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2010-02-12Administrator

Upcoming Eventslist of Events

2010-02-08 ALMA User Workshop
2010-03-22 2010 Panel Advisory Meeting

Colloquium list of Colloquia

Speaker:Prof. Amy Barger (U. Wisconsin (Madison))
Topic:The Cosmic Evolution of Active Galactic Nuclei
Time:2010-02-11 14:00 - 15:00
Place:R1203
Broadcast:Not available

Lunchbox Talk list of Luchbox Talks

Speaker:Luca Baiotti (Kyoto University)
Topic:TBD
Time:2010-03-10 12:00 - 13:00
Place:ASMAB 12F
Broadcast:Not available
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TEL: 886-2-3365-2200 FAX: 886-2-2367-7849
P.O. Box 23-141, Taipei 10617, Taiwan, R.O.C.
11F of Astronomy-Mathematics Building, NTU. No.1, Roosevelt Rd, Sec. 4, Taipei 10617, Taiwan, R.O.C.
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 sky map at 94GHz as an input to mock observations. At 94GHz, clusters are seen as cold spots on the CMB T-map. Here the sign is flipped, and clusters are shown as hot spots. The primary CMB signal acts as a significant noise source in a SZE cluster search. The bottom panels compare mock AMiBA observations of the same piece of sky with the 7-element (bottom-left) and the 13-element (bottom-right) configurations of 1.2m antennas. A deep survey mode of 400 hours integration is assumed. Cluster detections above 4 sigma are indicated by red circles. As demonstrated in the figure, the expansion from a 7 to 13 element interferometer will improve significantly the sensitivities to distant clusters of a few arcmin scales.
A model Sunyaev-Zel'dovich effect (SZE) sky map
Surface mass density profiles of the galaxy clusters A1689 and CL0024+1654 as reconstructed from full lensing analysis of Subaru weak lensing and ACS strong lensing data (figure taken and modified from Umetsu & Broadhurst 2008 and Umetsu et al. 2009).
Mass Profiles of the Galaxy Clusters A1689 and CL0024+1654
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. 2009, arXiv:0908.0069).
Joint constraints on the DM halo structure parameters from full lensing analysis (CL0024+1654)
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 evolved one because of coexistence of a variety of gas motion, such as infall of the envelope, rotation and outflows. The rotation of the outflow appearing in the velocity channel map is an outcome of the magneto-centrifugal force driven outflow model. Future observation with the ALMA telescope will reveal such structures, and greatly improve our understanding of the launching mechanism of the outflows. (Yamada et al. 2009, ApJ, 703, 1141)
The Telescope of theory: synthetic SiO(7-6) emission from a young low-mass protostellar object embedded in an infall envelope
Magnetic (B)-field maps of W51 e2/e8 from the SMA (red segments) at 870 μm and BIMA (blue segments) at 1.3 mm. The black and gray contours represent the strengths of the continuum emission at 870 μm and at 1.3 mm, respectively. The field lines near the collapsing core e2 and e8 are clearly shaped/pinched, most likely due to accretion. In comparison, the field lines in the 0.5 pc envelope is uniform, indicating the existence of a strong field.
Morphology of magnetic field in high mass star formation region - W51 e2 and e8 cores
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 along the leading edge of the bar connect the ring with the spiral arms (Hsieh et al. 2008).
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
Expected performance of AMiBA with the initial configuration (seven 60cm dishes, close-packed) after 1 month of observations, as compared with other high-l CMB experiments such as ACBAR (2002) and CBI (2004). Also shown are the WMAP best-fitting curve of the temperature CMB power spectrum (solid), and the secondary Sunyaev-Zel'dovich effect power spectrum (cross) from N-body/Hydrodynamic simulations (K.Y. Lin et al. 2004, ApJ, 608, 1L) which dominate the temperature anisotropy on small angular scales of l>2500. The first AMiBA CMB power spectrum data point is targeted around l=1000, which can be compared with existing high-precision measurements of other CMB experiments (e.g., WMAP). The second and third smaller scale structural data points will be targeted at the high angular multipoles of l~2000 and l~2500, where AMiBA will have much better sensitivities than other existing CMB experiments.
Expected performance of AMiBA
Top: The interface board and the 320x256 InGaAs array for the characterization system. Left: the AFM image of the QDs used in QDIPs. Right: the average charge inside the QDs at different temperature and voltages.
The WIRCam project initiated the optical/infrared (OIR) instrumentation development in ASIAA
An Artist's Conception of Interacting Galaxies
Interacting Galaxies
A niobium SIS mixer developed in ASIAA to operate at 850 GHz. The establishment of the SIS fabrication facility in ASIAA is one of the most important milestones in the SMA project. Not only does it securely supply key components in the SMA, it also leads to new technology development into new area of instrumentation, such as far-infrared detectors and SQUID. This is a collaborative effort between ASIAA and the Material Science Center in National Tsing Hua University, Taiwan. Internationally, we also collaborate with experts from the Purple Mountain Observatory in China, the National Astronomical Observatory of Japan, and the Smithsonian Astrophysical Observatory.
A niobium SIS mixer developed in ASIAA to operate at 850 GHz
A prototype W-band mixer developed for the AMiBA project. Left: a packaged module used in the AMiBA prototype; Right: the MMIC chip that the module contains. Working with the experts in National Taiwan University, we have been focusing on developing our capability and capacity in the research of MMIC. This is an effort to apply Taiwanese industrial niche in semiconductor foundry to the basic science research of astronomy.
A prototype W-band mixer developed for the AMiBA project
An Artist's conception of the brown dwarf ISO-Oph 102
Brown dwarf ISO-Oph 102
An Artist's conception of the brown dwarf ISO-Oph 102
Brown dwarf ISO-Oph 102
A wide low-mass binary was discovered in the Galactic plane (Phan-Bao et al, 2008, MNRAS, 383, 831). The primary is an M0 star and the secondary is an L0 dwarf, hereafter ASIAAa and ASIAAb respectively named after the Academia Sinica Institue of Astronomy and Astrophysics (ASIAA).
ASIAAa and ASIAAb
A wide low-mass binary was discovered in the Galactic plane (Phan-Bao et al, 2008, MNRAS, 383, 831). The primary is an M0 star and the secondary is an L0 dwarf, hereafter ASIAAa and ASIAAb respectively named after the Academia Sinica Institue of Astronomy and Astrophysics (ASIAA).
ASIAAa and ASIAAb
This artist's concept shows a still-forming protostar which is accreting material from a surrounding disk. Some of the material from the disk, rather than falling onto the star, is ejected outward in a bipolar jet. New measurements from the Submillimeter Array show that matter in the jet is rotating around the jet's axis in a sort of
A still-forming protostar which is accreting material from a surrounding disk