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]

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
Dark Matter Spikes in our Galactic Halo Dark Matter Spikes in our Galactic Halo Pearl Sandick

Dark Matter Spikes in our Galactic Halo Dark Matter Spikes in our Galactic Halo Pearl Sandick

Dark Matter Spikes in our Galactic Halo Dark Matter Spikes in our Galactic Halo Pearl Sandick the University of Texas at Austin in collaboration with Juerg Diemand, Katie Freese, &amp; Doug Spolyar Dark Matter Spikes in our Galactic Halo Dark

422 views • 28 slides
Galaxy Halo Assembly Simon White Max Planck Institute for Astrophysics Halo assembly for

Galaxy Halo Assembly Simon White Max Planck Institute for Astrophysics Halo assembly for

Arcetri, February 2009 Galaxy Halo Assembly Simon White Max Planck Institute for Astrophysics Halo assembly for neutralino CDM Typical first generation halos are similar in mass to the free- streaming mass limit Earth mass or below

2.07k views • 49 slides
Finding Galactic- halo substructure in the Gaia data Amina Helmi Stellar halo: treasure trove of

Finding Galactic- halo substructure in the Gaia data Amina Helmi Stellar halo: treasure trove of

Finding Galactic- halo substructure in the Gaia data Amina Helmi Stellar halo: treasure trove of merger relics t = 1 Gyr t = 2 Gyr Cosmological models characteristic: hierarchical growth: mergers Disrupted galaxies/debris naturally in a

732 views • 26 slides
Analysis of 2NM Separation for Minimal Pair Arrivals Investigating the relationship between

Analysis of 2NM Separation for Minimal Pair Arrivals Investigating the relationship between

Analysis of 2NM Separation for Minimal Pair Arrivals Investigating the relationship between separation minima and runway occupancy time Alan R. Groskreutz SESAR Innovation Days Dec 2, 2015 Overview Introduction Proposed Minimal-Pair

269 views • 24 slides
Project ECHO Nevada: Telementoring Providers to Help Im Improve Antimicrobial Stewardship

Project ECHO Nevada: Telementoring Providers to Help Im Improve Antimicrobial Stewardship

Project ECHO Nevada: Telementoring Providers to Help Im Improve Antimicrobial Stewardship August 15, 2017 Comparing Telemedicine and the ECHO Model 2 Anyt ytime, , Anywhere, Any Device 3 Project ECHO New Mexico 2003 - Sanjeev Arora

215 views • 10 slides
Geriatrics ECHO Clinic AIM Statement : The Geriatrics ECHO clinic will coach interprofessional

Geriatrics ECHO Clinic AIM Statement : The Geriatrics ECHO clinic will coach interprofessional

Geriatrics ECHO Clinic AIM Statement : The Geriatrics ECHO clinic will coach interprofessional teams on the principles of person-centered care for older adults with chronic health conditions. Disclaimer Video will be taken at this clinic and

762 views • 20 slides
EAE Echo Accreditation EAE Echo Accreditation Dr Kevin Fox Accreditation Project Lead, EAE Board

EAE Echo Accreditation EAE Echo Accreditation Dr Kevin Fox Accreditation Project Lead, EAE Board

EAE Echo Accreditation EAE Echo Accreditation Dr Kevin Fox Accreditation Project Lead, EAE Board Why did the EAE develop Why did the EAE develop Accreditation? To raise the standard of echo in Europe By encouraging learning By

429 views • 17 slides
Towards Incorporating Genetics in the ECHO-wide Cohort Council of Councils 7 September 2018

Towards Incorporating Genetics in the ECHO-wide Cohort Council of Councils 7 September 2018

Towards Incorporating Genetics in the ECHO-wide Cohort Council of Councils 7 September 2018 Matthew W. Gillman, MD, SM Director, Environmental influences on Child Health Outcomes (ECHO) Lynn R. Goldman, MD, MS, MPH Chair, ECHO External

667 views • 29 slides

More recommend