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1. Morphological Evidence for the eROSITA Bubbles Being Giant and Distant Structures

Author

Teng Liu, Andrea Merloni, Jeremy Sanders, Gabriele Ponti, Andrew Strong, Michael C. H. Yeung, Nicola Locatelli, Peter Predehl, Xueying Zheng, Manami Sasaki, Michael Freyberg, Konrad Dennerl, Werner Becker, Kirpal Nandra, Martin Mayer, and Johannes Buchner

Subjects
Milky Way Galaxy, Interstellar clouds, Diffuse interstellar clouds, Shocks, X-ray surveys, Active galactic nuclei, Astrophysics, QB460-466
Abstract

There are two contradictory views of the eROSITA bubbles: either a 10 ^4 pc scale pair of giant bubbles blown by the Galactic center (GC), or a 10 ^2 pc scale local structure coincidentally located in the direction of GC. A key element of this controversy is the distance to the bubbles. Based on the 3D dust distribution in the Galactic plane, we found three isolated, distant (500–800 pc) clouds at intermediate Galactic latitudes. Their projected morphologies perfectly match the X-ray shadows on the defining features of the north eROSITA bubble, i.e., the North Polar Spur (NPS) and the Lotus Petal Cloud (LPC), indicating that both the NPS and LPC are distant, with a distance lower limit of nearly 1 kpc. In the X-ray-dark region between the NPS and LPC, we found a few polarized radio arcs and attributed them to the bubble’s shock front. These arcs match up perfectly with the outer border of the NPS and LPC and provide a way to define the bubble’s border. The border defined in this way can be well described by the line-of-sight tangent of a 3D skewed cup model rooted in the GC. We conclude that, instead of being two independent, distant features, the NPS and LPC compose a single, giant bubble, which therefore is most plausibly a 10 kpc scale bubble rooted at the GC.

Published
2024
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2. NuSTAR Observations of Abell 665 and 2146: Constraints on Nonthermal Emission

Author

Randall A. Rojas Bolivar, Daniel R. Wik, Ayşegül Tümer, Fabio Gastaldello, Julie Hlavacek-Larrondo, Paul Nulsen, Valentina Vacca, Grzegorz Madejski, Ming Sun, Craig L. Sarazin, Jeremy Sanders, Damiano Caprioli, Brian Grefenstette, and Niels-Jorgen Westergaard

Subjects
Galaxy clusters, Abell clusters, Intracluster medium, Non-thermal radiation sources, Astronomical radiation sources, X-ray astronomy, Astrophysics, QB460-466
Abstract

Observations from past missions such as RXTE and Beppo-SAX suggested the presence of inverse Compton (IC) scattering at hard X-ray energies within the intracluster medium of some massive galaxy clusters. In subsequent years, observations by, e.g., Suzaku, and now NuSTAR, have not been able to confirm these detections. We report on NuSTAR hard X-ray searches for IC emission in two massive galaxy clusters, A665 and A2146. To constrain the global IC flux in these two clusters, we fit global NuSTAR spectra with three models: single (1T) and two-temperature (2T) models, and a 1T plus power-law component (T+IC). The temperature components are meant to characterize the thermal ICM emission, while the power law represents the IC emission. We find that the 3–30 keV A665 and 3–20 keV A2146 spectra are best described by thermal emission alone, with average global temperatures of kT = (9.15 ± 0.1) keV for A665 and kT = (8.29 ± 0.1) keV for A 2146. We constrain the IC flux to F _NT 0.14 μ G and >0.011 μ G for A665 and A2146, respectively.

Published
2023
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3. Full-sky photon simulation of clusters and active galactic nuclei in the soft X-rays for eROSITA

Author

Johan Comparat, Dominique Eckert, Alexis Finoguenov, Robert Schmidt, Jeremy Sanders, Daisuke Nagai, Erwin T. Lau, Florian Kaefer, Florian Pacaud, Nicolas Clerc, Thomas H. Reiprich, Esra Bulbul, Jacob Ider Chitham, Chia-Hsun Chuang, Vittorio Ghirardini, Violeta Gonzalez-Perez, Ghassem Gozaliazl, Charles C. Kirkpatrick, Anatoly Klypin, Andrea Merloni, Kirpal Nandra, Teng Liu, Francisco Prada, Miriam E. Ramos-Ceja, Mara Salvato, Riccardo Seppi, Elmo Tempel, and Gustavo Yepes

Subjects
Astronomy, QB1-991, Astrophysics, QB460-466
Abstract

The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) mission will measure the position and properties of about 100,000 clusters of galaxies and 3 million active galactic nuclei over the full sky. To study the statistical properties of this ongoing survey, it is key to estimate the selection function accurately. We create a set of full sky light-cones using the MultiDark and UNIT dark matter only N-body simulations. We present a novel method to predict the X-ray emission of galaxy clusters. Given a set of dark matter halo properties (mass, redshift, ellipticity, offset parameter), we construct an X-ray emissivity profile and image for each halo in the light-cone. We follow the eROSITA scanning strategy to produce a list of X-ray photons on the full sky. We predict scaling relations for the model clusters, which are in good agreement with the literature. The predicted number density of clusters as a function of flux also agrees with previous measurements. Finally, we obtain a scatter of 0.21 (0.07, 0.25) for the X-ray luminosity -- mass (temperature -- mass, luminosity -- temperature) model scaling relations. We provide catalogues with the model photons emitted by clusters and active galactic nuclei. These catalogues will aid the eROSITA end to end simulation flow analysis and in particular the source detection process and cataloguing methods.

Published
2020
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4. Low-scatter galaxy cluster mass proxies for the eROSITA all-sky survey

Author

Dominique Eckert, Alexis Finoguenov, Vittorio Ghirardini, Sebastian Grandis, Florian Kaefer, Jeremy Sanders, and Miriam Ramos-Ceja

Subjects
Astronomy, QB1-991, Astrophysics, QB460-466
Abstract

The on-going X-ray all-sky survey with the eROSITA instrument will yield large galaxy cluster samples, which will bring strong constraints on cosmological parameters. In particular, the survey holds great promise to investigate the tension between CMB and low-redshift measurements. The current bottleneck preventing the full exploitation of the survey data is the systematics associated with the relation between survey observable and halo mass. Numerous recent studies have shown that gas mass and core-excised X-ray luminosity exhibit very low scatter at fixed mass. We propose a new method to reconstruct these quantities from low photon count data and validate the method using extensive eROSITA-like simulations. We find that even near the detection threshold of ~50 counts the core-excised luminosity and the gas mass can be recovered with 20-30\% precision, which is substantially less than the scatter of the full integrated X-ray luminosity at fixed mass. When combined with an accurate calibration of the absolute mass scale (e.g. through weak gravitational lensing), our technique reduces the systematics on cosmological parameters induced by the mass calibration.

Published
2020
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5. Transparency and openness in science

Author

Jeremy Sanders, Jon Blundy, Anne Donaldson, Steve Brown, Rob Ivison, Miles Padgett, Kevin Padian, Katrin Rittinger, Kerry Rowe, Anthony Stace, Essi Viding, Chris Chambers, and Mark Chaplain

Subjects
Science
Published
2017
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6. Strong perturbation of a super-virial Magellanic circum-galactic medium

Author

Nicola Locatelli, Gabriele Ponti, Andrea Merloni, Xueying Zheng, Konrad Dennerl, Frank Haberl, Chandreyee Maitra, Jeremy Sanders, Manami Sasaki, and Franco Vazza

Abstract

Modern galaxy evolution theories predict a large fraction of ordinary matter to be distributed in the form of gas over the largest galactic scales, with most of the gas mass encompassing the peak and high tail of the overall temperature distribution1. Satellite galaxies however, may lose a large amount of this extended gas due to stripping and ram pressure generated by their in-fall onto a larger system2. The presence of highly ionized gas associated with the Small and Large Magellanic Clouds has been recently confirmed through indirect probes3,4. Using eROSITA/SRG data, in this work we show the first direct images of the X-ray emission from the hottest gas associated to the circum-galactic medium surrounding the Magellanic Clouds. We discover an extended hot gas phase at ~2.3×106 K. This temperature challenges the theoretical expectations from a virialized system5,6 implying that heating mechanisms are at play in the Magellanic Clouds circum-galactic medium. We also discover a strong perturbation that we identify as a cold front in the (Galactic) South direction of the Magellanic Clouds, morphologically connected to them both. The cold front -the first ever discovered at galactic scales (~10 kpc)- also appears to be coincident with enhanced polarization at radio frequencies, as well as with a tangential alignment of the magnetic field lines. The detected discontinuity in the properties of the gas surrounding the Magellanic Clouds is consistent with a gas reservoir being perturbed by the three-body interaction between the Magellanic Clouds and the Milky Way7,8. The Magellanic Clouds provide a unique laboratory for assessing the presence of a hot gas phase in in-falling satellite systems9. The detection of a still large reservoir of hot gas, together with the detection of a front connected with thermal heating and magnetic amplification corroborates and inform galaxy evolution theories10.

Published
2023
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7. Arcus: The Soft X-ray Grating Explorer

Author

Randall K Smith, Margaret Abraham, Grace Baird, Marshall Bautz, Jay Bookbinder, Joel Bregman, Laura Brenneman, Nancy Brickhouse, David Burrows, Vadim Burwitz, Joseph Bushman, Claude Canizares, Deepto Chakrabarty, Peter Cheimets, Elisa Costantini, Simon Dawson, Casey DeRoo, Abraham Falcone, Adam Foster, Luigi Gallo, Catherine E Grant, H Moritz Gunther, Ralf K Heilmann, Butler Hine, David Huenemoerder, Steve Jara, Jelle Kaastra, Ingo Kreykenbohm, Kristin Madsen, Michael McDonald, Michael McEachen, Randall McEntaffer, Herman Marshall, Eric Miller, Jon Miller, Elisabeth Morse, Richard Mushotzky, Kirpal Nandra, Michael Nowak, Frits Paerels, Robert Petre, Katja Poppenhaeger, Andrew Ptak, Paul Reid, Karolyn S Ronzano, Jeremy Sanders, Mark Schattenburg, Jonathan Schonfeld, Norbert Schulz, Alan Smale, Pasquale Temi, Lynne Valencic, Stephen Walker, Richard Willingale, Joern Wilms, and Scott Wolk

Subjects
Optics
Abstract

Arcus provides high-resolution soft X-ray spectroscopy in the 12-50 Å bandpass with unprecedented sensitivity, including spectral resolution > 2500 and effective area > 250 cm2. The three top science goals for Arcus are (1) to measure the effects of structure formation imprinted upon the hot baryons that are predicted to lie in extended halos around galaxies, (2) to trace the propagation of outflowing mass, energy, and momentum from the vicinity of the black hole to extragalactic scales as a measure of their feedback, and (3) to explore how stars form and evolve. Arcus uses the same 12 m focal length grazing-incidence Silicon Pore X-ray Optics (SPOs) that ESA has developed for the Athena mission; the focal length is achieved on orbit via an extendable optical bench. The focused X-rays from these optics are diffracted by high-efficiency Critical-Angle Transmission (CAT) gratings, and the results are imaged with flight-proven CCD detectors and electronics. Combined with the high-heritage NGIS LEOStar-2 spacecraft and launched into 4:1 lunar resonant orbit, Arcus provides high sensitivity and high efficiency observing of a wide range of astrophysical sources.

Published
2019
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9. Arcus: exploring the formation and evolution of clusters, galaxies, and stars

Author

Randall K. Smith, Marshall Bautz, Joel Bregman, Laura Brenneman, Nancy Brickhouse, Esra Bulbul, Vadim Burwitz, Joseph Bushman, Claude Canizares, Deepto Chakrabarty, Peter Cheimets, Elisa Costantini, Casey DeRoo, Abe Falcone, Adam Foster, Luigi Gallo, Catherine Grant, Hans Guenther, Ralf Heilmann, Sarah Heine, Butler Hine, David Huenemoerder, Steve Jara, Jelle Kaastra, Erin Kara, Ingo Kreykenbohm, Kristin Madsen, Herman Marshall, Michael McDonald, Randall McEntaffer, Jon Miller, Eric Miller, Richard Mushotzky, Kirpal Nandra, Michael Nowak, Frederik Paerels, Robert Petre, Katja Poppenhaeger, Andrew Ptak, Paul Reid, Karolyn Ronzano, Agata Rozanska, Jenna Samra, Jeremy Sanders, Mark Schattenburg, Jonathan Schonfeld, Norbert Schulz, Alan Smale, Pasquale Temi, Lynne Valencic, Stephen Walker, Joern Wilms, and Scott Wolk

Published
2022
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10. The eROSITA Final Equatorial-Depth Survey (eFEDS) - Characterization of morphological properties of galaxy groups and clusters

Author

Vittorio Ghirardini, Y. Emre Bahar, Esra Bulbul, Ang Liu, Nicolas Clerc, Florian Pacaud, Johan Comparat, Teng Liu, Miriam E. Ramos-Ceja, Duy Hoang, Jacob Ider-Chitham, Matthias Klein, Andrea Merloni, Kirpal Nandra, Naomi Ota, Peter Predehl, Thomas H. Reiprich, Jeremy Sanders, Tim Schrabback, Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: clusters: intracluster medium, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Space and Planetary Science, galaxies: clusters: general, X-rays: galaxies: clusters, 0103 physical sciences, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Understanding the cluster population of clusters of galaxies is of the utmost importance for using cluster samples in both astrophysical and cosmological studies. We present an in-depth analysis of the X-ray morphological parameters of the galaxy clusters and groups detected in the eROSITA Final Equatorial-Depth Survey (eFEDS). We study the eROSITA X-ray imaging data for a sample of 325 clusters and groups that are significantly detected in the eFEDS field. We characterize their dynamical properties by measuring a number of dynamical estimators: concentration, central density, cuspiness, ellipticity, power-ratios, photon asymmetry, and Gini coefficient. The galaxy clusters and groups detected in eFEDS, covering a luminosity range of more than three orders of magnitude and large redshift range out to 1.2 provide an ideal sample for studying the redshift and luminosity evolution of the morphological parameters and characterization of the underlying dynamical state of the sample. Based on these measurements we construct a new dynamical indicator, relaxation score, for all the clusters in the sample. We find no evidence for bimodality in the distribution of morphological parameters of our clusters, rather we observe a smooth transition from the cool-core to non-cool-core and from relaxed to disturbed states. A significant evolution in redshift and luminosity is also observed in the morphological parameters examined in this study after carefully taking into account the selection effects. We determine that our eFEDS-selected cluster sample, differently than ROSAT-based cluster samples, is not biased toward relaxed clusters, but contains a similar fraction of disturbed as SZ surveys., 21 pages, 10 figures, 2 tables, Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission

Published
2022
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11. Establishing the X-ray Source Detection Strategy for eROSITA with Simulations

Author

Teng Liu, Andrea Merloni, Johan Comparat, Kirpal Nandra, Jeremy Sanders, Georg Lamer, Johannes Buchner, Tom Dwelly, Michael Freyberg, Adam Malyali, Antonis Georgakakis, Mara Salvato, Hermann Brunner, Marcella Brusa, Matthias Klein, Vittorio Ghirardini, Nicolas Clerc, Florian Pacaud, Esra Bulbul, Ang Liu, Axel Schwope, Jan Robrade, Jörn Wilms, Thomas Dauser, Miriam E. Ramos-Ceja, Thomas H. Reiprich, Thomas Boller, Julien Wolf, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), and Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, galaxies: active, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, X-rays: galaxies, surveys, Space and Planetary Science, X-rays: galaxies: clusters, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, X-rays: diffuse background, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Instrumentation and Methods for Astrophysics (astro-ph.IM), catalogs, Astrophysics::Galaxy Astrophysics
Abstract

The eROSITA X-ray telescope on board the Spectrum-Roentgen-Gamma (SRG) satellite has started to detect new X-ray sources over the full sky at an unprecedented rate. Understanding the performance and selection function of the source detection is important for the subsequent scientific analysis of the eROSITA catalogs. Through simulations, we test and optimize the eROSITA source detection procedures, and we characterize the detected catalog quantitatively. Taking the eROSITA Final Equatorial-Depth Survey (eFEDS) as an example, we ran extensive photon-event simulations based on our best knowledge of the instrument characteristics, the background spectrum, and the population of astronomical X-ray sources. We introduce a method of analyzing source detection completeness, purity, and efficiency based on the origin of each photon. According to the source detection efficiency measured in the simulation, we chose a two-pronged strategy to build eROSITA X-ray catalogs, creating a main catalog using only the most sensitive band (0.2-2.3 keV) and an independent hard-band-selected catalog using multiband detection in a range up to 5 keV. Because our mock data are highly representative of the real eFEDS data, we used the mock catalogs to measure the completeness and purity of the eFEDS catalogs as a function of multiple parameters, such as detection likelihood, flux, and luminosity. These measurements provide a basis for choosing the eFEDS catalog selection thresholds. The mock catalogs (available with this paper) can be used to construct the selection function of active galactic nuclei and galaxy clusters. A direct comparison of the output and input mock catalogs also gives rise to a correction curve that converts the raw point-source flux distribution into the intrinsic number counts distribution., Comment: Accepted by A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission

Published
2021
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12. AGN Feedback and Gas Enrichment in Clusters of Galaxies

Author

Jeremy Sanders

Subjects
Physics, Physics and Astronomy (miscellaneous), Radio galaxy, Astrophysics::High Energy Astrophysical Phenomena, Astronomy, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Galaxy groups and clusters, Abell 2744, Intracluster medium, Galaxy group, Brightest cluster galaxy, Astrophysics::Galaxy Astrophysics, Galaxy cluster
Abstract

We examine deep Chandra observations of the nearby Perseus and Centaurus galaxy clusters to examine AGN feedback and enrichment of the intracluster medium. We show evidence of 100 Myr of activity by the central nucleus in Perseus, generating shocks, bubbles and sound waves, heating the cluster core. Despite the AGN activity there exist 10 solar masses of ∼ 5× 10 K gas embedded in an intracluster medium 5 to 10 times hotter than it. Transport properties of the intracluster medium are likely to be important. We observe and map the distribution of metals in the Centaurus cluster, and show that Type II supernova enrichment is important in even the core of this cluster. It has been relatively undisturbed for 8 Gyr with a close heating/cooling balance.

Published
2007
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13. 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, Den Herder, Jan-Willem, 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, Stefano Battistelli, Elia, Becker, Werner, Becker, Michaël, 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, Della Ceca, Roberto, 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, Alonso Herrero, Almudena, 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, Martino, Domitilla, 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, 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, Rodriguez Hidalgo, Paola, Roncarelli, Mauro, Rosario, David, Rossetti, Mariachiara, Rozanska, Agata, Rovilos, Emmanouil, Salvaterra, Ruben, Salvato, Mara, Di Salvo, Tiziana, Jeremy Sanders, 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, T. G., 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, In T Zand, Jean, Zane, Silvia, Zezas, Andreas, Zhang, Yuying, Zhuravleva, Irina, Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Dipartimento di Fisica e Chimica (DiFC), Università degli studi di Palermo - University of Palermo, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de recherche en astrophysique et planétologie (IRAP), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Columbia Astrophysics Laboratory (CAL), Columbia University [New York], Department of Astrophysical Sciences [Princeton], Princeton University, Département d'Astrophysique (ex SAP) (DAP), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire de Cosmologie, Astrophysique Stellaire & Solaire, de Planétologie et de Mécanique des Fluides (CASSIOPEE), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Institute for Computational Cosmology (ICC), Durham University, Dipartimento de Fisica Roma Tre (DF-Roma3), Università degli Studi Roma Tre, Mullard Space Science Laboratory (MSSL), University College of London [London] (UCL), Technische Universität München [München] (TUM), National Space Institute [Lyngby] (DTU Space), Technical University of Denmark [Lyngby] (DTU), 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), SRON Netherlands Institute for Space Research (SRON), Max-Planck-Institut für Extraterrestrische Physik (MPE), Department of Physics [Durham University], Ecole Polytechnique Fédérale de Lausanne (EPFL), Tokyo Metropolitan University [Tokyo], Department of Astronomy and Astrophysics [PennState], Pennsylvania State University (Penn State), Penn State System-Penn State System, Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Department of Physics [Coral Gables], University of Miami [Coral Gables], Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Swedish Institute of Space Physics [Kiruna] (IRF), Astronomical Institute of the Czech Academy of Sciences, Czech Academy of Sciences [Prague] (ASCR), HEPPI - LATMOS, Laboratoire Atmosphères, Milieux, Observations Spatiales (LATMOS), Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris - Site de Meudon (OBSPM), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astronomico di Palermo (OAPa), Istituto Nazionale di Astrofisica (INAF), Cavendish Laboratory, University of Cambridge [UK] (CAM), Università degli Studi di Roma Tor Vergata [Roma], Max-Planck-Institut für Astrophysik (MPA), Institut d'Astrophysique et de Géophysique [Liège], Université de Liège, Harvard-Smithsonian Center for Astrophysics (CfA), Harvard University [Cambridge]-Smithsonian Institution, PSL Research University (PSL), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Centro de Astrobiologia [Madrid] (CAB), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Leiden Observatory [Leiden], Universiteit Leiden [Leiden], School of Physics and Astronomy [Southampton], University of Southampton, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology in Zürich [Zürich] (ETH Zürich), Department of Computer Science, Penn State System, Astronomical Institute Anton Pannekoek (AI PANNEKOEK), University of Amsterdam [Amsterdam] (UvA), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Lawrence Livermore National Laboratory (LLNL), Max Plank Institute for Extraterrestial Life, Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Fisica e Chimica [Palermo] (DiFC), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Università degli Studi Roma Tre = Roma Tre University (ROMA TRE), Technische Universität Munchen - Université Technique de Munich [Munich, Allemagne] (TUM), Danmarks Tekniske Universitet = Technical University of Denmark (DTU), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Tokyo Metropolitan University [Tokyo] (TMU), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Astronomical Institute of the Czech Academy of Sciences (ASU / CAS), Czech Academy of Sciences [Prague] (CAS), HELIOS - LATMOS, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Harvard University-Smithsonian Institution, Université Paris sciences et lettres (PSL), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Instituto Nacional de Técnica Aeroespacial (INTA)-Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Universiteit Leiden, Eidgenössische Technische Hochschule - Swiss Federal Institute of Technology [Zürich] (ETH Zürich), Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), Astronomy, Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Université Fédérale Toulouse Midi-Pyrénées-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), Smithsonian Institution-Harvard University [Cambridge], Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Instituto Nacional de Técnica Aeroespacial (INTA), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Maiolino, Roberto [0000-0002-4985-3819], Reynolds, Christopher [0000-0002-1510-4860], Sijacki, Debora [0000-0002-3459-0438], Apollo - University of Cambridge Repository, Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), and Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Earth and Planetary Astrophysics (astro-ph.EP), astro-ph.SR, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics - Cosmology and Extragalactic Astrophysics, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Solar and Stellar Astrophysics, [SDU]Sciences of the Universe [physics], astro-ph.EP, astro-ph.CO, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), astro-ph.IM, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Earth and Planetary Astrophysics
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., Submitted in response to the call for White Papers for the definition of the L2 and L3 missions in the ESA Science program. More information: http://www.the-athena-x-ray-observatory.eu/. 19 pages, 12 figures, 4 tables

Published
2013

14. Book reviews

Author

Richard Cobbold, Jeremy Sanders, D J Richards, Brian Goodson, Richard Hill, Mitchell Reiss, D F A Henderson, Nik Gowing, Keith Hayward, Vladimir Kozin, Michael Howard, Arthur Hockaday, Robert O'Neill, Ian Lyall Grant, Alistair Horne, Edward Streator, David Kirkpatrick, D J M Jenkins, and John Appleby

Subjects
Political Science and International Relations
Published
1995
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15. The ASTRO-H X-ray Observatory

Author

Tadayuki Takahashi, Kazuhisa Mitsuda, Richard Kelley, Henri Aarts, Felix Aharonian, Hiroki Akamatsu, Fumie Akimoto, Steve Allen, Naohisa Anabuki, Lorella Angelini, Keith Arnaud, Makoto Asai, Marc Audard, Hisamitsu Awaki, Philipp Azzarello, Chris Baluta, Aya Bamba, Nobutaka Bando, Mark Bautz, Roger Blandford, Kevin Boyce, Greg Brown, Ed Cackett, Mara Chernyakova, Paolo Coppi, Elisa Costantini, Jelle de Plaa, Jan-Willem den Herder, Michael DiPirro, Chris Done, Tadayasu Dotani, John Doty, Ken Ebisawa, Megan Eckart, Teruaki Enoto, Yuichiro Ezoe, Andrew Fabian, Carlo Ferrigno, Adam Foster, Ryuichi Fujimoto, Yasushi Fukazawa, Stefan Funk, Akihiro Furuzawa, Massimiliano Galeazzi, Luigi Gallo, Poshak Gandhi, Keith Gendreau, Kirk Gilmore, Daniel Haas, Yoshito Haba, Kenji Hamaguchi, Isamu Hatsukade, Takayuki Hayashi, Kiyoshi Hayashida, Junko Hiraga, Kazuyuki Hirose, Ann Hornschemeier, Akio Hoshino, John Hughes, Una Hwang, Ryo Iizuka, Yoshiyuki Inoue, Kazunori Ishibashi, Manabu Ishida, Kosei Ishimura, Yoshitaka Ishisaki, Masayuki Ito, Naoko Iwata, Naoko Iyomoto, Jelle Kaastra, Timothy Kallman, Tuneyoshi Kamae, Jun Kataoka, Satoru Katsuda, Hajime Kawahara, Madoka Kawaharada, Nobuyuki Kawai, Shigeo Kawasaki, Dmitry Khangaluyan, Caroline Kilbourne, Masashi Kimura, Kenzo Kinugasa, Shunji Kitamoto, Tetsu Kitayama, Takayoshi Kohmura, Motohide Kokubun, Tatsuro Kosaka, Alex Koujelev, Katsuji Koyama, Hans Krimm, Aya Kubota, Hideyo Kunieda, Stephanie LaMassa, Philippe Laurent, Francois Lebrun, Maurice Leutenegger, Olivier Limousin, Michael Loewenstein, Knox Long, David Lumb, Grzegorz Madejski, Yoshitomo Maeda, Kazuo Makishima, Genevieve Marchand, Maxim Markevitch, Hironori Matsumoto, Kyoko Matsushita, Dan McCammon, Brian McNamara, Jon Miller, Eric Miller, Shin Mineshige, Kenji Minesugi, Ikuyuki Mitsuishi, Takuya Miyazawa, Tsunefumi Mizuno, Hideyuki Mori, Koji Mori, Koji Mukai, Toshio Murakami, Hiroshi Murakami, Richard Mushotzky, Hosei Nagano, Ryo Nagino, Takao Nakagawa, Hiroshi Nakajima, Takeshi Nakamori, Kazuhiro Nakazawa, Yoshiharu Namba, Chikara Natsukari, Yusuke Nishioka, Masayoshi Nobukawa, Masaharu Nomachi, Steve O'Dell, Hirokazu Odaka, Hiroyuki Ogawa, Mina Ogawa, Keiji Ogi, Takaya Ohashi, Masanori Ohno, Masayuki Ohta, Takashi Okajima, Atsushi Okamoto, Tsuyoshi Okazaki, Naomi Ota, Masanobu Ozaki, Fritzs Paerels, Stéphane Paltani, Arvind Parmar, Robert Petre, Martin Pohl, F. Scott Porter, Brian Ramsey, Rubens Reis, Christopher Reynolds, Helen Russell, Samar Safi-Harb, Shin-ichiro Sakai, Hiroaki Sameshima, Jeremy Sanders, Goro Sato, Rie Sato, Yohichi Sato, Kosuke Sato, Makoto Sawada, Peter Serlemitsos, Hiromi Seta, Yasuko Shibano, Maki Shida, Takanobu Shimada, Keisuke Shinozaki, Peter Shirron, Aurora Simionescu, Cynthia Simmons, Randall Smith, Gary Sneiderman, Yang Soong, Lukasz Stawarz, Yasuharu Sugawara, Hiroyuki Sugita, Satoshi Sugita, Andrew Szymkowiak, Hiroyasu Tajima, Hiromitsu Takahashi, Shin-ichiro Takeda, Yoh Takei, Toru Tamagawa, Takayuki Tamura, Keisuke Tamura, Takaaki Tanaka, Yasuo Tanaka, Makoto Tashiro, Yuzuru Tawara, Yukikatsu Terada, Yuichi Terashima, Francesco Tombesi, Hiroshi Tomida, Yohko Tsuboi, Masahiro Tsujimoto, Hiroshi Tsunemi, Takeshi Tsuru, Hiroyuki Uchida, Yasunobu Uchiyama, Hideki Uchiyama, Yoshihiro Ueda, Shiro Ueno, Shinichiro Uno, Meg Urry, Eugenio Ursino, Cor de Vries, Atsushi Wada, Shin Watanabe, Norbert Werner, Nicholas White, Takahiro Yamada, Shinya Yamada, Hiroya Yamaguchi, Noriko Yamasaki, Shigeo Yamauchi, Makoto Yamauchi, Yoichi Yatsu, Daisuke Yonetoku, Atsumasa Yoshida, and Takayuki Yuasa

Subjects
Physics, Spectrometer, business.industry, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Detector, X-ray, Imaging spectrometer, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, law.invention, Telescope, Optics, Cardinal point, Settore FIS/05 - Astronomia e Astrofisica, law, Observatory, Spectral resolution, business, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The joint JAXA/NASA ASTRO-H mission is the sixth in a series of highly successful X-ray missions initiated by the Institute of Space and Astronautical Science (ISAS). ASTRO-H will investigate the physics of the high-energy universe via a suite of four instruments, covering a very wide energy range, from 0.3 keV to 600 keV. These instruments include a high-resolution, high-throughput spectrometer sensitive over 0.3-2 keV with high spectral resolution of Delta E < 7 eV, enabled by a micro-calorimeter array located in the focal plane of thin-foil X-ray optics; hard X-ray imaging spectrometers covering 5-80 keV, located in the focal plane of multilayer-coated, focusing hard X-ray mirrors; a wide-field imaging spectrometer sensitive over 0.4-12 keV, with an X-ray CCD camera in the focal plane of a soft X-ray telescope; and a non-focusing Compton-camera type soft gamma-ray detector, sensitive in the 40-600 keV band. The simultaneous broad bandpass, coupled with high spectral resolution, will enable the pursuit of a wide variety of important science themes., 22 pages, 17 figures, Proceedings of the SPIE Astronomical Instrumentation "Space Telescopes and Instrumentation 2012: Ultraviolet to Gamma Ray"

Published
2012

16. Live imaging of alveologenesis in precision-cut lung slices reveals dynamic epithelial cell behaviour

Author

Khondoker M. Akram, Laura L. Yates, Róisín Mongey, Stephen Rothery, David C. A. Gaboriau, Jeremy Sanderson, Matthew Hind, Mark Griffiths, and Charlotte H. Dean

Subjects
Science
Abstract

The process of alveologenesis is incompletely understood, partly due to the lack of applicable real-time imaging methods. Here the authors describe the process of alveologenesis and the behaviour of epithelial cells in real-time, using widefield microscopy and image deconvolution in precision-cut lung slices, revealing the dominant role of epithelial cell migration.

Published
2019
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17. In vitro and in vivo modeling of lipid bioaccessibility and digestion from almond muffins: The importance of the cell-wall barrier mechanism

Author

Terri Grassby, Giuseppina Mandalari, Myriam M.-L. Grundy, Cathrina H. Edwards, Carlo Bisignano, Domenico Trombetta, Antonella Smeriglio, Simona Chessa, Shuvra Ray, Jeremy Sanderson, Sarah E. Berry, Peter R. Ellis, and Keith W. Waldron

Subjects
Almonds, Bioaccessibility, Ileostomy, In vitro digestion, Particle size, Nutrition. Foods and food supply, TX341-641
Abstract

This study compares in vitro and in vivo models of lipid digestion from almond particles within a complex food matrix (muffins) investigating whether the cell-wall barrier regulates the bioaccessibility of nutrients within this matrix. Muffins containing small (AF) or large (AP) particles of almond were digested in triplicate using an in vitro dynamic gastric model (DGM, 1 h) followed by a static duodenal digestion (8 h). AF muffins had 97.1 ± 1.7% of their lipid digested, whereas AP muffins had 57.6 ± 1.1% digested. In vivo digestion of these muffins by an ileostomy volunteer (0–10 h) gave similar results with 96.5% and 56.5% lipid digested, respectively. The AF muffins produced a higher postprandial triacylglycerol iAUC response (by 61%) than the AP muffins. Microstructural analysis showed that some lipid remained encapsulated within the plant tissue throughout digestion. The cell-wall barrier mechanism is the main factor in regulating lipid bioaccessibility from almond particles.

Published
2017
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18. Time-lapse Imaging of Alveologenesis in Mouse Precision-cut Lung Slices

Author

Khondoker Akram, Laura Yates, Róisín Mongey, Stephen Rothery, David Gaboriau, Jeremy Sanderson, Matthew Hind, Mark Griffiths, and Charlotte Dean

Subjects
Biology (General), QH301-705.5
Abstract

Alveoli are the gas-exchange units of lung. The process of alveolar development, alveologenesis, is regulated by a complex network of signaling pathways that act on various cell types including alveolar type I and II epithelial cells, fibroblasts and the vascular endothelium. Dysregulated alveologenesis results in bronchopulmonary dysplasia in neonates and in adults, disrupted alveolar regeneration is associated with chronic lung diseases including COPD and pulmonary fibrosis. Therefore, visualizing alveologenesis is critical to understand lung homeostasis and for the development of effective therapies for incurable lung diseases. We have developed a technique to visualize alveologenesis in real-time using a combination of widefield microscopy and image deconvolution of precision-cut lung slices. Here, we describe this live imaging technique in step-by-step detail. This time-lapse imaging technique can be used to capture the dynamics of individual cells within tissue slices over a long time period (up to 16 h), with minimal loss of fluorescence or cell toxicity.

Published
2019
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19. Validating the RedMIT/GFP-LC3 Mouse Model by Studying Mitophagy in Autosomal Dominant Optic Atrophy Due to the OPA1Q285STOP Mutation

Author

Alan Diot, Thomas Agnew, Jeremy Sanderson, Chunyan Liao, Janet Carver, Ricardo Pires das Neves, Rajeev Gupta, Yanping Guo, Caroline Waters, Sharon Seto, Matthew J. Daniels, Eszter Dombi, Tiffany Lodge, Karl Morten, Suzannah A. Williams, Tariq Enver, Francisco J. Iborra, Marcela Votruba, and Joanna Poulton

Subjects
mitophagy, mouse model, OPA1, ADOA, mitochondrial fragmentation, high content imaging, Biology (General), QH301-705.5
Abstract

Background: Autosomal dominant optic atrophy (ADOA) is usually caused by mutations in the essential gene, OPA1. This encodes a ubiquitous protein involved in mitochondrial dynamics, hence tissue specificity is not understood. Dysregulated mitophagy (mitochondria recycling) is implicated in ADOA, being increased in OPA1 patient fibroblasts. Furthermore, autophagy may be increased in retinal ganglion cells (RGCs) of the OPA1Q285STOP mouse model.Aims: We developed a mouse model for studying mitochondrial dynamics in order to investigate mitophagy in ADOA.Methods: We crossed the OPA1Q285STOP mouse with our RedMIT/GFP-LC3 mouse, harboring red fluorescent mitochondria and green fluorescent autophagosomes. Colocalization between mitochondria and autophagosomes, the hallmark of mitophagy, was quantified in fluorescently labeled organelles in primary cell cultures, using two high throughput imaging methods Imagestream (Amnis) and IN Cell Analyzer 1000 (GE Healthcare Life Sciences). We studied colocalization between mitochondria and autophagosomes in fixed sections using confocal microscopy.Results: We validated our imaging methods for RedMIT/GFP-LC3 mouse cells, showing that colocalization of red fluorescent mitochondria and green fluorescent autophagosomes is a useful indicator of mitophagy. We showed that colocalization increases when lysosomal processing is impaired. Further, colocalization of mitochondrial fragments and autophagosomes is increased in cultures from the OPA1Q285STOP/RedMIT/GFP-LC3 mice compared to RedMIT/GFP-LC3 control mouse cells that were wild type for OPA1. This was apparent in both mouse embryonic fibroblasts (MEFs) using IN Cell 1000 and in splenocytes using ImageStream imaging flow cytometer (Amnis). We confirmed that this represents increased mitophagic flux using lysosomal inhibitors. We also used microscopy to investigate the level of mitophagy in the retina from the OPA1Q285STOP/RedMIT/GFP-LC3 mice and the RedMIT/GFP-LC3 control mice. However, the expression levels of fluorescent proteins and the image signal-to-background ratios precluded the detection of colocalization so we were unable to show any difference in colocalization between these mice.Conclusions: We show that colocalization of fluorescent mitochondria and autophagosomes in cell cultures, but not fixed tissues from the RedMIT/GFP-LC3, can be used to detect mitophagy. We used this model to confirm that mitophagy is increased in a mouse model of ADOA. It will be useful for cell based studies of diseases caused by impaired mitochondrial dynamics.

Published
2018
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20. Pooled sequencing of 531 genes in inflammatory bowel disease identifies an associated rare variant in BTNL2 and implicates other immune related genes.

Author

Natalie J Prescott, Benjamin Lehne, Kristina Stone, James C Lee, Kirstin Taylor, Jo Knight, Efterpi Papouli, Muddassar M Mirza, Michael A Simpson, Sarah L Spain, Grace Lu, Franca Fraternali, Suzannah J Bumpstead, Emma Gray, Ariella Amar, Hannah Bye, Peter Green, Guy Chung-Faye, Bu'Hussain Hayee, Richard Pollok, Jack Satsangi, Miles Parkes, Jeffrey C Barrett, John C Mansfield, Jeremy Sanderson, Cathryn M Lewis, Michael E Weale, Thomas Schlitt, Christopher G Mathew, and UK IBD Genetics Consortium

Subjects
Genetics, QH426-470
Abstract

The contribution of rare coding sequence variants to genetic susceptibility in complex disorders is an important but unresolved question. Most studies thus far have investigated a limited number of genes from regions which contain common disease associated variants. Here we investigate this in inflammatory bowel disease by sequencing the exons and proximal promoters of 531 genes selected from both genome-wide association studies and pathway analysis in pooled DNA panels from 474 cases of Crohn's disease and 480 controls. 80 variants with evidence of association in the sequencing experiment or with potential functional significance were selected for follow up genotyping in 6,507 IBD cases and 3,064 population controls. The top 5 disease associated variants were genotyped in an extension panel of 3,662 IBD cases and 3,639 controls, and tested for association in a combined analysis of 10,147 IBD cases and 7,008 controls. A rare coding variant p.G454C in the BTNL2 gene within the major histocompatibility complex was significantly associated with increased risk for IBD (p = 9.65x10-10, OR = 2.3[95% CI = 1.75-3.04]), but was independent of the known common associated CD and UC variants at this locus. Rare (T) or decreased risk (IL12B p.V298F, and NICN p.H191R) of IBD. These results provide additional insights into the involvement of the inhibition of T cell activation in the development of both sub-phenotypes of inflammatory bowel disease. We suggest that although rare coding variants may make a modest overall contribution to complex disease susceptibility, they can inform our understanding of the molecular pathways that contribute to pathogenesis.

Published
2015
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23. Effect of breadmaking process on in vitro gut microbiota parameters in irritable bowel syndrome.

Author

Adele Costabile, Sara Santarelli, Sandrine P Claus, Jeremy Sanderson, Barry N Hudspith, Jonathan Brostoff, Jane L Ward, Alison Lovegrove, Peter R Shewry, Hannah E Jones, Andrew M Whitley, and Glenn R Gibson

Subjects
Medicine, Science
Abstract

A variety of foods have been implicated in symptoms of patients with Irritable Bowel Syndrome (IBS) but wheat products are most frequently cited by patients as a trigger. Our aim was to investigate the effects of breads, which were fermented for different lengths of time, on the colonic microbiota using in vitro batch culture experiments. A set of in vitro anaerobic culture systems were run over a period of 24 h using faeces from 3 different IBS donors (Rome Criteria-mainly constipated) and 3 healthy donors. Changes in gut microbiota during a time course were identified by fluorescence in situ hybridisation (FISH), whilst the small-molecular weight metabolomic profile was determined by NMR analysis. Gas production was separately investigated in non pH-controlled, 36 h batch culture experiments. Numbers of bifidobacteria were higher in healthy subjects compared to IBS donors. In addition, the healthy donors showed a significant increase in bifidobacteria (P

Published
2014
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25. Guiding Inspiratory Flow: Development of the In-Check DIAL G16, a Tool for Improving Inhaler Technique

Author

Mark Jeremy Sanders

Subjects
Diseases of the respiratory system, RC705-779
Abstract

Portable inhalers are divisible into those that deliver medication by patient triggering (pMDIs: a gentle slow inhalation) and those that use the patient’s inspiratory effort as the force for deaggregation and delivery (DPIs: a stronger deeper inspiratory effort). Patient confusion and poor technique are commonplace. The use of training tools has become standard practice, and unique amongst these is an inspiratory flow meter (In-Check) which is able to simulate the resistance characteristics of different inhalers and, thereby, guide the patient to the correct effort. In-Check’s origins lie in the 1960s peak expiratory flow meters, the development of the Mini-Wright peak flow meter, and inspiratory flow assessment via the nose during the 1970s–1980s. The current device (In-Check DIAL G16) is the third iteration of the original 1998 training tool, with detailed and ongoing assessments of all common inhaler resistances (including combination and breath-actuated inhaler types) summarised into resistance ranges that are preset within the device. The device works by interpolating one of six ranges with the inspiratory effort. Use of the tool has been shown to be contributory to significant improvements in asthma care and control, and it is being advocated for assessment and training in irreversible lung disease.

Published
2017
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