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

2. 11 September 2008 NSF 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. > 10 9 yr Magnetic field: B > 20 orders of magnitude –Mercury null; ISM; to Magnetars > 10^ 13 gauss

3. 11 September 2008 NSF 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}

4. 11 September 2008 NSF ALFA: A Camera for Arecibo 2004 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

5. 11 September 2008 NSF 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)

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

7. 11 September 2008 NSF

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) }

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

12. 11 September 2008 NSF The Baryonic Tully-Fisher Relation M*M* V rot (km/s) MdMd McGaugh et al 2000 100 V rot (km/s) 30030100300 30 10 9 10 11 10 7 10 9 10 11 10 7 Stellar TF BTF Coverage over Completeness Philosophy (M o ) (colors) H K’ I B

13. 11 September 2008 NSF 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 science is SKA precursor science

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

15. 11 September 2008 NSF

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

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

18. 11 September 2008 NSF Parkes HIPASS survey: Zwaan et al. 2003 ? 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) HIMF

19. 11 September 2008 NSF

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) }

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

23. 11 September 2008 NSF

25. Magnetic Fields GALFACTS

26. 11 September 2008 NSF

27. VLBI and Arecibo The impact of Arecibo’s sensitivity Arecibo added to the VLBA => 4.5 times better sensitivity (Day & Momjian 2005).

28. 11 September 2008 NSF 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 @64Mbps @128Mbps Fringe amplitude for 64Mbps Jb - TrJb - Wb Jb - ArTr - Wb Tr - Ar Wb - Ar Fringe amplitude for 128 Mbps Jb - TrJb - Wb Jb - ArTr - Wb Tr - ArWb - Ar QSO 3C395

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

30. 11 September 2008 NSF 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. (HST:Optical)‏ (VLA:Radio Wavlength 6cm)‏

31. 11 September 2008 NSF The Spectrum of Arp 220 – Prebiotic Molecules Methanimine (CH 2 NH) 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.

32. 11 September 2008 NSF