OBSERVATIONS OF TYPE II SUPERNOVAE &
|
|
- Marjorie Thompson
- 5 years ago
- Views:
Transcription
1 OBSERVATIONS OF TYPE II SUPERNOVAE & Ofer Yaron Weizmann Institute for Science In collaboration with: A. Gal-Yam, D. Perley, J. Groh, A. Horesh, E. Ofek, J. Sollerman, C. Fransson, A. Rubin, and others
2 Talk Outline Brief intro to observed CSM configurations What is Flash-Spectroscopy Unique events from the PTF/iPTF survey Additional events to construct a sample / statistics Future expectations (just around the corner ) 2
3 Various signatures of CSM interaction in CC-SNe M w, ρ w (r), ΔR / Δt Flash-spec events low M, high-ish ρ, small ΔR è emission lines gone within several days A continuum of transitional CSM extents è emission lines gone within several weeks OR multiple detached shells? è successive rebrightenings Type IIn SNe high M, ρ, ΔR persistent emission lines over months/years 3
4 SN 2010jl (PTF10aaxf) Ofek et al iptf14flu ~2 weeks from detection ~2 months later 4
5 New WISeREP 2.0 coming online soon. STAY TUNED 5
6 Evidence for pre-sn (enhanced/eruptive) mass-loss events SN precursor outbursts observed for Type IIn. (e.g. Precursor of SN 2010mc ejected 10-2 M Sun at v~2000 km/s 1 month prior to SN Ofek et al. 2013) and are likely common! >50% with at least 1 precursor brighter than M abs ~-14 and within ~100 days prior to SN. (Ofek et al. 2014) Pre SN mass-loss is not limited to Type IIn. Early spectra (Flash-Spectroscopy) reveal CSM around various Type II SNe. Can all these serve as some evidence for a causal connection between mass-loss episodes and the final SN explosion? How do the outer layers of a massive star know that it is about to explode? (or either receive information from the vigorous final burning stages taking place in the core?) 6
7 What is FLASH-SPECTROSCOPY è Prompt (action+reaction), Strong! Progenitor engulfed with a (relatively) optically thick wind / CSM (continuous or detached). 7
8 What is FLASH-SPECTROSCOPY è Prompt (action+reaction), Strong! Progenitor engulfed with a (relatively) optically thick wind / CSM (continuous or detached). SBO Shock breaks out from the hydrostatic surface (or either in a surrounding optically thick wind). 8
9 What is FLASH-SPECTROSCOPY è Prompt (action+reaction), Strong! Hot SBO flash ionizes the CSM. CSM reacts immediately to the strong radiation field. Recombination (min-hrs) è narrow (CSM-velocity) emission lines. (Light crossing time may smear spectral evolution.) With typical v exp ~10,000 km/s, CSM swept by ejecta within a few days (~5 d till 5e14 cm). 9
10 PTF/iPTF Was not only a powerful discovery machine Palomar Mountain Observatory, CA With human monitors at daylight in Europe during Palomar s night time è Quick response to young SN candidates (alerting & triggering of follow-ups). Discovery Follow-ups 48 robotic telescope, wide-field ~7 deg 2 (~1500 deg 2 / night), 1-day cadence. 10
11 iptf13ast (SN 2013cu) A Flash-Spectroscopy event showing WR-like wind signatures Discovered May 2013 in UGC 9379, ~100 Mpc. Keck spectrum obtained 4 hrs after photometric confirmation, ~15 hrs after explosion. Gal-Yam et al
12 iptf13ast (SN 2013cu) A Flash-Spectroscopy event showing WR-like wind signatures Strong He, N (N IV 7115) and Balmer lines indicate a WN6(h) classification. By day 6 the spectrum is featureless. Later spectra match prototypical Type IIb SNe (semistripped progenitor; low H envelope mass) From high Mdot, rel. low v wind and chemical abundance, progenitor likely a LBV / YHG (Groh 2014) Gal-Yam et al
13 The story of iptf13dqy = SN2013fs 13
14 iptf13dqy Flash-Spectroscopy in its extreme OY et al Discovery ~3 hrs from explosion. A set of 4 Keck spectra, 6-10 hrs. Apparent AB Magnitude Keck1 LRIS NOT ALFOSC FTS FLOYDS NOT ALFOSC P200 DBSP Hours from explosion PTF R band 3σ limits Polynomial Fit Days from explosion (MJD ) Absolute Magnitude NGC 7610 (~50 Mpc) P48 R-band 14
15 iptf13dqy Flash-Spectroscopy in its extreme Early Spectral evolution (6 hrs to 5 d) OY et al Scaled F λ + shift (erg cm -2 s -1 Ang -1 ) O IV O VI N V He II H O V KeckI +6.2 hr +7.2 hr +8.9 hr hr hr +1.4 d +1.9 d +2.0 d KeckII +2.1 d KeckII +5.1 d +5.3 d Rest Wavelength (Angstrom) NOT FTS NOT P200 FTS High-ionization emission lines (O VI) dominate during the first 10 hrs. He II persists till 2 days. Lines gradually disappearing till a Blue/Featureless spectrum by day 5. So assuming v CSM 100 km/s, SN ejecta ~ 10 4 km/s, CSM swept within 5 d CSM was emitted from progenitor within ~500 d before explosion (v CSM dependent), and is confined within 5 x cm. 15
16 iptf13dqy Flash-Spectroscopy in its extreme OY et al O VI He II O V Scaled F λ + shift (erg cm -2 s -1 Ang -1 ) O IV N V KeckI NOT FTS NOT P hr +7.2 hr +8.9 hr hr hr +1.4 d +1.9 d +2.0 d High-ionization emission lines (O VI) dominate during the first 10 hrs H KeckII KeckII +2.1 d +5.1 d +5.3 d Rest Wavelength (Angstrom) FTS He II persists till 2 days. λ -3 continuum-subtracted F λ (erg cm -2 s -1 Ang -1 ) [O II] O IV O VI Hδ Hγ He II Hβ O V / O IV Hα Rest Wavelength (Angstrom) 6-10 hrs Keck spectra, continuum subtracted N V Ep1-6.2 hr Ep2-7.2 hr Ep3-8.9 hr Ep hr Lines gradually disappearing till a Blue/Featureless spectrum by day 5. Light-crossing time effects, yet further constraining CSM extent. 4x10 14 r 2x
17 iptf13dqy Beginning HOT H WNL H50 Models kK NV 50kK 70kK Scaled F λ iptf13dqy IC1613 DR1 OVI CIV 100kK Keck Ep1 (6 h) Keck Ep4 (10 h) OIV CIV CIV CIII CIV HeII CIII CIII CIV 50kK 70kK OVI WC Models kK HeII OV 100kK 158kK Rest Wavelength (Ang.) Comparison to Wolf-Rayet families models (POWR) 17
18 iptf13dqy Later data reveal a standard Type IIP Later Spectra (days 8-57) km/s Developed P-Cygni lines. Spectra are typical of normal Type II. Scaled F λ + shift (erg cm -2 s -1 Ang -1 ) WHT NOT Lick FTS P200 FTS APO FTS +8.8 d d d d d d d d -4-5 Ca II Fe 4000 km/s Mg 5000 km/s Ca 5000 km/s P d Keck d Rest Wavelength (Angstrom) 18
19 iptf13dqy Later data reveal a standard Type IIP Scaled F λ + shift (erg cm -2 s -1 Ang -1 ) Ca II 6000 km/s Fe 4000 km/s Mg 5000 km/s P200 P200 Keck d d d d d d d d d d Rest Wavelength (Angstrom) Black markers: the expansion velocities of the standard Type II-P SN 2004et at days 30 and 50. Ca 5000 km/s Expansion velocity (km s -1 ) WHT NOT Lick FTS FTS APO FTS Hα Hβ Fe II (5169) Days from explosion Developed P-Cygni lines. Spectra are typical of normal Type II. As well as the expansion velocity evolution. 19
20 iptf13dqy Later data reveal a Type IIP Apparent AB Magnitude UVOT+P60 extrapolations to 1st P48 point P48 P60 Swift UVOT LCOGT UBVRI LCOGT griz RATIR UVW2 (+3.0) UVM2 (+3.0) UVW1 (+3.0) U (+2.0) B (+1.5) V (+1.0) g (+0.5) r,r i,i ( 0.5) z,z ( 1.0) Y ( 1.0) J ( 1.5) H ( 1.5) Days from explosion (MJD ) Multi-band LCs (first 2 months) Absolute Magnitude 20
21 O VI 3811,3834 Tin= 58 kk 4000 The three model spectra bracket the observed early spectrum; the 53kK model (dashed blue) best recovers the oxygen ionization structure. Tin= 48 kk Observed 5000 Rest Wavelength (Angstrom) H 6563 C IV 5812 O V 5597 He II Tin= 53 kk H 4861 N V 4604,4620 He II 4686 OIV 3411 iptf13dqy CMFGEN modeling of the early spectra 6000 è Mdot = (2-4) x 10-3 (vw=100 km/s) OR Mdot = (3-6) x 10-4 (vw=15 km/s) Rin ~(1-2) x 1014 cm Ofer Yaron, Weizmann Institute for Science Shocking SNe... Stockholm 05/
22 iptf13dqy Bolometrics 180 Blackbody Temperature [kk] Beginning HOT! Temp. regime acc. to model of 1st spectrum Blackbody Radius [cm] Bolometric luminosity estimates during the first 60 days, as obtained based on (1) photometry (SED fittings), (2) spectra and (3) BB temp. and radii. L bol (t~4 hrs) > ergs s Days from explosion (MJD ) Evolution of the BB temp. and radius based on the multiband photometry measurements. in agreement with the temp. estimates from modeling of the early spectra, showing the emission lines from highly ionized species at temp. above 50 kk Bolometric Luminosity [erg s 1 ] Days from explosion (MJD ) Multiband photometry Spectra L(R 2,T 4 ) 22
23 iptf13dqy Constraints from Radio Jansky VLA radio observations (PI Assaf Horesh) on days 70,100 after explosion (centered on 6.1, 22 GHz) resulted in NULL detections. The plotted colored curves display theoretical light curves of radio emission originating from the interaction of SN ejecta with an extended CSM. F ν [mjy] 10 1 Ṁ = 10 5 (22GHz) Ṁ = 10 4 (22GHz) Ṁ = 10 3 (22GHz) Ṁ= (6GHz) Ṁ = 10 5 (6GHz) 10 0 Ṁ = 10 4 (6GHz) Ṁ = 10 3 (6GHz) 22 GHz limits 6 GHz limits The measured limits rule out a wide range of MLRs. In particular that the MLR estimate required to explain the early optical data could not have been sustained over long periods Time since explosion [days] 23
24 Concluding the characterization of the CSM & MLR Our multi-wavelength observations require a confined nearby CSM density profile! Colored diagonal lines: Constant Mdots to 10-1 following: ρ w = Kr -2 = Mdot/4πv w r 2 24
25 Concluding the characterization of the CSM & MLR Mass-loss rate as a function of wind velocity, comparing values for interacting SNe to those of known types of stars (Smith, Handbook of SNe) Wind density parameters the lowest required to make a SN IIn Location of the pre-sn mass-loss episode of iptf13dqy Mdot ~ 10-3 M sun /yr, v w <~ 100 km/s (but over a short period!!!) 25
26 Motivated by the findings of iptf13ast/13dqy How common are flash ionized early spectra? PTF/iPTF sample CC-SNe, 84 of Type II, having a first spectrum within 10 days from the time of the SN pre-explosion limit. FI (Flash-Ionized) spectra all show Hα, Hβ and prominent He II λ4686 (by systematic EW measurement criterion). Khazov, OY, Gal-Yam et al
27 How common are flash ionized early spectra? Results All Flash-Ionized spectra found (12) are of Type II. Within 2 days from explosion, 8/11 SNe are FI or BF. Within 5 days from explosion, 1/5 of the Type II show FI. These FI fractions are a lower limit! There is evidence that late-stage enhanced mass-loss may also be common among progenitors of Low-Luminosity type IIP SNe (SN2016bkv, Hosseinzadeh et al. 2018) Khazov, OY, Gal-Yam et al
28 A plethora of theoretical studies to explain pre-sn outbursts/mass-loss e.g. Wave heating - Convectively driven hydrodynamic waves during late nuclear burning phases (core Ne/O ) able to deposit considerable energy in the envelope layers (Quataert & Shiode 2012, S&Q 2014) Wave-induced mass ejection models by Fuller 2017 predict large - but not extreme - MLRs: Msun/yr, and velocities <~ 100 km/s, like estimated for SN2013fs. The various models produce non-hydrostatitc pre-sn envelope configurations (density profiles) that are different from our prior expectations (therefore should affect fits to shock-cooling models etc ) Jim Fuller
29 What to expect in the nearby future Zwicky Transient Facility Reworked optics, HUGE camera. FOV: 47 sq. deg.!!! Covering ~5000 sq. deg. /night (2-3 visits/night) 1-day partnership cadence HSC, 1.7 deg 2 DES, 2.5 deg 2 PS1, 7 deg 2 PTF/iPTF, 7.3 deg 2 ZTF, 47 deg 2 LSST, 9.6 deg 2 1 deg 29
30 What to expect in the nearby future Zwicky Transient Facility Expected rate: 1..a few young (<1 day old) SN-II per week (to 20 mag) HSC, 1.7 deg PS1, 7 deg 2 Rate (1/week) DES, 2.5 deg h 10 1 Age of SN-II (hr) 24h PTF/iPTF, 7.3 deg 2 ZTF, 47 deg 2 LSST, 9.6 deg 2 1 deg 30
31 Example of a young type II from ZTF: Discovered May 8, with 2 days non-detection limit Spectrum at 8 days from discovery, just beginning to develop low-contrast P-Cyg lines. Discovered by ATLAS 2 d later, on May 10 31
32 What to expect in the nearby future ULTRASAT proposed wide-field UV satellite FOV > 200 sq. deg. Opening a new band (NUV, nm) and a new temporal cadence (1.5 min) not accessible to any other survey. Main science goals: Shock breakout and early shock cooling of CC- SNe. Emission from GW events NS-NS, NS-BH. Also: BlackGem, LSST 32
33 To conclude, take-home messages We have entered an era of < day 1 SN science - discovery and response. Early spectroscopy of CC-SNe directly probes the progenitor s ejecta, thus the progenitor s surface composition. It constrains the progenitor s mass-loss history, during the months-years prior to its demise; thus Placing important constraints on the final stages of massive star evolution as well as providing new sets of initial conditions for explosion models. We conclude that episodic enhanced (eruptive?) mass-loss by massive stars just prior to their terminal explosion, as proposed by several theoretical studies, also occurs among the progenitors of common types of CC-SNe. A continuum of CSM configurations exist, now verified by observations, extending from the short-lived FS events to the extended massive CSM of the standard (sustained interaction emission) Type IIn SNe. The nearby future will be illuminating (hectic?) Flash-Spectroscopy events are not rare, thus application of this method to future observations and samples is a promising prospect. 33
34 To conclude, take-home messages Utilizing cutting-edge technology (wide-field surveys operations and facilities), it is OUR - the observers - role to provide theorists and modelers of stellar evolution and stellar explosions with the required initial conditions and constraints, by gathering information from within the very first hours [and minutes] of SN explosions! 34
35 Thanks Hosts of flash-spectroscopy events (Johansson, in prep.) 35
The dynamical sky Two frontiers Joel Johansson, Uppsala university
The dynamical sky Two frontiers Joel Johansson, Uppsala university Time Wavelength Optical surveys faster! HSC, 1.7 deg 2 DES, 2.5 deg 2 PS1, 7 deg 2 PTF/iPTF, 7.3 deg 2 ZTF, 47 deg 2 LSST, 9.6 deg 2 Survey
More informationA new method to search for Supernova Progenitors in the PTF Archive. Frank Masci & the PTF Collaboration
A new method to search for Supernova Progenitors in the PTF Archive Frank Masci & the PTF Collaboration 1 The Palomar Transient Factory (PTF) Fully automated wide-field time-domain survey in optical Carried
More information10 Years of Super-Luminous Supernovae: Analytical and Numerical Models
F.O.E. meeting - 6/2/2015, Raleigh, NC 10 Years of Super-Luminous Supernovae: Analytical and Numerical Models Manos Chatzopoulos Enrico Fermi Postdoctoral Fellow FLASH Center for Computational Science
More informationEffects of low metallicity on the evolution and spectra of massive stars
Jose Groh (Geneva Observatory, Switzerland) Image credits: NASA/ESA/J. Hester & A. Loll, Arizona State U. (Crab Nebula) Effects of low metallicity on the evolution and spectra of massive stars Take Away:
More informationMass loss from stars
Mass loss from stars Can significantly affect a star s evolution, since the mass is such a critical parameter (e.g., L ~ M 4 ) Material ejected into interstellar medium (ISM) may be nuclear-processed:
More informationRadio Nebulae around Luminous Blue Variable Stars
Radio Nebulae around Luminous Blue Variable Stars Claudia Agliozzo 1 G. Umana 2 C. Trigilio 2 C. Buemi 2 P. Leto 2 A. Ingallinera 1 A. Noriega-Crespo 3 J. Hora 4 1 University of Catania, Italy 2 INAF-Astrophysical
More informationSupernova Shock Breakout. Lorenzo Sironi AST 541 Theoretical Seminar 11 th November 2009
Supernova Shock Breakout Lorenzo Sironi AST 541 Theoretical Seminar 11 th November 2009 SN Shock Breakout (SB) For any core-collapse SN, a flash of thermal UV (or soft X-ray) radiation is expected when
More informationElizabeth Lovegrove. Los Alamos National Laboratory
Elizabeth Lovegrove Los Alamos National Laboratory 06.08.2017 OUTLINE VLE SNe & Shock Breakout Theory CASTRO Simulations Prospects for Observations Conclusions & Future Work 06.08.2017 2 IN CASE YOU HAVE
More informationShock-induced formation and survival of dust in the dense CSM surrounding Type IIn supernovae
Shock-induced formation and survival of dust in the dense CSM surrounding Type IIn supernovae Arkaprabha Sarangi1,2 Eli Dwek1 & Richard G Arendt1 1) NASA Goddard Space Flight Center Observational Cosmology
More informationHUNTING FOR HIDDEN SUPERNOVAE. The Progenitor-Supernova-Remnant Connection
HUNTING FOR HIDDEN SUPERNOVAE Jacob Jencson The Progenitor-Supernova-Remnant Connection Caltech Astronomy Ringberg Castle Advisor: Mansi Kasliwal July 25, 2017 Optical searches are blind to supernovae
More informationWINDS OF HOT MASSIVE STARS III Lecture: Quantitative spectroscopy of winds of hot massive stars
WINDS OF HOT MASSIVE STARS III Lecture: Quantitative spectroscopy of winds of hot massive stars 1 Brankica Šurlan 1 Astronomical Institute Ondřejov Selected Topics in Astrophysics Faculty of Mathematics
More informationEarly Supernova Light Curves: Now and in the Future
Early Supernova Light Curves: Now and in the Future Anthony Piro George Ellery Hale Distinguished Scholar in Theoretical Astrophysics (Carnegie Observatories, Pasadena) Supernovae: The LSST Revolution
More informationGiant Eruptions (Supernova Impostors) Schuyler Van Dyk IPAC/Caltech USA
Giant Eruptions (Supernova Impostors) Schuyler Van Dyk IPAC/Caltech USA Supernova Impostors Observed outburst with ~10 49-50 erg, i.e., comparable to that of a SN Many impostors spectroscopically resemble
More informationStellar Populations: Resolved vs. unresolved
Outline Stellar Populations: Resolved vs. unresolved Individual stars can be analyzed Applicable for Milky Way star clusters and the most nearby galaxies Integrated spectroscopy / photometry only The most
More informationCORE-COLLAPSE SUPERNOVAE
CORE-COLLAPSE SUPERNOVAE Ryan Chornock (Ohio University) J. Hester & A. Loll/NASA/ESA WHY CC SUPERNOVAE ARE IMPORTANT Final deaths of massive (M > 8 M ) stars Formation of compact objects (i.e., NS/BH)
More informationStudies of core collapse SNe with NOT. Seppo Mattila Finnish Centre for Astronomy with ESO
Studies of core collapse SNe with NOT Seppo Mattila Finnish Centre for Astronomy with ESO Studies of core collapse SNe with the NOT (in Stockholm, Turku, Århus) Follow up of SNe with identified progenitors
More informationTHE 82ND ARTHUR H. COMPTON LECTURE SERIES
THE 82ND ARTHUR H. COMPTON LECTURE SERIES by Dr. Manos Chatzopoulos Enrico Fermi Postdoctoral Fellow FLASH Center for Computational Science Department of Astronomy & Astrophysics University of Chicago
More informationSupernova Explosions and Neutron Stars Bruno Leibundgut (ESO)
Supernova Explosions and Neutron Stars Bruno Leibundgut (ESO) What do we want to learn about supernovae? What explodes? progenitors, evolution towards explosion How does it explode? explosion mechanisms
More informationEarly time optical spectroscopy of supernova SN 1998S
A&A 367, 506 512 (2001) DOI: 10.1051/0004-6361:20000427 c ESO 2001 Astronomy & Astrophysics Early time optical spectroscopy of supernova SN 1998S G. C. Anupama, T. Sivarani, and G. Pandey Indian Institute
More informationPhotoionized winds of cool stars
Photoionized winds of cool stars Jonathan Mackey Argelander-Institut für Astronomie (aifa), Uni. Bonn Collaborators:! Shazrene Mohamed!(SAAO, Cape Town)! Vasilii Gvaramadze! (Lomonosov Moscow State University,
More informationStudies of peculiar transients with TNG Past results and future perspectives
Studies of peculiar transients with TNG Past results and future perspectives ANDREA PASTORELLO (INAF-OAPd) Padova, 2017 March 1-3 TNG Workshop New types of stellar transients The transient sky (past decade)
More informationiptf16fnl - a faint and fast TDE in an E+A galaxy
iptf16fnl - a faint and fast TDE in an E+A galaxy Nadia (Nadejda) Blagorodnova with Suvi Gezari, Tiara Hung, Shri Kulkarni, Brad Cenko, Lin Yan Unveiling the Physics Behind Extreme AGN Variability 12th
More informationChapter 10: Unresolved Stellar Populations
Chapter 10: Unresolved Stellar Populations We now consider the case when individual stars are not resolved. So we need to use photometric and spectroscopic observations of integrated magnitudes, colors
More informationarxiv: v1 [astro-ph] 3 Oct 2007
Peremennye Zvezdy 27, No.4, 2007 Variable Stars 27, No.4, 2007 SAI, INASAN, Astronet.ru Moscow, Russia 3 October 2007 arxiv:0710.0765v1 [astro-ph] 3 Oct 2007 PHOTOMETRIC OBSERVATIONS OF SUPERNOVA 2002hh
More informationLecture 8: Stellar evolution II: Massive stars
Lecture 8: Stellar evolution II: Massive stars Senior Astrophysics 2018-03-27 Senior Astrophysics Lecture 8: Stellar evolution II: Massive stars 2018-03-27 1 / 29 Outline 1 Stellar models 2 Convection
More informationEMISSION FROM ROTATING PAIR INSTABILITY SUPERNOVAE
AAS HEAD meeting, August 20, 2014 EMISSION FROM ROTATING PAIR INSTABILITY SUPERNOVAE Dr. Manos Chatzopoulos Enrico Fermi Postdoctoral Fellow Department of Astronomy & Astrophysics FLASH Center for Computational
More informationAge-redshift relation. The time since the big bang depends on the cosmological parameters.
Age-redshift relation The time since the big bang depends on the cosmological parameters. Lyman Break Galaxies High redshift galaxies are red or absent in blue filters because of attenuation from the neutral
More informationDiverse Energy Sources for Stellar Explosions. Lars Bildsten Kavli Institute for Theoretical Physics University of California Santa Barbara
Diverse Energy Sources for Stellar Explosions Lars Bildsten Kavli Institute for Theoretical Physics University of California Santa Barbara Traditional Energy Sources Core collapse to NS or BH depositing
More informationSupernovae. Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization
Supernovae Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization 1 Supernova Basics Supernova (SN) explosions in our Galaxy and others
More informationarxiv: v2 [astro-ph.sr] 20 Sep 2017
Astronomy & Astrophysics manuscript no. iptf13z-arxiv-v2-match-journal c ESO 217 September 21, 217 The bumpy light curve of Type IIn supernova iptf13z over 3 years A. Nyholm 1, J. Sollerman 1, F. Taddia
More informationEhsan Moravveji. WR124: A stellar fireball (HST WFPC2, NASA) Credit: Grosdidier (Uni. Montreal, CA)
Ehsan Moravveji moravveji@iasbs.ac.ir WR124: A stellar fireball (HST WFPC2, NASA) Credit: Grosdidier (Uni. Montreal, CA) The Latest SN statistics Stellar Evolutionary Scenarios vs. Initial Masses Progenitors
More informationHigh-Energy Neutrinos from Supernovae: New Prospects for the Next Galactic Supernova
High-Energy Neutrinos from Supernovae: New Prospects for the Next Galactic Supernova arxiv:1705.04750 Kohta Murase (Penn State) TeVPA 2017 @ Columbus, Ohio Neutrinos: Unique Probe of Cosmic Explosions
More informationSupernovae. Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization
Supernovae Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization 1 Supernova Basics Supernova (SN) explosions in our Galaxy and others
More informationHR Diagram, Star Clusters, and Stellar Evolution
Ay 1 Lecture 9 M7 ESO HR Diagram, Star Clusters, and Stellar Evolution 9.1 The HR Diagram Stellar Spectral Types Temperature L T Y The Hertzsprung-Russel (HR) Diagram It is a plot of stellar luminosity
More informationGRB history. Discovered 1967 Vela satellites. classified! Published 1973! Ruderman 1974 Texas: More theories than bursts!
Discovered 1967 Vela satellites classified! Published 1973! GRB history Ruderman 1974 Texas: More theories than bursts! Burst diversity E peak ~ 300 kev Non-thermal spectrum In some thermal contrib. Short
More informationSupernovae and possible NS-NS EM signatures. Keiichi Maeda
? Supernovae and possible NS-NS EM signatures Keiichi Maeda Outline SN (mostly) optical obs. vs. radiation models. @max. Early, before max. Late-phase. w/ radio and/or X-ray. How to connect these to Progenitor,
More informationProgenitor signatures in Supernova Remnant Morphology. Jacco Vink Utrecht University
Progenitor signatures in Supernova Remnant Morphology Jacco Vink Utrecht University The evolution of SNRs Heating by two shocks: 1. forward shocks heating ISM/CSM 2. reverse shock heating ejecta radius
More informationType Ibn Supernovae. Type Ibn Supernovae. Andrea Pastorello (INAF-OAPd) Andrea Pastorello (INAF-OAPd) Stockholm May 28 - June 1, 2018
Type Ibn Supernovae Type Ibn Supernovae Andrea Pastorello (INAF-OAPd) Stockholm May 28 - June 1, 2018 Andrea Pastorello (INAF-OAPd) Overview Introduction; SN 2006jc Heterogeneity of SN Ibn observables
More informationChapter 6: Stellar Evolution (part 2): Stellar end-products
Chapter 6: Stellar Evolution (part 2): Stellar end-products Final evolution stages of high-mass stars Stellar end-products White dwarfs Neutron stars and black holes Supernovae Core-collapsed SNe Pair-Instability
More informationStripped-envelope supernovae discovered by the Palomar Transient Factory. Christoffer Fremling
Stripped-envelope supernovae discovered by the Palomar Transient Factory Christoffer Fremling Cover image: NGC 5806, the host of iptf13bvn and PTF12os, imaged by the HST in multiple filters during 2004
More informationPresent and Future Large Optical Transient Surveys. Supernovae Rates and Expectations
Present and Future Large Optical Transient Surveys Supernovae Rates and Expectations Phil Marshall, Lars Bildsten, Mansi Kasliwal Transients Seminar Weds 12th December 2007 Many surveys designed to find
More informationStars with Mⵙ go through two Red Giant Stages
Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am Death of Stars Nuclear reactions in small stars How stars disperse carbon How low mass stars die The nature of white dwarfs
More informationRevealing new optically-emitting extragalactic Supernova Remnants
10 th Hellenic Astronomical Conference Ioannina, September 2011 Revealing new optically-emitting extragalactic Supernova Remnants Ioanna Leonidaki (NOA) Collaborators: P. Boumis (NOA), A. Zezas (UOC, CfA)
More informationPaul Broberg Ast 4001 Dec. 10, 2007
Paul Broberg Ast 4001 Dec. 10, 2007 What are W-R stars? How do we characterize them? What is the life of these stars like? Early stages Evolution Death What can we learn from them? Spectra Dust 1867: Charles
More informationThe Later Evolution of Low Mass Stars (< 8 solar masses)
The Later Evolution of Low Mass Stars (< 8 solar masses) http://apod.nasa.gov/apod/astropix.html The sun - past and future central density also rises though average density decreases During 10 billion
More informationGuiding Questions. Stellar Evolution. Stars Evolve. Interstellar Medium and Nebulae
Guiding Questions Stellar Evolution 1. Why do astronomers think that stars evolve? 2. What kind of matter exists in the spaces between the stars? 3. What steps are involved in forming a star like the Sun?
More informationSupernovae with SKA. Massimo Della Valle Capodimonte Observatory-INAF Naples
Supernovae with SKA Massimo Della Valle Capodimonte Observatory-INAF Naples Summary Supernova Taxonomy Radio-SN Observations (SKA will do it better) The impact of SKA on SN studies (CC-SNe; SNe-Ia; GRB-SNe,
More informationarxiv: v1 [astro-ph.he] 4 Dec 2017
MNRAS 000,?? (207) Preprint 5 December 207 Compiled using MNRAS LATEX style file v3.0 Electron scattering wings on lines in interacting supernovae Chenliang Huang ( 黄辰亮 ),,2 Roger A. Chevalier, Department
More informationPhotometric and Spectroscopic Observations of Type Ib Supernova SN 2012au by Kanata-Telescope
1 2012 December 14th Supernova meeting @ IPMU, Tokyo University Photometric and Spectroscopic Observations of Type Ib Supernova SN 2012au by Kanata-Telescope Katsutoshi Takaki (Hiroshima University) Coauthors
More informationReverberation Mapping in the Era of MOS and Time-Domain Surveys: from SDSS to MSE
Reverberation Mapping in the Era of MOS and Time-Domain Surveys: from SDSS to MSE Yue Shen Carnegie Obs -> University of Illinois at Urbana-Champaign MSE Science Team Meeting, July 29-31 2015, Big Island
More informationLobster X-ray Telescope Science. Julian Osborne
Lobster X-ray Telescope Science Julian Osborne What we want The whole high-energy sky right now 1.00E+13 1.00E+12 1 / f_lim (100 s) 1.00E+11 1.00E+10 1.00E+09 1.00E+08 0.0000001 0.000001 0.00001 0.0001
More informationISDT Report Time-domain Science
ISDT Report Time-domain Science Masaomi Tanaka (National Astronomical Observatory of Japan) G.C. Anupama (IIA) (Convener) ISDT time-domain group (15 members) * at this form Warren Skidmore (TMT) (Chapter
More informationRapidly Fading Supernovae from Massive Star Explosions. Io Kleiser - Caltech Advisor: Dan Kasen - UC Berkeley 31 October 2013
Rapidly Fading Supernovae from Massive Star Explosions Io Kleiser - Caltech Advisor: Dan Kasen - UC Berkeley 31 October 213 SN 21X Discovery Normalized Magnitude 2 4 1991T 1991bg 1994I 21X-g 21X-r 21X-i
More informationThe 2006 Outburst of RS Oph: What are the questions that need to be discussed --and answered?
The 2006 Outburst of RS Oph: What are the questions that need to be discussed --and answered? Sumner Starrfield School of Earth and Space Exploration Arizona State University WHY DO WE CARE? RS Oph may
More informationDust production in a variety of types of supernovae
2014/08/07 Dust production in a variety of types of supernovae Takaya Nozawa (NAOJ, Division of theoretical astronomy) Main collaborators: Keiichi Maeda (Kyoto University) Masaomi Tanaka (NAOJ) Takashi
More informationarxiv: v1 [astro-ph.he] 22 Dec 2016
Contents arxiv:1612.07459v1 [astro-ph.he] 22 Dec 2016 Thermal and non-thermal emission from circumstellar interaction...... 3 Roger A. Chevalier and Claes Fransson 1 Introduction..............................................
More informationCore-collapse supernovae are thermonuclear explosions
Core-collapse supernovae are thermonuclear explosions Doron Kushnir Collaborators: Boaz Katz (WIS), Kfir Blum (WIS), Roni Waldman (HUJI) 17.9.2017 The progenitors are massive stars SN2008bk - Red Super
More informationCompton Lecture #4: Massive Stars and. Supernovae. Welcome! On the back table:
Compton Lecture #4: Massive Stars and Welcome! On the back table: Supernovae Lecture notes for today s s lecture Extra copies of last week s s are on the back table Sign-up sheets please fill one out only
More informationExplosive/Eruptive LBV-like mass loss and Superluminous Supernovae (especially Type IIn)
Explosive/Eruptive LBV-like mass loss and Superluminous Supernovae (especially Type IIn) Nathan Smith University of Arizona/Steward Observatory In Tucson (not ASU in Tempe) Chandra/HST OVERVIEW SLSN IIn
More informationarxiv: v1 [astro-ph.sr] 1 Oct 2015
The True origin of Wolf-Rayet stars Jorick S. Vink 1 1 Armagh Observatory, College Hill, BT61 9DG Armagh, Northern Ireland, UK arxiv:1510.00227v1 [astro-ph.sr] 1 Oct 2015 The Wolf-Rayet (WR) phenomenon
More informationCosmic Explosions. Greg Taylor (UNM ) Astro 421
Cosmic Explosions Greg Taylor (UNM ) Astro 421 1 Cassiopeia A: Supernova Remnant E total ~ 10 46 J 2 An early gamma ray-burst Vela satellite 3 A Gamma Ray Burst Sampler 4 Burst Alert 5 The BeppoSAX Satellite
More informationThe Ṁass- loss of Red Supergiants
The Ṁass- loss of Red Supergiants Dr. Donald F. Figer Director, Center for Detectors Speaker: Yuanhao (Harry) Zhang RIT 9/12/13 1 9/12/13 2 Outline IntroducJon MoJvaJon Objects Method Need for SOFIA/FORCAST
More informationOptical/IR Counterparts of GW Signals (NS-NS and BH-NS mergers)
Optical/IR Counterparts of GW Signals (NS-NS and BH-NS mergers) Chris Belczynski 1,2 1 Warsaw University Observatory 2 University of Texas, Brownsville Theoretical Rate Estimates (MOSTLY NS-NS MERGERS:
More informationCosmic Ray acceleration at radio supernovae: perspectives for the Cerenkov Telescope Array
Cosmic Ray acceleration at radio supernovae: perspectives for the Cerenkov Telescope Array A.MARCOWITH ( LABORATOIRE UNIVERS ET PARTICULES DE MONTPELLIER, FRANCE) & M.RENAUD, V.TATISCHEFF, V.DWARKADAS
More informationSupernova events and neutron stars
Supernova events and neutron stars So far, we have followed stellar evolution up to the formation of a C-rich core. For massive stars ( M initial > 8 M Sun ), the contracting He core proceeds smoothly
More informationMapping the oxygen abundance in an elliptical galaxy (NGC 5128)
Mapping the oxygen abundance in an elliptical galaxy (NGC 5128) Jeremy R. Walsh, ESO Collaborators: George H. Jacoby, GMT Observatory, Carnegie; Reynier Peletier, Kapteyn Lab., Groningen; Nicholas A. Walton,
More informationarxiv:astro-ph/ v1 25 Sep 2006
**FULL TITLE** ASP Conference Series, Vol. **VOLUME**, **YEAR OF PUBLICATION** **NAMES OF EDITORS** Are Wolf-Rayet winds driven by radiation? arxiv:astro-ph/0609675v1 25 Sep 2006 Götz Gräfener & Wolf-Rainer
More informationGalaxies 626. Lecture 5
Galaxies 626 Lecture 5 Galaxies 626 The epoch of reionization After Reionization After reionization, star formation was never the same: the first massive stars produce dust, which catalyzes H2 formation
More informationType Ia supernovae observable nuclear astrophysics
Astrophysics and Nuclear Structure Hirschegg, January 27, 2013 Type Ia supernovae observable nuclear astrophysics Julius-Maximilians-Universität Würzburg, Germany W. Hillebrandt, S. Woosley, S. Sim, I.
More informationOptical counterparts of ULXs. S. Fabrika
Optical counterparts of ULXs S. Fabrika Examples of ULX counterparts NGC4559 X-7 Soria et al. 2005 NGC5408 X-1 Grise et al. 2012 Holmberg IX X-1 Pakull & Grise, 2008 Grise et al. 2006 Cseh et al. 2012
More informationHigh Redshift Universe
High Redshift Universe Finding high z galaxies Lyman break galaxies (LBGs) Photometric redshifts Deep fields Starburst galaxies Extremely red objects (EROs) Sub-mm galaxies Lyman α systems Finding high
More informationThe Supernova/Gamma-Ray Burst Connection. Jens Hjorth Dark Cosmology Centre Niels Bohr Institute University of Copenhagen
The Supernova/Gamma-Ray Burst Connection Jens Hjorth Dark Cosmology Centre Niels Bohr Institute University of Copenhagen Galama et al. 1998; Fynbo et al. 2000 SN 1998bw/GRB 980425 Galama et al. 1998 Collapsar
More informationEinführung in die Astronomie II
Einführung in die Astronomie II Teil 10 Peter Hauschildt yeti@hs.uni-hamburg.de Hamburger Sternwarte Gojenbergsweg 112 21029 Hamburg 15. Juni 2017 1 / 47 Overview part 10 Death of stars AGB stars PNe SNe
More informationMonitoring nearly 4000 nearby stellar systems with the OVRO-LWA in search of radio exoplanets
Monitoring nearly 4000 nearby stellar systems with the OVRO-LWA in search of radio exoplanets Marin M Anderson Caltech AASTCS 5: Radio Habitability May 11, 2017 OVRO-LWA 1 CME CME Mass Mass Understanding
More informationCh. 16 & 17: Stellar Evolution and Death
Ch. 16 & 17: Stellar Evolution and Death Stars have lives: born, evolve, die Mass determines stellar evolution: Really Low Mass (0.08 to 0.4 M sun ) Low Mass: (0.4 to 4 M sun ) Long lives High Mass (4
More informationLight curve modeling of core-collapse supernovae
UNIVERSITY OF SZEGED FACULTY OF SCIENCE AND INFORMATICS DOCTORAL SCHOOL OF PHYSICS Light curve modeling of core-collapse supernovae PhD thesis statements Andrea Nagy SUPERVISOR: Dr. József Vinkó associate
More informationPESSTO The Public ESO Spectroscopic Survey for Transient Objects
PESSTO The Public ESO Spectroscopic Survey for Transient Objects Morgan Fraser Institute of Astronomy, University of Cambridge, UK Stefano Benetti INAF - Osservatorio Astronomico di Padova, Italy Cosimo
More informationSupernova Remnants and Cosmic. Rays
Stars: Their Life and Afterlife Supernova Remnants and Cosmic 68 th Rays Brian Humensky Series, Compton Lecture #5 November 8, 2008 th Series, Compton Lecture #5 Outline Evolution of Supernova Remnants
More informationDECAM SEARCHES FOR OPTICAL SIGNATURES OF GW Soares-Santos et al arxiv:
DECAM SEARCHES FOR OPTICAL SIGNATURES OF GW150914 Soares-Santos et al. 2016 arxiv:1602.04198 Marcelle Soares-Santos The DES Collaboration Fermilab Moriond Cosmology Conference March 20, 2016 INTRODUCTION
More informationThe Red Supergiant Progenitors of Core-collapse Supernovae. Justyn R. Maund
The Red Supergiant Progenitors of Core-collapse Supernovae Justyn R. Maund Stellar Populations Workshop IAG-USP 1 st December 2015 Astronomy and Astrophysics at Sheffield 8 Academic staff 5 Postdocs 13
More informationDust production by various types of supernovae
Dust production by various types of supernovae Takaya Nozawa ( 野沢貴也 ) IPMU, University of Tokyo, Kashiwa, Japan Collaborators: T. Kozasa (Hokkaido Univ.), N. Tominaga (Konan Univ.) K. Maeda, M. Tanaka,
More informationProbing the End of Dark Ages with High-redshift Quasars. Xiaohui Fan University of Arizona Dec 14, 2004
Probing the End of Dark Ages with High-redshift Quasars Xiaohui Fan University of Arizona Dec 14, 2004 High-redshift Quasars and the End of Cosmic Dark Ages Existence of SBHs at the end of Dark Ages BH
More informationOptical studies of an ultraluminous X-ray source: NGC1313 X-2
Optical studies of an ultraluminous X-ray source: NGC1313 X-2 Jifeng Liu Harvard-Smithsonian Center for Astrophysics in collaboration with Joel Bregman, Jon Miller, Philip Kaaret outline background: ultraluminous
More informationMassive Star Outbursts and Their Optical Transients. Nathan Smith UC Berkeley. Hubble & Sandage 1953 (M31 & M33) Tammann & Sandage 1968 (NGC 2403)
Massive Star Outbursts and Their Optical Transients Nathan Smith UC Berkeley Hubble & Sandage 1953 (M31 & M33) Tammann & Sandage 1968 (NGC 2403) Luminous Blue Variables (LBVs) or Hubble-Sandage variables,
More informationIntroductory Astrophysics A113. Death of Stars. Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM
Goals: Death of Stars Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM Low Mass Stars (M
More informationClassification of nova spectra
International Workshop on Stellar Spectral Libraries ASI Conference Series, 2012, Vol. 6, pp 143 149 Edited by Ph. Prugniel & H. P. Singh Classification of nova spectra G. C. Anupama Indian Institute of
More informationHigh-mass stars in the Galactic center Quintuplet cluster
High-mass stars in the Galactic center Quintuplet cluster Adriane Liermann 1,2, Wolf-Rainer Hamann 2, Lidia M. Oskinova 2 and Helge Todt 2 1 Max-Planck-Institut für Radioastronomie, Bonn, Germany 2 Universität
More informationAstro 1050 Wed. Apr. 5, 2017
Astro 1050 Wed. Apr. 5, 2017 Today: Ch. 17, Star Stuff Reading in Horizons: For Mon.: Finish Ch. 17 Star Stuff Reminders: Rooftop Nighttime Observing Mon, Tues, Wed. 1 Ch.9: Interstellar Medium Since stars
More informationLiverpool Telescope 2
Liverpool Telescope 2 Chris Copperwheat Liverpool Telescope group: Robert Barnsley, Stuart Bates, Neil Clay, Chris Davis, Jon Marchant, Chris Mottram, Robert Smith, Iain Steele Liverpool Telescope 2 The
More informationS. Basa, Laboratoire d Astrophysique de Marseille, France
S. Basa, Laboratoire d Astrophysique de Marseille, France The transient sky distant sample of SMBHs, which in turn, hold the greatest promise of extending the existing M-σ relation beyond current limitations
More informationGuiding Questions. The Deaths of Stars. Pathways of Stellar Evolution GOOD TO KNOW. Low-mass stars go through two distinct red-giant stages
The Deaths of Stars 1 Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,
More informationThe Deaths of Stars 1
The Deaths of Stars 1 Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,
More informationTime Domain Astronomy at Caltech (ZTF) S. R. Kulkarni Director, Caltech Optical Observatories Principal Investigator, Zwicky Transient Facility (ZTF)
Time Domain Astronomy at Caltech (ZTF) S. R. Kulkarni Director, Caltech Optical Observatories Principal Investigator, Zwicky Transient Facility (ZTF) Time Domain Astronomy (TDA) has emerged! TDA is now
More informationStellar Models ASTR 2110 Sarazin
Stellar Models ASTR 2110 Sarazin Jansky Lecture Tuesday, October 24 7 pm Room 101, Nau Hall Bernie Fanaroff Observing the Universe From Africa Trip to Conference Away on conference in the Netherlands
More informationStellar Evolution: The Deaths of Stars. Guiding Questions. Pathways of Stellar Evolution. Chapter Twenty-Two
Stellar Evolution: The Deaths of Stars Chapter Twenty-Two Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come
More informationBrian Metzger Princeton University NASA Einstein Fellow
EM Counterparts of Neutron Star Binary Mergers and their Detection in the Era of Advanced LIGO Brian Metzger Princeton University NASA Einstein Fellow In Collaboration with: Edo Berger (Harvard CfA) Eliot
More informationYoung stellar objects and their environment
Recent Advances in Star Formation: Observations and Theory ASI Conference Series, 2012, Vol. 4, pp 107 111 Edited by Annapurni Subramaniam & Sumedh Anathpindika Young stellar objects and their environment
More informationGuiding Questions. The Deaths of Stars. Pathways of Stellar Evolution GOOD TO KNOW. Low-mass stars go through two distinct red-giant stages
The Deaths of Stars Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,
More informationarxiv:astro-ph/ v1 18 Nov 2003
Low frequency radio and X-ray properties of core-collapse supernovae arxiv:astro-ph/0311419 v1 18 Nov 2003 A. Ray 1, P. Chandra 1,2, F. Sutaria 3, and S. Bhatnagar 4,5 1 Tata Institute of Fundamental Research,
More informationSearching for the Progenitors of Subluminous Type Ia Supernovae with SN 2013bc
Hubble Space Telescope Cycle 11 General Observer Proposal Searching for the Progenitors of Subluminous Type Ia Supernovae with SN 2013bc Principal Investigator: Institution: Electronic mail: Maximilian
More information