The Galaxy Viewed at Very Short Time-Scales with the Berkeley Visible Image Tube (BVIT)
|
|
- Piers Newman
- 5 years ago
- Views:
Transcription
1 The Galaxy Viewed at Very Short Time-Scales with the Berkeley Visible Image Tube (BVIT) Barry Y. Welsh, O.H.W. Siegmund, J. McPhate, D. Rogers & J.V. Vallerga Space Sciences Laboratory University of California, Berkeley, CA
2 What is BVIT? The Berkeley Visible Imaging Tube (BVIT) is a visible microchannel plate photon counting detector designed to provide observers with very high time resolution imaging photometry. Enables a new time domain for astronomical observations with full imaging capability Time resolution (for each detected photon) ~ 100 picosec BVIT is a simple instrument with minimal observational setup requirements and a high degree of post acquisition data flexibility. Designed as a user facility instrument only available at the 10m South African Large Telescope (SALT)
3 Microchannel Plate Detectors γ Tube Window with photocathode MCP stack Charge distribution on strips Charge Cloud Very similar detectors are currently in-orbit on NASA s GALEX UV astronomy mission and COS on Hubble
4 Microchannel Plate Detectors Photocathode converts photon to electron γ Tube Window with photocathode MCP stack Charge distribution on strips Charge Cloud Very similar detectors are currently in-orbit on NASA s GALEX UV astronomy mission and COS on Hubble
5 Microchannel Plate Detectors Photocathode converts photon to electron γ Tube Window with photocathode MCP(s) amplify electron by 10 4 to 10 8 MCP stack Charge distribution on strips Charge Cloud Very similar detectors are currently in-orbit on NASA s GALEX UV astronomy mission and COS on Hubble
6 Microchannel Plate Detectors Photocathode converts photon to electron γ Tube Window with photocathode MCP(s) amplify electron by 10 4 to 10 8 Rear field accelerates electrons to anode MCP stack Charge distribution on strips Charge Cloud Very similar detectors are currently in-orbit on NASA s GALEX UV astronomy mission and COS on Hubble
7 Microchannel Plate Detectors Photocathode converts photon to electron γ Tube Window with photocathode MCP(s) amplify electron by 10 4 to 10 8 Rear field accelerates electrons to anode MCP stack Patterned anode measures charge centroid (X,Y) and time of photon arrival Charge distribution on strips Charge Cloud Very similar detectors are currently in-orbit on NASA s GALEX UV astronomy mission and COS on Hubble
8 Cross Delay-Line Anode Image Tube GaAs SuperGenII Photocathode Q.E. Cross-Delay Line Anode Test mask 10µm pinholes on 500µm centers. 30µm resolution.
9 BVIT Demo System on SALT (Jan 2009) The Berkeley-SAAO team carried out a commissioning/ engineering test-run with the BVIT installed on SALT for 10 nights in January A further 7 nights observations were performed by SAAO staff in March The BVIT detector The BVIT on SALT at prime focus
10 THE BVIT Instrument Package on SALT B &V + ND Filter Wheels + Shutter & BVIT HVPS Filter wheel controllers TDC electronics PC LVPS BVIT F.O.V = 1.9 arc min (enables source & comparison star observations)
11 The BVIT Demo Detector System Resolution Command, Control & real time Display Software for BVIT BVIT 25mm tube with amp and (in rack) TDC and HVPS
12 BVIT Observations on SALT Observations were carried out for a wide variety of astronomical objects in order to investigate which types were best suited for future in-depth study Objects included QSO s, AGN, Spiral galaxies, Globular Clusters, Flare Stars, CV systems, Low-Mass X-ray Binaries, Pulsars, asteroid transits Observational & instrumental constraints restricted observations to targets with 12.5 < Vmag < 22.0 Some objects (CV systems) were simultaneously observed with the SAAO 74 inch telescope + hi-speed photometer by Dr. Steve Potter During the March run, the black hole candidate GX (Vmag =15.5) was also observed with SALTICAM in order to compare data sets The BVIT+SALT observing efficiency was 58%, which is the highest value yet achieved with the SALT 10m telescope!
13 The SALT facility Both the Hobby-Eberly and SALT telescopes have had more than their fair share of engineering problems. SALT is presently closed for 3 months to re-engineer its tracking system Our data was taken when the tracking system had glitches and the multisegment mirror focus system had problems The effect of these facility problems resulted in stellar images suddenly going in and out of focus, and the stellar image sometimes moving several arc seconds during an exposure. The photon counting capability of BVIT, in which every photon is assigned an X,Y and t, meant that neither of these instrumental anomalies was a problem for data reduction. Note that SALT cannot produce accurate photometric fluxes
14 Source, Background and Comparison Star Plots (time versus counts)
15 Samples of BVIT Reduced Data: X-ray Transients Low-mass X-ray binaries are systems that include a low-mass companion that transfers material onto a neutron star or black hole. Most LMXRB systems have orbital periods of a few hours to days and XRT s undergo significant X-ray, optical and radio outbursts separated by long periods of quiescence Little information is currently known about short-time scale non-orbital emission variations in the optical. Although optical bursts generally lag behind those observed in X-rays (by re-processing), in several cases the optical burst emission LEADS the X-ray emission (perhaps due to synchrotron emission from a jet). (see Gandhi et al 2008) We observed the X-ray nova GX in the B-band with BVIT on SALT for ~ 500sec with the data shown here in 0.1 sec bins
16 GX 339-4: Black Hole candidate data binned at 0.1 sec X-ray Transients with BVIT Short period flare event on the BH accretion disk Power spectrum
17 Samples of BVIT Reduced Data: M-star flares CN Leo: dme Flare Star: emission structure observed < 0.1 sec
18 Samples of BVIT Reduced Data: CV Systems Magnetic cataclysmic variables (CVs) contain a white dwarf that is accreting material from a secondary (red dwarf) star down the field lines. In these polar systems the strong magnetic field of the white dwarf causes it to rotate synchronously with the orbital motion. We observed the UZ For system in the B-band with BVIT for ~ 2000sec and captured an entire an eclipse event. We show the BVIT data in time bins of 0.5s and compare it with similar (white light) data recorded with an STJ device by Perryman et al (2001)
19 Samples of BVIT Reduced Data: CV Systems
20 Optical pulsars and isolated neutron Stars Only 3 optical pulsars are sufficiently bright enough to be observed with BVIT: the Crab, PSR B and Vela. Light curve of the Crab pulsar recorded with BVIT on the Lick 1m Nickel Telescope in 2007 We have searched the ~ 2 hrs of pulsar data for the presence of giant optical pulses with no success.
21 Optical pulsars and isolated Neutron Stars In future observing runs we shall point the center of the BVIT f.o.v. at the radio position of several Rotating Radio Transients (RRATs) To date, ~ 20 RRATs have been detected and are characterized by short bursts of 2 to 30ms duration (100mJ to 10Jy) with time intervals between recurrent bursts ranging from 3 min to 3 hours. Obtaining a ratio of the optical-to-radio flux can place limits on the spectral slope of any proposed emission mechanism from a plausible magnetar. We shall also perform limited optical follow-up observations of gamma-ray bursts to search for very fast time-structure in their optical light curve emission
22 New BVIT tube for SALT New detectors for BVIT are in production, the detection efficiency is considerably better than our first detector, particularly in the red. We expect to upgrade the BVIT detector in mid New BVIT detector Comparison of detector photocathode efficiency
23 Photon counting counts EVERYTHING!! sec events with rise times of only 2 milli-sec?? Meteor Detection
24 Peak* Performance of the BVIT on SALT Detector FOV = 25mm circular, 1.9 arc min diam Spatial Resolution = 30 microns (0.14 ) Photocathode = S20 (replace with Supergen2) Timing Resolution = Time-stamped to 25 ns Filter selection = U, B or V-band Neutral Density Filter = ND0 to ND4 Max BVIT count rate = 2 MHz (whole detector) Max local count rate = 20 khz per arc sec 2 Stellar magnitude count rates U = 17.5 mag (1500 cts/sec) U = 22.0 mag (25 cts/sec) B = 17.0 mag (11000 cts/sec) B = 21.6 mag (170 cts/sec) Sky background count rates (Dark) = 25 cts/sec (U-band) (in 1 arc sec 2 ) (Grey) = 170 cts/sec (B-band) * Actual performance numbers depend on observing conditions etc etc
High Speed Optical Imaging Photon Counting Microchannel Plate Detectors for Astronomical and Space Sensing Applications
High Speed Optical Imaging Photon Counting Microchannel Plate Detectors for Astronomical and Space Sensing Applications Oswald Siegmund, John Vallerga, Barry Welsh, Jason McPhate, Anton Tremsin, Space
More informationFermi: Highlights of GeV Gamma-ray Astronomy
Fermi: Highlights of GeV Gamma-ray Astronomy Dave Thompson NASA GSFC On behalf of the Fermi Gamma-ray Space Telescope Large Area Telescope Collaboration Neutrino Oscillation Workshop Otranto, Lecce, Italy
More informationPulsars ASTR2110 Sarazin. Crab Pulsar in X-rays
Pulsars ASTR2110 Sarazin Crab Pulsar in X-rays Test #2 Monday, November 13, 11-11:50 am Ruffner G006 (classroom) Bring pencils, paper, calculator You may not consult the text, your notes, or any other
More informationThoughts on Astrophysics with nano/6u cubesats
18 July 2012 Thoughts on Astrophysics with nano/6u cubesats Harvey Butcher Stars & Planets Interstellar medium Transients Other ideas Recall: Space platforms can provide: Access to γ-ray, x-ray, UV, IR,
More informationEditorial comment: research and teaching at UT
Wednesday, March 23, 2017 Reading for Exam 3: Chapter 6, end of Section 6 (binary evolution), Section 6.7 (radioactive decay), Chapter 7 (SN 1987A), Background: Sections 3.1, 3.2, 3.3, 3.4, 3.5, 3.8, 3.10,
More informationGamma-ray observations of millisecond pulsars with the Fermi LAT. Lucas Guillemot, MPIfR Bonn. NS2012 in Bonn 27/02/12.
Gamma-ray observations of millisecond pulsars with the Fermi LAT Lucas Guillemot, MPIfR Bonn guillemo@mpifr-bonn.mpg.de NS2012 in Bonn 27/02/12 The Fermi Gamma-ray Space Telescope Fermi = Large Area Telescope
More informationAn Introduction to Radio Astronomy
An Introduction to Radio Astronomy Second edition Bernard F. Burke and Francis Graham-Smith CAMBRIDGE UNIVERSITY PRESS Contents Preface to the second edition page x 1 Introduction 1 1.1 The role of radio
More informationX-ray observations of X-ray binaries and AGN
X-ray observations of X-ray binaries and AGN Tomaso M. Be!oni (INAF - Osservatorio Astronomico di Brera) (Visiting Professor, Univ. of Southampton) OUTLINE Lecture I: Accretion onto compact objects, X-ray
More informationLearning Objectives: Chapter 13, Part 1: Lower Main Sequence Stars. AST 2010: Chapter 13. AST 2010 Descriptive Astronomy
Chapter 13, Part 1: Lower Main Sequence Stars Define red dwarf, and describe the internal dynamics and later evolution of these low-mass stars. Appreciate the time scale of late-stage stellar evolution
More informationNeutron Stars. We now know that SN 1054 was a Type II supernova that ended the life of a massive star and left behind a neutron star.
Neutron Stars Neutron Stars The emission from the supernova that produced the crab nebula was observed in 1054 AD by Chinese, Japanese, Native Americans, and Persian/Arab astronomers as being bright enough
More informationDiscovery of a New Gamma-Ray Binary: 1FGL J
Discovery of a New Gamma-Ray Binary: 1FGL J1018.6-5856 Robin Corbet (UMBC/NASA GSFC) on behalf of the Fermi-LAT collaboration, & M.J. Coe, P.G. Edwards, M.D. Filipovic, J.L. Payne, J. Stevens, M.A.P. Torres
More informationGamma-ray Astrophysics with VERITAS: Exploring the violent Universe
Gamma-ray Astrophysics with VERITAS: Exploring the violent Universe K. Ragan McGill University Soup & Science 11-Jan-2008 Soup & Science Jan. '08 1 How do we know about the Universe? Historically, all
More informationThe Stellar Graveyard
Life and Death of High Mass Stars (M > 8 M sun ) AST 101 Introduction to Astronomy: Stars & Galaxies Last stage: Iron core surrounded by shells of increasingly lighter elements. Announcements MIDTERM #2
More informationChapter 14. Outline. Neutron Stars and Black Holes. Note that the following lectures include. animations and PowerPoint effects such as
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). Chapter 14 Neutron
More informationLaura Barragán. Universidad Complutense de Madrid
. Universidad Complutense de Madrid Tutors: Erik Kuulkers & Peter Kretschmar INTEGRAL: International Gamma-Ray Astrophysics Laboratory The payload The mission The project IBIS (Imager on-board the Integral
More informationSources of GeV Photons and the Fermi Results
Sources of GeV Photons and the Fermi Results 1. GeV instrumentation and the GeV sky with the Fermi Gamma-ray Space Telescope 2. First Fermi Catalog of Gamma Ray Sources and the Fermi Pulsar Catalog 3.
More information3/13/18. Things to do. Synchrotron Radiation. Today on Stellar Explosions
ASTR 1040: Stars & Galaxies Prof. Juri Toomre TAs: Peri Johnson, Ryan Horton Lecture 17 Tues 13 Mar 2018 zeus.colorado.edu/astr1040-toomre Ring Nebula Today on Stellar Explosions Revisit Pulsars spinning
More informationMonday, October 21, 2013 Third exam this Friday, October 25. Third Sky Watch watch the weather! Review sheet posted today. Review Thursday, 5 6 PM,
Monday, October 21, 2013 Third exam this Friday, October 25. Third Sky Watch watch the weather! Review sheet posted today. Review Thursday, 5 6 PM, Room WEL 2.256 Lecture 19 posted today Reading: Chapter
More informationASTR Midterm 2 Phil Armitage, Bruce Ferguson
ASTR 1120-001 Midterm 2 Phil Armitage, Bruce Ferguson SECOND MID-TERM EXAM MARCH 21 st 2006: Closed books and notes, 1 hour. Please PRINT your name and student ID on the places provided on the scan sheet.
More information9.1 Years of All-Sky Hard X-ray Monitoring with BATSE
9.1 Years of All-Sky Hard X-ray Monitoring with CGRO BATSE Large Area Detector (LAD) BATSE 1 of 8 BATSE Colleen A. Wilson (NASA/MSFC), for the BATSE teams at MSFC and Southampton Abstract The hard X-ray
More informationStar systems like our Milky Way. Galaxies
Galaxies Star systems like our Milky Way Galaxies Contain a few thousand to tens of billions of stars,as well as varying amounts of gas and dust Large variety of shapes and sizes Gas and Dust in
More informationNeutron Stars. Neutron Stars and Black Holes. The Crab Pulsar. Discovery of Pulsars. The Crab Pulsar. Light curves of the Crab Pulsar.
Chapter 11: Neutron Stars and Black Holes A supernova explosion of an M > 8 M sun star blows away its outer layers. Neutron Stars The central core will collapse into a compact object of ~ a few M sun.
More informationNeutron Stars. Properties of Neutron Stars. Formation of Neutron Stars. Chapter 14. Neutron Stars and Black Holes. Topics for Today s Class
Foundations of Astronomy 13e Seeds Phys1403 Introductory Astronomy Instructor: Dr. Goderya Chapter 14 Neutron Stars and Black Holes Cengage Learning 2016 Topics for Today s Class Neutron Stars What is
More informationDistribution of X-ray binary stars in the Galaxy (RXTE) High-Energy Astrophysics Lecture 8: Accretion and jets in binary stars
High-Energy Astrophysics Lecture 8: Accretion and jets in binary stars Distribution of X-ray binary stars in the Galaxy (RXTE) Robert Laing Primary Compact accreting binary systems Compact star WD NS BH
More informationAn Introduction to Radio Astronomy
An Introduction to Radio Astronomy Bernard F. Burke Massachusetts Institute of Technology and Francis Graham-Smith Jodrell Bank, University of Manchester CAMBRIDGE UNIVERSITY PRESS Contents Preface Acknowledgements
More informationThe Mystery of Fast Radio Bursts and its possible resolution. Pawan Kumar
The Mystery of Fast Radio Bursts and its possible resolution Outline Pawan Kumar FRBs: summary of relevant observations Radiation mechanism and polarization FRB cosmology Wenbin Lu Niels Bohr Institute,
More informationThe Nature of Pulsars! Agenda for Ast 309N, Nov. 1. To See or Not to See (a Pulsar) The Slowing & Fading of Pulsars!
Agenda for Ast 309N, Nov. 1 Quiz 7 Card 10/30 feedback More on pulsars and other neutron stars Begin: the saga of interacting binary systems Card: questions for review Reading: - Kaler, ch. 7 Wheeler,
More informationAstronomy Stars, Galaxies and Cosmology Exam 3. Please PRINT full name
Astronomy 132 - Stars, Galaxies and Cosmology Exam 3 Please PRINT full name Also, please sign the honor code: I have neither given nor have I received help on this exam The following exam is intended to
More informationPic of the day: Star trails over the Canary Islands, gamma-ray telescope in the foreground.
Friday, October 14, 2011 Exam 3 next week. Review sheet on Monday. Reading: Section 6.7, Chapter 7, Chapter 8 - Sections 8.1, 8.2, 8.5, 8.6, 8.10, Reading, Chapter 9: all except 9.6.3, 9.6.4 (9.1 9.5.1
More informationAstronomy Ch. 22 Neutron Stars and Black Holes. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 22 Neutron Stars and Black Holes MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) In a neutron star, the core
More informationBringing Real-time Astronomical Observations into the Classroom
Bringing Real-time Astronomical Observations into the Classroom Prof. Lynn Cominsky Sonoma State University Department of Physics and Astronomy and NASA Education and Public Outreach Group Why do astronomical
More informationMonday, October 14, 2013 Reading: Chapter 8. Astronomy in the news?
Monday, October 14, 2013 Reading: Chapter 8 Astronomy in the news? Goal: To understand the nature and importance of SN 1987A for our understanding of massive star evolution and iron core collapse. 1 st
More informationToday in Astronomy 102: observations of stellarmass black holes
Today in Astronomy 102: observations of stellarmass black holes q Summary of distinctive features of celestial black holes. q The search for stellar-mass black holes: X-ray and γ-ray emission. Mass from
More informationSpecial Relativity. Principles of Special Relativity: 1. The laws of physics are the same for all inertial observers.
Black Holes Special Relativity Principles of Special Relativity: 1. The laws of physics are the same for all inertial observers. 2. The speed of light is the same for all inertial observers regardless
More informationChapter 17. Active Galaxies and Supermassive Black Holes
Chapter 17 Active Galaxies and Supermassive Black Holes Guidepost In the last few chapters, you have explored our own and other galaxies, and you are ready to stretch your scientific imagination and study
More informationComponents of Galaxies Stars What Properties of Stars are Important for Understanding Galaxies?
Components of Galaxies Stars What Properties of Stars are Important for Understanding Galaxies? Temperature Determines the λ range over which the radiation is emitted Chemical Composition metallicities
More informationNeutron Stars, Pulsars, Magnetars, and Black Holes the corpses of high-mass stars
Neutron Stars, Pulsars, Magnetars, and Black Holes the corpses of high-mass stars Combination X-ray & visible light image of the Crab Nebula Pulsar From Chandra X-ray Observatory and Hubble Space Telescope
More informationMulti-frequency. Observations Using REM at la Silla. Filippo Maria Zerbi INAF Osservatorio di Brera On behalf of the REM/ROSS team
Multi-frequency Observations Using REM at la Silla Filippo Maria Zerbi INAF Osservatorio di Brera On behalf of the REM/ROSS team A fast moving telescope Alt-az 60 cm f/8 RC silver-coated 2 Nasmyth foci
More informationGamma-Ray Astronomy. Astro 129: Chapter 1a
Gamma-Ray Bursts Gamma-Ray Astronomy Gamma rays are photons with energies > 100 kev and are produced by sub-atomic particle interactions. They are absorbed by our atmosphere making observations from satellites
More informationSpecial Topics in Nuclear and Particle Physics
Special Topics in Nuclear and Particle Physics Astroparticle Physics Lecture 5 Gamma Rays & x-rays Sept. 22, 2015 Sun Kee Kim Seoul National University Gamma ray astronomy gamma ray synchrotron radition
More informationTEV GAMMA RAY ASTRONOMY WITH VERITAS
1 TEV GAMMA RAY ASTRONOMY WITH VERITAS Tülün Ergin (U. of Massachusetts Amherst, MA) on behalf of the VERITAS Collaboration 2 Contents The VERITAS Experiment Results and the Performance Galactic Sources
More informationScience Olympiad Astronomy C Division Event Golden Gate Invitational
Science Olympiad Astronomy C Division Event Golden Gate Invitational University of California, Berkeley Berkeley, CA February 9, 2019 Team Number: Team Name: Instructions: 1) Please turn in all materials
More informationTime Resolved Astronomy with the SALT
Time Resolved Astronomy with the SALT D. A. H. Buckley * a,b, S. Crawford a, A.A.S. Gulbis a,b, J. McPhate c, K. H. Nordsieck d, S.B. Potter a, D. O Donoghue a, O.H.W. Siegmund c, P. Schellart a,b, M.
More informationToday. Logistics. Visible vs. X-ray X. Synchrotron Radiation. Pulsars and Neutron Stars. ASTR 1040 Accel Astro: Stars & Galaxies
ASTR 1040 Accel Astro: Stars & Galaxies Today Binary mass transfer Joys of nearest supernova: SN 1987A How mass transfer from binary companion can spin-up pulsar White dwarf supernovae from mass transfer
More informationAstronomy 104: Second Exam
Astronomy 104: Second Exam Stephen Lepp October 29, 2014 Each question is worth 2 points. Write your name on this exam and on the scantron. Short Answer A The Sun is powered by converting hydrogen to what?
More information- Synchrotron emission: A brief history. - Examples. - Cyclotron radiation. - Synchrotron radiation. - Synchrotron power from a single electron
- Synchrotron emission: A brief history - Examples - Cyclotron radiation - Synchrotron radiation - Synchrotron power from a single electron - Relativistic beaming - Relativistic Doppler effect - Spectrum
More informationAstronomy 422! Lecture 7: The Milky Way Galaxy III!
Astronomy 422 Lecture 7: The Milky Way Galaxy III Key concepts: The supermassive black hole at the center of the Milky Way Radio and X-ray sources Announcements: Test next Tuesday, February 16 Chapters
More informationOther Galaxy Types. Active Galaxies. A diagram of an active galaxy, showing the primary components. Active Galaxies
Other Galaxy Types Active Galaxies Active Galaxies Seyfert galaxies Radio galaxies Quasars Origin??? Different in appearance Produce huge amount of energy Similar mechanism a Galactic mass black hole at
More informationNeutron Stars. Neutron Stars Mass ~ 2.0 M sun! Radius ~ R sun! isolated neutron stars first seen only recently (1997)
Neutron Stars 1 2 M core > 1.4 M - collapse past WD! sun nuclei packed tightly together! protons absorb electrons; only neutrons left! collapse halted by neutron degeneracy pressure How do you find something
More informationLecture 11 Quiz 2. AGN and You. A Brief History of AGN. This week's topics
Lecture 11 Quiz 2 AGN and You March 25 2003 8:00 PM BPS 1420 1. What system of time do astronomers use rather than the standard day-month-year system? 2. In that system, how long would it be between noon
More informationThe Large Synoptic Survey Telescope
The Large Synoptic Survey Telescope Philip A. Pinto Steward Observatory University of Arizona for the LSST Collaboration 17 May, 2006 NRAO, Socorro Large Synoptic Survey Telescope The need for a facility
More informationPhysics HW Set 3 Spring 2015
1) If the Sun were replaced by a one solar mass black hole 1) A) life here would be unchanged. B) we would still orbit it in a period of one year. C) all terrestrial planets would fall in immediately.
More informationNotes for Wednesday, July 16; Sample questions start on page 2 7/16/2008
Notes for Wednesday, July 16; Sample questions start on page 2 7/16/2008 Wed, July 16 MW galaxy, then review. Start with ECP3Ch14 2 through 8 Then Ch23 # 8 & Ch 19 # 27 & 28 Allowed Harlow Shapely to locate
More informationA RADIO SEARCH FOR BLACK HOLES IN THE MILKY WAY GLOBULAR CLUSTER M10
(nrao/aui) LAURA SHISHKOVSKY, J. STRADER, L. CHOMIUK, L. TREMOU (MSU), J. MILLER-JONES, V. TUDOR (CURTIN), T. MACCARONE (TEXAS TECH), G. SIVAKOFF, C. HEINKE (U. ALBERTA) A RADIO SEARCH FOR BLACK HOLES
More informationTime-domain astronomy with the Fermi Gamma-ray Burst Monitor
Time-domain astronomy with the Fermi Gamma-ray Burst Monitor C. Michelle Hui (NASA/MSFC) on behalf of the Fermi GBM team TeVPA, Aug 11 2017 GBM: FOV >8sr Whole sky every ~90min Fermi Gamma-ray Space Telescope
More informationExtreme high-energy variability of Markarian 421
Extreme high-energy variability of Markarian 421 Mrk 421 an extreme blazar Previous observations outstanding science issues 2001 Observations by VERITAS/Whipple 10 m 2001 Light Curve Energy spectrum is
More informationNEUTRON STARS, GAMMA RAY BURSTS, and BLACK HOLES (chap. 22 in textbook)
NEUTRON STARS, GAMMA RAY BURSTS, and BLACK HOLES (chap. 22 in textbook) Neutron Stars For carbon detonation SN probably no remnant For core-collapse SN remnant is a neutron-degenerate core neutron star
More informationWhat are the Big Questions and how can Radio Telescopes help answer them? Roger Blandford KIPAC Stanford
What are the Big Questions and how can Radio Telescopes help answer them? Roger Blandford KIPAC Stanford Radio Astronomy in 1957 ~100 MHz ~100 Jy ~100 sources ~100 arcseconds 2 Radio Astronomy in 2007
More informationThis class: Life cycle of high mass stars Supernovae Neutron stars, pulsars, pulsar wind nebulae, magnetars Quark-nova stars Gamma-ray bursts (GRBs)
This class: Life cycle of high mass stars Supernovae Neutron stars, pulsars, pulsar wind nebulae, magnetars Quark-nova stars Gamma-ray bursts (GRBs)!1 Cas$A$ All$Image$&$video$credits:$Chandra$X7ray$ Observatory$
More informationGalaxies with Active Nuclei. Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes
Galaxies with Active Nuclei Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes Active Galactic Nuclei About 20 25% of galaxies do not fit well into Hubble categories
More informationA very wide field focusing telescope for Synoptic studies in the soft X-ray band
A very wide field focusing telescope for Synoptic studies in the soft X-ray band Paul Gorenstein Harvard-Smithsonian Center for Astrophysics Cambridge, MA 02138 Synoptic Telescopes, (Broad Coverage of
More informationRotating RAdio Transients (RRATs) ApJ, 2006, 646, L139 Nature, 2006, 439, 817 Astro-ph/
Rotating RAdio Transients (RRATs) ApJ, 2006, 646, L139 Nature, 2006, 439, 817 Astro-ph/0608311 Introduction 11 Rotating RAdio Transients (RRATs) (Mclaughlin et al 2006) Repeated, irregular radio bursts
More informationAST-1002 Section 0459 Review for Final Exam Please do not forget about doing the evaluation!
AST-1002 Section 0459 Review for Final Exam Please do not forget about doing the evaluation! Bring pencil #2 with eraser No use of calculator or any electronic device during the exam We provide the scantrons
More information29:50 Stars, Galaxies, and the Universe Second Hour Exam November 10, 2010 Form A
29:50 Stars, Galaxies, and the Universe Second Hour Exam November 10, 2010 Form A There are 20 questions (Note: There will be 32 on the real thing). Read each question and all of the choices before choosing.
More informationAstronomy 114. Lecture 27: The Galaxy. Martin D. Weinberg. UMass/Astronomy Department
Astronomy 114 Lecture 27: The Galaxy Martin D. Weinberg weinberg@astro.umass.edu UMass/Astronomy Department A114: Lecture 27 18 Apr 2007 Read: Ch. 25,26 Astronomy 114 1/23 Announcements Quiz #2: we re
More informationUnstable Mass Transfer
Unstable Mass Transfer When the mass ratios are large, or when the donor star has a deep convective layer (so R M-1/3), mass loss will occur on a dynamical timescale. The result will be common envelope
More informationOutbursts and State Transitions in Black Hole Candidates Observed by MAXI
Outbursts and State Transitions in Black Hole Candidates Observed by MAXI Hitoshi Negoro and MAXI Team Nihon University, -8 Kanda-Surugadai, Chiyoda, Tokyo, Japan -838 E-mail(HN): negoro@phys.cst.nihon-u.ac.jp
More informationMIDTERM #2. ASTR 101 General Astronomy: Stars & Galaxies. Can we detect BLACK HOLES? Black Holes in Binaries to the rescue. Black spot in the sky?
ASTR 101 General Astronomy: Stars & Galaxies Can we detect BLACK HOLES? NEXT Friday 04/03: MIDTERM #2 [Image by A. Hamilton] Black spot in the sky? Black Holes in Binaries to the rescue Black Holes in
More informationThe distance modulus in the presence of absorption is given by
Problem 4: An A0 main sequence star is observed at a distance of 100 pc through an interstellar dust cloud. Furthermore, it is observed with a color index B-V = 1.5. What is the apparent visual magnitude
More informationNeutron Stars. But what happens to the super-dense core? It faces two possible fates:
Neutron Stars When a massive star runs out of fuel, its core collapses from the size of the Earth to a compact ball of neutrons just ten miles or so across. Material just outside the core falls onto this
More informationHigh Redshift Universe
High Redshift Universe Finding high z galaxies Lyman break galaxies (LBGs) Photometric redshifts Deep fields Starburst galaxies Extremely red objects (EROs) Sub-mm galaxies Lyman α systems Finding high
More informationX-ray burst science with Astrosat
X-ray burst science with Astrosat A R Rao Tata Institute of Fundamental Research, India (arrao@tifr.res.in) 40 years of X-ray bursts: Extreme explosions in dense environments 19 June 2015 17-19 June 2015
More informationAstronomy Ch. 21 Stellar Explosions. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 21 Stellar Explosions MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A surface explosion on a white dwarf, caused
More informationThe Stellar Graveyard Neutron Stars & White Dwarfs
The Stellar Graveyard Neutron Stars & White Dwarfs White Dwarfs White dwarfs are the remaining cores of low-mass (M < 8M sun ) stars Electron degeneracy pressure supports them against gravity Density ~
More informationNames: Team: Team Number:
Astronomy C Michigan Region 8 March 11, 2017 Names: Team: Team Number: Directions 1. There is a separate answer sheet. Answers written elsewhere (e.g. on the test) will not be considered. 2. You may take
More informationQuasars and AGN. What are quasars and how do they differ from galaxies? What powers AGN s. Jets and outflows from QSOs and AGNs
Goals: Quasars and AGN What are quasars and how do they differ from galaxies? What powers AGN s. Jets and outflows from QSOs and AGNs Discovery of Quasars Radio Observations of the Sky Reber (an amateur
More informationQuasars ASTR 2120 Sarazin. Quintuple Gravitational Lens Quasar
Quasars ASTR 2120 Sarazin Quintuple Gravitational Lens Quasar Quasars Quasar = Quasi-stellar (radio) source Optical: faint, blue, star-like objects Radio: point radio sources, faint blue star-like optical
More informationAccretion in Binaries
Accretion in Binaries Two paths for accretion Roche-lobe overflow Wind-fed accretion Classes of X-ray binaries Low-mass (BH and NS) High-mass (BH and NS) X-ray pulsars (NS) Be/X-ray binaries (NS) Roche
More informationInternational Olympiad on Astronomy and Astrophysics (IOAA)
Syllabus of International Olympiad on Astronomy and Astrophysics (IOAA) General Notes 1. Extensive contents in basic astronomical concepts are required in theoretical and practical problems. 2. Basic concepts
More informationSupernovae, Neutron Stars, Pulsars, and Black Holes
Supernovae, Neutron Stars, Pulsars, and Black Holes Massive stars and Type II supernovae Massive stars (greater than 8 solar masses) can create core temperatures high enough to burn carbon and heavier
More informationAstronomy across the spectrum: telescopes and where we put them. Martha Haynes Discovering Dusty Galaxies July 7, 2016
Astronomy across the spectrum: telescopes and where we put them Martha Haynes Discovering Dusty Galaxies July 7, 2016 CCAT-prime: next generation telescope CCAT Site on C. Chajnantor Me, at 18,400 feet
More informationStellar Binary Systems and CTA. Guillaume Dubus Laboratoire d Astrophysique de Grenoble
Stellar Binary Systems and CTA Guillaume Dubus Laboratoire d Astrophysique de Grenoble Barcelona Cherenkov Telescope Array Meeting, 24-25 January 2008 X-ray binaries picture by H. Spruit relativistic outflow
More informationThe Eight-meter-wavelength Transient Array
The Eight-meter-wavelength Transient Array Steve Ellingson Cameron Patterson John Simonetti Dept. of Electrical & Computer Engineering Dept. of Electrical & Computer Engineering Dept. of Physics Virginia
More informationStudy of Cataclysmic Variable B7 in NGC 6791: From the Ground and from Space
Study of Cataclysmic Variable B7 in NGC 6791: From the Ground and from Space K. C. Magno College of Science, University of Notre Dame, Notre Dame, 46556 kmagno@nd.edu and P. M. Garnavich Department of
More informationRecent highlights from VERITAS
Recent highlights from VERITAS K. Ragan McGill University RICAP 2011, Rome, 26-May-2011 K. Ragan VERITAS RICAP '11 1 Outline Very high-energy (VHE) gamma-ray astrophysics Ground-based observations with
More informationAST 101 Introduction to Astronomy: Stars & Galaxies
AST 101 Introduction to Astronomy: Stars & Galaxies Life and Death of High Mass Stars (M > 8 M sun ) REVIEW Last stage: Iron core surrounded by shells of increasingly lighter elements. REVIEW When mass
More informationPhotometric Studies of GEO Debris
Photometric Studies of GEO Debris Patrick Seitzer Department of Astronomy, University of Michigan 500 Church St. 818 Dennison Bldg, Ann Arbor, MI 48109 pseitzer@umich.edu Heather M. Cowardin ESCG/Jacobs
More informationUniverse Now. 2. Astronomical observations
Universe Now 2. Astronomical observations 2. Introduction to observations Astronomical observations are made in all wavelengths of light. Absorption and emission can reveal different things on different
More informationGravitational Wave Astronomy using 0.1Hz space laser interferometer. Takashi Nakamura GWDAW-8 Milwaukee 2003/12/17 1
Gravitational Wave Astronomy using 0.1Hz space laser interferometer Takashi Nakamura GWDAW-8 Milwaukee 2003/12/17 1 In 2001 we considered what we can do using 0.1 hertz laser interferometer ( Seto, Kawamura
More informationInfrared Spectroscopy of the Black Hole Candidate GRO J
Infrared Spectroscopy of the Black Hole Candidate GRO J1655-40 1 Francis T. O Donovan March 19th, 2004 1 Based on a paper by F. T. O Donovan & P. J. Callanan (in preparation). Black Holes in the Sky At
More informationAstronomy. Chapter 15 Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes
Astronomy Chapter 15 Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes are hot, compact stars whose mass is comparable to the Sun's and size to the Earth's. A. White dwarfs B. Neutron stars
More informationPart two of a year-long introduction to astrophysics:
ASTR 3830 Astrophysics 2 - Galactic and Extragalactic Phil Armitage office: JILA tower A909 email: pja@jilau1.colorado.edu Spitzer Space telescope image of M81 Part two of a year-long introduction to astrophysics:
More informationFORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS
FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS Main Categories of Compact Systems Formation of Compact Objects Mass and Angular Momentum Loss Evolutionary Links to Classes of Binary Systems Future Work
More informationOVERVIEW OF A 3C279 s FLARE and SIMULATION OF AGNs
Gamma-ray Large Area Space Telescope OVERVIEW OF A 3C279 s FLARE and SIMULATION OF AGNs Alessandro Buzzatti Università degli Studi di Torino / SLAC Alessandro Buzzatti 1 Outline Overview of 3C279 flare
More informationNew physics is learnt from extreme or fundamental things
New physics is learnt from extreme or fundamental things New physics is learnt from extreme or fundamental things The Universe is full of extremes and is about as fundamental as it gets! New physics is
More informationDark Matter ASTR 2120 Sarazin. Bullet Cluster of Galaxies - Dark Matter Lab
Dark Matter ASTR 2120 Sarazin Bullet Cluster of Galaxies - Dark Matter Lab Mergers: Test of Dark Matter vs. Modified Gravity Gas behind DM Galaxies DM = location of gravity Gas = location of most baryons
More informationLecture Outlines. Chapter 23. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 23 Astronomy Today 8th Edition Chaisson/McMillan Chapter 23 The Milky Way Galaxy Units of Chapter 23 23.1 Our Parent Galaxy 23.2 Measuring the Milky Way Discovery 23-1 Early Computers
More informationGround Based Gamma Ray Astronomy with Cherenkov Telescopes. HAGAR Team
Ground Based Gamma Ray Astronomy with Cherenkov Telescopes HAGAR Team DHEP Annual Meeting, 7-8 April, 2016 Projects : HAGAR Telescope System Development of G-APD based imaging camera Calibration device
More informationESA Gaia & the multifrequency behavior of high-energy sources with ultra-low dispersion spectroscopy
Mem. S.A.It. Vol. 83, 342 c SAIt 2012 Memorie della ESA Gaia & the multifrequency behavior of high-energy sources with ultra-low dispersion spectroscopy R. Hudec 1,2, V. Šimon 1, L. Hudec 2, and V. Hudcová
More informationXenon Compton Telescopes at Columbia: the post LXeGRIT phase. E.Aprile. Columbia University
Xenon Compton Telescopes at Columbia: the post LXeGRIT phase E.Aprile Columbia University Seeon 2003 Sensitivity Goals for An Advanced Compton Telescope ~10-7 ph cm -2 s -1 ( 3σ) for narrow lines and ~
More information