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11 September 2008 NSF
ARECIBO
RADIO ASTRONOMY
Chris Salter for Murray Lewis
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. > 109 yr
• Magnetic field: B > 20 orders of magnitude– Mercury null; ISM; to Magnetars > 10^13 gauss
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}
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
11 September 2008 NSF
Pulsars
• Discovery -- (pALFA)
• timing, MSP timing, gravitational-waveenergy 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
J1903+03272.15 msec
95 d orbit
e 0.43667
1.74±0.04 Mo
11 September 2008 NSF
11 September 2008 NSF
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) }
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 September 2008 NSF
BTF from Resolved Rotation Curves
Need aperture synthesis HI maps - limits sample sizes
NRAO/AUI and NOAO/AURA/NSF Rector et al.
M33 starsHI
r, kpc10 30 50
100
200
300
V, km/s
HIH
HI b
d
Vrot
h
b ϒ*
KS 2005
11 September 2008 NSF
The Baryonic Tully-Fisher Relation
M*
Vrot (km/s)
Md
McGaugh et al 2000
100Vrot (km/s)
30030 100 300301
09
10
111
07
10
91
011
10
7Stellar TF BTF
M* =ϒ*L
M d =M* +1.4MHI
Coverage over CompletenessPhilosophy
(Mo) (Mo)
(colors)
H K’ I B
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
11 September 2008 NSF
• Looking at large redshifts
=> evolution in TF relation
• Looking for local very low mass objects => alfalfa
Exploit Sensitivity by
11 September 2008 NSF
11 September 2008 NSF
A Pilot Survey of HI in Field Galaxies at z ~ 0.2: Catinella et al ApJL
11 September 2008 NSF
Text
~5300 galaxies from alfalfa: RA 7.5 - 16.5 hr, dec 12 - 16°
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
11 September 2008 NSF
11 September 2008 NSF
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) }
11 September 2008 NSF
TOGS HI map from commensal observations in fall 2007
Dec. 21 - 26°; RA 3hr - 23 hr
11 September 2008 NSF
11 September 2008 NSF
11 September 2008 NSF
Magnetic Fields
GALFACTS
11 September 2008 NSF
11 September 2008 NSF
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
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 - Tr
Jb - Wb
Jb - Ar Tr - Wb
Tr - Ar Wb - Ar
Fringe amplitude for 128 Mbps
Jb - Tr Jb - Wb
Jb - Ar Tr - Wb
Tr - Ar Wb - ArQSO 3C395
11 September 2008 NSF
Exploiting 1 - 10 GHz
• Molecular line searches (Galactic starting)
• Molecular line searches extragalactic
ULIRGS, recent success
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)
11 September 2008 NSF
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