2021A&A...656A.146M


Query : 2021A&A...656A.146M

2021A&A...656A.146M - Astronomy and Astrophysics, volume 656A, 146-146 (2021/12-1)

Signatures of UV radiation in low-mass protostars. I. Origin of HCN and CN emission in the Serpens Main region.

MIROCHA A., KARSKA A., GRONOWSKI M., KRISTENSEN L.E., TYCHONIEC L., HARSONO D., FIGUEIRA M., GLADKOWSKI M. and ZOLTOWSKI M.

Abstract (from CDS):


Context. Ultraviolet radiation (UV) influences the physics and chemistry of star-forming regions, but its properties and significance in the immediate surroundings of low-mass protostars are still poorly understood.
Aims. Our aim is to extend the use of the CN/HCN ratio, already established for high-mass protostars, to the low-mass regime to trace and characterize the UV field around low-mass protostars on ∼0.6 x 0.6 pc scales.
Methods. We present 5' x 5' maps of the Serpens Main Cloud encompassing ten protostars observed with the EMIR receiver at the IRAM 30 m telescope in CN 1-0, HCN 1-0, CS 3-2, and some of their isotopologs. The radiative-transfer code RADEX and the chemical model Nahoon were used to determine column densities of molecules, gas temperature and density, and the UV field strength, G0.
Results. The spatial distribution of HCN and CS are closely correlated with CO 6-5 emission, that traces outflows. The CN emission is extended from the central protostars to their immediate surroundings also tracing outflows, likely as a product of HCN photodissociation. The ratio of CN to HCN total column densities ranges from ∼1 to 12 corresponding to G0 ≃ 101-103 for gas densities and temperatures typical for outflows of low-mass protostars.
Conclusions. UV radiation associated with protostars and their outflows is indirectly identified in a significant part of the Serpens Main low-mass star-forming region. Its strength is consistent with the values obtained from the OH and H2O ratios observed with Herschel and compared with models of UV-illuminated shocks. From a chemical viewpoint, the CN to HCN ratio is an excellent tracer of UV fields around low- and intermediate-mass star-forming regions.

Abstract Copyright: © A. Mirocha et al. 2021

Journal keyword(s): stars: protostars - ISM: jets and outflows - ISM: molecules - ISM: individual objects: Serpens Main - stars: formation - astrochemistry

VizieR on-line data: <Available at CDS (J/A+A/656/A146): list.dat fits/*>

Simbad objects: 20

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Number of rows : 20
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 [JCC87] IRAS 4B Y*O 03 29 12.058 +31 13 02.05           ~ 588 0
2 2MASS J08254384-5100326 Y*O 08 25 43.85 -51 00 32.7           ~ 310 1
3 LDN 483 DNe 18 17 35 -04 39.8           ~ 276 0
4 NAME Serpens Main Cloud MoC 18 29.2 +00 36           ~ 18 0
5 SH 2-68 N Y*O 18 29 48.09 +01 16 45.0           ~ 130 1
6 [EGE2007] Bolo 22 mm 18 29 48.8 +01 16 51           ~ 4 0
7 NAME SH 2-68 FIR 1 cor 18 29 49.63 +01 15 21.9           ~ 261 2
8 [EGE2007] Bolo 23 mm 18 29 50.20 +01 15 24.6           ~ 4 0
9 V* V371 Ser Or* 18 29 51.21240 +01 16 39.4860           ~ 111 1
10 NAME Serpens SMM 10 IR Y*O 18 29 52.20 +01 15 47.6           ~ 46 1
11 NAME Serpens SMM 4 cor 18 29 57.1 +01 13 15           ~ 134 0
12 IRAS 18274+0112 Y*O 18 29 57.73680 +01 14 05.6940           M4: 138 2
13 [EGE2007] Bolo 26 mm 18 29 59.20 +01 14 07.4           ~ 4 0
14 NAME SERPENS SMM 3 smm 18 29 59.7 +01 14 00           ~ 95 1
15 JCMTSE J183000.2+011251 Y*O 18 30 00.4 +01 12 50           ~ 53 0
16 [ACA2003] Ser A 7 cor 18 30 00.68 +01 13 01.2           ~ 18 1
17 [CED93] 8 smm 18 30 01.8 +01 15 07           ~ 18 0
18 [EGE2007] Bolo 30 cor 18 30 02.50 +01 15 24.5           ~ 3 0
19 RAFGL 2591 Y*O 20 29 24.8230 +40 11 19.590           ~ 605 0
20 LDN 1157 DNe 20 39 06.4 +68 02 13           ~ 549 0

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2023.01.30-23:09:41

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