Quick report on the Arcetri JEDI activity

C.  Codella  (INAF,  Arcetri)  

Dust & Complex Organic Molecules

Or COMs are daughter species, i.e. they are formed

in gas-phase following the release of parent species?

Are COMs formed on ices and then released into the gas phase?

CO freeze out on grains at T < 19 K, while H2O condansation occurrs at T at 150 K.

(1)  

(2) D-molecules and COMs Emissions are connected (Fontani+14; Codella+15)

(1) HDCO is a tracer of cavity walls (Fontani+, in prep.)

HDCO    (red  and  blue)  

220  AU  

(2)  L1157-­‐B1  

(3)  

(3) D-molecules are related to grain age processing?? (Palumbo+, in prep)

D-bearing molecules in outflows: chemical ‘’filters’’ of material created on grains

COMs: observations towards low-mass YSOs Acetaldehyde (CH3CHO)

Fontani et al. (2014) Codella et al. (2015)

CH3CHO spatial distribution follows the young (2000 yr) cavity produced by the impact of the jet with the ambient medium

COMs associated with the region enriched by iced species evaporated from dust mantles and released into the gas phase

JET  

COMs vs. Deuteration: next steps

First step of the PhD project of E. Bianchi

From L1157-B1 to Cep E…..

..then HH212

Glycolaldehyde: the IRAS4-A2 protostar

Santangelo et al. (in preparation)

Next step: the whole CALYPSO sample. Master thesis (University of Florence): M. De Simone

Spectra consistent with a T = 100-200 K

CH2OHCHO is the simplest of the monosaccharide sugars

Protostellar jets/disks: Kinematics and chemistry

Codella et al. (2014), Podio et al. (2015)

• Jet  rota=on  :  the  puzzling  case  of  RY  TAU  

Keplerian  disk  rota=on  clearly  detected  with    PdBI    No  clear  jet  rota=on  in  [FeII]  1.6mu  with  GEMINI/NIFS  (AO    FWHM:    0.”12  across  the  jet).    Rota%on  upper  limits  consistent  with  Disk  wind                                                                                      Coffey+  2015,  ApJ  in  press      

Disk  in  12CO(2-­‐1)   Jet:  Vrad  map    in  [FeII]  

• Jet  numerical  simula=ons  :  DG  Tau  and  RW  Aur  jets      with  PLUTO  code:    frames  of      different    jets  compared  to  HST/STIS  spectra  provide    constraints  on  magne=c  field    shape    at  launch  point                                              Rubini+  2014,  A&A  567,  13    

• Jet  diagnos=cs  :  the  jet  from  BD  ISO-­‐ChaI  217    

M*=  80  MJup        ;    bipolar  jet.        Analysis  with    X-­‐SHOOTER  spectra          Macc  =2.5x10-­‐11    Msol/yr                Mw  (Blue  +Red)  =  8  x  10-­‐12    Msol/yr  • Mw/Macc    consistent  with  disk  winds                                                                                                                                                                                        Whelan+  2014,  A&A  570,  59    

Observed     Simulated    

• Jet  feedback  on  disk  proper=es  :    1.  the  DEXTEROUS  project  :  excita=on  of    disk  instabili=es  by  asymmetric  jets                  (    in  progress  )                                                  2.  ALMA  project  for  observa=ons  of  B  shape    in  disks  with  rota=ng  jets                                                                                                                                                                (see  Baccioo's  talk)        

Guidi et al. (in preparation)

Radial properties of dust Effects of the CO snowline on grain growth

Homework

To create JEDI products: proposals, white book, proceedings, papers………

Homework

To create JEDI products: proposals, white book, proceedings, papers………

1. Main goal: Synergy between different expertises at different spectral windows;

2. Multiple components: different excitations and at different velocities: what happens to

H2? abundance measurements;

3. Jets’ properties from Class 0 to Class II: collimation, monopolarity?

4. Disks: near-IR to sub-mm to sample different emitting regions;

VLTI/ALMA?

5. Misaligned J-B in the disk/jet system?

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Tm

b (

K)

(a) CN 5-4 9/2-7/2 566.7 GHz - 37" - 82 K

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Tm

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(b) CN 5-4 11/2-9/2 566.9 GHz - 37" - 82 K

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Tm

b (

K)

(c) o-H2O 3

12 - 2

211153.1 GHz - 18" - 249 K

o-H2O 1

10 - 1

01 x 1.33 556.9 GHz - 38" - 61 K

p-H2O 1

11 - 0

00 x 1.06 1113.3 GHz - 19" - 53 K

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12

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b (

K)

(d) CO 10-9 1152.0 GHz - 18" - 304 K

13CO 10-9 x 10.59 1101.3 GHz - 19" - 291 K

-10 0 10 20 30 40V

LSR (km/s)

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(e) SO 1213

- 1112

558.1 GHz - 38" - 194 K

[C II] x 0.02 1900.5 GHz - 11" - 91 K

Monteporzio  kick-­‐off  meeBng…  

Homework

Homework