Science with ALMA Archive Masa Hayashi (NAOJ) East Asia ALMA Science Workshop, Korea (July 14, 2014)
Dec 18, 2015
Science with ALMA Archive
Masa Hayashi (NAOJ)
East Asia ALMA Science Workshop, Korea (July 14, 2014)
2
Archive Science
• Masa Hayashi (NAOJ): Science with ALMA Archive
• Aya Higuchi (Ibaraki): Science case with ALMA archive
• Tohru Nagao (Ehime): Extragalactic Studies with ALMA Archival Data
• Erik Muller (NAOJ): Using ALMA Archive; ALMA Science Archive substructure and operation
3
ALMA Status
ALMA (ESO/NAOJ/NRAO), S. Komugi (NAOJ/ALMA)
45 Antennas band4 band10band8
ALMA: a giant array of 66 antennasincl. ACA (Morita array) with four 12-m total power antennas
4Science
CapabilitiesCycle 0 (2011-2013)
>16 x 12m antennas Bands 3 (3.1mm), 6 (1.3mm), 7 (0.87mm), 9 (0.44mm) Max 400 m baseline (~0.3″ resolution)
Cycle 1 (2013-2014) 32 x 12m antennas ACA (9 x 7m, 2 x 12m TP antennas) Bands 3 (3.1mm), 6 (1.3mm), 7 (0.87mm), & 9 (0.44mm) Max 1 km baseline (~0.1″ resolution)
Cycle 2 (2014-2015) 34 x 12m antennas ACA (9 x 7m, 2 x 12m TP antennas) Bands 3, 4 (2.1mm), 6, 7, 8 (0.74mm), & 9 Max 1-1.5 km baseline (~0.1″ resolution) Polarization (Band 3, 6, & 7, no ACA)
7Publication with ALMA
Archive
As of 2014-07-09(ALMA publication statistics)
1/3 of ALMA publicationsare based on archival data.
There are only a few papers based on Cycle0 archival data.
PI Cycle0/1 (83)65%
Archive SV (37)32%
Archive Cycle0 (4)3%
Refereed ALMA publications (total: 124)
8
Jørgensen et al. 2012, ApJL
Discovery of the simplest sugar, Glycolaldehyde (HCOCH2OH) from the young “solar-mass” protostellar binary, IRAS 16293-2422
ALMA Archival Papers
ALMA SV Band 6 Data 16 antennas, 5.4 hours, 2
pointings
Pineda et al. 2012, A&AL
Mass ~ 3 M⊙
Source B (inflow - inverse P-Cygni profile)
Sources A (rotation)
9
Hirota et al. 2012, ApJL
ALMA Archival Papers
ALMA SV band 6 Data16 antennas, 20 minutes
Receding gas
Approaching gas
The first detection of vibrationally-excited water vapor emission in star forming regions
Revealing the disk and its kinematics around Orion KL Source I: A new tool to explore the vicinity of forming stars
10
Probing detailed physical and chemical conditions of protoplanetary disks
CO(3-2) Bergin et al. 2013, Nature
Tgas = 30 KMgas> 3.9 × 10−3 M⊙
ALMA Archival Papers
ALMA SV band 7 Data, 9 antennas, 2.4 hours(x10 more sensitive than the previous SMA observations) Spectrum of the central
region
HST image (1.7-2.2um)Debes et al. 2013, ApJ
SMA 2 nights =>
Hughes et al. 2011
CO(3-2)
160AU / 3” 100AU
NASA, ESA, Z. Levay (STScI/AURA)
TW Hydrae
11ALMA Archival
Papers
Iono et al. 2006
ALMA SV Band 7 Data17 antennas, 30 minutes
Clear [CII] 158μm line detection from the distant galaxy BR1202-0725 (z=4.7)
Wagg et al. 2012, ApJL
SMA 20 hours
12
Discovery of a clumpy molecular gas arm in merging galaxies
Stars will born in the clumps in the tidal molecular arms as predicted by numerical simulations
Espada et al. 2012, ApJL
ALMA Archival Papers
CO(2-1)
The Antennae
ALMA SV Band 6 Data14 antennas, 17
pointings
ALMA (ESO/NAOJ/NRAO)HST (NASA/ESA)
Numerical SimulationTeyssier et al. 2010, A&AL
Numerical SimulationMatsui et al. 2012,ApJ
Old Stars
Gas
Young Stars
The star formation efficiency in the tidal arm (~6 Gyr-1) is a factor of x10 higher than those in normal disk galaxies.
15
CO(3-2)
Quick Look with JVO
CO(3-2) emission from the AGB star R Sculptoris(Maercker et al. 2012, Nature)