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Smithsonian Astrophysical Observatory
13 February 2012
Lyndele von Schill North American ALMA Science Center (NAASC) Atacama Large MillimeterlSubmillimeter Array (ALMA) National Radio Astronomy Observatory (NRAO) 520 Edgemont Road Charlottesville, V A 22903
Dear Dr. von Schill:
The Smithsonian Astrophysical Observatory (SAO) is pleased to submit the attached Proposal ID # 000000000000405-VIOl for a nine (9) month Fixed Price Research and Development Contract with non-profit organizations in the amount of $1 00,000 for Wide Band Upgrade for ALMA A Study that could commence on 15 March 2012 and continue through 15 December 2012.
The program will be conducted by the Smithsonian Astrophysical Observatory in Cambridge, Massachusetts. The program will be performed under the direction of Dr. C. Edward Tong, as the Principal Investigator, within the Radio and Geoastronomy Division, with Dr. David Wilner as Associate Director of the Division.
Inquiries of a technical nature should be directed to Dr. C. Edward Tong, Mail Stop 42, Smithsonian Astrophysical Observatory, 60 Garden Street, Cambridge, Massachusetts 0213 8-1516, telephone (617) 496-7641, or e-mail [email protected]. Inquiries and documents of a contractual nature should be directed to Mr. Thomas G. Bonnenfant, Contract Specialist, at Mail Stop 23, same address, telephone (617) 495-7317, or e-mail [email protected].
Charles Alcock Director
cm Enclosure
S MITH SO N IA N I NS TIT UTI ON
60 Garden Street Cambridge MA 02138- 151 6
61 7.495.7000 Telephone
PROPOSAL TO
NATIONAL RADIO ASTRONOMY OBSERVATORY
FOR
WIDEBAND UPGRADE FOR ALMA – A STUDY
Proposal ID # 0405-V101
For the Period 15 March 2012 through 15 December 2012
February 2012
SMITHSONIAN ASTROPHYSICAL OBSERVATORY CAMBRIDGE, MASSACHUSETTS 02138
The Smithsonian Astrophysical Observatory is a member of the
Harvard-Smithsonian Center for Astrophysics
NATIONAL RADIO ASTRONOMY OBSERVATORY
FOR
WIDEBAND UPGRADE FOR ALMA - A STUDY
Proposal ID # 0405-VIOl
For the Period 15 March 2012 through 15 December 2012
Funds Requested: $100,000
Principal Investigator Associate Director Dr. C. Edward Tong Radio and Geoastronomy Senior Receiver Engineer Dr. David Wilner
February 2012
SMITHSONIAN ASTROPHYSICAL OBSERVATORY CAMBRIDGE, MASSACHUSETTS 02138
Director: Dr. Charles Alcock
The Smithsonian Astrophysical Observatory is a member ofthe
Harvard-Smithsonian Center for Astrophysics
Call for Proposals
PROPOSAL FORM
Call for Studies of Upgrades of the Atacama Large Millimeterlsubrnillimeter Array (ALMA)
Edward Tong PRINCIPAL INVESTIGATOR: ...................................................................................
Institution Smithsonian Astrophysical Observatory
e-mail [email protected] Telephone 617-496-7667
Address 60 Garden Street, MS 42, Cambridge, MA 02138
* Note: The Study Agreement shall be concluded between the NMSC and the Bidder/Institute.
Call for Proposals - HAASC Proposal Form page 2/4
1. CO-INVESTIGATOR(S)/ASSOCIATED INSTITUTION(S)
Namell nstitution Contact Info - emaillTelephone
Qizhou Zhang [email protected]
Jonathan Weintroub [email protected]
Ming-jye Wang [email protected]
Wei-hao Wang [email protected]
Ming-tang Chen [email protected]
2. SUBCONTRACTORS
The company's authorization to be proposed as subcontractor should be obtained by the Contractor prior to completion and signature of this Proposal Form.
Firms and Addresses: Subcontracted Parts:
Academia Sinica Institute of Astronomy & Astrophysics As per attached Statement (ASIAA) 11 F of Astronomy-Mathematics Bldg. of Work and budget. AS/NTU No.1, Roosevelt Rd. Sec. 4
Taipei, 10617, Taiwan, R.O.C.
Call for Proposals - NAASC Proposal Form page 3/4
3. EFFORT AND COST BREAKDOWN The Bidder shall estimate the effort (in Full Time Equivalent - FTE) to be deployed by Bidder and Associates/Subcontractors (items 4.1 through 4.5) until completion of the Study. as well as the corresponding total costs to be incurred by the Bidder (items 4.6 through 4.9).
Also, the Bidder shall indicate the level of financial support expected from ALMAINA (item 4.10). if any. consistent with item 4 of Annex 1.
Item Description Estimate and breakdown of Effort in FTE
4.1 Science 0 (0.5*) 4.2 Management 0 (O) 4.3 Engineering 0.05 (2*) 4.4 Others 0 (O)
Total FTE (items 4.1 to 4.4) 0.05 (2.5*)....
litem Description Estimated Cost in USD
4.6 FTE $11,336 4.7 Travels $13,500 4.8 Other Costs $75,164 4.9 Total cost (items 4.6 to 4.8) $100,000
4.10 Firm fixed price in USD to be paid by ALMAINA for the Study
$100,000
Call for Proposals - HAASe Proposal Form
4. DELIVERY SCHEDULE AND TERMS OF PAYMENT
page 4/4
The Bidder shall fill in the time allocated for completion of Milestone 1 and 2 (Items 5.2and 5.3) and shaH propose a payment plan according to the defined Milestones.
Time for completion of Milestone 2 (Item 5.3) shall not exceed 12 months from kickoff.Payment related to this milestone Is conditional on the acceptance of the Study byALMAINA.
Item
5.1
5.2
5.3
Milestone
Milestone 0: K1ck-off Meeting
Milestone 1: end of PHASE 1(= final definition of instrument conceptrequirements)
Milestone 2: end of PHASE 2(= Delivery of Final Study Report)
Time ofCompletion
To
To + .,. months
To + 9 months
PaymentAmount In USD
$33,333.33$33,333.33
$33,333.34
5.4 TOTAL FIRM AXED PRICE $100,000
5. COMMITMENTHaving read all documents listed in and annexed to the call for Proposals and havingassessed the situation and the nature and difficulties of the services, the undersignedhereby offers the "Study for Upgrades of the Atacama LargeMiIIlmeterisubmllUmet8r Array (ALMA)" in accordance with the provisions of thepresent Call for Proposals and, if awarded the Agreement, undertakes to cany out thework required according to first class trade practice, within the prescribed time limits. andat the prices set out in the Proposal Form.
Date, ~/t3P(Jf'" , .LSgnaW'" ~JI:5~V-
Thomas G. BonnenfantContracting Officer
N.B Any correction. deletion or other form of alteration herein must be initialed.
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Wideband Upgrade for ALMA - a Study !
Abstract We propose to conduct a comprehensive study to increase the IF bandwidth of the ALMA 2SB receivers from the current 2 x 4 - 8 GHz to 2 x 4 -14 GHz. This upgrade is a cost effective way to improve the capability of ALMA. Taking advantage of the current wideband upgrade work for the SMA, we plan to perform laboratory demonstration of a 2SB receiver operating between 210 and 275 GHz (Band 6) with a 10 GHz wide IF. Our study will also include a detailed science case for this wideband upgrade which will impact all receiver bands, as well as architecture designs for a digital system to handle the increased data bandwidth. The proposed work will be performed jointly by SAO and ASIAA.
1. Introduction
ALMA is the largest and most powerful millimeter/submillimeter wave interferometer ever built, and it incorporates a wide range of state-of-the-art technologies. As technology advances, it will be essential for ALMA to take advantage of developments that can cost-effectively enhance its scientific productivity. In the intermediate term, we believe that increasing the instantaneous bandwidth of the ALMA receiving systems is a significant and compelling upgrade for ALMA. Here we propose a comprehensive study of a wideband upgrade for ALMA, encompassing the areas of science, receiver front-end technology and fast digital backend (DBE) architecture. ALMA is made possible by large capital investments in antennas, electronics and other infrastructure. A wideband upgrade represents a cost effective approach to build on this existing investment to further enhance the scientific return of ALMA.
The Smithsonian Astrophysical Observatory (SAO) and the Academia Sinica Institute of Astronomy and Astrophysics (ASIAA), partners in the SMA, will jointly conduct the proposed study. We plan to leverage the work being done on the Submillimeter Array (SMA) to complete the proposed study of a wideband upgrade for ALMA. The SMA is currently embarking on a plan to upgrade its receivers to increase its Intermediate Frequency (IF) bandwidth to 18 GHz. The upgraded SMA will offer instantaneous sky coverage of up to 72 GHz, opening up a range of new science opportunities. This upgrade is timely because it takes advantage of recent developments in front-end and fast digital electronics. Many of the technologies that we are developing for the SMA bandwidth upgrade are applicable to the proposed ALMA upgrade.
This proposal includes several components: one is to demonstrate a sideband separating (2SB) SIS receiver operating over an IF band of 4-14 GHz for Band 6, a two and a half fold improvement over the current 4-8 GHz 2SB operation in ALMA. The challenge of handling the 4 x 10 GHz bandwidth (dual polarization and 2 SB) will be addressed by a study of possible fast digital backend architectures. In addition, we will complete a study of the various science goals that can be achieved with this wider IF bandwidth. Finally, we will organize a workshop, open to all interested scientists and technologists, to discuss new scientific opportunities and technological developments which would drive this proposed wideband upgrade.
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2. Science
With orders of magnitude improvement in sensitivity over current millimeter interferometers, ALMA enables transformational research in a wide range of scientific themes from nearby solar system bodies to distant dusty galaxies. While these promises are being realized as ALMA transitions into its operational phase, the 2.5 fold increase in bandwidth proposed here will further enhance ALMA's science capability by increasing the efficiency of spectral line observations and by improving the continuum sensitivity by a factor of ~1.6.
Millimeter and sub-millimeter wavebands are filled with molecular lines that trace the physical properties and chemical make-up of the interstellar medium. A wideband receiving system enables simultaneous coverage of multiple spectral lines in one observing session. While such a system benefits all ALMA bands, here we base our discussion on Band 6 (210 – 275 GHz). We propose to demonstrate 2SB receiver operation covering 4 – 14 GHz IF, covering the entire Band 6 in just 4 LO tunings.
Below, we discuss in more detail several science examples enabled by a wide band system which offers higher continuum sensitivity and which also enables simultaneous observation of many molecular species.
a. Star Formation A wideband receiver for Band 6 can cover the J=2-1 transitions of 12CO, 13CO, and C18O, the
SiO J=5-4 transition, H2CO (3-2) transition, the CH3CN J=12-11 ladder, the N2D+ (2-1) transition and the H30! line. In studies of molecular clouds and star formation, the low-density tracers, 12CO and SiO, reveal bipolar outflows launched from the accretion disks of newly formed protostars. The H2CO (3-2) transition, excited at high gas densities, probes the gravitationally driven inflows through the dense core toward the accretion disk of the protostellar envelope. The CH3CN ladders, with energy levels from 70 K to several 100 K, reveal the heated surface of the accretion disk itself, while deuteriated species such as N2D+ are most abundant in the interior of the cold disk. The H30! line traces the ionized gas in the innermost disk and outflow. A wideband receiver will capture, in one frequency tuning, gravitational collapse, protostellar accretion and outflow as well as ionization, the most important steps involved in star formation. This underscores the power of receivers with very wide IF bandwidth.
b. Formation and evolution of galaxies
The ALMA Band 6 is important for studying redshifted transitions from distant galaxies: CO(3-2) at z ~ 0.5, CO(4-3) at z ~ 1, as well as the CI line (z ~ 1.1) and the CII line (z ~ 7). The fractional frequency coverage, "#/#, after the proposed upgrade, will be comparable to that for Band 3. The upgraded 10 GHz coverage translates into "z/(1+z) ~ 0.04. The increased bandwidth enables targeting the CO lines in galaxies with only photometric redshifts as provided by recent deep optical surveys which gives "z/(1+z) < 0.02 for galaxies at z < 2. Clearly, this will greatly improve the observing efficiency and detection rates for high-redshift galaxies.
With the improved sensitivity from the increased bandwidth, the upgraded Band 6 receiver will be able to perform continuum surveys at the same speed as the current Band 7 receiver. Based on the faint-end 850 µm counts (Chen et al. 2011) and $ = 1.5, we forecast that the full ALMA with a wideband Band 6 receiver can blindly detect one dusty galaxy ( > 0.12 mJy at 5 %) in just 7 minutes of integration in a random pointing. Therefore, the proposed upgrade will
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Figure 2. Image of the LkCa15 disk showing a hole towards the center, which might have been cleared by a newly formed planet. (Images from Sean Andrews, SMA staff). !
significantly enhance ALMA's capability as a survey machine and as a ``z-machine'' for determining redshifts from molecular and fine structure lines.
The proposed 4-14 GHz IF coverage will also benefit the study of local galaxies. It will enable simultaneous observations of 12CO, 13CO, and C18O in the J = 2-1 transitions (see Figure 1), a combination not possible with the current Band 6 receiver. The upgrade will make the 1 mm continuum as easily accessible as the bright CO(2-1) line. Since the 1 mm continuum from dust in external galaxies is optically thin, this will provide a way to estimate the mass of the interstellar medium independent of the uncertain 12CO/H2 conversion calculation. The ratio of the 1 mm continuum to optically thin lines, such as 13CO(2-1) and C18O(2-1), also provides clues to the spatial variation of the gas-to-dust ratio and dust properties.
c. Planet-forming disks around other suns
Recent discoveries of several hundred exoplanets have brought great interest in the evolution of solar systems similar to our own. In the evolutionary time period leading up to planet formation, the residual gas and dust left over from star formation is in a disk-like orbit around a newly formed star. A characteristic temperature of these disks is that the brightness of the dust emission rises sharply through the submillimeter. This makes the submillimeter an ideal waveband to study extra-solar systems. In addition, the 1 mm window contains many of the brightest submillimeter molecular lines observed in disks.
Fig. 2 shows a hole in dust continuum emission towards the center of the disk around the star LkCal5 observed with the SMA. Possibly created by a newly formed but unseen planet, the hole is estimated to be 50 AU in diameter, about half the size of our solar system. ALMA will expand beyond the reach of the SMA to
Figure. 1: Spectral line survey of Arp 220 in the 1mm band obtained with the SMA (Martin et al. 2011). The grey vertical bars mark the identified lines. The two thick horizontal bars denote the spectral coverage of the proposed wide band receiving system.
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fainter and more distant systems, enabling us to better estimate the frequency and character of planet forming systems and determine whether solar systems such as ours with Earth-like planets are common.
While the dust continuum reveals the structure of the protoplanetary disk, molecular line emission reveals its composition. Targeted observations of individual lines or small sets of lines have advanced our understanding of molecular distributions in disks and tested aspects of existing disk chemistry models (Dutrey et al. 1997; Thi et al. 2004; Oberg et al. 2010, 2011). These include molecular lines and line pairs that probe e.g. deuteration (DCN/HCN and DCO+/HCO+), the shape and strength of the UV field (CN/HCN), fractional ionization (HCO+, N2D+ and H2D+) and evidence for grain surface chemistry (H2CO). The higher sensitivity of ALMA is bound to rapidly increase the number of the detected molecules and our overall understanding of the chemistry in planet forming disks. However, as long as the bandwidth remains small, the observations will by necessity continue to target only specific lines. Such targeted observations have inherent limitations: they do not leave much room for discoveries of new probes of disk processes, nor do they provide an unbiased view of the disk chemistry. Increasing the bandwidth to the proposed 2 x 10 GHz would enable observations of the entire 1 mm window in a just a few settings, making blind surveys almost 3 times more efficient and thus promoting a complete view of disk chemistry in statistically significant samples.
The larger bandwidth together with a flexible correlator would also make targeted observations substantially more flexible, enabling the simultaneous observation of tracers of disk ionization, UV irradiation and prebiotic chemistry at higher spectral resolution than may be possible or desired for blind line surveys.
d. Comets and solar system bodies Comets are messengers from the past bringing with them the original, primordial material that
formed our solar system. However on multiple passes through the solar system, these crossing comets may develop an evolved surface crust. The most pristine material in the centers of the comets is visible in a chance break-up of a crossing comet (Dello Russo et al. 2007) or in jets outgassing from the interior through cracks in a comet's surface. High-angular-resolution interferometry is capable of imaging and isolating the jet emission within the larger coma that is dominated by outgassing from the crust (Boissier et al. 2010).
The simultaneous coverage of the proposed ALMA Band 6 upgrade is advantageous in that it will allow a comparison of the CO, H2CO and CH3OH lines in the bandwidth before the asymmetric jet emission changes on the timescale of the rotation period of a comet, typically about 10 hours (Henry et al 2002).
These observations seek to derive a chemical inventory of the pristine material from the emission in the millimeter and other wave bands such as the near-IR. One addressable question concerns the origin of the comets. A working model posits two comet families: the first, the long period comets, formed in the giant planet zone and scattered into the Oort cloud by gravitational interactions, and the second, the short period or ecliptic comets, formed further out in the Kuiper belt region. So far, spectroscopy has not yielded a clear chemical distinction between the two. It is not known whether this results from a confusion of evolved with pristine material; whether there was little chemical differentiation in the early solar system, or whether this supports an alternative model. For example, it is possible that all the comets formed in the same region and
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were scattered during a period of instability in the solar system when the orbits of Jupiter and Saturn evolved through a 2:1 resonance (Gomes et al. 2005). A wider band receiver will facilitate a better understanding of the formation of comets.
3. Wideband Receiver Front-end The Superconductor-Insulator-Superconductor (SIS) mixer with quantum-limited sensitivity is
at the heart of all current ALMA receiver bands. ALMA has advanced this technology in both frequency coverage and sensitivity. However, another frontier lies in the IF bandwidth of the SIS mixer. While the current maximum operating IF of ALMA is 12 GHz, the SIS mixer has the potential to operate at even higher IF (Pan and Kerr 1996).
In order to increase the IF bandwidth, the capacitance of the SIS mixer has to be reduced. One successful approach is to use a series-connected distributed SIS mixer, first demonstrated by Tong et al (2005). In this design, the junctions act as low impedance matching elements giving a theoretical IF bandwidth of ~ 30 GHz, A prototype mixer (see Figure 3a) was fabricated at the Jet Propulsion Laboratory using small area high current density junctions. Good conversion efficiency was measured at SAO up to an IF of 20 GHz, the limit of the measurement setup.
We have recently introduced a 3-junction array design (see Fig. 3b) which uses larger lower current density junctions that are easier to fabricate. A mixer of this design for the SMA 220 GHz receiver has been fabricated by ASIAA. Receivers incorporating these mixer chips have been tested in the lab at SAO and deployed at the SMA in Hawaii. In this receiver setup, we employ a 4 – 14 GHz cryogenic isolator, an advanced version of the isolators used in ALMA Bands 9 and 10, followed by a CITCRYO1-12 amplifier, the same amplifier used in Band 10 receivers. Referring to Figure 4a, the measured double-side-band (DSB) noise temperature of one of these receivers are comparable to existing ALMA Band 6 receivers up to 12 GHz. The rise in noise temperature above 12 GHz is due to the limited IF bandwidth (~15 GHz) of this design, coupled with the higher noise temperature of the IF system above 12 GHz. A new batch of mixers with a modified design, which extends the IF bandwidth to > 18 GHz, has recently been produced at ASIAA. Referring to Fig. 4b, preliminary data from this batch demonstrates that an IF bandwidth of 4 – 14 GHz is readily achievable.
Three of the wideband 220 GHz receivers are now in routine operation at the SMA. Validation of these new receivers on the telescope has been performed by test observations towards Orion BN/KL. Referring to Figure 5, the black spectra show the standard SMA 4 – 6 GHz IF band; the additional higher spectral regions shown in red, green and blue were obtained
Figure 3: (a) left - 4-junction array fabricated at JPL in 2005. Array of 1 µm2 junctions at 13 kA/cm2. (b) right - 3-junction array fabricated at ASIAA in 2011. Array of 2 µm2 junctions at 7 kA/cm2
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sequentially by mapping the higher IF into the standard IF band, demonstrating the effectiveness of a wideband system.
Although the SMA is built as a DSB system using phase switching to separate the two
sidebands in the digital correlator, we plan to leverage our expertise in wideband receivers to develop wideband 2SB receivers for ALMA. This development involves a slight scaling of the new SMA 220 GHz wideband mixer mentioned above and integration of two of these mixers with a waveguide LO/signal combination block. The challenge of such a system lies in correctly phasing the IF outputs from the two mixers over the wide IF. Ultra-broadband quadrature hybrids are available commercially but their correct operation requires well-matched ports. Since the typical output impedance of an SIS mixer is normally quite different from 50-ohm and varies with the IF, we plan to use a wideband isolator following the SIS mixer. We have a number of 4 – 14 GHz isolators from Quinstar. There is also an in-house development effort at SAO, which has produced preliminary designs for wideband isolators, which could cover 4 – 14 GHz.
!!!!!!!!!!! !!!!!!!!! !Figure 4: Measured DSB receiver noise temperature as a function of IF for 220 GHz mixer chip fabricated at ASIAA. (a) Result from batch #1 (left plot). Low noise performance is achieved for signal frequencies of 194-254 GHz. (b) Preliminary result from batch #2 with even wider band design (right plot). IF bandwidth of mixer is clearly up to at least 14 GHz.
Figure 5: Upper- and lower- sideband spectra taken towards Orion BN/KL with a single LO setting using the wide-band receivers recently installed into SMA antennas 1 and 5. Note that the 2 sidebands are obtained simultaneously because of the DSB mode of operation of SMA receivers. The red, green and blue spectral regions are obtained sequentially with the wideband mixer.
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Wideband cryogenic amplifiers offering low noise over 4 – 14 GHz are also available at both SAO and ASIAA. Selected units of the CITCRYO1-12 amplifiers used in the new wideband SMA receivers have noise temperature of below 10 K up to 14 GHz. We will also work with Dr. Sander Weinreb of Caltech who is developing newer MMIC chips, which may offer better noise over this frequency range. SAO also has two low noise amplifiers on loan from NRAO (courtesy of Marion Popieszalski) with low noise performance over the target IF band.
By extrapolating the performance of the laboratory results achieved so far, we believe that we will be able to build, as part of our study, a laboratory prototype 2SB receiver (single polarization) over the frequency range of 210 – 275 GHz, with SSB noise temperature competitive to existing ALMA receivers but over an IF band extending from 4 to 14 GHz. The expected sideband separation ratio is in excess of 10 dB.
4. Wideband Digital Backend (DBE)
We will examine the possibility of adapting the wideband digital technology employed in the SMA’s wideband upgrade to ALMA. From a standpoint of the digital backend (DBE) ALMA differs from the SMA in that the IF is digitized in each of its 66 antennas. At ALMA, with the dual polarized receivers, a total bandwidth of 2 x 8 GHz is sampled and transmitted to the correlator.
At the time when ALMA was designed, analog-to-digital converters (ADC) capable of digitizing the 4 to 12 GHz IF in one block were not available. The ALMA IF is broken up into 2 GHz wide blocks and digitized at a rate of 4 GSample/s with a 3-bit ADC. Thus each ADC subsystem produces a payload of 12 Gb/s summing to 96 Gbit/s for each antenna. ALMA’s digital transmission system (DTS) is implemented with a "virtual parallel bus" using twelve 10Gbit/s links.
A faster ADC is clearly needed for the proposed ALMA upgrade to process a total of 4 x 10 GHz. In investigating ways to increase the processed bandwidth of the SMA, we have found that ADCs with rates of 20GSample/s, and wide band analog inputs have emerged in the marketplace. A 20 GSample/s ADC can accommodate a 10 GHz wide IF. The aggregate data rate assuming the same three bits of quantization would be 240 Gbit/s. Fiber networking running at 10 Gbit/s is now available off the shelf, and the standard is moving to 40 Gbit/s. The next crucial feasibility study is to focus on what networking protocols are appropriate to use on the existing fiber connections to the 66 ALMA antennas. We believe that the experience at the SMA harnessing the latest ADC technology to improve the ADC subsystem will be very useful to ALMA.
Finally the fibers carrying data from each ALMA antenna will feed a new digital back end. Our initial studies for the SMA have suggested that FX correlator architectures are superior to XF for wideband and high spectral resolution applications. Certainly the design of a 66 antenna DBE with 20 GHz bandwidth per polarization and capable of correlating all Stokes parameters is non-trivial, and production will be more costly. The proposed feasibility study will encompass the budget, scale and power consumption of an FPGA packetized correlator. Our current work on the SMA upgrade will be helpful in this regard as we are establishing a good understanding of the resource utilization of the station logic in the context of a small (8 antenna) array (Primiani et al. 2011). In a correlator for ALMA, with over 2000 baselines, we would need to extend this study to the regime of large number of antennas. The scale of the corner-turn - the operation
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whereby the station data is paired into baselines - may become the limiting factor in such a system. We would also study the implementation of a correlator in which higher spectral resolution is available with no loss in the uniform resolution across the entire IF band.
5. Significance of the Study to ALMA
There are a number of ways to improve the system performance of a radio interferometer. For example, one can add more antennas, introduce new frequency bands, improve the sensitivity of the receivers, or as we propose here increase the bandwidth of the instrumentation. Adding new antennas requires new capital investment and the number of antennas to be added has to be large to make significant impact. The 1.6 times increase in continuum sensitivity obtained from the proposed wideband upgrade is actually equivalent to the gain in continuum sensitivity from the addition of 30 antennas but at much lower cost. On the receiver side, since the ALMA SIS receivers are approaching quantum-limited sensitivity, any further improvement would be incremental.
The proposed increase in IF bandwidth differs from the introduction of new receiver bands in that it has a global impact on all the ALMA SIS receiver bands. This proposal is also rooted in the direction of advances in technology. While microwave ultra-wideband technology is gaining more attention, advances in fast digital technology in the past few years have been spectacular. Not only are ADCs with tens of GHz of bandwidth now available, the capability of processing the large bandwidth from these ultra fast ADCs has been made possible with newer generations of FPGA. It is expected that the cost of building fast digital hardware will further drop in time. The current fiber link between the individual ALMA antennas and the central processing station can easily be reconfigured to accommodate the higher data rate with modest investment only.
Multi-beam interferometry may be the ultimate upgrade of ALMA. We consider that an upgrade of the IF bandwidth is an intermediate step towards this final goal. An effective means of handling the extremely large data rate must be developed before a multi-beam system can be implemented. The exercise of increasing the IF bandwidth will help ALMA to move towards this goal in the more distant future.
6. Management Plan
The PI Edward Tong has 20 years of experience in developing and commissioning SIS receivers, and will bring his expertise of wideband receiver design. He will be working closely with Ming-jye Wang, director of the SIS fabrication facility at ASIAA, who will oversee the fabrication of the wideband mixer chips. Qizhou Zhang (SAO) and Wei-hao Wang (ASIAA), both key scientists for the SMA, will be at the forefront of further developing new scientific possibilities enabled by wideband observations. Jonathan Weintroub (SAO), who is a leader of the wideband digital upgrade for SMA, will be instrumental in formulating plans for future wideband digital systems in the context of a fast moving digital electronics world. Finally, Ming-tang Chen (ASIAA), who is a key player in various ALMA subsystems for both ALMA-NA and ALMA-EA, will be the coordinator of activities between SAO and ASIAA, and at the same time brings the realities of ALMA operation to our team.
In addition to the co-investigators mentioned above, a large number of scientists and engineering staff for the SMA, from both SAO and ASIAA, will make contributions to this proposal. Their participation in the ongoing SMA wideband upgrade will intersect with the
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proposed study. A partial list of the people involved is: Ray Blundell, Paul Grimes, Eric Keto, Rurik Primiani, Charlie Qi and Robert Wilson from SAO, as well as Derek Kubo, Chao-te Li and Chih-chiang Han from ASIAA.
The proposed start date of the study is March 15, 2012 and the end date is December 15, 2012. The details of each of the 3 main components of the proposal are discussed below. The deliverables of the study will be summarized at the end of each sub-section.
a. Science The SMA is on an upgrade path to achieve up to 72 GHz of instantaneous sky coverage. In
order to support this upgrade, the SMA science team is actively developing new science programs and new observation strategies, to take advantage of this wideband operation. We believe that the work done at the SMA would be useful as pathfinder for wideband instrumentation for ALMA.
We plan to organize a wideband instrumentation workshop in the fall of 2012 at SAO. A big part of the workshop will focus on new science enabled by wideband instrumentation at both the SMA and at ALMA. The workshop will be open to the community at large, and constitute a major push of wideband instrumentation for submillimeter radio interferometers. The science part of the deliverable will be a detailed report on future scientific output of a wideband ALMA based on this workshop.
b. Front-end Demonstration The SMA will have a full complement of 220 GHz receivers with extended IF coverage by
the end of 2012. Although the input bandwidth of these receivers (190 – 250 GHz) is somewhat different to the proposed demonstration band of 210 – 275 GHz, we plan to scale the SMA mixer by 10% to be compatible with ALMA Band 6 operation. The scaled mixer will achieve even higher IF bandwidth because the output capacitance of the mixer chip would be reduced by 10%.
A preliminary model of a 2SB mixer block for ALMA incorporating two scaled SMA mixers has been developed. We plan to work with Thomas Keating Company (UK) to have the blocks made by high-speed milling. The estimated delivery time for block, including the corrugated feed horn, is about 3 months, which is also typical of the time needed for a few SIS junction fabrication runs. From previous experience at ASIAA in wideband SIS mixer fabrication, the target current density of ~7 kA/cm2 for a 3-junction array of 1.6 µm diameter SIS junctions is well within the capability of the facility at ASIAA. For these designs, relatively high yield in addition to excellent junction quality factor ( > 20) is routinely achieved. The risk in this part of the project is minimal.
Two mixer assemblies will be made to allow for parallel testing at both SAO and ASIAA. Since other components are already available at both institutes, we expect a comprehensive laboratory measurement of a complete 2SB mixer to take place in the fall of 2012. The performance of our prototype receiver will be compared to ALMA Band 6 receivers. A detailed report of this hardware demonstration will be part of the deliverable.
c. Digital Backend Architecture The development of a wideband DBE for the SMA is currently an active project. We are
already designing a pathfinder instrument using a commercial 5 GSample/s 8-bit ADC, which is faster than the present ALMA ADC and has more dynamic range. We are investigating 20
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GSample/s parts from a number of manufacturers. We also understand the utilization requirements to build a wideband correlator using CASPER technology. At the SMA, the link between the antenna and the control building link is analog, however we are gaining experience in high speed networking technologies for the packetized correlator, which could be generalized to an upgrade to the ALMA DTS.
All of these investigations form the groundwork for our study of the application of these technologies to an ALMA upgrade. We will develop these ideas during the planned wideband ALMA workshop associated with this project as well as the CASPER workshop to be held in Green Bank. With the benefit of collegial input at the workshops, the deliverable will be a report on how our ideas for upgrading SMA’s digital signal processing may be applied as an upgrade to the ALMA digital back end.
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PROPOSAL BUDGET WORKSHEETS SUMMARY
Business Unit: Proposal 10: Version 10:
Period of Performance: 15-MAR-2012 through 15-DEC-2012 51400
000000000000405 V101
15-MAR-2012 thru 15-DEC-2012
Productive Labor AVG Rate Hours Dollars Total Hours Total Dollars
Travel Outside the USA Travel - Training/Conf in USA
Engineering Services
SAO Materials Burden @Rate 4.9%
SAO General &Administrative
SAO General &Administrative @Rate 13%
31X Equipment - taggable Greater Than Equal 5K Materials
Subcontracts
Material Base
TOTAL (Not including Management Fee)
Management Fee
TOTAL ESTIMATED COST
$11,140 $2,360
$11,336
$3,205
$28,041
$3,645
$10,000 $5,401
$50,000
$65,401
$97,087
$2,913
$100,000
$11,140 $2,360
$11,336
$3,205
$28,041
$3,645
$10,000 $5,401
$50,000
$65,401
$97,087
$2,913
$100,000
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TRAVEL SCHEDULE
Bud!!!!! Period: 1 15-MAR·2012 Thru 15-0EC:2012
Destination Purpose # Trips # Travellers OayslTrip Per Diem Total Per Diem Airfare Total Airfanl AuloRaIe Total Aulo Milc. Total
Taipei, Taiwan Meeting with collaborator. 1.00 2.00 5.00 $294 $2,940 $3,700 $7,400 $0 $0 $800 $11,140 Green aank WVA CASPER Workshop 1.00 1.00 7.00 $123 $861 $350 $350 $350 $350 $799 .$2,360
TOTAL TRAVEL for Budget F ____
ENGINEERING SERVICES SCHEDULE
Budget Period: 1 1S-MAR-2012 Thru 1S-DEC-2012
COST BASIS DESCRIPTION VENDOR COST
Quote CE Services of Edward Tong Edward Tong $11,336
TOTAL ENGINEERING SERVICES for Budget Peri
MATERIALS SCHEDULE
Budget Period: 1 15·MAR·2012 Thru 15·DEC·2012
COST BASIS DESCRIPTION VENDOR COST
Estimate Liquid Helium - 200 liters Linde Gas LLC $1,600 Estimate Misc. electronics parts Various $3,801
TOTAL MATERIALS for Budget Period: 1 n;<ID'f
13
Budget for ASIAA Sub-award
CATEGORY ITEM Unit Cost Quantity TOTAL COMMENT
Misc & Materials Mask, 2 sets, 4 each $1,100 8 $8,800 Misc & Materials 2" crystal quartz substrate, 1 per run $100 10 $1,000 Misc & Materials Liquid Hilium, in liters $17 200 $3,400 Operation Cost 10 runs, 4 days per run $120 40 $4,800 based on 250 days, 30K per year Manpower 10 runs, 10 man-days per run $200 10 $2,000 based on 250 days, 50K per year Manpower Lab testing, 21.33 man-day $150 21.33 $3,200 based on 250 days, 50K per year Misc & Materials Mixer block $10,000 1 $10,000 Quotation from Thomas Keating Travel Collaboration meeting in SAO for two $3,300 2 $6,600 5-day trip, ticket, accomodation and per diem. Travel Project workshop in SAO $3,400 3 $10,200 5-day trip, ticket, accomodation and per diem. in US$ Subtotal $50,000
EQUIPMENT Equal To or Greater Than 5K SCHEDULE
Budget Period: 1 1S-MAR-2012 Thru 1S-DEC-2012
COST BASIS DESCRIPTION VENDOR COST
Quote Mixer Block Thomas Keating L TO. $10,000
TOTAL EQUIPMENT Greater Than Equal to Sk for $10,000
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Budget Justification
Although the PI of the proposed study is from SAO, SAO and ASIAA are partners in equal footing in this work. A sub-award of $50,000 covers the cost of the ASIAA portion of the project, the budget of which is listed separately.
The PI, Edward Tong, is devoting approximately 80 hours of his time to this project. This cost is reflected under the engineering services section of the budget. For the estimate of effort in FTE on the NRAO proposal form, 2 numbers are provided. The numbers on the left represent the amount of FTE that SAO is charging to the proposal. The number on the right (in parenthesis) represents the global effort that we project to put in within the 9 months of the proposed study. This includes SAO’s own effort of wideband upgrade for the SMA that intersects with this proposal, in addition to the manpower needed in the ASIAA sub-award. Other federal scientists contributing to the proposal, including co-I Qizhou Zhang and Jonathan Weintroub, in addition to many SMA staff members, are also available to the study at no cost to ALMA.
A mixer block is needed for the hardware demonstration part of the study. Thomas Keating Company, who manufactured some of the SMA mixer blocks, has provided a quotation for the mixer block. This vendor is familiar with our requirements and given the short duration of the study, timely delivery of this key hardware is essential. The quoted price of $10,000 is in line with the cost of SMA mixer blocks. Other hardware related costs include liquid helium and the purchase of miscellaneous electronics supplies.
Travel to Taipei is required for Edward Tong and Qizhou Zhang to collaborate with ASIAA subcontractors (estimated travel cost of $11,140). Funds will also be used to support Jonathan Weintroub’s attendance at the CASPER workshop to be held in Green Bank, WVA (estimated travel cost of $2,360 for seven days). This is an important event for fast digital backend development in the astronomical community, in direct relation to the work proposed here.
ASIAA has a separate budget for the sub-award. The items include the cost of SIS mixer chip fabrication and testing; the purchase of one copy of the mixer block for testing in Taipei; and funds for travel to attend collaboration meetings and the study workshop to be held in Cambridge, MA.
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CONTRACTUAL AND COST INFORMATION INCLUDING CERTIFICATIONS
The Smithsonian Institution, an independent trust establishment was created by an act of the Congress of 1846 to carry out the terms of the will of James Smithson of England, who had bequeathed his entire estate to the United States of America "to found at Washington, under the name of the Smithsonian Institution, an establishment for the increase and diffusion of knowledge." After accepting the trust property for the United States, Congress vested responsibility for administering the trust in a Smithsonian Board of Regents. The Smithsonian performs research, educational and other special projects supported by grants and contracts awarded under the cost principles of Title 2 of the Code of Federal Regulations (CFR) Part 230 [formerly the Office of Management and Budget (OMB) Circular A-122: Cost Principles for Non-Profit Organizations] and the Federal Acquisition Regulation, Subpart 31.7 Contracts with Nonprofit Organizations. It is audited by the Defense Contract Audit Agency, Landover, Maryland. The Charter of the Smithsonian Institution carries a mandate for the "increase and diffusion of knowledge.” Therefore, any grant or contract that may be awarded as a result of this proposal must be unclassified, in order not to abridge the Institution's right to publish, without restriction, findings that result from this research project. Considering the nature of the proposed effort, it is requested that a Fixed Price (Best Effort) Research and Development Contract with reimbursement via electronic funds transfer be awarded to cover the proposed project in accordance with Subpart C, Section 215.22(e) of Title 2 CFR Part 215 [formerly OMB Circular A-110: Uniform Administrative Requirements for Grants and Agreements with Institutions of Higher Education, Hospitals and Other Non-Profit Organizations]. Pursuant to Subpart C, Section 215.33 and 215.34 of Title 2 CFR Part 215 [formerly OMB Circular A-110], it is requested that title to all exempt property and equipment purchased or fabricated under the proposed contract be vested irrevocably in the Institution upon acquisition. In accordance with an agreement between the Office of Naval Research and the Smithsonian, the Institution operates with predetermined fixed overhead rates with carry-forward provisions. The Indirect Cost and Fringe Benefits Rates are developed in accordance with Title 2 CFR Part 230 [formerly OMB Circular A-122]. The following approved rates, provided by ONR Negotiation Agreement dated 17 August 2011, shall be used for forward pricing and billing purposes for Fiscal Year 2011. The Fringe Benefits Rate will be applied to the Total Direct Labor Costs. The Material Overhead Rate will be applied to the cost of materials, equipment and subcontracts. The Direct Operating Overhead Rate will be applied to the Direct Labor and Benefits costs. The G&A Rate will be applied to the base consisting of total costs except the costs associated with the materials, equipment and subcontracts.
The following Approved Rates shall be used for forward pricing and billing purposes for Fiscal Year 2011: Material Burden Rate 4.9% (Cost of Materials, equipment and subcontracts) Personnel Leave Rate 19.3% (Total Direct Labor Costs less paid leave and training {Productive Labor}) Fringe Benefits Rate (Full/Part Time Employees) 26.8% (Total Direct Labor Costs) Fringe Benefits Rate (Intermittent Employees) 8.4%
(Total Direct Labor Costs)
Direct Operating Overhead Rate 26.7% (Total Direct Labor and Fringe Benefits Costs) General and Administrative Rate (G&A) 13.0% (Base consists of Direct Operating Activities less Net Costs Associated with materials, subcontracts and equipment) Central Engineering Overhead Rate 24.6% (Central Engineering Direct Labor and Benefits Costs)
Rate verification can be made by contacting Ms. Linda Shipp, Office of Naval Research, Indirect Costs/ONR 242, 800 N. Quincy Street, Room 704, Arlington, Virginia 22217, telephone (703) 696-8559, or e-mail [email protected]. Engineering services are provided by the Central Engineering Department as a Cost Center. Charges by the department to research projects are inclusive of Direct Labor, Fringe Benefits, and Central Engineering Overhead. In order to achieve full cost recovery on contract and grant work efforts, the Smithsonian Astrophysical Observatory [SAO] applies a 3.0% Management Fee to the total estimated direct and indirect costs of its projects. This calculated fixed-fee provides support to SAO for current and future investments in research, for investments in infrastructure and intellectual capital, for the risk assumed in performing requested work, and to cover ordinary and necessary business expenses that are nonreimbursable as a direct or indirect cost under the award. The requested fee will help SAO to quickly address future opportunities and needs, with expert staff, state-of-the-art analytical instruments, and special use equipment. It should be noted that SAO does not receive Facilities Capital Cost of Money. In general, Management Fee will be invoiced incrementally throughout the period-of-performance, based on expenses incurred, with the remainder of the fixed-fee collected at the completion of the award.
CERTIFICATIONS
Pursuant to FAR 52.204-8, ANNUAL REPRESENTATIONS AND CERTIFICATIONS (MAY 2011), for federally funded awards, the Smithsonian Astrophysical Observatory (SAO) is registered with the Online Representations and Certifications Application (ORCA). ORCA can be viewed at http://orca.bpn.gov, using SAO DUNS # 003261823.
Citations J. Boissier, D. Bockelée-Morvan, A.V. Rodionov, and J.F. Crifo, “First attempt atinterpreting millimetric observations of CO in comet C/1995 01 (Hale-Bopp) using 3D+thydrodynamical coma simulations,” Astronomy & Astrophysics, vol. 510, A24, Feb. 2010.
C.-C. Chen, L.L. Cowie, W.-H. Wang, A.J. Barger, and J.P. Williams, “Submillimeter sources behind the massive lensing clusters A370 and A2390,” ApJ, vol. 733, 64, 2011.
A. Dutrey, S. Guilloteau, and M. Guelin, “Chemistry of protosolar-like nebulae: the molecular content of the DM Tau and GG Tau disks,” A&A, vol. 317, L55, 1997.
N. Dello Russo, R.J. Vervack, H.A. Weaver, N. Biver, D. Bockelée-Morvan, J. Crovisier, and C.M. Lisse, “ Compositional homogeneity in the fragmented comet 73P/Schwassmann-Wachmann 3,” Nature, vol. 448, pp. 172-175, July 2007.
R. Gomes, H.F. Levison, K. Tsiganis, and A. Morbidelli, “Origin of the cataclysmic late heavy bombardment of the terrestrial planets,” Nature, vol. 435, pp. 466-469, May 2005.
F. Henry, D. Bockelée-Morvan, J. Crovisier, and J. Wink, “Observations of rotating jets of carbon monoxid in comet Hale Bopp with the IRAM interferometry,” Earth Moon and Planets, vol. 90, pp. 57-60, June 2002.
S. Martín, M. Krips, J. Martín-Pintado, S. Aalto, J.-H. Zhao, A.B. Peck, G.R. Petitpas, R. Monje, T.R. Greve, and T. An, “The Submillimeter Array 1.3 mm line survey of Arp 220, ” AA, vol. 527, pp. 36, 2011.
K. Oberg, C. Qi, J.K.J. Fogel, E.A. Bergin, S.M. Andrews, C. Espaillat, T.A. van Kempen, D.J. Wilner, and I. Pascucci, “The disk imaging survey of chemistry with SMA. I. Taurus protoplanetary disk data,” ApJ., vol. 720, 480, 2010.
K. Oberg, C. Qi, J.K.J. Fogel, E.A. Bergin, S.M. Andrews, C. Espaillat, D.J. Wilner, I. Pascucci, and J.H. Kastner, “Disk Imaging Survey of Chemistry with SMA. II. Southern Sky Protoplanetary Disk Data and Full Sample Statistics,” ApJ., vol. 734, 98, 2011.
R.A. Primiani, J. Weintroub, J. deWerd, "SMA Wideband Correlator, Memo 1: Polyphase Filter-bank Utilization," 2011, available at https://www.cfa.harvard.edu/twiki/pub/SMAwideband/MemoSeries/sma_wideband_utilization_1.pdf
K. Sakamoto, R.-Q. Mao, S. Matsushita, A.B. Peck, T. Sawada, and M.C. Wiedner, “Star-forming cloud complexes in the central molecular zone of NGC 253,” ApJ, vol. 735, 19, 2011.
S.K. Pan, and A.R. Kerr, “SIS mixer analysis with non-zero intermediate frequencies,” Proc. 7th Symp. Space THz Tech., pp. 195-206, 1996.
W.-F. Thi, G.-J. van Zadelhoff, and E.F. van Dishoeck, “Organic molecules in protoplanetary disks around T Tauri and Herbig Ae stars,” A&A, vol. 425, pp. 955-972, 2004.
C.E. Tong, R. Blundell, K.G. Megerian, J.A. Stern, S.-K. Pan, and M. Popieszalski, “A distributed lumped-element SIS mixer with very wide instantaneous bandwidth,” IEEE Trans. Appl. Supercond., vol. 15, pp. 490-494, June 2005.
Curriculum Vitae of Investigators
C. Edward Tong
Senior Receiver Engineer, Smithsonian Astrophysical Observatory, Tel: (617) 496-7641, 496-7667 60 Garden St., MS-42, Cambridge, MA 02138. E-mail: [email protected] a. Professional Preparation University of Hong Kong Bsc (Eng) : EE Major 1980 - 83 IRAM, Grenoble, France Pre-doc research associate 1985 - 88 Joseph Fourier University, Grenoble, France Ph.D. in Physics 1988 Communications Research Lab., Tokyo, Japan Post-doctoral Fellow 1989 - 91 b. Appointments Receiver Engineer (1991-present) Submillimeter Receiver Lab., Smithsonian Observatory.
c. Publications (Three most recent publications relevant to the proposed research) 1. C.E. Tong, R. Blundell, K.G. Megerian, J.A. Stern, S.K. Pan, and M. Popieszalsi, “A distributed
lumped-element SIS mixer with very wide instantaneous bandwidth,” IEEE Trans. Appl. Supercond.,vol. 17, pp. 371-374, June 2005.
2. C.E. Tong, L. Chen, and R. Blundell, “Theory of distributed mixing and amplification in a superconducting quasi-particle non-linear transmission line,” IEEE Trans. Microwave Theory & Tech., vol. 45(7), pp. 1086-1092, July 1997.
3. C.E. Tong, R. Blundell, K.G. Megerian, J.A. Stern, M. Popieszalski, and S.-K. Pan, “Gain enhancement in inductively-loaded SIS junction arrays,” IEEE Trans. Appl. Supercond., vol. 17(2), pp. 371-374, June 2007.
Qizhou Zhang Astrophysicist, Smithsonian Astrophysical Observatory, Tel: (617) 496-7655 60 Garden St., Cambridge, MA 02138. E-mail: [email protected]
a. Professional Preparation Nanjing University, China B.S. in Astronomy 1983 Harvard University M.S. in Astrophysics 1993
Harvard University Ph.D. in Astrophysics 1996
b. Appointments Astrophysicist Smithsonian Astrophysical Observatory, 1998 - present
c. Publications (Five most recent publications relevant to the proposed research) 1. IRDC G030.88+00.13: A Tale of Two Massive Clumps, Zhang, Qizhou, Wang, Ke, 2011, ApJ,
733, 26. 2. Fragmentation at the Earliest Phase of Massive Star Formation, Zhang, Qizhou, Wang, Yang,
Pillai, Thushara, Rathborne, Jill, 2009, ApJ, 696, 268 3. Observations of the Infrared Dark Cloud G28.34+0.06, Wang, Y., Zhang, Q., Pillai, T.,
Wyrowski, F., and Wu Y. 2008, ApJ, 672, L33. 4. SMA observations of Infrared Dark Clouds: A tale of two cores, Rathborne, J. M., Jackson, J.
M.,Zhang, Q., Simon R. 2008, ApJ, 689, 1141 5. Water Masers Associated with Infrared Dark Cloud, Wang, Y., Zhang, Q., Rathborne, J. M.,
Jackson, J., and Wu, Y., 2006, ApJ, 651, L125
d. Synergistic Activities
• Expert in star formation with 65 refereed publications in the past five years. • Submillimeter Array Time Allocation Committee, 2006- present, Chair, 2007-present. • Submillimeter Array Legacy Science Committee, 2004-2005. • Steering Committee for Chinese National Astronomical Observatories, 2001- present. • Panelist for NASA ATP Program, NSF University Radio Observatories Program, NSF China, The
Dutch National Science Foundation, and Chilean Research Fund Council grant proposals. Referee for major astronomy journals.
Jonathan Weintroub
Smithsonian Astrophysical Observatory, Tel: (617) 495-7319 60 Garden St., Cambridge, MA 02138. E-mail: [email protected]
a. Professional Preparation
University of Cape Town Electrical Engineering B.Sc (Eng) 1st Class Honors 1983
University of Cape Town Electrical Engineering M.Sc (Eng) 1986
Harvard University Applied Physics Ph.D. 1998
b. Appointments
2002 – present Electrical Engineer SAO Cambridge MA 2000 – 2002 Director of Product development EndPoints, Inc. Bedford, MA 1998 – 2000 Vice President of Engineering Cambridge Metrology, Inc. Cambridge, MA 1995 - 1998 Bosack-Kruger Research Fellow Harvard University Cambridge, MA 1993 - 1995 Teaching Fellow Harvard University Cambridge, MA 1988 - 1993 Senior Design Engineer Klein Associates, Inc. Salem, NH 1987 - 1988 Design Engineer Klein Associates, Inc. Salem, NH
c. Related Publications
1. Doeleman, S.S., Weintroub, J., Rogers, A.E.E. et al, “Event-horizon-scale structure in the supermassive black hole candidate at the Galactic Centre,” Nature, 455, 78, 2008.
2. Weintroub, J., “A Submillimeter VLBI Array,” Proceedings of 'The Universe Under the Microscope – Astrophysics at High Angular Resolution', Journal of Physics: Conference Series, 131, 12047, 2008.
3. Weintroub, J. And Huff, L.C., “Preliminary Results Obtained with a Multi-Beam Focused Side Scan,» Hydrographic Journal, Hydrographic Society, London, 61, 11, 1991.
d. Synergistic Activies
2009 - 2010 Chair of CASPER Advisory Board Global Collaboration 2008 - present Member of CASPER Advisory Board Global Collaboration 2002 - present Correlator Group Leader Submillimeter Array 1988 - 1993 Developed novel phase array side scan sonar Klein Associates, Inc. 1987 - present 15 years of industrial engineering experience Various appointments
Ming-jye Wang
Research Fellow, Institute of Astronomy and Astrophysics, Academia Sinica, (ASIAA) 11/F Astronomy-Mathematics Building, National Taiwan University, Tel: +886-2-23665337 No. 1, Roosevelt Rd., Sec. 4, Taipei 10617, Taiwan. E-mail: [email protected]
a. Professional Preparation National Tsing-Hua University B.S. in Physics 1985–1989 National Tsing-Hua University Ph.D. in Physics 1989-1994 Institute of Astronomy & Astrophysics, Academia Sinica Post-doctoral Fellow 1994-1999
b. Appointments 2009 - present Research Fellow ASIAA 2004 - 2009 Associate Research Fellow ASIAA 1999 - 2004 Assistant Research Fellow ASIAA
c. Publications (Three most recent publications relevant to the proposed research): 1. M. J. Wang, H. W. Cheng, Y. H. Ho, C. C. Chin, C. C. Chi, “Low noise Nb-based SIS miser for
sub-millimeter wave detection”, Journal of Phys. & Chem. Solids, vol. 62, pp. 1731-1736, 2000. 2. M. J. Wang, H. W. Cheng, P. K. Chuang, S. L .Wu, C. C. Chi, “New AlOx Thickness Control
process for SIS Tunnel Junctions Fabrication”, IEEE Trans. Appl. Supercond., vol. 13, pp. 1101-1103, Jun. 2003.
3. C.-T. Li, K.-Y. Liu, W.-C. Lu, C.-P. Chiu, T.-J. Chen, C.-W. Chen, Y.-C. Chang, M.-J. Wang and S.-C. Shi, “Development of 460 GHz and Dual Polarization SIS Mixers for the Submillimeter Array”, IEEE Trans. Appl. Supercond. Vol. 21, pp. 654-658, Jun. 2011.
Wei-Hao Wang Institute of Astronomy and Astrophysics, Academia Sinica (ASIAA) PO Box 23-141, Taipei 10617, Taiwan. Tel: +886-2-2366-5401 E-mail: [email protected]
Position Assistant Research Fellow 2009–present ASIAA
Educational Background
B.S. in Physics Dept. of Physics National Taiwan University 1996
M.S. in astronomy Institute of Astronomy National Central University, Taiwan 1998
Ph.D. in astronomy Institute for Astronomy University of Hawaii at Manoa 2006
Awards and Honors
Jansky Fellow, 2006–2009, National Radio Astronomy Observatory
Selected Papers Wang, W.-H., Barger, A. J., & Cowie, L. L. “A Ks and IRAC Selection of High-Redshift Extremely Red Objects,” 2012, ApJ, 744, 155 Wang, W.-H., Cowie, L. L., Barger, A. J., & Williams, J. P. "SMA Observations of GOODS 850-11 and GOODS 850-13 — First Examples of Multiple Submillimeter Sources Resolved by an Interferometer," 2011, ApJ, 726, L18 Wang, W.-H., Cowie, L. L., Barger, A. J., Keenan, R. C., & Ting, H.-C. "Ultradeep Ks Imaging in the GOODS-N," 2010, ApJS, 187, 251 Wang, W.-H., Barger, A. J., & Cowie, L. L. "Ultradeep Near-Infrared Observations of GOODS 850-5," 2009, ApJ, 690, 319 Wang, W.-H., Cowie, L. L., van Saders, J., Barger, A. J., Williams, J. P. "GOODS 850-5 -- A z>4 Galaxy Doscovered in the Submillimeter?" 2007, ApJL, 670, L89 Wang, W.-H., Cowie, L. L., Barger, A. J., "A Near-Infrared Analysis of the Submillimeter Background and the Cosmic Star-Formation History," 2006, ApJ, 647, 74 Wang, W.-H., Cowie, L. L., Barger, A. J. 2004, "An 850 Micron SCUBA Survey of the Hubble Deep Field-North GOODS Region," ApJ, 613, 655
Ming-tang Chen
Academia Sinica, Institute of Astronomy and Astrophysics, ASIAA Hawaii Operations, E-mail: [email protected] 645 N. A’ohoku Place, Hilo, HI 96720, USA. Telephone : +1 (808)-961-2931
EDUCATION BACKGROUND: B.S. (Physics), 1982-1986, National Cheng Kung University, Taiwan Ph.D (Physics), 1989-1993, University of Illinois at Urbana-Champaign, USA
PROFESSIONAL EMPLOYMENT: 1995 - Present, Research Assistant ….. Research Fellow, ASIAA 2003.11- Present, Deputy Director of ASIAA Hawaii Operations 2008.8 - 2010.9, Assistant Director, ASIAA 2011.6 - Present, Head of the Submillimeter Array (SMA) Operations in Hawaii
Recent Related Publications: 1. Huang Y.-D.; Raffin P.; Chen M.T., "Stiffness study of a hexapod telescope platform", IEEE Trans.
Ant. & Propagation: vol. 59(6), pp. 2022-2028, June, 2011. 2. Koch P.M.….Chen M.-T. et al., "1.2 m Shielded Cassegrain Antenna for Close-Packed Radio
Interferometer" , PASP: vol. 123(900), pp. 198-212, Feb, 2011. 3. Li C.T.; .. Chen M.T., et al, "AMiBA Wideband Analog Correlator", ApJ: vol. 716(1), pp. 746-757,
Jun 2010. 4. M.-T. Chen, et al, “ AMiBA: Broadband Heterodyne CMB Interferometry”, ApJ, vol. 694, pp.
1664-1669, April 2009.
Professional Experience • SMA receiver and antenna systems • Array for Microwave Background Anisotropy (AmiBA): receivers , hexapod mount & site development • ALMA: East-Asia Frontend Integration Center; Band-1 rprototype; nutator project, laser synthesizer • Digital correlator development based on hardware from the Collaboration for Astronomy Signal
Processing and electronic Research (CASPER) • Greenland Submillimeter telescope project for Very-Long-Baseline Interferometry. CURRENT RESEARCH/TECHNICAL INTEREST: Black hole science; imaging in radio wavelength; high-speed digital correlator; sub-mm; low-noise receiver technologies; adaptive radio-wave; Cosmology, CMB science.
