ALMA: Current Status and Future Possibilities

Helen Kirk Herzberg Astronomy & Astrophysics

National Research Council of Canada

ALMA Basics• 5000m above sea level on Chajnantor plateau • 3 arrays: 12 m array (50 dishes) + ACA/Morita

Array: 12x7 m dishes + TP array: 4x12 m dishes • max 12 m array size from ~150m to ~16km • frequencies ~84-1000 GHz in a series of bands

(~35 GHz band likely ready in the next few years) • currently ~1TB/day of science data taken

ALMA visit, March 11 !ALMA, c. NRAO

Observing Cycle 5• 12m array: >= 43 antennas, max spacing 160m to16km; ACA: >=

10 antennas. (all steady state values) • 1664 proposals submitted, including solar, polarization, VLBI,

large proposals,… • oversubscription rate, by hours: 12m: 4.1 (all), 3.6 in (NA), 5.3

(Can); ACA: 3.8 (all), 3.4 (NA), 11.5 (Can); Canada #s relative to 7.25% of NA contribution (NA fraction is ~36%; Canada not limited to 7.25% of NA)

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ACA"

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Total'Power' c. Stuartt Corder

Science Impact• Already >785 science papers already written, ~15%

Canadian co-authors, ~4% Canadian first authors • Canada ALMA papers are strong ones: AIPP 6.2 for

Canadian co-author vs 4.2 any author ALMA papers (stats to 2015)

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ALMA" Keck"

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Impact(per(Paper((201132015)(

AIPP" MIPP"

c. Dennis Crabtree

Avg & Median Impact Per Paper

Galactic ScienceJ White ea ’16: dust & gas in the disk of

HD141569

J White ea ’17: Fomalhaut debris disk

Kirk ea ’17: 1st detection of starless

core substruct

Freeman ea ’17: molecular clouds &

clusters in M83Friesen ea ’14: circumstellar accretion regions in forming

stars

Mann ea ’14: protostellar disks in Orion & the destruction by OB stars

Extragalactic Science

Sliwa ea ’17: chemical evolution in gals

Schirm ea ’16: PDR modelling in the

Antennae

Vantyghem ea 16: BCG’s molec. filament

Investigating overdensities around z > 6 galaxies through ALMA observations of [CII] 5

1.0��

Line

�0.30�0.150.000.150.300.450.60 1.0��

Continuum

�0.060�0.045�0.030�0.0150.0000.0150.0300.0450.060

264.1 264.4 264.7 265.1 265.4 265.7 266.0Frequency (GHz)

�0.4�0.2

0.00.20.40.60.81.0

mJy

beam

�1 [CII] z= 6.180

(a) CLM1-A (b) CFHQS J0210-A

(c) CFHQS J0210-B (d) J2054-A

(e) WMH5-B

Figure 3. The five line candidates found by the blind search of the deep ALMA cubes are shown here. Contours on the continuum images represent 0.9, 0.7and 0.5 times the peak flux in the corresponding line channel. a) A candidate found near the UV luminous LBG CLM1. ALMA data was originally taken byand analyzed in Willott et al. (2015b). b) A candidate found near the Quasar J0210-0456, originally analyzed by Willott et al. (2013). c) A candidate foundnear the quasar J2054-0005. The ALMA data of the quasar was taken and analyzed in Wang et al. (2013). d) A candidate found near the source WMH5, alsoanalyzed in Willott et al. (2015b). They point out the source and ackowledge it is likely a smaller galaxy undergoing a merger with the central source. Wemake an effort to fit the line profile separately.

with r = 12 00), except for the J2054 field where the candidate isfound just outside of the primary beam (⇠ 14.5 00 from the center).For this field the a circle with an angular radius equal to that of thecandidate is assumed to be searched. The redshift range searchedis found through the spectral coverage of the ALMA data cubes,found in Table 1, and the known rest frame emission of the [CII]line at 157.7 µm

Figure 5 displays the estimates for the luminosity function(LF) of [CII] emitters at high redshift from our study, as well asother recent measurements and predictions. Our data is shown forjust the companion galaxies, and also with both the companionsand their central primary galaxies. Where we have only one galaxyat > 109 L�, we treat our data as an upper limit. It is clear that ourmeasurements are all well above all the previous measurements and

c� 2016 RAS, MNRAS 000, 1–??

Coppin ea ’12 sf in high-z gals

Miller ea ’17: CII in high-z galaxies

Willott ea ’15: CII in high-z

galaxiesWilson ea ’14: AGN in Arp220?

ALMA 2030 Priorities• Improve archive usability

• more user-friendly, more data products (incl unintentional line detections), PI added data products,…

all science cases • Larger bandwidths & improved receiver sensitivity

• band 2+ (67-95 GHz) or band 2+3; new band 11 (1.1-1.6THz) • 2x bandwidth per observation; improved receiver components galactic chemistry (D2H+), CII line in intermediate redshift galaxies; continuum projects, spectral line surveys & redshift surveys

• Larger baselines• out to 30km or larger?; have several antennas fixed at very

remote stations (to 300km)? Would need more antennas! high-Z universe to 10pc scales: BH formation in SMG & AGN accretion, proper motions: star distances and exoplanet characterization (motions of 0.01AU out to 10’s pc)

• Improve mapping speed• multipixel receivers at most popular band(s) all science with extended emission / larger fields

• (Large single dish near ALMA site?: AtLAST (EU) / LST (Japan) / CCAT)

27 ANASAC f2f Meeting – 17 May 2016

Longer$Baselines$Enable$QualitaBvely$New$Science$

•  VLB$and$connected$element$arrays$–  ALMA$Phasing$Project$(NA,$ESO,$EA$HW/SW:$Doeleman,$MIT$+)$

•  Offered$for$Cycle$4$(1$Oct$2016=30$Sept$2017)$

–  ALMA$Phasing$System$Extensions$and$Enhancements$(HW/SW:$MaDhews,$MIT)$

–  Pulsars,$Magnetars$and$Transients$with$Phased$ALMA$(SW:$Cordes,$Cornell)$

–  ALMA0Extended0Array0(EA0T:0Kameno)0

Development$Workshop$8/19/16$

c. Al Wooten, NA sci devel. workshop

ALMA 2030 Priorities• Improve archive usability

• more user-friendly, more data products (incl unintentional line detections), PI added data products,…

all science cases • Larger bandwidths & improved receiver sensitivity

• band 2+ (67-95 GHz) or band 2+3; new band 11 (1.1-1.6THz) • 2x bandwidth per observation; improved receiver components galactic chemistry (D2H+), CII line in intermediate redshift galaxies; continuum projects, spectral line surveys & redshift surveys

• Larger baselines• out to 30km or larger?; have several antennas fixed at very

remote stations (to 300km)? Would need more antennas! high-Z universe to 10pc scales: BH formation in SMG & AGN accretion, proper motions: star distances and exoplanet characterization (motions of 0.01AU out to 10’s pc)

• Improve mapping speed• multipixel receivers at most popular band(s) all science with extended emission / larger fields

• (Large single dish near ALMA site?: AtLAST (EU) / LST (Japan) / CCAT)

27 ANASAC f2f Meeting – 17 May 2016

Longer$Baselines$Enable$QualitaBvely$New$Science$

•  VLB$and$connected$element$arrays$–  ALMA$Phasing$Project$(NA,$ESO,$EA$HW/SW:$Doeleman,$MIT$+)$

•  Offered$for$Cycle$4$(1$Oct$2016=30$Sept$2017)$

–  ALMA$Phasing$System$Extensions$and$Enhancements$(HW/SW:$MaDhews,$MIT)$

–  Pulsars,$Magnetars$and$Transients$with$Phased$ALMA$(SW:$Cordes,$Cornell)$

–  ALMA0Extended0Array0(EA0T:0Kameno)0

Development$Workshop$8/19/16$

c. Al Wooten, NA sci devel. workshop

NB: most recent development program proposals on band2+3 (NRAO) & hardware for doubling band3 (NRC)

were both turned down.

ALMA 2030 Priorities• Improve archive usability

• more user-friendly, more data products (incl unintentional line detections), PI added data products,…

all science cases • Larger bandwidths & improved receiver sensitivity

• band 2+ (67-95 GHz) or band 2+3; new band 11 (1.1-1.6THz) • 2x bandwidth per observation; improved receiver components galactic chemistry (D2H+), CII line in intermediate redshift galaxies; continuum projects, spectral line surveys & redshift surveys

• Larger baselines• out to 30km or larger?; have several antennas fixed at very

remote stations (to 300km)? Would need more antennas! high-Z universe to 10pc scales: BH formation in SMG & AGN accretion, proper motions: star distances and exoplanet characterization (motions of 0.01AU out to 10’s pc)

• Improve mapping speed• multipixel receivers at most popular band(s) all science with extended emission / larger fields

• (Large single dish near ALMA site?: AtLAST (EU) / LST (Japan) / CCAT)

27 ANASAC f2f Meeting – 17 May 2016

Longer$Baselines$Enable$QualitaBvely$New$Science$

•  VLB$and$connected$element$arrays$–  ALMA$Phasing$Project$(NA,$ESO,$EA$HW/SW:$Doeleman,$MIT$+)$

•  Offered$for$Cycle$4$(1$Oct$2016=30$Sept$2017)$

–  ALMA$Phasing$System$Extensions$and$Enhancements$(HW/SW:$MaDhews,$MIT)$

–  Pulsars,$Magnetars$and$Transients$with$Phased$ALMA$(SW:$Cordes,$Cornell)$

–  ALMA0Extended0Array0(EA0T:0Kameno)0

Development$Workshop$8/19/16$

c. Al Wooten, NA sci devel. workshop

ALMA Development Program Cycle 5 results

Study (prototyping) proposals due May 2017. 2 sub-categories: • General studies: 1 year, < $200,000:

• Neuroscope: Neural Machine Intelligence Tools for Discovery and Interpretation in Complex ALMA Data, PI E. Merényi (Rice U)

• Full-Mueller Mosaic Imaging with ALMA, PI S. Bhatnagar (NRAO) • Strategic studies: 2 years, < $400,000:

• Wideband Low-Noise Balanced IF Amplifiers for ALMA Band 6, with Future Application to ALMA Bands 3-10, PI A. Kerr (NRAO)

• Quantum-Limited Very-Wideband 4-Kelvin RF and IF Amplifiers for ALMA, PI O. Noroozian (NRAO)

Development (longer-term, telescope-implemented) proposals due Jan 2017: results not yet announced (https://science.nrao.edu/facilities/alma/alma-develop-old-022217/alma-develop-history) • Canadian PIs of prior year successful programs, both hardware

and software related

Canadian Hardware ProjectsNRC efforts in several areas of ALMA 2030 priorities and related work:

• power stability in mixers for Band 3 cartridges • hardware constraints for multi-pixel arrays • hardware constraints for increasing bandwidth

Current / previously funded development & study projects: • Band 3 Cold Cartridge Assembly Magnet and Heater

Installation for Deflux Operation, PI L. Knee (NRC); ongoing, cycle 2 development now close to implementation

• Prototype of a Complete Dual-Linear 2SB Block and a Single-Polarization Balanced 2SB Block, PI D. Henke (NRC); cycle 4 study, ongoing

• Millimetre Camera, PI S. Claude (NRC); cycle 2 study, completed & used in current multi-pixel receiver plans

6/9 funded development projects are hardware related 14/30 funded development studies are hardware related Band 3 cartridge

Previously funded development / study projects: • Cube Analysis and Rendering Tool for Astronomy (CARTA); PI: E

Rosolowksy (UofA), cycle 2. Initially a study project in cycle 1 • Cleaning Up Interactive Cleaning; PI: E. Rosolowsky (Uof A), cycle 4

2/9 funded development projects are software related 6/30 funded development studies are software related

Canadian Software Projects

Figure A2: Region statistics mode for a selected feature in the data cube. The statistics are calculated in the highlighted box. Each statistic has a profile over the different channels within the box. The profile for the average is shown in the second window. This is the average spectrum over the box.

A Visualization Portal for ALMA Data • Development Study Final Report • p. 11 of 33

Figure A3: One dimensional Gaussian fitting dialogue. This is the fit is applied to the profile found in the average spectral profile shown in Figure A2. The Manual Initial Conditions dialog allow careful seeding of the fits on spectra fits. The widths and peaks of the Gaussian are reported in the text information box.

A Visualization Portal for ALMA Data • Development Study Final Report • p. 12 of 33

example screen shots from initial (cycle1) CARTA prototype

Other Directions: Increased Community Engagement

• Fraction of successful Canadian PIs, A+B grade proposals: 10% of NA on 12m, 52% of NA on ACA (NB: includes a large proposal). Financial contribution 7.25%. Prior semesters cycle 0: 10%; cycles 1-4: 3-4% (NB: small number statistics). Canadian PI + coI proposals A+B grade 24% of total global allocation

• Most successful PIs are expert radio astronomers (57 Can PIs have applied, 26 with A-C grade, all cycles)

Support from the MAG (HIA) at all steps, including: • technical: maintenance of Band 3 receivers; science: documentation; training

workshops; proposal advice (through Helpdesk); phase 2 obs. prep.; observing; data (reduction) support, incl. visiting; press release help,…

Archival data can also be better exploited: • archive has lots of data!; NAOJ has quick-view images of datasets • NRAO: starting science ready data products (SRDP) project, leader Jeff Kern • NRC: Helen leading project to make CANFAR easily accessible to Canadian

community for ALMA science (talk to me if you want to be an early tester)

Thank You!

ALMA, c. ESO