Publications List for Carolin Crawford
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
The B3-VLA CSS Sample⋆
A&A 528, A110 (2011) Astronomy DOI: 10.1051/0004-6361/201015379 & c ESO 2011 Astrophysics The B3-VLA CSS sample VIII. New optical identifications from the Sloan Digital Sky Survey The ultraviolet-optical spectral energy distribution of the young radio sources C. Fanti1,R.Fanti1, A. Zanichelli1, D. Dallacasa1,2, and C. Stanghellini1 1 Istituto di Radioastronomia – INAF, via Gobetti 101, 40129 Bologna, Italy e-mail: [email protected] 2 Dipartimento di Astronomia, Università di Bologna, via Ranzani 1, 40127 Bologna, Italy Received 12 July 2010 / Accepted 22 December 2010 ABSTRACT Context. Compact steep-spectrum radio sources and giga-hertz peaked spectrum radio sources (CSS/GPS) are generally considered to be mostly young radio sources. In recent years we studied at many wavelengths a sample of these objects selected from the B3-VLA catalog: the B3-VLA CSS sample. Only ≈60% of the sources were optically identified. Aims. We aim to increase the number of optical identifications and study the properties of the host galaxies of young radio sources. Methods. We cross-correlated the CSS B3-VLA sample with the Sloan Digital Sky Survey (SDSS), DR7, and complemented the SDSS photometry with available GALEX (DR 4/5 and 6) and near-IR data from UKIRT and 2MASS. Results. We obtained new identifications and photometric redshifts for eight faint galaxies and for one quasar and two quasar candi- dates. Overall we have 27 galaxies with SDSS photometry in five bands, for which we derived the ultraviolet-optical spectral energy distribution (UV-O-SED). We extended our investigation to additional CSS/GPS selected from the literature. -
7.5 X 11.5.Doubleline.P65
Cambridge University Press 978-0-521-75618-1 - High Energy Astrophysics, Third Edition Malcolm S. Longair Index More information Name index Abell, George, 99, 101 Cappelluti, Nico, 729 Abraham, Robert, 733 Carter, Brandon, 434 Abramovitz, Milton, 206, 209 Caswell, James, 226 Adams, Fred, 353, 369 Cavaliere, Alfonso, 110 Amsler, Claude, 275 Cesarsky, Catherine, 187, 189 Anderson, Carl, 29, 30, 163 Challinor, Anthony, 115, 259 Arnaud, Monique, 110 Chandrasekhar, Subrahmanyan, 302, 429, 434, Arnett, David, 386 455 Arzoumanian, Zaven, 420 Charlot, Stephane,´ 729, 730, 747 Auger, Pierre, 29 Chwolson, O., 117 Cimatti, Andrea, 736, 748 Babbedge, T., 740 Clayton, Donald, 386 Backer, Donald, 417, 418 Clemmow, Phillip, 267 Bahcall, John, 55, 57, 58 Colless, Matthew, 108, 109 Bahcall, Neta, 105 Compton, Arthur, 231 Balbus, Steven, 455 Cordes, James, 420 Band, David, 264 Cowie, Lennox, 733, 736, 743, 745 Barger, Amy, 745 Cox, Donald, 357 Beckwith, Steven, 737, 744 Becquerel, Henri, 146 Damon, Paul, 297 Bekefi, George, 193 Davies, Rodney, 376 Bell(-Burnell), Jocelyn, 19, 406 Davis, Leverett, 373 Bennett, Charles, 16 Davis, Raymond, 32, 54, 55 Bethe, Hans, 57, 163, 166, 175 de Vaucouleurs, Gerard,´ 77, 78 Bignami, Giovanni, 197 Dermer, Charles, 505 Binney, James, 106, 153 Deubner, Franz-Ludwig, 51 Blaauw, Adriaan, 754 Diehl, Roland, 287 Blackett, Patrick, 29 Dirac, Adrian, 29 Blain, Andrew, 743 Djorgovski, George, 88 Bland-Hawthorn, Jonathan, 733 Dougherty, John, 267 Blandford, Roger, 251 Draine, Bruce, 351, 372, 373, 375, Blumenthal, George, 163, 175, -
Arxiv:1707.07134V1 [Astro-Ph.GA] 22 Jul 2017 2 Radio-Selected AGN
Astronomy Astrophysics Review manuscript No. (will be inserted by the editor) Active Galactic Nuclei: what’s in a name? P. Padovani · D. M. Alexander · R. J. Assef · B. De Marco · P. Giommi · R. C. Hickox · G. T. Richards · V. Smolciˇ c´ · E. Hatziminaoglou · V. Mainieri · M. Salvato Received: June 12, 2017 / Accepted: July 21, 2017 Abstract Active Galactic Nuclei (AGN) are energetic as- sic differences between AGN, and primarily reflect varia- trophysical sources powered by accretion onto supermassive tions in a relatively small number of astrophysical parame- black holes in galaxies, and present unique observational ters as well the method by which each class of AGN is se- signatures that cover the full electromagnetic spectrum over lected. Taken together, observations in different electromag- more than twenty orders of magnitude in frequency. The netic bands as well as variations over time provide comple- rich phenomenology of AGN has resulted in a large number mentary windows on the physics of different sub-structures of different “flavours” in the literature that now comprise a in the AGN. In this review, we present an overview of AGN complex and confusing AGN “zoo”. It is increasingly clear multi-wavelength properties with the aim of painting their that these classifications are only partially related to intrin- “big picture” through observations in each electromagnetic band from radio to γ-rays as well as AGN variability. We P. Padovani · E. Hatziminaoglou · V. Mainieri address what we can learn from each observational method, European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 the impact of selection effects, the physics behind the emis- Garching bei Munchen,¨ Germany sion at each wavelength, and the potential for future studies. -
Arxiv:Astro-Ph/9907379V1 27 Jul 1999
A subarcsecond resolution near-infrared study of Seyfert and ‘normal’ galaxies: II. Morphology Johan H. Knapen1 Isaac Shlosman2 Reynier F. Peletier3,4 1Department of Physical Sciences, University of Hertfordshire, Hatfield, Herts AL10 9AB, UK, E-mail: [email protected] 2 Department of Physics & Astronomy, University of Kentucky, Lexington, KY 40506-0055, USA, E-mail: [email protected] 3Dept. of Physics, University of Durham, South Road, Durham, DH1 3LE, UK 4School of Physics and Astronomy, University of Nottingham, Nottingham, NG7 2RD, UK, E-mail: [email protected] ABSTRACT We present a detailed study of the bar fraction in the CfA sample of Seyfert galaxies, and in a carefully selected control sample of non-active galaxies, to investigate the rela- tion between the presence of bars and of nuclear activity. To avoid the problems related to bar classification in the RC3, e.g., subjectivity, low resolution and contamination by dust, we have developed an objective bar classification method, which we conservatively apply to our new sub-arcsecond resolution near-infrared imaging data set (Peletier et al. 1999). We are able to use stringent criteria based on radial profiles of ellipticity and major axis position angle to determine the presence of a bar and its axial ratio. Concen- arXiv:astro-ph/9907379v1 27 Jul 1999 trating on non-interacting galaxies in our sample for which morphological information can be obtained, we find that Seyfert hosts are barred more often (79%±7.5%) than the non-active galaxies in our control sample (59%±9%), a result which is at the ∼ 2.5σ significance level. -
Not Yet Imagined: a Study of Hubble Space Telescope Operations
NOT YET IMAGINED A STUDY OF HUBBLE SPACE TELESCOPE OPERATIONS CHRISTOPHER GAINOR NOT YET IMAGINED NOT YET IMAGINED A STUDY OF HUBBLE SPACE TELESCOPE OPERATIONS CHRISTOPHER GAINOR National Aeronautics and Space Administration Office of Communications NASA History Division Washington, DC 20546 NASA SP-2020-4237 Library of Congress Cataloging-in-Publication Data Names: Gainor, Christopher, author. | United States. NASA History Program Office, publisher. Title: Not Yet Imagined : A study of Hubble Space Telescope Operations / Christopher Gainor. Description: Washington, DC: National Aeronautics and Space Administration, Office of Communications, NASA History Division, [2020] | Series: NASA history series ; sp-2020-4237 | Includes bibliographical references and index. | Summary: “Dr. Christopher Gainor’s Not Yet Imagined documents the history of NASA’s Hubble Space Telescope (HST) from launch in 1990 through 2020. This is considered a follow-on book to Robert W. Smith’s The Space Telescope: A Study of NASA, Science, Technology, and Politics, which recorded the development history of HST. Dr. Gainor’s book will be suitable for a general audience, while also being scholarly. Highly visible interactions among the general public, astronomers, engineers, govern- ment officials, and members of Congress about HST’s servicing missions by Space Shuttle crews is a central theme of this history book. Beyond the glare of public attention, the evolution of HST becoming a model of supranational cooperation amongst scientists is a second central theme. Third, the decision-making behind the changes in Hubble’s instrument packages on servicing missions is chronicled, along with HST’s contributions to our knowledge about our solar system, our galaxy, and our universe. -
Arxiv:1808.02136V2 [Astro-Ph.CO]
Correlations in the matter distribution in CLASH galaxy clusters Antonino Del Popoloa,b, Morgan Le Delliouc,d,∗, Xiguo Leee,1 aDipartimento di Fisica e Astronomia, University Of Catania, Viale Andrea Doria 6, 95125 Catania, Italy bINFN sezione di Catania, Via S. Sofia 64, I-95123 Catania, Italy cInstitute of Theoretical Physics, School of Physical Science and Technology, Lanzhou University, No.222, South Tianshui Road, Lanzhou, Gansu, 730000, Peoples Republic of China dInstituto de Astrof´sica e Ciˆencias do Espa¸co, Universidade de Lisboa, Faculdade de Ciencias, Ed. C8, Campo Grande, 1769-016 Lisboa, Portugal eInstitute of Modern Physics, Chinese Academy of Sciences, Post Office Box31, Lanzhou 730000, Peoples Republic of China Abstract We study the total and dark matter (DM) density profiles as well as their correlations for a sample of 15 high-mass galaxy clusters by extending our pre- vious work on several clusters from Newman et al. Our analysis focuses on 15 CLASH X-ray-selected clusters that have high-quality weak- and strong-lensing measurements from combined Subaru and Hubble Space Telescope observations. The total density profiles derived from lensing are interpreted based on the two- phase scenario of cluster formation. In this context, the brightest cluster galaxy (BCG) forms in the first dissipative phase, followed by a dissipationless phase where baryonic physics flattens the inner DM distribution. This results in the formation of clusters with modified DM distribution and several correlations between characteristic quantities of the clusters. We find that the central DM arXiv:1808.02136v2 [astro-ph.CO] 17 Jul 2019 density profiles of the clusters are strongly influenced by baryonic physics as found in our earlier work. -
Arxiv:1810.00890V2 [Astro-Ph.CO] 4 Jan 2019 Bologna, Italy 2 Stephen Walker Et Al
Noname manuscript No. (will be inserted by the editor) The Physics of Galaxy Cluster Outskirts Stephen Walker · Aurora Simionescu · Daisuke Nagai · Nobuhiro Okabe · Dominique Eckert · Tony Mroczkowski · Hiroki Akamatsu · Stefano Ettori · Vittorio Ghirardini Received: date / Accepted: date Stephen Walker Astrophysics Science Division, X-ray Astrophysics Laboratory, Code 662, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA E-mail: [email protected] Aurora Simionescu SRON, Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands Institute of Space and Astronautical Science (ISAS), JAXA, 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa, 252-5210, Japan Daisuke Nagai Department of Physics, Yale University, PO Box 208101, New Haven, CT, USA Yale Center for Astronomy and Astrophysics, PO Box 208101, New Haven, CT, USA Nobuhiro Okabe Department of Physical Science, Hiroshima University, 1-3-1 Kagamiyama, Higashi- Hiroshima, Hiroshima 739-8526, Japan Dominique Eckert Max-Planck-Institut f¨urextraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany Tony Mroczkowski European Southern Observatory (ESO), Karl-Schwarzschild-Str. 2, D-85748 Garching, Ger- many Hiroki Akamatsu SRON, Netherlands Institute for Space Research, Sorbonnelaan 2, 3584 CA Utrecht, The Netherlands Stefano Ettori INAF, Osservatorio di Astrofisica e Scienza dello Spazio, via Pietro Gobetti 93/3, 40129 Bologna, Italy INFN, Sezione di Bologna, viale Berti Pichat 6/2, I-40127 Bologna, Italy Vittorio Ghirardini Dipartimento di Fisica e Astronomia Universit di Bologna, Via Piero Gobetti, 93/2, 40129 Bologna, Italy INAF, Osservatorio di Astrofisica e Scienza dello Spazio, via Pietro Gobetti 93/3, 40129 arXiv:1810.00890v2 [astro-ph.CO] 4 Jan 2019 Bologna, Italy 2 Stephen Walker et al. -
Diffuse Radio Emission from Galaxy Clusters
Noname manuscript No. (will be inserted by the editor) Diffuse Radio Emission from Galaxy Clusters R. J. van Weeren · F. de Gasperin · H. Akamatsu · M. Br¨uggen · L. Feretti · H. Kang · A. Stroe · F. Zandanel Received: date / Accepted: date Abstract In a growing number of galaxy clusters dif- ICM. Cluster radio shocks (relics) are polarized sources fuse extended radio sources have been found. These mostly found in the cluster's periphery. They trace sources are not directly associated with individual clus- merger induced shock waves. Revived fossil plasma ter galaxies. The radio emission reveal the presence sources are characterized by their radio steep-spectra of cosmic rays and magnetic fields in the intracluster and often irregular morphologies. In this review we medium (ICM). We classify diffuse cluster radio sources give an overview of the properties of diffuse cluster ra- into radio halos, cluster radio shocks (relics), and re- dio sources, with an emphasis on recent observational vived AGN fossil plasma sources. Radio halo sources results. We discuss the resulting implications for the can be further divided into giant halos, mini-halos, underlying physical acceleration processes that oper- and possible \intermediate" sources. Halos are gener- ate in the ICM, the role of relativistic fossil plasma, ally positioned at cluster center and their brightness and the properties of ICM shocks and magnetic fields. approximately follows the distribution of the thermal We also compile an updated list of diffuse cluster ra- dio sources which will be available on-line (http:// galaxyclusters.com). We end this review with a dis- R. J. van Weeren cussion on the detection of diffuse radio emission from Leiden Observatory, Leiden University, PO Box 9513, 2300 the cosmic web. -
The Palermo Swift-BAT Hard X-Ray Catalogue
Astronomy & Astrophysics manuscript no. 15249 c ESO 2018 October 24, 2018 The Palermo Swift-BAT hard X-ray catalogue III. Results after 54 months of sky survey G. Cusumano1, V. La Parola1, A. Segreto1, C. Ferrigno1,2,3, A. Maselli1, B. Sbarufatti1, P. Romano1, G. Chincarini4,5, P. Giommi6, N. Masetti7, A. Moretti5, P. Parisi7,8, G. Tagliaferri5 1 INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, Via U. La Malfa 153, I-90146 Palermo, Italy 2 Institut f¨ur Astronomie und Astrophysik T¨ubingen (IAAT) 3 ISDC Data Centre for Astrophysics, Chemin d’Ecogia´ 16, CH-1290 Versoix, Switzerland 4 Universit`adegli studi di Milano-Bicocca, Dipartimento di Fisica, Piazza delle Scienze 3, I-20126 Milan, Italy 5 INAF – Osservatorio Astronomico di Brera, Via Bianchi 46, 23807 Merate, Italy 6 ASI Science Data Center, via Galileo Galilei, 00044 Frascati, Italy 7 INAF, Istituto di Astrofisica Spaziale e Fisica Cosmica di Bologna, via Gobetti 101, I-40129 Bologna, Italy 8 Dipartimento di Astronomia, Universit`adi Bologna, Via Ranzani 1, I-40127 Bologna, Italy ABSTRACT Aims. We present the Second Palermo Swift-BAT hard X-ray catalogue obtained by analysing data acquired in the first 54 months of the Swift mission. Methods. Using our software dedicated to the analysis of data from coded mask telescopes, we analysed the BAT survey data in three energy bands (15–30 keV, 15–70 keV, 15–150 keV), obtaining a list of 1256 detections above a significance threshold of 4.8 standard deviations. The identification of the source counterparts is pursued using two strategies: the analysis of field observations of soft X-ray instruments and cross-correlation of our catalogue with source databases. -
Arxiv:2011.11737V2 [Astro-Ph.HE] 15 Jan 2021
Draft version January 18, 2021 Typeset using LATEX twocolumn style in AASTeX63 The Radio Luminosity-Risetime Function of Core-Collapse Supernovae M. F. Bietenholz,1, 2 N. Bartel,2 M. Argo,3 R. Dua,4 S. Ryder,5, 6 and A. Soderberg7 1Hartebeesthoek Radio Astronomy Observatory, PO Box 443, Krugersdorp, 1740, South Africa 2Department of Physics and Astronomy, York University, Toronto, M3J 1P3, Ontario, Canada 3Jeremiah Horrocks Institute, University of Central Lancashire, Preston PR1 2HE, UK 4Birla Institute of Technology and Science, Pilani Campus, Pilani, India 5Dept. of Physics & Astronomy, Macquarie University, NSW 2109, Australia 6Astronomy, Astrophysics and Astrophotonics Research Centre, Macquarie University, Sydney, NSW 2109, Australia 7formerly at Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA (Accepted for publication in the Atrophysical Journal, January 18, 2021) ABSTRACT We assemble a large set of 2{10 GHz radio flux density measurements and upper limits of 294 different supernovae (SNe), from the literature and our own and archival data. Only 31% of SNe were detected. We characterize the SN radio lightcurves near the peak using a two-parameter model, with tpk being the time to rise to a peak and Lpk the spectral luminosity at that peak. Over all SNe in 1:7±0:9 25:5±1:6 −1 −1 our sample at D < 100 Mpc, we find that tpk = 10 d, and that Lpk = 10 erg s Hz , 25:5 −1 −1 and therefore that generally, 50% of SNe will have Lpk < 10 erg s Hz . These Lpk values are ∼30 times lower than those for only detected SNe. -
A Submillimetre Selected Quasar in the Field of Abell
A&A 411, 343–350 (2003) Astronomy DOI: 10.1051/0004-6361:20031291 & c ESO 2003 Astrophysics A submillimetre selected quasar in the field of Abell 478 K. K. Knudsen, P. P. van der Werf, and W. Jaffe Leiden Observatory, PO Box 9513, 2300 RA Leiden, The Netherlands e-mail: [kraiberg,pvdwerf,jaffe]@strw.leidenuniv.nl Received 4 June 2003 / Accepted 21 August 2003 Abstract. We present the discovery of a dusty quasar, SMM J04135+10277, located behind the galaxy cluster Abell 478. The quasar was discovered as the brightest source in a submillimetre survey of high redshift galaxies lensed by foreground rich clusters of galaxies in a project aimed at studying the cosmic star formation history of dusty galaxies. With submillimetre fluxes of S 850 = 25 ± 2.8mJyandS 450 = 55 ± 17 mJy this object is one of the brightest submillimetre sources known. Optical imaging revealed a point source with I = 19.4 ± 0.1 mag (corrected for galactic extinction). Follow-up optical spectroscopy showed this object to be a quasar at redshift z = 2.837 ± 0.003. The quasar was also detected at shorter infrared wavelengths with the Infrared Space Observatory. This object is the first quasar discovered by its submillimetre emission. Given the general lack of overlap between deep submillimetre and X-ray samples, usually interpreted as a low incidence of active nuclei in submillimetre samples, this is an unusual object. Analysis of number counts of quasars and of submillimetre galaxies bears out this suggestion. We compare the properties of SMM J04135+10277 to those of optically selected quasars with submillimetre emission, and argue that the optical faintness results from a large viewing angle with the direction of relativistic beaming, and not from abnormally high extinction. -
ASTRO-H White Paper-Clusters of Galaxies and Related Science
ASTRO-H Space X-ray Observatory White Paper Clusters of Galaxies and Related Science T. Kitayama (Toho University), M. Bautz (MIT), M. Markevitch (NASA/GSFC), K. Matsushita (Tokyo University of Science), S. Allen (Stanford University), M. Kawaharada (JAXA), B. McNamara (University of Waterloo), N. Ota (Nara Women’s University), H. Akamatsu (SRON), J. de Plaa (SRON), M. Galeazzi (University of Miami), G. Madejski (Stanford University), R. Main (University of Waterloo), E. Miller (MIT), K. Nakazawa (University of Tokyo), H. Russel (University of Waterloo1), K. Sato (Tokyo University of Science), N. Sekiya (JAXA/University of Tokyo), A. Simionescu (JAXA), T. Tamura (JAXA), Y. Uchida (JAXA/University of Tokyo), E. Ursino (University of Miami), N. Werner (Stanford University), I. Zhuravleva (Stanford University), and J. ZuHone (NASA/GSFC) on behalf of the ASTRO-H Science Working Group Abstract The next generation X-ray observatory ASTRO-H will open up a new dimension in the study of galaxy clusters by achieving for the first time the spectral resolution required to measure velocities of the intracluster plasma, and extending at the same time the spectral coverage to energies well beyond 10 keV. This white paper provides an overview of the capabilities of ASTRO-H for exploring gas motions in galaxy clusters including their cosmological implications, the physics of AGN feedback, dynamics of cluster mergers as well as associated high-energy processes, chemical enrichment of the intracluster medium, and the nature of missing baryons and unidentified