time dependence of agn pair echo and halo
play

Time dependence of AGN pair echo, and halo emission as a probe of - PowerPoint PPT Presentation

Mar 02, 2024 •167 likes •503 views

Time dependence of AGN pair echo, and halo emission as a probe of extragalactic magnetic fields FO, Murase & Kotera, 2017, in prep FO, Murase & Kotera, PoS(ICRC2017)869 FO, Murase & Kotera, A&A 568, A110 (2014) ICRC2017 Foteini

  1. Time dependence of AGN pair echo, and halo emission as a probe of extragalactic magnetic fields FO, Murase & Kotera, 2017, in prep FO, Murase & Kotera, PoS(ICRC2017)869 FO, Murase & Kotera, A&A 568, A110 (2014) ICRC2017 Foteini Oikonomou - Penn State Busan-19 July 2017 1

  2. Introduction/Motivation B in structured region TeV emitting blazar B in voids 2

  3. Introduction/Motivation B in structured region TeV emitting blazar B in voids Emission scenarios: leptonic hadronic 2

  4. Introduction/Motivation B in structured region TeV emitting blazar B in voids Inverse Compton Emission scenarios: leptonic Synchrotron hadronic 2

  5. Introduction/Motivation B in structured region TeV emitting blazar B in voids Inverse Compton Emission scenarios: leptonic Synchrotron hadronic 2

  6. Introduction/Motivation B in structured region TeV emitting blazar B in voids Inverse Compton Emission scenarios: leptonic Synchrotron hadronic 2

  7. Blazar gamma-ray emission E ≲ 260 GeV γ EBL e + e - x x x x γ >GeV Costamante, 2012 3

  8. Inverse-Compton echo E ≲ 260 GeV γ EBL e + e - x x x x γ >GeV FO, Murase & Kotera PoS(ICRC2017)869 10 3 Fermi H.E.S.S. 10 2 E 2 dN/dE [eV cm -2 s -1 ] 10 1 10 0 10 -1 1ES 1101-232, z = 0.18 10 -2 10 8 10 9 10 10 10 11 10 12 10 13 10 14 energy/eV 4

  9. Inverse-Compton echo E ≲ 260 GeV γ EBL e + e - x x x x γ >GeV FO, Murase & Kotera PoS(ICRC2017)869 10 3 10 3 Fermi Fermi H.E.S.S. H.E.S.S. 10 2 10 2 E 2 dN/dE [eV cm -2 s -1 ] E 2 dN/dE [eV cm -2 s -1 ] 10 1 10 1 10 0 10 0 10 -1 10 -1 1ES 1101-232, z = 0.18 10 -2 10 -2 10 8 10 9 10 10 10 11 10 12 10 13 10 14 10 8 10 9 10 10 10 11 10 12 10 13 10 14 energy/eV energy/eV 4

  10. Inverse-Compton echo E ≲ 260 GeV γ EBL e + e - x x x x γ >GeV FO, Murase & Kotera PoS(ICRC2017)869 10 3 10 3 10 3 B = 10 -16 G, θ V =0 ° Fermi Fermi ∆ T =1000000 yrs H.E.S.S. H.E.S.S. 10 2 10 2 10 2 E 2 dN/dE [eV cm -2 s -1 ] E 2 dN/dE [eV cm -2 s -1 ] E 2 dN/dE [eV cm -2 s -1 ] 10 1 10 1 10 1 10 0 10 0 10 0 10 -1 10 -1 10 -1 1ES 1101-232, z = 0.18 10 -2 10 -2 10 -2 10 8 10 8 10 9 10 9 10 10 10 10 10 11 10 11 10 12 10 12 10 13 10 13 10 14 10 14 10 8 10 9 10 10 10 11 10 12 10 13 10 14 energy/eV energy/eV energy/eV 4

  11. Inverse-Compton echo E ≲ 260 GeV E ≲ 260 GeV γ EBL γ EBL e + e - e + e - x x x x x x γ >GeV γ >GeV FO, Murase & Kotera PoS(ICRC2017)869 10 3 10 3 10 3 10 3 B = 10 -16 G, θ V =0 ° B = 10 -16 G, θ V =0 ° Fermi Fermi ∆ T =1000000 yrs ∆ T =1000000 yrs H.E.S.S. H.E.S.S. B = 10 -15 G, θ V =0 ° 10 2 10 2 10 2 10 2 E 2 dN/dE [eV cm -2 s -1 ] E 2 dN/dE [eV cm -2 s -1 ] E 2 dN/dE [eV cm -2 s -1 ] E 2 dN/dE [eV cm -2 s -1 ] 10 1 10 1 10 1 10 1 10 0 10 0 10 0 10 0 10 -1 10 -1 10 -1 10 -1 1ES 1101-232, z = 0.18 10 -2 10 -2 10 -2 10 -2 10 8 10 8 10 8 10 9 10 9 10 9 10 10 10 10 10 10 10 11 10 11 10 11 10 12 10 12 10 12 10 13 10 13 10 13 10 14 10 14 10 14 10 8 10 9 10 10 10 11 10 12 10 13 10 14 energy/eV energy/eV energy/eV energy/eV 4

  12. Inverse-Compton echo E ≲ 260 GeV E ≲ 260 GeV γ EBL γ EBL e + e - e + e - x x x x x x γ >GeV γ >GeV FO, Murase & Kotera PoS(ICRC2017)869 10 3 10 3 10 3 10 3 10 3 B = 10 -16 G, θ V =0 ° B = 10 -16 G, θ V =0 ° B = 10 -16 G, θ V =0 ° Fermi Fermi ∆ T =1000000 yrs ∆ T =1000000 yrs ∆ T =1000000 yrs H.E.S.S. H.E.S.S. B = 10 -15 G, θ V =0 ° B = 10 -15 G, θ V =0 ° 10 2 10 2 10 2 10 2 10 2 E 2 dN/dE [eV cm -2 s -1 ] E 2 dN/dE [eV cm -2 s -1 ] E 2 dN/dE [eV cm -2 s -1 ] E 2 dN/dE [eV cm -2 s -1 ] E 2 dN/dE [eV cm -2 s -1 ] B = 10 -14 G, θ V =0 ° 10 1 10 1 10 1 10 1 10 1 10 0 10 0 10 0 10 0 10 0 10 -1 10 -1 10 -1 10 -1 10 -1 1ES 1101-232, z = 0.18 10 -2 10 -2 10 -2 10 -2 10 -2 10 8 10 8 10 8 10 9 10 9 10 9 10 10 10 10 10 10 10 11 10 11 10 11 10 12 10 12 10 12 10 13 10 13 10 13 10 14 10 14 10 14 10 8 10 8 10 9 10 9 10 10 10 10 10 11 10 11 10 12 10 12 10 13 10 13 10 14 10 14 energy/eV energy/eV energy/eV energy/eV energy/eV 4

  13. Inverse-Compton Echo-Transient FO, Murase & Kotera, 2017 [PoS(ICRC2017)869] E ≲ 260 GeV E ≲ 260 GeV γ EBL γ EBL e + e - e + e - x x x x x x γ >GeV γ >GeV 10 3 10 3 steady transient B = 10 -16 G, θ V =0 ° B = 10 -18 G, θ V =0 ° ∆ T =1000000 yrs ∆ T =10 yrs B = 10 -15 G, θ V =0 ° B = 10 -17 G, θ V =0 ° 10 2 10 2 E 2 dN/dE [eV cm -2 s -1 ] E 2 dN/dE [eV cm -2 s -1 ] B = 10 -14 G, θ V =0 ° B = 10 -16 G, θ V =0 ° 10 1 10 1 10 0 10 0 10 -1 10 -1 10 -2 10 -2 10 8 10 9 10 10 10 11 10 12 10 13 10 14 10 8 10 9 10 10 10 11 10 12 10 13 10 14 energy/eV energy/eV 5

  14. Inverse-Compton pair halo emission Neronov & Semikoz 2009 Fermi PSF 10 4 E =10.0-100.0 GeV ∆ T =1000000.0 yrs 1ES 1101-232, z = 0.18 dN/d θ 2 [deg -2 ] 10 2 10 0 B = 10 -15.0 G B = 10 -16.0 G PRELIMINARY B = 10 -17.0 G 10 -2 0 0.1 0.2 0.3 0.4 0.5 θ 2 [deg 2 ] 6

  15. Inverse-Compton pair halo emission Neronov & Semikoz 2009 Fermi PSF 10 4 10 4 B = 10 -17.0 G E =10.0-100.0 GeV E =10.0-100.0 GeV ∆ T =1000000.0 yrs 1ES 1101-232, z = 0.18 dN/d θ 2 [deg -2 ] dN/d θ 2 [deg -2 ] 10 2 10 2 t =100.0 yrs t =10000.0 yrs t =1000000.0 yrs 10 0 10 0 B = 10 -15.0 G B = 10 -16.0 G PRELIMINARY B = 10 -17.0 G 10 -2 10 -2 0 0 0.1 0.1 0.2 0.2 0.3 0.3 0.4 0.4 0.5 0.5 θ 2 [deg 2 ] θ 2 [deg 2 ] 6

  16. Formalism FO, Murase, Kotera, PoS(ICRC 2017) 869 Blumenthal & Gould 1970 d N d N d ε d n d ε ⟨ d σ KN � � d E d t = d γ e dE c (1 − µ ) ⟩ d γ e Fast implementation for Fermi Analysis Redshift energy losses Parameter surveys Benchmark with Monte Carlo (ELMAG) Exact geometry Off-axis formalism Full Klein-Nishina cross-section *see also Neronov & Vovk 2010, Taylor et al 2011, Dermer et al. 2011, Murase et al. 2012, Ichiki et al. 2010, 7 Dolag et al. 2011, Huan et al. 2011

  17. B in structured region TeV emitting blazar B in voids Inverse Compton Emission scenarios: leptonic Synchrotron hadronic 8

  18. UHECR induced synchrotron pair echo/halo *sensitive to EGMFs in structured regions Gabici, Aharonian 2005,7 λ syn < λ IC Kotera, Allard, Lemoine 2011 FO, Murase, Kotera 2014 prompt synchrotron γ -rays e + e - UHECRs x x filament/galaxy cluster B > nG typically ~few Mpc Tavecchio 2014 deabsorbed 9 9

  19. UHECR induced synchrotron pair echo/halo *sensitive to EGMFs in structured regions Gabici, Aharonian 2005,7 λ syn < λ IC Kotera, Allard, Lemoine 2011 FO, Murase, Kotera 2014 prompt synchrotron γ -rays e + e - UHECRs x x filament/galaxy cluster B > nG typically ~few Mpc ◆ 2 ✓ ◆ ✓ B E e Guaranteed when λ syn < λ IC E γ , syn ∼ 68 GeV 10 19 eV 10 nG FO, Murase & Kotera, A&A 568, A110 (2014) 0.1 nG 2 10 B = 6nG Example 1ES 0229+200 Mean free path (Mpc) E 2 dN/dE [eV s − 1 cm − 2 ] B = 16nG 1 nG (L CR,ISO = 10 46.5 erg s -1 ) B = 100nG λ Inv. Compton 1 10 B = 316nG HESS 10 nG VERITAS λ synchrotron Fermi/LAT 0 10 9 − 1 10 − 2 10 E (eV) 8 9 10 11 12 13 14 10 10 10 10 10 10 10 9 E [eV]

  20. UHECR induced synchrotron pair echo/halo *sensitive to EGMFs in structured regions Gabici, Aharonian 2005,7 λ syn < λ IC Kotera, Allard, Lemoine 2011 FO, Murase, Kotera 2014 prompt synchrotron γ -rays e + e - UHECRs x x filament/galaxy cluster B > nG typically ~few Mpc ◆ 2 ✓ ◆ ✓ B E e Guaranteed when λ syn < λ IC E γ , syn ∼ 68 GeV 10 19 eV 10 nG FO, Murase & Kotera, A&A 568, A110 (2014) 0.1 nG 2 10 B = 6nG Example 1ES 0229+200 Mean free path (Mpc) E 2 dN/dE [eV s − 1 cm − 2 ] B = 16nG 1 nG (L CR,ISO = 10 46.5 erg s -1 ) B = 100nG λ Inv. Compton 1 10 B = 316nG HESS 10 nG VERITAS λ synchrotron Fermi/LAT 0 10 9 − 1 10 − 2 10 E (eV) 8 9 10 11 12 13 14 10 10 10 10 10 10 10 9 E [eV]

  21. Summary/Outlook New analytical formalism to constrain EGMF strength with blazar pair-echoes/halos Developed for time-dependent pair-echo and pair-halo emission (transient sources) Treatment of off-axis emission (important for radio galaxies) Important for Fermi-LAT parameter surveys Synchrotron emission by UHECRs can explain hard-spectrum ultra-high energy peaked blazars (UHBLs) and probes MF strength in structured regions 10

  22. UHECR induced synchrotron pair echo/halo *sensitive to EGMFs in structured regions GeV cm − 2 s − 1 Kotera et al. 2011 assuming CTA at 10 GeV: ~ 10 -10 GeV cm -2 s -1 ( θ source /1°) Fermi 10 yrs D = 100 Mpc 
 at level of total CR flux * + flux integrated up to D = 1 Gpc 
 B = 1 nG angular extension θ D = 1 Gpc 
 E γ = 1 − 100 GeV 10% of total CR flux L CR,19 = 10 46 erg s − 1 Kotera et al. 2011 11

  23. FO, Murase & Kotera, 2017 [PoS(ICRC2017)869] Back-up: UHECRs vs. UHE neutrals *sensitive to EGMFs in structured regions UHECR x x Murase 2009,12 Dermer et al. x x UHE photons (protons confined) 12 12

  24. FO, Murase & Kotera, 2017 [PoS(ICRC2017)869] Back-up: UHECRs vs. UHE neutrals *sensitive to EGMFs in structured regions UHECR x x Murase 2009,12 Dermer et al. x x UHE photons (protons confined) UHECR, B =100 nG 3 10 UHECR, B = 316 nG 1ES 0229+200 spectra not E 2 dN/dE [eV s − 1 cm − 2 ] UHE � , B=100 nG 2 10 UHE � , B = 316 nG distinguishable! HESS 1 10 VERITAS Fermi/LAT 0 10 − 1 10 UHE photons B 3 Mpc = 316 nG − 2 10 α = 2, E γ , ΜΑΧ = 10 19.5 eV L CR,j ~ 10 45 erg s -1 − 3 10 8 9 10 11 12 13 14 12 12 10 10 10 10 10 10 10 E [eV]

Download Presentation
Download Policy: The content available on the website is offered to you 'AS IS' for your personal information and use only. It cannot be commercialized, licensed, or distributed on other websites without prior consent from the author. To download a presentation, simply click this link. If you encounter any difficulties during the download process, it's possible that the publisher has removed the file from their server.

Recommend

OVERVIEW What is ECHO? Why did our hospice become involved with ECHO? How did we ECHO?

OVERVIEW What is ECHO? Why did our hospice become involved with ECHO? How did we ECHO?

ECHO? E xtension O f C ommunity H ealthcare O utcomes OVERVIEW What is ECHO? Why did our hospice become involved with ECHO? How did we ECHO? What difference did it make? Outcomes from ECHO If you are interested. To share

767 views • 35 slides
The Right Knowledge. In the Right Place. At the Right Time. ECHO: A Revolutionary Model for

The Right Knowledge. In the Right Place. At the Right Time. ECHO: A Revolutionary Model for

The Right Knowledge. In the Right Place. At the Right Time. ECHO: A Revolutionary Model for Expanding Access to Specialized Care in Underserved Settings 2018 VIM Alliance National Conference 1 Objectives 1. Describe the ECHO model and its

731 views • 37 slides
Three tales of echo by Brayden Isaiah and Kobie Echo Echo lost her voice because Hera knew what

Three tales of echo by Brayden Isaiah and Kobie Echo Echo lost her voice because Hera knew what

Three tales of echo by Brayden Isaiah and Kobie Echo Echo lost her voice because Hera knew what was going on Hera was chasing Zeus and Echo and she punished Echo by Echo chattered and gossiped with Hera losing her voice and repeating and

315 views • 5 slides
The three tales of Echo By Alexis and Bella :) Interesting facts Did you know that Echo was a

The three tales of Echo By Alexis and Bella :) Interesting facts Did you know that Echo was a

The three tales of Echo By Alexis and Bella :) Interesting facts Did you know that Echo was a Greek mortal and Hera is a goddess and Hera is very jealous of Echo. One Beautiful voice now gone It was a day where Echo hid Zeus in the forest

538 views • 5 slides
Dependence Structures of Financial Time Series Martin Gartner December 14, 2007 Martin Gartner

Dependence Structures of Financial Time Series Martin Gartner December 14, 2007 Martin Gartner

Motivation Pearsons Correlation Coefficient Copulae Copula-based dependence measures Estimation and Calibration of a Copula Empirical Results Research Outlook Dependence Structures of Financial Time Series Martin Gartner December 14,

779 views • 49 slides
Knowledge Representation in Practice: Project Halo and the Semantic Web Mark Greaves Vulcan,

Knowledge Representation in Practice: Project Halo and the Semantic Web Mark Greaves Vulcan,

Knowledge Representation in Practice: Project Halo and the Semantic Web Mark Greaves Vulcan, Inc. markg@vulcan.com (206) 342-2276 Talk Outline The Halo Vision Systems AI Vulcans Halo Program The Halo Pilot: The Limits

385 views • 35 slides
Closest Pair of Points Cormen et.al 33.4 Closest Pair of Points Closest pair. Given n points in

Closest Pair of Points Cormen et.al 33.4 Closest Pair of Points Closest pair. Given n points in

Closest Pair of Points Cormen et.al 33.4 Closest Pair of Points Closest pair. Given n points in the plane, find a pair with smallest Euclidean distance between them. Fundamental geometric problem. Graphics, computer vision, geographic

585 views • 19 slides
Control-dependence Analysis 2 Control-dependence Analysis 1. Introduction (motivation, overview)

Control-dependence Analysis 2 Control-dependence Analysis 1. Introduction (motivation, overview)

Class 4 Basic Analyses (4) Assign (see Schedule for links) Readings Control/program-dependence analysis Static single assignment and control dependence Problem Set 2: due 9/1/09 1 Control-dependence Analysis 2

254 views • 12 slides
Linear dependence and independence Linear dependence 1 Definition (linear (in)dependence) Let {

Linear dependence and independence Linear dependence 1 Definition (linear (in)dependence) Let {

L INEAR A LGEBRA Berkant Ustao glu CRYPTOLOUNGE . NET Linear dependence and independence Linear dependence 1 Definition (linear (in)dependence) Let { v 1 , v 2 , . . . , v k } be a set of vectors. If v k = a 1 v 1 + a 2

382 views • 25 slides
ECHO 1. Appreciate the concept and approach of ECHO in general and ECHO Liver in particular

ECHO 1. Appreciate the concept and approach of ECHO in general and ECHO Liver in particular

Dis isclosures Jordan Feld: Research: Abbott, Abbvie, Gilead, Janssen, Merck Introduction to o Liv Liver Disea Diseases s &amp; Consulting: Abbvie, Contravir, Gilead, Merck ECHO Ontar ario Liv Liver Hemant Shah: Consulting

469 views • 7 slides
Measuring Dependence and Conditional Dependence with Kernels Kenji Fukumizu The Institute of

Measuring Dependence and Conditional Dependence with Kernels Kenji Fukumizu The Institute of

Measuring Dependence and Conditional Dependence with Kernels Kenji Fukumizu The Institute of Statistical Mathematics, Japan June 25, 2014. ICML 2014, Causality Workshop 1 2 Introduction Dependence Measures Dependence measures and

950 views • 32 slides
PHP/MySQL Michael Powell Basic PHP Echo Statement: &lt;?php echo Hello World; ?&gt;

PHP/MySQL Michael Powell Basic PHP Echo Statement: &lt;?php echo Hello World; ?&gt;

PHP/MySQL Michael Powell Basic PHP Echo Statement: &lt;?php echo Hello World; ?&gt; Variable and Echo: &lt;?php $var=Hello World; echo $var; ?&gt; Include: &lt;?php include(menu.php); ?&gt; MySQL: Things You Need Database

353 views • 23 slides
Kia Ora, Bula Vinaka, Talofa Lava, Halo, Kia Orana, Halo Olketa and welcome to the Business Link

Kia Ora, Bula Vinaka, Talofa Lava, Halo, Kia Orana, Halo Olketa and welcome to the Business Link

Kia Ora, Bula Vinaka, Talofa Lava, Halo, Kia Orana, Halo Olketa and welcome to the Business Link Pacific Webinar Series! When: Thursday 21 May 2020, 2pm NZST Webinar: SME Finance in times of crisis. Presenter: Paul Wendland, BLP Deputy

369 views • 15 slides
Assessing the dependence of high-dimensional time series via sample autocovariances and

Assessing the dependence of high-dimensional time series via sample autocovariances and

Assessing the dependence of high-dimensional time series via sample autocovariances and correlations Johannes Heiny Ruhr University Bochum, Germany Joint work with Thomas Mikosch (Copenhagen), Richard Davis (Columbia), and Jianfeng Yao (HKU).

695 views • 50 slides
ISLAM &amp; SOCIETY The Society of Dependence IS BEING MUSLIM IN AMERICA AN OXYMORON? Last time

ISLAM &amp; SOCIETY The Society of Dependence IS BEING MUSLIM IN AMERICA AN OXYMORON? Last time

ISLAM &amp; SOCIETY The Society of Dependence IS BEING MUSLIM IN AMERICA AN OXYMORON? Last time we asked the question. How do we feel about it now? REALITY &amp; BEING REAL Generally, by the time you are Real, most of your hair has

354 views • 16 slides
HALO TRIP 2009 East St. Louis The Forgotten City Meet Halo Who are we? King Hall

HALO TRIP 2009 East St. Louis The Forgotten City Meet Halo Who are we? King Hall

HALO TRIP 2009 East St. Louis The Forgotten City Meet Halo Who are we? King Hall Students committed to providing legal aid to those in need. What do we do? Provide volunteer opportunities throughout the year. Fundraise

710 views • 56 slides
Possibilities for Future SR and FEL Development in the UK. Richard Walker Technical Director,

Possibilities for Future SR and FEL Development in the UK. Richard Walker Technical Director,

Possibilities for Future SR and FEL Development in the UK. Richard Walker Technical Director, Diamond Light Source, UK r.p.walker@diamond.ac.uk www.diamond.ac.uk DDBA Review Meeting, Nov 25-26 2013 Synchrotron and Free Electron Laser

642 views • 43 slides
A synthetic synchrotron diagnostic for runaways in tokamaks Mathias Hoppe 1 Ola Embrus 1 , Alex

A synthetic synchrotron diagnostic for runaways in tokamaks Mathias Hoppe 1 Ola Embrus 1 , Alex

A synthetic synchrotron diagnostic for runaways in tokamaks Mathias Hoppe 1 Ola Embrus 1 , Alex Tinguely 2 , Robert Granetz 2 , Adam Stahl 1 , Tnde Flp 1 1 Chalmers University of Technology, Gothenburg, Sweden 2 PSFC, Massachusetts

404 views • 28 slides
Synchrotron Light Sources the next big thing Brookhaven National Broad band, polarized Light

Synchrotron Light Sources the next big thing Brookhaven National Broad band, polarized Light

Synchrotron Light Sources the next big thing Brookhaven National Broad band, polarized Light Source well-collimated and very intense (and fixed in space!) Light beam output Where e-beam turns Synchrotron advantage high brightness

652 views • 5 slides
Longitudinal Single Bunch Instability by Coherent Synchrotron Radiation T. Agoh (KEK)

Longitudinal Single Bunch Instability by Coherent Synchrotron Radiation T. Agoh (KEK)

Longitudinal Single Bunch Instability by Coherent Synchrotron Radiation T. Agoh (KEK) Motivation Short bunch length for a high luminosity Topics 1. Introduction 2. CSR in KEKB and SuperKEKB 3. Longitudinal Instability in SuperKEKB LER 4.

702 views • 14 slides
http://cs246.stanford.edu Would like to do prediction: estimate a function f(x) so that y = f(x)

http://cs246.stanford.edu Would like to do prediction: estimate a function f(x) so that y = f(x)

Note to other teachers and users of these slides: We would be delighted if you found our material useful for giving your own lectures. Feel free to use these slides verbatim, or to modify them to fit your own needs. If you make use of a

963 views • 52 slides
Dr. Hans-Georg Eer http://ohm.hgesser.de/ v1.0, 10/06/2013 Hans-Georg Eer, TH Nuremberg

Dr. Hans-Georg Eer http://ohm.hgesser.de/ v1.0, 10/06/2013 Hans-Georg Eer, TH Nuremberg

e t t r r i i e e b e m m - - Slide set 2: b s s s s y y s s t t e B. e B. Crash courses C / bash n t t w u n m i i t t w i i c c k k l l u n G E. E. n G m for self-study e r r a a t t e a m m m m i i n P r r O L. i i t t e

1.12k views • 75 slides
Tutorial 1 : Setting Up Your Unix Environment to work with Synopsys Tools Authors : Bibhas Ghoshal

Tutorial 1 : Setting Up Your Unix Environment to work with Synopsys Tools Authors : Bibhas Ghoshal

Tutorial 1 : Setting Up Your Unix Environment to work with Synopsys Tools Authors : Bibhas Ghoshal (bibhas.ghoshal@gmail.com), Subhadip Kundu (dip224@gmail.com) This tutorial guides you to set up your design libraries for both VLSI Design and

270 views • 4 slides
Week 1- Introduction to model checking B. Srivathsan Chennai Mathematical Institute NPTEL-course

Week 1- Introduction to model checking B. Srivathsan Chennai Mathematical Institute NPTEL-course

Week 1- Introduction to model checking B. Srivathsan Chennai Mathematical Institute NPTEL-course July - November 2015 1 / 14 Course overview 2 / 14 What are we interested in? 3 / 14 What are we interested in? Software Controllers Code that

219 views • 21 slides

More recommend