Truncation of AGN jets by their interaction with an stellar cluster

Anabella Araudo, Astronomical Institute of the Czech Academy of Sciences, 2018-04-16 - 2018-04-19


We are interested in the effects of interaction of jets in Active Galactic Nuclei when they encounter various obstacles, namely, stars in Nuclear Star Cluster surrounding the nucleus and globular clusters passing across the inner jet, as well as dense clouds from the Broad Line Region. The interaction provides a scenario to address
non–thermal processes. In jet–star interactions a double bow–shock
structure is formed where particles get accelerated via diffusive
mechanism. Individual encounters have a limited effect, however, dense
clusters of massive stars can truncate the jet as the cluster crosses the
jet line near the jet launching region. Much of the jet kinetic energy
density is transferred to the shock and it becomes available to accelerate
particles. We conclude that the interaction of jets with clusters of
massive stars is a promising way to explain detectable levels of gamma
rays from Fanaroff–Riley class I of edge–brightened radio galaxies.

Fermi GBM transient searches with ADWO

Zsolt Bagoly, Konkoly Observatory, MTA CSFK, 2017-04-03 - 2017-04-06

Time: 20

We present a new method to search for non-triggered, short-duration transients in the data-set of the Fermi\\\'s Gamma-ray Burst Monitor (GBM). The method, called Automatized Detector Weight Optimization (ADWO), combines the data of all available detectors and energy channels, identifying those with the strongest signal. ADWO is ideal to search for electromagnetic (EM) counterparts of gravitational wave (GW) events, when the time of the event is well known from the GW-detectors\\\' observation as well as for identifying non-triggered short gamma-ray bursts (SGRBs). We have successfully identified short GRBS, and possible EM counterparts of GW transients GW150914 and LVT151012.

The 2013 outburst of KS 1947+300 as seen by Suzaku

Ralf Ballhausen, Dr. Karl Remeis-Observatory & ECAP, 2015-04-20 - 2015-04-24

Time: 20 min

KS 1947+300 is a transient X-ray binary consisting of a neutron star and a Be companion. The system underwent an outburst in 2013 after more than 10 years of quiescence, reaching a peak luminosity of ∼300 mCrab in the Swift/BAT band. We present a detailed study of two Suzaku observations of this outburst. The pulse profiles are found to
be highly energy-dependent showing an unusual evolution from one broad peak to two peaks towards higher energies. The continuum is modeled with an absorbed powerlaw with a high-energy cut-off and an additional blackbody component. We find indications
for the presence of fluorescent emission from both neutral and He-like iron, which is the first time multiple ionization states of iron are detected in this source. The pulse phase-resolved spectral analysis shows moderate spectral variation over pulse phase, involving both continuum components as well as the strength of the absorption. Determining the source-intrinsic variability is complicated by artificial parameter correlations of the
empirical continuum model. Taking these effects into account, we discuss spectral differences for different viewing angles as well as possible intrinsic parameter correlations.

Recent Advances in the UWE satellite series

Philip Bangert, Zentrum für Telematik, 2015-04-24 - 2015-04-24

Time: 20 Min

Recent advances in the University Würzburg Experimental satellite programm are the focus of this presentation. The UWE-3 satellite was launched in November 2013 and a short overview over the operational aspects since then will be given. An extensive software update on all satellite subsystems in February 2015 opened up new features and operational capabilities, mostly related to attitude control, of which in-orbit results will be presented. Besides the operation of UWE-3, the successor satellite UWE-4 and plans for future developments will be introduced.

A Suzaku, NuSTAR and XMM-Newton view on variable absorption and relativistic reflection in NGC 4151

Tobias Beuchert, Dr. Remeis Observatory & ECAP, 2017-04-04 - 2017-04-05

Time: 15

We disentangle X-ray disk reflection from complex line-of-sight absorption in NGC 4151 using Suzaku, NuSTAR, and XMM-Newton. Extending upon Keck et al. (2015), we develop a physically-motivated baseline model using the latest lamp-post reflection code relxillCp_lp, which includes a Comptonization continuum. We identify two components at heights of 1.2 and 15.0 gravitational radii using a long-look simultaneous Suzaku/NuSTAR observation but argue for a vertically extended corona as opposed to distinct primary sources. We also find two neutral absorbers (one full-covering and one partial-covering), an ionized absorber (logxi = 2.8), and a highly-ionized ultra-fast outflow, all reported previously. All analyzed spectra are well described by this baseline model. The bulk of the spectral variability on time-scales from days to years can be attributed to changes of both neutral absorbers, which are inversely correlated with the hard X-ray continuum flux. The observed evolution is either consistent with changes in the absorber structure (clumpy absorber in the outer BLR or a dusty radiatively driven wind) or a geometrically stable neutral absorber that becomes increasingly ionized at a rising flux level. The soft X-rays below 1 keV are dominated by photoionized emission from extended gas, which may act as a warm mirror for the nuclear radiation.

SGR and AXP - are they magnetars?

Gennady Bisnovatyi-Kogan, Space Research Institute, Moscow, 20 April 2015 - 24 April 2015

Time: 30-40

Some data are presented about observations of Soft Gamma-ray Repeaters
(SGR) and Anomalous X-ray Pulsars (AXP) in diff erent spectral
regions. It is noted that there are ordinary radiopulsars with very
strong magnetic fields, up to 10^14 Gs, and slow rotation, with periods
 8 seconds, which don\\\'t show any pecularity, or diff erences from a
stardard radiopuslar behaviour.
From the other side there are SGR with normal pulsar field ,
 10^12 Gs. The conclusion is made that there is an additional parameter
which determines an unusual behaviour of some neutron stars,
and anomalously small NS mass is suggested as such parameter.
The pulsars activity in the gamma-rays is connected with their relative
youth and is provided by the energy stored in the non-equilibrium
layer located in the crust of low-mass neutron stars. It is shown that
the mass and the thickness of the non-equilibrium layer increase nonlinearly
with decreasing of the NS mass.
The energy release happens due to mixing of the accreted matter
with the matter of the neutron star crust with super heavy nuclei, which
approache the NS surface and become unstable. The nuclear fission in
the low-density region initiates chain reactions leading to the nuclear
explosion. The outbursts are likely to be triggered by an instability
developing in the region where the matter accreted by the neutron star
is accumulated at the magnetic pole regions.
A possibility is analysed for an explanation of the phenomenon of
the AXP and SGR within a scenario of fall-back magnetic accretion
onto a young isolated neutron star. The X-ray emission of the pulsar in
this case is originated due to accretion of matter onto the surface of the
neutron star from the highly magnetized accretion disk, surrounding its

Simulator of stellar crowded fields

Martin Blazek, FEE CTU Prague, 2015-04-20 - 2015-04-24

Time: 10

Due to the existence of noise in astronomical data no certainty is given for the existence of mathematically exact result of stellar deconvolution and iterative or other methods such as aperture or profile photometry are commonly used. Iterative methods are important namely in the case of crowded fields (eg. globular clusters). For the tests of efficiency of those iterative methods on various stellar fields information about real fluxes of sources is essential. For that purpose simulator of artificial images with crowded stellar fields brings this initial information of source fluxes for robust statistical comparison of various deconvolution methods. Simulator GlencoeSim consider various settings of Point-Spread Functions, noise types and spatial distributions with the aim to produce as realistic astronomical optical stellar image as possible.

Deconvolution Algorithm WHIDE for Stellar Globullar Clusters

Martin Blazek, Czech Technical University, 2017-04-03 - 2017-04-07

Time: 20

In this talk the results on simulations and data processing based deconvolution is presented. Proposed WHIDE algorithm using Richardson-Lucy deconvolution is useful namely for astrometry and photometry of dense stellar fields such as Globular Clusters.

Bayerisch-Tschechische Hochschulagentur

Radka Bonacková, Bayerisch-Tschechische Hochschulagentur, 2018-04-17 - 2018-04-17

Time: 10 min.

Short presentation about the Bavarian-Czech Academic Agency

Small satellite options for astronomy

Noah Brosch, Tel Aviv University, 2017-04-03 - 2017-04-07

Time: 20

The cubesat philosophy, together with new technological developments, offers interesting possibilities for valuable astronomical investigation while keeping mission costs to a minimum. I will describe work on deployable mirrors that should allow launching mirrors larger than the satellite size, as well as other relatively low-cost solutions for detectors, etc. These in the context of an ultraviolet-imaging nano-satellite.

Long-Wavelength Radio Observations of Blazars

Paul Ray Burd, Uni Würzburg, 2016-04-18 - 2016-04-21


Active Galactic Nuclei (AGN) form plasma jets by accretion of material onto a central supermassive black hole in the center of the galaxy. The particles in the jets are accelerated to highly relativistic energies and bulk-relativistic plasma velocities are evident from the observation of apparent superluminal motion on parsec scales if the jet-inclination angles are small.
Such AGN are referred to as blazars and are subdivided into BL Lac objects and flat spectrum radio quasars (FSRQs).
The jets typically form lobes on kiloparsec scales, which are prominent in radio galaxies, which are considered to be the unbeamed counterparts of blazars.
The unification paradigm of AGN suggests that FSQRs and BL Lacs are the counterparts of FR1 and FR2 radio galaxies at low inclination angles and therefore at low radio frequencies the lobe emission should dominate the beamed flat-spectrum nuclear emission. There are many indications that this is a too simplified picture.
We observe a sample of high-frequency selected beamed blazar jet sources from the MOJAVE sample at low radio frequencies with LOFAR at 120-160 MHz and with the Giant Metrewave Radio Telescope (GMRT) at 610 MHz and compare their long-wavelength properties to higher-frequency radio data.

Long wavelength radio observations of Blazars

Paul Ray Burd, Uni Würzburg, 2017-04-03 - 2017-04-05

Time: 20 minutes

The unification paradigm of AGN suggests that BL Lacs and FSRQs are the counterparts of FR1 and FR2 radio galaxies at low inclination angles and therefore at low radio frequencies, the lobe emission should dominate the beamed flat-spectrum nuclear emission.
The low frequency properties of four high-frequency selected beamed blazar jet sources, from the MOJAVE 1 sample, observed with the Giant Metre Wave Radio Telescope (GMRT) at 610 MHz, are shown.

The Prospects of Machine Learning Algorithms in Radio Astronomy

Paul Ray Burd, Uni Würzburg, 2018-04-16 - 2018-04-18

Time: 20 min

to be submitted

Miniaturized X-ray telescope for VZLUSAT-1 nanosatellite with Timepix detector

Tomáš Báča, Czech Technical University in Prague, -

Time: 15

We present the application of a Timepix detector on the
VZLUSAT-1 nanosatellite. This project aims to verify the practicality of
the detector in conjunction with 1-D Lobster-Eye optics to observe
celestial sources between 5 and 20 keV. A modified USB Lite interface is
used for low-level control of the Timepix. An additional 8-bit Atmel
microcontroller is dedicated for commanding the detector and to process
the data onboard the satellite. We present software methods for onboard
post-processing of captured images, which are suitable for implementation
under the constraints of the low-powered embedded hardware. Several
measuring modes are prepared for different scenarios including single
picture exposure, solar UV-light triggered exposure, and long-term all-sky
monitoring. Following up VZLUSAT-1 project are NASA sounding rocket
experiments. We aim to test a larger telescope (approx. 1 m focal length)
together with Timepix detectors. Sounding rockets provide in-situ
measurement platform, which allows 5-minute experiments with data
recovery. We present results of preliminary experiments conducted at
Pennstate University in 50 m long vacuum tunnel.

On X-Ray orbital data from VZLUSAT-1 nanosatellite

Tomas Báča, Czech Technical University in Prague, 2018-05-16 - 2018-05-20

Time: 25

We present current results of X-Ray camera payload onboard VZLUSAT-1 nanosatellite, the first Czech CubeSat launched into Earth\\\'s orbit. Embedded hardware and software was designed from the ground up to allow real-time image processing, filtering and compressing of captured images onboard the 10 x 10 x 20 cm CubeSat. Together with miniature lobster-eye optics, the satellite can capture X-Ray photons from astronomical objects. The satellite was successfully launched on June 23rd, 2017 to a 510 km Sun-synchronous Low-Earth orbit. The embedded electronics onboard, for the X-Ray and gamma-ray telescope, utilizes the Timepix sensor which also serves as a dosimetric unit. Besides its primary mission, the payload successfully produces data for global maps of ionizing radiation in Low-Earth orbit. Currently, in February 2017 the sensor captured nearly 20 000 images, most of which were successfully downloaded. We will discuss and interpret the measured data in the context of X-Ray astronomy and radiation mapping, which are inherently interconnected.

The X-ray spectral and timing behaviour of the accreting pulsar V0332+53

Maria D. Caballero-Garcia, INAF-OAB, 20/04/14 - 26/04/14


The X-ray emission from accreting stellar-mass black holes in LMXBs has been studied for many decades. This is due to the length of
their X-ray outbursts, which have allowed intensive observing campaigns using data from satellites such as XMM-Newton, Chandra, SWIFT, RXTE, Suzaku, INTEGRAL, etc. In the case of HMXBs, and in particular for accreting X-ray pulsars, their X-ray emission is far from being understood. This is due to their short episodes of X-ray emission and complex physical properties, including strong magnetic fields. In this talk we present some preliminar results from the analysis of the recent outbursts from the Be X-ray pulsar V0332+53.

Initial follow-up of optical transients using BOOTES (part II)

Maria D. Caballero-Garcia, CTU-FEL (Prague), 2015-04-20 - 2015-04-24

Time: 20 min.

Important advances in the astrophysical research community during the recent years have been done thanks to the advent of robotic telescopes. They have been designed to perform continuous observing campaigns of the sky, inverting most of their time in the discovery and classification of new (sometimes unexpected) sources. BOOTES is a world-wide web of (50-60 cm) robotic telescopes that has been developed during the last years. Besides the follow-up of the Gamma-ray Bursts, the main goal is the follow-up of optical transients in the sky (either of known/unknown nature). We will show some of the results obtained from our own observing campaigns.

Initial follow-up of optical transients using BOOTES

Maria D. Caballero-Garcia, INAF-OAB, 20/04/14 - 26/04/14


Currently astronomy is having a precious time (in spite of the critical economical situation) for many reasons. One of them is because the continuous observing campaigns of the sky by telescopes that invert most of their time in the discovery and classification of new sources. This has led to important discoveries led by the astrophysical community in the recent years. BOOTES (Castro-Tirado et al.) is a web of 50-60 cm robotic telescopes distributed around the world and has been developed during the last years. This distribution is unique and allows observing campaigns of a source located anywhere in the sky. We will show that one of the goals is to observe and provide source classification of new (or poorly studied) optical transients.

Implementing an X-ray reverberation model in XSPEC

Maria D. Caballero-Garcia, ASU-CAS (Prague), 2016-03-19 - 2016-03-21

Time: 15 min

X-ray reverberation mapping has been revealed to be a valuable tool for knowing
the physical condition of the accreting black holes and the matter that surrounds them. This is an important case of interest for the exploitation of the data from the next generation of big X-ray satellites (e.g. Athena, Astro-H). Here we present a new theoretical model recently created at Prague, that has been developed for the study of X-ray astronomical data, aimed for its use in both timing and spectroscopy techniques.

First results from the use of the relativistic and slim disc model SLIMULX in XSPEC

Maria Caballero-Garcia, ASU-CAS (Prague), 2017-04-03 - 2017-04-05

Time: 20 min.

Ultra-Luminous X-ray sources (ULXs) are accreting black holes for which their X-ray properties have been seen to be different to the case of stellar-mass black hole binaries. For most of the cases their intrinsic energy spectra are well described by a cold accretion disc (thermal) plus a curved high-energy emission components. The mass of the black hole (BH) derived from the thermal disc component is usually in the range of 100-1000 solar masses, which have led to the idea that this might represent strong evidence of the Intermediate Mass Black Holes (IMBH), proposed to exist by theoretical studies but with no firm detection (as a class) so far. Recent theoretical and observational developments are leading towards the idea that these sources are instead stellar-mass BHs accreting at an unusual super-Eddington regime. In this talk we present a model (SLIMULX) that can be used in XSPEC for the fit of thermal spectra of slim discs around stellar mass black holes in the super-Eddington regime, which consistently takes all relativistic effects into account. Finally I will present the results that we have obtained from the fit of the X-ray spectra from NGC5408 X-1.

The THESEUS mission proposed for the M5 program

Alberto J. Castro-Tirado, IAA-CSIC, 2017-03-04 - 2017-03-06

Time: 15\' or 20\'

I wil present the mission concept for THESEUS, proposed for the ESA M5 Call, with a doublefold goal: i) to detect and follow-up
gamma-ray bursts in X-rays, optical and near-IR and ii) to conduct a deep survey in the X-ray band.

Upgrading RTS2 for high-speed adaptive observing

Ronan Cunniffe, FZU, 2018-04-16 - 2018-04-20

Time: 20 mins

The RTS2 observatory control system (BART, FRAM, BOOTES,
D50....) was designed around the traditional observing model:
pre-scripted observations made by slow cameras. Modern cameras can
achieve video framerates at low noise, with hugely increased data rates
at the price of much more sophisticted image processing. We are working
on re-engineering RTS2\\\'s camera architecture to support
high-performance cameras, and the corresponding data pipeline.
Separately, we are examining how to increase the flexibiility of the
RTS2 programming model, to use this improved feedback in real time.

Long-term Monitoring of Bright TeV Blazars with FACT

Daniela Dorner, Universität Würzburg, 2014-04-22 - 2014-04-26


The First G-APD Cherenkov Telescope (FACT) is operational since October
2011. Since then, more than 4300 hours of data have been recorded. The
major goals of the project are the proof of principle for silicon based
photosensors, aka Geiger-Mode Avalanche Photodiodes (G-APDs), in
Cherenkov Astronomy and the monitoring of bright TeV blazars.

The stable and homogeneous properties of the G-APDs provide a stable
and consistent performance of the detector showing that G-APDs are a
promising alternative as photosensors in a Cherenkov telescope.
Furthermore, observations during strong moon light are possible with
these devices allowing to enlarge the duty cycle of the telescope. This
provides ideal conditions for long-term monitoring.

Among few other sources, mainly the near blazars Mrk421 and Mrk501 have
been monitored with FACT at TeV energies. In the last 2.5 years,
several flaring activities have been detected and FACT participated in
several multi-wavelength campaigns.
With more than 450 hours for Mrk 421 and more than 600 hours from Mrk
510, FACT provides a very complete data sample where for both sources
more than 250 nights are covered.
With this data sample, studies on the flare behaviour and duty cycle of
the observed blazars can be carried out.

Results from 2.5 years of monitoring will be presented.

FACT - Result from More than Four Years of Monitoring

Daniela Dorner, Uni Würzburg, FAU Erlangen, 2016-04-18 - 2016-04-21

Time: 20

Since October 2011, the First G-APD Cherenkov Telescope (FACT) has been observing at TeV energies. The major goal of the project is the long-term monitoring of bright TeV blazars. In the last 4.5 years, more than 6200 hours of physics data have been collected. Using a camera with silicon based photosensors (SiPMs, aka G-APDs), observations during bright ambient light are carried out regularly without degradation of the sensors. Like this observational gaps are closed providing a denser and more regular data sample and enlarging the duty cycle of the instrument. Keeping the gain of the SiPMs stable with an online feedback system, a stable and homogeneous detector performance is achieved. Based on this and an automatic data taking procedure, the duty cycle of the instrument is increased further. An unbiased long-term data sample is achieved by an observing strategy to monitor a small sample of sources as much and as regularly as possible. An automatic quick look analysis provides results shortly after the data are taken allowing to send flare alerts within the same night. This allows for coordinated Target-of-Opportunity (ToO) observations and multi-wavelength (MWL) observations of interesting events.

Blazars are extremely variable objects emitting radiation across the electromagnetic spectrum. For the understanding of the emission mechanisms, simultaneous MWL bservations are crucial. Observations at very high energies are important to distinguish between different emission models. Therefore, FACT is an ideal instrument for studying TeV blazars in the MWL context.

Being bright at TeV energies, the blazars Mrk 421 and Mrk 501 are the main targets for FACT. They are monitored since January 2012 for a total of more than 1200 hours each and showed several flaring activities during that time. In addition, several other sources like for example the Crab Nebula, 1ES 1959+650 and 1ES 2344+54.1 are observed regularly.
1ES 1959+650 showed an enhanced flux in autumn 2015 when also bright outbursts at X-ray energies were measured with Swift. Mrk 501 underwent major outbursts in June 2012 and June 2014 during the yearly MWL campaigns. Mrk 421 showed a bright flare in April 2013 during which also a large MWL data sample is available. In December 2015, a smaller flare was registered, and within a ToO program, Integral and Swift observations were triggered to study the spectral energy distributions.
In this presentation, the results from more than four years of monitoring will be summarized and discussed in the MWL context.

M@TE - Monitoring at TeV Energies

Daniela Dorner, Uni Würzburg, FAU Erlangen, 2016-04-18 - 2016-04-21

Time: 10

Blazars are extremely variable objects emitting radiation across the electromagnetic spectrum and showing variability on time scales from minutes to years. For the understanding of the emission mechanisms, simultaneous multi-wavelength observations are crucial. Observations at very high energies are important to distinguish between different emission models. Furthermore, an unbiased data sample is needed to study the duty cycle of the objects.

A dedicated long-term monitoring program at TeV energies has been started by the FACT project more than four years ago. The success of the project nicely showed that the usage of silicon based photo sensors (SiPMs) is ideally suited for long-term monitoring, as they provide not only an excellent and stable detector performance, but also allow for observations during bright ambient light like full moon. This allows to increase the duty cycle of the instrument and close observational gaps. Due to the rotation of the Earth, the observation time in one site is limited to six hours. This makes it difficult to study typical variability time scales of few hours to one day. Therefore, the ultimate goal is 24/7 monitoring with a network of small telescopes around the globe (DWARF project).

The installation of an Imaging Air Cherenkov Telescope is planned at the site in San Pedro Martir in Mexico. For the M@TE (Monitoring at TeV energies) telescope, a mount from a previous experiment is being refurbished and will be equipped with a camera using the new generation of SiPMs. In the presentation, the status of the M@TE project will be reported and the scientific potential, including the possibility to extend monitoring campaigns to 12 hours by coordinated observations together with FACT, will be outlined.

Flaring Activity of 1ES 1959+650 at High Energies

Daniela Dorner, Uni Würzburg, FAU Erlangen, 2016-04-18 - 2016-04-21

Time: 10

In autumn 2015, the high frequency peaked BL Lac type object 1ES 1959+650 showed enhanced flux both in the X-ray and gamma-ray regime. The source was observed regularly with the X-ray Telescope onboard of the Swift satellite from August 2015 till January 2016. From the long-term monitoring of the First G-APD Cherenkov Telescope (FACT), more than 150 hours of observations are available in that time range. These data were analyzed in the multi-wavelength (MWL) context together with the Fermi data. In X-rays, a new highest historical count rate was measured. While simultaneous flaring activity is found in the optical and gamma-rays, there is also one flare in the gamma-ray regime without significant counterpart in the low energy peak of the spectral energy distribution. In the presentation, results from the MWL analysis will be discussed.

Radiation environment measurement onboard nanosatellite VZLUSAT1

Vladimír Dániel, Výzkumný a zkušební letecký ústav, -


Onboard nanosatellite VZLUSAT1 the Radiation Hardened Composites Housing (RHCH) material will be verified. For RHCH radiation properties evaluation the radiation environment sensors are used. Three XRB diodes are placed on the side wall of the nanosatellite. First sensor is placed without RHCH shielding, second with 1mm thick RHCH shield and third with 2mm thick RHCH shielding. For higher energies the spectral sensors based on CdTe material will be used inside the nanosatellite. The appropriate measurement electronics circuit is presented.

VZLUSAT-1 EQM and PFM testing campaign

Vladimír Dániel, Aerospace Research and Test Establishment, 2015-04-21 - 2015-04-24

Time: 15 minutes

The testing campaign of EQM and PFM model of 2U CubeSat VZLUSAT-1 is presented. The EQM testing campaign take part in the Q4 of 2014, the PFM campaign is planned to Q1 and Q2 of 2015. The testing campaign includes assembly of the nanosatellite in the cleanroom, functional testing of platform and payloads, vibration and shock tests and thermal vacuum testing. For the PFM the testing campaign includes also the end to end test of radio communication with ground segment.

VZLUSAT-1 CubeSat demonstration

Vladimír Dániel, Aerospace research and test establishment, 2016-04-18 - 2016-04-21

Time: 60

VZLUSAT-1 is a Czech 2U CubeSat type technological nanosatellites for the in-orbit demonstration of new technologies and products in Earth orbit. Demonstration of the Engineering Model (EM) of the VZLUSAT-1 will be presented. The demonstrator is assembled from the EM of the OBC, Miniaturized X-ray telescope with deployable optics and In-orbit demonstrator of Radiation hardened composite housing material (RHCH). The presentation will be done in the form of workshop including the real-time operation via umbilical connector and also the using the ground segment SW. Presentation also shows the details of observation modes, details about detectors, data processing and handling system and mission details. The presented Miniaturized X-ray telescope instrument is suitable for the astrophysical, Sun, moon, terrestrial gamma flash observation or radiation background monitoring. The In-orbit demonstrator of the RHCH is suitable for shielding the space radiation of the satellites, manned spacecrafts or habitats for the moon or mars. The CubeSat launch is planned to summer 2016 to 460km LEO.

Miniaturized X-ray telescope CubeSat payload for astrophysics, searching of gravitational waves sources or cometary mining

Vladimír Dániel, Aerospace research and test establishment, 2017-04-04 - 2017-04-06

Time: 15

The presentation describe the CubeSat idea with x-ray telescope targeting the astrophysics, searching of gravitational waves sources or cometary mining. Even there are three different topics the similarities and possible usage of same instrument will be discussed.

Lessons learnd from VZLUSAT-1 CubeSat mission

Vladimír Dániel, Czech Aerospace Research Centre, 2018-04-18 - 2018-04-19

Time: 15

Brief summary of the flight phase of VZLUSAT-1 CubeSat will be presented. The CubeSat VZLUSAT-1 was launched on June 2017 and is still operating on the orbit. The Operations, OBC, ADCS and Payload behaviour will be summarized.

Photometry at FRAM

Jan Ebr, Fyzikální ústav AV ČR, 2018-04-17 - 2018-04-18

Time: 10min

I will talk about photometric measurements at obotic telescopes used for atmospheric monitoring at astroparticle observatories.

Modelling X-ray beacons in curved space time

Sebastian Falkner, Dr. Karl Remeis Observatory & ECAP, 2017-04-04 - 2017-04-05

Time: 15+5

In accreting X-ray pulsars, strong magnetic fields funnel matter onto the magnetic poles of neutron stars forming localized emission regions for beamed X-rays. As the pulsar rotates, very characteristic periodic patterns, so called pulse profiles, are observed, which show a broad range of complexity. Because of the extreme compactness of neutron stars, investigating the information contained in these profiles requires to account for general relativistic effects, like light bending, which can lead to complex and non-intuitive connections between the observed pulse profiles and the intrinsic geometry.

We have developed a flexible ray tracing code, which calculates the observed time and energy dependent flux for arbitrary geometry and emission patterns of the emission regions. We present the result of a simultaneous fit of the energy-resolved pulse profiles of 4U 1626-67 (NuSTAR) based on an empirical emission pattern applied to a common two column geometry. We assume the emission pattern to be a mixture of Gaussian-like fan and pencil beam emission, which sufficiently describes the energy evolution of the observed pulse profiles.

Further we present a physical accretion column model combining the model from the simulations by Postnov et al. (2015) to obtain seed photon continua produced in the dense inner regions of the accretion column. In a thin outer layer these seed continua are imprinted with cyclotron resonant scattering features calculated using Monte Carlo simulations as described in Schwarm et al. (2017). From these emission patterns we derive the observed phase and energy dependent flux for different geometries using the relativistic ray tracing code and discuss the observational implications.

PICO - Search for Dark Matter with Bubble Chambers

Robert Filgas, IEAP, CTU in Prague, 2015-04-20 - 2015-04-22

Time: 20 minutes

The PICASSO and COUPP collaborations use superheated liquid detectors to search for cold dark matter through the direct detection of weakly interacting massive particles (WIMPs). These experiments, located in the underground laboratory of SNOLAB, Canada, detect phase transitions triggered by nuclear recoils in the keV range induced by interactions with WIMPs. We present details of the construction and operation of these detectors as well as the results, obtained by several years of observations. We also introduce PICO, a joint effort of the two collaborations to build a second generation ton-scale bubble chamber with 250 liters of active liquid.

GRB 111209A / SN 2011kl: a very luminous supernova related to an ultra-long GRB

Robert Filgas, IEAP CTU, 2016-04-18 - 2016-04-20

Time: 15-20

A new class of ultra-long-duration γ-ray bursts has recently been suggested. They may originate in the explosion of stars with much larger radii than those producing normal long-duration γ-ray bursts or in the tidal disruption of a star. No clear supernova has yet been associated with an ultra-long-duration γ-ray burst. Here we report that a supernova (SN 2011kl) was associated with the ultra-long-duration γ-ray burst GRB 111209A, at a redshift z of 0.677. This supernova is more than three times more luminous than type Ic supernovae associated with long-duration γ-ray bursts and its spectrum is distinctly different. The slope of the continuum resembles those of super-luminous supernovae but extends further down into the rest-frame ultraviolet implying a low metal content. The light curve evolves much more rapidly than those of super-luminous supernovae. This combination of high luminosity and low metal-line opacity cannot be reconciled with typical type Ic supernovae, but can be reproduced by a model where extra energy is injected by a strongly magnetized neutron star (a magnetar), which has also been proposed as the explanation for super-luminous supernovae. This work has been published in Nature.

Dark matter search results from PICO-2L and PICO-60 bubble chambers

Robert Filgas, IEAP CTU, 2016-04-18 - 2016-04-20

Time: 15-20

We report new data from 3 papers published last year from the operation of our 2 dark matter detectors located at SNOLAB, Canada. A 2-liter PICO-2L C3F8 bubble chamber and PICO-60, the largest bubble chamber to search for dark matter to date. These data provide the most sensitive direct detection constraints on WIMP-proton spin-dependent scattering to date, with significant sensitivity at low WIMP masses for spin-independent WIMP-nucleon scattering.

Space weather monitoring with Timepix

Robert Filgas, IEAP Czech Technical University in Prague, 2018-04-16 - 2018-04-20

Time: 20 minutes

Space radiation monitors have lately become increasingly interesting for space agencies and satellite developers. During the lifetime of the satellite, the dynamic development of the radiation environment caused by geomagnetic storms or solar eruptions can be studied. Continuous Earth magnetosphere monitoring allows us to obtain information on the composition, flux, spectrum and direction of the arrival of energetic particles, including time and space fluctuations of these parameters. In addition to scientific research, these data provide very valuable information about the effects of dangerous cosmic rays on satellites and spacecraft crews. I will present an overview of Timepix-based radiation monitors currently in space and in future missions.

Black Hole Spin Measurements in Lamp Post Geometry

Marco Fink, Remeis-Observatory & ECAP, 2016-04-18 - 2016-04-21

Time: 15 min

M. Fink, T. Dauser, T. Beuchert, S. Jeffreson, J. Tawabutr, J. Wilms, J.
Garcia, D. Walton

We analyze a sample of bare AGN spectra based on the sample introduced by Walton et al. (2012) using high signal-to-noise spectra from the XMM and NuStar archives. We model features of blurred reflection off an ionized accretion disk using the angle resolved RELXILL code, describing the irradiation of the disk in the lamp post geometry. By combining this advanced reflection model with Suzaku and joint XMM and NuSTAR observations, both outstanding in signal-to-noise and spectral coverage, we can put tight constraints on the spin parameter and we are able to constrain the height of the primary photon source in the lamp post geometry.

Frontier Research in Astrophysics: A Short Cruise

Giovannelli Franco, INAF-Istituto di Astrofisica e Planetologia Spaziali, 2015/04/20 - 2015/04/24

Time: 45 min (optimum)

In this short cruise I will discuss the most important old and new results obtained in astrophysics by means of space- and ground-based experiments that provided a strong acceleration on the knowledge of the physics of our Universe within the framework of current theoretical knowledge and its possible advancing.
Because of the obvious limits of my knowledge, and of the length of this paper, I will present a selection of results without any pretension of completeness.

Low energy indicators of high energy processes in X-ray pulsars: A possible general model

Giovannelli Franco, INAF-Istituto di Astrofisica e Planetologia Spaziali, 2015/04/20 - 2015/04/24

Time: 30 min (optimum)

Franco Giovannelli (1), Corinne Rossi (2), Gennady Bisnovatyi-Kogan (3, 4), Ivan Bruni (5),
Fabio Martinelli (6), Javier Salas-Procas (7)

(1) INAF - Istituto di Astrofisica e Planetologia Spaziali, Roma
(2) Dpt of Physics University of Roma “La Sapienza”
(3) Space Research Institute, Moscow
(4) National Research Nuclear University MEPhI, Moscow
(5) INAF - Osservatorio Astronomico di Bologna, Stazione Astronomica di Loiano
(6) Montecatini Val di Cecina Astronomical Centre
(7) Agrupación Astronómica de Huesca

In this paper we will discuss a long series of data obtained with observations of the X-ray pulsar A0535+26 and its optical Be-companion HDE 245770. The results demonstrate that optical luminosity brightening of HDE 245770, occurring around the periastron passage, precedes the subsequent X-ray outburst of A0535+26 of about 8 days. Such a delay is the time necessary to the matter coming from the Be star for crossing the temporary viscous accretion disk formed around the neutron star, until reaching its polar caps.
The model developed for explaining such a delay seems to be general for the class of X-ray pulsars and more, like CVs, and AGNs.

Time lag between low energy and high energy processes in cosmic sources

Giovannelli Franco, INAF-Istituto di Astrofisica e Planetologia Spaziali, 2017-04-03 - 2017-04-07

Time: 30 minutes

In close binaries with accretion disks, the time lag between high energy and low energy flashes is connected with effects of viscosity that define a radial motion of matter in the accretion disk.
In AGN flashes, the infalling matter has a low angular momentum, and the time lag is defined by the free-fall time to the gravitating center.
In this paper we will discuss quantitative models developed for galactic and extragalactic accreting sources.

Frontier Research in Astrophysics - An Updated Review

Giovannelli Franco, INAF-Istituto di Astrofisica e Planetologia Spaziali, 2017-04-03 - 2017-04-07

Time: 45 minutes

In this paper -- a short updated version of our review paper about \"The impact of space experiments on our knowledge of the physics of the Universe\" (Giovannelli & Sabau-Graziati, 2004) (GSG2004) and
subsequent updating (Giovannelli & Sabau-Graziati, 2012a, 2014a) - we will briefly discuss old and new results obtained in astrophysics, that marked substantially the research in this field. Thanks to the results, chosen by us following our knowledge and feelings, we will go along different
stages of the evolution of our Universe discussing briefly several examples of results that are the pillars carrying the Bridge between the Big Bang and Biology.

We will remark the importance of the joint venture of `active physics experiments\' and `passive physics experiments\' ground- and space-based either big either small in size that, with their results, are directed towards the knowledge of the physics of our universe. New generation experiments open up new prospects for improving our knowledge of the aforementioned main pillars.

The intermediate polar nature of the cataclysmic variable SS Cygni

Giovannelli Franco, INAF-Istituto di Astrofisica e Planetologia Spaziali, 2017-04-03 - 2017-04-07

Time: 30 minutes

The classification of SS Cyg as a dwarf nova (DN), a subclass of non-magnetic (NM) cataclysmic variable (CV) has been considered by most of the community well established because of a paper
appeared in Nature (Bath & van Paradijs, 1983), that was a bandwagon for all the
papers discussing SS Cyg behaviour both from experimental and theoretical points
of view, until nowadays in spite of the many arguments and circumstantial proofs about its possible intermediate polar nature, as claimed by Franco Giovannelli\'s group since more than 30 years.

The goal of this paper is to objectively discuss about the controversial nature of SS Cyg by using all the different interpretations of its multifrequency data in order to demonstrate undoubtedly its intermediate polar nature.

An updated view of our Universe in the gravitational-wave Era

Giovannelli Franco, INAF-Istituto di Astrofisica e Planetologia Spaziali, 2018/04/16 - 2018/04/20

Time: Optimum 60 minutes - Acceptable 45 minutes

I will discuss the main pillars of the Bridge between the Big Bang and Biology using the updated results coming from the big and small experiments space- and ground-based in the new era of Gravitational Wave Astronomy.
I will present a selection of solved and open problems that in my opinion marked the evolution of our knowledge of the physics governing our Universe.

Observing the Sun and Jupiter by the HF’s

Vojtěch Fárek, František Krejčí Observatory Karlovy Vary, 2016-04-18 - 2016-04-21

Time: 15 to 20 minutes

The problematic of solar flares, corona mass eruptions and not at last Jupiter’s energy interactions belong to one of the most-questioned topics within the research of our Solar System. Jupiter is the planet which spreads the biggest number of energy from all the planets in the Solar System, even more then it gets from the Sun. A lot of that energy is produced by a slow contraction of this planet and also by loads of chemical reactions. However, the interactions with Galilean moons, first of all Io, cannot be missed out. Actually, it is the main source of energy being spread into large space. The Earth can also be hit by this energy and its atmosphere can be affected. In this lecture, I will focus on modelling of Jupiter’s interactions in three important Io phases, called Io-Storm phases. The Sun and Jupiter can both be easily monitored by radio telescopes within high frequencies so I will also show how to make the measurement and I will comment the results.

Recent Advances in the Study of Black Holes using X-ray Reflection Spectroscopy

Javier Garcia, Caltech & Dr. Karl Remeis Observatory, 2017-04-04 - 2017-04-05

Time: 30 min

Reflection spectroscopy has proven to be a versatile tool for the study of
accreting black holes that allows one to constrain key physical parameters the
such as the spin of the black hole; the accretion disk\'s inner radius,
inclination, ionization state and Fe abundance; and, more recently, the
temperature, optical depth and geometry of the corona that produces the X-ray
emission. This talk is an overview of the state of the field that highlights
recent developments and the limitations of the models we use. I will describe a
major program now underway aimed at analyzing for a few dozen black holes the
thousands of spectra that were collected by NASA\'s RXTE satellite during its
1996-2012 mission. I will also discuss current outstanding issues in the
interpretation of the observational data, such as the large iron abundances
frequently required to fit the reflection spectra of both black hole binaries
and AGN.

Simultaneous NuSTAR - XMM-Newton observations of AGN

Andrea Gokus, Dr. Karl Remeis Observatory & ECAP, 2017-04-04 - 2017-04-05

Time: 10-15 minutes

Joint X-ray observations of the satellites XMM-Newton and NuSTAR have
become the main tool to study the 6.4 keV iron K alpha line emission in
the direct environment of black holes.
The soft (XMM-Newton) and hard
(NuSTAR) X-ray spectra together allow determining the continuum,
absorption, reflection and emission lines. In order to get better results in the future, the present study aims
to help improving the cross-calibration by analyzing all publicly
available simultaneous NuSTAR – XMM-Newton observations with good
Signal-to-Noise Ratio in a coherent way.

The Spectral Energy Distribution of the Candidate Neutrino Source TXS0506+056

Andrea Gokus, University of Wuerzburg / Dr. Remeis Observatory & ECAP, 2018-04-16 - 2018-04-18

Time: 15

The origin of extragalactic neutrinos with energies above 1 PeV is still unclear. One of the best
candidates are jets from Active Galactic Nuclei (AGN), in which particles are accelerated to
relativistic speeds. Blazars, a subclass of AGN, show jet orientations towards Earth and are
therefore of specific interest in the search for neutrinos, because we can directly look into the jet
and observe the underlying physical processes caused by the relativistic particles. Based on
hadronic emission models of the jet, interacting protons can produce cascades, in which
neutrinos are generated. These models predict a tight correlation between the neutrino flux and
the time-variable gamma-ray emission, which could be proven by linking neutrino detections to
gamma-ray flares.
On September 22th, IceCube detected the first extremely high energy (EHE) event that is
spatially and temporally coincident with the increase of gamma-ray emission from a single
source (TXS0506+056). We develop a model of a time-resolved, hybrid (leptonic & hadronic)
spectral energy distribution, and compare the results with multi-wavelength observations.

On one-parametric formula relating the frequencies of twin-peak quasi-periodic oscillations

Kateřina Goluchová, Silesian University in Opava, 2018-04-16 - 2018-04-19

Time: 10 min

Twin-peak quasi-periodic oscillations (QPOs) are observed in several low-mass X-ray binary systems containing neutron stars (NSs). Timing analysis of X-ray fluxes of more than dozen of such systems reveals remarkable correlations between the frequencies of two characteristic peaks present in the power density spectra. The individual correlations clearly differ, but they roughly follow a common individual pattern. High values of measured QPO frequencies and strong modulation of the X-ray flux both suggest that the observed correlations are connected to orbital motion in the innermost part of an accretion disc. Several attempts to model these correlations with simple geodesic
orbital models or phenomenological relations have failed in the past. We find and explore a surprisingly simple analytic relation that reproduces individual correlations for a group of several sources through a single parameter. When an additional free parameter is considered within our relation, it well reproduces the data of a large group of 14 sources. The very existence and form of this simple relation supports the hypothesis of the orbital origin of QPOs and provides the key for further development of QPO models.

X-ray emission of Centaurus A

Christina Graefe, Remeis Observatory, 2014-04-22 - 2014-04-25

Time: 15 min

C.Gräfe, T. Beuchert, T. Dauser, F. Fürst, N. Hell, M. Kadler, F. Krauß, A. Markowitz, C. Müller, R. Ojha, K. Pottschmidt, J. Wilms

Due to its proximity, Centaurus A allows us to study the X-ray emission of AGN in great detail and to disentangle its different emission regions. With Chandra and Suzaku observations, we study its X-ray properties in the 0.5-10 keV band.
We find an extended diffuse emission region with emission lines, and a varying hard component.

Centaurus A

Christina Graefe, Dr. Remeis Observatory/ECAP, FAU & Univ. Würzburg, 2016-04-18 - 2016-04-21


Active galactic nuclei (AGN) are among the most energetic objects in the universe, and have been extensively studied over decades. Most AGN can be studied in moderate spatial resolution only, because of the great distance to the objects. Being one of the closest AGN, Centaurus A has been observed by instruments covering all wavelengths. Despite these efforts, many open questions remain. Centaurus A is part of the TANAMI sample of southern radio-loud AGN studied by us with VLBI monitoring observations. Using also data from the X-ray satellites Chandra, XMM and Suzaku, we study its emission features to resolve both spatial and energetic features, and work on putting them in the context of AGN.

Quantum Imaging Detection and Directional Visualization of Space Radiation with SATRAM/Timepix Spacecraft Payload in LEO Orbit

Carlos Granja, Inst. Exper. Appl. Phys., Czech Tech. Univ. Prague, 2015-04-20 - 2015-04-24

Time: 30

The compact light weight SATRAM payload is operating in onboard ESA’s Proba-V satellite in low Earth orbit since May 2013. Equipped with the Timepix detector the device can determine the composition and spectral characteristics of ionizing radiation (X-ray, light and heavy charged particles) in the satellite environment. Single quantum counting capability and per-pixel energy sensitivity enable quantum-level detection, high resolution tracking, LET sensitivity and directional visualization of energetic charged particles over a wide dynamic range of particle fluxes, energies and wide field of view. A description of the payload is presented together with preliminary data results such as spatial and time correlated maps of particle flux along the satellite orbit.

On-site calibration of spacecraft gamma-ray spectrometer for the BepiColombo ESA/JAXA mission to Mercury by transportable gamma-ray station

Carlos Granja, Inst. Exper. Appl. Phys., Czech TU Prague, 2015-04-18 - 2015-04-21

Time: 20 min

A compact and transportable gamma-ray source station has been built to provide a discrete gamma-ray field in wide energy range (100 keV – 9 MeV). The station is designed for spacecraft payload qualification and preflight calibration of space radiation sensors on site at Test Centers of space agencies or large scale integrators. The gamma-ray field produced in the station, characterized by conventional HPGe detector, was first used in Prague to calibrate a flight-qualified instrument equipped with a LaBr3:Ce scintillation detector delivered by ESA. Results include gamma-ray spectra acquired in wide-energy range by both detectors. Typical measuring times for calibration of flight-version devices are between 2 to 10 min (up to 6.2 MeV) and 20 to 30 min (up to 8 MeV) with the detector placed at a distance 2 to 5 m from the station. In 2015 the station was shipped to the Russian space institute IKI in Moscow for testing and calibration of the Mercury Gamma-Ray and Neutron Spectrometer (MGNS) payload to be flown on board the Mercury Polar Orbiter (MPO) part of the ESA’s BepiColombo mission to Mercury in 2018. Results are presented of measurements performed on the MGNS gamma-ray spectrometer equipped CeBr3 and LaBr3 detectors.

Mapping of space radiation in LEO orbit by the SATRAM/Timepix payload on board the ESA Proba-V satellite

Carlos Granja, Inst. Exper. Appl. Phys., Czech TU Prague, 2015-04-18 - 2015-04-21

Time: 20 min

Detailed spatial- and time-correlated maps of the space radiation environment in Low Earth Orbit (LEO) are produced by the spacecraft payload SATRAM operating in open space on board the Proba-V satellite from ESA. Equipped with the hybrid semiconductor pixel detector Timepix, the compact radiation monitor payload provides the composition and spectral characterization of the mixed radiation field with quantum imaging sensitivity, single-particle counting, energetic charged particle directional tracking and dE/dx response in wide dynamic range in terms of particle type fluxes and dose rates. With a polar orbit (sun synchronous, 98° inclination) at the altitude of 820 km the payload samples the space radiation field at LEO covering the whole planet. Extensive results of long-period data evaluation in the form of time-and spatially-correlated maps of total dose rate (charged particles, X-rays) are presented including comparison between quiescent and geomagnetic storm/active periods induced by solar particle events (SPEs).

Mechanical measurement of Composite structures exposed to cosmic radiation in Earth orbit on board of a „CubeSat“ satelite

Petr Hana, Technical University of Liberec, Studentská 2, 461 17 Liberec, Czech Republic, 2014-04-22 - 2014-04-25


This article focuses on the comprehensive study and measurement of mechanical properties of new material structures with carbon fibber composites specifically designed for the construction of space satellites. Composite structures will be exposed to cosmic radiation in Earth orbit on board of a „CubeSat“ satelite. The aim was to develop a measurement methodology for determining the mechanical properties of composite structures in orbit. We realized a number of alumina and Composite Square vibrating plates samples with stickled thin piezoelectric plate used as piezoelectric transducer. It was compiled numerical simulation with given geometry including stickled thin piezoelectric sensor for description and evaluation mechanical properties.

IBWS workshops: Introductiona and Historical Background

Rene Hudec, ASU AV CR & CVUT, 2014-04-22 - 2014-04-25

Time: 20

I will give introduction and describe historical backround of IBWS workshops related to history of group of high energy astrophysics at Astronomical Institute Ondrejov

Analyses in Astronomical Photographic Archives

Rene Hudec, ASU AV CR & CVUT, 2014-04-22 - 2014-04-25

Time: 20

Recent status of analyses in Astronomical Photographic Archives with emphasis on analyses of high energy sources in optical light will be briefky presented and discussed

Baker Nunn Camera Databases and their application in high energy astrophysics

Rene Hudec, ASU AV CR & CVUT, 2014-04-22 - 2014-04-25


Baker Nunn Camera Databases and their application in high energy astrophysics will be introduced and discussed. The network cameras records enable analyses of optical sources up to mag 16 with fine time resolulution of few seconds and are hence perfectly suited e.g. for optical transient searches

IBWS Workshops Introduction and Historical Background

Rene Hudec, CTU in Prague & ASU AV CR, 2015-04-20 - 2015-04-24

Time: 15

A short introduction to IBWS Workshops and Historical Background will be given

Recent Results in Photographic Archives Digitization

Rene Hudec, CTU in Prague & ASU AV CR, 2015-04-20 - 2015-04-24

Time: 20

Recent Results in astronomical Photographic Archives Digitization will be given and and possible applications in high energy astrophysics will be discussed

ESA M4 Candidate Missions with Czech Participation

Rene Hudec, CTU in Prague & ASU AV CR, 2015-04-20 - 2015-04-24


ESA M4 Candidate Missions LOFT and THESEUS with Czech Participation will be presented and discussed

IBWS Introduction and Historical Background

Rene Hudec, ASU AV CR & CTU, 2016-04-18 - 2016-04-21

Time: 15

IBWS Introduction and Historical Background will be given


Rene Hudec, ASU AV CR & CTU, 2016-04-18 - 2016-04-21

Time: 15

SMILE was selected within ESA China call and represents satellite to study Earth magnetosphere by X rya and UV experiments. The project will be briefly presentd togeether with expected Czech participation.

UV LDS Camera as Picosatellite Payload

Rene Hudec, ASU AV CR & CTU, 2016-04-18 - 2016-04-21

Time: 15

The small UV low dispersive cameras for LDS star spectroscopy were used with Prof Karl Henize as PI in several US manned space missions (Gemini flights and Skylab). I will show and discuss obtained results along with suggestion of upgraded UV LDS camera as a scientific payload for a picosatellite such as BRITE.

BRITE CZ: Extending BRITE to X and UV

Rene Hudec, ASU AV CR & CTU, 2016-04-18 - 2016-04-21

Time: 15

We will give short overview of proposal submitted recently in the Czech Republic of funding of development and launch of Czech BRITE satellite, focussing on monitoring of X ray and UV sources.

IBWS Introduction and Historical Background

Rene Hudec, CVUT & ASU AV CR, 2017-04-03 - 2017-04-07

Time: 15

IBWS Introduction and Historical Background will be given

Astrophysical payloads for cubesatellites

Rene Hudec, CVUT & ASU AV CR, 2017-04-03 - 2017-04-07

Time: 20

Astrophysical payloads for cubesatellites will be discussed

JEUMICO Czech Bavarian Astronomical X Ray Optics Project

Rene Hudec, CVUT & ASU AV CR, 2017-04-03 - 2017-04-07

Time: 10

JEUMICO, the Czech Bavarian Astronomical X Ray Optics Project will be shortly presented

15 years of IBWS Workshops

Rene Hudec, ASU AV CR & CVUT, 2018-04-16 - 2018-04-20

Time: 15

I will briefly discuss the history and recent status of IBWS workshops

Astrophysics with digitized astronomical plate archives

Rene Hudec, ASU AV CR & CVUT, 2018-04-16 - 2018-04-20

Time: 20

I will discuss recent status of astrophysical analyses with digitized astronomical plate archives with emphasis on high energy and transient astrophysics.

Digitization and astrophysical use of Hewitt Camera Archive, UK

Rene Hudec, ASU AV CR & CVUT, 2018-04-16 - 2018-04-20

Time: 15

We will briefly present the status of digitization and astrophysical use of Hewitt Camera Archive, UK. These wide field images, so far litte used for astrophysical work, covers both northern as well as southern sky down to lim mag 13.

LDS spectroscopy with cubesats and photographic plates

Rene Hudec, ASU AV CR & CVUT, 2018-04-16 - 2018-04-20

Time: 15

I will briefly present the proposal for UV experiment based on LDS low dispersion spectroscopy of stars for cubesat mission as well as potential of LDS with digitized photographic plates taken by mostly Schmidt telescopes.


Adolf Inneman, Czech Technical University - Faculty of Electrical Engineering, 2016-04-20 - 2016-04-20

Time: 15

COLORES on BOOTES-2, calibration

Martin Jelinek, IAA CSIC, 2014-04-22 - 2014-04-26


A small lookup into spectroscopic calibration process and its results will be presented.

Observing GRBs with Robotic Telescopes

Martin Jelinek, -, 1.1.1970 - 31.12.2032

Time: 30

I will re-perform my PhD defense talk from last November. GRBs, Telescopes BOOTES, Spectrograph COLORES.

EMCCD Based Cameras in Astronomy

Martin Jelinek, ASÚ AV ČR, 2016-04-19 - 2016-04-21

Time: 20 min

Electron Multilying CCD devices were developped to overcome certain disadvantages of CCDs - the readout noise, and the slow readout. I will talk about their use in astronomy.

Robotic Telescopes in Ondřejov

Martin Jelinek, ASU AVCR, 2018-04-16 - 2018-04-20

Time: 20

There are two robotic telescopes in Ondřejov. Their primary task is to follow up and search for optical transients. I will present the recent upgrades as well as achievements of the two telescope systems.

Problematics of breeding pangolins in relativistic conditions

Martin Jelínek, ASÚ AV ČR, 4/4 - 7/4

Time: 40

Lets talk about what real problems are when trying to observe GRBs with robotic telescopes.

The Extended Radio Structure of High-z Blazars

Alexander Kappes, Julius-Maximillians University Wuerzburg, 2016-04-18 - 2016-04-21


Extragalactic radio-loud quasars have relativistic jets feeding the associated radio-lobes. These are observed in radio-galaxies, as well as in sources whose jet is aligned with the line of sight, i.e. blazars. The very existence of a dozen high-z blazars suggests that a much larger population of misaligned jetted AGNs must exist at z>4. Yet, such parent population proved to be very elusive and escaped detection in radio surveys so far. Similarly, extended radio emission of high-z blazars has not yet been detected. Both these results could be understood if synchrotron emission from the lobes of such objects is quenched by Compton scattering off the CMB. We use high-resolution long-wavelength LOFAR observations to search for extended emission in a sample of blazars with redshifts z>4. The results will yield improved angular resolution and sensitivity to faint extended optically-thin lobe structures in high-z blazars and test the CMB-quenching scenario.

Oblique Magnetic Fields and the Role of Frame Dragging

Vladimir Karas, Astronomical Institute ASCR, 2014-04-22 - 2014-04-23

Time: 15 min

Magnetic null points can develop near the ergosphere boundary of a rotating black hole by the combined effects of strong gravitational field and the frame-dragging mechanism. We show that the electric component does not vanish in the magnetic null, and so an efficient process or particle acceleration can occur. The situation is relevant for low-accretion-rate nuclei of some galaxies which exhibit episodic accretion events (such as the Milky Way\'s supermassive black hole) embedded in a large-scale magnetic field.

Plunging neutron stars as origin of organised magnetic field in galactic nuclei

Vladimir Karas, Astronomical Institute, 2017-04-03 - 2017-04-04

Time: 15

Black holes cannot support their own internal magnetic field like, for example, compact stars can. Despite this fact observations indicate that event horizons of supermassive black holes (SMBH) are threaded by field lines along which plasma streams flow. Various magnetohydrodynamical mechanisms have been suggested to generate turbulent magnetic fields on small scales, however, the origin of the large-scale component is unclear. We propose that dipole-type magnetic fields can be brought onto SMBH by magnetised neutron stars, which are expected to drift inward from a hidden population in the Nuclear Star Cluster.


Mannheim Karl, Universität Würzburg, Germany, 2017-04-04 - 2017-04-05

Time: 30min

The eASTROGAM mission concept, currently under study by ESA in the frame of the M5 call for proposals, will be presented. The mission goal is an all-sky MeV gamma-ray telescope with imaging, spectroscopic, and polarimetric observation capabilities across a broad band. eASTROGAM combines a double-sided Silicon strip tracker, a pixelated calorimeter, and an anti-coincidence dome. This mission will be key to understand AGN and other phenomena related to compact objects and their high-energy emissions.

The location of the gamma-ray emitting zone in blazars

Mannheim Karl, JMU Würzburg, 2018-04-16 - 2018-04-18


Gamma-rays can be expected from the ergospheres surrounding black holes, due to the Penrose process or its ramifications. However, due to the presence of accretion flows, the optical depth on the event horizon scale is generically very high. Therefore, gamma-ray in blazars are presumably emitted far from the central black hole, and this is in line with the obserrved absence of pair-absorption features due to recombination photons from the BLR. The frequent occurence of flares on ultrashort time scales is difficult to explain in this context, leaving only very few options which will be discussed in this presentation.

Mini-MegaTORTORA wide-field monitoring system with sub-second temporal resolution: observation of transient events

Sergey Karpov, Special Astrophysical Observatory, Russia, 2017-04-03 - 2017-04-08

Time: 15

Here we present the summary of first years of operation and the first results of a novel 9-channel wide-field optical monitoring system with sub-second temporal resolution, Mini-MegaTORTORA (MMT-9), which is in operation now at Special Astrophysical Observatory on Russian Caucasus. The system is able to observe the sky simultaneously in either wide (~900 square degrees) or narrow (~100 square degrees) fields of view, either in clear light or with any combination of color (Johnson-Cousins B, V or R) and polarimetric filters installed, with exposure times ranging from 0.1 s to hundreds of seconds.The real-time system data analysis pipeline performs automatic detection of rapid transient events, both near-Earth and extragalactic. The objects routinely detected by MMT also include faint meteors and artificial satellites.

Photometric calibration of a wide-field sky survey data from Mini-MegaTORTORA

Sergey Karpov, Institute of Physics, Czech Academy of Sciences, 2018-04-16 - 2018-04-20


In this talk I will briefly present the results and problems of an on-going activities to photometrically calibrate the data acquired over the last 4 years with Mini-MegaTORTORA wide-field monitoring system on various time scales.
(This talk is suggested for an image processing session)

OPS-SAT: An ESA CubeSat as an in-orbit experiment laboratory

Ali Kheirkhah, Zentrum für Telematik, -

Time: 15

There are every year a large number of new innovative ideas generated by ESA and the European industry for evolving European space technology and mission operations. Patents are filled, studies, prototypes and breadboards produced, but the majority of the innovations never makes to orbit. The reason is the well-known problem: “Has never flown - will never fly”. Obviously, the risk aversion is healthy when dealing with large expensive missions but leaves little room for innovation.
The idea of OPS-SAT emerged to try to change the current situation, by providing a low cost in-orbit hard – and software laboratory available for authorised experimenters to test, demonstrate and validate their developments.
OPS-SAT is the first CubeSat designed for ESA and is a safe experimental platform flying in LEO. OPS-SAT makes available a reconfigurable platform, at every layer from channel coding upwards, and is available for experimenters to demonstrate innovative new software and mission operation concepts.
This paper reports on the functionality and the design of OPS-SAT developed during the Phase A/B1 executed by TU Graz (Austria), Zentrum für Telematik (Germany) and MAGNA Steyr (Germany).

Earth Observation by Small Satellite Formations

Schilling Klaus, University Wuerzburg, 2016-04-18 - 2016-04-20

Time: 20

Coordinated observations by telescopes from several small satellites by photogrammetric methods enable 3D-images of the Earth\'s surface at interesting resolution. The application potential of such sensor networks formed by small satellite formations for other phenomena will be addressed.

Satellite Formations for Scientific Observations

Schilling Klaus, University Wuerzburg, 2018-04-17 - 2018-04-19

Time: 30 min

Formations of satellites offer exciting innovative potential for scientific observations, but require challenging autonomous reaction capabilities in order to coordinate attitude and orbit control. Distributed networked, cooperating very small satellites exhibit here increasing capabilities. Modern miniaturization technologies support realization of robust, cost-efficient small satellites with growing performance related to attitude and orbit control. Thus, networks of detectors composed of pico-satellites are possible, enabling by cooperating formations improved observation characteristics. In combination with sensor data fusion, innovative application approaches to Earth observation, but also for astronomical observations are supported.

SNRs in 3D

Matus Kocka, Masaryk University, 2014-04-22 - 2014-04-25

Time: 20 min



Matus Kocka, Masaryk University, 2014-04-22 - 2014-04-25


Short talk about new Slovak pico-sat (cube-sat).

SkCube, the VLF experiment and the ionosphere study not only by future SID network

Matus Kocka, SOSA, 2016-04-19 - 2016-04-20

Time: 30

SkCube is first Slovak satellite which will launch on board Falcon 9 in the beginning of the summer 2016. The satellite is 1U cubesat with unique design and experiments. The main scientific payload is VLF receiver able to operate in two readout modes. The goal is to study upper ionosphere environment, earth magnetosphere and strong lightnings. As the related project to our study of the ionosphere is proposal to build autonomous SID (sudden ionospheric disturbance) monitor network. The receivers in such network will be similar to the one in SkCube, network will be autonomous, low energy and maintenance-free with ability to use data from other already existing SID detectors. We took into account lessons learned from previous SID monitor initiatives in both Slovakia and Czech Republic.

Suitable propulsion systems for a 1U CubeSat

Alexander Kramer, Zentrum für Telematik, 2015-04-24 - 2015-04-24

Time: 10

In the scope of the \"Networked Pico-Satellite Distributed System Control\" project at the Zentrum für Telematik in Gerbrunn, Germany promising propulsion systems suitable for 1U CubeSat missions are examined. The CubeSat standard puts several restrictions on the design possibilities of miniaturized propulsion systems. For this reason only a limited number of already existing propulsive technologies are to be considered for application on a CubeSat. Some promising candidates for this purpose are presented including performance measurement results.

Ernie and Bert in the Radio: The TANAMI view of the IceCube PeV Neutrino events

Felicia Krauss, Remeis Observatory, 2014-04-22 - 2014-04-25


F. Krauss, M. Kadler, K. Mannheim, J. Wilms, T. Beuchert, J. Blanchard, C.Bürkel, B. Carpenter, D. Eisenacher, D. Elsässer, C. Gräfe, A. Kappes, A. Kreikenbohm, I. Kreykenbohm, M. Langejahn, C. Müller, R.Ojha, E. Ros, R. Schulz, J. Trüstedt, on behalf of the TANAMI collaboration

The IceCube Collaboration has published their first results on an excess neutrino flux above the atmospheric background. Due to low atmospheric background at PeV energies, the highest energy events (\'Ernie\' and \'Bert\') are the most likely ones to be of extraterrestrial origin.
We study the multiwavelength properties of AGN from the TANAMI sample that are positionally coincident with the two neutrino events. We combine multiwavelength data, including X-ray data from the XMM-Newton and the Swift satellite to construct broadband spectra.

Bert, Ernie, and Big Bird: Blazars as possible sources of IceCube PeV neutrinos

Felicia Krauß, Dr. Remeis Observatory/ECAP, FAU & Univ. Würzburg, 2016-04-18 - 2016-04-21

Time: 30

The IceCube Collaboration has published results on a neutrino flux significantly in excess of the atmospheric background. Due to low atmospheric background at PeV energies, the highest energy events are the most likely ones to be of extraterrestrial origin. We use broadband spectra in the IceCube integration period to calculate the expected number of neutrinos assuming a pion photoproduction model. We find a blazar outburst in positional and temporal agreement with the highest-energy neutrino event, whose PeV neutrino flux is high enough to explain the observed event.
Further, we use the TANAMI sample to search for hadronic signatures in the broadband spectrum and to study the spectral evolution during blazar outbursts.

Blazars as Potential High-Energy Neutrino Sources

Michael Kreter, University of Würzburg, 2016-04-18 - 2016-04-21

Time: 20

Jets from Active Galactic Nuclei (AGN) are among the best candidates for the recently detected
extraterrestrial neutrino flux. Specifically, gamma-ray blazars have been predicted to yield a
cumulative neutrino signal exceeding the atmospheric background above energies of 100 TeV,
assuming that both the neutrinos and the gamma-ray photons are produced by accelerated
protons in relativistic jets. Since the background spectrum falls steeply with increasing energy,
the individual events with the clearest signature of being of an extraterrestrial origin are those at
the highest energies. Hadronic AGN jet emission models predict a tight correlation between the
neutrino flux and the time-variable gamma-ray emission.
We develop a strategy to search for high-energy neutrinos from promising blazar jets from the
TANAMI sample using the ANTARES telescope, Fermi gamma-ray light curves, and time-
resolved multiwavelength SED data.
An unbinned maximum-likelihood method is applied to maximize the probability of a neutrino
detection with ANTARES or alternatively constrain the possible neutrino spectra for candidate
associations with IceCube neutrino events.

Blazars as Potential High-Energy Neutrino Sources

Michael Kreter, University of Wuerzburg, 2016-04-03 - 2016-04-06

Time: 20

Jets from Active Galactic Nuclei (AGN) are among the best candidates for the recently detected extraterrestrial neutrino flux. Specifically, gamma-ray blazars have been predicted to yield a cumulative neutrino signal exceeding the atmospheric background above energies of 100 TeV, assuming that both the neutrinos and the gamma-ray photons are produced by accelerated protons in relativistic jets. Hadronic AGN jet emission models predict a tight correlation between the neutrino flux and the time-variable gamma-ray emission but most very short flares on time scales of days or less can only yield a very small fluence, greatly reducing the probability of a neutrino detection as compared to longer high-fluence outbursts on time scales of months to years. Thus, only the absolute brightest short blazar flares provide a significant probability for a direct neutrino blazar-flare association based on timing arguments. We present a strategy to search for the most promising blazar-flare candidates using time-resolved multiwavelength SEDs.

RTS2 - upgrades and updates

Petr Kubánek, Fyzikální ústav Akademie věd, 2016-04-21 - 2016-04-22

Time: 15m

Review of RTS2 new features (TLEs, MPEC, own telescope error modeling). New telescopes and observatories using RTS2.

The Fit Statistics of Simultaneous Fits in ISIS

Matthias Kuehnel, Dr. Karl Remeis-Observatory & ECAP, 2015-04-20 - 2015-04-24

Time: 20

In a previous work we have introduced a new tool for analyzing multiple datasets and datatypes at the same time, which has been implemented into the Interactive Spectral Interpretation System (ISIS). However, the large number of degrees of freedom as well as many individual datasets lead to the question whether the traditional fit-statistics are still a good measure for the quality of a fit. We will present ongoing work and ideas for new fit statistics, which take, e.g., the physical context of the datasets into account. Furthermore, we show that by combining the residuals of all datasets weak features can be detected, which are not visible in an indivudal dataset.

BRITE-Constellation - Nanosatellites for Astrophysics

Rainer Kuschnig, TU Graz, 2016-04-17 - 2016-04-21

Time: 20 minutes

BRITE-Constellation consists of six 20cm cube satellites with a mass of about 7 kg each.
Three countries Austria, Canada and Poland funded pairs of those spacecrafts with a small (3cm)
aperture telescope/CCD camera instrument, one sensitive in blue and one in a red bandpass.
They were launch in sequence starting February 2013. The goal is to measure the brightness
variations of the brightest stars in the sky (<4 mag(V)) with high precision over a time span of up to
6 month. An overview of the technical design of the satellites will be given as well as a status
report and highlights of experiences with operating a fleet of nanosatellites during the pas

Orphan afterglow rate with future sky survey programs

József Kóbori, Eötvös University, 2015-04-20 - 2015-04-25

Time: 15

Gamma-ray bursts are high-energy astrophysical phenomena. After the prompt gamma-emission a multiwavelength afterglow can be observed produced when a highly relativistic outflow encounters the progenitor\'s circumburst medium. If the outflow is beamed into a narrow jet the shape of the detected lightcurve strongly depends on the angle enlcosed by the
observer\'s line of sight and the jet\'s symmetry axis. If this angle is larger than the jet original half opening angle the prompt emission might be missed and an orphan afterglow is detected. Using theoretical considerations we determine the expected rate of orphan afterglows to be detected by various future sky survey programs. Our results show
significantly lower rates compared to previous works.

Phenomena in D Ionospheric Layer

Vojtěch Laitl, František Krejčí Observatory Karlovy Vary, 2016-04-18 - 2016-04-21

Time: 15 to 20 minutes

The problem of electron density’s distribution in ionosphere has recently been questioned. However, the current models do not attempt to describe the D ionospheric layer, even though this area can be easily monitored by the signals of very low frequencies. In this lecture, I will show our model focused on the D-layer and its electron density. I will also discuss our results with experimental measurement and talk about other phenomena for whose investigation our model can be used, for example the behaviour of partially ionized gas which leads to formation of a low-temperature plasma. Ionization mechanism of some simple molecules, such as nitrogen’s oxides, can be shown by the approach of the Arrhenius equation. In accordance with our knowledge about the plasma’s aspects, we are able to model the breakdown of these simple molecules into free radicals and compute their spectral wavelength’s decay.

Evening Meeting on the City Observatory

Vojtěch Laitl, František Krejčí Observatory Karlovy Vary, 2016-04-18 - 2016-04-21

Time: 1 to 2 hours

You are welcome to attend an evening meeting organised on the František Krejčí Observatory Karlovy Vary. We will have enough time to discuss our scientific work together and get new contacts during this event. We will also prepare a lecture “Radio Astronomy across the Solar System” for you. There will be some refreshments for you, too. And if the weather is good, we can demonstrate our observatory and its equipment and observe the current interesting sky objects.

Hard X-ray Emission of Blazars and Other AGN with Swift/BAT

Marcus Langejahn, University Wurzburg, 2015-04-20 - 2015-04-24

Time: 20+5

The AGN subclass of blazars is notoriously hard to detect at hard X-rays due to their low emission in this energy range. Using the Swift/BAT all sky survey at 14-200 keV, and covering 104 months of integrated emission, we evaluate the signal-to-noise distributions compared to the background noise distribution for statistical samples of faint sources. This approach reveals a large number of hundreds of blazars in a frequency band with only a few associated sources currently known. Detection statistics differ substantially between different sources samples, allowing us to constrain the broadband spectral energy distributions and address the question of the nature of unassociated Fermi gamma-ray sources.

Pico-Satellite Formations in Würzburg

Ilham Mammadov, ZfT - Zentrum für Telematik, 2017-04-06 - 2017-04-07

Time: 10

Foremost, the current state of the missions within ZfT will be
presented. As a research institute, ZfT is involved in realizing several
satellite missions based on the low-cost but highly reliable CubeSat
platforms. Combining small satellite platforms and formation flying
techniques make previously impracticable satellite missions feasible.
Formation techniques and reliable on-board electronics design based on
COTS components are considered to be a key enabler in many fields of
space observation including astrophysics.

First Statistical Tests for Clumpy-Torus Models: Constraints from RXTE monitoring of Seyfert AGN

Alex Markowitz, Remeis Observatory, 2014-04-22 - 2014-04-26


We present an analysis of multi-timescale variability in line-of-sight X-ray
absorbing gas as a function of optical classification in a large sample of
Seyfert AGN to derive the first X-ray statistical constraints for clumpy-torus
models. We systematically search for discrete absorption events in the vast
archive of RXTE monitoring of 55 nearby type Is and Compton-thin type IIs.

We detect 12 eclipse events in 8 objects, roughly tripling the number previously
published from this archive. Peak column densities span $\sim 4-26 \times
10^{22}$ cm^{-2}$. Event durations span hours to years. The column
density profile for an eclipsing cloud in NGC 3783 is doubly spiked, possibly
indicating a cloud that is being tidally sheared.

We infer the clouds' distances from the black hole to span $\sim 0.3 - 140 \times
10^4 R_{\rm g}$. In seven objects, the clouds' distances are
commensurate with the outer portions of the BLR, or the inner
regions of infrared-emitting dusty tori. We discuss implications for cloud
distributions in the context of clumpy-torus models.

Recent outburst activity of the supersoft X-ray binary AG Draconis

Jaroslav Merc, Pavol Jozef Šafárik University in Košice, 2017-04-03 - 2017-04-07

Time: 10

AG Dra is a bright symbiotic binary consisting of a white dwarf and a pulsating cool giant. Moreover, it is the most intense X-ray source among symbiotic stars, and one of the best representatives of the supersoft X-ray objects. The system undergoes characteristic symbiotic activity with alternating quiescent and active stages. The active ones consist of several outbursts repeating at about a one-year interval. Using UV and X-ray observations, González-Riestra et al. (1999) showed that there are two types of outbursts: cool and hot ones. In our recent paper (Leedjärv et al. 2016) we demonstrated that the outbursts of AG Dra can be clearly distinguished also according to behavior of the prominent optical emission lines. In the presentation, recent outburst activity of AG Dra will be discussed.

Detecting Radio Frequency Interferences using a Recurrent Neural Network

Tobias März, Universität Würzburg, 2018-04-16 - 2018-04-18

Time: 20

An increasing threat in radio astronomy is RFI. The mobilization and digitization of
the society leads to an increasing communication through radio waves. Radio wave observations, as performed by astronomers, are often polluted by radio frequency interferences(RFI). A special case of this problem develops in the usage of large telescope arrays for radio interferometry measurements. Because of the amount and the large distances between the telescopes, individual signals can endanger the whole measurement.
This thesis proposes a recurrent neural network(RNN), a machine learning algorithm, to detect and filter the measurements which are RFI-polluted. The RNN uses a Long Short-Term Memory(LSTM)-cell implementation for the RNN, to evaluate and save the current state of the network.
To label the test and training data, an algorithm is developed, that compares each value with its neighbors, in order to determine, whether the measurement is RFI-polluted at that place. The RNN learns of these labels, to evaluate the measurements.
The batch size is a parameter of the RNN that is examined in more detail. It represents the amount of images, that the network gets inputted in one step. To find a good
fitting batch size, the RNN is tested with several different batch sizes, with the other parameters staying constant. For a batch size of 2, the networks displays a remarkably good prediction, while also having smaller fluctuations.
Upcoming telescope arrays, as for example the SKA, will generate enormous amount
of data, thus using a lot of memory space. Advantages of a neural network for this task are, that it can adapt to new forms of data, it can improve with new data and that it can recognize correlations between data people can not see and therefore do not use in traditional algorithms.
The measurement data used for training and testing the network come from the Giant Metrewave Radio Telescope (GMRT), located in India.

Measurement of mechanical properties of carbon-fibre composite on nanosatellite

Ondrej Nentvich, Czech Technical University in Prague, -

Time: 10-15

The goal of the measurement is to determine mechanical properties like resonant frequency and attenuation coefficient. Measurement on the nanosatellite is different compared to the spaceships or to the Earth. It is limited by space in the probe, weight of equipment and amount of data which is possible to transfer. Idea of the experiment is that coil excites beam, made from carbon-fibre composite. It produces oscillations which are recorded by microcontroller. Signal is evaluated by Fast Fourier Transform (FFT) and gives some peaks according to the resonant frequencies. Very precise frequencies are required so FFT has many points of transformation. Attenuation coefficient is gained from averaged signal and computed by method of logarithmic decrement of attenuation. All calculations are made on the orbit. Final data like resonant frequencies, attenuation coefficient, temperatures and position of the probe will be sent the earth but not sampled signal, because of amount of data.

Health monitor system on VZLUSAT1

Ondrej Nentvich, CVUT FEE, 2016-04-18 - 2016-04-22

Time: 15

Health monitoring system on VZLUSAT 1 tests aging of carbon-fibre material in space on LEO orbit. This talk is about this payload and its before-flight tests of this system using two different sensing methods of signal and comparing results between them.

Variable stars detection and classification in the archive of the D50 telescope

Filip Novotný, Gymnázium Jihlava/ AsÚ AV ČR, 2018-04-16 - 2018-04-18

Time: 10-15min

We present our approach to search for new variable stars in archival data of the D50 telescope. The pipeline uses a maximum variance method combined with a minimum path criteria to eliminate false positives. Both single-night and multi-night approaches are tested.

Future follow-up observations of gravitational wave sources with a fleet of nano-satellite

Masanori Ohno, Hiroshima University, 2018-04-17 - 2018-04-21

Time: 15

The gravitational wave astronomy era has begun since the detection of an electromagnetic counterpart from the gravitational wave of the double neutron star merger event GW170817. This event brought a great success of the electromagnetic follow-up observations in any wavelengths. However, an association of the gamma-ray emission is not conclusive yet, which is very important to investigate a relation between the compact object merger and short duration gamma-ray bursts (short GRBs). Continuous follow-up observations in gamma-ray band will bring a smoking gun for the origin of short GRBs. Another important role for the gamma-ray observation is a localization of the gravitational wave sources because only a gamma-ray observation can realize a simultaneous detection of the electromagnetic counterpart utilizing its all-sky coverage. For efficient following observations by other wavelengths, an arc-minutes scale localization is desired. We are planning to achieve such all-sky gamma-ray observations with arc-minutes localization accuracy by the idea of a fleet of nano-satellite. A preliminary estimation of localization accuracy by nine sets of 3U cube-sat equipped ~270cm^2 CsI scintillator revealed that we can localize about 10 short GRBs per year within 20 arc-minutes radius accuracy assuming an actual GRB parameter distribution reported in the Fermi-GBM catalog. In this contribution we will demonstrate our idea and latest results of localization accuracy analyses.

Simultaneous observations with TIGRE and X-ray facilities

Volker Perdelwitz, Hamburger Sternwarte, 2016-04-17 - 2016-04-22

Time: 20

The Telescopio Internacional de Guanajuato Robótico-Espectroscópico, a 1.2m spectroscopic telescope located in the Mexican highlands and operated by the universities of Hamburg, Guanajuato and Liège (TIGRE), has been in fully robotic operation since 2013. Designed for the study of stellar activity, it is being used frequently for simultaneous/quasi-simultaneous observations with X-ray facilities such as XMM-Newton and Chandra. In this talk we present results of some of these projects as well as an outlook on future ones, e.g. pointings accompanying the eROSITA survey.

Science with the BRITE photometry

Andrzej Pigulski, Astronomical Institute, University of Wroclaw, 2016-04-18 - 2016-04-20

Time: 30 minutes

The BRITE nano-satellites provide long-term photometry for the brightest stars in the sky. I will present an overview of the first scientific results achieved with the BRITE photometry focusing on hot pulsating stars and eclipsing binaries.

Hard X-ray monitoring for astrophysical application

Ladislav Pina, , -


This work addresses the issue of the X-ray monitoring for astrophysical applications. The proposed wide-field optical system has not been used in space yet. A novel approach is based on use of 1D \"Lobster eye\" optics in combination with Timepix X-ray detector in energy range 3 - 40 keV. The proposed project includes theoretical study and functional sample of Timepix X-ray detector with multifoil wide-field X-ray \"Lobster eye\" optics. Optics focusing X-rays on a detector is the only solution especially in cases where the intensity of X-ray radiation is below the sensitivity of the detector, e.g. while monitoring astrophysical objects in space, or phenomena in the Earth\'s atmosphere. The optical system could be used in a student rocket experiment at University of Colorado. Ideal opportunity is to extend the Cubesat of Pennsylvania State University with the hard X-ray telescope demonstrator consisting of optical module and Timepix detector.

X-ray monitoring for astrophysical applications on Cubesat

Ladislav Pina, Rigaku Innovative Technologies Europe, 2015-04-22 - 2015-04-23


The primary objective of the project VZLUSAT-1 is the development, manufacturing, qualification and experimental verification of products and technologies in Earth orbit (IOD – In-Orbit Demonstration). This work addresses the issue of X-ray monitoring for astrophysical applications. The proposed wide-field optical system has not been used in space yet. The proposed novel approach is based on the use of 1D \"Lobster eye\" optics in combination with Timepix X-ray detector in the energy range 3 - 40 keV. The proposed project includes theoretical study and a functional sample of the Timepix X-ray detector with multifoil wide-field X-ray \"Lobster eye\" optics. Using optics to focus X-rays on a detector is the only solution in cases the intensity of impinging X-ray radiation is below the sensitivity of the detector, e.g. while monitoring astrophysical objects in space, or phenomena in the Earth\'s atmosphere. On board the functions and features of Radiation Hardened Composite Housing (RHCH), Solar panels based on composite substrate and Hollow Retro Reflector Array based on composite (HRRA) will be verified. To verify the properties of the developed products the satellite is equipped by Health Monitoring system (HM). HM system includes temperature, volatiles, radiation and mechanical properties sensors. The custom ADCS algorithms are being developed within the project. Given the number of IOD experiments and the necessary power the 1U CubeSat is equipped with Composite Deployable Panels (CDP) where HM panels and additional Solar panels are located. Satellite platform is assembled from commercial parts. Mission VZLUSAT-1 is planned for 6 months with launch in 2016.

Gamma-ray bursts in our HEART

Sandor Pinter, Eötvös Loránd University, 2018-04-16 - 2018-04-20

Time: 15

I will briefly present the results and the future goals of our High Energy Astronomy Research Team (HEART) which is a joint collaboration of different researchers of several academic institutions (Czech, Japanese, American, and Hungarian) to better understanding the underlying physics of gamma-ray bursts (GRB). Our project is a multi-messenger investigation for the properties of GRBs and their host environments. For this on the one hand we are analysing the GRB light curves to separate the effects of the central engine from the intrinsic jet properties, on the other hand by revealing its fine structure and composition we are refining the Galactic foreground of the interstellar medium. By studying the GRBs\' spatial distribution we have discovered two of the largest-known formation in the Universe, also by studying the observed parameters of the known GRBs we have identified a third GRB class beside short and long GRBs.

Microvariability detection in type 2 quasars

Jana Polednikova, Instituto de Astrofisica de Canarias, 2014-04-22 - 2014-04-25


We present results from a project focused on searching optical microvariability (also known as "intra-night" variability) in type 2 (obscured) quasars. For our study, we have observed a sample of three bright (V $<$17) type 2 quasars from San Pedro M\'artir observatory in Mexico.

The sample was observed during an observation period of four days using Johnson’s V filter, resulting in at least two, quasi continuous intervals of observations per target during the observing period.

Statistical analysis of the microvariability was performed with one-way analysis of variance test (ANOVA) which proved to be a robust test for detecting microvariability.

Based on the results from the statistical analysis, we show that at least two out of the three observed targets are variable on the time scales of hours. So far, this is the first robust study which shows existence of optical microvariability in type 2 quasars.

Development of thin film Iridium coatings for astronomical X-ray mirrors

Anne-Catherine Probst, Hochschule Aschaffenburg, 2016-04-18 - 2016-04-21

Time: 10 minutes

To fulfill the stringent mass requirements of new generations of space-based observatories with large collecting area for investigations of astronomical X-rays sources, we consider a mirror technology based on thin coated glass sheets. For this purpose, glass substrates are formed by thermal treatment into precise Wolter I shape, whereas the coating has to provide high reflectivity for low energy X-rays. To provide best performance of the X-rays mirrors, low surface roughness is required on the coated slumped glasses.
Process development for slumped glasses and the coating of thin Iridium films are the focus of the INTRAAST project (Industry transfer of astronomical mirror technologies), a cooperation of the Aschaffenburg University of Applied Science (Germany) and the Max-Planck-Institute for Extraterrestrial Physics (Germany).
In this project thin film deposition of Iridium on thin glass substrates occurs in a PVD-sputtering process. Dependencies of the properties of the thin Iridium films such as coating stress and crystal structure on the deposition parameters will be discussed.

Development and characterization of Ir-based coatings for thin X-ray mirrors

Anne-Catherine Probst, University of Applied Sciences Aschaffenburg, 2017-04-05 - 2017-04-07

Time: 15 min

Astronomical X-ray sources are investigated using grazing incidence angle telescopes. To fulfill the mass constraints of future launchers, light-weight X-ray telescopes have to be realized. One possibility is to use thin X-ray mirrors with a reduced thickness of several hundred microns. A coating with a reflective high Z-material is usually applied on the surface of X-ray mirrors to enhance their reflectivity. At the Aschaffenburg University of Applied Sciences a reflective coating for thin X-ray mirrors is under development. It is based on a thin iridium film since the reflectivity of bulk iridium is quite high for photon energies below 10 keV. However, the developed iridium coatings have to depict simultaneously a high reflectivity and a low coating stress to avoid undesirable deformation of the mirror. Investigations on the correlations between the coating properties and the expected performance of the mirror will be presented. The works are performed within a cooperation of the Aschaffenburg University of Applied Sciences (Germany) and the Max-Planck-Institute for Extraterrestrial Physics (Germany) (INTRAAST project “Industry transfer of astronomical mirror technologies”) and within a Bavarian-Czech cooperation with the Czech Technical University in Prague on the development of X-ray mirrors (JEUMICO project “Joint European Mirror Competence”).

Development and tests of novel X-ray optical system for space applications

Ladislav Pína, Rigaku Innovation Technologies Europe s.r.o., -

Time: 15 min

This work addresses the issue of X-ray monitoring for astrophysical applications. A novel approach based on the use of 1D and 2D \"Lobster eye\" optics in combination with Timepix X-ray detector in the energy range 3 - 40 keV was proposed. Such wide-field optical system has not been used in space yet. Designed wide-field optical system combined with Timepix X-ray detector is described together with experimental results obtained during laboratory tests. Proposed project includes theoretical study and a functional sample of the Timepix X-ray detector with multifoil wide-field X-ray \"Lobster eye\" optics. Using optics to focus X-rays on a detector is the only solution in cases where intensity of impinging X-ray radiation is below the sensitivity of the detector, e.g. while monitoring astrophysical objects in space, or phenomena in the Earth\'s atmosphere. The optical system is considered to be used in a student rocket experiment.

Keywords: X-ray optics, multifoil optics, Lobster Eye, Timepix detector, CubeSat, rocket experiment

Multifoil Optics tests at Panter facility

Ladislav Pína, Czech Technical University in Prague, -

Time: 20

Galactic and extragalactic hydrogen in the X-ray spectra of GRBs

Istvan Racz, MTA CSFK Konkoly Observatory, 2017-04-03 - 2017-04-06

Time: 15

X-ray spectra of GRB show several hydrogen component in the Milky Way, in the intergalactic space, and in the host galaxy. Interpreting the X-ray spectra we need a precise galactic foreground correction. One can estimate the galactic foreground from spectroscopic measurements, using dust extinction maps, or all-sky hydrogen survey data. We estimated the galactic hydrogen column density from AKARI Far-Infrared Surveyor observations and Planck Av maps. We compare the results with other measurement, like LAB HI survey or Schlafly et al galactic dust extinction estimation for members of the Giant GRB ring.

The Fermi GBM GRBs\' multivariate statistics

Istvan Racz, MTA CSFK Konkoly Observatory, 2018-04-16 - 2018-04-20

Time: 15

Studying the GRBs\' gamma-ray spectra may reveal some physical information of bursts. The Fermi satellite observed more than two thousand GRBs. The FERMIGBRST catalogue contains GRB parameters (peak energy, spectral indices, intensity) estimated for both the total emission (fluence), and the emission during the interval of the peak flux. We used the Contingency analysis method to reveal an ordering of the spectra into a power law - Comptonized - smoothly broken power law - Band series. We found a relationship with linear discriminant analysis between the spectral categories and the model independent physical data. We interpreted this result as a temporal variation of the spectrum during the outburst. Our results show that there is a significant synchrotron radiation in the GBM spectra, but we found also a cooling effect appear in the later spectrum.

VLA observations of TANAMI-selected blazars

Jonas Ringholz, Universität Würzburg, 2017-04-03 - 2017-04-05

Time: 20

According to the unification model of active galactic nuclei, Bl Lac objects are considered to be the beamed and rotated counterparts of FR 1 galaxies and flat spectrum radio quasars the beamed and rotated counterparts of FR 2 galaxies. The radio luminosity and the extended emission of TANAMI-selected blazars are studied, analyzing 1.4 GHz and 4.5 GHz archival VLA data.

Large Scale Structure of Blazars at Low Radio Frequencies

Jonas Ringholz, Universität Würzburg, 2018-04-16 - 2018-04-18

Time: 20

Structural and Multiband Variability Analysis of 4C +01.28

Florian Rösch, JMU Würzburg, 2018-04-16 - 2018-04-18

Time: 20

The BL Lac object 4C +01.28 is a bright and very variable radio and gamma-ray emitter. At both energy bands, high-amplitude variability is observed on time scales of days to years. We study the radio and gamma-ray light curves observed by the Submillimeter Array (SMA) and Fermi/LAT and the parsec-scale jet structure observed by the Very Long Baseline Array (VLBA) over a period of more than eight years. We find a prominent bright and compact newly ejected feature in the parsec-scale jet, which seems to be associated with a prominent outburst in the millimeter and gamma-ray bands.

SpaceIL - Landing the First Israeli Spacecraft on the Moon

Diego Saikin, Czech Technical University in Prague, 2017-04-05, evening - 2017-02-07

Time: 10 minutes

SpaceIL is the only Israeli team participating in international Google Lunar XPRIZE competition: a modern race to the Moon. Founded by 3 young engineers at the end of 2010, SpaceIL is aiming to make history and land the first Israeli spacecraft on the Moon, inspiring a generation along the way.

Two recent GRB supernovae observed with GROND and VLT

Schmidl Sebastian, Thüringer Landessternwarte, 2015-04-20 - 2015-04-24

Time: 20 minutes

Long GRBs at low redshift (z < 1) can be accompanied by an observable type Ic Supernova. In the Swift era (2005+) typically 1-2 GRB-SNe are spectroscopically confirmed per year, resulting in a total sample size of only about 15 events so far.

Here I report about 2 recent GRB Supernovae (GRB 120714B at z= 0.40, GRB 130831A at z = 0.48), which were followed-up by GROND at the 2.2m telescope on La Silla and were pectroscopically confirmed with the VLT by our team. I discuss the light curves from the first hours up to several months after the burst in all 7 GROND bands (g\'r\'i\'z\'JHK). In addition, I present the results obtained from our VLT spectra around the time of the corresponding SN peak.

Self-consistent simulations of the observable flux of accreting neutron stars

Falkner Sebastian, Dr. Karl Remeis-Observatory & ECAP, 2015-04-20 - 2015-04-24

Time: 10

We present our ongoing work on self-consistent simulations
of the observable flux of accretion powered, magnetized X-ray pulsars. Applying a new Monte Carlo code simulating cyclotron resonant
scattering features by propagating photons in flexibly configurable
geometries, we produce intrinsic emission profiles of
an accretion column. Based on these emission profiles we calculate
the observed phase and energy dependent flux using a general
relativistic light bending code. We developed this code to simulate pulse
profiles of pulsars. It allows for arbitrary geometries and emission
profiles of the emission region (e.g., accretion column), while keeping
the computational time low.

GMRT image of PKS2155-304 at 1.4GHz

Michael Seeg, University Wuerzburg, 2017-04-03 - 2017-04-05

Time: 15

Archival data from the Giant Metrewave Radio Telescope (GMRT) of PKS2155-304 at 1.4GHz is presented. With a resolution of 3.91x2.86 arcsec new insights of the extended emission of this source can be obtained.
Active galactic nuclei (AGN) form highly relativistic particle jets by accreting matter onto a super massive black hole. If the angle to the line of sight to such an object is small, these objects are referred to as blazars, which ususally show a flat spectrum in the GHz regime due to the dominance of beamed core emission.
By observing in the MHz regime, unbeamed, extended emission become optically thin and allow to study the morphology of the extended structures and the ratio of luminosity emitted by them and the core structure.

Very soft X-rays: an almost neglected band for monitoring

Vojtech Simon, Astronomical Institute AS CR, 2014-04-22 - 2014-04-25


Monitoring of X-ray emission of the cosmic X-ray sources is usually carried out in the energies of emission of 2 or more keV. Nevertheless, absorption of X-rays in the interstellar medium is sufficiently small even for the energies as low as 0.2-0.5 keV, which gives us opportunity to study the processes which produce emission in this band. We will discuss the astrophysical binary sources and their emission processes which at least sometimes produce very intense, even dominant very soft X-ray emission (E<1 keV). Such emission is beyond the band in which most monitors operate. These emission processes thus often remain unexplored, and in some cases the objects even remain undetected if this very soft emission is transient.

The optical long-term activity of the high-energy sources: Perspectives for GAIA

Vojtech Simon, Astronomical Institute CAS & CTU in Prague, 2015-04-20 - 2015-04-24

Time: 30

We will discuss the possibilities of observing the optical counterparts of high-energy cosmic sources of various types in the data from the Gaia satellite. We will show that identification of optical afterglows of gamma-ray bursts can be made using their very specific color indices. We will also show how the active optical counterparts of binary high-energy sources can be classified and studied by the statistical methods even in the sampled data which will be provided by the Gaia satellite.

Monitoring the soft X-ray transient Aql X-1

Vojtech Simon, Astronomical Institute CAS & CTU in Prague, 2015-04-20 - 2015-04-24

Time: 25

We will show the long-term activity of the soft X-ray transient Aql X-1. This system which contains a mass-accreting neutron star displays outbursts with the recurrence time of about 200 - 300 days. The profile of the outburst largely differs for various energy bands not only as regards their profiles, but also as regards the duration of the event and the time of the peak intensity.

X-ray monitoring of cataclysmic variables

Vojtech Simon, Astronomical Institute CAS & CTU in Prague, 2016-04-18 - 2016-04-21

Time: 30

We will show that the available X-ray monitors can detect cataclysmic variables (CVs) which contain magnetized white dwarfs. This suggests that the mode of accretion is very important for the detection. The reason is that only a radial flow onto the accretion region on the magnetized white dwarf causes sufficiently hard X-ray spectrum to be observable by the current monitors. Monitoring the X-ray emission is important for observing the activity of such sources on long timescales (months, years). We will also show the possible ways of studying the faint X-ray CV emitters using these data.

Perspectives of the lobster-eye telescope: The promising types of cosmic X-ray sources

Vojtech Simon, AI CAS & FEL CVUT, 2017-04-03 - 2017-04-07

Time: 30

We show the astrophysical aspects of observing the X-ray sky with the planned lobster-eye telescope. This instrument is important because it is able to provide wide-field X-ray imaging. For the testing
observations, we propose to observe X-ray binaries (mostly persistent sources) in which matter transfers onto the compact object (mostly the neutron star). We show the typical X-ray spectra and the features of the long-term activity of such objects. Observing in the soft X-ray band is the most promising because the X-ray intensity is the highest in this band. Since these X-ray sources tend to accumulate toward the center of our Galaxy and in the vicinity of the galactic plane, we show that it is sufficient to monitor these areas.

Accuracy of DSLRs

Petr Skala, CVUT, 2014 4 22 - 2014 4 25


This talk deals with problematic whether is possible to use DSLR (digital single-lens reflex) cameras for precise measurement. Digital cameras have good cost to performance ratio thus they are good candidates as tools for digitalization of astronomy glass plates and photometric measurement. This paper show what affect output data accuracy of such devices.

Measurement of properties of wide field lenses

Petr Skala, CTU FEL, 2015 04 20 - 2015 04 24

Time: 15- 20 min

How to measure MTF and other important properties of wide field lenses if they are not spatially invariant?

Measurement of KV and Sonnenberg wide cameras

Petr Skala, CTU, 2016 04 18 - 2016 04 21

Time: 15 min

Gama ray burts are quick and dynamic objects, and observation with big telescopes require fast response and a bit of luck. Many observatories use all sky monitors wich takes images all night and can be able to detect GRB.

Astrometric calibration of ultra wide-field images

Petr Skala, CTU, 2018-05-16 - 2018-0520

Time: 20m

This work will introruce new method of astrometric calibration tailored specially for ultra wide-field systems like WILLIAM. Standard astrometric solution often fail to provide any result if processed image contain large amount of distortion as for examlpe from fish eye lens. Some algorithms produce result but accuracy is satisfactory only at center of field of view.
This work analised such images and propose new method that lead to mutch higher accuracy and succes ratio of calibration.

Study of radiation impact on orbit

Veronika Stehlikova, CTU FEE, -

Time: 5-10

The new carbon fiber material will be tested as shielding material for future usage on large satellites. The Cube carries three PIN diodes and one CdTe detector. PIN diodes are shielded with wolfram from behind to eliminate secondary radiation generated inside the probe. Active layers are orientated to the free space and each one of them has different shielding. One is protected by wolfram plate, the second by the tested carbon fiber and the last does not have any covering. Signal from diodes is amplified, led to another board and digitalized. Signals energy is awaited to begin about 10 keV. Data from new material measuring will be compared to reference diodes and final results will be processed on the Earth.

Radiation resistance measurement on VZLUSat-1

Veronika Stehlikova, CTU FEE, 2016-04-18 - 2016-04-22

Time: 15

The Measure payload on VZLUSat-1, which ought to be launched in summer 2016, will measure radiation environment in orbit. This payload will test a new shielding material with better radiation resistance as well. All before-flight tests were already performed and their results will be mentioned also in this article.

REX - Rocket X-ray experiment

Veronika Stehlikova, CVUT FEL, 2017-04-04 - 2017-04-07

Time: 15

An X-ray telescope planned for a rocket experiment. State of works, background and possible targets of observations during the mission.

High precision calibration of interstellar oxygen absorption

Jakob Stierhof, FAU Remeis Observatory, 2018-04-16 - 2018-04-18

Time: 10

I will shortly present the results of our experiments performed at BESSY to
measure the transition energies of neutral oxygen. We used a portable electron
beam ion trap (EBIT) to produce He-like ions of nitrogen and recorded the
fluorescence of the 1s-np transitions with large area solid-state detectors.
Simultaneously we recorded the photoion yield in an O2 gas cell.
We achieved a precision of 30 meV in our measurements by calibrating the
O2 Rydberg spectrum against the 1s-6p and 1s-7p transitions of He-like N VI.

Autonomous robotic telescopes in Ondrejov: D50 & BART

Jan Strobl, ASU AV CR, 2015-04-20 - 2015-04-24

Time: 30

We would like to present the actual state, recent advances and results of our autonomous robotic telescopes BART & D50, both located in historical part of observatory in Ondrejov, Czech Republic.

BART & D50: wide future

Jan Strobl, ASU AV CR, 2017-04-03 - 2017-04-07

Time: 15

We would like to shortly introduce autonomous robotic telescopes in Ondřejov Observatory in actual configuration and also discuss intended future changes and advances.

Tester for SMILE instrument SXI

Petr Suchánek, evolving systems consulting s.r.o., 19.4.2016 - 20.4.2016

Time: 5-10

A short talk based on current knowledge of the SXI instrument and several aspects on how testing of the instrument can be performed.

OpenStack: An Open Source Cloud Platform

Gabriel Szász, Red Hat Czech, s.r.o., 2014-03-22 - 2014-03-25

Time: 20

Cloud computing has already become an essential technology for any organization that depends on complex IT infrastructure. This technology enables agile-style development, it scales automatically with infrastructure needs and it provides a platform for high-availability applications.

The OpenStack project provides powerful open source tool for building your own public and/or private clouds. Nowadays, it is the second largest open source project on this planet, right after Linux.

This short talk gives a brief overview of the cloud computing technology and its impact on modern science. Then it introduces the OpenStack project and compares it to the other open source cloud projects that are currently available.

Dawn of the Scientific Cloud Computing

Gabriel Szász, Red Hat Czech, s.r.o., 2015-04-24 - 2015-04-20

Time: 20

Cloud computing is undoubtedly changing whole paradigm of the IT as we knew it. By standing on the edge of a revolution, we are finally getting closer to the solution of the data avalanche - one of the most prominent problems of the modern science.
We will discuss advantages of using cloud computing in contemporary astrophysics. In a short demo, we will also introduce OpenStack as an example of the open source cloud platform.

How may GRBs form? An overview of progenitor theories

Dorottya Szécsi, ASU CAS CZ, 2017-04-03 - 2017-04-07

Time: 30+10

The origin of GRBs is still an actively studied subject. On one hand, we have been collecting more and more observationally constrained properties of GRB-physics. On the other hand, new theoretical results on the progenitor evolution (be it stellar or compact object) have also emerged. My talk is a review of the existing progenitor models for both long-duration and short-duration GRBs. I will discuss their potentials and limitations, putting them in the context of recent observational discoveries.

Project JEUMICO – Bavarian-Czech Cooperation on the development of X-ray mirrors

Doehring Thorsten, Hochschule Aschaffenburg, 2016-04-18 (late in the evening) - 2016-04-21 (at early morning)

Time: 20 minutes + 10 min discussion

In 2015 a joint call of the Bavarian State Ministry of Education, Science and the Arts and the Ministry of Education, Youth and Sports of the Czech Republic for joint projects was published. The intention of this call was to enhance scientific cooperation between the Czech Republic and Bavaria. Scientists from Aschaffenburg University of Applied Sciences and from the Czech Technical University in Prague submitted a joint proposal for a bilateral project. The aim of the project JEUMICO, an abbreviation for “Joint European Mirror Competence”, is the effective combination of experience, expertise and instrumentation of the Bavarian and the Czech partner in design, development, manufacturing, simulation and testing of innovative X-ray mirrors by the application of thin films and nanotechnology. Within this field the partners have valuable and complementary experience. Funding was granted in early 2016 and the project was recently started officially with a kick-off meeting in Prague.

Optimization of lobster eye geometric parameters

Vladimir Tichy, University of Leicester, 2018-16-04 - 2018-20-04

Time: 15

A method of analytical calculating of effective collecting area (length) is presented. The method is applied to few reflectivity models. The method allows searching for optimal values of all geometric parameters of lobster eye with respect to common design considerations. The method is applicable for Schmidt as well as for Angel lobster eye design.

NANOX - Proposed Nano-Satellite X-Ray Monitor

Vladimír Tichý, Czech Technical University in Prague, 2014-04-22 - 2014-04-25

Time: 15

The concept of a nano-class satellite providing permanent monitoring of specified sky area in X-rays is presented. Using of Schmidt lobster optics is proposed. The results of experimental tests of the specimen of such optics show the mission is feasible.

Mathematical descriptions of multi-foil optics

Vladimír Tichý, Czech Technical University in Prague, 2015-04-20 - 2015-04-24

Time: 15

The contribution is aimed to methods
First, numerical method based on simplifying common ray-tracing procedure is presented.
Some optics, like Schmidt lobster eye does not require to
calculate traces of all rays are necessary to simulate but only of few ones.
Therefore, the presented method is extremely effective. Moreover, to simplify
the equations, the specific mathematical formalism is used. Because only few
simple equations are used only, the program code can be simple as well.

Optical study of nano-satellite x-ray monitor

Vladimír Tichý, Czech Technical University in Prague, 2015-04-20 - 2015-04-24

Time: 15

The Schmidt lobster eye design for a grazing incidence X-ray optics provides wide field of view of the order of many degrees, for this reason it can be a convenient approach for the construction of space X-ray monitors. Schmidt lobster eye is possible to assemble in various scales of dimensions and also dimensions and focal lengths acceptable for nano-class satellites are possible. In this paper, draft of nano-class space mission providing monitoring of specific sky area is presented. Preliminary optical design study for such mission is performed. Two of possible opticle designs are presented. For those designs, field of view, effective input area and other basic optical parameters are calculated.

Analytical modelling of lobster eye optics

Vladimír Tichý, Czech Technical University in Prague, Faculty of Electrical Engineering, 2016-04-18 - 2016-04-21

Time: 10

Analytical equations describing lobster eye optical parameters on dependence on its geometric parameters are
presented. Analytical method of calculating effective collecting length and its maximization is presented. The
results are applicable for a Schmidt as well as for an Angel lobster eye.

Public talk: Dark forces of the Universe (Přednáška pro veřejnost: Temná síla Vesmíru)

Martin Topinka, CTU, 2015-04-20 - 2015-04-24

Time: 60\'

Volně Inspirováno přednáškou předního světového kosmologa Michaela Turnera, autora prací o Velkém třesku, raném Vesmíru nebo temné energii.

Machine learning classification of short transient $\\gamma$-ray events

Martin Topinka, CTU, 2015-04-20 - 2015-04-24

Time: 30\'

+/- what the title says, trained on the INTEGRAL IBIS/ISGRI data.

Personal Space

Martin Topinka, CTU, 2015-04-20 - 2015-04-24

Time: 10\'

Igniting interest in astronomy by showing deep sky objects in the patch of the sky above your head. It\'s not a real talk, I am advertising that Personal Space is looking for a coder.

Vertical self-gravity in discs and outer edge effects

Audrey Trova, Astronomical institute, 2014-04-22 - 2014-04-23


For massive enough or/and extended gaseous disks, self-gravity is important and can partly govern hydrostatic equilibrium. According to Paczynski\'s approximation (Paczynski 1978), the vertical gravity field is a linear function of the surface density. This approximation, often used in the context of star formation and accretion in Active Galactic Nuclei, clearly fails in zones where gradients of density and thickness are noticeable (typically discs edges). By analytical means, we have estimated the vertical component caused by a vertically homogeneous disc (in integral and algebraic forms) with an accuracy better than 1%. At zeroth order, Paczynski\'s approximation can be corrected (i.e. Extended) and the new formula depends on the relative distance to the outer edge and the local disc thickness. We will present this two results which are interesting to better understand the impact of self gravity on the hydrostatic equilibrium and to better model the outer disc where most observations come from.

Ultra-high-energy fragments from beta-decay in the vicinity of supermassive black holes

Arman Tursunov, Silesian University in Opava, 2018-04-16 - 2018-04-20

Time: 15-30

Origin and mechanism of production of ultra-high-energy (UHE) particles with detected energies above 10^{20} eV in cosmic rays remain a subject of intensive discussions. It is generally believed that the sources of detected UHE particles should be of extragalactic origin. I will show that such particles can be produced within a neutron beta-decay in the dynamical environment and vicinity of supermassive black holes (SMBH) located at the centers of galaxies by extracting out the energy of the central SMBH. Magnetic fields, which are usually present around black holes, play the role of catalyzing element that increases the efficiency of the energy extraction. Taking into account the back-reaction of individual charged particles one can put constraints on the mass of SMBH and magnetic fields in its vicinity to produce UHE particles within the model. From this, it follows that these are more likely protons, which may escape from SMBH, while Sgr A* at the Galactic Center cannot serve as a source of such UHE particles, mainly due to its relatively low mass.

Distributed small systems for scientific applications in space

Tristan Tzschichholz, Zentrum für Telematik e.V., 2014-04-23 - 2014-04-23


Within the nationally funded YETE project, a distributed system of nodes is envisioned, capable of providing a platform for universal experiments and applications. The nodes may be small satellites, rovers, and groundstations. The goal of the project is to implement a universal wireless communication technology which allows seamless operation even in case of complete or partial node failure, as the wireless links go down even towards the sensor/ subsystem layer. The interal harness of a node is reduced to just the power lines. This particular approach is feasible for artificial aperture measurements (optical or RF), field strength measurements, radiation measurements, and so on especially in hazardous environments where system failures are to be expected. The system also allows for long chains of satellites or rovers (or a mix of both) for exploring surfaces of stellar objects.

Measurement of evaporation and evaluation of changes of the mechanical properties on nanosatellite

Martin Urban, Czech Technical University in Prague, -

Time: 10

The goal of the measurement of gas in space is detection of vaporization of some residual water or other substances from material. To check this there will be placed several different types of sensors in the probe. These sensors were assembled to the PCB Measurement board. Four of them are digital sensors with integrated thermometer. Last three sensors are HAL2 type measured by PicoCap2. These sensors are analogue and return value is ratio of capacity compared to nominal capacity. From these values are calculated humidity. Mechanical changes are evaluated by using Fast Fourier Transform. With FFT are analysed changes in resonance frequency by the time.

Volatiles payload on VZLUSAT-1 and thermal cycling in vacuum chamber

Martin Urban, CVUT FEE, 2016-04-18 - 2016-04-22

Time: 15

This talk is about before-flight tests on VZLUSAT-1 CubeSat satellite, which will be launched during summer 2016. Full function tests of the payload carrying several different sensors for measuring of humidity. Measuring in thermovacuum chamber during thermal cycling, according to QB50 mission requirements.

Earth’s thermal radiation sensors in attitude determination systems of small satellites

Ivo Vertat, University of West Bohemia in Pilsen, 2017-04-06 - 2017-04-06

Time: 10-15

Attitude determination of satellites could be very complex issue with expensive hardware and software solutions including camera star trackers, two axis sun sensors, earth horizon detectors, magnetometers with Kalman filtering and model of earth magnetic field, etc. Moreover, it could spend the most of resources (volume, mass, electric power) on small satellites like CubeSats. One of potentially interesting type of sensors for attitude determination systems in small satellites could be detectors of infrared thermal emission. Nowadays, these sensors are widely used in contactless thermometer and thermo-cameras resulting in low-cost of this technology. Infrared thermal sensors can be used for rough determination of small satellite orientation on LEO due to close proximity of relatively warm Earth’s disc.

Low Cost Camera System for Short Term Sounding Rocket Experiment

Ivo Vertat, University of West Bohemia, 2018-04-19 - 2018-04-20

Time: 15

In this talk the preparation of low cost industrial camera system for short term sounding rocket experiment will be described. The main purpose of prepared camera system during only several minutes mission in space is to confirm the right pointing of roentgen optics telescope to the target nebula. The secondary goal of the camera system is its testing in space environment for potential usage in small satellites. Space qualified camera systems for satellites are very expensive in order of several tens thousands of Euro and for short term and low-cost missions of sounding rockets or CubeSat missions there are inappropriate. We prepared a relatively common industrial camera Ximea MQ013CG-E2 with ThorLabs MVL50M23 lens for this purpose. The price of this camera hardware is less than 500 Euro. The preparation of camera includes mitigation of real camera properties and enhancing of image properties. There was also prepared a special regime of camera utilization during mission, because of many unknown aspects of sounding rocket mission and unknown real camera behavior in space. This covers shooting of images with variety of exposure settings, shooting of dark reference images during all space mission and logging the temperature condition of camera sensor during image shooting.

PilsenCube picosatellite - project overview

Ivo Veřtát, University of West Bohemia, -


The main goals of PilsenCube picosatellite project will be presented as well as the main idea of subsystem technical solution.

Pilsen Ground Station for VZLUSat-1

Ivo Veřtát, University of West Bohemia, 2016-04-19 - 2016-04-19

Time: 10-15

A talk about the ground control station of VZLUSat-1 for satellite commanding and operating. During the talk the web application for satellite operators will be presented as well as automatization of radio transmission and data handling.

RTS2 for people

Stanislav Vitek, CTU in Prague, 2014-04-22 - 2014-04-25

Time: 20

During this talk I will give short overview about how to control any RTS2 based telescope in
real-time with mobile web application.

Real-Time Image Processing In Astronomy

Stanislav Vitek, CTU FEE, 2018-04-18 - 2018-04-18

Time: 20

In this talk, I will briefly summarize the general ideas of real-time image processing in astronomy, and also introduce problems and challenges related to this topic. I will also show some examples of real-time processing pipelines.

The ATHENA end to end simulations

Joern Wilms, Remeis-Sternwarte & ECAP, 2015-04-22 (evening) - 2015-04-24

Time: 30\'

ATHENA, to be launched in 2028, is the next large X-ray observatory. The mission is currently in its definition phase. As part of the definition, a large number of science simulations are to be performed to understand the scientific performance of the mission. In this talk I will present an overview of the end-to-end simulation framework for the ATHENA mission.

Transition Edge Sensors

Joern Wilms, ECAP & Remeis-Sternwarte, 2016-04-18 - 2016-04-19

Time: 20\'

I will present a review of the physics of Transition Edge Sensors, using the example of the X-IFU instrument on Europe\'s future X-ray mission ATHENA. TES are cryogenic detectors operated at a few tens milli Kelvin. They have an energy resolution of a few eV, i.e., roughly comparable to X-ray gratings, and imaging capabilities, allowing the instruments to be used as integral field spectrometers.

Gamma-rays from binaries

Andrzej ZDZIARSKI, N. Copernicus Astronomical Center, 2017-04-03 - 2017-04-07

Time: 30

I will review the current status of gamma-ray observations from different types of interacting binaries. I will discuss, in particular, new results on Cyg X-1 and Cyg X-3.

Geometry of X-ray sources in accreting black-hole binaries

Andrzej ZDZIARSKI, N. Copernicus Astronomical Center, 2017-04-03 - 2017-04-07

Time: 30

Accreting binary stellar systems containing black holes and low-mass donors are transient, i.e., they outburst after a period of quiescence, and those with high-mass donors are persistent. Both of them exhibit two main luminous states, spectrally soft and hard. Their X-ray spectra in the soft and hard states are dominated by blackbody emission of accretion discs peaking around 1 keV, and by a component peaking around 100 keV from Compton scattering by mildly relativistic electrons, respectively. There is a general consensus about the nature of the soft state, in which an optically thick accretion disc emitting blackbody radiation extends down to the innermost stable circular orbit (ISCO) around the black hole. However, there is currently a heated controversy regarding the nature of the hard state. According to a long-dominant paradigm, the accretion disc in this state is truncated at a radius >> ISCO and replaced by a hot flow emitting hard X-rays. This explains many observed phenomena, e.g., spectral and variability differences between the states and transition to the hard state from quiescence (when the disc is certainly truncated) in transients. On the other hand, there have been numerous claims that the disc extends to ISCO also in the hard state, and the hard X-ray source is located on the black-hole rotation axis and very close to the horizon (a \'lamppost\'). I will discuss both the theoretical and observational arguments for the disc truncation and against the \'lamppost\' geometry.

Galactic Center Minispiral: Interaction modes of neutron stars

Michal Zajaček, Astronomical Institute, Academy of Sciences, -


Streams of gas and dust in the inner parsec of the Galactic Center form a distinct feature known as Minispiral, which has been studied in radio and infrared wavebands (Kunneriath et al., 2012). Large fraction of the Minispiral gas is ionized by radiation of stars present in the Nuclear Star Cluster (NSC). Based on the inferred mass in the inner parsec about 10^6 solar masses, over ~10^4 neutron stars should move in the sphere of gravitational influence of the SMBH. We estimate that a fraction of them propagate through denser (ionized) medium concentrated along three arms. Based on the density and the temperature of the gaseous medium, we discuss interaction regimes of magnetised neutron stars passing through the Minispiral region. The simulation results may be applied to other galactic nuclei hosting NSC where the expected distribution of interaction regimes may be quite different.

Passages of stars close to the Galactic center: can we detect any signal?

Michal Zajaček, Max Planck Institute for Radioastronomy, 2018-04-15 - 2018-04-20

Time: 30

Over the past 20 years, several bright stars were detected to orbit the supermassive black hole in the Galactic center. Their pericenter orbital speeds are several 1000 km/s. Given the properties of the local interstellar medium, we analyze the conditions for the formation of shocks while stars reach the pericentre. In addition, the observability of these shocks is discussed across the whole electromagnetic spectrum.

Epsilon Centauri and Epsilon Persei observed by space telescopes BRITE

Elzbieta Zoclonska, Nicolaus Copernicus Astronomical Center PAS, 2016-04-18 - 2016-04-22


Analyses of observations of two Beta Cephei stars carried out with small space telescopes of BRITE-Constellation are presented. Eps Centauri and Eps Persei are bright, massive stars with low-amplitude pulsations in visible light. Thanks to precision photometry from BRITE, the determination of multiple pulsation frequencies was possible. Additional ground-based spectroscopic observation were done for Eps Persei. The combination of both space photometry and ground-based spectroscopy led to determination of further properties of the pulsating star and the multi-object system of with this star is the primary member.

BART&D50: the new era

Jan Štrobl, ASÚ AV ČR, 2016-04-18 - 2016-04-21

Time: 15

We would like to shortly announce recent significant advances, concerning robotic telescopes BART and D50 in Ondrejov Observatory.


Elimination of barrel distortion using wide-field imaging system calibration

Elena Anisimova

CTU in Prague, FEE

Wide-field imaging systems are used as subsidiary monitoring equipment for robotic telescopes nowadays. These electro-optical systems usually complement the main telescope during acquisition of astronomical phenomena or support its operation e.g. evaluating the weather conditions. We have a deal with such kind of support for robotic telescopes as are BOOTES, TAD, BART and Pi of the Sky, which are or are planned to be integrated into GLORIA FP7 project until end of September 2014. Acquired images by mentioned imaging systems suffer from image distortion because of wide field of view of input lens (cca 180 deg.). It is mostly barrel distortion, which causes inability of astronomical software (IRAF, SExtractor) to process acquired image data. There are two ways how to solve this problem. Existing methods could be modified for processing of images taken by wide-field systems or lens distortion could be removed and existing algorithms could be applied. In the second case, it is necessary to carry out imaging system calibration and to apply geometrical transformations on processed image data. In this case, it is very important to find out, how elimination of distortion affects accuracy of astrometric and photometric measurement of stellar objects. In this paper we describe our experience in this area.

GRBspec - database and visualizing tool for GRB spectra

Martin Blazek


Blazek M., Janout P., Pata P., Ugarte Postigo A.

Flare Alerts for TeV Blazars from FACT

Daniela Dorner

Universität Würzburg

The First G-APD Cherenkov Telescope (FACT) is monitoring bright blazars at TeV energies. The main targets are the bright TeV blazars Mrk 421
and Mrk 501, but also other objects like 1ES 2344+51.4 and 1ES 1959+650 have been observed already with more than 200 hours each.

Thanks to using silicon based photosensors, observations during strong moon light are possible enlarging the duty cycle of the telescope. Also the stable performance of these photosensors makes the telescope an ideal instrument for long-term monitoring.

To provide fast response on the source activity and automatic flare alerts, a quick look analysis has been set up on-site. The results of this processing are immediately available on a public website allowing for fast flare alerts and target-of-opportunity observations.

In this presentation, results from the quick look analysis will be shown and the flare alert procedure explained.

AROM: Autonomous robotic observatory manager

Roman Dvořák


AROM (Autonomous robotic observatory manager) is a set
of open-source software for the control and management of
robotic observatories. The whole software is built upon a
system for controlling robots - ROS (Robotic operation sys-
AROM software is designed for use with small (amateur)
telescopes and fully autonomous observatories and is go-
ing to work on simple single-board computers like Odroid.
Software should be able to monitor all telescope states
which may affect observing quality. These conditions include
weather, air quality, observatory status, mount position and
many others.

Bolidozor radio meteor detection network

Roman Dvořák


Bolidozor represents a cooperative network project, which uses technical equipment owned by volunteer observers, who operate the detecting and measuring stations.

The core of the system is made of a network of meteor radio detectors that are gradually upgraded and extended to contain new measurement methods. The aim of the project is to measure the parameters of meteor flybys through the atmosphere, to calculate their dark flight and to locate the meterites in their impact ellipse.

Applications of iridium for satellites and in other high technology areas

Thorsten Döhring

Aschaffenburg University

Due to its unique physical and chemical properties the rare noble metal iridium is enabling fascinating applications for satellites and in other high technology areas. For example: The coating laboratory at Aschaffenburg University of Applied Sciences is sputtering thin iridium reflection layers for space-based astronomical X-ray mirrors and iridium coatings as diffusion barrier for hydrogen isotopes in sophisticated scientific experiments. Background on different applications of iridium and on some experimental realizations will be presented.

The 2011 giant outburst of 4U0115+634 as seen with Suzaku

Dominik Hertel

Dr. Karl Remeis-Observatory & ECAP

We present an analysis of X-ray spectra of the high mass X-ray binary 4U 0115+634 as observed with Suzaku in 2011, July.
We moedeled the X-ray spectra with an absorbed cutoff power law modified by iron fluorescence lines and cyclotron resonance features. Our results are consistent with the recent conclusion that the centroid energy of the fundamental cyclotron line of 4U 0115+634 remains constant for all absorved flux ranges, contrary to earlier claims.

Studying the variability of the X-ray spectral parameters of high-redshift host galaxies

Agnes Johanna Hortobagyi

Eötvös Loránd University, Budapest

Several results of measuring high-redshift X-rays are available for GRBs that have been detected by Swift. The standard process of fitting is usually by using general starting parameters - the variability of fittings hasn’t been examined yet throughoutly, as is the case with the robustness properties of the X-ray spectral fittings. With the available, more precise input datas we can examine the robustness of previous fittings, and test how sensitive is the result to the changes of the starting parameters.

GLORIA Project and Investigation of Cataclysmic Variables

Rene Hudec


GLORIA Project and Investigation of Cataclysmic Variables within this project will be briefly presented and discussed

GLORIA Project Telescopes BART and D50

Rene Hudec


GLORIA Project Telescopes BART and D50 will be briefly presented and discussed

Biomimetics and Astronomical X Ray Optics

Rene Hudec


Biomimetics and Astronomical X Ray Optics will be shortly discussed

Zernike polynomials used for stellar object fitting

Petr Janout

CTU Faculty of Electrical Engineering

A Point Spread Function (PSF) of theoretical astronomical imaging system is considered to be time and space invariant. It means that the PSF is invariable within an exposed image. This assumption is however not fulfilled especially in the case of real wide-field imaging systems which are used as subsidiary monitoring equipment for robotic telescopes nowadays. Mentioned systems could be used for robotic telescopes as are BOOTES, TAD, BART and Pi of the Sky, which are integrated into GLORIA FP7 project. Optical aberrations are expected to be space variant in real wide-field imaging systems, e.g. coma is expected to have strong dependency on distance from the captured image center. It has an impact on the efficiency of the stellar astrometry and photometry algorithms which usually work supposing space and time invariance of the imaging system’s PSF. In this paper we use Zernike polynomials to form PSF of such space variant system: we study dependency of the Zernike polynomial parameters on position of the stellar objects. We assume coma, astigmatism and spherical aberration of the system.

Cosmic rays and thunderstorms at Lomnický štít.

Ronald Langer

IEP SAS Kosice, Slovakia

Since March 2014 at Lomnický štít is operating the muon detector SEVAN in the continuous mode. Its measurements complement the long term detection of cosmic rays (CR) by neutron monitor. In presentation we review the existing profiles of measurements in several channels of SEVAN, that have different response to different types and energies of secondary CR particles at altitude 2634 m asl. We discuss a couple of events during 2014 and 2015 when short term increases of count rate by SEVAN have been observed around the time intervals of thunderstorm activity in the vicinity of Lomnický štít. Brief review of current status in research of so called thunderstorm ground enhancements (TGE) and of their possible relations to terrestrial gamma ray flashes (TGF) studied nowadays on satellites is done. One such event we reported earlier in the region of the magnetosphere geomagnetically conjugated with the site of strong thunderstorm activity on satellite CORONAS-F [1].
The work is supported by VEGA grant No 2/0026/16.
[1] R. Bučík, K. Kudela, and S. N. Kuznetsov, Satellite observations of lightning-induced hard X-ray flux enhancements in the conjugate region, Ann. Geophys., 24, 1969-1976, doi:10.5194/angeo-24-1969-2006, 2006

Miniaturized X-ray telescope for VZLUSAT-1

Michal Platkevic

IEAP, CTU in Prague

Presented Miniaturized X-ray telescope instrument is based on 1D Lobser eye optics and hybrid silicon pixel detector Timepix (256 x 256 pixels with pitch of 55 μm). Aim of this payload on the VZLUSAT-1 CubeSat is localization of different X-ray radiation sources.

Brightness distribution of GRB host galaxies using survival analysis

Istvan Racz

Konkoly Observatory of the Hungarian Academy of Science

Authors: I. Racz; Z. Bagoly; L. G. Balazs; L. V. Toth; I. Horvath

We studied the relationship between the Swift GRB data and the optical brightness of the host galaxy measured by the Keck telescope. We calculated the unbiased distribution of the host\'s optical brightness by making use the survival analysis. Based on the sample obtained from merging the Swift GRB table and the Keck optical data we studied also the dependence of this distribution on the GRB\'s data.

Vision in the Deep Sea: Mirror Eyes

Kateřina Remišová

Astronomical Institute ASCR, Charles University in Prague

Radiation resistance monitor on VZLUSAT-1: preliminary results

Veronika Stehlikova

Czech Technical University in Prague

The technological CubeSat VZLUSAT-1 was launched in June, 2017 and carries a number of scientific and commercial experiments aboard.
Several of them are focused on in-orbit investigation of a novel carbon-fibre composite developed by 5M company; examination of residual liquids evaporation, change of eigenfrequencies of the material according to the ageing of it, and shielding abilities against cosmic radiation.

The quality of shielding is evaluated as a comparative measurement between three channels with different shielding.
Each channel contains a calibrated biased PIN diode as a radiation sensor, which is sensitive to radiation in 2 keV to 20 keV energetic range.
Preliminary results from the in orbit measurements are presented in this paper.

Competing proposals for satellite components - a case study for engineering students

Doehring Thorsten

Hochschule Aschaffenburg

Future sales engineers are educated within the bachelor degree program „International Technical Sales Management“ at Aschaffenburg University of Applied Sciences. Based on skills acquired in previous semesters, the interactive lecture “project study” is given in their second year. As a case study the students have to prepare voluminous proposals for satellite components in competing teams. Thereby the complete set of original ESA tender documents including norms and standards is shocking them at first. Work sharing and teamwork reduces the effort. At the end of the semester the students acknowledge the learning effect at and the resulting proposals are already quite professional. It is the aim of this course to confront students with such sometimes painful exercise at university and under guidance of a professor with corresponding industrial experience - before they get shocked and overburdened in their first sales job by an extensive sales proposal.

Implementation of lobster eye optics to QSOFT software package

Vladimír Tichý

University of Leicester

QSOFT package represents a general tool for simulation of x-ray optics. The program code is based on sequential ray tracing algorithm. Currently simulation of lobster eye optics is being implemented and tested. Examples of results and their comparison to results of simplified ray tracing algorithm are presented.

Searching for data on Cracow astroplates

Kundera Tomasz

Astronomical Observatory of the Jagiellonian University

We shortly described our problems with gathering our astroplates in one place. Many reasons have caused they have not been properly preserved and stored.

Metadata for digitized astronomical plates

Richard Urban

CTU in Prague; EMS Prague-East

Metadata for digitized astronomical plates represent important issue for investigations using these databases. Description of metadata creation method used for digitization with digital camera will be presented. Metadata from envelopes of astronomical plates are manually transcribed into an electronic database.
Currently more than 2000 records of these plates are placed in electronical archive.
For more information please visit website .

Orbital motion of test particles around a rotating neutron star

Gabriela Urbancova

Silesian university in Opava / Astronomical Institute ASCR

Rotating neutron stars can be characterized by three main parameters - a gravitational mass $M$, an angular momentum $J$ and a quadrupole moment $Q$. In this presentation we will demonstrate combinations of $M$, $J$, $Q$ allowed by realistic equations of state of a dense nuclear matter. We will also discuss how these parameters affect orbital motion of test particles around rotating neutron stars. Our motivation is based on X-ray observations of binary systems with a neutron star accreting matter from its companion.

Small satellite development at the University of West Bohemia

Ivo Veřtát

University of West Bohemia

Identification of all fundamental weaknesses of standardized small satellites, called CubeSats, and the development of new solutions were the main goals of our project. The project focused on efficiency and reliability of solar power generation and accumulation, radiation susceptibility of electronics system and sufficient radio transmission data throughput toward the ground control station.

GLORIA: project status after two years of lifespan

Stanislav Vitek

CTU in Prague

This poster will give short overview about current status of GLORIA project.

D50 & BART : tandem of robotic telescopes in Ondrejov

Jan Štrobl


D50 & BART are autonomous robotic telescopes, located in Ondrejov Observatory. As expected, this poster will summarize the actual parameters, capabilities and observational program of these telescopes, which could be interesting especially for the BART telescope, as it\\\'s design and specialization has been changed radically. We would like to present also the idea of intended automated cooperation of both telescopes.