FAST Surveys&+FAST A
CRAFTS Commensal Radio Astronomy FAST Survey
GAS Galactic-plane and Andromeda Survey

Gain: FAST > 2 x Arecibo; Beam #: Arecibo 7 vs FAST 19
Arecibo Sky: 0d - 39d DEC vs FAST Sky: -14d - 66d DEC
Survey Speed: FAST  10 x Arecibo

continuous coverage
70MHz3GHz> 34
L HO> O@ LB@ KO@KLU
A

4B 0 4Nan, Li, Jin+ et al. 2011, IJMR-D, 20, 989(>190 citations)

Li & Pan, 2016, Radio Science, 51, 7
Li et al. 2018, IEEE Microwave, Vol. 19, Issue 3

RAA Mini-Volume !
FAST

SCI " 

eto
N’sroitEd
http://iopscience.iop.org/journal/1674-4527

A Mini-Volume on the Science Potential of FAST
Research in Astronomy and Astrophysics has publisheda mini-volume on the science potential of FAST … Theauthors quantified the science potential of FAST in

ambitious and forward-looking manners. … thedrive to facilitate major breakthroughs with the FAST
telescope gets underway in earnest.

• Fundamental Constants (Chen et al. 2019)• Cosmic Rays (James et al. 2019)• Exoplanets (Zarka et al. 2019);• Gravitational radiation (Hobbs et al. 2019)• Pulsar magnetospheres (Wang et al. 2019)• Phases of the Interstellar Medium (Heileset al. 2019)• Megamasers (Zhang et al. 2019)̽Ӿࢵᑀ਍̾FASTӫ‫ږ‬
Science ChinaPhysics, Mechanics & Astronomy[1] Jiang P., et al. Commissioning Progress of FAST, Sci.
China-Phys. Mech. Astron. xx, xx (2019)[2] Lu J. G., et al. Rotating Radio Transients Observed with
FAST, Sci. China-Phys. Mech. Astron. xx, xx (2019)[3] Yu Y., et al. FAST ultra-wideband observation for theabnormal emission-shift event of PSR B0919+06, Sci.
China-Phys. Mech. Astron. xx, xx (2019)[4] Lu J., et al. The Radiation Structure of PSR B2016+28
Observed with FAST, Sci. China-Phys. Mech. Astron. xx,xx (2019)[5] Zhang K., et al. Status and Perspectives of the CRAFTS
extragalactic HI survey, Sci. China-Phys. Mech. Astron. xx,xx (2019)[6] Wang H. F., et al. Pulsar Candidate Selection withEnsemble Nets for FAST Drift-scan Survey, Sci. ChinaPhys. Mech. Astron. xx, xx (2019)[7] Qian L., et al. The First Pulsar Discovered by FAST,
Sci. China-Phys. Mech. Astron. xx, xx (2019)

“Shared-Risk” Open Call
Day time 360h + Night time 960h

133 proposals, 2250h requested, 21 PI
institutes, CoI: 583
NAOC, PKU, NJU, SHAO, YNU, HKU, etc.

The oversubscription ratio for day time hours >5FAST෸ᳵ‫ړ‬ᯈ঩ާտNF)- (5 F OC ( )7=8 ,2IG BM AECBM ) %4 1 - %
3OI F HCM 5 CMB ) %Ԇ ձғဂப୩ ӾᑀᴺӤၹॠ෈‫ݣ‬‫ۅ‬Ԇձғ๫ 嵩 Ӿᑀᴺࢵਹॠ෈‫ݣ‬঩ ާғොᵄᵄ ܿᳪय़਍ᶥᰂ຋ Ӿᑀᴺࢵਹॠ෈‫ݣ‬֜ৼઊ ۹Ղय़਍ভ Ứ Ӿᑀᴺࢵਹॠ෈‫ݣ‬ྷႡ஛ Ⴔ܏य़਍/Ӿᑀᴺࢵਹॠ෈‫ݣ‬୻ ۡ Ӿᑀᴺࢵਹॠ෈‫ݣ‬ᮕᑀଘ ‫ܖ‬Ղय़਍எ ᅺ Ӿᑀᴺᔳᰂઊॠ෈‫ݣ‬ሴ ূ Ӿᑀᴺࢵਹॠ෈‫ݣ‬ෛዅॠ෈‫ݣ‬FAST෸ᳵ‫ړ‬ᯈߎᧃ঩ާտ
Paul Ho ӳԵॠ෈‫ݣ‬ୟٌၖ ߢ֡‫ੂݥ‬ຂॠ֛ᇔቘӾஞୟ ٩ ٖ܏ᬡय़਍/Ӿᑀᴺࢵਹॠ෈‫ݣ‬

FLAN
FAST L-band Array of Nineteen beams

The LargestL-band feed-horn array
1.05 – 1.45 GHz● 18K Tsys
● 19 BEAM FEED ARRAY● BEAM WIDTH 2.9’ at 21cm
● BEAM SPACING 270mm (~6’)● DUAL LINEAR POLARIZATION● POL. CROSS-COUPLING <-30 dB●

2018/5/24

220 full days
5280 hours
2-3 years

Drift !sidereal)#
Credit: L. Staveley-SmithMessage from Dr. Bell
Oct. 10, 20172019.7>120 candidates>80 confirmed

First FAST Science ResultsFAST’s First MSP
3FGL J0318.1+0252
FL8Y J0318.2+0254••Fermi unidentified source
GBT, Arecibo non-detection

PSR J0318+0253
p 5.19 ms; DM 26 pc cm-3
•
•••

•
•

2018.2.27 FAST one hour tracking
2018.4.12 Wang Pei and GZNU group
discovered the candidate
2018.4.18 Colin Clark found the 𝜸counterpart
2018.4.23 Pablo confirmed no X-ray,provided limits
2018.4.28 Published on Atel #10851
2018.5.02 IPTA released J0318+0253
to its members

Wang et al. 2018, Atel # 10851“FAST’s Discovery of a New Millisecond Pulsar (MSP) toward
the Fermi-LAT unassociated source 3FGL J0318.1+0252”

Pulsar Emission Mechanism
FAST Pulsar C12ୟᠿ2017.08.31 FAST drift discovery
2017.10.07 Parkes confirmation
P0=1608.88971 ms
DM=85
Zhang, DL et al. 2019 ApJ“PSR J1926-0652: A Pulsar with
Interesting Emission Properties Discoveredat FAST ”“…These complexities
pose challenges for theclassic carousel-typemodels. ”?

Commensal Radio
Astronomy FAST Survey
unprecedented
commensality

pulsar, galaxy, imaging, and FRB• Commissioning and survey demonstration• 1500 hours Parkes time for follow-up• Negotiation with GBT underway• Through collaboration with MPIfA, 100
hours/semester Effelsberg follow-up• PI programs (11+9) with proposing leadfrom PKU, NJU, SHAO, XAO, BNU, etc.
• Secured Arecibo DDT, Effelsberg opentime• GBT, Arecibo, Chandra, VLBI, GMRT,MWA proposals etc. submitted• Data facility (15PB+200 Tflops+100Gbs)
contract signed

Li et al. 2018, Invited Review
IEEE Microwave, Vol 19, Issue 3, p112

FAST Outlook

HI Galaxies from CRAFTS

𝑁>8𝜎; 2.3 π)≈ 6.5×105<𝑧>≈0.07

INcreasegaseous galaxies x20
Zhang, Wu, Li et al. 2019c.f. Duffy et al. 2008

Commensal Radio
Astronomy FAST Survey-G FQ

UNKW 2SQQ R FPUYL HO> O
5 D>H>TFBO
FHHFK RKTBHO 34 FI>DBO
19 O

Li et al. 2018

IEEE Microwave

M31ғAndromeda‣ Closest spiral galaxy at 0.8Mpc‣ No radio pulsar ever detected‣ dwarf groups + HVCs

Galactic-plane and Andromeda Survey‣ Deep coverage (1hr per pointing)‣ Column density ~ 5x1016 cm-2

‣ pulsar: 0.01 mJy; ~1000 new msp‣ Dwarf galaxy groups around M31‣ Galactic planeOH excitation temperaturepeaks around CMB
OH abundance tracks DMG
fraction

HIOH Absorption
No CO“Dust–Gas Scaling Relations and OH
Abundance in the Galactic ISM”
Nguyen…Li+PRIMO, ApJ

Quasardiffuse ISM“Where is OH and Does it Trace the Dark
Molecular Gas (DMG) ?”Li, Tang, +PRIMO, ApJS, 235,1

Dark Molecular Gas (DMG)

Pacific Rim Interstellar Matter Observer
PRIMO
The Milky Way

A V

A V>

2.7

<2.7

Pulsar Surveys

Liu et al.
2018

Dai & Zhu

http://crafts.bao.ac.cn

J0318+0253

The “Taurus” Pulsar
FAST discovers radio pulses from J0357

Taurus Molecular Cloud
Chandra X-ray Image
De Luca et al. 2011

Chapman … Li+ et al. ApJ 2011
P= 0.444 s$ DM=47.6
0.04 mJy ~500 MHz, 0.15mJy ~350 MHz
Li+ 2019 in prep.

The Sign of Cosmic Explosion on Earth ?

SNs: ~1.5 Myr ~2.3 Myr

Breitschwerdt et al. 2016 Nature
cf. Wallners et al. 2016 Nature
FAST discovered the first
nearby, recent supernova explosion?

Knie, K. et al. 2004, Phys. Rev. Lett.
Fimiani, L. et al. 3016, Phys. Rev. Lett.

Taurus Pulsar
VLBI Obs. Strategy
Challenges in P-band VLBI astrometry:••••

Very weak: 150 uJy at 327 MHz.
Only 32 MHz bandwidth at P-band
Very few VLBI observatories at 327 MHz.
in-beam referencing

Step 1: in-beam calibrator
Known calibrators (squares) and AO inVLBA --- waiting for correlation beam calibrators (dots) around PSR
J0357+3205 (star) .
Step 2: VLBI detection of target
VLBA + GBT + AO + FAST
Step 3: multi-epoch VLBI parallax measurement
VLBA + GBT + AO + FAST

FAST VLBI Challenges➡

➡

➡

➡

moving observatory
coordinate‘virtual’ phase referencepoint
No down-conversion
38 synced digitization
data stream➡

reference antenna?

➡

A FAST ‘Core’ Array
A Lost (maybe) argument to Carl Heiles
in Sydney Harbor, on April 21st, 2018

FAST VLBI System
FASTFront End

RF1Hz
10MHz

Converter

Correlator

ADC+ROACH 2

Mark VI

IFH-Maser

1Hz
10MHz

FAST (SEFD~1.4 Jy@L-band)
Recording rate 512 Mbits/s, Integration time = 60 min

FAST VLBI team (Zhang, H.Y. et al.) and Zhang, Bo 2017

FRB 121102

Duan et al. 2019
Zhang et al. 2018
Hundreds of pulses from
FRB121102, more than all
previous detections combined.
Periodicity search‣‣logN-LogS‣
Polarization: RM‣
DM variation‣
HI absorption
Astronomer’s Telegram

FAST - Aplus+
FAST A vs DSA/ : z.:iFAST
36xAT5(19 beam)

FAST+
36xAT5DSA
10DSA
110

Aperture

70,686707

71,393

159

1949

Tsys (1.4GHz)

20K

30K

30K

60K

30K

Gain (A/T, m2/K)

2600

152615

1.7

42Long baseline (m)300

30,00030,0001,183>21,318∆𝚯 (1.4GHz)

3’1.8”

1.8”45”<2.5”

FoV (1.4GHz, d2)

0.110101112

FAST - Aplus
RFI removal“Fast Converging Digital Adaptive Filter”
Finger, Curotto, Fuentes, Duan, Bronfman, Li 2018

LIGO Event: GW SourcesᲫᅩ

Exoplanet + Brown dwarf

Tidal Disruption EventၥFast Radio BrustCommensal Radio Astronomy FAST Survey
57% (2.3PI) Sky; drift scan; galaxies, imaging, pulsars&Galactic-plane and Andromeda Survey
M31+Galactic plane; 1h; 5x1016 cm-2 +1000 msp
HI, HI+OH Absorption, Pulsar DM, PTA(GW)=> A FAST View of Baryons