R. Vavrek's research while affiliated with Netherlands Space Office and other places

... Liaudat et al. proposed the multi-CCD PSF modeling method applied to telescope imaging observations of galaxies [18]. The team of the Euclid mission used a Shack-Hartmann sensor to measure wave aberration and evaluated the image quality by comparing it with the PSF [19]. ...

... Accurate measurement of background noise is also a serious issue for imaging science, where for example bad pixels, background noise, and uncertainties in the detector systematics limit sensitivity of aperture masking interferometry and kernel phase, 38 and for low-surface-brightness science such as with Euclid. 39 In each case it is normal for detectors to be rigorously calibrated on the ground before flight, and with dedicated observations in space; but at the levels of contrast and resolution required for aperture masking on JWST (ideally 10 −4 at a few λ/D) even small residual miscalibrations can seriously affect performance 2 and we require some method of self-calibration from science data themselves. ...

... In addition to providing tight constraints on the Universe expansion history, one of the major roles of current [1,2] or future spectroscopic surveys [3,4] is to provide an accurate measurement of the amount of primordial non-gaussianity (PNG) generated during inflation. In particular, these surveys will be focused on the well-known local PNG parameterized by f loc NL [5] such that the primordial gravitational potential field Φ(x) reads ...

... However, bypassing ground testing was a considerable risk, and today, such testing is deemed essential [9][10][11][12] . In fact, several space instruments, including GAIA 13 , TIRS 14,15 , and more recently Euclid [16][17][18] , have encountered unexpected SL issues after being deployed in space. When this happens, only limited mitigation methods can be implemented 13 , making SL a potential cause of mission failure. ...

... While the theoretical performances of the payload were extensively computed and simulated [7] , the actual performances after integration and alignment remained to be determined and compared to the predictions. The validation and qualification plan of the payload, performances wise, comprises two sequential steps: 1) determination of the optical performance of the telescope alone is first determined in ambient conditions after the final alignment which includes the search for the best focus with M2; 2) verification in thermo-vacuum conditions, after integration of the instruments with the telescope, of the stability of the alignment and testing of the optical performances. ...

... Fig.4 shows the resultant / accumulation for the CIB dipole components in each band for the two missions. (For the Euclid example we used the projected sky coverage from Laureijs et al. (2020). For Roman the area that will be observed has not been yet finalized. ...

... Systems engineers are living in a generation wherein modern systems are growing in complexity [4,5]. MBSE is the proposed solution by the researchers to cope with system complexity in a variety of SOI [6,7]. Various MBSE methodologies have been developed in recent years. ...

... We consider microlensing events with a peak time t 0 set to be the center of the WFIRST observations. Euclid will have more restrictive observing constraints and can only observe the same fields as WFIRST continuously for 20 days in a window centered 10 days earlier or later than WFIRST's window center (Gómez-Alvarez et al. 2018). ...

... Space telescopes such as Hubble [1], James Webb [2] or Euclid [3] provide breathtaking views of galactic fields and nebulae with unprecedented clarity, making astronomy more attractive to the media and the general public. This is encouraging a growing number of people to take an interest and to equip themselves to observe the night sky, but there are several challenges to be overcome. ...

... Specifically, the Euclid Wide Survey (WS) will observe ∼15,000 deg 2 of the sky down to a flux limit of ∼2 × 10 −16 erg cm −2 s −1 (Euclid Collaboration et al. 2022), while the Roman HLS will observe ∼2200 deg 2 down to a flux limit of ∼6 × 10 −17 erg cm −2 s −1 (Spergel et al. 2015). The Euclid Deep Survey will observe 50 deg 2 in three fields to a similar flux limit (Vavrek et al. 2016). ...