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Astrobiological moleculesin star-forming regions
(hot cores)
Víctor M. RivillaiALMA Fellow, Osservatorio Astrofisico di Arcetri
October 6 2015“From clouds to protoplanetary disks”, Berlin
Image credit: ALMA (ESO/NAOJ/NRAO)/L. Calçada (ESO) & NASA/JPL-Caltech/WISE Team
Maite Beltrán, Riccardo Cesaroni, Claudio Codella, Francesco Fontani, Paul Woods, Serena Viti, Paola Caselli, Anton Vasyunin, Hannah Calcutt
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Glycolaldehyde (GA) (CH2OHCHO) • The simplest sugar.• It can react with propenal (3-carbon sugar) to produce ribose, the central
constituent of RNA.
Important role in interstellar prebiotic chemistry
+RiboseGlycolaldehyde Propenal
RNA
Ethylene glycol (EG) (CH2OH)2
• The simplest sugar alcohol (sugar + hydrogen atoms)
• The reduced alcohol of glycolaldehyde
The SUGAR family• Sugars or monossacharides are the basic units of
carbohydrates.
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The SUGAR family• Still only a few detections…
but increasing interest!
Hollis+00,02, Crovisier04a, Fuente+04, Requena-Torres08, Beltrán+09, Jørgensen+12, Maury+14, Biver+14, Coutens+15, Brouillet+15, Lykke+15, Taquet+15, Rivilla+, in prep.
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Hot molecular cores: a perfect laboratory for astrochemistry
• Molecular environment surrounding massive stars (M > 8 Msun)• The most complex molecules have been detected in hot cores• The radiation from the star and/or shocks evaporates the complex
molecules from the grain mantles. • Very rich chemistry.
NASA- Lara Clemence
Complex molecules already detected: CH3OH, CH3CN, CH3CHO, C2H5OH, C2H5CN, CH3OCHO, CH3COCH3... (e.g. Fontani+07, Beltrán+09)
Good candidate for the detection of GA and EG
OUR TARGET: G31.41+0.31 HOT CORE
Fontani+07
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Observational campaigns
Wavelength (mm)(mm)
Telescope Frequency range (GHz) beam (arcsec x arcsec)7 GBT 45-46 163 IRAM 30m 81.2-89.0 282 IRAM 30m 167.9-175.7 141 SMA 219.45-221.45
229.35-231.351.7 x 3.5 (com)
0.90 x 0.75 (com + vex)1 PdB 103.63-103.7 4.4 x 5.42 PdB 143.61-143.68 4.1 x 3.23 PdB 220.23-220.50 0.5 x 1.1
• Single dish data wide frequency coverage detection of multiple transitions • Interferometric data spatial information
GBT IRAM 30m Submillimeter Array (SMA) Plateu de Bure (PdB)
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Beltrán+09
1.4 mm
2.1 mm
2.9 mm
Detection of glycolaldehyde in G31
• First detection outside the Galactic Center by Beltrán et al. (2009)
PdB o
bserva
tions
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Up to 30 “clean” (not blended) lines with Eup=5-113 K
Rivilla et al, in prep.
Detection of ethylene glycol in G31 (single-dish)
MADCUBA (MAdrid Data CUBe Analysis)
LTE simulated spectra
GBT
IRAM 30m
Tex~70 K
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Rivilla et al, in prep.
Detection of ethylene glycol in G31 (interferometer)
MADCUBA (MAdrid Data CUBe Analysis)
LTE simulated spectra
GBT
IRAM 30m
Submillimeter Array (SMA)
Tex~70 K
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GBT
IRAM 30m
Submillimeter Array (SMA)
MADCUBA (MAdrid Data CUBe Analysis)
LTE simulated spectra
Tex~70 K
Detection of ethylene glycol in G31 (interferometer)
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GBT
IRAM 30m
Submillimeter Array (SMA)
MADCUBA (MAdrid Data CUBe Analysis)
LTE simulated spectra
Tex~70 K
Detection of ethylene glycol in G31 (interferometer)
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Spatial distribution of GA and EG
• Compact spatial distribution • EG & GA: very similar morphology
GlycolaldehydeCOLOR SCALE = Ethylene glycol
White contours = CH3CN
Rivilla et al, in prep.• Integrated intensity maps of 5 unblended
lines of EG
• Spatial coherence supports identification
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Spatial distribution of GA and EG
YELLOW (EG)
CH3CN
Color scale: methyl formate (CH3OCHO)
Black contours: ethanol (CH3CH2OH)
• EG & GA peaks towards the continuum peak
excellent tracers of the gas located closer to the central massive protostar
Better understanding of the star formation process (accretion,
kinematics…)
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Kinematics of EG
ethylene glycol
• Velocity map shows a clear gradient interpreted as rotation (Cesaroni+2011)
CH3CN
•COMs are an excellent tool to study the PHYSICS of star formation
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Kinematics of EG
ethylene glycol
• Velocity map shows a clear gradient interpreted as rotation (Cesaroni+2011)
CH3CN
•COMs are an excellent tool to study the PHYSICS of star formation
•What about CHEMISTRY? How these molecules were formed?
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H CH2OCHO
(CH2OH)2(ethylene glycol)
(F) Woods+13, Fedoseev+15 (D) Beltrán+09,Woods+12
(E) Charnley&Rogers+05Fedoseev+15
(A) Sorrell+01, Woods+12
H
HCO
CH3OH
H2CO
CH2OHCHO(glycolaldehyde)
HCO
HCO
CO+H2CO
HOCCOH (glyoxal)
H
H
CH3O
CH3OH* 2H
HC2O(ketenyl)C
CH2CO(ketene)CH2CHOH
O
OCH2CHOH
HCH2OH
HCO
(B) Bennett&Kaisser07, Garrod+08, Butscher+15
CH2OH
OC2OH
Charnley&Rogers+05
H
O
H
H
HCO
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Observations
Chemical (+ physical) models
Laboratory experiments
Joint study is the only way to really understand how COMs are formed in the space
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Observations: EG/GA ratio
EG/GA is rather different between sources
EG/GA > 1
Do the differences arise from the origin
(the grains) or are a consequence of subsequent evolution?
Source [EG/GA]Hale-Bopp (comet) >6Lemmon (comet) >3Lovejov (comet) >5IRAS 16293-2422 1NGC 1333 IRAS2A 5NGC7129 FIRS2 2SgrB2N 1.3G31.41+0.31 4Orion hot core >10 W51e2 >16G34.3+0.2 >6G-0.02, G-0.11,G+0.693 1.2-1.6
Hollis+00,02, Crovisier04a, Fuente+04, Requena-Torres08, Beltrán+09, Jørgensen+12, Belloche+13 Maury+14, Biver+14, Coutens+15, Brouillet+15, Lykke+15, Taquet+15, Rivilla+, in prep.
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Chemical models and laboratory: EG/GA ratio
Fedoseev+15 Oberg+09
EG/GA<1
EG/GA>1CH3OH:CO EG/GA
Pure CH3OH >10
1:10 < 0.25
Different initial atom H density
OTHER EXPLANATIONS: - Different destruction efficiency in the gas phase? - Different timescales produce different ratios (Garrod+08).
Different compositions of the ices
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Astrobiological moleculesin star-forming regions
(hot cores)
Víctor M. RivillaiALMA Fellow, Osservatorio Astrofisico di Arcetri
October 6 2015“From clouds to protoplanetary disks”, Berlin
Image credit: ALMA (ESO/NAOJ/NRAO)/L. Calçada (ESO) & NASA/JPL-Caltech/WISE Team
Maite Beltrán, Riccardo Cesaroni, Claudio Codella, Francesco Fontani, Paul Woods, Serena Viti, Paola Caselli, Anton Vasyunin, Hannah Calcutt