Interstellar Extinction and Polarization in the Taurus Dark Clouds: The Optical Properties of Dust near the Diffuse/Dense Cloud Interface

By D. Whittet, P. Gerakines, J. Hough, S. Shenoy. 2001

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In Astronomy and Astrophysics

Citations in the corpus

Interpreting Spectral Energy Distributions from Young Stellar Objects. II. Fitting Observed SEDs Using a Large Grid of Precomputed Models (2006, methodology): “…situated in a distance range of 120 → 160AU (to rule out too luminous or too faint sources), that the foreground interstellar extinction was no more than AV = 20 (Whittet et al. 2001), and we used the condition that none of the sources appeared larger than the apertures used to measure the fluxes.”
Ultraviolet Survey of CO and H2 in Diffuse Molecular Clouds: The Reflection of Two Photochemistry Regimes in Abundance Relationships (2008, background): “…properties: the ratio of total to selective extinction (Cardelli & Clayton 1991; Larson et al. 2000; Barbaro et al. 2001; Patriarchi et al. 2001; Whittet et al. 2001; Ducati et al. 2003; Patriarchi et al. 2003; Valencic et al. 2004; Fitzpatrick & Massa 2005; Larson & Whittet 2005; Sofia et al.…”
Low-extinction windows in the inner Galactic Bulge (2001, background): “…to overestimation of the ratio of totalto-selective extinction RV , because several studies (Kenyon et al. 1994; Vrba & Rydgren 1985; and recently Whittet et al. 2001) suggested that the RV = 3.1 in most parts of the Taurus dark cloud complex, in regions where the visual extinction is lower than…”
Herbig Ae/Be Stars in nearby OB Associations (2004, background): “Although in moderately and highly embedded HAeBe stars this value is larger than that for normal interstellar reddening (e.g., Hernández et al. 2004; Whittet et al. 2001; Waters &Waelkens 1998), we useRV ¼ 3:1 for our stars because they have low visual extinction (AV < 1 mag); differences in RV…”
WATER, O2, AND ICE IN MOLECULAR CLOUDS (2008, methodology): “Whittet et al. (2001) have presented plots of the water ice columns versus cloud extinction in which a clear threshold AV for water ice is inferred.”
Observations of the Icy Universe (2015, background): “In Taurus, the ice band is only present at extinctions above AV= 3.2± 0.1 mag (Whittet et al., 2001), which corresponds to an ice formation threshold of AV= 1.6 mag considering that background stars trace both sides of the cloud.”
Cold Dark Clouds: The Initial Conditions for Star Formation (2007, background): “In Taurus, the water ice threshold is AthV (H2O) = 3.2 m ± 0.1m; a comparable threshold is observed for CO2 ice but for CO A th V (CO) = 6.8 m ± 1.6m (Whittet et al. 2001; Bergin et al. 2005; Whittet et al. 2007).”
Two-dimensional Radiative Transfer in Protostellar Envelopes. II. An Evolutionary Sequence (2003, methodology): “…the envelope we use the grain model from Paper I which has a size distribution that fits an extinction curve typical of the more dense regions of the Taurus molecular cloud, with RV , the ratio of total-to-selective extinction, equal to 4.3 (Whittet et al. 2001; Cardelli, Clayton, & Mathis 1989).”
Microscopic simulation of methanol and formaldehyde ice formation in cold dense cores (2009, result): “Laboratory spectra of CO mixed with either H2O or CH3OH show similar changes in the 4.7 μm CO feature, broadening and redshifting (Bisschop 2007; Bottinelli et al. in prep; Bouwman et al. 2007).”
The Efficiency of Grain Alignment in Dense Interstellar Clouds: a Reassessment of Constraints from Near-Infrared Polarization (2007, methodology): “…dark clouds in Taurus is the best available approximation: it is nearby (140 pc), lies in a direction of little general extinction, and is reasonably well-sampled by background field stars exhibiting substantial degrees of interstellar polarization (e.g. Whittet et al. 2001 and references therein).”
The chemical history of molecules in circumstellar disks - I. Ices (2009, unknown): “The amount of gaseous material left over near the end of the pre-collapse phase is also consistent with observations, which show that the onset of H2O ice formation is around anAV of 3 (Whittet et al. 2001).”
Radiative torque alignment: essential physical processes (2007, background): “Similarly, the change of the degree of polarization with optical depth observed by Whittet et al. (2001) was also explained by RATs in Lazarian (2003, 2007).”
ON THE FORMATION OF CO2 AND OTHER INTERSTELLAR ICES (2011, background): “…of interstellar ice, but significant quantities of other molecules are also present, including CO, CO2 and methanol (CH3OH) (Chiar et al. 1995, Whittet et al. 2001, 2007), with abundances with respect to water ranging into the tens of percent, dependent on the astronomical source (Gibb et al.…”
Simulation of the Formation and Morphology of Ice Mantles on Interstellar Grains (2007, background): “Observations in dense cloud assemblies such as Taurus show nowater ice below a threshold value ofAV ¼ 3:2 and linear growth of the column density of water ice above this value (Whittet et al. 2001).”
Two-dimensional Radiative Transfer in Protostellar Envelopes. I. Effects of Geometry on Class I Sources (2003, background): “This value of RV is typical of the denser regions in the Taurus molecular cloud (Whittet et al. 2001).”
Tracing Magnetic Fields with Aligned Grains (2007, background): “However, a more recent study by Whittet et al. (2001) showed that grains at the interface of the Taurus dark cloud do not exhibit the correlation of Rv and λmax.”
Interpreting Spectral Energy Distributions from Young Stellar Objects. I. A Grid of 200,000 YSO Model SEDs (2006, background): “Dust grains in embedded regions of Taurus show evidence for further grain growth, with RV ∼ 4 in the densest regions (Whittet et al. 2001), but recent models of near-IR images of Taurus protostars show that larger grain models are not well-distinguished from ISM grains (Wolf & Hillenbrand 2003;…”