# Presentation: 460023

## X-Ray Emission from Supernovae 

**X-Ray Emission from Supernovae **

** ****Stefan Immler**
- CRESST NASA/GSFC

## Overview

**Overview**

**X-Ray SN research** is a relatively young field of science that was enabled by advanced in space flight and technologies.
- Since X-rays (~ 0.2–100 keV) are absorbed by the Earth’s atmosphere, telescopes and detectors have to be brought above the Earth’s atmosphere by either sounding rockets, air-borne balloons, or satellites.
- Until 1980, all attempts to detect a SN in X-rays failed, placing limiting luminosities around 1040 – 1045 ergs/s.
- Since the launch of HEAO 2 (renamed *Einstein Observatory* after launch) in 1978, space-based instruments had a high enough sensitivity & spatial resolution to search for X-rays from SNe.

## X-Ray Supernovae

**X-Ray Supernovae**

-   32 SNe have been detected in X-rays over the past 26 years
-     In the near aftermath (days to months) after their explosions.
-   X-ray luminosities range from 1034 ergs/s (SN 1987A)
-     to some 1041 ergs/s (e.g., SNe 1988Z, 1995N, 2002hi).
-   Approx. half of all detections are from *Chandra*
-   *XMM-Newton* only resulted in one new detection (SN 2002ap)
-     but is very successful in follow-up observations to monitor
-     the long-term X-ray evolution of SNe (see this talk).
-   Due to its rapid response and multi-wavelength coverage,
*    **Swift* is playing an increasingly important role in probing CSM
-     interaction with UV and X-ray observations of young SNe.
**Golden Age of X-Ray SN Research**

## X-Ray Supernovae

**X-Ray Supernovae**

**SN****	****	****	****Type****	****Instrument**
- 1970G		II		Chandra
- 1978K		II		Rosat
- 1979C		IIL		Rosat
- 1980K		IIL		Einstein
- 1981K		II		Chandra
- 1986J		IIn		Rosat
- 1987A		Iipec	Ginga
- 1988Z		IIn		Rosat
- 1993J		IIb		Rosat
- 1994I		Ic		Chandra
- 1994W		IIP 		Rosat
- 1995N		IIn		Rosat
- 1998bw	Ib/c		BeppoSax
- 1998S		IIn		Chandra
- 1999em	IIP		Chandra
- 1999gi		IIP		Chandra

**SN****	****	****	****Type****	****Instrument**
- 2001em	Ib/c		Chandra
- 2001gd	Iib		Chandra
- 2001ig		II		Chandra
- 2002ap	Ib/c		XMM-Newton
- 2002hh	II		Chandra
- 2002hi		Iin		Chandra
- 2003gb	Ic		Chandra
- 2003L		Ic		Chandra
- 2004dj		Ic		Chandra
- 2004et		II		Chandra
- 2005ip		IIn		Swift
- 2005kd	IIn		Swift
- 2005ke	Ia		Swift
- 2006aj		Ib/c		Swift
- 2006bp	IIP		Swift
- 2006jc		Ib/c		Swift

**32 total  —  22 type II  —  9 type Ib/c  —  1 type Ia**

## SN 1980K:  The First X-Ray SN

**SN 1980K:  The First X-Ray SN**

** ****SN 1980K** (type IIL) was discovered with *Einstein*, 35 days after maximum,
-   at a luminosity of 2 x 1039 ergs/s (0.2–4 keV band).
-  Observation on day 82 showed that the SN has faded by a factor of ~5.
-  Spectrum was soft and thermal, ~0.5 keV (Einstein), ~0.4 keV (Rosat).
-  Despite the large error box, ~1 arcmin, the X-rays could be attributed to the SN.

- Canizares et al. 1982
- Chevalier et al. 1982

## X-Ray Production Mechanism

**X-Ray Production Mechanism**

- Several X-ray production mechanism have been proposed to explain the observed X-ray emission (among others):
-  Initial burst of X-rays as the SN shock breaks out of the surface of the star.
-   Short duration (< 1,000 s), hard X-rays (> 100 keV) plus soft BB continuum
-   (e.g., SN 2006aj/GRB060218)
-  Radioactivity of the ejecta (e.g., SN 1987A)
-  Compton scattering of -rays
-  Inverse Compton scattering of relativistic e– on UV photons produced
-   during the explosion (e.g., SN 2002ap)
-  Pulsar driven X-rays from plerionic SNR
-  Circumstellar interaction: Interaction of the SN shock with SN environment.
-   CSM interaction is the most important X-ray production mechanism

## Circumstellar Interaction

- Stefan Immler / NASA GSFC

**Circumstellar Interaction**

**Ultraviolet and X-rays emission**

##     The Swift Observatory

**    ****The *****Swift***** Observatory**

- Broad** wavelength band coverage**:
-   Gamma-rays
-   X-rays (0.2–10 keV)
-   Ultraviolet (photometry + grism)
-   Optical (photometry + grism)
- Paired with its **fast response**,
*Swift* is ideally suited to study SNe

## SN 2006X and SN 1979C in M100

**SN 2006X and SN 1979C in M100**

-   SN 2006X (young type Ia) not detected in the UV and in X-rays
-   SN 1979C (type II) is one of the oldest SN still visible in UV and X-rays

- UVOT *UVW1, UVW2, UVM2*

- XRT 0.2–10 keV

- UVOT *V, B, U*

## SN 1979C in M100

**SN 1979C in M100**

-  High X-ray luminosity, *L*x = 8  1038 ergs/s (0.3–2 keV) at *t* = 26 years
-  High and constant mass-loss rate of  1.5  10–4 M yr–1 over
-    >20,000 yrs in the history of the progenitor

- Swift XRT

- Chandra ACIS

- XMM-Newton

## SNe 1978K and 1979C

**SNe 1978K and 1979C**

-  SNe 1979C and 1978K are the oldest known X-ray emitting SNe
-  Surprisingly similar evolution
-  Evolution is best described by a *t*2 rise followed by a *t*–3 decline

## SN 1993J

- Rosat PSPC detected
- SN 1993J on day 6 after the explosion, at
*L*x = 3  1039 ergs/s
- (0.1–2.4 keV)
- A softening of the emission
- from originally
*kT* > 7 keV     at *t* = 6 days to
*kT* = 0.5 keV  at  *t* = 41 days

**SN 1993J**

- Zimmermann et al. 1994

## SN 1993J

- XMM-Newton observation showed a two-temperature thermal plasma spectrum:
*kT*high = (6.5±2) keV  and
*kT*low  = (0.34±0.04) keV
- at *t* = 10 years.

**SN 1993J**

- Zimmermann & Aschenbach 2003

## SN 1993J

**SN 1993J**

- Zimmermann & Aschenbach 2003
- Poster by Nymark, Chandra & Fransson 2007
- Radiative reverse shock with a number of temp?

- XMM-Newton observation showed a two-temperature thermal plasma spectrum:
*kT*high = (6.5±2) keV  and
*kT*low  = (0.34±0.04) keV
- at *t* = 10 years.

## SN 1993J

- Stefan Immler / NASA GSFC

- Swift optical

- Swift X-rays

- Swift UV

**SN 1993J**

- M81

- Late-time X-ray observations with *Rosat*,* XMM-Newton*, *Chandra*, and *Swift* allowed to construct the long-term X-ray lightcurve over a >12 year period.

## SN 1993J

**SN 1993J**

- Multi-mission X-ray lightcurve shows an overall (slow) *t*–0.3 rate of decline
- with some ‘bumps’ from CSM density jumps.

- Zimmermann & Aschenbach 2003
- Immler, Aschenbach & Wang 2001

## SN 1998S in NGC 3877

*Chandra* ACIS:  							*XMM-Newton* MOS:
*L*x = 2.2 x 1039 ergs/s (0.4–2 keV)		*L*x = 1.5 x 1039 ergs/s (0.4–2 keV)
- 2.4 yrs after the outburst					3.1 yrs after the outburst

**SN 1998S in NGC 3877**

## SN 1998S in NGC3877

*Chandra*:  										*XMM-Newton*:
- Possible softening of the emission:				day 1140: 5.6 keV (2=0.92)
- day 678:   10 keV								or two-component model with
- day 1048:   8 keV								kThigh =   8 keV
- 												kTlow = 0.8 keV (2=1.02)
- (Pooley et al. 2002)								(Immler et al. 2005b)

**SN 1998S in NGC3877**

## SN 2005ke in NGC 1371

**SN 2005ke in NGC 1371**

- UVOT ultraviolet

- XRT X-rays (258 ks)

-  First detection of a type Ia SN in X-rays from CSM interaction?
-  Mass-loss rate of the progenitor’s companion 3  106 *M* yr1
-  CSM density 4  107 cm3 at a distance of 3  1015 cm

- Immler et al. 2006

## SN 2005ke in NGC 1371

- Swift UV lightcurves of type Ia supernovae

- UV lightcurve shapes of Type Ia supernovae are surprisingly similar
- ... *except:*

**SN 2005ke in NGC 1371**

- see talk by Peter Milne

## SN 2005ke in NGC 1371

-  Excess ultraviolet emission detected for SN 2005ke
-  Caused by the interaction of the supernova shock with dense CSM?
-  Evidence for a companion star?

**SN 2005ke in NGC 1371**

## SN 2005ke in NGC 1371

-  First tentative detection of CSM interaction for a SN Ia in X-rays
-  UV excess independently confirms CSM interaction
-  Direct obs. evidence for a massive companion star in a SN Ia system
-  Companion’s mass-loss rate and CSM matter density can
-    be measured for the first time for a SN Ia:
-    *M* = 3  106 *M* yr1
-    **CSM = 4  107 cm3 at a distance of *r* = 3  1015 cm

- .

**SN 2005ke in NGC 1371**

## SN Ia Systems

**SN Ia Systems**

- A **thermonuclear (Type Ia) supernova** is a white dwarf that accretes matter from a
- companion star and explodes as it reaches the Chandrasekhar mass (1.4x Sun).
- Unsolved question:  ***what is the companion star?***
- Two scenarios how thermonuclear SN (Type Ia) systems could look like

- White Dwarf

- White Dwarf

- White Dwarf

- Massive Star

- I)

- II)

## SN 2005kd

**SN 2005kd**

-  Type IIn SN
-  High X-ray luminosity, *L*x = 1.5  1041 ergs/s (0.2–10 keV)
-  High mass-loss rate of some 10–4 M yr–1

- Swift opt/uv

- Swift X-ray

- Immler, Pooley & Brown 2007

## SN 2005ip

**SN 2005ip**

-  Type IIn SN at 30 Mpc
-  High X-ray luminosity, *L*x = 1.6  1040 ergs/s (0.2–10 keV)
-  High mass-loss rate of some 10–4 M yr–1

- Swift optical

- Swift X-ray

- Swift UV

- Immler & Pooley 2007

## SN 2006jc

**SN 2006jc**

- The brightest SN observed by Swift (13 mag)

- Swift optical

- Swift ultraviolet

## SN 2006jc

**SN 2006jc**

- See posters by S. Holland and M. Bufano

## SN 2006jc

**SN 2006jc**

- Swift optical/UV

- Chandra X-rays

- SN 2006jc is detected in X-rays with Chandra on day 40 after explosion and
- brightening in X-rays in the ongoing Swift obs, mass-loss rate 9 x 10–6 M yr–1

## SN 2006bp in NGC 3953

**SN 2006bp in NGC 3953**

- .

-  Type IIP (‘plateau’) SN at *d* = 14.9 Mpc
-  Observed with Swift <1 day after the explosion
-  Detection of X-ray emission < 1 day after the explosion
-  Earliest detection of a SN in X-rays (minus GRB/SN), *L*x = 2  1039 ergs/s

- Swift UV

- Swift X-ray

- Swift optical

- Immler et al. 2007

## SN 2006bp in NGC 3953

**SN 2006bp in NGC 3953**

-  Daily *Swift* observations allow timing analysis of X-ray flux
-  SN would have been missed with any other observatory (XMM, Chandra)
-  With *Swift* we are probing a previously unexplored time domain for SNe
-  The SN is fading below the detection threshold within 10 days
-  Detection of previously unknown, variable ULX in the host galaxy

- Immler et al. 2007

## SN 2006bp in NGC 3953

**SN 2006bp in NGC 3953**

-  Recovered in an XMM-Newton DDT observation 21 days after outburst
-  X-rays is inconsistent with inverse Compton scattered photospheric photons
-   on relativistic electrons due to high required Lorentz factors (~10–100)

- Immler et al. 2007

## SN 2006bp in NGC 3953

**SN 2006bp in NGC 3953**

## SN 1970G in M101

*Chandra* 1 Ms X-ray survey of M101
- Detection of a point-like X-ray source at the position of SN 1970G 35 years after its explosion

**SN 1970G in M101**

- Immler & Kuntz 2005

## SN 1970G in M101

*Chandra* 1 Ms survey of M101 (Kuntz et al. 2005)
- Detection of a point-like X-ray source at the position of SN 1970G
*L*x = 1 x 1037 ergs/s
- At an age of 35 years, SN 1970G is the oldest known X-ray SN
- Recovered in previous ROSAT HRI and PSPC obs
- X-ray rate of decline of
*L*x  *t*-*s* with index *s* = 2.7

**SN 1970G in M101**

- Immler & Kuntz 2005

## SN 1970G in M101

**SN 1970G in M101**

- Mass-loss rate history:  no evolution over >30,000 yrs

## SN 1981K in NGC 4258

**SN 1981K in NGC 4258**

*L*x = 1.2 x 1037 ergs/s
- 20 years after the explosion.

- Immler, Li, Yang
- & Wilson 2007

## X-Ray Lightcurves of SNe

**X-Ray Lightcurves of SNe**

## The Environments of SNe

**The Environments of SNe**

## The Environments of SNe

**The Environments of SNe**

## The Mass-Loss Rates of SNe

**The Mass-Loss Rates of SNe**

**IIn**

**IIP**

**Ib/c**

## Summary

- X-ray observations of young SNe are uniquely suited to:
-  Measure key physical parameters of CSM interaction, such as
-     mass-loss rates of the progenitors over significant time-scales in the
-     evolution of the progenitor as a function of SN type and progenitor,
-     CSM densities in the environments of SNe out to large radii,
-  Study the temporal evolution of the forward and reverse shock,
-  New observations with Swift are used to probe the previously unexplored
-     time domain of the early UV and X-ray emission (< days) and probe
-     links between GRBs/SNe by observing SN related long-duration GRBs.

**Summary**

## Thank you

*Thank you*