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październik/october 2018 |
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2018-10-05 |
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prof. LESZEK SOKOŁOWSKI |
OA UJ |
ZN OA 1493 |
Inflacja wieczna i ostatnia praca Hawkinga |
2018-10-12 |
|
prof. LESZEK SOKOŁOWSKI |
OA UJ |
ZN OA 1494 |
Inflacja wieczna i ostatnia praca Hawkinga cz. II |
Publiczna obrona rozprawy doktorskiej / Public defence of doctoral thesis |
2018-10-19 |
|
mgr MAGDALENA KULCZAK-JASTRZĘBSKA |
OA UJ |
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2018-10-26 |
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dr KATARZYNA MAŁEK |
Narodowe Centrum Badań Jądrowych, Warszawa |
ZN OA 1495 |
HELP project -- modeling spectral energy distributions of thousands IR galaxies -- dust attenuation influence for main physical parameters
The primary objective of the European Union founded HELP project is to
provide homogeneously calibrated multiwavelength catalogues covering
roughly 1300 deg2 of the extragalactic Herschel Space Observatory surveys
at wide redshift range. Millions of galaxies with UV--FIR photometry
makes HELP a perfect sample for testing spectral energy distribution
fitting (SED) codes, and to prepare tools for next-generation data. I am
going to present the project itself, and results of SED fitting pipeline
based on the pilot field for the HELP - ELAIS N1 (∼ 50,000
galaxies). I developed additional quality criteria of the fits which allow
to identify the best fits and to select peculiar galaxies (like for
example possible high-redshift galaxy candidates). I delivered the main
physical parameters of ELAIS N1 galaxies assuming three different dust
attenuation laws. We checked their influence on dust luminosity, star
formation rate, stellar mass etc. We will present our results by focusing
on the relation between stellar masses obtained with Calzetti 2000,
Charlot and Fall 2000 and Lo Faro et al., 2017 attenuation laws.
|
seminarium nadzwyczajne: godzina 14:00 / at 2:00 p.m. |
2018-10-26 |
|
prof. ALOK CHANDRA GUPTA |
Aryabhatta Research Institute of Observational Sciences - ARIES, Nainital, India |
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Variability and QPOs in Blazars with Space Based Telescopes
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listopad/november 2018 |
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2018-11-02 |
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Dzień Zaduszny / Holiday break |
2018-11-09 |
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dr WOJCIECH HELLWING |
Centrum Fizyki Teoretycznej PAN, Warszawa |
ZN OA 1496 |
Why and how we should test gravity on cosmological scales?
The GR is over 100 years old. The beautiful Einstein's relativity theory
of space-time and gravity is one of the founding block of modern physics
and cosmology in particular. In my talk, I shall discuss why one would
like (and actually really need) to design and convey tests of the theory
on cosmological scales. Then, I will also present a handful of theories
(called Modified Gravity) that aim to rival the ruling of GR at the
cosmological distances. Finally, I will present and discuss some
reasonable ways for conveying cosmological test of gravity, discuss why
most of them might fail and present some potentially promising avenues for
new class of such tests. Concluding with why you might want to stay tuned
for future in that field!
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2018-11-16 |
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dr hab. AGATA RÓŻAŃSKA |
Centrum Astronomiczne im. M.Kopernika, Warszawa |
ZN OA 1497 |
Ultraluminous X-ray sources -- new distance indicators?
We show, that broad-band NuSTAR and XMM-Newton data of three ULX sources
can be successfully fitted by single model component. Our single model
contains emission from non-spherical system: neutron star plus accretion
disk directed towards observer. We obtained the very good fit with the
reduced χ2 per degree of freedom equal 1.08 for P13, 1.01 for ULX1,
and 1.14 for ULX5. The normalization of our model constrains the distance
to the source. The resulting distances to P13 and ULX5 are in perfect
agreement with previous distance measurements to their host galaxies. Our
results confirm that P13, ULX1 and ULX5 may contain central hot neutron
star. When the outgoing emission is computed by integration over the
emitting surface and successfully fitted to the data, then the resulting
model normalization is the direct distance indicator.
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seminarium nadzwyczajne: godzina 14:00 / at 2:00 p.m. |
2018-11-16 |
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prof. GOPAL-KRISHNA |
Centre for Excellence in Basic Sciences -- CEBS, University of Mumbai, Mumbai, India |
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AGN variability: Some highlights and challenges |
2018-11-23 |
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dr hab. JERZY KRZESIŃSKI |
OA UJ |
ZN OA 1498 |
Questionable "exoplanetary" signals in sdBV and sdO subdwarf light curves
According to our investigations, some of the exoplanetary signatures found in
light curves of a couple of sdBVs (KIC 5807616 and KIC 10001893) might be of a
different origin than the exoplanet light reflection or radiation. Using light
curve simulations and Fourier transform techniques, we were able to show, that
a couple (or more) of recently reported candidates for exoplanets around these
evolved objects do not exist. At least one of the "exoplanetary candidate
systems" fails our frequency stability tests, others might be just artifacts.
We have also analyzed frequency changes of 0.256 c/d signal visible in the
light curve FT of the KIC 10449976 sdO star. Our simulations show that it is
difficult to reproduce the observed signal frequency variations by the weather
changes in the exoplanet atmosphere.
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2018-11-30 |
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mgr ANNA WÓJTOWICZ |
OA UJ |
ZN OA 1499 |
Jet production efficiency in the sample of the youngest radio galaxies
Compact radio galaxies, classified as Gigahertz-Peaked
Spectrum (GPS) sources based on their radio spectra, are believed to
represent the earliest phase in the evolution of radio-loud active
galactic nuclei (AGN).
We investigate the sample of 16 the youngest radio galaxies with measured
kinematic ages and available X-ray data from high-resolution Chandra or
XMM-Newton observations. We characterize the accretion properties and
derive the jet kinetic luminosities for our sources. We found out that
these youngest radio galaxies all accrete at high Eddington rates
(>1%), as such, they resemble more radio quasars and broad-line radio
galaxies, rather than other types of radio-loud AGN.
This, along with the fact that the objects from our sample seem
over-luminous in radio on the fundamental plane for the black hole
activity, implies also that the radiative efficiency of the compact lobes
is much higher than in the case of the evolved radio galaxies.
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grudzień/december 2018 |
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2018-12-07 |
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dr OLEH KOBZAR |
Instytut Fizyki Jądrowej PAN, Kraków |
ZN OA 1500 |
Search for ultra high energy cosmic rays from radiogalaxy Virgo A
Active galactic nuclei (AGNs) are considered to be one of the most
appropriate sources of ultra high energy cosmic rays (UHECRs, E > EeV).
Radiogalaxy Virgo A (M87) in the centre of a cluster of galaxies Virgo
Cluster (VC) can be a prominent source of UHECRs. We investigate the
possible contribution of Virgo A and the VC to the flux of events with
trans-GZK energies - extremely high energy cosmic rays EHECRs - from the
recent Auger and Telescope Array (TA) data sets (E > 52 EeV and E > 57
EeV, respectively). We simulate EHECR propagation from Virgo A and the VC
taking into account their deflections in galactic (GMF) and extragalactic
(EGMF) magnetic fields and show that there is no excess of EHECR arrival
directions from images of Virgo A/VC at different EHECR rigidities. By
means of event-by-event analysis we recover the extragalactic arrival
directions of EHECR events detected by Auger and TA for representative set
of nuclei H(p), He, N, Si, Fe, and find evidences of enhanced fluxes of
N-Si-Fe EHECRs from the Local Filament and Hot/Cold Spot regions. The
Local Filament with its enhanced magnetic field is an expected contributor
to the UHECR flux as the closest to the Earth last scattering centre,
whereas Hot/Cold Spot region is a part of a larger arc-like spot, possibly
created by diffusively spreading jet of UHECRs, accelerated in the
relativistic jet of Virgo A during a prominent nuclear outburst about 10
- 12 Myr ago.
|
2018-12-14 |
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prof. KRZYSZTOF BELCZYŃSKI |
CAMK, Warszawa |
ZN OA 1501 |
Gravitational-wave Astrophysics: BH-BH/NS-NS mergers with LIGO/Virgo
I will discuss the astrophysical importance of the recent LIGO/Virgo
direct detections of gravitational-waves. Despite the fact that massive
BH-BH dominance in gravitational-wave signal was predicted prior the
detections, it is not at all clear which one of the several formation
scenarios produces these massive mergers. This inhibits astrophysical
information inference from LIGO/Virgo observations, as conclusions are
different within each formation scenario. There is quite an opposite
problem with the recent detection of NS-NS merger in an old elliptical
host galaxy. None of the formation channels that can reproduce basic
properties of the detected BH-BH mergers, can recover the NS-NS merger
rate estimated by LIGO/Virgo. Despite the fact that the exact origin of
LIGO/Virgo sources is not yet known, several astrophysical implications
are beginning to emerge.
|
2018-12-21 |
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dr BARTOSZ GAUZA |
Department of Astronomy, University of Chile, Santiago, Chile |
ZN OA 1502 |
Searching for super-Jupiters around the nearest stars using ground based mid-infrared imaging
High contrast direct imaging surveys carried out in the optical and
near-infrared range have proven to be effective in finding brown dwarfs
and massive planets around stars at young ages (<500 Myr). Stars in the
solar vicinity though, are typically old, at ages over 1 Gyr, so that any
of their substellar companions had cooled down to temperatures below 1000 K.
At such temperatures the maximum flux emission shifts from near- to
mid-infrared, favoring their detection in this wavelength regime. I will
talk about the search for ultracool substellar companions to the nearest
northern stars (within 5 pc) using the mid-IR instrument CanariCam of the
10.4-m GTC telescope.
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2018-12-28 |
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przerwa świąteczna / Holiday break |
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styczeń/january 2019 |
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2019-01-04 |
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przerwa świąteczna / Holiday break |
2019-01-11 |
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dr ARTEM BOHDAN |
Deutsches Elektronen-Synchrotron, Zeuthen, Germany |
ZN OA 1503 |
Production of non-thermal electrons at nonrelativistic perpendicular shocks of young supernova remnants
The injection problem is a key and still unresolved issue of diffusive
shock acceleration theory. Electron injection mechanisms at high
Mach-number nonrelativistic perpendicular shocks are under consideration
here for parameters that are applicable to young SNR shocks. Using
high-resolution large-scale two-dimensional fully kinetic particle-in-cell
(PIC) simulations we explore the production of high-energy electrons in
the shock transition. Tracing individual particles we in detail analyze
the physics of the formation of non-thermal electron population. Ion
reflection off the shock leads to the formation of magnetic filaments in
the shock ramp, resulting from Weibel-type instabilities, and
electrostatic Buneman modes in the shock foot. Electrons are accelerated
via shock surfing acceleration (SSA) in the Buneman-instability region and
undergo further scattering in the Weibel-instability region via a
second-order Fermi-like process. The combination of these two processes
leads to the formation of a non-thermal electron population, but their
individual impact strongly depends on the Alfvenic Mach number and reduced
ion-to-electron mass ratio. We discuss the resulting electron spectra and
the relevance of our results to the physics of systems with real
ion-to-electron mass ratio and fully three-dimensional systems.
|
2019-01-18 |
|
dr hab. ŁUKASZ STAWARZ |
OA UJ |
ZN OA 1504 |
How to measure the masses (and spins) of astrophysical black holes
Astrophysical black holes span the range of mass from several up to tens
of billions solar masses. Stellar-mass black holes, believed to emerge
predominantly as the end-product of the evolution of massive stars, when
in a binary system with a main-sequence star, manifest most spectacularly
in the X-ray domain through the emission of their accretion disks; such
systems are called `X-ray Binaries'. Supermassive black holes (masses
exceeding million solar masses), on the other hand, believed to form via
accretion and black hole mergers in the centers of every massive galaxy,
can be accessed observationally in a broad range of frequencies, from
radio to γ-rays, due to the emission of their accretion disks and
relativistic outflows (jets) launched from the closest vicinities of the
black hole event horizons. Such accreting supermassive black holes are the
central engines of various types of active galaxies, including quasars,
blazars, Seyferts, and radio galaxies. They insert a direct gravitational
influence on the surrounding nearby stars and gas, and also shape the
evolution of the entire galaxies via interactions between the evolving
interstellar medium and nuclear outflows in a complex feedback loop. In
this talk I will review the methods used to measure the masses and spins
of astrophysical black holes, and comment on the prospects for imaging of
the nearest supermasive black holes at radio frequencies.
|
2019-01-25 |
|
prof. dr hab. EWA RONDIO |
Narodowe Centrum Badań Jądrowych, Świerk |
ZN OA 1505 |
Hyper-Kamiokande - the third generation detector to reveal the secrets of neutrino
Construction of the third generation gigantic water Cherenkov detector is
starting in Japan. Plans for
measurements of oscillation parameters, including CP violation phase,
neutrinos from the Sun and Supernove,
search for Dark Matter as well as proton decay searches will be presented.
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luty/february 2019 |
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2019-02-01 |
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Sesja / Exam break |
2019-02-08 |
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Sesja / Exam break |
2019-02-15 |
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Przerwa semestralna / Semester break |
2019-02-22 |
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marzec/march 2019 |
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2019-03-01 |
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dr MIGUEL FIGUEIRA |
Narodowe Centrum Badan Jadrowych, Warszawa |
ZN OA 1506 |
Star Formation: From Herschel HOBYS to ALMA
Feedback from high-mass stars such as
stellar winds, radiation pressure, photoionization pressure and supernovae
explosions can strongly modify the parental cloud in which they are born.
As a result, the next generation of stars in the same cloud is affected
and can present different physical properties. Just after their formation,
the ionizing photons from high-mass stars create an HII region whose
expansion compresses the neutral material and form a layer of dust and gas
where star formation is seen. Statistical studies showed an overdensity of
massive young objects towards these regions compared to places where no
feedback is at play. I will show the results of some of these regions
(RCW120, RCW79, NGC6334) observed in the Herschel Observations of OB Young
Stars (HOBYS) project and the follow-up studies made on the massive
objects founds towards the edge of these regions using ALMA. These
follow-up studies allow us to observe directly if the massive cores found
towards HII regions are a good place for the formation of massive
stars.
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2019-03-08 |
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prof. dr hab. MAREK BIESIADA |
Uniwersytet Śląski w Katowicach, Katowice |
ZN OA 1507 |
Gravitational lenses as a tool in cosmology
Gravitational lensing has evolved into
a mature research field with its own formalism and increasing stream of
data. I will briefly introduce the subject of strong lensing focusing on
its applications in cosmology. Then I will review the idea, which I've
been developing with my colleagues over last decade, that strong lensing
systems can be used as probes of dark energy models and non-standard
physics.
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2019-03-15 |
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dr hab. MAŁGORZATA BOGDAN |
Uniwersytet Wrocławski, Wrocław |
ZN OA 1508 |
Statistical learning under sparsity
We will discuss statistical issues behind analyses of large data sets. We
will explain an issue of overfitting and present several modern
statistical methods for dimensionality reduction in supervised and
unsupervised learning. Some of these methods were developed by our team in
collaboration with statisticians from Stanford University and Ecole
Polytechnique.
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2019-03-22 |
|
dr hab. KRZYSZTOF CHYŻY
dr hab. MAREK JAMROZY
dr BŁAŻEJ NIKIEL-WROCZYŃSKI |
Obserwatorium Astronomiczne UJ, Kraków |
ZN OA 1509 |
New results from LOFAR surveys
In this talk we will summarize the new results from the Low-Frequency
Array (LOFAR) surveys. After a short description of the LOFAR large radio
telescope network and the LOFAR surveys, we will briefly describe the
methods of identification of 231,716 radio sources located in the 424
square degrees HETDEX Spring Field. Then we will focus on a specific type
of radio galaxies, namely double-double radio galaxies, which have been
found in this area as many as 33 objects. Next we will discuss the study
of a sample of galaxy groups done with the LoTSS DR1 data. The new results
suggest that a significant number of galaxy groups might host radio
emission - including genuine, intergalactic structures. A fidelity
comparison between the existing, supra-GHz survey data and new low
frequency results from LoTSS will also be presented.
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2019-03-29 |
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dr PAWEŁ BIELEWICZ |
Narodowe Centrum Badań Jądrowych, Warszawa |
ZN OA 1510 |
Studies of statistical isotropy of the cosmic microwave background
Studies of the cosmic microwave background (CMB) are today one of the most
important pillars of observational cosmology. They provide information not
only on the initial conditions of the Universe but also on scales
comparable to the horizon of the observable Universe. This gives a unique
opportunity to pose important questions about very fundamental assumptions
made in the standard cosmological model such as statistical isotropy and
Gaussianity of the initial fluctuations. This also allows to test
deviations from the statistical isotropy predicted in models of the
Universe with multi-connected topology and deviations generated by
gravitational lensing of the CMB, predicted in the standard cosmological
model. Considerable effort spent on analyzing the statistical properties
of the CMB maps has resulted in several reports of a breaking of
statistical isotropy at large angular scales and detection of the
gravitational lensing effect. I will review these studies paying special
attention to the results obtained recently for the state-of-the-art data
from the Planck satellite.
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kwiecień/april 2019 |
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2019-04-05 |
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prof. AGNIESZKA JANIUK |
Centrum Fizyki Teoretycznej PAN, Warszawa |
ZN OA 1511 |
Simulations of short GRB central engines and their jets launching
Short gamma-ray bursts (GRBs) are presumably results of binary neutron
star mergers, which lead to the formation of a stellar mass black hole,
surrounded by remnant matter. The strong magnetic fields help collimate
jets of plasma, launched along the axis of the black hole rotation. We
study the structure and evolution of the accreting plasma in the short
GRBs and we model the formation of the base of relativistic,
Poynting-dominated jets, via the general relativistic MHD simulations.
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2019-04-12 |
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dr ANNA BARNACKA |
Department of Astronomy, Harvard University, USA
Obserwatorium Astronomiczne UJ, Kraków |
ZN OA 1512 |
Gravitational Lenses as High-Resolution Telescopes
The inner regions of active galaxies host the most extreme and energetic
phenomena in the universe including, relativistic jets, supermassive black hole
binaries, and recoiling supermassive black holes. However, many of these
sources can not be resolved with direct observations. I will present how strong
gravitational lensing can be used to elucidate the structures of these sources
from radio frequencies up to very high energy gamma rays.
Future surveys, including LSST, SKA, and Euclid, will provide observations for
hundreds of thousands of gravitationally lensed objects, which will allow us to
apply strong gravitational lensing to study the multi-wavelength structure for
large ensembles of sources. This large ensemble of gravitationally lensed
active galaxies will allow us to elucidate the physical origins of
multi-wavelength emissions, their connections to supermassive black holes, and
their cosmic evolution.
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2019-04-19 |
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Wielki Piątek / Holiday break |
2019-04-26 |
|
prof. SALVATORE CAPOZZIELLO |
University of Naples, Italy |
ZN OA 1513 |
Cosmographic reconstruction to discriminate between modified gravity and dark energy
Cosmography is a model independent approach, useful to
discriminate among concurring cosmological scenarios. After reviewing the
main features and shortcomings of LCDM model, we propose a cosmographic
approach, based on some polynomial series like Pade', Chebyschev, etc. to
investigate dark energy and modified gravity. The main result is that
series convergence seems a powerful tool to extend the matching with the
Hubble flow up to high redshift.
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maj/may 2019 |
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2019-05-03 |
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Święto 3. Maja / Holiday break |
2019-05-10 |
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dr MACIEJ BILICKI |
Centrum Fizyki Teoretycznej PAN, Warszawa |
ZN OA 1514 |
The large-scale structure of the Universe with machine learning
Astronomy has become big data science, with observational samples
now containing millions and soon billions of objects. I will present
how me and my collaborators take advantage of machine learning - a
branch of general artificial intelligence - to deal with today's
astronomical terabyte data volumes, especially in the context of the
large-scale structure of the Universe. For this we mostly use
supervised learning for regression (estimation of galaxy redshifts)
and for classification (identification of galaxies and quasars),
applied to the largest photometric datasets. In our studies these data
originate for instance from the Wide-field Infrared Survey Explorer
(WISE) observing the entire sky at mid-infrared wavelengths, and the
optical Kilo-Degree Survey performed with the VLT Survey Telescope. I
will also mention other machine-learning astronomical applications to
which I contributed, such as automated novelty detection or deep
learning studies in search for strong gravitational lenses.
|
godzina 10:00 / at 10:00 a.m. |
Publiczna obrona rozprawy doktorskiej / Public defence of doctoral thesis |
2019-05-17 |
|
mgr URSZULA PAJDOSZ-ŚMIERCIAK |
OA UJ |
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|
godzina 11:30 / at 11:30 a.m. |
Publiczna obrona rozprawy doktorskiej / Public defence of doctoral thesis |
2019-05-17 |
|
mgr WOJCIECH JURUSIK |
OA UJ |
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godzina 13:00 / at 1:00 p.m. |
2019-05-17 |
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prof. RYSZARD WIELEBINSKI |
Max Planck Institute for Radio Astronomy, Bonn, Germany |
ZN OA 1515 |
Low frequency astronomy Cosmic magnetic fields
Radio astronomy started at low radio frequencies. The intense radio waves from the Milky Way were soon
attributed to relativistic electrons emitting in magnetic fields. The angular resolution of antennas at
low radio frequencies was low indeed. Hence the move to higher frequencies followed. Also the detection
of the HI emission at 21cm wavelength, followed by detection of other molecular lines at even higher
frequencies moved the development of radio telescopes to cm, later mm and even to sub-mm wavelength. The
implementation of the homology principle (as first done in Effelsberg) led to the development of large
single dishes for high frequencies. The detection of radio polarization also allowed the study of magnetic
fields at higher frequencies.
The advent of computers led to a return to low frequency astronomy. The development of interferometry was
crucially coupled with the increase of digital computing power. Very Long Baseline (VLBI) astronomy became
possible at radio wavelength surpassing optical astronomy in angular resolution capabilities. The placing
of individual elements of large interferometer systems (like LOFAR) gave radio astronomers new observing
capabilities.
I have witnessed all these developments in my professional life. My first observations in Tasmania were at
2 MHz. In Cambridge I was lucky: I detected the first polarization of Galactic radio waves. I was
fortunate to become involved in the instrumentation of the Effelsberg radio telescope. The Max-Planck-Institute
für Radioastronomie in Bonn was later involved in mm wavelength project: IRAM, HHT, APEX, ALMA and SOFIA.
I was also involved in the low frequency developments, more as a retired onlooker: LOFAR and SKA. The
latest result, the detection of a black hole in the galaxy M87 is a consequence of all the previous developments.
|
2019-05-24 |
|
prof. XAVIER HERNANDEZ |
UNAM University, National University of Mexico, Mexico City, Mexico |
ZN OA 1516 |
Challenging a Newtonian prediction through Gaia wide binaries
Under Newtonian dynamics, the relative motion of the components of a binary star
should follow
a Keplerian scaling with separation. Once orientation effects and a distribution of
ellipticities
are accounted for, dynamical evolution can be modelled to include the effects of
Galactic tides
and stellar mass perturbers. This furnishes a
prediction for the relative velocity between the components of a binary and their
projected
separation. After reviewing recent work evidencing the existence of a critical
acceleration scale
in Elliptical Galaxies and Globular Clusters, I will show results showing such a
phenomenology in
Gaia wide binaries using the latest and most accurate astrometry available. The
results are
consistent with the Newtonian prediction for projected separations below 7000 AU,
but inconsistent
with it at larger separations, where accelerations are expected to be lower than the
critical
a0 value of MONDian gravity. This result challenges Newtonian gravity at low
accelerations and
shows clearly the appearance of gravitational anomalies of the type usually
attributed to dark
matter at galactic scales, now at much smaller stellar scales.
|
Odwołane / Cancelled |
2019-05-31 |
|
mgr ROMANA GROSSOVA |
Masaryk University, Brno, Czech Republic |
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czerwiec/june 2019 |
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2019-06-07 |
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dr hab. ŁUKASZ WYRZYKOWSKI |
Obserwatorium Astronomiczne Uniwersytetu Warszawskiego, Warszawa |
ZN OA 1517 |
Missing black holes and the dark matter puzzle
There should be millions of black holes in the Milky Way produced by the
regular evolution of massive stars. Moreover, Gravitational Wave
detections discovered massive black holes which could have been produced
by stars or potentially could partially originated from primordial black
holes and could explain part of the dark matter. I will present our hunt
for single galactic black holes using long term photometric observations
from OGLE and ground based followup observations of Gaia microlensing
events. In next couple of years Gaia epoch astrometry will solve the
degeneracies in microlensing events and will yield a discovery of nearby
black holes.
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2019-06-14 |
|
mgr AGNIESZKA MIROCHA |
Obserwatorium Astronomiczne UJ, Kraków |
ZN OA 1518 |
Tracing low-mass protostars' properties with IRAM 30m submillimeter telescope
Protostars are surrounded by dense, collapsing envelopes at the earliest
stages of star formation. Observations at long-wavelengths are required to
study deep embedded low-mass YSOs due to high dust extinction in the
optical range. There are many rotational lines of key molecules at
submillimeter range which are needed to characterize gas temperatures,
densities, the UV radiation. Especially, the molecular outflows are
strongly connected with the physical and chemical processes around
protostars. Here, we present maps in HCN, CN, CS and their isotopologues
obtained with IRAM 30m submillimeter telescope. In this analysis, we
concentrate on the Serpens Main star forming region, which contains
several of YSOs with strong molecular outflows. Targeted lines trace
molecular outflows as well as YSOs' closest neighbourhood. Based on
information from the molecular data, we are able to characterize the
population of low-mass protostars. Additionally, spectral energy
distribution (SED) fitting was applied in order to determine bolometric
luminosities, temperatures and evolutionary stages of the studied YSOs.
This way, we gain new insights into physical and chemical properties of
low-mass protostars in the Serpens Main region.
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2019-06-21 |
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piątek po Święcie Bożego Ciała / Holiday break |
2019-06-28 |
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wakacje / Holiday break |
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lipiec/july 2019 |
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sierpień/august 2019 |
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wrzesień/september 2019 |
|
Publiczna obrona rozprawy doktorskiej / Public defence of doctoral thesis |
2019-09-10 |
|
mgr DOMINIKA HUNIK-KOSTYRA |
OA UJ |
|
On the cubic conformal flow on S3 and other fully resonant systems |
2019-09-10 |
|
prof. ANDRZEJ ZDZIARSKI |
CAMK |
ZN OA 1519 |
The nature of the puzzling source Cyg X-3 |