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Variability Of Methanol And OH Masers Associated With
The Star-Forming Region G339.62-0.12
S t u d e n t : M a v i s S e i d u S u p e r v i s o r s : P r o f . D J v a n d e r Wa l t
D r S h a r m i l a G o e d h a r t
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• Introduction
• Observational Methods
1. Single dish
2. Inteferometer
• Results and Discussions
• Summary
• Recommendations
• References
L AY O U T
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• Star formation
A. The earliest stages of a star’s life is an intriguing mystery
• Massive star formation contribute greatly to the evolution of most galaxies
1. produce ultraviolet radiation
2. enrich the ISM through their supernova actions
• Formed in dynamic regions such as giant molecular clouds (site for star birth)
I N T R O D U C T I O N
image credit: Shubham Singh (Prince)
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• Masers are found to be associated with the early stages of massive stars
deBuizer (2000), Foster and Caswell(1989)
• Masers are known to form in
1.stellar regions; mostly in high-mass star forming regions (Caswell,1998)
• They are used to probe through obscured regions
• The maser spot distribution suggests the structure and conditions of the regions where they are formed.
I N T R O D U C T I O N
Figure 1. Interstellar cloud
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• Examples of masers: Methanol and OH masers
• The methanol and OH masers are known to be located in either
1. in the disk
2. or outside the HII region
I N T R O D U C T I O N
Outflows
Disk
Masers
Masers
Figure 2. Proposed location of some masers in star forming regions
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I N T R O D U C T I O N• Evidence of variability in specific
star forming regions from observational results. The origin of maser variability have been
• The underlying mechanism of the variability was unclear
• Proposed investigation of variability of OH masers
Figure 3. Variability of the 6.7 GHz methanol masers over 10 years monitoring
Goedhart et al., (2014)
Goedhart et al., (2014)
Goedhart et al., (2014), Maswanganye et al., (2015), Szymczak et al., Araya et al.,
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O B S E R VAT I O N A L M E T H O D S
Feeds
Primary reflector
Sub-reflector
Propagation of radio waves from source
Radio source
Declination axis
Euatorial mount
Focus Polarization
• Pointing correction using drift-scan observations
• Virgo A
−40 −30
0
2
4
TA(K
)
North
−40 −30V lsr (km/s)
0
2
4
East
−40 −30
0
2
4
6
8Centre
−40 −30
0
2
4West
−40 −30
0
2
4
South
Pointing observations for 2013d170
1 . S I N G L E D I S H O B S E R VAT I O N
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2 . I N T E R F E R O M E T R I C M E T H O D U S I N G K AT- 7
O B S E R VAT I O N A L M E T H O D S
• Maser imaging
• Flux calibration
• Bandpass and gain calibration
• Image model
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16 : 39 : 0042 : 0045 : 0048 : 0051 : 00RA (J2000)
30 : 00
−46 : 00 : 00
30 : 00
−45 : 00 : 00
−44 : 30 : 00
Dec
(J2000)
G339.62-0.12
G338.681-00.084
G338.88-00.08
G339.88-1.259
G340.054.0244
G339.925+0.557
G339.282+00.13
0.5
1.0
1.5
2.02.53.0
Fluxdensity(Jy/beam)
R E S U LT S A N D D I S C U S S I O N S
• Other maser fields were found closer to the G339.62-0.12 region
Figure 4. Continuum image of the star-forming region
16:45:5516:4616:46:0516:46:1016:46:1516:46:2016:46:2516:46:3016:46:3546:40 16:45:50 16:45:45 16:45:40 16:45:35 16:45:30 16:45:25 16:45:20
-45:37
-45:36
-45:38
-45:39
-45:40
-45:41
RGB img~1
1’ 14.59’ x 6.377’
N
EPowered by Aladin
denseCoredenseCore
Powered by Aladin
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Figure 5. OH maser sources in the field of view
R E S U LT S A N D D I S C U S S I O N S1667 MHz 1665 MHz
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R E S U LT S A N D D I S C U S S I O N S
• Each maser spectrum is unique
• Spectra spread over few km/s range (~10 km/s max)
Figure 6. Spectra of the G339.62-0.12 maser sources
0
20
40
60
80
100
120
6.7 GHz methanol
J
I
H
G
F
E
D
CB
A
Upper envelope
Lower envelope
Averaged spectra
0
10
20
30
40
50
60
70
Fluxdensity
(Jy)
1665 MHz OHE
DC
B
A
−40 −38 −36 −34 −32 −30 −28Vlsr (km s−1)
0
5
10
15
A
B
C
1667 MHz OH
• Investigating Variability
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T I M E S E R I E S
Figure 7. Time series plots of G339.62-0.12 at the 6.7 GHz maser transition
10
20
-37.27 km s−1
10
20-36.96 km s−1
15
30-36.21 km s−1
25
50
Fluxdensity
(Jy)
-36.04 km s−1
50
75-35.64 km s−1
56400 56600 56800 57000 57200 57400
MJD
0
15-33.71 km s−1
20
40
-33.53 km s−1
20
40-33.49 km s−1
25
50
-33.36 km s−1
60
90
Fluxdensity
(Jy)
-32.96 km s−1
20
40-32.04 km s−1
56400 56600 56800 57000 57200 57400
MJD
15
30-30.5 km s−1
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3.0
4.5-36.92 km s−1
9
12
-36.51 km s−1
12
16
Fluxdensity
(Jy)
-36.44 km s−1
4.5
6.0
7.5
-36.24 km s−1
56400 56600 56800 57000 57200
MJD(days)
0.8
1.6 -30.96 km s−1
Figure 8. OH maser time series for peak velocity channels in G339.62-0.12
40
50-37.49 km s−1
12
16 -37.01 km s−1
10
15
Fluxdensity
(Jy)
-36.67 km s−1
10.5
12.0-33.51 km s−1
56400 56600 56800 57000 57200
MJD
4
6 -31.79 km s−1
1667 MHz OH1665 MHz OH
T I M E S E R I E S• Different light curves for the OH maser at 1665 and 1667 MHz transitions
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• Time series for each maser, their periodogram and periodicity
−1 0 1 2Phase(rad)
0
20
FluxDensity
(Jy) Period = 206 ± 2 days
6.7 GHz CH3OH
-36.08 km s−1
−1 0 1 2Phase(rad)
−5.0
−2.5
0.0
2.5
5.0 Period = 209 ± 2 days
1665 MHz OH-37.01 km s−1
−1 0 1 2Phase(rad)
−4
−2
0
2
4Period = 214 ± 2 days
1667 MHz OH-36.44 km s−1
20
40
606.7 GHz CH3OH -36.08 km s−1
10
15
20
FluxDensity
(Jy) 1665 MHz OH
-37.01 km s−1
56400 56600 56800 57000 57200MJD
10
151667 MHz OH
-36.44 km s−1
0.0
0.2
0.4
0.6
6.7 CH3OH Period = 206 ± 2 days-36.08 km s−1
fit
0.0
0.2
0.4
Pow
er 1665 MHz OH Period = 209 ± 2 day
-37.01 km s−1
0.005 0.010 0.015 0.020 0.025 0.030 0.035 0.040Frequency (day−1)
0.00
0.25
0.50 1667 MHz OH Period = 214 ± 2 days-36.44 km s−1
P E R I O D I C I T Y
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40
60
80
6.7 GHz CH3OH-35.73 km s−1
7.5
10.0
12.5
FluxDensity
(Jy)
1665 MHz OH
-36.53 km s−1
56400 56600 56800 57000 57200MJD
5
6
7
1667 MHz OH
-36.24 km s−1
−1 0 1 2Phase(rad)
−20
0
20
Magnitude
Period = 208 ± 2 days
6.7 GHz CH3OH-35.73 km s−1
−1 0 1 2Phase(rad)
−2
0
2Period = 210 ± 1 day
1665 MHz OH-36.53 km s−1
−1 0 1 2Phase
−1
0
1
Magnitude
Period = 214.96 days
-36.24 km s−1
−1 0 1 2−5
0
5
10
P E R I O D I C I T Y
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I N V E S T I G AT I N G P E R I O D I C I T Y
Parfenov & Sobolev (2014) Sing and Deshpande (2012) van Der Walt et al., (2016)
Observer’s position
1.9 AU
Gap RegionDisk
Disk
Disk
Disk
Secondary
Primary
Trailing "shock"
θ
−1 0 1 2Phase(rad)
0
20
FluxDensity
(Jy) Period = 206 ± 2 days
6.7 GHz CH3OH
-36.08 km s−1
• Simple geometric model by Parfenov & Sobolev to investigate the maser periodicity
• The similarity is quite striking
−1 0 1 2Phase(rad)
−4
−2
0
2
4Period = 214 ± 2 days
1667 MHz OH-36.44 km s−1
0.00.51.01.52.02.53.03.54.04.5
0 50 100 150 200
Flu
x
Time (days)
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• All the investigated masers are highly variable
• Associated with some sort of periodicity (~ 205 to 215 ± 2 days)
• G339.62-0.12 star forming region is complex
1. The cause of the variability and periodicity is still being investigated
S U M M A RY
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• High sensitive maser observations in G339.62-0.12 are needed
1. OH maser spot map
R E C O M M E N D AT I O N S
denseCoreOH/IRDkNeb
339.625339.64583339.66667339.6875339.70833339.72917339.75
-00.16667
-00.1
-00.08333
339.60417 339.58333 339.5625 339.54167
-00.11667
-00.13333
-00.15
SPITZER MIPS1
1’ 13.85’ x 6.151’
N
EPowered by Aladin
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A C K N O W L E D G E M E N T
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R E F E R E N C E S1. Caswell, J. L., 1998, Positions of hydroxyl masers at 1665
and 1667 MHz, MNRAS, 297, 215-235(1998)
2. Forster, J. R., and Caswell, J. L., 1989, A&A, 213, 339-350(1989)
3. Goedhart, S., Maswanganye, J. P., Gaylard, M. J., van der Walt, D. J., 2014, Periodicity in Class II methanol masers in high-mass star-forming regions, MNRAS 437,1808–1820(2014).
4. Parfenov, S.Y., Sobolev, A.M., 2014, MNRAS, 444,620(2014)
5. van der Walt, D.J., Maswanganye, J. P., Etoka, S., Goedhart, S., van der Heever, S.P., 2016,Periodic Methanol masers in G9.62+0.20E, A&A (2016)
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