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SpaceTime with Stuart Gary | Astronomy, Space & Science News
In this episode of SpaceTime, we uncover significant advancements in our understanding of the universe and ongoing developments in space exploration.Astronomers Find the Universe's Missing MatterA groundbreaking study reveals that the universe's elusive normal matter is concealed within hot intergalactic gas filaments. This discovery, detailed in the journal Astronomy and Astrophysics, identifies a massive filament of gas, ten times the mass of the Milky Way, connecting four galaxy clusters. Utilizing the European Space Agency's XMM-Newton and JAXA's Suzaku X-ray space telescopes, researchers have successfully characterized this filament, providing crucial insights into the cosmic web's structure and supporting existing models of the universe.Concerns Grow Over Leaks Aboard the International Space StationFresh concerns regarding leaks aboard the International Space Station have led to delays in the SpaceX Axiom Spaceflight 4 mission. NASA is closely monitoring cabin pressure in the Russian segment of the station, where ongoing structural issues have been identified. Despite recent repairs, the situation remains a top safety priority as astronauts prepare for their upcoming mission.European Space Agency's Mars Rover ProgressThe European Space Agency's ExoMars rover, Rosalind Franklin, is back on track to land on Mars in 2028, seven years later than originally planned. This mission aims to search for signs of past life on the Red Planet and investigate its geochemical environment. With new funding and NASA's agreement to provide launch services, the Rosalind Franklin rover is undergoing final tests to ensure its success on the Martian surface.www.spacetimewithstuartgary.com✍️ Episode ReferencesAstronomy and Astrophysicshttps://www.aanda.org/European Space Agencyhttps://www.esa.int/NASAhttps://www.nasa.gov/Become a supporter of this podcast: https://www.spreaker.com/podcast/spacetime-space-astronomy--2458531/support.00:00 This is Space Time Series 28, Episode 76 for broadcast on 25 June 202501:00 Astronomers find the universe's missing matter12:15 Concerns grow over leaks aboard the International Space Station22:30 European Space Agency's Mars rover progress30:00 Science report: New insights into conversion therapy and health impacts
宇宙ばなしがベースになっている書籍「やっぱり宇宙はすごい（SB新書）」は好評発売中！おかげさまで即重版！Audibleでも！Audibleの無料体験はこちらから！著書「マーケティングをAIで超効率化！ChatGPT APIビジネス活用入門（講談社）」好評発売中！もう1つのチャンネル「となりのデータ分析屋さん」はこちら！Spotify /Apple Podcast個人ホームページはこちら！Twitter（_ryo_astro)ジングル作成：モリグチさんfromワクワクラジオソース：
Please meet Dr Anya Nugent … she is amazing … and she has some beautiful stories for us … let's hear all about unbelievably powerful Gamma Ray bursts and their host galaxies from an amazing Harvard and Smithsonian astrophysicist who uses incredible observatories like CHANDRA, XMM-Newton, ALMA, CHIME, MEERKAT, the VLA and even our old friend Hubble … to reveal new understandings of how our universe works.
The United Kingdom's robust and ambitious space sector has many personalities. Each year at the Better Satellite World Awards Dinner in December in London, the SSPI UK Chapter recognizes one of them as the Satellite Personality of the Year. In this podcast, we hear from the 2024 honoree, Dr. David Parker FRAeS, Non-Executive Board Member of the UK Space Agency and Visiting Professor at the University of Southampton. This interview was originally broadcast as part of the Personalities of the Space & Satellite Industry podcast series, which aired before Dr. Parker was named the 2024 Satellite Personality of the Year. Dr. David Parker has led a distinguished thirty-five-year career in the space sector, spanning industry, UK government and the European Space Agency (ESA). Until June 2023, he served as ESA's Director of Space Exploration at ESTEC in the Netherlands, overseeing astronaut missions to the International Space Station, Europe's involvement in Artemis and pioneering projects like training an astronaut with a physical disability. Previously, he was the Chief Executive of the UK Space Agency (2013-2016), where he led Tim Peake's ISS mission and negotiated ESA's first UK center in Harwell. Starting in the UK space industry in 1990, he contributed to projects like XMM-Newton and ExoMars. Dr. Parker holds a degree in Aeronautics and Astronautics and a PhD from NASA Langley Research Center. He has received several accolades, including the Royal Aeronautical Society's Geoffrey Pardoe award. He currently works part-time at ESA, serves on the UK Space Agency Board and is a Visiting Professor at the University of Southampton.
Mars-missioner, prøver fra Månens bagside, en rumstation, hele to store satellit-konstellationer og massevis af raketopsendelser. Det er bare nogle af de mange rumaktiviteter, Kina har gang i. I denne episode retter vi teleskopet mod Kina, fordi der sker så voldsomt mange spændende ting derovre i disse år, der også påvirker rumaktiviteterne i resten af verden. Men vi har trods alt talt med en dansk rumekspert i Kina – nemlig Thomas Schumann, der i flere år var vært på Radio4-podcasten Den Nye Rumalder, og som i dag har sin egen rumpodcast, Schumanns Rumraket. Thomas er især interesseret i Kinas Chang'e rummissioner, og det er også et af de områder hvor Kina mest direkte ligger i konkurrence med USA. Og der er næppe tvivl om at det nye store rumræs står mellem netop de to nationer. Hør meget mere om det, når vi taler med Thomas – og så er der selvfølgelig også korte rumnyheder, denne gang blandt andet om gigantiske rumobjekter, supernovaer og nye ESA-projekter. Lyt med
大阪開催の竹中工務店イベント「たてものめがね まちめがね」壇します31歳になりました！誕生日プレゼント送りたい！って方は書籍「やっぱり宇宙はすごい」を買ってください。もう持ってる方は、2冊目3冊目を買ってくれると僕がヒット作家になれるという最高の誕生日プレゼントになります。https://amzn.to/3UAeSr9ほしい物リストhttps://www.amazon.jp/hz/wishlist/ls/3D944KX18YFUU?ref_=wl_share集英社連載最新回「2026年には水星からリアル配信が見られるかも？ 計画実施まで21年かかったJAXA「みお」の水星探査」 を公開しました！Youtubeチャンネルも更新中！Instagram（ryo_astro）個人ホームページはこちら！Twitter（_ryo_astro)もう1つのチャンネル「となりのデータ分析屋さん」はこちら！Spotify /Apple Podcastお便りコーナーはこちら！ジングル作成：モリグチさんfromワクワクラジオソースhttps://www.nasa.gov/general/exoplanets-need-to-be-prepared-for-extreme-space-weather-chandra-finds/
Planets around other stars need to be prepared for extreme weather conditions, according to a new study from NASA's Chandra X-ray Observatory and ESA's XMM-Newton that examined the effects of X-rays on potential planets around the most common type of stars.
Europas Röntgensatellit XMM-Newton beobachtet seit 25 Jahren das heiße energiereiche Universum, zum Beispiel die Umgebung Schwarzer Löcher und das Leuchten riesiger Galaxienhaufen. Sein Namenspatron Isaac Newton wirkte an etlichen Todesurteilen mit. Lorenzen, Dirk www.deutschlandfunk.de, Sternzeit
The United Kingdom's robust and ambitious space sector has many personalities. In this podcast series, we introduce you to three whom the UK Chapter of SSPI is considering for its prestigious Personality of the Year Award in 2024. One of these three finalists will be named the 2024 Satellite Personality of the Year live at the Better Satellite World Awards Dinner in London on 2 December. Click here to join us there! Each of the three finalists is a star who has made significant contribution to the UK and global satellite industry and whose career is a study of performance and excellence at the highest level. In the first episode, we learn a bit more about Dr. David Parker FRAeS, Non-Executive Board Member of the UK Space Agency and Visiting Professor at the University of Southampton. Dr. David Parker has led a distinguished thirty-five-year career in the space sector, spanning industry, UK government and the European Space Agency (ESA). Until June 2023, he served as ESA's Director of Space Exploration at ESTEC in the Netherlands, overseeing astronaut missions to the International Space Station, Europe's involvement in Artemis and pioneering projects like training an astronaut with a physical disability. Previously, he was the Chief Executive of the UK Space Agency (2013-2016), where he led Tim Peake's ISS mission and negotiated ESA's first UK center in Harwell. Starting in the UK space industry in 1990, he contributed to projects like XMM-Newton and ExoMars. Dr. Parker holds a degree in Aeronautics and Astronautics and a PhD from NASA Langley Research Center. He has received several accolades, including the Royal Aeronautical Society's Geoffrey Pardoe award. He currently works part-time at ESA, serves on the UK Space Agency Board and is a Visiting Professor at the University of Southampton.
Un telescopio a raggi X da manuale. Venticinque anni di onorato servizio senza mai disturbare, raccogliendo una mole di dati tale da non riuscire a usarli tutti. Lui è Xmm-Newton, un telescopio spaziale di proprietà congiunta fra Esa e Nasa. Tutto perfetto, tranne un piccolo incidente durato tre giorni nel 2008, nove anni dopo il lancio. E siccome noi di Houston non perdoniamo niente, ne parliamo con Paolo Ferri in questo episodio, con una pillola sull'astronomia X di Stefano Ettori. Musiche: “Contagion”, Scott Buckley; “Sneaky Snooper”, instrumental brother
A new study using NASA's Chandra and ESA's XMM-Newton reveals that the interiors of neutron stars may contain a type of ultra-dense matter not found anywhere else in the Universe.
A study with Chandra and XMM-Newton indicates which stars near our Sun could have habitable exoplanets around them based on whether they receive lethal radiation from the stars they orbit.
La tertulia semanal en la que repasamos las últimas noticias de la actualidad científica. En el episodio de hoy:Cara B:-Argumentos contra la presencia de atmósferas en Trappist-I (00:00)-La causa autoinmune del síndrome de Guillain-Barré (en algunos pacientes) (38:12)-El agujero negro de Markarian 817 observado por XMM-Newton and NuSTAR (1:05:02)-Enormes agujeros negros (que son pequeños puntos rojos) en 4
Astronomers using NASA's Chandra, ESA's XMM-Newton, and other telescopes have determined that a giant black hole has destroyed a large star and strewn its contents into space.
Une équipe d'astrophysiciens rapporte la mesure de la polarisation des rayons X de la brillante galaxie de Seyfert NGC 4151 pour en déduire la géométrie de sa source d'émission. Elle a été observée avec le télescope spatial Imaging X-ray Polarimetry Explorer (IXPE), et complétée par des observations simultanées de XMM-Newton et NuSTAR. L'étude est publiée dans les Monthly Notices of the Royal Astronomical Society.
Astronomers have captured a spectacular, ongoing collision between at least three galaxy clusters. Data from Chandra, XMM-Newton, and a trio of radio telescopes are helping astronomers sort out what is happening in this jumbled scene.
The Rapidly Spinning Intermediate-Mass Black Hole 3XMM J150052 0+015452 by Z. Cao et al. on Wednesday 30 November A star tidally disrupted by a black hole can form an accretion disc with a super-Eddington mass accretion rate; the X-ray emission produced by the inner disc provides constraints on the black hole mass $M_bullet$ and dimensionless spin parameter $a_bullet$. Previous studies have suggested that the $M_bullet$ responsible for the tidal disruption event 3XMM J150052.0+015452 (hereafter J150052) is $sim$10$^{5} M_{odot}$, in the intermediate black hole (IMBH) regime. Fitting multi-epoch XMM-Newton and Chandra X-ray spectra obtained after 2008 during the source's decade-long decay, with our latest slim accretion disc model gives $M_bullet = 2.0^{+1.0}_{-0.3}times10^{5} M_{odot}$ (at 68% confidence) and $a_bullet > 0.97$ (a 84.1% confidence lower limit). The spectra obtained between 2008-2014 are significantly harder than those after 2014, an evolution that can be well explained by including the effects of inverse-Comptonisation by a corona on the early-time spectra. The corona is present when the source accretion rate is super-Eddington, while there is no evidence for its effect in data obtained after 2014, when the mass accretion rate is around the Eddington-limit. Based on our spectral study, we infer that the corona is optically thick and warm ($kT_e=2.3^{+2.7}_{-0.8}$ keV). Our mass and spin measurements of J150052 confirm it as an IMBH and point to a rapid, near extremal, spin. These $M_bullet$ and $a_bullet$ values rule out both vector bosons and axions of masses $sim10^{-16}$ eV. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.16936v1
Investigating the origin of optical and X-ray pulsations of the transitional millisecond pulsar PSR J1023+0038 by G. Illiano et al. on Friday 25 November PSR J1023+0038 is the first millisecond pulsar that was ever observed as an optical and UV pulsar. So far, it is the only optical transitional millisecond pulsar. The rotation- and accretion-powered emission mechanisms hardly individually explain the observed characteristics of optical pulsations. A synergistic model, combining these standard emission processes, was proposed to explain the origin of the X-ray/UV/optical pulsations. We study the phase lag between the pulses in the optical and X-ray bands to gain insight into the physical mechanisms that cause it. We performed a detailed timing analysis of simultaneous or quasi-simultaneous observations in the X-ray band, acquired with the XMM-Newton and NICER satellites, and in the optical band, with the fast photometers SiFAP2 (mounted at the 3.6 m Telescopio Nazionale Galileo) and Aqueye+ (mounted at the 1.8 m Copernicus Telescope). We estimated the time lag of the optical pulsation with respect to that in the X-rays by modeling the folded pulse profiles with two harmonic components. Optical pulses lag the X-ray pulses by $sim$ 150 $mu$s in observations acquired with instruments (NICER and Aqueye+) whose absolute timing uncertainty is much smaller than the measured lag. We also show that the phase lag between optical and X-ray pulsations lies in a limited range of values, $delta phi in$ (0 $-$ 0.15), which is maintained over timescales of about five years. This indicates that both pulsations originate from the same region, and it supports the hypothesis of a common emission mechanism. Our results are interpreted in the shock-driven mini pulsar nebula scenario. This scenario suggests that optical and X-ray pulses are produced by synchrotron emission from the shock that formed within a few light cylinder radii away ($sim$ 100 km) from the pulsar, where its striped wind encounters the accretion disk inflow. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12975v1
Taking a break: paused accretion in the symbiotic binary RT Cru by A. Pujol et al. on Friday 25 November Symbiotic binaries sometimes hide their symbiotic nature for significant periods of time. There is mounting observational evidence that in those symbiotics that are powered solely by accretion of red-giant's wind material onto a white dwarf, without any quasi-steady shell burning on the surface of the white dwarf, the characteristic emission lines in the optical spectrum can vanish, leaving the semblance of an isolated red giant spectrum. Here we present compelling evidence that this disappearance of optical emission lines from the spectrum of RT Cru during 2019 was due to a decrease in the accretion rate, which we derive by modeling the X-ray spectrum. This drop in accretion rate leads to a lower flux of ionizing photons and thus to faint/absent photoionization emission lines in the optical spectrum. We observed the white dwarf symbiotic RT Cru with XMM-Newton and Swift in X-rays and UV and collected ground-based optical spectra and photometry over the last 33 years. This long-term coverage shows that during most of the year 2019, the accretion rate onto the white dwarf was so low, $dot{M}= (3.2pm 0.06), times$10$^{-11}$ $M_{odot}$ yr$^{-1}$ (d/2.52 kpc)$^2$, that the historically detected hard X-ray emission almost vanished, the UV flux faded by roughly 5 magnitudes, the $U$, $B$ and $V$ flickering amplitude decreased, and the Balmer lines virtually disappeared from January through March 2019. Long-lasting low-accretion episodes as the one reported here may hamper the chances of RT Cru experiencing nova-type outburst despite the high-mass of the accreting white dwarf. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.13193v1
Investigating the origin of optical and X-ray pulsations of the transitional millisecond pulsar PSR J1023+0038 by G. Illiano et al. on Thursday 24 November PSR J1023+0038 is the first millisecond pulsar that was ever observed as an optical and UV pulsar. So far, it is the only optical transitional millisecond pulsar. The rotation- and accretion-powered emission mechanisms hardly individually explain the observed characteristics of optical pulsations. A synergistic model, combining these standard emission processes, was proposed to explain the origin of the X-ray/UV/optical pulsations. We study the phase lag between the pulses in the optical and X-ray bands to gain insight into the physical mechanisms that cause it. We performed a detailed timing analysis of simultaneous or quasi-simultaneous observations in the X-ray band, acquired with the XMM-Newton and NICER satellites, and in the optical band, with the fast photometers SiFAP2 (mounted at the 3.6 m Telescopio Nazionale Galileo) and Aqueye+ (mounted at the 1.8 m Copernicus Telescope). We estimated the time lag of the optical pulsation with respect to that in the X-rays by modeling the folded pulse profiles with two harmonic components. Optical pulses lag the X-ray pulses by $sim$ 150 $mu$s in observations acquired with instruments (NICER and Aqueye+) whose absolute timing uncertainty is much smaller than the measured lag. We also show that the phase lag between optical and X-ray pulsations lies in a limited range of values, $delta phi in$ (0 $-$ 0.15), which is maintained over timescales of about five years. This indicates that both pulsations originate from the same region, and it supports the hypothesis of a common emission mechanism. Our results are interpreted in the shock-driven mini pulsar nebula scenario. This scenario suggests that optical and X-ray pulses are produced by synchrotron emission from the shock that formed within a few light cylinder radii away ($sim$ 100 km) from the pulsar, where its striped wind encounters the accretion disk inflow. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12975v1
Taking a break: paused accretion in the symbiotic binary RT Cru by A. Pujol et al. on Thursday 24 November Symbiotic binaries sometimes hide their symbiotic nature for significant periods of time. There is mounting observational evidence that in those symbiotics that are powered solely by accretion of red-giant's wind material onto a white dwarf, without any quasi-steady shell burning on the surface of the white dwarf, the characteristic emission lines in the optical spectrum can vanish, leaving the semblance of an isolated red giant spectrum. Here we present compelling evidence that this disappearance of optical emission lines from the spectrum of RT Cru during 2019 was due to a decrease in the accretion rate, which we derive by modeling the X-ray spectrum. This drop in accretion rate leads to a lower flux of ionizing photons and thus to faint/absent photoionization emission lines in the optical spectrum. We observed the white dwarf symbiotic RT Cru with XMM-Newton and Swift in X-rays and UV and collected ground-based optical spectra and photometry over the last 33 years. This long-term coverage shows that during most of the year 2019, the accretion rate onto the white dwarf was so low, $dot{M}= (3.2pm 0.06), times$10$^{-11}$ $M_{odot}$ yr$^{-1}$ (d/2.52 kpc)$^2$, that the historically detected hard X-ray emission almost vanished, the UV flux faded by roughly 5 magnitudes, the $U$, $B$ and $V$ flickering amplitude decreased, and the Balmer lines virtually disappeared from January through March 2019. Long-lasting low-accretion episodes as the one reported here may hamper the chances of RT Cru experiencing nova-type outburst despite the high-mass of the accreting white dwarf. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.13193v1
Deep X-ray and radio observations of the first outburst of the young magnetar Swift J1818 0-1607 by A. Y. Ibrahim et al. on Thursday 24 November Swift J1818.0-1607 is a radio-loud magnetar with a spin period of 1.36 s and a dipolar magnetic field strength of B~3E14 G, which is very young compared to the Galactic pulsar population. We report here on the long-term X-ray monitoring campaign of this young magnetar using XMM-Newton, NuSTAR, and Swift from the activation of its first outburst in March 2020 until October 2021, as well as INTEGRAL upper limits on its hard X-ray emission. The 1-10 keV magnetar spectrum is well modeled by an absorbed blackbody with a temperature of kT_BB~1.1 keV, and apparent reduction in the radius of the emitting region from ~0.6 to ~0.2 km. We also confirm the bright diffuse X-ray emission around the source extending between ~50'' and ~110''. A timing analysis revealed large torque variability, with an average spin-down rate nudot~-2.3E-11 Hz^2 that appears to decrease in magnitude over time. We also observed Swift J1818.0-1607 with the Karl G. Jansky Very Large Array (VLA) on 2021 March 22. We detected the radio counterpart to Swift J1818.0-1607 measuring a flux density of S_v = 4.38+/-0.05 mJy at 3 GHz, and a half ring-like structure of bright diffuse radio emission located at ~90'' to the west of the magnetar. We tentatively suggest that the diffuse X-ray emission is due to a dust scattering halo and that the radio structure may be associated with the supernova remnant of this young pulsar, based on its morphology. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12391v1
Deep X-ray and radio observations of the first outburst of the young magnetar Swift J1818 0-1607 by A. Y. Ibrahim et al. on Wednesday 23 November Swift J1818.0-1607 is a radio-loud magnetar with a spin period of 1.36 s and a dipolar magnetic field strength of B~3E14 G, which is very young compared to the Galactic pulsar population. We report here on the long-term X-ray monitoring campaign of this young magnetar using XMM-Newton, NuSTAR, and Swift from the activation of its first outburst in March 2020 until October 2021, as well as INTEGRAL upper limits on its hard X-ray emission. The 1-10 keV magnetar spectrum is well modeled by an absorbed blackbody with a temperature of kT_BB~1.1 keV, and apparent reduction in the radius of the emitting region from ~0.6 to ~0.2 km. We also confirm the bright diffuse X-ray emission around the source extending between ~50'' and ~110''. A timing analysis revealed large torque variability, with an average spin-down rate nudot~-2.3E-11 Hz^2 that appears to decrease in magnitude over time. We also observed Swift J1818.0-1607 with the Karl G. Jansky Very Large Array (VLA) on 2021 March 22. We detected the radio counterpart to Swift J1818.0-1607 measuring a flux density of S_v = 4.38+/-0.05 mJy at 3 GHz, and a half ring-like structure of bright diffuse radio emission located at ~90'' to the west of the magnetar. We tentatively suggest that the diffuse X-ray emission is due to a dust scattering halo and that the radio structure may be associated with the supernova remnant of this young pulsar, based on its morphology. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12391v1
On the cosmic evolution of AGN obscuration and the X-ray luminosity function: XMM-Newton and Chandra spectral analysis of the 31 3 deg ^2 Stripe 82X by Alessandro Peca et al. on Wednesday 23 November We present X-ray spectral analysis of XMM and Chandra observations in the 31.3 deg$^2$ Stripe-82X (S82X) field. Of the 6181 X-ray sources in this field, we analyze a sample of 2937 active galactic nuclei (AGN) with solid redshifts and sufficient counts determined by simulations. Our results show a population with median values of spectral index $Gamma=1.94_{-0.39}^{+0.31}$, column density log$,N_{mathrm{H}}/mathrm{cm}^{-2}=20.7_{-0.5}^{+1.2}$ and intrinsic, de-absorbed, 2-10 keV luminosity log$,L_{mathrm{X}}/mathrm{erg,s}^{-1}=44.0_{-1.0}^{+0.7}$, in the redshift range 0-4. We derive the intrinsic fraction of AGN that are obscured ($22leqmathrm{log},N_{mathrm{H}}/mathrm{cm}^{-2}43$. This work constrains the AGN obscuration and spectral shape of the still uncertain high-luminosity and high-redshift regimes (log$,L_{mathrm{X}}/mathrm{erg,s}^{-1}>45.5$, $z>3$), where the obscured AGN fraction rises to $64pm12%$. We report a luminosity and density evolution of the X-ray luminosity function, with obscured AGN dominating at all luminosities at $z>2$ and unobscured sources prevailing at log$,L_{mathrm{X}}/mathrm{erg,s}^{-1}>45$ at lower redshifts. Our results agree with evolutionary models in which the bulk of AGN activity is triggered by gas-rich environments and in a downsizing scenario. Also, the black hole accretion density (BHAD) is found to evolve similarly to the star formation rate density, confirming the co-evolution between AGN and host-galaxy, but suggesting different time scales in their growing history. The derived BHAD evolution shows that Compton-thick AGN contribute to the accretion history of AGN as much as all other AGN populations combined. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.08030v2
Deep X-ray and radio observations of the first outburst of the young magnetar Swift J1818 0-1607 by A. Y. Ibrahim et al. on Wednesday 23 November Swift J1818.0-1607 is a radio-loud magnetar with a spin period of 1.36 s and a dipolar magnetic field strength of B~3E14 G, which is very young compared to the Galactic pulsar population. We report here on the long-term X-ray monitoring campaign of this young magnetar using XMM-Newton, NuSTAR, and Swift from the activation of its first outburst in March 2020 until October 2021, as well as INTEGRAL upper limits on its hard X-ray emission. The 1-10 keV magnetar spectrum is well modeled by an absorbed blackbody with a temperature of kT_BB~1.1 keV, and apparent reduction in the radius of the emitting region from ~0.6 to ~0.2 km. We also confirm the bright diffuse X-ray emission around the source extending between ~50'' and ~110''. A timing analysis revealed large torque variability, with an average spin-down rate nudot~-2.3E-11 Hz^2 that appears to decrease in magnitude over time. We also observed Swift J1818.0-1607 with the Karl G. Jansky Very Large Array (VLA) on 2021 March 22. We detected the radio counterpart to Swift J1818.0-1607 measuring a flux density of S_v = 4.38+/-0.05 mJy at 3 GHz, and a half ring-like structure of bright diffuse radio emission located at ~90'' to the west of the magnetar. We tentatively suggest that the diffuse X-ray emission is due to a dust scattering halo and that the radio structure may be associated with the supernova remnant of this young pulsar, based on its morphology. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.12391v1
On the cosmic evolution of AGN obscuration and the X-ray luminosity function: XMM-Newton and Chandra spectral analysis of the 31 3 deg ^2 Stripe 82X by Alessandro Peca et al. on Tuesday 22 November We present X-ray spectral analysis of XMM and Chandra observations in the 31.3 deg$^2$ Stripe-82X (S82X) field. Of the 6181 X-ray sources in this field, we analyze a sample of 2937 active galactic nuclei (AGN) with solid redshifts and sufficient counts determined by simulations. Our results show a population with median values of spectral index $Gamma=1.94_{-0.39}^{+0.31}$, column density log$,N_{mathrm{H}}/mathrm{cm}^{-2}=20.7_{-0.5}^{+1.2}$ and intrinsic, de-absorbed, 2-10 keV luminosity log$,L_{mathrm{X}}/mathrm{erg,s}^{-1}=44.0_{-1.0}^{+0.7}$, in the redshift range 0-4. We derive the intrinsic fraction of AGN that are obscured ($22leqmathrm{log},N_{mathrm{H}}/mathrm{cm}^{-2}43$. This work constrains the AGN obscuration and spectral shape of the still uncertain high-luminosity and high-redshift regimes (log$,L_{mathrm{X}}/mathrm{erg,s}^{-1}>45.5$, $z>3$), where the obscured AGN fraction rises to $64pm12%$. We report a luminosity and density evolution of the X-ray luminosity function, with obscured AGN dominating at all luminosities at $z>2$ and unobscured sources prevailing at log$,L_{mathrm{X}}/mathrm{erg,s}^{-1}>45$ at lower redshifts. Our results agree with evolutionary models in which the bulk of AGN activity is triggered by gas-rich environments and in a downsizing scenario. Also, the black hole accretion density (BHAD) is found to evolve similarly to the star formation rate density, confirming the co-evolution between AGN and host-galaxy, but suggesting different time scales in their growing history. The derived BHAD evolution shows that Compton-thick AGN contribute to the accretion history of AGN as much as all other AGN populations combined. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.08030v2
On the cosmic evolution of AGN obscuration and the X-ray luminosity function: XMM-Newton and Chandra spectral analysis of the 31 3 deg ^2 Stripe 82X by Alessandro Peca et al. on Tuesday 22 November We present X-ray spectral analysis of XMM and Chandra observations in the 31.3 deg$^2$ Stripe-82X (S82X) field. Of the 6181 X-ray sources in this field, we analyze a sample of 2937 active galactic nuclei (AGN) with solid redshifts and sufficient counts determined by simulations. Our results show a population with median values of spectral index $Gamma=1.94_{-0.39}^{+0.31}$, column density log$,N_{mathrm{H}}/mathrm{cm}^{-2}=20.7_{-0.5}^{+1.2}$ and intrinsic, de-absorbed, 2-10 keV luminosity log$,L_{mathrm{X}}/mathrm{erg,s}^{-1}=44.0_{-1.0}^{+0.7}$, in the redshift range 0-4. We derive the intrinsic fraction of AGN that are obscured ($22leqmathrm{log},N_{mathrm{H}}/mathrm{cm}^{-2}43$. This work constrains the AGN obscuration and spectral shape of the still uncertain high-luminosity and high-redshift regimes (log$,L_{mathrm{X}}/mathrm{erg,s}^{-1}>45.5$, $z>3$), where the obscured AGN fraction rises to $64pm12%$. We report a luminosity and density evolution of the X-ray luminosity function, with obscured AGN dominating at all luminosities at $z>2$ and unobscured sources prevailing at log$,L_{mathrm{X}}/mathrm{erg,s}^{-1}>45$ at lower redshifts. Our results agree with evolutionary models in which the bulk of AGN activity is triggered by gas-rich environments and in a downsizing scenario. Also, the black hole accretion density (BHAD) is found to evolve similarly to the star formation rate density, confirming the co-evolution between AGN and host-galaxy, but suggesting different time scales in their growing history. The derived BHAD evolution shows that Compton-thick AGN contribute to the accretion history of AGN as much as all other AGN populations combined. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.08030v2
Timescale-dependent X-ray to UV time lags of NGC 4593 using high-intensity XMM-Newton observations with Swift and AstroSat by Max W. J. Beard et al. on Monday 21 November We present a 140ks observation of NGC 4593 with XMM-Newton providing simultaneous and continuous PN X-ray and OM UV (UVW1 2910AA) lightcurves which sample short-timescale variations better than previous observations. These observations were simultaneous with 22d of Swift X-ray and UV/optical monitoring, reported previously, and 4d of AstroSat X-ray (SXT), far (FUV 1541AA), and near (NUV 2632AA) UV allowing lag measurements between them and the highly-sampled XMM. From the XMM we find that UVW1 lags behind the X-rays by 29.5$pm$1.3ks, $sim$half the lag previously determined from the Swift monitoring. Re-examination of the textit{Swift} data reveals a bimodal lag distribution, with evidence for both the long and short lags. However if we detrend the Swift lightcurves by LOWESS filtering with a 5d width, only the shorter lag (23.8$pm$21.2ks) remains. The NUV observations, compared to PN and SXT, confirm the $sim$30ks lag found by XMM and, after 4d filtering is applied to remove the long-timescale component, the FUV shows a lag of $sim$23ks. The resultant new UVW1, FUV, and NUV lag spectrum extends to the X-ray band without requiring additional X-ray to UV lag offset, which if the UV arises from reprocessing of X-rays, implies direct illumination of the reprocessor. By referencing previous Swift and HST lag measurements, we obtain an X-ray to optical lag spectrum which agrees with a model using the KYNreverb disc-reprocessing code, assuming the accepted mass of $7.63times10^{6}M_{odot}$ and a spin approaching maximum. Previously noted lag contribution from the BLR in the Balmer and Paschen continua are still prominent. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.10229v1
Variability In A Low-Mass AGN: Oscillation Or Eruption? by Robbie Webbe et al. on Monday 21 November Following the discovery of a new class of X-ray variability seen in four galaxies, dubbed Quasi-Periodic Eruptions (QPEs), we reconsider the variability seen in the low-mass AGN 2XMM J123103.2+110648 to ascertain whether it should be considered the fifth QPE host galaxy. We apply the autocorrelation function to two archival XMM-Newton observations to determine characteristic timescales for variability of $sim$ 13.52 ks and $sim$ 14.35 ks. The modelling of lightcurves, both folded at these timescales and unfolded, indicates that a Gaussian model is preferable over a sinusoidal model, with average durations for the bright phases of 6.17 ks and 7.69 ks. In a broad 0.2-1.0 keV band the average amplitude of the bright phases was found to be 2.86 and 8.56 times the quiescent count rate. The pattern of variability seen in 2XMM J123103.2+110648 cannot be definitively declared as a series of Quasi-Periodic Eruptions. Instead, this suggests there may be a continuum of quasi-periodic variability ranging from eruptions to oscillations being caused by a single mechanism. This offers the possibility of finding further sources that continue to bridge the gap between QPEs and Quasi-Periodic Oscillations. A targeted analysis of 47 observations of 11 other low-mass AGN $(log(M_{BH}) lesssim 6)$ found no evidence of QPE or QPO-like behaviour in a sample of other similar mass objects. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2211.10176v1
L'analyse des données archivées du télescope spatial XMM-Newton a dévoilé une variabilité très inhabituelle dans l'émission en rayons X mous de PSR J1311-3430, un pulsar milliseconde veuve noire en couple serré avec une étoile compagne de très faible masse (M ∼ 0,01 M⊙). Une périodicité de 2h transitoire est observée alors que la période orbitale du couple est de 1,5 heure. Aucun modèle n'explique cette observation… L'étude est publiée dans Astronomy&Astrophysics.
Broadband X-ray Spectral Analysis of the Dual AGN System Mrk 739 by Koki Inaba et al. on Monday 17 October We present the result of a broadband (0.5-70 keV) X-ray spectral analysis of the late-merger galaxy Mrk 739, which contains a dual active galactic nucleus (AGN), Mrk 739E and Mrk 739W, with a separation of $sim$3.4 kpc. The spectra obtained with NuSTAR, Chandra, XMM-Newton and Swift/BAT are simultaneously analyzed by separating the contributions from the two AGNs and extended emission with the Chandra data. To evaluate the reflection components from the AGN tori, we consider two models, a phenomenological one (pexrav and zgauss) and a more physically motivated one (XCLUMPY; Tanimoto et al. 2019). On the basis of the results with XCLUMPY, we find that the AGNs in Mrk 739E and Mrk 739W have intrinsic 2-10 keV luminosities of $1.0 times 10^{43}$ and $7.5 times 10^{41} rm{erg} rm{s}^{-1}$ absorbed by hydrogen column densities of $N_{rm{H}} < 6.5 times 10^{19} rm{cm}^{-2}$ and $N_{rm{H}} = 6.9^{+3.2}_{-1.7} times 10^{21} rm{cm}^{-2}$, respectively. The torus covering fraction of the material with $N_{rm{H}} > 10^{22} rm{cm}^{-2}$ in Mrk 739E, $C_{rm{T}}^{(22)} < 0.50$ at a 90% confidence limit, is found to be smaller than those found for late-merger ultra/luminous infrared galaxies, $C_{rm{T}}^{(22)} = 0.71pm0.16$ (mean and standard deviation; Yamada et al. 2021). Considering the small star formation rate of Mrk 739E, we suggest that the gas-to-mass ratio of the host galaxy is an important parameter to determine the circumnuclear environment of an AGN in late merger. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.08791v1
On the cosmic evolution of AGN obscuration and the X-ray luminosity function: XMM-Newton and Chandra spectral analysis of the 31 3 deg ^2 Stripe 82X by Alessandro Peca et al. on Monday 17 October We present X-ray spectral analysis of XMM and Chandra observations in the 31.3 deg$^2$ Stripe-82X (S82X) field. Of the 6181 unique X-ray sources in this field, we select and analyze a sample of 2937 candidate active galactic nuclei (AGN) with solid redshifts and sufficient counts determined by simulations. Our results show an observed population with median values of spectral index $Gamma=1.94_{-0.39}^{+0.31}$, column density log $N_H/rm{cm}^{-2}=20.7_{-0.5}^{+1.2}$ ($21.6_{-0.9}^{+0.7}$ considering upper limits) and intrinsic, de-absorbed, 2-10 keV luminosity log $L_X/rm{erg,s}^{-1}=44.0_{-1.0}^{+0.7}$, in the redshift range 0-4. Correcting for observational biases, we derive the intrinsic, model-independent, fraction of AGN that are obscured ($22leqrm{log},N_H/rm{cm}^{-2}43$. This work constrains the AGN obscuration and spectral shape of the still uncertain high-luminosity and high-redshift regimes (log $L_X/rm{erg,s}^{-1}>45.5$, $z>3$), where the obscured AGN fraction rises to $64pm12%$. The total, obscured, and unobscured X-ray luminosity functions (XLFs) are determined out to $z=4$. We report a luminosity and density evolution of the total XLF, with obscured AGN dominating at all luminosities at $z>2$ and unobscured sources prevailing at log $L_X/rm{erg,s}^{-1}>45$ at lower redshifts. Our results agree with the evolutionary models in which the bulk of AGN activity is triggered by gas-rich environments and in a downsizing scenario. Also, the black hole accretion density is found to evolve similarly to the star formation rate density, confirming the co-evolution scenario between AGN and host galaxy, but suggesting different time scales in their growing history. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.08030v1
The Planck clusters in the LOFAR sky III LoTSS-DR2: Dynamic states and density fluctuations of the intracluster medium by X. Zhang et al. on Sunday 16 October The footprint of LoTSS-DR2 covers 309 PSZ2 galaxy clusters, 83 of which host a radio halo and 26 host a radio relic(s). It provides us an excellent opportunity to statistically study the properties of extended cluster radio sources, especially their connection with merging activities. We aim to quantify cluster dynamic states to investigate their relation with the occurrence of extended radio sources. We also search for connections between intracluster medium (ICM) turbulence and nonthermal characteristics of radio halos in the LoTSS-DR2. We analyzed XMM-Newton and Chandra archival X-ray data and computed concentration parameters and centroid shifts that indicate the dynamic states of the clusters. We also performed a power spectral analysis of the X-ray surface brightness (SB) fluctuations to investigate large-scale density perturbations and estimate the turbulent velocity dispersion. The power spectral analysis results in a large scatter density fluctuation amplitude. We therefore only found a marginal anticorrelation between density fluctuations and cluster relaxation state, and we did not find a correlation between density fluctuations and radio halo power. Nevertheless, the injected power for particle acceleration calculated from turbulent dissipation is correlated with the radio halo power, where the best-fit unity slope supports the turbulent (re)acceleration scenario. Two different acceleration models, transit-time damping and adiabatic stochastic acceleration, cannot be distinguished due to the large scatter of the estimated turbulent Mach number. We introduced a new quantity $[kTcdot Y_X]_{r_mathrm{RH}}$, which is proportional to the turbulent acceleration power assuming a constant Mach number. This quantity is strongly correlated with radio halo power, where the slope is also unity. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.07284v1
Swift and XMM-Newton observations of an RS CVn type eclipsing binary SZ Psc: Superflare and coronal properties by Subhajeet Karmakar et al. on Sunday 16 October We present an in-depth study of a large and long duration ($>$1.3 days) X-ray flare observed on an RS CVn type eclipsing binary system SZ Psc using observations from Swift observatory. In the 0.35$-$10 keV energy band, the peak luminosity is estimated to be 4.2$times$10$^{33}$ erg s$^{-1}$. The quiescent corona of SZ Psc was observed $sim$5.67 d after the flare using Swift observatory, and also $sim$1.4 yr after the flare using the XMM-Newton satellite. The quiescent corona is found to consist of three temperature plasma: 4, 13, and 48 MK. High-resolution X-ray spectral analysis of the quiescent corona of SZ Psc suggests that the high first ionization potential (FIP) elements are more abundant than the low-FIP elements. The time-resolved X-ray spectroscopy of the flare shows a significant variation in the flare temperature, emission measure, and abundance. The peak values of temperature, emission measure, and abundances during the flare are estimated to be 199$pm$11 MK, 2.13$pm$0.05 $times 10^{56}$ cm$^{-3}$, 0.66$pm$0.09 Z$_{odot}$, respectively. Using the hydrodynamic loop modeling, we derive the loop length of the flare as 6.3$pm$0.5 $times 10^{11}$ cm, whereas the loop pressure and density at the flare peak are derived to be 3.5$pm$0.7 $times 10^{3}$ dyne cm$^{-2}$ and 8$pm$2 $times 10^{10}$ cm$^{-3}$, respectively. The total magnetic field to produce the flare is estimated to be 490$pm$60 G. The large magnetic field at the coronal height is supposed to be due to the presence of an extended convection zone of the sub-giant and the high orbital velocity. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.07170v1
Swift and XMM-Newton observations of an RS CVn type eclipsing binary SZ Psc: Superflare and coronal properties by Subhajeet Karmakar et al. on Sunday 16 October We present an in-depth study of a large and long duration ($>$1.3 days) X-ray flare observed on an RS CVn type eclipsing binary system SZ Psc using observations from Swift observatory. In the 0.35$-$10 keV energy band, the peak luminosity is estimated to be 4.2$times$10$^{33}$ erg s$^{-1}$. The quiescent corona of SZ Psc was observed $sim$5.67 d after the flare using Swift observatory, and also $sim$1.4 yr after the flare using the XMM-Newton satellite. The quiescent corona is found to consist of three temperature plasma: 4, 13, and 48 MK. High-resolution X-ray spectral analysis of the quiescent corona of SZ Psc suggests that the high first ionization potential (FIP) elements are more abundant than the low-FIP elements. The time-resolved X-ray spectroscopy of the flare shows a significant variation in the flare temperature, emission measure, and abundance. The peak values of temperature, emission measure, and abundances during the flare are estimated to be 199$pm$11 MK, 2.13$pm$0.05 $times 10^{56}$ cm$^{-3}$, 0.66$pm$0.09 Z$_{odot}$, respectively. Using the hydrodynamic loop modeling, we derive the loop length of the flare as 6.3$pm$0.5 $times 10^{11}$ cm, whereas the loop pressure and density at the flare peak are derived to be 3.5$pm$0.7 $times 10^{3}$ dyne cm$^{-2}$ and 8$pm$2 $times 10^{10}$ cm$^{-3}$, respectively. The total magnetic field to produce the flare is estimated to be 490$pm$60 G. The large magnetic field at the coronal height is supposed to be due to the presence of an extended convection zone of the sub-giant and the high orbital velocity. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.07170v1
A Swift X-ray view of the SMS4 sample -- X-ray properties of 31 quasars and radio galaxies by Alessandro Maselli et al. on Sunday 16 October We present Swift observations of 31 sources from the SMS4 catalog, a sample of 137 bright radio sources in the Southern Hemisphere. All these sources had no Chandra or XMM-Newton observations: 24 of these were observed with Swift through a dedicated proposal in 2015, and data for the remaining seven were retrieved from the Swift archive. The reduction and analysis of data collected by the Swift X-ray Telescope (XRT) led to 20 detections in the 0.3--10 keV band. We provide details of the X-ray emission in this band for these 20 detections, as well as upper limits for the remaining 11 SMS4 sources. When statistics allowed, we investigated the extent of the X-ray emission, the hardness ratio, and we carried out a spectral analysis. We matched the 20 X-ray detected sources with infrared (AllWISE, CatWISE2020) and optical (GSC 2.3.2, DES DR2) catalogs to establish associations with infrared and optical sources, and compared our results with previously published counterparts in these bands. Requiring a detection in both the infrared and the optical bands to establish a candidate counterpart for our X-ray detections, we obtain reliable counterparts for 18 sources, while the remaining two sources need further investigation to establish firm identifications. We find that ~35% of all the SMS4 sources lie below the lower limit of 10.9 Jy for the flux density at 178 MHz. We present the list of 56 SMS4 sources that in 2022 March remain to be observed in the X-rays with narrow-field instruments. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2208.04763v2
Spectral Evolution of Ultraluminous X-ray Pulsar NGC 300 ULX-1 by Mason Ng et al. on Wednesday 12 October We report on results from a one-year soft X-ray observing campaign of the ultraluminous X-ray pulsar NGC 300 ULX-1 by the Neutron star Interior Composition Explorer (NICER) during 2018--2019. Our analysis also made use of data from Swift/XRT and XMM-Newton in order to model and remove contamination from the nearby eclipsing X-ray binary NGC 300 X-1. We constructed and fitted a series of 5-day averaged NICER spectra of NGC 300 ULX-1 in the 0.4--4.0 keV range to evaluate the long-term spectral evolution of the source, and found that an absorbed power-law model provided the best fit overall. Over the course of our observations, the source flux (0.4--4.0 keV; absorbed) dimmed from $2times10^{-12}$ to below $10^{-13}{rm,erg,s^{-1},cm^{-2}}$ and the spectrum softened, with the photon index going from $Gammaapprox1.6$ to $Gammaapprox2.6$. We interpret the spectral softening as reprocessed emission from the accretion disk edge coming into view while the pulsar was obscured by the possibly precessing disk. Some spectral fits were significantly improved by the inclusion of a disk blackbody component, and we surmise that this could be due to the pulsar emerging in between obscuration episodes by partial covering absorbers. We posit that we observed a low-flux state of the system (due to line-of-sight absorption) punctuated by the occasional appearance of the pulsar, indicating short-term source variability nested in longer-term accretion disk precession timescales. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.05678v1
Multi-wavelength study of the galactic PeVatron candidate LHAASO J2108+5157 by S. Abe et al. on Wednesday 12 October LHAASO J2108+5157 is one of the few known unidentified Ultra-High-Energy (UHE) gamma-ray sources with no Very-High-Energy (VHE) counterpart, recently discovered by the LHAASO collaboration. We observed LHAASO J2108+5157 in the X-ray band with XMM-Newton in 2021 for a total of 3.8 hours and at TeV energies with the Large-Sized Telescope prototype (LST-1), yielding 49 hours of good quality data. In addition, we analyzed 12 years of Fermi-LAT data, to better constrain emission of its High-Energy (HE) counterpart 4FGL J2108.0+5155. We found an excess (3.7 sigma) in the LST-1 data at energies E > 3 TeV. Further analysis in the whole LST-1 energy range assuming a point-like source, resulted in a hint (2.2 sigma) of hard emission which can be described with a single power law with photon index Gamma = 1.6 +- 0.2 between 0.3 - 100 TeV. We did not find any significant extended emission which could be related to a Supernova Remnant (SNR) or Pulsar Wind Nebula (PWN) in the XMM-Newton data, which puts strong constraints on possible synchrotron emission of relativistic electrons. The LST-1 and LHAASO observations can be explained as inverse Compton dominated leptonic emission of relativistic electrons with cutoff energy of 100+70-30 TeV. The low magnetic field in the source imposed by the X-ray upper limits on synchrotron emission is compatible with a hypothesis of a TeV halo. Furthermore, the spectral properties of the HE counterpart are consistent with a hypothesis of Geminga-like pulsar, which would be able to power the VHE-UHE emission. LST-1 and Fermi-LAT upper limits impose strong constraints on hadronic scenario of pi-0 decay dominated emission from accelerated protons interacting with nearby molecular clouds, requiring hard spectral index, which is incompatible with the standard diffusive acceleration scenario. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.00775v3
Oxygen and iron in interstellar dust: an X-ray investigation by I. Psaradaki et al. on Wednesday 12 October Understanding the chemistry of the interstellar medium (ISM) is fundamental for the comprehension of the Galactic and stellar evolution. X-rays provide an excellent way to study the dust chemical composition and crystallinity along different sight-lines in the Galaxy. In this work we study the dust grain chemistry in the diffuse regions of the interstellar medium in the soft X-ray band (
The Jet Opening Angle and Event Rate Distributions of Short Gamma-ray Bursts from Late-time X-ray Afterglows by Alicia Rouco Escorial et al. on Wednesday 12 October We present a comprehensive study of 29 short gamma-ray bursts (SGRBs) observed $approx 0.8-60$ days post-burst using $Chandra$ and $XMM-Newton$. We provide the inferred distributions of SGRB jet opening angles and true event rates to compare against neutron star merger rates. We perform uniform analysis and modeling of their afterglows, obtaining 10 opening angle measurements and 19 lower limits. We report on two new opening angle measurements (SGRBs 050724A and 200411A) and eight updated values, obtaining a median value of $langle theta_{rm j} rangle approx 6.1^{circ}$ [-3.2$^{circ}$,+9.3$^{circ}$] (68% confidence on the full distribution) from jet measurements alone. For the remaining events, we infer $theta_{rm j}gtrsim 0.5-26^{circ}$. We uncover a population of SGRBs with wider jets of $theta_{rm j} gtrsim 10^{circ}$ (including two measurements of $theta_{rm j} gtrsim 15^{circ}$), representing $sim 28%$ of our sample. Coupled with multi-wavelength afterglow information, we derive a total true energy of $langle E_{rm true, tot} rangle approx 10^{49}-10^{50}$,erg which is consistent with MHD jet launching mechanisms. Furthermore, we determine a range for the beaming-corrected event rate of $mathfrak{R}_{rm true} approx360-1800$ Gpc$^{-3}$ yr$^{-1}$, set by the inclusion of a population of wide jets on the low end, and the jet measurements alone on the high end. From a comparison with the latest merger rates, our results are consistent with the majority of SGRBs originating from binary neutron star mergers. However, our inferred rates are well above the latest neutron star-black hole merger rates, consistent with at most a small fraction of SGRBs originating from such mergers. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.05695v1
TRAPUM upper limits on pulsed radio emission for SMC X-ray pulsar J0058-7218 by E. Carli et al. on Tuesday 11 October The TRAPUM collaboration has used the MeerKAT telescope to conduct a search for pulsed radio emission from the young Small Magellanic Cloud pulsar J0058-7218 located in the supernova remnant IKT 16, following its discovery in X-rays with XMM-Newton. We report no significant detection of dispersed, pulsed radio emission from this source in three 2-hour L-band observations using the core dishes of MeerKAT, setting an upper limit of 7.0 {mu}Jy on its mean flux density at 1284 MHz. This is nearly 7 times deeper than previous radio searches for this pulsar in Parkes L-band observations. This suggests that the radio emission of PSR J0058-7218 is not beamed towards Earth or that PSR J0058-7218 is similar to a handful of Pulsar Wind Nebulae systems that have a very low radio efficiency, such as PSR B0540-6919, the Large Magellanic Cloud Crab pulsar analogue. We have also searched for bright, dispersed, single radio pulses and found no candidates above a fluence of 93 mJy ms at 1284 MHz. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.04785v1
TRAPUM upper limits on pulsed radio emission for SMC X-ray pulsar J0058-7218 by E. Carli et al. on Tuesday 11 October The TRAPUM collaboration has used the MeerKAT telescope to conduct a search for pulsed radio emission from the young Small Magellanic Cloud pulsar J0058-7218 located in the supernova remnant IKT 16, following its discovery in X-rays with XMM-Newton. We report no significant detection of dispersed, pulsed radio emission from this source in three 2-hour L-band observations using the core dishes of MeerKAT, setting an upper limit of 7.0 {mu}Jy on its mean flux density at 1284 MHz. This is nearly 7 times deeper than previous radio searches for this pulsar in Parkes L-band observations. This suggests that the radio emission of PSR J0058-7218 is not beamed towards Earth or that PSR J0058-7218 is similar to a handful of Pulsar Wind Nebulae systems that have a very low radio efficiency, such as PSR B0540-6919, the Large Magellanic Cloud Crab pulsar analogue. We have also searched for bright, dispersed, single radio pulses and found no candidates above a fluence of 93 mJy ms at 1284 MHz. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.04785v1
Multi-wavelength study of the galactic PeVatron candidate LHAASO J2108+5157 by S. Abe et al. on Tuesday 11 October LHAASO J2108+5157 is one of the few known unidentified Ultra-High-Energy (UHE) gamma-ray sources with no Very-High-Energy (VHE) counterpart, recently discovered by the LHAASO collaboration. We observed LHAASO J2108+5157 in the X-ray band with XMM-Newton in 2021 for a total of 3.8 hours and at TeV energies with the Large-Sized Telescope prototype (LST-1), yielding 49 hours of good quality data. In addition, we analyzed 12 years of Fermi-LAT data, to better constrain emission of its High-Energy (HE) counterpart 4FGL J2108.0+5155. We found an excess (3.7 sigma) in the LST-1 data at energies E > 3 TeV. Further analysis in the whole LST-1 energy range assuming a point-like source, resulted in a hint (2.2 sigma) of hard emission which can be described with a single power law with photon index Gamma = 1.6 +- 0.2 between 0.3 - 100 TeV. We did not find any significant extended emission which could be related to a Supernova Remnant (SNR) or Pulsar Wind Nebula (PWN) in the XMM-Newton data, which puts strong constraints on possible synchrotron emission of relativistic electrons. The LST-1 and LHAASO observations can be explained as inverse Compton dominated leptonic emission of relativistic electrons with cutoff energy of 100+70-30 TeV. The low magnetic field in the source imposed by the X-ray upper limits on synchrotron emission is compatible with a hypothesis of a TeV halo. Furthermore, the spectral properties of the HE counterpart are consistent with a hypothesis of Geminga-like pulsar, which would be able to power the VHE-UHE emission. LST-1 and Fermi-LAT upper limits impose strong constraints on hadronic scenario of pi-0 decay dominated emission from accelerated protons interacting with nearby molecular clouds, requiring hard spectral index, which is incompatible with the standard diffusive acceleration scenario. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2210.00775v2
A deep study of A399-401: An application for wide-field facet calibration by J. M. G. H. J. de Jong et al. on Monday 10 October We examine the particle acceleration mechanism in the Mpc-scale bridge between Abell 399 and Abell 401 and assess in particular if the synchrotron emission originates from first-order or second-order Fermi re-acceleration. We use deep (~40 hours) LOw-Frequency ARray (LOFAR) observations from Abell 399 and Abell 401 and apply improved direction-dependent calibration to produce deep radio images at three different resolutions at 144 MHz. With a point-to-point analysis we find in the bridge trends between the radio emission from our new maps and X-ray emission from an XMM Newton observation. By analyzing our observations and results, we argue that second-order Fermi re-acceleration is currently the most favoured process to explain the emission from the radio bridge, where past AGN activity may be responsible for the supply of fossil plasma needed for in-situ re-acceleration. The radio halos from Abell 401 and Abell 399 are also consistent with a second-order Fermi re-acceleration model. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.13930v3
SWIFT J0503 7-2819: A nearly synchronous intermediate polar below the period gap? by Nikita Rawat et al. on Sunday 25 September Based on the X-ray observations from XMM-Newton and Swift, and optical observations from Transiting Exoplanet Survey Satellite (TESS) and AAVSO, we present temporal and spectral properties of probable intermediate polar SWIFT J0503.7-2819. The X-ray light curve shows two distinctive features, where possibly the second pole seems to be active during the middle of the XMM-Newton observations. Present analysis confirms and also refines the previously reported orbital period of SWIFT J0503.7-2819 as 81.65$pm$0.04 min. The X-ray and optical variations of this target have been found to occur at the period of $sim$ 65 min, which we propose as the spin period of the white dwarf (WD). The energy-dependent modulation at this period, which are due to the photoelectric absorption in the accretion flow, also assures this conjecture. Two temperature thermal plasma model well explains the X-ray spectra with temperatures of $sim$ 150 eV and $sim$ 18.5 keV, which is absorbed by a dense material with an average equivalent hydrogen column density of 3.8 $times$ 10$^{22}$ cm$^{-2}$ that partially covers $sim$ 27% of the X-ray source. An attempt is made to understand the accretion flow in this system using the present data of SWIFT J0503.7-2819. If the proposed spin period is indeed the actual period, then SWIFT J0503.7-2819 could be the first nearly synchronous intermediate polar below the period gap. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.11141v1
SWIFT J0503 7-2819: A nearly synchronous intermediate polar below the period gap? by Nikita Rawat et al. on Sunday 25 September Based on the X-ray observations from XMM-Newton and Swift, and optical observations from Transiting Exoplanet Survey Satellite (TESS) and AAVSO, we present temporal and spectral properties of probable intermediate polar SWIFT J0503.7-2819. The X-ray light curve shows two distinctive features, where possibly the second pole seems to be active during the middle of the XMM-Newton observations. Present analysis confirms and also refines the previously reported orbital period of SWIFT J0503.7-2819 as 81.65$pm$0.04 min. The X-ray and optical variations of this target have been found to occur at the period of $sim$ 65 min, which we propose as the spin period of the white dwarf (WD). The energy-dependent modulation at this period, which are due to the photoelectric absorption in the accretion flow, also assures this conjecture. Two temperature thermal plasma model well explains the X-ray spectra with temperatures of $sim$ 150 eV and $sim$ 18.5 keV, which is absorbed by a dense material with an average equivalent hydrogen column density of 3.8 $times$ 10$^{22}$ cm$^{-2}$ that partially covers $sim$ 27% of the X-ray source. An attempt is made to understand the accretion flow in this system using the present data of SWIFT J0503.7-2819. If the proposed spin period is indeed the actual period, then SWIFT J0503.7-2819 could be the first nearly synchronous intermediate polar below the period gap. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.11141v1
X-ray spectral and timing analysis of the Compton Thick Seyfert 2 galaxy NGC 1068 by Indrani Pal et al. on Wednesday 21 September We present the timing and spectral analysis of the Compton Thick Seyfert 2 active galactic nuclei NGC 1068 observed using {it NuSTAR} and {it XMM-Newton}. In this work for the first time we calculated the coronal temperature ($rm{kT_{e}}$) of the source and checked for its variation between the epochs if any. The data analysed in this work comprised of (a) eight epochs of observations with {it NuSTAR} carried out during the period December 2012 to November 2017, and, (b) six epochs of observations with {it XMM-Newton} carried out during July 2000 to February 2015. From timing analysis of the {it NuSTAR} observations, we found the source not to show any variations in the soft band. However, on examination of the flux at energies beyond 20 keV, during August 2014 and August 2017 the source was brighter by about 20% and 30% respectively compared to the mean flux of the three 2012 {it NuSTAR} observations as in agreement with earlier results in literature. From an analysis of {it XMM-Newton} data we found no variation in the hard band (2 $-$ 4 keV) between epochs as well as within epochs. In the soft band (0.2 $-$ 2 keV), while the source was found to be not variable within epochs, it was found to be brighter in epoch B relative to epoch A. By fitting physical models we determined $rm{kT_{e}}$ to range between 8.46$^{+0.39}_{-0.66}$ keV and 9.13$^{+0.63}_{-0.98}$ keV. From our analysis, we conclude that we found no variation of $rm{kT_{e}}$ in the source. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.10261v1
Constraining leptonic emission scenarios for the PeVatron candidate HESS J1702-420 with deep XMM-Newton observations by L. Giunti et al. on Tuesday 20 September The unidentified TeV source HESS J1702-420 has recently been proposed as a new hadronic PeVatron candidate, based on the discovery of a small-scale emission sub-region with extremely hard gamma-ray spectrum up to 100 TeV (named HESS J1702-420A). Given the difficulty to discriminate between a hadronic or leptonic origin of the TeV emission, based on the H.E.S.S. measurement alone, we opted for a multi-wavelength approach. A deep X-ray observation was carried out using the XMM-Newton satellite, with the goal of probing a possible association with a hidden leptonic accelerator. No evidence of a clear counterpart for HESS J1702-420A was found in the X-ray data. After excluding an association with all nearby X-ray point sources, we derived strict upper limits on the diffuse X-ray emission and average magnetic field in the HESS J1702-420A region. We additionally report the serendipitous discovery of a new extended X-ray source, whose association with HESS J1702-420A is not obvious but cannot be ruled out either. A set of scripts dedicated to the multi-wavelength modeling of X-ray and gamma-ray data, based on Gammapy, Naima and Xspec, was developed in the context of this work and is made publicly available along with this paper. arXiv: http://arxiv.org/abs/http://arxiv.org/abs/2209.09566v1
Magnetars... resten van overleden sterren, waar we het in het verleden al wel eens over hebben gehad (https://www.nporadio2.nl/podcasts/zimmerman-in-space/5718/44-magnetars-miljoenen-keren-sterker-dan-de-sterkste-magneten-op-aarde). Maar wat weten we eigenlijk over het binnenste van magnetars? Een recente ontdekking laat mogelijk wat meer licht over deze kwestie schijnen. De eerdere aflevering over magnetars: https://www.nporadio2.nl/podcasts/zimmerman-in-space/5718/44-magnetars-miljoenen-keren-sterker-dan-de-sterkste-magneten-op-aarde NICER telescoop: https://heasarc.gsfc.nasa.gov/docs/nicer/ XMM-Newton telescoop van ESA: https://xmm-tools.cosmos.esa.int/external/xmm_news/20th_Anniversary/ Sterrenbeeld Schild: https://nl.wikipedia.org/wiki/Schild_(sterrenbeeld) Wat is - denken we - de dwarsdoorsnede van een neutronenster: https://skyandtelescope.org/astronomy-news/whats-inside-neutron-stars/ Het gierenmuseum: https://www.maisondesvautours.fr/
Astronomers working with the NASA's Chandra X-Ray Observatory and ESA's XMM-Newton have developed a technique to watch quasars and track the expansion of the Universe over the last 9 billion years. What they found is that the mysterious dark energy that's currently accelerating the expansion of the Universe doesn't appear to be a fixed amount. It's changing, and appears to be increasing over time. If true, it's a groundbreaking discovery in cosmology, and it could just fortel the end of the Universe.Support Universe Today Podcast
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