1. Radio Astronomy -- Other Than ALFA Surveys
430-MHz Arecibo + DRAO-ST image of a region of the Perseus-Pisces Supercluster.
(Courtesy: Phil Kronberg)
Chris Salter (NAIC/Arecibo Observatory)
AUSAC Meeting · March 9 − 10, 2008

2. The Rules of the Game Pre-Nov 2006:
-- 50% of R.A. telescope time for non ALFA survey astronomy (~2400 hr per yr).
-- Rx available: 327, 430 & 610 MHz; LBW, SBW, SBH, CB, CBH & XB.
Post-Nov 2006:
-- 20% of R.A. telescope time for non ALFA- survey astronomy (~750 hr per yr).
-- Rx available: 327 & 430 MHz; LBW, CB &
XB; (plus SBW, SBH & CBH on “campaign” basis).
AUSAC Meeting · March 9 − 10, 2008

3. PSR J1903+0327 – Confirming its High Mass
Constraints on mass based on GBT and Ar timing.
“Classical” contribution to advance of periastron is not large.
J is more massive than any other NS with a precise mass determination.
The J mass excludes the “softest” EOSs.
Companion is likely to be a massive white dwarf or main sequence star.
PSR Period = 2.15 ms
Binary Period = 95 day
Orbital Eccentricity = 0.44
PSR mass = 1.67±0.01Mo → implications for EOS of cold ultra-dense matter.
(Courtesy: Paulo Freire)
AUSAC Meeting · March 9 − 10, 2008

4. Red Dwarf “Pulsars” – TVLM 513
Arecibo provides the wide bandwidth and high spectral resolution not available with the VLA → dynamic spectra of the pulses from TVLM 513.
Pulses resolved in both time and frequency → Brightness temperature > 1015 K for this electron cyclotron maser emission.
Radio emission occurs at electron cyclotron frequency → magnetic field strength of kiloGauss.
HSA (including Arecibo) used for VLBI follow-up observations.
AUSAC Meeting · March 9 − 10, 2008

5. The Cosmic 3He Abundance
(PI: Tom Bania)
3He measurements can be used to test the theory of stellar nucleo-synthesis, put limits on models of Galactic chemical evolution and constrain Big-Bang nucleo-synthesis.
Mass loss from PNe should be substantially enriched in 3He, and its abundance is an important test of stellar evolution theory.
3He+ has a hyperfine transition at 8665 MHz, which is detected in a composite Arecibo spectrum for NGC6210 and 6891.
Find Arecibo X-band baselines are much better than those at L-band.
AUSAC Meeting · March 9 − 10, 2008

6. HI Forbidden-Velocity Wings
2004-6: Arecibo (LBW and ALFA) + GBT observations of 22 FVWs.
12-13 show shell-type structure; “missing” SNRs?
9-10 show cloud-type structure; halo clouds or HVCs?
HVC
004-6:
LDS
b=−0.5°
(Courtesy: Ji-hyun Kang)
AUSAC Meeting · March 9 − 10, 2008

7. High-Resn HI Image of Smith’s Cloud
GBT image has HPBW = 9‘
Arecibo ALFA image has HPBW = 3.5‘
Smith’s Cloud is an HVC plunging into the Galaxy and displaying signs of interaction
Arecibo images show evidence for hydrodynamic phenomena
Low-velocity gas (red) appears to wrap around the Cloud, interpreted as gas stripped from the Cloud and decellerated by Milky Way halo gas
GBT
(Courtesy: Jay Lockman)
ALFA
AUSAC Meeting · March 9 − 10, 2008

8. The Molecular Spectra of ULIRGs
Arp 220
IC 860 Zw
CH2NH
HCN v2=1, J=3 transition
H2CO
HCN
(v2=1)
CH triplet (λ9 cm)
Excited OH
(main line)
Co-added H119α-H127α (λ9 cm)
rms noise = 50 μJy/bm
AUSAC Meeting · March 9 − 10, 2008

9. Zeeman Effect in ULIRG Megamasers
(PI’s: Tim Robishaw & Carl Heiles)
Many OH megamasers in ULIRGs show Zeeman splitting of individual components yielding typical line-of-sight magnetic fields of mGauss.
Following-up their initial detection of this phenomenon for ULIRGS, the P.I.’s are now making a Zeeman survey all suitable ULIRG OHMs in the Arecibo sky.
Linear polarization of the OHM in Arp 220 yields a Rotation Measure.
To resolve the Zeeman components spatially, VLBI has been made using the HSA (including Arecibo) allowing investigation of the origins of the magnetic fields.
AUSAC Meeting · March 9 − 10, 2008

10. An H2O Megamaser at z = 2.64
(PI’s: Paola Castangia & Violetta Impellizzeri)
MG J is a gravitationally lensed QSO at z = 2.64.
H2O megamaser emission detected from it at Ef & VLA. Line is blueshifted relative to the QSO by 300 kms-1.
Being monitored at Ar for variability of line and continuum and to search for redshifted components. If such components are found indicates a “disk maser” rather than a “jet maser”.
After first 4 sessions, line profile appears very stable. No conclusive evidence yet for redshifted components.
AUSAC Meeting · March 9 − 10, 2008