(Sub)mm-wave galactic astronomy in Chile:
an historical perspective
Leonardo Bronfman
Astronomy Department, Universidad de Chile

Tsukuba University
30 September 2015

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Giant Molecular Clouds and Massive Star Formation inthe Southern Milky Way© 2000, Alexander Mellingen: optical image.

Barnard’s dilemma (1900)
Holes in the heavens or obscuring matter?

Dame et al. 2001: CO(1-0) image.

Face-on sketch view of the Galaxy obtained from optical, infrared, and mm data
(Churchwell et al. 2009)

Tsukuba University
30 September 2015

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1.2m mm-wave Telescopes: Molecular Clouds in the Milky Way(P. Thaddeus, Columbia University) Twin telescopes built at Columbia University (1976-1982)
 Southern Mini to Cerro Tololo, Chile (1982)
 Northern Mini to CFA (1986)
 Resolution = 8.3 ´ @ 115 GHz

Tsukuba University
30 September 2015

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Atacama: The driest desert in the world

Mars Rover Test

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Astronomical Observatories in northern Chile; 1980

1971 Las Campanas (CARSO))

1969 La Silla (ESO)

1966 Cerro Tololo (CTIO-NOAO)

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Early radio astronomy in Chile : Maipú Observatory (1959-2000)
43-46 MHz; 528 dipoles in 10.000 m2; first in Latin America(J. May, Universidad de Chile)

Tsukuba University
30 September 2015

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First complete CO survey of the Galaxy

Tsukuba University
30 September 2015

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The Norma G331.5 molecular complex
Among the most massive in the Galaxy (1985)

Page 9INDIVIDUAL CLOUD ANALYSIS:THE CO EMISSION IS DOMINATED BY GMCs WHICH TRACE THE SPIRAL ARMS
MSc. P. García et al. 2013: new 4th quadrant analysis

Page 10IRAS
BLUE = 12 um
GREEN = 60 um
RED= 100 um

FAR INFRARED (FIR) CONTINUUM EMISSION MAP OF THE MILKY WAY; DUST IS HEATED BY YOUNGMASSIVE STARS (30 K); MOLECULAR GAS IS ASSOCIATED WITH THE DUSTMOLECULAR LINE EMISSION CAN BE OBSERVED TOWARD BRIGHTEST FIR POINT-SOURCES TODETERMINE THE DISTANCES TO THE EMBEDDED MASSIVE STARS; 1 ARCMIN RESOLUTION NEEDEDPage 11SEST (Swedish ESO Sub‐millimeter Telescope); La Silla Observatory, 1988
15m diameter antenna; 100 – 345 GHz frequency range; Res. = 50” @ 100 GHz

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BLUE: CO(1-0)
RED: CS(2-1): 1200 UC H II REGIONS FROM IRAS PSC OBSERVED WITH SEST AND ONSALA 20M
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MASSIVE STARS FORM IN THE DENSE
CORES OF GIANT MOLECULAR CLOUDSCOLOR: CO(1-0) INTEGRATED IN
VELOCITY, WITHIN RANGES OFPROPOSED SPIRAL ARMS
CROSSES: MASSIVE STAR FORMINGREGIONS DETECTED IN CS(2-1) WITH
SEST.

G331.5
21NORMA G331.5: D = 7.4 KPC IN TANGENTOF NORMA SPIRAL ARM.

Page19Tokyo-Onsala-ESO-Calán
The G331.5-0.1
Galactic CO survey
GMC/MSFR
in a
T. Hasegawa, 1995
CO J=2-1 line @ 1.3 mm (230GHz) 60 cm survey telescope,Resolution = 9´= wavelength/diameter•Distance: 7.
•FM⊙ATLASGALC18O contours by 10% of
peak emission (NANTEN)
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The G331.5-0.1 GMC/MSFR in Norma•Distance: 7.
•FM⊙Nagoya University NANTEN Telescope (Y. Fukui, 1995)
86 – 115 GHz coverage, 4m antenna, Las Campanas ObservatoryPage 16

NANTEN MAP OF NORMA G331.5; RESOLUTION 2.5 arcmin
3.5 MILLION SOLAR MASSES G331.5-0.1 GMC/MSFR inNorma•Distance: 7.
•FM⊙

ATLASGAL
C18O contours by 10% of
peak emission (NANTEN)
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ZOOMING IN WITHSEST 15 m TELESCOPE
RES. = 22 arcsec .
SIMBA BOLOMETER(2001)
G331.5 MOLECULAR
CLOUD CORE:
CONTINUUM EMISSION
FROM COLD DUSTHEATED BY PROTO ANDFORMING STARS

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CCATCONCEPTIN THE MEANTIME: THE ALMA SITE AT 5000 m, ATACAMA, CHILE

GENERAL VIEW OF PAMPA CHAJNANTOR, 1995

70 km from San Pedro town; 170 km from Calama, major mining city
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Site survey expedition for NAOJ LMSA (proto ALMA); 1994

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ALMA Site in Chile
NAOJ Test Interferometer (1996)

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Atacama Submillimeter Telescope Experiment(Japan ASTE 10 m Telescope, NAOJ , 2004)
Frequency range up to 800 GHz

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TRANSPORT OF ASTE
TO PAMPA LA BOLA AT
4850 M , CHILE , ALMA
SITE, MARCH 2002
(S. SAKAMOTO)

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NANTEN II Telescope moved from Las Campanas to ALMA Site in 2005.
(Up to 810 GHz)

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Atacama Pathfinder
Experiment (APEX
12 m Telescope)
Chajnantor (ALMA
site, Chile, 5.050 m)
MPIfR, ESO, Onsala(2005)
230 Ghz to 1 THz

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Page 26

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Back to science: The G331.5 GMC/Massive Star Forming Region
observed with APEX LABOCA camera at 0.87 mm
G331.5 GMC•Distance: 7.5 kpc•FIR luminosity:
3.6 × 106 L⊙• Contours: NANTEN
C18O GMC mass: 3.5 ×106 M⊙• Color: APEX/LABOCA
0.87 mm dust continuumemission
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CS(7-6) OBSERVED WITH ASTE AT 343 GHz (22” res)
DISCOVERY OF A MASSIVE MOLECULAR OUTFLOW
AT G331.5 GMC CORE IN NORMA SPIRAL ARM

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VERY MASSIVE AND LUMINOUS HIGH VELOCITY MOLECULAR OUTFLOW;INFANCY OF A HIGH MASS STAR

Beuther et al.2002b

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A massive molecular outflow in G331.5‐0.1:
Unresolved with available single dish telescopes•APEX CO (7-6): Res 7.7”
@ 800 GHz•Velocity width (ZP)160 km/s
•Dynamic timescale: lessthan 3×103 yrs.
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Contours: APEX-LABOCA 0.87 mm continuum
Colors: SPITZER-IRAC mid infrared

APEX spectra of shocked gas inclump MM3; High velocity
molecular outflow G331.512-0.103

MM4G331.5414-00.0675+B
MM2
G331.5582-00.1206
MM6MM5+DMM3+CMM1

G331.4904-00.1173+APage 31

The Atacama Large (sub)Mm Array
Largest radio telescope in the world.
66 antennas: 54x12m + 12x7m, 35 to 950 GHz.
North America, Europe, East Asia collaboration in ChilePage 32

G331.5 ALMA Observations (2012)

1 CH3OCH3 8(4,5)-7(3.4)
2 HCO+ v=0 4-3
3 34SO2 v=0 20(0,20)-19(1,19)
4 SO2 v=0 13(4,10)-13(3,11)
5 SO2 v=0 15(4,12)-15(3,13)
6 SO2 v=0 11(4,8)-11(3,9)
7 CH3OCH3 18(2,17)-17(1,16)

8 SO2 V=0 8(4,4)-8(3,5)
9 SO2 v=0 9(4,6)-9(3,7)
10 Unidentified
11 SO2 v=0 7(4,4)-7(3,5)
12 SO2 v=0 6(4,2)-6(3,3)
13 SO2 v=0 17(4,14)-17(3,15)
14 SO2 v=0 5(4,2)-5(3,3)

15 SO2 v=0 4(4,0)-4(3,1)
16 SO2 v=0 20(0,20)-19(1,19)
17 34SO2 v=0 23(4,20)-23(3,21)
18 Unidentified
19 CH3OCHO v=0 29(12,18)-28(12,17)A
20 CH3OHv t=0 4(1,3)-3(0,3)
21 S18O 9(9)-8(8)1 34SO2 v=0 15(4,12)-15(3,13)
2 34SO2 v=0 11(4,8)-11(3,9)
3 CH3OCH3 35(2,33)-35(1,34)
4 Possible SO2 v=0 5(5,1)-6(4,2)
5 34SO2 v=0 8(4,4)-8(3,5)
6 NH2CHO 17(0,17)-16(0,16)

7 Unidentified (possible
34SO2 v=0 9(4,6)-9(3,7) )8 H13CN v=0 J=4-3
9 SO2 v=0 26(9,17)-27(8,20)
10 34SO2 v=0 7(4,4)-7(3,5)
11 34SO2 v=0 6(4,2)-6(3,3)

12 HC3N v=0 J=38-37
13 34SO2 v=0 6(4,2)-6(3,3)
14 CO v=0 3-2
15 CH3OHv t=0 5(4,2)-6(3,3)-- /CH3OHv t=0 5(4,1)-6(3,4)++
16 NS J=15/2-13/2,Omega=1/2,F=17/2-15/2,I=f

22 Unidentified
23 CH3CCH v=0 21(3)-20(3)24 CH3CCH v=0 21(2)-20(2)25 CH3CCH v=0 21(1)-20(1) / CH3CCH v=0 21(0)-20(0)26 Unidentified (possible 34SO2 v=0 15(2,14)-14(1,13))
27 SO2 v=0 25(3,23)-25(2,24)
28 CH3OCH3 12(3,10)-11(2,9)

17 SO2v2=1 19(1,19)-18(0,18)
18 SO2 v=0 16(4,12)-16(3,13)
19 SO2 v=0 19(1,19)-18(0,18)
20 H13CO+ 4-3
21 SiO v=0 8-7
22 SO+ J=15/2-13/2,Omega=1/2,I=ePage 33

*Channel maps of SiO line
obtained with ALMA.
Cental map: projected shellstructure
Crosses: high velocity
molecular outflow lobes.
•Outflow inclination = 10oPage 34

1985
MINI:
Resolution
8.3` (500¨)

Model of G331.5
Molecular Outflow
ALMA Resolution: 1”(2012)
Timescale less than
1000 years(Total life 1 MY)
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 In the meantime: relocation of the Southern MINI to Cerro
Calán, (OAN Universidad de Chile, 2009)

L. Bronfman
University of Chile

Page 36 The 1.2 m telescope at U. Chile OAN, Cerro Calán Hands-on training for Astronomy students
 Engineering graduate and undergraduate theses.
 Receiver upgraded using state-of-the-art digital technology

Digital sideband separating mixer using FPGA
digital technology (ROACH).
Southern Mini at Cerro Calán, July 2013
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ALMA Band 1 prototype receiverDesigned and built at U. Chile(NAOJ Cryogenics, Y. Sekimoto)Page 38

U. Chile Lab. Support for Tsukuba University Project

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Thanks

2009 Setember

In memory of Prof. Jorge May (1936-2011)

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