Current Status of MIRIS Jeonghyun Pyo, MIRIS Team (KASI) Survey Science Group Workshop High 1 Resort 2015 January 26
Members of MIRIS Team Development Team 한원용 (PI), 이대희 (PM), 가능현, 김일중, 남욱원, 문봉곤, 박성준, 박영식, 박원기, 육인수, 이덕행, 이미현, 이성호, 이창희, 정웅섭, 차상목, 표정현 ( 이상천문연 ), 진호 ( 경희대 ), T. Matsumoto (ASIAA) Science Advisers (SOC) 박수종 ( 경희대 ), 박창범 (KIAS), 선광일 ( 천문연 ), 안경진 ( 조선대 ), 윤태석 ( 경북대 ), 이재우 ( 세종대 ), 이형목, 임명신 ( 이상서울대 ), 조정연 ( 충남대 ), T. Matsumoto(ASIAA) Collaborating Institutions ISAS/JAXA
Instrument MIRIS = Multipurpose InfraRed Imaging System Main payload of STSAT-3, launched on 2013 Nov. 20 SOC + EOC Orbit Altitude ~ 620 km Eccentricity 0.002 Inclination 97.8 deg. LTAN 22.3 o clock
Main Sciences Cosmic Infrared Background Radiation Measure the absolute background and fluctuation Paα Emission Line of the Galaxy Study WIM(warm ionized medium) Compare Paα with Hα and FIR
MIRIS SOC Telescope: refractive, aperture 8cm Resolution: 51.6 51.6 FoV: 3.67 3.67 Observation Wavelength: Broadband filters: 1.1 μm and 1.6 μm bands Narrow filter: Paα line (1.876 μm), Paα continuum lines 0.2 0.4 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 2.3 1.6 μm-band 1.1 μm-band Paα cont. λ [μm] Visible Paα line
Temperature Control MIRIS SOC Telescope: ~195 K (passive cooling) Detector: 90 K (active cooling w/ motor)
Observation Strategy Integration per frame: 2 seconds Integration for 10 frames (20 seconds), then reset the detector Dark current exposures for 4 minutes, followed by sky exposures for 8 minutes Effective sky exposure time per observation: 8 min. 9 / 11 = 6.5 min.
Cosmic Infrared Background Leinert et al. (1998) Sky brightness at near-ir (in space) = Zodiacal Light + Integrated Starlight + Diffuse Galactic Light + Extragalactic Background Light (EBL) Issues EBL = CIB? Source of CIB? First stars (Pop. III) or remainders after subtraction processes Intrahalo Light?
Cosmic Infrared Background Targets: NEP, NGP, SGP 7 7 pointing observations with 50% overlap 4 times observations of ~10 10 area Wavelengths: 1.1 μm and 1.6 μm bands Observe for 8 minutes for each band (effective exposure: 6.5 minutes) Additional observations: NEP Monitoring Observe NEP every two days (1.1 μm and 1.6 μm bands) Can be used to study zodiacal light and for instrument calibration
Cosmic Infrared Background Observation Strategy (e.g., NEPWF) ~10 ~10
Cosmic Infrared Background NEP Wide Field Observations (2014. 3.) 1.1 μm band 1.6 μm band
Cosmic Infrared Background NEP Wide Field Observations (2014. 9.) 1.1 μm band 1.6 μm band
Cosmic Infrared Background NGP Wide Field Observations (2014. 3.) 1.1 μm band 1.6 μm band
Cosmic Infrared Background SGP Wide Field Observations (2014. 10.) 1.1 μm band 1.6 μm band
Cosmic Infrared Background NEP Monitoring Observations : Observe the north ecliptic pole every another day Monitoring and calibration of the detector condition Variation of background brightness due to ZL Useful for ZL study, but no good data in near-ir @ 9 μm (Pyo et al. 2010) @ 3.6 μm (Krick et al. 2010) Time in years starting from Dec. 1 2013
Cosmic Infrared Background NEP Monitoring Observations 1.1 μm band 1.6 μm band 2014 April 16 June 17 August 16 October 16
Cosmic Infrared Background NEP Monitoring Observations 1.1 μm band 1.6 μm band
Cosmic Infrared Background Observations of Deep Fields Observed To be observed
Cosmic Infrared Background Guest Observations Observations of Dark Clouds (Prof. Matsuura, ISAS) On and off observations of dark clouds to study extragalactic background light Observations of Galaxy Clusters (Prof. Matsumoto and Mr. Min Gyu Kim) To study intrahalo light of galaxy clusters
Paα Galactic Plane Survey Cover 360 along the Galactic plane within 3 < b < 3 Total 228 fields: 106 north + 106 south fields + 16 additional fields Effective exposure: ~20 min. per field per filter 2014 Apr.~2014 Aug.: l = 80 to 100 (complete) 2014 Nov.~2015 Mar.: l = 100 to 280 (on going)
Paα Galactic Plane Survey Preliminary Results Paα line filter (PAAL) image Paα dual continuum filter (PAAC) image Paα emission line (PAAL PAAC) image Paα emission line image (bottom) was made by subtraction: PAAL 0.55 PAAC
Paα Galactic Plane Survey Paα emission is mainly from massive star formation regions. Smaller interstellar extinction for Paα emission than for H α emission Hα emission (Finkbeiner 2003) Paα emission (MIRIS) E(B-V) (Schlegel et al. 1998)
Paα Galactic Plane Survey l = +350 to +50 Hα emission (Finkbeiner 2003) Paα emission (MIRIS) E(B-V) (Schlegel et al. 1998) Eagle Nebula Omega Nebula Galactic Center
Paα Galactic Plane Survey l = +50 to +100 Hα emission (Finkbeiner 2003) Paα emission (MIRIS) Cygnus-X complex E(B-V) (Schlegel et al. 1998)
Paα Galactic Plane Survey Paα-line filter Eagle Nebula Paα cont. filter Paα emission Credit: ESO
Paα Galactic Plane Survey Paα-line filter Omega Nebula Paα cont. filter Paα emission Credit: ESO
Paα Observations Nearby H II regions on the Gould Belt: Orion, λ Orionis, IC434, Barnard Loop, Rosette, Gum, California, ζ Ophiuchi Nearby Galaxies: M31, SMC, LMC Star-forming Clouds: ρ Ophiuchi, BFS11-B, Mon R2, NGC1579, Perseus Cloud Planetary Nebulae: Helix Nebula
Paα Observations Preliminary Results: LMC 1.1 μm band 1.6 μm band Paα-line filter Paα cont. filter
Data Reduction SOCdr: Data reduction pipeline for SOC images Python-based, Astropy-powered Use external programs, Astrometry.net, SExtractor and Montage for post-processing Components of SOCdr: getfits(): Wraps functions to query database and to convert raw data to FITS format MainProcessing: Class wrapping main processing components PostProcessing: Class wrapping post-processing components
Plans Orbits / day Mission 1 st Phase (1 mo) 2014 Mar. 2 nd Phase (5 mo) Apr.~Aug. 3 rd Phase (2 mo) Sep.~Oct. 4 th Phase (5 mo) Nov.~2015 Mar. 5 th Phase (8 mo) 2015 Apr.~ CIRB Survey 8 7 Paα Galactic Plane Survey 7 7 User time Calibration (NEP monitoring) 2 1 (2 obs. every other day) 1 1
Plans Homepage: http://miris.kasi.re.kr MIRIS Workshop: 2015 Jan. 28 (Wed) @ KASI Guest Observations: 2015 Apr. ~ Nov. Public Data Release: 2015 Q2