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- Bergfors, C., et al.
(författare)
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Characterization of close visual binaries from the AstraLux Large M Dwarf Survey
- 2016
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Ingår i: Monthly notices of the Royal Astronomical Society. - : Oxford University Press (OUP). - 0035-8711 .- 1365-2966. ; 456:3, s. 2576-2585
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Tidskriftsartikel (refereegranskat)abstract
- We present Very Large Telescope/Spectrograph for INtegral Field Observations in the Near Infrared (VLT/SINFONI) J, H + K spectra of seven close visual pairs in M dwarf binary/triple systems, discovered or observed by the AstraLux M dwarf survey. We determine the spectral types to within +/- 1.0 subclasses from comparison to template spectra and the strength of K-band water absorption, and derive effective temperatures. The results are compared to optical spectral types of the unresolved binary/multiple systems, and we confirm that our photometric method to derive spectral types in the AstraLux M dwarf survey is accurate. We look for signs of youth such as chromospheric activity and low surface gravity, and find an age in the range 0.25-1 Gyr for the GJ 852 system. Strong Li absorption is detected in optical spectra of the triple system J024902 obtained with the Fiberfed Extended Range Optical Spectrograph (FEROS) at the European Southern Observatory (ESO)-Max-Planck-Gesellschaft (MPG) 2.2 m telescope. The equivalent width of the absorption suggests an age consistent with the beta Pic moving group. However, further observations are needed to establish group membership. Ongoing orbital monitoring will provide dynamical masses and thus calibration of evolutionary models for low mass stars.
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| 4. |
- Lu, Lu, 1984-, et al.
(författare)
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MEPicides : α,β-Unsaturated Fosmidomycin N-acyl Analogsas inhibitors that selectively target DXR from Plasmodium falciparum, the deadliest causative parasite of human Malaria
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Annan publikation (övrigt vetenskapligt/konstnärligt)abstract
- Fosmidomycin and FR-9000098 have been confirmed to show parasiticidal activity against Plasmodium falciparum, targeting DXR involved in the MEP pathway. We designed a construct of PfDXR that has successfully been overexpressed in E. coli BL21(DE3) C43, and purified by IMAC and SEC, with the final yield of 1.2 mg/ 8 L culture. PfDXR was concentrated to 20 mg/ml, and co-crystallized with previously tested inhibitors in the FR-9000098 scaffold in the presence of Mn2+. Three FR-9000098 analogues with double-bonded Ca-Cband/or a phenyl ring with various lengths to N1, showed inhibitory activities with IC50s roughly 50 nM. Three crystals were in triclinic P1space group, with similar dimensions in the unit cell (51Å, 56Å, 86Å, 103°, 103°, 101°). All four complex structures have been crystallographically determined at resolutions in the range 1.86 Å, 2.45 Å, 2.13Å, 2.05 Å. Given the high similarity in structures, the initial phases were determined by rigid body refinement with search model PfDXR-FN3 complex, followed by restrained refinement in refmac5. Subsequently, the ligands and surrounding amino acid residues were manually rebuilt with theqdstools in O. the Ca-Cbbonds of the three ligands were altered from a single to double bond based on the structure of FR9000098. In addition, two ligands were extended at the Cdwith a phenyl group, and with the benzyl group connected by two carbons. N-terminal NADPH binding domains from four complexes undergo minor rigid body movement, and more details of conformational changes in the flap region are discussed.
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| 5. |
- Rodet, L., et al.
(författare)
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Dynamical masses of M-dwarf binaries in young moving groups I. The case of TWA22 and GJ2060
- 2018
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Ingår i: Astronomy and Astrophysics. - : EDP Sciences. - 0004-6361 .- 1432-0746. ; 618
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Tidskriftsartikel (refereegranskat)abstract
- Context. Evolutionary models are widely used to infer the mass of stars, brown dwarfs, and giant planets. Their predictions are thought to be less reliable at young ages (<200 Myr) and in the low-mass regime (< 1 M-circle dot). GJ 2060AB and TWA22AB are two rare astrometric M-dwarf binaries, respectively members of the AB Doradus (AB Dor) and Beta Pictoris (beta Pic) moving groups. As their dynamical mass can be measured to within a few years, they can be used to calibrate the evolutionary tracks and set new constraints on the age of young moving groups.Aims. We provide the first dynamical mass measurement of GJ 2060 and a refined measurement of the total mass of TWA22. We also characterize the atmospheric properties of the individual components of GJ 2060 that can be used as inputs to the evolutionary models.Methods. We used NaCo and SPHERE observations at VLT and archival Keck/NIRC2 data to complement the astrometric monitoring of the binaries. We combined the astrometry with new HARPS radial velocities (RVs) and FEROS RVs of GJ 2060. We used a Markov chain MonteCarlo (MCMC) module to estimate posteriors on the orbital parameters and dynamical masses of GJ 2060AB and TWA22AB from the astrometry and RVs. Complementary data obtained with the integral field spectrograph VLT /SINFONI were gathered to extract the individual near-infrared (1.1-2.5 mu m) medium-resolution (R similar to 1500 2000) spectra of GJ 2060A and B. We compared the spectra to those of known objects and to grids of BT-SETTL model spectra to infer the spectral type, bolometric luminosities, and temperatures of those objects.Results. We find a total mass of 0 : 18 +/- 0 : 02 M-circle dot for TWA22, which is in good agreement with model predictions at the age of the fi Pic moving group. We obtain a total mass of 1 : 09 +/- 0 : 10 M-circle dot for GJ 2060. We estimate a spectral type of M1 +/- 0.5, L/L-circle dot = -1.20 +/- 0.05 dex, and T-eff = 3700 +/- 100 K for GJ 2060 A. The B component is a M3 +/- 0 : 5 dwarf with L/L-circle dot = 1.63 +/- 0.05 dex and T-eff = 3400 +/- 100 K. The dynamical mass of GJ 2060AB is inconsistent with the most recent models predictions (BCAH15, PARSEC) for an AB Dor age in the range 50-150 Myr. It is 10%-20% (1-2 sigma, depending on the assumed age) above the model's predictions, corresponding to an underestimation of 0.10-0.20 M fi. Coevality suggests a young age for the system (similar to 50 Myr) according to most evolutionary models.Conclusions. TWA22 validates the predictions of recent evolutionary tracks at similar to 20 Myr. On the other hand, we evidence a 1-2 sigma mismatch between the predicted and observed mass of GJ 2060 AB. This slight departure may indicate that one of the stars hosts a tight companion. Alternatively, this would confirm the model's tendency to underestimate the mass of young low-mass stars.
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| 7. |
- Warell, J, et al.
(författare)
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Mercury's integral phase curve : Phase reddening and wavelength dependence of photometric quantities
- 2008
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Ingår i: Planetary and Space Science. - : Elsevier BV. - 0032-0633 .- 1873-5088. ; 56:15, s. 1939-1948
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Tidskriftsartikel (refereegranskat)abstract
- We present results of a five-filter photometric study of Mercury's integral phase curve in the Johnson-Cousins UBVRI system, performed with the 0.90-m Westerlund Telescope in Uppsala, Sweden. CCD observations were made of the integrated disk for the phase angle range 22-152 degrees, and the study is the first to cover the extended visible spectrum of Mercury. The observations are analyzed with Hapke's semi-empirical radiative transfer-based light-scattering model and photometric quantities are derived. A statistically significant phase reddening effect of -9 +/- 6 mmag/ deg / mu m is determined for Mercury based on color index observations. which is similar to that of the Moon. Phase coefficients fit to integral absolute magnitude data and Hapke models in combination with color index data provide a phase reddening effect of -11 +/- 13 mmag/ deg / mu m which does however not provide statistically significant evidence for its presence. Phase coefficients indicate that phase reddening may be decreasing in magnitude with wavelength. As for the case with the Moon, the value of the phase integral increases with wavelength, but at an eight times higher rate. This value is consistent with the difference in the rate of change in the spectral slope-emission angle relation for the two bodies. We attribute these differences with Mercury's redder spectral slope and an increase with wavelength of the backscattering lobe amplitude in the double Henyey-Greenstein particle phase function formulation. The normal albedo of integral Mercury at 1064 nm, pertinent to the return pulse energy of the BepiColombo laser altimeter (BELA) is estimated to 0.23 +/- 0.06 with it range of 0.13-0.33 for 99% of the surface. (C) 2008 Elsevier Ltd. All rights reserved.
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