Interactive Analysis with EXSAS

Zimmermann, H. U.; Belloni, T.; Boese, G.; Izzo, C.; Kahabka, P.; Schwentker, O.

doi:10.1007/978-1-4615-3388-7_16

Cited by 65 publications

(76 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Probabilities P , are related to maximum likelihood values L, by the relation P = 1 − e −L . Thus a likelihood L of 10 corresponds to a Gaussian significance of 4.0σ (Cruddace et al 1988;Zimmermann et al 1994).…”

Section: Pspcmentioning

confidence: 99%

X-ray emission from the Sculptor galaxy NGC 300

Read

Pietsch

2001

A&A

View full text Add to dashboard Cite

Abstract. We report here the results of a full analysis of all the ROSAT PSPC spectral imaging observations and all the ROSAT HRI high resolution imaging observations of the very nearby (D = 2.1 Mpc) Sculptor galaxy, NGC 300. Many point sources are detected within the field, several of them showing evidence for variability, and we present full source lists detailing their X-ray properties, and attempt to classify them on the basis of their temporal, spectral and multi-wavelength characteristics. A black hole X-ray binary candidate, a supersoft source and several supernova remnants and H ii regions are detected in X-rays, as is unresolved, possibly diffuse emission, accounting for perhaps ∼20% of the total NGC 300 X-ray (0.1−2.4 keV) luminosity (5.8 × 10 38 erg s −1 ). We compare the X-ray source luminosity distribution of NGC 300 with that of other nearby galaxies, and we also compare NGC 300 with its Sculptor neighbours, concluding that it is a quite an unremarkable system, showing no unusual X-ray (or other multi-wavelength) properties. It may be one of the best examples of a completely typical normal quiescent late-type spiral galaxy.

show abstract

Section: Pspcmentioning

confidence: 99%

X-ray emission from the Sculptor galaxy NGC 300

Read

Pietsch

2001

A&A

View full text Add to dashboard Cite

show abstract

“…The total integration time of 35 ks (9.6 h) consisted of nine observation intervals. The individual light curves were extracted with standard tasks of the exsas/Midas (Zimmermann et al 1993) software packages, corrected to the barycenter, and combined to a common light curve profile. (Schuh et al 2003) and ESO-Midas routines.…”

Section: Introductionmentioning

confidence: 99%

X-ray spectroscopy and photometry of the long-period polar AI Trianguli with XMM-Newton

Traulsen

Reinsch

Schwarz

et al. 2010

A&A

View full text Add to dashboard Cite

Context. The energy balance of cataclysmic variables with strong magnetic fields is a central subject in understanding accretion processes on magnetic white dwarfs. With XMM-Newton, we perform a spectroscopic and photometric study of soft X-ray selected polars during their high states of accretion. Aims. On the basis of X-ray and optical observations of the magnetic cataclysmic variable AI Tri, we derive the properties of the spectral components, their flux contributions, and the physical structure of the accretion region in soft polars.Methods. We use multi-temperature approaches in our xspec modeling of the X-ray spectra to describe the physical conditions and the structures of the post-shock accretion flow and the accretion spot on the white-dwarf surface. In addition, we investigate the accretion geometry of the system by completing a timing analysis of the photometric data. Results. Flaring soft X-ray emission from the heated surface of the white dwarf dominates the X-ray flux during roughly 70% of the binary cycle. This component deviates from a single black body and can be described by a superimposition of mildly absorbed black bodies with a Gaussian temperature distribution between kT bb,low := 2 eV and kT bb,high = 43.9 +3.3 −3.2 eV, and N H,ISM = 1.5 +0.8 −0.7 ×10 20 cm −2 . In addition, weaker hard X-ray emission is visible nearly all the time. The spectrum from the cooling post-shock accretion flow is most closely fitted by a combination of thermal plasma mekal models with temperature profiles adapted from prior stationary two-fluid hydrodynamic calculations. The resulting plasma temperatures lie between kT MEKAL,low = 0.8 +0.4 −0.2 keV and kT MEKAL,high = 20.0 +9.9 −6.1 keV; additional intrinsic, partial-covering absorption is on the order of N H,int = 3.3 +2.5 −1.2 × 10 23 cm −2 . The soft X-ray light curves show a dip during the bright phase, which can be interpreted as self-absorption in the accretion stream. Phase-resolved spectral modeling supports the picture of one-pole accretion and self-eclipse. One of the optical light curves corresponds to an irregular mode of accretion. During a short XMM-Newton observation at the same epoch, the X-ray emission of the system is clearly dominated by the soft component.

show abstract

“…V1334 Tau was previously identified as a Weak-lined T Tauri Star (WTTS) with a K1 spectral type by Wichmann et al (1996) using observations from the ROSAT All-Sky-Survey (Zimmermann et al 1993) combined with optical spectra. More recently, V1334 Tau was reclassified as a G2 star (Nguyen et al 2012 , which is in agreement with the known motion of the Taurus-Aurigae association (μ α =7.2 and μ δ =−20.9, Bertout & Genova 2006).…”

Section: The V1334 Tau Systemmentioning

confidence: 99%

The Mysterious Dimmings of the T Tauri Star V1334 Tau

Rodriguez

Zhou

Cargile

et al. 2017

ApJ

View full text Add to dashboard Cite

We present the discovery of two extended ∼0.12 mag dimming events of the weak-lined T Tauri star V1334. The start of the first event was missed but came to an end in late 2003, and the second began in 2009 February, and continues as of 2016 November. Since the egress of the current event has not yet been observed, it suggests a period of >13 years if this event is periodic. Spectroscopic observations suggest the presence of a small inner disk, although the spectral energy distribution shows no infrared excess. We explore the possibility that the dimming events are caused by an orbiting body (e.g., a disk warp or dust trap), enhanced disk winds, hydrodynamical fluctuations of the inner disk, or a significant increase in the magnetic field flux at the surface of the star. We also find a ∼0.32 day periodic photometric signal that persists throughout the 2009 dimming which appears to not be due to ellipsoidal variations from a close stellar companion. High-precision photometric observations of V1334 Tau during K2 campaign 13, combined with simultaneous photometric and spectroscopic observations from the ground, will provide crucial information about the photometric variability and its origin.

show abstract

Interactive Analysis with EXSAS

Cited by 65 publications

References 0 publications

X-ray emission from the Sculptor galaxy NGC 300

X-ray emission from the Sculptor galaxy NGC 300

X-ray spectroscopy and photometry of the long-period polar AI Trianguli with XMM-Newton

The Mysterious Dimmings of the T Tauri Star V1334 Tau

Contact Info

Product

Resources

About