Tumor Risks and Genotype-Phenotype-Proteotype Analysis in 358 Patients With Germline Mutations in SDHB and SDHD

Succinate dehydrogenase B (SDHB) and D (SDHD) subunit gene mutations predispose to adrenal and extraadrenal pheochromocytomas, head and neck paragangliomas (HNPGL), and other tumor types. We report tumor risks in 358 patients with SDHB (n = 295) and SDHD (n = 63) mutations. Risks of HNPGL and pheochromocytoma in SDHB mutation carriers were 29% and 52%, respectively, at age 60 years and 71% and 29%, respectively, in SDHD mutation carriers. Risks of malignant pheochromocytoma and renal tumors (14% at age 70 years) were higher in SDHB mutation carriers; 55 different mutations (including a novel recurrent exon 1 deletion) were identified. No clear genotype-phenotype correlations were detected for SDHB mutations. However, SDHD mutations predicted to result in loss of expression or a truncated or unstable protein were associated with a significantly increased risk of pheochromocytoma compared to missense mutations that were not predicted to impair protein stability (most such cases had the common p.Pro81Leu mutation). Analysis of the largest cohort of SDHB/D mutation carriers has enhanced estimates of penetrance and tumor risk and supports in silicon protein structure prediction analysis for functional assessment of mutations. The differing effect of the SDHD p.Pro81Leu on HNPGL and pheochromocytoma, risks suggests differing mechanisms of tumorigenesis in SDH-associated HNPGL and pheochromocytoma. Hum Mutat 31:41-51, 2010. (C) 2009 Wiley-Liss, Inc.

Evidence for a modifier of onset age in Huntington disease linked to the HD gene in 4p16

Huntington disease (HD) is a neurodegenerative disorder caused by the abnormal expansion of CAG repeats in the HD gene on chromosome 4p16.3. A recent genome scan for genetic modifiers of age at onset of motor symptoms (AO) in HD suggests that one modifier may reside in the region close to the HD gene itself. We used data from 535 HD participants of the New England Huntington cohort and the HD MAPS cohort to assess whether AO was influenced by any of the three markers in the 4p16 region: MSX1 (Drosophila homeo box homologue 1, formerly known as homeo box 7, HOX7), Delta2642 (within the HD coding sequence), and BJ56 (D4S127). Suggestive evidence for an association was seen between MSX1 alleles and AO, after adjustment for normal CAG repeat, expanded repeat, and their product term (model P value 0.079). Of the variance of AO that was not accounted for by HD and normal CAG repeats, 0.8% could be attributed to the MSX1 genotype. Individuals with MSX1 genotype 3/3 tended to have younger AO. No association was found between Delta2642 (P=0.44) and BJ56 (P=0.73) and AO. This study supports previous studies suggesting that there may be a significant genetic modifier for AO in HD in the 4p16 region. Furthermore, the modifier may be present on both HD and normal chromosomes bearing the 3 allele of the MSX1 marker.

Interaction of normal and expanded CAG repeat sizes influences age at onset of Huntington disease

Huntington disease (HD) is a neurodegenerative disorder caused by the abnormal expansion of CAG repeats in the HD gene on chromosome 4p16.3. Past studies have shown that the size of expanded CAG repeat is inversely associated with age at onset (AO) of HD. It is not known whether the normal Huntington allele size influences the relation between the expanded repeat and AO of HD. Data collected from two independent cohorts were used to test the hypothesis that the unexpanded CAG repeat interacts with the expanded CAG repeat to influence AO of HD. In the New England Huntington Disease Center Without Walls (NEHD) cohort of 221 HD affected persons and in the HD-MAPS cohort of 533 HD affected persons, we found evidence supporting an interaction between the expanded and unexpanded CAG repeat sizes which influences AO of HD (P = 0.08 and 0.07, respectively). The association was statistically significant when both cohorts were combined (P=0.012). The estimated heritability of the AO residual was 0.56 after adjustment for normal and expanded repeats and their interaction. An analysis of tertiles of repeats sizes revealed that the effect of the normal allele is seen among persons with large HD repeat sizes (47-83). These findings suggest that an increase in the size of the normal repeat may mitigate the expression of the disease among HD affected persons with large expanded CAG repeats. (C) 2003 Wiley-Liss, Inc.

Treatment Foster Care for Improving Outcomes in Children and Young People: A Systematic Review

Objective: To assess the impact of treatment foster care (TFC) on psychosocial and behavioral outcomes, delinquency, placement stability, and discharge status for children and adolescents who, for reasons of severe medical, social, psychological and behavioural problems, were placed in out-of-home care in restrictive settings or at risk of placement in such settings. Method: Electronic bibliographic databases, web searches, and article reference lists were used to identify randomized controlled trials (RCTs) investigating the effectiveness of TFC with children and young people. The Cochrane Collaboration’s criteria were used to assess the methodological quality of studies that met the inclusion criteria. Wherever possible, extracted outcome data from similar studies were synthesized with random effects meta-analyses. Results: A total of 5 studies including 390 participants were included in this review. Data suggest that TFC may be a useful intervention for children and young people with complex emotional, psychological, and behavioural need, who are at risk of placements in nonfamily settings that restrict their liberty and opportunities for social inclusion. Conclusion: Although the inclusion criteria for this systematic review set a study design threshold higher than that of previous reviews, the findings mirror those of earlier reviews. While the results of individual studies generally indicate that TFC is a promising intervention for children and youth experiencing mental health problems, behavioral problems, or problems of delinquency, the evidence base is not robust and more research is needed due to the limited number of studies in this area.

A one pot three-step process for the synthesis of an array of arylated benzimidazoribosyl nucleosides

A three-step one pot reaction/purification protocol was developed to facilitate rapid access to benzimidazole-based nucleosides, for which benzoylated benzimidazoribosyl nucleosides incorporating boronic esters were key reaction intermediates.

Open Adoption: Adoptive Parents' Experiences of Birth Family Contact and Talking to Their Child about Adoption

The trend towards more open adoption presents adopters with unique parenting challenges associated with satisfying the child’s curiosity about their origins, and maintaining relationships with birth family through contact. This paper focuses on the experiences of 20 sets of adoptive parents who were interviewed as part of the Northern Ireland Care Pathways and Outcomes Study. Interviews were analysed following the principles of Interpretative Phenomenological Analysis (IPA). It explores adoptive parents’ experience of talking to their child about adoption, and of post-adoption contact with members of the birth family. Adopters discussed adoption sensitively with their child, but were concerned that difficult and complex family histories would present a risk to the child’s self-esteem and emotional well-being. All forms of contact proved emotionally and practically burdensome, however adopters were committed to making it work for the child’s benefit, and were open to increased contact should the child wish it in the future. There was little relationship with birth family outside of formal contact. The study reveals a need for a mechanism to facilitate communication with birth family if adopters are to be able to respond to the child’s changing need for contact and information.

A chemoenzymatic synthesis of 5a-carba-alpha-D-mannose-6-phosphate

An efficient chemical synthesis of 5a-carba-alpha-D-mannose and its enzymatic elaboration to 5a-carba-alpha-D-mannose-6-phosphate, using yeast hexokinase, is described.

A 330-360 GHz spectral survey of G34.3+0.15 - III. The outer halo

We have undertaken a 330-360 GHz molecular line survey of the halo gas surrounding the hot core associated with G34.26+0.15. In contrast to our molecular line survey of the hot core itself, where 338 lines from at least 38 species were detected, only 18 lines from 9 species were detected in the halo. The lines are mainly single transitions of simple di atomic and triatomic molecules. Lower limits to their column densities have been evaluated by an LTE method. In the case of methanol, where four transitions were detected, the rotation temperature and column density have been evaluated by the rotation diagram technique. We have modified the previous depth-dependent chemical model developed in Paper II to calculate the column densities observed along a general line of sight drawn through the model cloud. The model is also extended to produce beam-averaged column densities for better comparison with those observed. We compare the model column densities with those observed and make recommendations for future depth-dependent chemical modelling of hot cores.

A survey of molecular line emission towards ultracompact HII regions

We have used the JCMT to survey molecular line emission towards 14 ultracompact HII regions (G5.89, G9.62, G10.30, G10.47, G12.21, G13.87, G29.96, G31.41, G34.26, G43.89, G45.12, G45.45, G45.47, and G75.78). For each source, we observed up to ten 1 GHz bands between 200 and 350 GHz, covering lines of more than 30 species including multiple transitions of CO isotopes, CH3OH, CH3CCH, CH3CN and HCOOCH3, and sulphuretted molecules. The number of transitions detected varied by a factor of 20 between sources; which were chosen following observations of high-excitation ammonia (Cesaroni et al. 1994a) and methyl cyanide (Olmi et al. 1993). In half our sample (the line-poor sources), only (CO)-O-17: (CO)-O-18, SO, (CS)-S-34 and CH3OH were detected. In the line-rich sources, we detected over 150 lines, including high excitation lines of CH3CN, HCOOCH3; C2H5CN, CH3OH, and CH3CCH. We have calculated the physical conditions of the molecular gas. To reproduce the emission from the line-rich sources requires both a hot, dense compact core and an ambient cloud consisting of less dense, cooler gas. The hot cores, which are less than 0.1 pc in size; reach densities of at least 10(8) cm(-3) and temperatures of more than 80 K. The line-poor sources can be modelled without a hot core by a 20-30 K, 10(5) cm(-3) cloud. We find no correlation between the size of the HII region and the current physical conditions in the molecular environment. A comparison with chemical models (Millar et al. 1997) confirms that grain surface chemistry is important in hot cores.

Sulphur chemistry and evolution in hot cores

We compare the results of our JCMT spectral line survey of molecular gas towards ultracompact HII regions with the predictions of models of sulphur chemistry in hot cores. We investigate the range of evolutionary models that are consistent with the observed physical conditions and chemical abundances, and see to what extent it is possible to constrain core ages by comparing abundances with the predictions of chemical models. The observed abundance ratios vary little from source to source, suggesting that all the sources are at a similar evolutionary stage. The models are capable of predicting the observed abundances of H2S, SO, SO2, and CS. The models fail to predict the amount of OCS observed, suggesting that an alternative formation route is required. An initial H2S abundance from grain mantle evaporation of similar to 10(-7) is preferred.

A 330-360 GHz spectral survey of G34.3+0.15 .2. Chemical modelling

We describe a detailed depth-and time-dependent model of the molecular cloud associated with the ultracompact H II region G 34.3+0.15. Previous work on observations of NH3 and CS indicates that the molecular cloud has three distinct physical components:- an ultracompact hot core, a compact hot core and an extended halo. We have used the physical parameters derived from these observations as input to our detailed chemical kinetic modelling. The results of the model calculations are discussed with reference to the different chemistries occuring in each component and are compared with abundances derived from our recent spectral line survey of G 34.3+0.15 (Paper I).

A 330-360 GHz spectral survey of G 34.3+0.15 .1. Data and physical analysis

A 330--360 GHz spectral survey of the hot molecular core associated with the 'cometary' ultracompact HII region G 34.3+/-0.15 observed with the James Clerk Maxwell Telescope has detected 338 spectral lines from at least 35 distinct chemical species plus 19 isotopomers. 70 lines remain unidentified. Chemical abundance and rotation temperature have been determined by rotation diagram analysis for 12 species, and lower limits to abundance found for 38 others.

Chemical evolution in the circumstellar structure of B5 IRS1

The B5 dark cloud has been identified as a site of low-mass star formation. We report a survey of a selection of the molecular species modelled by the B5 dynamical and chemical model of Charnley et al. at the positions of circumstellar HCN clumps in B5 IRS1. All of the key species observed yield either abundances or upper limits to abundances below both the standard and the predicted values, appearing to show evidence of depletion and/or destruction if the transitions observed are thermalized. Our results are not in good agreement with the model, and they bring into question the interpretation of the structure of B5 IRS1 proposed by Fuller et al. It was expected that HCN clump C might exhibit a higher excitation than HCN clump A, since it appeared to be located within the blueshifted molecular outflow. However, there is no significant difference observed between the two clumps, suggesting that the near-infrared and optical nebulosity is evidence of a reflection nebula rather than shocked material in the outflow. Finally, it is observed that our results are more consistent with gas-grain models than with those models excluding gas-grain interaction.

THE DETECTION OF HOT ETHANOL IN G34.3+0.15

Hot molecular cores in star-forming regions are known to have gas-phase chemical compositions determined by the evaporation of material from the icy mantles of interstellar grains, followed by subsequent reactions in the gas phase. Current models suggest that the evaporated material is rich in hydrogenated species, such as water, methane and methanol. In this paper, we report the detection of 14 rotational transitions of ethanol in the submillimetre spectrum of the molecular cloud associated with the ultra-compact H II region G34.3+0.15. We derive a rotation temperature of 125 K and a beam-averaged column density of 2.0x10(15) cm(-2), corresponding to a fractional abundance on the order of 4x10(-9). This large abundance, which is a lower limit due to the likelihood of beam dilution, cannot be made by purely gas-phase processes, and we conclude that the ethanol must be formed efficiently in the grain surface chemistry. Since it has been argued previously that methanol is formed via surface chemistry, it appears that alcohol formation may be a natural by-product of surface reactions.