1 / 44

SKA in context

SKA in context. z=8. Fields of View. 1deg^2 With Full Sensitivity at subarcsec resolution. RMS sensitivity in 8hrs at 1.4 GHz = 23 nJy. China KARST Canada LAR US Large-N+Small-D Australia Luneburg Lenses Europe: phased array. Australia: Cylindrical Telescopes. India: Preloaded

zurina
Download Presentation

SKA in context

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  1. SKA in context z=8

  2. Fields of View 1deg^2 With Full Sensitivity at subarcsec resolution

  3. RMS sensitivity in 8hrs at 1.4 GHz = 23 nJy

  4. China KARST Canada LAR US Large-N+Small-D Australia Luneburg Lenses Europe: phased array Australia: Cylindrical Telescopes India: Preloaded parabolas • “White Papers” issued • for each concept in 2002 • Reviewed by EMT/ISAC and revised 2003

  5. Concept USA: ‘Nd’ • 4640 x 12m parabolic antennas • Full Xcorr inner 2300 ants (35 km), outer ‘stations’ of 13 ants • Advantage: works to high frequency (> 20 GHz) • Disadvantage: no ‘full-sky, full-array’ multibeaming

  6. Concept Euro: nD – Phased arrays

  7. SKA poster (multi-beams) Advantages: many simultaneous beams, fast response Disadvantage: Max. frequency = 1.4 GHz Disadvantage: max freq = 1.4 GHz

  8. SKA and VLBI “SKV”

  9. The SKV – Scaled arrays to 5000 km

  10. Centimeter observations of thermal sources at mas resolution X PP-disks X NGC1068 Disk SKV +

  11. SKV Science • Dust obscured star and black hole formation history • a.starburst – AGN connection/discrimination: T_B(5s,8hrs,20mas,1.4GHz)=200K (SSCs, EG HII, SNR,… imaging to z=0.5) • b. counting RSNe to z = 3, imaging expansion to z=0.05 • c. mapping OH megamasers to z = 0.3 • Imaging water maser disks to z=0.06 • Imaging (faint) GRBs • High redshift radio absorption lines (HI, molecular): probing dense ISM, evolution physical constants • (SM)BH physics: low luminosity AGN -- Jet/accretion disk connection, XDAFs, Extragalactic microQuasars

  12. SKV Science • Protoplanetary disks, jets, and planets: imaging thermal emission at subAU scales, astrometry – Jovian planets around non-flaring solar-type stars to 50pc (30,000 stars!), Jupiter bursts to 100 pc. • Solar-Stellar connection: imaging coronal activity to 5pc (30 stars) • Extragalactic pulsars/stellar masers – proper motions • Geodesy – millimeter accuracy => Earth quake prediction? • Scattering and Scintillation – uas astronomy, turbulent ISM/IPM

  13. SKV Science • Proper motions of low luminosity AGN to Virgo – ‘mass map’ of the local supercluster • Epoch of Reionization – 21cm absorption by neutral IGM toward 1st radio loud AGN/GRBs/Star forming galaxies • For more details see: http://www.euska.org/workshops/hr_ws_MPIfR_Bonn.html

  14. Epoch of Reionization End of ‘Dark age’ sets the fundamental benchmark for cosmic structure formation – formation first luminous objects

  15. Evolution of the neutral IGM (Gnedin): ‘Cosmic Phase transition’ HI fraction Ionizing intensity density Gas Temp

  16. Discovery of the EoR Gunn-Peterson Absorption => f(HI) > 0.01 at z=6.3(Fan et al. 2002) CMB large scale (>10deg) polarization => f(HI) < 0.5 at z=17(Kogut et al. 2003)

  17. Studying the pristine IGM beyond the EOR: HI 21cm observations with the SKA and LOFAR SKA: A/T = 20000 m^2/K => nJy sensitivity at 1.4 GHz, mJy at 200 MHz Freq range = 0.1 to 20 GHz Resolution = 0.1” at 1.4GHz

  18. Imaging the neutral IGM at z=8.5(Tozzi 2002) Galaxies: 6uJy at 2’ res (= 20 mK) tCDM and OCDM 30 Mpc comoving QSOs: 3uJy/beam at 2’ res With and without soft Xray pre-heating.

  19. Difficulty with (LSS) emission observations: Confusion Continuum sources (di Matteo et al.2002) Free-Free emission (Oh & Mack 2002)

  20. Cosmic Webafter reionization = Ly alpha forest (d <= 10) 1422+23 z=3.62 Womble 1996 N(HI) = 1e13 -- 1e15 cm^-2, f(HI/HII) = 1e-5 -- 1e-6 => Before reionization N(HI) =1e18 – 1e21 cm^-2

  21. Cosmic Web before reionization: HI 21cm Forest Z=9 Z=7 Carilli, Gnedin, Owen 2002 Absorption – best done at (sub)arcsecond resolution => 1000 km baselines • Mean optical depth (z = 10) = 1% = ‘Radio Gunn-Peterson effect’ • Narrow lines (1 to 10%, few km/s) = HI 21cm forest (d = 10)

  22. SKA observations of absorption before the EOR A/T =2000 m^2/K 240 hrs 1 kHz/channel z = 10 z = 8

  23. Absorption in primordial disks toward GRBs/Starbursts? N/Dz << minihalos and IGM (<1e-4x) but t>> minihalos and IGM (>50x) => Use much fainter radio sources (0.1 mJy): GRB afterglow within disk? or Starburst radio emission? Furlanetto & Loeb 2002 t > 1

  24. Radio sources beyond the EOR?

  25. Luminous radio sources at very high z Radio galaxy: 0924-220 (van Breugel et al) z = 5.19 S_151 = 600 mJy Quasar: 0913+5821 (Momjian et al.) z = 5.12 S_151 = 150 mJy M_BH = 1e9 M_sun 10mas 1” • (sub)arcsec resolution preferred: decrease confusion, allow imaging

  26. CO 3-2 at z=6.42 1148+5251 z=6.42 46.6 GHz VLA detection of CO 3-2 emission from most distant QSO – within the EoR (Walter, Carilli, Bertoldi) M(dust) = 1e8 M_sun M(H_2) = 2e10 M_sun M_BH = 1 – 5e9 M_sun M_dyn > 1e10 M_sun S_190MHz = 0.1 mJy predicted if dust is heated by star formation

  27. Radio sources beyond the EOR: sifting problem (1/1400 per 20 sq.deg.) 1.4e5 at z > 6 S_120 > 6mJy 2240 at z > 6

  28. Summary: SKA study of the EoR • ‘Complex’ reionization -- GP: F(HI) > 0.01 at z=6.4, CMB pol: F(HI) < 0.5 at z= 20. • Neutral IGM is opaque => need observations longward of 1mm • Neutral, pristine IGM: realm of low frequency radio astronomy. • HI 21cm emission probes large scale structure. • HI 21cm absorption probes intermediate to small scale structure (radio GP effect, ‘21cm forest’, minihalos, proto-disks) – (sub)arcsec resolution decreases confusion, allows imaging. • Constrain: z_reion, detailed structure formation, nature of first luminous sources, ionizing background, IGM heating and cooling. • LOFAR should provide first detections of the neutral IGM at z>6. • SKA will allow for detailed studies.

  29. ISSC: SKA planning schedule • 2002 Design concept “white papers” • 2002 Director Appointed: Management plan with ISSC • 2003 Updated design concept “white papers” • 2003 “White papers” on possible locations • 2004 Updated “white papers” on locations • 2005 Choice of SKA location • 2005 Full Proposals for designs to ISSC • 2007 SKA “facility definition” (may merge designs) • 2010-12 SKA construction begins ? • 2015-17 SKA completed ?

  30. ISAC Mandates: • Revise science case and requirements, involving larger community, and put in context of future capabilities at other wavelengths. Goal: new Taylor-Braun document by Aug. 2004. • Evaluate (w. EMT) proposed SKA designs and advise ISSC. Goal: final design and site choice by ISSC in 2007 • Current documentation: • Science with the Square Kilometer Array, R. Taylor & R. Braun, 1999 (www.skatelescope.org/ska_science.shtml) • Perspectives on Radio Astronomy: Science with Large Antenna Arrays, ed. M. van Haarlem, 1999 (ASTRON) • SKA memo series: Groningen (2002), Bologna (2002), and Berkeley(2001), science working group reports (www.skatelescope.org/ska_memos.shtml)

  31. Discovery of the EOR(Becker et al. 2002) Fast reionization at z= 6.3 => opaque at l_obs < 1 mm

  32. Lower limit to z_reio: GP Effect Fan et al. 2002 White et al. 2003 f(HI) > 0.01 at z = 6.3

  33. Upper limit to z_reio: CMB anisotropies Briggs

  34. Thompson scattering => polarization • Large scale structure (10’s deg) => relic of EOR • t = Ln_es_e = 0.17 => z_reion = 10 to 20(Kogut et al. 2003) f(HI) < 0.5 at z = 20 Kogut et al. WMAP f(HI) > 0.01 at z = 6.3

  35. IGM Thermal History: Spin, CMB, Kinetic and the 21cm signal Tozzi 2002 T_s T_CMB T_K • Initially T_S= T_CMB • T_S couples to T_K via Lya scattering • T_K = 0.026 (1+z)^2 (wo. heating) • T_CMB = 2.73 (1+z) • T_S = T_CMB => no signal • T_S = T_K < T_CMB => Absorption against CMB • T_S > T_CMB => Emission

  36. Evolution of <temperatures> in the simulation

  37. Confusion by free-free emission during EOR (Oh & Mack 2003)

  38. Detection limits Running rms: S_120 > 6 mJy in 240 hrs KS of noise: S_120 > 12mJy

  39. Absorption by minihalos (d > 100)(Furlanetto & Loeb 2002) N/Dz(minihalos) = N/Dz(IGM) = 10/unit z at z=8, t > 0.02

  40. Inverse Compton losses off the CMB = U_B (radio lobe)

  41. CDM structure formation (PS) Efstathiou 1995 M_BH = 0.006 M_spheroid N(1e11, z=6 – 8) = 3/arcmin^2

  42. Evolution of space density of luminous QSOs (Fan et al. 2003)

  43. USS samples (de Breuck et al.) z>8 radio galaxies?

More Related