A Holistic View of the GRB-SN Connection Alicia M Soderberg

A Holistic View of the GRB-SN Connection

Alicia M Soderberg Harvard University

(Credit: M. Bietenholz)

Monday, April 19, 2010 12 Years since GRB 980425

d=38 Mpc

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 12 Years since GRB 980425

d=38 Mpc

Happy Birthday

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 GRB-SN Connection

L ~ 1053 erg/s L ~ 1042 erg/s Emission Process =? Ni-56 decay Δt ~ seconds Δt ~ 1 month Hard X-ray Optical

(Credit: P. Challis)

Monday, April 19, 2010 Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 SN 1998bw at z=0.009

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 SN 1998bw at z=0.009 SN 2003dh at z=0.169

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 SN 1998bw at z=0.009 SN 2003lw at z=0.10 SN 2003dh at z=0.169

SN 2006aj at z=0.03

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 SN 1998bw at z=0.009 SN 2003lw at z=0.10 SN 2003dh at z=0.169

Most GRBs accompanied by Broad-lined SNe Ic

SN 2006aj at z=0.03

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 A GRB-SN Connection

Young SN Ibc Homologous v < 50,000 km/s M ~ M☉ E ~ 1051 erg

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 A GRB-SN Connection

Young SN Ibc Homologous reverse shock v < 50,000 km/s M ~ M☉ E ~ 1051 erg forward shock

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 A GRB-SN Connection

Young SN Ibc optical photosphere Homologous reverse shock v < 50,000 km/s radio/X-ray M ~ M☉ emission E ~ 1051 erg forward shock

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 A GRB-SN Connection

BH/NS Young SN Ibc optical photosphere Homologous reverse shock v < 50,000 km/s radio/X-ray M ~ M☉ emission E ~ 1051 erg forward shock

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 A GRB-SN Connection

BH/NS Young SN Ibc optical photosphere Homologous reverse shock v < 50,000 km/s radio/X-ray M ~ M☉ emission E ~ 1051 erg forward shock

gamma-rays

GRB Jet Thin Pancake v ~ 0.999c M ~ 10-5 M☉ E ~ 1051 erg

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 A GRB-SN Connection

BH/NS optical photosphere

reverse shock Young SN Ibc Freely-expanding radio/X-ray emission

forward shock RS FS

Afterglow

GRB Jet Decelerated

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Energy-velocity coupling

Optical Photosphere Ordinary SNe Ibc: Homologous Homologous E ~ v-5 Optical ~ E tot Radio ~ 0.01% x E tot

Radio/X-ray v = c v ~ c possible Blastwave (but E is tiny) (Tan, Matzner, McKee 2001) Kinetic Energy

Velocity

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Energy-velocity coupling

Optical Photosphere GRB-SNe

Homologous

Radio/X-ray v = c Blastwave Kinetic Energy

(Credit: A. MacFadyen) GRB = decoupled ejecta Velocity E > 0.01% at v ~ c

Requires a central engine

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Energy-velocity coupling

Optical Broadband Photosphere Afterglow Decoupled GRB-SNe

Homologous

Radio/X-ray v = c Blastwave Kinetic Energy

(Credit: A. MacFadyen) GRB = decoupled ejecta Velocity E > 0.01% at v ~ c

Requires a central engine

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 8-yr Radio Hunt for Engine-driven SNe Ibc

Target optically discovered SNe Ibc

IAUC• 8542: why? 2005ck; 2005ci; nearly Var STAR IN Nor all GRBs have a SNhttp://scully.cfa.harvard.edu/~cgi/PrinterVersion • IAUCsatellites 8542: miss 2005ck; weak 2005ci; GRBs, Var off-axis STAR IN GRBs Nor

SN The following International Astronomical Union Circular may be linked-to from your own Web pages, but must not otherwise be redistributed (see these notes on the conditions under which • circularsSN arediscoveries made available on our WWW rapidly, site). publicly announced

Read IAUC 8541 Read IAUC 8543

View IAUC 8542 in .dvi, .ps or .PDF format. CircularsDisplay: IAUC, IAUC number CBET, ATEL,Clear GCN

Circular No. 8542 Central Bureau for Astronomical Telegrams INTERNATIONAL ASTRONOMICAL UNION Mailstop 18, Smithsonian Astrophysical Observatory, Cambridge, MA 02138, U.S.A. [email protected] or FAX 617-495-7231 (subscriptions) [email protected] (science) URL http://cfa-www.harvard.edu/iau/cbat.html ISSN 0081-0304 KAIT Phone 617-495-7440/7244/7444 (for emergency use only)

SUPERNOVA 2005ck Independent discoveries of a supernova in the Abell galaxy cluster 1656 have been reported on unfiltered CCD images by H. Pugh and W. Li (LOSS/KAIT; cf. IAUC 8541) and by R. Quimby, F. Castro, P. Hoeflich, J. C. Wheeler (all at the University of Texas), and C. Gerardy (of Imperial College); Quimby's group used the ROTSE-IIIb telescope (cf. IAUC 8508). Pugh and Li provide the following precise position for SN 2005ck: R.A. = 13h02m18s.72, Decl. = +28o20'45".5 (equinox 2000.0), which is 58".3 east and 24".3 south of the center of an apparent host galaxy. Quimby et al. report position end figures 18s.77, 43".8 for the new object. Approximate magnitudes for SN 2005ck: 2004 Dec. 15, [18.8 (ROTSE-IIIb); 2005 Jan. 14, [18.8 (ROTSE-IIIb); Apr. 17.26 UT, [19.5 (KAIT); May 23.25, [18.5 (KAIT); June 1.26, 19.0: (KAIT; hint of object near limit of image); 5.27, 18.7 (ROTSE-IIIb); 8.25, 18.6 (ROTSE-IIIb); 12.24, 18.6 (KAIT); 13.24, 18.5 (KAIT). Quimby adds that a spectrum (range 420-890 nm) of SN 2005ck, obtained on June 13.22 with the 9.2-m Hobby-Eberly Telescope (+ Marcario Low-Resolution Spectrograph) by S. C. Odewhan and E. Terrazas, shows it to be a type-Ia supernova; the spectrum is very similar to that of SN 1994D near maximum light (Patat et al. 1996, MNRAS 278, 111). Using 1994D as a template, they find an approximate redshift of z = 0.08, ruling out any association to the neighboring Coma-cluster galaxies, Amateur Astronomers Robotic Searches leaving the host as yet unidentified.

SUPERNOVA 2005ci IN NGC 5682 Monday, April 19, 2010 M. Modjaz, R. Kirshner, and P. Challis, Harvard-Smithsonian Center for Astrophysics, report that a spectrogram (range 340-740 nm) of SN 2005ci (cf. IAUC 8541), obtained by M. Calkins on June

1 of 2 1/3/10 9:59 PM VLA Intensive Survey of “Naked” SNe (2002-present)

Prompt radio follow-up Very Large Array t ~ few days

Local SNe Ibc z < 0.04

7 year survey ~200 SNe Ibc

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 VLA Intensive Survey of “Naked” SNe (2002-present)

Prompt radio follow-up Very Large Array t ~ few days

Local SNe Ibc z < 0.04

7 year survey ~200 SNe Ibc

8.5 GHz

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Radio Luminosity Light-curves SNe Ibc x 104 = GRB afterglows

Nearby GRBs

(AMS 2007)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Radio Luminosity Light-curves SNe Ibc x 104 = GRB afterglows

Nearby GRBs

(AMS 2007) < 1% of SNe Ibc harbor GRBs

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Radio Modeling of SNe Ibc

• measure peak ﬂux, peak frequency -1 Synchrotron Self-Absorbed ν -2 -2 TB ∝ Lν ν R - • assume near equipartition (e & B)

ν5/2

9/19 -1 R ∝ Lν ν 23/19 -1

E ∝ Lν ν (AMS et al. Nature, 2008)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 VLA Intensive Survey of “Naked” SNe

Ordinary Type Ibc SNe v ≈0.15c E ≈ 1047 erg

Engine-driven Supernovae Γβ > 1 48 EK > 10 erg

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 The Ordinary SN 2007gr

NGC 1058 d=10 Mpc

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 The Ordinary SN 2007gr Freely expanding 26 Lν ~ 10 erg/s/Hz v ~ 0.2c E ~ 2 x 1046 erg (AMS et al., 2010)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 The Ordinary SN 2007gr

(Paragi et al., 2010)

Low S/N VLBI data at t=84 days

Fν = 60 μJy (expect 150 +- 40 μJy) decoupled jet, v > 0.6c ?

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 The Ordinary SN 2007gr

(Paragi et al., 2010)

(AMS et al., 2010) Low S/N VLBI data at t=84 days εe/εB < 10-9

Fν = 60 μJy (expect 150 +- 40 μJy) VLBI likely suffers from systematic effects decoupled jet, v > 0.6c ? Free-expansion more natural explanation

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 The Ordinary SN 2007gr

(Paragi et al., 2010)

(AMS et al., 2010) Low S/N VLBI data at t=84 days εe/εB < 10-9

Fν = 60 μJy (expect 150 +- 40 μJy) VLBI likely suffers from systematic effects decoupled jet, v > 0.6c ? Free-expansion more natural explanation

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 The Extra-ordinary SN 2009bb

NGC 3278 (40 Mpc)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 The Extra-ordinary SN 2009bb

NGC 3278 (40 Mpc)

SN 2009bb Discovered: Mar 21 2009 Explosion Date: Mar 19 +/- 1 day NO coincident GRB 48 EΥ < 10 erg

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 An Engine-driven SN without a GRB trigger

28 Lν ~ 5x10 erg/s/Hz (more luminous than 142 VISioNS SNe Ibc)

VLA + Giant Meterwave Radio Telescope Synchrotron self-absorbed radio spectra

300 MHz 22 GHz

(AMS et al. Nature, 2010) Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 An Engine-driven SN without a GRB trigger

v ≈ 0.9c Γ ~ 1.3 E > 1049 erg

(AMS et al. Nature, 2010)

Shock acceleration 53 requires Etot > 10 erg

09bb powered by a central engine

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 An Engine-driven SN without a GRB trigger

v ≈ 0.9c Γ ~ 1.3 E > 1049 erg

(AMS et al. Nature, 2010)

Shock acceleration 53 requires Etot > 10 erg

09bb powered by a central engine

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Independent Measurement of the Volumetric Rates

Long GRBs Supernovae Ibc 0.5 Gpc-3 yr-1 (on-axis) jets ~ 5-10 deg 2 x 104 Gpc-3 yr-1 50 Gpc-3 yr-1

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Independent Measurement of the Volumetric Rates

Long GRBs Supernovae Ibc 0.5 Gpc-3 yr-1 (on-axis) jets ~ 5-10 deg 2 x 104 Gpc-3 yr-1 50 Gpc-3 yr-1

+1.6 x 0.7 -0.6% =

VISioNs

✓ Consistent with rate of nearby GRBs

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Long-wavelength surveys are becoming a more powerful tool

PS1

Nearby GRB-SNe (z < 0.1) Υ-ray satellites ➠ 0.3 engine-driven SN/yr

optical + radio ➠ 1 engine-driven SN/yr

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Long-wavelength surveys are becoming a more powerful tool

PS1

Nearby GRB-SNe (z < 0.1) Υ-ray satellites ➠ 0.3 engine-driven SN/yr

optical + radio ➠ 1 engine-driven SN/yr

3 x higher discovery rate

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Welcome, GRB100316D / SN2010bh z=0.059

(Chornock et al. 2010) Broad-lined SN Ic Fastest GRB-SN

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Welcome, GRB100316D / SN2010bh z=0.059

(Chornock et al. 2010) Broad-lined SN Ic Fastest GRB-SN

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 First Systematic Study of Type Ibc Optical Light-Curves (Drout, AMS et al., in prep)

25 local SNe Ibc GOAL: (d < 150 Mpc) Luminosities of ordinary SNe Ibc

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 First Systematic Study of Type Ibc Optical Light-Curves

“Apples to Apples”

SN1998bw (d = 38 Mpc) SN2006aj (d=150 Mpc)

MR: “5-10% probability that GRBs and SNe produce similar Ni-56”

Extinction: “most SNe Ibc are extincted by E(B-V) > 0.3”

(Drout, AMS et al., in prep)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Conclusions

• Most long GRBs associated with SNe (e.g. 2010bh)

• GRB-SNe marked by decoupled ejecta components

• Radio orphan afterglows can reveal relativistic SNe without gamma-ray counterparts (e.g. 2009bb)

• SN2007gr is an ordinary SN

• The rate of engine-driven SNe is 0.7% of SNe Ibc

• SN2010bh is the most recent and fastest GRB-SN to date

• Ordinary SN Ibc can be as optically luminous as GRB-SNe

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 An Interesting Additional Point: Explosion Site Metallicity is High

SN2009bb

SNe GRBs

(Levesque, AMS et al. , ApJ 2010)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 An Interesting Additional Point: Explosion Site Metallicity is High

SN2009bb

SNe GRBs

Low metallicity is NOT(Levesque, required AMS et al.for , ApJ a relativistic2010) explosion

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Volumetric Rates

GRBs Supernovae Ibc 0.5 Gpc-3 yr-1 (on-axis) jets ~ 5-10 deg 2 x 104 Gpc-3 yr-1 50 Gpc-3 yr-1

x 0.1-1% =

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Volumetric Rates

GRBs Supernovae Ibc 0.5 Gpc-3 yr-1 (on-axis) jets ~ 5-10 deg 2 x 104 Gpc-3 yr-1 50 Gpc-3 yr-1

x 0.1-1% =

FAINT Radio/X-ray Emission STRONG Radio/X-ray Emission “Orphan Afterglow”

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 VLA Intensive Survey of “Naked” SNe (2002-present)

Very Large Array

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 VLA Intensive Survey of “Naked” SNe (2002-present)

Very Large Array

Only 15% detection rate

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Nov 2008 issue

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 #19 Even Oprah is convinced

Nov 2008 issue

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Optical Properties of SNe Ibc

• light-curves for 25 SNe Ibc from 2004-2006

• maximum light ➔ Nickel-56 mass

• compare with GRB-SNe Maria Drout Harvard-CfA REU 2009 SN 2004dk

Palomar 60-inch

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Optical Properties of SNe Ibc

• light-curves for 25 SNe Ibc from 2004-2006

• maximum light ➔ Nickel-56 mass

• compare with GRB-SNe Maria Drout Harvard-CfA REU 2009 SN 2004dk

Palomar 60-inch (Drout, AMS, et al. in prep)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Departures from Equipartition

Total Energy Budget Skyrockets when away from equipartition

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Why just 0.1-1% ?

Fast Rotation? Binary Companion?

High Mass?

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Why just 0.1-1% ? Low Metallicity? Low metallicity Consistent with data? inhibits mass loss retains angular momentum

Metallicity GRBs

Host galaxies a proxy for progenitor

small, faint hosts ➔ low metallicity Initial Mass (Heger et al., 2003) (Fruchter et al., 2006)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Why just 0.1-1% ? Low Metallicity? Low metallicity Consistent with data? inhibits mass loss retains angular momentum

Metallicity GRBs

Host galaxies a proxy for progenitor

small, faint hosts ➔ low metallicity Initial Mass (Heger et al., 2003) (Fruchter(Savaglio et al., et 2006)al., 2008)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Why just 0.1-1% ? Low Metallicity? Low metallicity Consistent with data? inhibits mass loss retains angular momentum

Metallicity GRBs

Host galaxies a proxy for progenitor small, faint hosts ➔Models low metallicity Initial Mass (Heger et al., 2003) (Fruchter(Savaglio et al., et 2006)al., 2008)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Conclusions

Conclusion #1: Most long-duration GRBs associated with SNe Ibc

Conclusion #2: < 1% of SNe Ibc harbor on-axis relativistic outﬂows

Conclusion #3: < 10% of SNe Ibc harbor off-axis relativistic outﬂows

48 Conclusion #4: Central-engine SNe require EK > 10 erg at Γβ > 1

Conclusion #5: We can discover ordinary SNe through shock-breakout X-rays

Conclusion #6: We can discover engine-driven SNe without a satellite trigger

Conclusion #7: Low metallicity is NOT required for a relativistic explosion

Conclusion #8: Lack of detected gamma-rays is NOT evidence for absence

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 VLA Intensive Survey of “Naked” SNe

Ordinary Type Ibc SNe v ≈0.15c E ≈ 1047 erg

Engine-driven Supernovae Γβ > 1 48 EK > 10 erg

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 VLA Intensive Survey of “Naked” SNe

Ordinary Type Ibc SNe v ≈0.15c E ≈ 1047 erg

Engine-driven Supernovae Γβ > 1 48 EK > 10 erg

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Are we sure SN2008D was not a gamma-ray burst?

SN 2008D at t=133 days VLBI ➔ sub-mas resolution 2 epochs: 30 and 133 days after explosion

R (trans) < 0.6 mas (3σ) ➔ v < 0.7c Proper motion < 0.3 mas in 100 days (3σ)

On-axis Jet: R (trans) = R / Υ (beaming)

GRB 030329 (z=0.17) is proof of concept (Taylor et al., 2004) At d=30 Mpc, expect 2.7 mas at 133 days

Off-axis Jet: Flux Centroid shift is best tool (Granot & Loeb, 2003) At d=30 Mpc, expect 1 mas / 100 days

(Bietenholz, AMS, Bartel, 2009) Regardless, an engine-driven SN requires 48 EK >10 erg coupled to relativistic ejecta Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Are we sure SN2008D was not a gamma-ray burst?

SN 2008D at t=133 days VLBI ➔ sub-mas resolution 2 epochs: 30 and 133 days after explosion

R (trans) < 0.6 mas (3σ) ➔ v < 0.7c Proper motion < 0.3 mas in 100 days (3σ)

On-axis Jet: R (trans) = R / Υ (beaming)

GRB 030329 (z=0.17) is proof of concept (Taylor et al., 2004) At d=30 Mpc, expect 2.7 mas at 133 days

Off-axis Jet: Flux Centroid shift is best tool (Granot & Loeb, 2003) At d=30 Mpc, expect 1 mas / 100 days

SN 2008D at t=133 days VLBI ➔ sub-mas resolution 2 epochs: 30 and 133 days after explosion

R (trans) < 0.6 mas (3σ) ➔ v < 0.7c Proper motion < 0.3 mas in 100 days (3σ)

On-axis Jet: R (trans) = R / Υ (beaming)

GRB 030329 (z=0.17) is proof of concept (Taylor et al., 2004) At d=30 Mpc, expect 2.7 mas at 133 days

Off-axis Jet: Flux Centroid shift is best tool (Granot & Loeb, 2003) At d=30 Mpc, expect 1 mas / 100 days

Young Supernova Free Expansion Double Shock System Optical = bulk ejecta (thermal) Radio/X-ray = fast ejecta (non-thermal)

Cas A

(Credit: R. Fesen)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Unique Electromagnetic Signals Radio & X-ray Emission

Young Supernova Free Expansion reverse shock Double Shock System Optical = bulk ejecta (thermal) Radio/X-ray = fast ejecta (non-thermal)

forward shock Cas A

(Credit: R. Fesen)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Unique Electromagnetic Signals Radio & X-ray Emission

optical photosphere Young Supernova Free Expansion reverse shock Double Shock System radio/X-ray Optical = bulk ejecta (thermal) emission Radio/X-ray = fast ejecta (non-thermal)

forward shock Cas A

(Credit: R. Fesen)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Unique Electromagnetic Signals Radio & X-ray Emission

BH/NS optical photosphere Young Supernova Free Expansion reverse shock Double Shock System radio/X-ray Optical = bulk ejecta (thermal) emission Radio/X-ray = fast ejecta (non-thermal)

forward shock Cas A

(Credit: R. Fesen)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Optical Follow-up

Broad-lined SN Ibc SN2009bb vphot ~ 22,500 km/s MV ~ -18.8 mag

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Radio/X-ray provide tools to answer open ?’s

Pre-Explosion Mass Loss History

(Credit: A. Spitkovsky) Particle Acceleration in Ampliﬁed Magnetic Fields

SN-GRB Connection

⇔

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 The Discovery of SN2008D: Key Players

NASA’s Swift satllite

Alicia Soderberg Edo Berger •Launched in 2004 •Orbit = 90 min •Three instruments: - gamma-ray (BAT) - X-ray (XRT) - UV-optical (UVOT) Neil Gehrels (PI Swift)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 The Discovery of SN2008D: Key Players

NASA’s Swift satllite

Cosmic Intervention

SN 2007uy Alicia Soderberg Edo Berger •Launched in 2004 •Orbit = 90 min •Three instruments: - gamma-ray (BAT) - X-ray (XRT) - UV-optical (UVOT) Neil Gehrels (PI Swift)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 The Birth of a Supernova: 2008D

Type Ibc supernova

t=0 t=hrs 1.7 d

X-ray UV/Optical

• Spectra reveal a very young SN Ibc

• earliest spectra ever taken of a SN

• X-ray pulse marks onset of explosion

(AMS et al. 2008)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Scientiﬁc & Public Notoriety

BONUS! 2009 night-sky guide pullout inside SPECIAL ISSUE January 2009

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Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Homologous Explosions: SNe Ibc

Photosphere compact v ~ 10,000 km/s remnant unshocked ejecta optical photosphere reverse shock ∝ v-5 shocked material radio/X-ray emission

forward shock

Kinetic Energy Kinetic Blastwave v ~ 50,000 km/s

Velocity

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Homologous Explosions: SNe Ibc

Photosphere compact v ~ 10,000 km/s remnant unshocked ejecta optical photosphere reverse shock ∝ v-5 shocked material radio/X-ray emission

forward shock

Kinetic Energy Kinetic Blastwave v ~ 50,000 km/s

Velocity

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Homologous Explosions: SNe Ibc

Photosphere compact v ~ 10,000 km/s remnant unshocked ejecta optical photosphere reverse shock ∝ v-5 shocked material radio/X-ray emission

forward shock

Kinetic Energy Kinetic Blastwave v ~ 50,000 km/s

Velocity

F XR < 10-3-10-6 Fopt

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 What we lose out on....

Non-thermal Synchrotron Emission e-

Encodes shock physics, explosion geometry, local environment SN1993J VLBI 4.9 GHz (Credit: M. Bietenholz) Monday, April 19, 2010 Stripped-Envelope Supernovae

BONUS! 2009 night-sky guide pullout inside SPECIAL ISSUE January 2009

The world’s best-selling astronomy magazine 10 STORIESTOP

Seeing a star’s2008 dying gasp • Phoenix tastes martian dirt • Brightest blast ever seen • The power behind aurorae • Fermi space telescope in orbit • How light makes binary asteroids • MESSENGER visits Mercury • The cosmos’ secret “dark flow” • A solar system just like home • Hot gravitational lens survey PLUS! Is our galaxy www.Astronomy.com running out of gas? p. 38 $5.95 Alicia M. Soderberg How Johannes Kepler 01 37 Vol. • Issue 1 Issue revolutionized astronomy p. 56 Hubble Fellow Learn the winter sky p. 70 0 72246 46770 1 Harvard-Smithsonian CfA Institute for Theory and Computation Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 GRB-SN study is limited to low-z

(Adapted from AMS et al, Nature, 2004)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 GRB-SN study is limited to low-z

SN 1998bw z=0.009

52 EK~10 erg, Mej ~ 10 Msun

(Adapted from AMS et al, Nature, 2004)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 GRB-SN study is limited to low-z

SN 2003lw z=0.1

(Malesani et al. 2004)

(Adapted from AMS et al, Nature, 2004)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 GRB-SN study is limited to low-z

SN 2006aj z=0.03 (Mazzali et al. 2006)

(Adapted from AMS et al, Nature, 2004)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 GRB-SN study is limited to low-z

XRF 020903 z=0.251 (Soderberg et al. 2005)

(Adapted from AMS et al, Nature, 2004)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 GRB-SN study is limited to low-z

SN 2003dh z=0.17 (Matheson et al. 2004)

(Adapted from AMS et al, Nature, 2004)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Extending technique to a more distant sample is tough

Red Bumps (Bloom et al. 2002)

(Adapted from AMS et al, Nature, 2004)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Extending technique to a more distant sample is tough

Red Bumps (Bloom et al. 2002)

(Adapted from AMS et al, Nature,Conclusion 2004) #1: Most long-duration GRBs associated with SNe Ibc

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Of-axis jets eventually become SPHERICAL

(Zhang & MacFadyen 2009)

Monday, April 19, 2010 Of-axis jets eventually become SPHERICAL

(AMS 2007)

(Zhang & MacFadyen 2009)

Monday, April 19, 2010 Of-axis jets eventually become SPHERICAL

< 10% of SNe Ibc harbor off-axis GRBs (AMS 2007) (Zhang & MacFadyen 2009)

Monday, April 19, 2010 Central Engines in GRB-SNe

• z < 0.1 GRBs low in Erel

• all show a SN copious non-rel ejecta

• more common factor of x 3-10

• continuum: SNe to GRBs?

(Adapted from AMS et al, Nature, 2004)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Central Engines in GRB-SNe

• z < 0.1 GRBs low in Erel

• all show a SN copious non-rel ejecta

• more common factor of x 3-10 low-z • continuum: SNe to GRBs?

(Adapted from AMS et al, Nature, 2004)

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Evidence for a GRB-SN connection

Spectra reveal SNe Ibc

Optical Light-curves Most gamma-ray bursts associated with supernovae

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010 Evidence for a GRB-SN connection

Spectra reveal SNe Ibc

Optical Light-curves

Alicia M. Soderberg Apr 20, 2010 Kyoto Talk Monday, April 19, 2010