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Present status of JASMINE projectsN.Gouda1) and JASMINE Working Group

1:National Astronomical Observatory of Japan

JASMINE---Japan Astrometry Satellite Mission for INfrared Exploration---

Nano-JASMINE Small-JASMINE JASMINE

Commission 8 science meeting @ IAU GA2829 Aug. 2012

Hop: Nano-JASMINE launch date: Nov.2013~March.2014very small nano-satellite: 35kg, (50cm)3

the diameter of a primary mirror: 5cmthe first space astrometry in Japan

Step: Small-JASMINE target launch date : ~2017step -by-step approach to JASMINE forboth science and techniquesthe diameter of a primary mirror: 30cmweight of a satellite: ~400kgsurvey towards the restricted regions of the Galactic bulgearound the Galactic center and some target objects (e.g. X-ray binaries)

Jump: JASMINE target launch date: the first half of 2020’sthe diameter of a primary mirror: 80cmweight of a satellite: ~1500kgsurvey towards the whole region of the Galactic bulge

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1 Nano-JASMINE

First space astrometry in Japanuse of a very small satellite (nano-satellite)Nano-JASMINE satellite:

• size~(50cm)3

• weight~35 kg• 5cm diameter

of a primary mirror with a focal length of ~1.67m

• Target accuracy of parallaxes:~3mas at zw=7.5mag, operation in zw-band(0.6~1.0 m)

• Orbit: sun-synchronized orbit ~800km• Observing strategy :Hipparcos and Gaia type

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Objectives of Nano-JASMINE

*first demonstration of space astrometry in JAPANWe can experience almost the same process from the preliminary design, development to the operation as that in a big satellite.

*Examinations of technical issues for Small-JASMINE and JASMINE・on-board processing: stellar image extractor・ feed back of stellar images to attitude control

*To get proper motions with high accuracies combininga Nano-JASMINE catalogue with the Hipparcos catalogue

proper motion

The position of a star measured by N-J in 2014 will make it possible to derive the accurate proper motion

2014

Determination of orbit elements of binaries with long periods(10 ~40years)

N-J can provide brightstars(G<6mag) which Gaia cannot detect because of saturations.

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Launch: Nov.2013( ~Mar.2014)!!Launcher：*Cyclone4(Yuzhnoye: Ukraine)

Development of spacecraft bus system

Prof.Nakasuka’s laboratory at the University of Tokyo

Spaceport@Alcantara, BrazilCollaboration on N-J data analysis with Gaia data analysis team is ongoing.HIPPARCOS＋Nano-JASMINE=>proper motion with more accuracies

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Hipparcos Tycho2 Nano-JASMINELimiting magnitude

（selected）

（effective）

(complete)

（~complete） （complete）

Number of stars 120,000 2,500,000 200,000 （<7.5mag）

500,000 （<9mag）

Position ,Parallaxaccuracy

1mas （<10mag） 7mas （<7mag）

25mas （<10.5mag）

60mas （<11.5mag ）

3~4 （ <7.5mag ）4~5mas （@~9mag）

+++++++++++++++++0.75mas(<7.5mag)

combined with HIP

Proper motion, 0.8mas/yr 2.5mas/yr 2~4mas/yr（<7.5mag)~0.1mas/yr(<7.5mag),

~0.2mas/yr(<9mag),combined with HIP

3.7812

VVV 15V 9z

Remark: N-J can provide bright stars(G<6mag) which Gaia cannot detectbecause of saturations.

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Accuracy map of parallax

Flight Model

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Fabrication of telescope

Optical component(deposited by Cr and Au)

All mirrors and their structural supports are shaped out of aluminum alloys

Assembled telescopeTotally weigh: 1.7kg

All reflecting surfaces were fabricated with diamond turning machine

12cm

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Schedule of Nano-JASMINE mission(Oct. 2009: CDR for EM)

Oct.2010: FM was fabricated

Now: under some tests of the FMpreparation for data analysis and operation

Nov. 2013(~ Mar.2014): Launch

~2-3 years operation

~ 2015: Data release v1:proper motion combined with the HIPPARCOScatalogue using about 0.5~1 year data of the N-J

~ 2016-2017: v2:more accurate proper motions , parallaxes, photometry variations, etc.

.

Good scientific targets：bright stars（G<6mag)

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2. Small-JASMINE Astrometric Measurement in Hw-band(1.1m~1.7m)Infrared astrometry missions have advantage in surveying theGalactic bulge, hidden by interstellar dust in optical bands!Accuracy:

parallax:10 as ~70 as for Hw<11.5mag

proper motion:10as/yr ~70 as/yr for Hw<11.5mag

position:8 as ~40 as for Hw<11.5mag

Survey Area: Near the Galactic center+ some directions toward interesting target objects

Maser objects measured by VERA and /or Gaia will be used to calibrate distortions of frames. Blue points represent objects which will be certainly observed by VERA. Red points show objects which may be observed.

An example of the survey region in the Small-JASMINE mission

region1(higher accuracies)

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Cf. VERAVERA is the only VLBI array dedicated to phase-referencing astrometryperformed in Japan.

Schematic view of single-beam (left) and dual-beam (right) VLBI stations.In dual-beam mode, two adjacent sources are observed simultaneously, and atmospheric fluctuations, which are common to the two sources, are cancelled out as far as relative positions of two sources are measured.

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The Number of Objects: about several tens of thousands in the Galactic bulge

Observing strategy : Frames –Link MethodThe target launch date is around ~2017Mission life: ~3 yearsOrbits: sun synchronized orbit ~550km Launcher: solid rocket under development by JAXA

Small JASMINE

Development effort of NAOJ with JAXA (Japan Aerospace eXploration Agency)and universities in JapanInternational collaboration with JMAPS team @USNO

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Advantage of JASMINE, Small-JASMINESmall-JASMINE and JASMINE are the unique space astrometric

measurements in Hw-band and Kw-band to get the accurate astrometric data for many stars in the Galactic bulge.

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Small-JASMINE: ~ a few 103 stars of the bulge in its small survey area (region1)(with <0.1)

* Gaia: ~a few stars in the same area as that in Small-JASMINE (with <0.1)------------------------------------------------------------------------------------------------JASMINE: ~a few 106 stars of the bulge in the survey area (with <0.1)* Gaia: ~400 stars in the same area as that in JASMINE (with <0.1)

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/ /

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Survey area ofSmall-JASMINE

Scientific targets of Small-JASMINE１．The origin and evolution of the Galactic bulge

＊3D-distributions of stellar positions and velocities in the bulgeX-shape of orbitsGrav. potentialclassical bulge vs pseudo bulge origin? effects on galaxy formations and evolutions

＊star formation history in the Galactic bulge２．Astrophysics around the Galactic center

＊Formation of Super massive black hole at the Galactic centerEffect on stellar velocity distribution＊Motion of star clusters the origins of star clusters,

the gravitational potential field around the Galactic center＊existence of an inner bar structure effect on star formation around the center＊Frequent and long-period monitor of SgｒA* existence of QPOInformtion of spin of SM-BH

３．Compact celestial objects＊Determination of orbit element X-ray binaries Big revolution! physics of accretion disk and jets

a good candidate：Cyg X-1:(l=71°, b=+3°), period:5.6 days( unmeasurable by Gaia) companion star: mv~9mag , change of the position: 40~50μasmeasurable by Small-JASMINE

４．Extra-planets＊detection of planes by astrometric method＊secondary eclipse of planets the surface temperature and the orbit elements of the planets

５．Gravitational lens６．Stellar physics, Star formation＊3-Ddistribution of inter -stellar dust＊annual parallax and proper motions of Mira-type variable stars in the bulge

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International collaboration on scientific observationswith APOGEE project

The Apache Point Observatory Galactic Evolution Experiment

2.5m telescope at the Apache Point ObservatorySpring 2011 – Spring 2014

100,000 giants to magnitude H=12.57000 stars in the Galactic bulge

R~20000- 30000, S/N~100Wavelength-range: 1.52-1.69m

velocity error 0.5 km/s

Gazing at the Inner Galaxy

PI: S. Majewski (UVa)High-resolution H-band spectroscopic survey

Bulge

2.5m telescope

APOGEE-SouthSteven R. Majewski (UVa), Ricardo P. Schiavon (Gemini), Carlos Allende Prieto (IAC), Nobuo Arimoto (NAOJ), Martin Asplund (MPA), Beatriz Barbuy (IAG), Timothy C. Beers (NOAO), Jonathan Bird (OSU), Dmitry Bizyaev (APO), Michael Blanton (NYU), James Bullock (UCI), Joleen Carlberg (DTM), Jeff Carlin (RPI), M ́arcio Catelan (PUC-Chile), Cristina Chiappini (AIP, Geneve, INAF), Mei-Yin Cho (Academia Sinica IAA), Edgardo Costa (U. de Chile), Jeffrey Crane (OCIW), Ka ́tia Cunha (UofA/ON-Brazil), Roelof de Jong (AIP), Damian Fabbian (IAC), Peter Frinchaboy (TCU), Jay Frogel, Anibal Garc ́ıa Hernandez (IAC), Ana Elia Garc ́ıa P ́erez (UVa), Doug Geisler (Concepci ́on), Leo Girardi (Padova), Naoteru Gouda (NAOJ), Andy Gould (OSU), Eva Grebel (Heidelberg), Fred Hearty (UVa), Vanessa Hill (Observatoire de la Coˆte d’Azur), Jon Holtzman (NMSU), Inese Ivans (UU), Paula Jofr ́e (MPA), Jennifer Johnson (OSU), Kathryn Johnston (Columbia), Daniel Kelson (OCIW), Juna Kollmeier (OCIW), David Law (U.Toronto), Sara Lucatello (Padova), Suvrath Mahadevan (PSU), Sarah Martell (Heidelberg), Patrick McCarthy (OCIW), Andrew McWilliam (OCIW), Szabolcs Meszaros (IAC), Dante Minniti (PUC-Chile), Ricardo Mun ̃oz (U. de Chile), David Nidever (UVa), Robert W. O’Connell (UVa), Chris Palma (PSU), Kaike Pan (APO), Eric Persson (OCIW), Mark Phillips (OCIW), Marc Pinsonneault (OSU), Marina Rejkuba (ESO), Annie Robin (Besanc ̧on), Helio J. Rocha-

Pinto (UFRJ), Ata Sarajedini (U. Florida), Ralph Scho ̈nrich (MPA), Mathias Schultheis (Besanc ̧on), Kris Sellgren (OSU), Steve Shectman (OCIW), Matthew Shetrone (HET), Michael Siegel (Swift-PSU), Joshua Simon (OCIW), Michael Skrutskie (UVa), Verne Smith (NOAO), Chris Sneden (UT), Jennifer Sobeck (U. Chicago), Mathias Steinmetz (AIP), Andrew W. Stephens (Gemini), Ian Thompson (OCIW), Takuji Tsujimoto (NAOJ),

Elena Valenti (ESO), Kim Venn (UVic), Sandro Villanova (Concepci ́on), John Wilson (UVa), Gail Zasowski (UVa), Manuela Zoccali (PUC-Chile)

The 2.5-m du Pont telescope at Las CampanasObservatory

~90000 stars in the bulge mission time: 2014~2019

Powerful scientific collaboration between JASMINE and APOGEE

Observing strategy and data reduction

Survey area (region1)~1 degree 1 degree

toward the Galacticbulge

Field of view: 0.61degree 0.61 degreeStage 1: Stellar images on this field of view will be taken with an integration time of 7 seconds. 16 sets of stellar images exposed successively 16 times on a field of view is termed ``a small-frame''.Stage 2: The telescope moves towards another adjacent field of view (small-frame) overlapping the previous small-frame (overlapping area is about a half of the frame). In about 45 minutes, the telescope takes the stellar images over the whole survey region, covering it by 16 small-frames.Stage 3:We repeat the procedure at the stage 1 and 2 during the whole mission life and finally about ~9,000 large- frames will be observed. Combining these large- frames allows to determine the astrometric parameters using calibration stars whose astrometric parameters have been already determined accurately. Linear and annual variation of size, location, orientation, distortions of each large-frame can be fixed by calibration stars.

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Preliminary design of Small-JASMINE instrument• Optics design: Modified Korsch System (3mirrors) • Material: Synthetic Silica (a candidate)• Aperture size: 0.3m• Focal length: 3.9m• Field of view: 0.61 degree 0.61 degree

• Detector: Hw-band: HgCdTe(H4RG), Number of detectors: 1

pixel size:10mthe number of pixels:4096 4096potential well:100,000

read-out noise :30e

Structure model of the mission system (JAXA)

J, H-bands for photometry

Pointing stability of the telescopeCritical noise

*smearing of stellar images due to fluctuations of the telescope pointing

stability of the telescope pointingRequirements:

Pointing stability in the Small-JASMINE mission:370 mas/7 sec OK ( disturbance from a reaction wheel

in the bus system and etc.: <300mas/7s)

Stray light:Reduction of the effect by baffle hood + material with very low reflectance which is set inside thetelescope

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Stellar image on the detector

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Thermal stability of the instruments

At stage2:Critical Systematic Error sources:

small-frames may have different sizes and distortions at each time caused by the change of the telescope geometry according to temperature time variations. The relative distances of the stellarimages will be artificially changed with increasing time

This fact requires very small temperature variations around the telescope and also the small change of the telescope geometry

Requirement for Small-JASMINE :Within ~0.1nm/45minutes variations of the positions of stellar images on the focal plane (tentative) for region 1

Within ~0.1nm/45minutes variations of the positions of stellar images on the focal plane

Low CTE materials should be used for the mirrors and the structure of the telescope:e.g. Synthetic Silica

CTE ：~10-7@180Kabout 0.6K time-variations of temperature should be attained within around 45 minutes for the region1 survey by Small-JASMINE.

This requirement will be attainable.

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1st order of deformation(expansion, shrink) on the focal plane2nd order of deformation(gradient) on the focal plane

We can estimate time variations of this kind of deformation with an accuracy of 0.1nm/45min by using overlapped stars on the frametime variations of 3rd order and higher orders of deformation on the focal plane

Stability of time variations with less than 0.1nm/45min is attainable due to the temperature stability and the use of low CTE materials

*Thermal stability of the telescope geometryDemonstration experiments are ongoing.

Telescope structure model

Laser interferometer to measure thermal

variations of geometry of the telescope

Accuracy of 20pm(rms) for measuring variations during an hour is attained!!

*Randomization of some systematic errors by combining many small-fields and/or large-frames

Demonstration experiments are ongoing.

experimental setup

第53回 宇宙科学技術連合講演会 28

大フレーム視野角

・・・小フレーム

・ 姿勢マヌーバ＋静定: 0.45deg@30sec・ １枚あたりの撮影時間：3sec・ 指向安定度：280mas@3sec・ 指向制御精度：0.1deg

半視野分

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Integration SystemDesign task of the integration system

• Satellite system-Compatibility of the bus system-Control system of the pointing ofthe telescope

-Thermal structure

Small-JASMINE Ｓａｔｅｌｌｉｔｅ ｓｙｓｙｔｅｍ

Ｍｉｓｓｉｏｎsystem

Ｂｕｓ system Ｔｈｅｒｍａｌ ｃｏｎｔｒｏｌ

Ｓｔｒｕｃｔｕｒｅ

Ｔｅlｅｍｅｔｒｙ

Ｄａｔａ ｈａｎｄｌｉｎｇ

Electronic powerAttitude control

2nd propulsion

commission the task to companies prospects are almost good

Orbit and attitude of the satellite

Sun synchronized orbit: ~550km

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Direction of the bulge

Summer season Spring and autumn season

Thermal controlRequirements: less than 180K at the detectorsless than 200k at the telescope

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This will be attainable using the following thermal model and attitude of the satellite

190K~200K at the telescope

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170K~180K at the detectors

Cooling with Peltier cooling system

Structure

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Data handling

Telemetryamount of scientific data/day:

0.94GB/day for 5 ×5 pixels stellar window2GB/day for 7 ×7 pixels stellar window

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Downlink with X-band communications equipmentwith ~10Mbps for the scientific data

GS(Ground Station)JAXA(Japan), NAOJ(Japan)+GS in China(international collaboration)

+GS in Europe(?)

★Electric powerelectric requirements: 63.9W<supplied power :150W from the bus system

★Mass: 124kg (mission system)~237kg (bus system)

Total:361kg <402kg(upper limit)

★Cost : <１ billion Japanese yen(upper limit)for the mission system

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Management and Schedule・ JASMINE project office at NAOJ 2004.4~・ Small-JASMINE working group at JAXA 2009.1~・Proposal of Small-JASMINE mission to small science-satellite missions executed by JAXA ~2012

Selection process at JAXA/ISAS(Oct.? 2012 ~ March 2012)If Small-JASMINE will be selected as a small science satellite mission,

then・Launch of Small-JASMINE ~2017(target)・Operation ~3 years・Final Data release ~2021(target)

Michael Perryman has become an official member of the Small-JASMINE working group

International cooperation for Small-JASMINEis very important factor for the selection process at JAXA

We hope that some international communities can contribute to the Small-JASMINE mission.

Of course, we welcome proposals of scientific research collaborations.

If Commission 8 could officially support the Small-JASMINE mission, that would be most helpful for our JASMINE team in the selection process at JAXA.

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Jasmine

We would like to ask you for your continuous cooperation and encouragement