AUSAC Meeting · March 17-18, 2008 Radio Astronomy -- Other Than ALFA Surveys Chris Salter (NAIC/Arecibo Observatory)‏

AUSAC Meeting · March 17-18, 2008 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; (SBW, SBH & CBH on “campaign” basis).

AUSAC Meeting · March 17-18, 2008 Pulsar Study: The “Planets Pulsar” Alex Wolszczan is completing a 17-yr study of the “planets pulsar”, PSR B His timing fits includes; All PSR parameters Astrometric parameters Three planets (including the mutual perturbations of Planets b & c) DM variations (3 rd panel). Highlights of 17-yr Study of B First exoplanets. First detection of planets in mean motion resonance (MMR 3:2). First multiplanet system. First terrestrial-mass system. First dynamical analog of the inner solar system (scaled down by a factor of ~2). 430-MHz Raw Residuals 1400-MHz Raw Residuals Residuals including DM Variations Dispersion Measure (DM) Variations

AUSAC Meeting · March 17-18, 2008 Continuum Studies Combining DRAO Interferometer and Arecibo 400-MHz data, Kronberg et al. have imaged an 8 º  8 º region in the P-P supercluster to examine the nature of the low-level emission. The Arecibo images were CLEANed before being combined with those from DRAO. The angular resolution of the image is 10 arcmin. Minchin et al observed galaxies from the Scuba Local Universe Galaxy Survey (SLUGS) at 3, 5, 7 & 9 GHz to characterize their synchrotron emission to find its contribution to their 850 µm fluxes. This allowed corrected estimates of their cold dust masses.

HI emission from Disk Galaxies at z~0.2  Sample selected from SDSS according to redshift ( o ), disk morphology, and relative isolation.  Observations in standard position-switching mode, L-band wide.  41 galaxies targeted.  26 detections + 8 tentative ones  HI mass 3 − 8  M סּ  ON-source integration time between 1 and 4 hr per object  280 hr telescope time including overheads. B. Catinella (MPA, Arecibo), M. Haynes, R. Giovanelli (Cornell), J. Gardner, A. Connolly (UPitt)

SDSSARECIBOz= SDSSARECIBOz= Catinella et al. in preparation

Gas fraction vs stellar mass Black: Virgo cluster (GOLDMINE + ALFALFA, Gavazzi et al. 2008) z ~ 0 z ~ 0.2 Catinella et al. in preparation Evolution effects? Need a fair sample of massive (HI, M * ), z~0 galaxies for comparison!! Virgo cluster

AUSAC Meeting · March 17-18, 2008 HI from Black-hole Host Galaxies Ho, Darling & Greene Ho, Darling and Greene have made a large survey of 154 nearby Type-1 (broad-lined) AGNs whose black-hole masses and accretion rates are known. This enables them to constrain a number of properties of relevance to the relationship between BHs and their hosts. HI was detected in a high percentage of the targets. HI spectra yield: Maximum rotation velocity of disk. Estimate of galaxy luminosity via Tully-Fisher. Using the optical disk size, an estimate of the dynamical mass of the galaxy. A first-order estimate for the cold-gas content of the galaxy.

AUSAC Meeting · March 17-18, 2008 HI from Black-hole Host Galaxies II Ho, Darling & Greene Black-hole mass vs Dynamical mass of host galaxy B-band Tully-Fisher relation for sample. Apart from larger scatter, No gross differences between active And inactive galaxies. Distribution of MHI/LB for the host galaxies and a large sample of inactive galaxies. Similar distribution for later types, but early type active galaxies appear more gas-rich.

AUSAC Meeting · March 17-18, 2008 Molecular Line Studies: IRAS No. of Galactic H 2 CO masers = 7 A recent Arecibo H 2 CO survey of low-mass star forming regions showed these masers are exclusively associated with high-mass star formation. ` The H 2 CO maser in IRAS was discovered at Arecibo in Three short-term H 2 CO flares (∆t<3 months) have been observed to date via systematic Arecibo monitoring. The flare amplitudes appear to be linearly decreasing. The outbursts appear periodic (P ~ 8 months)‏ The next flare is predicted to occur in Apr 08, and will be looked for. The H 2 CO flares are time-correlated with 6.67-GHz CH 3 OH flares. Most of the CH 3 OH frequency components show flares that are delayed by a month, but one is prompt. High resolution follow-up with the EVLA and MERLIN is planned to investigate the phenomenon in detail. Araya, Hofner, Linz, Kurtz & Creech-Eakman

AUSAC Meeting · March 17-18, 2008 Line detections in IC 860: (Top) HCN v 2 =1, J=4 and excited-OH (4660 MHz) absorption lines: (Bottom) H 2 CO and CH 2 NH emission lines, Pre-biotic Molecules and Other Lines in ULIRGs (a) Arp 220(b) Other ULIRGs v 2 =1 direct l-type absorption lines of HCN (J = 4, 5 and 6. An excitation temperature of ~ K is implied. Non-detection of the J=2 level is likely to be due is to free-free absorption in the foreground ionized ISM. Emission from the 1 10 –1 11 methanimine (CH 2 NH) multiplet, (the 6 transitions shown by vertical lines.) This is likely to represent weak maser emission. Latest News: Detection of v 2 =1, J=3, HCN in Arp 220 (2645 MHz) gives a line-center optical depth,  ~ 3 at 1630 MHz. IC 860 H109α recombination line in NGC 3628 (ULIRG = Ultra-Luminous Infra-Red Galaxy)

AUSAC Meeting · March 17-18, 2008 Future Option: Single-Pixel “pdev/edev” Note: All but X-band would use an instantaneous bandwidth of 1 GHz, which is presently available. The anticipated “single-pixel” mode of operation for the new “pdev/edev” spectrometers offers exciting possibilities for, e.g. broad-band (bandwidths up to 2 GHz) pulsar observing, and line searches in Galactic and extragalactic targets. Reasonable parameters for a Galactic spectral scan, (velocity resolution ~ 0.5 kms -1 ), could be: