An ammonia spectral map of the L1495-B218 filaments in the taurus molecular cloud. II. CCS and HC 7 N chemistry and three modes of star formation in the filaments

Young Min Seo, Liton Majumdar, Paul F. Goldsmith, Yancy L. Shirley, Karen Willacy, Derek Ward-Thompson, Rachel Friesen, David Frayer, Sarah E. Church, Dongwoo Chung, Kieran Cleary, Nichol Cunningham, Kiruthika Devaraj, Dennis Egan, Todd Gaier, Rohit Gawande, Joshua O. Gundersen, Andrew I. Harris, Pekka Kangaslahti, Anthony C.S. ReadheadLorene Samoska, Matthew Sieth, Michael Stennes, Patricia Voll, Steve White

Research output: Contribution to journalArticle

4 Citations (Scopus)

Abstract

We present deep CCS and HC 7 N observations of the L1495-B218 filaments in the Taurus molecular cloud obtained using the K-band focal plane array on the 100 m Green Bank Telescope. We observed the L1495-B218 filaments in CCS J N = 2 1 -1 0 and HC 7 N J = 21-20 with a spectral resolution of 0.038 km s -1 and an angular resolution of 31″. We observed strong CCS emission in both evolved and young regions and weak emission in two evolved regions. HC 7 N emission is observed only in L1495A-N and L1521D. We find that CCS and HC 7 N intensity peaks do not coincide with NH 3 or dust continuum intensity peaks. We also find that the fractional abundance of CCS does not show a clear correlation with the dynamical evolutionary stage of dense cores. Our findings and chemical modeling indicate that the fractional abundances of CCS and HC 7 N are sensitive to the initial gas-phase C/O ratio, and they are good tracers of young condensed gas only when the initial C/O is close to solar value. Kinematic analysis using multiple lines, including NH 3 , HC 7 N, CCS, CO, HCN, and HCO + , suggests that there may be three different star formation modes in the L1495-B218 filaments. At the hub of the filaments, L1495A/B7N has formed a stellar cluster with large-scale inward flows (fast mode), whereas L1521D, a core embedded in a filament, is slowly contracting because of its self-gravity (slow mode). There is also one isolated core that appears to be marginally stable and may undergo quasi-static evolution (isolated mode).

Original languageEnglish (US)
Article number134
JournalAstrophysical Journal
Volume871
Issue number2
DOIs
StatePublished - Feb 1 2019

Fingerprint

molecular clouds
star formation
ammonia
filaments
chemistry
spectral resolution
gas
kinematics
tracer
hubs
gravity
dust
focal plane devices
extremely high frequencies
angular resolution
tracers
modeling
telescopes
vapor phases
gravitation

Keywords

  • ISM: Clouds
  • ISM: Molecules
  • radio lines: ISM
  • stars: Formation
  • surveys

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

An ammonia spectral map of the L1495-B218 filaments in the taurus molecular cloud. II. CCS and HC 7 N chemistry and three modes of star formation in the filaments . / Seo, Young Min; Majumdar, Liton; Goldsmith, Paul F.; Shirley, Yancy L.; Willacy, Karen; Ward-Thompson, Derek; Friesen, Rachel; Frayer, David; Church, Sarah E.; Chung, Dongwoo; Cleary, Kieran; Cunningham, Nichol; Devaraj, Kiruthika; Egan, Dennis; Gaier, Todd; Gawande, Rohit; Gundersen, Joshua O.; Harris, Andrew I.; Kangaslahti, Pekka; Readhead, Anthony C.S.; Samoska, Lorene; Sieth, Matthew; Stennes, Michael; Voll, Patricia; White, Steve.

In: Astrophysical Journal, Vol. 871, No. 2, 134, 01.02.2019.

Research output: Contribution to journalArticle

Seo, YM, Majumdar, L, Goldsmith, PF, Shirley, YL, Willacy, K, Ward-Thompson, D, Friesen, R, Frayer, D, Church, SE, Chung, D, Cleary, K, Cunningham, N, Devaraj, K, Egan, D, Gaier, T, Gawande, R, Gundersen, JO, Harris, AI, Kangaslahti, P, Readhead, ACS, Samoska, L, Sieth, M, Stennes, M, Voll, P & White, S 2019, ' An ammonia spectral map of the L1495-B218 filaments in the taurus molecular cloud. II. CCS and HC 7 N chemistry and three modes of star formation in the filaments ', Astrophysical Journal, vol. 871, no. 2, 134. https://doi.org/10.3847/1538-4357/aaf887
Seo, Young Min ; Majumdar, Liton ; Goldsmith, Paul F. ; Shirley, Yancy L. ; Willacy, Karen ; Ward-Thompson, Derek ; Friesen, Rachel ; Frayer, David ; Church, Sarah E. ; Chung, Dongwoo ; Cleary, Kieran ; Cunningham, Nichol ; Devaraj, Kiruthika ; Egan, Dennis ; Gaier, Todd ; Gawande, Rohit ; Gundersen, Joshua O. ; Harris, Andrew I. ; Kangaslahti, Pekka ; Readhead, Anthony C.S. ; Samoska, Lorene ; Sieth, Matthew ; Stennes, Michael ; Voll, Patricia ; White, Steve. / An ammonia spectral map of the L1495-B218 filaments in the taurus molecular cloud. II. CCS and HC 7 N chemistry and three modes of star formation in the filaments In: Astrophysical Journal. 2019 ; Vol. 871, No. 2.
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T1 - An ammonia spectral map of the L1495-B218 filaments in the taurus molecular cloud. II. CCS and HC 7 N chemistry and three modes of star formation in the filaments

AU - Seo, Young Min

AU - Majumdar, Liton

AU - Goldsmith, Paul F.

AU - Shirley, Yancy L.

AU - Willacy, Karen

AU - Ward-Thompson, Derek

AU - Friesen, Rachel

AU - Frayer, David

AU - Church, Sarah E.

AU - Chung, Dongwoo

AU - Cleary, Kieran

AU - Cunningham, Nichol

AU - Devaraj, Kiruthika

AU - Egan, Dennis

AU - Gaier, Todd

AU - Gawande, Rohit

AU - Gundersen, Joshua O.

AU - Harris, Andrew I.

AU - Kangaslahti, Pekka

AU - Readhead, Anthony C.S.

AU - Samoska, Lorene

AU - Sieth, Matthew

AU - Stennes, Michael

AU - Voll, Patricia

AU - White, Steve

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N2 - We present deep CCS and HC 7 N observations of the L1495-B218 filaments in the Taurus molecular cloud obtained using the K-band focal plane array on the 100 m Green Bank Telescope. We observed the L1495-B218 filaments in CCS J N = 2 1 -1 0 and HC 7 N J = 21-20 with a spectral resolution of 0.038 km s -1 and an angular resolution of 31″. We observed strong CCS emission in both evolved and young regions and weak emission in two evolved regions. HC 7 N emission is observed only in L1495A-N and L1521D. We find that CCS and HC 7 N intensity peaks do not coincide with NH 3 or dust continuum intensity peaks. We also find that the fractional abundance of CCS does not show a clear correlation with the dynamical evolutionary stage of dense cores. Our findings and chemical modeling indicate that the fractional abundances of CCS and HC 7 N are sensitive to the initial gas-phase C/O ratio, and they are good tracers of young condensed gas only when the initial C/O is close to solar value. Kinematic analysis using multiple lines, including NH 3 , HC 7 N, CCS, CO, HCN, and HCO + , suggests that there may be three different star formation modes in the L1495-B218 filaments. At the hub of the filaments, L1495A/B7N has formed a stellar cluster with large-scale inward flows (fast mode), whereas L1521D, a core embedded in a filament, is slowly contracting because of its self-gravity (slow mode). There is also one isolated core that appears to be marginally stable and may undergo quasi-static evolution (isolated mode).

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KW - ISM: Clouds

KW - ISM: Molecules

KW - radio lines: ISM

KW - stars: Formation

KW - surveys

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