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151. Multi-wavelength campaign on NGC 7469

Author

Arav, N., Xu, X., Kriss, G. A., Chamberlain, C., Miller, T., Behar, E., Kaastra, J. S., Ely, J. C., Peretz, U., Mehdipour, M., Branduardi-Raymont, G., Bianchi, S., Cappi, M., Costantini, E., De Marco, B., di Gesu, L., Ebrero, J., Kaspi, S., Middei, R., Petrucci, P.-O., Ponti, G., Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), and Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)

Subjects
galaxies: clusters: individual: NGC 7469, [SDU]Sciences of the Universe [physics], ultraviolet: galaxies, galaxies: abundances, galaxies: Seyfert
Abstract

International audience; Context. AGN outflows are thought to influence the evolution of their host galaxies and their super massive black holes. To better understand these outflows, we executed a deep multiwavelength campaign on NGC 7469. The resulting data, combined with those of earlier epochs, allowed us to construct a comprehensive physical, spatial, and temporal picture for this AGN wind. Aims: Our aim is to determine the distance of the UV outflow components from the central source, their abundances and total column-density, and the mechanism responsible for their observed absorption variability. Methods: We studied the UV spectra acquired during the campaign as well as from three previous epochs (2002-2010). Our main analysis tools are ionic column-density extraction techniques and photoionization models (both equilibrium and time-dependent models) based on the code CLOUDY. Results: For component 1 (at -600 km s-1) our findings include the following: metallicity that is roughly twice solar; a simple model based on a fixed total column-density absorber, reacting to changes in ionizing illumination that matches the different ionic column densities derived from four spectroscopic epochs spanning 13 years; and a distance of R = 6+2.5-1.5 pc from the central source. Component 2 (at -1430 km s-1) has shallow troughs and is at a much larger R. For component 3 (at -1880 km s-1) our findings include: a similar metallicity to component 1; a photoionization-based model can explain the major features of its complicated absorption trough variability and an upper limit of 60 or 150 pc on R. This upper limit is consistent and complementary to the X-ray derived lower limit of 12 or 31 pc for R. The total column density of the UV phase is roughly 1% and 0.1% of the lower and upper ionization components of the warm absorber, respectively. Conclusions: The NGC 7469 outflow shows super-solar metallicity similar to the outflow in Mrk 279, carbon and nitrogen are twice and four times more abundant than their solar values, respectively. Similar to the NGC 5548 case, a simple model can explain the physical characteristics and the variability observed in the outflow.

Published
2020

152. Continuous and pulsed selective laser melting of Ti6Al4V lattice structures: Effect of post-processing on microstructural anisotropy and fatigue behaviour

Author

Karami, K. (author), Blok, A. (author), Weber, L.R.M. (author), Ahmadi, S.M. (author), Petrov, R.H. (author), Nikolic, Ksenija (author), Borisov, E.V. (author), Leeflang, M.A. (author), Ayas, C. (author), Zadpoor, A.A. (author), Mehdipour, M. (author), Reinton, T.E. (author), Popovich, V. (author), Karami, K. (author), Blok, A. (author), Weber, L.R.M. (author), Ahmadi, S.M. (author), Petrov, R.H. (author), Nikolic, Ksenija (author), Borisov, E.V. (author), Leeflang, M.A. (author), Ayas, C. (author), Zadpoor, A.A. (author), Mehdipour, M. (author), Reinton, T.E. (author), and Popovich, V. (author)

Abstract

Additive manufacturing technologies in general and laser powder bed fusion (L-PBF) in particular have been on the rise in different applications, including biomedical implants. The effects of the various L-PBF process parameters on the microstructure and properties of Ti6Al4V lattice structures have been studied before. However, the relationship between the different modes of laser scanning and the resulting microstructure, internal imperfections, and surface morphology is still underexplored. In this study, the aforementioned parameters and their effect on the compressive mechanical properties and fatigue behaviour of lattice titanium have been studied for both continuous and pulsed laser scanning modes. Moreover, the influence of various combinations of post-processing treatments, such as hot isostatic pressing (HIP), sandblasting, and chemical etching, on the quasi-static mechanical properties and fatigue endurance of the resulting materials were investigated. It was found that continuous laser strategy results in fewer imperfections and higher fatigue resistance, while pulsed laser showed a more homogenous microstructure; likely leading to a more isotropic behaviour. Furthermore, the continuous mode showed larger prior β grains preferentially oriented in the building direction, while pulsed specimens exhibited finer equiaxed grains with no preferred orientations. The highest level of fatigue life was obtained by using an optimized combination of HIP, sandblasting, and chemical etching., (OLD) MSE-5, (OLD) MSE-3, Biomaterials & Tissue Biomechanics, Structural Optimization and Mechanics

Published
2020
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153. Zero valent iron core–iron oxide shell nanoparticles as small magnetic particle imaging tracers

Author

Gloag, L, Mehdipour, M, Ulanova, M, Mariandry, K, Nichol, MA, Hernández-Castillo, DJ, Gaudet, J, Qiao, R, Zhang, J, Nelson, M, Thierry, B, Alvarez-Lemus, MA, Tan, TT, Gooding, JJ, Braidy, N, Sachdev, PS, Tilley, RD, Gloag, L, Mehdipour, M, Ulanova, M, Mariandry, K, Nichol, MA, Hernández-Castillo, DJ, Gaudet, J, Qiao, R, Zhang, J, Nelson, M, Thierry, B, Alvarez-Lemus, MA, Tan, TT, Gooding, JJ, Braidy, N, Sachdev, PS, and Tilley, RD

Abstract

Zero valent iron core–iron oxide shell nanoparticles coated with a multi-phosphonate brush co-polymer are shown to be small and effective magnetic nanoparticle imaging tracers.

Published
2020

154. Intensive disc-reverberation mapping of Fairall 9:first year of Swift and LCO monitoring

Author

Santisteban, J. V. Hernandez, Edelson, R., Horne, K., Gelbord, J. M., Barth, A. J., Cackett, E. M., Goad, M. R., Netzer, H., Starkey, D., Uttley, P., Brandt, W. N., Korista, K., Lohfink, A. M., Onken, C. A., Page, K. L., Siegel, M., Vestergaard, M., Bisogni, S., Breeveld, A. A., Cenko, S. B., Dalla Bonta, E., Evans, P. A., Ferland, G., Gonzalez-Buitrago, D. H., Grupe, D., Joner, M. D., Kriss, G., LaPorte, S. J., Mathur, S., Marshall, F., Mehdipour, M., Mudd, D., Peterson, B. M., Schmidt, T., Vaughan, S., Valenti, S., Santisteban, J. V. Hernandez, Edelson, R., Horne, K., Gelbord, J. M., Barth, A. J., Cackett, E. M., Goad, M. R., Netzer, H., Starkey, D., Uttley, P., Brandt, W. N., Korista, K., Lohfink, A. M., Onken, C. A., Page, K. L., Siegel, M., Vestergaard, M., Bisogni, S., Breeveld, A. A., Cenko, S. B., Dalla Bonta, E., Evans, P. A., Ferland, G., Gonzalez-Buitrago, D. H., Grupe, D., Joner, M. D., Kriss, G., LaPorte, S. J., Mathur, S., Marshall, F., Mehdipour, M., Mudd, D., Peterson, B. M., Schmidt, T., Vaughan, S., and Valenti, S.

Abstract

We present results of time-series analysis of the first year of the Fairall 9 intensive disc-reverberation campaign. We used Swift and the Las Cumbres Observatory global telescope network to continuously monitor Fairall 9 from X-rays to near-infrared at a daily to subdaily cadence. The cross-correlation function between bands provides evidence for a lag spectrum consistent with the tau proportional to lambda(4/3) scaling expected for an optically thick, geometrically thin blackbody accretion disc. Decomposing the flux into constant and variable components, the variable component's spectral energy distribution is slightly steeper than the standard accretion disc prediction. We find evidence at the Balmer edge in both the lag and flux spectra for an additional bound-free continuum contribution that may arise from reprocessing in the broad-line region. The inferred driving light curve suggests two distinct components, a rapidly variable (100 d) component with an opposite lag to the reverberation signal.

Published
2020

155. Interstellar oxygen along the line of sight of Cygnus X-2

Author

Sub Inorganic Chemistry and Catalysis, Inorganic Chemistry and Catalysis, Psaradaki, I., Costantini, E., Mehdipour, M., Rogantini, D., De Vries, C. P., De Groot, F., Mutschke, H., Trasobares, S., Waters, L. B.F.M., Zeegers, S. T., Sub Inorganic Chemistry and Catalysis, Inorganic Chemistry and Catalysis, Psaradaki, I., Costantini, E., Mehdipour, M., Rogantini, D., De Vries, C. P., De Groot, F., Mutschke, H., Trasobares, S., Waters, L. B.F.M., and Zeegers, S. T.

Published
2020

159. Interstellar oxygen along the line of sight of Cygnus X-2

Author

Psaradaki, I., primary, Costantini, E., additional, Mehdipour, M., additional, Rogantini, D., additional, de Vries, C. P., additional, de Groot, F., additional, Mutschke, H., additional, Trasobares, S., additional, Waters, L. B. F. M., additional, and Zeegers, S. T., additional

Published
2020
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160. Intensive disc-reverberation mapping of Fairall 9: first year of Swift and LCO monitoring

Author

Hernández Santisteban, J V, primary, Edelson, R, additional, Horne, K, additional, Gelbord, J M, additional, Barth, A J, additional, Cackett, E M, additional, Goad, M R, additional, Netzer, H, additional, Starkey, D, additional, Uttley, P, additional, Brandt, W N, additional, Korista, K, additional, Lohfink, A M, additional, Onken, C A, additional, Page, K L, additional, Siegel, M, additional, Vestergaard, M, additional, Bisogni, S, additional, Breeveld, A A, additional, Cenko, S B, additional, Dalla Bontà, E, additional, Evans, P A, additional, Ferland, G, additional, Gonzalez-Buitrago, D H, additional, Grupe, D, additional, Joner, M D, additional, Kriss, G, additional, LaPorte, S J, additional, Mathur, S, additional, Marshall, F, additional, Mehdipour, M, additional, Mudd, D, additional, Peterson, B M, additional, Schmidt, T, additional, Vaughan, S, additional, and Valenti, S, additional

Published
2020
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162. Space Telescope and Optical Reverberation Mapping Project. XI. Disk-wind Characteristics and Contributions to the Very Broad Emission Lines of NGC 5548

Author

Dehghanian, M., primary, Ferland, G. J., additional, Kriss, G. A., additional, Peterson, B. M., additional, Korista, K. T., additional, Goad, M. R., additional, Chatzikos, M., additional, Guzmán, F., additional, Rosa, G. De, additional, Mehdipour, M., additional, Kaastra, J., additional, Mathur, S., additional, Vestergaard, M., additional, Proga, D., additional, Waters, T., additional, Bentz, M. C., additional, Bisogni, S., additional, Brandt, W. N., additional, Bontà, E. Dalla, additional, Fausnaugh, M. M., additional, Gelbord, J. M., additional, Horne, Keith, additional, McHardy, I. M., additional, Pogge, R. W., additional, and Starkey, D. A., additional

Published
2020
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164. Quasi-multipliers on Group Algebras Related to a Locally Compact Group.

Author

Mehdipour, M. J. and Moghimi, GH. R.

Abstract

In this paper, we first characterize quasi-multipliers of (M(G)0*)* and show that the Banach algebra of all quasi-multipliers of (M(G)0*)* is isometrically isomorphic to (M(G)0*)*. We also establish that quasi-multipliers of (M(G)0*)* are separately continuous. Then, we investigate the existence of weakly compact quasi-multipliers of (M(G)0*)*. Finally, we prove that the Banach algebra of quasimultipliers of (M(G)0*)* is commutative if and only if G is abelian and discrete. [ABSTRACT FROM AUTHOR]

Published
2022
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165. Multiwavelength campaign on Mrk 509

Author

Kriss, G. A., Arav, N., Edmonds, D., Ely, J., Kaastra, J. S., Bianchi, S., Cappi, M., Costantini, E., Ebrero, J., Mehdipour, M., Paltani, S., Petrucci, Pierre-Olivier, Ponti, G., Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), and Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])

Subjects
quasars: absorption lines, X-rays: galaxies, [SDU]Sciences of the Universe [physics], ultraviolet: galaxies, galaxies: nuclei, galaxies: Seyfert, galaxies: individual: Mrk 509
Abstract

International audience; Aims: To elucidate the location, physical conditions, mass outflow rate, and kinetic luminosity of the outflow from the active nucleus of the Seyfert 1 galaxy Mrk 509, we used coordinated UV and X-ray spectral observations in 2012 to follow up our lengthier campaign conducted in 2009. Methods: We observed Mrk 509 with the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST) on 2012-09-03 and 2012-10-11 coordinated with X-ray observations using the High Energy Transmission Grating on the Chandra X-ray Observatory. Our far-ultraviolet spectra used grating G140L on COS to cover wavelengths from 920-2000 Å at a resolving power of ∼2000, and gratings G130M and G160M to cover 1160-1750 Å at a resolving power of ∼15, 000. Results: We detect variability in the blueshifted UV absorption lines on timescales spanning 3-12 years. The inferred densities in the absorbing gas are greater than log n cm-3 ∼ 3. For ionization parameters ranging over log U = -1.5 to -0.2, we constrain the distances of the absorbers to be closer than 220 pc to the active nucleus. Conclusions: The impact on the host galaxy appears to be confined to the nuclear region. All COS and FUSE spectra used in the paper are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/623/A82

Published
2019

166. Advances in the Application of Magnetic Nanoparticles for Sensing

Author

Gloag, L, Mehdipour, M, Chen, D, Tilley, RD, Gooding, JJ, Gloag, L, Mehdipour, M, Chen, D, Tilley, RD, and Gooding, JJ

Abstract

Magnetic nanoparticles (MNPs) are of high significance in sensing as they provide viable solutions to the enduring challenges related to lower detection limits and nonspecific effects. The rapid expansion in the applications of MNPs creates a need to overview the current state of the field of MNPs for sensing applications. In this review, the trends and concepts in the literature are critically appraised in terms of the opportunities and limitations of MNPs used for the most advanced sensing applications. The latest progress in MNP sensor technologies is overviewed with a focus on MNP structures and properties, as well as the strategies of incorporating these MNPs into devices. By looking at recent synthetic advancements, and the key challenges that face nanoparticle-based sensors, this review aims to outline how to design, synthesize, and use MNPs to make the most effective and sensitive sensors.

Published
2019

167. Space Telescope and Optical Reverberation Mapping Project. X. Understanding the Absorption-line Holiday in NGC 5548

Author

Dehghanian, M., Ferland, G. J., Kriss, G. A., Peterson, B. M., Mathur, S., Mehdipour, M., Guzmán, F., Chatzikos, M., Van Hoof, P. A.M., Williams, R. J.R., Arav, N., Barth, A. J., Bentz, M. C., Bisogni, S., Brandt, W. N., Crenshaw, D. M., Bonta, E. Dalla, De Rosa, G., Fausnaugh, M. M., Gelbord, J. M., Goad, M. R., Gupta, A., Horne, Keith, Kaastra, J., Knigge, C., Korista, K. T., McHardy, I. M., Pogge, R. W., Starkey, D. A., Vestergaard, M., Dehghanian, M., Ferland, G. J., Kriss, G. A., Peterson, B. M., Mathur, S., Mehdipour, M., Guzmán, F., Chatzikos, M., Van Hoof, P. A.M., Williams, R. J.R., Arav, N., Barth, A. J., Bentz, M. C., Bisogni, S., Brandt, W. N., Crenshaw, D. M., Bonta, E. Dalla, De Rosa, G., Fausnaugh, M. M., Gelbord, J. M., Goad, M. R., Gupta, A., Horne, Keith, Kaastra, J., Knigge, C., Korista, K. T., McHardy, I. M., Pogge, R. W., Starkey, D. A., and Vestergaard, M.

Abstract

The Space Telescope and Optical Reverberation Mapping Project (AGN STORM) on NGC 5548 in 2014 is one of the most intensive multiwavelength AGN monitoring campaigns ever. For most of the campaign, the emission-line variations followed changes in the continuum with a time lag, as expected. However, the lines varied independently of the observed UV-optical continuum during a 60-70 day "holiday," suggesting that unobserved changes to the ionizing continuum were present. To understand this remarkable phenomenon and to obtain an independent assessment of the ionizing continuum variations, we study the intrinsic absorption lines present in NGC 5548. We identify a novel cycle that reproduces the absorption line variability and thus identify the physics that allows the holiday to occur. In this cycle, variations in this obscurer's line-of-sight covering factor modify the soft X-ray continuum, changing the ionization of helium. Ionizing radiation produced by recombining helium then affects the level of ionization of some ions seen by the Hubble Space Telescope. In particular, high-ionization species are affected by changes in the obscurer covering factor, which does not affect the optical or UV continuum, and thus appear as uncorrelated changes, a "holiday." It is likely that any other model that selectively changes the soft X-ray part of the continuum during the holiday can also explain the anomalous emission-line behavior observed.

Published
2019

168. Multiwavelength campaign on Mrk 509: XVI. Continued HST/COS monitoring of the far-ultraviolet spectrum

Author

Physics, Kriss, G. A., Arav, Nahum, Edmonds, Douglas, Ely, J. C., Kaastra, J. S., Bianchi, S., Cappi, M., Costantini, E., Ebrero, J., Mehdipour, M., Paltani, S., Petrucci, P. O., Ponti, G., Physics, Kriss, G. A., Arav, Nahum, Edmonds, Douglas, Ely, J. C., Kaastra, J. S., Bianchi, S., Cappi, M., Costantini, E., Ebrero, J., Mehdipour, M., Paltani, S., Petrucci, P. O., and Ponti, G.

Abstract

Aims. To elucidate the location, physical conditions, mass outflow rate, and kinetic luminosity of the outflow from the active nucleus of the Seyfert 1 galaxy Mrk 509, we used coordinated UV and X-ray spectral observations in 2012 to follow up our lengthier campaign conducted in 2009. Methods. We observed Mrk 509 with the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST) on 2012-09-03 and 2012-10-11 coordinated with X-ray observations using the High Energy Transmission Grating on the Chandra X-ray Observatory. Our far-ultraviolet spectra used grating G140L on COS to cover wavelengths from 920-2000 Å at a resolving power of ∼2000, and gratings G130M and G160M to cover 1160-1750 Å at a resolving power of ∼15, 000. Results. We detect variability in the blueshifted UV absorption lines on timescales spanning 3-12 years. The inferred densities in the absorbing gas are greater than log n cm -3 ∼ 3. For ionization parameters ranging over log U =-1.5 to-0.2, we constrain the distances of the absorbers to be closer than 220 pc to the active nucleus. Conclusions. The impact on the host galaxy appears to be confined to the nuclear region. © 2019 G. A. Kriss et al.

Published
2019

169. The First Swift Intensive AGN Accretion Disk Reverberation Mapping Survey

Author

Edelson, R., Gelbord, J., Cackett, E., Peterson, B. M., Horne, K., Barth, A. J., Starkey, D. A., Bentz, M., Brandt, W. N., Goad, M., Joner, M., Korista, K., Netzer, H., Page, K., Uttley, P., Vaughan, S., Breeveld, A., Cenko, S. B., Done, C., Evans, P., Fausnaugh, M., Ferland, G., Gonzalez-Buitrago, D., Gropp, J., Grupe, D., Kaastra, J., Kennea, J., Kriss, G., Mathur, S., Mehdipour, M., Mudd, D., Nousek, J., Schmidt, T., Vestergaard, M., Villforth, C., Edelson, R., Gelbord, J., Cackett, E., Peterson, B. M., Horne, K., Barth, A. J., Starkey, D. A., Bentz, M., Brandt, W. N., Goad, M., Joner, M., Korista, K., Netzer, H., Page, K., Uttley, P., Vaughan, S., Breeveld, A., Cenko, S. B., Done, C., Evans, P., Fausnaugh, M., Ferland, G., Gonzalez-Buitrago, D., Gropp, J., Grupe, D., Kaastra, J., Kennea, J., Kriss, G., Mathur, S., Mehdipour, M., Mudd, D., Nousek, J., Schmidt, T., Vestergaard, M., and Villforth, C.

Published
2019

170. Space Telescope and Optical Reverberation Mapping Project. X. Understanding the Absorption-line Holiday in NGC 5548

Author

Physics, Dehghanian, M., Ferland, G. J., Kriss, G. A., Peterson, B. M., Mathur, S., Mehdipour, M., Guzman, F., Chatzikos, M., van Hoof, P. A. M., Williams, R. J. R., Arav, Nahum, Barth, A. J., Bentz, M. C., Bisogni, S., Brandt, W. N., Crenshaw, D. M., Dalla Bonta, E., De Rosa, G., Fausnaugh, M. M., Gelbord, J. M., Goad, M. R., Gupta, A., Horne, Keith, Kaastra, J., Knigge, C., Korista, K. T., McHardy, I. M., Pogge, R. W., Starkey, D. A., Vestergaard, M., Physics, Dehghanian, M., Ferland, G. J., Kriss, G. A., Peterson, B. M., Mathur, S., Mehdipour, M., Guzman, F., Chatzikos, M., van Hoof, P. A. M., Williams, R. J. R., Arav, Nahum, Barth, A. J., Bentz, M. C., Bisogni, S., Brandt, W. N., Crenshaw, D. M., Dalla Bonta, E., De Rosa, G., Fausnaugh, M. M., Gelbord, J. M., Goad, M. R., Gupta, A., Horne, Keith, Kaastra, J., Knigge, C., Korista, K. T., McHardy, I. M., Pogge, R. W., Starkey, D. A., and Vestergaard, M.

Abstract

The Space Telescope and Optical Reverberation Mapping Project (AGN STORM) on NGC 5548 in 2014 is one of the most intensive multiwavelength AGN monitoring campaigns ever. For most of the campaign, the emission-line variations followed changes in the continuum with a time lag, as expected. However, the lines varied independently of the observed UV-optical continuum during a 60-70 day "holiday," suggesting that unobserved changes to the ionizing continuum were present. To understand this remarkable phenomenon and to obtain an independent assessment of the ionizing continuum variations, we study the intrinsic absorption lines present in NGC 5548. We identify a novel cycle that reproduces the absorption line variability and thus identify the physics that allows the holiday to occur. In this cycle, variations in this obscurer's line-of-sight covering factor modify the soft X-ray continuum, changing the ionization of helium Ionizing radiation produced by recombining helium then affects the level of ionization of some ions seen by the Hubble Space Telescope. In particular, high-ionization species are affected by changes in the obscurer covering factor, which does not affect the optical or UV continuum, and thus appear as uncorrelated changes, a "holiday." It is likely that any other model that selectively changes the soft X-ray part of the continuum during the holiday can also explain the anomalous emission-line behavior observed.

Published
2019

171. III. Spectral energy distribution and the AGN wind photoionisation modelling, plus detection of diffuse X-rays from the starburst with Chandra HETGS

Author

Mehdipour, M., Kaastra, J. S., Costantini, E., Behar, E., Kriss, G. A., Bianchi, S., Branduardi-Raymont, G., Cappi, M., Ebrero, J., Di Gesu, L., Kaspi, S., Mao, J., De Marco, B., Middei, R., Peretz, U., Petrucci, Pierre-Olivier, Ponti, G., Ursini, F., Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), and Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])

Subjects
X-rays: galaxies, [SDU]Sciences of the Universe [physics], galaxies: active, galaxies: individual: NGC 7469, galaxies: Seyfert, techniques: spectroscopic
Abstract

International audience; We investigate the physical structure of the active galactic nucleus (AGN) wind in the Seyfert-1 galaxy NGC 7469 through high-resolution X-ray spectroscopy with Chandra HETGS and photoionisation modelling. Contemporaneous data from Chandra, HST, and Swift are used to model the optical-UV-X-ray continuum and determine the spectral energy distribution (SED) at two epochs, 13 yr apart. For our investigation we use new observations taken in December 2015-January 2016, and historical ones taken in December 2002. We study the impact of a change in the SED shape, seen between the two epochs, on the photoionisation of the wind. The HETGS spectroscopy shows that the AGN wind in NGC 7469 consists of four ionisation components, with their outflow velocities ranging from - 400 to - 1800 km s-1. From our modelling we find that the change in the ionising continuum shape between the two epochs results in some variation in the ionisation state of the wind components. However, for the main ions detected in X-rays, the sum of their column densities over all components remains in practice unchanged. For two of the four components, which are found to be thermally unstable in both epochs, we obtain 2 < r < 31 pc and 12 < r < 29 pc using the cooling and recombination timescales. For the other two thermally stable components, we obtain r < 31 pc and r < 80 pc from the recombination timescale. The results of our photoionisation modelling and thermal stability analysis suggest that the absorber components in NGC 7469 are consistent with being a thermally driven wind from the AGN torus. Finally, from analysis of the zeroth-order ACIS/HETG data, we discover that the X-ray emission in the range 0.2-1 keV is spatially extended over 1.5-12''. This diffuse soft X-ray emission is explained by coronal emission from the nuclear starburst ring in NGC 7469. The star formation rate inferred from this diffuse soft X-ray emission is consistent with those found by far-infrared studies of NGC 7469. The tables of the reduced spectra are only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr (ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/615/A72

Published
2018

172. Multi-wavelength campaign on NCG 7469

Author

Middei, R., Bianchi, S., Cappi, M., Petrucci, Pierre-Olivier, Ursini, F., Arav, N., Behar, E., Branduardi-Raymont, G., Costantini, E., De Marco, B., Di Gesu, L., Ebrero, J., Kaastra, J., Kaspi, S., Kriss, G. A., Mao, J., Mehdipour, M., Paltani, S., Peretz, U., Ponti, G., Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), and Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])

Subjects
X-rays: galaxies, [SDU]Sciences of the Universe [physics], Astrophysics::High Energy Astrophysical Phenomena, quasars: general, galaxies: active, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies: Seyfert
Abstract

International audience; We conducted a multi-wavelength 6-month campaign to observe the Seyfert Galaxy NGC 7469, using the space-based observatories HST, Swift, XMM-Newton and NuSTAR. We report the results of the spectral analysis of the seven simultaneous XMM-Newton and NuSTAR observations. The source shows significant flux variability within each observation, but the average flux is less variable among the different pointings of our campaign. Our spectral analysis reveals a prominent narrow neutral Fe Kα emission line in all the spectra and weaker contributions from Fe Kβ, neutral Ni Kα, and ionized iron. We find no evidence for variability or relativistic effects acting on the emission lines, which indicates that they originate from distant material. In the joint analysis of XMM-Newton and NuSTAR data, a constant photon index is found (Γ = 1.78 ± 0.02) together with a high energy cut-off Ecut = 170-40+60 keV. Adopting a self-consistent Comptonization model, these values correspond to an average coronal electron temperature of kT = 45-12+15 keV and, assuming a spherical geometry, an optical depth τ = 2.6 ± 0.9. The reflection component is consistent with being constant and the reflection fraction is in the range R = 0.3-0.6. A prominent soft excess dominates the spectra below 4 keV. This is best fit with a second Comptonization component, arising from a warm corona with an average kT = 0.67 ± 0.03 keV and a corresponding optical depth τ = 9.2 ± 0.2.

Published
2018

173. Anatomy of the AGN in NGC 5548

Author

Mao, Junjie, Kaastra, J. S., Mehdipour, M., Gu, Liyi, Costantini, E., Kriss, G. A., Bianchi, S., Branduardi-Raymont, G., Behar, E., Di Gesu, L., Ponti, G., Petrucci, Pierre-Olivier, Ebrero, J., Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), and Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])

Subjects
X-rays: galaxies, [SDU]Sciences of the Universe [physics], Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, galaxies: individual: NGC 5548, galaxies: Seyfert, techniques: spectroscopic
Abstract

International audience; The X-ray narrow emission line region (NELR) of the archetypal Seyfert 1 galaxy NGC 5548 has been interpreted as a single-phase photoionized plasma that is absorbed by some of the warm absorber components. This scenario requires those overlaying warm absorber components to have larger distance (to the central engine) than the X-ray NELR, which is not fully consistent with the distance estimates found in the literature. Therefore, we reanalyze the high-resolution spectra obtained in 2013-2014 with the Reflection Grating Spectrometer (RGS) aboard XMM-Newton to provide an alternative interpretation of the X-ray narrow emission features. We find that the X-ray narrow emission features in NGC 5548 can be described by a two-phase photoionized plasma with different ionization parameters (logξ = 1.3 and 0.1) and kinematics (vout = -50 and -400 km s-1), and no further absorption by the warm absorber components. The X-ray and optical NELR might be the same multi-phase photoionized plasma. Both X-ray and optical NELR have comparable distances, asymmetric line profiles, and the underlying photoionized plasma is turbulent and compact in size. The X-ray NELR is not the counterpart of the UV/X-ray absorber outside the line of sight because their distances and kinematics are not consistent. In addition, X-ray broad emission features that we find in the spectrum can be accounted for by a third photoionized emission component. The RGS spectrum obtained in 2016 is analyzed as well, where the luminosity of most prominent emission lines (the O VII forbidden line and O VIII Lyα line) are the same (at a 1σ confidence level) as in 2013-2014.

Published
2018

174. Atmospheric gas dynamics in the Perseus cluster observed with Hitomi*

Author

Aharonia, F., Aharonian, F., Akamatsu, H., Akimoto, F., Allen, S. W., Angelini, L., Audard, M., Awaki, H., Axelsson, M., Bamba, A., Bautz, M. W., Blandford, R., Brenneman, L. W., Brown, G. V., Bulbul, E., Cackett, E. M., Canning, R. E. A., Chernyakova, M., Chiao, M. P., Coppi, P. S., Costantini, E., Plaa, J., Vries, C. P., Den Herder, J. -W, Done, C., Dotani, T., Ebisawa, K., Eckart, M. E., Enoto, T., Ezoe, Y., Fabian, A. C., Ferrigno, C., Foster, A. R., Fujimoto, R., Fukazawa, Y., Furuzawa, A., Galeazzi, M., Gallo, L. C., Gandhi, P., Giustini, M., Goldwurm, A., Gu, L., Guainazzi, M., Haba, Y., Hagino, K., Hamaguchi, K., Harrus, I. M., Hatsukade, I., Hayashi, K., Hayashi, T., Hayashida, K., Hiraga, J. S., Hornschemeier, A., Hoshino, A., Hughes, J. P., Ichinohe, Y., Iizuka, R., Inoue, H., Inoue, S., Inoue, Y., Ishida, M., Ishikawa, K., Ishisaki, Y., Iwai, M., Kaastra, J., Kallman, T., Kamae, T., Kataoka, J., Katsuda, S., Kawai, N., Kelley, R. L., Kilbourne, C. A., Kitaguchi, T., Kitamoto, S., Kitayama, T., Kohmura, T., Kokubun, M., Koyama, K., Koyama, S., Kretschmar, P., Krimm, H. A., Kubota, A., Kunieda, H., Laurent, P., Lee, S. -H, Leutenegger, M. A., Limousin, O., Loewenstein, M., Long, K. S., Lumb, D., Madejski, G., Maeda, Y., Maier, D., Makishima, K., Markevitch, M., Matsumoto, H., Kyoko Matsushita, Mccammon, D., Mcnamara, B. R., Mehdipour, M., Miller, E. D., Miller, J. M., Mineshige, S., Mitsuda, K., Mitsuishi, I., Miyazawa, T., Mizuno, T., Mori, H., Mori, K., Mukai, K., Murakami, H., Mushotzky, R. F., Nakagawa, T., Nakajima, H., Nakamori, T., Nakashima, S., Nakazawa, K., Nobukawa, K. K., Nobukawa, M., Noda, H., Odaka, H., Ohashi, T., Ohno, M., Okajima, T., Ota, N., Ozaki, M., Paerels, F., Paltani, S., Petre, R., Pinto, C., Porter, F. S., Pottschmidt, K., Reynolds, C. S., Safi-Harb, S., Saito, S., Sakai, K., Sasaki, T., Sato, G., Sato, K., Sato, R., Sawada, M., Schartel, N., Serlemtsos, P. J., Seta, H., Shidatsu, M., Simionescu, A., Smith, R. K., Soong, Y., Stawarz, Ł., Sugawara, Y., Sugita, S., Szymkowiak, A., Tajima, H., Takahashi, H., Takahashi, T., Takeda, S., Takei, Y., Amagawa, T. T., Tamura, T., Tanaka, K., Tanaka, T., Tanaka, Y., Tanaka, Y. T., Tashiro, M. S., Tawara, Y., Terada, Y., Erashima, Y. T., Tombesi, F., Tomida, H., Tsuboi, Y., Tsujimoto, M., Tsunemi, H., Tsuru, T. G., Uchida, H., Uchiyama, H., Uchiyama, Y., Ueda, S., Ueda, Y., Uno, S., Urry, C. M., Ursino, E., Wang, Q. H. S., Watanabe, S., Werner, N., Wilkins, D. R., Williams, B. J., Yamada, S., Yamaguchi, H., Yamaoka, K., Yamasaki, N. Y., Yamauchi, M., Yamauchi, S., Yaqoob, T., Yatsu, Y., Yonetoku, D., Zhuravleva, I., Zoghbi, A., AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), and Commissariat à l'énergie atomique et aux énergies alternatives ( CEA )

Subjects
galaxies: clusters: individual, galaxies: clusters: intracluster medium, Active galactic nucleus, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], individual (NGC 1275) [galaxies], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, galaxies: individual, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, clusters: individual (Perseus) [galaxies], 01 natural sciences, Intracluster medium, 0103 physical sciences, Emission spectrum, Brightest cluster galaxy, 010303 astronomy & astrophysics, STFC, Astrophysics::Galaxy Astrophysics, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Settore FIS/05, 010308 nuclear & particles physics, Velocity gradient, RCUK, Velocity dispersion, Astronomy and Astrophysics, Redshift, ST/J003697/2, clusters: intracluster medium [galaxies], Space and Planetary Science, X-rays: galaxies: clusters, Electron temperature, galaxies: clusters [X-rays], ST/L00075X/1, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

著者人数: Hitomi Collaboration 197名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 林, 佑; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子）, Number of authors: Hitomi Collaboration 197 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Hayashi, Tasuku; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 201710-31, 資料番号: SA1170334000

Published
2018

175. Atomic data and spectral modeling constraints from high-resolution X-ray observations of the Perseus cluster with Hitomi

Author

Hitomi, C, Aharonian, F, Akamatsu, H, Akimoto, F, Allen, Sw, Angelini, L, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, Mw, Blandford, R, Brenneman, Lw, Brown, Gv, Bulbul, E, Cackett, Em, Chernyakova, M, Chiao, Mp, Coppi, Ps, Costantini, E, de Plaa, J, de Vries, Cp, den Herder, J, Done, C, Dotani, T, Ebisawa, K, Eckart, Me, Enoto, T, Ezoe, Y, Fabian, Ac, Ferrigno, C, Foster, Ar, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, Lc, Gandhi, P, Giustini, M, Goldwurm, A, Liyi, G, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, Im, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hell, N, Hiraga, Js, Hornschemeier, A, Hoshino, A, Hughes, Jp, Ichinohe, Y, Iizuka, R, Inoue, H, Inoue, Y, Ishida, M, Ishikawa, K, Ishisaki, Y, Iwai, M, Kaastra, J, Kallman, T, Kamae, T, Kataoka, J, Katsuda, S, Kawai, N, Kelley, Rl, Kilbourne, Ca, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, K, Koyama, S, Kretschmar, P, Krimm, Ha, Kubota, A, Kunieda, H, Laurent, P, Lee, S, Leutenegger, Ma, Limousin, O, Loewenstein, M, Long, Ks, Lumb, D, Madejski, G, Maeda, Y, Maier, D, Makishima, K, Markevitch, M, Matsumoto, H, Matsushita, K, Mccammon, D, Mcnamara, Br, Mehdipour, M, Miller, Ed, Miller, Jm, Mineshige, S, Mitsuda, K, Mitsuishi, I, Miyazawa, T, Mizuno, T, Mori, H, Mori, K, Mukai, K, Murakami, H, Mushotzky, Rf, Nakagawa, T, Nakajima, H, Nakamori, T, Nakashima, S, Nakazawa, K, Nobukawa, Kk, Nobukawa, M, Noda, H, Odaka, H, Ohashi, T, Ohno, M, Okajima, T, Ota, N, Ozaki, M, Paerels, F, Paltani, S, Petre, R, Pinto, C, Porter, Fs, Pottschmidt, K, Reynolds, Cs, Safi-Harb, S, Saito, S, Sakai, K, Sasaki, T, Sato, G, Sato, K, Sato, R, Sawada, M, Schartel, N, Serlemtsos, Pj, Seta, H, Shidatsu, M, Simionescu, A, Smith, Rk, Soong, Y, Stawarz, Ł, Sugawara, Y, Sugita, S, Szymkowiak, A, Tajima, H, Takahashi, H, Takahashi, T, Takeda, S, Takei, Y, Tamagawa, T, Tamura, T, Tanaka, T, Tanaka, Y, Tanaka, Yt, Tashiro, Ms, Tawara, Y, Terada, Y, Terashima, Y, Tombesi, F, Tomida, H, Tsuboi, Y, Tsujimoto, M, Tsunemi, H, Tsuru, Tg, Uchida, H, Uchiyama, H, Uchiyama, Y, Ueda, S, Ueda, Y, Uno, S, Urry, Cm, Ursino, E, Watanabe, S, Werner, N, Wilkins, Dr, Williams, Bj, Yamada, S, Yamaguchi, H, Yamaoka, K, Yamasaki, Ny, Yamauchi, M, Yamauchi, S, Yaqoob, T, Yatsu, Y, Yonetoku, D, Zhuravleva, I, Zoghbi, A, Raassen, Ajj, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
FOS: Physical sciences, Astrophysics, X-rays: general, 01 natural sciences, Measure (mathematics), X-ray, nickel, benchmark, iron, Settore FIS/05 - Astronomia e Astrofisica, general [X-rays], excited state, 0103 physical sciences, data analysis [methods], Calibration, Emission spectrum, Sensitivity (control systems), cluster, dielectric, 010306 general physics, 010303 astronomy & astrophysics, Collisional excitation, plasma, instrumentation: spectrographs, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Resolution (electron density), temperature, resolution, Astronomy and Astrophysics, Plasma, calibration, sensitivity, methods: data analysis, recombination, 13. Climate action, Space and Planetary Science, spectral, data management, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, spectrographs [instrumentation]
Abstract

著者人数: Hitomi Collaboration 194名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子）, Number of authors: Hitomi Collaboration 194 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 2017-12-13, 資料番号: SA1170337000

Published
2018

176. Recurring obscuration in NGC 3783

Author

Kaastra, J.S., Mehdipour, M., Behar, E., Bianchi, S., Branduardi-Raymont, G., Brenneman, L., Cappi, M., Costantini, E., Marco, B. de, Gesu, L., Ebrero, J., Kriss, G.A., Mao, J., Peretz, U., Petrucci, P.-O., Ponti, G., and Walton, D.

Published
2018

177. Hitomi observations of the LMC SNR N 132 D: Highly redshifted X-ray emission from iron ejecta

Author

Aharonian, Hitomi, C, Felix, Akamatsu, H, Akimoto, F, Allen, Sw, Angelini, L, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, Mw, Blandford, R, Brenneman, Lw, Brown, Gv, Bulbul, E, Cackett, Em, Chernyakova, M, Chiao, Mp, Coppi, Ps, Costantini, E, de Plaa, J, de Vries, Cp, den Herder, J, Done, C, Dotani, T, Ebisawa, K, Eckart, Me, Enoto, T, Ezoe, Y, Fabian, Ac, Ferrigno, C, Foster, Ar, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, Lc, Gandhi, P, Giustini, M, Goldwurm, A, Liyi, G, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, Im, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hiraga, Js, Hornschemeier, A, Hoshino, A, Hughes, Jp, Ichinohe, Y, Iizuka, R, Inoue, H, Inoue, Y, Ishida, M, Ishikawa, K, Ishisaki, Y, Iwai, M, Kaastra, J, Kallman, T, Kamae, T, Kataoka, J, Katsuda, S, Kawai, N, Kelley, Rl, Kilbourne, Ca, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, K, Koyama, S, Kretschmar, P, Krimm, Ha, Kubota, A, Kunieda, H, Laurent, P, Lee, S, Leutenegger, Ma, Limousin, O, Loewenstein, M, Long, Ks, Lumb, D, Madejski, G, Maeda, Y, Maier, D, Makishima, K, Markevitch, M, Matsumoto, H, Matsushita, K, Mccammon, D, Mcnamara, Br, Mehdipour, M, Miller, Ed, Miller, Jm, Mineshige, S, Mitsuda, K, Mitsuishi, I, Miyazawa, T, Mizuno, T, Mori, H, Mori, K, Mukai, K, Murakami, H, Mushotzky, Rf, Nakagawa, T, Nakajima, H, Nakamori, T, Nakashima, S, Nakazawa, K, Nobukawa, Kk, Nobukawa, M, Noda, H, Odaka, H, Ohashi, T, Ohno, M, Okajima, T, Ota, N, Ozaki, M, Paerels, F, Paltani, S, Petre, R, Pinto, C, Porter, Fs, Pottschmidt, K, Reynolds, Cs, Safi-Harb, S, Saito, S, Sakai, K, Sasaki, T, Sato, G, Sato, K, Sato, R, Sato, T, Sawada, M, Schartel, N, Serlemtsos, Pj, Seta, H, Shidatsu, M, Simionescu, A, Smith, Rk, Soong, Y, Stawarz, Ł, Sugawara, Y, Sugita, S, Szymkowiak, A, Tajima, H, Takahashi, H, Takahashi, T, Takeda, S, Takei, Y, Tamagawa, T, Tamura, T, Tanaka, T, Tanaka, Y, Tanaka, Yt, Tashiro, Ms, Tawara, Y, Terada, Y, Terashima, Y, Tombesi, F, Tomida, H, Tsuboi, Y, Tsujimoto, M, Tsunemi, H, Tsuru, Tg, Uchida, H, Uchiyama, H, Uchiyama, Y, Ueda, S, Ueda, Y, Uno, S, Urry, Cm, Ursino, E, Watanabe, S, Werner, N, Wilkins, Dr, Williams, Bj, Yamada, S, Yamaguchi, H, Yamaoka, K, Yamasaki, Ny, Yamauchi, M, Yamauchi, S, Yaqoob, T, Yatsu, Y, Yonetoku, D, Zhuravleva, I, Zoghbi, A, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], observational [methods], FOS: Physical sciences, Astrophysics, 01 natural sciences, individual objects (N 132 D) [ISM], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Spectral resolution, 010306 general physics, Large Magellanic Cloud, Ejecta, Supernova remnant, 010303 astronomy & astrophysics, Line (formation), ISM: supernova remnants, instrumentation: spectrographs, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), supernova remnants [ISM], individual (N 132 D) [X-rays], Astronomy and Astrophysics, X-rays: individual (N 132 D), Redshift, Interstellar medium, Supernova, ISM: individual object (N 132 D), 13. Climate action, Space and Planetary Science, methods: observational, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], spectrographs [instrumentation]
Abstract

著者人数: Hitomi Collaboration 193名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 田中, 靖郎; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子）, Number of authors: Hitomi Collaboration 193 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tanaka, Yasuo; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 2017-12-06, 資料番号: SA1170341000

Published
2018

178. Hitomi X-ray studies of giant radio pulses from the Crab pulsar

Author

Aharonian, Hitomi, C, Felix, Akamatsu, H, Akimoto, F, Allen, Sw, Angelini, L, Audard, M, Awaki, H, Axelsson, M, Bamba, A, Bautz, Mw, Blandford, R, Brenneman, Lw, Brown, Gv, Bulbul, E, Cackett, Em, Chernyakova, M, Chiao, Mp, Coppi, Ps, Costantini, E, de Plaa, J, de Vries, Cp, den Herder, J, Done, C, Dotani, T, Ebisawa, K, Eckart, Me, Enoto, T, Ezoe, Y, Fabian, Ac, Ferrigno, C, Foster, Ar, Fujimoto, R, Fukazawa, Y, Furuzawa, A, Galeazzi, M, Gallo, Lc, Gandhi, P, Giustini, M, Goldwurm, A, Liyi, G, Guainazzi, M, Haba, Y, Hagino, K, Hamaguchi, K, Harrus, Im, Hatsukade, I, Hayashi, K, Hayashi, T, Hayashida, K, Hiraga, Js, Hornschemeier, A, Hoshino, A, Hughes, Jp, Ichinohe, Y, Iizuka, R, Inoue, H, Inoue, Y, Ishida, M, Ishikawa, K, Ishisaki, Y, Iwai, M, Kaastra, J, Kallman, T, Kamae, T, Kataoka, J, Katsuda, S, Kawai, N, Kelley, Rl, Kilbourne, Ca, Kitaguchi, T, Kitamoto, S, Kitayama, T, Kohmura, T, Kokubun, M, Koyama, K, Koyama, S, Kretschmar, P, Krimm, Ha, Kubota, A, Kunieda, H, Laurent, P, Lee, S, Leutenegger, Ma, Limousin, Oo, Loewenstein, M, Long, Ks, Lumb, D, Madejski, G, Maeda, Y, Maier, D, Makishima, K, Markevitch, M, Matsumoto, H, Matsushita, K, Mccammon, D, Mcnamara, Br, Mehdipour, M, Miller, Ed, Miller, Jm, Mineshige, S, Mitsuda, K, Mitsuishi, I, Miyazawa, T, Mizuno, T, Mori, H, Mori, K, Mukai, K, Murakami, H, Mushotzky, Rf, Nakagawa, T, Nakajima, H, Nakamori, T, Nakashima, S, Nakazawa, K, Nobukawa, Kk, Nobukawa, M, Noda, H, Odaka, H, Ohashi, T, Ohno, M, Okajima, T, Oshimizu, K, Ota, N, Ozaki, M, Paerels, F, Paltani, S, Petre, R, Pinto, C, Porter, Fs, Pottschmidt, K, Reynolds, Cs, Safi-Harb, S, Saito, S, Sakai, K, Sasaki, T, Sato, G, Sato, K, Sato, R, Sawada, M, Schartel, N, Serlemtsos, Pj, Seta, H, Shidatsu, M, Simionescu, A, Smith, Rk, Soong, Y, Stawarz, Ł, Sugawara, Y, Sugita, S, Szymkowiak, A, Tajima, H, Takahashi, H, Takahashi, T, Takeda, S, Takei, Y, Tamagawa, T, Tamura, T, Tanaka, T, Tanaka, Y, Tanaka, Yt, Tashiro, Ms, Tawara, Y, Terada, Y, Terashima, Y, Tombesi, F, Tomida, H, Tsuboi, Y, Tsujimoto, M, Tsunemi, H, Tsuru, Tg, Uchida, H, Uchiyama, H, Uchiyama, Y, Ueda, S, Ueda, Y, Uno, S, Urry, Cm, Ursino, E, Watanabe, S, Werner, N, Wilkins, Dr, Williams, Bj, Yamada, S, Yamaguchi, H, Yamaoka, K, Yamasaki, Ny, Yamauchi, M, Yamauchi, S, Yaqoob, T, Yatsu, Y, Yonetoku, D, Zhuravleva, I, Zoghbi, A, Terasawa, T, Sekido, M, Takefuji, K, Kawai, E, Misawa, H, Tsuchiya, F, Yamazaki, R, Kobayashi, E, Kisaka, S, Aoki, T, AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Hitomi, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Magnetosphere, X-rays: stars, Astrophysics, 01 natural sciences, Article, Radio observatory, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, pulsars: individual (B0531+21), 010306 general physics, 010303 astronomy & astrophysics, stars [radio continuum], stars [X-rays], High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Crab Pulsar, X-ray, Astronomy and Astrophysics, Pulse (physics), Space and Planetary Science, individual (B0531+21) [pulsars], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], radio continuum: stars, Phase width
Abstract

著者人数: Hitomi Collaboration 203名（所属. 宇宙航空研究開発機構宇宙科学研究所(JAXA)(ISAS): 堂谷, 忠靖; 海老沢, 研; 萩野, 浩一; 林, 克洋; 飯塚, 亮; 井上, 芳幸; 石田, 学; 石川, 久美; 岩井, 将親; 国分, 紀秀; 小山, 志勇; 前田, 良知; 満田, 和久; 中川, 貴雄; 尾崎, 正伸; 佐藤, 悟郎; 佐藤, 理江; Simionescu, Aurora; 菅原, 泰晴; 高橋, 忠幸; 竹井, 洋; 田村, 隆幸; 冨田, 洋; 辻本, 匡弘; 上田, 周太朗; 渡辺, 伸; 山崎, 典子）, Number of authors: Hitomi Collaboration 203 (Affiliation. Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency (JAXA)(ISAS): Dotani, Tadayasu; Ebisawa, Ken; Hagino, Kouichi; Hayashi, Katsuhiro; Iizuka, Ryo; Inoue, Yoshiyuki; Ishida, Manabu; Ishikawa, Kumi; Iwai, Masachika; Kokubun, Motohide; Koyama, Shu; Maeda, Yoshitomo; Mitsuda, Kazuhisa; Nakagawa, Takao; Ozaki, Masanobu; Sato, Goro; Sato, Rie; Simionescu, Aurora; Sugawara, Yasuharu; Takahashi, Tadayuki; Takei, Yoh; Tamura, Takayuki; Tomida, Hiroshi; Tsujimoto, Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Masahiro; Ueda, Shutaro; Watanabe, Shin; Yamasaki, Noriko Y.), Accepted: 2017-07-27, 資料番号: SA1170340000

Published
2018

179. Interstellar dust along the line of sight of GX 3+1

Author

Rogantini, D., primary, Costantini, E., additional, Zeegers, S. T., additional, de Vries, C. P., additional, Mehdipour, M., additional, de Groot, F., additional, Mutschke, H., additional, Psaradaki, I., additional, and Waters, L. B. F. M., additional

Published
2019
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180. A Wind-based Unification Model for NGC 5548: Spectral Holidays, Nondisk Emission, and Implications for Changing-look Quasars

Author

Dehghanian, M., primary, Ferland, G. J., additional, Peterson, B. M., additional, Kriss, G. A., additional, Korista, K. T., additional, Chatzikos, M., additional, Guzmán, F., additional, Arav, N., additional, De Rosa, G., additional, Goad, M. R., additional, Mehdipour, M., additional, and van Hoof, P. A. M., additional

Published
2019
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182. Space Telescope and Optical Reverberation Mapping Project. X. Understanding the Absorption-line Holiday in NGC 5548

Author

Dehghanian, M., primary, Ferland, G. J., additional, Kriss, G. A., additional, Peterson, B. M., additional, Mathur, S., additional, Mehdipour, M., additional, Guzmán, F., additional, Chatzikos, M., additional, van Hoof, P. A. M., additional, Williams, R. J. R., additional, Arav, N., additional, Barth, A. J., additional, Bentz, M. C., additional, Bisogni, S., additional, Brandt, W. N., additional, Crenshaw, D. M., additional, Bontà, E. Dalla, additional, De Rosa, G., additional, Fausnaugh, M. M., additional, Gelbord, J. M., additional, Goad, M. R., additional, Gupta, A., additional, Horne, Keith, additional, Kaastra, J., additional, Knigge, C., additional, Korista, K. T., additional, McHardy, I. M., additional, Pogge, R. W., additional, Starkey, D. A., additional, and Vestergaard, M., additional

Published
2019
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183. The First Swift Intensive AGN Accretion Disk Reverberation Mapping Survey

Author

Edelson, R., primary, Gelbord, J., additional, Cackett, E., additional, Peterson, B. M., additional, Horne, K., additional, Barth, A. J., additional, Starkey, D. A., additional, Bentz, M., additional, Brandt, W. N., additional, Goad, M., additional, Joner, M., additional, Korista, K., additional, Netzer, H., additional, Page, K., additional, Uttley, P., additional, Vaughan, S., additional, Breeveld, A., additional, Cenko, S. B., additional, Done, C., additional, Evans, P., additional, Fausnaugh, M., additional, Ferland, G., additional, Gonzalez-Buitrago, D., additional, Gropp, J., additional, Grupe, D., additional, Kaastra, J., additional, Kennea, J., additional, Kriss, G., additional, Mathur, S., additional, Mehdipour, M., additional, Mudd, D., additional, Nousek, J., additional, Schmidt, T., additional, Vestergaard, M., additional, and Villforth, C., additional

Published
2019
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184. Photoionized emission and absorption features in the high-resolution X-ray spectra of NGC 3783

Author

Mao, Junjie, primary, Mehdipour, M., additional, Kaastra, J. S., additional, Costantini, E., additional, Pinto, C., additional, Branduardi-Raymont, G., additional, Behar, E., additional, Peretz, U., additional, Bianchi, S., additional, Kriss, G. A., additional, Ponti, G., additional, De Marco, B., additional, Petrucci, P.-O., additional, Di Gesu, L., additional, Middei, R., additional, Ebrero, J., additional, and Arav, N., additional

Published
2019
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185. HST/COS observations of the newly discovered obscuring outflow in NGC 3783

Author

Kriss, G. A., primary, Mehdipour, M., additional, Kaastra, J. S., additional, Rau, A., additional, Bodensteiner, J., additional, Plesha, R., additional, Arav, N., additional, Behar, E., additional, Bianchi, S., additional, Branduardi-Raymont, G., additional, Cappi, M., additional, Costantini, E., additional, De Marco, B., additional, Di Gesu, L., additional, Ebrero, J., additional, Kaspi, S., additional, Mao, J., additional, Middei, R., additional, Miller, T., additional, Paltani, S., additional, Peretz, U., additional, Peterson, B. M., additional, Petrucci, P.-O., additional, Ponti, G., additional, Ursini, F., additional, Walton, D. J., additional, and Xu, X., additional

Published
2018
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187. Recurring obscuration in NGC 3783

Author

Kaastra, J. S., primary, Mehdipour, M., additional, Behar, E., additional, Bianchi, S., additional, Branduardi-Raymont, G., additional, Brenneman, L., additional, Cappi, M., additional, Costantini, E., additional, De Marco, B., additional, di Gesu, L., additional, Ebrero, J., additional, Kriss, G. A., additional, Mao, J., additional, Peretz, U., additional, Petrucci, P.-O., additional, Ponti, G., additional, and Walton, D., additional

Published
2018
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188. XIPE: the x-ray imaging polarimetry explorer

Author

Soffitta, P., Bellazzini, R., Bozzo, E., Burwitz, V., Castro Tirado, A. J., Costa, E., Courvoisier, T., Feng, H., Gburek, S., Goosmann, R., Karas, V., Boettcher, M., Bogdanov, S., Bombaci, I., Bonino, R., Braga, J., Brandt, W., Brez, A., Bucciantini, N., Burderi, L., Caiazzo, I., Matt, G., Campana, R., Campana, S., Capitanio, F., Cappi, M., Cardillo, M., Casella, P., Catmabacak, O., Cenko, B., Cerda Duran, P., Cerruti, C., Muleri, F., Chaty, S., Chauvin, M., Chen, Y., Chenevez, J., Chernyakova, M., Cheung Teddy, C. C., Christodoulou, D., Connell, P., Corbet, R., Coti Zelati, F., Nandra, K., Covino, S., Cui, W., Cusumano, G., D'Ai, A., D'Ammando, F., Dadina, M., Dai, Z., De Rosa, A., De Ruvo, L., Degenaar, N., Pearce, M., Del Santo, M., Del Zanna, L., Dewangan, G., Di Cosimo, S., Di Lalla, N., Di Persio, G., Di Salvo, T., Dias, T., Done, C., Dovciak, M., Poutanen, J., Doyle, G., Ducci, L., Elsner, R., Enoto, T., Escada, J., Esposito, P., Eyles, C., Fabiani, S., Falanga, M., Falocco, S., Reglero, V., Fan, Y., Fender, R., Feroci, M., Ferrigno, C., Forman, W., Foschini, L., Fragile, C., Fuerst, F., Fujita, Y., Gasent Blesa, J. L., Sabau Maria, D., Gelfand, J., Gendre, B., Ghirlanda, G., Ghisellini, G., Giroletti, M., Goetz, D., Gogus, E., Gomez, J. L., Gonzalez, D., Gonzalez Riestra, R., Santangelo, A., Gotthelf, E., Gou, L., Grandi, P., Grinberg, V., Grise, F., Guidorzi, C., Gurlebeck, N., Guver, T., Haggard, D., Hardcastle, M., Tagliaferri, G., Hartmann, D., Haswell, C., Heger, A., Hernanz, M., Heyl, J., Ho, L., Hoormann, J., Horak, J., Huovelin, J., Huppenkothen, D., Tenzer, C., Iaria, R., Inam Sitki, C., Ingram, A., Israel, G., Izzo, L., Burgess, M., Jackson, M., Ji, L., Jiang, J., Vink, J., Johannsen, T., Jones, C., Jorstad, S., Kajava, J. J. E., Kalamkar, M., Kalemci, E., Kallman, T., Kamble, A., Kislat, F., Kiss, M., Weisskopf, M. C., Klochkov, D., Koerding, E., Kolehmainen, M., Koljonen, K., Komossa, S., Kong, A., Korpela, S., Kowalinski, M., Krawczynski, H., Kreykenbohm, I., Zane, S., Kuss, M., Lai, D., Lan, M., Larsson, J., Laycock, S., Lazzati, D., Leahy, D., Li, H., Li, J., L. X., Li, Agudo, I., Li, T., Li, Z., Linares, M., Lister, M., Liu, H., Lodato, G., Lohfink, A., Longo, F., Luna, G., Lutovinov, A., Antonelli, A., Mahmoodifar, S., Maia, J., Mainieri, V., Maitra, C., Maitra, D., Majczyna, A., Maldera, S., Malyshev, D., Manfreda, A., Manousakis, A., Attina, P., Manuel, R., Margutti, R., Marinucci, A., Markoff, S., Marscher, A., Marshall, H., Massaro, F., Mclaughlin, M., Medina Tanco, G., Mehdipour, M., Baldini, L., Middleton, M., Mignani, R., Mimica, P., Mineo, T., Mingo, B., Miniutti, G., Mirac, S. M., Morlino, G., Motlagh, A. V., Motta, S. E., Bykov, A., Mushtukov, A., Nagataki, S., Nardini, F., Nattila, J., Navarro, G. J., Negri, B., Negro, M., Nenonen, S., Neustroev, V., Nicastro, F., Carpentiero, R., Norton, A., Nucita, A., O'Brien, P., O'Dell, S., Odaka, H., Olmi, B., Omodei, N., Orienti, M., Orlandini, M., Osborne, J., Cavazzuti, E., Pacciani, L., Paliya, V. 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E., Kalamkar, M., Kalemci, E., Kallman, T., Kamble, A., Kislat, F., Kiss, M., Klochkov, D., Koerding, E., Kolehmainen, M., Koljonen, K., Komossa, S., Kong, A., Korpela, S., Kowalinski, M., Krawczynski, H., Kreykenbohm, I., Kuss, M., Lai, D., Lan, M., Larsson, J., Laycock, S., Lazzati, D., Leahy, D., Li, H., Li, J., Li, L. -X., Li, T., Li, Z., Linares, M., Lister, M., Liu, H., Lodato, G., Lohfink, A., Longo, F., Luna, G., Lutovinov, A., Mahmoodifar, S., Maia, J., Mainieri, V., Maitra, C., Maitra, D., Majczyna, A., Maldera, S., Malyshev, D., Manfreda, A., Manousakis, A., Manuel, R., Margutti, R., Marinucci, A., Markoff, S., Marscher, A., Marshall, H., Massaro, F., Mclaughlin, M., Medina-Tanco, G., Mehdipour, M., Middleton, M., Mignani, R., Mimica, P., Mineo, T., Mingo, B., Miniutti, G., Mirac, S. M., Morlino, G., Motlagh, A. V., Motta, S. E., Mushtukov, A., Nagataki, S., Nardini, F., Nattila, J., Navarro, G. 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S., Schwope, A., Severgnini, P., Sharon, M., Shaw, A., Shearer, A., Shesheng, X., Shih, I. -C., Silva, K., Silva, R., Silver, E., Smale, A., Spada, F., Spandre, G., Stamerra, A., Stappers, B., Starrfield, S., Stawarz, L., Stergioulas, N., Stevens, A., Stiele, H., Suleimanov, V., Sunyaev, R., Slowikowska, A., Tamborra, F., Tavecchio, F., Taverna, R., Tiengo, A., Tolos, L., Tombesi, F., Tomsick, J., Tong, H., Torok, G., Torres, D. F., Tortosa, A., Tramacere, A., Trimble, V., Trinchieri, G., Tsygankov, S., Tuerler, M., Turriziani, S., Ursini, F., Uttley, P., Varniere, P., Vincent, F., Vurgun, E., Wang, C., Wang, Z., Watts, A., Wheeler, J. C., Wiersema, K., Wijnands, R., Wilms, J., Wolter, A., Wood, K., Wu, K., Wu, X., Xiangyu, W., Xie, F., Xu, R., Yan, S. -P., Yang, J., Yu, W., Yuan, F., Zajczyk, A., Zanetti, D., Zanin, R., Zanni, C., Zappacosta, L., Zdziarski, A. A., Zech, A., Zhang, H., Zhang, S., Zhang, W., Zoghbi, A., Jan-Willem A. den Herder, Tadayuki Takahashi, Marshall Bautz, Castro-Tirado, A., Weisskopf, M., Lumb, D., Ness, J., Petrucci, P., Pinazo, H., Akbar, A., Atteia, J., Cheung Teddy, C., Gasent-Blesa, J., Gomez, J., Kajava, J., Li, L., Mirac, S., Motlagh, A., Motta, S., Navarro, G., Paliya, V., Pili, A., Rossi, M., Schulz, N., Shih, I., Torres, D., Wheeler, J., Yan, S., and Zdziarski, A.

Subjects
X-ray Astronomy, High-energy astronomy, Polarimetry, X-ray optics, X-ray telescope, Condensed Matter Physic, 01 natural sciences, Observatory, 0103 physical sciences, Electronic, Optical and Magnetic Materials, Spectral resolution, Electrical and Electronic Engineering, 010303 astronomy & astrophysics, Gas Pixel Detector, Physics, X-ray astronomy, ta115, 010308 nuclear & particles physics, Electronic, Optical and Magnetic Material, Applied Mathematics, Vega, Astronomy, Computer Science Applications1707 Computer Vision and Pattern Recognition, Condensed Matter Physics, Computer Science Applications, Applied Mathematic, Electronic, Optical and Magnetic Materials, Computer Vision and Pattern Recognition, X-ray optic
Abstract

XIPE, the X-ray Imaging Polarimetry Explorer, is a mission dedicated to X-ray Astronomy. At the time of writing XIPE is in a competitive phase A as fourth medium size mission of ESA (M4). It promises to reopen the polarimetry window in high energy Astrophysics after more than 4 decades thanks to a detector that efficiently exploits the photoelectric effect and to X-ray optics with large effective area. XIPE uniqueness is time-spectrally-spatially- resolved X-ray polarimetry as a breakthrough in high energy astrophysics and fundamental physics. Indeed the payload consists of three Gas Pixel Detectors at the focus of three X-ray optics with a total effective area larger than one XMM mirror but with a low weight. The payload is compatible with the fairing of the Vega launcher. XIPE is designed as an observatory for X-ray astronomers with 75 % of the time dedicated to a Guest Observer competitive program and it is organized as a consortium across Europe with main contributions from Italy, Germany, Spain, United Kingdom, Poland, Sweden.

Published
2016

189. Space Telescope and Optical Reverberation Mapping Project. X. Understanding the Absorption-Line Holiday in NGC 5548

Author

Dehghanian, M., Ferland, G. J., Kriss, G. A., Peterson, B. M., Mathur, S., Mehdipour, M., Guzman, F., Chatzikos, M., Van Hoof, P. A. M., Williams, R. J. R., Arav, N., Barth, A. J., Bentz, M. C., Bisogni, S., Brandt, W. N., Crenshaw, D. M., Bonta, E. Dalla, De Rosa, G., Fausnaugh, M. M., Gelbord, J. M., Goad, M. R., Gupta, A., Horne, Keith, Kaastra, J., Knigge, C., Korista, K. T., Hardy, I. M. Mc, Pogge, R. W., Starkey, D. A., Vestergaard, M., Dehghanian, M., Ferland, G. J., Kriss, G. A., Peterson, B. M., Mathur, S., Mehdipour, M., Guzman, F., Chatzikos, M., Van Hoof, P. A. M., Williams, R. J. R., Arav, N., Barth, A. J., Bentz, M. C., Bisogni, S., Brandt, W. N., Crenshaw, D. M., Bonta, E. Dalla, De Rosa, G., Fausnaugh, M. M., Gelbord, J. M., Goad, M. R., Gupta, A., Horne, Keith, Kaastra, J., Knigge, C., Korista, K. T., Hardy, I. M. Mc, Pogge, R. W., Starkey, D. A., and Vestergaard, M.

Abstract

The flux variations in the emission lines in active galactic nuclei (AGNs) are driven by variations in the ionizing continuum flux --which are usually reflected in the observable UV-optical continuum. The "Reverberation mapping" technique measures the delay between line and continuum variations to determine the size of the line emitting region, this is the basis for measurements of the central black hole mass in AGNs. The Space Telescope and Optical Reverberation Mapping Project (AGN STORM) on NGC 5548 in 2014 is the most intensive multi-wavelength AGN monitoring campaign ever. For most of the campaign, the emission-line variations followed changes in the continuum with a time lag, as expected. However, the lines varied independently of the observed UV-optical continuum during a 60 -- 70 day "holiday." To understand this remarkable phenomenon, we study the intrinsic absorption lines present in NGC 5548. We identify a novel cycle that reproduces the absorption line variability and thus identify the physics that allows the holiday to occur. In our model, variations in this obscurer's line-of-sight covering factor modify the soft X-ray continuum. This leads to changes in the ionization of helium gas in the broad-line region. Ionizing radiation produced by recombining helium then affects the ionization of other species as observed during the AGN STORM holiday. It is likely that any other model which selectively changes the soft X-ray part of the continuum during the holiday can also explain the anomalous emission line behavior observed., Comment: This is the version accepted by ApJ. Will be published shortly

Published
2018
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190. Photoionized emission and absorption features in the high-resolution X-ray spectra of NGC 3783

Author

Mao, Junjie, Mehdipour, M., Kaastra, J. S., Costantini, E., Pinto, C., Branduardi-Raymont, G., Behar, E., Peretz, U., Bianchi, S., Kriss, G. A., Ponti, G., De Marco, B., Petrucci, P. -O., Di Gesu, L., Middei, R., Ebrero, J., Arav, N., Mao, Junjie, Mehdipour, M., Kaastra, J. S., Costantini, E., Pinto, C., Branduardi-Raymont, G., Behar, E., Peretz, U., Bianchi, S., Kriss, G. A., Ponti, G., De Marco, B., Petrucci, P. -O., Di Gesu, L., Middei, R., Ebrero, J., and Arav, N.

Abstract

Our Swift monitoring program triggered two joint XMM-Newton, NuSTAR and HST observations on 11 and 21 December 2016 targeting NGC 3783, as its soft X-ray continuum was heavily obscured. Consequently, emission features, including the O VII radiative recombination continuum, stand out above the diminished continuum. We focus on the photoionized emission features in the December 2016 RGS spectra and compare them to the time-averaged RGS spectrum obtained in 2000--2001 when the continuum was unobscured. A two-phase photoionized plasma is required to account for the narrow emission features. These narrow emission features are weakly varying between 2000--2001 and December 2016. We also find a statistically significant broad emission component in the time-averaged RGS spectrum in 2000--2001. This broad emission component is significantly weaker in December 2016, suggesting that the obscurer is farther away than the X-ray broad-line region. In addition, by analyzing the archival high-resolution X-ray spectra, we find that nine photoionized absorption components with different ionization parameters and kinematics are required for the warm absorber in X-rays., Comment: accepted to A&A

Published
2018
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191. The First Swift Intensive AGN Accretion Disk Reverberation Mapping Survey

Author

Edelson, R., Gelbord, J., Cackett, E., Peterson, B. M., Horne, K., Barth, A. J., Starkey, D. A., Bentz, M., Brandt, W. N., Goad, M., Joner, M., Korista, K., Netzer, H., Page, K., Uttley, P., Vaughan, S., Breeveld, A., Cenko, S. B., Done, C., Evans, P., Fausnaugh, M., Ferland, G., Gonzalez-Buitrago, D., Gropp, J., Grupe, D., Kaastra, J., Kennea, J., Kriss, G., Mathur, S., Mehdipour, M., Mudd, D., Nousek, J., Schmidt, T., Vestergaard, M., Villforth, C., Edelson, R., Gelbord, J., Cackett, E., Peterson, B. M., Horne, K., Barth, A. J., Starkey, D. A., Bentz, M., Brandt, W. N., Goad, M., Joner, M., Korista, K., Netzer, H., Page, K., Uttley, P., Vaughan, S., Breeveld, A., Cenko, S. B., Done, C., Evans, P., Fausnaugh, M., Ferland, G., Gonzalez-Buitrago, D., Gropp, J., Grupe, D., Kaastra, J., Kennea, J., Kriss, G., Mathur, S., Mehdipour, M., Mudd, D., Nousek, J., Schmidt, T., Vestergaard, M., and Villforth, C.

Abstract

Swift intensive accretion disk reverberation mapping of four AGN yielded light curves sampled $\sim$200-350 times in 0.3-10 keV X-ray and six UV/optical bands. Uniform reduction and cross-correlation analysis of these datasets yields three main results: 1) The X-ray/UV correlations are much weaker than those within the UV/optical, posing severe problems for the lamp-post reprocessing model in which variations in a central X-ray corona drive and power those in the surrounding accretion disk. 2) The UV/optical interband lags are generally consistent with $ \tau \propto \lambda^{4/3} $ as predicted by the centrally illuminated thin accretion disk model. While the average interband lags are somewhat larger than predicted, these results alone are not inconsistent with the thin disk model given the large systematic uncertainties involved. 3) The one exception is the U band lags, which are on average a factor of $\sim$2.2 larger than predicted from the surrounding band data and fits. This excess appears due to diffuse continuum emission from the broad-line region (BLR). The precise mixing of disk and BLR components cannot be determined from these data alone. The lags in different AGN appear to scale with mass or luminosity. We also find that there are systematic differences between the uncertainties derived by javelin vs. more standard lag measurement techniques, with javelin reporting smaller uncertainties by a factor of 2.5 on average. In order to be conservative only standard techniques were used in the analyses reported herein., Comment: 25 pages, 9 tables, 6 figures, published in ApJ. The paper has been revised to conform to the published version. Please note that the data (Table 2) are available at the Digital Repository at the University of Maryland, https://drum.lib.umd.edu/handle/1903/21536

Published
2018
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192. HST/COS observations of the newly discovered obscuring outflow in NGC 3783

Author

Kriss, G. A., Mehdipour, M., Kaastra, J. S., Rau, A., Bodensteiner, J., Plesha, R., Arav, N., Behar, E., Bianchi, S., Branduardi-Raymont, G., Cappi, M., Costantini, E., De Marco, B., Di Gesu, L., Ebrero, J., Kaspi, S., Mao, J., Middei, R., Miller, T., Paltani, S., Peretz, U., Peterson, B. M., Petrucci, P. -O., Ponti, G., Ursini, F., Walton, D. J., Xu, X., Kriss, G. A., Mehdipour, M., Kaastra, J. S., Rau, A., Bodensteiner, J., Plesha, R., Arav, N., Behar, E., Bianchi, S., Branduardi-Raymont, G., Cappi, M., Costantini, E., De Marco, B., Di Gesu, L., Ebrero, J., Kaspi, S., Mao, J., Middei, R., Miller, T., Paltani, S., Peretz, U., Peterson, B. M., Petrucci, P. -O., Ponti, G., Ursini, F., Walton, D. J., and Xu, X.

Abstract

To understand the nature of transient obscuring outflows in active galactic nuclei, we observed the Seyfert 1 galaxy NGC 3783 on two occasions in December 2016 triggered by Swift monitoring indicating strong soft X-ray absorption in November. We obtained ultraviolet spectra using COS on HST and optical spectra using FEROS on the MPG/ESO 2.2-m telescope that were simultaneous with X-ray spectra from XMM-Newton and NuSTAR. We find new components of broad, blue-shifted absorption associated with Ly$\alpha$, \ion{N}{v}, \ion{Si}{iv}, and \ion{C}{iv} in our COS spectra. The absorption extends from velocities near zero in the rest-frame of the host galaxy to $-6200$ $\rm km~s^{-1}$. These features appear for the first time in NGC 3783 at the same time as the heavy soft X-ray absorption seen in the XMM-Newton X-ray spectra. The X-ray absorption has a column density of $\sim 10^{23}~\rm cm^{-2}$, and it partially covers the X-ray continuum source. The X-ray absorption becomes more transparent in the second observation, as does the UV absorption. Combining the X-ray column densities with the UV spectral observations yields an ionization parameter for the obscuring gas of log $\xi =1.84^{+0.4}_{-0.2}$ $\rm erg~cm~s^{-1}$. Despite the high intensity of the UV continuum in NGC 3783, F(1470 \AA)=$8 \times 10^{-14}~\rm erg~cm^{-2}~s^{-1}~\AA^{-1}$, the well known narrow UV absorption lines are deeper than in earlier observations in unobscured states, and low ionization species such as \ion{C}{iii} appear, indicating that the narrow-line gas is more distant from the nucleus and is being shadowed by the gas producing the obscuration. Despite the high continuum flux levels in our observations of NGC 3783, moderate velocities in the UV broad line profiles have substantially diminished. We suggest that a collapse of the broad line region has led to the outburst and triggered the obscuring event., Comment: 24 pages, 29 figures, uses aa.cls. Accepted for publication in A&A, 10/29/2018

Published
2018
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193. Recurring obscuration in NGC 3783

Author

Kaastra, J. S., Mehdipour, M., Behar, E., Bianchi, S., Branduardi-Raymont, G., Brenneman, L., Cappi, M., Costantini, E., De Marco, B., di Gesu, L., Ebrero, J., Kriss, G. A., Mao, J., Peretz, U., Petrucci, P. -O., Ponti, G., Walton, D., Kaastra, J. S., Mehdipour, M., Behar, E., Bianchi, S., Branduardi-Raymont, G., Brenneman, L., Cappi, M., Costantini, E., De Marco, B., di Gesu, L., Ebrero, J., Kriss, G. A., Mao, J., Peretz, U., Petrucci, P. -O., Ponti, G., and Walton, D.

Abstract

Obscuration of the continuum emission from active galactic nuclei by streams of gas with relatively high velocity (> 1000 km/s) and column density (>3E25 per m2) has been seen in a few Seyfert galaxies. This obscuration has a transient nature. In December 2016 we have witnessed such an event in NGC 3783. The frequency and duration of these obscuration events is poorly known. Here we study archival data of NGC 3783 in order to constrain this duty cycle. We use archival Chandra/NuSTAR spectra taken in August 2016. We also study the hardness ratio of all Swift XRT spectra taken between 2008-2017. In August 2016, NGC 3783 also showed evidence for obscuration. While the column density of the obscuring material is ten times lower than in December 2016, the opacity is still sufficient to block a significant fraction of the ionising X-ray and EUV photons. From the Swift hardness ratio behaviour we find several other epochs with obscuration. Obscuration with columns >1E26 per m2 may take place in about half of the time. Also in archival X-ray data taken by ASCA in 1993 and 1996 we find evidence for obscuration. Obscuration of the ionising photons in NGC 3783 occurs more frequently than previously thought. This may not always have been recognised due to low spectral resolution observations, too limited spectral bandwidth or confusion with underlying continuum variations., Comment: 9 pages, 7 figures, submitted to Astronomy and Astrophysics

Published
2018
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194. Multi-wavelength campaign on NGC 7469 IV. The broad-band X-ray spectrum

Author

Middei, R., Bianchi, S., Cappi, M., Petrucci, P-O., Ursini, F., Arav, N., Behar, E., Branduardi-Raymont, G., Costantini, E., De Marco, B., Di Gesu, L., Ebrero, J., Kaastra, J., Kaspi, S., Kriss, G. A., Mao, J., Mehdipour, M., Paltani, S., Peretz, U., Ponti, G., Middei, R., Bianchi, S., Cappi, M., Petrucci, P-O., Ursini, F., Arav, N., Behar, E., Branduardi-Raymont, G., Costantini, E., De Marco, B., Di Gesu, L., Ebrero, J., Kaastra, J., Kaspi, S., Kriss, G. A., Mao, J., Mehdipour, M., Paltani, S., Peretz, U., and Ponti, G.

Abstract

We conducted a multi-wavelength six-month campaign to observe the Seyfert galaxy NGC~7469, using the space-based observatories \textit{HST}, \textit{Swift}, \textit{XMM-Newton} and \textit{NuSTAR}. Here we report the results of the spectral analysis of the 7 simultaneous \textit{XMM-Newton} and \textit{NuSTAR} observations. The sources shows significant flux variability within each observation, but the average flux is less variable among the different pointings of our campaign. Our spectral analysis reveals a prominent narrow neutral \ion{Fe} K$\alpha$ emission line in all the spectra, with weaker contributions from Fe K$\beta$, neutral Ni K$\alpha$ and ionised iron. We find no evidence for variability or relativistic effects acting on the emission lines, which indicates that they originate from distant material. Analysing jointly \textit{XMM-Newton} and \textit{NuSTAR} data a constant photon index is found ($\Gamma$=$1.78\pm0.02$), together with a high energy cut-off $E_{\rm{cut}}=170^{+60}_{-40}$ keV. Adopting a self-consistent Comptonization model, these values correspond to an average coronal electron temperature of kT=$45^{+15}_{-12}$ keV and, assuming a spherical geometry, an optical depth $\tau=2.6\pm0.9$. The reflection component is consistent with being constant, with a reflection fraction in the range $R=0.3-0.6$. A prominent soft excess dominates the spectra below 4 keV. This is best fit with a second Comptonization component, arising from a \virg{warm corona} with an average $kT=0.67\pm0.03$ keV and a corresponding optical depth $\tau=9.2\pm0.2$., Comment: 11 pages, 5 figures, accepted by A&A

Published
2018

195. Multi-wavelength campaign on NGC 7469: III. Spectral energy distribution and the AGN wind photoionisation modelling, plus detection of diffuse X-rays from the starburst with Chandra HETGS

Author

Mehdipour, M., Kaastra, J. S., Costantini, E., Behar, E., Kriss, G. A., Bianchi, S., Branduardi-Raymont, G., Cappi, M., Ebrero, J., Di Gesu, L., Kaspi, S., Mao, J., De Marco, B., Middei, R., Peretz, U., Petrucci, P. -O., Ponti, G., Ursini, F., Mehdipour, M., Kaastra, J. S., Costantini, E., Behar, E., Kriss, G. A., Bianchi, S., Branduardi-Raymont, G., Cappi, M., Ebrero, J., Di Gesu, L., Kaspi, S., Mao, J., De Marco, B., Middei, R., Peretz, U., Petrucci, P. -O., Ponti, G., and Ursini, F.

Abstract

We investigate the physical structure of the AGN wind in the Seyfert-1 galaxy NGC 7469 through high-resolution X-ray spectroscopy with Chandra HETGS and photoionisation modelling. Contemporaneous data from Chandra, HST, and Swift are used to model the optical-UV-X-ray continuum and determine the spectral energy distribution (SED) at two epochs, 13 years apart. For our investigation we use new observations taken in December 2015-January 2016, and historical ones taken in December 2002. We study the impact of a change in the SED shape, seen between the two epochs, on the photoionisation of the wind. The HETGS spectroscopy shows that the AGN wind in NGC 7469 consists of four ionisation components, with their outflow velocities ranging from -400 to -1800 km/s. From our modelling we find that the change in the ionising continuum shape between the two epochs results in some variation in the ionisation state of the wind components. However, for the main ions detected in X-rays, the sum of their column densities over all four components, remains in practice unchanged. For two of the four components, which are found to be thermally unstable in both epochs, we obtain 2 < r < 31 pc and 12 < r < 29 pc using the cooling and recombination timescales. For the other two thermally stable components, we obtain r < 31 pc and r < 80 pc from the recombination timescale. The results of our photoionisation modelling and thermal stability analysis suggest that the absorber components in NGC 7469 are consistent with being a thermally-driven wind from the AGN torus. Finally, from analysis of the zeroth-order ACIS/HETG data, we discover that the X-ray emission between 0.2-1 keV is spatially extended over 1.5-12". This diffuse soft X-ray emission is explained by coronal emission from the nuclear starburst ring in NGC 7469., Comment: Accepted for publication in Astronomy & Astrophysics (A&A), 14 pages, 12 figures

Published
2018
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196. Reduced data for the Swift Intensive Accretion Disk Reverberation Mapping Survey

Author

Edelson, R, Edelson, R, Gelbord, J., Cackett, E., Peterson, B. M., Horne, K., Barth, A. J., Starkey, D. A., Bentz, M., Brandt, W. N., Goad, M., Joner, M., Korista, K., Netzer, H., Page, K., Uttley, P., Vaughan, S., Breeveld, A., Cenko, S. B., Done, C., Evans, P., Fausnaugh, M., Ferland, G., Gonzalez-Buitrago, D., Gropp, J., Grupe, D., Kaastra, J., Kennea, J., Kriss, G., Mathur, S., Mehdipour, M., Nousek, J., Schmidt, T., Vestergaard, M., Villforth, C., Edelson, R, Edelson, R, Gelbord, J., Cackett, E., Peterson, B. M., Horne, K., Barth, A. J., Starkey, D. A., Bentz, M., Brandt, W. N., Goad, M., Joner, M., Korista, K., Netzer, H., Page, K., Uttley, P., Vaughan, S., Breeveld, A., Cenko, S. B., Done, C., Evans, P., Fausnaugh, M., Ferland, G., Gonzalez-Buitrago, D., Gropp, J., Grupe, D., Kaastra, J., Kennea, J., Kriss, G., Mathur, S., Mehdipour, M., Nousek, J., Schmidt, T., Vestergaard, M., and Villforth, C.

Abstract

Since 2014, the Niel Gehrels Swift observatory has conducted a series of intensive accretion disk reverberation mapping (IDRM) campaigns of bright AGN. This archive contains reduced data from the first four of these campaigns. We are making the data publicly available to facilitate uniform modeling and analysis of these data. Please feel free to download and use the data as you wish. This table will be updated as more IDRM campaigns are published and as the data reduction (mostly dropout filtering) improves. If these data result in publications, please cite the source paper: "The First Swift Intensive AGN Accretion Disk Reverberation Mapping Survey" by Edelson et al. (2019 ApJ 870 123; available at http://iopscience.iop.org/article/10.3847/1538-4357/aaf3b4/meta). Also please note: © AAS. Reproduced with permission. TABLE NOTES: Column 1: Object name. Column 2: Filter/band used to measure the data point. Column 3: Cadence number, where the most significant digit refers to the object and the next three refer to the visit number for that object. Column 4: Modified Julian Day at the midpoint of the exposure. Column 5: Duration of the integration in that filter/band, in seconds. Column 6: Mean flux of the data point. UVOT fluxes are given in units of 10^-{14} erg/cm2/s/A and X-ray fluxes in units of ct/s. Column 7: Uncertainty on the flux, in the same units as Column 6.

Published
2018

197. Space Telescope and Optical Reverberation Mapping Project. XIII. An Atlas of UV and X-Ray Spectroscopic Signatures of the Disk Wind in NGC 5548.

Author

Dehghanian, M., Ferland, G. J., Peterson, B. M., Kriss, G. A., Korista, K. T., Goad, M. R., Chatzikos, M., Bentz, M. C., Guzmán, F., Mehdipour, M., and De Rosa, G.

Subjects
OPTICAL telescopes, SPACE telescopes, SPECTRAL lines, ATLASES, X-rays, SOUND reverberation, ACCRETION disks
Abstract

The unusual behavior of the spectral lines of NGC5548 during the STORM campaign demonstrated a missing piece in the structure of AGNs. For a two-month period in the middle of the campaign, the spectral lines showed a deficit in flux and a reduced response to the variations of the UV continuum. This was the first time that this behavior was unequivocally observed in an AGN. Our previous papers explained this as being due to a variable disk wind that acts as a shield and alters the SED. Here, we use Cloudy to create an atlas of photoionization models for a variety of disk winds, in order to study their effects on the SED. We show that the winds have three different cases: Case 1 winds are transparent, fully ionized, and have minimal effects on the intrinsic SED, although they can produce some line emission, especially He ii or FeKα. We propose that this is the situation in most of the AGNs. Case 2 winds, which have a He++–He+ ionization front, block part of the XUV continuum but transmit much of the Lyman continuum. They lead to the observed abnormal behavior. Case 3 winds have a H+ ionization front and block much of the Lyman continuum. The results show that the presence of these winds has important effects on the spectral lines of AGNs. They will thus have an effect on the measurements of the black hole mass and the geometry of the AGN. This atlas of spectral simulations can serve as a guide to future reverberation campaigns. [ABSTRACT FROM AUTHOR]

Published
2021
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198. Evaluation of Serum Nitric Oxide Level in Patients with Oral Lichen Planus

Author

Mehdipour, M., Taghavi Zenouz, A., Bahramian, A., Gholizadeh, N., and Boorghani, M.

Subjects
stomatognathic diseases, stomatognathic system, Oxidative stress, Original Article, Nitric oxide, Lichen planus
Abstract

Statement of Problem: Oral lichen planus (OLP) is a chronic inflammatory oral mucosal disease with indefinite etiology. In recent researches, free radicals have been deliberated as the possible etiology of inflammatory and autoimmune diseases. Purpose: This study was aimed to evaluate the stress oxidative status with the nitric oxide (NO) index in a sample of Iranian population. Materials and Method: In this descriptive-comparative study, serum NO level was assessed in 20 OLP patients as the case group and 20 healthy individuals as the control group. Collected data were analyzed by adopting two Sample t-test, using SPSS 16 software. The statistical significance level was set at p< 0.05. Results: The mean serum NO levels in OLP patients and healthy controls were 17.1±3.4 ng/ml and 14.5±2.7 ng/ml respectively; which revealed a significant statistical difference (p= 0.009). Conclusion: The results of the current study with its limitation may support the premise that higher serum levels of NO in patients with OLP might activate the process of lymphocytes and cellular immunity system; hence, possibly endorsing the effect of serum NO in pathogenesis of lichen planus.

Published
2014

199. Derivations on Banach algebras of connected multiplicative linear functionals

Author

Ghasemi, M. and Mehdipour, M. J.

Abstract

Let Aand Bbe Banach algebras with σ(B)≠∅. Let θ,ϕ,γ∈σ(B)and Der(A×θϕ,γB)be the set of all linear mappings d:A×B→A×Bsatisfying d((a,b)·θ(x,y))=d(a,b)·ϕ(x,y)+(a,b)·γd(x,y)for all a,x∈Aand b,y∈B. In this paper, we characterize elements of Der(A×θϕ,γB)in the case where Ahas a right identity. We then investigate the concept of centralizing for elements of Der(A×θϕ,γB)and determine dependent elements of Der(A×θϕ,γB). We also apply some results to group algebras.

Published
2021
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200. Thermal stability of winds driven by radiation pressure in super-Eddington accretion discs.

Author

Pinto, C, Mehdipour, M, Walton, D J, Middleton, M J, Roberts, T P, Fabian, A C, Guainazzi, M, Soria, R, Kosec, P, and Ness, J-U

Subjects
*RADIATION pressure, *X-ray binaries, *ACCRETION (Astrophysics), *EDDINGTON mass limit, *SPECTRAL energy distribution, *THERMAL stability, *ACTIVE galactic nuclei
Abstract

Ultraluminous X-ray sources (ULXs) are mainly powered by accretion in neutron stars or stellar-mass black holes. Accreting at rates exceeding the Eddington limit by factors of a few up to hundreds, radiation pressure is expected to inflate the accretion disc, and drive fast winds that have in fact been observed at significant fractions of the speed of light. Given the super-Eddington luminosity, the accretion disc will be thicker than in sub-Eddington accretors such as common active galactic nuclei and X-ray binaries, leading to a different spectral energy distribution and, possibly, a different thermal status of the wind. Here, we show the first attempt to calculate the photoionization balance of the winds driven by strong radiation pressure in thick discs with a focus on ULXs hosting black holes or non-magnetic neutron stars. We find that the winds are generally in thermally stable equilibrium, but long-term variations in the accretion rate and the inclination due to precession may have significant effects on the wind appearance and stability. Our model trends can explain the observed correlation between the spectral residuals around 1 keV and the ULX spectral state. We also find a possible correlation between the spectral hardness of the ULX, the wind velocity, and the ionization parameter in support of the general scenario. [ABSTRACT FROM AUTHOR]

Published
2020
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