# Presentations

## 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
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
magnetosphere.

## 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.

## 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

#### Time:

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.

## 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.

## 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

#### Time:

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

#### Time:

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.

## Long-term Monitoring of Bright TeV Blazars with FACT

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

#### Time:

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, -

#### Time:

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.

## 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.

## 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

Abstract
=======
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.

## 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.

## 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

#### Time:

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

#### Time:

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

#### Time:

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

#### Time:

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

## SMILE PROJECT AND CZECH PARTICI[ATION

### 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

### 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

## COLORES on BOOTES-2, calibration

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

#### Time:

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.

## 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

#### Time:

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.

## eASTROGAM

### 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.

## 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.

## 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.

TBD

## SkCube

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

#### Time:

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

#### Time:

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.

### 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

#### Time:

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

### 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

#### Time:

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.

## Distributed small systems for scientific applications in space

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

#### Time:

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.

## PilsenCube picosatellite - project overview

### Ivo Veřtát, University of West Bohemia, -

#### Time:

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.

## 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, -

#### Time:

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.

## Epsilon Centauri and Epsilon Persei observed by space telescopes BRITE

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

#### Time:

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.

# Posters

## 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

#### CTE FEE

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

#### Bolidozor

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-
tem).
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

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.

## 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.

## GLORIA Project and Investigation of Cataclysmic Variables

### Rene Hudec

#### ASU AV CR & CVUT

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

## GLORIA Project Telescopes BART and D50

### Rene Hudec

#### ASU AV CR & CVUT

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

## Biomimetics and Astronomical X Ray Optics

### Rene Hudec

#### CVUT & ASU AV CR

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.

## 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

#### 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.

## 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.

## 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.