NASA's Chandra Sees Brightest Supernova Ever N. Smith et al. 2007, astro-ph/0612617v2.

Slides:



Advertisements
Similar presentations
Insights from Radio Wavelengths into Supernova Progenitors Laura Chomiuk Jansky Fellow, Michigan State University.
Advertisements

SN 1987A spectacular physics Bruno Leibundgut ESO.
The Flavours of SN II Light Curves Iair (“ya-eer”) Arcavi Advisor: Avishay Gal-Yam.
Lecture 20 White dwarfs.
The electromagnetic spectrum is A. all of the colors of light you can see with your eyes. B. all of the different types of electromagnetic waves. C. a.
Protostars, nebulas and Brown dwarfs
Stephen C.-Y. Ng McGill University. Outline Why study supernova? What is a supernova? Why does it explode? The aftermaths --- Supernova remnants Will.
The Deaths of Stars The Southern Crab Nebula (He2-104), a planetary nebula (left), and the Crab Nebula (M1; right), a supernova remnant.
Compact remnant mass function: dependence on the explosion mechanism and metallicity Reporter: Chen Wang 06/03/2014 Fryer et al. 2012, ApJ, 749, 91.
NuSTAR CIT JPL Columbia LLNL DSRI UCSC SLAC Spectrum The Nuclear Spectroscopic Telescope Array (NuSTAR) Hard X-ray ( keV) Small Explorer (SMEX) mission.
Supernovae Supernova Remnants Gamma-Ray Bursts. Summary of Post-Main-Sequence Evolution of Stars M > 8 M sun M < 4 M sun Subsequent ignition of nuclear.
RX J alias Vela Jr. The Remnant of the Nearest Historical Supernova : Impacting on the Present Day Climate? Bernd Aschenbach Vaterstetten, Germany.
The Story of Pulsational Pair-Instability SNe Briana Ingermann & Parke Loyd.
A Chandra view to Exploding Stars SN2014J R. Margutti Harvard nothing.
From Progenitor to Afterlife Roger Chevalier SN 1987AHST/SINS.
Low-luminosity GRBs and Relativistic shock breakouts Ehud Nakar Tel Aviv University Omer Bromberg Tsvi Piran Re’em Sari 2nd EUL Workshop on Gamma-Ray Bursts.
Supernovae from Massive Stars: light curves and spectral evolution Bruno Leibundgut ESO.
Stars and the HR Diagram Dr. Matt Penn National Solar Observatory
Neutron Star Formation and the Supernova Engine Bounce Masses Mass at Explosion Fallback.
Massive Star burps, then explodes Department of Physics National Tsing Hua University G.T. Chen 2007/5/1 April 4, 2007
Gamma-ray bursts Discovered in 1968 by Vela spy satellites
Two Supermassive Black Holes in the Same Galaxy. Profile of the Galaxy – NGC Discovered by NASA’s Chandra X-ray Observatory - Nucleus of the galaxy.
Supernovae Historically: “new stars” in sky Seen in 1006, 1054, 1181, 1572, 1604, 1680 SN 1054 visible in daytime sky for many months (Chinese records)
An X-ray Study of the Bright Supernova Remnant G with XMM-Newton SNRs and PWNe in the Chandra Era Boston, MA – July 8 th, 2009 Daniel Castro,
Radio studies of mysterious Type IIn supernovae Poonam Chandra National Centre for Radio Astrophysics Tata Institute of Fundamental Research Collaborators:
Active Galaxy Jets – An exhausting business Diana Worrall University of Bristol.
Supernovae and Gamma-Ray Bursts. Summary of Post-Main-Sequence Evolution of Stars M > 8 M sun M < 4 M sun Subsequent ignition of nuclear reactions involving.
Star Formation. Introduction Star-Forming Regions The Formation of Stars Like the Sun Stars of Other Masses Observations of Brown Dwarfs Observations.
A multi-colour survey of NGC253 with XMM-Newton Robin Barnard, Lindsey Shaw Greening & Ulrich Kolb The Open University.
Chapter 19 Star Formation
© 2010 Pearson Education, Inc. Chapter 21 Galaxy Evolution.
Dec. 6, Review: >8Msun stars become Type II SNe As nuclear burning proceeds to, finally, burning Silicon (Si) into iron (Fe), catastrophe looms.
SNLS-03D3bb Andy Howell University of Toronto and the Supernova Legacy Survey (SNLS)
Precise Cosmology from SNe Ia Wang Xiao-feng Physics Department and Tsinghua Center for Astrophysics, Tsinghua University 2005, 9, 22, Sino-French Dark.
A panchromatic view of the restless SN2009ip reveals the explosive ejection of a massive stellar envelope.
High Mass Stellar Evolution Astrophysics Lesson 13.
Multi-Epoch Star Formation? The Curious Case of Cluster Stephen Eikenberry University of Florida 11 April 2007.
22 nd February 2007 Poonam Chandra Unusual Behavior in Radio Supernovae Poonam Chandra Jansky Fellow, National Radio Astronomy Observatory Astronomy Department,
Gamma-Ray Bursts Energy problem and beaming * Mergers versus collapsars GRB host galaxies and locations within galaxy Supernova connection Fireball model.
The Transient Sky Eran Ofek CALTECH Shri Kulkarni Arne Rau Mansi Kasliwal Brian Cameron Avishay Gal-Yam Dale Frail Collaborators:
Ay 123 Lecture 11 - Supernovae & Neutron Stars Timescales for HS Burning faster and faster..
Radio and X-ray observations of SN 2009ip Poonam Chandra National Centre for Radio Astrophysics January 4, 2013 Collaborators: Raffaella Margutti (Harvard),
Are Stellar Eruptions a Common Trait of SNe IIn? Baltimore, MD 06/29/11 Ori Fox NPP Fellow NASA Goddard Based on arXiv:
Stochastic Wake Field particle acceleration in GRB G. Barbiellini (1), F. Longo (1), N.Omodei (2), P.Tommasini (3), D.Giulietti (3), A.Celotti (4), M.Tavani.
Circumstellar interaction of supernovae and gamma-ray bursts Circumstellar interaction of supernovae and gamma-ray bursts Poonam Chandra National Radio.
Chapter 12 Space Exploration. Section 12.1 page 428 Explaining the Early Universe GALAXY – collection of stars, planets, gas and dust held together by.
Earth & Space Science March 2015
ETA CARINAE – NATURE’S OWN HADRON COLLIDER We still do not know one thousandth of one percent of what nature has revealed to us. - Albert Einstein -
NGC4603 Cepheids in NGC4603 Planetary Nebula Luminosity Function Number.
Progenitor stars of supernovae Poonam Chandra Royal Military College of Canada.
Death of sun-like Massive star death Elemental my dear Watson Novas Neutron Stars Black holes $ 200 $ 200$200 $ 200 $ 200 $400 $ 400$400 $ 400$400.
I.Death of Stars White Dwarfs Neutron Stars Black Holes II.Cycle of Birth and Death of Stars (borrowed in part from Ch. 14) Outline of Chapter 13 Death.
Y. Matsuo A), M. Hashimoto A), M. Ono A), S. Nagataki B), K. Kotake C), S. Yamada D), K. Yamashita E) Long Time Evolutionary Simulations in Supernova until.
Chapter 12 Space Exploration. Section 12.1 page 428 Explaining the Early Universe GALAXY – collection of stars, planets, gas and dust held together by.
Study of the type IIP supernova 2008gz Roy et al. 2011, MNRAS accepted.
A New Window on Radio and X-ray emission from Strongly Interacting Supernovae Poonam Chandra Royal Military College of Canada Collaborators: Roger Chevalier,
Heaviest Stellar Black Hole in Nearby Galaxy CXC release Oct. 17, 2007 A M  in an eclipsing binary in the nearby spiral Galaxy Messier 33 ……Nature.
A black hole: The ultimate space-time warp Ch. 5.4 A black hole is an accumulation of mass so dense that nothing can escape its gravitational force, not.
Stochastic wake field particle acceleration in Gamma-Ray Bursts Barbiellini G., Longo F. (1), Omodei N. (2), Giulietti D., Tommassini P. (3), Celotti A.
Chapter 13 Post Main Sequence Stellar Evolution. The Sun.
American Astronomical Society – Austin, TX (2008) Patrick Slane (CfA) In collaboration with: D. Helfand (Columbia) S. Reynolds (NC State) B. Gaensler (U.
CIfAR Stanford 2008 SN Ia Rates: Theory, Progenitors, and Implications.
Gamma-Ray Bursts Please press “1” to test your transmitter.
CSI in SNRs You-Hua Chu Inst of Astron and Astroph
Supernovae and Gamma-Ray Bursts
Mid-infrared Observations of Aged Dusty Supernovae
Ay 123: Supernovae contd...
Dying Star Reveal More Evidence for New Kind of Black Hole
Chandra Science Highlight
Pair Instability Supernovae
Presentation transcript:

NASA's Chandra Sees Brightest Supernova Ever N. Smith et al. 2007, astro-ph/ v2

SN 2006GY  first detected by an optical robotic telescope as part of the Texas Supernova Search project on September 18,  peak magnitude of −22  the total radiated energy Erad = (1.0 ± 0.2) × erg  Host galaxy : NGC 1260  distance : 73.1 Mpc

Fig. 5. — Soft band (0.5 – 2 keV) Chandra images of NGC Panel a shows the raw Chandra data (after our astrometric correction) with red and blue arrows indicating the KAIT positions of the SN and galaxy nucleus, respectively. Panel b is a Gaussian-smoothed version of this image, in which the sources are more clearly apparent. Panel c is a maximum likelihood reconstruction of the 0.5 – 2 keV image (see text for details). Panel d shows the Chandra PSF at the location of the galaxy on the same spatial scale as the other panels.

Light Curve It had a very slow rise to maximum that took about 70 days and stayed brighter than −21 mag for about 100 days.

Spectrum

the Hα line of SN 2006gy implies the wind speed to be about 200 km s −1 (V w1 = 20); the shock velocity to be about 4500 km s −1 (V s4 = 0.45)

Possible Mechanism  (1) H recombination/thermal radiation of the supernova ejecta  (2) interaction of the supernova blast wave with circumstellar material  (3) energy from radioactive decay of 56 Ni

Problems-(1)  thermal emission from the H-recombination front in the supernova debris would require a huge ejected mass of order 100 M ⊙ or more. A heavy H envelope might help explain the unusually slow speed of only about 4000 km s −1 indicated by the H line, and might provide a natural explanation for the long duration and rise time of the SN because of time needed for energy to diffuse out of the massive envelope.  However, Instead of 70 d, the observed peak luminosity would seem to require an age of d since explosion (assuming linear motion), or (more likely) rapid deceleration at early times.

Problems-(2)  The mass-loss rate for the progenitor from x-ray data is about 5 × 10 −4 M ⊙ yr −1. We find that it falls short of the circumstellar density that would be needed to power the visual light curve of SN 2006gy by three orders of magnitude. That account for why we observe a relatively weak and soft (i.e., unabsorbed) X-ray flux from SN 2006gy.  In order to power the luminosity of SN 2006gy with CSM interaction, the environment created by the progenitor star must be extraordinarily dense. So the required progenitor mass-loss rate even further to about 0.5 M ⊙ yr −1. The only type of star known to have a mass-loss rate higher than 0.1 M ⊙ yr −1 would be an LBV during a giant eruption.

Problems-(3)  The extreme luminosity of SN 2006gy would require an extraordinarily high Ni mass of roughly 22 M ⊙ to be synthesized in the explosion. The large Ni mass implicates a progenitor star that began its life with a mass well above 100 M ⊙.  The only way to get such an extraordinarily high Ni mass to power the radiated energy would be from a pair-instability supernova, where the star ’ s core is obliterated instead of collapsing to a black hole.

Other argument  With the observed Hα luminosity and densities, it is difficult to avoid a nebular mass below 2 M ⊙, and it could plausibly be as high as 20 – 30 M ⊙. The nebular shells around LBVs with L > 10 6 L ⊙, which descend from stars have initial masses of 80 – 150 M ⊙. Interestingly, such large masses are consistent with the about 12.5 M ⊙ nebula around η Carinae.  the pair-instability models of Scannapieco et al. (2005) predict extremely long durations (100 days), slow expansion speeds of 5000 km s −1, and the presence of H in the spectrum, all of which are consistent with SN 2006gy.

Conclusion  SN 2006gy may have been a very massive star that exploded as an LBV before it could shed its H envelope, preventing them from ever becoming Wolf-Rayet stars, and it may have done so by the pair-instability mechanism.  If this hypothesis of explosion as a massive LBV is correct, it would have important consequences for our understanding of stellar evolution.

Reference  _releases/press_ html _releases/press_ html  N. Smith et al. 2007, astro- ph/ v2 THANK YOU VERY MUCH!