Zoltán Haiman. “Feedback
Effects on Population III Star Formation.” In AIP Conference Proceedings.
American Institute of Physics, 2008. https://doi.org/10.1063/1.2905582.
ieee: G. L. Bryan, I. D. McGreer, A. Mesinger, and Z. Haiman, “Feedback effects
on population III star formation,” in AIP Conference Proceedings, Santa
Fe, NM, United States, 2008.
ista: 'Bryan GL, McGreer ID, Mesinger A, Haiman Z. 2008. Feedback effects on population
III star formation. AIP Conference Proceedings. FIRST STARS III: First Stars II
Conference.'
mla: Bryan, Greg L., et al. “Feedback Effects on Population III Star Formation.”
AIP Conference Proceedings, American Institute of Physics, 2008, doi:10.1063/1.2905582.
short: G.L. Bryan, I.D. McGreer, A. Mesinger, Z. Haiman, in:, AIP Conference Proceedings,
American Institute of Physics, 2008.
conference:
end_date: 2007-07-20
location: Santa Fe, NM, United States
name: 'FIRST STARS III: First Stars II Conference'
start_date: 2007-07-15
date_created: 2024-09-06T09:39:10Z
date_published: 2008-03-11T00:00:00Z
date_updated: 2024-09-30T07:46:06Z
day: '11'
doi: 10.1063/1.2905582
extern: '1'
language:
- iso: eng
main_file_link:
- url: https://doi.org/10.1063/1.2905582
month: '03'
oa_version: None
publication: AIP Conference Proceedings
publication_identifier:
issn:
- 0094-243X
publication_status: published
publisher: American Institute of Physics
quality_controlled: '1'
scopus_import: '1'
status: public
title: Feedback effects on population III star formation
type: conference
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
year: '2008'
...
---
_id: '17752'
abstract:
- lang: eng
text: Supermassive black hole binaries (BHBs) produced in galaxy mergers recoil
at the time of their coalescence due to the emission of gravitational waves (GWs).
We simulate the response of a thin, 2D disk of collisionless particles, initially
on circular orbits around a 10^6 M_sun BHB, to kicks that are either parallel
or perpendicular to the initial orbital plane. Typical kick velocities (v_k) can
exceed the sound speed in a circumbinary gas disk. While the inner disk is strongly
bound to the recoiling binary, the outer disk is only weakly bound or unbound.
This leads to differential motions in the disturbed disk that increase with radius
and can become supersonic at ~700 Schwarzschild radii for v_k ~500 km/s, implying
that shocks form beyond this radius. We indeed find that kicks in the disk plane
lead to immediate strong density enhancements (within weeks) in a tightly wound
spiral caustic, propagating outward at the speed v_k. Concentric density enhancements
are also observed for kicks perpendicular to the disk, but are weaker and develop
into caustics only after a long delay (>1 year). Unless both BH spins are low
or precisely aligned with the orbital angular momentum, a significant fraction
(> several %) of kicks are sufficiently large and well aligned with the orbital
plane for strong shocks to be produced. The shocks could result in an afterglow
whose characteristic photon energy increases with time, from the UV (~10eV) to
the soft X-ray (~100eV) range, between one month and one year after the merger.
This could help identify EM counterparts to GW sources discovered by LISA.
article_processing_charge: No
article_type: original
author:
- first_name: Zoltán
full_name: Lippai, Zoltán
last_name: Lippai
- first_name: Zsolt
full_name: Frei, Zsolt
last_name: Frei
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
citation:
ama: Lippai Z, Frei Z, Haiman Z. Prompt shocks in the gas disk around a recoiling
supermassive black hole binary. The Astrophysical Journal. 2008;676(1):L5-L8.
doi:10.1086/587034
apa: Lippai, Z., Frei, Z., & Haiman, Z. (2008). Prompt shocks in the gas disk
around a recoiling supermassive black hole binary. The Astrophysical Journal.
American Astronomical Society. https://doi.org/10.1086/587034
chicago: Lippai, Zoltán, Zsolt Frei, and Zoltán Haiman. “Prompt Shocks in the Gas
Disk around a Recoiling Supermassive Black Hole Binary.” The Astrophysical
Journal. American Astronomical Society, 2008. https://doi.org/10.1086/587034.
ieee: Z. Lippai, Z. Frei, and Z. Haiman, “Prompt shocks in the gas disk around a
recoiling supermassive black hole binary,” The Astrophysical Journal, vol.
676, no. 1. American Astronomical Society, pp. L5–L8, 2008.
ista: Lippai Z, Frei Z, Haiman Z. 2008. Prompt shocks in the gas disk around a recoiling
supermassive black hole binary. The Astrophysical Journal. 676(1), L5–L8.
mla: Lippai, Zoltán, et al. “Prompt Shocks in the Gas Disk around a Recoiling Supermassive
Black Hole Binary.” The Astrophysical Journal, vol. 676, no. 1, American
Astronomical Society, 2008, pp. L5–8, doi:10.1086/587034.
short: Z. Lippai, Z. Frei, Z. Haiman, The Astrophysical Journal 676 (2008) L5–L8.
date_created: 2024-09-06T09:40:05Z
date_published: 2008-03-20T00:00:00Z
date_updated: 2024-09-30T07:50:45Z
day: '20'
doi: 10.1086/587034
extern: '1'
intvolume: ' 676'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1086/587034
month: '03'
oa: 1
oa_version: Published Version
page: L5-L8
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Prompt shocks in the gas disk around a recoiling supermassive black hole binary
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 676
year: '2008'
...
---
_id: '17756'
abstract:
- lang: eng
text: At the epoch of reionization, when the high-redshift inter-galactic medium
(IGM) is being enriched with metals, the 63.2 micron fine structure line of OI
is pumped by the ~ 1300 AA soft UV background and introduces a spectral distortion
in the Cosmic Microwave Background (CMB). Here we use a toy model for the spatial
distribution of neutral oxygen, assuming metal bubbles surround dark matter halos,
and compute the fluctuations of this distortion, and the angular power spectrum
it imprints on the CMB. We discuss the dependence of the power spectrum on the
velocity of the winds polluting the IGM with metals, the minimum mass of the halos
producing these winds, and on the cosmic epoch when the OI pumping occurs. We
find that, although the clustering signal of the CMB distortion is weak \delta
y_{rms} ~ 10^{-7} (roughly corresponding to a temperature anisotropy of few nK),
it may be reachable in deep integrations with high-sensitivity infrared detectors.
Even without a detection, these instruments should be able to useful constraints
on the heavy element enrichment history of the IGM.
article_processing_charge: No
article_type: original
author:
- first_name: Carlos
full_name: Hernandez‐Monteagudo, Carlos
last_name: Hernandez‐Monteagudo
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Licia
full_name: Verde, Licia
last_name: Verde
- first_name: Raul
full_name: Jimenez, Raul
last_name: Jimenez
citation:
ama: Hernandez‐Monteagudo C, Haiman Z, Verde L, Jimenez R. Oxygen pumping. II. Probing
the inhomogeneous metal enrichment at the epoch of reionization with high‐frequency
CMB observations. The Astrophysical Journal. 2008;672(1):33-39. doi:10.1086/523872
apa: Hernandez‐Monteagudo, C., Haiman, Z., Verde, L., & Jimenez, R. (2008).
Oxygen pumping. II. Probing the inhomogeneous metal enrichment at the epoch of
reionization with high‐frequency CMB observations. The Astrophysical Journal.
American Astronomical Society. https://doi.org/10.1086/523872
chicago: Hernandez‐Monteagudo, Carlos, Zoltán Haiman, Licia Verde, and Raul Jimenez.
“Oxygen Pumping. II. Probing the Inhomogeneous Metal Enrichment at the Epoch of
Reionization with High‐frequency CMB Observations.” The Astrophysical Journal.
American Astronomical Society, 2008. https://doi.org/10.1086/523872.
ieee: C. Hernandez‐Monteagudo, Z. Haiman, L. Verde, and R. Jimenez, “Oxygen pumping.
II. Probing the inhomogeneous metal enrichment at the epoch of reionization with
high‐frequency CMB observations,” The Astrophysical Journal, vol. 672,
no. 1. American Astronomical Society, pp. 33–39, 2008.
ista: Hernandez‐Monteagudo C, Haiman Z, Verde L, Jimenez R. 2008. Oxygen pumping.
II. Probing the inhomogeneous metal enrichment at the epoch of reionization with
high‐frequency CMB observations. The Astrophysical Journal. 672(1), 33–39.
mla: Hernandez‐Monteagudo, Carlos, et al. “Oxygen Pumping. II. Probing the Inhomogeneous
Metal Enrichment at the Epoch of Reionization with High‐frequency CMB Observations.”
The Astrophysical Journal, vol. 672, no. 1, American Astronomical Society,
2008, pp. 33–39, doi:10.1086/523872.
short: C. Hernandez‐Monteagudo, Z. Haiman, L. Verde, R. Jimenez, The Astrophysical
Journal 672 (2008) 33–39.
date_created: 2024-09-06T09:44:50Z
date_published: 2008-01-01T00:00:00Z
date_updated: 2024-09-30T08:39:17Z
day: '01'
doi: 10.1086/523872
extern: '1'
intvolume: ' 672'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1086/523872
month: '01'
oa: 1
oa_version: Published Version
page: 33-39
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Oxygen pumping. II. Probing the inhomogeneous metal enrichment at the epoch
of reionization with high‐frequency CMB observations
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 672
year: '2008'
...
---
_id: '17762'
abstract:
- lang: eng
text: "We conduct a Markov Chain Monte Carlo study of the Dvali-Gabadadze-Porrati
self-accelerating braneworld scenario given the cosmic microwave background (CMB)
anisotropy, supernovae and Hubble constant data by implementing an effective dark
energy prescription for modified gravity into a standard Einstein-Boltzmann code.
We find no way to alleviate the tension between distance measures and horizon-scale
growth in this model. Growth alterations due to perturbations propagating into
the bulk appear as excess CMB anisotropy at the lowest multipoles. In a flat cosmology,
the maximum likelihood Dvali-Gabadadze-Porrati model is nominally a 5.3\U0001D70E
poorer fit than \U0001D6ECCDM. Curvature can reduce the tension between distance
measures but only at the expense of exacerbating the problem with growth leading
to a 4.8\U0001D70E result that is dominated by the low multipole CMB temperature
spectrum. While changing the initial conditions to reduce large-scale power can
flatten the temperature spectrum, this also suppresses the large angle polarization
spectrum in violation of recent results from the five-year Wilkinson Microwave
Anisotropy Probe. The failure of this model highlights the power of combining
growth and distance measures in cosmology as a test of gravity on the largest
scales."
article_number: '103509'
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Wenjuan
full_name: Fang, Wenjuan
last_name: Fang
- first_name: Sheng
full_name: Wang, Sheng
last_name: Wang
- first_name: Wayne
full_name: Hu, Wayne
last_name: Hu
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Lam
full_name: Hui, Lam
last_name: Hui
- first_name: Morgan
full_name: May, Morgan
last_name: May
citation:
ama: Fang W, Wang S, Hu W, Haiman Z, Hui L, May M. Challenges to the DGP model from
horizon-scale growth and geometry. Physical Review D. 2008;78(10). doi:10.1103/physrevd.78.103509
apa: Fang, W., Wang, S., Hu, W., Haiman, Z., Hui, L., & May, M. (2008). Challenges
to the DGP model from horizon-scale growth and geometry. Physical Review D.
American Physical Society. https://doi.org/10.1103/physrevd.78.103509
chicago: Fang, Wenjuan, Sheng Wang, Wayne Hu, Zoltán Haiman, Lam Hui, and Morgan
May. “Challenges to the DGP Model from Horizon-Scale Growth and Geometry.” Physical
Review D. American Physical Society, 2008. https://doi.org/10.1103/physrevd.78.103509.
ieee: W. Fang, S. Wang, W. Hu, Z. Haiman, L. Hui, and M. May, “Challenges to the
DGP model from horizon-scale growth and geometry,” Physical Review D, vol.
78, no. 10. American Physical Society, 2008.
ista: Fang W, Wang S, Hu W, Haiman Z, Hui L, May M. 2008. Challenges to the DGP
model from horizon-scale growth and geometry. Physical Review D. 78(10), 103509.
mla: Fang, Wenjuan, et al. “Challenges to the DGP Model from Horizon-Scale Growth
and Geometry.” Physical Review D, vol. 78, no. 10, 103509, American Physical
Society, 2008, doi:10.1103/physrevd.78.103509.
short: W. Fang, S. Wang, W. Hu, Z. Haiman, L. Hui, M. May, Physical Review D 78
(2008).
date_created: 2024-09-06T09:49:53Z
date_published: 2008-11-10T00:00:00Z
date_updated: 2024-09-30T09:16:05Z
day: '10'
doi: 10.1103/physrevd.78.103509
extern: '1'
external_id:
arxiv:
- '0808.2208'
intvolume: ' 78'
issue: '10'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: ' https://doi.org/10.48550/arXiv.0808.2208'
month: '11'
oa: 1
oa_version: Preprint
publication: Physical Review D
publication_identifier:
issn:
- 1550-7998
- 1550-2368
publication_status: published
publisher: American Physical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Challenges to the DGP model from horizon-scale growth and geometry
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 78
year: '2008'
...
---
_id: '17773'
abstract:
- lang: eng
text: The notion that microparsec-scale black holes can be used to probe gigaparsec-scale
physics may seem counterintuitive, at first. Yet, the gravitational observatory
LISA will detect cosmologically-distant coalescing pairs of massive black holes,
accurately measure their luminosity distance and help identify an electromagnetic
counterpart or a host galaxy. A wide variety of new black hole studies and a gravitational
version of Hubble’s diagram become possible, if host galaxies are successfully
identified. Furthermore, if dark energy is a manifestation of large-scale modified
gravity, deviations from general relativistic expectations could become apparent
in a gravitational signal propagated over cosmological scales, especially when
compared to the electromagnetic signal from a same source. Finally, since inspirals
of white dwarfs into massive black holes at cosmological distances may permit
pre-merger localizations, we suggest that careful monitoring of these events and
any associated electromagnetic counterpart could lead to high-precision cosmological
measurements with LISA.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: Kristen
full_name: Menou, Kristen
last_name: Menou
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Bence
full_name: Kocsis, Bence
last_name: Kocsis
citation:
ama: Menou K, Haiman Z, Kocsis B. Cosmological physics with black holes (and possibly
white dwarfs). New Astronomy Reviews. 2008;51(10-12):884-890. doi:10.1016/j.newar.2008.03.020
apa: Menou, K., Haiman, Z., & Kocsis, B. (2008). Cosmological physics with black
holes (and possibly white dwarfs). New Astronomy Reviews. Elsevier BV.
https://doi.org/10.1016/j.newar.2008.03.020
chicago: Menou, Kristen, Zoltán Haiman, and Bence Kocsis. “Cosmological Physics
with Black Holes (and Possibly White Dwarfs).” New Astronomy Reviews. Elsevier
BV, 2008. https://doi.org/10.1016/j.newar.2008.03.020.
ieee: K. Menou, Z. Haiman, and B. Kocsis, “Cosmological physics with black holes
(and possibly white dwarfs),” New Astronomy Reviews, vol. 51, no. 10–12.
Elsevier BV, pp. 884–890, 2008.
ista: Menou K, Haiman Z, Kocsis B. 2008. Cosmological physics with black holes (and
possibly white dwarfs). New Astronomy Reviews. 51(10–12), 884–890.
mla: Menou, Kristen, et al. “Cosmological Physics with Black Holes (and Possibly
White Dwarfs).” New Astronomy Reviews, vol. 51, no. 10–12, Elsevier BV,
2008, pp. 884–90, doi:10.1016/j.newar.2008.03.020.
short: K. Menou, Z. Haiman, B. Kocsis, New Astronomy Reviews 51 (2008) 884–890.
date_created: 2024-09-06T10:02:53Z
date_published: 2008-05-01T00:00:00Z
date_updated: 2024-09-30T11:28:25Z
day: '01'
doi: 10.1016/j.newar.2008.03.020
extern: '1'
external_id:
arxiv:
- '0803.3627'
intvolume: ' 51'
issue: 10-12
language:
- iso: eng
main_file_link:
- open_access: '1'
url: ' https://doi.org/10.48550/arXiv.0803.3627'
month: '05'
oa: 1
oa_version: Preprint
page: 884-890
publication: New Astronomy Reviews
publication_identifier:
issn:
- 1387-6473
publication_status: published
publisher: Elsevier BV
quality_controlled: '1'
scopus_import: '1'
status: public
title: Cosmological physics with black holes (and possibly white dwarfs)
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 51
year: '2008'
...
---
_id: '17778'
abstract:
- lang: eng
text: The earliest generation of stars and black holes must have established an
early ‘Lyman–Werner’ background (LWB) at high redshift, prior to the epoch of
reionization. Because of the long mean free path of photons with energies hν <
13.6 eV, the LWB was nearly uniform. However, some variation in the LWB is expected
due to the discrete nature of the sources, and their highly clustered spatial
distribution. In this paper, we compute the probability distribution function
(PDF) of the LW flux that irradiates dark matter (DM) haloes collapsing at high
redshift (z≈ 10). Our model accounts for (i) the clustering of DM haloes, (ii)
Poisson fluctuations in the number of corresponding star-forming galaxies and
(iii) scatter in the LW luminosity produced by haloes of a given mass (calibrated
using local observations). We find that >99 per cent of the DM haloes are illuminated
by an LW flux within a factor of 2 of the global mean value. However, a small
fraction, ∼10^−8 to 10^−6, of DM haloes with virial temperatures Tvir≳ 10^4 K
have a close luminous neighbour within ≲10 kpc, and are exposed to an LW flux
exceeding the global mean by a factor of >20, or to J21,LW > 10^3 (in units of
10^−21 erg s^−1 Hz^−1 sr^−1 cm^−2). This large LW flux can photodissociate H2
molecules in the gas collapsing due to atomic cooling in these haloes, and prevent
its further cooling and fragmentation. Such close halo pairs therefore provide
possible sites in which primordial gas clouds collapse directly into massive black
holes (MBH≈ 10^4−6M⊙), and subsequently grow into supermassive (MBH≳ 10^9M⊙) black
holes by z≈ 6.
article_processing_charge: No
article_type: original
author:
- first_name: Mark
full_name: Dijkstra, Mark
last_name: Dijkstra
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: Andrei
full_name: Mesinger, Andrei
last_name: Mesinger
- first_name: J. Stuart B.
full_name: Wyithe, J. Stuart B.
last_name: Wyithe
citation:
ama: 'Dijkstra M, Haiman Z, Mesinger A, Wyithe JSB. Fluctuations in the high-redshift
Lyman-Werner background: Close halo pairs as the origin of supermassive black
holes. Monthly Notices of the Royal Astronomical Society. 2008;391(4):1961-1972.
doi:10.1111/j.1365-2966.2008.14031.x'
apa: 'Dijkstra, M., Haiman, Z., Mesinger, A., & Wyithe, J. S. B. (2008). Fluctuations
in the high-redshift Lyman-Werner background: Close halo pairs as the origin of
supermassive black holes. Monthly Notices of the Royal Astronomical Society.
Oxford University Press. https://doi.org/10.1111/j.1365-2966.2008.14031.x'
chicago: 'Dijkstra, Mark, Zoltán Haiman, Andrei Mesinger, and J. Stuart B. Wyithe.
“Fluctuations in the High-Redshift Lyman-Werner Background: Close Halo Pairs as
the Origin of Supermassive Black Holes.” Monthly Notices of the Royal Astronomical
Society. Oxford University Press, 2008. https://doi.org/10.1111/j.1365-2966.2008.14031.x.'
ieee: 'M. Dijkstra, Z. Haiman, A. Mesinger, and J. S. B. Wyithe, “Fluctuations in
the high-redshift Lyman-Werner background: Close halo pairs as the origin of supermassive
black holes,” Monthly Notices of the Royal Astronomical Society, vol. 391,
no. 4. Oxford University Press, pp. 1961–1972, 2008.'
ista: 'Dijkstra M, Haiman Z, Mesinger A, Wyithe JSB. 2008. Fluctuations in the high-redshift
Lyman-Werner background: Close halo pairs as the origin of supermassive black
holes. Monthly Notices of the Royal Astronomical Society. 391(4), 1961–1972.'
mla: 'Dijkstra, Mark, et al. “Fluctuations in the High-Redshift Lyman-Werner Background:
Close Halo Pairs as the Origin of Supermassive Black Holes.” Monthly Notices
of the Royal Astronomical Society, vol. 391, no. 4, Oxford University Press,
2008, pp. 1961–72, doi:10.1111/j.1365-2966.2008.14031.x.'
short: M. Dijkstra, Z. Haiman, A. Mesinger, J.S.B. Wyithe, Monthly Notices of the
Royal Astronomical Society 391 (2008) 1961–1972.
date_created: 2024-09-06T10:13:39Z
date_published: 2008-12-11T00:00:00Z
date_updated: 2024-09-30T11:57:59Z
day: '11'
doi: 10.1111/j.1365-2966.2008.14031.x
extern: '1'
intvolume: ' 391'
issue: '4'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1111/j.1365-2966.2008.14031.x
month: '12'
oa: 1
oa_version: Published Version
page: 1961-1972
publication: Monthly Notices of the Royal Astronomical Society
publication_identifier:
issn:
- 0035-8711
- 1365-2966
publication_status: published
publisher: Oxford University Press
quality_controlled: '1'
scopus_import: '1'
status: public
title: 'Fluctuations in the high-redshift Lyman-Werner background: Close halo pairs
as the origin of supermassive black holes'
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 391
year: '2008'
...
---
_id: '17787'
abstract:
- lang: eng
text: One of the most dramatic signatures of the reionization era may be the enormous
ionized bubbles around luminous quasars (with radii reaching ~40 comoving Mpc),
which may survive as "fossil" ionized regions long after their source shuts off.
Here we study how the inhomogeneous intergalactic medium (IGM) evolves inside
such fossils. The average recombination rate declines rapidly with time, and the
brief quasar episode significantly increases the mean free path inside the fossil
bubbles. As a result, even a weak ionizing background generated by galaxies inside
the fossil can maintain it in a relatively highly and uniformly ionized state.
For example, galaxies that would ionize 20%-30% of hydrogen in a random patch
of the IGM can maintain 80%-90% ionization inside the fossil for a duration much
longer than the average recombination time in the IGM. Quasar fossils at z≲ 10
thus retain their identity for nearly a Hubble time and appear "gray," distinct
from both the average IGM (which has a "Swiss cheese" ionization topology and
a lower mean ionized fraction) and the fully ionized bubbles around active quasars.
More distant fossils, at z≳ 10, have a weaker galaxy-generated ionizing background
and a higher gas density, so they can attain a Swiss cheese topology similar to
the rest of the IGM, but with a smaller contrast between the ionized bubbles and
the partially neutral regions separating them. Analogous He III fossils should
exist around the epoch of He II/He III reionization at z ∼ 3, although rapid recombination
inside the He III fossils is more common. Our model of inhomogeneous recombination
also applies to "double-reionization" models and shows that a nonmonotonic reionization
history is even more unlikely than previously thought.
article_processing_charge: No
article_type: original
author:
- first_name: Steven R.
full_name: Furlanetto, Steven R.
last_name: Furlanetto
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
- first_name: S. Peng
full_name: Oh, S. Peng
last_name: Oh
citation:
ama: Furlanetto SR, Haiman Z, Oh SP. Fossil Ionized bubbles around dead quasars
during reionization. The Astrophysical Journal. 2008;686(1):25-40. doi:10.1086/591047
apa: Furlanetto, S. R., Haiman, Z., & Oh, S. P. (2008). Fossil Ionized bubbles
around dead quasars during reionization. The Astrophysical Journal. American
Astronomical Society. https://doi.org/10.1086/591047
chicago: Furlanetto, Steven R., Zoltán Haiman, and S. Peng Oh. “Fossil Ionized Bubbles
around Dead Quasars during Reionization.” The Astrophysical Journal. American
Astronomical Society, 2008. https://doi.org/10.1086/591047.
ieee: S. R. Furlanetto, Z. Haiman, and S. P. Oh, “Fossil Ionized bubbles around
dead quasars during reionization,” The Astrophysical Journal, vol. 686,
no. 1. American Astronomical Society, pp. 25–40, 2008.
ista: Furlanetto SR, Haiman Z, Oh SP. 2008. Fossil Ionized bubbles around dead quasars
during reionization. The Astrophysical Journal. 686(1), 25–40.
mla: Furlanetto, Steven R., et al. “Fossil Ionized Bubbles around Dead Quasars during
Reionization.” The Astrophysical Journal, vol. 686, no. 1, American Astronomical
Society, 2008, pp. 25–40, doi:10.1086/591047.
short: S.R. Furlanetto, Z. Haiman, S.P. Oh, The Astrophysical Journal 686 (2008)
25–40.
date_created: 2024-09-06T10:19:49Z
date_published: 2008-10-10T00:00:00Z
date_updated: 2024-09-30T13:04:56Z
day: '10'
doi: 10.1086/591047
extern: '1'
intvolume: ' 686'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1086/591047
month: '10'
oa: 1
oa_version: Preprint
page: 25-40
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Fossil Ionized bubbles around dead quasars during reionization
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 686
year: '2008'
...
---
_id: '17788'
abstract:
- lang: eng
text: Nongravitational processes, such as feedback from galaxies and their active
nuclei, are believed to have injected excess entropy into the intracluster gas,
and therefore to have modified the density profiles in galaxy clusters during
their formation. Here we study a simple model for this so-called preheating scenario,
and ask (1) whether it can simultaneously explain both global X-ray scaling relations
and number counts of galaxy clusters, and (2) whether the amount of entropy required
evolves with redshift. We adopt a baseline entropy profile that fits recent hydrodynamic
simulations, modify the hydrostatic equilibrium condition for the gas by including
≈20% nonthermal pressure support, and add an entropy floor K0 that is allowed
to vary with redshift. We find that the observed luminosity-temperature (L − T)
relations of low-redshift (⟨ z⟩ = 0.05) HIFLUGCS clusters and high-redshift (⟨
z⟩ = 0.80) WARPS clusters are best simultaneously reproduced with an entropy floor
that evolves from ≈200 h^−1/3 keV cm^ 2 at z ≈ 0.8 to ≳300 h^−1/3 keV cm^ 2 at
z < 0.05. This evolution may take place predominantly at low redshift (z≲ 0.2).
If we restrict our analysis to the subset of bright (kT≳ 3 keV) clusters, we find
that the evolving entropy floor can mimic a self-similar evolution in the L −
T scaling relation. This degeneracy with self-similar evolution is, however, lifted
when 0.5 keV ≲ kT≲ 3 keV clusters are included. Using the cosmological parameters
from the WMAP 3 yr data, but treating σ8 as a free parameter, our model can reproduce
the number counts of the X-ray galaxy clusters in the 158 deg2 ROSAT PSPC survey,
with a best-fit value of σ8 = 0.80 ± 0.05.
article_processing_charge: No
article_type: original
author:
- first_name: Wenjuan
full_name: Fang, Wenjuan
last_name: Fang
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
citation:
ama: Fang W, Haiman Z. An evolving entropy floor in the intracluster gas? The
Astrophysical Journal. 2008;680(1):200-213. doi:10.1086/587780
apa: Fang, W., & Haiman, Z. (2008). An evolving entropy floor in the intracluster
gas? The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/587780
chicago: Fang, Wenjuan, and Zoltán Haiman. “An Evolving Entropy Floor in the Intracluster
Gas?” The Astrophysical Journal. American Astronomical Society, 2008. https://doi.org/10.1086/587780.
ieee: W. Fang and Z. Haiman, “An evolving entropy floor in the intracluster gas?,”
The Astrophysical Journal, vol. 680, no. 1. American Astronomical Society,
pp. 200–213, 2008.
ista: Fang W, Haiman Z. 2008. An evolving entropy floor in the intracluster gas?
The Astrophysical Journal. 680(1), 200–213.
mla: Fang, Wenjuan, and Zoltán Haiman. “An Evolving Entropy Floor in the Intracluster
Gas?” The Astrophysical Journal, vol. 680, no. 1, American Astronomical
Society, 2008, pp. 200–13, doi:10.1086/587780.
short: W. Fang, Z. Haiman, The Astrophysical Journal 680 (2008) 200–213.
date_created: 2024-09-06T10:20:50Z
date_published: 2008-06-10T00:00:00Z
date_updated: 2024-09-30T13:33:11Z
day: '10'
doi: 10.1086/587780
extern: '1'
intvolume: ' 680'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1086/587780
month: '06'
oa: 1
oa_version: Published Version
page: 200-213
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: An evolving entropy floor in the intracluster gas?
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 680
year: '2008'
...
---
_id: '17789'
abstract:
- lang: eng
text: Light-travel time delays distort the apparent shapes of H II regions surrounding
bright quasars during early stages of cosmic reionization. Individual H II regions
may remain undetectable in forthcoming redshifted 21 cm experiments. However,
the systematic deformation along the line of sight may be detectable statistically,
either by stacking tomographic 21 cm images of quasars identified, for example,
by the James Webb Space Telescope, or as small-scale anisotropy in the three-dimensional
21 cm power spectrum. Here we consider the detectability of this effect. The anisotropy
is largest when H II regions are large and expand rapidly, and we find that if
bright quasars contributed to the early stages of reionization, then they can
produce significant anisotropy, on scales comparable to the typical sizes of H
II regions of the bright quasars (≲30 Mpc). The effect therefore cannot be ignored
when analyzing future 21 cm power spectra on small scales. If 10% of the volume
of the intergalactic medium at z≃ 10 is ionized by quasars with typical ionizing
luminosity of S≳ 5 × 10^56 s^−1, the distortions cause an ≳10 percent enhancement
of the 21 cm power spectrum in the radial (redshift) direction, relative to the
transverse directions. The level of this anisotropy exceeds that due to redshift-space
distortion and has the opposite sign. We show that ongoing experiments such as
Murchison Widefield Array (MWA, formerly known as the Mileura Widefield Array)
should be able to detect this effect. A detection would reveal the presence of
bright quasars and shed light on the ionizing yield and age of the ionizing sources
and the distribution and small-scale clumping of neutral intergalactic gas in
their vicinity.
article_processing_charge: No
article_type: original
author:
- first_name: Shiv
full_name: Sethi, Shiv
last_name: Sethi
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
citation:
ama: Sethi S, Haiman Z. Can we detect the anisotropic shapes of quasar H ii regions
during reionization through the small‐scale redshifted 21 cm power spectrum? The
Astrophysical Journal. 2008;673(1):1-13. doi:10.1086/523787
apa: Sethi, S., & Haiman, Z. (2008). Can we detect the anisotropic shapes of
quasar H ii regions during reionization through the small‐scale redshifted 21
cm power spectrum? The Astrophysical Journal. American Astronomical Society.
https://doi.org/10.1086/523787
chicago: Sethi, Shiv, and Zoltán Haiman. “Can We Detect the Anisotropic Shapes of
Quasar H Ii Regions during Reionization through the Small‐scale Redshifted 21
Cm Power Spectrum?” The Astrophysical Journal. American Astronomical Society,
2008. https://doi.org/10.1086/523787.
ieee: S. Sethi and Z. Haiman, “Can we detect the anisotropic shapes of quasar H
ii regions during reionization through the small‐scale redshifted 21 cm power
spectrum?,” The Astrophysical Journal, vol. 673, no. 1. American Astronomical
Society, pp. 1–13, 2008.
ista: Sethi S, Haiman Z. 2008. Can we detect the anisotropic shapes of quasar H
ii regions during reionization through the small‐scale redshifted 21 cm power
spectrum? The Astrophysical Journal. 673(1), 1–13.
mla: Sethi, Shiv, and Zoltán Haiman. “Can We Detect the Anisotropic Shapes of Quasar
H Ii Regions during Reionization through the Small‐scale Redshifted 21 Cm Power
Spectrum?” The Astrophysical Journal, vol. 673, no. 1, American Astronomical
Society, 2008, pp. 1–13, doi:10.1086/523787.
short: S. Sethi, Z. Haiman, The Astrophysical Journal 673 (2008) 1–13.
date_created: 2024-09-06T10:21:39Z
date_published: 2008-01-20T00:00:00Z
date_updated: 2024-09-30T13:47:04Z
day: '20'
doi: 10.1086/523787
extern: '1'
intvolume: ' 673'
issue: '1'
language:
- iso: eng
main_file_link:
- open_access: '1'
url: https://doi.org/10.1086/523787
month: '01'
oa: 1
oa_version: Published Version
page: 1-13
publication: The Astrophysical Journal
publication_identifier:
issn:
- 0004-637X
- 1538-4357
publication_status: published
publisher: American Astronomical Society
quality_controlled: '1'
scopus_import: '1'
status: public
title: Can we detect the anisotropic shapes of quasar H ii regions during reionization
through the small‐scale redshifted 21 cm power spectrum?
type: journal_article
user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345
volume: 673
year: '2008'
...
---
OA_place: repository
OA_type: free access
_id: '17804'
abstract:
- lang: eng
text: Primordial gas in protogalactic DM halos with virial temperatures Tvir≳ 104
K begins to cool and condense via atomic hydrogen. Provided that this gas is irradiated
by a strong UV flux and remains free of H2 and other molecules, it has been proposed
that the halo with Tvir ∼ 104 K may avoid fragmentation and lead to the rapid
formation of an SMBH as massive as M ≈ 105–106 M☉. This "head start" would help
explain the presence of SMBHs with inferred masses of several times 109 M☉, powering
the bright quasars discovered in the SDSS at redshift z≳ 6. However, high-redshift
DM halos with Tvir ∼ 104 K are likely already enriched with at least trace amounts
of metals and dust produced by prior star formation in their progenitors. Here
we study the thermal and chemical evolution of low-metallicity gas exposed to
extremely strong UV radiation fields. Our results, obtained in one-zone models,
suggest that gas fragmentation is inevitable above a critical metallicity, whose
value is between Zcr ≈ 3 × 10−4 Z☉ (in the absence of dust) and as low as Zcr
≈ 5 × 10−6 Z☉ (with a dust-to-gas mass ratio of about 0.01Z/Z☉). We propose that
when the metallicity exceeds these critical values, dense clusters of low-mass
stars may form at the halo nucleus. Relatively massive stars in such a cluster
can then rapidly coalesce into a single more massive object, which may produce
an intermediate-mass BH remnant with a mass up to M≲ 102–103 M☉.
article_processing_charge: No
article_type: original
arxiv: 1
author:
- first_name: K.
full_name: Omukai, K.
last_name: Omukai
- first_name: R.
full_name: Schneider, R.
last_name: Schneider
- first_name: Zoltán
full_name: Haiman, Zoltán
id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36
last_name: Haiman
orcid: 0000-0003-3633-5403
citation:
ama: Omukai K, Schneider R, Haiman Z. Can supermassive black holes form in metal‐enriched
high‐redshift protogalaxies? The Astrophysical Journal. 2008;686(2):801-814.
doi:10.1086/591636
apa: Omukai, K., Schneider, R., & Haiman, Z. (2008). Can supermassive black
holes form in metal‐enriched high‐redshift protogalaxies? The Astrophysical
Journal. American Astronomical Society. https://doi.org/10.1086/591636
chicago: Omukai, K., R. Schneider, and Zoltán Haiman. “Can Supermassive Black Holes
Form in Metal‐enriched High‐redshift Protogalaxies?” The Astrophysical Journal.
American Astronomical Society, 2008. https://doi.org/10.1086/591636.
ieee: K. Omukai, R. Schneider, and Z. Haiman, “Can supermassive black holes form
in metal‐enriched high‐redshift protogalaxies?,” The Astrophysical Journal,
vol. 686, no. 2. American Astronomical Society, pp. 801–814, 2008.
ista: Omukai K, Schneider R, Haiman Z. 2008. Can supermassive black holes form in
metal‐enriched high‐redshift protogalaxies? The Astrophysical Journal. 686(2),
801–814.
mla: Omukai, K., et al. “Can Supermassive Black Holes Form in Metal‐enriched High‐redshift
Protogalaxies?” The Astrophysical Journal, vol. 686, no. 2, American Astronomical
Society, 2008, pp. 801–14, doi:10.1086/591636.
short: K. Omukai, R. Schneider, Z. Haiman, The Astrophysical Journal 686 (2008)
801–814.
date_created: 2024-09-06T11:33:03Z
date_published: 2008-08-20T00:00:00Z
date_updated: 2024-11-12T10:11:29Z
day: '20'
doi: 10.1086/591636
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arxiv:
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page: 801-814
publication: The Astrophysical Journal
publication_identifier:
eissn:
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issn:
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publisher: American Astronomical Society
quality_controlled: '1'
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title: Can supermassive black holes form in metal‐enriched high‐redshift protogalaxies?
type: journal_article
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author:
- first_name: Matthew Richard
full_name: Robinson, Matthew Richard
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last_name: Robinson
orcid: 0000-0001-8982-8813
- first_name: Jill G.
full_name: Pilkington, Jill G.
last_name: Pilkington
- first_name: Tim H.
full_name: Clutton-Brock, Tim H.
last_name: Clutton-Brock
- first_name: Josephine M.
full_name: Pemberton, Josephine M.
last_name: Pemberton
- first_name: Loeske. E.B.
full_name: Kruuk, Loeske. E.B.
last_name: Kruuk
citation:
ama: Robinson MR, Pilkington JG, Clutton-Brock TH, Pemberton JM, Kruuk LEB. Environmental
heterogeneity generates fluctuating selection on a secondary sexual trait. Current
Biology. 2008;18(10):751-757. doi:10.1016/j.cub.2008.04.059
apa: Robinson, M. R., Pilkington, J. G., Clutton-Brock, T. H., Pemberton, J. M.,
& Kruuk, L. E. B. (2008). Environmental heterogeneity generates fluctuating
selection on a secondary sexual trait. Current Biology. Elsevier. https://doi.org/10.1016/j.cub.2008.04.059
chicago: Robinson, Matthew Richard, Jill G. Pilkington, Tim H. Clutton-Brock, Josephine
M. Pemberton, and Loeske. E.B. Kruuk. “Environmental Heterogeneity Generates Fluctuating
Selection on a Secondary Sexual Trait.” Current Biology. Elsevier, 2008.
https://doi.org/10.1016/j.cub.2008.04.059.
ieee: M. R. Robinson, J. G. Pilkington, T. H. Clutton-Brock, J. M. Pemberton, and
L. E. B. Kruuk, “Environmental heterogeneity generates fluctuating selection on
a secondary sexual trait,” Current Biology, vol. 18, no. 10. Elsevier,
pp. 751–757, 2008.
ista: Robinson MR, Pilkington JG, Clutton-Brock TH, Pemberton JM, Kruuk LEB. 2008.
Environmental heterogeneity generates fluctuating selection on a secondary sexual
trait. Current Biology. 18(10), 751–757.
mla: Robinson, Matthew Richard, et al. “Environmental Heterogeneity Generates Fluctuating
Selection on a Secondary Sexual Trait.” Current Biology, vol. 18, no. 10,
Elsevier, 2008, pp. 751–57, doi:10.1016/j.cub.2008.04.059.
short: M.R. Robinson, J.G. Pilkington, T.H. Clutton-Brock, J.M. Pemberton, L.E.B.
Kruuk, Current Biology 18 (2008) 751–757.
date_created: 2020-04-30T11:02:13Z
date_published: 2008-05-20T00:00:00Z
date_updated: 2021-01-12T08:15:17Z
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doi: 10.1016/j.cub.2008.04.059
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page: 751-757
publication: Current Biology
publication_identifier:
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publication_status: published
publisher: Elsevier
quality_controlled: '1'
status: public
title: Environmental heterogeneity generates fluctuating selection on a secondary
sexual trait
type: journal_article
user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87
volume: 18
year: '2008'
...