Investigating the origin of stellar jets with SPHERE HH 30 - HST Linda Podio (INAF-Arcetri) & Simone Antoniucci (INAF-Rome) SPHERE Consortium SVT proposal (1 target): Dec 1-12 2014 P94 EGTO-Other Science (2 targets): Jan 1-8, Mar 29-31 2015 P95 GTO-Other Science (1 target): April 1-7 2015 TEAM: F. Bacciotti (INAF-Arcetri), B. Nisini, T. Giannini (INAF-Rome), R. Gratton, M. Turatto, S. Desidera (INAF-Padova), E. Lagadec (Cote d Azur, PI GTO-Other Science), G. Chauvin, M. Benisty, M. Bonnefoy (IPAG-Grenoble)
JETS & DISKS are tightly connected MHD models: the jet is launched & accelerated by magneto-centrifugal forces Jets may remove angular momentum from the disk DISK WIND Konigl & Pudritz 2007 STELLAR WIND Sauty et al. 2002 1-10 AU < 0.1 AU X-WIND Shu et al. 1994, 2000 OPEN QUESTIONS: What is the jet launching mechanism? What is the jet feedback on the disk in the region of planet formation?
Jet dynamical feedback on the protoplanetary disk Effects of jet magnetic torque on the disk: - angular momentum removal - density structure of the disk - pressure bumps - migration Zanni & Ferreira 2013 Jet asymmetry: - same mass loss rate Ṁ jet ~ n H *V jet - different momentum Ṗ jet ~ Ṁ jet *V jet does it affects the disk? e.g., inclined and eccentric orbits HH 34 - VLT DG Tau B - Keck Podio et al. 2011
Jet irradiation feedback on the protoplanetary disk DG Tau: bipolar X-ray jet - CHANDRA X-ray/UV from jet shocks: irradiation of disk surface? Gudel et al. 2008 Podio et al. 2006, 2009 Panoglou et al. 2012 Shielding by dusty winds : does it affects photoevaporation and disk clearing?
High Angular Resolution Observations of Jets narrow-band imaging HH 30 with HST 0.1 Ray et al 1996, Bacciotti et al. 1999 AO imaging [S II] 6731 A DG TAU with CFHT 0.1 Dougados et al. 2000 long-slit spectrum [S II] 6731 A DG TAU with STIS/HST 0.1 - R=6000 Maurri et al. 2014 IFU image [Fe II] + H2 DG TAU with SINFONI 0.2 - R=3000 Agra-Amboage et al. 2014
High Angular Resolution Observations of Jets narrow-band imaging HH 30 with HST 0.1 Ray et al 1996, Bacciotti et al. 1999 DG TAU with CFHT Limits of previous high AO imaging angular resolution observations: 0.1 [S II] 6731 A Dougados et al. 2000 1) resolution 0.1 2) poor contrast for bright sources, e.g. Herbigs DG TAU with STIS/HST 3) coronagraph 0.3 long-slit spectrum 0.1 - R=6000 [S II] 6731 A Maurri et al. 2014 IFU image [Fe II] + H2 DG TAU with SINFONI 0.2 - R=3000 Agra-Amboage et al. 2014
Observing with SPHERE Goal: understand HOW the jet is launched (in particular for Herbigs) understand IF and HOW the jet affects the disk structure Need: to image the jet down to a few AUs from the source > high spatial resolution (< 0.1 ), high contrast (10 2 10 5 ) images HST 0.6um images DL Tau jet HST coronagraph: stop radius (> 300 mas) too large to probe the innermost regions of disks and jets Grady et al. 2004
Observing with SPHERE JET PROPERTIES Emission lines VIS - NIR Source = guide star Nearby systems (d~100 pc) Contrast 10^3-10^5 Associated to disks Interesting FOV 1. 5 x 1. 5 ZIMPOL (optical) NB imaging + coronagraph [O I], Hα + adjacent cont IRDIS (NIR) NB imaging + coronagraph [Fe II], H2, Paβ, Brγ + adjacent cont IFS (NIR) NIR lines & adj cont simultaneously low spectral resolution = NB imaging coronagraph? EXP TIME: 1 hours per target/line
Target for SVT & EGTO-P94: The twin jets from ZCma Z CMa jet Z CMa: 07 03 43.2-11 33 06.2, Nov-Mar V = 8.8 mag, d~1150 pc continuum Poetzel et al. 1989 High V Binary system (0.1 sep): FU Ori star + eruptive Herbig Be star of EXor type (Benisty+ 2010) The Herbig component underwent two major outbursts in 2008 and 2010, attributed to enhanced accretion events The binary system is associated to twin jets detected in optical and NIR lines Herbig FU Ori Keck-OSIRIS [FeII] Low V Whelan et al. 2010 Canovas et al. 2012
SPHERE-SVT-P95 proposal on ZCma (PI: S. Antoniucci) SCIENCE CASE ZCMA is a unique laboratory to: 1) investigate connection btw accretion and ejection > by imaging the ejection knots (200-400 mas away) associated to the 2008-2010 accretion outbursts to link accretion and ejection events 2) test the magneto-centrifugal scenario for intermediate mass stars > by measuring collimation and accretion/ejection efficiency (Mjet/Macc) 3) test the universality of MHD models > by comparing with jets from low-mass stars (TTSs) 4) investigate the interaction btw the twin jets and the envelope/disks > by taking high angular res images in the line & cont emission OBSERVING MODES Objective: Imaging in Hα, [O I], [Fe II] lines Instruments: ZIMPOL-NB + coro, IRDIS-NB + coro, IFS (+ coro?) Angular resolution: ~20 mas in the optical, ~30-50 mas in the NIR Distance from source: down to 0.05-0.1 (50-100 AU) Integration time: 1 hour per line (~3 hours)
Target for EGTO-P94, GTO-P95: The Jet from HD 163296 HST + 1 coronagraph Grady et al. 2000 Apache/GFP + coronagraph [S II] 6731 Å XShooter/VLT - slit offset to avoid the star cont Wassel et al. 2006 Ellerbroek, Podio et al. 2014 HD 163296: 17 56 21-21 57 21.870 > observable in Mar Jul R = 6.86 mag, d~120 pc > ideal to observe very close to the source (~6-12 AU) with AO young Herbig AeBe star with disk (cont) + bipolar jet (knots seen in optical+nir lines) periodic ejection events (from proper motion/radial velocity + knots distance > τ ~16 years) optical fading+nir brightening at ejection events > evidence of dust along the jet?
GTO-P95 observations of HD 163296 (PI: L. Podio) SCIENCE CASE resolve the jet close to the driving source (down to 0.05 =6 AU) > test MHD models infer jet properties: width, density & temperature (from [Fe II]) > jets from intermediate-mass stars vs low-mass stars? infer the mass loss rate > accretion/ejection efficiency dust in the jet (from [Fe II] lines)? > disk shielding? detect new knots > test jet periodicity? detect molecular gas (H2) > wide angle disk-wind? Ellerbroek, Podio et al. 2014 OBSERVING MODES ZIMPOL + NB filters: imaging in [O I] 6300 Å, Hα 6563 Å > jet width/collimation IRDIS + NB filters: imaging in [Fe II] 1.64 µm, H2 2.12 µm > atomic/molecular jet IFS: [Fe II] 1.25, 1.53, 1.64 µm lines > ne, Te, dust. Accurate continuum subtraction. Coronagraph + AO: image close to the star (~50-100 mas), res down to ~20 mas
CONCLUSIONS Structure of jets, launch mechanism : Important clues on disk evolution and planet formation YSO sources of jets are optimally suited for AO coronagraphic imaging and/or IFU jet tracers in the VIS NIR Well doable with SPHERE Need a few hours observation per target
OPEN QUESTIONS A few technical aspects: How to use the ETC? It is optimised for planets, output=contrast vs distance Is it enough 1 hr integration per line/target (30 min line + 30 adj cont)? Is it possible to use IRDIS-K (H2 line) with IFS-J-H ([Fe II] lines) simultaneously? Occulting the star IRDIS: 4QPM (IWA~0.05, Visitor) vs ALC (IWA~0.15-0.2, Service) sensitivity losses? Crucial to understand how close to the source we can observe Occulting the star ZIMPOL: 4QPM (IWA~λ/D, no in P95) vs CLC (D~93-1240 mas) For jets we use field-stabilized mode?