radio and far infrared observations of agb mass loss
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Radio and Far Infrared Radio and Far Infrared Observations of AGB Mass Observations of AGB Mass
LossLoss
Arancha Castro-CarrizoArancha Castro-Carrizo
ccarrizo@iram.fr
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
IntroductionIntroduction
Structure in AGB CSEsStructure in AGB CSEs
Rings mainly in the opticalRings mainly in the optical
IntroductionIntroduction
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
Structure in AGB CSEsStructure in AGB CSEs
Rings mainly in the opticalRings mainly in the optical
IntroductionIntroduction
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))
IntroductionIntroduction
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
IntroductionIntroduction
IRAM PdB+PVIRAM PdB+PV
Mapping molecular gasMapping molecular gas
IntroductionIntroduction
A few peculiar AGB:A few peculiar AGB:
CO atlas of CSEs by CO atlas of CSEs by Neri et al 1998 Neri 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
TT CygTT Cyg Olofsson et al 2000 U CamU Cam Lindqvist et al
1999
IRAM PdBIRAM PdB
A few peculiar AGB:A few peculiar AGB:
CO atlas of CSEs by CO atlas of CSEs by Neri et al 1998 Neri 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
IntroductionIntroduction
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
IRAM PdB+PVIRAM PdB+PV
Pi.01 Gru
1 GruChiu et al 2006 12CO J=2-1
Molecular emission from Molecular emission from 2003 2003
SMASMA
X Her & V Hya
X HerX Her CO 1-0CO 1-0
Molecular emission from Molecular emission from 2003 2003
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
Molecular emission from Molecular emission from 2003 2003
IRAM Survey of IRAM Survey of 1212COCO
Molecular emission from Molecular emission from 2003 2003
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
IRAM IRAM Survey of Survey of 1212CO CO
R CassiopeiaR Cassiopeia
Radial brightness increases Radial brightness increases Mass loss fluctuations Mass loss fluctuations
IRAM PdB+PVIRAM PdB+PV
X Her
X HerculisX HerculisCO J=1-0CO J=1-0
Axis-symmetricAxis-symmetric
hour-glass structurehour-glass structure
IRAM IRAM Survey of Survey of 1212CO CO
IRAM PdB+PVIRAM PdB+PV
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
IRAM IRAM Survey of Survey of 1212CO CO
IRAM PdB+PVIRAM PdB+PV
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 IRAM Survey of Survey of 1212CO CO
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
IRAM IRAM Survey of Survey of 1212CO CO
IRAM PdB+PVIRAM PdB+PV
Overall sphericalOverall spherical
Axisymmetric inner Axisymmetric inner structurestructure
Velocity gradientVelocity gradient
CO CO JJ=1-0=1-0
RX BootisRX Bootis
IRAM IRAM Survey of Survey of 1212CO CO
IRAM PdB+PVIRAM PdB+PV
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
IRAM PdB+PVIRAM PdB+PV
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))
IRAM IRAM Survey of Survey of 1212CO CO
Schöier et al (in prep.)
IRAM IRAM Survey of Survey of 1212CO CO
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
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