Masers and Star Formation in Perseus Spiral Arm

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Masers and Star Formation in Perseus Spiral Arm
N.Novgorod, 2007

• Sobolev A. M.
• Ural State University, Ekaterinburg, Russia

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Perseus Spiral Arm in l-Vlsr diagram
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Class II masers in G34.20.1

• Ultracompact HII region

ATCA (Ellingsen Sobolev priv. comm.)
protostar

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Hunter etal. (2006)grey scale 1.3 mm cont.
SMA red contours 3.6 cm cont. VLA blue
symbols water maserssquares methanol masers
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S 233 IR
Porras, Cruz-Gonzalez, Salas (2000)
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Hachisuka etal. (2006)grey scale 220 GHz
continuum cones show velocities of water masers
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class I masers at 25 GHz in ???-1(Johnston
etal. 1995)
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class I masers at 25 GHz in ???-1(model by
Sobolev, Wallin Watson 1998)
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12 GHz methanol masers at W3(OH)
observations
hint of the turbulent model
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So, masers tell us about

• kinematics and fundamental characteristics of
  turbulence
• in the regions of star formation

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Voronkov, Brooks, Sobolev etal. (2006)
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Models of class I maser pumping

• (Sobolev, Ostrovskii etal., 2005)

• 4 regimes distinguished by
• the set of transitions displaying
• the highest brightness temperature
• J-1-(J-1)0E series 4-1-30E at 36.1, 5-1-40E at
  84.5 GHz , etc.
• represented by SgrB2,
  G1.6-0.025
• J0-(J-1)1A series 70-61A at 44.1, 80-71A at
  95.2 GHz, etc.
• represented by DR21W, NGC2264
  and OMC-2
• J2-J1E series at about 25 GHz OMC-1
• J-2-(J-1)-1E series 9-2-8-1E at 9.9 11-2-10-1E
  line at 104.3 GHz
• represented by G343.12-0.06
  and W33A

Log Tb
Log density
Beaming20, Tk 50 K, log(Nm/dV)10
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BIMA spectra of methanol maser candidatesSutton,
Sobolev, Ellingsen, Cragg et al. (2001)
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Models allow to determine physical parameters
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Class II masers in W3(OH) (Menten et al. 1991)
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Sobolev, Cragg Godfrey 1997, MNRAS
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Methanol and hydroxyl maser pumpingCragg,
Sobolev Godfrey (2002)
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At which wavelengths strong 6.7 GHz masers get
their source and sink?
source
sink
Ostrovskii Sobolev (2002)
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So, masers tell us about

• physical and chemical parameters
• in the regions of star formation

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class II maser in G9.62 shows periodic
variability
(Goedhart etal. 2004)
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Causes of variability

• Changes of the pumping conditions
• Changes of background
• Changes of geometry

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G9.620.20 interferometry variability in
different maser spots is synchronized with the
speed of light (Goedhart etal. 2004)
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model with n106 cm-3
Among physical parameters only the dust
temperature can react sufficiently fast to the
changes of the radiation from the distant object.
Models show that the changes in the dust
temperature by a few can explain G9.62020
variability
br ightness
TdustTgas
model with n105 cm-3
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So, masers

• tell us about
• variability of the stellar objects
• which is likely to reflect details of
• accretion process

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Xu, Reid, Zheng Menten (2005)
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New bright 12 GHz masers detected at HartRAO (in
cooperation with M.Gaylard, Xu Ye and M.Voronkov)
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• Masers provide possibility to
• determine accurate distances to the sources by
  absolute method
• study MSF processes on the scales from a.u. to
  10 kpc
• make search for a new types of objects, including
  protostellar
• study nature of these objects through
• - study of the source structure
• - study of kinematics
• - determination of the values of physical
  parameters in masing regions and their
  environment, including
• characteristics of turbulence
• dust properties
• study of the chemical status
• etc.

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Unified catalogues of class II methanol masers
Malyshev Sobolev (2003) contains data on 495
sources published parameters of the 6, 12 and
107 GHz lines and associated CS and SiO

• Xu etal. (2003) contains data on 482 sources
  published parameters of the 6 GHz line, distances
  and association with IRAS sources
• Pestalozzi et al. (2005) contains data on 519
  sources published parameters of the 6 GHz line
  and distance estimates

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Masers and CO in the Vlsr-l diagram
(T. M. Dame, Dap Hartmann, and P. Thaddeus, 2000)
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Perseus Spiral Arm in l-Vlsr diagram
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Resonances in Galactic Disk
Corotation radius velocity of galactic rotation
equals velocity of rotation of the spiral pattern
OCl and OB-stars
Cepheids
Corotation region lies from 8.9 to 10.8 kpc, i.e.
in Perseus Spiral Arm (e.g., Popova Loktin,
2006)
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Open stellar clusters
195 OCl with lg t lt7.8 and 192 older OCl.
Young OCl with (lg t lt7.8)
OCl with lg t gt 7.8
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Canadian Galactic Plane Survey
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Kirsanova
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Class II methanol masers sources from Perseus
Spiral Arm
G133.951.06 G136.841.14 G173.482.45
G173.592.44 G173.692.87
G183.35-0.58 G189.030.78 G196.45-1.68
G232.621.00 G269.45-1.47
G70.141.73 G78.620.98 G85.400.00
G90.901.50 G94.60-1.80 G98.021.44
G108.75-0.96 G111.24-0.76 G111.540.78
G123.06-6.31 G133.721.22
27 sources are known
???????? Malyshev Sobolev, 2003 Pestalozzi,
2005
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Radial velocities of CS(2-1) and CH3OH masers at
6.7 GHz
Spread of maser velocities
,
(
(
Maser peak position
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Positions of class II CH3OH maser sources in the
plane of the Galaxy (bottom view)
Vmas Vcs gt 0.75 km/s
Onsala sources
Vmas Vcs lt - 0.75 km/s
from the literature
Vmas Vcs lt 0.75 km/s
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Hachisuka etal. (2006)grey scale 220 GHz
continuum PdB cones show velocities of continuum
sources (upper panel)
and water masers (lower panel)
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Sobolev etal. (in prep.)
Sobolev, Sutton, Wyrowski, Stanke, Menten etal.
(in prep.)
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Sobolev etal. (in prep.)
Sobolev, Sutton, Wyrowski, Stanke, Menten etal.
(in prep.)
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DV map
VLSR map
Sobolev, Sutton, Wyrowski, Stanke, Menten etal.
(in prep.)
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Possible circumstellar disk in W3(H2O)Shchekinov
Sobolev (AA, 2004)

• Synchrotron emission (brightness, spectrum,
  wiggling, polarization)
• Dust emission
• Water maser properties
• can be explained in both disk and jet
  hypothesis

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(Sutton, Sobolev, Salii, Malyshev, Ostrovskii,
Zinchenko 2004)

• Outflow region in the methanol lines
• Class I masers potential tracers of protostars
• (Strelnitskij 1982), (Sobolev Strelnitskij
  1983)

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(Sutton, Sobolev, Salii, Malyshev, Ostrovskii,
Zinchenko 2004)

• possible protostars in the outflow region

o
o
o
o
o
o
o
o
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S 231/235 complex
Heyer etal. (1996)
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Gas kinematics around S235
??? DSS, ??????? ??????
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HCODelingha millimeter-wave telescope
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Hora etal. (2004)
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S235A/B Fabri-Perot interferometery, SAO RAN 6m
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NGC 7129

• B
  R

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IRAS 024556034

• B
  R

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IRAS 030355819
12x12

• VLA NVSS Ks 2MASS
  R POSS

1.5x1.5
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IRAS 023956244

• VLA NVSS Ks 2MASS
  R POSS

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IRAS 030253034
VLA NVSS Ks 2MASS
R POSS
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IRAS 023106133
VLA NVSS Ks 2MASS
R POSS
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K-band images
Clusters 053583543 (S231, S233IR),
053823547 (g173.692.87, S235), 054802545
(g183.35-0.57), 195893320 (g70.141.72, S99),
22142, 225665830 (g108.75-0.96, S152)
12x12
053583543 1.5x1.5
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K-band images
Compact clusters multiple 022196152 (W3-IRS5),
022326138 (W3(OH)), 060562131 (g189.030.78,
S247), 231166111 (NGC7538A)
12x12
022196152 1.5x1.5
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K-band images
Rich single clusters S252A
(g189.780.34),S255 (g192.60-0.05),S269
(g196.45-1.68)
12x12
S252A 1.5x1.5
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K-band images
Single clusters G85.41-0.00,
NGC 7538G, G188.950.89, 09015-4843
12x12
G188.950.89 1.5x1.5
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K-band images
Isolated multiple system?
213815000
12x12
213815000 1.5x1.5
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Isolated multiple systems? K-band images
(1.5x1.5) of IRAS sources
023956244 024856902 025416208
045794703 051683634
053632454 07006-0654 211445430
213815000 214135442
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No source in K 004945617
(g123.06-6.31), 024556034 (g136.841.14),
202563951 (g78.620.98), 210744949
(g90.911.51) numerous HII regions, 213065540
(OH, S128, dust in K), 214186552 (NGC 7129,
H2O), 231395939 (g111.24-0.77)
12x12
004945617 1.5x1.5
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No source in K
K 12x12
210744949 VLA NVSS 12x12
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H2O

• CH3OH

5 without associations Total28
10 without associations Total56
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H2O

• CH3OH

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THANKS

• A LOT!

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Ural region
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EKATERINBURG (born 1723)Capital of the
UralsUSSR name was Sverdlovsk
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