Krajnovic et al. (2020) presents HST/WFC3 and HST/ACS observations of 12 galaxies from the ATLAS3D sample. The HST/WFC3 images are centered on the nucleaus of the galaxy, while HST/ACS images are executed in parallel mode and point 360" away from the nuclei. Specific information about the data reduction can be found in Krajnovic et al.
The booklet contains the submitted abstracts for the conference. Some contributions were not presented in the conference, others were late additions.
Each presented contribution, where the authors submitted their slides or poster have been given a separate DOI.
Photographic emulsion is a non-linear light detector which makes it difficult to perform photometry with digitized plates using conventional software. Inexpensive flatbed scanners (often used to digitize plates) provide image quality acceptable for photometry, but introduce complex image distortions (notably, the hacksaw pattern) that complicate astrometry and source identification. VaST is a photometry package designed from the ground up to handle such images. It relies on SExtractor for source detection/photometry, matches source lists derived from plates exposed at different epochs and cross-calibrates their magnitude scales to construct lightcurves of all the detected objects. An array of statistical methods can be applied to these lightcurves to identify variable objects. Accurate celestial positions of variable objects are measured by using nearby sources to compute local corrections to the approximate plate solution obtained with Astrometry.net. VaST is used mostly with the Moscow collection plates, but is intended to be a general-purpose tool for lightcurve extraction from a series of digitized photographic images.
We will describe the capabilities of the Observatorium Wendelstein (University of Munich,LMU), mainly of its 2m telescope with its three operational imaging and spectroscopic instruments. We will describe their performances based on a few science examples, partly survey type programs. Finally, we will discuss strategies how to benefit from the
Wendelstein Observatory in times of up-coming new major astronomy resources.
The Transiting Exoplanet Survey Satellite (TESS) has been gathering light curves for thousands of
nearby stars. Although its primary goal is to find planets, the 2-minute cadence light curves
obtained by TESS for pre-selected stars, with precision better than 1 percent, are also ideal to search
for variability effects caused by a binary companion, such as reflection and eclipses. The
brightness of TESS pre-selected targets also makes them ideal for ground-based follow-up,
allowing for thorough characterisation of the observed systems and providing constraints for
binary evolution models. In this talk, we will show recent discoveries in the field of compact
binary stars made possible by TESS, as well as discuss the desired follow-up observations for these
In this paper we are presenting optical telescopes of Astronomical Observatory of I. I. Mechnikov Odessa National University. We are describing technical characteristics and scientific program for each telescope. Here we also present a description of the tools with which the unique collections of astroplates were obtained under the program “The Sky Service”. Odessa Observatory (46.28 N, 30.45 E, altitude 64 m, observation code 086) its outlying observation posts: Mayaki (46.39 N, 30.27 E, altitude 25 m, observation code 583) and Kryzhanovka (46.37 N, 30.48 E, altitude 40 m, observation code A85) have a good geographical location (southwestern part of the territory of Ukraine), as well as a good astroclimate (up to 200 clear nights). Telescopes are equipped with modern CCD and PMT light detectors. Odessa Observatory has its own mechanical and optical workshops which are used to create new telescopes and manufacture and repair of other astronomical equipment.
The Arts and Humanities are among the early adopters of computer technology. In the late 1940s, the linguist and Jesuit Father Roberto Busa S.J. convinced Thomas J Watson and IBM that the exploration of Thomas Aquinas' works could be more efficient using new digital methods. The index Thomisticus and the Corpus Thomisticum - a digital lemmatized collection of all works of Thomas Aquinas have gone through all phases of technological development - via punched cards, magnetic tapes and the WWW - and are still accessible today. Since then, a multitude of artifacts and resources have been digitized, so that by now although only a fraction of the entire cultural heritage is digitally available, a critical mass for the development of digital research methods nevertheless exists. The talk will show exemplary which strategies Digital Humanities use to generate, interlink and explore knowledge from historical sources.
Digitizing an archive of photographic plates yields a set of image files and accompanying metadata files. To handle and process these data efficiently, we have developed a Python package PyPlate. PyPlate provides methods to read data from CSV and FITS files, to make calculations with various observation timestamps, to create consistent and easily readable FITS headers, to write plate metadata into a database, to extract sources from plate images, to carry out astrometric and photometric calibration on the extracted sources, and to output the source data to a database or files on disk. We will show how the PyPlate software was used for building the APPLAUSE database and discuss how it can be applied elsewhere.
In this talk, I will describe the efforts done by the Wendelstein observatory in following up known exoplanets and planet candidates both spectroscopically and photometrically. We are currently installing a high-resolution spectrograph, calibrated with an LFC, and a simultaneous 3-channel camera that covers photometric bands between u and Ks. With the latter, we are currently performing a transit survey where we observe primary and secondary in order to determine their Transit Colour Signature (TraCS).