111 results on '"Guainazzi, Matteo"'
Search Results
2. A systematic study of the ultra-fast outflow responses to luminosity variations in active galactic nuclei.
- Author
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Xu, Yerong, Pinto, Ciro, Rogantini, Daniele, Barret, Didier, Bianchi, Stefano, Guainazzi, Matteo, Ebrero, Jacobo, Alston, William, Kara, Erin, and Cusumano, Giancarlo
- Subjects
ACTIVE galactic nuclei ,SOFT X rays ,HARD X-rays ,SEYFERT galaxies ,UNIDENTIFIED flying objects - Abstract
Context. Ultra-fast outflows (UFOs) have been revealed in a large number of active galactic nuclei (AGN) in the past two decades. Their extreme velocities and high ionization states make them a promising candidate for AGN feedback on the evolution of the host galaxy. However, their exact underlying driving mechanism is not yet fully understood. Aims. Given that the variability of UFOs may be used to distinguish among different launching mechanisms, we aim to search for and characterize the responses of the UFO properties to the variable irradiating luminosity. Methods. We perform a high-resolution time- and flux-resolved spectroscopy of archival XMM-Newton observations on six highly accreting narrow-line Seyfert 1 (NLS1) galaxies, selected by UFO detection and sufficient exposure times. The state-of-the-art methods of the blind Gaussian line scan and photoionization model scan are used to identify UFO solutions. We search for ionized winds and investigate the structure of ionized winds and their responses to the luminosity variations. The location, density, and kinetic energy of UFOs are estimated as well. Results. The powerful photoionization model scan reveals three previously unreported UFOs in RE J1034+396, PG 1244+026 and I ZW 1 with a detection significance above 3σ, and two new warm absorbers (WAs) in RE J1034+396. Five out of six (83%) AGN in our sample host multi-phase ionized winds, where outflows in I ZW 1 are energy-conserved. The relatively low-ionization entrained UFOs are discovered in four (66%) AGN of our sample, supporting the shocked outflow interpretation for ionized winds in AGN. We notice that two out of seven (28%) UFOs in our sample seem to respond to the radiation field and three (43%) UFOs hint at a radiatively accelerated nature, requiring further observations. Combined with published works, we do not find any correlations between UFO responses and AGN properties except for a tentative (∼1.8σ) anti-correlation between the UFO acceleration and the Eddington ratio, to be confirmed by further observations and an enlarged sample. The kinetic energy of UFOs, mostly detected in soft X-rays, is found to have a large uncertainty. We, therefore, cannot conclude whether soft X-ray UFOs have sufficient energy to drive the AGN feedback, although they are very promising based on some reasonable assumptions. The primary UFO in I ZW 1 (detected in the hard X-ray) is the only case in our sample to possess conclusively sufficient energy to affect the host galaxy. [ABSTRACT FROM AUTHOR]
- Published
- 2024
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3. Ionized outflows from active galactic nuclei as the essential elements of feedback
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Laha, Sibasish, Reynolds, Christopher S., Reeves, James, Kriss, Gerard, Guainazzi, Matteo, Smith, Randall, Veilleux, Sylvain, and Proga, Daniel
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- 2021
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4. The quest for dual and binary supermassive black holes: A multi-messenger view
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De Rosa, Alessandra, Vignali, Cristian, Bogdanović, Tamara, Capelo, Pedro R., Charisi, Maria, Dotti, Massimo, Husemann, Bernd, Lusso, Elisabeta, Mayer, Lucio, Paragi, Zsolt, Runnoe, Jessie, Sesana, Alberto, Steinborn, Lisa, Bianchi, Stefano, Colpi, Monica, del Valle, Luciano, Frey, Sándor, Gabányi, Krisztina É., Giustini, Margherita, Guainazzi, Matteo, Haiman, Zoltan, Herrera Ruiz, Noelia, Herrero-Illana, Rubén, Iwasawa, Kazushi, Komossa, S., Lena, Davide, Loiseau, Nora, Perez-Torres, Miguel, Piconcelli, Enrico, and Volonteri, Marta
- Published
- 2019
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5. Selection of Compton-thick AGN from a hard photometric sample using XMM–Newton observations.
- Author
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Mostafa, Reham, Guainazzi, Matteo, and Ibrahim, Alaa
- Subjects
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MARKOV chain Monte Carlo , *ACTIVE galactic nuclei , *SEYFERT galaxies - Abstract
We present a selection technique to detect Compton-thick (CT) active galactic nuclei (AGNs) in the 3XMM/SDSS-DR7 cross-correlation. A subsample of 3481 X-ray sources that are detected in the hard band (2–8 keV) and have photometric redshifts constitute our parent sample. We first applied an automated spectral-fitting procedure to select highly absorbed sources (N H > 1023 cm−2). We found 184 highly absorbed candidates. Then, we performed the Bayesian Monte Carlo Markov chains (MCMCs) selection technique to find CT AGNs. We also tested the MCMC selection technique by applying Monte Carlo simulations. We found that the method is accurate at 90 per cent independently of the nature of the underlying source. Our sample contains 52 bona fide CT AGNs. The CT AGNs were selected to have a range >0.75 of probability of being CT when either fitting with the two models Torus and MYTorus. About 75 per cent of CT AGNs in our sample had probabilities >90 per cent. From the spectral analysis, we significantly found an anticorrelation between the equivalent width of the neutral Fe K α line and the X-ray luminosity at 2–10 keV, the so-called X-ray Baldwin effect. [ABSTRACT FROM AUTHOR]
- Published
- 2023
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6. Hydrodynamic simulations of the disc of gas around supermassive black holes (HDGAS) – I. Molecular gas dynamics.
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Raouf, Mojtaba, Viti, Serena, García-Burillo, S, Richings, Alexander J, Schaye, Joop, Bemis, Ashley, Nobels, Folkert S J, Guainazzi, Matteo, Huang, Ko-Yun, Schaller, Matthieu, Impellizzeri, Violette, and Holdship, Jon
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INTERSTELLAR medium ,MOLECULAR dynamics ,ACTIVE galactic nuclei ,WIND power ,GALACTIC evolution ,GAS dynamics ,SUPERMASSIVE black holes ,STAR formation - Abstract
We present hydrodynamic simulations of the interstellar medium (ISM) within the circumnuclear disc (CND) of a typical active galactic nucleus (AGN)-dominated galaxy influenced by mechanical feedback from an AGN. The simulations are coupled with the CHIMES non-equilibrium chemistry network to treat the radiative-cooling and AGN-heating. A focus is placed on the central 100 pc scale where AGN outflows are coupled to the ISM and constrained by observational Seyfert-2 galaxies. AGN-feedback models are implemented with different wind-velocity and mass-loading factors. We post-process the simulation snapshots with a radiative-transfer code to obtain the molecular emission lines. We find that the inclusion of an AGN promotes the formation of CO in clumpy and dense regions surrounding supermassive black holes (SMBHs). The CO(1-0) intensity maps (<6 Myr) in the CND seem to match well with observations of NGC 1068 with a best match for a model with 5000 km s
−1 wind-velocity and a high mass-loading factor. We attempt to discern between competing explanations for the apparent counter-rotating gas disc in the NGC 1068 through an analysis of kinematic maps of the CO line emission. We suggest that mechanical AGN-feedback could explain the alignment-stability of position-angle across the different CND radii around the SMBH through momentum and energy loading of the wind. It is the wind-velocity that drives the disc out of alignment on a 100 pc scale for a long period of time. The position–velocity diagrams are in broad agreement with the predicted Keplerian rotation-curve in the model without AGN, but the AGN models exhibit a larger degree of scatter, in better agreement with NGC 1068 observations. [ABSTRACT FROM AUTHOR]- Published
- 2023
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7. Constraints on the ultrafast outflows in the narrow-line Seyfert 1 galaxy Mrk 1044 from high-resolution time- and flux-resolved spectroscopy.
- Author
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Xu, Yerong, Pinto, Ciro, Rogantini, Daniele, Bianchi, Stefano, Guainazzi, Matteo, Kara, Erin, Jin, Chichuan, and Cusumano, Giancarlo
- Subjects
SEYFERT galaxies ,ACTIVE galactic nuclei ,TIME-resolved spectroscopy ,GALAXY spectra ,BLACK holes ,X-ray spectroscopy ,KINETIC energy ,GALACTIC evolution - Abstract
Ultrafast outflows (UFOs) have been revealed in a large number of active galactic nuclei (AGN) and are regarded as promising candidates for AGN feedback on the host galaxy. The nature and launching mechanism of UFOs are not yet fully understood. Here we perform a time- and flux-resolved X-ray spectroscopy on four XMM–Newton observations of a highly accreting narrow-line Seyfert 1 (NLS1) galaxy, Mrk 1044, to study the dependence of the outflow properties on the source luminosity. We find that the UFO in Mrk 1044 responds to the source variability quickly and its velocity increases with the X-ray flux, suggesting a high-density (|$10^{9}\!-\!4.5\times 10^{12}\, \mathrm{cm}^{-3}$|) and radiatively driven outflow, launched from the region within a distance of |$98\!-\!6600\, R_\mathrm{g}$| from the black hole. The kinetic energy of the UFO is conservatively estimated (|$L_\mathrm{UFO}\sim 4.4~{{\ \rm per\ cent}}\, L_\mathrm{Edd}$|), reaching the theoretical criterion to affect the evolution of the host galaxy. We also find that emission lines, from a large-scale region, have a blueshift of 2700–4500 km s
−1 in the spectra of Mrk 1044, which is rarely observed in AGN. By comparing with other sources, we propose a correlation between the blueshift of emission lines and the source accretion rate, which can be verified by a future sample study. [ABSTRACT FROM AUTHOR]- Published
- 2023
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8. Solar abundance ratios of the iron-peak elements in the Perseus cluster
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Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W., Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W., Blandford, Roger, Brenneman, Laura W., Brown, Gregory V., Bulbul, Esra, Cackett, Edward M., Chernyakova, Maria, Chiao, Meng P., Coppi, Paolo S., Costantini, Elisa, de Plaa, Jelle, den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E., Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C., Ferrigno, Carlo, Foster, Adam R., Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C., Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M., Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S., Hornschemeier, Ann, Hoshino, Akio, Hughes, John P., Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L., Kilbourne, Caroline A., Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A., Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A., Limousine, Olivier, Loewenstein, Michael, Long, Knox S., Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R., Mehdipour, Missagh, Miller, Eric D., Miller, Jon M., Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F., Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K., Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stéphane, Petre, Robert, Pinto, Ciro, Porter, Frederick S., Pottschmidt, Katja, Reynolds, Christopher S., Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemitsos, Peter J., Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K., Soong, Yang, Stawarz, Lukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shinʼichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T., Tashiro, Makoto S., Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Go Tsuru, Takeshi, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shinʼichiro, Urry, Megan C., Ursino, Eugenio, de Vries, Cor P., Watanabe, Shin, Werner, Norbert, Wik, Daniel R., Wilkins, Dan R., Williams, Brian J., Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y., Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, and Zoghbi, Abderahmen
- Published
- 2017
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9. Obscuring Environment and X-Ray Variability of Compact Symmetric Objects Unveiled with XMM-Newton and NuSTAR.
- Author
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Sobolewska, Małgosia, Siemiginowska, Aneta, Migliori, Giulia, Ostorero, Luisa, Stawarz, Łukasz, and Guainazzi, Matteo
- Subjects
SOFT X rays ,X-rays ,GAMMA ray bursts ,RADIO programs ,ACTINIC flux ,PLASMA temperature ,SUPERMASSIVE black holes - Abstract
Compact symmetric objects (CSOs) show radio features such as jets, lobes, and hot spots, which are contained within their host galaxies, and likely represent a recent radio activity. A subpopulation of CSOs with high intrinsic X-ray column densities has been inferred from shallow, soft X-ray band exposures, and observed to cluster in the linear radio size versus 5 GHz radio power plane, which suggests that a dense circumnuclear medium may dramatically influence the growth of compact radio structures. Here, we report on the first detection of two CSOs, 2021+614 and J1511+0518, at energies above 10 keV with NuSTAR. We model the NuSTAR data jointly with the new XMM-Newton data of J1511+0518, and with the archival XMM-Newton data of 2021+614. A toroidal reprocessor model fits the data well and allows us to robustly confirm the X-ray properties of the CSO absorbers and continuum. In both sources, we find intrinsic X-ray absorbing column densities in excess of 10
23 cm−2 , hard photon indices of the primary emission, Γ ∼ 1.4–1.7, Fe K α line emission, and variability of the intrinsic X-ray flux density on the timescale of years. The studied X-ray continua are dominated by the primary power-law emission at energies above 3 keV, and by the scattered component at energies below 3 keV. An additional soft X-ray component, modeled with a hot, collisionally ionized plasma with temperature kT ∼ 1 keV, is required by the XMM-Newton data in J1511+0518, which is corroborated by the tentative evidence for the extension in the archival Chandra image of the source. [ABSTRACT FROM AUTHOR]- Published
- 2023
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10. Temperature Structure in the Perseus Cluster Core Observed with Hitomi
- Author
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Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W, Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W, Blandford, Roger, Brenneman, Laura W, Brown, Gregory V, Bulbul, Esra, Cackett, Edward M, Chernyakova, Maria, Chiao, Meng P, Coppi, Paolo S, Costantini, Elisa, Plaa, Jelle De, Vries, Cor P. De, Den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E, Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C, Ferrigno, Carlo, Foster, Adam R, Fujimoto, Ryuichi, Fukazawa, Yasushi, Furukawa, Maki, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C, Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S, Hornschemeier, Ann, Hoshino, Akio, Hughes, John P, Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Iwai, Masachika, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Kato, Yuichi, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L, Kilbourne, Caroline A, Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A, Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A, Limousin, Olivier, Loewenstein, Michael, Long, Knox S, Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, Mccammon, Dan, Mcnamara, Brian R, Mehdipour, Missagh, Miller, Eric D, Miller, Jon M, Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F, Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K, Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Altani, Stephane P ´, Petre, Robert, Pinto, Ciro, Porter, Frederick S, Pottschmidt, Katja, Reynolds, Christopher S, Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J, Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K, Soong, Yang, Stawarz, Łukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin´Ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T, Tashiro, Makoto S, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shin´Ichiro, Urry, C. Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R, Williams, Brian J, Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamauchi, Noriko Y. Yamasaki 22. Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, and Zoghbi, Abderahmen
- Subjects
Astrophysics - Abstract
The present paper investigates the temperature structure of the X-ray emitting plasma in the core of the Perseus cluster using the 1.8-20.0 keV data obtained with the Soft X-ray Spectrometer (SXS) onboard the Hitomi Observatory. A series of four observations were carried out, with a total effective exposure time of 338 ks and covering a central region _ 7′ in diameter. The SXS was operated with an energy resolution of _5 eV (full width at half maximum) at 5.9 keV. Not only fine structures of K-shell lines in He-like ions but also transitions from higher principal quantum numbers are clearly resolved from Si through Fe. This enables us to perform temperature diagnostics using the line ratios of Si, S, Ar, Ca, and Fe, and to provide the first direct measurement of the excitation temperature and ionization temperature in the Perseus cluster. The observed spectrum is roughly reproduced by a single temperature thermal plasma model in collisional ionization equilibrium, but detailed line ratio diagnostics reveal slight deviations from this approximation. In particular, the data exhibit an apparent trend of increasing ionization temperature with increasing atomic mass, as well as small differences between the ionization and excitation temperatures for Fe, the only element for which both temperatures can be measured. The best-fit two-temperature models suggest a combination of 3 and 5 keV gas, which is consistent with the idea that the observed small deviations from a single temperature approximation are due to the effects of projection of the known radial temperature gradient in the cluster core along the line of sight. Comparison with the Chandra/ACIS and the XMM-Newton/RGS results on the other hand suggests that additional lower-temperature components
- Published
- 2018
- Full Text
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11. The origin of high-energy emission in the young radio source PKS 1718–49
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Sobolewska, Małgosia, Migliori, Giulia, Ostorero, Luisa, Siemiginowska, Aneta, Stawarz, Łukasz, Guainazzi, Matteo, and Hardcastle, Martin J.
- Subjects
radio lobes ,accretion ,X-ray active galactic nuclei ,non-thermal radiation sources ,radio jets ,galaxy evolution ,active galaxies ,gamma-rays ,extragalactic radio sources - Abstract
We present a model for the broadband radio-to-γ-ray spectral energy distribution of the compact radio source PKS 1718 − 649. Because of its young age ($\simeq$100 yr) and proximity (z = 0.014), PKS 1718 − 649 offers a unique opportunity to study the nuclear conditions and the jet/host galaxy feedback process at the time of the initial radio jet expansion. PKS 1718 − 649 is one of a handful of young radio jets with γ-ray emission that has been confirmed by the Fermi/LAT detector. We show that in PKS1718−649 this γ-ray emission can be successfully explained by Inverse Compton scattering of the UV photons, presumably from an accretion flow, off nonthermal electrons in the expanding radio lobes. The origin of the X-ray emission in PKS 1718 − 649 is more elusive. While Inverse Compton scattering of the IR photons emitted by a cold gas in the vicinity of the expanding radio lobes contributes significantly to the X-ray luminosity, the data require an additional source of X-rays, e.g., a weak X-ray corona or a radiatively inefficient accretion flow, as expected from a LINER-type nucleus, such as that of PKS 1718 − 649. We find that the jet in PKS 1718 − 649 has low power, L$_{j} \simeq$ 2 $\times$ 10$^{42}$ erg s$^{-1}$, and expands in an environment with density n$_{0} \simeq$ 3-20 cm$^{-3}$. The inferred mass accretion rate and gas mass reservoir within 50–100 pc of the galactic center are consistent with estimates from the literature obtained by tracing molecular gas in the innermost region of the host galaxy with SINFONI and the Atacama Large Millimeter/submillimeter Array.
- Published
- 2022
12. The X-ray view of optically selected dual AGN.
- Author
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De Rosa, Alessandra, Vignali, Cristian, Severgnini, Paola, Bianchi, Stefano, Bogdanović, Tamara, Charisi, Maria, Guainazzi, Matteo, Haiman, Zoltan, Komossa, S, Paragi, Zsolt, Perez-Torres, Miguel, Piconcelli, Enrico, Ducci, Lorenzo, Parvatikar, Manali, and Serafinelli, Roberto
- Subjects
ACTIVE galactic nuclei ,X-rays ,X-ray detection ,GALACTIC X-ray sources - Abstract
We present a study of optically selected dual Active Galactic Nuclei (AGN) with projected separations of 3–97 kpc. Using multiwavelength (MWL) information (optical, X-ray, mid-IR), we characterized the intrinsic nuclear properties of this sample and compared them with those of isolated systems. Among the 124 X-ray-detected AGN candidates, 52 appear in pairs and 72 as single X-ray sources. Through MWL analysis, we confirmed the presence of the AGN in >80 per cent of the detected targets in pairs (42 out of 52). X-ray spectral analysis confirms the trend of increasing AGN luminosity with decreasing separation, suggesting that mergers may have contributed to triggering more luminous AGN. Through X-ray/mid-IR ratio versus X-ray colours, we estimated a fraction of Compton-thin AGN (with 10
22 cm−2 < NH < 1024 cm−2 ) of about 80 per cent, while about 16 per cent are Compton-thick sources (with NH > 1024 cm−2 ). These fractions of obscured sources are larger than those found in samples of isolated AGN, confirming that pairs of AGN show higher obscuration. This trend is further confirmed by comparing the de-reddened [O iii ] emission with the observed X-ray luminosity. However, the derived fraction of Compton-thick sources in this sample at the early stages of merging is lower than that reported for late-merging dual-AGN samples. Comparing NH from X-rays with that derived from E (B − V) from narrow-line regions, we found that the absorbing material is likely to be associated with the torus or broad-line regions. We also explored the X-ray detection efficiency of dual-AGN candidates, finding that, when observed properly (at on-axis positions and with long exposures), X-ray data represent a powerful way to confirm and investigate dual-AGN systems. [ABSTRACT FROM AUTHOR]- Published
- 2023
- Full Text
- View/download PDF
13. Athena Charged Particle Diverter (CPD) scientific assessment: preliminary results on the WFI residual background
- Author
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FIORETTI, Valentina, MOLENDI, SILVANO, Zlamal, Jakub, Galgoczi, Gabor, Breuer, Jean-Paul, Werner, Norbert, MINEO, TERESA, LOTTI, Simone, Perinati, Emanuele, GUAINAZZI, MATTEO, Boudin, Nathalie, and Ferreira, Ivo
- Abstract
Soft protons deflected by the CPD can potentially be scattered at lower energy and still reach the detection plane. Proton scattering measurements with samples of the Athena CPD surface, WFI baffle, and other compositions with different levels of roughness are currently being finalized, together with the validation of proton scattering simulations, to study the impact of secondary proton scattering. Preliminary results indicate that protons are indeed scattered with the CPD surface, with a level of mean roughness > tens of nm, with an efficiency almost uniform in scattering angle and large energy losses (>90% at 100 keV). The presence of heavier elements increases the scattering efficiency, while the impact of the roughness is still under investigation. SRIM and Geant4 simulations modelling the surface roughness are currently ongoing, and preliminary SRIM simulations are in general consistent with the measured distributions, but discrepancies in the energy losses are still under study. Preliminary results on the WFI CPD simulation aimed to confirm its compliance with the residual background requirement and to estimate the impact of secondary proton scattering were obtained with a combined simulation of the Athena SPO and the proton interaction with the WFI optical filters and detection plane, assuming no roughness on the exposed surfaces. The statistical uncertainty of the present results, with few protons reaching the WFI, is not yet enough to perform a final CPD scientific assessment and characterization of the secondary proton scattering. We can however conclude with current SRIM simulations that the WFI residual background level), if the CPD is present, is well within the requirement of 5 ✕ 10-4 counts cm-2 s-1 keV-1 in the 2 - 7 keV energy range, with a maximum level of (3.4±2.0) ✕ 10-5 counts cm-2 s-1 keV-1 obtained with only the OBF filter. Most of the protons generating background counts scatter with the filter wheel structure as the last scattering interaction. Current results indicate that no corrective measures are required to minimise the secondary proton scattering or increase the CPD efficiency, but the adoption of vanes or coatings in the filter wheel structure could help reduce the secondary proton flux at the WFI.
- Published
- 2021
14. The excitation mechanisms of X-ray oxygen emission-lines
- Author
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Reynaldi, Victoria, Guainazzi, Matteo, Bianchi, Stefano, Andruchow, Ileana, García, Federico, López, Iván, Salerno, Nicolás, Storchi-Bergmann, T., Forman, W., Overzier, R., Riffel, R., and Astronomy
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Physics ,Active galactic nucleus ,010308 nuclear & particles physics ,Continuum (design consultancy) ,galaxies: active ,X-ray ,chemistry.chemical_element ,Astronomy and Astrophysics ,Astrophysics ,Plasma ,plasmas ,01 natural sciences ,Oxygen ,galaxies: Seyfert ,chemistry ,Space and Planetary Science ,0103 physical sciences ,High resolution spectra ,Emission spectrum ,line: formation ,010303 astronomy & astrophysics ,Excitation - Abstract
We present the Catalogue of High REsolution Spectra of Obscured Sources (CHRESOS) from the XMM-Newton Science Archive. It comprises soft X-ray emission-lines from C to Si and the Fe 3C and Fe 3G L-shell transitions. Here, we concentrate on the oxygen emission-lines O VII(f) and O VIII Lyα to shed light onto the physical processes with which their formation can be related to: active galactic nucleus vs. star-forming regions. We are analysing the relationships between the oxygen lines and the luminosities of: [OIII]λ5007, [OIV]25.89μm, MIR-12μm, FIR-60μm, FIR-100μm, and hard X-rays continuum bands.
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- 2021
15. General Relativity studies through X-ray spectroscopy of the Fe (and others) K α fluorescent lines
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Guainazzi, Matteo
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- 2009
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16. “The ESA XMM-Newton Science Operations Centre: Making Basic Space Science Available to the Whole Scientific World”
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Gabriel, Carlos, Guainazzi, Matteo, and Metcalfe, Leo
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- 2006
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17. The physics and astrophysics of X-ray outflows from Active Galactic Nuclei
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Laha, Sibasish, Smith, Randall, Tzanavaris, Panayiotis, Kallman, Tim, Veilleux, Sylvain, Tombesi, Francesco, Kriss, Gerard, GUAINAZZI, MATTEO, GASPARI, MASSIMO, Kaastra, Jelle, Markowitz, Alex, Crenshaw, Mike, Behar, Ehud, Fukumura, Keigo, Longinotti, Anna Lia, Rozanska, Agata, Ebrero, Jacobo, Ferland, Gary, Ricci, Claudio, Done, Chris, Proga, Daniel, Revalski, Mitchell, and Vayner, Andrey
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High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Astrophysics of Galaxies ,Astrophysics::Galaxy Astrophysics - Abstract
The highly energetic outflows from Active Galactic Nuclei detected in X-rays are one of the most powerful mechanisms by which the central supermassive black hole (SMBH) interacts with the host galaxy. The last two decades of high resolution X-ray spectroscopy with XMM and Chandra have improved our understanding of the nature of these outflowing ionized absorbers and we are now poised to take the next giant leap with higher spectral resolution and higher throughput observatories to understand the physics and impact of these outflows on the host galaxy gas. The future studies on X-ray outflows not only have the potential to unravel some of the currently outstanding puzzles in astronomy, such as the physical basis behind the MBH$-\sigma$ relation, the cooling flow problem in intra-cluster medium (ICM), and the evolution of the quasar luminosity function across cosmic timescales, but also provide rare insights into the dynamics and nature of matter in the immediate vicinity of the SMBH. Higher spectral resolution ($\le 0.5$ eV at $1$ keV) observations will be required to identify individual absorption lines and study the asymmetries and shifts in the line profiles revealing important information about outflow structures and their impact. Higher effective area ($\ge 1000 \rm \,cm^{2}$) will be required to study the outflows in distant quasars, particularly at the quasar peak era (redshift $1\le z\le 3$) when the AGN population was the brightest. Thus, it is imperative that we develop next generation X-ray telescopes with high spectral resolution and high throughput for unveiling the properties and impact of highly energetic X-ray outflows. A simultaneous high resolution UV + X-ray mission will encompass the crucial AGN ionizing continuum, and also characterize the simultaneous detections of UV and X-ray outflows, which map different spatial scales along the line of sight., Comment: A Science White Paper submitted to the Astro2020 Decadal Survey
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- 2019
18. On Calibrations Using the Crab Nebula as a Standard Candle
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Weisskopf, Martin, Guainazzi, Matteo, Jahoda, Keith, Shaposhnikov, Nikolai, ODell, Stephen, Zavlin, Vyacheslav, Wilson-Hodge, Colleen, and Elsner, Ronald
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Astronomy - Abstract
Inspired by a recent paper (Kirsch et al. 2005) on possible use of the Crab Nebula as a standard candle for calibrating X-ray response func tions, we examine possible consequences of intrinsic departures from a single (absorbed) power law upon such calibrations. We limited our analyses to three more modern X-ray instruments -- the ROSAT/PSPC, th e RXTE/PCA, and the XMM-Newton/EPIC-pn. The results are unexpected an d indicate a need to refine two of the three response functions studi ed. The implications for Chandra will be discussed.
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- 2009
19. An XMM–Newton study of active–inactive galaxy pairs.
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Guainazzi, Matteo, De Rosa, Alessandra, Bianchi, Stefano, Husemann, Bernd, Bogdanovic, Tamara, Komossa, Stefanie, Loiseau, Nora, Paragi, Zsolt, Pérez-Torres, Miguel, Piconcelli, Enrico, and Vignali, Cristian
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- *
COMPTON scattering , *ACTIVE galactic nuclei , *GALAXIES , *BLACK holes - Abstract
While theory and simulations indicate that galaxy mergers play an important role in the cosmological evolution of accreting black holes and their host galaxies, samples of active galactic nuclei (AGNs) in galaxies at close separations are still small. In order to increase the sample of AGN pairs, we undertook an archival project to investigate the X-ray properties of an SDSS-selected sample of 32 galaxy pairs with separations ≤150 kpc containing one optically identified AGN, which were serendipitously observed by XMM–Newton. We discovered only one X-ray counterpart among the optically classified non-active galaxies, with a weak X-ray luminosity (≃ 5 × 1041 erg s−1). 59 per cent (19 out of 32) of the AGNs in our galaxy pair sample exhibit an X-ray counterpart, covering a wide range in absorption-corrected X-ray luminosity (5 × 1041–2 × 1044 erg s−1). More than 79 per cent of these AGNs are obscured (column density N H > 1022 cm−2), with more than half thereof (i.e. about 47 per cent of the total AGN sample) being Compton-thick. AGN/no-AGN pairs are therefore more frequently X-ray obscured (by a factor ≃1.5) than isolated AGNs. When compared to a luminosity and redshift-matched sample of bona fide dual AGN, AGN/no-AGN pairs exhibit one order-of-magnitude lower X-ray column density in the same separation range (>10 kpc). A small sample (4 objects) of AGN/no-AGN pairs with sub-pc separation is all heavily obscured, driving a formal anticorrelation between the X-ray column density and the galaxy pair separation in these systems. These findings suggest that the galactic environment has a key influence on the triggering of nuclear activity in merging galaxies. [ABSTRACT FROM AUTHOR]
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- 2021
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20. The Hot Universe with XRISM and Athena
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Guainazzi, Matteo and Tashiro, Makoto S.
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High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Astrophysics::Earth and Planetary Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Instrumentation and Methods for Astrophysics (astro-ph.IM) - Abstract
X-ray spectroscopy is key to address the theme of "The Hot Universe", the still poorly understood astrophysical processes driving the cosmological evolution of the baryonic hot gas traceable through its electromagnetic radiation. Two future X-ray observatories: the JAXA-led XRISM (due to launch in the early 2020s), and the ESA Cosmic Vision L-class mission Athena (early 2030s) will provide breakthroughs in our understanding of how and when large-scale hot gas structures formed in the Universe, and in tracking their evolution from the formation epoch to the present day., Proceedings of the IAU Symposium IAUS342, "Perseus in Sicily: from black hole to cluster outskirts". 8 pages, 3 figures
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- 2018
21. Glimpse of the highly obscured HMXB IGR J16318−4848 with Hitomi
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Aharonian , Felix, Akamatsu , Hiroki, Akimoto , Fumie, Allen , StevenW., Angelini , Lorella, Audard , Marc, Awaki , Hisamitsu, Axelsson , Magnus, Bamba , Aya, Bautz , MarshallW., Blandford , Roger, Brenneman , LauraW., Brown , GregoryV., Bulbul , Esra, Cackett , EdwardM., Chernyakova , Maria, Chiao , MengP., Coppi , PaoloS., Costantini , Elisa, De Plaa , Jelle, de Vries , CorP., Den Herder , Jan-Willem, Done , Chris, Dotani , Tadayasu, Ebisawa , Ken, Eckart , MeganE., Enoto , Teruaki, Ezoe , Yuichiro, Fabian , AndrewC., Ferrigno , Carlo, Foster , AdamR., Fujimoto , Ryuichi, Fukazawa , Yasushi, Furuzawa , Akihiro, Galeazzi , Massimiliano, Gallo , LuigiC., Gandhi , Poshak, Giustini , Margherita, Goldwurm , Andrea, Gu , Liyi, Guainazzi , Matteo, Haba , Yoshito, Hagino , Kouichi, Hamaguchi , Kenji, Harrus , IlanaM., Hatsukade , Isamu, Hayashi , Katsuhiro, Hayashi , Takayuki, Hayashida , Kiyoshi, Hiraga , JunkoS., Hornschemeier , Ann, Hoshino , Akio, Hughes , JohnP., Ichinohe , Yuto, Iizuka , Ryo, Inoue , Hajime, Inoue , Yoshiyuki, Ishida , Manabu, Ishikawa , Kumi, Ishisaki , Yoshitaka, Iwai , Masachika, Kaastra , Jelle, Kallman , Tim, Kamae , Tsuneyoshi, Kataoka , Jun, Katsuda , Satoru, Kawai , Nobuyuki, Kelley , RichardL., Kilbourne , CarolineA., Kitaguchi , Takao, Kitamoto , Shunji, Kitayama , Tetsu, Kohmura , Takayoshi, Kokubun , Motohide, Koyama , Katsuji, Koyama , Shu, Kretschmar , Peter, Krimm , HansA., Kubota , Aya, Kunieda , Hideyo, Laurent , Philippe, Lee , Shiu-Hang, Leutenegger , MauriceA., Limousin , OlivierO., Loewenstein , Michael, Long , KnoxS., Lumb , David, Madejski , Greg, Maeda , Yoshitomo, Maier , Daniel, Makishima , Kazuo, Markevitch , Maxim, Matsumoto , Hironori, Matsushita , Kyoko, Mccammon , Dan, McNamara , BrianR., Mehdipour , Missagh, Miller , EricD., Miller , JonM., Mineshige , Shin, Mitsuda , Kazuhisa, Mitsuishi , Ikuyuki, Miyazawa , Takuya, Mizuno , Tsunefumi, Mori , Hideyuki, Mori , Koji, Mukai , Koji, Murakami , Hiroshi, Mushotzky , RichardF., Nakagawa , Takao, Nakajima , Hiroshi, Nakamori , Takeshi, Nakashima , Shinya, Nakazawa , Kazuhiro, Nobukawa , KumikoK., Nobukawa , Masayoshi, Noda , Hirofumi, Odaka , Hirokazu, Ohashi , Takaya, Ohno , Masanori, Okajima , Takashi, Ota , Naomi, Ozaki , Masanobu, Paerels , Frits, Paltani , Stéphane, Petre , Robert, Pinto , Ciro, Porter , FrederickS., Pottschmidt , Katja, Reynolds , ChristopherS., Safi-Harb , Samar, Saito , Shinya, Sakai , Kazuhiro, Sasaki , Toru, Sato , Goro, Sato , Kosuke, Sato , Rie, Sawada , Makoto, Schartel , Norbert, Serlemtsos , PeterJ., Seta , Hiromi, Shidatsu , Megumi, Simionescu , Aurora, Smith , RandallK., Soong , Yang, Stawarz , Łukasz, Sugawara , Yasuharu, Sugita , Satoshi, Szymkowiak , Andrew, Tajima , Hiroyasu, Takahashi , Hiromitsu, Takahashi , Tadayuki, Takeda , Shiníchiro, Takei , Yoh, Tamagawa , Toru, Tamura , Takayuki, Tanaka , Takaaki, Tanaka , Yasuo, Tanaka , YasuyukiT., Tashiro , MakotoS., Tawara , Yuzuru, Terada , Yukikatsu, Terashima , Yuichi, Tombesi , Francesco, Tomida , Hiroshi, Tsuboi , Yohko, Tsujimoto , Masahiro, Tsunemi , Hiroshi, Tsuru , Takeshi, Uchida , Hiroyuki, Uchiyama , Hideki, Uchiyama , Yasunobu, Ueda , Shutaro, Ueda , Yoshihiro, Uno , Shiníchiro, Urry , C.Megan, Ursino , Eugenio, Watanabe , Shin, Werner , Norbert, Wilkins , DanR., Williams , BrianJ., Yamada , Shinya, Yamaguchi , Hiroya, Yamaoka , Kazutaka, Yamasaki , NorikoY., Yamauchi , Makoto, Yamauchi , Shigeo, Yaqoob , Tahir, Yatsu , Yoichi, Yonetoku , Daisuke, Zhuravleva , Irina, Zoghbi , Abderahmen, Nakaniwa , Nozomi, 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 ), and Hitomi
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Astrophysics::High Energy Astrophysical Phenomena ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] - Abstract
International audience; We report on a Hitomi observation of IGR J16318−4848, a high-mass X-ray binary system with an extremely strong absorption of N_H ∼ 10^24 cm^−2. Previous X-ray studies revealed that its spectrum is dominated by strong fluorescence lines of Fe as well as continuum emission lines. For physical and geometrical insight into the nature of the reprocessing material, we utilized the high spectroscopic resolving power of the X-ray microcalorimeter (the soft X-ray spectrometer: SXS) and the wide-band sensitivity by the soft and hard X-ray imagers (SXI and HXI) aboard Hitomi. Even though the photon counts are limited due to unintended off-axis pointing, the SXS spectrum resolves Fe Kα_1 and Kα_2 lines and puts strong constraints on the line centroid and line width. The line width corresponds to a velocity of 160$$^{+300}_{-70}$$ km s^−1. This represents the most accurate, and smallest, width measurement of this line made so far from the any X-ray binary, much less than the Doppler broadening and Doppler shift expected from speeds that are characteristic of similar systems. Combined with the K-shell edge energy measured by the SXI and HXI spectra, the ionization state of Fe is estimated to be in the range of Fe i–iv. Considering the estimated ionization parameter and the distance between the X-ray source and the absorber, the density and thickness of the materials are estimated. The extraordinarily strong absorption and the absence of a Compton shoulder component have been confirmed. These characteristics suggest reprocessing materials that are distributed in a narrow solid angle or scattering, primarily by warm free electrons or neutral hydrogen. This measurement was achieved using the SXS detection of 19 photons. It provides strong motivation for follow-up observations of this and other X-ray binaries using the X-ray Astrophysics Recovery Mission and other comparable future instruments.
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- 2018
22. X-ray Properties and the Environment of Compact Radio Sources
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Siemiginowska, Aneta, Sobolewska, Malgorzata, Guainazzi, Matteo, Hardcastle, Martin, Migliori, Giulia, Ostorero, Luisa, and Stawarz, Lukasz
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Compact Radio Sources - Published
- 2018
23. Search for thermal X-ray features from the Crab nebula with Hitomi Soft X-ray Spectrometer
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Aharonian, Felix, Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W., Angelini, Lorella, Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W., Blandford, Roger, Brenneman, Laura W., Brown, Greg V., Bulbul, Esra, Cackett, Edward M., Chernyakova, Maria, Chiao, Meng P., Coppi, Paolo S., Costantini, Elisa, de Plaa, Jelle, de Vries, Cor P., den Herder, Jan-Willem, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E., Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C., Ferrigno, Carlo, Foster, Adam R., Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C., Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana M., Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko S., Hornschemeier, Ann, Hoshino, Akio, Hughes, John P., Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Yoshiyuki, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Kaastra, Jelle, Kallman, Tim, Kamae, Tsuneyoshi, Kataoka, Jun, Katsuda, Satoru, Kawai, Nobuyuki, Kelley, Richard L., Kilbourne, Caroline A., Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Katsuji, Koyama, Shu, Kretschmar, Peter, Krimm, Hans A., Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lee, Shiu-Hang, Leutenegger, Maurice A., Limousin, Olivier O., Loewenstein, Michael, Long, Knox S., Lumb, David, Madejski, Greg, Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R., Mehdipour, Missagh, Miller, Eric D., Miller, Jon M., Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Mukai, Koji, Murakami, Hiroshi, Mushotzky, Richard F., Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko K., Nobukawa, Masayoshi, Noda, Hirofumi, Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stephane, Petre, Robert, Pinto, Ciro, Porter, Frederick S., Pottschmidt, Katja, Reynolds, Christopher S., Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sato, Toshiki, Sawada, Makoto, Schartel, Norbert, Serlemtsos, Peter J., Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K., Soong, Yang, Stawarz, Lukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew, Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shinichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki T., Tashiro, Makoto S., Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi Go, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Uno, Shinichiro, Urry, C. Megan, Ursino, Eugenio, Watanabe, Shin, Werner, Norbert, Wilkins, Dan R., Williams, Brian J., Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y., Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Zhuravleva, Irina, Zoghbi, Abderahmen, Tominaga, Nozomu, and Moriya, Takashi J.
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Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
The Crab nebula originated from a core-collapse supernova (SN) explosion observed in 1054 A.D. When viewed as a supernova remnant (SNR), it has an anomalously low observed ejecta mass and kinetic energy for an Fe-core collapse SN. Intensive searches were made for a massive shell that solves this discrepancy, but none has been detected. An alternative idea is that the SN1054 is an electron-capture (EC) explosion with a lower explosion energy by an order of magnitude than Fe-core collapse SNe. In the X-rays, imaging searches were performed for the plasma emission from the shell in the Crab outskirts to set a stringent upper limit to the X-ray emitting mass. However, the extreme brightness of the source hampers access to its vicinity. We thus employed spectroscopic technique using the X-ray micro-calorimeter onboard the Hitomi satellite. By exploiting its superb energy resolution, we set an upper limit for emission or absorption features from yet undetected thermal plasma in the 2-12 keV range. We also re-evaluated the existing Chandra and XMM-Newton data. By assembling these results, a new upper limit was obtained for the X-ray plasma mass of
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- 2017
24. The Spin of the Supermassive Black Hole in MCG-05-23-16
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Wang, Yu, Ghasemi-Nodehi, M., Guainazzi, Matteo, and Bambi, Cosimo
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High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
We present the results of a multi-epoch and multi-instrument study of the supermassive black hole at the center of the galaxy MCG-05-23-16 aiming at the determination of its spin. We have analyzed high quality X-ray data of MCG-05-23-16 from XMM-Newton, Suzaku, and NuSTAR obtained over a period of about 10~years. We have built a double-reflection spectral model that well describes the observed spectrum based on prior results suggesting that the iron K$\alpha$ line includes both a broad component from the disk's reflection spectrum and a narrow component due to fluorescence and scattering off material by more distant matter. Our measurement of the black hole spin parameter is $a_* = 0.856\pm0.006$ (99\% confidence level)., Comment: 13 pages, 6 figures. Withdrawal reason: error in the data analysis
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- 2017
25. PKS 1718-649: a broad-band study of a young radio jet
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Sobolewska, Malgosia, Siemiginowska, Aneta, Migliori, Giulia, Guainazzi, Matteo, Hardcastle, Martin, Ostorero, Luisa, and Stawarz, Lukasz
- Published
- 2017
26. $Hitomi$ constraints on the 3.5 keV line in the Perseus galaxy cluster
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Hitomi Collaboration, Aharonian, Felix A., Akamatsu, Hiroki, Akimoto, Fumie, Allen, Steven W., Angelini, Lorella, Arnaud, Keith A., Audard, Marc, Awaki, Hisamitsu, Axelsson, Magnus, Bamba, Aya, Bautz, Marshall W., Blandford, Roger D., Brenneman, Laura W., Brown, Gregory V., Bulbul, Esra, Cackett, Edward M., Chernyakova, Maria, Chiao, Meng P., Coppi, Paolo, Costantini, Elisa, de Plaa, Jelle, Herder, Jan-Willem den, Done, Chris, Dotani, Tadayasu, Ebisawa, Ken, Eckart, Megan E., Enoto, Teruaki, Ezoe, Yuichiro, Fabian, Andrew C., Ferrigno, Carlo, Foster, Adam R., Fujimoto, Ryuichi, Fukazawa, Yasushi, Furuzawa, Akihiro, Galeazzi, Massimiliano, Gallo, Luigi C., Gandhi, Poshak, Giustini, Margherita, Goldwurm, Andrea, Gu, Liyi, Guainazzi, Matteo, Haba, Yoshito, Hagino, Kouichi, Hamaguchi, Kenji, Harrus, Ilana, Hatsukade, Isamu, Hayashi, Katsuhiro, Hayashi, Takayuki, Hayashida, Kiyoshi, Hiraga, Junko, Hornschemeier, Ann E., Hoshino, Akio, Hughes, John P., Ichinohe, Yuto, Iizuka, Ryo, Inoue, Hajime, Inoue, Shota, Inoue, Yoshiyuki, Ishibashi, Kazunori, Ishida, Manabu, Ishikawa, Kumi, Ishisaki, Yoshitaka, Itoh, Masayuki, Iwai, Masachika, Iyomoto, Naoko, Kaastra, Jelle S., Kallman, Timothy, Kamae, Tuneyoshi, Kara, Erin, Kataoka, Jun, Katsuda, Satoru, Katsuta, Junichiro, Kawaharada, Madoka, Kawai, Nobuyuki, Kelley, Richard L., Khangulyan, Dmitry, Kilbourne, Caroline A., King, Ashley L., Kitaguchi, Takao, Kitamoto, Shunji, Kitayama, Tetsu, Kohmura, Takayoshi, Kokubun, Motohide, Koyama, Shu, Koyama, Katsuji, Kretschmar, Peter, Krimm, Hans A., Kubota, Aya, Kunieda, Hideyo, Laurent, Philippe, Lebrun, Francois, Lee, Shiu-Hang, Leutenegger, Maurice, Limousin, Olivier, Loewenstein, Michael, Long, Knox S., Lumb, David, Madejski, Grzegorz M., Maeda, Yoshitomo, Maier, Daniel, Makishima, Kazuo, Markevitch, Maxim, Matsumoto, Hironori, Matsushita, Kyoko, McCammon, Dan, McNamara, Brian R., Mehdipour, Missagh, Miller, Eric D., Miller, Jon M., Mineshige, Shin, Mitsuda, Kazuhisa, Mitsuishi, Ikuyuki, Miyazawa, Takuya, Mizuno, Tsunefumi, Mori, Hideyuki, Mori, Koji, Moseley, Harvey, Mukai, Koji, Murakami, Hiroshi, Murakami, Toshio, Mushotzky, Richard F., Nakagawa, Takao, Nakajima, Hiroshi, Nakamori, Takeshi, Nakano, Toshio, Nakashima, Shinya, Nakazawa, Kazuhiro, Nobukawa, Kumiko, Nobukawa, Masayoshi, Noda, Hirofumi, Nomachi, Masaharu, O'Dell, Steve L., Odaka, Hirokazu, Ohashi, Takaya, Ohno, Masanori, Okajima, Takashi, Ota, Naomi, Ozaki, Masanobu, Paerels, Frits, Paltani, Stephane, Parmar, Arvind, Petre, Robert, Pinto, Ciro, Pohl, Martin, Porter, F. Scott, Pottschmidt, Katja, Ramsey, Brian D., Reynolds, Christopher S., Russell, Helen R., Safi-Harb, Samar, Saito, Shinya, Sakai, Kazuhiro, Sameshima, Hiroaki, Sasaki, Toru, Sato, Goro, Sato, Kosuke, Sato, Rie, Sawada, Makoto, Schartel, Norbert, Serlemitsos, Peter J., Seta, Hiromi, Shidatsu, Megumi, Simionescu, Aurora, Smith, Randall K., Soong, Yang, Stawarz, Lukasz, Sugawara, Yasuharu, Sugita, Satoshi, Szymkowiak, Andrew E., Tajima, Hiroyasu, Takahashi, Hiromitsu, Takahashi, Tadayuki, Takeda, Shin'ichiro, Takei, Yoh, Tamagawa, Toru, Tamura, Keisuke, Tamura, Takayuki, Tanaka, Takaaki, Tanaka, Yasuo, Tanaka, Yasuyuki, Tashiro, Makoto, Tawara, Yuzuru, Terada, Yukikatsu, Terashima, Yuichi, Tombesi, Francesco, Tomida, Hiroshi, Tsuboi, Yohko, Tsujimoto, Masahiro, Tsunemi, Hiroshi, Tsuru, Takeshi, Uchida, Hiroyuki, Uchiyama, Hideki, Uchiyama, Yasunobu, Ueda, Shutaro, Ueda, Yoshihiro, Ueno, Shiro, Uno, Shin'ichiro, Urry, C. Meg, Ursino, Eugenio, de Vries, Cor P., Watanabe, Shin, Werner, Norbert, Wik, Daniel R., Wilkins, Dan R., Williams, Brian J., Yamada, Shinya, Yamaguchi, Hiroya, Yamaoka, Kazutaka, Yamasaki, Noriko Y., Yamauchi, Makoto, Yamauchi, Shigeo, Yaqoob, Tahir, Yatsu, Yoichi, Yonetoku, Daisuke, Yoshida, Atsumasa, Zhuravleva, Irina, Zoghbi, Abderahmen, Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Hitomi, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)
- Subjects
galaxies: clusters: individual ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,galaxies: clusters: intracluster medium ,clusters: individual: A426 [galaxies] ,Astrophysics::High Energy Astrophysical Phenomena ,[ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph] ,Dark matter ,FOS: Physical sciences ,Astrophysics ,Astrophysics::Cosmology and Extragalactic Astrophysics ,galaxies: clusters: individual (A426) ,01 natural sciences ,dark matter ,X-ray ,Settore FIS/05 - Astronomia e Astrofisica ,gas ,0103 physical sciences ,calorimeter ,Emission spectrum ,Spectroscopy ,010303 astronomy & astrophysics ,Galaxy cluster ,Astrophysics::Galaxy Astrophysics ,Line (formation) ,High Energy Astrophysical Phenomena (astro-ph.HE) ,Physics ,Nebula ,010308 nuclear & particles physics ,dark matter: decay ,Astronomy and Astrophysics ,charge exchange ,Astrophysics - Astrophysics of Galaxies ,K-line ,Galaxy ,flux ,Space and Planetary Science ,clusters: intracluster medium [galaxies] ,Astrophysics of Galaxies (astro-ph.GA) ,X-rays: galaxies: clusters ,galaxy: cluster ,galaxies: clusters [X-rays] ,Astrophysics - High Energy Astrophysical Phenomena ,[PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph] ,signature ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
High-resolution X-ray spectroscopy with Hitomi was expected to resolve the origin of the faint unidentified E=3.5 keV emission line reported in several low-resolution studies of various massive systems, such as galaxies and clusters, including the Perseus cluster. We have analyzed the Hitomi first-light observation of the Perseus cluster. The emission line expected for Perseus based on the XMM-Newton signal from the large cluster sample under the dark matter decay scenario is too faint to be detectable in the Hitomi data. However, the previously reported 3.5 keV flux from Perseus was anomalously high compared to the sample-based prediction. We find no unidentified line at the reported high flux level. Taking into account the XMM measurement uncertainties for this region, the inconsistency with Hitomi is at a 99% significance for a broad dark-matter line and at 99.7% for a narrow line from the gas. We do not find anomalously high fluxes of the nearby faint K line or the Ar satellite line that were proposed as explanations for the earlier 3.5 keV detections. We do find a hint of a broad excess near the energies of high-n transitions of Sxvi (E=3.44 keV rest-frame) -- a possible signature of charge exchange in the molecular nebula and another proposed explanation for the unidentified line. While its energy is consistent with XMM pn detections, it is unlikely to explain the MOS signal. A confirmation of this interesting feature has to wait for a more sensitive observation with a future calorimeter experiment., Discussion of systematics significantly expanded. 9 pages, 5 figures; ApJ Lett. in press
- Published
- 2017
27. The Athena space X‐ray observatory and the astrophysics of hot plasma†.
- Author
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Barret, Didier, Decourchelle, Anne, Fabian, Andy, Guainazzi, Matteo, Nandra, Kirpal, Smith, Randall, and den Herder, Jan‐Willem
- Subjects
ASTROPHYSICS ,X-rays ,PLASMA astrophysics ,HIGH temperature plasmas ,X-ray spectroscopy ,GALACTIC X-ray sources ,ACCRETION (Astrophysics) - Abstract
The properties (temperature, density, chemical composition, velocity) of hot astrophysical plasma and the physical processes affecting them (heating/cooling, turbulence, shocks, acceleration) can be probed by high‐resolution X‐ray spectroscopy, to be complemented by high‐spatial‐resolution imaging. The paper presents the status of the European Space Agency's Advanced Telescope for High Energy Astrophysics (Athena) mission, particularly focusing on the science performance of its two focal‐plane instruments for studies of extended X‐ray sources: the wide‐field imager and the X‐ray integral field unit. This paper then provides a brief summary of the breakthroughs expected with Athena on the astrophysics of hot plasma, building on the vast heritage of the discoveries and revolutionary results obtained by Chandra and XMM‐Newton in this field. As of November 12, 2019, Athena successfully concluded its feasibility study, and has since then moved into the definition phase, with a launch date scheduled in the early 2030s. [ABSTRACT FROM AUTHOR]
- Published
- 2020
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28. Stingray Software The Code of the Spectral-timing Revolution: Black Holes, a Library, and a GUI.
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Migliari, Simone, Balm, Paul, Vallés, Ricardo, Bachetti, Matteo, Huppenkothen, Danicla, Stevens, Abigai, Guainazzi, Matteo, and Kuulkers, Erik
- Published
- 2019
29. Summary of the 2015 IACHEC meeting
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Li, Xiaobo, Zhang, Shu, Grant, Catherine, Guainazzi, Matteo, Miller, Eric, Natalucci, Lorenzo, and Nevalainen, Jukka
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Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics::Instrumentation and Methods for Astrophysics ,FOS: Physical sciences ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) - Abstract
We summarize the outcome of the 10th meeting of the International Astronomical Consortium for High Energy Calibration (IACHEC), held in Beijing (People's Republic of China) in April 2015. Over 80 scientists directly involved in the calibration of operational and future high-energy missions gathered during 3.5 days to discuss the status of the X-ray payload inter-calibration, as well as possible ways to improve it. A recent study on a large sample of galaxy clusters confirmed that the calibration of the effective area shape above 2 keV between XMM-Newton/EPIC and Chandra/ACIS is consistent, but showed a significant discrepancy at lower energies. Temperatures measured by EPIC are therefore smaller, the difference being largest for the highest temperatures, up to ~20% at kT=10 keV (Schellenberger et al. 2015). The latest multi-mission study of the Crab Nebula above 10 keV shows a +/-13% agreement in the relative normalization of the INTEGRAL, NuSTAR, RXTE, and {\it Suzaku} hard X-ray instruments., 7 pages. See http://web.mit.edu/iachec/papers/index.html for a full list of IACHEC publications
- Published
- 2015
30. 3C 273 with NuSTAR: Unveiling the AGN
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Madsen, Kristin K., F��rst, Felix, Walton, Dominic J., Harrison, Fiona A., Nalewajko, Krzysztof, Madejski, Greg M., Ballantyne, David R., Boggs, Steve E., Brenneman, Laura W., Christensen, Finn E., Craig, William W., Fabian, Andrew C., Forster, Karl, Grefenstette, Brian W., Guainazzi, Matteo, Hailey, Charles J., Matt, Giorgio, Stern, Daniel, Walter, Roland, and Zhang, William W.
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Astrophysics of Galaxies - Abstract
We present results from a 244\,ks \textit{NuSTAR} observation of 3C\,273 obtained during a cross-calibration campaign with the \textit{Chandra}, \textit{INTEGRAL}, \textit{Suzaku}, \textit{Swift}, and \textit{XMM-Newton} observatories. We show that the spectrum, when fit with a power-law model using data from all observatories except \textit{INTEGRAL} over the 1--78\,keV band, leaves significant residuals in the \textit{NuSTAR} data between 30--78\,keV. The \nustar\ 3--78\,keV spectrum is well-described by an exponentially cutoff power-law ($\Gamma = 1.646 \pm 0.006$, E$_\mathrm{cutoff} = 202_{-34}^{+51}$\,keV) with a weak reflection component from cold, dense material. There is also evidence for a weak ($EW = 23 \pm 11$ eV) neutral iron line. We interpret these features as arising from coronal emission plus reflection off an accretion disk or distant material. Beyond 80\,keV \textit{INTEGRAL} data show clear excess flux relative to an extrapolation of the AGN model fit to \nustar. This high-energy power-law is consistent with the presence of a beamed jet, which begins to dominate over emission from the inner accretion flow at 30-40 keV. Modeling the jet locally (in the \textit{NuSTAR} + \textit{INTEGRAL} band) as a power-law, we find the coronal component is fit by $\Gamma_\mathrm{AGN} = 1.638 \pm 0.045$, $E_\mathrm{cutoff} = 47 \pm 15$\,keV, and jet photon index by $\Gamma_\mathrm{jet} = 1.05 \pm 0.4$. We also consider \textit{Fermi}/LAT observations of 3C\,273 and here the broad-band spectrum of the jet can be described by a log-parabolic model, peaking at $\sim 2$\,MeV. Finally, we investigate the spectral variability in the \textit{NuSTAR} band and find an inverse correlation between flux and $\Gamma$., Comment: Accepted in ApJ
- Published
- 2015
31. Concept of X-ray Astronomy Recovery Mission.
- Author
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Makoto Tashiro, Hironori Maejima, Toda, Kenichi, Kelley, Richard, Reichenthal, Lillian, Lobell, James, Petre, Robert, Guainazzi, Matteo, Costantini, Elisa, Edison, Mark, Fujimoto, Ryuichi, Grim, Martin, Kiyoshi Hayashida, den Herder, Jan-Willem, Yoshitaka Ishisaki, Paltani, Stephane, Kyoko Matsushita, Koji Mori, Sneiderman, Gary, and Yoh Takei
- Published
- 2018
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32. Design of the charged particle diverter for the ATHENA mission.
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Ferreira, Ivo, Ayre, Mark, Bavdaz, Marcos, Guainazzi, Matteo, Stefanescu, Alexander, Komárek, M., Valenta, T., Hynek, R., Závodník, M., Sobotka, P., Pejchal, T., Badin, V., Kalousek, R., Bačovský, J., Horák, M., Flajšman, L., Wojewoda, O., and Zlámal, J.
- Published
- 2018
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33. Summary of the 2014 IACHEC Meeting
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Burrows, David, Fabio Gastaldello, Grant, Catherine E., Guainazzi, Matteo, Madsen, Kristin, Miller, Eric, Nevalainen, Jukka, Plucinsky, Paul P., and Sembay, Steve
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FOS: Physical sciences ,Astrophysics - Instrumentation and Methods for Astrophysics ,Instrumentation and Methods for Astrophysics (astro-ph.IM) - Abstract
We present the main results of the 9th meeting of the International Astronomical Consortium for High Energy Calibration (IACHEC), held in Warrenton (Virginia) in May 2014. Over 50 scientists directly involved in the calibration of operational and future high-energy missions gathered during 3.5 days to discuss the status of the X-ray payloads inter-calibration, as well as possible ways to improve it. Sect.2 of this Report summarises our current understanding of the energy-dependent inter-calibration status., International Astronomical Consortium for High-Energy Calibration, IACHEC: http://web.mit.edu/iachec/
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- 2014
34. Investigating the origin of the Fe emission lines of the Seyfert 1 galaxy Mrk 205.
- Author
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Laha, Sibasish, Ghosh, Ritesh, Tripathi, Shruti, and Guainazzi, Matteo
- Subjects
COMPTON scattering ,SEYFERT galaxies ,ACTIVE galactic nuclei ,HARD X-rays ,SUPERMASSIVE black holes ,SOFT X rays ,X-ray spectra - Abstract
We have investigated the nature and origin of the Fe K emission lines in Mrk 205 using observations with Suzaku and XMM–Newton , aiming to resolve the ambiguity between a broad emission line and multiple unresolved lines of higher ionization. We detect the presence of a narrow Fe K α emission line along with a broad-band Compton reflection hump at energies |$E\gt 10\rm \, \, {\rm keV}$|. These are consistent with reflected emission of hard X-ray photons off a Compton-thick material of |$N_{\rm H}\ge 2.15\times 10^{24}\rm \, \, {\rm cm^{-2}}$|. In addition we detect a partially covering ionized absorption with ionization parameter |$\log (\xi /\rm \, erg\, cm\, s^{-1})=1.9_{-0.5}^{+0.1}$| , column density |$N_{\rm H}=(5.6_{-1.9}^{+2.0})\times 10^{22}\rm \, \, {\rm cm^{-2}}$| , and a covering factor of |$0.22_{-0.06}^{+0.09}$|. We detect the presence of emission arising out of ionized disc reflection contributing in the soft and hard X-rays consistently in all the observations. We however, could not definitely ascertain the presence of a relativistically broadened Fe line in the X-ray spectra. Using relativistic reflection models, we found that the data are unable to statistically distinguish between the scenarios when the supermassive black hole is non-rotating and when it is maximally spinning. Using the disc reflection model we also find that the accretion disc of the active galactic nucleus may be truncated at a distance 6 R
G < R < 12 RG , which may suggest why there may not be any broad Fe line. The Eddington rate of the source is low (λEdd = 0.03), which points to an inefficient accretion, possibly due to a truncated disc. [ABSTRACT FROM AUTHOR]- Published
- 2019
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- View/download PDF
35. Evidence for radiation pressure compression in the X-ray narrow-line region of Seyfert galaxies.
- Author
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Bianchi, Stefano, Guainazzi, Matteo, Laor, Ari, Stern, Jonathan, and Behar, Ehud
- Subjects
- *
RADIATION pressure , *SEYFERT galaxies , *THERMAL instability , *ACTIVE galactic nuclei , *IONIZING radiation , *X-rays - Abstract
The observed spatial and kinematic overlap between soft X-ray emission and the narrow-line region (NLR) in obscured active galactic nuclei (AGNs) yields compelling evidence that relatively low-density gas co-exists with higher density gas on scales as large as 100 s of pc. This is commonly interpreted as evidence for a constant gas pressure multiphase medium, likely produced by thermal instability. Alternatively, radiation pressure compression (RPC) also leads to a density distribution, since a gas pressure (and hence density) gradient must arise within each cloud to counteract the incident ionizing radiation pressure. RPC leads to a well-defined ionization distribution, and a differential emission measure (DEM) distribution with a universal slope of ∼−0.9, weakly dependent on the gas properties and the illuminating radiation field. In contrast, a multiphase medium does not predict the form of the DEM. The observed DEMs of obscured AGN with XMM – Newton Reflection Grating Spectrometer spectra (the CHRESOS sample) are in striking agreement with the predicted RPC DEM, providing a clear signature that RPC is the dominant mechanism for the observed range of densities in the X-ray NLR. In contrast with the constant gas pressure multiphase medium, RPC further predicts an increasing gas pressure with decreasing ionization, which can be tested with future X-ray missions using density diagnostics. [ABSTRACT FROM AUTHOR]
- Published
- 2019
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- View/download PDF
36. CIELO-RGS: a catalog of soft X-ray ionized emission lines.
- Author
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Mao, Junjie, Kaastra, Jelle S., Guainazzi, Matteo, González-Riestra, Rosario, Santos-Lleó, Maria, Kretschmar, Peter, Grinberg, Victoria, Kalfountzou, Eleni, Ibarra, Aitor, Matzeu, Gabi, Parker, Michael, and Rodríguez-Pascual, Pedro
- Subjects
SOFT X rays ,PLASMA astrophysics ,ACTIVE galactic nuclei ,CATALOGS ,SUPERNOVA remnants ,X-ray binaries - Abstract
Context. High-resolution X-ray spectroscopy has advanced our understanding of the hot Universe by revealing physical properties like kinematics, temperature, and abundances of the astrophysical plasmas. Despite technical and scientific achievements, the lack of scientific products at a level higher than count spectra is hampering complete scientific exploitation of high-quality data. This paper introduces the Catalog of Ionized Emission Lines Observed by the Reflection Grating Spectrometer (CIELO-RGS) onboard the XMM-Newton space observatory. Aims. The CIELO-RGS catalog aims to facilitate the exploitation of emission features in the public RGS spectra archive. In particular, we aim to analyze the relationship between X-ray spectral diagnostics parameters and measurements at other wavelengths. This paper focuses on the methodology of catalog generation, describing the automated line-detection algorithm. Methods. A moderate sample (∼2400 observations) of high-quality RGS spectra available at XMM-Newton Science Archive is used as our starting point. A list of potential emission lines is selected based on a multi-scale peak-detection algorithm in a uniform and automated way without prior assumption on the underlying astrophysical model. The candidate line list is validated via spectral fitting with simple continuum and line profile models. We also compare the catalog content with published literature results on a small number of exemplary sources. Results. We generate a catalog of emission lines (1.2 × 10
4 ) detected in ∼1600 observations toward stars, X-ray binaries, supernovae remnants, active galactic nuclei, and groups and clusters of galaxies. For each line, we report the observed wavelength, broadening, energy and photon flux, equivalent width, and so on. [ABSTRACT FROM AUTHOR]- Published
- 2019
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- View/download PDF
37. Disclosing the properties of low-redshift dual AGN through XMM-Newton and SDSS spectroscopy.
- Author
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De Rosa, Alessandra, Vignali, Cristian, Husemann, Bernd, Bianchi, Stefano, Bogdanović, Tamara, Guainazzi, Matteo, Herrero-Illana, Rubén, Komossa, S, Kun, Emma, and Loiseau, Nora
- Subjects
ACTIVE galactic nuclei ,ASTRONOMICAL observations ,STELLAR evolution ,STAR clusters ,GALAXIES ,X-ray diffraction - Abstract
We report on an optical (SDSS) and X-ray (XMM- Newton) study of an optically selected sample of four dual AGN systems at projected separations of 30–60 kpc. All sources are detected in the X-ray band (0.3–10keV); seven objects are optically identified as Seyfert, while one source, optically classified as a low-ionization nuclear emission-line region (LINER), is likely powered by accretion in virtue of its relatively high X-ray luminosity (1.2 × 10
41 erg s−1 ). Six of the eight objects are obscured in X-rays with NH ≥ 1023 cm−2 ; three of these, whose X-ray spectrum is dominated by a reflection component, are likely Compton-thick (NH ≥ 1024 cm−2 ). This finding is in agreement with the hypothesis that galaxy encounters are effective in driving gas inflow toward the nuclear region, thus increasing the obscuration. We compare the absorption properties in our dual AGN with those in larger samples observed in X-rays but selected in different ways (optical, IR, and hard X-rays). We find that the obscured (NH ≥ 1022 cm−2 ) AGN fraction within the larger sample is 84 ± 4 per cent (taking into account the 90 per cent error on the NH measure) up to large pair separations (∼100 kpc). This is statistically higher than the fraction of obscured AGN in isolated galaxies found in X-ray surveys. [ABSTRACT FROM AUTHOR]- Published
- 2018
- Full Text
- View/download PDF
38. An X-ray view of central engines of low-luminosity quasars (LLQSO) in the local Universe.
- Author
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Laha, Sibasish, Ghosh, Ritesh, Guainazzi, Matteo, and Markowitz, Alex G
- Subjects
ACTIVE galactic nuclei ,QUASARS ,GALACTIC nuclei ,GALAXIES ,SUPERMASSIVE black holes ,RADIO sources (Astronomy) - Abstract
We have carried out a systematic X-ray spectral analysis of a sample of low-luminosity quasars (LLQSO) to investigate the nature of the central engines of these sources. The optically selected LLQSO sample consists of close, known bright active galactic nuclei (AGN) which serves as an important link between the powerful quasars at higher redshift and local Seyfert galaxies. We find that although the bolometric luminosities of the LLQSOs are lower than those of the higher redshift quasars by almost an order of magnitude, their distribution of the Eddington rate $$\lambda _{\rm \, Edd}$$ is similar. We detect a strong anticorrelation between α
OX and $$L_{2500 \mathring{\rm A}}$$, as has also been detected in several other quasar studies with large sample sizes, indicating that as the UV luminosity of the source increases, the X-ray luminosity decreases. We do not detect any significant neutral obscuration ($$N_{\rm H}\ge 10^{22}\rm \, \, {\rm cm^{-2}}$$) in the X-ray spectra of the LLQSOs, and hence rule out obscuration as a possible cause for their lower luminosity. We conclude that the central engines of the LLQSOs function similarly to those of the higher redshift quasars, and the difference is possibly because of the fact that the LLQSOs have lower black hole masses. We do not find any correlation between the molecular gas in the host galaxies and accretion states of the AGN. This indicates that the presence of molecular gas in the host galaxies of the LLQSOs does not significantly influence the instantaneous accretion rates of their SMBHs. [ABSTRACT FROM AUTHOR]- Published
- 2018
- Full Text
- View/download PDF
39. The soft X-ray polarization in obscured AGN
- Author
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BIANCHI STEFANO, MATT GIORGIO, TAMBORRA FRANCESCO, CHIABERGE MARCO, GUAINAZZI MATTEO, MARINUCCI, ANDREA, Bianchi, Stefano, Matt, Giorgio, Tamborra, Francesco, Chiaberge, Marco, Guainazzi, Matteo, and Marinucci, Andrea
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics - Astrophysics of Galaxies ,Astrophysics::Galaxy Astrophysics - Abstract
The soft X-ray emission in obscured active galactic nuclei (AGN) is dominated by emission lines, produced in a gas photoionized by the nuclear continuum and likely spatially coincident with the optical narrow line region (NLR). However, a fraction of the observed soft X-ray flux appears like a featureless power law continuum. If the continuum underlying the soft X-ray emission lines is due to Thomson scattering of the nuclear radiation, it should be very highly polarized. We calculated the expected amount of polarization assuming a simple conical geometry for the NLR, combining these results with the observed fraction of the reflected continuum in bright obscured AGN., 6 pages, 3 figures, to appear in 'X-ray Polarimetry: A New Window in Astrophysics', edited by R. Bellazzini, E. Costa, G. Matt and G. Tagliaferri
- Published
- 2009
40. A broad-line region origin for the iron Kα line in NGC 7213
- Author
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BIANCHI, STEFANO, LA FRANCA, Fabio, MATT GIORGIO, GUAINAZZI MATTEO, JIMENEZ BAILÓN ELENA, LONGINOTTI ANNA LIA, NICASTRO FABRIZIO, PENTERICCI LAURA, Bianchi, Stefano, LA FRANCA, Fabio, Matt, Giorgio, Guainazzi, Matteo, JIMENEZ BAILÓN, Elena, LONGINOTTI ANNA, Lia, Nicastro, Fabrizio, and Pentericci, Laura
- Published
- 2008
41. X-ray Variability Study of Polar Scattered Seyfert 1 Galaxies
- Author
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Beuchert, Tobias, Wilms, Jörn, Matthias Kadler, Lia Longinotti, Anna, Guainazzi, Matteo, Miniutti, Giovanni, and La Calle, Ignacio
- Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Astrophysics of Galaxies (astro-ph.GA) ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We study 12 Seyfert 1 galaxies with a high level of optical polarization. Optical light emerging from the innermost regions is predominantly scattered in a polar region above the central engine directly in our line of sight. These sources show characteristics of Seyfert 2 galaxies such as, e.g., polarized broad lines. The polarization signatures suggest a viewing angle of 45 degrees classifying them as intermediate Seyfert 1/2 types. The unified model predicts this line of sight to pass through the outer layer of the torus resulting in significant soft X-ray variability due to a strongly varying column density. The aim is to find evidence for this geometrical assumption in the spectral variability of all available historical observations of these sources by XMM-Newton and Swift., Conference proceedings for the 10th INTEGRAL/BART Workshop on 22-25 April 2013, Karlovy Vary (Carlsbad), Czech Republic
- Published
- 2013
42. Summary of the 2013 IACHEC Meeting
- Author
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Grant, Catherine E., Guainazzi, Matteo, Natalucci, Lorenzo, Nevalainen, Jukka, Plucinsky, Paul P., Pollock, Andrew, and Sembay, Steve
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,FOS: Physical sciences ,Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Instrumentation and Methods for Astrophysics (astro-ph.IM) - Abstract
We present the main results of the 8th International Astronomical Consortium for High Energy Calibration (IACHEC) meeting, held in Theddingworth, Leicestershire, between March 25 and 28, 2013. Over 50 scientists directly involved in the calibration of operational and future high-energy missions gathered during 3.5 days to discuss the status of the X-ray payload inter-calibration, as well as possible ways to improve it. Sect. 4 of this Report summarises our current understanding of the energy-dependent inter-calibration status., International Astronomical Consortium for High-Energy Calibration, IACHEC: http://web.mit.edu/iachec/
- Published
- 2013
43. Multi-epoch analysis of the X-ray spectrum of the active galactic nucleus in NGC 5506.
- Author
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Sun, Shangyu, Guainazzi, Matteo, Ni, Qingling, Wang, Jingchun, Qian, Chenyang, Shi, Fangzheng, Wang, Yu, and Bambi, Cosimo
- Subjects
- *
SUPERMASSIVE black holes , *ACTIVE galactic nuclei , *X-ray diffraction , *SPECTRUM analysis , *GALACTIC nuclei - Abstract
We present a multi-epoch X-ray spectroscopy analysis of the nearby narrow-line Seyfert I galaxy NGC 5506. For the first time, spectra taken by
Chandra, XMM–Newton, Suzaku , andNuSTAR – covering the 2000–2014 time span – are analysed simultaneously, using state-of-the-art models to describe reprocessing of the primary continuum by optical thick matter in the active galactic nucleus environment. The main goal of our study is determining the spin of the supermassive black hole (SMBH). The nuclear X-ray spectrum is photoelectrically absorbed by matter with column density ≃ 3 × 1022 cm−2. A soft excess is present at energies lower than the photoelectric cut-off. Both photoionized and collisionally ionized components are required to fit it. This component is constant over the time-scales probed by our data. The spectrum at energies higher than 2 keV is variable. We propose that its evolution could be driven by flux-dependent changes in the geometry of the innermost regions of the accretion disc. The black hole spin in NGC 5506 is constrained to be 0.93 $\pm _{ 0.04 }^{0.04}$ at 90 per cent confidence level for one interesting parameter. [ABSTRACT FROM AUTHOR]- Published
- 2018
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44. In-flight verification of the calibration and performance of the ASTRO-H (Hitomi) Soft X-ray Spectrometer.
- Author
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Leutenegger, Maurice A., Audard, Marc, Boyce, Kevin R., Brown, Gregory V., Meng P. Chiao, Eckart, Megan E., Ryuichi Fujimoto, Akihiro Furuzawa, Guainazzi, Matteo, Haas, Daniel, Takayuki Hayashi, den Herder, Jan-Willem, Ryo Iizuka, Manabu Ishida, Yoshitaka Ishisaki, Naomichi Kikuchi, Kilbourne, Caroline A., Shu Koyama, Sho Kurashima, and Yoshitomo Maeda
- Published
- 2018
- Full Text
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45. Spatially Resolved Chandra HETG Spectroscopy of the NLR Ionization Cone in NGC 1068
- Author
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Evans, Daniel A., Ogle, Patrick M., Marshall, Herman L., Nowak, Mike A., Bianchi, Stefano, Guainazzi, Matteo, Longinotti, Anna Lia, Dewey, Dan, Schulz, Norbert S., Noble, Mike S., Houck, John, and Canizares, Claude R.
- Subjects
High Energy Astrophysical Phenomena (astro-ph.HE) ,Cosmology and Nongalactic Astrophysics (astro-ph.CO) ,Astrophysics::High Energy Astrophysical Phenomena ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena ,Astrophysics::Galaxy Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present initial results from a new 440-ks Chandra HETG GTO observation of the canonical Seyfert 2 galaxy NGC 1068. The proximity of NGC 1068, together with Chandra's superb spatial and spectral resolution, allow an unprecedented view of its nucleus and circumnuclear NLR. We perform the first spatially resolved high-resolution X-ray spectroscopy of the `ionization cone' in any AGN, and use the sensitive line diagnostics offered by the HETG to measure the ionization state, density, and temperature at discrete points along the ionized NLR. We argue that the NLR takes the form of outflowing photoionized gas, rather than gas that has been collisionally ionized by the small-scale radio jet in NGC 1068. We investigate evidence for any velocity gradients in the outflow, and describe our next steps in modeling the spatially resolved spectra as a function of distance from the nucleus., 5 pages, 2 figures, 1 video. To appear in refereed Proceedings of "X-ray Astronomy 2009: Present Status, Multi-Wavelength Approach and Future Perspectives", Bologna, Italy, September 7-11, 2009, AIP, eds. A. Comastri, M. Cappi, and L. Angelini
- Published
- 2009
46. A BLR origin for the iron K$\alpha$ line in NGC7213
- Author
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Bianchi, Stefano, La Franca, Fabio, Matt, Giorgio, Guainazzi, Matteo, Bailon, Elena Jimenez, Longinotti, Anna Lia, Nicastro, Fabrizio, and Pentericci, Laura
- Subjects
Astrophysics - Abstract
The X-ray spectrum of NGC7213 is known to present no evidence for Compton reflection, a unique result among bright Seyfert 1s. The observed neutral iron K$\alpha$ line, therefore, cannot be associated with a Compton-thick material, like the disc or the torus, but is due to Compton-thin gas, with the Broad Line Region (BLR) as the most likely candidate. To check this hypothesis, a long Chandra HETG observation, together with a quasi-simultaneous optical spectroscopic observation at the ESO NTT EMMI were performed. We found that the iron line is resolved with a FWHM=$2 400^{+1 100}_{-600}$ km/s, in perfect agreement with the value measured for the broad component of the H$\alpha$, $2640^{+110}_{-90}$ km/s. Therefore, NGC7213 is the only Seyfert 1 galaxy whose iron K$\alpha$ line is unambiguously produced in the BLR. We also confirmed the presence of two ionised iron lines and studied them in greater detail than before. The resonant line is the dominant component in the Fe XXV triplet, therefore suggesting an origin in collisionally ionised gas. If this is the case, the blueshift of around 1000 km/s of the two ionised iron lines could be the first measure of the velocity of a starburst wind from its X-ray emission., Comment: 5 pages, 4 figures, accepted for publication in MNRAS Letters
- Published
- 2008
47. The properties of unobscured AGN observed by XMM-Newton
- Author
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Bianchi, Stefano, Guainazzi, Matteo, Matt, Giorgio, and Bonilla, Nuria Fonseca
- Subjects
Astrophysics::High Energy Astrophysical Phenomena ,Astrophysics (astro-ph) ,FOS: Physical sciences ,Astrophysics::Cosmology and Extragalactic Astrophysics ,Astrophysics ,Astrophysics::Galaxy Astrophysics - Abstract
Multiwavelength analysis on large samples of AGN provides an excellent tool to understand the physics of these objects. We present the largest catalog of XMM-Newton targeted AGN, all with high SNR X-ray spectra. It includes all the radio-quiet objects observed by XMM-Newton, in targeted observations of the AGN panel. The principal X-ray properties of the catalog are complemented by multiwavelength data found in the literature (optical magnitudes, radio fluxes, Hbeta FWHM, BH masses). We present here some results on the correlation of these quantities. In particular, we find convincing evidence for an `Iwasawa effect' on the narrow component of the Fe Kalpha line and a correlation between the soft-to-hard X-ray luminosity ratio and the Hbeta FWHM., 2 pages, 2 figures, conference proceedings to appear in "The Central Engine of Active Galactic Nuclei", ed. L. C. Ho and J.-M. Wang (San Francisco: ASP)
- Published
- 2006
48. On the scientific impact of the uncertainties in the Athena mirror effective area.
- Author
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Guainazzi, Matteo, Willingale, Richard, Brenneman, Laura, Bulbul, Esra, den Herder, Jan-Willem, Kuulkers, Erik, Ness, Jan-Uwe, and Natalucci, Lorenzo
- Published
- 2022
- Full Text
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49. Athena charged particle diverter simulations: effects of micro-roughness on proton scattering using Geant4.
- Author
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Breuer, Jean-Paul, Galgóczi, Gábor, Fioretti, Valentina, Zlámal, Jakub, Liska, Petr, Werner, Norbert, Santin, Giovanni, Boudin, Nathalie, Ferreira, Ivo, Guainazzi, Matteo, von Kienlin, Andreas, Lotti, Simone, Mineo, Teresa, Molendi, Silvano, and Perinati, Emanuele
- Published
- 2022
- Full Text
- View/download PDF
50. Geant4 simulation of the residual background in the ATHENA wide field imager from protons deflected by the charged particle diverter.
- Author
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Galgóczi, Gábor, Breuer, Jean-Paul, Fioretti, Valentina, Zlámal, Jakub, Werner, Norbert, Čalkovský, Vojtěch, Boudin, Nathalie, Ferreira, Ivo, Guainazzi, Matteo, von Kienlin, Andreas, Lotti, Simone, Mineo, Teresa, Molendi, Silvano, and Perinati, Emanuele
- Published
- 2022
- Full Text
- View/download PDF
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