eROSITA on SRG

Predehl, P.; Andritschke, Robert; Becker, Werner; Bornemann, W.; Bräuninger, H.; Brunner, H.; Böller, Thomas; Burwitz, V.; Burkert, Wolfgang; Clerc, N.; Churazov, E.; Coutinho, Diogo; Dennerl, K.; Eder, Josef; Emberger, Valentin; Eraerds, Tanja; Freyberg, M. J.; Friedrich, Péter; Fürmetz, Maria; Georgakakis, A.; Großberger, C.; Haberl, F.; Hälker, Olaf; Hartner, Gisela; Hasinger, G.; Hoelzl, Johannes; Huber, Heinrich J.; Kienlin, A. von; Kink, W.; Kreykenbohm, I.; Lamer, G.; Lomakin, I.; Lapchov, Igor; Lovisari, Lorenzo; Meidinger, Norbert; Merloni, A.; Mican, Benjamin; Mohr, J. J.; Müller, S.; Nandra, K.; Pacaud, F.; Pavlinsky, M.; Perinati, E.; Pfeffermann, E.; Pietschner, Daniel; Reiffers, Jonas; Reiprich, T. H.; Robrade, J.; Salvato, M.; Santangelo, A.; Sasaki, M.; Scheuerle, H.; Schmid, Christian; Schmitt, J. H. M. M.; Schwope, A. D.; Sunyaev, R.; Tenzer, C.; Tiedemann, Lars; Xu, Weizong; Yaroshenko, Valeri; Walther, Sabine; Wille, M.; Wilms, J.; Zhang, Yuying

doi:10.1117/12.2055426

Cited by 32 publications

(10 citation statements)

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“…A perhaps more promising instrument to search for direct‐impact mergers is the upcoming satellite mission eROSITA (Predehl et al ), which has a large field of view ∼1° (allowing it to cover M31 in just a few pointings) and is scheduled to launch around 2013. A 1‐h integrated exposure by eROSITA would reach a depth at soft X‐rays ∼0.5–2 keV of ∼10 −14 erg cm −2 s −1 , corresponding to a luminosity of L X ∼ 10 36 erg s −1 at the distance of M31, comparable to the predicted peak brightness of direct‐impact mergers given reasonably optimistic assumptions (ε rad ≳ 0.1).…”

Section: Discussionmentioning

confidence: 99%

Optical and X-ray transients from planet-star mergers

Metzger

Giannios

Spiegel

2012

Monthly Notices of the Royal Astronomical Society

103

118

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We evaluate the prompt electromagnetic signatures of the merger between a massive close-in planet (a 'hot Jupiter') and its host star, events with an estimated Galactic rate of ∼0.1-1 yr −1 . Depending on the ratio of the mean density of the planetρ p to that of the starρ , a planet-star merger results in three possible outcomes. Ifρ p /ρ 5, then the planet directly plunges below the stellar atmosphere before being disrupted by tidal forces. The dissipation of orbital energy creates a hot wake behind the planet, producing a extreme ultraviolet (EUV)/soft X-ray transient that increases in brightness and temperature as the planet sinks below the stellar surface. The peak luminosity L EUV/X 10 36 erg s −1 is achieved weeks to months prior to merger, after which the stellar surface is enshrouded by an outflow driven by the merger. The final stages of the inspiral are accompanied by an optical transient powered by the recombination of hydrogen in the outflow, which peaks at a luminosity of ∼10 37 -10 38 erg s −1 on a time-scale ∼days.If the star is instead significantly denser (ρ p /ρ 5), then the planet overflows its Roche lobe above the stellar surface. Forρ p /ρ 1 mass transfer is stable, resulting in the planet being accreted on the relatively slow time-scale set by tidal dissipation. However, for an intermediate-density range 1 ρ p /ρ 5 mass transfer may instead be unstable, resulting in the dynamical disruption of the planet into an accretion disc around the star. Outflows from the super-Eddington accretion disc power an optical transient with a peak luminosity of ∼10 37 -10 38 erg s −1 and characteristic duration ∼week-months. Emission from the disc itself becomes visible once the accretion rate decreases below the Eddington rate, resulting in a bolometric brightening and shift of the spectral peak to ultraviolet (UV) wavelengths. Optical transients from both direct-impact merger and tidal-disruption events in some ways resemble classical novae, but can be distinguished by their higher ejecta mass and lower velocity around hundreds of km s −1 , and by hard pre-and post-cursor emission, respectively. The most promising search strategy is with combined surveys of nearby massive galaxies (e.g. M31) at optical, UV and X-ray wavelengths with cadences from days to months.

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Section: Discussionmentioning

confidence: 99%

Optical and X-ray transients from planet-star mergers

Metzger

Giannios

Spiegel

2012

Monthly Notices of the Royal Astronomical Society

103

118

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“…TDSS-only targets fill ∼10 spectra per square degree. SPIDERS aims to characterize a subset of X-ray sources identified by eROSITA (extended Roentgen Survey with an Imaging Telescope Array; Predehl et al 2014). However, until the first catalog of eROSITA sources is available, SPIDERS will target sources from the RASS (Roentgen All-Sky Survey; Voges et al 1999) and XMMNewton (X-ray Multi-mirror Mission; Jansen et al 2001).…”

Section: Eboss Tdss and Spidersmentioning

confidence: 99%

The Fourteenth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the Extended Baryon Oscillation Spectroscopic Survey and from the Second Phase of the Apache Point Observatory Galactic Evolution Experiment

Abolfathi

Aguado

Aguilar

et al. 2018

ApJS

Self Cite

947

466

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“…These include the aforementioned RXJ1713-39 and Vela Jr, as well as more typical thermal plasma dominated objects, such as G38.7+1.4 [58], G296.7-0.9 [59], G299.2-2.9 [60], and G308-1.4 [61]. It is quite likely that additional Galactic SNRs will be identified as part of the eROSITA all-sky survey [62], which will be about 30 times more sensitive than ROSAT.…”

Section: X-ray Identification Of Snrsmentioning

confidence: 99%

“…The number of Galactic SNRs should continue to grow with better all sky surveys at X-ray wavelengths, such as eROSITA [62], and emission line surveys, including the Isaac Newton Telescope Photometric Hα Survey IPHAS [80,81], its southern hemisphere VLT counterpart VPHAS [82], and the UKIRT wide field imaging survey of Fe+ (UWIFE) [83]. The follow-up from detections of γ-ray sources is also likely to continue to pay dividends in this regard.…”

Section: The Galaxymentioning

confidence: 99%

Galactic and Extragalactic Samples of Supernova Remnants: How They Are Identified and What They Tell Us

Long

2017

Handbook of Supernovae

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Supernova remnants (SNRs) arise from the interaction between the ejecta of a supernova (SN) explosion and the surrounding circumstellar and interstellar medium. Some SNRs, mostly nearby SNRs, can be studied in great detail. However, to understand SNRs as a whole, large samples of SNRs must be assembled and studied. Here, we describe the radio, optical, and X-ray techniques which have been used to identify and characterize almost 300 Galactic SNRs and more than 1200 extragalactic SNRs. We then discuss which types of SNRs are being found and which are not. We examine the degree to which the luminosity functions, surface-brightness distributions and multi-wavelength comparisons of the samples can be interpreted to determine the class properties of SNRs and describe efforts to establish the type of SN explosion associated with a SNR. We conclude that in order to better understand the class properties of SNRs, it is more important to study (and obtain additional data on) the SNRs in galaxies with extant samples at multiple wavelength bands than it is to obtain samples of SNRs in other galaxies.

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eROSITA on SRG

Cited by 32 publications

References 0 publications

Optical and X-ray transients from planet-star mergers

Optical and X-ray transients from planet-star mergers

The Fourteenth Data Release of the Sloan Digital Sky Survey: First Spectroscopic Data from the Extended Baryon Oscillation Spectroscopic Survey and from the Second Phase of the Apache Point Observatory Galactic Evolution Experiment

Galactic and Extragalactic Samples of Supernova Remnants: How They Are Identified and What They Tell Us

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