2019A B-ranked tracks with successful observations:

Project ID	P.I.	# Tracks	Title (hover for abstract)
2019A-S063	Mark Gurwell	9	Titan 1.1mm Band Spectral Line Imaging Survey We seek to revolutionize our inventory of molecular species in the atmosphere of Titan, capitalizing on the new broad bandwidth SWARM provides. We propose a 32 GHz continuous spectrum, moderately spatially resolving Titan, covering 247 to 279 GHz. While many species previously detected will be covered in this tuning (HCN and isotopologues, CH3CN, H3CN, CH3C2H, HNC, C2H5CN, etc), it will also cover dozens to hundreds of lines from heavier molecular species such as pentadiynenitrile (HC5N), vinyl cyanide (C2H3CN), adenine (C5N5H5), guanine (C5N5H5O), thymine (C5N2H6O2), glycine (C2NH5O2), and alanine (C3NH7O2), to name just a few. Many of these heavier species are precursors to and important for biological systems. While individual lines of such species may be undetectable at our noise goal, we can use spectral stacking at the known frequencies of the lines to increase our sensitivity by factors of up to 10 for some species. Due to the fact that these species are optically thin, the majority of their observed emission will appear near the disk limb. Therefore, it is advantageous to resolve Titan to emphasize this emission. Since Titan is ~0.8" in diameter (considering the mid-stratospheric height of limb sensitivity), this requires VEX configuration. To be certain we are obtaining a good global flux spectrum, we also need low resolution (COM) observations to anchor the imaging. Due to the well known structure of Titan's continuum, we will be able to phase and amplitude self-calibrate our data, lessening our weather stability requirements. An excellent byproduct of these observations will measurements of the latitudinal and vertical abundances of the strongly detected species, along with direct detection of stratospheric winds on Titan through measurement of Doppler shifts in the strong cores of molecular lines of HNC, HCN, and CH3CN. While this was recently done using ALMA (Lellouch, Gurwell et al 2019) from 2016, Titan's circulation pattern changes on seasonal timescales, and the 3 year span since those observations represents a significant seasonal change given Titan's 29.5 year orbit. Therefore, these SMA observations will be uniquely interesting and noteworthy. We request 45 hours on source (roughly 2 tracks in COM and 7 in VEX assuming 5 hours on source per track), in ~2.5mm pwv conditions to reach 6 K per beam rms per 140 kHz channel, at 0.5"x0.4" resolution, moderately resolving the 0.8" disk. Per beam, 6K rms/channel will allow for excellent measurements of Doppler shifts since these pressure broadened lines are typically 30-100 K in emission and will span several channels. For detection of weak species, binning to 1.12 MHz will give rms of 2 K per channel, with spectral stacking allowing even more effective noise suppression, perhaps down to 0.2-0.5 K for some species. Given the 70 K continuum temperature of Titan, these effective noise levels provide unprecedented sensitivity *even compared to ALMA*. The combination of comprehensive continuous coverage over 32 GHz, access to many lines, fine spectral resolution, and sensitivity, has never been achieved and will provide a rich data set from which to measure the molecular inventory of Titan's stratosphere.
2019A-S006	Charles Law	5	Searching for Ionized Accretion Flows around 0.1 pc Scale Clusters with O-Type StarsEarly O-type stars must gain tens of Msun after the onset of an HII region excited by their own radiation. How mass accretion takes place in the presence of strong outward thermal pressure during the HII region phase is a mystery. Our studies of a hyper compact HII region G10.6 demonstrate that such an accretion occurs in ionized gas and is driven by the gravitational pull of the massive star or a cluster of stars. This proposal seeks observations in a set of millimeter hydrogen recombination lines in a sample of hyper compact HII regions similar to G10.6 to search for and spatially resolve the accretion flow. This study will provide important clues to the formation of the most massive stars in the Universe.
2019A-S045	Tomasz Kaminski	2	What is K4-47? Investigating the Most Molecularly Complex Planetary Nebula to DateK4-47 was long thought to be an ordinary planetary nebula. Recent single-dish millimeter observations revealed however that it is unusually rich in complex molecules and istotopologues of, otherwise rare, CNO isotopes. The isotopic ratios are so unusual that it is difficult to classify K4-47 or explain its origin. It may be a product of an unexplored eruptive mechanism occurring in an aging stellar interior or a remnant of a recent stellar merger. We propose to use the SMA in an extended configuration to map its molecular emission for the first time. In this exploratory mapping project we would like to investigate the relative distribution of strongest 12C- and 13C-bearing molecules and look for lines of AlF. Detection of the latter may open a way to detect the radioactive isotope of 26Al in the future. Maps of the less exotic species will be used to asses the optical depth and fractionation effects on the measured isotopic ratios.
2019A-S031	Matthew Ashby	2	The Impact of Radio Jets on Star Formation in AGN Host GalaxiesPanchromatic SED modeling by Podigachoski et al. (2015) revealed intriguing hints of a possible causal connection between radio jet age (a proxy for AGN age) and star formation (SF) in powerful high-redshift radio galaxies. Specifically, SF in the hosts of long-lived radio-loud AGNs is systematically low, compared to that in the hosts of young AGNs. If confirmed, this would be strong new evidence for AGN feedback (e.g., Croton et al. 2006; Cresci & Miaolino 2018). Here we propose a first test of this idea with a pilot study to characterize the disks in four radio-loud AGNs from Podigachoski et al: two with short, young jets (3C 124 and 3C 298) and two with extended, mature jets (3C270.1 and 3C 297). We will combine the SMA measurements with our existing Spitzer(IRAC/IRS/MIPS), Herschel (PACS/SPIRE), and radio-frequency data to disentangle the contributions to the galaxies' luminosity. In this way we will determine whether the hosts of the older jets still contain or have instead exhausted their reservoirs of molecular gas, the fuel for SF, as traced by the thermal dust continuum (and possibly CO).
2019A-S007	Glen Petitpas	3	The Beautiful and Enigmatic Spiral Galaxy NGC 7331I propose here to improve and expand up my previous observations of the remarkable spiral galaxy NGC 7331. The spiral arms are very bright in CO J=2-1 which allows a rare chance to study warmer molecular gas in the outer spiral arms. No molecular gas is detected in the center of this galaxy when traced with the lower-J transitions of CO, but despite this the nucleus of this galaxy exhibits LINER activity and shows bright 850 micron emission suggesting the presence of star formation and warm dust. The data proposed here will allow us to address the following: a) Are the higher-J transitions of CO better tracers of morphology and dynamics in more active environments? b) Do the temperature and density of molecular gas correlate with the large scale morphology? and c) Does the past history of interaction affect the mass distribution of molecular clouds? We will take advantage of the dual receiver capability of the SMA to observe CO J=2-1 and J=3-2 simultaneously, meaning we request here only three tracks: one in Extended and two in Compact (owing to the smaller 345 GHz beam needing more mosaic points).
2019A-S004	David Clements	2	A Rosetta Stone for Distant Dusty Star-Forming Galaxies: SERVS, Herschel and the SMAThe discovery of a substantial population of high redshift far-IR luminous objects through colour selection of '500-risers' in Herschel data has been a surprise and a challenge for current models of galaxy formation and evolution. Understanding this population is difficult since they are both rare and faint in the optical/near-IR. A clear view of the optical-to-far-IR SEDs of such objects, necessary for understanding their stellar mass, star formation history and much more, is thus lacking. The advent of the SERVS deep IRAC survey data, now cross matched to deep optical/near-IR data in the 4.5 sq. deg. of the XMM-LSS field, can provide the missing link in understanding this population if we can obtain cross identifications. SMA observations will allow this, even in cases where the Herschel sources are blends of multiple fainter sources. We here propose SMA observations of a complete flux limited sample of five 500-risers, to obtain cross-IDs and thence to determine the full SEDs and stellar properties of these important but poorly understood objects.
2019A-A011	Yuji Urata	3	Search for Bright submm GRB afterglows Toward Radio PolarimetryBasis of our successful measurement of the first radio polarization for the GRB afterglow by the coordinated SMA and ALMA program, we propose continuation of (1) detecting bright submm GRB afterglows toward radio polarimetry, (2) decoding the radiation of afterglows for estimating the radiated energy in afterglow phase, and then (3) understanding diversity of GRB progenitor stars. In this program, we intend to conduct calorimetry of GRB including non-energized electron contribution with the radio polarization by coordinated SMA and ALMA observations. A 30 solar-mass progenitor star is typically used in long-GRBs models, in which all electrons are energized by the relativistic shock and emit the synchrotron radiation as afterglows. However, a substantial fraction of the electrons likely remains cool and emit non-observable radiation. These non-energized electrons increase the total energy and require a significant revision of the standard mass of progenitor star. As we demonstrated with previous programs, initial SMA rapid observations are crucial to identify bright submm GRB afterglows for the radio polarimetry and to decode complex radiation components.
2019A-S044	Tomasz Kaminski	3	The aftermath of a stellar collision in the Galactic BulgeEWS 2002-BLG-360 (or BLG-360) belongs to a rare class of objects known as red novae which erupt in stellar-merger events. They give us a chance to study most catastrophic forms of binary interaction of non-compact stars, including the common-envelope phase understanding of which is central to modern astrophysics. We propose to obtain spectral and continuum flux measurements of BLG-360 which is the least studied of the five known Galactic red-nova remnants. The SMA has recently detected it for the first time as a millimeter-wave source. The requested fellow-up measurements will constrain the gas and dust content in the merger remnant and will provide basis for imaging of the merger site with ALMA at longest baselines. This project is part of a larger program aiming to explain why and how non-compact stars merge.
2019A-S059	Michael McCollough	4	Using SMA to probe the jet emission in microquasar Cyg X-3 during radio outburst Cygnus X-3 is a unique X-ray binary (XRB) with a Wolf-Rayet star for a mass-donating companion. It is relatively bright in the radio virtually all of the time and is shown to undergo giant radio outbursts (up to 20 Jy) with associated jet-like structures moving away from Cygnus X-3 at 0.3-0.9c. This last characteristic makes Cygnus X-3 a member of a subclass of XRBs called "microquasars" which are similar to quasars/AGNs in that they exhibit highly collimated relativistic jets. We are proposing to make a series of short daily SMA observations starting at the beginning of a major flare and to follow its evolution. This will allow us to probe the spectral and structural evolution of flare as well as be part of a larger multi-frequency campaign to examine the spectral energy distribution of major radio flares in Cygnus X-3.
2019A-H004	Mark Gurwell	1	UH RADAR PROGRAMThis project is set to account for the UH RADAR program for bird counting, requiring the SMA to protect the receivers and not observe.

Current or completed Large Scale Programs spanning ALL semesters:

Project ID	P.I.	# Tracks	Title (hover for abstract)
2012B-S097	Qizhou Zhang	3	Star Formation in the Central Molecular ZoneThe inner 500 pc of our Galaxy, known as the central molecular zone (CMZ), is a star-forming environment with very extreme physical properties. Despite its large reservoir of dense gas that could form massive stars and clusters similar to the starbursts seen in galaxies, CMZ has a star formation rate a factor of 10 lower than the Schmidt-Kennicutt law. Because of the heavy extinction in the optical and infrared wavelengths, however, existing observations may miss a deeply embedded protostellar population. To investigate this scenario, we conducted a mini-survey with the SMA towards a sample of dense clouds with highest star formation potential, i.e. surface density >10^24 cm^-2 in CMZ at 280 GHz. The data reveal that most of them present compact dust continuum peaks possibly from protostellar cores. Are these peaks associated with embedded protostars? How do they compare with normal molecular cores in the Galactic disk? To address these questions, we propose to observe them in the 230 GHz band, to test protostellar nature of these objects via abundant molecular lines in this band. The SMA data will be supplemented with continuum and NH3 lines datasets obtained from the VLA. This is a pilot program to a large scale SMA project that images a significant area of the CMZ to census a population of deeply embedded protostellar objects. A lack of current star formation in the CMZ challenges a well established star formation (Schmidt-Kennicutt) law. The SMA observations play a unique role in solving this puzzle by probing young stellar populations that are possibly hidden from optical and IR observations due to heavy extinction, as well as radio continuum observations due to a lack of HII regions.
2013A-S079	Michael Dunham	3	(p)MASSES: (pilot) Mass Assembly of Stellar Systems and their Evolution with the SMAStars are assembled in molecular clouds through the gravitational collapse of dense cores of gas and dust. The final masses of stars are set during the protostellar stage by the complex interaction of many interrelated physical processes, including the underlying core mass function, core and disk fragmentation, the formation and evolution of protostellar disks, and mass-loss through direct ejection of jets and entrainment of surrounding material in molecular outflows. Several key questions related to the growth of stars and origins of the stellar initial mass function (IMF) are yet to be answered, including: (1) When, where, and how do cores and disks fragment into multiple systems? (2) What role do disks play in the transfer of mass from cores to stars? (3) To what extent do outflows regulate the protostellar mass accretion process? To answer these questions, we propose to conduct a 230 and 345 GHz, continuum and molecular line emission survey of a large sample of protostars in the nearby Perseus molecular cloud. Here we submit a small, pilot study of 4 targets in order to determine necessary sensitivities, verify our technical setup, and demonstrate the validity of our observations in answering the key science questions motivating this program.
2013B-S091	Eric Keto	61	CMZWe propose to exploit the SMA's unique combination of large primary beam, high angular resolution, and large instantaneous bandwidth to conduct the first sub-pc scale survey of the largest reservoir of dense gas in our Galaxy -- the central molecular zone (CMZ), the inner 500 pc of the Milky Way. This survey of the mm continuum and spectral line transitions will provide: (i) a complete census of the most massive and dense cloud cores; (ii) the location, strength and nature of strong shocks; (iii) the relationship of star formation to environmental conditions such as density, shocks, and large-scale flows. The high angular resolution of the SMA is necessary to find the highest density gas and image the distribution of shocks within individual star- forming clouds. The survey seeks to address fundamental open questions about the CMZ. What are the environmental conditions that lead to the formation of the most massive stars ($>$100 \Msun)? How do mass and energy flows shape the CMZ, regulate star formation, and control the activity of the central supermassive black hole? This survey will not only address immediate science goals but also provide a resource for future studies. Insofar as the CMZ resembles the central regions of other barred spiral galaxies, starburst galaxies in a quiescent phase, and the highly dense and energetic environment expected in galaxies in the early universe, this data set can be used as our nearest proxy for these environments.
2014A-S093	Michael Dunham	55	MASSES: Mass Assembly of Stellar Systems and their Evolution with the SMAStars are assembled in molecular clouds through the gravitational collapse of dense cores of gas and dust. The final masses of stars are set during the protostellar stage by the complex interaction of many interrelated physical processes, including the mass infall rate, core and disk fragmentation, ejection from multiple systems, the formation and evolution of protostellar disks, and mass-loss through jets and outflows. Several key questions related to the growth of stars and origins of the stellar initial mass function (IMF) are yet to be answered, including: (1) When, where, and how do cores and disks fragment into multiple systems? (2) What role do disks play in the transfer of mass from cores to stars? (3) To what extent do outflows regulate the protostellar mass accretion process? To answer these questions, we propose to conduct a 230 and 345 GHz, continuum and molecular line emission survey of all 73 protostars in the nearby Perseus molecular cloud. Our program will enable significant progress in answering all three of these questions and ultimately determining how stars are assembled from the surrounding dense gas.
2017A-S060	Garrett "Karto" Keating	27	The Millimeter-wave Intensity Mapping Experiment (mmIME)Molecular gas is central to the formation of stars in galaxies, but at high redshift, it has been well-studied in only a handful of the most luminous systems. Recent surveys with ALMA have hinted at a significant population (larger than theoretically expected) of molecular gas-rich (i.e., CO-bright) main sequence-like galaxies at high redshift, although these surveys have been limited in volume. While instruments like ALMA afford incredible sensitivity and resolution for performing studies of individual systems, it is suboptimal for blindly surveying for such objects over the large volumes required to reduce the impact of cosmic variance and sampling biases. We instead propose to use the SMA, whose larger bandwidth and primary beam make it more well-suited for a blind, large volume survey, covering a total area of ~100 sq. arcmin, between 195-203/211-219/227-235 GHz, within four regions within areas that are rich in multi-wavelength data sets. With these observations, we will use direct detection, stacking, and intensity mapping techniques, which will allow us to probe the abundance and physical properties of molecular gas in galaxies in a volume of nearly a million cubic megaparsecs. The proposed measurement will additionally leverage line intensity mapping efforts with both VLA, ACA, and ALMA, enabling cross-correlation between a multitude of line species. Relevant SMA Publications ------------------------- No SMA publications to date, as our first observations were completed in Feb 2016. Analysis of these data is on-going, and we are presently finalizing our results for publication. We expect to submit said publication in September/October 2017. Summary of Relevant Pilot Projects ---------------------------------- Proposal is a large-scale continuation of 2016B-S044, and is the successor to a recently completed intensity mapping experiment with CARMA. This proposal leverages two existing programs: a large-scale campaign with VLA at 1cm, and a recently completed (Cycle 4) 40-hour program with the ACA at 3mm. We also plan to propose for additional time with ACA and VLA, which will require cross- correlation with SMA data to fully enable the science potential of new data with these instruments. This proposal additionally builds off of two separate awards: one archival study focused on searching SMA calibrator fields for blind detections of spectral line emission from high-redshift objects, and one technical study looking at the feasibility of daytime observing with the SMA. The calibrator study, which is being conducting by the PI Keating and M. Fuchs, has made steady progress towards the development of a software pipeline, capable of digesting calibrator data and producing -- from a variety of instrument setups and array configurations -- bandpass, gain, and spectral SEFD/flux correction factors, with the goal of automatically being capable of producing calibrated image cubes for all calibrator observations performed by the SMA. At the time of proposal submission, we estimate that the first version of this pipeline will be ready to deploy in September 2017. The daytime observing project, which is also being led by the PI (with significant help from numerous members of the SMA staff), has also made significant progress in the past 6 months, and early tests seem to indicate that the array may be capable of operating up to 22 hours a day under "normal" weather conditions. One significant factor that was limiting daytime observations -- the degradation of pointing during post-sunrise observations -- has already been solved, allowing for generally good array performance until approximately noon HST (i.e., 18 hours of observations a day). Progress is now underway looking at methods for realtime phase correction and improved bandpass calibration techniques, as well as isolating sources of crosstalk/coupling within the system. We anticipate these efforts to offer improved observing capabilities moving forward toward the proposed observations, although we have estimated our time/sensitivity requirements with what we believe to be feasible at the time of proposal submission.
2017B-S075	Jan Forbrich	32	SMA Survey of Resolved Dust and Simultaneous CO Observations of GMCs in M31We propose a powerful and unique SMA survey to detect and resolve dust continuum emission in a large population of (~100) Giant Molecular Clouds (GMCs) in the famous Andromeda galaxy M31. As demonstrated in our pilot study, the SMA wideband upgrade is now enabling resolved interferometric dust continuum detections of individual GMCs in M31 at 230 GHz, the first such detections beyond the Magellanic Clouds. Our observations will provide the most robust, dust-derived measurements of the physical properties of GMCs within an external disk galaxy. We also propose to acquire simultaneous observations of 12CO(2-1) and 13CO(2-1) emission to measure the gas content of the GMCs with identical uv coverage. We will combine these measurements to characterize the fundamental physical properties of the GMC population across M31 to a degree only comparable in many key aspects to Milky Way studies. This project will enable much high-impact science including: 1) high-fidelity measurements of the GMC masses and shapes leading to an improved GMC mass function in M31, 2) direct measurements of the infamous CO "X" factor in individual GMCs and its variation across the galaxy, 3) a significantly improved assessment of Larson's scaling relations in M31 GMCs, and 4) a detailed assessment of cloud-scale star formation laws in M31, utilizing extensive existing multi-wavelength data. These results will provide an important calibration for the use of CO observations in deriving basic gas and star formation properties of external galaxies. Additional science goals include an assessment of dust emission vs optical extinction in M31. The survey will provide a unique SMA legacy that will remain unsurpassed for many years, in particular exceeding what can practically be done with ALMA due to the combination of wideband sensitivity and nearby distance of this northern target.