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The 8 most recent public experiments

Mohammad M. Rahman, Mayra A. Machuca, Mohammad F. Khan, Christopher K. Barlow, Ralf B. Schittenhelm, Anna Roujeinikova  

Mass spectrometry data supporting the publication: Molecular Basis of Unexpected Specificity of ABC Transporter-Associated Substrate-Binding Protein DppA from Helicobacter pylori, Mohammad M. Rahman et al., Journal of Bacteriology, Vol 201, Issue 20, e00400-19. DOI:10.1128/JB.00400-19 A detailed description of the data processing and location of files may be found in the Read Me.

Blake T. Riley, Sheena McGowan, Ashley M. Buckle  

Crystallisation & diffraction experiment details available in PDB:6nvb. If you use this data, please cite: Acta Cryst. (2019) F75, Crystal structure of the inhibitor-free form of the serine protease kallikrein-4 B. T. Riley, D. E. Hoke, S. McGowan & A. M. Buckle.

Blake T. Riley, Xingchen Chen, David E. Hoke, Ashley M. Buckle, Jonathan M. Harris  

If you use this data, please cite: Chen, X. et al. Potent, multi-target serine protease inhibition achieved by a simplified β-sheet motif. PLoS One 14, e0210842 (2019). Processed data available at PDB:6bvh. Crystallisation & diffraction experiment details below: --- Crystallisation: - Protein solution: 20 mg/mL bovine trypsin, 50 mM MES pH 6.0, 50 mM benzamidine, 1mM CaCl2 - Reservoir buffer: 2.3 M (NH4)2SO4 and 0.1M MES pH 6.0 Sitting drops: 4 μL protein solution & 4 μL reservoir buffer, at room temperature Crystal soaking: - Inhibitor exchange buffer: 0.1 M MES, pH 6.0, 2.5 M (NH4)2SO4, 1 mM CaCl2 - Process: 6 hours in inhibitor exchange buffer, 48 hours in fresh inhibitor exchange buffer + saturating SFTI-TCTR(N12,N14) cyclopeptide rinse 3 times in 10 μL fresh inhibitor exchange buffer Cryoprotectant: - 0.1 M MES, pH 6.0, 2.5 M (NH4)2SO4, 1 mM CaCl2, 20 v/v% glycerol - Flash frozen in LN2 Irradiation source: ELLIOTT GX-13 Cu Kα rotating anode, λ=1.542 Å, 45 kV, 30 mA Cryocooling: 100 K N2 vapour stream Capture source: RIGAKU RAXIS IV++ Image Plate, Monash University

Marcus J. Kitchen, Genevieve A. Buckley, Timur E. Gureyev, Megan J. Wallace, Nico Andres-Thio, Kentaro Uesugi, Naoto Yagi, and Stuart B. Hooper  

Please cite: Kitchen, M. J., Buckley, G. A., Gureyev, T. E., Wallace, M. J., Andres-Thio, N., Uesugi, K., Yagi, N., & Hooper, S B. CT dose reduction factors in the thousands using X-ray phase contrast. Scientific Reports 7, 15953. (2017). Dataset information: ttps:// Uploader: Genevieve_PC User folder name: bapcxi Uploaded from: MU00017665:E:\MyTardis_data\LowDose_CT_data

These tables contain second order polynomial coefficients for calculating galaxy absolute magnitudes in the redshift range 0 < z < 1.2 from single observed colors using the method of Beare et al. 2014 (ApJ, 797, 104). These coefficients are used to calculate absolute magnitudes in "The z < 1.2 optical luminosity function for a sample of ~410 000 galaxies in Bootes" (Beare, R.A., Brown, M. J. I., & Pimbblet, K., submitted to ApJ) and in a forthcoming paper by the same authors: "Evolution of the stellar mass function and the infrared luminosity function of galaxies since z = 1.2". The tables assume h = 0.7 and Omega_0 = 0.3. Tables are provided for determining the following absolute magnitudes: Bessell U, B, V, R and I; NEWFIRM J; Johnson K; Sloan g, r and i. Observed colors are derived from the following apparent magnitudes: NDWFS Bw; Bessell R and I; NEWFIRM J and Ks; IRAC [3.6 micron] and [4.5 micron]. The recommended colors for different absolute magnitudes and redshift ranges are as follows: abs U (Bessell) z = 0.0 to 0.8:(Bw − R) z = 0.8 to 1.2: (R − I) abs B (Bessell) z = 0.0 to 0.4:(Bw − R) z = 0.4 to 0.8: (R − I) z = 0.8 to 1.2: (I − J) abs V (Bessell) z = 0.0 to 0.5: (R − I) z = 0.5 to 1.2: (I − J) abs R (Bessell) z = 0.0 to 0.19: (R − I) z = 0.19 to 1.2: (I − J) abs I (Bessell) z = 0.0 to 0.46: (I − J) z = 0.46 to 1.2: (R − J) abs J (NEWFIRM) z = 0.0 to 0.53: (R − I) z = 0.53 to 1.2: (I − J) abs K (Johnson) z = 0.0 to 0.6: (Ks − ch1) where ch1 = [3.6 micron] z = 0.56 to 1.2: (ch1 - ch2) ) where ch1 = [3.6 micron] and ch2 = [4.5 micron] abs u (Sloan u) z = 0.0 to 1.2:(Bw − R) abs gs (Sloan g) z = 0.0 to 0.5:(Bw − R) z = 0.45 to 0.8: (R − I) z = 0.8 to 1.2: (I − J) abs rs (Sloan r) z = 0.0 to 1.2: (R − J) abs is (Sloan i) z = 0.0 to 0.7: (I − J) z = 0.7 to 1.2: (J − Ks) abs zs (Sloan z) z = 0.0 to 1.2: (J − Ks)

This archive contains data in CSV format from Tables 2 to 6 of, "An accurate new method of calculating absolute magnitudes and K-corrections applied to the Sloan filter set", (Beare, R., Brown, M. J. I., & Pimbblet, K. 2014, ApJ, 797, 104). The 10 tables list second order polynomial coefficients for use in determining absolute magnitudes from observed colors, two alternative colors being given for each of the Sloan u, g, r, i, z-bands, as described in the paper. The tables assume h = 0.7 and Omega_0 = 0.3. The recommended colors for different absolute magnitudes and redshift ranges are as follows: abs u z = 0.0 to 0.5: (u − g) preferred, (g − r) alternative abs g z = 0.0 to 0.34:(g − r) z = 0.34 to 0.5: (r − i) abs r z = 0.0 to 0.25 (g − i) z = 0.25 to 0.5 (r − z) abs i z = 0.0 to 0.5: (r − z) preferred, (g − i) alternative abs z z = 0.0 to 0.5: (r − z) preferred, (g − i) alternative ABSTRACT We describe an accurate new method for determining absolute magnitudes, and hence also K-corrections, which is simpler than most previous methods, being based on a quadratic function of just one suitably chosen observed color. The method relies on the extensive and accurate new set of 129 empirical galaxy template SEDs from Brown et al. (2014). A key advantage of our method is that we can reliably estimate random errors in computed absolute magnitudes due to galaxy diversity, photometric error and redshift error. We derive K-corrections for the five Sloan Digital Sky Survey filters and provide parameter tables for use by the astronomical community. Using the New York Value-Added Galaxy Catalog we compare our K-corrections with those from kcorrect. Our K-corrections produce absolute magnitudes that are generally in good agreement with kcorrect. Absolute g, r, i, z-band magnitudes differ by less than 0.02 mag, and those in the u-band by ~0.04 mag. The evolution of rest-frame colors as a function of redshift is better behaved using our method, with relatively few galaxies being assigned anomalously red colors and a tight red sequence being observed across the whole 0.0 < z < 0.5 redshift range.

Full methods and results for the ALE meta-analysis of task-switching fMRI studies presented in Jamadar, Thienel, Karayanidis (2014)

Michael J. I. Brown, John Moustakas, J.-D. T. Smith, Elisabete da Cunha, T. H. Jarrett, Masatoshi Imanishi, Lee Armus, Bernhard R. Brandl, J. E. G. Peek  

This is the archive for "An Atlas of Galaxy Spectral Energy Distributions From The UV to the Mid-Infrared". The first folder contains the spectral energy distributions and csv tables of galaxy information, photometry and foreground dust extinction values. The folders named after individual galaxies contain the images from which the photometry was measured. The relevant paper was published in the Astrophysical Journal Supplement Series and is available via A brief video introduction to the atlas is available via The beta version of the atlas, which was released when the paper was submitted, is available via The abstract of the paper follows. We present an atlas of 129 spectral energy distributions for nearby galaxies, with wavelength coverage spanning from the ultraviolet to the mid-infrared. Our atlas spans a broad range of galaxy types, including ellipticals, spirals, merging galaxies, blue compact dwarfs, and luminous infrared galaxies. We have combined ground-based optical drift-scan spectrophotometry with infrared spectroscopy from Spitzer and Akari with gaps in spectral coverage being filled using Multi-wavelength Analysis of Galaxy Physical Properties spectral energy distribution models. The spectroscopy and models were normalized, constrained, and verified with matched-aperture photometry measured from Swift, Galaxy Evolution Explorer, Sloan Digital Sky Survey, Two Micron All Sky Survey, Spitzer, and Wide-field Infrared Space Explorer images. The availability of 26 photometric bands allowed us to identify and mitigate systematic errors present in the data. Comparison of our spectral energy distributions with other template libraries and the observed colors of galaxies indicates that we have smaller systematic errors than existing atlases, while spanning a broader range of galaxy types. Relative to the prior literature, our atlas will provide improved K-corrections, photometric redshifts, and star-formation rate calibrations.