Hipparcos distance estimates of the Ophiuchus and the Lupus cloud complexes

By Marco Lombardi, C. Lada, Joao F. Alves. 2008

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We combine extinction maps from the Two Micron All Sky Survey (2MASS) with Hipparcos and Tycho parallaxes to obtain reliable and high-precision estimates of the distance to the Ophiuchus and Lupus dark complexes. Our analysis, based on a rigorous maximumlikelihood approach, shows that the ρ-Ophiuchi cloud is located at (119 ± 6) pc and the Lupus complex is located at (155 ± 8) pc; in addition, we are able to put constraints on the thickness of the clouds and on their orientation on the sky (both these effects are not included in the error estimate quoted above). For Ophiuchus, we find some evidence that the streamers are closer to us than the core. The method applied in this paper is currently limited to nearby molecular clouds, but it will find many natural applications in the GAIA-era, when it will be possible to pin down the distance and three-dimensional structure of virtually every molecular cloud in the Galaxy.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/3da58dfe74b1758dc32aef5d90f85ac23e221ec9

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Citations in the corpus

• BANYAN. XI. The BANYAN Σ Multivariate Bayesian Algorithm to Identify Members of Young Associations with 150 pc (2018, background): “BANYAN Σ in- 1 The Lupus star-forming region is slightly above this limit at ∼ 155 pc (Lombardi et al. 2008), and the distance of the Chamaeleon star-forming region has recently been revised above 150 pc; (Voirin et al. 2017) THE BANYAN Σ ALGORITHM TO IDENTIFY YOUNG ASSOCIATION MEMBERS 3 cludes a…”
• Dust grain growth in ρ-Ophiuchi protoplanetary disks (2010, background): “…the outer disk structure; adopting for all the YSOs in our sample the current estimate of ∼130 pc for the distance to the ρ-Oph star forming region (Wilking et al. 2008; Lombardi et al. 2008), the range in projected phyical separation translates into a range in angular separation of ∼0.05−4′′.”
• Mapping the Shores of the Brown Dwarf Desert. I. Upper Scorpius (2007, background): “However, more recent studies have measured the distance to be between 119-135 pc (de Geus et al. 1989; Lombardi et al. 2008; Mamajek 2008).”
• ON THE STAR FORMATION RATES IN MOLECULAR CLOUDS (2010, methodology): “These are the Pipe Nebula (Lombardi et al. 2006), the Ophiuchus cloud and the Lupus cloud complex (Lombardi et al. 2008), the Taurus, Perseus and California clouds (Lombardi et al 2010; Lada et al. 2009), the RCrA cloud (Alves, Lombardi & Lada 2010, in preparation) and the Orion cloud complex…”
• PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS. II. EXTENSION TO FAINTER SOURCES (2010, background): “Each high angular resolution map covers 4′′ on a side, corresponding to 500AU at the adopted distance of 125 pc to the Ophiuchus clouds (de Geus et al. 1989; Knude & Høg 1998; Lombardi et al. 2008; Loinard et al. 2008).”
• PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS (2009, background): “Each 1See http://cfa-www.harvard.edu/∼cqi/mircook.html. high angular resolution map covers 4′′ on a side, corresponding to 500 AU at the adopted distance of 125 pc to the Ophiuchus clouds (de Geus et al. 1989; Knude & Høg 1998; Lombardi et al. 2008; Loinard et al. 2008).”
• THE SPITZER c2d LEGACY RESULTS: STAR-FORMATION RATES AND EFFICIENCIES; EVOLUTION AND LIFETIMES (2008, methodology): “Lombardi et al. (2008) also derived a distance to the Lupus complex of 155± 8 pc, with some evidence that individual Lupus clouds were at different distances, both consistent with our assumed values of 150± 20 pc for Lupus I and IV and 200 ± 20 pc for Lupus III.”
• A LARGE CATALOG OF ACCURATE DISTANCES TO MOLECULAR CLOUDS FROM PS1 PHOTOMETRY (2014, result): “This well-studied cloud is believed to reside at a distance of 119 pc (Lombardi et al. 2008), consistent with our measurement.”
• Probing the evolution of molecular cloud structure: From quiescence to birth (2009, background): “Molecular cloud properties and the derived parameters Cloud Da MH2 × 104 AV σdata σ f it NYSOb Star-forming clouds, physical resolution 0.1 pc Ophiuchus 1191 0.6 2 4.3 0.48c 300 Taurus 1402 0.81 1.8 1.5 0.49 300 Serpens 2593 3.6 3 2.4 0.51 300 Cha I 1654 0.23 1.3 1.3 0.35 200 Cha II 1504 0.15 1.3 1.”
• RESOLVED IMAGES OF LARGE CAVITIES IN PROTOPLANETARY TRANSITION DISKS (2011, background): “This young star with spectral type G3 is still embedded in the L1688 dark cloud in the nearby Ophiuchus star-forming region, d ≈ 125pc (e.g., Lombardi et al. 2008; Loinard et al. 2008).”
• LARGE-SCALE ASYMMETRIES IN THE TRANSITIONAL DISKS OF SAO 206462 AND SR 21 (2014, unknown): “SR 21 is a young G3 star (2.5M ) in the ρ-Ophiuchus star forming region at a distance of 119 pc (Lombardi et al. 2008).”