923 results on '"Paragi, Z"'
Search Results
202. Double-peaked Emission Lines Due to a Radio Outflow in KISSR 1219
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Kharb, P., primary, Subramanian, S., additional, Vaddi, S., additional, Das, M., additional, and Paragi, Z., additional
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- 2017
- Full Text
- View/download PDF
203. FRB 121102 Is Coincident with a Star-forming Region in Its Host Galaxy
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Bassa, C. G., primary, Tendulkar, S. P., additional, Adams, E. A. K., additional, Maddox, N., additional, Bogdanov, S., additional, Bower, G. C., additional, Burke-Spolaor, S., additional, Butler, B. J., additional, Chatterjee, S., additional, Cordes, J. M., additional, Hessels, J. W. T., additional, Kaspi, V. M., additional, Law, C. J., additional, Marcote, B., additional, Paragi, Z., additional, Ransom, S. M., additional, Scholz, P., additional, Spitler, L. G., additional, and Langevelde, H. J. van, additional
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- 2017
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204. Towards the origin of the radio emission in AR Scorpii, the first radio-pulsing white dwarf binary
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Marcote, B., primary, Marsh, T. R., additional, Stanway, E. R., additional, Paragi, Z., additional, and Blanchard, J. M., additional
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- 2017
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205. Resolved, expanding jets in the Galactic black hole candidate XTE J1908+094
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Rushton, A. P., primary, Miller-Jones, J. C. A., additional, Curran, P. A., additional, Sivakoff, G. R., additional, Rupen, M. P., additional, Paragi, Z., additional, Spencer, R. E., additional, Yang, J., additional, Altamirano, D., additional, Belloni, T., additional, Fender, R. P., additional, Krimm, H. A., additional, Maitra, D., additional, Migliari, S., additional, Russell, D. M., additional, Russell, T. D., additional, Soria, R., additional, and Tudose, V., additional
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- 2017
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206. Unveiling multiple AGN activity in galaxy mergers
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De Rosa, A., primary, Bianchi, S., additional, Bogdanović, T., additional, Decarli, R., additional, Heidt, J., additional, Herrero-Illana, R., additional, Husemann, B., additional, Komossa, S., additional, Kun, E., additional, Loiseau, N., additional, Guainazzi, M., additional, Paragi, Z., additional, Perez-Torres, M., additional, Piconcelli, E., additional, Schawinski, K., additional, and Vignali, C., additional
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- 2017
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207. Transient Astrophysics with the Square Kilometre Array
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Fender, R., Stewart, A., Macquart, J. -P, Donnarumma, I., Murphy, T., Adam Deller, Paragi, Z., and Chatterjee, S.
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High Energy Astrophysical Phenomena (astro-ph.HE) ,FOS: Physical sciences ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
This chapter provides an overview of the possibilities for transient and variable-source astrophysics with the Square Kilometre Array. While subsequent chapters focus on the astrophysics of individual events, we focus on the broader picture, and how to maximise the science coming from the telescope. The SKA as currently designed will be a fantastic and ground-breaking facility for radio transient studies, but the scientifc yield will be dramatically increased by the addition of (i) near-real-time commensal searches of data streams for events, and (ii) on occasion, rapid robotic response to Target-of-Opprtunity style triggers., Review chapter on Transients for new SKA science book. Published online by Proceedings of Science
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- 2015
208. What is the progenitor of the Type Ia SN 2014J?
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Pérez-Torres, M. A., Lundqvist, P., Beswick, R. J., Björnsson, C. I., Muxlow, T. W. B., Paragi, Z., Ryder, S., Alberdi, A., Fransson, C., Marcaide, J. M. M., Martí-Vidal, I., Ros, E., Argo, M. K., and Guirado, J. C.
- Abstract
We report the deepest radio interferometric observations of the closest Type Ia supernova in decades, SN 2014J, which exploded in the nearby galaxy M 82. These observations represent, together with radio observations of SNe 2011fe, the most sensitive radio studies of a Type Ia SN ever. We constrain the mass-loss rate from the progenitor system of SN 2014J to dot{M} ≲ 7.0EE{-10} msunyr (for a wind speed of 100 kms). Our deep upper limits favor a double-degenerate scenario-involving two WD stars-for the progenitor system of SN 2014J, as such systems have less circumstellar gas than our upper limits. By contrast, most single-degenerate scenarios, i.e., the wide family of progenitor systems where a red giant, main-sequence, or sub-giant star donates mass to a exploding white dwarf, are ruled out by our observations. The evidence from SNe 2011fe and 2014J points in the direction of a double-degenerate scenario for both.
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- 2015
209. e-MERLIN observations of the puzzling TeV source HESS J1943+213
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Gabanyi, K. E., Dubner, G., Giacani, E., Frey, S., and Paragi, Z.
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High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Astrophysics of Galaxies ,Astrophysics::Galaxy Astrophysics - Abstract
HESS J1943+213 is a TeV source close to the Galactic plane proposed to be a BL Lac object. Our high resolution EVN observation failed to recover two thirds of the source flux density detected simultaneously by the WSRT. Our recent e-MERLIN observations in L and C bands show only a point source with flux density comparable to the EVN detection. Thus the structure responsible for the missing flux density has to be larger than 2". It may be related to the presumed extragalactic source (thus would have a kpc-scale size), or to the Galactic foreground material close to the line of sight to the source., 4 pages, 1 figure, appears in the proceedings of the 12th European VLBI Network Symposium and Users Meeting (7-10 October 2014, Cagliari, Italy), eds. A. Tarchi, M. Giroletti & L. Feretti. Proceedings of Science, PoS(EVN 2014)078
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- 2015
210. Compact radio emission indicates a structured jet was produced by a binary neutron star merger.
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Ghirlanda, G., Salafia, O. S., Paragi, Z., Giroletti, M., Yang, J., Marcote, B., Blanchard, J., Agudo, I., An, T., Bernardini, M. G., Beswick, R., Branchesi, M., Campana, S., Casadio, C., Chassande-Mottin, E., Colpi, M., Covino, S., D'Avanzo, P., D'Elia, V., and Frey, S.
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- 2019
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211. VLBI observations of four radio quasars at z > 4: blazars or not?
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Cao, H.M., Frey, S., Gabanyi, K.E., Paragi, Z., Yang, J., Cseh, D., Hong, X.Y., An, T., Cao, H.M., Frey, S., Gabanyi, K.E., Paragi, Z., Yang, J., Cseh, D., Hong, X.Y., and An, T.
- Abstract
Contains fulltext : 173579.pdf (preprint version ) (Open Access)
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- 2017
212. Radio spectra of bright compact sources at z > 4.5
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Coppejans, R., Velzen, S. van, Intema, H.T., Müller, C., Frey, S., Coppejans, D.L., Cseh, D., Williams, W.L., Falcke, H., Körding, E.G., Orrú, E., Paragi, Z., Gabányi, K.É., Coppejans, R., Velzen, S. van, Intema, H.T., Müller, C., Frey, S., Coppejans, D.L., Cseh, D., Williams, W.L., Falcke, H., Körding, E.G., Orrú, E., Paragi, Z., and Gabányi, K.É.
- Abstract
Contains fulltext : 168631.pdf (publisher's version ) (Open Access)
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- 2017
213. Revealing HI gas in emission and absorption on pc to kpc scales in a galaxy at z ~ 0.017
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Gupta, N., Srianand, R., Farnes, J. S., Pidopryhora, Y., Vivek, M., Paragi, Z., Noterdaeme, P., Oosterloo, T., Petitjean, P., Gupta, N., Srianand, R., Farnes, J. S., Pidopryhora, Y., Vivek, M., Paragi, Z., Noterdaeme, P., Oosterloo, T., and Petitjean, P.
- Abstract
We present a detailed study of the quasar-galaxy pair: J1243+4043 - UGC07904. The sight line of the background quasar ( $z_q$= 1.5266) passes through a region of the galaxy ($z_g$=0.0169) at an impact parameter of 6.9 kpc with high metallicity (0.5 Z$_\odot$) and negligible dust extinction. We detect HI 21-cm absorption from the foreground galaxy at arcsecond and milliarcsecond scales. For typical cold neutral medium (CNM) temperatures in the Milky Way, this 21-cm absorber can be classified as a damped Ly$\alpha$ absorber (DLA). We infer the harmonic mean spin temperature of the gas to be $\sim$400 K and for a simple two-phase medium we estimate the CNM-fraction to be $f_{\rm CNM}$ = 0.27. This is remarkably consistent with the CNM fraction observed in the Galaxy and less than that of high-redshift DLAs. The quasar exhibits a core-jet morphology on milliarcsecond scales, corresponding to an overall extent of $\sim$9 pc at $z_g$. We show that the size of CNM absorbing clouds associated with the foreground galaxy is $>$5 pc and they may be part of cold gas structures that extend beyond $\sim$35 pc. Interestingly, the rotation measure of quasar J1243+4043 is higher than any other source in samples of quasars with high-$z$ DLAs. However, we do not find any detectable differences in RMs and polarization fraction of sight lines with or without high-$z$ ($z\ge2$) DLAs or low-$z$ ($z\le0.3$) 21-cm absorbers. Finally, the foreground galaxy UGC07904 is also part of a galaxy group. We serendipitously detect HI 21-cm emission from four members of the group, and a $\sim$80 kpc long HI bridge connecting two of the other members. The latter, together with the properties of the group members, suggests that the group is a highly interactive environment., Comment: 14 pages, 11 figures, 3 tables. Submitted to MNRAS (referee's comments from Minor revision incorporated)
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- 2017
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214. The radio structure of the peculiar narrow-line Seyfert 1 galaxy candidate J1100+4421
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Gabányi, K. É., Frey, S., Paragi, Z., Järvelä, E., Morokuma, T., An, T., Tanaka, M., Tar, I., Gabányi, K. É., Frey, S., Paragi, Z., Järvelä, E., Morokuma, T., An, T., Tanaka, M., and Tar, I.
- Abstract
Narrow-line Seyfert 1 galaxies (NLS1) are an intriguing subclass of active galactic nuclei. Their observed properties indicate low central black hole mass and high accretion rate. The extremely radio-loud NLS1 sources often show relativistic beaming and are usually regarded as younger counterparts of blazars. Recently, the object SDSS J110006.07+442144.3 was reported as a candidate NLS1 source. The characteristics of its dramatic optical flare indicated its jet-related origin. The spectral energy distribution of the object was similar to that of the gamma-ray detected radio-loud NLS1, PMN J0948+0022. Our high-resolution European Very Long Baseline Interferometry Network observations at 1.7 and 5 GHz revealed a compact core feature with a brightness temperature of >~ 10^(10) K. Using the lowest brightness temperature value and assuming a moderate Lorentz factor of ~9 the jet viewing angle is <~ 26 deg. Archival Very Large Array data show a large-scale radio structure with a projected linear size of ~150 kpc reminiscent of double-sided morphology., Comment: 8 pages, 5 figures. Accepted for publication in MNRAS
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- 2017
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215. Towards the origin of the radio emission in AR Sco, the first radio-pulsing white dwarf binary
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Marcote, B., Marsh, T. R., Stanway, E. R., Paragi, Z., Blanchard, J. M., Marcote, B., Marsh, T. R., Stanway, E. R., Paragi, Z., and Blanchard, J. M.
- Abstract
The binary system AR Sco contains an M star and the only known radio-pulsing white dwarf. The system shows emission from radio to X-rays, likely dominated by synchrotron radiation. The mechanism that produces most of this emission remains unclear. Two competing scenarios have been proposed: Collimated outflows, and direct interaction between the magnetospheres of the white dwarf and the M star. The two proposed scenarios can be tested via very long baseline interferometric radio observations. We conducted a radio observation with the Australian Long Baseline Array (LBA) on 20 Oct 2016 at 8.5 GHz to study the compactness of the radio emission. Simultaneous data with the Australian Telescope Compact Array (ATCA) were also recorded for a direct comparison of the obtained flux densities. AR Sco shows radio emission compact on milliarcsecond angular scales ($\lesssim 0.02\ \mathrm{AU}$, or $4\ \mathrm{R_{\odot}}$). The emission is orbitally modulated, with an average flux density of $\approx 6.5\ \mathrm{mJy}$. A comparison with the simultaneous ATCA data shows that no flux is resolved out on mas scales, implying that the radio emission is produced in this compact region. Additionally, the obtained radio light curves on hour timescales are consistent with the optical light curve. The radio emission in AR Sco is likely produced in the magnetosphere of the M star or the white dwarf, and we see no evidence for a radio outflow or collimated jets significantly contributing to the radio emission., Comment: 4 pages, 2 figures, accepted for publication in A&A
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- 2017
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216. Double-Peaked Emission Lines due to A Radio Outflow in KISSR1219
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Kharb, P., Subramanian, S., Vaddi, S., Das, M., Paragi, Z., Kharb, P., Subramanian, S., Vaddi, S., Das, M., and Paragi, Z.
- Abstract
We present the results from 1.5 and 5 GHz phase-referenced VLBA and 1.5 GHz Karl G. Jansky Very Large Array (VLA) observations of the Seyfert 2 galaxy KISSR1219, which exhibits double peaked emission lines in its optical spectrum. The VLA and VLBA data reveal a one-sided core-jet structure at roughly the same position angles, providing evidence of an AGN outflow. The absence of dual parsec-scale radio cores puts the binary black hole picture in doubt for the case of KISSR1219. The high brightness temperatures of the parsec-scale core and jet components ($>10^6$ K) are consistent with this interpretation. Doppler boosting with jet speeds of $\gtrsim0.55c$ to $\gtrsim0.25c$, going from parsec- to kpc-scales, at a jet inclination $\gtrsim50^\circ$ can explain the jet one-sidedness in this Seyfert 2 galaxy. A blue-shifted broad emission line component in [O {\sc iii}] is also indicative of an outflow in the emission line gas at a velocity of $\sim350$ km s$^{-1}$, while the [O {\sc i}] doublet lines suggest the presence of shock-heated gas. A detailed line ratio study using the MAPPINGS III code further suggests that a shock+precursor model can explain the line ionization data well. Overall, our data suggest that the radio outflow in KISSR1219 is pushing the emission line clouds, both ahead of the jet and in a lateral direction, giving rise to the double peak emission line spectra., Comment: 15 pages, 7 figures, ApJ accepted
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- 2017
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217. Simultaneous X-ray, gamma-ray, and Radio Observations of the repeating Fast Radio Burst FRB 121102
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Scholz, P., Bogdanov, S., Hessels, J. W. T., Lynch, R. S., Spitler, L. G., Bassa, C. G., Bower, G. C., Burke-Spolaor, S., Butler, B. J., Chatterjee, S., Cordes, J. M., Gourdji, K., Kaspi, V. M., Law, C. J., Marcote, B., McLaughlin, M. A., Michilli, D., Paragi, Z., Ransom, S. M., Seymour, A., Tendulkar, S. P., Wharton, R. S., Scholz, P., Bogdanov, S., Hessels, J. W. T., Lynch, R. S., Spitler, L. G., Bassa, C. G., Bower, G. C., Burke-Spolaor, S., Butler, B. J., Chatterjee, S., Cordes, J. M., Gourdji, K., Kaspi, V. M., Law, C. J., Marcote, B., McLaughlin, M. A., Michilli, D., Paragi, Z., Ransom, S. M., Seymour, A., Tendulkar, S. P., and Wharton, R. S.
- Abstract
We undertook coordinated campaigns with the Green Bank, Effelsberg, and Arecibo radio telescopes during Chandra X-ray Observatory and XMM-Newton observations of the repeating fast radio burst FRB 121102 to search for simultaneous radio and X-ray bursts. We find 12 radio bursts from FRB 121102 during 70 ks total of X-ray observations. We detect no X-ray photons at the times of radio bursts from FRB 121102 and further detect no X-ray bursts above the measured background at any time. We place a 5$\sigma$ upper limit of $3\times10^{-11}$ erg cm$^{-2}$ on the 0.5--10 keV fluence for X-ray bursts at the time of radio bursts for durations $<700$ ms, which corresponds to a burst energy of $4\times10^{45}$ erg at the measured distance of FRB 121102. We also place limits on the 0.5--10 keV fluence of $5\times10^{-10}$ erg cm$^{-2}$ and $1\times10^{-9}$ erg cm$^{-2}$ for bursts emitted at any time during the XMM-Newton and Chandra observations, respectively, assuming a typical X-ray burst duration of 5 ms. We analyze data from the Fermi Gamma-ray Space Telescope Gamma-ray Burst Monitor and place a 5$\sigma$ upper limit on the 10--100 keV fluence of $4\times10^{-9}$ erg cm$^{-2}$ ($5\times10^{47}$ erg at the distance of FRB 121102) for gamma-ray bursts at the time of radio bursts. We also present a deep search for a persistent X-ray source using all of the X-ray observations taken to date and place a 5$\sigma$ upper limit on the 0.5--10 keV flux of $4\times10^{-15}$ erg s$^{-1}$ cm$^{-2}$ ($3\times10^{41}$ erg~s$^{-1}$ at the distance of FRB 121102). We discuss these non-detections in the context of the host environment of FRB 121102 and of possible sources of fast radio bursts in general., Comment: 13 pages, 5 figures, published in ApJ
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- 2017
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218. FRB 121102 is coincident with a star forming region in its host galaxy
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Bassa, C. G., Tendulkar, S. P., Adams, E. A. K., Maddox, N., Bogdanov, S., Bower, G. C., Burke-Spolaor, S., Butler, B. J., Chatterjee, S., Cordes, J. M., Hessels, J. W. T., Kaspi, V. M., Law, C. J., Marcote, B., Paragi, Z., Ransom, S. M., Scholz, P., Spitler, L. G., van Langevelde, H. J., Bassa, C. G., Tendulkar, S. P., Adams, E. A. K., Maddox, N., Bogdanov, S., Bower, G. C., Burke-Spolaor, S., Butler, B. J., Chatterjee, S., Cordes, J. M., Hessels, J. W. T., Kaspi, V. M., Law, C. J., Marcote, B., Paragi, Z., Ransom, S. M., Scholz, P., Spitler, L. G., and van Langevelde, H. J.
- Abstract
We present optical, near- and mid-infrared imaging of the host galaxy of FRB 121102 with the Gemini North telescope, the Hubble Space Telescope and the Spitzer Space Telescope. The FRB 121102 host galaxy is resolved, revealing a bright star forming region located in the outskirts of the irregular, low-metallicity dwarf galaxy. The star forming region has a half-light radius of 0.68 kpc (0.20 arcsec), encompassing the projected location of the compact (<0.7 pc), persistent radio source that is associated with FRB 121102. The half-light diameter of the dwarf galaxy is 5 to 7 kpc, and broadband spectral energy distribution fitting indicates that it has a total stellar mass of M*~10^8 Msun. The metallicity of the host galaxy is low, 12+log10 ([O/H])=8.0+-0.1. The properties of the host galaxy of FRB 121102 are comparable to those of extreme emission line galaxies, also known to host hydrogen-poor superluminous supernovae and long-duration gamma-ray bursts. The projected location of FRB 121102 within the star forming region supports the proposed connection of FRBs with newly born neutron stars or magnetars., Comment: 6 pages, 2 figures, submitted to ApJL; v2 has correct r' band magnitude
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- 2017
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219. Swift J1644+5734: the EVN view
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Paragi, Z., Yang, J., Komossa, S., van der Horst, A., Gurvits, L. I., Campbell, R. M., Giannios, D., An, T., Paragi, Z., Yang, J., Komossa, S., van der Horst, A., Gurvits, L. I., Campbell, R. M., Giannios, D., and An, T.
- Abstract
A small fraction of Tidal Disruption Events (TDE) produce relativistic jets, evidenced by their non-thermal X-ray spectra and transient radio emission. Here we present milliarcsecond-resolution imaging results on TDE J1644+5734 with the European VLBI Network (EVN). These provide a strong astrometric constraint on the average apparent jet velocity <0.27, that constrains the intrinsic jet velocity for a given viewing angle., Comment: 4 pages, 2 figures. Accepted for publication in the Proceedings of the IAU Symposium No. 324, New Frontiers in Black Hole Astrophysics. v2 is identical to v1; corrected a typo only in the metadata
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- 2017
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220. The direct localization of a fast radio burst and its host
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Chatterjee, S., Law, C. J., Wharton, R. S., Burke-Spolaor, S., Hessels, J. W. T., Bower, G. C., Cordes, J. M., Tendulkar, S. P., Bassa, C. G., Demorest, P., Butler, B. J., Seymour, A., Scholz, P., Abruzzo, M. W., Bogdanov, S., Kaspi, V. M., Keimpema, A., Lazio, T. J. W., Marcote, B., McLaughlin, M. A., Paragi, Z., Ransom, S. M., Rupen, M., Spitler, L. G., van Langevelde, H. J., Chatterjee, S., Law, C. J., Wharton, R. S., Burke-Spolaor, S., Hessels, J. W. T., Bower, G. C., Cordes, J. M., Tendulkar, S. P., Bassa, C. G., Demorest, P., Butler, B. J., Seymour, A., Scholz, P., Abruzzo, M. W., Bogdanov, S., Kaspi, V. M., Keimpema, A., Lazio, T. J. W., Marcote, B., McLaughlin, M. A., Paragi, Z., Ransom, S. M., Rupen, M., Spitler, L. G., and van Langevelde, H. J.
- Abstract
Fast radio bursts are astronomical radio flashes of unknown physical nature with durations of milliseconds. Their dispersive arrival times suggest an extragalactic origin and imply radio luminosities orders of magnitude larger than any other kind of known short-duration radio transient. Thus far, all FRBs have been detected with large single-dish telescopes with arcminute localizations, and attempts to identify their counterparts (source or host galaxy) have relied on contemporaneous variability of field sources or the presence of peculiar field stars or galaxies. These attempts have not resulted in an unambiguous association with a host or multi-wavelength counterpart. Here we report the sub-arcsecond localization of FRB 121102, the only known repeating burst source, using high-time-resolution radio interferometric observations that directly image the bursts themselves. Our precise localization reveals that FRB 121102 originates within 100 mas of a faint 180 uJy persistent radio source with a continuum spectrum that is consistent with non-thermal emission, and a faint (25th magnitude) optical counterpart. The flux density of the persistent radio source varies by tens of percent on day timescales, and very long baseline radio interferometry yields an angular size less than 1.7 mas. Our observations are inconsistent with the fast radio burst having a Galactic origin or its source being located within a prominent star-forming galaxy. Instead, the source appears to be co-located with a low-luminosity active galactic nucleus or a previously unknown type of extragalactic source. [Truncated] If other fast radio bursts have similarly faint radio and optical counterparts, our findings imply that direct sub-arcsecond localizations of FRBs may be the only way to provide reliable associations., Comment: Nature, published online on 4 Jan 2017, DOI: 10.1038/nature20797
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- 2017
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221. The Repeating Fast Radio Burst FRB 121102 as Seen on Milliarcsecond Angular Scales
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Marcote, B., Paragi, Z., Hessels, J. W. T., Keimpema, A., van Langevelde, H. J., Huang, Y., Bassa, C. G., Bogdanov, S., Bower, G. C., Burke-Spolaor, S., Butler, B. J., Campbell, R. M., Chatterjee, S., Cordes, J. M., Demorest, P., Garrett, M. A., Ghosh, T., Kaspi, V. M., Law, C. J., Lazio, T. J. W., McLaughlin, M. A., Ransom, S. M., Salter, C. J., Scholz, P., Seymour, A., Siemion, A., Spitler, L. G., Tendulkar, S. P., Wharton, R. S., Marcote, B., Paragi, Z., Hessels, J. W. T., Keimpema, A., van Langevelde, H. J., Huang, Y., Bassa, C. G., Bogdanov, S., Bower, G. C., Burke-Spolaor, S., Butler, B. J., Campbell, R. M., Chatterjee, S., Cordes, J. M., Demorest, P., Garrett, M. A., Ghosh, T., Kaspi, V. M., Law, C. J., Lazio, T. J. W., McLaughlin, M. A., Ransom, S. M., Salter, C. J., Scholz, P., Seymour, A., Siemion, A., Spitler, L. G., Tendulkar, S. P., and Wharton, R. S.
- Abstract
The millisecond-duration radio flashes known as Fast Radio Bursts (FRBs) represent an enigmatic astrophysical phenomenon. Recently, the sub-arcsecond localization (~ 100mas precision) of FRB121102 using the VLA has led to its unambiguous association with persistent radio and optical counterparts, and to the identification of its host galaxy. However, an even more precise localization is needed in order to probe the direct physical relationship between the millisecond bursts themselves and the associated persistent emission. Here we report very-long-baseline radio interferometric observations using the European VLBI Network and the 305-m Arecibo telescope, which simultaneously detect both the bursts and the persistent radio emission at milliarcsecond angular scales and show that they are co-located to within a projected linear separation of < 40pc (< 12mas angular separation, at 95% confidence). We detect consistent angular broadening of the bursts and persistent radio source (~ 2-4mas at 1.7GHz), which are both similar to the expected Milky Way scattering contribution. The persistent radio source has a projected size constrained to be < 0.7pc (< 0.2mas angular extent at 5.0GHz) and a lower limit for the brightness temperature of T_b > 5 x 10^7K. Together, these observations provide strong evidence for a direct physical link between FRB121102 and the compact persistent radio source. We argue that a burst source associated with a low-luminosity active galactic nucleus or a young neutron star energizing a supernova remnant are the two scenarios for FRB121102 that best match the observed data., Comment: 13 pages, 5 figures, accepted to ApJL
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- 2017
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222. Resolved, expanding jets in the Galactic black hole candidate XTE J1908+094
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Rushton, A. P., Miller-Jones, J. C. A., Curran, P. A., Sivakoff, G. R., Rupen, M. P., Paragi, Z., Spencer, R. E., Yang, J., Altamirano, D., Belloni, T., Fender, R. P., Krimm, H. A., Maitra, D., Migliari, S., Russell, D. M., Russell, T. D., Soria, R., Tudose, V., Rushton, A. P., Miller-Jones, J. C. A., Curran, P. A., Sivakoff, G. R., Rupen, M. P., Paragi, Z., Spencer, R. E., Yang, J., Altamirano, D., Belloni, T., Fender, R. P., Krimm, H. A., Maitra, D., Migliari, S., Russell, D. M., Russell, T. D., Soria, R., and Tudose, V.
- Abstract
Black hole X-ray binaries undergo occasional outbursts caused by changing inner accretion flows. Here we report high-angular resolution radio observations of the 2013 outburst of the black hole candidate X-ray binary system J1908+094, using data from the VLBA and EVN. We show that following a hard-to-soft state transition, we detect moving jet knots that appear asymmetric in morphology and brightness, and expand to become laterally resolved as they move away from the core, along an axis aligned approximately $-11$\degree\ east of north. We initially see only the southern component, whose evolution gives rise to a 15-mJy radio flare and generates the observed radio polarization. This fades and becomes resolved out after 4 days, after which a second component appears to the north, moving in the opposite direction. From the timing of the appearance of the knots relative to the X-ray state transition, a 90\degree\ swing of the inferred magnetic field orientation, the asymmetric appearance of the knots, their complex and evolving morphology, and their low speeds, we interpret the knots as working surfaces where the jets impact the surrounding medium. This would imply a substantially denser environment surrounding XTE J1908+094 than has been inferred to exist around the microquasar sources GRS 1915+105 and GRO J1655-40., Comment: 17 pages, 9 figures, accepted in MNRAS
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- 2017
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223. Searching for a pair of accreting supermassive black holes in J1425+3231
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Gabányi, K. É., Frey, S., Paragi, Z., An, T., Komossa, S., Gabányi, K. É., Frey, S., Paragi, Z., An, T., and Komossa, S.
- Abstract
In hierarchical structure formation scenarios, merging galaxies are expected to be seen in different phases of their coalescence. Simulations suggest that simultaneous activity of the supermassive black holes (SMBHs) in the centres of the merging galaxies may be expected at kpc-scale separations. Currently, there are no direct observational methods which allow the selection of a large number of such dual active galactic nuclei (AGN) candidates. SDSS J142507.32+323137.4 was reported as a promising candidate source based on its optical spectrum. Here we report on our sensitive e-MERLIN observations performed at $1.6$ and at $5$ GHz, which show that the optical spectrum of the source can be more straightforwardly explained with jet-cloud interactions instead of the dual AGN scenario., Comment: 4 pages, 1 figure. Accepted for publication in the Proceedings of the IAU Symposium No. 324, New Frontiers in Black Hole Astrophysics
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- 2017
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224. VLBI observations of four radio quasars at $z>4$: blazars or not?
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Cao, H. -M., Frey, S., Gabányi, K. É., Paragi, Z., Yang, J., Cseh, D., Hong, X. -Y., An, T., Cao, H. -M., Frey, S., Gabányi, K. É., Paragi, Z., Yang, J., Cseh, D., Hong, X. -Y., and An, T.
- Abstract
Blazars are active galactic nuclei (AGN) whose relativistic jets point nearly to the line of sight. Their compact radio structure can be imaged with very long baseline interferometry (VLBI) on parsec scales. Blazars at extremely high redshifts provide a unique insight into the AGN phenomena in the early Universe. We observed four radio sources at redshift $z>4$ with the European VLBI Network (EVN) at 1.7 and 5 GHz. These objects were previously classified as blazar candidates based on X-ray observations. One of them, J2134$-$0419 is firmly confirmed as a blazar with our VLBI observations, due to its relativistically beamed radio emission. Its radio jet extended to $\sim$10 milli-arcsec scale makes this source a promising target for follow-up VLBI observations to reveal any apparent proper motion. Another target, J0839+5112 shows a compact radio structure typical of quasars. There is evidence for flux density variability and its radio "core" has a flat spectrum. However, the EVN data suggest that its emission is not Doppler-boosted. The remaining two blazar candidates (J1420+1205 and J2220+0025) show radio properties totally unexpected from radio AGN with small-inclination jet. Their emission extends to arcsec scales and the Doppler factors of the central components are well below 1. Their structures resemble that of double-lobed radio AGN with large inclination to the line of sight. This is in contrast with the blazar-type modeling of their multi-band spectral energy distributions. Our work underlines the importance of high-resolution VLBI imaging in confirming the blazar nature of high-redshift radio sources., Comment: 11 pages, 4 figures, 5 tables, MNRAS accepted
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- 2017
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225. Multiple AGN in the crowded field of the compact group SDSS J0959+1259
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De Rosa, A., Bianchi, S., Bogdanović, T., Decarli, R., Herrero-Illana, R., Husemann, B., Komossa, S., Kun, E., Loiseau, N., Paragi, Z., Perez-Torres, M., Piconcelli, E., Schawinski, K., Vignali, C., De Rosa, A., Bianchi, S., Bogdanović, T., Decarli, R., Herrero-Illana, R., Husemann, B., Komossa, S., Kun, E., Loiseau, N., Paragi, Z., Perez-Torres, M., Piconcelli, E., Schawinski, K., and Vignali, C.
- Abstract
We present a multiwavelength study of a newly discovered compact group (CG), SDSS J0959+1259, based data from XMM-Newton, Sloan Digital Sky Survey (SDSS) and the Calar Alto optical imager BUSCA. With a maximum velocity offset of 500km s−1, a mean redshift of 0.035, and a mean spatial extension of 480kpc, this CG is exceptional in having the highest concentration of nuclear activity in the local Universe, established with a sensitivity limit LX > 4 × 1040ergs−1 in 2-10keV band and R-band magnitude MR < −19. The group is composed of two type-2 Seyferts, one type-1 Seyfert, two LINERs and three star-forming galaxies. Given the high X-ray luminosity of LINERs which reaches ∼1041ergs−1, it is likely that they are also accretion driven, bringing the number of active nuclei in this group to five out of eight (AGN fraction of 60 per cent). The distorted shape of one member of the CG suggests that strong interactions are taking place among its galaxies through tidal forces. Therefore, this system represents a case study for physical mechanisms that trigger nuclear activity and star formation in CGs
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- 2017
226. Multi-messenger observations of a binary neutron star merger
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Abbott, B., Abbott, R., Abbott, T., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R., Adya, V., Affeldt, C., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Altin, P., Amato, A., Ananyeva, A., Anderson, S., Anderson, W., Angelova, S., Antier, S., Appert, S., Arai, K., Araya, M., Areeda, J., Arnaud, N., Arun, K., Ascenzi, S., Ashton, G., Ast, M., Aston, S., Astone, P., Atallah, D., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Bader, M., Bae, S., Baker, P., Baldaccini, F., Ballardin, G., Ballmer, S., Banagiri, S., Barayoga, J., Barclay, S., Barish, B., Barker, D., Barkett, K., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Barthelmy, S., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J., Bawaj, M., Bayley, J., Bazzan, M., Becsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A., Berger, B., Bergmann, G., Bero, J., Berry, C., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I., Billingsley, G., Billman, C., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., Bizouard, M., Blackburn, J., Blackman, J., Blair, C., Blair, D., Blair, R., Bloemen, S., Bock, O., Bode, N., Boer, M., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P., Branchesi, M., Brau, J., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Broida, J., Brooks, A., Brown, D., Brunett, S., Buchanan, C., Buikema, A., Bulik, T., Bulten, H., Buonanno, A., Buskulic, D., Buy, C., Byer, R., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J., Callister, T., Calloni, E., Camp, J., Canepa, M., Canizares, P., Cannon, K., Cao, H., Cao, J., Capano, C., Capocasa, E., Carbognani, F., Caride, S., Carney, M., Diaz, J., Casentini, C., Caudill, S., Cavagli, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C., Cerd-Durn, P., Cerretani, G., Cesarini, E., Chamberlin, S., Chan, M., Chao, S., Charlton, P., Chase, E., Chassande-Mottin, E., Chatterjee, D., Chatziioannou, K., Cheeseboro, B., Chen, H., Chen, X., Chen, Y., Cheng, H., Chia, H., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H., Cho, M., Chow, J., Christensen, N., Chu, Q., Chua, A., Chua, S., Chung, A., Chung, S., Ciani, G., Ciolfi, R., Cirelli, C., Cirone, A., Clara, F., Clark, J., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P., Cohen, D., Colla, A., Collette, C., Cominsky, L., Constancio, M., Conti, L., Cooper, S., Corban, P., Corbitt, T., Cordero-Carrion, I., Corley, K., Cornish, N., Corsi, A., Cortese, S., Costa, C., Coughlin, M., Coughlin, S., Coulon, J., Countryman, S., Couvares, P., Covas, P., Cowan, E., Coward, D., Cowart, M., Coyne, D., Coyne, R., Creighton, J., Creighton, T., Cripe, J., Crowder, S., Cullen, T., Cumming, A., Cunningham, L., Cuoco, E., Dal Canton, T., Dlya, G., Danilishin, S., D'Antonio, S., Danzmann, K., Dasgupta, A., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E., Day, B., De, S., Debra, D., Degallaix, J., De laurentis, M., Deleglise, S., Del Pozzo, W., Demos, N., Denker, T., Dent, T., De Pietri, R., Dergachev, V., De Rosa, R., DeRosa, R., De Rossi, C., DeSalvo, R., De Varona, O., Devenson, J., Dhurandhar, S., Diaz, M., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Palma, I., Di Renzo, F., Doctor, Z., Dolique, V., Donovan, F., Dooley, K., Doravari, S., Dorrington, I., Douglas, R., Alvarez, M., Downes, T., Drago, M., Dreissigacker, C., Driggers, J., Du, Z., Ducrot, M., Dupej, P., Dwyer, S., Edo, T., Edwards, M., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S., Eisenstein, R., Essick, R., Estevez, D., Etienne, Z., Etzel, T., Evans, M., Evans, T., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W., Fauchon-Jones, E., Favata, M., Fays, M., Fee, C., Fehrmann, H., Feicht, J., Fejer, M., Fernandez-Galiana, A., Ferrante, I., Ferreira, E., Ferrini, F., Fidecaro, F., Finstad, D., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R., Fitz-Axen, M., Flaminio, R., Fletcher, M., Fong, H., Font, J., Forsyth, P., Forsyth, S., Fournier, J., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fries, E., Fritschel, P., Frolov, V., Fulda, P., Fyffe, M., Gabbard, H., Gadre, B., Gaebel, S., Gair, J., Gammaitoni, L., Ganija, M., Gaonkar, S., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gehrels, N., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, A., Ghosh, S., Giaime, J., Giardina, K., Giazotto, A., Gill, K., Glover, L., Goetz, E., Goetz, R., Gomes, S., Goncharov, B., Gonzlez, G., Castro, J., Gopakumar, A., Gorodetsky, M., Gossan, S., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Granata, M., Grant, A., Gras, S., Gray, C., Greco, G., Green, A., Gretarsson, E., Griswold, B., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G., Guo, X., Gupta, A., Gupta, M., Gushwa, K., Gustafson, E., Gustafson, R., Halim, O., Hall, B., Hall, E., Hamilton, E., Hammond, G., Haney, M., Hanke, M., Hanks, J., Hanna, C., Hannam, M., Hannuksela, O., Hanson, J., Hardwick, T., Harms, J., Harry, G., Harry, I., Hart, M., Haster, C., Haughian, K., Healy, J., Heidmann, A., Heintze, M., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I., Hennig, J., Heptonstall, A., Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hofman, D., Holt, K., Holz, D., Hopkins, P., Horst, C., Hough, J., Houston, E., Howell, E., Hreibi, A., Hu, Y., Huerta, E., Huet, D., Hughey, B., Husa, S., Huttner, S., Huynh-Dinh, T., Indik, N., Inta, R., Intini, G., Isa, H., Isac, J., Isi, M., Iyer, B., Izumi, K., Jacqmin, T., Jani, K., Jaranowski, P., Jawahar, S., Jimenez-Forteza, F., Johnson, W., Jones, D., Jones, R., Jonker, R., Ju, L., Junker, J., Kalaghatgi, C., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J., Kapadia, S., Karki, S., Karvinen, K., Kasprzack, M., Katolik, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Kefelian, F., Keitel, D., Kemball, A., Kennedy, R., Kent, C., Key, J., Khalili, F., Khan, I., Khan, S., Khan, Z., Khazanov, E., Kijbunchoo, N., Kim, C., Kim, J., Kim, K., Kim, W., Kim, Y., Kimbrell, S., King, E., King, P., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J., Kleybolte, L., Klimenko, S., Knowles, T., Koch, P., Koehlenbeck, S., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W., Kowalska, I., Kozak, D., Krmer, C., Kringel, V., Krishnan, B., Krlak, A., Kuehn, G., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B., Lai, K., Landry, M., Lang, R., Lange, J., Lantz, B., Lanza, R., Larson, S., Lartaux-Vollard, A., Lasky, P., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lee, C., Lee, H., Lee, K., Lehmann, J., Lenon, A., Leonardi, M., Leroy, N., Letendre, N., Levin, Y., Li, T., Linker, S., Littenberg, T., Liu, J., Lo, R., Lockerbie, N., London, L., Lord, J., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J., Lousto, C., Lovelace, G., Lck, H., Lumaca, D., Lundgren, A., Lynch, R., Ma, Y., Macas, R., Macfoy, S., Machenschalk, B., MacInnis, M., Macleod, D., Hernandez, I., Magaa-Sandoval, F., Zertuche, L., Magee, R., Majorana, E., Maksimovic, I., Man, N., Mandic, V., Mangano, V., Mansell, G., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Mrka, S., Mrka, Z., Markakis, C., Markosyan, A., Markowitz, A., Maros, E., Marquina, A., Marsh, P., Martelli, F., Martellini, L., Martin, I., Martin, R., Martynov, D., Mason, K., Massera, E., Masserot, A., Massinger, T., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., McCarthy, R., McClelland, D., McCormick, S., McCuller, L., McGuire, S., McIntyre, G., McIver, J., McManus, D., McNeill, L., Mcrae, T., McWilliams, S., Meacher, D., Meadors, G., Mehmet, M., Meidam, J., Mejuto-Villa, E., Melatos, A., Mendell, G., Mercer, R., Merilh, E., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P., Miao, H., Michel, C., Middleton, H., Mikhailov, E., Milano, L., Mueller, A., Mueller, B., Miller, J., Millhouse, M., Milovich-Goff, M., Minazzoli, O., Minenkov, Y., Ming, J., Mishra, C., Mitra, S., Mitrofanov, V., Mitselmakher, G., Mittleman, R., Moffa, D., Moggi, A., Mogushi, K., Mohan, M., Mohapatra, S., Montani, M., Moore, C., Moraru, D., Moreno, G., Morriss, S., Mours, B., Mow-Lowry, C., Mueller, G., Muir, A., Mukherjee, A., Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muniz, E., Muratore, M., Murray, P., Napier, K., Nardecchia, I., Naticchioni, L., Nayak, R., Neilson, J., Nelemans, G., Nelson, T., Nery, M., Neunzert, A., Nevin, L., Newport, J., Newton, G., Ng, K., Nguyen, P., Nguyen, T., Nichols, D., Nielsen, A., Nissanke, S., Nitz, A., Noack, A., Nocera, F., Nolting, D., North, C., Nuttall, L., Oberling, J., O'Dea, G., Ogin, G., Oh, J., Oh, S., Ohme, F., Okada, M., Oliver, M., Oppermann, P., Oram, R., O'Reilly, B., Ormiston, R., Ortega, L., O'Shaughnessy, R., Ossokine, S., Ottaway, D., Overmier, H., Owen, B., Pace, A., Page, J., Page, M., Pai, A., Pai, S., Palamos, J., Palashov, O., Palomba, C., Pal-Singh, A., Pan, H., Pang, B., Pang, P., Pankow, C., Pannarale, F., Pant, B., Paoletti, F., Paoli, A., Papa, M., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perez, C., Perreca, A., Perri, L., Pfeiffer, H., Phelps, M., Piccinni, O., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I., Pirello, M., Pitkin, M., Poe, M., Poggiani, R., Popolizio, P., Porter, E., Post, A., Powell, J., Prasad, J., Pratt, J., Pratten, G., Predoi, V., Prestegard, T., Price, L., Prijatelj, M., Principe, M., Privitera, S., Prodi, G., Prokhorov, L., Puncken, O., Punturo, M., Puppo, P., Prrer, M., Qi, H., Quetschke, V., Quintero, E., Quitzow-James, R., Raab, F., Rabeling, D., Radkins, H., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K., Ramos-Buades, A., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D., Ren, W., Reyes, S., Ricci, F., Ricker, P., Rieger, S., Riles, K., Rizzo, M., Robertson, N., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J., Roma, V., Romano, R., Romel, C., Romie, J., Rosinska, D., Ross, M., Rowan, S., Rdiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Sakellariadou, M., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sampson, L., Sanchez, E., Sanchez, L., Sanchis-Gual, N., Sandberg, V., Sanders, J., Sassolas, B., Sathyaprakash, B., Saulson, P., Sauter, O., Savage, R., Sawadsky, A., Schale, P., Scheel, M., Scheuer, J., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R., Schonbeck, A., Schreiber, E., Schuette, D., Schulte, B., Schutz, B., Schwalbe, S., Scott, J., Scott, S., Seidel, E., Sellers, D., Sengupta, A., Sentenac, D., Sequino, V., Sergeev, A., Shaddock, D., Shaffer, T., Shah, A., Shahriar, M., Shaner, M., Shao, L., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D., Siellez, K., Siemens, X., Sieniawska, M., Sigg, D., Silva, A., Singer, L., Singh, A., Singhal, A., Sintes, A., Slagmolen, B., Smith, B., Smith, J., Smith, R., Somala, S., Son, E., Sonnenberg, J., Sorazu, B., Sorrentino, F., Souradeep, T., Spencer, A., Srivastava, A., Staats, K., Staley, A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S., Stone, R., Stops, D., Strain, K., Stratta, G., Strigin, S., Strunk, A., Sturani, R., Stuver, A., Summerscales, T., Sun, L., Sunil, S., Suresh, J., Sutton, P., Swinkels, B., Szczepanczyk, M., Tacca, M., Tait, S., Talbot, C., Talukder, D., Tanner, D., Tpai, M., Taracchini, A., Tasson, J., Taylor, J., Taylor, R., Tewari, S., Theeg, T., Thies, F., Thomas, E., Thomas, M., Thomas, P., Thorne, K., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K., Toland, K., Tonelli, M., Tornasi, Z., Torres-Forn, A., Torrie, C., Toyr, D., Travasso, F., Traylor, G., Trinastic, J., Tringali, M., Trozzo, L., Tsang, K., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tuyenbayev, D., Ueno, K., Ugolini, D., Unnikrishnan, C., Urban, A., Usman, S., Vahlbruch, H., Vajente, G., Valdes, G., Van Bakel, N., Van Beuzekom, M., van den Brand, J., van den Broeck, C., Vander-Hyde, D., van der Schaaf, L., van Heijningen, J., van Veggel, A., Vardaro, M., Varma, V., Vass, S., Vasuth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetro, F., Vicere, A., Viets, A., Vinciguerra, S., Vine, D., Vinet, J., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S., Wade, A., Wade, L., Wade, M., Walet, R., 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A., Zorn, J., Zywucka, N., Fender, R., Broderick, J., Stewart, A., Ter Veen, S., Shulevski, A., Kavic, M., Simonetti, J., League, C., Tsai, J., Obenberger, K., Nathaniel, K., Taylor, G., Dowell, J., Liebling, S., Estes, J., Lippert, M., Sharma, I., Farella, B., Abeysekara, A., Alfaro, R., Alvarez, C., Arceo, R., Arteaga-Velzquez, J., Rojas, D., Solares, H., Barber, A., Becerril, A., Belmont-Moreno, E., BenZvi, S., Berley, D., Bernal, A., Brisbois, C., Caballero-Mora, K., Capistrn, T., Carramiana, A., Cotti, U., Cotzomi, J., De Leon, S., De Leon, C., De la Fuente, E., Hernandez, R., Dichiara, S., Dingus, B., DuVernois, M., Ellsworth, R., Engel, K., Enriquez-Rivera, O., Fiorino, D., Fleischhack, H., Fraija, N., Garcia-Gonzlez, J., Garfias, F., Gerhardt, M., Muoz, A., Gonzlez, M., Goodman, J., Hampel-Arias, Z., Harding, J., Hernandez, S., Hernandez-Almada, A., Hona, B., Hntemeyer, P., Iriarte, A., Jardin-Blicq, A., Joshi, V., Kaufmann, S., Kieda, D., Lara, A., Lauer, R., Lennarz, D., 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Becker, K., Bellido, J., Berat, C., Bertaina, M., Bertou, X., Biermann, P., Biteau, J., Blaess, S., Blanco, A., Blazek, J., Bleve, C., Bohacova, M., Bonifazi, C., Borodai, N., Botti, A., Brack, J., Brancus, I., Bretz, T., Bridgeman, A., Briechle, F., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caccianiga, L., Cancio, A., Canfora, F., Caruso, R., Castellina, A., Catalani, F., Cataldi, G., Cazon, L., Chavez, A., Chinellato, J., Chudoba, J., Clay, R., Cerutti, A., Colalillo, R., Coleman, A., Collica, L., Coluccia, M., Conceicao, R., Consolati, G., Contreras, F., Cooper, M., Coutu, S., Covault, C., Cronin, J., D'Amico, S., Daniel, B., Dasso, S., Daumiller, K., Dawson, B., Day, J., De Almeida, R., De Jong, S., De Mauro, G., Neto, J., De Mitri, I., De Oliveira, J., De Souza, V., Debatin, J., Deligny, O., Castro, M., Diogo, F., Dobrigkeit, C., D'Olivo, J., Dorosti, Q., Dos Anjos, R., Dova, M., Dundovic, A., Ebr, J., Engel, R., Erdmann, M., Erfani, M., Escobar, C., Espadanal, J., Etchegoyen, A., Falcke, H., Farmer, J., Farrar, G., Fauth, A., Fazzini, N., Feldbusch, F., Fenu, F., Fick, B., Figueira, J., Filipcic, A., Freire, M., Fujii, T., Fuster, A., Gaior, R., Garcia, B., Gemmeke, H., Gherghel-Lascu, A., Ghia, P., Giaccari, U., Giammarchi, M., Giller, M., Glas, D., Glaser, C., Golup, G., Berisso, M., Vitale, P., Gonzlez, N., Gorgi, A., Gottowik, M., Grillo, A., Grubb, T., Guarino, F., Guedes, G., Halliday, R., Hampel, M., Hansen, P., Harari, D., Harrison, T., Harvey, V., Haungs, A., Hebbeker, T., Heck, D., Heimann, P., Herve, A., Hojvat, C., Holt, E., Homola, P., Horandel, J., Horvath, P., Hrabovsky, M., Huege, T., Hulsman, J., Insolia, A., Isar, P., Jandt, I., Johnsen, J., Josebachuili, M., Jurysek, J., Kaapa, A., Kampert, K., Keilhauer, B., Kemmerich, N., Kemp, J., Kieckhafer, R., Klages, H., Kleifges, M., Kleinfeller, J., Krause, R., Krohm, N., Kuempel, D., Mezek, G., Kunka, N., Awad, A., Lago, B., LaHurd, D., Lauscher, M., Legumina, R., De Oliveira, M., Letessier-Selvon, A., Lhenry-Yvon, I., Link, K., Lo Presti, D., Lopes, L., Lopez, R., Casado, A., Lorek, R., Luce, Q., Lucero, A., Malacari, M., Mallamaci, M., Mandat, D., Mantsch, P., Mariazzi, A., Maris, I., Marsella, G., Martello, D., Martinez, H., Bravo, O., Meza, J., Mathes, H., Mathys, S., Matthiae, G., Mayotte, E., Mazur, P., Medina, C., Medina-Tanco, G., Melo, D., Menshikov, A., Merenda, K., Michal, S., Micheletti, M., Middendorf, L., Miramonti, L., Mitrica, B., Mockler, D., Mollerach, S., Montanet, F., Morello, C., Morlino, G., Mueller, M., Mueller, S., Mussa, R., Naranjo, I., Niculescu-Oglinzanu, M., Niechciol, M., Niemietz, L., Niggemann, T., Nitz, D., Nosek, D., Novotny, V., Nozka, L., Nunez, L., Oikonomou, F., Olinto, A., Palatka, M., Pallotta, J., Papenbreer, P., Parente, G., Parra, A., Paul, T., Pech, M., Pedreira, F., Kala, J., Pea-Rodriguez, J., Pereira, L., Perlin, M., Perrone, L., Peters, C., Petrera, S., Phuntsok, J., Pierog, T., Pimenta, M., Pirronello, V., Platino, M., Plum, M., Poh, J., Porowski, C., Prado, R., Privitera, P., Prouza, M., Quel, E., Querchfeld, S., Quinn, S., Ramos-Pollan, R., Rautenberg, J., Ravignani, D., Ridky, J., Riehn, F., Risse, M., Ristori, P., Rizi, V., De Carvalho, W., Fernandez, G., Rojo, J., Roncoroni, M., Roth, M., Roulet, E., Rovero, A., Ruehl, P., Saffi, S., Saftoiu, A., Salamida, F., Saleh, A., Salina, G., Sanchez, F., Sanchez-Lucas, P., Santos, E., Sarazin, F., Sarmento, R., Sarmiento-Cano, C., Sato, R., Schauer, M., Scherini, V., Schieler, H., Schimp, M., Schmidt, D., Scholten, O., Schovnek, P., Schroder, F., Schumacher, J., Sciutto, S., Segreto, A., Shadkam, A., Shellard, R., Sigl, G., Silli, G., Smida, R., Snow, G., Sommers, P., Sonntag, S., Soriano, J., Squartini, R., Stanca, D., Stanic, S., Stasielak, J., Stassi, P., Stolpovskiy, M., Strafella, F., Streich, A., Suarez, F., Suarez-Duran, M., Sudholz, T., Suomijarvi, T., Supanitsky, A., Supik, J., Swain, J., Szadkowski, Z., Taboada, A., Taborda, O., Timmermans, C., Peixoto, C., Tomankova, L., Tome, B., Elipe, G., Travnicek, P., Trini, M., Tueros, M., Ulrich, R., Unger, M., Urban, M., Galicia, J., Valio, I., Valore, L., Van Aar, G., Van Bodegom, P., Van den Berg, A., Van Vliet, A., Varela, E., Cardenas, B., Vazquez, R., Veberic, D., Ventura, C., Quispe, I., Verzi, V., Vicha, J., Villaseor, L., Vorobiov, S., Wahlberg, H., Wainberg, O., Walz, D., Watson, A., Weber, M., Weindl, A., Wiedenski, M., Wiencke, L., Wilczynski, H., Wirtz, M., Wittkowski, D., Wundheiler, B., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zepeda, A., Zimmermann, B., Ziolkowski, M., Zong, Z., Zuccarello, F., Schulze, S., Corral-Santana, J., De Gregorio-Monsalvo, I., Gonzlez-Lopez, J., Hartmann, D., Ishwara-Chandra, C., Martin, S., Mehner, A., Misra, K., Michalowski, M., Resmi, L., Paragi, Z., Agudo, I., An, T., Beswick, R., Casadio, C., Frey, S., Kettenis, M., Marcote, B., Moldon, J., Szomoru, A., Langevelde, H., Cwiek, A., Cwiok, M., Czyrkowski, H., Dabrowski, R., Kasprowicz, G., Mankiewicz, L., Nawrocki, K., Opiela, R., Piotrowski, L., Wrochna, G., Zaremba, M., Zarnecki, A., Haggard, D., Nynka, M., Ruan, J., Bland, Phil, Booler, T., Devillepoix, H., De Gois, J., Hancock, Paul, Howie, Robert, Paxman, Jonathan, Sansom, Eleanor, Towner, Martin, Tonry, J., Stubbs, C., Denneau, L., Heinze, A., Stalder, B., Weiland, H., Eatough, R., Kramer, M., Kraus, A., Piro, L., Gonzlez, J., Butler, N., Khandrika, H., Kutyrev, A., Lee, W., Ricci, R., Ryan, R., Sanchez-Ramirez, R., Veilleux, S., Wieringa, M., Burgess, J., Van Eerten, H., Fontes, C., Korobkin, O., Wollaeger, R., Camilo, F., Foley, A., Goedhart, S., Makhathini, S., Oozeer, N., Smirnov, O., and Woudt, P.
- Abstract
© 2017. The American Astronomical Society. All rights reserved. On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma -ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40 8 8-+ Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 M. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient's position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nu
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- 2017
227. Resolved, expanding jets in the Galactic black hole candidate XTE J1908+094
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Rushton, A., Miller-Jones, J., Curran, P., Sivakoff, G., Rupen, M., Paragi, Z., Spencer, R., Yang, J., Altamirano, D., Belloni, T., Fender, R., Krimm, H., Maitra, D., Migliari, S., Russell, D., Russell, T., Soria, Roberto, Tudose, V., Rushton, A., Miller-Jones, J., Curran, P., Sivakoff, G., Rupen, M., Paragi, Z., Spencer, R., Yang, J., Altamirano, D., Belloni, T., Fender, R., Krimm, H., Maitra, D., Migliari, S., Russell, D., Russell, T., Soria, Roberto, and Tudose, V.
- Abstract
Black hole X-ray binaries undergo occasional outbursts caused by changing inner accretion flows. Here we report high angular resolution radio observations of the 2013 outburst of the black hole candidate X-ray binary system XTE J1908+094, using data from the Very Long Baseline Array and European VLBI Network. We show that following a hard-to-soft state transition, we detect moving jet knots that appear asymmetric in morphology and brightness, and expand to become laterally resolved as they move away from the core, along an axis aligned approximately −11° east of north. We initially see only the southern component, whose evolution gives rise to a 15-mJy radio flare and generates the observed radio polarization. This fades and becomes resolved out after 4 days, after which a second component appears to the north, moving in the opposite direction. From the timing of the appearance of the knots relative to the X-ray state transition, a 90° swing of the inferred magnetic field orientation, the asymmetric appearance of the knots, their complex and evolving morphology, and their low speeds, we interpret the knots as working surfaces where the jets impact the surrounding medium. This would imply a substantially denser environment surrounding XTE J1908+094 than has been inferred to exist around the microquasar sources GRS 1915+105 and GRO J1655−40.
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- 2017
228. The VSOP 5 GHz Active Galactic Nucleus Survey. III. Imaging Results for the First 102 Sources
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Scott, W. K., Fomalont, E. B., Lovell, J. E. J., Moellenbrock, G. A., Dodson, R. G., Edwards, P. G., Coldwell, G. V., Fodor, S., Frey, S., Gurvits, L. I., Lister, M. L., Mosoni, L., Paragi, Z., Piner, B. G., Shen, Z.-Q., Taylor, A. R., Tingay, S. J., Horiuchi, S., Hirabayashi, Hisashi, and Murata, Yasuhiro
- Subjects
Physics ,Astrophysics::High Energy Astrophysical Phenomena ,Astronomy and Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,law.invention ,Telescope ,Core (optical fiber) ,symbols.namesake ,Amplitude ,Space and Planetary Science ,law ,Angular diameter ,Brightness temperature ,Very-long-baseline interferometry ,symbols ,Visibility ,Doppler effect ,Astrophysics::Galaxy Astrophysics - Abstract
著者人数: 20名, Accepted: 2004-05-07, 資料番号: SA1003420000
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- 2004
229. LOFT as a discovery machine for jetted Tidal Disruption Events
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Rossi, E. M., Donnarumma, I., Fender, R., Jonker, P., Komossa, S., Paragi, Z., PRANDONI, ISABELLA, and ZAMPIERI, Luca
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Astrophysics::High Energy Astrophysical Phenomena ,Physics::Space Physics ,Astrophysics::Instrumentation and Methods for Astrophysics ,Astrophysics::Earth and Planetary Astrophysics - Abstract
Questo e' un White Book pubblicato solo su arXiv This is a White Paper in support of the mission concept of the Large Observatory for X-ray Timing (LOFT), proposed as a medium-sized ESA mission. We discuss the potential of LOFT for the study of jetted tidal disruption events. For a summary, we refer to the paper.
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- 2015
230. Very Long Baseline Interferometry with the SKA
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Paragi, Z., Godfrey, L., Reynolds, C., Rioja, M. J., Deller, A., Zhang, B., Gurvits, L., Bietenholz, M., Szomoru, A., Bignall, H. E., Boven, P., Charlot, P., Dodson, R., Frey, S., Garrett, M. A., Imai, H., Lobanov, A., Reid, M. J., Ros, E., van Langevelde, H. J., Zensus, A. J., Zheng, X. W., Alberdi, A., Agudo, I., An, T., Argo, M., Beswick, R., Biggs, A., Brunthaler, A., Campbell, B., Cimo, G., Colomer, F., Corbel, S., Conway, J. E., Cseh, D., Deane, R., Falcke, H. D. E., Gawronski, M., Gaylard, M., Giovannini, G., Giroletti, M., Goddi, C., Goedhart, S., Gómez, J. L., Gunn, A., Kharb, P., Kloeckner, H. R., Koerding, E., Kovalev, Y., Kunert-Bajraszewska, M., Lindqvist, M., Lister, M., Mantovani, F., Marti-Vidal, I., Mezcua, M., McKean, J., Middelberg, E., Miller-Jones, J. C. A., Moldon, J., Muxlow, T., O'Brien, T., Perez-Torres, M., Pogrebenko, S. V., Quick, J., Rushton, A., Schilizzi, R., Smirnov, O., Sohn, B. W., Surcis, G., Taylor, G. B., Tingay, S., Tudose, V. M., van der Horst, A., van Leeuwen, J., Venturi, T., Vermeulen, R., Vlemmings, W. H. T., de Witt, A., Wucknitz, O., Yang, J., Gabänyi, K., and Jung, T.
- Abstract
Adding VLBI capability to the SKA arrays will greatly broaden the science of the SKA, and is feasible within the current specifications. SKA-VLBI can be initially implemented by providing phased-array outputs for SKA1-MID and SKA1-SUR and using these extremely sensitive stations with other radio telescopes, and in SKA2 by realising a distributed configuration providing baselines up to thousands of km, merging it with existing VLBI networks. The motivation for and the possible realization of SKA-VLBI is described in this paper.
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- 2015
231. The Search for Binary Black holes in Seyferts with Double Peaked Emission Lines
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Kharb, P., Das, M., Subramanian, S., and Paragi, Z.
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Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Astrophysics::Galaxy Astrophysics - Abstract
We discuss results from very long baseline interferometry (VLBI) observations of two Seyfert galaxies with double peaked emission lines in their SDSS optical spectra. Such AGN are potential candidates for the presence of binary black holes, which can be resolved on parsec-scales with VLBI. Our observations do not detect twin radio cores but rather nuclear outflows in these Seyferts. These outflows could be interacting with the emission line clouds producing the double peaks in the emission lines., Comment: Refereed proceedings of the RETCO-II meeting held at ARIES, Nainital, India from 6-8 May 2015, to be published in the ASI Conference Series. Edited by I. Chattopadhyay, A. Nandi, S. Das and S. Mandal
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- 2015
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232. Incoherent transient radio emission from stellar-mass compact objects in the SKA era
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Corbel, S., Miller-Jones, J. C. A., Fender, R. P., Elena Gallo, Maccarone, T. J., O Brien, T. J., Paragi, Z., Rupen, M. P., Rushton, A. P., Sabatini, S., Sivakoff, G. R., Strader, J., and Woudt, P. A.
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Solar and Stellar Astrophysics ,FOS: Physical sciences ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics::Galaxy Astrophysics - Abstract
The universal link between the processes of accretion and ejection leads to the formation of jets and outflows around accreting compact objects. Incoherent synchrotron emission from these outflows can be observed from a wide range of accreting binaries, including black holes, neutron stars, and white dwarfs. Monitoring the evolution of the radio emission during their sporadic outbursts provides important insights into the launching of jets, and, when coupled with the behaviour of the source at shorter wavelengths, probes the underlying connection with the accretion process. Radio observations can also probe the impact of jets/outflows (including other explosive events such as magnetar giant flares) on the ambient medium, quantifying their kinetic feedback. The high sensitivity of the SKA will open up new parameter space, enabling the monitoring of accreting stellar-mass compact objects from their bright, Eddington-limited outburst states down to the lowest-luminosity quiescent levels, whose intrinsic faintness has to date precluded detailed studies. A census of quiescently accreting black holes will also constrain binary evolution processes. By enabling us to extend our existing investigations of black hole jets to the fainter jets from neutron star and white dwarf systems, the SKA will permit comparative studies to determine the role of the compact object in jet formation. The high sensitivity, wide field of view and multi-beaming capability of the SKA will enable the detection and monitoring of all bright flaring transients in the observable local Universe, including the ULXs, ... [Abridged] This chapter reviews the science goals outlined above, demonstrating the progress that will be made by the SKA. We also discuss the potential of the astrometric and imaging observations that would be possible should a significant VLBI component be included in the SKA., Comment: To be published in: "Advancing Astrophysics with the Square Kilometre Array", Proceedings of Science, PoS(AASKA14)
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- 2015
- Full Text
- View/download PDF
233. Very long baseline interferometry with the SKA
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Paragi, Z., Godfrey, L., Gurvits, L., and et al
- Abstract
Adding VLBI capability to the SKA arrays will greatly broaden the science of the SKA, and is feasible within the current specifications. SKA-VLBI can be initially implemented by providing phased-array outputs for SKA1-MID and SKA1-SUR and using these extremely sensitive stations with other radio telescopes, and in SKA2 by realising a distributed configuration providing baselines up to thousands of km, merging it with existing VLBI networks. The motivation for and the possible realization of SKA-VLBI is described in this paper.
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- 2014
234. Future mmVLBI Research with ALMA: A European vision
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Tilanus, R. P. J., Krichbaum, T. P., Zensus, J. A., Baudry, Alain, Vlemmings, W., Abraham, Z., Afonso, J., Agudo, I., Alberdi, A., Alcolea, J., Altamirano, D., Asadi, S., Assaf, K., Augusto, P., Baczko, A-K., Boeck, M., Boller, T., Bondi, M., Boone, F., Bourda, G., Brajsa, R., Brand, J., Britzen, S., Bujarrabal, V., Cales, S., Casadio, C., Casasola, V., Castangia, P., Cernicharo, J., Charlot, P., Chemin, L., Clenet, Y., Colomer, F., Combes, F., Cordes, J., Coriat, M., Cross, N., D'Ammando, F., Dallacasa, D., Desmurs, J-F., Eatough, R., Eckart, A., Eisenacher, D., Etoka, S., Felix, M., Fender, R., Ferreira, M., Freeland, E., Frey, S., Fromm, C., Fuhrmann, L., Gabanyi, K., Galvan-Madrid, R., Giroletti, M., Goddi, C., Gomez, J., Gourgoulhon, E., Gray, M., Di Gregorio, I., Greimel, R., Grosso, N., Guirado, J., Hada, K., Hanslmeier, A., Henkel, C., Herpin, Fabrice, Hess, P., Hodgson, J., Horns, D., Humphreys, E., Kramer, B. Hutawarakorn, Ilyushin, V., Impellizzeri, V., Ivanov, V., Julião, M., Kadler, M., Kerins, E., Klaassen, P., Klooster, K. Van 'T, Kording, E., Kozlov, M., Kramer, M., Kreikenbohm, A., Kurtanidze, O., Lazio, J., Leite, A., Leitzinger, M., Lepine, J., Levshakov, S., Lico, R., Lindqvist, M., Liuzzo, E., Lobanov, A., Lucas, Philippe, Mannheim, K., Marcaide, J., Markoff, S., Martí-Vidal, I., Martins, C., Masetti, N., Massardi, M., Menten, K., Messias, H., Migliari, S., Mignano, A., Miller-Jones, J., Minniti, D., Molaro, P., Molina, S., Monteiro, A., Moscadelli, L., Mueller, C., Müller, A., Muller, S., Niederhofer, F., Odert, P., Olofsson, H., Orienti, M., Paladino, R., Panessa, F., Paragi, Z., Paumard, T., Pedrosa, P., Pérez-Torres, M., Perrin, G., Perucho, M., Porquet, D., Prandoni, I., Ransom, S., Reimers, D., Rejkuba, M., Rezzolla, L., Richards, A., Ros, E., Roy, A., Rushton, A., Savolainen, T., Schulz, R., Silva, M., Sivakoff, G., Soria-Ruiz, R., Soria, R., Spaans, M., Spencer, R., Stappers, B., Surcis, G., Tarchi, A., Temmer, M., Thompson, M., Torrelles, J., Truestedt, J., Tudose, V., Venturi, T., Verbiest, J., Vieira, J., Vielzeuf, P., Vincent, F., Wex, N., Wiik, K., Wiklind, T., Wilms, J., Zackrisson, E., Zechlin, H., Bremer, M., Bremer, Michael, Falcke, H., FORMATION STELLAIRE 2014, Laboratoire d'astrodynamique, d'astrophysique et d'aéronomie de bordeaux (L3AB), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB), AUTRES, M2A 2014, Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid 28850, Spain, Ctr Astrobiol CSIC INTA, Lab Astrofis Mol, Madrid, SSE 2014, Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), Centro de Biologia Molecular e Ambiental (CBMA), Universidade do Minho, Max-Planck-Institut für Extraterrestrische Physik (MPE), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut für Physik (Institut für Physik), Universität Potsdam, National Center for Atmospheric Research [Boulder] (NCAR), Institute for Geophysics, Astrophysics and Meteorology [Graz] (IGAM), Karl-Franzens-Universität Graz, OncoRay - National Center for Radiation Research in Oncology, Medical Faculty Carl Gustav Carus, TU Dresden, Space Research Institute of Austrian Academy of Sciences (IWF), Austrian Academy of Sciences (OeAW), Onsala Space Observatory (OSO), Chalmers University of Technology [Göteborg], DAM Île-de-France (DAM/DIF), Direction des Applications Militaires (DAM), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Milieux aquatiques, écologie et pollutions (UR MALY), Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA), University of Utrecht, Utrecht University [Utrecht], Departamento de Química, Universidade de Coimbra [Coimbra], Kapteyn Astronomical Institute [Groningen], University of Groningen [Groningen], GoLP/Instituto Plasmas e Fusa˜o Nuclear, Instituto Superior Técnico, Universidade Técnica de Lisboa (IST), ONERA - The French Aerospace Lab [Toulouse], ONERA, Onsala Space Observatory, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Universidade do Minho = University of Minho [Braga], and University of Potsdam = Universität Potsdam
- Subjects
[PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Astrophysics::Galaxy Astrophysics ,[SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM] - Abstract
Very long baseline interferometry at millimetre/submillimetre wavelengths (mmVLBI) offers the highest achievable spatial resolution at any wavelength in astronomy. The anticipated inclusion of ALMA as a phased array into a global VLBI network will bring unprecedented sensitivity and a transformational leap in capabilities for mmVLBI. Building on years of pioneering efforts in the US and Europe the ongoing ALMA Phasing Project (APP), a US-led international collaboration with MPIfR-led European contributions, is expected to deliver a beamformer and VLBI capability to ALMA by the end of 2014 (APP: Fish et al. 2013, arXiv:1309.3519). This report focuses on the future use of mmVLBI by the international users community from a European viewpoint. Firstly, it highlights the intense science interest in Europe in future mmVLBI observations as compiled from the responses to a general call to the European community for future research projects. A wide range of research is presented that includes, amongst others: - Imaging the event horizon of the black hole at the centre of the Galaxy - Testing the theory of General Relativity an/or searching for alternative theories - Studying the origin of AGN jets and jet formation - Cosmological evolution of galaxies and BHs, AGN feedback - Masers in the Milky Way (in stars and star-forming regions) - Extragalactic emission lines and astro-chemistry - Redshifted absorption lines in distant galaxies and study of the ISM and circumnuclear gas - Pulsars, neutron stars, X-ray binaries - Testing cosmology - Testing fundamental physical constants
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- 2014
235. The VSOP Survey II: Reduction Methods
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MOELLENBROCK, G.A., LOVELL, J., FOMALONT, E., DODSON, R., DOUGHERTY, S., EDARDS, P., FREY, S., GURVITS, L., LISTER, M., MURPHY, D., PARAGI, Z., PINTER, G., SCOTT, W., SHEN, Z., TINGAY, S., ASAKI, Y., JAUNCEY, D., LANGSTON, G., MEIER, D., MOFFET, D., PRESTON, R., TAYLOR, R., HORIUCHI, Shinji, HIRABAYASHI, H., MURATA, Yasuhiro, and WAJIMA, Kiyoaki
- Abstract
VSOPシンポジウム(2000年1月19日-21日. 宇宙科学研究所(ISAS)), 相模原市, 神奈川県, VSOP Symposium (January 19-21, 2000. Institute of Space and Astronautical Science(ISAS)), Sagamihara, Kanagawa Japan, 著者人数: 26名, 資料番号: SA6000155036
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- 2000
236. The VSOP Survey III: Statistical Results
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LOVELL, J.E.J., HORIUCHI, S., MOELLENBROCK, G., FOMALONT, E., DONSON, R., DOUGHERTY, S., EDWARDS, P., FREY, S., GURVITS, L., LISTER, M., MURPHY, D., PARAGI, Z., PINTER, B., SCOTT, W., SHEN, Z.-Q., TINGAY, S., CARLSON, B., SHIBATA, K. M., QUICK, J., COSTA, M., TZIOUMIS, A., TRIGILIO, C., NAKAJIMA, J., XINYONG, H., WEI, W., HIRABAYASHI, Hisashi, and INOUE, M.
- Abstract
VSOPシンポジウム(2000年1月19日-21日. 宇宙科学研究所(ISAS)), 相模原市, 神奈川県, VSOP Symposium (January 19-21, 2000. Institute of Space and Astronautical Science(ISAS)), Sagamihara, Kanagawa Japan, 著者人数: 29名, 資料番号: SA6000155037
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- 2000
237. VSOP Observations of 3C 216
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PARAGI, Z., FREY, S., FEJES, I., PORCAS, R. W., SCHILIZZI, R. T., and VENTURI, T.
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VSOPシンポジウム(2000年1月19日-21日. 宇宙科学研究所(ISAS)), 相模原市, 神奈川県, VSOP Symposium (January 19-21, 2000. Institute of Space and Astronautical Science(ISAS)), Sagamihara, Kanagawa Japan, 資料番号: SA6000155014
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- 2000
238. VLBI observations of four radio quasars at z > 4: blazars or not?
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Cao, H. M., primary, Frey, S., additional, Gabányi, K. É., additional, Paragi, Z., additional, Yang, J., additional, Cseh, D., additional, Hong, X.-Y., additional, and An, T., additional
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- 2017
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239. The Host Galaxy and Redshift of the Repeating Fast Radio Burst FRB 121102
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Tendulkar, S. P., primary, Bassa, C. G., additional, Cordes, J. M., additional, Bower, G. C., additional, Law, C. J., additional, Chatterjee, S., additional, Adams, E. A. K., additional, Bogdanov, S., additional, Burke-Spolaor, S., additional, Butler, B. J., additional, Demorest, P., additional, Hessels, J. W. T., additional, Kaspi, V. M., additional, Lazio, T. J. W., additional, Maddox, N., additional, Marcote, B., additional, McLaughlin, M. A., additional, Paragi, Z., additional, Ransom, S. M., additional, Scholz, P., additional, Seymour, A., additional, Spitler, L. G., additional, van Langevelde, H. J., additional, and Wharton, R. S., additional
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- 2017
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240. The Repeating Fast Radio Burst FRB 121102 as Seen on Milliarcsecond Angular Scales
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Marcote, B., primary, Paragi, Z., additional, Hessels, J. W. T., additional, Keimpema, A., additional, Langevelde, H. J. van, additional, Huang, Y., additional, Bassa, C. G., additional, Bogdanov, S., additional, Bower, G. C., additional, Burke-Spolaor, S., additional, Butler, B. J., additional, Campbell, R. M., additional, Chatterjee, S., additional, Cordes, J. M., additional, Demorest, P., additional, Garrett, M. A., additional, Ghosh, T., additional, Kaspi, V. M., additional, Law, C. J., additional, Lazio, T. J. W., additional, McLaughlin, M. A., additional, Ransom, S. M., additional, Salter, C. J., additional, Scholz, P., additional, Seymour, A., additional, Siemion, A., additional, Spitler, L. G., additional, Tendulkar, S. P., additional, and Wharton, R. S., additional
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- 2017
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241. A direct localization of a fast radio burst and its host
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Chatterjee, S., primary, Law, C. J., additional, Wharton, R. S., additional, Burke-Spolaor, S., additional, Hessels, J. W. T., additional, Bower, G. C., additional, Cordes, J. M., additional, Tendulkar, S. P., additional, Bassa, C. G., additional, Demorest, P., additional, Butler, B. J., additional, Seymour, A., additional, Scholz, P., additional, Abruzzo, M. W., additional, Bogdanov, S., additional, Kaspi, V. M., additional, Keimpema, A., additional, Lazio, T. J. W., additional, Marcote, B., additional, McLaughlin, M. A., additional, Paragi, Z., additional, Ransom, S. M., additional, Rupen, M., additional, Spitler, L. G., additional, and van Langevelde, H. J., additional
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- 2017
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242. On the nature of bright compact radio sources at z > 4.5
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Coppejans, R., Frey, S., Cseh, D., Müller, C., Paragi, Z., Falcke, H., Gabányi, K.É., Gurvits, L.I., An, T., Titov, O., Coppejans, R., Frey, S., Cseh, D., Müller, C., Paragi, Z., Falcke, H., Gabányi, K.É., Gurvits, L.I., An, T., and Titov, O.
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Contains fulltext : 161148.pdf (preprint version ) (Open Access)
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- 2016
243. What are the megahertz peaked-spectrum sources?
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Coppejans, R., Cseh, D., Velzen, S. van, Falcke, H., Intema, H.T., Paragi, Z., Müller, C., Williams, W.L., Frey, S., Gurvits, L.I., Körding, E.G., Coppejans, R., Cseh, D., Velzen, S. van, Falcke, H., Intema, H.T., Paragi, Z., Müller, C., Williams, W.L., Frey, S., Gurvits, L.I., and Körding, E.G.
- Abstract
Contains fulltext : 157960.pdf (publisher's version ) (Open Access)
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- 2016
244. Unveiling multiple AGN activity in galaxy mergers
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De Rosa, A., Bianchi, S., Bogdanovic, T., Decarli, R., Heidt, J., Herrero-Illana, R., Husemann, B., Komossa, S., Kun, E., Loiseau, N., Guainazzi, M., Paragi, Z., Perez-Torres, M., Piconcelli, E., Schawinski, K., Vignali, C., De Rosa, A., Bianchi, S., Bogdanovic, T., Decarli, R., Heidt, J., Herrero-Illana, R., Husemann, B., Komossa, S., Kun, E., Loiseau, N., Guainazzi, M., Paragi, Z., Perez-Torres, M., Piconcelli, E., Schawinski, K., and Vignali, C.
- Abstract
In this paper we present an overview of the MAGNA (Multiple AGN Activity) project aiming at a comprehensive study of multiple supemassive black hole systems. With the main goal to characterize the sources in merging systems at different stages of evolution, we selected a sample of objects optically classified as multiple systems on the basis of emission line diagnostics and started a massive multiband observational campaign. Here we report on the discovery of the exceptionally high AGN density compact group SDSS~J0959+1259. A multiband study suggests that strong interactions are taking place among its galaxies through tidal forces, therefore this system represents a case study for physical mechanisms that trigger nuclear activity and star formation. We also present a preliminary analysis of the multiple AGN system SDSS~J1038+3921.}, Comment: Proceedings paper for "XMM-Newton: The Next Decade" (held in 2016 May); accepted to be published in Astronomische Nachrichten / Astronomical Notes (AN)
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- 2016
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245. Four dual AGN candidates observed with the VLBA
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Gabányi, K. É., An, T., Frey, S., Komossa, S., Paragi, Z., Hong, X. -Y., Shen, Z. -Q., Gabányi, K. É., An, T., Frey, S., Komossa, S., Paragi, Z., Hong, X. -Y., and Shen, Z. -Q.
- Abstract
According to hierarchical structure formation models, merging galaxies are expected to be seen in different stages of their coalescence. However, currently there are no straightforward observational methods neither to select nor to confirm a large number of dual active galactic nuclei (AGN) candidates. Most attempts involve the better understanding of double-peaked narrow emission line sources, to distinguish the objects where the emission lines originate from narrow-line kinematics or jet-driven outflows from those which might harbour dual AGN. We observed four such candidate sources with the Very Long Baseline Array (VLBA) at 1.5 GHz with $\sim$ 10 milli-arcsecond angular resolution where spectral profiles of AGN optical emission suggested the existence of dual AGN. In SDSS J210449.13-000919.1 and SDSS J23044.82-093345.3, the radio structures are aligned with the optical emission features, thus the double-peaked emission lines might be the results of jet-driven outflows. In the third detected source SDSS J115523.74+150756.9, the radio structure is less extended and oriented nearly perpendicular to the position angle derived from optical spectroscopy. The fourth source remained undetected with the VLBA but it has been imaged with the Very Large Array at arcsec resolution a few months before our observations, suggesting the existence of extended radio structure. In none of the four sources did we detect two radio-emitting cores, a convincing signature of duality., Comment: 35 pages, 3 figures, 2 tables, accepted for publication in ApJ
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- 2016
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246. On the nature of FRB 150418: clues from European VLBI Network and e-MERLIN observations
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Giroletti, M., Marcote, B., Garrett, M., Paragi, Z., Yang, J., Hada, K., Muxlow, T. W. B., Cheung, C. C., Giroletti, M., Marcote, B., Garrett, M., Paragi, Z., Yang, J., Hada, K., Muxlow, T. W. B., and Cheung, C. C.
- Abstract
We investigate the nature of the compact, and possibly variable nuclear radio source in the centre of WISE J0716-19, the proposed host galaxy of fast radio burst, FRB 150418. We observed WISE J0716-19 at 5.0 GHz with the European VLBI Network four times between 2016 March 16 and June 2. At three epochs, we simultaneously observed the source with e-MERLIN at the same frequency. We detected a compact source in the EVN data in each epoch with a significance up to ~8sigma. The four epochs yielded consistent results within their uncertainties, for both peak surface intensity and positions. The mean values for these quantities are I_peak = (115+-9) {\mu}Jy/beam and r.a. = 07:16:34.55496(7), dec. = -19:00:39.4754(8), respectively. The e-MERLIN data provided ~3-5sigma detections, at a position consistent with those of the EVN data. The presence of emission on angular scales intermediate between the EVN and e-MERLIN is consistent with being null. The brightness temperature of the EVN core is Tb~10^8.5K, close to the value required by Akiyama & Johnson (2016) to explain the radio properties of WISE J0716-19 in terms of interstellar induced short-term variability. Our observations provide direct, independent evidence of the existence of a nuclear compact source in WISE J0716-19, a physical scenario with no evident connection with FRB 150418. However, the EVN data do not show indication of the variability observed with the VLA., Comment: 4 pages, accepted for publication in A&A Letters to the Editor
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- 2016
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247. No apparent superluminal motion in the first-known jetted tidal disruption event Swift J1644+5734
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Yang, J., Paragi, Z., van der Horst, A. J., Gurvits, L. I., Campbell, R. M., Giannios, D., An, T., Komossa, S., Yang, J., Paragi, Z., van der Horst, A. J., Gurvits, L. I., Campbell, R. M., Giannios, D., An, T., and Komossa, S.
- Abstract
The first-known tidal disruption event (TDE) with strong evidence for a relativistic jet -- based on extensive multi-wavelength campaigns -- is Swift J1644+5734. In order to directly measure the apparent speed of the radio jet, we performed very long baseline interferometry (VLBI) observations with the European VLBI network (EVN) at 5 GHz. Our observing strategy was to identify a very nearby and compact radio source with the real-time e-EVN, and then utilise this source as a stationary astrometry reference point in the later five deep EVN observations. With respect to the in-beam source FIRST J1644+5736, we have achieved a statistical astrometric precision about 12 micro-arcsecond (68 % confidence level) per epoch. This is one of the best phase-referencing measurements available to date. No proper motion has been detected in the Swift J1644+5734 radio ejecta. We conclude that the apparent average ejection speed between 2012.2 and 2015.2 was less than 0.3c with a confidence level of 99 %. This tight limit is direct observational evidence for either a very small viewing angle or a strong jet deceleration due to interactions with a dense circum-nuclear medium, in agreement with some recent theoretical studies., Comment: 5 pages, 3 figures, 4 table, accepted by MNRAS Letters
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- 2016
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248. The LOFT mission concept: a status update
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den Herder, Jan-Willem A., Takahashi, Tadayuki, Bautz, Marshall, Feroci, M., Bozzo, E., Brandt, Søren, Hernanz, M., van der Klis, M., Liu, L.-P., Orleanski, P., Pohl, M., Santangelo, A., Schanne, S., Stella, L., Takahashi, T., Tamura, H., Watts, A., Wilms, J., Zane, S., Bhattacharyya, S., Agudo, I., Ahangarianabhari, M., Albertus, C., Alford, M., Alpar, A., Altamirano, D., Alvarez, L., Amati, L., Amoros, C., Andersson, Niclas, Antonelli, A., Argan, A., Artigue, R., Artigues, B., Atteia, J.-L., Azzarello, P., Bakala, P., Ballantyne, D., Baldazzi, G., Baldo, M., Balman, S., Barbera, M., van Baren, C., Barret, D., Baykal, A., Begelman, M., Behar, O., Belloni, T., Bernardini, F., Bertuccio, G., Bianchi, S., Bianchini, A., Binko, P., Blay, P., Bocchino, F., Bode, M., Bodin, Peter, Bombaci, I., Bonnet Bidaud, J.-M., Boutloukos, S., Bouyjou, F., Bradley, L., Braga, J., Briggs, M. S., Brown, Elliot John, Buballa, M., Bucciantini, N., Burderi, L., Burgay, M., Bursa, M., Budtz-Jørgensen, Carl, Cackett, E., Cadoux, F., Cais, P., Caliandro, G. A., Campana, S., Cao, Xianyi, Capitanio, F., Casares, J., Casella, P., Castro-Tirado, A. J., Cavazzuti, E., Cavechi, Y., Celestin, S., Cerda-Duran, P., Chakrabarty, D., Chamel, N., Château, F., Chen, Y., Chenevez, Jérôme, Chernyakova, M., Coker, J., Cole, R., Collura, A., Coriat, M., Cornelisse, R., Costamante, L., Cros, A., Cui, W., Cumming, A., Cusumano, G., Czerny, B., D'Aì, A., D'Ammando, F., D'Elia, V., Dai, Zhuojun, Del Monte, E., De Luca, A., De Martino, D., Dercksen, J. P. C., De Pasquale, M., De Rosa, A., Del Santo, M., Di Cosimo, S., Degenaar, N., den Herder, J. W., Diebold, S., Di Salvo, T., Dong, Y., Donnarumma, I., Doroshenko, V., Doyle, G., Drake, S. A., Durant, M., Emmanoulopoulos, D., Enoto, T., Erkut, M. H., Esposito, P., Evangelista, Y., Fabian, A., Falanga, M., Favre, Y., Feldman, C., Fender, R., Feng, Huan, Ferrari, V., Ferrigno, C., Finger, M. H., Fraser, G. W., Frericks, M., Fullekrug, M., Fuschino, F., Gabler, M., Galloway, D. K., Gálvez Sanchez, J. L., Gandhi, P., Gao, Z., Garcia-Berro, E., Gendre, B., Gevin, O., Gezari, S., Giles, A. B., Gilfanov, M., Giommi, P., Giovannini, G., Giroletti, M., Gogus, E., Goldwurm, A., Goluchová, K., Götz, D., Gou, L., Gouiffes, C., Grandi, P., Grassi, M., Greiner, J., Grinberg, V., Groot, P., Gschwender, M., Gualtieri, L., Guedel, M., Guidorzi, C., Guy, L., Haas, D., Haensel, P., Hailey, M., Hamuguchi, K., Hansen, Flemming, Hartmann, D. H., Haswell, C. A., Hebeler, K., Heger, A., Hempel, M., Hermsen, W., Homan, J., Hornstrup, Allan, Hudec, R., Huovelin, J., Huppenkothen, D., Inam, S. C., Ingram, A., In't Zand, J. J. M., Israel, G., Iwasawa, K., Izzo, L., Jacobs, H. M., Jetter, F., Johannsen, T., Jenke, P. A., Jonker, P., Josè, J., Kaaret, P., Kalamkar, K., Kalemci, E., Kanbach, G., Karas, V., Karelin, D., Kataria, D., Keek, L., Kennedy, T., Klochkov, D., Kluzniak, W., Koerding, E., Kokkotas, K., Komossa, S., Korpela, S., Kouveliotou, C., Kowalski, A. F., Kreykenbohm, I., Kuiper, L. M., Kunneriath, D., Kurkela, A., Kuvvetli, Irfan, La Franca, F., Labanti, C., Lai, D., Lamb, F. K., Lachaud, C., Laubert, P. P., Lebrun, F., Li, X., Liang, E., Limousin, O., Lin, D., Linares, M., Linder, D., Lodato, G., Longo, F., Lu, F., Lund, Niels, Maccarone, T. J., Macera, D., Maestre, S., Mahmoodifar, S., Maier, D., Malcovati, P., Malzac, J., Malone, C., Mandel, I., Mangano, V., Manousakis, A., Marelli, M., Margueron, J., Marisaldi, M., Markoff, S. B., Markowitz, A., Marinucci, A., Martindale, A., Martínez, G., McHardy, I. M., Medina-Tanco, G., Mehdipour, M., Melatos, A., Mendez, M., Mereghetti, S., Migliari, S., Mignani, R., Michalska, M., Mihara, T., Miller, J. 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S., Rea, N., Reddy, S., Reig, P., Reina Aranda, M., Remillard, R., Reynolds, C., Rezzolla, L., Ribo, M., de la Rie, R., Riggio, A., Rios, A., Rischke, D. H., Rodríguez-Gil, P., Rodriguez, J., Rohlfs, R., Romano, P., Rossi, E. M. R., Rozanska, A., Rousseau, A., Rudak, B., Russell, D. M., Ryde, F., Sabau-Graziati, L., Sakamoto, T., Sala, G., Salvaterra, R., Salvetti, D., Sanna, A., Sandberg, J., Savolainen, T., Scaringi, S., Schaffner-Bielich, J., Schatz, H., Schee, J., Schmid, C., Serino, M., Shakura, N., Shore, S., Schnittman, J. D., Schneider, Raphael, Schwenk, A., Schwope, A. D., Sedrakian, A., Seyler, J.-Y., Shearer, A., Slowikowska, A., Sims, M., Smith, P. J., Sobolewska, M., Sochora, V., Soffitta, P., Soleri, P., Song, L., Spencer, A., Stamerra, A., Stappers, B., Staubert, R., Steiner, A. W., Stergioulas, N., Stevens, A. L., Stratta, G., Strohmayer, T. E., Stuchlik, Z., Suchy, S., Suleimanov, V., Tamburini, F., Tauris, T., Tavecchio, F., Tenzer, C., Thielemann, F. K., Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Torok, G., Torrejon, J. M., Torres, D. F., Torresi, Elena, Tramacere, A., Traulsen, I., Trois, A., Turolla, R., Turriziani, S., Typel, S., Uter, P., Uttley, P., Vacchi, A., Varniere, P., Vaughan, S., Vercellone, S., Vietri, M., Vincent, F. H., Vrba, V., Walton, D., Wang, Z., Watanabe, Shigeki, Wawrzaszek, R., Webb, N., Weinberg, N., Wende, H., Wheatley, P., Wijers, R., Wijnands, R., Wille, Mads, Wilson-Hodge, C. A., Winter, B., Walk, S. J., Wood, K., Woosley, S. E., Wu, X., Xu, Ruichao, Yu, Wenye, Yuan, Y., Zampa, N., Zampieri, L., Zdunik, L., Zdziarski, A., Zech, A., Zhang, S., Zingale, M., and Zwart, F.
- Published
- 2016
249. Swift J1644+5734: the EVN view
- Author
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Paragi, Z., primary, Yang, J., additional, Komossa, S., additional, van der Horst, A., additional, Gurvits, L. I., additional, Campbell, R. M., additional, Giannios, D., additional, and An, T., additional
- Published
- 2016
- Full Text
- View/download PDF
250. Searching for a pair of accreting supermassive black holes in J1425+3231
- Author
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Gabányi, K. É., primary, Frey, S., additional, Paragi, Z., additional, An, T., additional, and Komossa, S., additional
- Published
- 2016
- Full Text
- View/download PDF
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