Download Ecm Titanium 1.61 [UPD]
Free download 2016 ECU TITANIUM V1.61 with 26000+ drivers, fit for ECU software (Kess v2 or KTAG with Ksuite) and editing maps ith many modules checksum, to work directly on main sections: air control, torque, fuel injection system, radiator, turbo and many other variants are available.
Download Ecm Titanium 1.61
NEW generation of drivers. Drivers who offer an organized and powerful interface to create and manage projects for ECM Tuning V1.61 modified files. After reading the file stored in the ECU memory, all you have to do is upload the file and the software starts a search for the presence of both the compatible drivers database.
ECM Titanium Management Tools 1.2 was available to download from the developer's website when we last checked. We cannot confirm if there is a free download of this software available. The program is included in Education Tools. This free tool was originally produced by Alientech S.r.l.
You can install this free PC software on Windows XP/XP Professional/Vista/7/8/10/11 32-bit. The following versions: 1.2 and 1.0 are the most frequently downloaded ones by the program users. We recommend checking the downloaded files with any free antivirus. The most frequent installer filenames for the program include: ECM2001.exe, ecm_tools.exe and Titanium.exe etc.
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The overall scheme for producing the Ti6Al4V/IL/HA composites is presented in Figure 1. The intermediate layers on the surface of the Ti6Al4V substrates were synthesized in the first stage. In all our experiments, 0.20 mm-thick Ti6Al4V alloy foil was used (marked as T, grade 5, 99.7% purity; Strem Chemicals, Inc., Bischheim, France). The electrochemical method of anodic oxidation in 0.3% hydrofluoric acid solution (t = 20 min, U = 5 V) was used to produce TiO2 nanoporous coatings (T5). As a result of etching in a ca. 5.8 M hydrochloric acid solution and chemical oxidation in 30% hydrogen peroxides solution (t = 6 h, T = 85 C under a reflux condenser), TiO2 nanofiber coatings (TNF6C) were obtained. Alkali-sodium treatment of the titanium alloy in 7 M sodium hydroxide solution (t = 48 h, T = 65 C) led to titanate coatings (T-S).
Using new methane absorption coefficients from Karkoschka and Tomasko (2009, submitted to Icarus, "Methane Absorption Coefficients for the Jovian Planets from Laboratory, Huygens, and HST Data"), we fit Uranus near-IR spectra previously analyzed in Sromovsky et al. (2006, Icarus 182, 577-593, Fink and Larson, 1979 J- and H-band), Sromovsky and Fry (2008, Icarus 193, 252-266, 2006 NIRC2 J- and H-band, 2006 SpeX) using Irwin et al. (2006, Icarus 181, 309-319) methane absorption coefficients. Because the new absorption coefficients usually result in higher opacities at the low temperatures seen in Uranus' upper troposphere, our previously derived cloud altitudes are expected to generally rise to higher altitudes. For example, using Lindal et al. (1987, JGR 92, 14987-15001) model D temperature and methane abundance profiles, we are better able to fit the J-band 43-deg. south bright band with the new coefficients (chi-square=205, vs. 315 for Irwin), with the pressure of the upper tropospheric cloud decreasing to 1.6 bars (from 2.4 bars using Irwin coefficients). Improvements in fitting H-band spectra from the same latitude are not as readily obtained. Derived upper tropospheric cloud pressures are very similar using the two absorption datasets (1.6-1.7 bars), but the character of the fits differs. New Karkoschka and Tomasko coefficients better fit some details in the 1.5-1.58 micron region, but Irwin fits the broad absorption band wing at 1.61-1.62 microns better, and the fit chi-square values are similar (K&T: 243, Irwin: 220). Results for a higher methane concentration (Lindal et al. model F) were similar. Whether the new coefficients will simply raise derived altitudes across the planet or will result in fundamental changes in structure is as yet unclear. This work was suported by NASA planetary astronomy and planetary atmospheres programs.
We present a survey of the intrinsic UV absorption lines in active galactic nuclei (AGN). We limit our study to the ultraviolet spectra of type 1 AGN with a redshift of z
Orthogonality constrained density functional theory (OCDFT) provides near-edge X-ray absorption (NEXAS) spectra of first-row elements within one electronvolt from experimental values. However, with increasing atomic number, scalar relativistic effects become the dominant source of error in a nonrelativistic OCDFT treatment of core-valence excitations. In this work we report a novel implementation of the spin-free exact-two-component (X2C) one-electron treatment of scalar relativistic effects and its combination with a recently developed OCDFT approach to compute a manifold of core-valence excited states. The inclusion of scalar relativistic effects in OCDFT reduces the mean absolute error of second-row elements core-valence excitations from 10.3 to 2.3 eV. For all the excitations considered, the results from X2C calculations are also found to be in excellent agreement with those from low-order spin-free Douglas-Kroll-Hess relativistic Hamiltonians. The X2C-OCDFT NEXAS spectra of three organotitanium complexes (TiCl4, TiCpCl3, TiCp2Cl2) are in very good agreement with unshifted experimental results and show a maximum absolute error of 5-6 eV. In addition, a decomposition of the total transition dipole moment into partial atomic contributions is proposed and applied to analyze the nature of the Ti pre-edge transitions in the three organotitanium complexes.