ngVLA計画概要と日本における活動報告、SWG-Jの活動とサイエンスケースの紹介
永井 洋（国立天文台）
On Behalf of ngVLA Study GroupA next-generation Very Large Array (ngVLA)
Next generation Very Large Array (2034-)

Very Large Array (1980-)

X 10 sensitivity
X 40 angular resolution

 27 x 25-meter antennas
 Max resolution 40 mas
 73 MHz – 50 GHz

 Project led by NRAO
 Seeking ~25% contribution frominternational partners

 248 x 18-meter +19 x 6-meter antennas
 Max resolution 1 mas (and 0.1 mas with LBA)
 1 GHz – 116 GHz (Bridging SKA and ALMA)

Timeline:
2024 – Construction Begins
2028 – Early Science
2034 – Full Science Operations

ngVLA Key Science Goals(ngVLA memo #19)
1. Unveiling the Formation of Solar System Analogues on Terrestrial Scales
2. Probing the Initial Conditions for Planetary Systems and Life with Astrochemistry
3. Charting the Assembly, Structure, and Evolution of Galaxies Over Cosmic Time
4. Using Pulsars in the Galactic Center as Fundamental Tests of Gravity
5. Understanding the Formation and Evolution of Stellar and Supermassive
BH’s in the Era of Multi-Messenger Astronomy
ngvla.nrao.edu

Array Components
Main Array (MA)Short Baseline Array (SBA)Long Baseline Array (LBA) 214 x 18m offset Gregorianantennas
 Up to 1000 km baselines
 Fixed antenna locations near VLAsite 19 x 6m antennas
 4 x 18m in TP mode to fill in (u, v)hole for imaging extended
structure 30 x 18m antennas locatedacross continent for baselines up
to ~9000km
 Operate in VLBI mode Max angular resolution = 0.1 mas

RadiusCollecting Area Fraction

0 km < R < 1.3 km

44%

1.3 km < R < 36 km

35%

36 km < R < 1000 km

21%

Receiving Bands
Six frequency bands covering 1.2 – 116 GHz are planned. Highest frequency
resolution is 400 Hz (0.1 km/s at 1.2GHz) and highest instantaneous
bandwidth is 20 GHz per pol.
Band#fLGHzfH
GHzRF BWGHzMajor Emission Line

12
3
45
6

1.2
3.5
12.3
20.5
30.5
70.0

3.5
12.3
20.5
34.0
50.5
116

2.3
8.8
8.2
13.5
20.0
46.0

HI
H2CO
H2O, NH3SO, SiO, CH3OH, CS
CO, HCN, HCO+, DCN

Angular Resolution

Terrestrial zone planet formation: 1AU @ 140pc

100 Rs @ z=0 10 x higher angularresolution than ALMA if
we compare the highest
angular resolution.
 100 x times higher if wecompare the at theoverlap frequency(100GHz) LBA adds 10x resolution
 10mas = 1AU at 140pc= 80pc at z = 3
 0.1mas = 100Rs at z = 0

Sensitivity
Assuming 1 hour integration

Bridging SKA & ALMA
Complementary suite from cm to submm arrays for the mid-21st century
 < 0.3cm: superb forchemistry, dust, finestructure lines, andwarm dust continuum 0.3 to 3cm: ngVLA
superb for terrestrial
planet formation, dense
gas history, baryon
cycling > 3cm: SKA superb forpulsars, reionization, HI+ continuum surveys

Concept Development in the US
Initiate science
NRAO ngVLA
investigation at AAS Project officelaunched
Technical workshop
SAC formed

Science casedevelopment byWG

Science bookpublished

Submitted toAstro2020

Optics workshop

ngVLA-SKA
alliance meeting

TAC formed
Science workshop

Communitystudies program

Session at URSI

System designreference
published

Workshops

Astro2020
reportWorkshops
Workshops

2015

2016

2017

Astrophysical Frontiers Conference November 20182018

Science Book2019

2020

Radio/MM Astrophysical Frontiers Conference July 2019

Status in Japan20192020

NAOJ ngVLA Study GroupngVLA Workshop

ngVLA Kickoff Meeting Established April 2019
 Purpose: Stimulate community
interest and promote ngVLAGroup lead: D. Iono (NAOJ)
Project scientist: M. Momose (Ibaraki)
Technical lead: A. Gonzalez (NAOJ)

 Sep 17-20, 2019 @ NAOJ, Mitaka
 Purpose: 1st international ngVLA
workshop to promote ngVLA inJapan ~100 participants 34 talks, 4 posters

 Jan 31, 2020 using Zoom
 Purpose: introduction to ngVLAand science prospects
 81 participants

ngVLA workshop
Sep 2019, NAOJ Mitaka

Science Working Groups
OutputGoalCompile ngVLA science use cases tuned to the Japanesecommunity

 ngVLA-J Memo series
 ngVLA-J Science Book

Science Working Groups (SWGs)
1. 惑星形成と惑星系円盤
2. 様々な天体階層における星形成と星間化学)
3. 宇宙史の中での銀河進化
4. 銀河中心パルサーを用いた重力理論の検証
5. ブラックホールの形成・進化とタイムドメイン・マルチメッセンジャー天文学

Timeline

2020 1

The contents of the memo series will
be used as the basic material for theScience Book, which will be written inplain Japanese language.

ASJ
Special session

ASJ
2

Kickoff Meeting

3456

SWG Meetings

7891011SWG Workshop

122021 1Memo Series

234567Science Book

8910

Science Working GroupsGroup Leads
SWG1

SWG2

SWG3

Advisory
SWG4

SWG5

M. Fukagawa
NAOJ

K. Kohno

University of Tokyo

M. Momose

Ibaraki University

K. Tachihara

D. IonoNagoya University

NAOJ

K. Niinuma

Yamaguchi University

H. Nagai
NAOJ

A. Gonzalez
NAOJ

T. Hasegawa
NAOJ

N. Sakai
Riken

SWG1

SWG2

SWG3

SWG4

SWG5
othersSWG5会合履歴
第1回 5/28（参加者約40名）
今西昌俊 Molecular gas around actively massaccreting supermassive black holes
泉琢磨 高空間分解能で探るAGN直近の物理・化学的性質
秦和弘 AGN/SMBHジェット
竹川俊也 銀河系中心領域における中間質量ブラックホールの探査
稲吉恒平 Hunting of hidden wandering massive BHs with ngVLA- From ALMA to ngVLA –第2回 9/3 (SWG4との合同開催、参加者約40名)
出口真輔 ファラデートモグラフィー
沖野大貴 Global VLBI + ngVLAで探るAGNジェット形状
澤田佐藤聡子 1ミリ秒角分解能観測が暴くAGNサブパーセク領域の分子多相構造
笹田真人 重力波観測ランO3における電磁波対応天体の探査と今後の展開
浦田裕次 Gamma-ray bursts & Transient Science
SWG1-4も同様に2回のオンライン会合を実施

SWG5のサイエンスケースの一部紹介
秦これまでのVLBI観測を発展させ、個別天体の研究から統計へ

澤田佐藤

沖野SWG5のサイエンスケースの一部紹介

竹川稲吉
笹田

米国版サイエンスケース

17ngvla.nrao.edu

appendix

18

The Formation and Evolution of Black Holes in theEra of Multi-Messenger Astronomy
Supermassive Black Hole Pairs and Binaries

Burke-Spolaor, S.; Blecha, L.; Bogdanović, T.; Comerford, J. M.; Lazio, J.; Liu, X.; Maccarone, T.
J.; Pesce, D.; Shen, Y.; Taylor, G.

Compact Binary Mergers as Traced by Gravitational Waves

Corsi, A.; Frail, D. A.; Lazzati, D.; Carbone, D.; Murphy, E. J.; Owen, B. J.; Sand, D. J.;
O'Shaughnessy, R.

Radio Emission from Short Gamma-ray Bursts in the Multi-messenger Era

Lloyd-Ronning, N.

Revealing the Galactic Population of Black Holes

Maccarone, T. J.; Chomiuk, L.; Strader, J.; Miller-Jones, J.; Sivakoff, G.

Local Constraints on Supermassive Black Hole Seeds from a Next Generation
Very Large Array

Plotkin, R. M.; Reines, A. E.

Accretion and Jets in Local Compact Objects

Coppejans, D. L.; Miller-Jones, J. C.; Körding, E. G.; Sivakoff, G. R.; Rupen, M. P.

Tidal Disruption Events

van Velzen, S.; Bower, G. C.; Metzger, B. D.

Intermediate-Mass Black Holes in Globular Cluster Systems

Wrobel, J. M.; Miller-Jones, J. C. A.; Nyland, K. E.; Maccarone, T. J.

Science with Pulsar Timing Arrays and the ngVLA

Chatterjee, S.

Offset Active Galactic Nuclei

Blecha, L.; Brisken, W.; Burke-Spolaor, S.; Civano, F.; Comerford, J.; Darling, J.; Lazio, T. J. W.;
Maccarone, T. J.

Serendipitous Fast Transient Science with the ngVLA

Law, C. J.; Bower, G. C.; Burke-Spolaor, S.; Butler, B. J.; Demorest, P.; Lazio, T. J. W.; Linford,J. D.

19Flares from Coalescing Black Holes in the Centimeter-Wavelength Transient SkyRavi, V.

SMBH related science categorized in other
Key Science Goals
An ngVLA Wide Area AGN Survey

Kirkpatrick, A.; Hall, K.; Nyland, K.; Lacy, M.; Prandoni, I.

High-resolution Imaging of Radio Jets Launched by Active Galactic Nuclei:
New Insights on Formation, Structure, and Evolution Enabled by the ngVLA

Lister, M. L.; Kellermann, K. I.; Kharb, P.

From Megaparsecs To Milliparsecs: Galaxy Evolution and Supermassive
Black Holes with NANOGrav and the ngVLA

Taylor, S. R.; Simon, J.

Probing Obscured Massive Black Hole Accretion and Growth since Cosmic
Dawn

Rujopakarn, W.; Nyland, K.; Kimball, A. E.; Prandoni, I.

Young Radio AGN in the ngVLA EraPatil, P.; Nyland, K.; Harwood, J. J.; Kimball, A.; Mukherjee, D.

Precision Gas-dynamical Mass Measurement of Supermassive Black Holes
with the ngVLA

Boizelle, B. D.; Nyland, K.; Davis, T. A.

Radio Jet-ISM Feedback on Sub-Galactic Scales

Nyland, K.; Mukherjee, D.; Lacy, M.; Prandoni, I.; Harwood, J. J.; Alatalo, K.;
Bicknell, G.; Emonts, B.

Accreting Supermassive Black Holes in Nearby Low-Mass Galaxies

Nyland, K.; Alatalo, K.

How Do20
Cold Gas Outflows Shape Galaxies?

Bolatto, A. D.; Armus, L.; Leroy, A. K.; Veilleux, S.; Walter, F.; Mushotzky,R.

Contexts• SMBH Formation• Search for SMBH binaries, offset AGNs, low mass AGNs, IMBH in Globularclusters, TDEs

• Stellar BH Evolution• Increasing the sample of stellar mass BHs• SMBH-Galaxy Evolution• AGN outflow/jet feedback• Jets/Accretion Physics• Disk-Jet connection, Jet production• AGN Survey• Radio-quiet AGNs, Dust-obscured AGNs
21

Supermassive Black Hole Pairs andBurke-Spolaor et al.
Binaries22Searching dual AGNs allowing for merger-rate estimates
to constrain PTA searches (Synergy with NANOGrav).

Local Constraints on Supermassive Black HoleSeeds from ngVLA
Plotkin & Reines• Seach for massive(not supermassive)
BH in nearby lowmass galaxies
log LR = 0.6 log LX + 0.78 log MBH + 7.33
(e.g., Merloni et al. 2003; Falcke et al. 2004;
Plotkinet al. 2012),

23

IMBH in Globular Cluster Systems
Wrobel et al.

24

Tidal Disruption Eventsvan Velzen et al.

25

An ngVLA Wide Area AGN Survey
Kirkpatrick et al.

Propose a 10 deg2 survey in the Stripe 82 field using the 8 GHz band with an rms depth of 1 μJy beam−1. We willdetect ∼130,000 galaxies, including radio-quiet AGN out to z ∼ 7.
26

Key Performance Matrix

Key Operation Concepts
Proposal Evaluation
Peer review system will beadopted. Proposals will beevaluated based on scientificmerit and technical feasibility

Time Allocation

Dynamic SchedulingPIs awarded time and notsensitivity.This is different
from ALMA

Time allocated dynamicallyaccording to the priority built
into the queue.

Array Availability

Data Product28 will automatically
Pipeline
generate Science Ready Data
Products for most standard
projects (~80%). Expert
mode will exist too.

Operated from theArray Operation Centerin Socorro NM

No reconfiguration, meaningthat the array will used
continuously with minimum
downtime. Subarrays will be
used for maintenance andcommissioning activities