ISDT Report Time-domain Science
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1 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 editor) Manjari Bagchi (Tata Institute) Varun Bhalerao (IUCAA) U.S. Kamath (IIA) Lucas Macri (Texas A&M) Keiichi Maeda (Kyoto) Shashi Pandey (ARIES) Masaomi Tanaka (NAOJ) (Convener) Nozomu Tominaga (Konan) Lingzhi Wang (NAOC) Xiaofeng Wang (Tsinghua) Chao Wu (NAOC) Xufeng Wu (PMO) Enrico Ramirez-Ruiz (UCSC)
2 Update of Detailed Science Case 1. Introduction 2. Overview 3. Fundamental physics and cosmology 4. The early Universe 5. Galaxy formation and the intergalactic medium Thirty Meter Telescope Detailed Science Case: 2007 TMT Science Advisory Committee 6. Extragalactic supermassive black holes 7. Exploration of nearby galaxies 8. The formation of stars and planets 9. Exoplanets 10. Our solar system No section for time-domain science
3 Time-domain science?? Supernovae Tidal disruption Pulsar GRBs Cataclysmic variable AGNs Microlensing Planet transit Asteroids Stellar pulsation RR Lyrae Cepheids... Eclipsing binary YSOs Asteroid occultation Luminous blue variable
4 Time-domain science?? DSC 2014 Type Ia SN Core-collapse SN SN progenitor GW sources GRBs Tidal disruption CVs Pulsars Cepheids 5.! TIME-DOMAIN SCIENCE 53! 5.1! Overview... 53! 5.2! Understanding the Nature of Type Ia Supernovae... 54! 5.2.1! Characterizing high-z Type Ia Supernovae: Towards a Better Standard Candle... 54! 5.2.2! Unveiling Explosion Mechanism of Type Ia Supernovae... 55! 5.3! Identifying Shock Breakout of Core-Collapse Supernovae... 56! 5.4! Tracing high-z Universe with Supernovae... 57! 5.5! Hunt for Progenitor Systems of Supernovae... 58! 5.5.1! Detecting Progenitor and Companion of Supernovae... 58! 5.5.2! Characterizing Circumstellar environment around Supernovae... 59! 5.5.3! Probing the Final Stages of Massive Star Evolution: LBVs and Supernova Impostors... 60! 5.6! Identification of Gravitational-Wave Sources... 60! 5.7! Understanding Progenitors of Gamma-ray Bursts: Connection to Supernovae and Kilonovae... 61! 5.8! Probing High-z Universe with Gamma-ray Bursts... 62! 5.9! Studying Tidal Disruption Events and Supermassive Black Holes... 63! 5.10! Cataclysmic Variables ! ! Investigating the Dissipative Process in Cataclysmic Variable Accretion Discs and Disc Evolution During Outburst Cycles... 65! ! Revealing Geometry and Populations of Classical Novae... 66! 5.11! Companions of Binary Radio Pulsars... 67! 5.12! Improving the Hubble Constant and Measuring Extragalactic Distances... 68! 5.13! Summary of Requirements... 69! 5.14! References... 72!!!
5 Time-domain science?? Target of opportunity observations Type Ia SN GW sources Tidal disruption Core-collapse SN GRBs Classical novae Rapid response (telescope, operation) Time-resolved observations CVs, X-ray binary (accretion disk) Rapid sampling (instruments) Pulsars Monitoring observations Cepheids RR Lyrae Binaries AGNs Flexible time allocation
6 Frontier: Short timescale transients Theoretically expected Swift! Supernovae Nova Figure from LSST Science Book (after PTF collaboration, Rau+09, Kasliwal+,Kulkarni+)
7 16 18 High cadence ROTSE Magnitude Deep KISS iptf LSST Subaru HSC PTF PTF SDSS Pan-STARRS SNLS Subaru HSC HST Cadence (days)
8 First transient survey with Subaru/HSC (2014 July 2-3 UT) New image Subtracted image Ref New Sub Ref New Sub 1.5 deg Tominaga et al.
![The moment of supernova explosion 10 45 10 44 10 43 2 hr!! 0 0.2 0.4 0.6 Days Deep, high-cadence survey (g = 27 mag) Bolometric luminosity [erg s -1 ] 10 45 10 44 10 43 10 42 2 10 45 10 44 10 43 0 0.](/docs-images/88/115320866/images/9-3.jpg "2 0.4 0.")
9 The moment of supernova explosion hr!! Days Deep, high-cadence survey (g = 27 mag) Bolometric luminosity [erg s -1 ] Tominaga Days since the peak (rest frame) [Days] supernovae at z~2 TMT/MOBIE spectroscopy within 30 min New window to study supernovae (SFRs, SN progenitor, SN kinetic energy)
10 Paradigm shift in 2020s: Gravitational waves Advanced LIGO (US) - Advanced Virgo (Europe) - KAGRA (Japan) NS-NS merger with 200 Mpc LIGO KAGRA Multi-messenger astronomy Virgo - Compact binaries - Properties of dense matter - r-process nucleosynthesis -...
11 1 deg SDSS
12 GW alert error e.g. 6 deg x 6 deg (not box shape in reality) No electromagnetic counterpart No gravitational wave astronomy GW detection Subaru HSC 1.5 deg 1 deg EM transient search w/ wide-field telescope (e.g., LSST, HSC) LSST 3.5 deg Source identification (TMT)
13 Smoking gun: spectroscopic identification Log flux (F ) + constant U Type Ia LGRB-SN B V R I J H 1.5 days 5.0 days 10.0 days Wavelength (A) MT & Hotokezaka 13 Optical/NIR spectroscopy with MOBIE+IRIS ~25 mag for Mpc ( > 100 SNe within localization area) NS merger = extremely broad-line, red spectra
14 GRB as a probe of high-z Universe (by Antonino Cucchiara yesterday) Chornock+13 - Metal abundances - HI column density - Ly alpha escape fraction - Intervening systems TMT/IRIS can reach z=8-10! Need more interaction with other ISDTs
15 Observed Magnitude Response time (day) min Required response time Response with 5 min GRB (NIR, HR) 1 hour 1 day SN shock breakout (opt) LBV (opt) TDE (opt) SN CSM (opt, HR) High-z SNe Ia (NIR) High-z SNe (NIR) Low-z SNe Ia (opt) Response time (min) GW source (NIR) DSC 2014
16 Discussion (yesterday) System for ToO? Telescope/instruments become ready in 5 min Unique capability of TMT Human judge can easily take more time To maximize the scientific outcome of TMT: Ideally need automated system Prepare templates for observing modes (so that observers can quickly select) Inter-partner ToO observations? => Key program
17 Another frontier: Time-resolved observations 75 ms spectroscopic sampling for cataclysmic variables (also for X-ray binaries) Skidmore et al. 2004
18 Required sampling time DSC 2014 by Warren Skidmore Sampling with 10 msec (100 Hz)
19 Discussion (yesterday) To fully utilize 30m aperture 10 ms sampling 80 % efficiency (= 20% dead time) Accurate, absolute time stamp (direct comparison with multi-wavelength data) Need only a small part of FOV FOV How many pixels? 2 ms 2 ms 10 ms 10 ms t exp read + α exp read + α Need input from instrument groups
20 Summary Time-domain science needs TMT 11 science cases in updated DSC Time-domain science in 2020s Synergy with LSST/HSC transient surveys Synergy with gravitational wave telescopes Time-resolved observations with 30m aperture Requirement from time-domain science Response within 5 min (=> telescope/operation) 10 msec sampling with >80% efficiency (=> instruments) Need more communication with instrument groups Key program <=> inter-partner ToO program?
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