A Far Ultraviolet Spectroscopic Explorer Survey of Interstellar Molecular Hydrogen in Translucent Clouds

By B. Rachford, T. Snow, Jason Tumlinson, J. Michael Shull, W. Blair, R. Ferlet, S. Friedman, C. Gry, E. Jenkins, D. Morton and 5 more. 2002

234 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/f9f5dc51f89b7779e6cf1e453ce7fc45c5959374

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Citations in the corpus

Neutral Atomic Phases of the Interstellar Medium in the Galaxy (2003, unknown): “Early estimates of the gas temperature from Copernicus observations found T01 ¼ 77 17 K (Savage et al. 1977), while recent estimates using the Far Ultraviolet Spectroscopic Explorer report T01 ¼ 68 15K (Rachford et al. 2002).”
THE ATOMIC-TO-MOLECULAR TRANSITION IN GALAXIES. II: H i AND H2 COLUMN DENSITIES (2008, methodology): “Savage et al. (1977) and Bohlin et al. (1978) (for Copernicus) and Rachford et al. (2002, 2008) (for FUSE ) report measurements of the molecular hydrogen columns in the Milky Way disk for lines of sight at low galactic latitude (b <∼ 10 ◦), using stars as background sources.”
Interstellar Carbon in Translucent Sight Lines (2004, background): “Rachford et al. (2002) argue that the HD 24534 sight line does not likely contain a translucent cloud, and at most could be composed of 50% translucent cloud material.”
Ultraviolet Survey of CO and H2 in Diffuse Molecular Clouds: The Reflection of Two Photochemistry Regimes in Abundance Relationships (2008, background): “Figure 2 presents a sample of two FUSE sight lines with H2 absorption profiles that differ by a factor of 13 in N(H2).”
THE DARK MOLECULAR GAS (2010, unknown): “…1021 cm−2 ≡ N̄ N0 = 5.26N̄22Z ′, (3) where N0 = 1.9 × 1021Z ′−1 cm−2 is the radial column density corresponding to a visual extinction of unity (Bohlin et al. 1978; Rachford et al. 2002), N̄22 ≡ N̄/(1022 cm−2), Z ′ ≡ Z/Z⊙ is the metallicity relative to solar, and assuming that the gas to dust…”
STUDIES OF DIFFUSE INTERSTELLAR BANDS V. PAIRWISE CORRELATIONS OF EIGHT STRONG DIBs AND NEUTRAL HYDROGEN, MOLECULAR HYDROGEN, AND COLOR EXCESS (2010, methodology): “We therefore use the – 7 – results of our original, homogeneous data analysis, as presented by Rachford et al. (2002).”
The global dust SED: tracing the nature and evolution of dust with DustEM (2010, methodology): “Here we use the standard value of 5.8 × 1021 cm−2 mag−1 also found by Rachford et al. (2002) towards “translucent lines of sight” (fH2 ∼ 0.5, 1<∼ AV <∼ 3).”
Calibration of X-ray absorption in our Galaxy (2013, background): “Most of the FUSE observations of bright sources reported by Rachford et al. (2002, 2009) are close to the X-ray profile indicating that when the signal to noise and sensitivity are good all the molecular hydrogen can be detected in UV absorption.”
INVESTIGATING THE COSMIC-RAY IONIZATION RATE IN THE GALACTIC DIFFUSE INTERSTELLAR MEDIUM THROUGH OBSERVATIONS OF H+3 (2011, background): “Absorption lines from electronic transitions of H2 have been observed in the UV along many of the sight lines in this study (from which the aforementioned values of T01 are derived; Savage et al. 1977; Rachford et al. 2002, 2009).”
A Herschel [C ii] Galactic plane survey - I. The global distribution of ISM gas components (2013, background): “We assume a constant kinetic temperature of T H2kin = 70 K, following the results from Rachford et al. (2002), and a corresponding Rul = 4.3×10−10 s−1 cm−3 (Flower & Launay 1977) for collisions with H2.”
The initial conditions of stellar protocluster formation - I. A catalogue of Spitzer dark clouds (2009, methodology): “To convert to the molecular hydrogen column density,NH2 we adopt Av = 10−21× NH2 (6) from Bohlin et al. (1978), although the more recent work by Draine (2003), based on the observations of Rachford et al. (2002), suggests a 50% larger column density per magnitude of extinction.”
Diffuse Atomic and Molecular Clouds (2006, background): “…3 R 4 R 0 P 5 R 5 P 4 R 5 P 4 Figure 2 (Top) Spectrum of H2 obtained with Far Ultraviolet Spectroscopic Explorer (FUSE) and model fit in red (adapted from Rachford et al. 2002); (bottom) spectrum of H3+ (adapted from McCall et al. 2002). et al. (2001) found a rich spectrum of absorption lines from…”
The Far-Ultraviolet Spectra of TW Hydrae. II. Models of H2 Fluorescence in a Disk (2004, background): “However, the low molecular fraction towards TWHya is consistent with a low extinction (Savage et al. 1977; Rachford et al. 2002), and is not consistent with material found towards star-forming regions.”
A Model for Atomic and Molecular Interstellar Gas: The Meudon PDR Code (2006, methodology): “T01 versus TK The temperature T01, which is often used as a measure of the kinetic temperature (cf. Rachford et al. 2002), is defined as T01 ¼ 170:5= ln N (H2; J ¼ 1) 9N (H2; J ¼ 0) : We check this assumption by plotting on Figure 13 the calculated T01 as a function of themean kinetic temperature…”
An Analysis of the Shapes of Interstellar Extinction Curves. V. The IR-through-UV Curve Morphology (2007, background): “We note that Rachford et al. (2002) have found positive trends of bump width and far-UV curvature with the fraction of hydrogen atoms in the form H2.”
Planck 2013 results. XI. All-sky model of thermal dust emission (2013, background): “We also note again that this column density is below that for which significant H2 is seen in the diffuse ISM (Gillmon et al. 2006; Wakker 2006; Rachford et al. 2002, 2009).”