radio and far infrared observations of agb mass loss

Radio and Far Infrared Radio and Far Infrared Observations of AGB Mass Observations of AGB Mass

LossLoss

Arancha Castro-CarrizoArancha Castro-Carrizo

[email protected]

mailto:[email protected]

Introduction

IntroductionIntroduction

What about the presence of asymmetries in the AGB mass loss?

…before 2003

Structure in AGB CSEsStructure in AGB CSEs

IRC+10216

Mauron & Huggins (1999) Guélin et al. (2000)

CFHT V-BAND PDBI CN(2-1)

DUST

15” = 400 yrD = 80 pc

Rings mainly in the opticalRings mainly in the optical





Masers of OH, SiO, and HMasers of OH, SiO, and H22O (with VLBI); O (with VLBI);

spots close to the star denoting anisotropy spots close to the star denoting anisotropy in the innermost regions, incomplete in the innermost regions, incomplete clumpy shells, predominantly in clumpy shells, predominantly in expansion, with some other complex expansion, with some other complex motionsmotions

SiO v=1 J=1-0 Desmurs et al 2000

IRC+10011 VLBA

Masers of OH, SiO, and HMasers of OH, SiO, and H22O (with VLBI); O (with VLBI);

spots close to the star denoting anisotropy spots close to the star denoting anisotropy in the innermost regions, incomplete in the innermost regions, incomplete clumpy shells, predominantly in clumpy shells, predominantly in expansion, with some other complex expansion, with some other complex motionsmotions




NIR; monitoring inner dust NIR; monitoring inner dust shell emissionshell emission

Weigelt et al. (2002)

FIR ImagingFIR Imaging

ISO/ISOPHOT imagingISO/ISOPHOT imaging ((Izumiura et al 1996Izumiura et al 1996))


IRAS imagingIRAS imaging (survey by (survey by Young et al 1993Young et al 1993, , Hawkins 1990Hawkins 1990, , Waters et al 1994Waters et al 1994, , Izumiura et al 1997Izumiura et al 1997))

Izumiura et al 1996

90μm

160μm

Y CVn

15”x20”

30”x90”

A few peculiar AGB:A few peculiar AGB:

CO atlas of CSEs by CO atlas of CSEs by Neri et al 1998Neri et al 1998

• TT Cyg, U Cam – TT Cyg, U Cam – Olofsson et al 2000 Olofsson et al 2000 && Lindqvist et al 1999 Lindqvist et al 1999

• CWCW Leo – Leo – Fong et al 2003Fong et al 2003

Mapping molecular gasMapping molecular gas


IRAM PdB+PVIRAM PdB+PV




CO atlas of CSEs by CO atlas of CSEs by Neri et al 1998 Neri et al 1998



TT CygTT Cyg Olofsson et al 2000 U CamU Cam Lindqvist et al

1999

IRAM PdBIRAM PdB


CO atlas of CSEs by CO atlas of CSEs by Neri et al 1998 Neri et al 1998





CW Leo CW Leo 1212CO CO JJ=1-0=1-0

BIMA+NRAO 12mBIMA+NRAO 12m Fong et al 2003

After background removal

From FIR to cm from 2003

from FIR to radiofrom FIR to radio

…from 2003

What about the presence of asymmetries in the AGB mass loss?

FIR from 2003

MIRIAD project to image with SST MIPS (70,160MIRIAD project to image with SST MIPS (70,160μμm) m) dust around AGB dust around AGB

Imaging in the Far InfraredImaging in the Far Infrared

FIR from 2003 FIR from 2003

ISOPHOT imaging of AGB starsISOPHOT imaging of AGB stars ((IRC-10529 by IRC-10529 by Hashimoto & Izumiura 2004Hashimoto & Izumiura 2004, , Mchunu, Speck & Meixner 2005Mchunu, Speck & Meixner 2005))

MLHES program by Akari MLHES program by Akari (see poster by (see poster by Ueta et alUeta et al))

FIR, R Hya

R Hya R Hya FIR imagingFIR imagingCoverage of the observation runs

Ueta et al. 2006

FIR from FIR from 2003 2003

FIR, R Hya

Spitzer MIPS 70μm

Ueta et al. 2006

100”

Wareing et al. 2006

100”

Gas density after 40 000 yr

R HyaR Hya FIR data & modelFIR data & model

FIR from FIR from 2003 2003

SiO maser in AGB CSEs, monitoring; SiO maser in AGB CSEs, monitoring; Cotton et al 2004, 2006Cotton et al 2004, 2006, , Diamond & Kemball 2003Diamond & Kemball 2003, , Boboltz & Diamond 2005 Boboltz & Diamond 2005

Masers

MasersMasers

• Emission is confined to a ring of ~ 2xREmission is confined to a ring of ~ 2xR2.22.2μμmm

• Short lifetime for individual spots Short lifetime for individual spots

• Diameter of the SiO ring show variations of 3-14% Diameter of the SiO ring show variations of 3-14%

• The degree of linear polarization also changes The degree of linear polarization also changes

• Possibly rotation for the snapshots of some stars, IK Tau, Possibly rotation for the snapshots of some stars, IK Tau, oo Ceti, etc Ceti, etc

VLBA

Boboltz & Diamond 2005

Masers from 2003 Masers from 2003

Masers

MasersMasers• 2828SiO & SiO & 2929SiO maser emission;SiO maser emission; discussion on the SiO maser pumping mechanism, radiative or discussion on the SiO maser pumping mechanism, radiative or

collisionalcollisional ((Soria-Ruiz et al 2004-2007Soria-Ruiz et al 2004-2007))

VLBAVLBAIRC+10011IRC+10011

• Compact emission distributed in Compact emission distributed in ring-like structures ring-like structures

• Different layers for the different SiO Different layers for the different SiO masersmasers

• HH22O IR line overlapping plays a role O IR line overlapping plays a role in the amplification of the pumping in in the amplification of the pumping in O-rich AGB CSEs (TX Cam, R Leo)O-rich AGB CSEs (TX Cam, R Leo)

Masers from 2003 Masers from 2003

21cm HI emission

21cm H21cm HII emission emission

Observations with NRT by Observations with NRT by Le Bertre & Gerard 2004-2006Le Bertre & Gerard 2004-2006 (with (with beam 4’x22’) and with VLA by beam 4’x22’) and with VLA by Matthews & Reid 2007Matthews & Reid 2007 (with (with resolutions ~ 100”)resolutions ~ 100”)

• Asymmetries in EP Aqr, X Her, likely interaction with Asymmetries in EP Aqr, X Her, likely interaction with the ISM for Y CVn (NRT)the ISM for Y CVn (NRT)

• Axisymmetric RS Cnc and weak shell-like structure in Axisymmetric RS Cnc and weak shell-like structure in R Cas (VLA)R Cas (VLA)

R CasR CasRS CncRS Cnc

HI from 2003 HI from 2003

Mapping molecular gas Mapping molecular gas

…from 2003

1212CO CO JJ=2-1 @ 230 GHz=2-1 @ 230 GHz

Lindqvist et al. (in prep)U CamU Cam

CN 2-1 CN 2-1 JJ=5/2-3/2 =5/2-3/2 FF=7/2-5/2=7/2-5/2@ 226.875 GHz@ 226.875 GHz

CN 2-1 CN 2-1 JJ=3/2-1/2 =3/2-1/2 FF=5/2-3/2=5/2-3/2@ 226.660 GHz@ 226.660 GHz

Molecular emission from Molecular emission from 2003 2003


Pi.01 Gru

1 GruChiu et al 2006 12CO J=2-1


SMASMA

X Her & V Hya

X HerX Her CO 1-0CO 1-0


Hirano et al 2004

BIMABIMA

SMASMA

Nakashima 2005

V HyaV Hya CO 3-2CO 3-2

IRAM Survey of IRAM Survey of 1212COCO

46 stars46 stars, selected to represent the , selected to represent the diversity of AGB starsdiversity of AGB stars (evolutionary status, initial mass, chemical class, variability (evolutionary status, initial mass, chemical class, variability types, peculiar CO profiles) and types, peculiar CO profiles) and few early post-AGB starsfew early post-AGB stars

Aims: Aims: Determination of the mass-loss historyDetermination of the mass-loss history, geometry, , geometry, kinematics, clumpiness, photodissociation radius, ejections of kinematics, clumpiness, photodissociation radius, ejections of “post-AGB” winds, etc “post-AGB” winds, etc


IRAM Survey of IRAM Survey of 1212COCO


A Castro-Carrizo, R Neri, JM Winters, R Lucas & M Grewing (IRAM)A Castro-Carrizo, R Neri, JM Winters, R Lucas & M Grewing (IRAM)

V Bujarrabal, G Quintana-Lacaci, J Alcolea (OAN)V Bujarrabal, G Quintana-Lacaci, J Alcolea (OAN)

H Olofsson, FL SchH Olofsson, FL Schööier, M Lindqvist (SO,OSO)ier, M Lindqvist (SO,OSO)

Strategy: Strategy: map map 1212CO CO JJ=2-1 & 1-0=2-1 & 1-0

• PdB inteferometric observations PdB inteferometric observations Track-sharing Track-sharing 2 sources = 2 tracks 2 sources = 2 tracks

• PV telescope data for short-spacing PV telescope data for short-spacing OTF maps, raster mapping, [0,0]OTF maps, raster mapping, [0,0]

IRAM IRAM Survey of Survey of 1212CO CO

CO CO JJ=1-0=1-0


R CassiopeiaR Cassiopeia

Radial brightness increases Radial brightness increases Mass loss fluctuations Mass loss fluctuations


X Her

X HerculisX HerculisCO J=1-0CO J=1-0

Axis-symmetricAxis-symmetric

hour-glass structurehour-glass structure



TX CamelopardalisTX Camelopardalis

Non-centered hook-like structureNon-centered hook-like structure

Pronounced haloPronounced halo

CO CO JJ=2-1 & CO =2-1 & CO JJ=1-0 =1-0



AxisymmetricAxisymmetric

X-shaped remnantX-shaped remnant

V HydraeV HydraeCO CO JJ=1-0=1-0

data just from 1 trackdata just from 1 track


IRAM PdB+PV

IRC +50049IRC +50049CO CO JJ=1-0=1-0

CO CO JJ=1-0=1-0

CO CO JJ=2-1=2-1



Overall sphericalOverall spherical

Axisymmetric inner Axisymmetric inner structurestructure

Velocity gradientVelocity gradient

CO CO JJ=1-0=1-0

RX BootisRX Bootis



Chi Cyg

χ χ CygniCygni Survey of CO in CSEsSurvey of CO in CSEs

CO J=2-1CO J=2-1CO CO JJ=1-0=1-0


Modeling with radiative transfer LVG codes, Modeling with radiative transfer LVG codes, including higher-including higher-JJ CO lines from APEX CO lines from APEX

• uvuv plane ( plane (SchSchööier, Olofsson & Lindqvist et alier, Olofsson & Lindqvist et al))

• image plane (image plane (Bujarrabal, Quintana-Lacaci, Alcolea et alBujarrabal, Quintana-Lacaci, Alcolea et al))


Schöier et al (in prep.)


Does asymmetry already start on the AGB?Does asymmetry already start on the AGB?

Conclusions

ConclusionsConclusions

Mass-loss rates are not constant in timeMass-loss rates are not constant in time (arc/rings), (arc/rings), and these variations are diverseand these variations are diverse

AGB CSEs show anisotropiesAGB CSEs show anisotropies in the different mass-loss in the different mass-loss phases, collimated outflows also in the AGB, clumpiness, phases, collimated outflows also in the AGB, clumpiness, etc etc

Some Some AGB CSEs AGB CSEs present present at large scale at large scale (FIR, HI) (FIR, HI) asymmetries due to interaction with ISM asymmetries due to interaction with ISM

YesYes

radio and far infrared observations of agb mass loss

Documents

agb imaging

agb cses rings

sio ring

cotton et

young et

desmurs et

waters et

hirano et