Statistical Properties of Molecular Clouds in the Galactic Center

By T. Oka, T. Hasegawa, F. Sato, M. Tsuboi, A. Miyazaki, M. Sugimoto. 2001

152 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/c4e65fddc480a2f977bd85d07849b97140bfaa4b

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In Astronomy and Astrophysics

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Citations in the corpus

• Cloud-scale Molecular Gas Properties in 15 Nearby Galaxies (2018, background): “In contrast, clouds situated in regions with low gas density (e.g., the outer Galaxy; Heyer et al. 2001) or high ambient pressure (e.g., the Galactic Center; Oka et al. 2001) tend to show much higher velocity dispersions than expected for self-virialized clouds.”
• Variations in the Galactic star formation rate and density thresholds for star formation (2012, methodology): “We have usedH = 20pc assuming hydrostatic equilibrium (H/R = vT /vc); the circular velocity vc ≈ 100kms−1 while the turbulent velocityvT ≡ √ 8 ln 2σv = 20kms−1 (Oka et al. 2001).”
• What controls star formation in the central 500 pc of the Galaxy (2013, background): “The threshold density depends onσ andκ, both of which increase towards the Galactic centre (e.g. Morris & Serabyn 1996; Oka et al. 2001; Longmore et al. 2013a; Shetty et al. 2012), and hence it is possible that gravitational stability inhibits star formation in the CMZ.”
• The CO-to-H2 Conversion Factor (2013, methodology): “Based on observations of the Galactic center (Oka et al. 2001) and starburst galaxies (e.g., Rosolowsky & Blitz 2005), ΣGMC likely does vary with environment.”
• Molecular Clouds in the Milky Way (2015, methodology): “The set of Galactic Center cloud points are parallel to Equation 2 but are vertically displaced, corresponding to αvir between 3 and 10.”
• PHYSICAL PROPERTIES OF MOLECULAR CLOUDS FOR THE ENTIRE MILKY WAY DISK (2016, methodology): “This is compatible with the analysis of Oka et al. (2001), who found that the σv−R relation in the Galactic center area (Rgal < 3 kpc) has a significantly larger normalization than that found at larger Galactic radii.”
• MOLECULAR GAS AND STAR FORMATION IN NEARBY DISK GALAXIES (2013, background): “Sample and Galaxy Properties We present measurements for galaxies meeting the following criteria: 1) a HERACLES CO map containing a clear CO detection (S/N> 5 over a significant area and multiple channels), 2) Spitzer data at 24µm, and 3) inclination .”
• Massive Perturber-driven Interactions between Stars and a Massive Black Hole (2006, background): “…PERTURBERS IN THEGALACTIC CENTER MP type ra (pc) Np Mp (M⊙) β (µ, σ) 〈 M2p 〉1/2 (M⊙) Rp (pc) References Observed GMCs <100 ~100 104 − 108 1.2 3× 106 −3× 107 5 Oka et al. (2001); Güsten & Philipp (2004) Observed clusters<100 ~10 102 − 105 1.3 (8.2, 1.1) 4.8 × 103 − 2.4×104 1 Figer et al.…”
• The Resolved Properties of Extragalactic Giant Molecular Clouds (2008, background): “Finally, Oka et al. (2001) measured the GMC properties near the Galactic Center, finding that those clouds have line widths a factor of 3 to 5 times larger than similar clouds in the disk and suggesting that this is due to the large pressure in this region.”