Simulations of Accretion Powered Supernovae in the Progenitors of Gamma Ray Bursts
EVLA Constraints on the Progenitors of Supernovae Type Ia · EVLA Constraints on the Progenitors of...
Transcript of EVLA Constraints on the Progenitors of Supernovae Type Ia · EVLA Constraints on the Progenitors of...
![Page 1: EVLA Constraints on the Progenitors of Supernovae Type Ia · EVLA Constraints on the Progenitors of Supernovae Type Ia Laura Chomiuk (Jansky Fellow, Harvard-Smithsonian CfA) Alicia](https://reader033.fdocuments.in/reader033/viewer/2022050413/5f8a276635f8373a35081893/html5/thumbnails/1.jpg)
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)
![Page 2: EVLA Constraints on the Progenitors of Supernovae Type Ia · EVLA Constraints on the Progenitors of Supernovae Type Ia Laura Chomiuk (Jansky Fellow, Harvard-Smithsonian CfA) Alicia](https://reader033.fdocuments.in/reader033/viewer/2022050413/5f8a276635f8373a35081893/html5/thumbnails/2.jpg)
What are the progenitors of Type Iasupernovae (and how do they explode)?
2
Single Degenerate or Double Degenerate?
![Page 3: EVLA Constraints on the Progenitors of Supernovae Type Ia · EVLA Constraints on the Progenitors of Supernovae Type Ia Laura Chomiuk (Jansky Fellow, Harvard-Smithsonian CfA) Alicia](https://reader033.fdocuments.in/reader033/viewer/2022050413/5f8a276635f8373a35081893/html5/thumbnails/3.jpg)
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
![Page 4: EVLA Constraints on the Progenitors of Supernovae Type Ia · EVLA Constraints on the Progenitors of Supernovae Type Ia Laura Chomiuk (Jansky Fellow, Harvard-Smithsonian CfA) Alicia](https://reader033.fdocuments.in/reader033/viewer/2022050413/5f8a276635f8373a35081893/html5/thumbnails/4.jpg)
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.
![Page 5: EVLA Constraints on the Progenitors of Supernovae Type Ia · EVLA Constraints on the Progenitors of Supernovae Type Ia Laura Chomiuk (Jansky Fellow, Harvard-Smithsonian CfA) Alicia](https://reader033.fdocuments.in/reader033/viewer/2022050413/5f8a276635f8373a35081893/html5/thumbnails/5.jpg)
5
(fν < 15 µJy at 10 Mpc)
![Page 6: EVLA Constraints on the Progenitors of Supernovae Type Ia · EVLA Constraints on the Progenitors of Supernovae Type Ia Laura Chomiuk (Jansky Fellow, Harvard-Smithsonian CfA) Alicia](https://reader033.fdocuments.in/reader033/viewer/2022050413/5f8a276635f8373a35081893/html5/thumbnails/6.jpg)
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
![Page 7: EVLA Constraints on the Progenitors of Supernovae Type Ia · EVLA Constraints on the Progenitors of Supernovae Type Ia Laura Chomiuk (Jansky Fellow, Harvard-Smithsonian CfA) Alicia](https://reader033.fdocuments.in/reader033/viewer/2022050413/5f8a276635f8373a35081893/html5/thumbnails/7.jpg)
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
![Page 8: EVLA Constraints on the Progenitors of Supernovae Type Ia · EVLA Constraints on the Progenitors of Supernovae Type Ia Laura Chomiuk (Jansky Fellow, Harvard-Smithsonian CfA) Alicia](https://reader033.fdocuments.in/reader033/viewer/2022050413/5f8a276635f8373a35081893/html5/thumbnails/8.jpg)
VLA Limits
Panagia et al.2006
![Page 9: EVLA Constraints on the Progenitors of Supernovae Type Ia · EVLA Constraints on the Progenitors of Supernovae Type Ia Laura Chomiuk (Jansky Fellow, Harvard-Smithsonian CfA) Alicia](https://reader033.fdocuments.in/reader033/viewer/2022050413/5f8a276635f8373a35081893/html5/thumbnails/9.jpg)
EVLA Limits
Panagia et al.2006
![Page 10: EVLA Constraints on the Progenitors of Supernovae Type Ia · EVLA Constraints on the Progenitors of Supernovae Type Ia Laura Chomiuk (Jansky Fellow, Harvard-Smithsonian CfA) Alicia](https://reader033.fdocuments.in/reader033/viewer/2022050413/5f8a276635f8373a35081893/html5/thumbnails/10.jpg)
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!
![Page 11: EVLA Constraints on the Progenitors of Supernovae Type Ia · EVLA Constraints on the Progenitors of Supernovae Type Ia Laura Chomiuk (Jansky Fellow, Harvard-Smithsonian CfA) Alicia](https://reader033.fdocuments.in/reader033/viewer/2022050413/5f8a276635f8373a35081893/html5/thumbnails/11.jpg)
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