351 research outputs found
Wallpapers of distinction
No full textCatalog was intended to showcase different wallpaper patterns from the 1920's.1 volume, colored illustrations an
Canarium galokense Daly, Raharim. & Federman 2015, sp. nov.
No full textCanarium galokense Daly, Raharim. & Federman, sp. nov. (Figs 1; 14). Small to medium-sized trees, leaves 3-5-jugate; distinguished from C. betamponae Daly, Raharim. & Federman , sp. nov. and C. globosum Daly, Raharim. & Federman , sp. nov. by the stipules closer to the petiole base (7-10 vs 11-30 mm in the other two), the much longer stipular scar (2-6 vs 1-2 mm long), the fruit broadly oblong to broadly ovoid (vs globose to ovoid), and the fruit surface lenticellate (vs smooth and usually glossy). TYPUS. — Madagascar. Antsiranana, Diana, Ambilobe, Anaborano, Galoko Mountains, 300-400 m, 10.II.2006 (m fl), D. C. Daly, J. Raharimampionona & R. Ranaivojaona 13100 (holo-, NY!; iso-, MO!, P!, TEF!). PARATYPI. — Madagascar. Antsiranana, Diana, Ambilobe, Anaborano, Galoko Mountains, 300-400 m, 13°35’19”S, 48°42’33”E 10. II.2006, D. C. Daly, J. Raharimampionona & R. Ranaivojaona 13101 (NY, TEF), 700 m, 13°38’31”S, 48°40’25”E, 25.XI.2006, M. Callmander, J. Vasaha & Malaza 600 (G, MO, P, TAN). DISTRIBUTION AND ECOLOGY. — To date, Canarium galokense, sp. nov. is known only from the Sambirano region in the Galoko mountains, in forest on steep slopes with rock outcrops and relatively closed canopy to 25 m, at 300-700 m elevation. Known to flower in Feb. and fruit in Nov. DESCRIPTION Trees, reproductive size 10-25 m × 10-26 cm diam. Outer bark (Daly et al. 13100) relatively smooth, with some raised lenticels, very finely & shallowly fissured, inner bark orangish. Leaves 21-41 cm long, 3-5-jugate; petiole 3.7-7.7 cm long, petiole and rachis with scattered to sparse thick erect golden hairs to 0.1 mm long and capitate glands; stipules inserted 3-10 mm from petiole insertion, 4.5-10 mm long, orbicular with constricted base, subcoriaceous, stipular scar 2-4 mm long; basal petiolules 9-15 mm long, other laterals 6-18 mm long, terminal one 16-31 mm long, pulvinuli inconspicuous; leaflet margin flat; leaflets thickly chartaceous, drying grayish brown, sometime slightly glossy; basal leaflets 5-10.3 × 2.3- 5.1 cm, (broadly) ovate, other laterals 8.3-13.8 × 2.8-6 cm, (oblong-)lanceolate to ovate, terminal one 8-14 × 2.8-6 cm, elliptic; leaflet apex gradually and usually narrowly acuminate, the acumen (2) 5-10 mm long, base of laterals symmetrical to slightly oblique, rounded to truncate; secondary vein framework brochidodromous, secondaries in 8-13 pairs, spreading to almost straight, insertion on midvein excurrent, spacing slightly decreasing toward the extremes, initial angle often subperpendicular, decreasing distally, perpendicular epimedial tertiary veins present, intercostal tertiaries alternate-percurrent and random-reticulate with some admedial branching, quaternaries regular-polygonal; on abaxial side all veins narrowly prominent, on adaxial side the midvein narrowly prominulous but sunk in a groove, the rest narrowly prominulous, both surfaces with a few scattered capitate glands along the midvein and rest of surface with scattered glands or glabrous. Staminate inflorescences to 20 cm long with secondary axes to 2.7 cm long, the axes with dense to sparse flexuous darkly ferrugineous hairs to 0.25 mm long and capitate glands; bracts on secondary axes 1.5-3 mm long, subulate. Staminate buds 5.7-6 mm long; calyx 2-2.1 × 4 mm overall, taller than ovariodisk, lobes 0.5-0.7 mm long, rounded depressed-deltate, abaxial surface with dense glands and dense flexuous hairs to 0.1 mm long; petals 5-5.1 × 2.1 mm, exposed part longer than calyx, obovate, abaxial surface with dense, flexuous hairs to 0.2 mm; stamens inserted at base of ovariodisk, 3.9-4 mm long with anthers 1.4-1.6 mm long, narrowly ovate in dorsiventral view, lanceolate in lateral view; ovariodisk 1.6-1.8 × 0.8-1 mm, ovoid, apex obtuse. Pistillate flowers unknown. Infructescences to 12 cm long with secondary axes to 7 cm long, fruiting pedicel 4-5 mm long, cylindrical; fruits 3.5-4 × 2.5-3 cm, broadly oblong or broadly ovoid, apex truncate, base obtuse, the surface with fine, slightly raised lenticels; pyrene trigonous but the apex obtuse. NOTES Canarium galokense, sp. nov. belongs to a group of species including C. betamponae, sp. nov., C, globosum, sp. nov. and C. subsidarium, sp. nov. that all have 3-5-jugate leaves, usually small and oblong leaflets, and similarly sized fruits. They are compared in Table 1 under C. betamponae, sp. nov. Moreover, C. galokense, sp. nov. is distinguished from all three by its much longer stipular scar (2-6 vs 1-2 mm long), inflorescence hairs dark-ferrugineous, the fruit broadly oblong to broadly ovoid (vs globose to ovoid), and the fruit surface lenticellate (vs glabrous and usually glossy). It is further distinguished from C. betamponae, sp. nov. and C. globosum, sp. nov. by the stipules closer to petiole insertion (7-10 vs 11-30 mm in the latter two).Published as part of Daly, Douglas C., Raharimampionona, Jeannie & Federman, Sarah, 2015, A revision of Canarium L. (Burseraceae) in Madagascar, pp. 277-345 in Adansonia 37 (2) on pages 308-310, DOI: 10.5252/a2015n2a2, http://zenodo.org/record/520890
Ultraviolet survey of CO and H2 in diffuse molecular clouds: the reflection of two photochemistry regimes in abundance relationships
No full textWe carried out a comprehensive far-UV survey of 12CO and H2 column densities along diffuse molecular Galactic sight lines. This sample includes new measurements of CO from HST spectra along 62 sight lines and new measurements of H2 from FUSE data along 58 sight lines. In addition, high-resolution optical data were obtained at the McDonald and European Southern Observatories, yielding new abundances for CH, CH+, and CN along 42 sight lines to aid in interpreting the CO results. These new sight lines were selected according to detectable amounts of CO in their spectra and provide information on both lower density (<=100 cm-3) and higher density diffuse clouds. A plot of logN(CO) versus logN(H2) shows that two power-law relationships are needed for a good fit of the entire sample, with a break located at logN(CO,cm-2)=14.1 and logN(H2)=20.4, corresponding to a change in production route for CO in higher density gas. Similar logarithmic plots among all five diatomic molecules reveal additional examples of dual slopes in the cases of CO versus CH (break at logN=14.1, 13.0), CH+ versus H2 (13.1, 20.3), and CH+ versus CO (13.2, 14.1). We employ both analytical and numerical chemical schemes in order to derive details of the molecular environments. In the denser gas, where C2 and CN molecules also reside, reactions involving C+ and OH are the dominant factor leading to CO formation via equilibrium chemistry. In the low-density gas, where equilibrium chemistry studies have failed to reproduce the abundance of CH+, our numerical analysis shows that nonequilibrium chemistry must be employed for correctly predicting the abundances of both CH+ and CO
Interstellar CN And CH+ In Diffuse Molecular Clouds: C-12/C-13 Ratios And Cn Excitation
No full textWe present very high signal-to-noise ratio absorption-line observations of CN and CH+ along 13 lines of sight through diffuse molecular clouds. The data are examined to extract precise isotopologic ratios of (CN)-C-12/(CN)-C-13 and (CH+)-C-12/(CH+)-C-13 in order to assess predictions of diffuse cloud chemistry. Our results on (CH+)-C-12/(CH+)-C-13 confirm that this ratio does not deviate from the ambient C-12/C-13 ratio in local interstellar clouds, as expected if the formation of CH+ involves nonthermal processes. We find that (CN)-C-12/(CN)-C-13, however, can be significantly fractionated away from the ambient value. The dispersion in our sample of (CN)-C-12/(CN)-C-13 ratios is similar to that found in recent surveys of (CO)-C-12/(CO)-C-13. For sight lines where both ratios have been determined, the (CN)-C-12/(CN)-C-13 ratios are generally fractionated in the opposite sense compared to (CO)-C-12/(CO)-C-13. Chemical fractionation in CO results from competition between selective photodissociation and isotopic charge exchange (ICE). An inverse relationship between (CN)-C-12/(CN)-C-13 and (CO)-C-12/(CO)-C-13 follows from the coexistence of CN and CO in diffuse cloud cores. However, an ICE reaction with CN may mitigate the enhancements in (CN)-C-12/(CN)-C-13 for lines of sight with low (CO)-C-12/(CO)-C-13 ratios. For two sight lines with high values of (CO)-C-12/(CO)-C-13, our results indicate that about 50% of the carbon is locked up in CO, which is consistent with the notion that these sight lines probe molecular cloud envelopes where the transition from C+ to CO is expected to occur. An analysis of CN rotational excitation yields a weighted mean value for T-01((CN)-C-12) of 2.754 +/- 0.002 K, which implies an excess over the temperature of the cosmic microwave background (CMB) of only 29 +/- 3 mK. This modest excess eliminates the need for a local excitation mechanism beyond electron and neutral collisions. The rotational excitation temperatures in (CN)-C-13 show no excess over the temperature of the CMB.Robert A. Welch Foundation F-634McDonald Observator
A comparison of UV surface brightness and HI surface densities for spiral galaxies
No full textShaya and Federman (1987) suggested that the ambient ultraviolet flux at 1000 A permeating a spiral galaxy controls the neutral hydrogen (HI) surface density in the galaxy. They found that the atomic envelopes surrounding small molecular clouds, because of their great number, provide the major contribution to the HI surface density over the stellar disk. The increase in HI surface density with later Hubble types was ascribed to the stronger UV fields from more high-mass stars in later Hubble types. These hypotheses are based on the observations of nearby diffuse interstellar clouds, which show a sharp atomic-to-molecular transition (Savage et al. 1977), and on the theoretical framework introduced by Federman, Glassgold, and Kwan (1979). Atomic envelopes around interstellar clouds in the solar neighborhood arise when a steady state is reached between photodissociation of H2 and the formation of H2 on grains. The photodissociation process involves photons with wavelengths between 912 A and 1108 A. Shaya and Federman used H-alpha flux as an approximate measure for the far UV flux and made their comparisons based on averages over Hubble type. Here, researchers compare, on an individual basis, UV data obtained with space-borne and balloon-borne instruments for galaxies with measurements of HI surface density (Warmels 1988a, b). The comparisons substantiate the conclusion of Shaya and Federman that the far UV field controls the HI content of spiral galaxies
Canarium obovatum Daly, Raharim. & Federman 2015, sp. nov.
No full textCanarium obovatum Daly, Raharim. & Federman, sp. nov. (Figs 1; 23 F-G) Small trees, stipules 5-8 mm long, ovate, stipular scars 1-1.6 mm long, leaflets coriaceous, pistillate inflorescences 13-19 cm long, the axes with dense to sparse flexuous hairs to 0.5 mm long; distinguished from C. lamianum Daly, Raharim. & Federman , sp. nov. by the leaves 1-2-jugate (vs (2)3-4 jugate in C. lamianum, sp. nov.) on fertile branchlets, petiole usually longer (5.6-19.5 vs 2.5-6.5 cm), lateral petiolules longer (10-27 vs 4-12 mm), terminal petiolules longer (10-27 vs 4-12 mm), leaflets usually (oblong-)obovate (vs at least some leaflets shaped otherwise), the apex narrowly (not broadly) short-acuminate, intercostal tertiary venation mixed opposite-alternate percurrent (vs irregular-reticulate), pistillate calyx 5.6-6 vs 6.8-8 mm long. TYPUS. — Madagascar. [Toamasina,] Est (Nord): Environs Ouest d’Andasibe (à l’Ouest d’Andapa), sur la piste de Bealanana, 24.IV.1967, R. Capuron (Service Forestier) 27803 (holo-, NY!; iso-, P!). PARATYPUS. — Toamasina, Ambodirina, Réserve Naturelle Intégrale Betampona, 325-375, 17°55’53”S, 49°12’12”E, 02.II.2006, D.C. Daly, R. Ranaivojaona & R.B. Iambana 13064 (MO, NY, P[P04799624]). DISTRIBUTION AND ECOLOGY. — Canarium obovatum, sp. nov. is known from only two localities, south of Andapa and in Betampona National Park, in moist forests on steep slopes at 325-375 m elevation. Flowering Apr. ETYMOLOGY. — The specific epithet refers to the predominant leaflet shape. DESCRIPTION Trees, reproductive size 10- 15 m. Outer bark gray, sparsely cracked, sparsely lenticellate. Leaves 25-34 cm long, 1-2-jugate (to 4-jugate on sterile branchlets); petiole 5.6-19.5 cm long, petiole and rachis with dense erect (some flexuous) golden hairs 0.3-0.5 mm long also with scattered raised ferrugineous lenticels; stipules 5-10 mm from petiole insertion, 5-8 mm long, ovate, constricted at base and often appearing stipitate, with erect to ascending golden hairs to 0.2 mm long, the scar 1-1.5 mm long; basal petiolules 10-25 mm long, other laterals 10-27 mm long, terminal one 23-50 mm long (to 60 mm on sterile branchlets), petiolules not canaliculate, pulvinuli relatively inconspicuous; basal leaflets 6-9.5 × 4-8 cm, broadly (ob)ovate to subrotund, other laterals 9-13 × 3.8-8.4 cm, (broadly) obovate to oblong-obovate to oblong, terminal leaflet 12-16.5 × 3.9-10.6 cm, (broadly) obovate; leaflet apex abruptly and narrowly short-acuminate, the acumen 2-12 mm long, apex tip acute, glandular-apiculate; leaflet base symmetric, acute or less often obtuse; margin flat; leaflets coriaceous, drying brown sometimes glossy on abaxial side; secondary vein framework brochidodromous but looping at margin, secondaries in 7-12 pairs, spreading to arcuate, not discolorous, spacing abruptly decreasing at base, angle slightly acute to perpendicular and decreasing toward apex and usually toward the base; intercostal tertiaries opposite- or alternate-percurrent, some perpendicular intersecondaries and epimedial tertiaries present, quaternaries irregular-reticulate; on abaxial side all veins narrowly prominent except midvein broader, the midvein with sparse spiky golden hairs to 0.5 mm long, rest of veins and surface with such hairs to 0.2 mm long; on adaxial side the midvein narrowly prominulous but usually sunk in a groove, secondaries narrowly prominulous and sometimes sunk, rest flat to narrowly prominulous, with scattered flexuous golden hairs to 0.3 mm long on midvein and base of secondaries (to 0.5 mm on sterile specimen). Pistillate inflorescences 13-19 cm long, secondary axes to 7 cm long, axes with dense flexuous hairs to 0.5 mm long; bracts on primary and secondary axes to 8 mm long, rotund and slightly acuminate, semi-clasping, persistent in young fruit, bracteoles 4.7-5 mm long, much shorter than buds, ovate, constricted at base, persistent in young fruit, on all bracts the abaxial side with ascending flexuous golden hairs to 0.2 mm long, adaxially with erect to ascending flexuous golden hairs to 0.25 mm long; pedicel 5-10 mm long, clavate. Pistillate flowers c. 9 mm long at anthesis; calyx 5.6-6 mm × 7.1-8.3 mm overall, campanulate, the lobes 2.7-3.1 mm long, rounded depressed-deltate, abaxial surface with pubescence as on inflorescence axes but shorter, to 0.3 mm long, adaxial surface with dense appressed hairs to 0.6 mm long; corolla spreading at anthesis, exposed portion only 3 mm beyond calyx, abaxial surface with dense, flexuous or ascending, pale golden hairs to 0.5 mm long. Immature fruits oblong (some slightly obovoid), with dense golden hairs to 0.6 mm long, descending near base of fruit, ascending near apex. NOTES Like C. pulchrebracteatum, C. obovatum, sp. nov. has stipules 5-8 mm long, terminal leaflets obovate (to elliptic or rarely ovate in C. obovatum, sp. nov.), a comparable number of secondary veins (collectively 5-12) and fine, stiff hairs on the abaxial midvein (to 0.5 mm long in C. obovatum, sp. nov., to 0.25 mm long in C. pulchrebracteatum). Canarium obovatum, sp. nov. is distinguished by the stipular scar shorter (1-1.5 vs (1) 2-3.5 mm), fewer leaflet pairs (1-2 vs (1) 3-4), longer lateral petiolules (10-27 vs 4-17 mm), the basal petiolules longer (10-25 vs 4-11), all leaflets usually obovate (vs at least some leaflets shaped otherwise), and the fruit densely pubescent (vs glabrous). Like C. lamianum, sp. nov., C. obovatum, sp. nov. has small stipules 0.3-0.8 mm long and ovate (to orbicular in C. lamianum, sp. nov.) with constricted base, short stipular scars 1-1.6 mm long, coriaceous leaflets of similar size, inflorescences of comparable length (up to 19 cm), the axes with dense to sparse flexuous hairs (but up to 0.5 mm long in C. obovatum, sp. nov. and to 0.25 mm long in C. lamianum, sp. nov.). Canarium obovatum, sp. nov. is distinguished by having fewer leaflet pairs (1-2 vs (2)3-4), the petiole usually longer (5.6-19.5 vs 2.5-6.5 mm), the lateral petiolules longer (10-27 vs 4-12 mm long), terminal petiolules longer (10-27 vs 4-12 mm), leaflets usually (oblong-)obovate (vs at least some leaflets shaped otherwise), the apex narrowly (not broadly) short-acuminate, the intercostal tertiary venation mixed opposite-alternate percurrent (vs irregular-reticulate), the midvein abaxially with sparse spiky golden hairs to 0.5 mm long (vs scattered appressed hairs and occasionally scattered bristles to 0.05 mm), and pistillate calyx 5.6-6 vs 6.8-8 mm long.Published as part of Daly, Douglas C., Raharimampionona, Jeannie & Federman, Sarah, 2015, A revision of Canarium L. (Burseraceae) in Madagascar, pp. 277-345 in Adansonia 37 (2) on pages 326-328, DOI: 10.5252/a2015n2a2, http://zenodo.org/record/520890
THE FORMATION OF SH VIA S + H IN X-RAY DOMINATED REGIONS
No full textAuthor Institution: Department of Physics, University of Cincinnati, Cincinnati, OH; Department of Physics \& Astronomy, University of Toledo, Toledo, OH; Department of Physics \& Astronomy and the Center for Simulation Physics, University of GeorgiaA. Dalgarno first suggested thirty-two years ago that doubly-ionized elements reacting with H could lead to the formation of molecules in regions with a significant X-ray flux. However, few investigations of the effects of on the formation of molecules have actually been conducted. Recent studies have found the reaction rate coefficients to be orders of magnitude higher than previously thought. This fact, combined with a renewed interest in the physics and chemistry of X-ray Dominated Regions (XDRs), points to a need to study the effects of on molecule formation. We investigated how S + H affects the formation of SH for atomic gas exposed to an X-ray continuum typical of an Active Galactic Nucleus (AGN). As long as the fraction of S + H reactions which lead to SH formation exceeds a few percent, this process will be the dominant formation pathway for SH. This potentially has major consequences for our understanding of sulfur chemistry in galaxies where the energetics is dominated by AGN activity
[18F]FDG PET/CT for evaluating early response to neoadjuvant chemotherapy in pediatric patients with sarcoma: a prospective single-center trial.
No full textIntroduction: This is a prospective, single-center trial in pediatric patients with sarcoma aiming to evaluate [18F]FDG PET/CT as a tool for early response assessment to neoadjuvant chemotherapy (neo-CTX).
Methods: Bone or soft tissue sarcoma patients with (1) baseline [18F]FDG PET/CT within 4 weeks prior to the start of neo-CTX (PET1), (2) early interim [18F]FDG PET/CT (6 weeks after the start of neo-CTX (PET2), (3) evaluation of neo-CTX response by histology or MRI, and (4) definitive therapy after neo-CTX (surgery or radiation) were included. Semiquantitative PET parameters (SUVmax, SUVmean, SUVpeak, MTV and TLG) and their changes from PET1 to PET2 (ΔPET) were obtained. The primary endpoint was to evaluate the predictive value of PET1, PET2 and ΔPET parameters for overall survival (OS) and time to progression (TTP). The secondary outcome was to evaluate if [18F]FDG PET/CT can predict the response to neo-CTX assessed by histopathology or MRI. Primary and secondary outcomes were also evaluated in a subpopulation of patients with bone involvement only.
Results: Thirty-four consecutive patients were enrolled (10 females; 24 males; median age 15.1 years). 17/34 patients (50%) had osteosarcoma, 13/34 (38%) Ewing's sarcoma, 2/34 (6%) synovial sarcoma and 2/34 (6%) embryonal liver sarcoma. Median follow-up was 39 months (range 16-84). Eight of 34 patients (24%) died, 9/34 (27%) were alive with disease, and 17/34 (50%) had no evidence of residual/recurrent disease. Fifteen of 34 (44%) and 19/34 (56%) were responders and non-responders, respectively. PET2-parameters were associated with longer TTP (p < 0.02). ΔMTV was associated with tissue response to neo-CTX (p = 0.047). None of the PET1, PET2 or ΔPET parameters were associated with OS.
Conclusion: [18F]FDG PET/CT performed 6 weeks after the start of neo-CTX can serve as an early interim biomarker for TTP and pathologic response but not for OS in pediatric patients with sarcoma
A study of extended red emission in reflection nebulae
No full textIn the first part of this thesis spectroscopic observations of the Red Rectangle nebula are presented. A link is made between the most prominent unique emission line features, which are superimposed on the broad emission spectrum of the Red Rectangle, with the absorption features of the diffuse interstellar bands (DIBs). The shape of the emission lines are shown to be temperature dependent with the bandwidth decreasing by 4Å and the the peak wavength altering by 5Å in the cooler outer parts of the nebula when compared with the hotter inner regions. Both peak wavelength and bandwidth can be extrapolated to the values of the associated DIBs. A possible common carrier is discussed for the absorption/emission line pairs. In the second part polarimetric observations of two reflection nebulae, NGC 7023 and NGC 2023, are presented in the B, V, R, I, and V, R, I wavebands respectively. Through the use of colour and polarization colour diagrams a search was made for intrinsic emission, also known as extended red emission (ERE). Two such regions were found in NGC 7023, one 64"S and the other 53"N of HD 200775, in which there was a reduction in the R and I polarizations when compared with the values expected from scattering alone together with an increase in reddening. Calculations show that the ERE contributes as much as 22% of the light in the R waveband and approximately 16% in the I waveband. For NGC 2023 two suspected regions were investigated, the first 62"ENE and the second 84"ENE of HD 37903. It was found that the region nearest to the central star was unlikey to be a region of ERE however the second region exhibited a decrease in the R polarization together with an increase in R intensity but this was not shown to be the case in the I waveband. Several explanations are provided to explain this behaviour. The ERE is thus shown to be localised and varying in quantity between different positions in a nebula. None of the emission line features prominent in the Red Rectangle were found in the spectrum of the filament 84"ENE of HD 37903 and the implications of this are discussed
ASTRONOMICAL DETECTIONS OF VACUUM ULTRAVIOLET TRANSITIONS OF CH
No full textAuthor Institution: Department of Physics and Astronomy, University of Toledo, Toledo, OH 43606In the 1990s, three unidentified absorption lines near 1370 \AA\ and another one near 1270 \AA\ were detected in {\it Hubble Space Telescope (HST)} spectra of diffuse interstellar sight lines. These features were suspected of belonging to molecular carriers; the widest one at 1369.13 \AA\ was hypothesized as being a vacuum ultraviolet (VUV) analogue of the ubiquitous diffuse interstellar bands seen in the visible. Eventually, all four features were assigned by Watson in 2001 to Rydberg transitions of CH, previously observed in laboratory spectra by Herzberg and Johns in 1969. Since all CH column densities to date have used optical CH transitions, especially the 4300 \AA\ doublet, we analyzed {\it HST} spectra of sight lines with optically-derived CH abundances to confirm Watson's assignment of the VUV lines by measuring consistent -values for them. In addition, we expanded the survey by searching for additional VUV transitions of interstellar CH. Two more CH bands were detected, near 1694 \AA\ and near 1549 \AA. Both measured -values and, for the wider lines, predissociation lifetimes are found to be in agreement with theoretical calculations by, e.g., van Dishoeck in 1987. The 1369.13 \AA\ transition from the (or ) band remains the strongest and widest VUV feature of CH
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