1. ARECIBO ASTRONOMY SURVEYS
Murray Lewis
Head Radio Astronomy Group
11 September 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 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 NSF

4. 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 NSF

5. ALFA: A Camera for Arecibo
Installed 2004 Apr
Surveys initiated Feb 2005
7 beams x 2 pol (linear) = 14 “pixels”
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 NSF

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8. 2.15 msec
95 d orbit e
1.74±0.04 Mo J
11 September NSF

9. 11 September NSF

10. 11 September NSF

11. 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 NSF

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

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

14. 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 GHz+ facility
This exactly matches Arecibo, so
Arecibo’s science is SKA precursor science
11 September NSF

15. 11 September NSF

16. A Pilot Survey of HI in Field Galaxies at z ~ 0
A Pilot Survey of HI in Field Galaxies at z ~ 0.2: Catinella et al ApJL
11 September NSF

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

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

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20. 11 September 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) }
11 September NSF

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

29. 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
Tr - Ar
Wb - Ar
11 September NSF

30. 11 September NSF