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TMT and Time Domain Science

TMT and Time Domain Science. G.C. Anupama Indian Institute of Astrophysics. TMT Science and Instrumentation Workshop. 2014 November 5-6, ARIES. VARIABILITY TREE. Time Domain Science. Transients Gamma-Ray Burst Sources Supernovae Novae LBV Stellar Flares Tidal Disruption Events

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TMT and Time Domain Science

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  1. TMT and Time Domain Science G.C. Anupama Indian Institute of Astrophysics TMT Science and Instrumentation Workshop. 2014 November 5-6, ARIES

  2. VARIABILITY TREE

  3. Time Domain Science • Transients • Gamma-Ray Burst Sources • Supernovae • Novae • LBV • Stellar Flares • Tidal Disruption Events • AGN flares • GW events • Variability Stellar – orbital, rotation, pulsation, accretion, evolution Galaxies – nuclear activity Fig. Source: LSST Science Book

  4. In the Era of Large Surveys, TMT is perfectly poised for time domain science Figs - Volume probed by various surveys as a function of transient magnitude. Red Cross: Minimum survey volume to detect single transient event. Lines for each survey – one transient event in the specified cadence period. Source: LSST Science Book

  5. TMT capabilities for transients IRIS, Spectra, S/N ~ 10 (~ 1 hour) (Point source) J ~ 24.1 H ~ 23.7 K ~ 22.9 Seeing limited Imaging, S/N~100 J ~ 27.3 H ~ 26.2 K ~ 25.5 (TMT_INS_TEC_10_001_REL02) TMT is optimized both in AO and seeing-limited modes for rapid response: ~5min without instrument change; ~10 min with instrument change K~30 mag, 3σ in 3 hours – detections z>5 Courtesy, Josh Bloom, Berkeley (WFOS-MOBIE, spectroscopic capabilities)

  6. 11 Time-Domain Science 11.1 Overview 11.2 Understanding the Nature of Type Ia Supernovae 11.2.1 Characterizing high-z Type Ia Supernovae: Towards a Better Standard Candle 11.2.2 Unveiling Explosion Mechanism of Type Ia Supernovae 11.3 Identifying Shock Breakout of Core-Collapse Supernovae 11.4 Tracing high-z Universe with Supernovae 11.5 Hunt for Progenitor Systems of Supernovae 11.5.1 Detecting Progenitor and Companion of Supernovae 11.5.2 Characterizing Circumstellar environment around Supernovae 11.5.3 Probing the Final Stages of Massive Star Evolution: LBVs and Supernova Impostors 11.6 Identification of Gravitational-Wave Sources 11.7 Understanding Progenitors of Gamma-ray Bursts: Connection to Supernovae and Kilonovae 11.8 Probing High-z Universe with Gamma-ray Bursts 11.9 Studying Tidal Disruption Events and Supermassive Black Holes 11.10 Cataclysmic Variables. 11.10.1 Investigating the Dissipative Process in Cataclysmic Variable Accretion Discs and Disc Evolution During Outburst Cycles. 11.10.2 Revealing Geometry and Populations of Classical Nova 11.11 Companions of Binary Radio Pulsars 11.12 Improving the Hubble Constant and Measuring Extragalactic Distances. 11.13 Time domain studies of AGN and Blazar Variability 11.14 Summary of Requirements. 11.15 References. Study of Transients And Variablity – A Few Science Cases in the TMT Detailed Science Cases Document (TMT-DSC-2014-draftV0.5.docx) Dated: 26 August 2014

  7. Supernovae Thermonuclear SNe (Type Ia)‏ Explosion of white dwarf in binary systems Energy - explosive C and O burning (fusion of C & O to Ni)‏ - deflagration or detonation Maximum luminosity ~109 L_sun Core-collapse SNe Spectrum: H (Type II); No hydrogen (Ib, Ic) ‏Core collapse of massive stars (>8 M_sun) with large envelopes (still burning)‏ Energy: gravity Maximum luminosity – 108 – 1010 L_sun Pair Instability SNe Z < 0.1 : KAIT, CfA, CSP, PTF; SKYMAPPER 0.1 < Z < 1 : SNLS, Essence, SDSS; DES, PANSTARRS, GAIA, LSST Z > 1 : HST-GOODS, WFC3; JWST, TMT, E-ELT, WFIRST

  8. Type Ia Supernovae Single degenerate – accreting WDs – possible progenitors: supersoft X-ray sources, recurrent novae, symbiotic novae Double degenerate – WD merger Early observations may allow us to test whether SNe Ia arise from single degenerate, double degenerate or sub-Chandra scenarios Super Chandra SN Ia show unburned carbon in their outer layers, visible only at early times, but also seen in other lower luminosity Ia High Velocity Ca II and Si II at early times detected in some SNe – related to shells or disks or progenitor material causing over densities in SN spectra Evidence of circumstellar material – narrow hydrogen emission, absorption features, light echoes

  9. Type Ia PTF11kx – Symbiotic RNe Progenitor? PTF 11kx – z=0.04660 (Dilday et al. 2012) High resolution Keck spectra (R~48,000) (-1d, +9d, +20d, +44d) Narrow CaII H&K features blue shifted by ~100 km/s (early spectrum) – develop into emission Narrow absorption lines of NaI, FeII, TiII and HeI. Blue shifted at ~65 km/s. Na I lines increase in depth over time. Hydrogen Balmer series seen in absorption blue shifted at ~65 km/s. H-alpha and H-beta show P-Cygni profiles. Absorption systems very similar to that seen in the recurrent nova RS Oph that has a red giant secondary (Patat+ 2011) First evidence for the presence of a red giant secondary TMT should be able to detect such systems in SNe Ia z~0.1 with good S/N

  10. Type Ia SD Progenitors – Early Light Curve Early Photometric Observations should reveal signatures of collision of supernova with its companion (Kasen 2010) Luminosity due to collision is prominent at times t<8 days, for viewing angles looking down on the collision region for SN having collided with a red giant. Dominant in X-ray, but R-J tail seen in UV/optical. Bump in B-band at t<5 days due to interaction with RG companion Detection in high redshift SN Ia with the TMT (UV shifted to optical + time dilation)

  11. Core Collapse Supernovae • Study of the shock break-out phase – IIP shock breakout in optical bands (Tominaga et al. 2011 – theoretical light curves for range of progenitor masses)‏ • Early phase – typing, sub classes, peculiarities (follow-up important – change in types)‏, pre-explosion dust and its composition • Late phase (nebular) observations • Evolution of line profile and kinematic studies; explosion geometry (Spectropolarimetry useful tool) • SNe IIP as standard candles – correlation of Fe II velocities with I band luminosity – extend beyond the existing correlation upto z~0.3 • Study of type-IIn SNe (luminous) at z~6 • Normal IIn SNe – z~2 • Strength and duration of the prominent emission lines present spectroscopic detection of 2<z<6 IIn SNe for ~3-15 years after outburst • Luminous / Pair Instability SNe – The most massive, metal poor stars‏ (metal poor pockets in the nearby universe)‏ • Progenitors – star formation history and IMF, metallicity – host galaxy local environment / integrated

  12. Gamma Ray Bursts (GRBs) • GRB are brief, sudden, intense flash of gamma-ray radiation • Prompt and afterglow emission, • Cosmological (z ~ 0.1 to 8.3), • Very Energetic (1050 to 1055 ergs), • Short, long Bi-modality in duration • Supernovae Connections – long bursts Associated SNe – Ic hypernovae Are all LBGRBs associated with SNe? Is there a heterogeneity in the SN type? • Dark GRBs • Orphan GRBs Polarimetry – geometry, jets, circumburst medium Late phase observations of GRB afterglows - Spectroscopy • Host Galaxy – morphology, location of the GRB in the host galaxy, possible progenitors

  13. Stellar Tidal Disruption Events Strong transient outbursts from galactic nuclei – star, planet or gas cloud tidally disrupted and partially accreted by the central non-active SMBH Transient variability may also arise during inspiral and merger phases of binary SMBHs Flashes in X-rays and UV. Optical flare, lasting several months expected when star disintegrates outside the event horizon Two optical events detected in SDSS survey data. One by Panstarrs.

  14. Stellar Tidal Disruption Events Optical Flares Panstarrs TDE – PS1-10jh (Gezari+ 2012) – Discovery 2010 May 31 z: 0.1696; mg 19.8 (peak) MBH ~ 2 106 M_sun (Mr-MBH correlation) Spectrum – Broad, high ionization He II lines – interpreted as the disruption of a helium star. Guillochan+ (2013) – suggest TDE produces a temporary accretion disc analogous to accretion disc in a normal thermal AGN, and that broad He II from a temporary BLR. Gaskell & Rojas Lobos (2013) – smoothed spectrum – H-alpha also present. - consistent with Guillochan et al.

  15. Stellar Tidal Disruption Events Optical Flares SDSS TDE (van Velzen+ 2011) z: 0.136, 0.251; Mg -18.3, -20.4 MBH ~ 6-20 106 M_sun, 2-10 107 M_sun (Mr-MBH correlation) Spectrum – H-alpha emission in TDE2 few days after detection of flare

  16. Interest in Stellar TDE Light emitted after disruption sensitive to black-hole mass and spin – large samples of TDE will allow properties of SMBHs to be studied without relying on scaling relations with global properties of galaxies TDEs are the only probes to obtain large samples of dormant SMBHs Testing existence of IMBHs in Globular Clusters and dwarf galaxies Detailed observations of emission from large sample of TDEs – new area for testing/understanding of accretion physics, constrain properties of disrupted stars

  17. Follow-up of Gravitational Wave Sources Accelerating Massive Objects in Asymmetric System Generates GW. Possible Sources - NS-NS(BH) collision (candidate of short GRBs); Core-collapse of Massive stars Light Curves and spectroscopy - identification GW detection ~ 100 deg2 Localization Search with Subaru/LSST/ZTF Spectroscopy with TMT Identification of GW sources LIGO(USA) KAGRA (Japan) IndIGO (LIGO-India) Future: LISA, DECIGO (in space)

  18. Cataclysmic Variables • Interacting Binary stars – Accreting white dwarf primary with a main-sequence M star secondary. • Nova Systems - Outburst due to thermonuclear runaway in the accreted hydrogen-rich material. • Outbursts can reach Mv = -10 – among the brightest transient sources known. • Outburst intervals of decades (recurrent novae) to thousands (classical novae) years • Outburst most sensitive to the mass of the accreting WD • Dwarf Nova systems - Outbursts occur due to disc instabilities, with the periodicity and amplitudes dependent on the accretion rate. At the highest accretion rates, there is no outburst (novalikes). • Between nova outbursts, the systems exist as dwarf novae or novalikes. White Dwarf Accretion Disc

  19. Cataclysmic Variables: Some Open Questions • Sources of rapid variability Variety of observed wavelength/amplitude dependencies • Novae eruption mechanisms Super-Eddington eruptions • Pulsating white dwarf properties and excitation mechanisms • Source of negative superhumps in AM CVn systems • Dwarf Nova Outbursts Disc Instability and Mass Transfer Instability outburst models DNO and QPO models • Orbital angular momentum loss and the period gap CV formation and evolution in the field and Globular Clusters • White Dwarf mass evolution, AM CVn and SN1a progenitors

  20. Dwarf Novae – Disc Instability SS Cyg Flare lasting 2½ minutes Fireball from the disc Broad band photometry combined with Time-resolved spectroscopy can provide Information regarding various disc activities, Spatial distribution of the instabilities (seen as Flickering), etc.

  21. Geometry and Populations of Novae Nova Cyg 1992 He Nova V445 Pup Recurrent nova T Pyxidis GK Persei 1901 The shape and ejected material kinematics of a nova shell : The shell burning process Collimation effects and environment immediately around the progenitor Non-spherical ejection – important consequences for understanding the observed properties Interactions with shell and circumstellar environment Example: TMT + AO: For a nova at 5kpc which is ejecting mass at 1000 km/s As seen from the Earth, the ejected shell will have a size of 10 mas (0.01") in around 87 days. For a very fast nova, the time taken would be around 9 days. Coronographic spot required to mask the central star. Nova GK Per 1901

  22. Nova Populations The high luminosity and frequency of appearance make novae ideal for probing properties of close binary systems in extragalactic (different) stellar populations Novae have been observed in more than a dozen galaxies, some as distant as the Coma cluster. Extragalactic novae also follow the MMRD relation (distance estimators) – presence of faint, fast CNe in M31 (Kasliwal+ 2011) Are there two distinct populations of novae – do they depend on the Hubble type? Are some recurrent novae progenitirs of Type Ia supernovae?

  23. Study of Compact Objects (Including Massive Black Holes) Neutron Stars Companions of radio binary pulsars Magnetars AGN Activity Long term Variability Intra-night Variability Flares

  24. Summary Time Domain Science is vast and varied Transients – ToO, time resolved, time critical (and non-time dependent) Variability studies - Time resolved science, time critical Discussed a few possible science cases related to Transients

  25. Time Domain ISDT Conveners: G.C. Anupama, Masaomi Tanaka Members: Manjari Bagchi, Varun Bhalerao, U.S. Kamath, Lucas Macri, Keiichi Maeda, Shashi Pandey, Enrico Ramirez-Ruiz, Warren Skidmore, Nozomu Tominaga, Lingzhi Wang, Xiaofeng Wang, Chao Wu, Xufeng Wu Invite participation in the Time Domain ISDT

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