evla constraints on the progenitors of supernovae type ia · evla constraints on the progenitors of...

Atacama Large Millimeter/submillimeter ArrayExpanded Very Large Array

Robert C. Byrd Green Bank TelescopeVery Long Baseline Array

EVLA Constraints on the Progenitorsof Supernovae Type Ia

Laura Chomiuk (Jansky Fellow, Harvard-Smithsonian CfA)Alicia M. Soderberg (Harvard)Roger Chevalier (Virginia)Carles Badenes (Tel Aviv)Claes Fransson (Stockholm)

What are the progenitors of Type Iasupernovae (and how do they explode)?

2

Single Degenerate or Double Degenerate?

How does radio trace circumstellar material?Optical Photosphere

~10,000 km/sForward Shock

~60,000 km/s

Swept-Up Circumstellar Material /Radio Emission

Synchrotron Emission

Energy densities of magnetic fieldand relativistic electrons scale with

post-shock energy density:Reverse

Shock

Relativistic electron

How does radio trace circumstellar material?Optical Photosphere

~10,000 km/sForward Shock

~60,000 km/s

Swept-Up Circumstellar Material /Radio Emission

Synchrotron Emission

Energy densities of magnetic fieldand relativistic electrons scale with

post-shock energy density:Reverse

Shock

Relativistic electron

No radio emission has ever been

detected from a SN Ia.

5

(fν < 15 µJy at 10 Mpc)

We can extend models for SNe Ibc to SNe Ia.

Current limits on Type Ia SNe

EVLA

Mdot / vwind = 10-10 10-9 10-8 10-7 10-6

M/yr / km/s

More bandwidth, More sensitivity

Can routinely reach rms ~ 7 µJy beam-1 in a 1 hour observation at 6 GHz.

SN 2010fz

“OSRO” 256 MHz BW -- 19 µJy bm-1 rms “RSRO” 2 GHz BW -- 7 µJy bm-1 rms

Chomiuk et al. 2010:NRAO eNews; ATEL 2467

VLA Limits

Panagia et al.2006

EVLA Limits

Panagia et al.2006

Conclusions

• The EVLA can detect the interaction of SNe Ia withcircumstellar material, testing single degenerate models.

• We have obtained five wide-band EVLA observations ofnearby SNe Ia.

• So far, all non-detections.

• The data are inconsistent with some single degeneratemodels. More detailed modeling is needed.

• Early optical detection and prompt EVLA triggering is key.

• EVLA program for 3 years and ~15 SNe …Stay tuned!

EVLA TargetsPhase (DaysFrom Max Light)

Bandwidth /3σ limit

DistanceID

256 MHz< 150 µJy bm-1

2 GHz< 18 µJy bm-1

2 GHz< 39 µJy bm-1

2 GHz< 21 µJy bm-1

1 GHz< 48 µJy bm-1

256 MHz< 45 µJy bm-1

-14(Kasliwal et al., ATEL2957)

101 MpcPTF 10ygu

3641 MpcSN 2010ko

1626 MpcSN 2010ih

-1023 MpcSN 2010fz

034 MpcSN 2010ev

-837 MpcPTF 10icb