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Infrared Space Astrometry Infrared Space Astrometry missions: JASMINEmissions: JASMINE

Naoteru GoudaNaoteru Gouda Director of JASMINE Project OfficeDirector of JASMINE Project Office National Astronomical Observatory of JapanNational Astronomical Observatory of Japan

7 August, 2015

★★JASMINEJASMINEー Japan Astrometry Satellite Mission for INfrared Exploration －

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2017(?)-

2021(?)-

the late 2020s

◎Japanese group is promoting space astrometry missions, 　　 JASMINE 　 projects series, in international collaboration with 　　 Gaia DPAC team. JASMINE will play complementary roles of Gaia missions.

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§1. Nano-JASMINE First space astrometry in Japan use 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 ~1.67mAll Sky Survey in zw-band(0.6~1.0m)Target precision of parallaxes: ~3mas( zw<7.5mag) Orbit: sun-synchronized orbit ~800km Observing strategy :Hipparcos and Gaia type

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Flight Model was accomplished in Oct. 2010.

Fabrication of telescopeAll mirrors and their structural supports are shaped out of aluminum alloys

All reflecting surfaces were fabricated with diamond turning machine

BeamBeam--combinercombiner M1M1 M2M2

M3M4M5

BeamBeam--combinercombiner M1M1 M2M2

M3M4M512 cm17 cm

BeamBeam--combinercombiner M1M1

12 cm17 cm

BeamBeam--combinercombiner M1M1

Optical component(deposited by Cr and Au)

Assembled telescopeTotally weigh: 1.7kg

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The development of the spacecraft bus system has been done in collaboration with Prof Nakasuka’s laboratory at the University of Tokyo.

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Objectives of Nano-JASMINE

*first demonstration of space astrometry in JAPAN

We 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

*To get proper motions with high precisions by combining

a Nano-JASMINE catalogue with the Hipparcos catalogue

proper motion

The position of a star measured by N-J in 2017 will make it possible to derive the accurate proper motion

2017

*Determination of orbits of binaries with long periods(10 ~40years)

proper motion precision~ 0.1mas/yr

★Complement of the Gaia mission＊ It is hard for the Gaia mission to measure the centroids of the bright stars(<6mag) due to the saturation of stellar images on its detectors.

＊ At present, Gaia is the unique space astrometry mission operating the whole sky survey. The validation of the quality of the Gaia data requires other independent data of, in particular, proper motions measured 　 over the whole sky for their calibrations.

Nano-JASMINE

The data analysis software of Nano-JASMINE has been developing in good collaboration with Gaia DPAC team (in particular, CU3).

In addition, Gaia team (in particular, CU9) and JASMIE team are aiming to make a data archive together composed of the Gaia catalogue and the Nano-JASMINE catalogue (funds: EU-FP7 of GENIUS)

◎We are promoting Nano-JASMINE in close relation to the Gaia mission.

JASMINE team greatly appreciate Gaia team’s strong support!

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Nano-JASMINE （ NJ ） Catalogue (All sky survey)

Number of stars 520,000 stars (-1　mag<zw<9　mag)(200,000 stars(-1　mag<zw<　7.5　mag)

Position precision 2-3 mas@<7.5mag 3-4mas @9mag

Parallax precision 3-4mas @<7.5mag 4-5mas@9mag (NJ data only)~0.75mas@<7.5mag ~1.2mas@9mag (by using NJ data and Hipparcos catalogue)

Proper motion precision

2-4mas/yr　　@<7.5mag 　 3-6mas/yr@9mag　　　(NJ data only)　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　　~0.1　mas/yr　@<7.5mag　　　~0.2　mas/yr@9mag　　　　　　　　　　　　　　　　　　　　( by using NJ data and Hipparcos catalogue)

Frequency of observation

　More　than　6　times　a　year.　

D. Michalik, IAU289

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★Scientific outputs expected by Nano-JASMINE

〇 binary systems with long periodse.g. Polaris A and B with the orbital period of 29.59 yrs

〇 the birthplaces of massive starse.g. Betelgeuse in Orion

〇 the structure and evolution of massive star formation regions

〇 the positions and motions of neaby star clusters

e.g. Hyades and Pleiades clusters

〇 discrimination between optical double stars and physical binaries

e.g. Mizar and Alcor (degree of confidence: 1.1P)=>8.3 (HIP+NJ)

〇 origin of runaway stars

By science working group(Chair: Prof.Nishi (Niigata Univ.))

e.g. inner motions of maser spots measured by VERA relative to a star

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Preparatory state of Nano-JASMINE

*Maintenance of FM: continuous tests of performance of the telescope

Measurement of PSF

*Ground stations:

*Data analysis: The software has been developing in good collaboration with Gaia DPAC team (CU3&CU9)!

Tokyo station:3m antenna at the University of TokyoUplink and downlink of HK dataof the satellite

Mizusawa station:10m antenna at Mizusawa campusof NAOJ.Downlink of scientific data

*Trainings simulating actual operation:

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Launch Launcher ：　　　 *Cyclone4 (Yuzhnoye: Ukraine)

Spaceport@Alcantara, Brazil

Launch schedule at the present time:the end of 2015

The launch has been pushed back due to delays in the construction of the Alcantara Space Center launch sitein Brazil.

Yuzhnoye company told us in Feb.2014 that we will have tests for adjusting the rocket/satellite interface in Ukraine using our EM in April , 2014.

Instability of political situation in Ukraine since Feb. 2014…

We are concerning about the further postpone of the launch.

It is very difficult to find another launch service because we have some constraints (cost, orbit, separation mechanism etc.) for the launch of Nano-JASMINE.

We have possibility now that ESA can launch the Nano-JASMINE satellite in late 2017. Gaia team is strongly supporting the launch by ESA.

The schedule of the tests in Ukraine is still uncertain.The construction of the space port has not started again yet.

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§2. Small-JASMINE

Nuclear bulge around the Galactic center

Astrometric Measurement in Hw-band(1.1m~1.7m)Infrared astrometry missions have advantage in surveying theGalactic nuclear bulge, hidden by interstellar dust in optical bands!Precision: parallax: 10 as ~20 as for Hw<11.5mag　　　 　 proper motion: 10as/yr ~50 as/yr for Hw<11.5mag photometry(Hw-band) <0.01 mag

Survey modes１． survey for the key project in spring and autumn 2. survey for open use in summer and winter

some directions toward interesting target objects

(e.g CygX-1, planetary systems of brown dwarfs, star-forming regions besides the area near the center)

We have been aiming at the submission of a proposal for the Small-JASMINE mission to the small science satellite program executed by JAXA.

Phenomena with short periods

Advantage of Small-JASMINE:High frequent measurements of the same target

every 100 minutes!

Merging of small BHs (dynamical friction)

Effect on stellar phase space distribution

★main scientific objective of Small-JASMINE

初代ブラックホール星質量？ 大質量？

ブラックホール成長合体？ガス降着？

楕円銀河

SMBH

バルジ

円盤銀河 バルジ

SMBH

ダークマター宇宙階層的構造形成

原始銀河矮小銀河

多重BH銀河？

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ブラックホール・銀河バルジ質量関係 銀河中心外BH

ブラックホール超巨大化

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？ ？

SJ’s data will determine whether the SMBH was formed through merging process of multiple black holes with more than 99.7% confidence level.

By science working group(Chair: Prof.Umemura (Tsukuba Univ.))

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Distribution function

1 ． Why do supper massive black holes(SMBHs)

exit in our universe? merging of small BHs?

one of the biggest issues in astrophysics!

need observational data on SMBHs

*precise and detailed data =>nearest SMBH

SMBH at our Galactic center (4 million times the solar mass)

SJ will provide scientific outputs over the widely spread fieldsof astronomy and astrophysics.

A. .Astrophysics around the Galactic center

Enough number of stars measured with high precisionsby SJ

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2. Prediction of future activity around the Galactic center

Gas fueling is very important for activities of galactic nuclei, the growth of SMBH,

nuclear star bursts and the formation of super star clusters in a galactic central region.

Bar potential with the figure rotation Ω 　

rotating bar=>Complicated orbits: coexistence of X1 and X2 orbits

Losing angular momentum and energy of gas

For example, SJ will determine whether the pattern speed Ωof the potential has a value larger than ~150km/s/kpc with more than 99.7% confidence level. If yes, it is easy for gas to transport to the region around the center.*A numerical simulation suggests that the gas can accrete to the central region of the Galaxyif the pattern angular speed is larger than around 150km/s/kpc.

*Galactic model: bar (Ferres model)+bulge (exponential profile) + disk (Sofue model)+ dark halo (NFW) +supermassive black hole

*need to clarify transport mechanism of gas to galactic centers

*detailed and precise observational data our Galactic center

SJ’s data will constrain models of the gravitational potential in the Galactic nuclear bulge region (within ~300pc away from the Galactic center)

◎ candidate of key processes for transportation of gas :

bar structure at the galactic nuclear bulge region

(within ~300pc away from the Galactic center)

*Existence of an inner bar? If yes, feature of the (inner) bar potential?

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(3) Motion of star clusters the origins of star clusters around the Galactic center

(5) Compact celestial objects Determination of orbit element of X-ray binaries and -ray binaries

Big revolution! physics of accretion disk and jets, etc.

　　　 *a good candidate of X-ray bursts ： Cyg X-1:(l=71°, b=+3°)

period:5.6 days( unmeasurable by Gaia) companion star: mv~9mag , change of the position:

40~50μas measurable by Small-JASMINE

*Cas: WD or NS=>1degree of confidence, HESS J0632: NS or BH (2

(6) Extra-planets

detection of planets by astrometric method *determination of mass with precisions of <20% for stars measured by RV

*primary star: low-mass star(late M-dwarf, brawn dwarf): H-10mag,V=16-18mag

(7)Gravitational lens: Search of Wormholes!?

(8)Stellar physics, Star formation＊ 3-Ddistribution of inter -stellar dust

＊ annual parallax and proper motions of Mira-type variable stars in the bulge

(4)Anaysis of symbiotic X-ray binaries

the origin of X-ray emission spread along the galactic plane.

B. Astrophysics besides the Galactic center

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Small JASMINE

Development effort of NAOJ with JAXA (Japan Aerospace eXploration Agency)

and universities in Japan

The target launch date is around ~2021

Mission life: ~3 years

Orbits: sun synchronized orbit ~550km

Launcher: Epsilon launch vehicle(solid rocket) provided by JAXA

Design of Small-JASMINE instrument• Optics design: Modified Korsch System (3mirrors) • Material: Clearceram • Aperture size: 0.3m• Focal length: 3.9m• Field of view: 0.6 degree times 0.6 degree• Detector: Hw-band: HgCdTe(H4RG), Number of detectors: 1 pixel size:10m

the number of pixels:4096 times 4096 potential well:100,000 read-out noise :30e

J, H-bands for photometry: 2×H1RG

*Information of radial velocities , chemical composition and photometry (in other bands) is complementary to Small-JASMINE for the scientific targets in the Galaxy.

Cooperation with APOGEE-2(S ) is very strong synergy for studies of the Galactic bulge.

MOU for powerful scientific collaboration between APOGEE-2(S), SDSS-IV collaboration and Small-JASMINE has been concluded.

International scientfic collaborationAPOGEE-2(S) project: High-resolution H-band spectroscopic survey at the Las Canpanas Observatory

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★We have accomplished the conceptual design of the satellite system in which the mission requirements and system requirements are satisfied.

○capabilitiy of the mission instrument 　＊ decrease in the stray light　　＊ decrease in contamination and outgas ＊ thermal environment around the telescope(278K ) and detector(<170K).　　＊ the stability of the thermal structure　　　　 　＊ poiting stability of the telescope

○telemetry ： X-band for downlink of scientific data○command & data Handling ： no big issues○attitude control ： no big issues○electric power ： enough margin

○data anaysis ：

○cost(including the budget for risk management) ：　　 within the upper limit(8.5 billion JPN) for the small science satellite program executed by JAXA.

We will perform multiple steps to verify the feasibility of the critical techniques by constructing various manufacturing models (BBM, EM, PFM and FM) *optics, (thermal stable) structure, thermal control

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The establishment of the Small-JASMINE working group at JAXA (Japan Aerospace Exploration Agency) was approved in January 2009 by a science committee of ISAS (Institute of Space and Astronautical Science) of JAXA. The WG is entitled to apply for R&D funds and to submit a mission proposal. JASMINE-WG has got the funds for R&D and has been promoting some feasibility tests for some key techniques necessary to realize the Small-JASMINE satellite.Our working group has been aiming at submitting a mission proposal for the ISAS call for small-sized scientific satellite mission proposals.

Last year, we submitted the mission proposal to ISAS/JAXA. SJ got the highest scores among the proposed “ 4 science missions” for its scientific significance and feasibility.However, it is regret that SJ did not remain as a final candidate (the final candidate is an engineering mission (the first landing on the moon in Japan),not a science mission.

The ISAS call will be opened in this August and the dead line is this November.We are now preparing the revised documents necessary to submit the mission proposal with our best efforts. Thank you very much for your strong support!

★Present status

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Jasmine

Thank you for your attention.