Radio Astronomy Other Than ALFA Surveys FVW 39

Radio Astronomy -- Other Than ALFA Surveys FVW 39. 0+4. 0: An HI Forbidden Velocity Wing, Blue = +80 – +95 km/s Green = +95 – +110 km/s Red = +110 – +135 km/s Stars = Early-type stars in field Triangles = Pulsars (Courtesy: Ji-hyun Kang ) Chris Salter (NAIC/Arecibo Observatory) AUSAC Meeting April 19 − 20, 2010

The Official Rules of the Game • Post-Nov 2006: -- 20% of R. A. telescope time for non ALFAsurvey astronomy (~750 hr per yr). -- Rxs available: 327, 430 & 750 MHz, ALFA, LBW, SBW, CB & XB; (plus SBH & CBH on a “campaign” basis). AUSAC Meeting April 19 − 20, 2010

Radio and γ-Ray Pulsars • Arecibo pulsar, J 2021+3651 is found to be one of the strongest γ-ray emitters by Fermi/GLAST. • Of 9 new γ-ray pulsars in the Arecibo sky from Fermi/GLAST, J 1907+0602 is found to be a radio pulsar (P=0. 10664 s). With S 1. 4 GHz= 3 μJy, and a distance ~ 3 kpc, it is the second least luminous pulsar known! Arecibo timing of 'unidentified' Fermi source, J 2214+3002, has permitted the detection of the object as a γ-ray pulsar. Fermi pulsar, J 2017+0603, has been observed several times at Arecibo, and found to have a 'supersharp' pulse profile. As it is likely a MSP-WD binary, it is a good NANOGrav candidate. AUSAC Meeting April 19 − 20, 2010

Four-Frequency High Precision Timing of a Msec Pulsar The detection of gravitational waves with pulsars will requires high timing precision: effects at 10 ns level can limit the sensitivity to gravitational waves. Goals of project: Identify and mitigate the effect of variability in the ISM (interstellar weather) in precision pulsar timing observations. Tube size Radio waves travel through bananashaped tube Tube offset from direct line-of-sight Earth Pulsar Solar System Barycentre ISM acts like warped glass, distorting the trajectory of the propagating radio waves (tube). As the volume of interstellar space changes, the tube wanders → arrival time variations. Target: PSR J 1713+0747, the most stable millisecond pulsar in the Arecibo sky. Observations: 327 MHz, 430 MHz, L and S bands; 20 transits over 6 months. Data recorded simultaneously for timing (ASP, high time resolution), for ISM analysis (WAPP, higher frequency resolution), and a VLBI baseband recorder (Mark 5 A). AUSAC Meeting April 19 − 20, 2010

S-band observations, lower timing precision due to lower flux. L-band observations, systematic trends (associated with ISM? ) Ph. D. Thesis: Ryan Shannon ~1 microsec ~ 2 hours Combine all TOAs to form “grand” arrival time at this epoch 430 MHz Key Analysis: Connect residual To. A (top) and pulsar dynamic spectra (right) and determine if the dynamic spectra encode ISM delays? AUSAC Meeting April 19 − 20, 2010 327 MHz

Apparent > c Wave Propagation in the ISM HI Emission Spectrum PSR Absorption Spectrum PSR Delay Spectrum The group velocity of the ISM is > c near the HI resonance line due to “anomalous dispersion”. Delay Spectra for 3 Consecutive Days The plot above shows the expected absorption and delay spectra after propagation though a cloud of HI in the ISM with TS= 100 K, tau = 1. Potential tool for studying the HI properties of the ISM. (Note: It does NOT violate Special Relativity!) AUSAC Meeting April 19 − 20, 2010

HI Forbidden-Velocity Wings HVC LDS b=− 0. 5° • Arecibo 004 -6: (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? FVW's 173. 0+1. 5 & 173. 0+0. 0: Red = +45 – +35 km/s, Green = +35 – +25 km/s, Blue = +25 – +15 km/s. The HI emission coincides with a weak continuum shell. FVW G 40. 0+0. 5: Red = -100 – -90 km/s, Green = -90 – -80 km/s, Blue = -80 – -70 km/s. AUSAC Meeting April 19 − 20, 2010

Zeeman Effect in ULIRG Megamasers • The P. I. ’s have been granted 450 hr to make a Zeeman survey all suitable ULIRG OHMs in the Arecibo sky. • Many OH megamasers in ULIRGs show Zeeman splitting of individual components yielding typical line-of-sight magnetic fields of 0. 3 -18 m. G. Minimum energy and equipartition suggest ULIRG magnetic fields of 1 m. G < B < 10 m. G. • B is similar to the values in Galactic OH masers, suggesting conditions of massive star formation are similar to those in the Milky Way. • 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 April 19 − 20, 2010

Molecular Lines in Galaxies CH 2 NH H 2 CO HCN (v 2=1) H 2 O maser in host galaxy of QSO J 0414+0534 (z=2. 64) monitored at 6 -week intervals. Top Formaldehyde Absorption and (bottom) excited-line OH maser emission in LIRG, NGC 660 AUSAC Meeting April 19 − 20, 2010 Excited OH (main line) Molecules in Zw 049. 057

700 – 800 MHz Gallery HI absorption in the host galaxy of CTA 21 against the continuum emission of the central quasar Globular Cluster Pulsar Observations M 5 A M 13 A at Arecibo on 20 & 21 September 2009 Redshift, z = 0. 906 CTA 21 is seen at 46% of the present age of the Universe M 13 C M 15 A M 15 B M 15 C Observed CH main line at 724 MHz in W 51 AUSAC Meeting April 19 − 20, 2010

An Arecibo Galactic Chemistry Survey • First proposal made in 2007 to make a 1 – 10 GHz survey of a number of representative Galactic sources using the Mock Spectrometer in single-pixel mode. • Unbiased spectral line surveys → information needed to characterize physical and chemical conditions. • The full range 1 – 10 GHz is relatively unexplored for Galactic sources and many complex molecules have lines at λ < 3 cm. • “Line confusion” is very much less in this range than at millimeter wavelengths. AUSAC Meeting April 19 − 20, 2010

Precursor Observations • Observations made in Oct-Nov 2008. • Targets were star-forming region, NGC 2264, and C-rich, evolved PPN, CRL 618. • The single-pixel Mock mode was not ready, so the precursor observations were made with the WAPPs. • A shallow, but full, 1 – 10 GHz coverage was made for both objects with a velocity resolution of 0. 7 kms-1. Excited satellite line OH maser in PPN, CRL 618 Methanol in NGC 2264 -IRS 1 AUSAC Meeting April 19 − 20, 2010 HC 3 N in NGC 2264 -IRS 1

Test Set-Up: Oct 5 th 2009 • A second proposal was submitted in Feb. 2009 to make a full 1 – 10 GHz survey of the ultra-compact source W 51 e 2 in W 51 IRS 1. This was graded 'A', and awarded 112 hr. • A preliminary version of the single-pixel Mock mode was made available by Phil Perillat this fall. • An hour's test time was used to try out a first AGCS C-band set-up for the Mocks on October 5 th 2009. • This had a velocity resolution of 0. 3 kms-1, and covered a total band of about 500 MHz, about 50% of the potential coverage (only a single Mock band being available. ) • 4 ON/OFF scans were acquired on W 51 e 2 and the data reduced to get a check of the resulting spectra. AUSAC Meeting April 19 − 20, 2010

Radio Recombination Lines H 138β H 110α H 139β H 161γ H 111α H 140β H 112α H 141β AUSAC Meeting April 19 − 20, 2010

Molecular Lines H 213 CO H 141β Excited OH Satellite Line (2Π J=½ F=0– 1) ½ H 2 CO AUSAC Meeting April 19 − 20, 2010

Muchas Gracias AUSAC Meeting April 19 − 20, 2010

HI Absorption in the Host Galaxy of QSO CTA 21 Analog-to-Digital migration of TV transmissions in June 2009 temporarily freed up the 700– 800 MHz band. Arecibo has provided and commissioned a receiver. CTA 21 at arcsec resolution: contours= radio; greyscale=optical HI absorption in the host Optical Spectrum of CTA galaxy of CTA 21 against the 21 continuum emission of the central quasar Central Frequency = 745. 5 MHz AUSAC Meeting April 19 − 20, 2010 Flux Density (Jy) Observed at Arecibo on 20 & 21 September 2009 Redshift, z = 0. 906 Distance = 7, 335, 000 light years CTA 21 is seen at 46% of CTA 21 at milliarcsec resolution the present age of the Universe 10 1 0. 1 10000 Frequency (MHz) Radio Spectrum of CTA 21

The Molecular Spectra of ULIRGs Arp 220 Zw 049. 057 IC 860 CH 2 NH HCN v 2=1, J=3 transition H 2 CO CH triplet (λ 9 cm) HCN (v 2=1) Excited OH (main line) Co-added H 119α-H 127α (λ 9 cm) rms noise = 50 μJy/bm AUSAC Meeting April 19 − 20, 2010

The 10000 ASP Times of Arrival 6 months Project in progress: (Ryan’s dissertation: coming in August 2010!) Requirements for mitigating ISM effects: Wide bandwidth instrumentation: ISM effects are mitigated by both a) observing at higher frequencies and b) observing with wider bandwidths. Also require instruments with high frequency resolution to perform dynamic spectra analysis (i. e. , Mock) complementary to wide bandwidth timing instruments (GUPPI-clone). Need sensitive telescope (i. e. Arecibo) to identify and mitigate propagation effects Ryan would like to thank the AO Staff (especially Tapasi Ghosh) for assistance with the observations 6 months AUSAC Meeting April 19 − 20, 2010

Results • Detected 14 B fields. • Detected fields in 5/8 ULIRGs. • First extragalactic Zeeman splitting detections in emission lines. – Only previous extragalactic Zeeman detection was HI in absorption in high-velocity cloud around Perseus A (Kazes et al. 1991; Sarma et al. 2005). • B is similar to local sites of OH masers. – Conditions in regions of massive star formation are similar to those in Milky Way. • B is consistent with inferred synchrotron fields. – Probing gas closer to typical ISM density. AUSAC Meeting April 19 − 20, 2010