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We share the following new configuration files for JWST NIRISS Slitless Spectroscopy: F115W + GR150C F115W + GR150R F150W + GR150C F150W + GR150R F200W + GR150C F200W + GR150R We use JWST comissioning data from program 1085, the NIRISS-FOCUS-FIELD, which are observations of the outer LMC. We optimise Grizli model fits to the grism spectra of stars in individual exposures with MAG_AUTO < 21.5 and 1 < FLUX_RADIUS < 2 that have the positions x_flt and y_flt in the associated direct image (in the rotated Grizli dispersed frame). In each case, we get best fits to DYDX_A_0 (trace centre in y) and DLDP_A_0 (wavelength zeropoint in x). These parameters are measured in the Grizli convention where all spectra have been rotated to have the dispersion roughly parallel to array rows and with wavelength increasing "toward the right". Only those fits with a chi-squared < 50000 are used. The field dependence of these parameters across the detector are fit with a low-order 2D Polynomial model with astropy.modeling.models.Polynomial2D. Degree = 2 is used for the more sparsely sampled F200W and degree = 3 is used for the the bluer filters that better fill the detector frame. These fits are then iterated to remove outliers. New coefficients for DYDX_{}_0 and DLDP_{}_0 are calculated and provided in the configuration files in this release. PNG files show the field dependence for each parameter in each filter + grism combination. List of files available in the tar file GR150C.F115W.221215.conf GR150C.F150W.221215.conf GR150C.F200W.221215.conf GR150R.F115W.221215.conf GR150R.F150W.221215.conf GR150R.F200W.221215.conf f115w_gr150c_dldp_a_0.png f115w_gr150c_dydx_a_0.png f115w_gr150r_dldp_a_0.png f115w_gr150r_dydx_a_0.png f150w_gr150c_dldp_a_0.png f150w_gr150c_dydx_a_0.png f150w_gr150r_dldp_a_0.png f150w_gr150r_dydx_a_0.png f200w_gr150c_dldp_a_0.png f200w_gr150c_dydx_a_0.png f200w_gr150r_dldp_a_0.png f200w_gr150r_dydx_a_0.png Installation Download the tar file into the CONF directory of your Grizli installation and unpack. An example of how to do this in python is shown below. import os import grizli os.chdir(os.path.join(grizli.GRIZLI_PATH, 'CONF')) if not os.path.exists('GR150C.F115W.221215.conf'): os.system('wget "https://zenodo.org/record/7447545/files/niriss_config_221215.tar.gz?download=1" -O niriss_config_221215.tar.gz') os.system('tar xzvf niriss_config_221215.tar.gz')

SPEX is a software package for fitting astrophysical X-ray spectra. It has been developed since the 1970s at SRON Netherlands Institute for Space Research. SPEX is an interactive command-line program for the computation of emergent spectra of optically thin plasmas such as stellar coronal loop structures, supernova remnants (also including transient ionization effects), photo-ionized plasmas, and optically thick plasmas. These model spectra can be fitted to measured X-ray spectra from various X-ray observatories, like XMM-Newton and Chandra. SPEX has been optimized for high-resolution X-ray spectroscopy, which makes it especially suitable for analyzing grating and micro-calorimeter spectra.

The aim of the project VITAMINE_5G is to develop an inline process monitoring system for the process of laser metal deposition with wire (LMD-w). Using 5G, the aggregated data is transmitted latency-free in the Fraunhofer Edge-Cloud. By transferring the visualized data to VR glasses, immersive remote monitoring of the process is enabled.

A Python framework to combine existing astrophysical simulation codes in numerical experiments. With AMUSE you can simulate objects such as star clusters, proto-planetary disks and galaxies.

This volume, Volume 2, is a supplementary text and consists of a text edition of his astronomical legacy, prepared for the printing press in the 1650s, but only now finalized and published. Volume 1 presents Marggrafe’s biography.

The design, development, and fabrication of a 67.5 kHz capacitive micromachined ultrasonic transducer (CMUT) suited for Martian anemometry is presented in this thesis. The CMUT is a clamped membrane structure that vibrates on the application of an electric field, generating ultrasound. The Martian environment is 95 % carbon dioxide (CO2) with atmospheric pressures around ~ 600 Pa. This produces a high mismatch at the device-air interface leading to higher ultrasonic signal attenuation. To have lower signal attenuation in such conditions, the device's operating frequency is limited to 100 kHz. The CMUTs capable of generating frequencies less than 100 kHz either needed a larger Silicon area or higher operating voltages. This is a problem for the portability and the battery operation of the devices, respectively. The devices presented in this thesis are designed and fabricated using low-cost commercially available surface micromachining technique, PolyMUMPs. PolyMUMPs process from MEMSCAP inc. is a three-layer polysilicon surface micromachining process. The CMUT devices proposed in this thesis make use of two out of three polysilicon layers. COMSOL Multiphysics simulations were used to analyze the device's critical design parameters like the operating frequency, breakdown voltage, and frequency response. These simulations helped investigate the operability of devices under the Martian environment. Simulation results show that the designed single cell 170-μm radius membrane had a resonant frequency of 68 kHz. The device exhibits a static displacement of ~90 nm under 16 V DC bias. Using the developed single cell model, an 8×10 array CMUT anemometer was fabricated and evaluated that resonated at 67.5 kHz frequency in the lab environment. This proposed CMUT anemometer can operate for a supply <38 V. The acoustic performance of the device was evaluated by using a commercial air-coupled capacitive microphone, CAP1, and with another similar CMUT chip in the lab environment. Successful transmit-receive of ultrasound from the developed 2D array to CAP1 and another CMUT chip for separation in the range of 1-16 cm were performed from the pitch-catch experiments. The parameters like the speed of sound, near/far field transition point, and attenuation were found for each case. The experimental results show that the parameters can be accurately measured this developed technology with a ±2% accuracy. Anemometry using the developed CMUT chips was performed using the pitch-catch experimental setup having a 10 cm separation between the two chips. Air pressure was directed towards the chips to imitate wind-like conditions. The pressurized air was directed to the transmitter first and later on the receiver to have the anemometry measurements. Accurate measurements were made with the help of the CMUT system. The pressurized air was later directed at different angles, and it was found that the chips using the proposed CMUT devices were responsive to the angular winds. This property enables the CMUT chips to determine the wind direction when connected as a sonic anemometer. A comparison of the CMUT-based system with the commercial anemometer was made and same results were obtained.

A gallery of the visualizations of the 41 primary sources (figures from the respective papers) referenced in the systematic literature review: "Visualizations for the Evolution of Variant-Rich Systems: A Systematic Mapping Study"

Supplementary Material. Title of the paper "Immersive Virtual Reality to improve the competence to manage classroom climate in secondary schools". Published in the journal Educación XX1, 26, nº1 (2023)