Science with Radio Pulsar Astrometry
|
|
|
- Stephanie Baker
- 5 years ago
- Views:
Transcription
1 Science with Radio Pulsar Astrometry Shami Chatterjee Cornell University August 2012
2 Astrometry is a force multiplier Precise astrometry improves the science return from new discoveries.
3 Astrometry is a force multiplier Precise astrometry improves the science return from new discoveries. Astrophysics: Compare apparent L γ with absolute Emission geometry, luminosity evolution. Ė = Iω ω.
4 Astrometry is a force multiplier Precise astrometry improves the science return from new discoveries. Astrophysics: Compare apparent L γ with absolute Ė = Iω ω. Emission geometry, luminosity evolution. Origins: Use µ and τ to trace path back to birth sites and associations with massive star clusters, SNRs.
5 Astrometry is a force multiplier Precise astrometry improves the science return from new discoveries. Astrophysics: Compare apparent L γ with absolute Ė = Iω ω. Emission geometry, luminosity evolution. Origins: Use µ and τ to trace path back to birth sites and associations with massive star clusters, SNRs. Relativistic winds: Calibrate energetics of PWNe, probe interaction with ISM and bulk flows.
6 Astrometry is a force multiplier Precise astrometry improves the science return from new discoveries. Astrophysics: Compare apparent L γ with absolute Ė = Iω ω. Emission geometry, luminosity evolution. Origins: Use µ and τ to trace path back to birth sites and associations with massive star clusters, SNRs. Relativistic winds: Calibrate energetics of PWNe, probe interaction with ISM and bulk flows. Gravitational physics: Astrometric parameters for stable recycled pulsars independent of pulse timing. Shklovskii effect corrections, break timing degeneracies.
7 Astrometry is a force multiplier Precise astrometry improves the science return from new discoveries. Astrophysics: Compare apparent L γ with absolute Ė = Iω ω. Emission geometry, luminosity evolution. Origins: Use µ and τ to trace path back to birth sites and associations with massive star clusters, SNRs. Relativistic winds: Calibrate energetics of PWNe, probe interaction with ISM and bulk flows. Gravitational physics: Astrometric parameters for stable recycled pulsars independent of pulse timing. Shklovskii effect corrections, break timing degeneracies. Galactic electron density modeling: improve DM-based distance estimates for entire population.
8 Astrometry is a force multiplier Precise astrometry improves the science return from new discoveries. Astrophysics: Compare apparent L γ with absolute Ė = Iω ω. Emission geometry, luminosity evolution. Origins: Use µ and τ to trace path back to birth sites and associations with massive star clusters, SNRs. Relativistic winds: Calibrate energetics of PWNe, probe interaction with ISM and bulk flows. Gravitational physics: Astrometric parameters for stable recycled pulsars independent of pulse timing. Shklovskii effect corrections, break timing degeneracies. Galactic electron density modeling: improve DM-based distance estimates for entire population. Other science: velocity distributions, frame ties, NS cooling, etc.
9 The VLBA: An Astrometry Machine
10 Talk Outline Applying VLB astrometry to pulsar timing: Can we improve our sensitivity to gravitational waves? Astrophysics: NS mass for PSR J Astrometry for Fermi-detected pulsars. Previews of coming attractions.
11 Pulsar Timing Arrays and Gravitational Waves Time an array of exceptionally stable pulsars. Correlated timing residuals gravitational waves. NanoHz frequencies multi-year timing campaigns.
12 Noise-induced errors in astrometry Pulse timing: Noise power absorbed by astrometric fit terms ( θ, µ, π).
13 Noise-induced errors in astrometry Pulse timing: Noise power absorbed by astrometric fit terms ( θ, µ, π). White noise: post-fit residuals similar, but parameters altered. (Madison et al. 2012)
14 Noise-induced errors in astrometry Pulse timing: Noise power absorbed by astrometric fit terms ( θ, µ, π). White noise: post-fit residuals similar, but parameters altered. Red noise: post-fit residuals much lower. (Madison et al. 2012)
15 Noise-induced errors in astrometry Pulse timing: Noise power absorbed by astrometric fit terms ( θ, µ, π). White noise: post-fit residuals similar, but parameters altered. Red noise: post-fit residuals much lower. Effects are worse for redder noise. Effects worse for shorter data spans; reduced by denser sampling.
16 Pulse Timing and Astrometry If we can pin down astrometric parameters with independent obs, the significance of any signal in the residuals should be improved: fewer parameters to fit. (Madison et al. 2012)
17 T(f) Pulse Timing and Astrometry If we can pin down astrometric parameters with independent obs, the significance of any signal in the residuals should be improved: fewer parameters to fit. (Madison et al. 2012) Transmission function: (following Blandford, Romani, & Narayan 1984) yr, Timing f [yr 1 ]
18 T(f) Pulse Timing and Astrometry If we can pin down astrometric parameters with independent obs, the significance of any signal in the residuals should be improved: fewer parameters to fit. (Madison et al. 2012) Transmission function: (following Blandford, Romani, & Narayan 1984) yr, Timing yr, VLB θ f [yr 1 ]
19 T(f) Pulse Timing and Astrometry If we can pin down astrometric parameters with independent obs, the significance of any signal in the residuals should be improved: fewer parameters to fit. (Madison et al. 2012) Transmission function: (following Blandford, Romani, & Narayan 1984) yr, Timing f [yr 1 ]
20 T(f) Pulse Timing and Astrometry If we can pin down astrometric parameters with independent obs, the significance of any signal in the residuals should be improved: fewer parameters to fit. (Madison et al. 2012) Transmission function: (following Blandford, Romani, & Narayan 1984) yr, Timing yr, VLB θ,µ f [yr 1 ]
21 T(f) Pulse Timing and Astrometry If we can pin down astrometric parameters with independent obs, the significance of any signal in the residuals should be improved: fewer parameters to fit. (Madison et al. 2012) Transmission function: (following Blandford, Romani, & Narayan 1984) yr, Timing f [yr 1 ]
22 T(f) Pulse Timing and Astrometry If we can pin down astrometric parameters with independent obs, the significance of any signal in the residuals should be improved: fewer parameters to fit. (Madison et al. 2012) Transmission function: (following Blandford, Romani, & Narayan 1984) yr, Timing yr, VLB θ,µ,π f [yr 1 ]
23 T(f) Pulse Timing and Astrometry If we can pin down astrometric parameters with independent obs, the significance of any signal in the residuals should be improved: fewer parameters to fit. (Madison et al. 2012) Transmission function: (following Blandford, Romani, & Narayan 1984) yr, Timing f [yr 1 ]
24 T(f) Pulse Timing and Astrometry If we can pin down astrometric parameters with independent obs, the significance of any signal in the residuals should be improved: fewer parameters to fit. (Madison et al. 2012) Transmission function: (following Blandford, Romani, & Narayan 1984) yr, Timing yr, VLB θ,µ,π f [yr 1 ]
25 Gravitational Waves and Astrometry If we can pin down astrometric parameters with independent obs, the significance of any signal in the residuals should be improved: fewer parameters to fit. The path length difference between a pair of pulsars is a search parameter: parallaxes can vastly reduce the search space.
26 Gravitational Waves and Astrometry If we can pin down astrometric parameters with independent obs, the significance of any signal in the residuals should be improved: fewer parameters to fit. The path length difference between a pair of pulsars is a search parameter: parallaxes can vastly reduce the search space. Reference frame mismatch between ICRF and DE405 etc: may require an ensemble coordinate offset. Conceptually easy, but changes fitting procedure.
27 Talk Outline Applying VLB astrometry to pulsar timing: Can we improve our sensitivity to gravitational waves? Astrophysics: NS mass for PSR J Astrometry for Fermi-detected pulsars. Previews of coming attractions.
28 PSR J : an LMXB/MSP transition object Optical variability: accretion disk as recently as Radio pulsations: MSP (Archibald et al. 2009) Transition object from LMXB to recycled MSP.
29 PSR J : an LMXB/MSP transition object Optical variability: accretion disk as recently as Radio pulsations: MSP (Archibald et al. 2009) Transition object from LMXB to recycled MSP. P = 1.69 ms, Orbit = 4.75 hr. Variations in DM and P orbit. Frequency dependent eclipses. X-ray emission shows orbital modulation.
30 Declination offset (mas) PSR J : VLBA astrometry 10 5 Best astrometric fit Error ellipses for observations VLBA obs, : Right Ascension offset (mas) µ a = 4.76 ± 0.03 mas/yr µ d = ± 0.04 mas/yr π = 0.73 ± 0.02 mas D = pc (Deller et al. 2012)
31 PSR J : NS mass estimate Optical observations: companion T 5700 K. Photometry: physical size of Roche lobe as function of D. D = 2.20 (M c /M ) 1/3 kpc (Thorstensen & Armstrong 2005).
32 PSR J : NS mass estimate Optical observations: companion T 5700 K. Photometry: physical size of Roche lobe as function of D. D = 2.20 (M c /M ) 1/3 kpc (Thorstensen & Armstrong 2005). Pulsar timing: Mass ratio M psr /M c = 7.1 ± 0.1.
33 PSR J : NS mass estimate Optical observations: companion T 5700 K. Photometry: physical size of Roche lobe as function of D. D = 2.20 (M c /M ) 1/3 kpc (Thorstensen & Armstrong 2005). Pulsar timing: Mass ratio M psr /M c = 7.1 ± 0.1. ( M psr = (7.1 ± 0.1) D 2.20±0.02kpc) 3 M
34 PSR J : NS mass estimate Optical observations: companion T 5700 K. Photometry: physical size of Roche lobe as function of D. D = 2.20 (M c /M ) 1/3 kpc (Thorstensen & Armstrong 2005). Pulsar timing: Mass ratio M psr /M c = 7.1 ± 0.1. ( M psr = (7.1 ± 0.1) D 2.20±0.02kpc) 3 M VLBA astrometry: D = pc. NS Mass = 1.71 ± 0.16M.
35 PSR J : NS mass estimate Optical observations: companion T 5700 K. Photometry: physical size of Roche lobe as function of D. D = 2.20 (M c /M ) 1/3 kpc (Thorstensen & Armstrong 2005). Pulsar timing: Mass ratio M psr /M c = 7.1 ± 0.1. ( M psr = (7.1 ± 0.1) D 2.20±0.02kpc) 3 M VLBA astrometry: D = pc. NS Mass = 1.71 ± 0.16M. Roche lobe not filled? If so, lower limit on mass.
36 Talk Outline Applying VLB astrometry to pulsar timing: Can we improve our sensitivity to gravitational waves? Astrophysics: NS mass for PSR J Astrometry for Fermi-detected pulsars. Previews of coming attractions.
37 The Fermi gamma-ray space telescope LAT: Imaging high-energy gamma-ray telescope. 20 MeV 300 GeV; FoV covers 20% of the sky. Continous scanning: whole sky imaged every 3 hours.
38 Fermi 3-month all-sky image Note: Crab, Vela, Geminga, J , and Unidentified...
39 Fermi 3-month all-sky image Note: Crab, Vela, Geminga, J , and Unidentified Many new pulsars, especially recycled ones!
40 Gamma ray luminosity vs Spindown Ė Suggestive? But distance uncertainty limits usefulness...
41 Case study: PSR J Mass from Shapiro delay = 1.97(4) M (Demorest et al. 2010). Rules out most exotic quark matter equations of state.
42 Case study: PSR J Mass from Shapiro delay = 1.97(4) M (Demorest et al. 2010). Highest reliably measured NS mass. At D=1.2 kpc, L γ is also > 100% of Ė.... Happenstance? Coincidence?
43 Case study: PSR J Mass from Shapiro delay = 1.97(4) M (Demorest et al. 2010). Highest reliably measured NS mass. At D=1.2 kpc, L γ is also > 100% of Ė.... Happenstance? Coincidence?... Or might Ė = Iω ω be larger than expected?
44 Case study: PSR J Mass from Shapiro delay = 1.97(4) M (Demorest et al. 2010). Highest reliably measured NS mass. At D=1.2 kpc, L γ is also > 100% of Ė.... Happenstance? Coincidence?... Or might Ė = Iω ω be larger than expected? A precise distance may constrain the NS moment of inertia.
45 Ongoing astrometry programs Fermi/VLBA: A dozen γ-ray selected pulsars being followed. e.g., PSR J : 4 epochs observed.
46 Ongoing astrometry programs Fermi/VLBA: A dozen γ-ray selected pulsars being followed. e.g., PSR J : 4 epochs observed.
47 Ongoing astrometry programs Fermi/VLBA: A dozen γ-ray selected pulsars being followed. e.g., PSR J : 4 epochs observed.
48 Ongoing astrometry programs Fermi/VLBA: A dozen γ-ray selected pulsars being followed. e.g., PSR J : 4 epochs observed.
49 Ongoing astrometry programs Fermi/VLBA: A dozen γ-ray selected pulsars being followed. e.g., PSR J : 4 epochs observed. Can we do more? Yes we can! PSRπ: A large VLBA campaign on 280 pulsars!
50 Ongoing astrometry programs Fermi/VLBA: A dozen γ-ray selected pulsars being followed. e.g., PSR J : 4 epochs observed. Can we do more? Yes we can! PSRπ: A large VLBA campaign on 280 pulsars! 3 5 epochs observed (of 8) on 60 pulsars at 512 Mbps. Preliminary parallaxes down to 10 µas for best 4. At least 55 of 60 look promising... Can expand sample once 2 Gbps bit rates available at VLBA.
51 PSRPi: a preview of coming attractions
52 PSRPi: more coming attractions
53 A distance measuring service Is YOUR Neutron Star: A radio emitter? Brighter than ~1 mjy? Closer than ~8 kpc? North of 25 in Dec? Measure a parallax* with the VLBA! *Certain conditions, exclusions, and limitations apply. Please talk to the presenter or consult your friendly local expert about why the VLBA may be right for YOU!
54 A distance measuring service Is YOUR Neutron Star: A radio emitter? Brighter than ~1 mjy? Closer than ~8 kpc? North of 25 in Dec?... Limited Time Offer... Measure a parallax* with the VLBA! *Certain conditions, exclusions, and limitations apply. Please talk to the presenter or consult your friendly local expert about why the VLBA may be right for YOU!
55 Collaborators and Acknowledgements VLBA astrometry collaboration: Adam Deller, Walter Brisken, Joseph Lazio, James Cordes, Miller Goss, et al. Fermi pulsar collaboration: Scott Ransom, Fernando Camilo, Paul Ray, Michael Kramer, Lucas Guillemot, Maura McLaughlin, David Smith, Agnes Fienga, Gilles Theureau, Roger Romani, David Thompson, et al. NANOGrav:
New Radio Millisecond Pulsars in Fermi (formerly) Unassociated Sources
New Radio Millisecond Pulsars in Fermi (formerly) Unassociated Sources Scott Ransom (NRAO) For the Fermi Pulsar Search Consortium (PSC) Fermi Pulsars Currently 24 blind search pulsars (16 in Sci) Currently
Astrometric Observations of Neutron Stars
Astrometric Observations of Neutron Stars Shami Chatterjee 21 July 2009 Overview Neutron Stars are laboratories for extreme physics. Overview Neutron Stars are laboratories for extreme physics. We need
Radio counterparts of gamma-ray pulsars
Radio counterparts of gamma-ray pulsars Lucas Guillemot, MPIfR Bonn guillemo@mpifr-bonn.mpg.de on behalf of the Fermi LAT Collaboration IAU Symposium 2012, Beijing 20/08/12 117 gamma-ray pulsars! 41 young
Gamma-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
Discovery of a transitional Redback millisecond pulsar J !
Discovery of a transitional Redback millisecond pulsar J1227-4853! By Jayanta Roy!! JBCA, University of Manchester!! and!! National Centre for Radio Astrophysics (NCRA-TIFR) Neutron stars at the crossroads,
Measurements of Neutron Star Masses with a strong emphasis on millisecond binary radio pulsar timing
Measurements of Neutron Star Masses with a strong emphasis on millisecond binary radio pulsar timing David Nice, Lafayette College Physics of Neutron Stars 2014, Saint Petersburg 1. Motivation 2. How to
The Hunt for New Pulsars with the Green Bank Telescope
The Hunt for New Pulsars with the Green Bank Telescope Ryan Lynch Postdoctoral Fellow McGill University What we'll talk about... Two most recent large-area GBT pulsar surveys the 350 MHz Drift Scan Survey
Fermi-LAT Searches for gamma-ray pulsars
Fermi-LAT Searches for gamma-ray pulsars Pablo Saz Parkinson (pablo@scipp.ucsc.edu) for the LAT Collaboration Santa Cruz Institute for Particle Physics (SCIPP) IAU Symposium 291 Beijing, 20 August 2012
VLBI structure of PSR B /LS2883 during the 2007 and 2010 periastron passages
VLBI structure of PSR B1259-63/LS2883 during the 2007 and 2010 periastron passages Javier Moldón Marc Ribó Josep M. Paredes Simon Johnston, Ryan Shannon (ATNF -CSIRO) Adam Deller (NRAO/Berkeley) High Energy
Detecting Gravitational Waves. (and doing other cool physics) with Millisecond Pulsars. NANOGrav. Scott Ransom
Detecting Gravitational Waves (and doing other cool physics) with Millisecond Pulsars NANOGrav Scott Ransom What s a Pulsar? Rotating Neutron Star! Size of city: R ~ 10-20 km Mass greater than Sun: M ~
TeV Emission from Millisecond Pulsars in Compact Binaries? Mallory Roberts Eureka Scientific/NRL
TeV Emission from Millisecond Pulsars in Compact Binaries? Mallory Roberts Eureka Scientific/NRL Binary Period in Days Millisecond Pulsars Spun up by a low mass companion such that their spin period P
Pulsar Overview. Kevin Stovall NRAO
Pulsar Overview Kevin Stovall NRAO IPTA 2018 Student Workshop, 11 June, 2018 Pulsars Pulsars ~2,700 pulsars known Act as clocks, therefore provide a means for studying a variety of physical phenomena Strongly
Sources 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.
Pulsar Observations with the Fermi Large Area Telescope
Pulsar Observations with the Fermi Large Area Telescope First Light sky survey (4 days of exposure)) Launch: 11 June 2008 Gottfried Kanbach & Matthew Baring for the Fermi-LAT Collaboration 1 The high-energy
Fermi Large Area Telescope:
Fermi Large Area Telescope: Early Results on Pulsars Kent Wood Naval Research Lab kent.wood@nrl.navy.mil for the Fermi LAT Collaboration Tokyo Institute of Technology 7 March 2009 K. Wood (NRL) 1/30 Fermi
Probing Relativistic Gravity with the Double Pulsar
Probing Relativistic Gravity with the Double Pulsar Marta Burgay INAF Osservatorio Astronomico di Cagliari The spin period of the original millisecond pulsar PSR B1937+21: P = 0.0015578064924327 ± 0.0000000000000004
discovers a radio-quiet gamma-ray millisecond Journal Group
Einstein@Home discovers a radio-quiet gamma-ray millisecond pulsar @CHEA Journal Group Contribution of the paper Contribution of the paper Millisecond Pulsars (MSPs) Ver y rapid rotating neutron star
Radio Searches for Pulsars in the Galactic Center
Radio Searches for Pulsars in the Galactic Center J.Deneva (GMU, resident at NRL), P.Ray (NRL), S.Hyman (SBC), D.Frail (NRAO), N.Kassim (NRL), M. Kerr (NRL), J.Lazio (JPL) Outline Motivation. Types of
The Parkes Multibeam Pulsar Survey - III. Young Pulsars and the Discovery and Timing of 200 Pulsars
Haverford College Haverford Scholarship Faculty Publications Physics 2003 The Parkes Multibeam Pulsar Survey - III. Young Pulsars and the Discovery and Timing of 200 Pulsars M. Kramer J. F. Bell R. N.
Implications of a VLBI Distance to the Double Pulsar J A/B
arxiv:0902.0996v1 [astro-ph.sr] 5 Feb 2009 Implications of a VLBI Distance to the Double Pulsar J0737 3039A/B A.T. Deller 1, M. Bailes 1, S.J. Tingay 2 1 Centre for Astrophysics and Supercomputing Swinburne
imin...
Pulsar Timing For a detailed look at pulsar timing and other pulsar observing techniques, see the Handbook of Pulsar Astronomy by Duncan Lorimer and Michael Kramer. Pulsars are intrinsically interesting
WHAT ARE GALACTIC FIELD BLACK WIDOWS AND REDBACKS GOOD FOR? (EVERYTHING BUT GRAVITY WAVES) Mallory Roberts Eureka Scientific Jan. 22, 2013 Aspen, CO
WHAT ARE GALACTIC FIELD BLACK WIDOWS AND REDBACKS GOOD FOR? (EVERYTHING BUT GRAVITY WAVES) Mallory Roberts Eureka Scientific Jan. 22, 2013 Aspen, CO THE Black Widow PSR B1957+20 1.6 ms pulsar discovered
Pulsars and Radio Transients. Scott Ransom National Radio Astronomy Observatory / University of Virginia
Pulsars and Radio Transients Scott Ransom National Radio Astronomy Observatory / University of Virginia TIARA Summer School on Radio Astronomy 2016 Radio Transients Non-thermal emission Emission types
The Neutron Star Zoo. Stephen C.-Y. Ng ( 吳志勇 ) HKU
The Neutron Star Zoo Stephen C.-Y. Ng ( 吳志勇 ) HKU Overview Introduction to neutron stars Different classes of neutron stars: Radio Pulsars MSPs Magnetars DINS CCOs Unification 6/12/2017 NAOC Stephen Ng
Particle acceleration during the gamma-ray flares of the Crab Nebular
Particle acceleration during the gamma-ray flares of the Crab Nebular SLAC Accelerator seminar SLAC 15 June 2011 R. Buehler for the LAT collaboration and A. Tennant, E. Costa, D. Horns, C. Ferrigno, A.
Stellar 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
Pulsars. in this talk. Pulsar timing. Pulsar timing. Pulsar timing. Pulsar timing. How to listen to what exotic. are telling us! Paulo César C.
How to listen to what exotic Pulsars are telling us! in this talk 1. 2. 3. Test of gravitational theories using binary pulsars 4. Probing the equation of state of super-dense matter Paulo César C. Freire
Cooling Limits for the
Cooling Limits for the Page et al. 2004 Youngest Neutron Stars Cooling from the Youngest NSs SNR Zone NSs younger than ~50 kyr offer strong constraints on rapid cooling - the associated physical processes
A Pulsar Timing Array for Gravitational Wave Detection. Paul Demorest, NRAO
A Pulsar Timing Array for Gravitational Wave Detection Paul Demorest, NRAO About 10% of known radio pulsars are recycled millisecond pulsars (MSPs). These are spun up by accreting matter from a companion
Discovery 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
Recent Radio Observations of Pulsars
Recent Radio Observations of Pulsars R. N. Manchester Australia Telescope National Facility, CSIRO Sydney Australia Summary A pulsar census Recent pulsar surveys Pulse modulation and drifting subpulses
22 Years of a Pulsar-Be Binary System: From Parkes to the Heavens (Fermi) Ryan Shannon Postdoctoral Fellow, CSIRO Astronomy and Space Science
Credit: CSIRO/John Sarkissian 22 Years of a Pulsar-Be Binary System: From Parkes to the Heavens (Fermi) Ryan Shannon Postdoctoral Fellow, CSIRO Astronomy and Space Science Big Picture and Talk Outline
Pulsar Astronomy with GLAST Steve Thorsett UC Santa Cruz GLAST
Pulsar Astronomy with Steve Thorsett UC Santa Cruz Discovery of Neutron Stars: Pulsars In 1967, Jocelyn Bell discovered a strange, pulsating radio source (dubbed LGM 1) http://www.ggw.org/asras/ snimages/
X-ray emission properties vary with spin-down age. Crab-like pulsars (< 10 4 yrs)
X-ray emission properties vary with spin-down age Crab-like pulsars (< 10 4 yrs) X-ray emission properties vary with spin-down age Crab-like pulsars (< 10 4 yrs) Cooling neutron stars ( ~10 5-10 6 yrs)
The (obscene) Challenges of Next-Generation Pulsar Surveys
The (obscene) Challenges of Next-Generation Pulsar Surveys Scott Ransom NRAO / Univ. of Virginia Charlottesville, VA Haslam 408MHz Survey Summary: The Pulsar Search Problem Pulsars are faint we are sensitivity
MILLISECOND PULSARS. Merve Çolak
MILLISECOND PULSARS Merve Çolak OUTLINE Corbet Diagram (again) P-P(dot) Diagram MSPs and Their History Properties of MSPs Spin-up of Neutron Stars Spin-down of MSPs MSP Evolution Recent MSP Evolution Model
Pulsar Studies with the Shanghai TianMa Radio Telescope
Pulsar Studies with the Shanghai TianMa Radio Telescope Speaker:Zhen Yan * Shanghai Astronomical Observatory, CAS *On behalf of the Shanghai TianMa Radio Telescope Team 2017/7/12 1 Outline Introduction
The Fermi Large Area Telescope View of Gamma-ray Pulsars
The Fermi Large Area Telescope View of Gamma-ray Pulsars 1 Tyrel J. Johnson, D.A. Smith2, M. Kerr3, & P. R. den Hartog4 on behalf of the Fermi Large Area Telescope Collaboration and the Pulsar Timing and
MILLISECOND PULSAR POPULATION
MILLISECOND PULSAR POPULATION on Formation and Evolution Of Neutron Stars 11/12/2017 COMPANY NAME Outline 1. Millisecond Pulsars 2.Current Population 3.Applications 4.Future Prospects 4.1.Potential Science
SKADS Virtual Telescope: Pulsar Survey IV: Globular Cluster Pulsars
SKADS Virtual Telescope: Pulsar Survey IV: Globular Cluster Pulsars PI: S. Ransom Co-I: M. Kramer We propose to use the SKADS Virtual Telescope (SVT) to search Globular clusters for fast rotating pulsars
In Search of New MSPs for Pulsar Timing Arrays. Kevin Stovall, NRAO Socorro NANOGrav Collaboration
In Search of New MSPs for Pulsar Timing Arrays Kevin Stovall, NRAO Socorro NANOGrav Collaboration NRAO Postdoc Symposium, March 27, 2017 NANOGrav = US/Canada-based collaboration working to detect nhz GW
Recent Results in Pulsars: A Pulsar Renaissance. Scott Ransom
Recent Results in Pulsars: A Pulsar Renaissance Scott Ransom NRAO Charlottesville NAIC/NRAO Single-Dish Summer School 2005 What s a Pulsar? Discovered in 1967 by Jocelyn Bell and Antony Hewish at Cambridge
Pulsars and Timing. Lucas Guillemot, Ismaël Cognard.!! Rencontre CTA, Observatoire de Paris, 28/11/13
Pulsars and Timing Lucas Guillemot, Ismaël Cognard Rencontre CTA, Observatoire de Paris, 28/11/13 Pulsars radio emission cone γ-ray emission fan beam Pulsars are rapidly rotating highly magnetized neutron
Observations radio de pulsars binaires relativistes a Nancay
Observations radio de pulsars binaires relativistes a Nancay Ismael Cognard icognard@cnrs-orleans.fr LPC2E, CNRS - Universite d'orleans, France Nancay Radio Telescope I.Cognard - Pulsars binaires relativistes
Pulsars are Cool. Seriously. Scott Ransom National Radio Astronomy Observatory / University of Virginia
Pulsars are Cool. Seriously. Scott Ransom National Radio Astronomy Observatory / University of Virginia Neutron Stars Spin rates up to 716 Hz 1.2-2 Solar masses 10-12 km radii Central densities several
NS masses from radio timing: Past, present and future. Paul Demorest (NRAO) Symposium on Neutron Stars, Ohio U., May 2016
NS masses from radio timing: Past, present and future Paul Demorest (NRAO) Symposium on Neutron Stars, Ohio U., May 2016 Overview Review of how to measure neutron star masses via radio pulsar timing. Summary
The 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,
Fermi-Large Area Telescope Observations of Pulsar Wind Nebulae and their associated pulsars
Fermi-Large Area Telescope Observations of Pulsar Wind Nebulae and their associated pulsars Marie-Hélène Grondin CENBG, Bordeaux (France) on behalf of the Fermi-LAT Collaboration and the Pulsar Timing
Gravity Tests with Radio Pulsars
Gravity Tests with Radio Pulsars Norbert Wex Paris, June 21 st, 2010 Regimes of Gravity Tests (1) Quasi-stationary weak-field regime Solar system experiments (2) Quasi-stationary strong-field regime (3)
New Binary and Millisecond Pulsars from Arecibo Drift-Scan Searches
Binary Radio Pulsars ASP Conference Series, Vol. 328, 2005 F. A. Rasio and I. H. Stairs New Binary and Millisecond Pulsars from Arecibo Drift-Scan Searches M. A. McLaughlin, D. R. Lorimer, D. J. Champion
Future Gamma-Ray Observations of Pulsars and their Environments
Future Gamma-Ray Observations of Pulsars and their Environments David J. Thompson NASA Goddard Space Flight Center GLAST Large Area Telescope Collaboration djt@egret.gsfc.nasa.gov D. Thompson 363 rd Heraeus
The Time Evolution of Pulsar Wind Nebulae
The Time Evolution of Pulsar Wind Nebulae Okkie de Jager, S. Ferreira (NWU, South Africa) Science with the New Generation of High Energy Gamma-Ray Experiments (6th Workshop), Padova 8 10 October 2008 Contents
Isolated Neutron Stars: Calvera and Beyond
Isolated Neutron Stars: Calvera and Beyond Bob Rutledge McGill University Collaborators: Derek Fox and Andrew Shevchuk (PSU) Monica Turner (McGill) Jason Hessels, Ben Stappers X-ray Observations of Isolated
Recent Observations of Supernova Remnants
1 Recent Observations of Supernova Remnants with VERITAS Tülün Ergin (U. of Massachusetts Amherst, MA) on behalf of the VERITAS Collaboration (http://veritas.sao.arizona.edu) 2 Contents Supernova Remnants
The Formation of the Most Relativistic Pulsar PSR J
Binary Radio Pulsars ASP Conference Series, Vol. 328, 2005 F. A. Rasio and I. H. Stairs The Formation of the Most Relativistic Pulsar PSR J0737 3039 B. Willems, V. Kalogera, and M. Henninger Northwestern
Neutron Stars: Observations
Neutron Stars: Observations Ian Jones School of Mathematics, University of Southampton, UK Neutron star observations: overview From the observational point of view, neutron stars come in many different
Accretion 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
Pulsar Wind Nebulae as seen by Fermi-Large Area Telescope
Pulsar Wind Nebulae as seen by Fermi-Large Area Telescope Marie-Hélène Grondin Centre d'etudes Nucléaires de Bordeaux- Gradignan SNR/PWN Workshop Montpellier, 2010 June 1 th M.-H. Grondin, SNR/PWN Wokshop,
Remnants and Pulsar Wind
High Energy Supernova Remnants and Pulsar Wind Nebulae F. Giordano Dipartimento Interateneo di Fisica and INFN Sez. Bari For the Fermi-LAT Collaboration Scineghe 2010 The Afterlife of a star IC443 Crab
Evolution of the radio outflow in LS 5039 and PSR B
Evolution of the radio outflow in LS 539 and PSR B1259 63 Javier Moldón ASTRON Netherlands Institute for Radio Astronomy/Universitat de Barcelona M. Ribó, Josep M. Paredes Universitat de Barcelona Variable
Pulsar Sources for SEXTANT
Pulsar Sources for SEXTANT Paul Ray Space Science Division Naval Research Laboratory SEXTANT is supported by the NASA Space Technology Mission Directorate Energy Sources in X-ray Pulsars Rotational Kinetic
Fermi: 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
LIGO Status and Advanced LIGO Plans. Barry C Barish OSTP 1-Dec-04
LIGO Status and Advanced LIGO Plans Barry C Barish OSTP 1-Dec-04 Science Goals Physics» Direct verification of the most relativistic prediction of general relativity» Detailed tests of properties of gravitational
Pulsars 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
What 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
Gamma-ray binaries as pulsars spectral & variability behaviour Guillaume Dubus. Laboratoire d Astrophysique de Grenoble UMR 5571 UJF / CNRS
Gamma-ray binaries as pulsars spectral & variability behaviour Guillaume Dubus Laboratoire d Astrophysique de Grenoble UMR 5571 UJF / CNRS Image: Mirabel 2006 1 Pulsars & massive stars Young pulsars, magnetic
Pulsar Winds in High Energy Astrophysics
Pulsar Winds in High Energy Astrophysics Dmitry Khangulyan Institute of Space and Astronautical Science (ISAS/JAXA) The extreme Universe viewed in very high energy gamma-rays, Kashiwa 09/25/2012 OUTLINE
A Detailed Study of. the Pulsar Wind Nebula 3C 58
A Detailed Study of Collaborators: D. J. Helfand S. S. Murray S. Ransom F. D. Seward B. M. Gaensler E. V. Gotthelf E. van der Swaluw the Pulsar Wind Nebula 3C 58 Pulsar Wind Nebulae Young NS powers a particle/magnetic
A pulsar wind nebula associated with PSR J as the powering source of TeV J
A pulsar wind nebula associated with PSR J2032+4127 as the powering source of TeV J2032+4130, ASTRON, the Netherlands Institute for Radio Astronomy, and Departament d Astronomia i Meteorologia, Institut
Gamma-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
Radio timing observations of the pulsar by Kaspi et al. (1994) have
TIMING OBSERVATIONS OF THE SMC BINARY PSR J0045?7319 V. M. KASPI IPAC/Caltech/Jet Propulsion Laboratory Pasadena, CA, USA 91125 R. N. MANCHESTER AND M. BAILES ATNF/CSIRO Epping, Australia AND J. F. BELL
Fermi Gamma Ray Space Telescope: Launch+509. Roger Blandford KIPAC Stanford (With considerable help from Fermi team members working at Stanford)
Fermi Gamma Ray Space Telescope: Launch+509 Roger Blandford KIPAC Stanford (With considerable help from Fermi team members working at Stanford) 2 2 A Cosmic Reflection on Fermi s First Year Goals To summarize
The distance and radius of the neutron star PSR B
The distance and radius of the neutron star PSR B0656+14 Walter F. Brisken, 1 S. E. Thorsett, 2 A. Golden, 3 &W.M.Goss 1 ABSTRACT We present the result of astrometric observations of the radio pulsar PSR
Observing Galactic Sources at GeV & TeV Energies (A Short Summary)
1 Observing Galactic Sources at GeV & TeV Energies (A Short Summary) Tülün Ergin Univ. of Massachusetts, Amherst Air Cherenkov Telescopes 2 Past IACTs: HEGRA, Whipple, CANGAROO Present/Future IACTs: H.E.S.S.,
Lecture 13: Binary evolution
Lecture 13: Binary evolution Senior Astrophysics 2017-04-12 Senior Astrophysics Lecture 13: Binary evolution 2017-04-12 1 / 37 Outline 1 Conservative mass transfer 2 Non-conservative mass transfer 3 Cataclysmic
Les Pulsars gamma. avec GLAST
Les Pulsars gamma Gamma-ray Pulsars avec GLAST and search for gamma-quiet ones with Fermi David Smith Centre d Etudes Nucléaires de Bordeaux-Gradignan ( CENBG - in2p3 - CNRS ) David A. Smith, for the Fermi
Compact Binaries - 3 ASTR2110 Sarazin
Compact Binaries - 3 ASTR2110 Sarazin Zoology of Binary Stars X-ray Binary Pulsar Spin-Up Accreted material has high angular momentum Spins up neutron star (true of ~all X-ray binary pulsars) Millisecond
Prospects of continuous gravitational waves searches from Fermi-LAT sources
S. Mastrogiovanni for the LIGO Scientific Collaboration and the Virgo Collaboration Prospects of continuous gravitational waves searches from Fermi-LAT sources Outline Aim of the talk: I would like to
Millisecond Pulsar Populations in Globular Clusters
Millisecond Pulsar Populations in Globular Clusters David C. Y. Hui Department of Astronomy & Space Science Chungnam National University 1. Introduction 2. Dynamical formation of millisecond pulsars (MSPs)
Cherenkov Telescope Array ELINA LINDFORS, TUORLA OBSERVATORY ON BEHALF OF CTA CONSORTIUM, TAUP
Cherenkov Telescope Array A SENSITIVE PROBE OF EXTREME UNIVERSE ELINA LINDFORS, TUORLA OBSERVATORY ON BEHALF OF CTA CONSORTIUM, TAUP 2015 1 The CTA Observatory SST ( 4m) LST ( 23m) MST ( 12m) South North
TeV γ-ray observations with VERITAS and the prospects of the TeV/radio connection
TeV γ-ray observations with VERITAS and the prospects of the TeV/radio connection Matthias Beilicke for the VERITAS collaboration Washington University in St.Louis, Physics Department and McDonnell Center
arxiv:astro-ph/ v1 1 Sep 2005
For the Astrophysical Journal Letters Preprint typeset using L A TEX style emulateapj v. 2/19/04 GETTING ITS KICKS: A VLBA PARALLAX FOR THE HYPERFAST PULSAR B1508+55 S. Chatterjee 1, W. H. T. Vlemmings
Paul Demorest (NRAO) for NANOGrav collaboration, CHIME pulsar team John Galt Symposium, DRAO, Sept 23, 2014
Pulsars and CHIME: Gravitational Waves, the ISM and More! Paul Demorest (NRAO) for NANOGrav collaboration, CHIME pulsar team John Galt Symposium, DRAO, Sept 23, 2014 Outline Pulsar stuff: Pulsar timing
Measuring MNS, RNS, MNS/RNS or R
Measuring MNS, RNS, MNS/RNS or R Sebastien Guillot Advisor: Robert Rutledge Galileo Galilei Institute, Firenze March 2014 Some Reviews Lattimer and Prakash, 2007 Miller C., 2013 Heinke et al., 2013 Reminder
Pulsar Observation and Data Analysis Ryan Shannon Postdoctoral Fellow, CSIRO Astronomy and Space Science
Credit: John Sarkissian Pulsar Observation and Data Analysis Ryan Shannon Postdoctoral Fellow, CSIRO Astronomy and Space Science Outline What are pulsars? What are the requirements for instrumentation/observing
Identification of compact objects in X-ray/gamma-ray binaries and the exploration of long-period exoplanets by high-precision astrometry
X-ray binary Gaia Gaia-JASMINE Joint Meeting @NAOJ, 6-9 Dec. 2016 exoplanet ESA/ATG NAOJ Identification of compact objects in X-ray/gamma-ray binaries and the exploration of long-period exoplanets by high-precision
FORMATION 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
Introduction to Pulsar Timing. David Nice Lafayette College. International Pulsar Timing Array Student Workshop Banff, Alberta 16 June 2014
Introduction to Pulsar Timing David Nice Lafayette College International Pulsar Timing Array Student Workshop Banff, Alberta 16 June 2014 1. Extremely short overview 2. Measuring TOAs 3. What s in a timing
Observations of Gamma ray Spiders with the Fermi Large Area Telescope
Observations of Gamma ray Spiders with the Fermi Large Area Telescope Tyrel J. Johnson1 with P. S. Ray2, F. Camilo3, J. Roy4,5, and M. S. E. Roberts6 on behalf of the Fermi LAT collaboration 1. George
Long-term radio observations of orbital phase wander in six eclipsing pulsar binaries. Brian Prager Department of Astronomy University of Virginia
Long-term radio observations of orbital phase wander in six eclipsing pulsar binaries. Brian Prager Department of Astronomy University of Virginia Collaborators: Scott Ransom (NRAO), Phil Arras (UVa),
The Secret Life of Neutron Stars. Jeremy Heyl Harvard-Smithsonian CfA
The Secret Life of Neutron Stars Jeremy Heyl Harvard-Smithsonian CfA The Life of a 10 M Star PNS 10 5 yr 10 6 yr 10 7 yr 10 8 yr 10 9 yr 10 10 yr PMS MS Radio Pulsars Thermal Accretion-, Nuclear-, GWpowered
Anomalous X-ray Pulsars
Anomalous X-ray Pulsars GRBs: The Brightest Explosions in the Universe Harvard University, May 23, 2002 Vicky Kaspi Montreal, Canada What are Anomalous X-ray Pulsars? exotic class of objects 1st discovered
A pulsar wind nebula associated with PSR J as the powering source of TeV J
A pulsar wind nebula associated with PSR J2032+4127 as the powering source of TeV J2032+4130 Javier Moldón Netherlands Institute for Radio Astronomy Extreme Astrophysics in an Ever-Changing Universe Crete,
X-ray Observations of Rotation Powered Pulsars
X-ray Observations of Rotation Powered Pulsars George Pavlov (Penn State) Oleg Kargaltsev (George Washington Univ.) Martin Durant (Univ. of Toronto) Bettina Posselt (Penn State) Isolated neutron stars
New Insights from the Optical Study of Spiders
New Insights from the Optical Study of Spiders Rene Breton University of Manchester with many collaborators (V. Dhillon, J. Hessels, M. van Kerkwijk, M. Roberts, ) EWASS 25 June 2015 SDO/AIA/AEI Why Do
Collaborators: N. Wex, R. Eatough, M. Kramer, J. M. Cordes, J. Lazio
Kuo Liu Laboratoire de Physique et Chimie de l Environnement, LPCE UMR 6115 CNRS, F-45071 Orleans Cedex 02 Station de radioastronomie de Nancay, Observatoire de Paris, CNRS/INSU, F- 18330 Nancay, France
Progress in Pulsar detection
Progress in Pulsar detection With EINSTEIN & EXOSAT: 7 radio pulsars detected in X-rays With ROSAT, ASCA & BSAX: 33 radio pulsars detected in X-rays After ~8 yrs with XMM & Chandra: 81 radio pulsars detected
Gravity with the SKA
Gravity with the SKA Strong-field tests of gravity using Pulsars and Black Holes Michael Kramer Jodrell Bank Observatory University of Manchester With Don Backer, Jim Cordes, Simon Johnston, Joe Lazio
4U E. Bozzo. M. Falanga, A. Papitto, L. Stella, R. Perna, D. Lazzati G. Israel, S. Campana, V. Mangano, T. Di Salvo, L.
X-Ray Eclipse Time Delays in 4U2129+47 E. Bozzo M. Falanga, A. Papitto, L. Stella, R. Perna, D. Lazzati G. Israel, S. Campana, V. Mangano, T. Di Salvo, L. Burderi Università di Roma Tor Vergata, Italy
An 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