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NATIONAL RADIO ASTRONOMY OBSERVATORY
2017223
The Next Generation Very Large Array
A next genera*on VLA • Thermal imaging at milli-arcsecond resolu8on • 10x effec(ve area and resolu(on of JVLA • ~300x18m antennas; ~300km baselines
•No8onal Frequency range: 1.2 –116GHz • Located in southwest US, centered on present loca8on of JVLA •Reasonably conceived baseline design • Low technical risk (could be built today)
•Need to iron out a number of challenges/op8ons • e.g., frequency bands, configura8on, phase calibra8on… • A Series of Compromises and tough decisions
The Next Generation Very Large Array
The Next Generation Very Large Array
Located in US South West JVLA: Good 3mm site, elev. ~ 2200m
40% in core: b < 3km ~ 1” at 30GHz 70% in mid: b < 30km ~ 0.1” 100% in long: b < 500km ~ 0.01”
The Next Generation Very Large Array
Radio Facili*es in the 2030’s
Complementary suite from meter to submm, appropriate for the mid-21st century • < 0.3cm: ALMA 2030 superb for chemistry, dust, fine structure lines • 0.3 to 3cm: ngVLA superb for terrestrial planet formation, dense gas history, baryon cycling • > 3cm: SKA superb for pulsars, reionization, HI + contnuum surveys
Eff ec 8v e co lle c8 ng a re a
Frequency [GHz]
Angular resolu*on
The Next Generation Very Large Array
Highly Synergis*c with Other Facili*es on Similar Timescales • SKA
• Atomic/non-thermal • Molecular/thermal
• LUVOIR/HABEX • Image earth-like planets • Image forming planets
• OST (FIR surveyor) • C/WNM & WIM • Cold Molecular Medium
Origins Space Telescope
Large UV/Opt/IR surveyor
The Next Generation Very Large Array
Science WG1: The cradle of life • Image the inner "terrestrial-zone" of planet forma4on in protoplanetary disks • The inner regions of protoplanetary disks are op8cally thick at shorter wavelengths. • The ngVLA will image gap-structures indica8ng planet forma8on on solar system scales, determine the growth of grains, and image accre8on onto proto-planets themselves. •Probing dust gaps on 1 AU scales in the nearest major star-forming regions requires baselines 10x the Jansky VLA baselines, with a sensi8vity adequate to achieve a few K brightness at 1 cm wavelength and 9 mas resolu8on.
The Next Generation Very Large Array
Seeing Pebbles and Rocks hips://science.nrao.edu/science/mee8ngs/2015/aas225/next-gen-vla/NGVLA_AAS2015_Hughes.pptx
ci en
cy (Q
a
At a given wavelength, large grains (a>λ) are the most efficient emiiers
Grain size ≈ Wavelength of observa8on Need long wavelengths to see pebbles
The Next Generation Very Large Array
Science WG 3: Galaxy Assembly through Cosmic Time •Cold gas emission, dynamics
• Importance of ground state CO(J=1→0) line; dense gas tracers •Con8nuum emission
• Synchrotron, free-free (as unbiased SFR tracers), dust •AGN and supermassive black holes
• BH mass; radio emission from radio-quiet AGN; weak radio AGN; mul8ple AGN; AGN feedback; Sunyaev-Zeldovich Effect from quasar/starburst winds;
•Polarimetry and cosmic magne8sm • CO line can be linearly polarized through the Goldreich-Kylafis (G-K) effect; CO(1-0) @z=0.85, Mgas=1010M¤ è a few % polariza8on will be detected with ngVLA (see also Li & Henning 2011, Nature 479, 499); G-K + PAH è anomalous microwave emission? ; Zeeman; Faraday rota8on è accre8on rates onto SMBH such as SgrA*
• Synergies with other facili8es hip://arxiv.org/abs/1510.06411
The Next Generation Very Large Array
VLA è ngVLA: instantaneous bandwidth (& FoV)
• Looks very airac8ve already; essen8al for both • (1) blind redshi{ survey using CO lines of pre- selected objects, and • (2) constraining CO LF (i.e., blind line emiier search)
• Bandwidth ra8o = 3:1 (e.g., 15 – 45 GHz) – CO(1-0) redshi{: 6.68 - 1.56 (15 - 45 GHz) – Similar redshi{ coverage for Lyα using op8cal telescopes equipped with IFU (such as MUSE)
hip://arxiv.org/abs/1510.06411
“ngVLA CO(1-0) molecular deep field”
hip://arxiv.org/abs/1510.06411
11GHz – 33 GHz (z=2.5 – 9.5), 30 hours integra8on è 10μJy/beam (1σ), df=2MHz
18GHz - 50GHz, 12 arcmin2 è ~200 CO(1-0) detec8ons predicted (da Cunha et al. 2013, ApJ, 765, id. 9)
The Next Generation Very Large Array
RedshiTed [CI] and [CII] using ngVLA ??? •[CI] at z = 3.3 – 10.5 (115 – 70 GHz) •Neutral ISM tracer, “CO-dark” gas, •molecular oulows, ..
•[CII] at z > 15 !? (f < 116 GHz) • ngVLA + 30 hrs integ è L[CII]~2x106 L¤ •è ~100 - 1000 8me weaker [CII] emiiers than “normal” galaxies (LBGs) at z = 5 – 6
Capak et al. 2015, Nature, 522, 455 • 9 “normal” galaxies (i.e., 1~4 L* galaxies)
• ALMA Band 7 (~300GHz cont. + [CII]) • 20min. on-source, 0.6 arcsec resolu8on
The Next Generation Very Large Array
Science WG 4: *me domain, fundamental physics, and cosmology
•The highest impact topics: •Galac8c Center pulsar discovery and 8ming • Electromagne8c counterparts to gravita8onal wave sources • Astrometry (“real-8me cosmology”)
•Other topics: • Fundamental constant evolu8on; par8cle accelera8on and plasma physics; Star-Planet interac8ons; etc.
hip://library.nrao.edu/public/memos/ngvla/NGVLA_09.pdf
The Next Generation Very Large Array
Real-*me cosmology with NGVLA astrometry •Real 8me cosmology may soon be possible • Extragalac8c parallax: sta8s8cal and individual • Long-period gravita8onal waves can be directly constrained or detected • Isotropy of expansion tests •Growth of large scale structure: mass •Objects appear smaller as they recede: distance. •Real-8me BAO evolu8on
The Next Generation Very Large Array
Revealing the Plasma physics of star-planet interac*ons
The Next Generation Very Large Array
Milestones and Community Engagement to Date
ü ngVLA Project Office: ü Established mid Sept 2016.
ü ngVLA Science Advisory Council: üMembership Announced Sept. 30
ü ngVLA Community Studies: ü 13 Science & 13 Technical Studies Approved Nov. 2
ü ngVLA Technical Advisory Council ü Announced Feb. 15
The Next Generation Very Large Array
Start Wed 9/14/16
Finish Mon 7/1/19
Nov '16 Jan '17 Mar '17 May '17 Jul '17 Sep '17 Nov '17 Jan '18 Mar '18 May '18 Jul '18 Sep '18 Nov '18 Jan '19 Mar '19 May '19 Sci Book First Draft Thu 6/1/17 - Fri 12/1/17
Sci Book Second Draft Mon 12/4/17 - Fri 6/15/18
Sci Book Final Draft Mon 6/18/18 - Fri 12/14/18
Ref. Design First Draft Mon 10/31/16 - Fri 4/28/17
Ref. Design 1.5 Draft Mon 5/15/17 - Fri 11/24/17
Reference Design Second Draft Mon 11/27/17 - Tue 7/31/18
Ref. Design Final Draft Wed 8/1/18 - Community Study Development
Mon 10/31/16 - Tue 8/15/17
Fri 6/15/18
Fri 12/14/18
ocs Published (TRL1)
D esign D
Tue 7/31/18
Com m unity Study Final Reports D
ue Tue 8/15/17
Today
Tenta*ve Road to Astro 2020 Goal: PDR-level ‘proposal’ to 2020 Decade Survey
Compelling science program & defensibly costed design of all major elements
The Next Generation Very Large Array
Tenta*ve long-term construc*on
https://science.nrao.edu/futures/ngvla
2017223
The Next Generation Very Large Array
A next genera*on VLA • Thermal imaging at milli-arcsecond resolu8on • 10x effec(ve area and resolu(on of JVLA • ~300x18m antennas; ~300km baselines
•No8onal Frequency range: 1.2 –116GHz • Located in southwest US, centered on present loca8on of JVLA •Reasonably conceived baseline design • Low technical risk (could be built today)
•Need to iron out a number of challenges/op8ons • e.g., frequency bands, configura8on, phase calibra8on… • A Series of Compromises and tough decisions
The Next Generation Very Large Array
The Next Generation Very Large Array
Located in US South West JVLA: Good 3mm site, elev. ~ 2200m
40% in core: b < 3km ~ 1” at 30GHz 70% in mid: b < 30km ~ 0.1” 100% in long: b < 500km ~ 0.01”
The Next Generation Very Large Array
Radio Facili*es in the 2030’s
Complementary suite from meter to submm, appropriate for the mid-21st century • < 0.3cm: ALMA 2030 superb for chemistry, dust, fine structure lines • 0.3 to 3cm: ngVLA superb for terrestrial planet formation, dense gas history, baryon cycling • > 3cm: SKA superb for pulsars, reionization, HI + contnuum surveys
Eff ec 8v e co lle c8 ng a re a
Frequency [GHz]
Angular resolu*on
The Next Generation Very Large Array
Highly Synergis*c with Other Facili*es on Similar Timescales • SKA
• Atomic/non-thermal • Molecular/thermal
• LUVOIR/HABEX • Image earth-like planets • Image forming planets
• OST (FIR surveyor) • C/WNM & WIM • Cold Molecular Medium
Origins Space Telescope
Large UV/Opt/IR surveyor
The Next Generation Very Large Array
Science WG1: The cradle of life • Image the inner "terrestrial-zone" of planet forma4on in protoplanetary disks • The inner regions of protoplanetary disks are op8cally thick at shorter wavelengths. • The ngVLA will image gap-structures indica8ng planet forma8on on solar system scales, determine the growth of grains, and image accre8on onto proto-planets themselves. •Probing dust gaps on 1 AU scales in the nearest major star-forming regions requires baselines 10x the Jansky VLA baselines, with a sensi8vity adequate to achieve a few K brightness at 1 cm wavelength and 9 mas resolu8on.
The Next Generation Very Large Array
Seeing Pebbles and Rocks hips://science.nrao.edu/science/mee8ngs/2015/aas225/next-gen-vla/NGVLA_AAS2015_Hughes.pptx
ci en
cy (Q
a
At a given wavelength, large grains (a>λ) are the most efficient emiiers
Grain size ≈ Wavelength of observa8on Need long wavelengths to see pebbles
The Next Generation Very Large Array
Science WG 3: Galaxy Assembly through Cosmic Time •Cold gas emission, dynamics
• Importance of ground state CO(J=1→0) line; dense gas tracers •Con8nuum emission
• Synchrotron, free-free (as unbiased SFR tracers), dust •AGN and supermassive black holes
• BH mass; radio emission from radio-quiet AGN; weak radio AGN; mul8ple AGN; AGN feedback; Sunyaev-Zeldovich Effect from quasar/starburst winds;
•Polarimetry and cosmic magne8sm • CO line can be linearly polarized through the Goldreich-Kylafis (G-K) effect; CO(1-0) @z=0.85, Mgas=1010M¤ è a few % polariza8on will be detected with ngVLA (see also Li & Henning 2011, Nature 479, 499); G-K + PAH è anomalous microwave emission? ; Zeeman; Faraday rota8on è accre8on rates onto SMBH such as SgrA*
• Synergies with other facili8es hip://arxiv.org/abs/1510.06411
The Next Generation Very Large Array
VLA è ngVLA: instantaneous bandwidth (& FoV)
• Looks very airac8ve already; essen8al for both • (1) blind redshi{ survey using CO lines of pre- selected objects, and • (2) constraining CO LF (i.e., blind line emiier search)
• Bandwidth ra8o = 3:1 (e.g., 15 – 45 GHz) – CO(1-0) redshi{: 6.68 - 1.56 (15 - 45 GHz) – Similar redshi{ coverage for Lyα using op8cal telescopes equipped with IFU (such as MUSE)
hip://arxiv.org/abs/1510.06411
“ngVLA CO(1-0) molecular deep field”
hip://arxiv.org/abs/1510.06411
11GHz – 33 GHz (z=2.5 – 9.5), 30 hours integra8on è 10μJy/beam (1σ), df=2MHz
18GHz - 50GHz, 12 arcmin2 è ~200 CO(1-0) detec8ons predicted (da Cunha et al. 2013, ApJ, 765, id. 9)
The Next Generation Very Large Array
RedshiTed [CI] and [CII] using ngVLA ??? •[CI] at z = 3.3 – 10.5 (115 – 70 GHz) •Neutral ISM tracer, “CO-dark” gas, •molecular oulows, ..
•[CII] at z > 15 !? (f < 116 GHz) • ngVLA + 30 hrs integ è L[CII]~2x106 L¤ •è ~100 - 1000 8me weaker [CII] emiiers than “normal” galaxies (LBGs) at z = 5 – 6
Capak et al. 2015, Nature, 522, 455 • 9 “normal” galaxies (i.e., 1~4 L* galaxies)
• ALMA Band 7 (~300GHz cont. + [CII]) • 20min. on-source, 0.6 arcsec resolu8on
The Next Generation Very Large Array
Science WG 4: *me domain, fundamental physics, and cosmology
•The highest impact topics: •Galac8c Center pulsar discovery and 8ming • Electromagne8c counterparts to gravita8onal wave sources • Astrometry (“real-8me cosmology”)
•Other topics: • Fundamental constant evolu8on; par8cle accelera8on and plasma physics; Star-Planet interac8ons; etc.
hip://library.nrao.edu/public/memos/ngvla/NGVLA_09.pdf
The Next Generation Very Large Array
Real-*me cosmology with NGVLA astrometry •Real 8me cosmology may soon be possible • Extragalac8c parallax: sta8s8cal and individual • Long-period gravita8onal waves can be directly constrained or detected • Isotropy of expansion tests •Growth of large scale structure: mass •Objects appear smaller as they recede: distance. •Real-8me BAO evolu8on
The Next Generation Very Large Array
Revealing the Plasma physics of star-planet interac*ons
The Next Generation Very Large Array
Milestones and Community Engagement to Date
ü ngVLA Project Office: ü Established mid Sept 2016.
ü ngVLA Science Advisory Council: üMembership Announced Sept. 30
ü ngVLA Community Studies: ü 13 Science & 13 Technical Studies Approved Nov. 2
ü ngVLA Technical Advisory Council ü Announced Feb. 15
The Next Generation Very Large Array
Start Wed 9/14/16
Finish Mon 7/1/19
Nov '16 Jan '17 Mar '17 May '17 Jul '17 Sep '17 Nov '17 Jan '18 Mar '18 May '18 Jul '18 Sep '18 Nov '18 Jan '19 Mar '19 May '19 Sci Book First Draft Thu 6/1/17 - Fri 12/1/17
Sci Book Second Draft Mon 12/4/17 - Fri 6/15/18
Sci Book Final Draft Mon 6/18/18 - Fri 12/14/18
Ref. Design First Draft Mon 10/31/16 - Fri 4/28/17
Ref. Design 1.5 Draft Mon 5/15/17 - Fri 11/24/17
Reference Design Second Draft Mon 11/27/17 - Tue 7/31/18
Ref. Design Final Draft Wed 8/1/18 - Community Study Development
Mon 10/31/16 - Tue 8/15/17
Fri 6/15/18
Fri 12/14/18
ocs Published (TRL1)
D esign D
Tue 7/31/18
Com m unity Study Final Reports D
ue Tue 8/15/17
Today
Tenta*ve Road to Astro 2020 Goal: PDR-level ‘proposal’ to 2020 Decade Survey
Compelling science program & defensibly costed design of all major elements
The Next Generation Very Large Array
Tenta*ve long-term construc*on
https://science.nrao.edu/futures/ngvla