Search

Your search keyword '"Rodriguez, Jerome"' showing total 161 results
Start Over Author "Rodriguez, Jerome"

Refine your results

161 results on '"Rodriguez, Jerome"'

152. AN XMM-NEWTON SPECTRAL AND TIMING STUDY OF IGR J16207 - 5129: AN OBSCURED AND NON-PULSATING HMXB

Author

Tomsick, John A., Chaty, Sylvain, Rodriguez, Jerome, Walter, Roland, Kaaret, Philip, and Tovmassian, Gagik

Abstract

We report on a [?]12 hr XMM-Newton observation of the supergiant high-mass X-ray binary (HMXB) IGR J16207 - 5129. This is only the second soft X-ray (0.4-15 keV, in this case) study of the source since it was discovered by the International Gamma-Ray Astrophysics Laboratory satellite. The average energy spectrum is very similar to those of neutron star HMXBs, being dominated by a highly absorbed power-law component with a photon index of G = 1.15+0.07 -0.05. The spectrum also exhibits a soft excess below [?]2 keV and an iron Ka emission line at 6.39 +- 0.03 keV. For the primary power-law component, the column density is (1.19+0.06 -0.05) x 1023 cm-2, indicating local absorption, likely from the stellar wind, and placing IGR J16207 - 5129 in the category of obscured IGR HMXBs. The source exhibits a very high level of variability with an rms noise level of 64% +- 21% in the 10-4-0.05 Hz frequency range. Although the energy spectrum suggests that the system may harbor a neutron star, no pulsations are detected with a 90% confidence upper limit of [?]2% in a frequency range from [?]10-4 to 88 Hz. We discuss similarities between IGR J16207 - 5129 and other apparently nonpulsating HMXBs, including other IGR HMXBs as well as 4U 2206+54 and 4U 1700 - 377.

Published
2009

156. The Hot and Energetic Universe: A White Paper presenting the science theme motivating the Athena+ mission

Author

Nandra, Kirpal, Barret, Didier, Barcons, Xavier, Fabian, Andy, Herder, Jan-Willem Den, Piro, Luigi, Watson, Mike, Adami, Christophe, Aird, James, Afonso, Jose Manuel, Alexander, Dave, Argiroffi, Costanza, Amati, Lorenzo, Arnaud, Monique, Atteia, Jean-Luc, Audard, Marc, Badenes, Carles, Ballet, Jean, Ballo, Lucia, Bamba, Aya, Bhardwaj, Anil, Battistelli, Elia Stefano, Becker, Werner, Becker, Michaël De, Behar, Ehud, Bianchi, Stefano, Biffi, Veronica, Bîrzan, Laura, Bocchino, Fabrizio, Bogdanov, Slavko, Boirin, Laurence, Boller, Thomas, Borgani, Stefano, Borm, Katharina, Bouché, Nicolas, Bourdin, Hervé, Bower, Richard, Braito, Valentina, Branchini, Enzo, Branduardi-Raymont, Graziella, Bregman, Joel, Brenneman, Laura, Brightman, Murray, Brüggen, Marcus, Buchner, Johannes, Bulbul, Esra, Brusa, Marcella, Bursa, Michal, Caccianiga, Alessandro, Cackett, Ed, Campana, Sergio, Cappelluti, Nico, Cappi, Massimo, Carrera, Francisco, Ceballos, Maite, Christensen, Finn, Chu, You-Hua, Churazov, Eugene, Clerc, Nicolas, Corbel, Stephane, Corral, Amalia, Comastri, Andrea, Costantini, Elisa, Croston, Judith, Dadina, Mauro, D'Ai, Antonino, Decourchelle, Anne, Ceca, Roberto Della, Dennerl, Konrad, Dolag, Klaus, Done, Chris, Dovciak, Michal, Drake, Jeremy, Eckert, Dominique, Edge, Alastair, Ettori, Stefano, Ezoe, Yuichiro, Feigelson, Eric, Fender, Rob, Feruglio, Chiara, Finoguenov, Alexis, Fiore, Fabrizio, Galeazzi, Massimiliano, Gallagher, Sarah, Gandhi, Poshak, Gaspari, Massimo, Gastaldello, Fabio, Georgakakis, Antonis, Georgantopoulos, Ioannis, Gilfanov, Marat, Gitti, Myriam, Gladstone, Randy, Goosmann, Rene, Gosset, Eric, Grosso, Nicolas, Guedel, Manuel, Guerrero, Martin, Haberl, Frank, Hardcastle, Martin, Heinz, Sebastian, Herrero, Almudena Alonso, Hervé, Anthony, Holmstrom, Mats, Iwasawa, Kazushi, Jonker, Peter, Kaastra, Jelle, Kara, Erin, Karas, Vladimir, Kastner, Joel, King, Andrew, Kosenko, Daria, Koutroumpa, Dimita, Kraft, Ralph, Kreykenbohm, Ingo, Lallement, Rosine, Lanzuisi, Giorgio, Lee, J, Lemoine-Goumard, Marianne, Lobban, Andrew, Lodato, Giuseppe, Lovisari, Lorenzo, Lotti, Simone, McCharthy, Ian, McNamara, Brian, Maggio, Antonio, Maiolino, Roberto, Marco, Barbara De, Martino, Domitilla De, Mateos, Silvia, Matt, Giorgio, Maughan, Ben, Mazzotta, Pasquale, Mendez, Mariano, Merloni, Andrea, Micela, Giuseppina, Miceli, Marco, Mignani, Robert, Miller, Jon, Miniutti, Giovanni, Molendi, Silvano, Montez, Rodolfo, Moretti, Alberto, Motch, Christian, Nazé, Yaël, Nevalainen, Jukka, Nicastro, Fabrizio, Nulsen, Paul, Ohashi, Takaya, O'Brien, Paul, Osborne, Julian, Oskinova, Lida, Pacaud, Florian, Paerels, Frederik, Page, Mat, Papadakis, Iossif, Pareschi, Giovanni, Petre, Robert, Petrucci, Pierre-Olivier, Piconcelli, Enrico, Pillitteri, Ignazio, Pinto, C, Plaa, Jelle De, Pointecouteau, Etienne, Ponman, Trevor, Ponti, Gabriele, Porquet, Delphine, Pounds, Ken, Pratt, Gabriel, Predehl, Peter, Proga, Daniel, Psaltis, Dimitrios, Rafferty, David, Ramos-Ceja, Miriam, Ranalli, Piero, Rasia, Elena, Rau, Arne, Rauw, Gregor, Rea, Nanda, Read, Andy, Reeves, James, Reiprich, Thomas, Renaud, Matthieu, Reynolds, Chris, Risaliti, Guido, Rodriguez, Jerome, Hidalgo, Paola Rodriguez, Roncarelli, Mauro, Rosario, David, Rossetti, Mariachiara, Rozanska, Agata, Rovilos, Emmanouil, Salvaterra, Ruben, Salvato, Mara, Salvo, Tiziana Di, Sanders, Jeremy, Sanz-Forcada, Jorge, Schawinski, Kevin, Schaye, Joop, Schwope, Axel, Sciortino, Salvatore, Severgnini, Paola, Shankar, Francesco, Sijacki, Debora, Sim, Stuart, Schmid, Christian, Smith, Randall, Steiner, Andrew, Stelzer, Beate, Stewart, Gordon, Strohmayer, Tod, Strüder, Lothar, Sun, Ming, Takei, Yoh, Tatischeff, V, Tiengo, Andreas, Tombesi, Francesco, Trinchieri, Ginevra, Tsuru, TG, Ud-Doula, Asif, Ursino, Eugenio, Valencic, Lynne, Vanzella, Eros, Vaughan, Simon, Vignali, Cristian, Vink, Jacco, Vito, Fabio, Volonteri, Marta, Wang, Daniel, Webb, Natalie, Willingale, Richard, Wilms, Joern, Wise, Michael, Worrall, Diana, Young, Andrew, Zampieri, Luca, Zand, Jean In't, Zane, Silvia, Zezas, Andreas, Zhang, Yuying, and Zhuravleva, Irina

Subjects
astro-ph.HE, astro-ph.SR, 13. Climate action, Astrophysics::High Energy Astrophysical Phenomena, astro-ph.EP, Astrophysics::Instrumentation and Methods for Astrophysics, astro-ph.CO, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, astro-ph.IM
Abstract

This White Paper, submitted to the recent ESA call for science themes to define its future large missions, advocates the need for a transformational leap in our understanding of two key questions in astrophysics: 1) How does ordinary matter assemble into the large scale structures that we see today? 2) How do black holes grow and shape the Universe? Hot gas in clusters, groups and the intergalactic medium dominates the baryonic content of the local Universe. To understand the astrophysical processes responsible for the formation and assembly of these large structures, it is necessary to measure their physical properties and evolution. This requires spatially resolved X-ray spectroscopy with a factor 10 increase in both telescope throughput and spatial resolving power compared to currently planned facilities. Feedback from supermassive black holes is an essential ingredient in this process and in most galaxy evolution models, but it is not well understood. X-ray observations can uniquely reveal the mechanisms launching winds close to black holes and determine the coupling of the energy and matter flows on larger scales. Due to the effects of feedback, a complete understanding of galaxy evolution requires knowledge of the obscured growth of supermassive black holes through cosmic time, out to the redshifts where the first galaxies form. X-ray emission is the most reliable way to reveal accreting black holes, but deep survey speed must improve by a factor ~100 over current facilities to perform a full census into the early Universe. The Advanced Telescope for High Energy Astrophysics (Athena+) mission provides the necessary performance (e.g. angular resolution, spectral resolution, survey grasp) to address these questions and revolutionize our understanding of the Hot and Energetic Universe. These capabilities will also provide a powerful observatory to be used in all areas of astrophysics.

157. INVESTIGATING THE OPTICAL COUNTERPART CANDIDATES OF FOUR INTEGRAL SOURCES LOCALIZED WITH CHANDRA.

Author

Özbey Arabacı, Mehtap, Kalemci, Emrah, Tomsick, John A., Halpern, Jules, Bodaghee, Arash, Chaty, Sylvain, Rodriguez, Jerome, and Rahoui, Farid

Subjects
OPTICAL spectroscopy, SOLAR flares, SOLAR activity, SOLAR radiation, STARS
Abstract

We report on the optical spectroscopic follow-up observations of the candidate counterparts to four INTEGRAL sources: IGR J04069+5042, IGR J06552–1146, IGR J21188+4901, and IGR J22014+6034. The candidate counterparts were determined with Chandra, and the optical observations were performed with 1.5 m RTT-150 telescope (TÜBİTAK National Observatory, Antalya, Turkey) and 2.4 m Hiltner Telescope (MDM Observatory, Kitt Peak, Arizona). Our spectroscopic results show that one of the two candidates of IGR J04069+5042 and the one observed for IGR J06552–1146 could be active late-type stars in RS CVn systems. However, according to the likelihood analysis based on Chandra and INTEGRAL, two optically weaker sources in the INTEGRAL error circle of IGR J06552–1146 have higher probabilities to be the actual counterpart. The candidate counterparts of IGR J21188+4901 are classified as an active M-type star and a late-type star. Among the optical spectra of four candidates of IGR J22014+6034, two show Hα emission lines, one is a late-type star, and the other is an M type. The likelihood analysis favors a candidate with no distinguishing features in the optical spectrum. Two of the candidates classified as M-type dwarfs, are similar to some IGR candidates claimed to be symbiotic stars. However, some of the prominent features of symbiotic systems are missing in our spectra, and their NIR colors are not consistent with those expected for giants. We consider the IR colors of all IGR candidates claimed to be symbiotic systems and find that low-resolution optical spectrum may not be enough for conclusive identification. [ABSTRACT FROM AUTHOR]

Published
2012
Full Text
View/download PDF

160. The enhanced X-ray Timing and Polarimetry mission—eXTP

Author

ShuangNan Zhang, Andrea Santangelo, Marco Feroci, YuPeng Xu, FangJun Lu, Yong Chen, Hua Feng, Shu Zhang, Søren Brandt, Margarita Hernanz, Luca Baldini, Enrico Bozzo, Riccardo Campana, Alessandra De Rosa, YongWei Dong, Yuri Evangelista, Vladimir Karas, Norbert Meidinger, Aline Meuris, Kirpal Nandra, Teng Pan, Giovanni Pareschi, Piotr Orleanski, QiuShi Huang, Stephane Schanne, Giorgia Sironi, Daniele Spiga, Jiri Svoboda, Gianpiero Tagliaferri, Christoph Tenzer, Andrea Vacchi, Silvia Zane, Dave Walton, ZhanShan Wang, Berend Winter, Xin Wu, Jean J. M. in’ t Zand, Mahdi Ahangarianabhari, Giovanni Ambrosi, Filippo Ambrosino, Marco Barbera, Stefano Basso, Jörg Bayer, Ronaldo Bellazzini, Pierluigi Bellutti, Bruna Bertucci, Giuseppe Bertuccio, Giacomo Borghi, XueLei Cao, Franck Cadoux, Francesco Ceraudo, TianXiang Chen, YuPeng Chen, Jerome Chevenez, Marta Civitani, Wei Cui, WeiWei Cui, Thomas Dauser, Ettore Del Monte, Sergio Di Cosimo, Sebastian Diebold, Victor Doroshenko, Michal Dovciak, YuanYuan Du, Lorenzo Ducci, QingMei Fan, Yannick Favre, Fabio Fuschino, José Luis Gálvez, Min Gao, MingYu Ge, Olivier Gevin, Marco Grassi, QuanYing Gu, YuDong Gu, DaWei Han, Bin Hong, Wei Hu, Long Ji, ShuMei Jia, WeiChun Jiang, Thomas Kennedy, Ingo Kreykenbohm, Irfan Kuvvetli, Claudio Labanti, Luca Latronico, Gang Li, MaoShun Li, Xian Li, Wei Li, ZhengWei Li, Olivier Limousin, HongWei Liu, XiaoJing Liu, Bo Lu, Tao Luo, Daniele Macera, Piero Malcovati, Adrian Martindale, Malgorzata Michalska, Bin Meng, Massimo Minuti, Alfredo Morbidini, Fabio Muleri, Stephane Paltani, Emanuele Perinati, Antonino Picciotto, Claudio Piemonte, JinLu Qu, Alexandre Rachevski, Irina Rashevskaya, Jerome Rodriguez, Thomas Schanz, ZhengXiang Shen, LiZhi Sheng, JiangBo Song, LiMing Song, Carmelo Sgro, Liang Sun, Ying Tan, Phil Uttley, Bo Wang, DianLong Wang, GuoFeng Wang, Juan Wang, LangPing Wang, YuSa Wang, Anna L. Watts, XiangYang Wen, Jörn Wilms, ShaoLin Xiong, JiaWei Yang, Sheng Yang, YanJi Yang, Nian Yu, WenDa Zhang, Gianluigi Zampa, Nicola Zampa, Andrzej A. Zdziarski, AiMei Zhang, ChengMo Zhang, Fan Zhang, Long Zhang, Tong Zhang, Yi Zhang, XiaoLi Zhang, ZiLiang Zhang, BaoSheng Zhao, ShiJie Zheng, YuPeng Zhou, Nicola Zorzi, J. Frans Zwart, ITA, GBR, FRA, DEU, ESP, DNK, POL, CZE, CHN, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, eXTP, Zhang, ShuangNan, Santangelo, Andrea, Feroci, Marco, Xu, YuPeng, Lu, FangJun, Chen, Yong, Feng, Hua, Zhang, Shu, Brandt, Søren, Hernanz, Margarita, Baldini, Luca, Bozzo, Enrico, Campana, Riccardo, De Rosa, Alessandra, Dong, YongWei, Evangelista, Yuri, Karas, Vladimir, Meidinger, Norbert, Meuris, Aline, Nandra, Kirpal, Pan, Teng, Pareschi, Giovanni, Orleanski, Piotr, Huang, QiuShi, Schanne, Stephane, Sironi, Giorgia, Spiga, Daniele, Svoboda, Jiri, Tagliaferri, Gianpiero, Tenzer, Christoph, Vacchi, Andrea, Zane, Silvia, Walton, Dave, Wang, ZhanShan, Winter, Berend, Wu, Xin, in’ t Zand, Jean J. M., Ahangarianabhari, Mahdi, Ambrosi, Giovanni, Ambrosino, Filippo, Barbera, Marco, Basso, Stefano, Bayer, Jörg, Bellazzini, Ronaldo, Bellutti, Pierluigi, Bertucci, Bruna, Bertuccio, Giuseppe, Borghi, Giacomo, Cao, XueLei, Cadoux, Franck, Ceraudo, Francesco, Chen, TianXiang, Chen, YuPeng, Chevenez, Jerome, Civitani, Marta, Cui, Wei, Cui, WeiWei, Dauser, Thoma, Del Monte, Ettore, Di Cosimo, Sergio, Diebold, Sebastian, Doroshenko, Victor, Dovciak, Michal, Du, YuanYuan, Ducci, Lorenzo, Fan, QingMei, Favre, Yannick, Fuschino, Fabio, Gálvez, José Lui, Gao, Min, Ge, MingYu, Gevin, Olivier, Grassi, Marco, Gu, QuanYing, Gu, YuDong, Han, DaWei, Hong, Bin, Hu, Wei, Ji, Long, Jia, ShuMei, Jiang, WeiChun, Kennedy, Thoma, Kreykenbohm, Ingo, Kuvvetli, Irfan, Labanti, Claudio, Latronico, Luca, Li, Gang, Li, MaoShun, Li, Xian, Li, Wei, Li, ZhengWei, Limousin, Olivier, Liu, HongWei, Liu, XiaoJing, Lu, Bo, Luo, Tao, Macera, Daniele, Malcovati, Piero, Martindale, Adrian, Michalska, Malgorzata, Meng, Bin, Minuti, Massimo, Morbidini, Alfredo, Muleri, Fabio, Paltani, Stephane, Perinati, Emanuele, Picciotto, Antonino, Piemonte, Claudio, Qu, JinLu, Rachevski, Alexandre, Rashevskaya, Irina, Rodriguez, Jerome, Schanz, Thoma, Shen, ZhengXiang, Sheng, LiZhi, Song, JiangBo, Song, LiMing, Sgro, Carmelo, Sun, Liang, Tan, Ying, Uttley, Phil, Wang, Bo, Wang, DianLong, Wang, GuoFeng, Wang, Juan, Wang, LangPing, Wang, YuSa, Watts, Anna L., Wen, XiangYang, Wilms, Jörn, Xiong, ShaoLin, Yang, JiaWei, Yang, Sheng, Yang, YanJi, Yu, Nian, Zhang, WenDa, Zampa, Gianluigi, Zampa, Nicola, Zdziarski, Andrzej A., Zhang, AiMei, Zhang, ChengMo, Zhang, Fan, Zhang, Long, Zhang, Tong, Zhang, Yi, Zhang, XiaoLi, Zhang, ZiLiang, Zhao, BaoSheng, Zheng, ShiJie, Zhou, YuPeng, Zorzi, Nicola, Zwart, J. Frans, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Gravity (chemistry), Computer science, space mission: eXTP, X-ray timing, Polarimetry, General Physics and Astronomy, FOS: Physical sciences, 01 natural sciences, 7. Clean energy, Physics and Astronomy (all), Settore FIS/05 - Astronomia E Astrofisica, Observatory, X-ray instrumentation, 0103 physical sciences, X-ray polarimetry, Ground segment, Aerospace engineering, 010306 general physics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), High Energy Astrophysical Phenomena (astro-ph.HE), Spacecraft, sezele, business.industry, Payload, Gravitational wave, Astrophysics::Instrumentation and Methods for Astrophysics, Space Science, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

In this paper we present the enhanced X-ray Timing and Polarimetry mission - eXTP. eXTP is a space science mission designed to study fundamental physics under extreme conditions of density, gravity and magnetism. The mission aims at determining the equation of state of matter at supra-nuclear density, measuring effects of QED, and understanding the dynamics of matter in strong-field gravity. In addition to investigating fundamental physics, eXTP will be a very powerful observatory for astrophysics that will provide observations of unprecedented quality on a variety of galactic and extragalactic objects. In particular, its wide field monitoring capabilities will be highly instrumental to detect the electro-magnetic counterparts of gravitational wave sources. The paper provides a detailed description of: (1) the technological and technical aspects, and the expected performance of the instruments of the scientific payload; (2) the elements and functions of the mission, from the spacecraft to the ground segment., Accepted for publication on Sci. China Phys. Mech. Astron. (2019)

Published
2019
Full Text
View/download PDF

161. LOCALIZING INTEGRAL SOURCES WITH CHANDRA: X-RAY AND MULTI-WAVELENGTH IDENTIFICATIONS AND ENERGY SPECTRA.

Author

Tomsick, John A., Bodaghee, Arash, Chaty, Sylvain, Rodriguez, Jerome, Rahoui, Farid, Halpern, Jules, Kalemci, Emrah, and Özbey Arabaci, Mehtap

Subjects
*X-ray spectra, *ACTIVE galaxies, *WAVELENGTHS, *ACTIVE galactic nuclei, *NEAR infrared radiation
Abstract

We report on Chandra observations of 18 hard X-ray (>20 keV) sources discovered with the INTEGRAL satellite near the Galactic plane. For 14 of the INTEGRAL sources, we have uncovered one or two potential Chandra counterparts per source. These provide soft X-ray (0.3-10 keV) spectra and subarcsecond localizations, which we use to identify counterparts at other wavelengths, providing information about the nature of each source. Despite the fact that all of the sources are within 5° of the plane, four of the IGR sources are active galactic nuclei (AGNs; IGR J01545+6437, IGR J15391-5307, IGR J15415-5029, and IGR J21565+5948) and four others are likely AGNs (IGR J03103+5706, IGR J09189-4418, IGR J16413-4046, and IGR J16560-4958) based on each of them having a strong IR excess and/or extended optical or near-IR emission. We compare the X-ray and near-IR fluxes of this group of sources to those of AGNs selected by their 2-10 keV emission in previous studies and find that these IGR AGNs are in the range of typical values. There is evidence in favor of four of the sources being Galactic (IGR J12489-6243, IGR J15293-5609, IGR J16173-5023, and IGR J16206-5253), but only IGR J15293-5609 is confirmed as a Galactic source as it has a unique Chandra counterpart and a parallax measurement from previous optical observations that puts its distance at 1.56 ± 0.12 kpc. The 0.3-10 keV luminosity for this source is (1.4+1.0– 0.4) × 1032 erg s–1, and its optical/IR spectral energy distribution is well described by a blackbody with a temperature of 4200-7000 K and a radius of 12.0-16.4 R☼. These values suggest that IGR J15293-5609 is a symbiotic binary with an early K-type giant and a white dwarf accretor. We also obtained likely Chandra identifications for IGR J13402-6428 and IGR J15368-5102, but follow-up observations are required to constrain their source types. [ABSTRACT FROM AUTHOR]

Published
2012
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results