2022A&A...659A..67M


Query : 2022A&A...659A..67M

2022A&A...659A..67M - Astronomy and Astrophysics, volume 659A, 67-67 (2022/3-1)

Chemical survey of Class I protostars with the IRAM-30 m.

MERCIMEK S., CODELLA C., PODIO L., BIANCHI E., CHAHINE L., BOUVIER M., LOPEZ-SEPULCRE A., NERI R. and CECCARELLI C.

Abstract (from CDS):

Context. Class I protostars are a bridge between Class 0 protostars (≤105 yr old), and Class II (≥106 yr) protoplanetary disks. Recent studies show gaps and rings in the dust distribution of disks younger than 1 Myr, suggesting that planet formation may start already at the Class I stage. To understand what chemistry planets will inherit, it is crucial to characterize the chemistry of Class I sources and to investigate how chemical complexity evolves from Class 0 protostars to protoplanetary disks. Aims. There are two goals: (i) to perform a census of the molecular complexity in a sample of four Class I protostars, and (ii) to compare the data with the chemical compositions of earlier and later phases of the Sun-like star formation process. Methods. We performed IRAM-30 m observations at 1.3 mm towards four Class I objects (L1489-IRS, B5-IRS1, L1455-IRS1, and L1551-IRS5). The column densities of the detected species were derived assuming local thermodynamic equilibrium (LTE) or large velocity gradients (LVGs). Results. We detected 27 species: C-chains, N-bearing species, S-bearing species, Si-bearing species, deuterated molecules, and interstellar complex organic molecules (iCOMs; CH3OH, CH3CN, CH3CHO, and HCOOCH3). Among the members of the observed sample, L1551-IRS5 is the most chemically rich source. Different spectral profiles are observed: (i) narrow lines (∼1 km s–1) towards all the sources, (ii) broader lines (∼4 km s–1) towards L1551-IRS5, and (iii) line wings due to outflows (in B5-IRS1, L1455-IRS1, and L1551-IRS5). Narrow c-C3H2 emission originates from the envelope with temperatures of 5-25 K and sizes of ∼2''-10''. The iCOMs in L1551-IRS5 reveal the occurrence of hot corino chemistry, with CH3OH and CH3CN lines originating from a compact (∼0.''15) and warm (T > 50 K) region. Finally, OCS and H2S seem to probe the circumbinary disks in the L1455-IRS1 and L1551-IRS5 binary systems. The deuteration in terms of elemental D/H in the molecular envelopes is: ∼10-70% (D2CO/H2CO), ∼5-15% (HDCS/H2CS), and ∼1-23% (CH2DOH/CH3OH). For the L1551-IRS5 hot corino we derive D/H ∼2% (CH2DOH/CH3OH). Conclusions. Carbon chain chemistry in extended envelopes is revealed towards all the sources. In addition, B5-IRS1, L1455-IRS1, and L1551-IRS5 show a low-excitation methanol line that is narrow and centered at systemic velocity, suggesting an origin from an extended structure, plausibly UV-illuminated. The abundance ratios of CH3CN, CH3CHO, and HCOOCH3 with respect to CH3OH measured towards the L1551-IRS5 hot corino are comparable to that estimated at earlier stages (prestellar cores, Class 0 protostars), and to that found in comets. The deuteration in our sample is also consistent with the values estimated for sources at earlier stages. These findings support the inheritance scenario from prestellar cores to the Class I phase when planets start forming.

Abstract Copyright: © ESO 2022

Journal keyword(s): astrochemistry - stars: formation - ISM: molecules

VizieR on-line data: <Available at CDS (J/A+A/659/A67): table1.dat sp/*>

Simbad objects: 29

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Number of rows : 29
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 NAME W 3 OH HII 02 27 04.1 +61 52 22           ~ 990 2
2 3C 84 Sy2 03 19 48.1599902040 +41 30 42.108850836   13.10 12.48 11.09   ~ 3805 3
3 NAME LDN 1455 IRS 1 cor 03 27 39.08 +30 13 03.1           ~ 151 0
4 LDN 1455 DNe 03 28 00.6480 +30 07 58.800           ~ 180 1
5 [JCC87] IRAS 2A Y*O 03 28 55.55 +31 14 36.7           ~ 435 3
6 [HSW2018] NGC 1333-17 smm 03 29 03.73 +31 16 03.8           ~ 80 0
7 [JCC87] IRAS 4A Y*O 03 29 10.49 +31 13 30.8           ~ 678 1
8 Barnard 1 MoC 03 33 16.3 +31 07 51           ~ 302 0
9 NAME Perseus Cloud SFR 03 35.0 +31 13           ~ 1237 0
10 IRAS 03445+3242 Y*O 03 47 41.603 +32 51 43.79           ~ 188 0
11 LDN 1471 DNe 03 48.0 +32 54           ~ 309 0
12 IRAS 04016+2610 Y*O 04 04 43.07064 +26 18 56.3904           ~ 247 0
13 LDN 1489 DNe 04 04 47.5 +26 19 42           ~ 213 0
14 LDN 1551 DNe 04 31 30.0 +18 12 30           ~ 794 1
15 RAFGL 5123 Y*O 04 31 34.07736 +18 08 04.9020           K3V/M3III 841 0
16 V* HL Tau Or* 04 31 38.5107609312 +18 13 57.859747968   15.89 14.49 14.39   K5 1342 0
17 Mrk 1506 Sy1 04 33 11.0956735296 +05 21 15.619461552   15.72 15.05 10.08   ~ 1934 2
18 IRAS 04302+2247 Y*O 04 33 16.50096 +22 53 20.4000           ~ 158 0
19 LDN 1527 DNe 04 39 53 +25 45.0           ~ 575 0
20 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4009 0
21 LDN 1544 DNe 05 04 16.6 +25 10 48           ~ 793 0
22 V* V883 Ori Or* 05 38 18.1018261392 -07 02 26.017707120   14.80       F:I: 138 0
23 HH 212 HH 05 43 51.41 -01 02 53.1           ~ 346 1
24 V* TW Hya TT* 11 01 51.9053285064 -34 42 17.033218380   11.94 10.50 10.626 9.18 K6Ve 1759 1
25 HD 100546 Be* 11 33 25.4408872296 -70 11 41.241297948   6.71 6.30   6.64 A0VaekB8_lB 729 1
26 NAME IRAS 16293-2422B Y*O 16 32 22.63 -24 28 31.8           ~ 240 0
27 NAME IRAS 16293-2422A Y*O 16 32 22.869 -24 28 36.11           ~ 148 0
28 [HMH2007] 67 Y*O 18 29 06.20 +00 30 43.3           ~ 21 1
29 3C 454.3 Bla 22 53 57.7480438728 +16 08 53.561508864   16.57 16.10 15.22   ~ 2697 2

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2022.09.24-19:30:07

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