Research Gallery

Some galaxies host so-called starburst phenomena, characterized by the intensive formation of stars. The ALCHEMI team has conducted a wide-frequency spectral scan in the starburst galaxy NGC 253 using the (...more)

We present ALMA observations of dense gas tracers HCN (1−0) and HCO+ (1-0) for three green valley galaxies and two galaxies on the star-forming main sequence, all with comparable molecular (...more)

Protoplanetary disks, that are rotating disks of gas and dust surrounding young stars, become the birthplace of planets. However, details of the formation process of these disks remain unclear. In (...more)

In the early phase of star formation, protostellar disks are formed to grow the central protostars into stars. The disks will later evolve into protoplanerary disks to form planets like (...more)

Multiple systems are common outcome in the star-forming regions. However, the formation process of multiple system remains unclear due to the complex dynamic. To address this, we analyze the ALMA (...more)

Star formation quenching refers to the process by which galaxies cease forming stars, transitioning from actively star-forming to passive states. Many mechanisms have been proposed to explain star formation quenching. (...more)

The molecular phase of the interstellar medium (ISM) hosts star formation. Measuring its properties, e.g. density and kinematics, is key to understanding star formation and ISM properties. The low-J CO (...more)

Left panel: The 12CO (J = 2–1) molecular line emission at 2.3 km s−1 with respect to the systemic velocity of the monopolar outflow associated with the protostellar system HH (...more)

left: 850 μm continuum emission of the northern part of OMC-3 region including G208-N2 observed with the JCMT SCUBA-2 (Yi et al. 2018) in contours overlaid on the Hershel PACS (...more)

With the ALMA large program eDisk, we identified hot dust disks around a number of protostars. One of such objects, R Cr A IRS 7B-a, exhibits a peak brightness temperature (...more)

Internal photos of the Laser Synthesizer instrument. Left - top view of optical components including FBG assembly that houses optical filters, couplers and switch; Amonics erbium doped fiber amplifier along (...more)

Internal photos of LORTM instrument. Left - top view of optical components including Sumitomo Mach Zehnder modulators (x2), Centellax RF power amplifiers (x2), Amonics erbium doped fiber amplifier, fiber Bragg (...more)

Left panels: The distributions of molecular gas for three MaNGA-selected green valley galaxies (from top to bottom: Galaxy 1, Galaxy 2, and Galaxy 3) based on ALMA CO observations. Middle (...more)

Improvement in resolution and sensitivity from SMA subcompact (left, resolution of 2”) to SMA extended (middle, resolution of 0.7”) to ALMA (resolution of 0.26”) towards the high-mass star-forming cores W51 (...more)

We have realized the epitaxial growth of ultrathin δ-NbN films on 3C-SiC/HRSi substrates. Even with a thickness of 1.3 nm (~3 unit-cells), the δ-NbN film shows a superconducting transition above (...more)

ALMA image of the dust ring (red) and gaseous spirals (blue) of the circumstellar disk AB Aurigae. (...more)

High-resolution Band 7 continuum negative image of SDP.81. This is the highest-resolution submillimeter observation of a strong lensing galaxy to date. (...more)

Figure 1: ALMA composite image of HH 212, showing a pseudo-disk (green) and a Keplerian disk (bright green) in dust continuum, and a bipolar jet in HCO+ gas (red). (Lee (...more)

NA 12m Vertex prototype antenna at the JVLA site in Socorro, New Mexico. (...more)

Delegation from Taiwan during the ALMA inauguration in March 2013 at the OSF in Chile. (...more)

the procured NA 12m Vertex prototype antenna at the JVLA site in Socorro, New Mexico. (...more)

the latest tuCASA-ASIAA imaging workshop held at National Normal University ShiDa (...more)

the ALMA alternative laser synthesizer (...more)

Nutating subreflector in the laboratory at ASIAA. (...more)

EA-FEIC staff members celebrating the delivery of the very last front-end for Europe in 2012. (...more)

EA FEIC team delivering the first front end to Chile in 2008. (...more)

One of the front ends during testing and integration at the EA FEIC in Taichung, Taiwan. Pictured is the tilt table holding the cryogenic dewar (in blue) in which the (...more)

After its month-long journey from Taiwan, the first of the two Front-End Service Vehicles is being tested at the ALMA Operations Support Facility in Chile. In this photo, the FESV (...more)

Circumstellar disk and ambient gas surrounding the protostar, L1489 IRS (white cross), from an ALMA cycle-0 observation with an integration time of 74 minutes at a resolution of 1" (blue (...more)

An aerial view of the technical building at the AOS at 5000m (...more)

To the right are the three antenna assembly sites belonging to the Japanese, North American and European partners; in the upper middle section is the operations building, and in the (...more)

ALMA antennas on the Chajnantor plateau in Chile. (Picture Credit: C. Padilla, ALMA, ESO/NAOJ/NRAO) (...more)

Installation of the first ALMA nutator in Chile. January 2013 (...more)

EA-FEIC staff members celebrating the delivery of the last receiver front-end system for our ALMA-Japan partner (blue cylinder-shaped object in the middle of the photo). (...more)

First ALMA nutator on a N.A. antenna, january 2013 (...more)

Blue shifted disk wind from HD 163296. The grey-scale shows the CO J=2-1 integrated intensity of the blue shifted wind from HD 163296. The 4σ level is indicated by the (...more)

The CO J=3-2 channel map unveils for the first time at sub-millimeter frequencies the vertical structure details of a protoplanetary disks, showing the back and front side of the flared (...more)

Integrated emission map of H13CO+ (4-3) with contours showing 3, 5 and 7 sigma (left), and DCO+ (5-4) with contours showing 3 and 5 sigma. The H13CO+ is centrally peaked (...more)

CO(2-1) integrated intensity map of the newly discovered molecular arm close to NGC4039 (Espada et al. 2012 ApJ, 760L, 25E). The plus signs indicate the clumps. (...more)

Cryogenic IF Low Noise Amplifier (LNA) for ALMA for 4-12 GHz using 0.15 mHEMT (...more)

Voltage-Controlled Oscillator MMIC for ALMA Band-1 using 2um GaAs HBT (...more)

Conceptual image of ALMA, which is currently under construction. ALMA will consist of the“12m Array” of up to sixty-four 12 m telescopes, and “Atacama Compact Array (ACA)”of four 12m and (...more)

Left: To install receiver cartridges into a dewar, the dewar is mounted on a “tilt table” to give sufficient space for the installation of the cartridge. In the picture, the (...more)

In September 2005, Academia Sinica (AS) signed an agreement with National Institutes of Natural Sciences of Japan (NINS) to join the ALMA-Japan project. AS President Yuan T. Lee shakes hands (...more)