Radio and X-ray observations of SN

2009ipPoonam Chandra

National Centre for Radio AstrophysicsJanuary 4, 2013

Collaborators: Raffaella Margutti (Harvard), Alicia Soderberg (Harvard), Roger Chevalier (University of Virginia)and more……..

Radio Observations: Karl G. Jansky Very Large Array

SN 2009ip – Radio Observations

Radio observations since September 26, 2012 till Dec 2, 2012, in K (22.5 GHz) and X (8.5 GHz) bands with the JVLA.

Date of Obs

Frequency (GHz)

Flux Density (uJy)

Sep 26.11 21.19 <131

Sep 26.14 8.94 <65

Sep 26.63 18 <66 (ATCA, Hancock et al. 2012)

Oct 16.06 21.25 79+/-29

Oct 17.12 21.19 108+/-40

Oct 26.04 8.85 44+/-15

Nov 06.06

21.19 <94

Nov 12.97

8.99 <92

Dec 01.99

21.25 <305

Dec 02.93

8.99 <544

Possible Detection?

SN 2009ip – X-ray observations

X-ray telescopes

XMM

Swift

SN 2009ip- Swift-XRT X-ray observations

Swift-XRT observations started from Sep 4 2012 until Dec 2012 in photon counting mode.

No X-ray emission during the decay of 2012a outburst i.e t<22nd Sept (3-sigma~3E-3 cps, 12.2ks).

No detection even during the rise time of the 2012b Sept 22nd < t < Oct 1st (3-sigma 1.1E-3 cps, 31.4ks).

X-ray emission detected starting from Oct 1st when 2012b outburst in 2012 reaches UV/optical peak.

Detection until Oct 16th and then no detection from Oct 20th onwards.

SN 2009ip – Swift X-ray observations

SN 2009ip- XMM-Newton X-ray observations

XMM-Newton observations on 3th Nov 2012. XMM observations for ~60ks for EPIC-PN and MOS in full frame thin filter mode.

SN detection, 4.5 sigma for a region of 10” (total 132 photons in 55 ks)

Data best fit with T>10 keV and NH~1E21 cm-2

Flux absorbed 1.7E-14 erg/s/cm2 and unabsorbed 1.9E-14 erg/s/cm2.

We use XMM parameters to fit Swift spectrum as well.

SN 2009ip – X-ray observations

Excess emission?

Swift spectrum around the peak (86ks)

Contaminating sourcePresence of contaminating source ~14” away

from the SN (Campana et al. 2012, Atel 4444).

XMM, Swift-XRT have not enough spatial resolution to exclude the contaminating source completely.

Study contamination by merging Swift non-detections as well as post SN detections.

Swift X-ray source at 22 23 09.19, -28 56 48.7 with uncertainty of 3.8” (12” away from SN).

SN 2009ip – X-ray observations

Contaminating source3.4 sigma detection of the contaminating

source.

Contaminating source count rate 3E-4 cps.

Source contaminates SN flux at the level of ~1.6E-4 cps or 6x10-15 erg/s/cm2.

This corresponds to luminosity 5x1038 erg/s, much less than SN luminosity (~1.5x1039 erg/s).

So not significant contamination.

SN 2009ip – radio and X-ray light curves

Peak radio and X-ray luminosities

2009ip

Thank You.

CollaboratorsRaffaella Margutti, Harvard

Alicia Soderberg, Harvard-Smithsonian

Roger Chevalier, University of Virginia

And more……..

Supernova Classification(based on optical spectra and light

curve)

Supernovae

HydrogenType II

Narrow H lines

Type IIn

No narrow H lines

Type IIP/IIL

No Hydrogen

Type I

SiliconType Ia

No SiliconType Ib/c

PlateauType IIP

LinearType IIL

HeliumType Ib

No HeliumType Ic

Circumstellar interaction

Circumstellar wind (1E-5 Msun/Yr)

Explosion center

Reverse Shock~1000 km/s

Forward Shock~10,000 km/s

Ejecta

Circumstellar medium density ~1/r2

Circumstellar interaction

Hot ejectaX-rays

SynchrotronRadio

Forward Shock ~109 K

Reverse shock ~ 107 K

Type IIn supernovaeVery diverse stellar evolution and mass loss history.

SN 1988z, extremely bright even after 20 years

SN 1994w faded only in 130 days.

SN 2005gl: LBV progenitor?

SN 2006gy, extremely bright: PISN progenitor?

SN 2002ic, SN 2005gj: Hybrid between Ia/IIN.

SNe 2001em, 1995N, 2008fz: Type Ib/c properties

SN 2009ip: episodic ejections before turning into true supernova

Multiwaveband campaign to understand Type IIn supernovae

Observe most the Type IIN supernovae with the JVLA telescope (PI: Chandra).

If detected in radio, follow with Swift-XRT (PI: Soderberg).

Follow radio bright and/or Swift detected Type IIN supernova with ChandraXO. Get spectroscopy, separate from nearby contamination (PI: Chandra).

If bright enough, do spectroscopy with XMM-Newton (PI: Chandra).

NIR photometry with PAIRITEL (PI: Soderberg).

Low frequency radio follow up with the GMRT

Chandra, Soderberg, Chevalier, Fransson, Chugai

SN 2009ipA Very Unique Type IIn supernova in NGC 7259 at 66

million light year away. Earlier supernova imposter which had repeated eruptions,

in 2009, 2010. Flared in July 2012 and then exploded as supernova in

September 2012 (speed 13,000 km/s)

Clear link with LBV progenitors (like SN 2005gl, 2006jc etc.)

10 year before explosion HST image shows the progenitor to be ~50-80Msun (massive blue progenitor)

SN 2009ip first SN to have both a massive blue progenitor and LBV like eruptions.