A PPMAP analysis of the filamentary structures in Ophiuchus L1688 and L1689

Howard, A D P, Whitworth, A P ORCID: https://orcid.org/0000-0002-1178-5486, Griffin, M J ORCID: https://orcid.org/0000-0002-0033-177X, Marsh, K A and Smith, M W L ORCID: https://orcid.org/0000-0002-3532-6970 2021. A PPMAP analysis of the filamentary structures in Ophiuchus L1688 and L1689. Monthly Notices of the Royal Astronomical Society 504 (4) , pp. 6157-6178. 10.1093/mnras/stab1166

PDF - Accepted Post-Print Version Download (20MB)

Abstract

We use the Point Process MAPping (PPMAP) algorithm to reanalyse the Herschel and SCUBA-2 observations of the L1688 and L1689 subregions of the Ophiuchus molecular cloud. PPMAP delivers maps with high resolution (here 14 arcsec, corresponding to ∼0.01pc at ∼140pc⁠), by using the observations at their native resolutions. PPMAP also delivers more accurate dust optical depths, by distinguishing dust of different types and at different temperatures. The filaments and pre-stellar cores almost all lie in regions with NH2≳7×1021cm−2 (corresponding to AV ≳ 7). The dust temperature, T, tends to be correlated with the dust opacity index, β, with low T and low β concentrated in the interiors of filaments. The one exception to this tendency is a section of filament in L1688 that falls – in projection – between the two B stars: S1 and HD147889; here T and β are relatively high, and there is compelling evidence that feedback from these two stars has heated and compressed the filament. Filament FWHMS are typically in the range 0.10 to 0.15pc⁠. Most filaments have line-densities in the range 25 to 65M⊙pc−1⁠. If their only support is thermal gas pressure, and the gas is at the canonical temperature of 10K⁠, the filaments are highly supercritical. However, there is some evidence from ammonia observations that the gas is significantly warmer than this, and we cannot rule out the possibility of additional support from turbulence and/or magnetic fields. On the basis of their spatial distribution, we argue that most of the starless cores are likely to disperse (rather than evolving to become pre-stellar).

Item Type:	Article
Date Type:	Publication
Status:	Published
Schools:	Advanced Research Computing @ Cardiff (ARCCA) Physics and Astronomy
Publisher:	Royal Astronomical Society
ISSN:	0035-8711
Funders:	STFC
Date of First Compliant Deposit:	1 July 2021
Date of Acceptance:	31 March 2021
Last Modified:	18 Jun 2024 16:24
URI:	https://orca.cardiff.ac.uk/id/eprint/142325

Citation Data

Cited 3 times in Scopus. View in Scopus. Powered By Scopus® Data

Actions (repository staff only)

Edit Item