The Distribution of Thermal Pressures in the Interstellar Medium from a Survey of C I Fine-Structure Excitation

By E. Jenkins, T. Tripp. 2001

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We used the Space Telescope Imaging Spectrograph (STIS) with its smallest entrance aperture (0.″03 wide slit) and highest resolution echelle gratings (E140H and E230H) to record the interstellar absorption features for 10 different multiplets of neutral carbon at a resolving power of λ/Δλ = 200,000 in the UV spectra of 21 early-type stars. Our objective was to measure the amount of C I in each of its three fine-structure levels of the ground electronic state, so that we could determine the thermal pressures in the absorbing gas and how much they vary in different regions. Our observations are principally along directions out to several kiloparsecs in the Galactic plane near longitudes l = 120° and 300°, with the more distant stars penetrating nearby portions of the Perseus and Sagittarius-Carina arms of the Galaxy. We devised a special analysis technique to decipher the overlapping absorption features in the different multiplets, each with different arrangements of the closely spaced transitions. In order to derive internally consistent results for all multiplets, we found that we had to modify the relative transition f-values in a way that made generally weak transitions stronger than amounts indicated in the current literature. We compared our measured relative populations of the excited fine-structure levels to those expected from equilibria calculated with collisional rate constants for various densities, temperatures, and compositions. The median thermal pressure for our entire sample was p/k = 2240 cm-3 K, or slightly higher if the representative temperatures of the material are much above or below a most favorable temperature of 40 K for the excitation of the first excited level at a given pressure. For gas that is moving outside the range of radial velocities permitted by differential Galactic rotation between us and the targets, about 15% of the C I indicates a thermal pressure p/k > 5000 cm-3 K. For gas within the allowed velocities, this fraction is only 1.5%. This contrast reveals a relationship between pressure enhancements and the kinematics of the gas. Regardless of velocity, we usually can register the presence of a very small proportion of the gas that seems to be at p/k ≳ 105 cm-3 K. We interpret these ubiquitous wisps of high-pressure material to arise either from small-scale density enhancements created by converging flows in a turbulent medium or from warm turbulent boundary layers on the surfaces of dense clouds moving through an intercloud medium. For turbulent compression, our C I excitations indicate that the barytropic index γeff ≳ 0.90 must apply if the unperturbed gas starts out with representative densities and temperatures n = 10 cm-3 and T = 100 K. This value for γeff is larger than that expected for interstellar material that remains in thermal equilibrium after it is compressed from the same initial n and T. However, if regions of enhanced pressure reach a size smaller than ∼0.01 pc, the dynamical time starts to become shorter than the cooling time, and γeff should start to approach the adiabatic value cp/cv = 5/3. Some of the excited C I may arise from the target stars' H II regions or by the effects of optical pumping from the submillimeter line radiation emitted by them. We argue that these contributions are small, and our comparisons of the velocities of strongly excited C I to those of excited Si II seem to support this outlook. For six stars in the survey, absorption features from interstellar excited O I could be detected at velocities slightly shifted from the persistent features of telluric origin. These O I* and O I** features were especially strong in the spectra of HD 93843 and HD 210839, the same stars that show exceptionally large C I excitations. In appendices of this paper, we present evidence that (1) the wavelength resolving power of STIS in the E14OH mode is indeed about 200,000, and (2) the telluric O I* and O I** features exhibit some evidence for macroscopic motions, since their broadenings are in excess of that expected for thermal Doppler broadening at an exospheric temperature T = 1000 K.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4fbc2c359dfcca1a1391aa10c10d1f8594908453

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Citations in the corpus

Neutral Atomic Phases of the Interstellar Medium in the Galaxy (2003, methodology): “The calculated range in two-phase (CNM+WNM) thermal pressures over the column densities from Ncl ¼ 3 1018 to 1 1020 cm 2 is in reasonably good agreement with the thermal pressures of P=k ¼ 103 104 K cm 3 that are observed in the local ISM (Jenkins et al. 1983; Jenkins & Tripp 2001).”
The evolution of the cosmic microwave background temperature Measurements of TCMB at high redshift from carbon monoxide excitation (2010, background): “For example, the accuracy of the oscillator strengths of C0 fine-structure levels (e.g. Jenkins & Tripp, 2001; Morton, 2003) is subject to discussions.”
The Millennium Arecibo 21 Centimeter Absorption-Line Survey. IV. Statistics of Magnetic Field, Column Density, and Turbulence (2005, background): “PCNM is from Jenkins & Tripp (2001) and Wolfire et al. (2003).”
THE THREE-PHASE INTERSTELLAR MEDIUM REVISITED (2005, result): “This is comfortingly similar to the range of most observations reported by Jenkins & Tripp (2001).”
Atomic Data for Resonance Absorption Lines. III. Wavelengths Longward of the Lyman Limit for the Elements Hydrogen to Gallium (2003, background): “C i: Additional experimental data are needed to check whether the astrophysical results of Jenkins & Tripp (2001) are more reliable than the theoretical values adopted here.”
REGULATION OF STAR FORMATION RATES IN MULTIPHASE GALACTIC DISKS: A THERMAL/DYNAMICAL EQUILIBRIUM MODEL (2010, background): “For these fiducial parameters, and taking midplane thermal pressure Pth,0/k ∼ 3000 K cm−3 (see Jenkins & Tripp 2001 and Wolfire et al. 2003), ρsd = 0.05 M⊙ pc −3 (Holmberg & Flynn 2000), and ΣGBC <∼ 2 M⊙ pc−2 (Dame et al. 1987, 2001; Bronfman et al. 1988; Luna et al. 2006; Nakanishi & Sofue 2006)…”
The VLT-UVES survey for molecular hydrogen in high-redshift damped Lyman α systems: physical conditions in the neutral gas (2005, methodology): “In the Galactic ISM, fine-structure excitation of C I has been used to study the distribution of thermal pressure (see Jenkins & Tripp 2001).”
Molecular Cloud Evolution. I. Molecular Cloud and Thin Cold Neutral Medium Sheet Formation (2005, background): “As is well known (Field, Goldsmith & Habing 1969), at the mean midplane thermal pressure of the ISM (∼ 2250 K cm−3 or sightly higher, Jenkins & Tripp 2001), the atomic medium is thermally bistable.”
A High-Resolution Survey of Low-Redshift QSO Absorption Lines: Statistics and Physical Conditions of O VI Absorbers (2007, background): “Evidence of wavelength calibration problems have also been noted when comparing lines that should have identical component structure (e.g., Jenkins & Tripp 2001; Tripp et al. 2005).”
A Far Ultraviolet Spectroscopic Explorer Survey of Interstellar Molecular Hydrogen in Translucent Clouds (2002, background): “Based on the strong CH (and CH+) absorption seen by Crane, Lambert, & Sheffer (1995) at the same velocity as the blue components of C i and O i seen by Jenkins & Tripp (2001), we assume that all the observed H2 is also associated with this component.”
Probing the Interstellar Medium near Star-forming Regions with Gamma-Ray Burst Afterglow Spectroscopy: Gas, Metals, and Dust (2007, background): “In cold and dense regions, however, the recombination rate (proportional to the electron and carbon densities) is sufficiently large that cold clouds frequently show detectable absorption from C I transitions (e.g. Jenkins & Tripp 2001).”
Molecular Cloud Formation behind Shock Waves (2004, background): “First the Jenkins & Tripp (2001) results suggest an abundance of weak shocks are active in the galactic ISM.”
HERSCHEL SURVEY OF GALACTIC OH+, H2O+, AND H3O+: PROBING THE MOLECULAR HYDROGEN FRACTION AND COSMIC-RAY IONIZATION RATE (2014, methodology): “Excitation of the fine-structure levels of O i has been used to find nH ≈ 5–25 cm−3 in diffuse gas (Sonnentrucker et al. 2002, 2003), while excitation of C i has been used to determine thermal pressures that are consistent with nH ≈ 10–100 cm−3 (Jenkins & Tripp 2001, 2011).”