Sciences with ngVLA
MOMOSE, Munetake(Ibaraki Univ., Project Scientist)

ngVLA: Key features• Goal: 10x collecting area of JVLA/ALMA

http://ngvla.nrao.edu/‣ 18m dishes x 214 (160μm surface)• Frequency range: 1.2 –116 GHz‣ bridging between ALMA and SKA• Spatial resolution: 10x better than JVLA/ALMA‣ Thermal imaging at “mas” resolution with baseline up to 300–1,000 km• Start early science operation in ~2028, full operation in ~2034

5 Key Science Goals(ngVLA memo #19)
• Unveiling the Formation of Solar System Analogues• Probing the Initial Conditions for Planetary Systems and Life with
Astrochemistry• Charting the Assembly, Structure, and Evolution of Galaxies Over
Cosmic Time

• Using Pulsars in the Galactic Center as Fundamental Tests of Gravity• Understanding the Formation and Evolution of Stellar andSupermassive BH’s in the Era of Multi-Messenger Astronomy

KSG1 : Unveiling the Formation of Solar System
Analogues• orbital motion of planets and related
features on monthly timescales‣ simulated 100 GHz ngVLA

observations of a newborn planetarysystem comprising a Jupiter analogue
orbiting at 5 au from a Solar type star

Ricci et al. (2018)

KSG1 : Inner regions are optically thick at
submm wavelengths
HL Tau Disk image at λ=1mm with ALMA

ngVLA will
cover this area

ALMA
partnershipet al. (2015)
1asec = 140au

KSG2 : Probing the Initial Conditions forPlanetary Systems and Life with Astrochemistry• simulated line survey towards Sgr. B2‣ a line of “pre-biotic” molecules with T=200K, N=1012-14 cm-2 will be detectable without confusion

Credit: Brett McGuire (NRAO)KSG2 : Importance of N-bearing molecules• a building block for a larger N-bearing molecules (including NH2CHO, glycine, etc.)• information about the location of NH3 snowline in a protoplanetary disk
NH3

(figure from wikipedia)

inversion transition@ 23GHz(λ≈1.3cm)

The temperature structure andits evolution in the disk are determinedby various factors

KSG3 : Charting the Assembly, Structure, and Evolutionof Galaxies from the First Billions Years to the Present• simulated images of SMG (SFR=400M⦿/yr) at z=4.4‣ higher-J transitions of CO are not inadequate to reveal dense & cold molecular clouds forming new stars

Credit: Caitlin Casey (UT Austin)KSG3 : “Cold” molecular clouds as high as z ≈ 5• CO, the fundamental tracer of molecular clouds• higher-J transitions of CO are not inadequate to reveal dense & cold molecular clouds forming new stars
Density of MCs (as a function of z)
Gas

NGVLA

ALMA
(red) Constraints by ALMA
spectroscopic survey towards HUDF
(green) ngVLA will improve the estimate
Decarli+2016

KSG4 : Using Pulsars in the Galactic Center as
Fundamental Tests of Gravity• The ngVLA sensitivity and frequency

coverage will probe deeper than currently
possible into the GC area looking forpulsars, which are moving clocks in thespace-time potential of Sgr A*• New tests of theories of gravity,

constraints on exotic binaries, SF history,
stellar dynamics and evolution, and ISM
at the GC• Estimates are as high as 1,000 PSRs.

Only known example is PSR J1745-2900
magnetar, which are extremely rare (<1%)
Credit: R. Wharton

KSG5 : Understanding the Formation and Evolution ofBlack Holes in the Era of Multi-Messenger Astronomy• Unaﬀected by dust obscuration andwith the angular resolution to separate
Galactic sources from backgroundobjects using proper motions, thengVLA will enable a search for accreting
black holes across the entire Galaxy.

• Key to understanding GW discoveries

An artist’s impressionof NS merger
Credit: ESO

Credit: LIGO/VIRGO

Science meeting in Japan
https://alma-intweb.mtk.nao.ac.jp/~ngvla/workshops/mitaka2019/• Sep. 17-19, 2019 at NAOJ Mitaka• ~ 100 participants in Japan, Taiwan,
Korea, with NRAO key personnel• Many “original” ideas‣ Diversified science fields (e.g., Sun andsolar system)‣ Synergies with other projects in Japan‣ Related to ALMA/SKA science cases(e.g., molecular/HI/ionized gas)

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Working Groups
in Japan• Review the science cases listed in the “Science Book” & “White Papers”‣ http://aspbooks.org/a/volumes/table_of_contents/?book_id=592‣ https://ngvla.nrao.edu/page/scicase• Discuss our original ideas to be reflected in the ngVLA-J’s “Project book”
and memosKSG programs vs. other science
Driving Case & Possible Pilot

Type

Band(s)Tsubarray (hours)

SubarrayYear 1

Year 2

Year 3

KSG1 Taurus disks

Continuum

6, 4

176

305

305

Main

KSG2 Sgr B2(N), IRAS 16293

Molecules

5, 4, 3

120

120

0

Main

KSG3 COSMOS

CO

5, 4, 3

105

105

105

KSG3 Spiderweb galaxy

Molecules

6, 5, 4

123

0

0

ngVLA
Reference
Observing
Program

KSG3 Virgo cluster galaxy

Molecules

6

132

132

KSG3 M81 grp, in galaxies

HI

1

213

KSG3 M81 grp, near galaxies

HI

1

KSG4 Galactic Center pulsars

Continuum

Synopsis

KSG5 LIGO events

Note

Done

Plains + Core
Main

Half done

132

Plains + Core

Slow progress

213

213

Plains + Core

264

264

264

Core

3

99

99

99

Main

Continuum

1

142

142

142

Main

KSG5 LIGO proper motions

Continuum

3

470

470

470

Long Baseline

KSG5 LISA events

Continuum

4

0

0

400

Plains + Core

KSG5+4 Stellar BHs, Pulsars

Continuum

2

169

169

169

Plains + Core

KSG5 Pulsar Timing ArrayContinuum

1, 2

312

312

312

Mid Baseline

Total Hours for Key Science Goals (KSGs)

~1550

~1560

~1840

Total Hours for Other Science = 6000 – KSG Hours

~4450

~4440

~4160

21
courtesy:
Eric Murphy (NRAO; project scientist)

Co-observe

Co-observe
Skip Mid, Long

Relationship with SKA
SKA and ngVLA Key Science Drivers
CosmicDawn/EoR

Cradle of Life
Transient /FRB Searches

Extragalactic
ContinuumStudies(3cm)

Cosmology

Low & High-z
HIcourtesy: Eric Murphy (NRAO)

Prebiotics(3, 7, 10mm)
Pulsars
Searches &TimingCosmicMagnetism

PlanetFormation

Extragalactic
Molecular Gas

GC Pulsars
Stellar-Mass
Black Holes
Local Group HI

LIGO/LISA
Follow-Up

Relationship with SKA
SKA and ngVLA Key Science Drivers
Wide FOV

Cosmic 2~10,000 deg
Dawn/EoR

2
Cradleof Life<<1 deg

Transient / 2~30,000 deg
FRB Searches

Extragalactic
Continuum~1,000
deg2
Studies(3cm)

Cosmology~30,000
deg2

Low & High-z~1,000 deg2
HIcourtesy: Eric Murphy (NRAO)

GC<<1Pulsars
deg2

Local
<10Groupdeg2 HI

Pinpoint Imaging

Prebiotics<1 deg2(3, 7, 10mm)
Pulsars
Searches>1,000
deg&2
TimingCosmic 2~30,000 deg
Magnetism

Planet 2<<1 deg
Formation

Extragalactic~3 deg2
Molecular Gas

Stellar-Mass~10 deg2Black Holes
LIGO/LISA<10 deg2
Follow-Up

Relationship with SKA
SKA andandngVLA
ngVLAKey
KeyScience
ScienceDrivers
Drivers
SKA
SKA HPSO’s require >103 x more survey area<< 1 deg2(3 cm)

Cradle of Life

Total: ~90,000 deg2

courtesy: Eric Murphy (NRAO)> 1000 deg2

Pulsars
Searches

LIGO/LISA Extragalactic
Follow-Up Prebiotics
Molecular

GC Pulsars<< 1 deg2< 10

GC Pulsars
Local Group HI~ 1000 deg2

~ 1000 deg2

Extragalactic
Continuum~ 10,000 deg2

Cosmic Dawn/ EoR

Low & High-z
HI(3, 7, 10mm)

Low &High-z HI

Cosmology

Pulsars
Searches &TimingTotal: ~40 deg2<< 1 deg2
Molecular Gas(3, 7, & 10 mm)

PlanetFormation(3cm)

Transient /FRB Searches~ 30,000 deg2

Transient / FRB

CosmicMagnetism~ 30,000 deg2

~ 30,000 deg2

Cosmic Magnetism

Extragalactic
ContinuumStudiesCosmology

CosmicDawn/EoR

PlanetExtragalactic
Formation

Cradle of Life

Local Group HI

Overlap< 10 deg2

LIGO/LISA
Follow-Up

~ 10

~3

<< 1

deg2

Prebiotics
Stellar-Mass
Stellar-Mass
Black
Holes

Black HolesQuestions ?

Discussion

Initiating science working groups in JP
KSG1
KSG4

• Thank you for your interest !
• The community’s interests cover wide areas40

of potential sciences with ngVLA• Please join science working group(s) and32• “Others” include:‣ Molecular clouds formation (1)‣ Evolved stars (1) / Sun (1)‣ Engineering (1)/Telescope system (1)• A new member is always welcome# of People

enjoy the discussion !

KSG2
KSG5

37
32

Total 143
from 90 individuals(As of March 30th)

32

25

24
16

12

8
0

KSG3
Others5
Category

How do we proceed discussion ?
• Tentative Leaders‣ SubWG 1: Momose, M. (Ibaraki)‣ SubWG 4: Niinuma, K. (Yamaguchi)‣ SubWG 2: Tachihara, K. (Nagoya)‣ SubWG 5: Nagai, H. (NAOJ)‣ SubWG 3: Iono, D. (NAOJ)‣ Others: contact individually• Each SubWG works independently, but a joint meeting of multiple SWGs will also
be possible if needed‣ The style of the meeting would be at the discretion of each leader‣ Remote connection (ZOOM) and mailing lists can be cared by NAOJ

Timeline• 2020. 4: initiating SWGs, start discussion‣ Review the science documents in NRAO site
‣ Our original ideas• 2021. 7 or 8 : Project Book in Japanese‣ Summarize the discussions in all SWGs
‣ The (tentative) leader of each SWG + the members of the study group in NAOJ
will be the main authors of the project book

‣ Comments by advisory members & all the working group members

Possible products from SWGs
• Any inputs to the project book (either English or Japanese)• Original article for ngVLA(-J) memo series (English, style-file will be
provided)• Original research paper for refereed journal and arXiv (English or
Japanese)Questions ?