Gas and dust in the pre-main-sequence multiple system GG Tauri

David W Koerner, A. I. Sargent, S. V W Beckwith

Research output: Contribution to journalArticle

29 Citations (Scopus)

Abstract

We present 1.4 and 2.7 mm aperture synthesis maps of the gas and dust continuum emission around GG Tauri, a very young component of a pre-main-sequence multiple star system; both GG Tau and its apparent companion, GG Tau/c, at 1500 AU separation, are themselves binaries. At 1.4 mm, dust continuum emission ∼750 AU in extent is associated with GG Tau, and a secondary peak is near GG Tau/c. Spectral line images in the (1→0) and (2→1) transitions of 13CO reveal gaseous structure around GG Tau, elongated along the GG Tau-GG Tau/c axis (P.A. ≈ 184°). There is some suggestion that the gas associated with GG Tau/c alone is extended in a different direction (P.A. ∼ 90°-135°). Marked changes in the morphology and velocity structure of the molecular emission near GG Tau/c also indicate that this system is differently oriented. Clumps between the two systems may be vestiges of a connecting bar. GG Tau and GG Tau/c appear to have originated in a common cloud; their different systemic orientations suggest that they formed from an initially prolate cloud rather than from an extensive (≥ 1500 AU), highly flattened disk.

Original languageEnglish (US)
JournalAstrophysical Journal
Volume408
Issue number2 PART 2
StatePublished - May 10 1993
Externally publishedYes

Fingerprint

dust
gases
gas
continuums
clumps
velocity structure
suggestion
line spectra
apertures
stars
synthesis
young

Keywords

  • Binaries: general
  • Binaries: visual
  • Circumstellar matter
  • Planetary systems
  • Stars: formation
  • Stars: individual (GG Tauri)

ASJC Scopus subject areas

  • Space and Planetary Science

Cite this

Koerner, D. W., Sargent, A. I., & Beckwith, S. V. W. (1993). Gas and dust in the pre-main-sequence multiple system GG Tauri. Astrophysical Journal, 408(2 PART 2).

Gas and dust in the pre-main-sequence multiple system GG Tauri. / Koerner, David W; Sargent, A. I.; Beckwith, S. V W.

In: Astrophysical Journal, Vol. 408, No. 2 PART 2, 10.05.1993.

Research output: Contribution to journalArticle

Koerner, DW, Sargent, AI & Beckwith, SVW 1993, 'Gas and dust in the pre-main-sequence multiple system GG Tauri', Astrophysical Journal, vol. 408, no. 2 PART 2.
Koerner, David W ; Sargent, A. I. ; Beckwith, S. V W. / Gas and dust in the pre-main-sequence multiple system GG Tauri. In: Astrophysical Journal. 1993 ; Vol. 408, No. 2 PART 2.
@article{63a7b7f883ef4a02b7a8a029afe7828b,
title = "Gas and dust in the pre-main-sequence multiple system GG Tauri",
abstract = "We present 1.4 and 2.7 mm aperture synthesis maps of the gas and dust continuum emission around GG Tauri, a very young component of a pre-main-sequence multiple star system; both GG Tau and its apparent companion, GG Tau/c, at 1500 AU separation, are themselves binaries. At 1.4 mm, dust continuum emission ∼750 AU in extent is associated with GG Tau, and a secondary peak is near GG Tau/c. Spectral line images in the (1→0) and (2→1) transitions of 13CO reveal gaseous structure around GG Tau, elongated along the GG Tau-GG Tau/c axis (P.A. ≈ 184°). There is some suggestion that the gas associated with GG Tau/c alone is extended in a different direction (P.A. ∼ 90°-135°). Marked changes in the morphology and velocity structure of the molecular emission near GG Tau/c also indicate that this system is differently oriented. Clumps between the two systems may be vestiges of a connecting bar. GG Tau and GG Tau/c appear to have originated in a common cloud; their different systemic orientations suggest that they formed from an initially prolate cloud rather than from an extensive (≥ 1500 AU), highly flattened disk.",
keywords = "Binaries: general, Binaries: visual, Circumstellar matter, Planetary systems, Stars: formation, Stars: individual (GG Tauri)",
author = "Koerner, {David W} and Sargent, {A. I.} and Beckwith, {S. V W}",
year = "1993",
month = "5",
day = "10",
language = "English (US)",
volume = "408",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "2 PART 2",

}

TY - JOUR

T1 - Gas and dust in the pre-main-sequence multiple system GG Tauri

AU - Koerner, David W

AU - Sargent, A. I.

AU - Beckwith, S. V W

PY - 1993/5/10

Y1 - 1993/5/10

N2 - We present 1.4 and 2.7 mm aperture synthesis maps of the gas and dust continuum emission around GG Tauri, a very young component of a pre-main-sequence multiple star system; both GG Tau and its apparent companion, GG Tau/c, at 1500 AU separation, are themselves binaries. At 1.4 mm, dust continuum emission ∼750 AU in extent is associated with GG Tau, and a secondary peak is near GG Tau/c. Spectral line images in the (1→0) and (2→1) transitions of 13CO reveal gaseous structure around GG Tau, elongated along the GG Tau-GG Tau/c axis (P.A. ≈ 184°). There is some suggestion that the gas associated with GG Tau/c alone is extended in a different direction (P.A. ∼ 90°-135°). Marked changes in the morphology and velocity structure of the molecular emission near GG Tau/c also indicate that this system is differently oriented. Clumps between the two systems may be vestiges of a connecting bar. GG Tau and GG Tau/c appear to have originated in a common cloud; their different systemic orientations suggest that they formed from an initially prolate cloud rather than from an extensive (≥ 1500 AU), highly flattened disk.

AB - We present 1.4 and 2.7 mm aperture synthesis maps of the gas and dust continuum emission around GG Tauri, a very young component of a pre-main-sequence multiple star system; both GG Tau and its apparent companion, GG Tau/c, at 1500 AU separation, are themselves binaries. At 1.4 mm, dust continuum emission ∼750 AU in extent is associated with GG Tau, and a secondary peak is near GG Tau/c. Spectral line images in the (1→0) and (2→1) transitions of 13CO reveal gaseous structure around GG Tau, elongated along the GG Tau-GG Tau/c axis (P.A. ≈ 184°). There is some suggestion that the gas associated with GG Tau/c alone is extended in a different direction (P.A. ∼ 90°-135°). Marked changes in the morphology and velocity structure of the molecular emission near GG Tau/c also indicate that this system is differently oriented. Clumps between the two systems may be vestiges of a connecting bar. GG Tau and GG Tau/c appear to have originated in a common cloud; their different systemic orientations suggest that they formed from an initially prolate cloud rather than from an extensive (≥ 1500 AU), highly flattened disk.

KW - Binaries: general

KW - Binaries: visual

KW - Circumstellar matter

KW - Planetary systems

KW - Stars: formation

KW - Stars: individual (GG Tauri)

UR - http://www.scopus.com/inward/record.url?scp=12044251860&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=12044251860&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:12044251860

VL - 408

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 2 PART 2

ER -