The Experts below are selected from a list of 360 Experts worldwide ranked by ideXlab platform
A Ederoclite - One of the best experts on this subject based on the ideXlab platform.
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the peculiar optical spectrum of 4c 22 25 imprint of a massive black hole binary
The Astrophysical Journal, 2010Co-Authors: Roberto Decarli, M Dotti, C Montuori, T Liimets, A EderocliteAbstract:We report the discovery of peculiar features in the optical spectrum of 4C+22.25, a flat spectrum radio quasar at z = 0.4183 observed in the Sloan Digital Sky Survey and in a dedicated spectroscopic follow-up from the Nordic Optical Telescope. The Hβ and Hα lines show broad profiles (FWHM ~ 12,000 km s–1), faint fluxes, and extreme offsets (Δv = 8700 ± 1300 km s–1) with respect to the narrow emission lines. These features show no significant variation in a time lag of ~3.1 yr (rest frame). We rule out possible interpretations based on the superposition of two sources or on recoiling black holes, and discuss the virtues and limitations of a massive black hole binary scenario.
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the peculiar optical spectrum of 4c 22 25 imprint of a massive black hole binary
arXiv: Cosmology and Nongalactic Astrophysics, 2010Co-Authors: Roberto Decarli, M Dotti, C Montuori, T Liimets, A EderocliteAbstract:We report the discovery of peculiar features in the optical spectrum of 4C+22.25, a flat spectrum radio quasar at z=0.4183 observed in the SDSS and in a dedicated spectroscopic follow-up from the Nordic Optical Telescope. The Hbeta and Halpha lines show broad profiles (FWHM~12,000 km/s), faint fluxes and extreme offsets (Delta v=8,700+/-1,300 km/s) with respect to the narrow emission lines. These features show no significant variation in a time lag of ~3.1 yr (rest frame). We rule out possible interpretations based on the superposition of two sources or on recoiling black holes, and we discuss the virtues and limitations of a massive black hole binary scenario.
Catalin Miron - One of the best experts on this subject based on the ideXlab platform.
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einstein bohr recoiling double slit gedanken experiment performed at the molecular level
29th International Conference on Photonic Electronic and Atomic Collisions (ICPEAC) JUL 22-28 2015 Toledo SPAIN, 2015Co-Authors: Xiaojing Liu, Quan Miao, Faris Gelmukhanov, Minna Patanen, O Travnikova, Christophe Nicolas, Hans Agren, K Ueda, Catalin MironAbstract:Double-slit experiments illustrate proof for wave–particle complementarity. The essence of Einstein–Bohr's debate about wave–particle duality was whether the momentum transfer between a particle and a recoiling slit could mark the path, thus destroying the interference. We realized this recoiling double-slit gedanken experiment by resonant X-ray photoemission from molecular oxygen for geometries near equilibrium (coupled slits) and in a dissociative state far away from equilibrium (decoupled slits). Interference is observed in the former case, while the electron momentum transfer quenches the interference in the latter case.
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einstein bohr recoiling double slit gedanken experiment performed at the molecular level
Nature Photonics, 2015Co-Authors: Xiaojing Liu, Quan Miao, Faris Gelmukhanov, Minna Patanen, O Travnikova, Christophe Nicolas, Hans Agren, K Ueda, Catalin MironAbstract:The authors observe electron interference using the Auger electron emitted from an O2 molecule ionized by a soft X-ray photon. The interference disappears when the location of the O+ can be determined from the final state observed.
Quan Miao - One of the best experts on this subject based on the ideXlab platform.
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einstein bohr recoiling double slit gedanken experiment performed at the molecular level
29th International Conference on Photonic Electronic and Atomic Collisions (ICPEAC) JUL 22-28 2015 Toledo SPAIN, 2015Co-Authors: Xiaojing Liu, Quan Miao, Faris Gelmukhanov, Minna Patanen, O Travnikova, Christophe Nicolas, Hans Agren, K Ueda, Catalin MironAbstract:Double-slit experiments illustrate proof for wave–particle complementarity. The essence of Einstein–Bohr's debate about wave–particle duality was whether the momentum transfer between a particle and a recoiling slit could mark the path, thus destroying the interference. We realized this recoiling double-slit gedanken experiment by resonant X-ray photoemission from molecular oxygen for geometries near equilibrium (coupled slits) and in a dissociative state far away from equilibrium (decoupled slits). Interference is observed in the former case, while the electron momentum transfer quenches the interference in the latter case.
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einstein bohr recoiling double slit gedanken experiment performed at the molecular level
Nature Photonics, 2015Co-Authors: Xiaojing Liu, Quan Miao, Faris Gelmukhanov, Minna Patanen, O Travnikova, Christophe Nicolas, Hans Agren, K Ueda, Catalin MironAbstract:The authors observe electron interference using the Auger electron emitted from an O2 molecule ionized by a soft X-ray photon. The interference disappears when the location of the O+ can be determined from the final state observed.
Zoltan Haiman - One of the best experts on this subject based on the ideXlab platform.
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prompt shocks in the gas disk around a recoiling supermassive black hole binary
The Astrophysical Journal, 2008Co-Authors: Zoltan Lippai, Z Frei, Zoltan HaimanAbstract: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, two-dimensional disk of collisionless particles, initially on circular orbits a round a 10 6 MBHB, to kicks that are either parallel or perpendicular to the initial orbital plane. Typical kick velocities (vkick) can exceed the sound speed in a circumbinary gas disk. While the inner disk is strongly boun d 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 vkick = 500 km s -1 , 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, propagati ng outward at the speedv kick. Concentric density enhancements are also observed for kicks perpendicular to t he disk, but are weaker and develop into caustics only after a long delay (> one 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 wi th 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. Subject headings:black hole physics - galaxies: nuclei - gravitational waves
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prompt shocks in the gas disk around a recoiling supermassive black hole binary
arXiv: Astrophysics, 2008Co-Authors: Zoltan Lippai, Z Frei, Zoltan HaimanAbstract: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.
Ryan C Hickox - One of the best experts on this subject based on the ideXlab platform.
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the xmm newton spectrum of a candidate recoiling supermassive black hole an elusive inverted p cygni profile
The Astrophysical Journal, 2013Co-Authors: G Lanzuisi, F Civano, S Marchesi, A Comastri, E Costantini, Martin Elvis, V Mainieri, Ryan C HickoxAbstract:We present a detailed spectral analysis of new XMM-Newton data of the source CXOC J100043.1+020637, also known as CID-42, detected in the COSMOS survey at z = 0.359. Previous works suggested that CID-42 is a candidate recoiling supermassive black hole (SMBH) showing also an inverted P-Cygni profile in the X-ray spectra at ~6?keV (rest) with an iron emission line plus a redshifted absorption line (detected at 3? in previous XMM-Newton and Chandra observations). Detailed analysis of the absorption line suggested the presence of ionized material flowing into the black hole at high velocity. In the new long XMM-Newton observation, while the overall spectral shape remains constant, the continuum 2-10?keV flux decrease of ~20% with respect to previous observation and the absorption line is undetected. The upper limit on the intensity of the absorption line is EW < 162?eV. Extensive Monte Carlo simulations show that the nondetection of the line is solely due to variation in the properties of the inflowing material, in agreement with the transient nature of these features, and that the intensity of the line is lower than the previously measured with a probability of 98.8%. In the scenario of CID-42 as a recoiling SMBH, the absorption line can be interpreted as being due to an inflow of gas with variable density that is located in the proximity of the SMBH and recoiling with it. New monitoring observations will be requested to further characterize this line.
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the xmm newton spectrum of a candidate recoiling supermassive black hole an elusive inverted p cygni profile
arXiv: High Energy Astrophysical Phenomena, 2013Co-Authors: G Lanzuisi, F Civano, S Marchesi, A Comastri, E Costantini, Martin Elvis, V Mainieri, Ryan C HickoxAbstract:We present a detailed spectral analysis of new XMM-Newton data of the source CXOC J100043.1+020637, also known as CID-42, detected in the COSMOS survey at z = 0.359. Previous works suggested that CID-42 is a candidate recoiling supermassive black holes showing also an inverted P-Cygni profile in the X- ray spectra at ~6 keV (rest) with an iron emission line plus a redshifted absorption line (detected at 3sigma in previous XMM-Newton and Chandra observations). Detailed analysis of the absorption line suggested the presence of ionized material inflowing into the black hole at high velocity. In the new long XMM-Newton observation, while the overall spectral shape remains constant, the continuum 2-10 keV flux decreased of ~20% with respect to previous observation and the absorption line is undetected. The upper limit on the intensity of the absorption line is EW<162 keV. Extensive Monte Carlo simulations show that the non detection of the line is solely due to variation in the properties of the inflowing material, in agreement with the transient nature of these features, and that the intensity of the line is lower than the previously measured with a probability of 98.8%. In the scenario of CID-42 as recoiling SMBH, the absorption line can be interpreted as due to inflow of gas with variable density and located in the proximity of the SMBH and recoiling with it. New monitoring observations will be requested to further characterize this line.