Astronomy & Astrophysics in India : Emerging challenges in Data - PowerPoint PPT Presentation

Astronomy & Astrophysics in India : Emerging challenges in Data Flow Tarun Souradeep, IUCAA, Pune NKN 2 nd Annual Workshop IISc. , Bangalore 17 th Oct 2013

Dynamic range of phenomena 10 -35 sec

Billion light years(lys) Million lys Thousand lys Rapid Ad Advanc nce e in Obser erva vatio tiona nal l capab abil ility ity  Da Data a drive ven scienc ence Model eling ing phen enomena with high gher er dyna namic rang nge e increasing easingly y possibl sible e with growth th in computation on (Den ensity sity (gm/cc) c): : cosm smic =10 -29 29 ,Ear Earth=10, h=10, Neutron utron star ar=1 =10 12) 2) Light days

Knowledge & Data flow in A&A Observations: Theoretical Modeling Data acquisition Numerical simulation Large volume, high sampling Large dynamic range, rates, rapid response Diverse physics Follow up Data Distribution Multiple analysis centers, Public , large distributed, global science collaborations Data Analysis Huge data, v multi-parameter

Numerical Simulations in Astrophysics Examples of simulations : Common features :   Involve upto 10 9 or more “ particles ” Large scale structure of the Universe   Formation & interaction of galaxies Complex interactions between particles:  gravity, magneto-hydrodynamics etc Formation of stars and solar systems   Long time-scale evolution, many steps Complex structure of the Sun Galaxy formation & evolution Collision of 2 gas clouds Large scale Universe : Complex leading to formation of stars web of cold dark matter

Astrophysics via large numerical simulation • Gravitational contraction/collapse/stellar dynamics N-body simulation, Smoothed Particle Hydrodynamics • Gas Dynamics - often supersonic, relativistic SPH, CFD • MHD, Poynting Flows CFD+Maxwell • Radiative Transfer PDE solvers, Green ’ s Function, Monte Carlo • Stellar structure and evolution PDE, Nuclear Chemistry, Thermodynamics • Particle acceleration PIC, Monte Carlo • Merger of neutron stars/black holes Numerical Relativity

Ongoing HPC-based Astronomy Research • IUCAA, Pune: MHD, Dynamos, N-body simulation, Structure formation, Radiative transfer, Molecular chemistry, Dust scattering, CMB analysis, Gravitational Waves, Pulsar search, Automated classification.... (IUCAA is linked to A&A research community in the University of India) • TIFR, Mumbai: Stellar structure, Helioseismology, Gravitational lensing • IIA, Bangalore: Radiative transfer, MHD, N-body simulation, Star Formation • IISc, Bangalore: Plasma astrophysics, Galaxy dynamics, Hydrodynamics • HRI, Allahabad: Cosmological simulations, Accretion hydrodynamics • IISER, Mohali: N-body simulation, Structure formation • Delhi University: Solar MHD, Gravitational Waves • SNBNCBS, Kolkata: Accretion flows, Molecular chemistry • NCRA, Pune: Real-time radio interferometry, Pulsar search & timing • • +++

Plenitude of Observations

Planck CMB sky map Planck: 12 million pixels of temperature/polarization (COBE detection: 4000 pixels) Measurements of the Cosmic Microwave Background Tarun Souradeep 9

CMB Maps at Planck Frequencies Planck Early Release 2011 Credit: ESA, HFI & LFI consortia 30 GHz 44 GHz 70 GHz 100 GHz 143 GHz 217 GHz 353 GHz 545 GHz 857 GHz

SZ clusters from Planck Tarun Souradeep 11

Large Observational data sets Sloan Digital Sky Survey 8000 deg 2 287 million objects 1.3 million spectra 10 TB imaging data 2 TB catalogue data

Large surveys 470,992,970 point sources, 1,647,599 extended source 13

6283 catalogues 14

Time Domain Astronomy  Real-time search in and characterization of 4-D data arrays  position (x,y), colour (wavelength), time  Large surveys are in the offing at many places across the world including India. Indian interest will include the processing of data from local as well as some of the international facilities  Most of the computation will be for automatic detection, characterization and classification of transient events, on which the decision of follow-up operations will be based  Need both large network bandwidth and high compute power

Catalina Real-Time Transients Survey CSS090426:074240+544425 CSS090429:135125-075714 CSS090429:101546+033311 Blazar 2EG J0744+5438 Flare star Dwarf Nova Vastly different physical phenomena, and yet they look the same ! Which ones are the most interesting and worthy of follow-up ? CRITICAL: Rapid, automated transient classification & distribution

International Virtual Observatory Alliance

Imminent transient Data deluge • Now: data streams of ~ 0.1 TB / night, ~ 10 - 10 2 transients / night (CRTS, PQ, PTF, various SN surveys, asteroid surveys)  Forthcoming on a time scale ~ 1 - 5 years: ~ 1 TB / night, ~10 4 transients / night (PanSTARRS, A major, Skymapper, VISTA, VST…) qualitative change!  Forthcoming in ~ 8 - 10 years: LSST, ~ 30 TB / night, ~ 10 5 - 10 6 transients / night   Observational follow-up needs: Transient  Rapid photometric/positional monitoring classification  Rapid spectroscopy technologies  Information/computation infrastructure are essential

Mega-Science ventures in Indian A&A (upcoming & advanced proposals)

ASTROSAT FIVE astronomy payloads for simultaneous multi-band observations: 1. 2x 40-cm Ultraviolet Imaging Telescopes (UVIT) 1. 3 Large Area Xenon 2. Proportional Counters (LAXPC) 3. A Soft X-ray Telescope (SXT) 4. A Cadmium-Zinc-Telluride 5. coded-mask imager (CZTI) 6. A Scanning Sky Monitor (SSM) 7. consisting of three one-dimensional 8. position-sensitive proportional 9. counters with coded masks. 20

Thirty Meter Telescope 30m equivalent primary mirror, 492 segments, 1.4m each, FOV 20 arcmin, 0.31 to 28 micron, Angular resolution with AO ~7 mas Caltech University of California Canada Japan China India (TMT-India proposal) 21

Square-kilometer array (SKA) Proposed/Ongoing Indian participation • Next big step in Radio Astronomy (an international telescope) • Total collecting area of 1 million sq. meters (about 30 times the GMRT) ! • Will be spread over a much larger area : ~ thousand km !! (contintental size)

LIGO-India proposal GW observatory on Indian soil 4km arm length Laser interferometer

A Century long Wait • Einstein’s Gravitation (1916 - ):  Beauty : symmetry in fundamental physics – mother of gauge theories  & precision : matches all experimental tests till date to high precision Gravitational Waves -- travelling space-time ripples GW  Astronomy link are a fundamental prediction Astrophysical systems are sources of copious GW emission: 96% universe does not emit Electromagnetic signal ! • Existence of GW inferred beyond doubt (Nobel Prize 1993) • GW emission efficiency (10% of mass for BH mergers) >> • Feeble effect of GW on a Detector  strong sources EM radiation via Nuclear fusion (0.05% of mass) Energy/mass emitted in GW from binary >> EM radiation in the lifetime GW Hertz experiment ruled out. • Universe is buzzing with GW signals from cores of astrophysical Only astrophysical systems involving huge masses and accelerating events Bursts (SN, GRB), mergers, accretion, stellar cannibalism ,… very strongly are potential detectable sources of GW signals. • Extremely Weak interaction, hence, has been difficult to detect directly But also implies GW carry unscreened & uncontaminated signals

Global Network of Adv. GW Observatories Network  1. Detection confidence 2. Duty cycle 3. Source direction 4. Polarization info. GEO: 0.6km VIRGO: 3km LIGO-LHO: 2km+ 4km KAGRA 3 km (2017) Time delays in milliseconds India provides almost largest possible baselines. (Antipodal baseline 42ms) LIGO-LLO: 4km LIGO-India

LIGO- India: … the opportunity Science Gain from Strategic Geographical Relocation Source localization error Courtesy: S. Fairhurst Launch of Gravitational wave Astronomy

Highly Multi- disciplinary Astro ++

Data from Gravitational wave experiments  Data comprised of IFO  Gravitational wave channel (ASQ)  Environmental monitors Env CH  Internal engineering monitors  Multiple data products beyond raw data Health  Reduced data sets  Level 1: gravitational wave and environmental channels  Level 3: only gravitational wave data.  Different sampling rates 1TB of raw data per day!

GW Data volume Time series data sampled at 16Hz - 16kHz Thousands of monitoring channels “ science channels ” : ~1% of total data per detector: 2B x 16kHz = 32kBps = ~1TB/year Advanced LIGO data volume: ~1petabyte / year

LIGO-India Site search High data connectivity required from a LIGO-India site at relatively remote, underdeveloped region in India. Conflicting Requirements: • Low ‘seismicity’ (ground noise PSD) • Low human generated noise, ….. • Air connectivity, road connectivity, data connectivity, … • Proximity to Academic institutions, labs, industry preferred, …