The Wideband Sensitivity Upgrade Project → Program: The First ALMA 2030 Roadmap upgrade

The Atacama Large Millimeter/submillimeter Array (ALMA) is the most sensitive radio telescope ever built for high-resolution observations at millimeter and submillimeter wavelengths. Inaugurated in March 2013, more than ten years ago, it has been steadily providing astronomers with data that has generated more than 3000 scientific papers.

Since its inception ALMA recognized the need for keeping the observatory at the forefront of astronomy, and established the ALMA Development Program. This program promotes hardware, software, and infrastructure improvements for ALMA. Each of the ALMA partners (North America, Europe, and East Asia) administers the development program for their region, including the discussion of ideas for future developments with their com- munities, and soliciting and selecting proposals for those improvements. In 2015 the ALMA Director tasked the ALMA Science Advisory Committee (ASAC) with recommending devel- opments that ALMA should consider implementing by the year 2030. Those recommendations were collected and prioritized, and the strategic ALMA2030 Development Roadmap [1] was born.

That roadmap showcased that the original science goals of ALMA had been largely achieved, and proposed new science goals for the ALMA2030 era, based around finding the Origins of Galaxies, Origins of Chemical Com- plexity, and the Origins of Planets.

This roadmap declared several development avenues for achieving those goals with ALMA, with the Wideband Sensitivity Upgrade (WSU) as its topmost priority. The confirmation of the WSU as the first large development project for ALMA triggered the assembly of several ALMA-wide studies and Working Groups (WGs), such as the Signal Chain WG, Front End/Digitizer WG, and the Correlator WG. They generated multiple reports with recom- mendations for the upgrade of the ALMA system, and a new Integrated Operational Team (IXT), the Integrated Development Team (IDT), was chartered with creating a unified Conceptual System Design Description (CoSDD), and managing the engineering requirements for the WSU projects in collaboration with the rest of the IXTs.

In this talk we will show how the ALMA partnership has been refining the requirements and the timeline for the different WSU related developments, with the goal of having an initial WSU-wide project plan and requirements by April 2024, while at the same time the development projects have been progressing through different review stages, from Conceptual to Preliminary Design Reviews.

Transcript

1. The Wideband Sensitivity Upgrade Project The First ALMA 2030 Roadmap upgrade Juande Santander-Vela JAO Development Systems Engineer AT-RASC 2024-05-20
2. The Wideband Sensitivity Upgrade Project The First ALMA 2030 Roadmap upgrade Juande Santander-Vela JAO Development Systems Engineer AT-RASC 2024-05-20 Program
3. Talk Outline • Who am I • Quick Intro to ALMA • From Construction to Operations • The ALMA Development Program and Roadmap • The Wideband Sensitivity Upgrade • Concept • Management • Timeline • Next Steps
4. Who am I? • Juande Santander-Vela • Electronics Engineer, Software Developer, Software Analyst Background • 2009: Ph.D. in 2009 on bringing radio astronomy data into the Virtual Observatory (UGR, IAA-CSIC) • 2009-2011: Applied Scientist (ESO) • 2011: ALMA Query Interface Developer (ESO) • 2012-2013: WfEver Scientist, VIA-SKA Project Manager (IAA-CSIC) • 2014-2018: System Engineer TM, SDP (SKA Organisation) • 2018-2019: Project Scientist/Engineer (MINECON, Chile) • 2019-2022: Head of Software Development (SKAO) • 2022-: Development Systems Engineer (JAO)
5. ALMA overview • (Sub)millimeter interferometer located at 5000 m site in Atacama desert in Chile International partnership of North America, Europe, and East Asia • 66 configurable antennas mm • Array configurations between 0.16 and 16 km angular resolution as fine as 0.005'' at 950 GHz λ ≈ 0.3 − 9
6. AOS (High-site) Fact sheet • ALMA antennas at 5000 m • ALMA staff obliged to wear oxygen outside • Oxygenated building • Location of correlators OSF (Base Camp) Fact sheet • OSF is at 2900 m • Staff sleep here • Astronomers work here • Night-time observing only, with daytime observations in Santiago Santiago ALMA operation sites
9. to the atmospheric transmission windows. These windows and the tuning ranges are outlined in Figure 4.1. This illustrates the broad, deep absorption features, mostly due to H2 O in the lower few km of the atmosphere, as well as some O2 transitions. The many narrow features seen in this plot are mostly from stratospheric O3 , along with some transitions of CO and other trace species. In Cycle 9, Bands 3, 4, 5, 6, 7, 8, 9, and 10 are available, and the basic characteristics of the bands are outlined in Table 4.1. Each of the ALMA receiver bands is described in more detail in the following sections as well as in the references listed in Table 4.2. 100 200 300 400 500 600 700 800 900 1000 Frequency (GHz) 0 20 40 60 80 100 Transmission (%) Transmission in All ALMA Bands at Zenith 1 2 3 4 5 6 7 ALMA Bands and Transmission
10. From Construction to Operations • ALMA declared in Operations in 2013 (after ORR) • Some deferred capabilities (from 2005 rebaselining) became part of the ALMA Development Program. • Band 1 and Band 2 are the last Bands to be delivered to the observatory. • Band 1 already being used for Cycle 10 • Band 2 passed their Manufacturing Readiness Review, construction in progress.
13. First time all front-ends are installed!
14. ALMA Development Program • Governed by the Principles for ALMA Development Program (2013) • Addresses: • Missing Capabilities • Obsolescence • New Capabilities • Establishes funding level at 15 MUSD/year • Share is proportional to share of Operational costs
15. ALMA Development Program • Governed by the Principles for ALMA Development Program (2013) • Addresses: • Missing Capabilities • Obsolescence • New Capabilities • Establishes funding level at 15 MUSD/year • Share is proportional to share of Operational costs Key Principle: the ALMA Development Program must be driven by science – its purpose is to enhance the scientific capability and or impact of ALMA, within the bounds imposed by the availability of resources both for the development projects and for the ongoing operation of the observatory.
16. Context: Facilities in the next decade • Many wonderful new facilities coming online over the next decade • Share many of the same science themes as ALMA • origins of galaxies • origins of stars • origins of planets ALMA TMT 30 meter ESO 39 meter JWST Nancy Grace Roman Telescope ngVLA GMT 25 meter Vera Rubin Telescope Need for a cohesive ALMA roadmap with a vision that keeps ALMA relevant
17. Context: Facilities in the next decade • Many wonderful new facilities coming online over the next decade • Share many of the same science themes as ALMA • origins of galaxies • origins of stars • origins of planets • Only one ALMA! • premier telescope for sensitive, high-angular resolution submillimeter observations • a replacement for ALMA is not on the horizon, so we must continuously enhance its capabilities ALMA TMT 30 meter ESO 39 meter JWST Nancy Grace Roman Telescope ngVLA GMT 25 meter Vera Rubin Telescope Need for a cohesive ALMA roadmap with a vision that keeps ALMA relevant
18. ALMA 2030 Roadmap Process THE ALMA DEVELOPMENT ROADMAP J. Carpenter, D. Iono, L. Testi, N. Whyborn, A. Wootten, N. Evans (The ALMA Development Working Group) Approved by the Board by written procedure pursuant Art. 11 of the Board’s Rules of Procedure 2018
19. New Fundamental Science Drivers • Origins of Galaxies: Trace the cosmic evolution of key elements from the first galaxies (z>10) through the peak of star formation (z=2–4) by detecting their cooling lines, both atomic ([CII], [OIII]) and molecular (CO), and dust continuum, at a rate of 1-2 galaxies per hour. • Origins of Chemical Complexity: Trace the evolution from simple to complex organic molecules through the process of star and planet formation down to solar system scales (~10-100 au) by performing full- band frequency scans at a rate of 2-4 protostars per day. • Origins of Planets: Image protoplanetary disks in nearby (150 pc) star formation regions to resolve the Earth forming zone (~ 1 au) in the dust continuum at wavelengths shorter than 1mm, enabling detection of the tidal gaps and inner holes created by planets undergoing formation.
20. New Fundamental Science Drivers • Origins of Galaxies: Trace the cosmic evolution of key elements from the first galaxies (z>10) through the peak of star formation (z=2–4) by detecting their cooling lines, both atomic ([CII], [OIII]) and molecular (CO), and dust continuum, at a rate of 1-2 galaxies per hour. • Origins of Chemical Complexity: Trace the evolution from simple to complex organic molecules through the process of star and planet formation down to solar system scales (~10-100 au) by performing full- band frequency scans at a rate of 2-4 protostars per day. • Origins of Planets: Image protoplanetary disks in nearby (150 pc) star formation regions to resolve the Earth forming zone (~ 1 au) in the dust continuum at wavelengths shorter than 1mm, enabling detection of the tidal gaps and inner holes created by planets undergoing formation. The original science goals of ALMA were considered achieved in 2019!
21. Wideband Sensitivity Upgrade (WSU): Top Priority of the ALMA 2030 Roadmap • Upgrade of the bandwidth and throughput of the ALMA system • upgraded receivers with increased bandwidth and improved receiver temperatures • more powerful correlator • increased data reduction capacity Correlator Archives Data processing Astronomers Antennas Receivers Back end Upgrade!
22. Array Operations Site (AOS) at 5000m Operations Support Facility (OSF) at 3000m Existing Antenna to AOS Fibers IF Switches & Anti-aliasing filters Digitizers & Digital Signal Processing Data Transmission System Antenna New or upgraded components are in blue CONTROL, TelCal, Scheduling, OT, Archive, Pipeline Back End Front End Receivers New fiber 2nd Generation Correlator & Upgraded ACAS in new OSF Correlator Room The Wideband Sensitivity Upgrade
23. ALMA Management: From IPTs to IxTs • ALMA construction was based around a number of contracts, but for the more critical items Integrated Product Teams existed across the ALMA collaboration: • Antenna IPT • Front End IPT • Back End IPT • Correlator IPT • Computing IPT • Systems Engineering and Integration IPT • Site IPT
24. ALMA Management: From IPTs to IxTs • ALMA construction was based around a number of contracts, but for the more critical items Integrated Product Teams existed across the ALMA collaboration: • Antenna IPT • Front End IPT • Back End IPT • Correlator IPT • Computing IPT • Systems Engineering and Integration IPT • Site IPT Integrated Engineering Team (IET)
25. ALMA Management: From IPTs to IxTs • ALMA construction was based around a number of contracts, but for the more critical items Integrated Product Teams existed across the ALMA collaboration: • Antenna IPT • Front End IPT • Back End IPT • Correlator IPT • Computing IPT • Systems Engineering and Integration IPT • Site IPT Integrated Computing Team (ICT) Integrated Engineering Team (IET)
26. ALMA Management: From IPTs to IxTs • ALMA construction was based around a number of contracts, but for the more critical items Integrated Product Teams existed across the ALMA collaboration: • Antenna IPT • Front End IPT • Back End IPT • Correlator IPT • Computing IPT • Systems Engineering and Integration IPT • Site IPT Integrated Computing Team (ICT) Integrated Engineering Team (IET) Integrated Science Team (IST) Integrated Science Operations Team (ISOpT)
27. The Integrated Operations Teams (IxTs) ALMA Management Team (AMT) Integrated Engineering Team (IET) Integrated Computing Team (ICT) Integrated Science Team (IST) Integrated Science Operations Team (ISOpT)
28. The Integrated Operations Teams (IxTs) ALMA Management Team (AMT) Integrated Engineering Team (IET) Integrated Computing Team (ICT) Integrated Science Team (IST) Integrated Science Operations Team (ISOpT) Control, Archive, everything SW and ICT infra
29. The Integrated Operations Teams (IxTs) ALMA Management Team (AMT) Integrated Engineering Team (IET) Integrated Computing Team (ICT) Integrated Science Team (IST) Integrated Science Operations Team (ISOpT) Control, Archive, everything SW and ICT infra Engineering, including Signal chain and Infra
30. The Integrated Operations Teams (IxTs) ALMA Management Team (AMT) Integrated Engineering Team (IET) Integrated Computing Team (ICT) Integrated Science Team (IST) Integrated Science Operations Team (ISOpT) Control, Archive, everything SW and ICT infra Engineering, including Signal chain and Infra Science definitions, including science requirements
31. The Integrated Operations Teams (IxTs) ALMA Management Team (AMT) Integrated Engineering Team (IET) Integrated Computing Team (ICT) Integrated Science Team (IST) Integrated Science Operations Team (ISOpT) Control, Archive, everything SW and ICT infra Engineering, including Signal chain and Infra Science definitions, including science requirements Operational science definitions, including cycle capabilities
32. The Integrated Operations Teams (IxTs) ALMA Management Team (AMT) Integrated Engineering Team (IET) Integrated Computing Team (ICT) Integrated Science Team (IST) Integrated Science Operations Team (ISOpT) Control, Archive, everything SW and ICT infra Engineering, including Signal chain and Infra Science definitions, including science requirements Operational science definitions, including cycle capabilities Who manages the integration of development projects?
33. The Integrated Development Team ALMA Management Team (AMT) Integrated Engineering Team (IET) Integrated Computing Team (ICT) Integrated Science Team (IST) Integrated Science Operations Team (ISOpT) The Integrated Development Team oversees development projects, and request the AMT for support from the other IxTs for their own domains of expertise
34. The Integrated Development Team ALMA Management Team (AMT) Integrated Engineering Team (IET) Integrated Computing Team (ICT) Integrated Science Team (IST) Integrated Science Operations Team (ISOpT) Integrated Development Team (IDT) The Integrated Development Team oversees development projects, and request the AMT for support from the other IxTs for their own domains of expertise IDT Est. 2021
35. The Integrated Development Team ALMA Management Team (AMT) Integrated Engineering Team (IET) Integrated Computing Team (ICT) Integrated Science Team (IST) Integrated Science Operations Team (ISOpT) Integrated Development Team (IDT) The Integrated Development Team oversees development projects, and request the AMT for support from the other IxTs for their own domains of expertise IDT Est. 2021 It’s all an overall ALMA team effort!
36. Integrated Development Team EA EU NA • Shun Ishii • Gie Han Tan • Todd Hunter • Carla Crovari • Juande Santander-Vela • Tzu-Chiang Shen JAO Plus deputies!
37. JAO Development Team • In charge of managing the projects and their integration with the Joint ALMA Observatory • Lead by ALMA Deputy Director for Development, Álvaro González • Includes the JAO representatives in IDT, plus… • Christian Saldías, Development Technology & Infrastructure PM • Theodoros Nakos, Development Architect
38. JAO Development Team • In charge of managing the projects and their integration with the Joint ALMA Observatory • Lead by ALMA Deputy Director for Development, Álvaro González • Includes the JAO representatives in IDT, plus… • Christian Saldías, Development Technology & Infrastructure PM • Theodoros Nakos, Development Architect Can be considered the WSU Program Office
39. Working groups created using ALMA-wide expertise to focus on the next step definition. The WSU program planning and implementation phases
40. Working groups created using ALMA-wide expertise to focus on the next step definition. The WSU program planning and implementation phases 1 THE ALMA DEVELOPMENT ROADMAP J. Carpenter, D. Iono, L. Testi, N. Whyborn, A. Wootten, N. Evans (The ALMA Development Working Group) Approved by the Board by written procedure pursuant Art. 11 of the Board’s Rules of Procedure
41. Working groups created using ALMA-wide expertise to focus on the next step definition. We’re here! The WSU program planning and implementation phases 1 THE ALMA DEVELOPMENT ROADMAP J. Carpenter, D. Iono, L. Testi, N. Whyborn, A. Wootten, N. Evans (The ALMA Development Working Group) Approved by the Board by written procedure pursuant Art. 11 of the Board’s Rules of Procedure
42. Working groups created using ALMA-wide expertise to focus on the next step definition. We’re here! It’s a collection of projects The WSU program planning and implementation phases 1 THE ALMA DEVELOPMENT ROADMAP J. Carpenter, D. Iono, L. Testi, N. Whyborn, A. Wootten, N. Evans (The ALMA Development Working Group) Approved by the Board by written procedure pursuant Art. 11 of the Board’s Rules of Procedure
43. Working groups created using ALMA-wide expertise to focus on the next step definition. We’re here! It’s a collection of projects The WSU program planning and implementation phases → program 1 THE ALMA DEVELOPMENT ROADMAP J. Carpenter, D. Iono, L. Testi, N. Whyborn, A. Wootten, N. Evans (The ALMA Development Working Group) Approved by the Board by written procedure pursuant Art. 11 of the Board’s Rules of Procedure
44. Lots of work so far • Input from the WGs started in 2019: • Signal Chain WG • Front End/Digitizer • Second Generation Correlator • Initial CoSDD release and internal review Q2 2022. • System Requirements Review in Q4 2022 • Input from additional ICT/ ISOpT WGs in 2023 • Data Processing, Distribution, and Access • Data Acquisition • Followed by even more WGs…
45. • Second generation ICT/ISOpT WGs: • Array Calibration & Science Observing Strategies (ACSOS) • Data Model (DM) • Data Processing (DP) • Data Transfer and Archive Storage (DTAS) • User Interfaces to the Data (UID) • ISOpT WGs: • Spurious Signals • IST WGs: • Data Rates Ramp-Up Plan (DRRUP) • IET/ICT/IST/ISOpT: • Deployment Concept Lots of work so far (cont.) Collected in an updated Conceptual System Design Description (CoSDD) Also input to the ALMA System Technical Requirements
46. WSU Challenge: Don’t Disturb Science • Main message from ALMA Science Advisory Committee: minimize the WSU impact on science. • Current Deployment Concept: Parallel Deployment
47. Parallel Deployment Concept
48. Parallel Deployment Concept
49. Parallel Deployment Concept
50. When is all of this happening?
51. Top-Level Notional Timeline: From Today to WSU Operations 2024 2025 2026 2027 2028 2029 2030 Start of Cycle 16 with WSU System
52. Top-Level Notional Timeline: From Today to WSU Operations 2024 2025 2026 2027 2028 2029 2030 Start of Cycle 16 with WSU System WSU Call for Proposals WSU System Review and Program Plan Review Delta SRR/Initial Program Plan Rev. Go/ NoGo WSU
53. Top-Level Notional Timeline: From Today to WSU Operations 2024 2025 2026 2027 2028 2029 2030 Start of Cycle 16 with WSU System WSU Call for Proposals WSU System Review and Program Plan Review Delta SRR/Initial Program Plan Rev. Go/ NoGo WSU Dev Projects PDRs Dev Projects CDRs
54. Top-Level Notional Timeline: From Today to WSU Operations 2024 2025 2026 2027 2028 2029 2030 Start of Cycle 16 with WSU System WSU Call for Proposals WSU System Review and Program Plan Review Delta SRR/Initial Program Plan Rev. Go/ NoGo WSU ATAC ready for WSU integration tests OCRO construction Construction of new AOS- OSF fibers Instrumentation starts to arrive at OSF Dev Projects PDRs Dev Projects CDRs
55. Top-Level Notional Timeline: From Today to WSU Operations 2024 2025 2026 2027 2028 2029 2030 Start of Cycle 16 with WSU System WSU Call for Proposals WSU System Review and Program Plan Review Delta SRR/Initial Program Plan Rev. Go/ NoGo WSU ATAC ready for WSU integration tests OCRO construction Construction of new AOS- OSF fibers Instrumentation starts to arrive at OSF Dev Projects PDRs Dev Projects CDRs Steady retrofitting of WSU antennas #10 - #33, 2 per month Deploy WSU components at OSF in 4 antennas Deploy WSU comp. in 5 ant. @AOS Steady retrofitting of WSU antennas #34 - #66, 3 per month (TBC)
56. Top-Level Notional Timeline: From Today to WSU Operations 2024 2025 2026 2027 2028 2029 2030 Start of Cycle 16 with WSU System WSU Call for Proposals WSU System Review and Program Plan Review Delta SRR/Initial Program Plan Rev. Go/ NoGo WSU ATAC ready for WSU integration tests OCRO construction Construction of new AOS- OSF fibers Instrumentation starts to arrive at OSF Dev Projects PDRs Dev Projects CDRs Steady retrofitting of WSU antennas #10 - #33, 2 per month Deploy WSU components at OSF in 4 antennas Deploy WSU comp. in 5 ant. @AOS Steady retrofitting of WSU antennas #34 - #66, 3 per month (TBC) Science operations interleaved with WSU commissioning Science observations in separate APE WSU Science Verification & data release (TBC)
57. Top-Level Notional Timeline: From Today to WSU Operations 2024 2025 2026 2027 2028 2029 2030 Start of Cycle 16 with WSU System WSU Call for Proposals WSU System Review and Program Plan Review Delta SRR/Initial Program Plan Rev. Go/ NoGo WSU ATAC ready for WSU integration tests OCRO construction Construction of new AOS- OSF fibers Instrumentation starts to arrive at OSF Dev Projects PDRs Dev Projects CDRs Steady retrofitting of WSU antennas #10 - #33, 2 per month Deploy WSU components at OSF in 4 antennas Deploy WSU comp. in 5 ant. @AOS Steady retrofitting of WSU antennas #34 - #66, 3 per month (TBC) Science operations interleaved with WSU commissioning Science observations in separate APE WSU Science Verification & data release (TBC) Online software TRR and E2E tests Data Processing Transition Development and Commissioning of SW/ Comp/SciOps deliverables for WSU AIVC Planning of WSU Software / Computing / Sci Ops deliverables Design/ Development/ Deployment/ Commissioning of SW/Comp/SciOps deliverables
58. Next Steps • Advanced Technology ALMA Correlator (ATAC) and OSF Correlator Room (OCRO) PDRs in week of June 10th • Delta SRR and Initial Program Plan Review in week June 9th • WSU IF Processor (Digital Backend and IF Switch/Contitioner) PDR in October/November 2024 • Data Transmission Subsystem PDR also in October/November 2024 • WBS and Cost Review in November 2024 • WSU System Review in March 2025 • WSU Approval from ALMA Board, expected April 2025
59. Next Steps (in parallel) • Ongoing work on the Assembly, Integration, Verification, and Commissioning (AIVC) Plan, expected ~September. • Main task: to verify dates, efforts, and feasibility of Parallel Deployment concept. • Additional work on the Data Processing transition, also expected ~September. • Mostly focused on the ALMA-specific needs for the next generation processing architecture.
60. Conclusions • The Wideband Sensitivity Upgrade (WSU) is moving forward in definition. • The core of the WSU (enhanced signal chain with new digitization, correlation, and data processing) is expected to be available in Cycle 16* (October 2029). • Lot’s of work for preparation already carried out, with final green light expected in ALMA Board for April 2025. * Planning in progress, and all usual caveats
61. One more thing…
62. Other ALMA Talks at AT-RASC • May 21st, 10:00-10:20: “Spectrum management and radio frequency interference at ALMA”, by Giorgio Siringo and Sean Dougherty. (Session EACFJ, Room E1: Latest news and observatory report) • May 22nd, 9:00-9:20: “ALMA – Observatory Report”, by Sean Dougherty et al. (Session J11, Room J2: Latest news and observatory report)
63. Other ALMA Posters at AT-RASC • Poster Session J, Electromagnetic Analyses and Characterization of the ALMA Band 6 Receiver Optics, Lehmensiek Robert et al.
64. Thank you! Questions?
65. T he Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of Europe, North America and East Asia in cooperation with the Republic of Chile. ALMA is funded in Europe by the European Southern Observatory (ESO), in North America by the U.S. National Science Foundation (NSF) in cooperation with the National Research Council of Canada (NRC) and the National Science Council of Taiwan (NSC) and in East Asia by the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Academia Sinica (AS) in Taiwan. ALMA construction and operations are led on behalf of Europe by ESO, on behalf of North America by the National Radio Astronomy Observatory (NRAO), which is managed by Associated Universities, Inc. (AUI) and on behalf of East Asia by the National Astronomical Observatory of Japan (NAOJ). The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.
66. Additional Slides
67. Future Developments at the ALMA Observatory John Carpenter Joint ALMA Observatory Science with the Hubble and James Webb Space Telescopes VII: Stars, Gas, & Dust in the Universe 29 April - 2 May 2024
68. ALMA overview • (Sub)millimeter interferometer located at 5000 m site in Atacama desert in Chile - international partnership of North America, Europe, and East Asia • 66 configurable antennas • mm • Array configurations between 0.16 and 16 km - angular resolution as fine as 0.005 at 950 GHz λ ≈ 0.3 − 9 ′ ′
69. ALMA operation sites AOS (High-site) Fact sheet • ALMA antennas at 5000 m • ALMA staff obliged to wear oxygen outside • Oxygenated building • Location of correlators OSF (Base Camp) Fact sheet • OSF is at 2900 m • Staff sleep here • Astronomers work here • Night-time observing only, with daytime observations in Santiago Santiago
70. ALMA Capabilities Spectroscopy Continuum Polarization VLBI Imaging 10 receiver bands
71. A survey of gas, dust, and stars in star-forming galaxies when the Universe was ~1 Gyr old (4 ≲ z ≲ 6) [CII] 158 μm Herrera-Camus and the CRISTAL Large Program Team
72. Herrera-Camus et al. in prep. Gas, dust and stars on kiloparsec scales when the Universe was 1 Gyr old
73. ALMA / JWST images of nearby galaxies ALMA Carbon Monoxide images JWST near/mid-infrared images • Probes “fuel” for star formation on scale of individual GMCs • Cloud masses, surface density, pressure, etc… vs. environment • Traces embedded stars • Measures star formation rate vs. environment PHANGS collaboration
74. Hunting for (proto)planets ALMA JWST Tracers of embedded planets •annular gaps in the dust continuum •kinematic distortions in the Keplerian velocity field •circumplanetary disks Dust continuum Carbon monoxide (single velocity) Wagner et al (2024) Cugno et al. (2024) Pinte et al. (2019) Tracers of embedded planets •direct detection of planets •spiral features in scattered light SAO 206462 F187N protoplanet location HD 97048
75. Spectroscopy of circumstellar disks Booth et al. (2024a, b) van Dishoeck et al. (2023) ALMA JWST Spectroscopic probes of the chemistry in the outer (ALMA) and inner (JWST) disk •implications for radial transport and radial variations in chemical composition
76. New facilities in the next decade • Many wonderful new facilities coming online over the next decade • Share many of the same science themes as ALMA - origins of galaxies - origins of stars - origins of planets • Only one ALMA! - premier telescope for sensitive, high-angular resolution submillimeter observations - a replacement for ALMA is not on the horizon, so we must continuously enhance its capabilities ALMA TMT 30 meter ESO 39 meter JWST Nancy Grace Roman Telescope ngVLA GMT 25 meter Vera Rubin Telescope
77. ALMA Development Roadmap Carpenter et al. (2018, arXiv 1902.02856)
78. Wideband Sensitivity Upgrade (WSU): Top Priority of the ALMA 2030 Roadmap • Upgrade of the bandwidth and throughput of the ALMA system - upgraded receivers with increased bandwidth and improved receiver temperatures - more powerful correlator - increased data reduction capacity Correlator Archives Data processing Astronomers Antennas Receivers Back end Upgrade!
79. The Wideband Sensitivity Upgrade Array Operations Site (AOS) at 5000m Operations Support Facility (OSF) at 3000m Existing Antenna to AOS Fibers IF Switches & Anti-aliasing filters Digitizers & Digital Signal Processing Data Transmission System Antenna New or upgraded components are in blue CONTROL, TelCal, Scheduling, OT, Archive, Pipeline Back End Front End Receivers New fiber 2nd Generation Correlator & Upgraded ACAS in new OSF Correlator Room
80. Wideband Sensitivity Upgrade: Overview • Available bandwidth • Correlated bandwidth • Observing speed Factor of 2-4 increase in the available IF bandwidth. ALMA 2030 Band 2 Band 6 Band 8 Band 1 Band 3 Band 4 Band 5 Band 6 Band 7 Band 8 Band 9 Band 10 Available instantaneous bandwidth per polarization (GHz) 0 8 16 24 32 Current receivers (2SB unless noted) Under development / construction Goal 4x upgrade (goal) 2x upgrade Goal DSB DSB
81. Wideband Sensitivity Upgrade: Overview • Available bandwidth • Correlated bandwidth • Observing speed Band 1 Band 2 Band 3 Band 4 Band 5 Band 6 Band 7 Band 8 Band 9 Band 10 Factor increase in correlated bandwidth 0 10 20 30 40 50 60 70 Low spectral resolution High spectral resolution High spectral resolution ~ 0.1 km/s
82. Wideband Sensitivity Upgrade: Overview • Available bandwidth • Correlated bandwidth • Observing speed Increase in Band 6 observing speed with ALMA 2030 Observing mode Increase in speed over current system* Continuum 4.8x (with goal of 9.6x) Spectral line 2.2-4.7x Increase in observing speed results from • improved receiver temperatures • improved digital efficiency • wider bandwidth (continuum) Spectral scans will see further speed increases due to larger correlated bandwidth. * To reach same sensitivity as current system with single tuning
83. The power of molecular spectroscopy in disks • Gas mass - dust traces only ~ 1% of the total disk mass - use molecules to trace the dominant disk component (H2 ) • Chemistry and the chemical compositions of planets • 3D velocity and temperature structure of disks • Detect embedded planets through velocity distortions • With vastly improved spectral grasp and improved line (and continuum!) sensitivity, the Wideband Sensitivity Upgrade will be a tremendous advance for disk studies. Dust HD 163296 Öberg et al. (2021)
84. The WSU Advantage c-C3 H2 3(3,0)-2(2,1)
85. The WSU Advantage c-C3 H2 3(3,0)-2(2,1)
86. The WSU Advantage Band 6v2 IF=12 GHz c-C3 H2 3(3,0)-2(2,1)
87. The WSU Advantage Band 6v2 IF=12 GHz c-C3 H2 3(3,0)-2(2,1)
88. The WSU Advantage Band 6v2 IF=12 GHz SiO J=5-4 c-C3 H2 6(0,6)-5(1,5) HC3 N J=24-23 C17O J=2-1 H2 CO 3(2,1)-2(2,0) C15N N=2-1 H2 S 2(2,0)-2(1,1) c-C3 H2 3(3,0)-2(2,1) SO 3Σ 6(5)-5(4) SO2 11(1,11)-10(0,10) c-C3 H2 5(2,3)-4(3,2) 13CS J=5-4 C34S J=5-4 HC3 N J=28-27 t-HCOOH 11(2,10)-10(2,9) SO 3Σ 2(3)-3(2) SO 3Σ 8(9)-8(8) SO 3Σ 5(6)-4(5) c-C3 H2 5(3,3)-4(2,2) HC18O+ J=3-2 HC3 N J=25-24 H2 CS 7(0,7)-6(0,6) CS J=5-4 HC3 N J=27-26 CN N=2-1 t-HCOOH 10(4,6)-9(4,5) H2 CO 3(1,2)-2(1,1) c-C3 H2 4(3,2)-3(2,1) c-C3 H2 3(2,1)-2(1,2) H2 CS 7(1,6)-6(1,5) SO2 10(5,5)-11(4,8) NO J=5/2-3/2 DCO+ J=3-2 … and up to 40 additional spectral windows!
89. Star formation Class I Class II 300 AU Envelope DCO+ Outflow cavity CCH Hot core HCOOH Sakai et al. (2017) Tychoniec et al. (2021) Low-velocity flow CO High velocity jet SiO Sputtering CH3 OH Centrifugal barrier CCH
90. Molecular probes of star formation with ALMA 2030 Tychoniec et al. (2021)
91. Molecular probes of star formation with ALMA 2030 Tychoniec et al. (2021)
92. Probing the origins of galaxies Zheng et al. (2017) McLead et al. (2016) MACS1149-JD zphot = 9.44 ± 0.12 • Candidate galaxy at photometric redshift of z=9.4 • Universe only 500 Myr old! • Spectroscopy needed to determine redshift - large uncertainties - contaminants at lower redshift
93. ALMA spectral scan search for Oxygen in MACS1194-JD zphot = 9.44 Redshift probability distribution
94. ALMA spectral scan search for Oxygen in MACS1194-JD zphot = 9.44 Hashimoto et al. (2018) z=9.11 zspec = 9.11 Redshift probability distribution
95. ALMA spectral scan search for Oxygen in MACS1194-JD zphot = 9.44 Hashimoto et al. (2018) • ALMA 2030 upgrade will be at least 3 times faster plus any improvements from lower receiver noise z=9.11 zspec = 9.11 Redshift probability distribution
96. Summary • Technical upgrades - Available bandwidth : factor of 2-4 increase - Correlated bandwidth : more than an order of magnitude increase with ~ 0.1 km / s resolution - Observing speed : 2.2-4.7x faster for spectral lines, 4.8x faster for continuum (Band 6 upgrade) • Scientific impact - Planet formation : comprehensive studies of physical, kinematic, and chemical structure of disks - Star formation : efficient surveys of all stages in the star formation process - Galaxy formation : probe the formation and evolution of galaxies across cosmic time • First wideband receivers for ALMA - Band 2 : production to start in 2023 - Band 6 : prototype under development - Band 8 : proposal to be submitted to ALMA Board in November 2023 • Digital signal chain - Correlator (ATAC), Data Transmission System (DTS), and Digitizers under construction; new AOS-OSF fiber under study WSU Description: a) ALMA Memo 621 b) arXiv 2211.00195 Goal is to have first science with the WSU by end of the decade.
97. Beyond the WSU … follow the Roadmap! • Main science goals of the ALMA Roadmap - Origins of Galaxies - Origins of Chemical Complexity - Origins of Planets • WSU provides large gains in spectral grasp - further increases in spectral grasp beyond WSU are more limited - significant increases in sensitivity from lower receiver noise are also limited since receivers approaching quantum limit • Next steps in the ALMA Development Roadmap - more collecting area (i.e., more antennas!) for significant increases in sensitivity (5-10x!) - longer baselines open exciting possibilities for improved angular resolution - community-led workshops will be held to discuss ideas • ALMA is just scratching the surface to identify embedded planets in disks by measuring velocity perturbations • Also mapping the chemical composition of disks to understand the formation of planets • Clear synergy with planet searches and infrared spectroscopy by JWST and AO imaging on large telescopes • JWST is discovering significant populations of galaxies at very high redshifts (z > 10), when Universe was < 500 Myr old • ALMA can probe the build-up of the ISM and measure dynamical masses z = 9.1