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ARECIBO RADIO ASTRONOMY

ARECIBO RADIO ASTRONOMY. Chris Salter for Murray Lewis. Across whole Arecibo pgm. Mass -range investigated dynamically ~56 orders of magnitude Micro-meteorites -- asteroids -- neutron stars -- -- galaxy clusters Time duration: ∆t > 23 orders of magnitude

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ARECIBO RADIO ASTRONOMY

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  1. ARECIBO RADIO ASTRONOMY Chris Salter for Murray Lewis 11 September 2008 NSF

  2. Across whole Arecibo pgm. • Mass-range investigated dynamically • ~56 orders of magnitude • Micro-meteorites -- asteroids -- neutron stars -- -- galaxy clusters • Time duration: ∆t > 23 orders of magnitude • Crab giant pulses 10-9 sec; Galaxy Evoln. > 109 yr • Magnetic field: B > 20 orders of magnitude • Mercury null; ISM; to Magnetars > 10^13 gauss 11 September 2008 NSF

  3. Traditional Arecibo topics • Pulsars -- (pALFA), timing MSP • 21 cm HI • Extra-galactic {alfalfa, AGES, (AUDS), ([ZoA]) } • Galactic {Disk-Halo, (I-gALFA), [TOGS,TOGS2,GALFACTS2]} • OTHER • Magnetic Fields {(GALFACTS), (ULIRGs) } • VLBI • Multi-UGC, CGCG, SDSS, IRAS, 2MASS, (GLAST)} • Molecular-line {Arp 220, ULIRGs} 11 September 2008 NSF

  4. ALFA: A Camera for Arecibo • Installed 2004 Apr • Surveys initiated Feb 2005 • 7 beams x 2 pol (linear) = 14 “pixels” • 1225-1525 MHz full range • Unmatched sensitivity (SEFD = 2.4 to 3 Jy) • 3.3’ x 3.8’ beams on 11’ X 13’ ellipse • Unprecedented capability for mapping the sky • Survey consortia self-organized by community 2004 11 September 2008 NSF

  5. Pulsars • Discovery -- (pALFA) • timing, MSP timing, gravitational-waveenergy density • timing noise investigations • high-time resolution studies • tests of general relativity • physics of extreme environments (B, Eqn. State) • ISM studies (using pulsars as probes of ISM, etc) • precision astrometry (parallaxes, proper motions, etc) • pulsar time scales (inertial & dynamical) 11 September 2008 NSF

  6. 2.15 msec 95 d orbit e 0.43667 1.74±0.04 Mo J1903+0327 11 September 2008 NSF

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  9. Traditional Arecibo topics • Pulsars -- (pALFA), timing MSP • 21 cm HI • Extra-galactic {alfalfa, AGES, (AUDS), ([ZoA]) } • Galactic {Disk-Halo, (I-gALFA), [TOGS,TOGS2,GALFACTS2]} • OTHER • Magnetic Fields {(GALFACTS), (ULIRGs) } 11 September 2008 NSF

  10. HI STUDIES • Trace phase change from ionized to neutral species • HI eliminated via phase change to molecular species • Traces accumulation of visible baryons into galaxies -- Tully Fisher Relation 11 September 2008 NSF

  11. 300 200 V, km/s 100 30 10 50 r, kpc BTF from Resolved Rotation Curves M33 stars HI Need aperture synthesis HI maps - limits sample sizes HI H Vrot h d b HI KS 2005 NRAO/AUI and NOAO/AURA/NSF Rector et al. 11 September 2008 NSF

  12. The Baryonic Tully-Fisher Relation BTF Stellar TF 1011 1011 H K’ I B Md M* (Mo) (Mo) 109 109 (colors) 107 107 McGaugh et al 2000 30 100 300 100 300 30 Vrot (km/s) Vrot (km/s) Philosophy Coverage over Completeness 11 September 2008 NSF

  13. Arecibo as an HI telescope in the coming era of active SKA survey- optimized pathfinders (ASKAP, MSKAP) to be followed by the SKA whence Arecibo? The mid-range SKA is a 0.3-3 GHz+ facility That exactly matches Arecibo, so Arecibo’s scienceis SKA precursor science 11 September 2008 NSF

  14. Exploit Sensitivity by • Looking at large redshifts => evolution in TF relation • Looking for local very low mass objects => alfalfa 11 September 2008 NSF

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  16. A Pilot Survey of HI in Field Galaxies at z ~ 0.2: Catinella et al ApJL 11 September 2008 NSF

  17. Text ~5300 galaxies from alfalfa: RA 7.5 - 16.5 hr, dec 12 - 16° 11 September 2008 NSF

  18. HIMF • Previous surveys have detected few (if any) objects with low HI. • At low mass end, HIMF estimates differ by >10X: • Rosenberg & Schneider (2000) • versus • Zwaan et al. (1997) ? Parkes HIPASS survey: Zwaan et al. 2003 11 September 2008 NSF

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  21. Traditional Arecibo topics • Pulsars -- (pALFA), timing MSP • 21 cm HI • Extra-galactic {alfalfa, AGES, (AUDS), ([ZoA]) } • Galactic {Disk-Halo, (I-gALFA), [TOGS,TOGS2,GALFACTS2]} • OTHER • Magnetic Fields {(GALFACTS), (ULIRGs) } 11 September 2008 NSF

  22. TOGS HI map from commensal observations in fall 2007 Dec. 21 - 26°; RA 3hr - 23 hr 11 September 2008 NSF

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  25. Magnetic Fields GALFACTS 11 September 2008 NSF

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  27. VLBI and AreciboThe impact of Arecibo’s sensitivity • Arecibo added to the VLBA => 4.5 times better sensitivity (Day & Momjian 2005). 11 September 2008 NSF

  28. VLBI Highlights Post-Painting MK5A Disk-recorded:Three successful Mk5A disk-based runs using L, C and X-band, with HAS, EVN & Global network. These represent; (1) a study of the Zeeman effect for compact components in ULIRGs, (2) jet and counter-jet emission in the giant radio galaxy, NGC315 and, (3) measuring the expansion velocity of SN2008D associated with the transient X-ray source in NGC2770 (Target of Opportunity). E-VLBI test over the existing OC3 (155Mbps-shared with UPR) line: Arecibo data arriving at JIVE Fringe amplitude for 128 Mbps @128Mbps @64Mbps Jb - Tr Jb - Wb Fringe amplitude for 64Mbps Jb - Tr Jb - Wb Jb - Ar Tr - Wb Jb - Ar Tr - Wb QSO 3C395 Tr - Ar Wb - Ar Wb - Ar Tr - Ar 11 September 2008 NSF

  29. Exploiting 1 - 10 GHz • Molecular line searches (Galactic starting) • Molecular line searches extragalactic ULIRGS, recent success 11 September 2008 NSF

  30. A Spectral Scan of Arp 220:1.1 – 10 GHz Arp 220 is a star-burst galaxy at a distance of 250 Mly. It is forming stars at 100-times the rate of the Milky Way. It is the result of a collision between 2 galaxies now in the final stages of merging. (VLA:Radio Wavlength 6cm)‏ (HST:Optical)‏ 11 September 2008 NSF

  31. The Spectrum of Arp 220 – Prebiotic Molecules Methanimine (CH2NH) observed for the first time outside of the Milky Way (where it has only been observed in one source!)‏ This is probably a maser emitter. “Bending” transitions of HCN observed for the very first time in the radio region. These lines are at L-, C-, C-Hi & X-band. STOP PRESS: HCN at S-band. 11 September 2008 NSF

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