multi-frequency agn survey with kvn - ホーム | 国立天 … ae lee, ilje cho, dawoon jeong,...
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MASK TEAM: Taehyun Jung, Do-Young Byun, Bong Won Sohn, Minsun Kim, Guangyao Zhao, Jan Wagner, Kiyoaki Wajima, Cristian Saez de Cea, Woojin Kwon, Jeong Ae Lee, Ilje Cho, Dawoon Jeong, Dongsoo Ryu, Jongsoo Kim
Multi-frequency AGN Survey with KVN Finding more high-frequency sources & Maximizing the KVN uniqueness
Challenges of AGN Jets, 20 Jan. 2017 @ NAOJ, Mitaka, Tokyo
KVN Legacy Program (planned)
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Intro
Radio Surveys
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Radio Sources Interferometer
http://skyview.gsfc.nasa.gov/images/high_res_radio.jpg
FIRST NVSS SUMSS WENSS
Frequency 1400 MHz 1400 MHz 843 MHz 325 MHz
Area (deg2) 10,000 33,700 8,000 10,100
Resolution 5” 45” 43” 54”
Detection limit 1 mJy 2.5 mJy 3.5 mJy 15 mJy
Coverage δ > +22° δ > -40° δ > -30° δ > +30°
Sources/deg2 90 60 50 20
# of Sources 946,432 1,773,484 211,050 229,420
References Becker+1995 Condon+1998 Bock+1998 Rengelink+1997
WENSS: Westerbork Northern Sky Survey
FIRST: VLA Faint Images of the Radio Sky at Twenty Centimeters Survey
NVSS: NRAO VLA Sky Survey (NVSS)
SUMSS: Sydney University Molonglo Sky Survey
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> 3400 sources are available
Radio Sources VLBI
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Radio Fundamental Catalog of Compact Radio Sources (L. Petrov)
11,448 (up to date)
http://astrogeo.org
Num
ber
of Sourc
es
Time (year)
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Name Wavelength # of Sources Reference
CJF survey 18 & 6 cm 293 Pollack et al. 2003
ICRF/RDV 13 & 3.6 cm ~ 500 Ojha et al. 2004
VLBA Calibrator Survey 13 & 3.6 cm > 3400 Kovalev et al. 2007
VSOP VLBApls 6 cm 374 Fomalont et al. 2000
VSOP Survey 6 cm ~ 300 Dodson et al. 2008
VIPS 6 cm 1127 Helmboldt et al. 2007
2cm Survey 2 cm 250 Kovalev et al. 2005
MOJAVE 2 cm > 133 Lister & Homan 2005
VERA FSS / GaPS 1.35 cm 500 Petrov et al. 2007
ICRF 22 & 43 GHz 1.37 & 0.7 cm ~100 Lanyi et al. 2010
GMVA 3mm 3 mm 123 Lee et al. 2008
TANAMI 3.5 & 1.3 cm 80 Ojha et al. 2010
KVN Q-CAL survey 7 mm 638 Petrov et al. 2012
KVN W/D-CAL survey 3.5 & 2.3 mm > 500 (W) Lee et al. (In prep.)
KVN K-CAL survey 1.3 cm > 400 (K) Lee et al. (in prep.)
VLBI Surveys
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Untill now...
• Number of sources at mm-wavelengths are still very limited - more than ~3400 sources are available at 3.6 cm,
while ~160 sources are available shorter than 3 mm (Dhanya+ in prep)
3414 sources at 3.6 cm (Beasely 2002) 109 sources at 3 mm (Lee+ 2008) 164 sources at 3 mm (Dhanya+ in prep)
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mm-VLBI study of AGN
• High-frequency VLBI (mm-VLBI) observations are required to understand of the physical processes at the innermost region in AGN and in the vicinity of suppermassive black holes - much less affected by the source intrinsic opacity effects
• Determination of the phyiscal parameters of the innermost & most compact component (e.g. the jet base) - constraints for current jet and shock models (Blandford & Königl 1979, Königl 1981, Marscher & Gear 1985 etc)
- multi-band spectra & VLBI structures
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• mm-VLBI observations have been successfully conducted at different frequencies (43/86/129/230GHz) with the available VLBI network (VLBA, GMVA, HAS, EHT)
• However, above 86GHz are still demanding and general properties of the millimeter VLBI sky are not very well known
• mm-VLBI observations (> 20 GHz, <15 mm) are very difficult - atmospheric coherence time < 1 min - antenna efficiency is less efficient - receivers are less sensitive - sources are weaker than cm wavelengths - tropospheric water vapour absorption
mm-VLBI observations
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Difficulties in mm-VLBI
• Sensitivity (Image)
ΔIm=SEFD/[ηs⋅(N⋅(N−1)⋅Δν⋅tint)1/2] Jy/beam
• Radio telescope performance - Surface accuracy, High Tsys, Rx performance …
• Radio Emission
• Non-thermal • 15~20% of AGNs are radio-loud
others are mostly radio-quiet
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Coherence Function
Coherence Time
Coherence
*Typical value of atmospheric phase stability ~ 10-13
VLBI Sensitivity
(A. Roy) Pico Veleta – Onsala baseline Source : BL Lac Frequency : 86 GHz
Errors coming from the ATMOSPHERE are still remain the most serious difficulty which significantly degrade the sensitivity and imaging capability of mm and sub-mm VLBI observation
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Korean VLBI Network
Simultaneous Multi-Frequency VLBI System
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KVN Yonsei Observatory
KVN Tamna Observatory
KVN Ulsan Observatory
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22GHz
43GHz
86GHz
129GHz
Beams from antenna
Multi-Frequency
Receiving System
4Ch Receiver @ Yonsei
Han et al. (2008)
Band K Q W D
Freq. Range 21.25-23.25 42.11-44.11 85-95 125-142
Trx (K) 30-40 70-80
(40-50 KUS) 80-100 50-80
Full Polarization
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2 ( )
2 ( )
h h h h
str g C inst trop ion LO
l l l l
str g C inst trop ion LO
h lr /h lr
2 2
0
2 22 ( ) 2 1 ( )
h h
l l
str g g ion LO LOhh l h h h l h l
l h
Self-calibration at lower frequency
l
str 2 ( )l l
g C inst trop ion LO
By doing Self-calibration again for longer solution interval, we can get an image at higher frequency
Core-shift
diff in maser lines
slow varying term
ionosphere instrument Source
Structure
Frequency Phase Transfer (FPT)
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FPT applied using K-band solint 0.3
24 hours
43GHz
NRAO150 0133+476 3C84 1308+326 3C279 3C345 NRAO530 SGR-A 3C454.3 2255-282
0202+149 1023+131 3C273 1633+382 NRAO512 FAS 1921-293 BLLAC NRAO150
FPT applied using Q-band solint 0.1
129GHz
86GHz
NRAO150 0133+476 3C84 1308+326 3C279 3C345 NRAO530 SGR-A 3C454.3 2255-282
0202+149 1023+131 3C273 1633+382 NRAO512 FAS 1921-293 BLLAC NRAO150
FPT applied suing K-band solint 0.3
24 hours
High frequency VLBI Phase Calibration by Lower Frequency Phase Solutions
Fringe Solution SNRs at 22GHz (solint 0.3)
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Power of Simultaneous
Multi-Frequency Receiving System
30min
22 GHz
43 GHz
86 GHz
129 GHz
Ceff 22GHz 43GHz 86GHz 129GHz
22 GHz - 0.97 0.91 0.88
43 GHz 0.97 - 0.97 0.96
86 GHz 0.91 0.97 - 0.99
129GHz 0.88 0.96 0.99 -
SNR~213 (~90% of theoretical SNR)
𝜙 ℎ𝑖𝑔ℎ
∝𝜈ℎ𝜈𝑙𝜙𝑙𝑜𝑤
non-dispersive characteristic of troposphere
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Power of Simultaneous
Multi-Frequency Receiving System
30min
22 GHz
43 GHz
86 GHz
129 GHz
Ceff 22GHz 43GHz 86GHz 129GHz
22 GHz - 0.97 0.91 0.88
43 GHz 0.97 - 0.97 0.96
86 GHz 0.91 0.97 - 0.99
129GHz 0.88 0.96 0.99 -
SNR~213 (~90% of theoretical SNR)
𝜙 ℎ𝑖𝑔ℎ
∝𝜈ℎ𝜈𝑙𝜙𝑙𝑜𝑤
non-dispersive characteristic of troposphere
Using the KVN, more than 30min integration is achievable even at 130 GHz!! while only ~12 sec integration is a nomial integration time at 130 GHz
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KVN Sensitivity by FPT
Frequency Band 22 GHz 43 GHz 86 GHz 129 GHz
Bandwidth (MHz) 64 (Total 256MHz ~ 1Gbps)
System temperature (K) 100 150 200 250
SEFD (Jy) 1329 1993 4229 4983
Integration time (sec) 20 1800 (30 min)
Sensitivity (mJy) 29.8 4.7 10.5 11.8
5σ Sensitivity (mJy) 149.2 23.6 52.4 60.0
※ Aperture efficiency : K ~ 0.6, Q ~ 0.6, W ~ 0.45, D ~ 0.4
Frequency Band 22 GHz 43 GHz 86 GHz 129 GHz
Bandwidth (MHz) 512 MHz for each band
System temperature (K) 100 150 200 250
SEFD (Jy) 1329 1993 4229 4983
Integration time (sec) 20 1800 (30 min)
Sensitivity (mJy) 10.5 1.7 3.7 5.0
5σ Sensitivity (mJy) 52.7 8.3 18.5 25.0
1Gbps Multi-Freq. Obs Mode
8Gbps Multi-Freq. Obs Mode
ΔIm=SEFD/[ηs⋅(N⋅(N−1)⋅Δν⋅tint)1/2] Jy/beam
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21.7GHz Peak ~ 26.4 Jy/beam Beam 8.5 x 3.5 mas -78.8°
43.4GHz Peak ~ 20.6 Jy/beam Beam 3.12 x 1.78 mas -82.6°
86.8GHz Peak ~ 12.7 Jy/beam Beam 1.59 x 0.87 mas -81.8°
130 GHz Peak ~ 5.0 Jy/beam Beam 1.09 x 0.58 mas -81.4°
First KVN’s 4-Frequency Simultaneous Observation VLBI Images Source: 3C279 43/86/130GHz visibility phases are calibrated by 22GHz’s
Phase reference
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Example: J0502+1338
43 GHz
86 GHz 129 GHz
KVN single dish flux at 22GHz ~ 0.3 Jy (No SD detection at 43GHz)
KT-KU 22 GHz
KT-KY
KU-KY
Corr
ela
ted A
mplitu
de (m
Jy)
UV distance (Mega wavelength)
43 GHz
86 GHz 129 GHz
22 GHz
43 GHz
86 GHz 129 GHz
22 GHz
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Example: J0502+1338
43 GHz
86 GHz 129 GHz
KVN single dish flux at 22GHz ~ 0.3 Jy (no detection at 43GHz)
KT-KU 22 GHz
KT-KY
KU-KY
Am
plitu
de (m
Jy)
UV distance (Mega wavelength) Credit: B. W. Sohn
2016
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KVN Sensitivity by FPT
Frequency Band 22 GHz 43 GHz 86 GHz 129 GHz
Bandwidth (MHz) 64 (Total 256MHz ~ 1Gbps)
System temperature (K) 100 150 200 250
SEFD (Jy) 1329 1993 4229 4983
Integration time (sec) 20 1800 (30 min)
Sensitivity (mJy) 29.8 4.7 10.5 11.8
5σ Sensitivity (mJy) 149.2 23.6 52.4 60.0
※ Aperture efficiency : K ~ 0.6, Q ~ 0.6, W ~ 0.45, D ~ 0.4
Frequency Band 22 GHz 43 GHz 86 GHz 129 GHz
Bandwidth (MHz) 512 MHz for each band
System temperature (K) 100 150 200 250
SEFD (Jy) 1329 1993 4229 4983
Integration time (sec) 20 1800 (30 min)
Sensitivity (mJy) 10.5 1.7 3.7 5.0
5σ Sensitivity (mJy) 52.7 8.3 18.5 25.0
1Gbps Multi-Freq. Obs Mode
8Gbps Multi-Freq. Obs Mode
ΔIm=SEFD/[ηs⋅(N⋅(N−1)⋅Δν⋅tint)1/2] Jy/beam
Overcome the difficulties in the atmosphere
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Number of VLBI sources at mm-wavelengths are still very limited - more than ~3400 sources are available at 3.6 cm,
while ~120 sources are available shorter than 3 mm
> 3400 sources at 3.6 cm (Beasely 2002) ~120 sources at 3 mm (Lee+ 2008)
Uniqueness: Simultaneous Multi-frequency mm-VLBI observation of AGNs
• Most of AGNs are variable on time scales • Simultaneous observations at multi-frequencies can provide important
clues on physical conditions, especially in particular compact systems
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• Sample: 1533 sources Known K-band VLBI sources 837 + KVN K-band fringe survey 426 (※ 43 common sources)
Samples based on KVNCS J. A. Lee (submitted)
Goal: Constructing Multi-Frequency VLBI Catalog of AGNs Utilizing KVN’s uniqueness & playing a leading role in mm-VLBI
Multi-frequency AGN Survey with KVN
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Number of VLBI sources at mm-wavelengths are very limited
3414 sources at 3.6 cm (Beasely+2002) 109 sources at 3 mm (Lee+2008)
Simultaneous Multi-frequency mm-VLBI observation of AGNs is Unique
• Most of AGNs are variable on time scales
• Simultaneous observations at multi-frequencies can provide important clues on physical conditions, especially in particular compact systems
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MASK Pilot Observations • Common sources of ALMA & KVNCS Calibrators (Dec<0°)
– 76% VLBI detection (57/75 detection at 3mm)
Raw 86GHz Phase FPTed 86GHz Phase Calibrated 86GHz Phase
24 hour experiment
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MASK Pilot Observations • Common sources of ALMA & KVNCS Calibrators (Dec<0°)
– 76% VLBI detection (57/75 detection at 3mm)
Raw 86GHz Phase FPTed 86GHz Phase Calibrated 86GHz Phase
24 hour experiment
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(Known) K-band Calibrators (858) Petrov et al. (2007), Lanyi et al. (2010), Petrov et al. (2011), Petrov (2012), Petrov et al. (2012)
Sky Coverage ~ 68% (Dec>32.5°)
KVN Single Dish Survey (1533) Sky Coverage ~ 99% (Dec>32.5°) - more than two sources overlap ~ 89% - single source area ~ 10% - empty area ~ 1%
circle radius ~ 5° (J.A. Lee+ accepted)
KVN K-band Single
Dish Calibrator Survey
(J.A. Lee)
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First Detection Statistics of MASK Observations - Preliminary Results-
• 2016A season (2016 April – September)
– Detection test for KVNCS common sources (154 sources) in CARMA & SMA catalogues
– Observations: All 154 sources have been observed !!
• Detection results for all 154 sources
– W-band: 5 src detected by only KW, 1 src detected by only QW
– D-band: 1 src detected by only KD, 6 src detected by only QD
( ) # of non-detected sources
FPT(total 154src) # of Detection Detection Rate
KQ 150 (4) 97%
KW 137 (17) 89%
KD 98 (56) 64%
QW 133 (21) 86%
QD 103 (51) 67%
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First Detection Statistics of MASK Observations - Preliminary Results-
• 2016A season (2016 April – September)
– Detection test for KVNCS common sources (154 sources) in CARMA & SMA catalogues
– Observations: All 154 sources have been observed !!
• Detection results for all 154 sources
– W-band: 5 src detected by only KW, 1 src detected by only QW
– D-band: 1 src detected by only KD, 6 src detected by only QD
( ) # of non-detected sources
FPT(total 154src) # of Detection Detection Rate
KQ 150 (4) 97%
KW 137 (17) 89%
KD 98 (56) 64%
QW 133 (21) 86%
QD 103 (51) 67%
Detected sources @ W/D band from K-band FPT
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MASK as a KVN Legacy Program
• Large science projects, not reproducible by any reasonable number or combination of smaller observations
• General and lasting importance to the broad astronomical community with KVN data yielding a substantial and coherent database
• Enabling timely and effective opportunities for follow-on observations and for archival research
• Maximizing the KVN Uniqueness (4-freq. simultaneous VLBI) • What KVN (instrument) CAN DO
What KVN (instrument) canNOT do • Large & homogeneous DB for statistical study of a broad range of
astrophysical & cosmological issues
• 1st MASK detection survey (2016 – 2017)
– 30min per source, total ~1500 sources
– net obs. time 750 hr (~ 1000 hr incl. overhead)
– So far, 10% (~150 sources) completed
• 2nd MASK Imaging survey (2018 -)
– based on 1st detection survey results
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On-going Works • Data reduction and performance evaluation
– error estimation of amplitude calibration & pipeline updates
• 1st MASK Catalog Release (~150 sources, pilot survey)
• Contructing MASK DB
• 2nd MASK survey : KVNCS common sources with (up to date) ALMA calibrators
• Multi-wavelength database (gamma-ray to radio) Synergy!
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MOJAVE (Lister & Homan 2005)
VLBI Polarimetry
(Lanyi et al. 2010)
Celestial Reference Frame
Astrometry & VLBI Calibrators - ICRF / Accurate source position
Statistical Study - (high resolution) source structure / compactness / brightness temperature / spectral index - population / classification - r-ray connection, variability - polarimetry - cosmological evolution / AGN evolution
Credit: Roen Kelly
Origin of Jets: Understanding BH-Disk-Jet
(Lee et al. 2016)
Brightness Temp. vs Frequency (Ojha et al. 2010)
TANAMI Survey
Statistical study of AGN classification & γ-ray connection
compactness/structure, variability, Tb
(Kovalev et al. 2005)
MASK Synergies
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For the most powerful mm-VLBI network
People Role
Taehyun Jung Coordinator
Do-Young Byun Advisor (KVN PI)
Bong Won Sohn Advisor, Database
Dongsoo Ryu Advisor
Minsun Kim Sample & Database
Woojin Kwon Sample & Database
Cristian Saez de Cea Sample & Database
Jeong Ae Lee Sample & Database
Jan Wagner Data analysis, Pipeline
Guangyao Zhao Data analysis, Pipeline
Kiyoaki Wajima Data analysis
Ilje Cho Data analysis, Scheduling
Dawoon Jeong Data analysis
Jongsoo Kim Advisor
MASK Team Members
MASK will provide most extensive mm-VLBI catalog at multiple friquencies and play an important role to uncover mm-VLBI sky
Thank you !