Infrared Space Astrometry mission for the Galactic Bulge

1. Infrared Space Astrometry mission for the Galactic Bulge Naoteru Gouda JASMINE Project Office National Astronomical Observatory of Japan 3 Dec. 2013 1

2. §1. Galactic Bulges §2. Surveys of the bulge of the Milky Way galaxy (the Galactic bulge) §3. Astrometry and Upcoming space astrometry missions §4. Small-JASMINE project §5. WISH as an infrared space astrometry mission

3. ：key tracers of galaxy formations Bulges are complex! §1. Galactic Bulges Box/Peanut bulges (aka pseudo-bulges): e.g. ESO 597-G 036 [NASA] Disk-like bulges (aka pseudo-bulges): e.g. NGC 6782 [NASA] Classical bulges: e.g. M81 [NASA] Box/Peanut bulges(aka pseudo-bulges) Disk-like bulges(aka pseudo-bulges) Classical bulges 〇stick out of the disk 〇box or peanut-like morphology 〇usually featureless 〇usually does not show young stellar populations or star-forming regions 〇kinematically cold: dynamically supported by rotation of its stars 〇the inner parts of bars that grow vertically thick due to dynamical instabilities! 〇 stick out of disk plane (not as flat as the disk) 〇more or less sphroidal 〇featureless: no spiral arms, bars, rings,… 〇mostly old stars 〇kinematically hot: dynamically supported by stellar velocity dispersions 〇seem to be built mostly by mergers, fast bursts of star formation 〇 as flat as the disk 〇substructures: nuclear bars, spiral arms, rings,… 〇young stellar populations or ongoing star formation 〇kinematically cold: dynamically supported by rotation of its stars 〇seem to be built mostly via disk instabilities: continuous, smooth process ・Formations and evolutionary processes of galaxies Key issue: Features of each type, origin and evolution ・Orbits of stars, phase space density in complex structures of bulges

4. Co-evolutions of super massive BH s and bulges ★Supper massive BH at the galactic center Activity of the galaxy Origin and evolution of the super massive black hole at the Galactic center? merging of smalland/or medium BHs? gas accretion? ★The mass of SMBH correlates with the mass of the bulge. (Marconi & Hunt 2003, ApJ, 589, L21) Magorrian relation (STScI/NASA) Connected growth of BHs and bulges!?

5. high-quality observational data( both kinematical and chemical) to test the theories regarding the origin and subsequent history of the bulges §2. Surveys of the bulge of the MW =>The Milky Way: very important target galaxy!! It is possible to observe in the Milky Way indivisual stars in many directions and to obtain information on their 3-dimensional positions, 3-dimensional velocities and metalicitywith good accuracies, which is, in, general, still not possible for galaxies outside the MW. The Milky Way box/peanut bulge! COBE/Diffuse Infrared Background Experiment, etc. Vertically thin long bar + vertically thick inner part(box/peanut) *Bars themselves can evolve secularly through angular momentum transport, producing different boxy/peanut and X-shaped bulges The properties of the bar affects dynamics : spiral arm location, resonances, gas inflow, etc. Clarification of the Galactic bar/bulge and its origin  Very important for studies of the formation and evolution of disk- galaxies

6. VVV survey: ZYJHKs Photometry＋100epochs in Ks Bulge 300 sq deg. VISTA 4.1m telescope at ESO sensitivity:0.84 to 2.5 microns ★Surveys of the bulge of the MW are necessary and important! APOGEEsurvey: High-resolution H-band spectroscopic survey 2.5m telescope at the Apache Point Observatory APOGEE-1(SDSS-III): 100,000 giants to magnitude H=12.5 Bulge stars:7000 R~20000- 30000, S/N~100 Wavelength1.52-1.69mm velocity error 0.5 km/s 15 elements error of 0.1 dex APOGEE-2(S) (SDSS-IV) has been proposed to NSF The same instrument as that of APOGEE-1 will be set at Las Canpanas Observatory ~90,000stars in the bulge Mission period: 2014-2019

7. Photometry, radial velocities and elemental abundances of stars in the bulge of the MW Furthermore we need astrometric parameter: ・annual parallax ・proper motion ★VVV, APOGEE, BRAVA, ARGOS,・・・ 3-dimensional positions and velocities of stars will be provided.

8. Trace of a star :Helical motionannual parallatic ellipse　＋　proper motion(straight line) §3. Astrometry and Upcoming space astrometry missions Astrometry: Fundamental task of measuring stellar positions Repeated measurements 2D-positions of stars in space Helical motion of a star 8

9. 1. Apparent annual elliptical motion *Parallactic Ellipse (annual parallax) Distances of stars 2. Systematic displacement of stellar positions Proper motion *Proper motion + Distance Tangential velocities of stars Helical motions of stars Astrometry＝＞ important information of distances and tangential velocities of stars 9

10. Very important information !! Binary systems, Planetary systems, Gravitational lens effects, effects of starspot, etc. Periodic residual motions Physical characters such as mass of binary stars, mass of planets etc. Residual motions from the helical motion

11. Space Astrometry Projects Remark: Infrared astrometry mission (Small-JASMINE) has advantage in observing stars in the Galactic bulge, hidden by interstellar dust in optical bands. 11

12. (fit error of 0.05mag) G = V - 0.0257 - 0.0924 · (V-IC) - 0.1623 · (V-IC)2 + 0.0090 · (V-IC)3 ★Gaia(ESA’s mission) *Gaia will be launched at 19th Dec. ,2013. *The final catalogue will be released in 2021. *all sky survey in an optical band *G-band（0.33-1.0 micron）、　6mag＜G<20mag *accuracies of parallax: 7~300mas(6<G<20mag) 12 The predicted errors vary over the sky

13. §4. Small-JASMINE project Astrometric Measurement in Hw-band (1.1mm~1.7mm) Infrared astrometry missions have advantage in surveying the Galactic bulge, hidden by interstellar dust in optical bands! Accuracy: parallax: 10 m as ~70 m as for Hw<11.5mag *10 m as distance accuracy:~640pc@8kpc proper motion: 10m as/yr ~70 m as/yr for Hw<11.5mag *tangential velocity accuracy: 0.4~2.8km/s @8kpc (if the distance is accurately determined) position: 8 m as ~40 m as for Hw<11.5mag photometry(Hw-band) <0.01 mag Survey Area: Near the Galactic center + some directions toward interesting target objects (e.g CygX-1, planeray systems, browndwarfs. star-forming regions besides the area near the center) 13

14. The Number of Objects: toward the Galactic bulge： <10kpc: ~120,000(6kpc<d<10kpc: 88,000) （highest accuracy region : <10kpc :10,000, 6kpc<d<10kpc: 6,700) Multi color photometry: J, H and Hw(astrometry) The target launch date is around ~2019 Hw<11.5mag ＊Proposal of SJ mission to small science-satellite missions executed by JAXA in Feb.2014. Mission life:~3 years Orbits: sun synchronized orbit~550km Launcher: Epsilon launch vehicle(solid rocket) provided by JAXA Small JASMINE Development effort of NAOJ with JAXA (Japan Aerospace eXploration Agency) and universities in Japan 14

15. Advantage of Small-JASMINE Small-JASMINE is a unique space astrometric measurement in Hw-band to get the accurate astrometric data for many stars in our Galactic bulge. Survey area of Small-JASMINE Small-JASMINE: ~ a few 103stars of the bulge inits small survey area (with <0.1) Gaia: ~a few stars of the bulge in the same area as that in Small-JASMINE (with <0.1) ★Another advantage: High time resolution!! Small-JASMINE will measure the same target every 100 minutes if the target is located towards the Galactic bulge . If a target is located toward other direction and Small-JASMINE can measure it in summer or winter season, Small-JASMINE measure it frequently as needed. *Gaia can measure the same target every one or two months. 15

16. Scientific targets of Small-JASMINE 1. The origin and evolution of the Galactic bulge 　＊3D-distributions of stellar positions and velocities in the inner part of the bulge its origin and relation to galaxy formations and evolutions 　　＊star formation history in the Galactic bulge 2. Astrophysics around the Galactic center ＊Formation of Super massive black hole at the Galactic center Effect 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 QPO Informtion of spin of SM-BH

17. Good candidates of g-ray bursts: LS5039,J1018,LSI+61 Scientific targets of Small-JASMINE 3. Compact celestial objects ＊Determination of orbit element of X-ray binaries and g-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 * *the Galactic ridge X-ray dim point sources CVs(cataclysmic variables, symbiotic star) or late-type stars 4. Extra-planets ＊detection of planets by astrometric method (e.:g. primary star low-mass star(late M-dwarf, brawn dwarf): H-10mag,V=16-18mag) 5. Gravitational lens: Search of Wormholes!? 6. Stellar physics, Star formation ＊3-Ddistribution of inter -stellar dust ＊annual parallax and proper motions of Mira-type variable stars in the bulge

18. Cooperation with APOGEE-S and VVV is very strong synergy for studies of the Galactic bulge. Information of radial velocities , chemical composition and photometry (in other bands) is complementary to Small-JASMINE for these scientific targets in the Galaxy. MOU forpowerful scientific collaboration between APOGEE-2(S), SDSS-IV collaboration and Small-JASMINE has been concluded.

19. Design of Small-JASMINE instrument Optics design: Modified Korsch System (3mirrors) Material: Synthetic Silica Aperture size: 0.3m Focal length: 3.9m Field of view: 0.6 degree 0.6 degree Detector: Hw-band: HgCdTe(H4RG), Number of detectors: 1 pixel size:10mm the number of pixels:4096 4096 potential well:100,000 read-out noise :30e J, H-bands for photometry Structure model of the mission system (JAXA) 19

20. Integration System Design task of the integration system Satellite system -Compatibility of the bus system -Control system of the pointing of the telescope -Thermal structure Small-JASMINE　Ｓａｔｅｌｌｉｔｅ　ｓｙｓｙｔｅｍ Ｍｉｓｓｉｏｎ　system Ｂｕｓ　system Ｔｈｅｒｍａｌ　ｃｏｎｔｒｏｌ Ｓｔｒｕｃｔｕｒｅ Ｔｅlｅｍｅｔｒｙ Ｄａｔａ　ｈａｎｄｌｉｎｇ Electronic power Attitude control 2nd propulsion commission the task to companies prospects are almost good 第53回　宇宙科学技術連合講演会 20

21. ★Small-JASMINE will provide many interesting results in wide fields of astronomy and astrophysics. We need astrometric measurements for the Galactic bulge survey with larger area which overs the whole region of the bulge than the survey area of the Small-JASMINE. however

22. §5 . WISH as an infrared space astrometry mission WISH：wide survey with accurate measurements in infrared bands WISH has high possibility to play a role as an infrared astrometry mission for the Galactic bulge astrometric measurements with achievement of ~10mas accuracy WISH Pointing stability（70mas/3sec) of the telescope and thermal stability(~0.1K/30h) of the instruments are requiredin the design of the WISH satellite. Required stability of the pointing of the telescope for WISH(70mas/300sec) is sufficient enough to achieve 10μas precisions of asttrometric measurements. *The Galactic bulge survey with area of 6°(b)×16°(l) *Precisions of ~10μas（K<11mag) *necessary observation time: 0.6years/5years(1.4months/1year: 20days in spring and 20days in autumn) *option: survey area of 3°(b)×16°(l) 0.3years/5years

23. Our JASMINE team is willing to contribute to the WISH mission for the resolution of technical issues, the development of the satellite, and data analysis if WISH will play a role as an infrared astrometry mission for the Galactic bulge!! We hope that the WISH mission will be successful.

24. Jasmine Thank you for your attention.