HST (OPTICAL) Harms + 1994 M87 Walker+2007 VLBA( Radio Interferometry, VLBI) Junor+1999
1um / 2.4m http://asd.gsfc.nasa.gov/archive/hubble/ 3mm / 300m 3mm / 45m
Japanese VLBI, D=2000km
Radio IR Visible UV X- ray γ -ray Realized Telescopes VLBI High Resolution Lobanov, A.P. 2003, SKA Memo 38
Antenna Diameter of Source Station 1,2 Flux 1 Integration Time kS 2 2 BT T T 1 2 bandwidth Receiver noise
OCTAVE (Network base) Whitney 2011
OCTAVE : Optically Connected Array for VLBI Exploration SINET4 JGN-X Tomakomai11m Local Access line H.U Y.U. Wideband 10GbE Network Kashima34m Yamaguchi 32m NAOJ Otemachi Correlation Center NIFS KEK GSI 32m Gifu11m
In scientific operation as an element of JVN (Japanese VLBI network)
VLBI Observation of Fermi /LAT Un-associated Gamma-ray Sources • Identify the un- identified γ -ray sources using “high sensitivity” VLBI – search for new γ -ray emitting VLBI sources Fermi/LAT 3-years all sky map, Fermi Webpage
Niinuma+2013 AP-RASC'13, Taipei Taiwan, 2013 Sep 7 VLBI observation for Fermi-FoVs • Obs. Status: – Date: 2012 Dec 1, 2, 3, 8, 24, total of 70-hrs – 1-baseline: Yamaguchi – Tsukuba (~800 km) – Freq. (ΔB): 8.4 (0.512) GHz – Maximum angular resolution: 9 mili-arcsec – T_int: 3 min (for every sources) – S ν_min : ~ 2 mJy (T B_min > 3 x 10^5) : observations (~ 0.8 mJy (T B_min ~ 1.4 x 10 5 ) : calculation) • Target: – We conducted observations for 150 un-IDs ( = 845 sources which are 70% of all our targets) *all δ >= 0 deg sources, and several δ < 0 deg sources
AP-RASC'13, Taipei Taiwan, 2013 Sep 7 Detection of new VLBI sources • Total of 27 new VLBI sources – 17 detections – 10 marginal detections • All VLBI sources were found one by one for each un-IDs – These VLBI sources are • possible counterpart to each unIDs? new VLBI source within Fermi-FoV • γ -ray emitting blazars? – Further multi- ν VLBI obs. will be planed to know morphology and radio spectra Niinuma+2013 won YSA2013
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