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Publications for Dr. Peter L. Capak 1 of 21 Publication Summary 369
Publications for Dr. Peter L. Capak Publication Summary 369 Publications 319 Refereed Publications Accepted or Submitted 50 Un-refereed Publications Top 1% of Cited Researchers in 2017-2019 >30,000 Citations >1,600 Citations on first author papers 99 papers with >100 citations, 6 as first author. H Index = 99 First Author publications 1) Capak et al., 2015, “Galaxies at redshifts 5 to 6 with systematically low dust content and high [C II] emission”, Nature, 522, 455 2) Capak et al., 2013, “Keck-I MOSFIRE Spectroscopy of the z ~ 12 Candidate Galaxy UDFj-39546284”, ApJL, 733, 14 3) Capak et al., 2011, “A massive protocluster of galaxies at a redshift of z~5.3” , Nature, 470, 233 4) Capak et al., 2010, “Spectroscopy and Imaging of three bright z>7 candidates in the COSMOS survey”, ApJ, 730, 68 5) Capak et al., 2008, "Spectroscopic Confirmation Of An Extreme Starburst At Redshift 4.547", ApJL, 681, 53 6) Capak et. al., 2007, "The effects of environment on morphological evolution between 0<z<1.2 in the COSMOS Survey", ApJS, 172, 284 7) Capak et. al., 2007, "The First Release COSMOS Optical and Near-IR Data and Catalog", ApJS, 172, 99 8) Capak, 2004, “Probing global star and galaxy formation using deep multi-wavelength surveys”, Ph.D. Thesis 9) Capak et. al., 2004, "A Deep Wide-Field, Optical, and Near-Infrared Catalog of a Large Area around the Hubble Deep Field North", AJ, 127, 180 Other Publications (P. Capak was a leading author in bolded entries) 10) Faisst et al., 2020, “The ALPINE-ALMA [CII] survey: Multi-Wavelength Ancillary Data. -
Source-Plane Reconstruction of the Giant Gravitational Arc in A2667: a Candidate Wolf–Rayet Galaxy At
SOURCE-PLANE RECONSTRUCTION OF THE GIANT GRAVITATIONAL ARC IN A2667: A CANDIDATE WOLF–RAYET GALAXY AT z ∼ 1 Shuo Cao, Giovanni Covone, Eric Jullo, Johan Richard, Luca Izzo, Zong-Hong Zhu To cite this version: Shuo Cao, Giovanni Covone, Eric Jullo, Johan Richard, Luca Izzo, et al.. SOURCE-PLANE RE- CONSTRUCTION OF THE GIANT GRAVITATIONAL ARC IN A2667: A CANDIDATE WOLF– RAYET GALAXY AT z ∼ 1. Astronomical Journal, American Astronomical Society, 2015, 149, pp.8. 10.1088/0004-6256/149/1/3. hal-01109685 HAL Id: hal-01109685 https://hal.archives-ouvertes.fr/hal-01109685 Submitted on 26 Jan 2015 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. The Astronomical Journal, 149:3 (8pp), 2015 January doi:10.1088/0004-6256/149/1/3 C 2015. The American Astronomical Society. All rights reserved. SOURCE-PLANE RECONSTRUCTION OF THE GIANT GRAVITATIONAL ARC IN A2667: A CANDIDATE WOLF–RAYET GALAXY AT z ∼ 1 Shuo Cao1,2, Giovanni Covone2,3, Eric Jullo4, Johan Richard5, Luca Izzo6,7, and Zong-Hong Zhu1 1 Department of Astronomy, Beijing Normal University, 100875 Beijing, China; [email protected] 2 Dipartimento di Scienze Fisiche, Universita` di Napoli “Federico II,” Via Cinthia, I-80126 Napoli, Italy 3 INFN Sez. -
POSTERS SESSION I: Atmospheres of Massive Stars
Abstracts of Posters 25 POSTERS (Grouped by sessions in alphabetical order by first author) SESSION I: Atmospheres of Massive Stars I-1. Pulsational Seeding of Structure in a Line-Driven Stellar Wind Nurdan Anilmis & Stan Owocki, University of Delaware Massive stars often exhibit signatures of radial or non-radial pulsation, and in principal these can play a key role in seeding structure in their radiatively driven stellar wind. We have been carrying out time-dependent hydrodynamical simulations of such winds with time-variable surface brightness and lower boundary condi- tions that are intended to mimic the forms expected from stellar pulsation. We present sample results for a strong radial pulsation, using also an SEI (Sobolev with Exact Integration) line-transfer code to derive characteristic line-profile signatures of the resulting wind structure. Future work will compare these with observed signatures in a variety of specific stars known to be radial and non-radial pulsators. I-2. Wind and Photospheric Variability in Late-B Supergiants Matt Austin, University College London (UCL); Nevyana Markova, National Astronomical Observatory, Bulgaria; Raman Prinja, UCL There is currently a growing realisation that the time-variable properties of massive stars can have a funda- mental influence in the determination of key parameters. Specifically, the fact that the winds may be highly clumped and structured can lead to significant downward revision in the mass-loss rates of OB stars. While wind clumping is generally well studied in O-type stars, it is by contrast poorly understood in B stars. In this study we present the analysis of optical data of the B8 Iae star HD 199478. -
Does the Fornax Dwarf Spheroidal Have a Central Cusp Or Core?
Research Collection Journal Article Does the Fornax dwarf spheroidal have a central cusp or core? Author(s): Goerdt, Tobias; Moore, Ben; Read, J.I.; Stadel, Joachim; Zemp, Marcel Publication Date: 2006-05 Permanent Link: https://doi.org/10.3929/ethz-b-000024289 Originally published in: Monthly Notices of the Royal Astronomical Society 368(3), http://doi.org/10.1111/ j.1365-2966.2006.10182.x Rights / License: In Copyright - Non-Commercial Use Permitted This page was generated automatically upon download from the ETH Zurich Research Collection. For more information please consult the Terms of use. ETH Library Mon. Not. R. Astron. Soc. 368, 1073–1077 (2006) doi:10.1111/j.1365-2966.2006.10182.x Does the Fornax dwarf spheroidal have a central cusp or core? , Tobias Goerdt,1 Ben Moore,1 J. I. Read,1 Joachim Stadel1 and Marcel Zemp1 2 1Institute for Theoretical Physics, University of Zurich,¨ Winterthurerstrasse 190, CH-8057 Zurich,¨ Switzerland 2Institute of Astronomy, ETH Zurich,¨ ETH Honggerberg¨ HPF D6, CH-8093 Zurich,¨ Switzerland Accepted 2006 February 8. Received 2006 February 7; in original form 2005 December 21 ABSTRACT The dark matter dominated Fornax dwarf spheroidal has five globular clusters orbiting at ∼1 kpc from its centre. In a cuspy cold dark matter halo the globulars would sink to the centre from their current positions within a few Gyr, presenting a puzzle as to why they survive undigested at the present epoch. We show that a solution to this timing problem is to adopt a cored dark matter halo. We use numerical simulations and analytic calculations to show that, under these conditions, the sinking time becomes many Hubble times; the globulars effectively stall at the dark matter core radius. -
Archons (Commanders) [NOTICE: They Are NOT Anlien Parasites], and Then, in a Mirror Image of the Great Emanations of the Pleroma, Hundreds of Lesser Angels
A R C H O N S HIDDEN RULERS THROUGH THE AGES A R C H O N S HIDDEN RULERS THROUGH THE AGES WATCH THIS IMPORTANT VIDEO UFOs, Aliens, and the Question of Contact MUST-SEE THE OCCULT REASON FOR PSYCHOPATHY Organic Portals: Aliens and Psychopaths KNOWLEDGE THROUGH GNOSIS Boris Mouravieff - GNOSIS IN THE BEGINNING ...1 The Gnostic core belief was a strong dualism: that the world of matter was deadening and inferior to a remote nonphysical home, to which an interior divine spark in most humans aspired to return after death. This led them to an absorption with the Jewish creation myths in Genesis, which they obsessively reinterpreted to formulate allegorical explanations of how humans ended up trapped in the world of matter. The basic Gnostic story, which varied in details from teacher to teacher, was this: In the beginning there was an unknowable, immaterial, and invisible God, sometimes called the Father of All and sometimes by other names. “He” was neither male nor female, and was composed of an implicitly finite amount of a living nonphysical substance. Surrounding this God was a great empty region called the Pleroma (the fullness). Beyond the Pleroma lay empty space. The God acted to fill the Pleroma through a series of emanations, a squeezing off of small portions of his/its nonphysical energetic divine material. In most accounts there are thirty emanations in fifteen complementary pairs, each getting slightly less of the divine material and therefore being slightly weaker. The emanations are called Aeons (eternities) and are mostly named personifications in Greek of abstract ideas. -
Highlights and Discoveries from the Chandra X-Ray Observatory1
Highlights and Discoveries from the Chandra X-ray Observatory1 H Tananbaum1, M C Weisskopf2, W Tucker1, B Wilkes1 and P Edmonds1 1Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, MA 02138. 2 NASA/Marshall Space Flight Center, ZP12, 320 Sparkman Drive, Huntsville, AL 35805. Abstract. Within 40 years of the detection of the first extrasolar X-ray source in 1962, NASA’s Chandra X-ray Observatory has achieved an increase in sensitivity of 10 orders of magnitude, comparable to the gain in going from naked-eye observations to the most powerful optical telescopes over the past 400 years. Chandra is unique in its capabilities for producing sub-arcsecond X-ray images with 100-200 eV energy resolution for energies in the range 0.08<E<10 keV, locating X-ray sources to high precision, detecting extremely faint sources, and obtaining high resolution spectra of selected cosmic phenomena. The extended Chandra mission provides a long observing baseline with stable and well-calibrated instruments, enabling temporal studies over time-scales from milliseconds to years. In this report we present a selection of highlights that illustrate how observations using Chandra, sometimes alone, but often in conjunction with other telescopes, have deepened, and in some instances revolutionized, our understanding of topics as diverse as protoplanetary nebulae; massive stars; supernova explosions; pulsar wind nebulae; the superfluid interior of neutron stars; accretion flows around black holes; the growth of supermassive black holes and their role in the regulation of star formation and growth of galaxies; impacts of collisions, mergers, and feedback on growth and evolution of groups and clusters of galaxies; and properties of dark matter and dark energy. -
The Orbital Motion of the Quintuplet Cluster—A Common Origin for the Arches and Quintuplet Clusters?∗
The Astrophysical Journal, 789:115 (20pp), 2014 July 10 doi:10.1088/0004-637X/789/2/115 C 2014. The American Astronomical Society. All rights reserved. Printed in the U.S.A. THE ORBITAL MOTION OF THE QUINTUPLET CLUSTER—A COMMON ORIGIN FOR THE ARCHES AND QUINTUPLET CLUSTERS?∗ A. Stolte1,B.Hußmann1, M. R. Morris2,A.M.Ghez2, W. Brandner3,J.R.Lu4, W. I. Clarkson5, M. Habibi1, and K. Matthews6 1 Argelander Institut fur¨ Astronomie, Auf dem Hugel¨ 71, D-53121 Bonn, Germany; [email protected] 2 Division of Astronomy and Astrophysics, UCLA, Los Angeles, CA 90095-1547, USA; [email protected], [email protected] 3 Max-Planck-Institut fur¨ Astronomie, Konigstuhl¨ 17, D-69117 Heidelberg, Germany; [email protected] 4 Institute for Astronomy, University of Hawai’i, 2680 Woodlawn Drive, Honolulu, HI 96822, USA; [email protected] 5 Department of Natural Sciences, University of Michigan-Dearborn, 125 Science Building, 4901 Evergreen Road, Dearborn, MI 48128, USA; [email protected] 6 Caltech Optical Observatories, California Institute of Technology, MS 320-47, Pasadena, CA 91225, USA; [email protected] Received 2014 January 16; accepted 2014 May 14; published 2014 June 20 ABSTRACT We investigate the orbital motion of the Quintuplet cluster near the Galactic center with the aim of constraining formation scenarios of young, massive star clusters in nuclear environments. Three epochs of adaptive optics high-angular resolution imaging with the Keck/NIRC2 and Very Large Telescope/NAOS-CONICA systems were obtained over a time baseline of 5.8 yr, delivering an astrometric accuracy of 0.5–1 mas yr−1. -
X-Ray Jets Aneta Siemiginowska
Chandra News Issue 21 Spring 2014 Published by the Chandra X-ray Center (CXC) X-ray Jets Aneta Siemiginowska The Active Galaxy 4C+29.30 Credit: X-ray: NASA/CXC/SAO/A.Siemiginowska et al; Optical: NASA/STScI; Radio: NSF/NRAO/VLA Contents X-ray Jets HETG 3 Aneta Siemiginowska 18 David Huenemoerder (for the HETG team) 10 Project Scientist’s Report 20 LETG Martin Weisskopf Jeremy Drake 11 Project Manager’s Report 23 Chandra Calibration Roger Brissenden Larry David Message of Thanks to Useful Web Addresses 12 Harvey Tananbaum 23 The Chandra Team Belinda Wilkes Appointed as CIAO 4.6 13 Director of the CXC 24 Antonella Fruscione, for the CIAO Team Of Programs and Papers: Einstein Postdoctoral Fellowship 13 Making the Chandra Connection 29 Program Sherry Winkelman & Arnold Rots Andrea Prestwich Chandra Related Meetings Cycle 14 Peer Review Results 14 and Important Dates 30 Belinda Wilkes ACIS Chandra Users’ Committee 14 Paul Plucinsky, Royce Buehler, 34 Membership List Gregg Germain, & Richard Edgar HRC CXC 2013 Science Press 15 Ralph Kraft, Hans Moritz Guenther 35 Releases (SAO), and Wolfgang Pietsch (MPE) Megan Watzke The Chandra Newsletter appears once a year and is edited by Paul J. Green, with editorial assistance and layout by Evan Tingle. We welcome contributions from readers. Comments on the newsletter, or corrections and additions to the hardcopy mailing list should be sent to: [email protected]. Spring, 2014 3 X-ray Jets many unanswered questions, including the nature of relativistic jets, jet energetics, particle content, parti- Aneta Siemiginowska cle acceleration and emission processes. Both statis- tical studies of large samples of jets across the entire The first recorded observation of an extragalac- electromagnetic spectrum and deep broad-band imag- tic jet was made almost a century ago. -
THE MAGELLANIC CLOUDS NEWSLETTER an Electronic Publication Dedicated to the Magellanic Clouds, and Astrophysical Phenomena Therein
THE MAGELLANIC CLOUDS NEWSLETTER An electronic publication dedicated to the Magellanic Clouds, and astrophysical phenomena therein No. 115 — 2 February 2012 http://www.astro.keele.ac.uk/MCnews Editor: Jacco van Loon Figure 1: The Small Magellanic Cloud and Galactic globular cluster 47 Tucanae, two of the most beautiful objects in the Southern sky (from Kalirai et al. 2012; South is up and East is to the right). Image courtesy of and c Stephane Guisard, http://www.astrosurf.com/sguisard 1 Editorial Dear Colleagues, It is my pleasure to present you the 115th issue of the Magellanic Clouds Newsletter. There is a lot of attention to star clusters, pulsating stars, binary stars, and the dynamics of the Magellanic System; don’t miss some of the very interesting proceedings papers. It is not yet too late to register for the workshop on mass return from stars to galaxies, at STScI in March, but abstracts need to be in by 3 February (!): http://www.stsci.edu/institute/conference/mass-loss-return The next meeting which should be of interest to readers of this newsletter, is the Magellanic Clouds meeting in Perth, Australia in September – see the announcement at the end of the newsletter for more details. Thanks to those of you who supplied illustrations for this issue. They remain welcome. Also, don’t hesitate to use the ”announcement” type of submission to post results, ideas, requests for observations, et cetera. This is a forum, for discussion and collaboration. The next issue is planned to be distributed on the 1st of April 2012. -
Corporate Rating Component Scores North America Q4 2020
Corporate Rating Component Scores North America Q4 2020 FALSE NA Corporate Rating Component Scores Oct. 31, 2020 Corporate Rating Component Scores North America Methodology," which is the criteria we use for rating corporate industrial companies and utilities. We list the scores for the 2308 public ratings in NA that are within the scope of our corporate methodology, accompanied by charts that show the distribution of aggregated scores. We believe that the list and charts enhance benchmarking across industries and rating levels for all market participants. We disclose these scores in line with the information we provide in our rating research publications, such as research updates and full analyses. By releasing all scores for public corporate ratings in NA, S&P Global Ratings confirms its commitment to deliver greater transparency and insight into the ratings process and simplify access for all market participants. Ratings are organized alphabetically by industry sector. The scores reflect the building blocks of the corporate ratings framework (see chart 1). Modifiers and components related to our group rating methodology or government-related entity methodology are indicated only where they have a positive or negative effect on the rating. The report reflects corporate credit ratings and scores as of Oct. 31, 2020. This document will not be updated for future rating actions or score revisions. To keep it concise, the list only discloses scores for the main rated entity of larger corporate groups. We omit certain entities such as subsidiaries or holding companies where the ratings are linked to those on their parent companies. In this report, we highlight changes since Jan. -
121012-AAS-221 Program-14-ALL, Page 253 @ Preflight
221ST MEETING OF THE AMERICAN ASTRONOMICAL SOCIETY 6-10 January 2013 LONG BEACH, CALIFORNIA Scientific sessions will be held at the: Long Beach Convention Center 300 E. Ocean Blvd. COUNCIL.......................... 2 Long Beach, CA 90802 AAS Paper Sorters EXHIBITORS..................... 4 Aubra Anthony ATTENDEE Alan Boss SERVICES.......................... 9 Blaise Canzian Joanna Corby SCHEDULE.....................12 Rupert Croft Shantanu Desai SATURDAY.....................28 Rick Fienberg Bernhard Fleck SUNDAY..........................30 Erika Grundstrom Nimish P. Hathi MONDAY........................37 Ann Hornschemeier Suzanne H. Jacoby TUESDAY........................98 Bethany Johns Sebastien Lepine WEDNESDAY.............. 158 Katharina Lodders Kevin Marvel THURSDAY.................. 213 Karen Masters Bryan Miller AUTHOR INDEX ........ 245 Nancy Morrison Judit Ries Michael Rutkowski Allyn Smith Joe Tenn Session Numbering Key 100’s Monday 200’s Tuesday 300’s Wednesday 400’s Thursday Sessions are numbered in the Program Book by day and time. Changes after 27 November 2012 are included only in the online program materials. 1 AAS Officers & Councilors Officers Councilors President (2012-2014) (2009-2012) David J. Helfand Quest Univ. Canada Edward F. Guinan Villanova Univ. [email protected] [email protected] PAST President (2012-2013) Patricia Knezek NOAO/WIYN Observatory Debra Elmegreen Vassar College [email protected] [email protected] Robert Mathieu Univ. of Wisconsin Vice President (2009-2015) [email protected] Paula Szkody University of Washington [email protected] (2011-2014) Bruce Balick Univ. of Washington Vice-President (2010-2013) [email protected] Nicholas B. Suntzeff Texas A&M Univ. suntzeff@aas.org Eileen D. Friel Boston Univ. [email protected] Vice President (2011-2014) Edward B. Churchwell Univ. of Wisconsin Angela Speck Univ. of Missouri [email protected] [email protected] Treasurer (2011-2014) (2012-2015) Hervey (Peter) Stockman STScI Nancy S. -
The Future Exploration of Saturn 417-441, in Saturn in the 21St Century (Eds. KH Baines, FM Flasar, N Krupp, T Stallard)
The Future Exploration of Saturn By Kevin H. Baines, Sushil K. Atreya, Frank Crary, Scott G. Edgington, Thomas K. Greathouse, Henrik Melin, Olivier Mousis, Glenn S. Orton, Thomas R. Spilker, Anthony Wesley (2019). pp 417-441, in Saturn in the 21st Century (eds. KH Baines, FM Flasar, N Krupp, T Stallard), Cambridge University Press. https://doi.org/10.1017/9781316227220.014 14 The Future Exploration of Saturn KEVIN H. BAINES, SUSHIL K. ATREYA, FRANK CRARY, SCOTT G. EDGINGTON, THOMAS K. GREATHOUSE, HENRIK MELIN, OLIVIER MOUSIS, GLENN S. ORTON, THOMAS R. SPILKER AND ANTHONY WESLEY Abstract missions, achieving a remarkable record of discoveries Despite the lack of another Flagship-class mission about the entire Saturn system, including its icy satel- such as Cassini–Huygens, prospects for the future lites, the large atmosphere-enshrouded moon Titan, the ’ exploration of Saturn are nevertheless encoura- planet s surprisingly intricate ring system and the pla- ’ ging. Both NASA and the European Space net s complex magnetosphere, atmosphere and interior. Agency (ESA) are exploring the possibilities of Far from being a small (500 km diameter) geologically focused interplanetary missions (1) to drop one or dead moon, Enceladus proved to be exceptionally more in situ atmospheric entry probes into Saturn active, erupting with numerous geysers that spew – and (2) to explore the satellites Titan and liquid water vapor and ice grains into space some of fi Enceladus, which would provide opportunities for which falls back to form nearly pure white snow elds both in situ investigations of Saturn’s magneto- and some of which escapes to form a distinctive ring sphere and detailed remote-sensing observations around Saturn (e.g.