The Center for Astrochemical Studies at MPE Paola Caselli Max- Planck- Ins-tute for Extraterrestrial Physics Credit: ESA/Herschel/SPIRE
OUTLINE Background Research The Center for Astrochemical Studies at MPE (CAS@MPE) Future
Molecular clouds and star formaeon The Milky Way seen in the opecal ~ 100,000 light years CO(1-0) Taurus-Auriga 5 pc NH 3 cores (Benson & Myers 1989) Caselli et al. 2002 Caselli et al. 2002 N 2 H + (1-0) 0.1 pc
Protoplanetary disks Pre- stellar cores as astrophysical laboratories Boley 2009! Quiescent molecular clouds High- mass star forming regions Pre- stellar cores 13 CO(1-0)-FCRAO Narayanan et al. 2008 Nearby cluster forming regions! 1.3 mm continuum - IRAM 30m Ward-Thompson et al. 1999 Composite Spitzer Gutermuth et al. 2008 Herschel/PACS-70µm Henning et al. 2010
Freeze- out and dynamical Eme scales t ambipolar 2.5 10 13 x(e) yr 4.5 10 8 / n H yr t free fall = 3π 32Gρ 4 10 7 / n H yr t freeze out = 10 9 /n H yr 1 αn d πa d 2 v t (Walmsley 1991; Bergin & Tafalla 2007)
Evidence of freeze- out: the missing mass Using CO observaeons: 2.3 M! lost to view (out of 8 M! ) Color: dust emission CO hole dust peak 0.05 ly Molecules freeze out onto dust grains in the center of pre- stellar cores Dust grain
Pre- stellar cores: freeze- out & deuterium fraceonaeon Color: dust emission (Ward- Thompson et al. 1999)_ Color: N 2 H + (1-0); contour: N 2 D + (2-1) N 2 D + (2-1) peaks at dust peak Caselli et al. 2002 Caselli et al. 1999 N 2 D + /N 2 H + ~ 0.03-0.7 (Crapsi et al. 2005; Pagani et al. 2007) NH 2 D/NH 3 ~ 0.06-0.4 (Shah & Wooden 2001; Crapsi et al. 2007) D 2 CO/H 2 CO ~ 0.01-0.1 (Bacmann et al. 2003) DCN/HCN ~ 0.01-0.04 (Turner 2001) DNC/HNC ~ 0.02-0.09 (Hirota et al. 2003) DCO + /HCO + ~ 0.04 (Butner et al. 1995; Caselli et al. 2002) c- C 3 D 2 /c- C 3 H 2 ~ 0.01-0.02 (Spezzano et al. 2013) N 2 H + (1-0) peaks away from dust peak "# D-fraction increases toward core center N 2 D + /N 2 H + ~ 0.2
Importance of spin states (e.g. Hugo et al. 2009) and H 2 tunneling reaceons on dust surface (e.g. Sipilä et al. 2013)
Surprisingly strong ortho- H 2 D + Led to strong revision of astrochemical models (e.g. Roberts et al. 2003) T B (K) 0.8 Caselli et al. 2003, 2008 Vastel et al. 2006 (see also Parise et al. 2010) 0.4 0.0 6.5 7.0 7.5 8.0 V LSR (km s - 1 )
FIRST DETECTION OF para- H 2 D + TOWARD IRAS16293-2422 para- H 2 D + SOFIA/GREAT Brünken et al., Nature, in press
The molecular gas in the cool envelope has been subject to chemical processing for at least one million years. Brünken et al., Nature, in press.
Deuterated molecules are good probes of pre- stellar core central regions, the future stellar cradles! N(NH 3 ) @ VLA USING INTERFEROMETERS D- fraceonaeon increases to ~0.4 in the central 3000 AU; The gas temperature drops to ~6 K in the central 1000 AU; At 1000 AU (~ 10 6 cm - 3 ): no NH 3 (and N 2 ) freeze- out? N(NH 2 D) @ PdBI L1544 Loss of specific angular momentum toward small scales (factor of ~15 from 10000 to 2000 AU). Crapsi, Caselli, Walmsley & Tafalla 2007
The pre- stellar core physical/chemical structure (?) Region to be explored with ALMA and NOEMA Keto & Caselli 2008, 2010; Caselli 2011, IAU 280
First deteceon of ortho- H 2 D + with ALMA 200 AU Friesen et al. 2014, in press
D/H in water D/H in organics Ceccarelli, Caselli, Bocklelèe- Morvan, Mousis, Pizzarello, Robert, Semenov 2014, PPVI
15 NNH + and N 15 NH + (Bizzocchi et al. 2010, 2013) 14 N/ 15 N = 1050±220 14 N/ 15 N in PSC larger than protosolar value! disagreement with model predic-ons (see also Wirström et al. 2012; Hily- Blant et al. 2013) Gerin et al. 2009 observed 14 N/ 15 N fractionation in N 2 H + 14 N/ 15 N = 1110±240 14 N/ 15 N
Enhanced 15 N abundances in HCN and HNC ( 14 N/ 15 N 160 290) found in two Class 0 sources Wampfler et al. 2013
Vasyunin et al., in prep. Tes-ng reac-ng desorp-on from dust grain surfaces See also, e.g., Broten et al. 1984; Walmsley et al. 1984; Mabhews et al. 1985; Remijan et al. 2006; Requena- Torres et al. 2007; Marcelino et al. 2007
DetecEon of CH 2 DOH in L1544: first evidence of surface deuteraeon in pre- stellar core CH 3 OH CH 3 OH CH 3 OH CH 3 OH traces the region where CO is freezing out (R ~ 4000 AU) CH 2 DOH/CH 3 OH = 0.10±0.03 [to be compared with D frac ~ 0.4 within 1000 AU; Crapsi et al. 2007] Bizzocchi et al. 2014
Detectability of Glycine in Solar- type System Precursors Jiménez- Serra et al. 2014
First deteceon of water vapor in a pre- stellar core Caselli et al. 2012 MAIN RESULTS: 1. Unveiled gravitational infall within the central 1,000 AU 2. Total mass of water vapor: ~0.5 Earth masses 3. Total mass of water ice: ~2.6 Jupiter masses " plenty of water to seed future planets and moons. ESA PRESS RELEASE
Bridging the gaps Young protoplanetary disks Protoplanetary disks Solar and planetary systems! Hubble Boley 2009 Douglas, Caselli et al. 2013! Quiescent molecular clouds High- mass star forming regions Pre- stellar cores! 13 CO(1-0)-FCRAO Narayanan et al. 2008 Nearby cluster forming regions 1.3 mm continuum - IRAM 30m Ward-Thompson et al. 1999 Composite Spitzer Gutermuth et al. 2008 Herschel/PACS-70µm Henning et al. 2010
Connect state- of- the- art models and observaeons to link star with planet formaeon and unveil physical/chemical processes
Study environmental effects André et al. 2010
Pre- stellar cores in massive star forming regions ALMA Cycle 0 N 2 D + (3-2) data have allowed us to locate and study massive pre- stellar cores embedded in infrared dark clouds, precursors of high- mass stars and stellar clusters. Tan et al. 2013 Constraints on star formaeon theories (data consistent with Turbulent Core AccreEon Model).
IRDC: extended CO freeze- out and virial equilibrium Hernandez et al. (2011, 2012) MIR extinction map CO freeze-out 2 pc
IRDC: extended SiO emission widespread shocks? Jimenez- Serra et al. (2010; 2014); Henshaw et al. (2013) Extinction map
The dawn of protoplanetary disks Caselli & Ceccarelli 2012 Boley 2009 Ilee, Boley, Caselli et al. 2011
The need of high angular resolueon 0.02 SimulaEon of ALMA observaeons of dust conenuum emission at 300 GHz of a selfgravitating protoplanetary disk around 1M $ star using 3D radiaeve transfer (Douglas, Caselli et al. 2013).
Douglas et al. 2013
The need of laboratory work: from weeds to orchids Jørgensen et al. 2012
http://www.spacetelescope.org/images/opo9545c/
Ceccarelli et al. 2014, PPVI [Adapted from: Bergin et al. 2007 + Caselli & Ceccarelli 2012 + Dullemond et al. 2007 + 2010 + Öberg et al. 2011 + Semenov 2011] See also, e.g., Willacy et al. 1998, 2000; Aikawa et al. 2006; Vasyunin et al. 2008, 2011; Woitke et al. 2010; Kamp et al. 2011; Walsh et al. 2012, 2013; Albertsson et al. 2014
ALMA imaging of the CO snowline of HD163296 (Mathews et al. 2013) DCO + /HCO + ~ 0.3; DCO + in a 110-160 AU ring (T = 19-21 K)
The Center for Astrochemical Studies at MPE (CAS@MPE)
IniEal Laboratory Setup Atomic Clock Modulation Synthesizer 20 GHz AMC Absorption Cell Detector Amplifier MulEplier Chains Spectrum Experiment Control
Center for Astrochemical Studies NOEMA, ALMA,
László Szücs Felipe Alves Jeff Bailey Rumpa Choudhuri Seyit Hocuk Jake Laas Nicole Bailey Wing- Fai Thi Anton Vasyunin Bo Zhao Angelika Langer Basmah Riaz Andy Pon Paola Caselli Alexei Ivlev Ana Chacòn Anna Punanova Olli Sipilä Vlas Sokolov