Radio and Far Infrared Observations of AGB Mass Loss Arancha Castro-Carrizo

Introduction Introduction What about the presence of asymmetries in the AGB mass loss? …before 2003

Structure in AGB CSEs IRC Mauron & Huggins (1999)Guélin et al. (2000) CFHT V-BAND PDBI CN(2-1) DUST 15” = 400 yr D = 80 pc  Rings mainly in the optical Introduction Introduction

Structure in AGB CSEs  Rings mainly in the optical Introduction Introduction  Masers of OH, SiO, and H 2 O (with VLBI); spots close to the star denoting anisotropy in the innermost regions, incomplete clumpy shells, predominantly in expansion, with some other complex motions SiO v=1 J=1-0 Desmurs et al 2000 IRC+10011VLBA

 Masers of OH, SiO, and H 2 O (with VLBI); spots close to the star denoting anisotropy in the innermost regions, incomplete clumpy shells, predominantly in expansion, with some other complex motions Structure in AGB CSEs  Rings mainly in the optical Introduction Introduction  NIR; monitoring inner dust shell emission Weigelt et al. (2002)

FIR Imaging  ISO/ISOPHOT imaging (Izumiura et al 1996) Introduction Introduction  IRAS imaging (survey by Young et al 1993, Hawkins 1990, Waters et al 1994, Izumiura et al 1997) Izumiura et al μm 160μm Y CVn 15”x20” 30”x90”

 A few peculiar AGB:  CO atlas of CSEs by Neri et al 1998 TT Cyg, U Cam – Olofsson et al 2000 & Lindqvist et al 1999 CW Leo – Fong et al 2003 Mapping molecular gas Introduction Introduction Introd molecular gas IRAM PdB+PV

Mapping molecular gas Mapping molecular gas Introduction Introduction Introd molecular gas  A few peculiar AGB:  CO atlas of CSEs by Neri et al 1998 TT Cyg, U Cam – Olofsson et al 2000 & Lindqvist et al 1999 CW Leo – Fong et al 2003 CW Leo – Fong et al 2003 TT Cyg TT Cyg Olofsson et al 2000 U Cam U Cam Lindqvist et al 1999 IRAM PdB

 A few peculiar AGB:  CO atlas of CSEs by Neri et al 1998 TT Cyg, U Cam – Olofsson et al 2000 & Lindqvist et al 1999 CW Leo – Fong et al 2003 CW Leo – Fong et al 2003 Mapping molecular gas Introduction Introduction Introd molecular gas CW Leo 12 CO J=1-0 BIMA+NRAO 12m Fong et al 2003 After background removal

From FIR to cm from 2003 from 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 (70,160μm) dust around AGB Imaging in the Far Infrared FIR from 2003 FIR from 2003  ISOPHOT imaging of AGB stars ( IRC by Hashimoto & Izumiura 2004, Mchunu, Speck & Meixner 2005)  MLHES program by Akari (see poster by Ueta et al)

FIR, R Hya R Hya FIR imaging Coverage of the observation runs Ueta et al FIR from 2003 FIR from 2003

FIR, R Hya Spitzer MIPS 70μm Ueta et al ” Wareing et al ” Gas density after yr R Hya FIR data & model FIR from 2003 FIR from 2003

 SiO maser in AGB CSEs, monitoring; Cotton et al 2004, 2006, Diamond & Kemball 2003, Boboltz & Diamond 2005 Masers Masers Emission is confined to a ring of ~ 2xR 2.2μm 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, o Ceti, etc Possibly rotation for the snapshots of some stars, IK Tau, o Ceti, etc VLBA Boboltz & Diamond 2005 Masers from 2003 Masers from 2003

Masers Masers 28 SiO & 29 SiO maser emission; discussion on the SiO maser pumping mechanism, radiative or collisional ( Soria-Ruiz et al ) VLBA IRC Compact emission distributed in ring-like structures Different layers for the different SiO masers Different layers for the different SiO masers H 2 O IR line overlapping plays a role in the amplification of the pumping in O-rich AGB CSEs (TX Cam, R Leo) H 2 O IR line overlapping plays a role in the amplification of the pumping in O-rich AGB CSEs (TX Cam, R Leo) Masers from 2003 Masers from 2003

21cm HI emission Observations with NRT by Le Bertre & Gerard (with beam 4’x22’) and with VLA by Matthews & Reid 2007 (with resolutions ~ 100”) Asymmetries in EP Aqr, X Her, likely interaction with the ISM for Y CVn (NRT) Axisymmetric RS Cnc and weak shell-like structure in R Cas (VLA) Axisymmetric RS Cnc and weak shell-like structure in R Cas (VLA) R Cas RS Cnc HI from 2003 HI from 2003

Molecular lines Mapping molecular gas …from 2003

12 CO 230 GHz Lindqvist et al. (in prep) U Cam CN 2-1 J=5/2-3/ GHz CN 2-1 J=3/2-1/ GHz Molecular emission from 2003 Molecular emission from 2003 IRAM PdB+PV

Pi.01 Gru  1 Gru Chiu et al CO J=2-1 Molecular emission from 2003 Molecular emission from 2003 SMA

X Her & V Hya X Her CO 1-0 Molecular emission from 2003 Molecular emission from 2003 Hirano et al 2004 BIMA SMA Nakashima 2005 V Hya CO 3-2

IRAM Survey of 12 CO 46 stars, selected to represent the diversity of AGB stars (evolutionary status, initial mass, chemical class, variability types, peculiar CO profiles) and few early post-AGB stars Aims: Determination of the mass-loss history, geometry, kinematics, clumpiness, photodissociation radius, ejections of “post-AGB” winds, etc Molecular emission from 2003 Molecular emission from 2003

IRAM Survey of 12 CO Molecular emission from 2003 Molecular emission from 2003 A Castro-Carrizo, R Neri, JM Winters, R Lucas & M Grewing (IRAM) V Bujarrabal, G Quintana-Lacaci, J Alcolea (OAN) H Olofsson, FL Schöier, M Lindqvist (SO,OSO)

Strategy: map 12 CO J=2-1 & 1-0 PdB inteferometric observations Track-sharing  2 sources = 2 tracks PdB inteferometric observations Track-sharing  2 sources = 2 tracks Observational stratregy PV telescope data for short-spacing OTF maps, raster mapping, [0,0] PV telescope data for short-spacing OTF maps, raster mapping, [0,0] IRAM Survey of 12 CO IRAM Survey of 12 CO

CO J=1-0 R Cas IRAM Survey of 12 CO IRAM Survey of 12 CO R Cassiopeia Radial brightness increases  Mass loss fluctuations IRAM PdB+PV

X Her X Herculis CO J=1-0 Axis-symmetric Axis-symmetric hour-glass structure hour-glass structure IRAM Survey of 12 CO IRAM Survey of 12 CO IRAM PdB+PV

TX Cam TX Camelopardalis Non-centered hook-like structure Pronounced halo CO J=2-1 & CO J=1-0 IRAM Survey of 12 CO IRAM Survey of 12 CO IRAM PdB+PV

V Hya Axisymmetric X-shaped remnant V Hydrae CO J=1-0 data just from 1 track IRAM Survey of 12 CO IRAM Survey of 12 CO IRAM PdB+PV

IRC CO J=1-0 CO J=2-1 IRAM Survey of 12 CO IRAM Survey of 12 CO IRAM PdB+PV

RX Boo Overall spherical Axisymmetric inner structure Velocity gradient CO J=1-0 RX Bootis IRAM Survey of 12 CO IRAM Survey of 12 CO IRAM PdB+PV

Chi Cyg χ Cygni Survey of CO in CSEs Survey of CO in CSEs CO J=2-1 CO J=1-0 IRAM PdB+PV

 Modeling with radiative transfer LVG codes, including higher-J CO lines from APEX Modeling uv plane (Schöier, Olofsson & Lindqvist et al)uv plane (Schöier, Olofsson & Lindqvist et al) image plane (Bujarrabal, Quintana-Lacaci, Alcolea et al)image plane (Bujarrabal, Quintana-Lacaci, Alcolea et al) IRAM Survey of 12 CO IRAM Survey of 12 CO

Mdot fluctuations Schöier et al (in prep.) IRAM Survey of 12 CO IRAM Survey of 12 CO

Does asymmetry already start on the AGB? Conclusions Conclusions  Mass-loss rates are not constant in time (arc/rings), and these variations are diverse  AGB CSEs show anisotropies in the different mass-loss phases, collimated outflows also in the AGB, clumpiness, etc  Some AGB CSEs present at large scale (FIR, HI) asymmetries due to interaction with ISM Yes