Cyanopolyyne line survey towards high-mass star-forming regions with TMRT

Wang, Y. X.; Zhang, J. S.; Yan, Y. T.; Qiu, Jiali; Chen, J. L.; Zhao, Jianbao; Zou, Y. P.; WU, XUAN; He, Xiang; Gong, Y.; Cai, Jiawei

doi:10.1051/0004-6361/202142450

Cited by 3 publications

(2 citation statements)

References 123 publications

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“…where k and W are the Boltzmann constant and the integrated line intensity, respectively, Q(T rot ) = 4.58 T rot + 0.28 is the partition function for HC 3 N (Wang et al 2022), T rot and N are the rotational temperature and the column density, respectively, and the Sµ 2 , ν and E u values are taken from the CDMS catalog (see Section 2.2).…”

Section: Line Widthmentioning

confidence: 99%

A Possible Chemical Clock in High-mass Star-forming Regions: N(HC3N)/N(N2H+)?

Wang,

Zhang,

et al. 2023

Preprint

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We conducted observations of multiple HC 3 N (J = 10−9, 12−11 and 16−15) lines and N 2 H + (J = 1−0) line toward a large sample of 61 ultracompact (UC) Hii regions, through the Institut de Radioastronomie Millmétrique 30 m and the Arizona Radio Observatory 12 m telescopes. The N 2 H + J = 1−0 line is detected in 60 sources and HC 3 N is detected in 59 sources, including 40 sources with three lines, 9 sources with two lines, and 10 sources with one line. Using the rotational diagram, the rotational temperature and column density of HC 3 N were estimated toward sources with at least two HC 3 N lines. For 10 sources with only one HC 3 N line, their parameters were estimated, taking one average value of T rot . For N 2 H + , we estimated the optical depth of the N 2 H + J = 1−0 line, based on the line intensity ratio of its hyperfine structure lines. Then the excitation temperature and column density were calculated. When combining our results in UC Hii regions and previous observation results on high-mass starless cores (HMSCs) and high-mass protostellar cores (HMPOs), the N (HC 3 N)/N (N 2 H + ) ratio clearly increases with the evolution of high mass star-forming regions (HMSFRs). Moreover, positive correlations between the ratio and other evolutionary indicators (dust temperature, bolometric luminosity, and luminosity-to-mass ratio) are found. Thus we propose the ratio of N (HC 3 N)/N (N 2 H + ) as a reliable chemical clock of HMSFRs.

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Section: Line Widthmentioning

confidence: 99%

A Possible Chemical Clock in High-mass Star-forming Regions: N(HC3N)/N(N2H+)?

Wang,

Zhang,

et al. 2023

Preprint

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“…He et al (2021) andWang et al (2022).4.4.2. Outflow Orientations Indicated by H 2 O Maser and SiO J = 5-4 Emissions H 2 O, SiO masers, and SiO nonmasing emissions have been employed in previous studies to investigate outflows, as demonstrated by…”

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confidence: 99%

Masers and Star Formation Activities in W51A

Zhang,

Chen,

Wang

et al. 2024

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Concurrently with the maser flare observed in W51-North during the 3 month monitoring of H2O, NH3, and CH3OH maser variability from 2020 January to April using the Tianma 65 m Radio Telescope, we conducted Very Large Array mappings for these three maser species across the entirety of W51A region. After finding the ring-shaped H2O maser which might trace the disk surrounding the protostar residing in W51-North, the NH3 (9,6) maser delineated a jet which might be illuminated in the luminosity outburst possibly caused by the infalling streamer’s interaction with the protostar’s disk. An analysis of the comprehensive distribution of maser spots allowed us to affirm that W51N4 or ALMAmm31 serves as the primary source of the Lacy jet. Furthermore, we observed that class I methanol maser spots may extend beyond the locations of the H2O and NH3 (9,6) masers within the outflow. Additionally, emissions from other NH3 maser transitions coincided with specific 1.3 mm continuum sources. The arrangement of H2O maser spots in the vicinity of W51e2-E potentially indicates episodic accretions in this source. Combining the data from the Atacama Large Millimeter/submillimeter Array data archive for W51-North, W51e2, and W51e8, we have discovered that the H2O, NH3, and CH3OH masers, as well as the HC3N and SiO emissions are found to be good tools for tracing outflow in this work for W51A.

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A Possible Chemical Clock in High-mass Star-forming Regions: N(HC₃N)/N(N₂H⁺)?

Wang

Zhang

et al. 2023

ApJS

Self Cite

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We conducted observations of multiple HC3N (J = 10−9, 12−11, and 16−15) lines and the N2H+ (J = 1−0) line toward a large sample of 61 ultracompact (UC) H ii regions, through the Institut de Radioastronomie Millmétrique 30 m and the Arizona Radio Observatory 12 m telescopes. The N2H+ J = 1−0 line is detected in 60 sources and HC3N is detected in 59 sources, including 40 sources with three lines, 9 sources with two lines, and 10 sources with one line. Using the rotational diagram, the rotational temperature and column density of HC3N were estimated toward sources with at least two HC3N lines. For 10 sources with only one HC3N line, their parameters were estimated, taking one average value of T rot. For N2H+, we estimated the optical depth of the N2H+ J = 1−0 line, based on the line intensity ratio of its hyperfine structure lines. Then the excitation temperature and column density were calculated. When combining our results in UC H ii regions and previous observation results on high-mass starless cores, the N(HC3N)/N(N2H+) ratio clearly increases from the region stage. This means that the abundance ratio changes with the evolution of high-mass star-forming regions (HMSFRs). Moreover, positive correlations between the ratio and other evolutionary indicators (dust temperature, bolometric luminosity, and luminosity-to-mass ratio) are found. Thus we propose the ratio of N(HC3N)/N(N2H+) as a reliable chemical clock of HMSFRs.

show abstract

Cyanopolyyne line survey towards high-mass star-forming regions with TMRT

Cited by 3 publications

References 123 publications

A Possible Chemical Clock in High-mass Star-forming Regions: N(HC3N)/N(N2H+)?

A Possible Chemical Clock in High-mass Star-forming Regions: N(HC3N)/N(N2H+)?

Masers and Star Formation Activities in W51A

A Possible Chemical Clock in High-mass Star-forming Regions: N(HC₃N)/N(N₂H⁺)?

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