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2012-01-31Faculty Positions in ASIAA [Online Application]
2012-02-28誠徵無線電波研發工程師3名
2012-03-31Substitute Military Service
2012-03-31誠徵電腦系統管理人員乙名
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Upcoming Eventslist of Events

2012-02-06TIARA Winter School on High Redshift Galaxies
2012-03-222012 Advisory Panel Meeting
2012-05-30East Asia VLBI Workshop 2012

Colloquium list of Luchbox Talks

Speaker:Prof. Yasushi Suto (The University of Tokyo)
Topic:Colors of a second Earth
Time/Place:2012-02-03 14:00~15:00 [R1203]

Special Seminar list of Luchbox Talks

Speaker:Prof. Yasushi Suto (The University of Tokyo)
Topic:Cosmological implications of inhomogeneities in intra-cluster gas
Time/Place:2012-02-02 15:30~16:30 [R1203]
Speaker:Tsvi Piran (Racah Institute for Physics, The Hebrew University)
Topic:TBA
Time/Place:2012-02-10 14:00~15:00 [R1108]

AS/NTU Joint Colloquium list of Luchbox Talks

Lunch Talk list of Luchbox Talks

Speaker:Ramon Brasser (ASIAA)
Topic:Oort Cloud and Scattered Disc formation during a late instability in the Solar System
Time/Place:2012-01-30 12:00~13:00 [R1203]
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TEL: 886-2-3365-2200 FAX: 886-2-2367-7849 web@asiaa.sinica.edu.tw
P.O. Box 23-141, Taipei 10617, Taiwan, R.O.C.
11F of Astronomy-Mathematics Building, AS/NTU. No.1, Roosevelt Rd, Sec. 4, Taipei 10617, Taiwan, R.O.C.
Magnetic field strength map for the collapsing core W51 e2, calculated with the polarization-intensity gradient method (Koch, Tang & Ho, 2012, ApJ in press).
Mapping the Magnetic Field Strength in Molecular Clouds: W51 e2
Magnetic field strength map for the collapsing core W51 e2, calculated with the polarization-intensity gradient method (Koch, Tang & Ho, 2012, ApJ in press).
Mapping the Magnetic Field Strength in Molecular Clouds: W51 e2
Model-free direct reconstruction of full mass profiles for five massive galaxy clusters, A1689, A1703, A370, Cl0024+17, and RXJ1347-11, from combined weak and strong gravitational lensing (Umetsu et al. 2011, ApJ in press, arXiv:1011.3044).
Full mass profiles of five massive galaxy clusters
B field map (red-segments) inferred from the polarization of thermal dust emission at 870 micron (black contours) is shown. The asterisk, star, cross and plus mark the position of BN, source I, SMA1 and source n, respectively. The square marks the BN-I center, where the trajectories of BN and I are overlapped ~ 500 yr ago. The BN-I center is also the origin of the 0.3 pc explosive molecular outflows.
Shaped B field lines in the massive star-forming region Orion BN/KL
Magnetic (B)-field maps of massive starformation region W51 e2/e8 from the SMA (red segments) at 870 μm and BIMA (blue segments) at 1.3 mm. At 0.5 pc scale, the B field is uniform across the envelope, indicating that the B field is dominant over turbulence and the envelope is stable at this scale. At 0.02 pc scale, the B field lines are shaped by gravity. A hourglass-shape B field morphology is resolved toward the ultracompact HII region e2 and possibly also toward e8. These results indicate that the role of B field varies in different scales.
Morphology of magnetic field in high mass star formation region - W51 e2 and e8 cores
A Subaru Suprime-Cam image of one of the clusters used in the analysis, A2390, (2.7 billion light years from the Earth). The purple hue shows the dark matter distribution measured by the gravitational lensing effect on distant galaxies (typically 8 billion light years from the Earth), where the darker color indicates the denser dark matter concentration. It shows that the dark matter distribution is elongated along the northwest-southeast direction.
Direct measurement of dark matter halo ellipticity of massive clusters
Hubble Deep Feild and its surrounding field in the infrared. The color image is a combination and deep images taken at 2.1 um (blue) by CFHT, 3.6 and 4.5 um (green) by Spitzer, and 5.8 and 8.0 um (red) by Spitzer.
Infrared Hubble Deep Field
Maps of the large-scale structure of galaxies (purple) and gas temperature distributions within the cluster (pink). Brighter pink indicates higher temperature. The filamentary structure is found outside the cluster in the top-left direction, in contact with the hotter gas realm. The other fields in which there are few galaxies (black) contact the cooler realm. The white line represents 10 million light-years.
Correlation between the temperature of the intra-cluster medium of galaxy cluster A1689 and its surrounding environment of the large-scale-structure.
Artist's conception of molecular outflow from a massive young stellar system in Orion
Explosive disintegration of a massive young stellar system in Orion
Artist's conception of molecular outflow from a massive young stellar system in Orion
Explosive disintegration of a massive young stellar system in Orion
Joint constraints on the dark-matter halo structure parameters of the galaxy cluster CL0024+1654 (z=0.395) from full lensing analysis of Subaru weak lensing and ACS strong lensing data (Umetsu et al. 2010, ApJ, in press; arXiv:0908.0069).
Joint constraints on the DM halo structure parameters from full lensing analysis (CL0024+1654)
Thermal Sunyaev-Zel'dovich effect (tSZE) images of six galaxy clusters observed with the 7-element AMiBA (AMiBA-7) in 2007. Figure taken and modified from Wu et al. 2009, ApJ, 694, 1619.
AMiBA-7 tSZE maps
Phase-locked loop evaluation board for GaAs HBT Voltage-Controlled Oscillator MMIC module
Phase-locked loop evaluation board
Subaru BRZ pseudo color image of the central 3'x3' region of the galaxy cluster CL0024+1654 (taken and modified from Umetsu et al. 2010, arXiv:0908.0069).
Lensing galaxy cluster CL0024+1654 (z=0.395)
Cryogenic IF Low Noise Amplifier (LNA) for ALMA for 4-12 GHz using 0.15 mHEMT
Cryogenic IF Low Noise Amplifier
Voltage-Controlled Oscillator MMIC for ALMA Band-1 using 2um GaAs HBT
Voltage-Controlled Oscillator for ALMA Band-1
The figure demonstrates simulated deep AMiBA cluster surveys via the Sunyaev-Zel'dovich effect (SZE) based on N-body/Hydrodynamic simulations. The top-left panel shows a model SZ sky map, and the top-right panel shows a realization of SZE (top-left) + CMB
A model Sunyaev-Zel'dovich effect (SZE) sky map
SiO(7-6) image generated by non-LTE radiative transfer simulations along with MHD simulation. The low-mass (0.6 solar mass) object at the earliest stage of star formation shows significant irregular morphology compared with the currently observed, more ev
The Telescope of theory: synthetic SiO(7-6) emission from a young low-mass protostellar object embedded in an infall envelope
The central region of the Seyfert 1 galaxy NGC 1097 mapped with the SMA in 12CO(2-1) (lower-right image). NGC 1097 is a nearby galaxy with a large-scale bar (left image), and hosts a circumnuclear starburst ring (upper-right image). Straight dust lanes al
The central region of the Seyfert 1 galaxy NGC 1097
Snapshots of density structures at 100 (top) and 1000 (bottom) years, respectively, for different anisotropy in the ambient mass distribution induced by magnetic field (Shang et al. 2006, ApJ, 649, 845).
Snapshots of density structures