2020A&A...640A..75D


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.26CET14:21:06

2020A&A...640A..75D - Astronomy and Astrophysics, volume 640A, 75-75 (2020/8-1)

Seeds of Life in Space (SOLIS). X. Interstellar complex organic molecules in the NGC 1333 IRAS 4A outflows.

DE SIMONE M., CODELLA C., CECCARELLI C., LOPEZ-SEPULCRE A., WITZEL A., NERI R., BALUCANI N., CASELLI P., FAVRE C., FONTANI F., LEFLOCH B., OSPINA-ZAMUDIO J., PINEDA J.E. and TAQUET V.

Abstract (from CDS):


Context. The interstellar complex organic molecules (iCOMs) are C-bearing molecules containing at least six atoms; two main proposals for their formation are suggested: a direct formation in the icy mantle of the dust grains and formation through the reaction in gas phase of released grain mantle species. The shocked gas along outflows driven by low-mass protostars is a unique environment to study how the iCOMs can be formed as the composition of the dust mantles is sputtered into the gas phase.
Aims. The chemical richness in shocked material associated with low-mass protostellar outflows has been so far studied in the prototypical L1157 blue-shifted outflow to investigate the iCOM formation routes. To understand whether the case of L1157-B1 is unique, we imaged and studied the IRAS 4A outflows in the NGC 1333 star forming region.
Methods. We used the NOrthern Extended Millimeter Array interferometer as part of the IRAM Seeds Of Life in Space (SOLIS) Large Program to image the large-scale bipolar outflows driven by the IRAS 4A system in the 3 mm band, and we compared the observation with the GRAINOBLE+ astrochemical model.
Results. We report the first detection, in the IRAS 4A outflows, of several iCOMs: six lines of methanol (CH3OH), eight of acetaldehyde (CH3CHO), one of formamide (NH2CHO), and four of dimethyl ether (CH3OCH3), all sampling upper excitation energy up to ∼30 K. We found a significant chemical differentiation between the southeast outflow driven by the IRAS 4A1 protostar, showing a richer molecular content, and the north-southwest one driven by the IRAS 4A2 hot corino. The CH3OH/CH3CHO abundance ratio is lower by a factor of ∼4 in the former; furthermore, the ratio in the IRAS 4A outflows is lower by a factor of ∼10 with respect to the values found in different hot corinos.
Conclusions. After L1157-B1, the IRAS 4A outflow is now the second outflow to show an evident chemical complexity. Given that CH3OH is a grain surface species, the astrochemical gas-phase model run with GRAINOBLE+ reproduced our observation assuming that acetaldehyde is formed mainly through the gas-phase reaction of the ethyl radical (CH3CH2) and atomic oxygen. Furthermore, the chemical differentiation between the two outflows suggests that the IRAS 4A1 outflow is likely younger than that of the IRAS 4A2. Further investigation is needed to constrain the age of the outflow. In addition, observation of even younger shocks are necessary. In order to provide strong constraints on the CH3CHO formation mechanisms it would be interesting to observe CH3CH2, but given that its frequencies are not known, future spectroscopic studies on this species are needed.

Abstract Copyright: © M. De Simone et al. 2020

Journal keyword(s): astrochemistry - instrumentation: interferometers - stars: formation - ISM: jets and outflows - ISM: molecules - ISM: individual objects: NGC 1333 IRAS 4A

VizieR on-line data: <Available at CDS (J/A+A/640/A75): list.dat fits/*>

Simbad objects: 25

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Number of rows : 25

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3582 3
2 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 403 3
3 [SVS76] NGC 1333 13A smm 03 29 03.73 +31 16 03.8           ~ 53 0
4 V* V512 Per Or* 03 29 03.7567945196 +31 16 03.959183877           ~ 352 0
5 [JCC87] IRAS 4A2 Y*O 03 29 10.413 +31 13 32.20           ~ 89 1
6 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 608 1
7 [JCC87] IRAS 4A1 Y*O 03 29 10.510 +31 13 31.01           ~ 80 1
8 [JCC87] IRAS 4 FIR 03 29 10.9 +31 13 26           ~ 468 0
9 NGC 1333 OpC 03 29 11 +31 18.6           ~ 1231 1
10 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 562 0
11 [KJD2006] SMM J033335+31075 PoC 03 33 21.3 +31 07 28           ~ 79 0
12 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1086 0
13 4C 32.14 QSO 03 36 30.10760600 +32 18 29.3422210     17.50 16.6   ~ 584 1
14 EM* LkHA 101 Em* 04 30 14.438 +35 16 24.03   17.91 15.71 13.33   F 301 1
15 [CAZ2013] HH 212 MMS Y*O 05 43 51.41 -01 02 53.2           ~ 7 0
16 IRAS 16293-2422 cor 16 32 22.56 -24 28 31.8           ~ 1058 1
17 NAME IRAS 16293-2422B Y*O 16 32 22.63 -24 28 31.8           ~ 188 0
18 LDN 483 DNe 18 17 35 -04 39.8           ~ 214 0
19 [KVV2010] SMM4-W out 18 29 11.60 +01 13 18.1           ~ 8 0
20 EM* MWC 349 ** 20 32 45.499080 +40 39 36.74124   15.88 13.15 12.13   Bep 710 0
21 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 493 0
22 [DE95] LDN 1157 B2 out 20 39 09.3 +68 00 44           ~ 61 0
23 [DE95] LDN 1157 B1 out 20 39 11 +68 01.3           ~ 188 0
24 3C 454.3 QSO 22 53 57.74798 +16 08 53.5611   16.57 16.10 15.22   ~ 2528 2
25 NAME Cep E HII 23 03 12.779 +61 42 25.75           ~ 156 0

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2020.10.26-14:21:06

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