The Impact of the 12 m Telescope on Millimeter Science: Setting the Stage for the Future

The Impact of the 12 m Telescope on Millimeter Science: Setting the Stage for the Future Lucy M. Ziurys and the Staff of the Arizona Radio Observatory T R * (K) 0.4 0.3 0.2 0.1 CH 3 OCH 3 CH 3 OCH 3 SO 2 HCOOH HCC 13 CCN HCOOCH3 HCOOCH 3 CH 3 OH Sgr B2(N) 111.5 GHz CH 3 CH 2 CN CH 3 CCCN HOCH 2 COCH 3 CH 3 CCCN HCOOCH 3 HCOOCH 3 (CH 2 OH) 2 13 CCCS CH3 OH 0.0-730 -530-330 -130 70 270 470 670 V LSR (km/s) 1

The 12 M Telescope and John Payne 12 m Telescope began as the 36 ft. in late 1960 s - began as a bolometer facility (Frank Low) - discovery of CO in 1970 at the 36 ft. - emphasis shifted to spectral lines pgraded to 12 m in 1984 Remained a world class telescope for spectroscopy 12 m: 2006 John Payne played the major role in making the this telescope a renowned spectroscopic instrument in mm astronomy CO: J= 1-0: Orion Wilson et al 1970 2

Some of John s Many Contributions At the 36 ft. pgraded Telescope Servo System - improved performance Spectrometer backends: the Filter Banks - John built the Multiplexer allowed for multiple upgrades to filter banks (2 MHz, 30 khz filters) - Also built the Switcher flexibility to easily change between various resolutions Nutating Sub-reflector - one of first small, fast systems Servos, multiplexer, switcher till in use today at the 12 m Switcher Multiplexer 3

pgrade from the 36 ft. to the 12 m - surface improvements needed in mid 1970 s - Dents in the dish due to falling of feed legs - with John Findlay and John replaced machined surface with new back-up structure and panels (the 12 m) Holography at the 12 m with LES 8 satellite - improved overall surface accuracy (65 microns rms from > 100 microns) - also aided by shaped compensating sub-reflector 4

A Huge Contribution to 12 m receivers Key to replacing old Schottky systems with SIS receivers in late 1980 s First SIS receiver was 3 mm (WR-10) - fill with liquid helium Replaced with the J-T Rocket systems - employed closed cycle refrigerators Receiver Wavelength 3 mm HI 90 115 GHz 1 mm LOW 200 260 GHz 3 mm LO 65 90 GHz 2 mm 125-180 GHz 1 mm HIGH 260-300 GHz 1 mm 8 beam 200 250 GHz 3 mm LO STILL unique in world 1mm LOW/ 1mm HIGH In rxr bay at 12 m 5

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Many important innovations in the 12 m receivers John brought Joule -Thompson systems to 12 m Designed mechanical infrastructure - building each mixer into an insert (rockets) - placing many inserts in one large dewar - spare inserts for quick replacement (2/3 mm dewar; 1 mm dewar) - designed cross-grid for dual polarization - installed M-P s for SSB operation Rockets 1 mm system Cross-Grid Rockets in Dewar 8

Led to a highly versatile, molecular-line machine Complete coverage of 1,2, and 3 mm windows - never achieved at any other telescope All receivers very sensitive (SIS junctions) AND STABLE - still competitive with the world s best Dual polarization - two independent answers, besides extra integration time SINGLE-SIDEBAND - Invaluable for line searches, accurate calibration Nice suite of multiple resolution backends (Filter banks, MAC) easy to switch between receivers, backends - moving a few cables, central selection mirror, cross-grid Coupled with a fast, efficient control system, the 12 m has been able to do great science INTEGRATION OF THE COMPLETE SYSTEM AND ALL COMPONENTS WORKED WELL 9

Highlights of the 12 m Scientific Contributions Astrochemistry - Detection of many new molecules - 12 m created the field Extragalactic - ISM in external galaxies - CO at high red-shifts Comets and the Solar System - Molecule studies in comets - planetary atmospheres Star Formation - Outflows, disks, protostars in dense clouds - Cloud structure and dynamics Evolved Stars - Detection and structure of circumstellar envelopes - Mass loss to the ISM Astrobiology 10

2 3 4 5 6 7 8 9 10 H 2 CH + H 2 O C 3 NH 3 SiH 4 CH 3 OH CH 3 CHO CH 3 CO 2 H CH 3 CH 2 OH OH CN H 2 S HNC H 3 O + CH 4 NH 2 CHO CH 3 NH 2 HCO 2 CH 3 (CH 3 ) 2 O SO CO SO 2 HCN H 2 CO CHOOH CH 3 CN CH 3 CCH CH 3 C 2 CN CH 3 CH 2 CN SO + CS NNH + CH 2 H 2 CS HC CCN CH 3 NC CH 2 CHCN C 7 H H(C C) 3 CN SiO C 2 HNO NH 2 HNCO CH 2 NH CH 3 SH H(C C)2 CN H 2 C 6 H(C C) 2 CH 3 SiS SiC CCS HOC + HNCS NH 2 CN C 5 H C 6 H CH 2 OHCHO C 8 H CH 3 COCH 3 CH 3 (C C) 2 CN (CH 2 OH) 2 NO CP NH 2 NaCN CCCN H 2 CCO HC 2 CHO c-ch 2 OCH 2 11 NS CO + H + 3 MgNC HCO + 2 C 4 H CH 2 =CH 2 H 2 CC(OH)H H(C C)4 CN HCl HF NNO AlNC CCCH c-c 3 H 2 H 2 C 4 NaCl SH HCO SiCN c-c 3 H CH 2 CN HC 3 NH + KCl HD HCO + SiNC CCCO C 5 C 5 N AlCl OCS H 2 D + C 3 S SiC 4 H(C C) AlF CCH MgCN HCCH H 2 C 5 CN 3 ~100 Carbon Molecules PN HCS + KCN HCNH + HCCNC SiN c-sicc HCCN HNCCC Total = 128 NH CCO H 2 CN H 2 COH + CH c-sic 3 Known Interstellar Molecules 11 Silicon Species 9 Metal Containing Molecules WHAT else??? 12 13 11

A Confusion Limited Survey of SgrB2(N) 0.4 0.3 0.2 TR * (K) 0.1 Sgr B2(N) 111.5 GHz CH3 OCH 3 HCC 13 CCN HCOOCH3 CH3 CH 2 CN HOCH2 COCH 3 HCOOCH3 HCOOH CH3 CCCN CH3 CCCN HCOOCH3 (CH2 OH) 2 HCOOCH3 CH3 OH CH3 OCH 3 13 CCCS CH3 OH SO2 0.0-730 -530-330 -130 70 270 470 670 V LSR (km/s) 12

A Confusion Limited Survey of SgrB2(N) 1.0 0.8 0.6 T R * (K) 0.4 0.2 0.0 143.0 143.2 143.4 143.6 Frequency (MHz) 143.8 144.0x10 3 13

A Real Link to the Origin of Life? Darwinian evolution implies best chemical solutions for life Life did not always choose the best Many alternative biochemical possibilities WHY only 20 amino acids in living systems? Other amino acids work in proteins WHY ribose and deoxyribose in DNA, ATP? Why not glycerol, a hexose or a tetrose? Terrestrial Life did not have time to sample all chemical possibilities - reflects what was present by chance Synthetic Contingencies Early Earth lost original carbon Earth constantly bombarded by organic material (comets, meteorites, dust) Organics came from interstellar chemistry 14 H O RIBOSE OH O Phosphate ester OH OH Base pair Ribose DNA ALTERNATIVES TO RIBOSE

Detection of Glycolaldehyde Observed 40 transitions of CH 2 OHCHO in range 67 165 GHz (12 m) All favorable transitions in 10-70 K range Accounted for all possible contaminants Modeled relative intensities Showed a physical connection exists Halfen et al 2005 93043 15

Detection of Glycolaldehyde Observed 40 transitions of CH 2 OHCHO in range 67 165 GHz (12 m) All favorable transitions in 10-70 K range Accounted for all possible contaminants Modeled relative intensities Showed a physical connection exists Halfen et al 2005 16

Detection of Glycolaldehyde Observed 40 transitions of CH 2 OHCHO in range 67 165 GHz (12 m) All favorable transitions in 10-70 K range Accounted for all possible contaminants Modeled relative intensities Showed a physical connection exists Halfen et al 2005 17

Detection of Glycolaldehyde Observed 40 transitions of CH 2 OHCHO in range 67 165 GHz (12 m) All favorable transitions in 10-70 K range Accounted for all possible contaminants Modeled relative intensities Showed a physical connection exists Halfen et al 2005 18

The 12 m (now ARO) remains a competitive instrument 12 m C 3 O in IRC+10216 Tenenbaum et al (2006) IRAM CO does not control chemistry in C-rich circumstellar shells 19

Studies of Oxygen-Rich Supergiant Star VY Canis Majoris First clear detection of HCO+ in a circumstellar envelope Ions important in circumstellar chemistry VYCMa: IR image Bipolar outflow 12 m/smt baseline 20

An Inspiration to Many Students. 21

An Inspiration to Many Students. Astrobiology.Washington Exchange Winter School 22

The Tradition Continues At the Arizona Radio Observatory s SMT keep tradition handed down from John Payne - insert concept for receivers - dual polarization, SSB mixers - reliable backends - stable front-end and backends high quality spectroscopy With a little help from our friends Inserts at SMT SMT 1.4 1.2 1.0 0.8 TR* (K) 0.6 0.4 0.2 0.0 37 Indentified Features 35 nidentified Features ~6 lines per 100 km/s T RMS = 0.003 K (theoretical) New ARO Filter Banks OCS 13 CS C2 H 5 OH C2 H 5 CN C2 H 3 CN C2 H 3 CN C2 H 3 CN C2 H 3 CN CH3 CHO + C 2 H 5 CN CH3 CHO + C 2 H 3 CN HCOOCH3 CH3 CHO C2 H 5 OH C2 H 5 OH HNCO CH3 CHO NH2 CHO (CH3 ) 2 O HCOOH C2 H 3 CN + C 2 H 5 CN CH3 CHO HCOOCH3 C2 H 5 CN C2 H 3 CN C2 H 5 CN HCOOCH3 HCOOCH3 + C 2 H 3 CN C2 H 3 CN C2 H 5 CN HCOOCH3 HCOOCH3 C2 H 5 OH + (CH 2 OH) 2 CH3 NH 2 (CH3 ) 2 O CH3 CHO 231000 231200 231400 231600 231800 232000 Frequency (MHz) 23

Circa 1989 Arizona Radio Observatory Thanks, John, for showing us the way. 24