Histogram of oriented gradients: a technique for the study of molecular cloud formation

J. D. Soler; H. Beuther; M. Rugel; Y. Wang; P. C. Clark; S. C. O. Glover; P. F. Goldsmith; M. Heyer; L. D. Anderson; A. Goodman; Th. Henning; J. Kainulainen; R. S. Klessen; S. N. Longmore; N. M. McClure-Griffiths; K. M. Menten; J. C. Mottram; J. Ott; S. E. Ragan; R. J. Smith; J. S. Urquhart; F. Bigiel; P. Hennebelle; N. Roy; P. Schilke

doi:10.1051/0004-6361/201834300

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Volume 622 (February 2019)

A&A, 622 (2019) A166

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Fig. 8

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Longitude–velocity (LV) diagrams of the HI emission (from THOR, left panel) and ¹³CO emission (from GRS, right panel) toward the region presented in Fig. 7. In the HI LV diagram, the shadow around 0 ≤ v_LSR ≤ 45 km s⁻¹ and the vertical line around 0 ≤ v_LSR ≤ 75 km s⁻¹ correspond to absorption toward the supernova remnant (SNR) G34.7-0.4 (W44) and the HII region G34.256+0.146, respectively.

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