VLBI observations: VLBI observations: from AGN to young SNRfrom AGN to young SNR

Eduardo Ros & J. Anton ZensusEduardo Ros & J. Anton Zensus

MPIfR, Bonn, GermanyMPIfR, Bonn, Germany

Kashi, Sep 9Kashi, Sep 9thth 2005 2005

Pic

ture

: E. M

idde

lber

g (M

PIfR

)

The quest for resolutionThe quest for resolution Resolution = Observing wavelength / Telescope diameterAngularResolution

Optical (5000A)Diameter Instrument

Radio (4cm)Diameter Instrument

1 2mm Eye 140m GBT+1 10cm Amateur Telescope 8km VLA-B0.05 2m HST 160km MERLIN0.001 100m Interferometer 8200km VLBI

Jupiter and Io as seen from Earth1 arcmin 1 arcsec 0.05 arcsec 0.001 arcsec

Simulated with Galileo photo

Atmosphere gives 1" limit without corrections which are easiest in radio

The VLBI conceptThe VLBI concept

Resolution Resolution // DD !! cm to mm cm to mmD D !! 10 1044 km km

Beats Beats HSTHST in a in a factor 10factor 1022 ! !Radio interferometry Radio interferometry with unlimited with unlimited baselinesbaselinesNo link between No link between antennasantennasUses antennas built Uses antennas built for other reasonsfor other reasons

Beyond the Earth Limits: Beyond the Earth Limits: Space VLBISpace VLBI

VSOP VSOP Mission Mission (Japan, 1997-(Japan, 1997-today) – 8 m today) – 8 m dish, 23,000 dish, 23,000 km orbitkm orbit

Projects:Projects:– ARISE ARISE

(USA)(USA)– VSOP-2 (JP)VSOP-2 (JP)– RadioAstron RadioAstron

(RUS)(RUS)

Pushing towards high frequencies: Pushing towards high frequencies: millimetre VLBImillimetre VLBI

Successful Successful transatlantic transatlantic detections up to detections up to 2mm2mmRegular Regular operations of a operations of a 3mm network: 3mm network: Global Global Millimetre VLBI Millimetre VLBI ArrayArrayPushing towards Pushing towards 5/10 5/10 as as resolutions: resolutions: imaging the event imaging the event horizon in BHs?horizon in BHs?

VLBI science samplesVLBI science samples

CAPABILITY EXAMPLE SCIENCE

High resolution continuum High resolution continuum

Movies and polarizationMovies and polarization

Phase referencing to detect Phase referencing to detect weak sourcesweak sources

Phase referencing for positionsPhase referencing for positions

High resolution spectral lineHigh resolution spectral line

Spectral line moviesSpectral line movies

Geodesy and astrometryGeodesy and astrometry

Jet formation Jet formation

Jet dynamics and magnetic fieldsJet dynamics and magnetic fields

Detect survey sources, distinguish Detect survey sources, distinguish starbursts from AGNstarbursts from AGN

Accurate proper motionsAccurate proper motions

Accretion disks and extra galactic Accretion disks and extra galactic distancesdistances

Stellar environmentsStellar environments

Plate motions, EOP, reference framesPlate motions, EOP, reference frames

Active Galactic NucleiActive Galactic Nuclei

3C 120 – the movie3C 120 – the movie

Bottom: Contours Bottom: Contours intensity / Color intensity / Color polarized fluxpolarized fluxTop: Color intensity / Top: Color intensity / Lines B vectorsLines B vectorsResolution 50 Resolution 50 asasIntensity polarization Intensity polarization variations suggest jet-variations suggest jet-cloud interactioncloud interaction

GGómez et al., ómez et al., Science 289, 2317 (2000)Science 289, 2317 (2000)

The 2cm Survey – AGN KinematicsThe 2cm Survey – AGN Kinematics

1994-2001 measurements1994-2001 measurements110 sources studied110 sources studiedTypical speeds between 0 and 15c, up to 34cTypical speeds between 0 and 15c, up to 34cSpeed measurements consistent with Doppler factors Speed measurements consistent with Doppler factors varvar calculated from variabilitycalculated from variabilitySimilar speeds within the same jetSimilar speeds within the same jetData not consistent with ballistic modelsData not consistent with ballistic modelsMany jets show bends and twists, 30% of features show Many jets show bends and twists, 30% of features show non-radial motionsnon-radial motionsEGRET sources show faster speeds than non-EGRETEGRET sources show faster speeds than non-EGRET

Kellermann et al. ApJ 609, 539 (2004)Kellermann et al. ApJ 609, 539 (2004)

The twin jets in NGC 1052The twin jets in NGC 1052The radio galaxy NGC 1052 shows two twin jets with mildly relativistic plasma travelling at 0.25c. Movie produced from single VLBA observations at the 2cm Survey over almost 10 yr

Mov

ie:

M.

Ka

dler

& E

duar

do R

os (

MP

IfR

)

AGN at pc scales

Jet:Jet: VLBI imaging Accretion disk:Accretion disk:

X-ray spectroscopy

Young Supernova RemnantsYoung Supernova Remnants

SN 1054 – Crab NeulaSN 1054 – Crab Neula

1st observation: 05 Jul 1054

VLT Observations, 1999

Chaco Canyon Anasazi

What can we learn from RSNWhat can we learn from RSN

Interaction properties of the shock and the Interaction properties of the shock and the circumstellar matter (CSM): clumps, shell, circumstellar matter (CSM): clumps, shell, etc.etc.

Shock front: Rayleigh-Taylor instabilities, Shock front: Rayleigh-Taylor instabilities, particle acceleration mechanism, etc.particle acceleration mechanism, etc.

Progenitor system (single, binary)Progenitor system (single, binary)

Wind properties: mass-loss historyWind properties: mass-loss history

Type I b/c, II SNeType I b/c, II SNe

Type Ia SNeType Ia SNe

Radio SN modelsRadio SN models

Power law: N(E)Power law: N(E)=N=N00EE--pp

Environment densityEnvironment density: : // r r--nn

Radius of the (self-similar) expanding SN: Radius of the (self-similar) expanding SN: R R // t tmm, with , with mm=(=(nn-3)/(-3)/(nn-2)-2)

Mini-shell model Mini-shell model (Chevalier 1982)(Chevalier 1982)

S S // t t

=(1-=(1-pp)/2, )/2, =-(3-3=-(3-3mm--))

Radio SN modelsRadio SN models

Flux density at 5 GHz at t=1 day+t0 Spectral index

Time evolution

Optical depth

Attenuation from a clumpy medium

Attenuation from a continous medium

Optical depth at 5 GHz at t=1 day+t0

Thermal, ionised hydrogen

Time evolution, 0=5/3

Sta

ndar

d m

odel

Wei

ler

& V

an D

yk

Type Ib SN1983N Type Ib SN1983N @ @

1.4 and 5 GHz1.4 and 5 GHz

Type Ic SN1990BType Ic SN1990B @ @

1.4, 5, and 8.4 GHz1.4, 5, and 8.4 GHz

Taken from Weiler et al. (2002)Taken from Weiler et al. (2002)

8.4 GHz

1.4 GHz

5 GHz

1.4 GHz5 GHz

VLA VLA

1.4 GHz

(Sort of) canonical RSNe(Sort of) canonical RSNe

Type IType III SN19 SN1979C79C @ @

1.4, 5, and 15 GHz1.4, 5, and 15 GHz

Type IType II I SN19SN1980K @ 80K @

1.4 and 5 GHz1.4 and 5 GHz

(from Weiler et al. 2002)(from Weiler et al. 2002)

1.4 GHz

5 GHz

15 GHz

5 GHz

1.4 GHz

……and less canonical RSNeand less canonical RSNe

SN 1987A in the Large Magellanic SN 1987A in the Large Magellanic CloudsClouds

Image: Hubble Space Telescope Heritage

SN 1987ASN 1987A

Quick flux density evolution and low Brightness: evolution with the environmentVLBI shows a rapid expansion (≥ 19000 km/s)SN 1987A was unexpectedly brighter in radio at 1990.5 Complex environment is responsible

SN 1987A in the LMC, radioSN 1987A in the LMC, radio

Age: 5810 days;

Expansion: 3500±100 km s-1,

X-ray measurements, 5000±1000 km s-1

Staveley-Smith et al. (2004)

VLA, Feb. 1999

NucleusNucleus

SN1986J VLBISN1986J VLBI

(Pérez-Torres et al. 2002, MNRAS, L23)

SN 1986J in SN 1986J in NGC 891NGC 891

Explosion: 1982Explosion: 1982

First discovered First discovered in radio (1986), in radio (1986), afterwards, ist afterwards, ist optical optical counterpartcounterpart

VLBI structure is VLBI structure is non-symmetricnon-symmetric

SN1986J

NGC 891*

SN 1986J in NGC 891SN 1986J in NGC 891

Mean angular size Mean angular size »» 4.7 mas (0.22 pc) 4.7 mas (0.22 pc) !! v v»» 6300 km s 6300 km s-1-1 between 1998.74 and 1999.14between 1998.74 and 1999.14RR// t tmm, m=0.90, m=0.90§§0.06 (very close to free expansion)0.06 (very close to free expansion)Anisotropic brightness distribution: shell structure likely Anisotropic brightness distribution: shell structure likely due to a collision with a clumpy or filamentary winddue to a collision with a clumpy or filamentary wind

For standard vFor standard vwindwind=10 km s=10 km s-1-1, SN 1986J samples the , SN 1986J samples the CSM at time CSM at time »» 11000 yr; dM/dt 11000 yr; dM/dt »» 2 2££ 10 10-4-4 M M¯̄ yr yr-1-1 !! M Msweptswept»» 2.2 M2.2 M¯̄

Momentum conservation implies that MMomentum conservation implies that Menvenv ¸̧ 12 M 12 M¯̄

Single star scenario favouredSingle star scenario favoured

SN 1986J in NGC 891SN 1986J in NGC 891

Bietenholz et al. Science

A bright, compact radio component has been discovered, with an inverted radio spectrum

SN 2001gd in NGC 5033SN 2001gd in NGC 5033

Pre-discovery imagePre-discovery image

SN2001gdSN2001gd

NGC 5033

Image taken on 13 Jan 2002

SN 2001gd at SN 2001gd at 3.6 cm 3.6 cm

VLA

26.02.2002

08.04.2003

VLBI

VLBI

3.6 mJy

1.0 mJy

Pérez-Torres et al. (MNRAS, 2005)

Beam = 1.23 x 0.51 mas

1 mas @ 21.6 Mpc ~ 0.11 pc

VLBI image of SN 2001gdVLBI image of SN 2001gd

Angular estimates:Angular estimates:– Optically thick source:Optically thick source:

a=0.37a=0.37§§0.02 mas0.02 mas

b/a=0.45b/a=0.45§§0.22 mas0.22 mas

– Optically thin sphere:Optically thin sphere:0.390.39§§0.01 mas0.01 mas

– Optically thin ellipsoidOptically thin ellipsoida=0.41a=0.41§§0.02 mas0.02 mas

b/a=0.45b/a=0.45§§0.21 mas0.21 mas

Distance Inferred velocitiesDistance Inferred velocities

(Mpc) (1000 km s(Mpc) (1000 km s-1-1))

13.513.5 14.4 – 16.3 14.4 – 16.3

21.621.6 23 - 26 23 - 26

Pérez-Torres et al., MNRAS (2005)

The galaxies The galaxies M 81 & M 82M 81 & M 82

M 82: Starburst M 82: Starburst galaxygalaxy

M 81: Spiral galaxyM 81: Spiral galaxy

M82

M81

Images: APOD 12/30/2004 (left) & 04/01/2004 (right)

GALEX: UV image

The starburst galaxy M 82The starburst galaxy M 82

More than 50 radio sources, most of them are SNR.More than 50 radio sources, most of them are SNR.

Size from 1 to 15 lt-yrSize from 1 to 15 lt-yr

Pedlar et al. (2004)

SNR in SNR in M 82M 82

25 mas ~ 1 lt-yr

43.31+592 43.31+592 in M 82in M 82

Expansion speed 9850 km/s

Free expansion known since 1972. Probable explosion in the 1960s

Low pressure region?

SN1979C in M 100

SN 1979C in M100 (D=16.1 Mpc)SN 1979C in M100 (D=16.1 Mpc)

ttexplosionexplosion=April 4=April 4thth 1979 1979

VVexpansionexpansion=9200 km s=9200 km s-1-1 at t at t»» 45d 45d

Type II SN-LType II SN-LProgenitor: binary systemProgenitor: binary system

MMprogenprogen»» 17-18 M 17-18 M¯̄ (Van Dyk et al. 1999)(Van Dyk et al. 1999)

Radio emission interpreted within the mini-Radio emission interpreted within the mini-shell model shell model (Chevalier 1982)(Chevalier 1982)

(Mar

caid

e et

al.

200

2, A

&A

, 38

4, 4

08)

VLBI VLBI observations, observations, 18cm, 20 yr 18cm, 20 yr

after explosionafter explosion

Source size is model Source size is model dependent:dependent:– Optically thick disk: Optically thick disk:

4.574.57§§0.25 mas0.25 mas– Optically thin shell of Optically thin shell of

width 0.3 rwidth 0.3 routout: : 3.603.60§§0.17 mas0.17 mas

– Optically thin ring: Optically thin ring: 3.103.10§§0.14 mas0.14 mas

Best model: optically Best model: optically thin shellthin shell

(Marcaide et al. 2002, A&A, 384, 408)(Marcaide et al. 2002, A&A, 384, 408)

22.017.062.0;

mtR m

Strong deceleration in SN 1979CStrong deceleration in SN 1979C

SN 1979C – VLBI resultsSN 1979C – VLBI results

Strong deceleration phaseStrong deceleration phase

vvwindwind=10 km s=10 km s-1-1

dM/dt=1.2dM/dt=1.2££ 10 10-4-4 M M¯̄ yr yr-1-1

m=0.62 m=0.62 (strong interaction with CSM, s=2, (strong interaction with CSM, s=2, CSMCSM// r r-s-s))

ttbreakbreak=6=6§§2 yr2 yr

MMsweptswept=1.6 M=1.6 M¯̄

MMenvenv=0.9 M=0.9 M¯̄

Binary star scenario favouredBinary star scenario favoured

M 81 on April 26M 81 on April 26thth 19931993

SN 1993J

SN 1993J in M 81SN 1993J in M 81

Discovery of radio Discovery of radio shell structure shell structure (Marcaide et al. Nature, 1995)(Marcaide et al. Nature, 1995)

First supernova First supernova movie movie (Marcaide et al. (Marcaide et al. Science, 1995)Science, 1995)

Expansion at 15000 Expansion at 15000 km skm s-1-1 Deceleration Deceleration discovered. discovered.

Marcaide et al. Nature 373, 44-45 (1995)

Deceleration in the Deceleration in the expansion of SN 1993Jexpansion of SN 1993J

R ~ tm

m = (n - 3) / (n-s)

V ~ 9000 km/s after ~ 1300 days(M

arca

ide

et a

l. 1

997,

Ap

.J.4

86,

L31

)

Last results on the SN 1993J Last results on the SN 1993J evolutionevolution

The angular expansion has now been monitored for 12 years: – Changes in the deceleration, – Dependence of the angular size with the wavelength– Spectral index evolution. – The shell is circular and the expansion of the shock front is

isotropic.

SN 1993J – The movieSN 1993J – The movie

Young Supernova Remnant after the explosion of SN 1993J in M81 twelve years and half ago

Marcaide et al. (1995-2005)

SN 1993J – VLBI resultsSN 1993J – VLBI results

Self-similar expansion with m=0.86Self-similar expansion with m=0.86

Pre-supernova wind with s=1.66 (Pre-supernova wind with s=1.66 (CSMCSM// r r-s-s))

Outer layers of progenitor have n=11.2 (Outer layers of progenitor have n=11.2 (EJEJ»» r r-n-n))

Width of radio shell Width of radio shell »» 0.3 0.3 ££ outer radius outer radius

No emission from any central source > 0.5 mJyNo emission from any central source > 0.5 mJy

No evidence for large Rayleigh-Taylor No evidence for large Rayleigh-Taylor instabilitesinstabilites

SN1979C SN1986J SN2001gd SN1993J

Distance (Mpc) 16.1 9.6 21.6 3.63Time since explosion (yr) » 25 » 19 <1 >12

(L6cm / L6cm SN1993J)peak » 1.6 » 13 »2 1 Resolved by VLBI? Not yet Yes Not yet YesOptically thin phase? Yes Yes Likely yes Yes Radio brightness structure shell distorted shell --- ~smooth shell

(dM/dt) / (Msun/yr) »10-4 » 2 x 10-4 ? » 5 x 10-5

Deceleration parameter (m) 0.62 0.90 1.0? » 0.83 Asymmetric expansion? No Yes ? No (<5%)Circumstellar medium --- clumpy ? » smooth

Mswept / Msun 1.6 2.2 ? » 0.4

Menv / Msun 0.9 12 ? » 0.2-0.4

Explosion scenario Binary Single ? Binary Magnetic field amplification Turbulent ? Turbulent

tbreak (years) 6§2 ---- ---- » 1

Summary on young SNRSummary on young SNR

Compiled by M. A. Pérez-Torres

On VLBI arrays…On VLBI arrays…

The European VLBI NetworkThe European VLBI Network

Not shown: Arecibo Not shown: Arecibo (PR), Shanghai & (PR), Shanghai & Urumqi (CN), Urumqi (CN), Hartebeesthoek Hartebeesthoek (ZA)(ZA)Oncoming new Oncoming new telescopes:telescopes:– 40 m dish – Yebes, 40 m dish – Yebes,

Guadalajara, SpainGuadalajara, Spain– 70 m dish – 70 m dish –

Cagliari, Sardinia, Cagliari, Sardinia, ItalyItaly

– 100 m Kashi 100 m Kashi telescope – China ?telescope – China ?

Adding the Kashi telescope to the EVN…Adding the Kashi telescope to the EVN…

EVN SensitivitiesEVN Sensitivities

Eb+Mc+On+Tr+Jb2+Eb+Mc+On+Tr+Jb2+Cm+Wb+Nt+Sh+Ur+Cm+Wb+Nt+Sh+Ur+Hh Hh !! 32 32 JyJy

Sh+Ur+Hh Sh+Ur+Hh !! 452 452 JyJy

Eb+Mc+On+Tr+Jb2+Eb+Mc+On+Tr+Jb2+Cm+Wb+Nt+Sh+Ur+Cm+Wb+Nt+Sh+Ur+HhHh+Kashi+Kashi !! 18 18 JyJy

Sh+Ur+HhSh+Ur+Hh+Kashi+Kashi !! 74 74 JyJy

Image thermal noiseImage thermal noise150min integration time150min integration time

l6cm 6cm 256 Mbps rate256 Mbps rate

International Max Planck Research School International Max Planck Research School for Radio and Infrared Astronomy for Radio and Infrared Astronomy

at the Universities of Bonn and Cologneat the Universities of Bonn and Cologne

Graduate school Graduate school programprogram38 schools so far in 38 schools so far in GermanyGermanyPartnership MPIfR-Partnership MPIfR-University of BonnUniversity of Bonn26 students from 14 26 students from 14 nationalitiesnationalitiesWorldwide call for Worldwide call for applicationsapplications

http://www.mpifr-bonn.mpg.de/imprs