Twenty-Six-Year Monitoring of Water Masers · IRAS sources in cool interstellar clouds...

Rudnitskij et al. TwentyRudnitskij et al. Twenty--Six Year Monitoring of Six Year Monitoring of Water Masers Water Masers

IAU Symposium 242, Alice SpringsIAU Symposium 242, Alice Springs

11

TwentyTwenty--SixSix--Year Monitoring Year Monitoring of Water Masersof Water Masers

G.M. RudnitskijG.M. Rudnitskij11, M.I. Pashchenko, M.I. Pashchenko11, V.F. Esipov, V.F. Esipov11, , V.A. SamodurovV.A. Samodurov22, I.A. Subaev, I.A. Subaev22, A.M. Tolmachev, A.M. Tolmachev22 and E.E. Lekhtand E.E. Lekht1,31,3

11Sternberg Astronomical Institute, Moscow State University, Sternberg Astronomical Institute, Moscow State University, 13 13 UniversitetskijUniversitetskij prospektprospekt, Moscow, 119992 Russia (, Moscow, 119992 Russia ([email protected]@sai.msu.ru))

22Pushchino Radio Astronomy Observatory,Pushchino Radio Astronomy Observatory, AstrospaceAstrospace Center of theCenter of the LebedevLebedevInstitute of Physics, Russian Academy of Sciences, Pushchino,Institute of Physics, Russian Academy of Sciences, Pushchino,Moscow Region, 142290 RussiaMoscow Region, 142290 Russia ((samsam@@praoprao..ruru))

33Instituto Nacional de AstrofInstituto Nacional de Astrofíísica, sica, ÓÓptica y Electrptica y Electróónica,nica,Luis Enrique Erro No. 1, Apdo Postal 51 y 216, 72840 TonantzintLuis Enrique Erro No. 1, Apdo Postal 51 y 216, 72840 Tonantzintla, Puebla,la, Puebla,MMééxico ([email protected])xico ([email protected])


IAU Symposium 242, Alice SpringsIAU Symposium 242, Alice Springs22

Contents of the workContents of the work

A sample of HA sample of H22O maser emission sources has been observed O maser emission sources has been observed since since 1980.1980. The sample includes 125 sources (65 starThe sample includes 125 sources (65 star--forming forming regions and 60 lateregions and 60 late--type variable stars)type variable stars)..The purpose of this work is to study the variability of the HThe purpose of this work is to study the variability of the H22O O maser emission on a long time interval. The observations are maser emission on a long time interval. The observations are carried out on the average once per month.carried out on the average once per month.Since 1994 lateSince 1994 late--type stars are observed also type stars are observed also spectroscopicallyspectroscopicallyto find out correlation between maser variations and optical to find out correlation between maser variations and optical emission linesemission lines..



Radio spectroscopyRadio spectroscopy

•• RTRT--22 radio telescope 22 radio telescope (Pushchino, Moscow (Pushchino, Moscow Region)Region)

•• HeliumHelium--cooled FET amplifier cooled FET amplifier of the 1.35of the 1.35--cm band cm band ((TTNN =150=150––200 200 K)K)

•• 20482048--channel channel autocorrelation autocorrelation spectrometer spectrometer ((velocity velocity resolutionresolution 0.082 0.082 kmkm//s)s)

•• Sensitivity at the Sensitivity at the 33σσ level level about 10 about 10 JanskysJanskys



StarStar--forming regionsforming regions

HII regionsHII regionsYoung stellar clusters Young stellar clusters ((W31)W31)Bipolar outflowsBipolar outflowsIRAS sources in cool interstellar cloudsIRAS sources in cool interstellar cloudsProtoplanetaryProtoplanetary discs (S255, NGC 7538 and discs (S255, NGC 7538 and others)others)



Maser in a Maser in a protoplanetaryprotoplanetarydisc (S255)disc (S255)

SS255255: H: H22O line profileO line profile5 February 20025 February 2002

Radial velocity, LSR, km/sRadial velocity, LSR, km/s

Flu

x de

nsi

ty,

Flu

x de

nsi

ty, J

yJy



SgrSgr B2B2HH22O flaresO flares

45 50 55 60 65 70 75 80

27.09.2004

16.06.2004

22.07.2004

1000 Jy

Sgr B2

22.04.2004

23.09.2003

31.03.2000

10.11.1998

23.01.1998

11.05.1991

26.12.1989

14.11.1986

13.03.1986

Flux

den

sity

, Jy

Radial velocity VLSR , km/s

Rapid variability in the HRapid variability in the H22O maser W33BO maser W33B2727--28 April 2006, UT 22:35:0728 April 2006, UT 22:35:07--04:52:0204:52:02

58 spectra (6.5 min exposure each)58 spectra (6.5 min exposure each)



NGC 7538NGC 7538

1984 1988 1992 1996 2000 20040

200

400

600

800

NGC7538

-55.9 km/s

-56.5

-54.6 (N+S)

-58-62

-46.6

. -53.6-60

-53.6

-60

-68.8

-60

-64

-64

Inte

grat

ed fl

ux, J

y km

/s

-70 -65 -60 -55 -50 -45

0

50

100

150

200

250

27.03.2002

10.04.2001

NGC7538Fl

ux d

ensi

ty, J

y

Radial velocity VLSR , km/s

outflow

Protoplanetary disk

Bipolar

c

c

o o

c

c

c

oo

o

c c

c

o

c

o

o

North

Southern component of the core of HII region

Northern component of the core of HII region

9

85

2

1

O

O

O

O

O

Toward observer

n

Model: rotating disc and Model: rotating disc and bipolar outflowbipolar outflow

0

25

50

75

100

125

0

10

20

30

40

50

-69.7/-64.8-74/-69.7

(a)

-49.2/-45.9 -52.2/-49.2

(b)9 8

Intrgrated flux, Jy km/s

0

50

100

150

200

250

21

0

25

50

75

100

125

1996 1998 2000 2002 2004

0

25

50

75

100

125

Time (Years)

(c)1 9

-58.4

-58.2

-58.0

-57.8

-57.6

-57.4

1996 1998 2000 2002 2004 2006

0

20

40

60

80

100

43

21B

A

1514

1312

1110

98

76

54

32

1(a)

Rad

ial v

eloc

ity V

LSR ,

km/s

13

1

1512

11

10

9

8

7

5

6

4

32b

2a

(b)Fl

ux d

ensi

ty, J

y

Time (Years)

NGC 7538

Sample HSample H22O spectraO spectra

Integrated HIntegrated H22O line fluxO line flux

TurbulentTurbulentvortexvortex

AnticorrelationAnticorrelation

Velocity drifts of the Velocity drifts of the H2O features (chains)H2O features (chains)

1998 2000 2002 2004-60.4

-60.3

-60.2

-60.1

-60.0

-59.9



Stellar masersStellar masersHH22OO

Y Y CasCas, IK , IK TauTau, W , W EriEri, RS , RS EriEri, , R R TauTau, NV , NV AurAur, IRC+60154, , IRC+60154, AW AW TauTau, , IRC+60169, IRC+60169, U Lyn, U Lyn, GX Mon, GX Mon, VY VY CMaCMa, Z Pup, , Z Pup, QX Pup, X QX Pup, X HyaHya, , U U CVnCVn, , RU RU HyaHya, Y Lib, WX Ser, , Y Lib, WX Ser, VX VX SgrSgr, , IRCIRC––10414, 10414, V1111 V1111 OphOph, , RW RW LyrLyr, , IIRCRC––20540, 20540, RT RT AqlAql, , V391 V391 CygCyg, SY , SY AqlAql, DR , DR CygCyg, , NML NML CygCyg, , UU Peg, AM UU Peg, AM CepCep, , PZ PZ CasCas

HH22O + O + HHαα

R R AqlAql, RR , RR AqlAql, , U U AurAur, , RX BooRX Boo, , R R CasCas, S , S CrBCrB, , R R CrtCrt, , S S CrtCrt, , U Her, U Her, W W HyaHya, , R Leo, R R Leo, R LMiLMi, , U U OriOri, R Peg, , R Peg, S PerS Per, R Tri, , R Tri, RS RS VirVir, , RT RT VirVir

Semiregular Semiregular varibales varibales underlinedunderlined



Optical spectroscopyOptical spectroscopy

125125--cm telescope, Crimeacm telescope, CrimeaGrating spectrographGrating spectrographCCD cameras,CCD cameras, Santa Barbara Instruments GroupSanta Barbara Instruments GroupSensitivity in the Sensitivity in the HHαα region: a spectrum of an region: a spectrum of an 11th magnitude star can be obtained in a 1011th magnitude star can be obtained in a 10--min min exposure.exposure.



Optical spectrum Optical spectrum HH22O line O line HHαα--HH22O integrated flux O integrated flux

MiraMira--type variable R Leo, type variable R Leo, PP = 310= 310dd



14

12

10

8mvis

(AFOEV)

100

200

300F(Hα),10-10

эрг см-2с-1

50500 51000 51500 52000

-21

-20

-19

JD-2400000

lgF(H2O),

Вт м-2

1997.0 1998.0 1999.0 2000.0 2001.0 2002.0

U Aur P = 408d

14121086

(a)mvis

100

150

200

(b)F(Hα),10-10

erg cm-2s-1

50000 51000 52000 53000

-20

-19

-18

(c)

JD-2400000

logF(H2O),

W m-2

1996.0 1998.0 2000.0 2002.0 2004.0

S CrB, P = 360d

MiraMira--type variables S type variables S CrB CrB and U and U AurAur: : visual light curves, visual light curves,

HHαα and Hand H22O integrated fluxesO integrated fluxes



Model: Shock wave in a Model: Shock wave in a mira’smira’s atmosphereatmosphere

Shock 1 Hα

Shock 2 H2O

Star

Postshockmaser shell

Twenty-Six-Year Monitoring of Water Masers · IRAS sources in cool interstellar clouds...

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