Podcasts about rosat

STERNENGESCHICHTEN LIVE TOUR 2025! Tickets unter https://sternengeschichten.live Als man Geminga entdeckt hat, wusste man zwar, dass da was ist, aber nicht wo genau und um was es sich handelt. Heute wissen wir mehr, aber Geminga ist immer noch ein Himmelskörper voller Rätsel. Mehr erfahrt ihr in der neuen Folge der Sternengeschichten. Wer den Podcast finanziell unterstützen möchte, kann das hier tun: Mit PayPal (https://www.paypal.me/florianfreistetter), Patreon (https://www.patreon.com/sternengeschichten) oder Steady (https://steadyhq.com/sternengeschichten)

(00:00) Start och snack om kommande jubileum och lottovinst på 1,3 miljarder kronor (07:03) Remnant II, en kommersiell och kritikerrosad succé - och full med hemligheter (14:50) Baldur´s Gate 3 släppt med buller och bång (24:14) Linux har gått om macOS som den näst största plattformen på Steam (25:54) Star Wars Jedi Survivor till PS4/Xbox One trots tekniska problem på PS5 och Xbox Series S/X (28:33) Xbox avslöjar vad man kommer att se och testa på Gamescom 2023 i Köln (36:53) Switch 2-rykten säger att det blir en större skärm, mer lagringsutrymme och lansering oktober 2024 (42:47) Nintendo Switch är såld I 129 miljoner exemplar, Zelda Tears of the Kingdom I 18,5 miljoner exemplar (51:33) Ny kommande uppdatering till PS5 möjliggör att man kan stänga det enerverande uppstartsljudet (58:01) En spelare har klarat Elden Ring genom att spela på en digital saxofon (1:06:24) Battlefield kan komma att rebootas (1:12:30) Ratatan, spirituell uppföljare till Patapon fick igenom finansiering på Kickstarter (1:16:14) Xbox börjar sälja reservdelar till handkontroller på sin servicesida (1:18:14) Veckans spelsläpp: Wrestle Quest, Legend Bowl, Stray till Xbox, Atlas Fallen Musik: Baldur's Gate 3 Original Soundtrack - Down By The River Vi som gör podcasten om tv-spel, videospel, datorspel och allt som har med Xbox, PlayStation, Nintendo och PC att göra heter Andreas och Henrik. Mer information finns att läsa på vår hemsida ⁠⁠https://www.gejmapod.se⁠⁠ och följ oss gärna på Twitter ⁠⁠https://twitter.com/GejmaPod⁠⁠. Gå med i vår Discord: ⁠https://discord.gg/CSN7jHrUCg⁠

The Origin and Distance of the High-Velocity Cloud MI by J. T. Schmelz et al. on Wednesday 21 September The high-velocity, neutral hydrogen feature known as MI may be the result of a supernova that took place about 100,000 years ago at a distance of 163 pc. Low-velocity HI data show a clear cavity, a structure indicative of regions evacuated by old exploding stars, centered on the spatial coordinates of MI, (l,b) = (165o, 65.o5). The invisible companion of the yellow giant star, 56 Ursae Majoris, may be the remains of the supernova that evacuated the cavity and blasted MI itself outward at 120 km/s. The mass and energy of MI are easily in line with what is expected from a supernova. The X-rays seen by ROSAT are consistent with an origin in the resulting bow shock. Ironically, this scenario for MI only came together because we were exploring low-velocity gas in the direction of high-velocity clouds. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2207.08707v2

The Origin and Distance of the High-Velocity Cloud MI by J. T. Schmelz et al. on Wednesday 21 September The high-velocity, neutral hydrogen feature known as MI may be the result of a supernova that took place about 100,000 years ago at a distance of 163 pc. Low-velocity HI data show a clear cavity, a structure indicative of regions evacuated by old exploding stars, centered on the spatial coordinates of MI, (l,b) = (165o, 65.o5). The invisible companion of the yellow giant star, 56 Ursae Majoris, may be the remains of the supernova that evacuated the cavity and blasted MI itself outward at 120 km/s. The mass and energy of MI are easily in line with what is expected from a supernova. The X-rays seen by ROSAT are consistent with an origin in the resulting bow shock. Ironically, this scenario for MI only came together because we were exploring low-velocity gas in the direction of high-velocity clouds. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2207.08707v2

When it comes to the Comet Elenin controversy—I fear that I may end up in the same corner as all those who have said that the comet is actually a doomsday comet that will hit the earth. I have never said it will hit the earth but I most certainly know that all comets, asteroids and other celestial bodies that pass near the earth can cause all sorts of chaos. The whole idea of comets being harbingers of doom dates back to biblical times and the legends of bearded stars, dragons and flying boars of Celtic lore.I see Elenin as an opportunity for a counter intelligence cover for other activity going on in space as there have been several things to pay attention to lately. Comet Honda hasn't captured the imaginations of the fringe crowd, there wasn't too much fanfare for the UARS or ROSAT satellite fall and neither has 2005 YU55 an asteroid that will passing near the earth sometime in November.Originally Broadcast On 09/30/2011

In unserer aktuellen Folge sprechen wir mit Johanna Dumet über die Installation "Modeleur ombre et lumière Chanel" (1996) von Sylvie Fleury - eine Wandmalerei in vier pudrigen Rosatönen. Außerdem geht es um klassische Sonntage in Frankreich und Johannas Erfolg der letzten Jahre.

Josh and Leah had a pretty big hangovers, If you don't drink cava everyday what are you drinking? OUR FIRST CONTEST! Listen to the episode to decipher what you have to do. Thanks Wanner Construction! Find us on all social medias and the YOUTUBES

Aquest és el primer conte de la tercera temporada: "Fantasies de Nadal". És conte inventat d'en Roger Giménez pels seus fills i tots els nens que vulguin escoltar. Es tracta d'un misterios nas que tenia fred i calor... Música: Happy Ukulele - Jason Shaw - Creative Commons

Heute vor 30 Jahren startete in Cape Canaveral der in Deutschland entwickelte Röntgensatellit ROAT. Mit ihm wurde ein neues Fenster zum Weltall geöffnet – ein Fenster, das den Blick auf besonders energiereiche Prozesse im Universum freigab. Von Hermann-Michael Hahn www.deutschlandfunk.de, Sternzeit Hören bis: 19.01.2038 04:14 Direkter Link zur Audiodatei

Today I am being joined on the podcast by the Otoski’s, Cindy and Rob.  Rob and Cindy are both long time visitors to the island and friends of the show.  While on the island they split time between the Renaissance and the Marriott, giving them a multifaceted view of the Aruba vacation experience.  Together they are part of the group that founded and runs the Renaissance Oceans Suites Aruba Timeshares Facebook or ROSAT for short.   Rob and Cindy were actually supposed to be on the island at the time of recording but because the world is all sorts of upside down now instead Rob posted a hypothetical “What If..” style trip report, photos, and all.     Some of the places mentioned in this episode of the podcast are:   Renaissance Ocean Suites Marriott Surf Club Bully Taxi Superfoods Montefort Ship Jolly Pirates Pinchos Zeerover LG Smith Coco Loco Pinchos Yemanja Papygayo Maroc

Large X-ray surveys are a powerful tool to study the large-scale structure (LSS) of the Universe. The scientific impact of LSS studies using active galactic nuclei (AGN) in X-ray surveys can be significantly increased by conducting wider and deeper X-ray surveys and studying the surface brightness fluctuations of the unresolved cosmic X-ray background (CXB). In the first part of this Thesis, we have investigated the prospects of using the AGN sample to be detected by the upcoming eROSITA all-sky survey (eRASS) for LSS studies. We show that eRASS will detect about 3 million AGN in the 0.5-2.0 keV band. This will result in a ~30 times larger number of sources and a ~30 times better sensitivity than its 25 year old predecessor, the ROSAT all-sky survey (RASS). We show that this unprecedented AGN sample will have a median luminosity of ~10^44 erg/s, which is typical for the entire AGN population in this energy band. It will have a median redshift of z ~ 1 and approximately 40% of the objects will be in the redshift range of z = 1-2, where the bulk of the X-ray emission of AGN is produced. About 10^4 - 10^5 AGN are predicted to be beyond redshift z = 3 and about 2 000 - 30 000 beyond z = 4, which will potentially include some of the earliest AGN in the Universe. We demonstrate that, given these unique properties, the eRASS-AGN sample will be able to significantly improve our current knowledge of the AGN spatial density as a function of redshift and luminosity over a wide range of cosmic time. Further, we show that it will enable us, for the first time, to perform detailed redshift- and luminosity-resolved studies of the clustering strength of X-ray selected AGN. All these measurements will dramatically improve our understanding of the growth of supermassive black holes over cosmic time and its implications for galaxy evolution. We demonstrate for the first time that, given the breadth and depth of eRASS, it will be possible to use AGN as a cosmological probe via baryon acoustic oscillation (BAO) measurements. We will be able to convincingly detect BAOs in the currently uncharted redshift range of z ~ 1-2, which will improve the constraints on the current cosmological model. In the second part of this Thesis, we have conducted the most accurate measurement to date of the brightness fluctuations of the unresolved CXB in the 0.5-2.0 keV band for angular scales of < ~17'. For this we used the XBOOTES survey, the currently largest continuous survey of the X-ray telescope Chandra. We find that on small angular scales (< ~2') the observed power spectrum of the brightness fluctuations is broadly consistent with the conventional AGN clustering model, although with a 30% deviation. This deviation nevertheless presents a good opportunity to improve our understanding of clustering properties of unresolved AGN by testing more sophisticated clustering models with our measurement. For angular scales of > ~2' we measure a significant excess with up to an order of magnitude difference in comparison to the standard AGN clustering model. We demonstrate that an instrumental origin can be excluded. However, we also show that the excess can neither be explained with any known X-ray source population by looking at strength of its clustering signal and the shape of its energy spectrum. It might be caused by more than one type of source but the dominant source appears to have extragalactic origin. Finally, we make predictions on how eRASS will be able to advance the studies of the unresolved CXB.

On this news-packed episode of Talking Space, we discuss the space shuttle Endeavour officially being handed over to the California Science Center, and also discuss the controversey of trying to bring a shuttle to Houston as well as Ohio. This segment includes a classic clip from a STS-134 briefing with a question asked by our own Gene Mikulka. We then discuss former Space Shuttle Launch Integration Manager Mike Moses, who will be leaving NASA to join Virgin Galactic. We also discuss the second drop test of Space Ship 2, which did not go as smooth as expected. We then get into a deep discussion of the next proposed NASA budget and some intersting areas which are being affected by the budget and others that aren't. We then talk about a possible 2013 abort test of the Orion capsule as well as a 2012 drop test of Sierra Nevada's Dreamchaser. We then continue with another satellite coming in for a reentry similar to UARS, except this time it's ROSAT. We finish off our discussions with the Soyuz getting NASA's ok to keep flying as well as a launch this week, for the first time, of a Soyuz from somewhere other than the Baikonour Cosmodrome. We finish off with an interview conducted by Mark with another amazing speaker from the 100 Year Star Ship Symposium, Chantelle Louis. For more information on the upcoming Soyuz launch from French Guyana, check outhttp://threelaunchersontheequator.com For more information on Chantelle Louis and to see her work, visit her website athttp://chantellelouis.com Host this week: Sawyer Rosenstein. Panel Members: Gina Herlihy, Gene Mikulka and Mark Ratterman Show Recorded - 10/17/2011

Für den in der letzten Raumzeit-Ausgabe ausführlich behandelten Satellit ROSAT steht in den kommenden Wochen der Wiedereintritt in die Erdatmosphäre bevor. Der nicht mehr steuerbare Satellit wird zum allergrößten Teil verglühen, es muss aber damit gerechnet werden, dass bis zu 30 einzelne Trümmerteile die Erdoberfläche erreichen könnten. Rund um den Wiedereintritt gibt es viele Fragen, die wir in dieser Ausgabe behandeln möchten. Nach aktuellen Berechnungen steht der Wiedereintritt des ROSAT-Satelliten in die Erdatmosphäre für Ende Oktober 2011 an.

Die Röntgenastronomie hat in den 70er Jahren vollkommen neue Einblicke ins All ermöglicht und trug in erheblichem Maße zum heutigen Basiswissen über unser Universum bei. Die ROSAT-Mission - unter Federführung des Max-Planck-Instituts für extraterrestrische Physik und in Kooperation mit der NASA und dem DLR - ermöglichte Anfang der 90er Jahre einen Durchbruch in der umfangreichen Kartografie des Universums und in der Erforschung von Röntgenquellen im All überhaupt.

In this work a new method for the detection of faint, both point-like and extended, astronomical objects based on the integrated treatment of source and background signals is described. This technique is applied to public data obtained by imaging methods of high-energy observational astronomy in the X-ray spectral regime. These data are usually employed to address current astrophysical problems, e.g. in the fields of stellar and galaxy evolution and the large-scale structure of the universe. The typical problems encountered during the analysis of these data are: spatially varying cosmic background, large variety of source morphologies and intensities, data incompleteness, steep gradients in the data, and few photon counts per pixel. These problems are addressed with the developed technique. Previous methods extensively employed for the analysis of these data are, e.g., the sliding window and the wavelet based techniques. Both methods are known to suffer from: describing large variations in the background, detection of faint and extended sources and sources with complex morphologies. Large systematic errors in object photometry and loss of faint sources may occur with these techniques. The developed algorithm is based on Bayesian probability theory, which is a consistent probabilistic tool to solve an inverse problem for a given state of information. The information is given by a parameterized model for the background and prior information about source intensity distributions quantified by probability distributions. For the background estimation, the image data are not censored. The background rate is described by a two-dimensional thin-plate spline function. The background model is given by the product of the background rate and the exposure time which accounts for the variations of the integration time. Therefore, the background as well as effects like vignetting, variations of detector quantum efficiency and strong gradients in the exposure time are being handled properly which results in improved detections with respect to previous methods. Source probabilities are provided for individual pixels as well as for correlations of neighboring pixels in a multi-resolution analysis. Consequently, the technique is able of detecting point-like and extended sources and their complex morphologies. Furthermore, images of different spectral bands can be combined probabilistically to further increase the resolution in crowded regions. The developed method characterizes all detected sources in terms of position, number of source counts, and shape including uncertainties. The comparison with previous techniques shows that the developed method allows for an improved determination of background and source parameters. The method is applied to data obtained by the ROSAT and Chandra X-ray observatories whereas particularly the detection of faint and extended sources is improved with respect to previous analyses. This lead to the discovery of new galaxy clusters and quasars in the X-ray band which are confirmed in the optical regime using additional observational data. The new technique developed in this work is particularly suited to the identification of objects featuring extended emission like clusters of galaxies.

This composite image of the galaxy cluster Abell 3376 shows X-ray data from the Chandra X-ray Observatory and the ROSAT telescope along with an optical image from the Digitized Sky Survey and radio emission observed by the Very Large Array.

This dissertation presents the analysis of a large and deep XMM-Newton survey of the second large Local Group spiral galaxy M 31. The survey observations, taken between June 2006 and February 2008, together with re-analysed archival observations from June 2000 to July 2004 cover, for the first time, the whole D25 ellipse of M 31 with XMM-Newton down to a limiting luminosity of ~10^35 erg/s in the 0.2-4.5 keV band. The main goal of the thesis was a study of the different source populations of M 31 that can be observed in X-rays. Therefore a catalogue was created, which contains all 1948 sources detected in the 0.2-12.0 keV range. 961 of these sources were detected in X-rays for the first time. Source classification and identification was based on X-ray hardness ratios, spatial extent of the sources, and by cross correlating with catalogues in the X-ray, optical, infrared and radio wavelengths. An additional classification criterion was the long-term temporal variability of the sources in X-rays. This variability allows us to distinguish between X-ray binaries and active galactic nuclei. Furthermore, supernova remnant classifications of previous studies that did not use long-term variability as a classification criterion, could be validated. Including previous Chandra and ROSAT observations in the long-term variability study allowed me to detect additional transient or at least highly variable sources, which are good candidates for being X-ray binaries. Fourteen of the 40 supersoft source (SSS) candidates correlated with optical novae and therefore can be considered the supersoft emission of the optical novae. Among them is the first nova/SSS detected in a globular cluster of M 31. Correlations with previous ROSAT and Chandra studies revealed that only three SSSs are visible for at least one decade. This result underlines the strong long-term variability found for the class of SSSs. In addition the correlations demonstrated that strict selection criteria have to be applied to securely select SSSs. An investigation of the spatial distribution of the 25 supernova remnants (SNRs) and 37 SNR candidates showed that many of these sources are consistent with the location of the 10 kpc dust ring and other star forming regions in M 31. This connection between SNRs and star forming regions implies that most of the remnants are from type II supernovae. The brightest sources of M 31 belong to the class of X-ray binaries (XRBs). Ten low mass XRBs (LMXBs) and 26 LMXB candidates were identified based on their temporal variability. In addition 36 LMXBs and 17 LMXB candidates were identified due to correlations with globular clusters and globular cluster candidates. From the LMXBs located in globular clusters one is a black hole candidate and another a neutron star candidate. From optical and X-ray colour-colour diagrams, possible high mass XRB (HMXB) candidates were selected. Two of these candidates have an X-ray spectrum as is expected for an HMXB containing a neutron star primary. To investigate the logN-logS relations of sources in the field of M 31, a catalogue of sources detected in the 2.0-10.0 keV energy range was created. The slope of the logN-logS relation for the whole galaxy is consistent with the expectation for spiral galaxies (Colbert et al. 2004). Subtracting the background logN-logS relation, the region beyond the D25 ellipse still contains about 13 sources/deg^2 of M 31 with fluxes above the completeness limit of ~3.2x10^{-14} erg/cm^2/s (~2.3x10^36 erg/s at the distance of M 31). The radial dependence of the source distribution in M 31's disc can be well fitted with an exponential profile, for limiting fluxes of ~3.2x10^{-14} erg/cm^2/s and 10^{-13} erg/cm^2/s (~7.3x10^36 erg/s). About 60% of all sources with fluxes above 3.2x10^{-14} erg/cm^2/s are background sources. While the contribution of background sources lies at ~20% in the inner disc region, the fraction increases to >~80% in the outer areas of M 31. For the dust ring region, the slope of the logN-logS relation as well as the number of sources and their dependence on the star forming rate were consistent with the universal logN-logS relation predicted from theoretical considerations of HMXBs (Grimm et al. 2003). These findings propose that the dust ring region contains a population of HMXBs. A comparison of the number of X-ray binaries (XRBs) obtained from the logN-logS study to the ones listed in the source catalogue showed that many XRBs detected in the logN-logS study with fluxes between 10^{-13} erg/cm^2/s and 3.2x10^{-14} erg/cm^2/s, or (independent from the flux) those XRBs located in the inner disc of M 31, remain without XRB classification in the source catalogue. The results presented in this thesis gave us deeper insights in the properties of the population of X-ray sources in M 31. Nevertheless, about 65% of all sources detected in the field of M 31 can be classified as ``hard" sources only, i.e. it is not possible to decide whether these sources are X-ray binaries or Crab-like supernova remnants in M 31, or active galactic nuclei. Deeper observations in the X-ray and at other wavelengths are needed to classify these sources.

In this thesis we address the subject of the unification of radio-loud Active Galactic Nuclei (AGN) (FRI/FRII galaxies, BL Lac objects and quasars) with a statistical and multiwavelength approach, paying particular attention to the X-ray band which carries precious information on the innermost regions of AGN. A large sample of 2260 AGN of different kinds was created by cross-correlating the ROSAT catalogs with various radio surveys and, for each source, data were collected in the radio, optical and soft X-ray bands. 1682 objects are formally classified as radio-loud and are analyzed in this thesis. The main purpose of this thesis is to test the unified scheme for radio-loud AGN by investigating if the correlations between luminosities at different frequencies are consistent with the basic assumption that BL Lac objects and radio-loud quasars are relativistically beamed counterparts of FRI and FRII radio galaxies, respectively. Although this is the key hypothesis of the unification scheme for radio-loud AGN, these questions have not been carefully analyzed so far. The results of this thesis are in general agreement with the relativistic beaming scenario, however, some complications have been highlighted. Tight relationships between the nuclear emission in the three wavebands considered are confirmed for all classes and we were able to better constrain the parameters of the correlations due to the larger number of objects compared to previous investigations. However, for FRI galaxies and BL Lac objects, more than one emission component is required, at least in the X-ray band, to explain in a relativistic beaming scenario the different parameters observed for the correlations. One component can easily be associated with the jet, whereas the other remains so far unknown. A possible problematic aspect of the unified scheme is that, among the FRI galaxies, the counterparts of Low-energy-peaked BL Lacs have not been found. Absorption with N_H > 10^{22} cm^{-2} is present in FRII galaxies and plays, together with relativistic beaming, a major role in the unification with radio-loud quasars. Allowing for absorption, only one emission component is required at all frequencies to account for the observed correlations in both classes. Flat-spectrum quasars (FSRQ) appear to be more beamed than steep-spectrum quasars (SSRQ) only at radio frequencies, but not in the optical and X-ray bands. This might imply that quasars are disk-dominated in the X-ray and optical band, and jet-dominated at radio frequencies. On the other hand, FRI galaxies and BL Lacs appear to be globally jet-dominated. A parameter which might account for the FRI/BL Lac - FRII/quasar dichotomy is the accretion rate. At low, sub-Eddington values jets are weak but the emission from them dominates that from the disk and these sources are classified as FRI galaxies or BL Lacs, depending on the viewing angle. At values close to the Eddington limit the disk emission is comparable to that from the jet, which is also more powerful due to the higher accretion rate, and either a FRII galaxy or a radio-loud quasar is produced in this case.