Korea-ALMA Report

Aran-Lyo
Jongsoo Kim andMembers of ALMA group in KASIPeople in EA ARC Korean Node(http://alma.kasi.re.kr)

ARC Korean Node
• QA2 (qualification assurance phase 2)
Oh- A-Ran Lyo, Woojin Kwon, Kijeong Yim, Se-Heon• P2G (phase 2 generation)- Jihyun Kang, Se-Heon Oh• AoD (Astronomer on Duty)- A-Ran Lyo (2 shifts, July-August)- Sujin Kim (Solar observation, December)Town Hall Meeting 2016

SNU : 21 March

KIAS: 18 MarchKASI: 28 MarchStatistics for ALMA KoreanProposals
Cycle

deadlines

submitted

ProvedC2

5 Dec 2013

184C323 Apr 2015

256C421 Apr 2016

358

G19.61+0.23(Cho et al. 2016, ApJ, 826, 157)

3.5mm continuum (color) + SiO maser (contour)

A case study of extraplanar molecular gas
in a Virgo spiral using the ALMA&

NGC 4522 (a Virgo spiral) provides an opportunity tostudy the impact of ICM pressure on the dense/star
forming gas and its fate in the extraplanar space
after stripping.

,The ALMA CO data

The ALMA observations (cycle 3)
12m arrayIn band 3,12CO (1-0); 115.271 GHz
13CO (1-0); 110.201 GHz
In two regions,Hα (black contours)
12CO (2-1) (blue contours;
single dish, Vollmer et al. 2008)

the center of the galaxy
the peak of extraplanar COJanuary 12 (12CO, 46 antennas), January 19 (13CO, 43 antennas), 2016
On-source time: ~51 min (12CO) and ~276 min (13CO)
Shortest baseline: 15m, Longest baseline: 331m
RMS (~6 arcsec using ‘taper’ and 5 km/s) noise:~2.1 mJy/beam (12CO)~0.7 mJy/beam (13CO)

The first case where 13CO gas has been detected
outside the stellar disk in a galaxy undergoing ram
pressure stripping.

The Molecular Gas Properties of HI Monsters ALMA science case (Cycle 3)
Aeree Chung (Yonsei), Daisuke Iono (NAOJ), Min S. Yun (Umass)
HI Monsters: Galaxies with extremely high HI-to-stellar mass ratio at 0.04
< z < 0.08 identified in ALFALFA survey (z limited by the depth of theALFALFA catalog in 2008 and the CO coverage of the upper most band of
the redshift search receiver built for the Large Millimeter Telescope): Figure– M(HI) vs. M(star) of COLDGASS sample in blue with upper limits in green for nondetections (Saintonge 2011, MNRAS, 415, 32). HI Monster sample in red.

Also large molecular gas mass of the HI monster sample as inferred fromsingle-dish CO observations, yet star forming is not active for such highcool/cold gas mass ! What are they in the context of galaxy evolution?

Lee, Chung, et al. 2014

Questions for the ALMA: How gas and star formation areregulated in these galaxies with a large gas reservoir?

Overall, regularly rotating molecular gas disk, yet various
peculiarities in kinematics! in the process of accretionor structural formation?

15”

No other telescope can image the moleculargas of these systems with this resolution (>10elements across the disk) in reasonable
integration hours (~ a few hrs in this case)ASTE/ALMA multibeam receiver system
1) Wide band (ALMA B7+B8) feed horn

단위: mm

S11: reflection

92) GPU Spectrometer
KFFTSpec: data flow and functions inside GPU serverInternal synthetic
signal generator

Monitoring &Control Interface*

Time division
into Tint –length
slices of dataSettings &schedule queue*
Command lineinterface* Required for ALMA/ASTE spectrometer, not present in KFFTSpec of 03/2016

GPU #1
Stream 1

GPU #1
Stream 2

DMADMA

Unpack

UnpackPost-proc

Post-proc…

GPU #NStr. M-1

GPU #N
Stream M

DMA

DMA

Spectralprocessing

Ring Buffer
containing >1 GByte oftime-stamped data frames

continuous dispatching to next idle GPU(s)Spectralprocessing

DRXP*
DTS receiver

read

Spectralprocessing

Baseband filewrite

Spectralprocessing

10G/40G Net

De-framing

Alternate sources
for baseband data…

Unpack

Unpack…

Post-proc

Post-proc

Assembly of final auto/cross-power spectra and statisticsLocal or remote storage

Spectral power (uncalibrated)

H2O and SiO maser lines
Orion KL H2O
2016 March 15
22 GHz Yonsei

Velocity (km/s)

512 MHz bandwidth
32k channels
3.75 seconds avg.

Spectral Channel (N)Orion KL SiO
2016 March 15
43 GHz Yonsei

Velocity (km/s)

Spectral Channel (N)