ALMA Science WorkshopMay 14, 2004 Present and Future Thomas W. Folkers Arizona Radio Observatory

ALMA Science Workshop May 14, 2004

Present and Future

Present and Future

Thomas W. Folkers

Arizona Radio ObservatoryArizona Radio ObservatoryArizona Radio ObservatoryArizona Radio Observatory

ARO’s Observing PhilosophyARO’s Observing Philosophy

• On site support personnel. ( Operators )On site support personnel. ( Operators )• Emphasize remote observing.Emphasize remote observing.• Service observing.Service observing.

Staff Astronomers for observer support.Staff Astronomers for observer support.Useful for targets of opportunity.Useful for targets of opportunity.

• Priority observing queuing. ( SMT )Priority observing queuing. ( SMT )Switch to higher frequency for PWV < 2mm.Switch to higher frequency for PWV < 2mm.

• (2) Calls for proposals per year.(2) Calls for proposals per year.• 20% Time available to outside observers.20% Time available to outside observers.

Present CapabilitiesPresent Capabilities

SMT: SpecificationsSMT: Specifications

• Elevation:Elevation: 10,435 ft.10,435 ft.• Dish:Dish: 10 Meter. f/D = 0.3510 Meter. f/D = 0.35• Surface:Surface: 60 Adjustable CFRP Panels.60 Adjustable CFRP Panels.• Accuracy:Accuracy: 15 microns15 microns RMS. RMS.• Pointing:Pointing: < 2 arc seconds, RMS on Sky.< 2 arc seconds, RMS on Sky.• Tracking:Tracking: < 0.2 arc seconds. RMS< 0.2 arc seconds. RMS• Freq Coverage:Freq Coverage:210 – 500 GHz.210 – 500 GHz.

600 – 800 GHz with PI Inst.600 – 800 GHz with PI Inst.• Observing Window:Observing Window: 24 Hrs/day, 9 Months/year.24 Hrs/day, 9 Months/year.

SMT ReceiversSMT Receivers• Spectral Line:Spectral Line:

230 GHz SIS230 GHz SIS• 210-275 GHz DSB Single Pixel210-275 GHz DSB Single Pixel

345 GHz SIS345 GHz SIS• 320-375 GHz DSB Dual Polarization320-375 GHz DSB Dual Polarization

SORAL DesertStar 7 Channel 345 Array + 4 (230 GHz).SORAL DesertStar 7 Channel 345 Array + 4 (230 GHz).• 3 345 GHz Pixels implemented.3 345 GHz Pixels implemented.

490 GHz SIS490 GHz SIS• 425-500 GHz DSB Single Pixel425-500 GHz DSB Single Pixel• 385-420 GHz with Ziurys Lab LO System.385-420 GHz with Ziurys Lab LO System.

• Continuum:Continuum: 19 Channel 345 GHz Bolometer19 Channel 345 GHz Bolometer

• Array of 19 870µm pixelsArray of 19 870µm pixels 4 Color Bolometer4 Color Bolometer

• 13001300µmµm, 870, 870µmµm, 450, 450µmµm, 350, 350µmµm Single Pixels Single Pixels

SMT BackendsSMT Backends• Spectral Line:Spectral Line:

Filters Banks:Filters Banks:• 128 x 62.5 kHz Filters.128 x 62.5 kHz Filters.• 256 x 250 kHz Filters.256 x 250 kHz Filters.• 256 x 1 MHz Filters.256 x 1 MHz Filters.

Acousto-Optical-Spectrometers:Acousto-Optical-Spectrometers:• (3) Units of 2048 Channels each.(3) Units of 2048 Channels each.

– (2) 1 GHz Bandwidth. 1MHz Resolution.(2) 1 GHz Bandwidth. 1MHz Resolution.– (1) 250 MHz Bandwidth. 385 kHz Resolution.(1) 250 MHz Bandwidth. 385 kHz Resolution.

Chirp Transform Spectrometer:Chirp Transform Spectrometer:• 4096 Channels. 183 MHz Bandwidth. 43KHz Resolution.4096 Channels. 183 MHz Bandwidth. 43KHz Resolution.• (1) Unit Installed.(1) Unit Installed.• (2) More in the works.(2) More in the works.

All Backends usable simultaneously.All Backends usable simultaneously.

• Continuum Backends:Continuum Backends: Digitizes 20 Channels simultaneously.Digitizes 20 Channels simultaneously.

Control System on the SMTControl System on the SMT

• Graphical User Interface. ( Xwindows )Graphical User Interface. ( Xwindows )• Network Based Distributed Parallel Network Based Distributed Parallel

Processing.Processing.• Remote:Remote:

Observing.Observing. Debugging.Debugging. Operation Possible.Operation Possible.

• High Data Rates. 100ms Dump Rate. ( Up to High Data Rates. 100ms Dump Rate. ( Up to 20X for OTF) 20X for OTF) **

• Non-Propriety Hardware. ( PCI / ISA / PC104 )Non-Propriety Hardware. ( PCI / ISA / PC104 )• Non-Propriety Operating Systems. ( Linux )Non-Propriety Operating Systems. ( Linux )• Compatible with 12 Meter.Compatible with 12 Meter.

* Versus old VAX/CAMAC based System

SMT Control RoomSMT Control Room

SMT Computer Room (Before)SMT Computer Room (Before)

SMT Computer Room (After)SMT Computer Room (After)

12CO(2-1) map of the Gem OB1 region obtained using OTF mapping at the HHSMT. The image shows the line integrated intensity, in antenna temperature units, smoothed to the beam size of the telescope at this frequency (i.e., 32"). The contours range from 10 to 140 K km/s in steps of 5 K km/s. The antenna beam is shown in the small box in the upper right-hand corner. Approximately 87,000 spectra have gone into this 0.75 º x 1 º map. An RMS of 0.25 K per binned point was reached for the whole map in 22 hours of observation with a single pixel receiver.

NOTE: Before smoothing, the original number of individual spectra contained in this map is 6 times as many. (522,000)

Fast OTF Mapping at the SMT

19 Ch Bolometer Continuum OTF

Bolometer sensitivity: For weather ~ 2mm PWV, 400”x300” map with default pars 150 mJy rms in 35 mins ON-OFF Sequence 600mJy/√secs

Bolometer sensitivity: For weather ~ 2mm PWV, 400”x300” map with default pars 150 mJy rms in 35 mins ON-OFF Sequence 600mJy/√secs

SMT Observing ModesSMT Observing Modes

• Spectral Line:Spectral Line: Position Switched:Position Switched:

• Relative.Relative.• Absolute.Absolute.

Beam Switched ( Up to 240” Beam Throw ).Beam Switched ( Up to 240” Beam Throw ). MappingMapping

• Grid Mapping ( PS, APS )Grid Mapping ( PS, APS )• Total Power MappingTotal Power Mapping• On-The-Fly Mapping ( OTF )On-The-Fly Mapping ( OTF )

• ContinuumContinuum Switched or Total Power ON/OFFS ( Sequences )Switched or Total Power ON/OFFS ( Sequences ) Sky TipsSky Tips MappingMapping

• On-The-Fly Mapping ( OTF )On-The-Fly Mapping ( OTF )• Grid MappingGrid Mapping

• VLBIVLBI 2 mm ( New JT System )2 mm ( New JT System ) 1 mm ( New JT System )1 mm ( New JT System )

• 3434µarcsec ( HHT – Pico Veleta )µarcsec ( HHT – Pico Veleta )

SMT Weather StatisticsSMT Weather Statistics% of Time% of Time

2000-2000-20012001

<0.0<0.066

<0.075<0.075 <0.15<0.15 <0.30<0.30

OctoberOctober 0.80.8 2.62.6 18.718.7 38.238.2

NovemberNovember 8.58.5 15.715.7 59.259.2 83.483.4

DecemberDecember 7.67.6 15.615.6 52.952.9 76.476.4

JanuaryJanuary 15.315.3 22.822.8 55.855.8 72.272.2

FebruaryFebruary 5.15.1 9.69.6 50.750.7 76.576.5

MarchMarch 3.83.8 9.49.4 49.549.5 84.484.4

AprilApril 5.55.5 11.811.8 50.350.3 75.575.5

MayMay 0.40.4 1.21.2 19.319.3 69.069.0

JuneJune 0.30.3 1.01.0 10.310.3 45.145.1

2003-2003-20042004 <0.06<0.06 <0.07<0.07

55<0.15<0.15 <0.30<0.30

OctoberOctober 0.30.3 2.22.2 27.827.8 57.757.7



JanuaryJanuary 1.01.0 2.32.3 32.332.3 72.272.2


MarchMarch 5.25.2 11.611.6 44.044.0 71.571.5

AprilApril 5.05.0 10.310.3 44.344.3 75.775.7

MayMay

JuneJune

2002-2002-20032003 <0.06<0.06 <0.07<0.07

55<0.15<0.15 <0.30<0.30

OctoberOctober 2.22.2 4.24.2 20.020.0 55.555.5



JanuaryJanuary 7.17.1 15.315.3 53.253.2 87.187.1


MarchMarch 13.013.0 18.318.3 45.845.8 74.074.0

AprilApril 5.85.8 11.111.1 52.452.4 89.989.9

MayMay 3.23.2 6.26.2 31.631.6 71.671.6

JuneJune 0.80.8 1.21.2 9.79.7 58.058.0

2001-2001-20022002

<0.0<0.066

<0.075<0.075 <0.15<0.15 <0.30<0.30

OctoberOctober 2.02.0 4.64.6 23.323.3 54.654.6

NovemberNovember 3.43.4 4.6 4.6 19.119.1 60.660.6


JanuaryJanuary 11.411.4 16.916.9 43.943.9 70.570.5


MarchMarch 15.515.5 24.524.5 68.868.8 90.390.3

AprilApril 1.51.5 4.74.7 27.527.5 77.477.4

MayMay 5.35.3 9.09.0 33.933.9 85.385.3

JuneJune 0.10.1 0.20.2 6.76.7 35.835.8

225 GHz Tipper Opacity. PWV(mm) = tau225 * 19

12M: Specifications12M: Specifications

• Elevation:Elevation: 6,280 ft.6,280 ft.

• Dish:Dish: 12 Meter. f/D = 1.1512 Meter. f/D = 1.15

• Surface:Surface: 72 Adjustable Al. Panels.72 Adjustable Al. Panels.

• Accuracy:Accuracy: 75 75 µm rms.µm rms.

• Pointing:Pointing: < 5” rms on Sky.< 5” rms on Sky.

• Tracking:Tracking: < 1” rms< 1” rms

• Freq Coverage:Freq Coverage:68 – 265 GHz.68 – 265 GHz.

• Observing Window:Observing Window: 24 Hrs/day, 10 24 Hrs/day, 10 Months/year.Months/year.

12 Meter Receivers12 Meter Receivers

• 3 mm SIS Low3 mm SIS Low68 – 90 GHz SSB Dual Polarization.68 – 90 GHz SSB Dual Polarization.

• 3 mm SIS High3 mm SIS High90 - 116 GHz SSB Dual Polarization.90 - 116 GHz SSB Dual Polarization.

• 2 mm SIS2 mm SIS133 - 180 GHz SSB Dual Polarization133 - 180 GHz SSB Dual Polarization

• 1 mm SIS1 mm SIS200 - 265 GHz SSB Dual Polarization200 - 265 GHz SSB Dual Polarization

12 M Backends12 M Backends

• Filters Banks:Filters Banks: (1) 128 x 30 kHz.(1) 128 x 30 kHz. (1) 256 x 100 kHz.(1) 256 x 100 kHz. (1) 256 x 250 kHz.(1) 256 x 250 kHz. (1) 256 x 500 kHz.(1) 256 x 500 kHz. (2) 256 x 1 MHz.(2) 256 x 1 MHz. (2) 256 x 2 MHz.(2) 256 x 2 MHz.

• Millimeter Autocorrelator:Millimeter Autocorrelator: Configurable from 2048 – 32768 Configurable from 2048 – 32768

Channels.Channels. Resolutions from 6.1 to 781.2 kHz per Resolutions from 6.1 to 781.2 kHz per

Channel.Channel.• Digital Continuum Backend:Digital Continuum Backend:

1 - 8 Channels.1 - 8 Channels.

12 Meter Observing Modes12 Meter Observing Modes

• Spectral Line:Spectral Line: Position Switched:Position Switched:

• Relative.Relative.• Absolute.Absolute.

Frequency SwitchedFrequency Switched Beam SwitchedBeam Switched MappingMapping

• Grid Mapping ( PS, APS, FS )Grid Mapping ( PS, APS, FS )• Total Power MappingTotal Power Mapping• On-The-Fly Mapping ( OTF )On-The-Fly Mapping ( OTF )

• ContinuumContinuum Switched or Total Power ON/OFFS ( Sequences )Switched or Total Power ON/OFFS ( Sequences ) Sky TipsSky Tips MappingMapping

• On-The-Fly Mapping ( OTF )On-The-Fly Mapping ( OTF )• Grid MappingGrid Mapping

• VLBIVLBI 2 mm2 mm 1 mm1 mm

ARO, the FutureARO, the Future

New ReceiversNew Receivers

2mm, 1.3mm & 1mm2mm, 1.3mm & 1mmClosed Cycle JT ReceiverClosed Cycle JT Receiver

JT Optics 1.3mm Configuration Shown

Exploded ViewExploded View

345 GHz & 490 GHz345 GHz & 490 GHzDual Polarization SSB Closed Cycle JT ReceiverDual Polarization SSB Closed Cycle JT Receiver

New BackendsNew Backends

2048 Channel 1 MHz Filters Banks

• Fully Software Configurable: (2) Banks of 1024 Channels ( 1 GHz BW ) (4) Banks 0f 512 Channels. ( 512 MHz BW ) (8) Banks of 256 Channels. (256 MHZ BW )

• Self Calibrating.• Auto Failure Detection.• State of the Art Technology.• Surface Mount Devices.• Compact.

New Filterbank Card—32 Channels

IF Processor Card

Forbes Filters, Test SetupForbes Filters, Test Setup

New ComputersNew Computers

• 12 Meter:12 Meter: All Sun Solaris systems scheduled for All Sun Solaris systems scheduled for

replacement, summer 2004.replacement, summer 2004. Fast Dual Processor Xeon Linux Systems.Fast Dual Processor Xeon Linux Systems. Dual Flat-Panel Video Displays.Dual Flat-Panel Video Displays. Observer’s Workstation Already Installed.Observer’s Workstation Already Installed.

• SMT:SMT: Replacing Remaining Sun Workstations Replacing Remaining Sun Workstations

with Additional Fast Linux Machines.with Additional Fast Linux Machines.• Tucson:Tucson:

Replacing Sun Workstations with Fast Replacing Sun Workstations with Fast Linux Machines for Visiting Astronomers.Linux Machines for Visiting Astronomers.

12 Meter, New UPS System12 Meter, New UPS System

•Powerware 9330 UPS

•40 KVA.

•All systems can now be placed on UPS.

• Installation Summer 2004.

Late Breaking ResultsLate Breaking Results

CS J=8->7 391 GHz

IRC+10216

• 390 GHz LO was provided by 390 GHz LO was provided by the Ziurys Lab.the Ziurys Lab.

• 490 GHz Receiver at the 490 GHz Receiver at the SMT.SMT.

• Relatively Unexplored Relatively Unexplored Region.Region.

• Relatively High Atmospheric Relatively High Atmospheric Transmission.Transmission.

• 50% Atmospheric 50% Atmospheric Transmission Achieved for Transmission Achieved for 1mm PWV.1mm PWV.

• Best Accessible High Best Accessible High Transition of CS.Transition of CS.

• 10m Beamwidth of the SMT 10m Beamwidth of the SMT is 19" at 391 GHz.is 19" at 391 GHz.

CS J=8->7 in IRC+10216 391 GHzCS J=8->7 in IRC+10216 391 GHz

New Atmospheric WindowNew Atmospheric Window385-420 GHz385-420 GHz

Highest Transition of CS giving over 50 % atmospheric transmission.

Arizona Radio ObservatoryArizona Radio Observatory

http://aro.as.arizona.edu/

Documents

ALMA Science WorkshopMay 14, 2004 Present and Future Thomas W. Folkers Arizona Radio Observatory