korean large telescope : the plan yong-ik byun 邊鎔翊 yonsei university, seoul 延世大學校,...

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Korean Large Telescope : The Plan Yong-Ik Byun 邊邊邊 Yonsei University, Seoul 邊邊邊邊邊 , 邊邊 ( 邊邊 )

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Page 1: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

Korean Large Telescope : The Plan

Yong-Ik Byun 邊鎔翊Yonsei University, Seoul 延世大學校 , 首爾 ( 漢

城 )

Page 2: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

Recent Effort for Korean Access to Large Telescopes

• 1996-1998 Plan for 4-meter Korean telescope Failed to get funded (partially due to national economic crisis in 1997/8)

• 2001-2005 Participation to CFHT 3.6-meter 14 nights/year

• 2003.6 Community Forum for 8-meter plans • 2004.1- 2004.12 STRM committee activity

(Strategic Technical Road Map)

• 2005.1- present Preparation for Korea-Mexico joint project

Page 3: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

World Telescopes

0

5

10

15

20

25

30

35

Mir

ror

size

(m

ete

rs)

1920 1940 1960 1980 2000 2020 2040 Year

4m class

very large

tel.

Korea Now

Korea large

Tel

4m class

very large

tel.

Korea Now

Korea large

Tel

Page 4: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

WHY DO WE NEED BIG ONE?WHY DO WE NEED BIG ONE?

• to carry out internationally competitive sciences

• to support growing astronomy community in Korea

We need more National Facilities and Research Institutes

Page 5: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

Astronomers in Korea Astronomers in Korea

Universities : 75 professors/postdocs

23 related departments in 19 Universities

KASI : 57 research scientistsKorea Astronomy & Space Science institutepreviously KAO

Others : 7 research scientists

Total # of PhD Astronomers 139 # of IAU National Members 67

500

Page 6: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

STRM Committee Discussions (Strategic Technical Road Map)

• what size? what kind of telescope? and why?

• how to decrease risk factors?

Roadmap for long term development

Page 7: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

WeaknessWeakness

OpportunityOpportunity

Rapid growth of Korean astronomyAbundant telescope operation experienceCFHT participation and lessons learntR&D experience on (small) missions

Shortage of R&D manpower

Lack of management experience for large project

National emphasis on large basic sciences

Large Infra-facilities available in Sci/Tech

Technology transfer not very difficult

SWOT AnalysisSWOT Analysis (Strength, Weakness, Opportunity, and Threat)(Strength, Weakness, Opportunity, and Threat)

StrengthStrength

Page 8: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

STRM committee : PLAN A

• construction of KST, a copy of LSST 8.4m

• rationale

TOP wide field telescope venturing into new science KST can be built with full cooperation of LSST, at smaller cost placed in different hemisphere, its contribution will be only second to LSST itself will open up opportunities in survey astronomy mainly, but still covers a variety of subjects from solar system to cosmology will be an excellent prelude to participation into 25/30-meter giants

Page 9: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

21C Leading Facilities for Astronomy

LSST GSMT

JWST ALMA

2011

2015

2010

2012

2012

KST 2012

Page 10: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )
Page 11: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

Primary 8.4mSecondary 3.4mTertiary 5.2m

USD150M

LSST 협력체 : NOAO, AURA, UofA, UofW etc ~100 과학기술자

Page 12: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

Photometry 24 mag / 10 sec FOV 7 sq.degree No AO requirement, but requires quantum leap in Electronic & IT Technology. This is GOOD !

Detector dimension : 2.3G pixels readout < 2 seconds data production > 20TB/day Supermassive Storage industrial Realtime analysis challenges

Page 13: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

STRM committee : PLAN A

• construction of KST, a copy of LSST 8.4m

• rationale

BEST wide field telescope venturing into new science KST can be built with full cooperation of LSST, at smaller cost placed in different hemisphere, its contribution will be only second to LSST itself will open up opportunities in survey astronomy mainly, but still covers a variety of subjects from solar system to cosmology will be an excellent prelude to participation into 25/30-meter giants

Page 14: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

KST benefits - extremely competitive in ELT era - especially for variability sciences - also for deep wide field mapping of universe DM & DE issues

//

Page 15: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

Plan A failed to obtain community agreement !

• community reaction

understands the importance of specialized telescope to maximize Korean contribution to world astronomy also understands survey science can be important for most areas of astronomy beyond 2010 HOWEVER, larger fraction favored multi-purpose general telescope over a special facility (LST project cost also increases to USD250M, a copy over 150M)

• STRM committee then prepared PLAN B

sought possible partnerships for 8-meter class telescope identifies Mexico dual 6.5 meter telescopes plan draft plan prepared for joint construction details

Page 16: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

2005. 1 Official Korea-Mexico Joint Plan 2005. 1 Official Korea-Mexico Joint Plan submitted to Korean Government submitted to Korean Government

DUAL 6.5-meter Telescopes

WFT NFT

Wide-Field and A0 Magellan-like

Wide-Field and A0 Magellan-like

TelescopesTelescopes

Page 17: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

PLAN B

• Total Cost : USD 160M, Korea to cover 80M with 50% share

• Major Partners (tentative) and roles

- Korea : KASI + Universities + Companies telescope construction, some

instrumentation - Mexico : UNAM + INAOE

site preparation/infrastructure, some optics - USA : U.Arizona + Magellan Consortium

telescope design & technology, optics - UK : Durham U.

spectrograph IFU construction

Page 18: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

TIMELINE : 7 YEAR

• Phase 1 (2006-2008) - Telescope 1&2 design - Optics and Construction for #1 - Optics for #2

• Phase 2 (2009-2012) - Installation of #1 by 2009Q4 - Construction and Installation of #2 by 2010Q4 - Instruments construction and installation #1 by 2010Q4, #2 by 2011Q4 - commissioning runs through 2012

Page 19: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

MKO

LMT

SPM

America del Norte de noche

Page 20: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

SPM

LBT

Kitt Peak

Lick

Palomar

MMT

Lowell

NIGHT SKY IN THE DESERT

San Pedro Martir: Sky brightness > 21.6 mag/sq sec

Page 21: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

Seasonal transparencySeasonal transparency

Page 22: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

Sierra de San Pedro Mártir, Baja California México2890 m above sea level, Lat: 31° 02’ 39 N Long: 115° 27’ 49 W

Page 23: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

SPM Telescope Facility Proposal (basics, tentative)SPM Telescope Facility Proposal (basics, tentative)

Wide FieldWide Field

Optimized for integral-field (3D) Optimized for integral-field (3D) spectroscopy spectroscopy

Field of view: > 1.5° in diameter Field of view: > 1.5° in diameter visible to NIRvisible to NIR

11stst - Generation Instrumentation: - Generation Instrumentation: 3D-spectroscopy set: WFC, ADC, 3D-spectroscopy set: WFC, ADC,

IFU, spectrographs (0.33-1.8µm)IFU, spectrographs (0.33-1.8µm) Wide-field tunable imager (narrow Wide-field tunable imager (narrow

band) band)

Telescope complementary pair

Narrow FieldNarrow Field

Optimized for image quality & Optimized for image quality & Adaptive Optics Adaptive Optics

Fields: ~15’ and ~1’ (MCAO) Fields: ~15’ and ~1’ (MCAO) Visible to thermal IR Visible to thermal IR

11stst - Generation Instrumentation: - Generation Instrumentation: High-resolution/precision High-resolution/precision

spectrograph (~1 m/s)spectrograph (~1 m/s) AO Imager-Spectro-Coronograph AO Imager-Spectro-Coronograph

(NIR)(NIR) IR General purpose imager-IR General purpose imager-

spectrometer (1.2-22microns)spectrometer (1.2-22microns)

Guest & replicated instruments Guest & replicated instruments

Page 24: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

Wide-field Integral-field spectroscopy:Wide-field Integral-field spectroscopy:

Definitively a most interesting and powerful unfulfilled niche in Definitively a most interesting and powerful unfulfilled niche in modern observational astronomy modern observational astronomy

But …But …

Is it possible and affordable?Is it possible and affordable?

Yes! actually just optimizing a present-day proven telescope Yes! actually just optimizing a present-day proven telescope concept like the Magellan 6.5 m telescopes concept like the Magellan 6.5 m telescopes

Page 25: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

KAOS ConceptKAOS Concept (Modified Gemini / Subaru) (Modified Gemini / Subaru)

KAOS Purple Book, 20021.5 degree field of view

Modifying an existing general-purpose facility can be very expensive, conflicts with other operations and is not necessarily the most efficient route

Page 26: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

Wide Field Sampling & Integration: Wide Field Sampling & Integration: compromising solutionscompromising solutions

1.5° Field of View(5400”)

1.77 square degrees

Lots of sampling elements:2.4x107 squared arcsecs

=>

A. Full wavelength coverage with a sparse spatial coverage (integral field spectroscopy system)

B. Full spatial coverage with a sparse wavelength coverage (tunable imager)

Page 27: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

KAOS Sampling (~ 4800 fibers)

Fix and movable IFUs(add-ons)

Target and Survey Observations:

Not incompatible Observing operation maximized by a specialized program/team to exploit every pointing Wide-Integral-Field Spectroscopy (basic set of observing modes):

Optimal (~full) spatial and spectral coverage & resolution Excellent data for an extremely wide range of astronomical projects (point and extended objects)

Coordination of both telescopes

Wide-Integrated-Spectroscopic SPM Telescope(4000-8000 fibers)

1. Fixed high spatial resolution IFU: 0.25” sampling of a few arc-secs 2. Fixed medium-resolution IFU: 0.5”-1.0” sampling of a few arc-min3. Extra or a few movable medium-resolution IFUs4. ~2” – Fiber sea sampling rest of field (as in KAOS)5. Vis & NIR “arms”

Page 28: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

Maps of a) the stellar surface brightness, b) the mean streaming velocity, c) the velocity dispersion, d) the Mgb line-strength, and e) the Hbeta line-strength of NGC 4365. The maps are based on two partially overlapping SAURON pointings.

Page 29: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

SAURON maps of NGC 7742, based on 1 pointing, exposed for 3x1800 + 1x900 s. The field-of-view is 33"x41" and the spatial sampling is 0"8x0.8". The top panels show the emission-line intensity distributions of O[III] and Hbeta, followed by a colour-coded reconstructed image composed of [OIII] (blue), blue continuum (green), red continuum (red) derived from the SAURON data, and a similar colour-coded image composed of HST/WFPC2 exposures with the F336W (blue), F555W (green) and F814 (red) filters. The bottom row shows (from left to right) the derived gas velocity and velocity dispersion fields, and the stellar velocity and velocity dispersion fields.

Page 30: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

dR dm dlR m l--- = --- = ---

Tunable imaging: Tunable imaging: full field of view coveragefull field of view coverageover finite wavelength intervalsover finite wavelength intervals

m = 2 l cos

R = m N

100 - 1000 4 - 40 1.5 - 15 m

Page 31: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

NGC 7130: TF NGC 7130: TF (H(H, [NII], [SII], [SIII]), [NII], [SII], [SIII])

Can now observe arbitrary lines at an arbitrary redshift...

Luminous IR NGC 7130H, [NII]6583, [SII]6717, [SII]6717

Page 32: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

TF charge shuffle imagingTF charge shuffle imaging

Ratio maps are possible in non-photometric conditions...

Page 33: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

OSIRIS: OSIRIS: TF TF RResolving esolving PPowerower

.mN

Finesse: ,1111

2222adr NNNN

350 400 450 500 550 600 650 70025.5

26

26.5

27

27.5

28

28.5

29

29.5

30

30.5

Wavelength (nm)

Effe

ctiv

e fi

ness

e

Effective finesse for blue OSIRIS TF

600 650 700 750 800 850 900 950 100040

41

42

43

44

45

46

47

Wavelength (nm)

Effe

ctiv

e fi

ness

e

Effective finesse for red OSIRIS TF

400 500 600 700 800 900 10000

200

400

600

800

1000

1200

1400

1600

1800

Wavelength (nm)

Re

solv

ing

po

we

r

OSIRIS TF: Available resolving powers

Page 34: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

Narrow field telescope:Narrow field telescope:Observational nichesObservational niches

Adaptive OpticsAdaptive Optics– Increases resolution (~diffraction limit)Increases resolution (~diffraction limit)– Increases sensitivity for faint sourcesIncreases sensitivity for faint sources– Adaptive Optics performance far better in good-seeing sitesAdaptive Optics performance far better in good-seeing sites– Wide science: provides ultra-high resolution imaging, Wide science: provides ultra-high resolution imaging,

coronography, high resolution spectroscopy, …coronography, high resolution spectroscopy, … Near-IR and mid-IR imager/spectrographNear-IR and mid-IR imager/spectrograph High resolution/stability spectrometer High resolution/stability spectrometer

Page 35: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

Seeing statistics (DIMM 2000-2003, 15 m height)Seeing statistics (DIMM 2000-2003, 15 m height)

Page 36: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

Seasonal changesSeasonal changes

Page 37: Korean Large Telescope : The Plan Yong-Ik Byun 邊鎔翊 Yonsei University, Seoul 延世大學校, 首爾 ( 漢城 )

SummarySummary

Korean Community now aims for 6.5-meter Korean Community now aims for 6.5-meter dual telescopes at SPM with Mexico dual telescopes at SPM with Mexico

Fund raising effort is on-going Fund raising effort is on-going (USD5M for 2006)(USD5M for 2006)

Biggest concern is whether KLT would give Biggest concern is whether KLT would give us what we want, ie. Competitive scientific us what we want, ie. Competitive scientific edge in the error of much bigger telescopesedge in the error of much bigger telescopes

Efforts are being made to identify scientific Efforts are being made to identify scientific agenda which need to be reflected into agenda which need to be reflected into telescope/instrument designtelescope/instrument design