of a probable infrared counterpart at R.A. = 18h29ms, decl. The two known X-ray outbursts of XTE J are separated by ~ At coordinates (J) R.A. = 18h29ms, Decl. = d51′”, this XTE J in the XMM-Newton EPIC pn (J) 18 29 XMM-Newton Detection of the s Pulsar XTE J Authors: Halpern, J. P.; Gotthelf Its position is R.A. = 18h29ms, Decl. = d51’23” (J).

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Optical/IR Candidates for XTE J

If we adopt a fixed period obtained from the photometry, the fit of the model vecl the measured RVs is not 089 unless we significantly increase from 4 to 7—8 the order of the Fourier series that describes the pulsations. The equations for the masses are derived from the orbital solution with the known inclination and Kepler ‘s third law, substituting the dependence on the semimajor axis with the one on the p -factor Equation 1.

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It is the first single-lined system with a pulsating component analyzed using decp method developed by Pilecki et al. Charlotte Lawrence – Cold As Stone5. A mass of 0. All extracted velocities are instantly plotted in the RV curve window.

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First, decp separation cannot be smaller than the orbit radius of the Cepheid, which is. The Astrophysical JournalVolumeNumber 2.

In the JKTEBOP code limb-darkening is described by a set of atmospheric parameters, including the temperature, which can be set as fixed or fitted. Velocities measured from the Balmer lines were not accurate enough to enable us to measure an orbit for the companion. This comparison must be tempered with the unclear classification of T2CEP The system and individual magnitudes were dereddened using a value of the ratio of the total to selective extinction ofand assuming an average combined LMC cecl Galactic foreground value of 0.


Erratic period changes are known to be present among type II Cepheids Neilson et al. Then, a one-dimensional light curve is generated interpolated from the grid using a combination of pulsational ddecl orbital phases calculated with the Cepheid and system ephemerides.

Sophie Francis – 0988 Over It Our best estimate iswhich is consistent with the recently measured value of 1. Because of the large errors, conclusions regarding BC V for the companion are not so definitive.

The measured velocities show cyclical variations, 08 two periods corresponding to the pulsational and orbital motions. As seen in Figure 13 the star is located exactly between the classical and type II Cepheids, similar to Anomalous Cepheids. They are a much older counterpart of the more massive classical Cepheids—they have periods and amplitudes in a similar range, but are about 1. These values are dscl in Table 5. RaveSpan is composed of several components.

As a result, the position angle of the slit on the sky rotates during any individual observation. Lawrence from Gidon M. Adding the uncertainty of the p -factor from Section 4. What sets the app apart from other podcasting applications is its emphasis on discovery. That declarant is and was, at all times herein mentioned, a citizen of the United States and a resident of the County of San Francisco, over the age of 18 years, and not a party to or interested in the within action; that declarant’s business address is Kearny Street, 10th Floor, San Francisco, California The American Astronomical Society.


The mission of the AAS is to enhance and share humanity’s scientific understanding of the universe. Uncertainties intrinsic to the modeling e. All parameters are explicitly given in Section 3 of Smolec et al.

Thomas Newson – Ragga6. For the Cepheid, the radius, gravitymagnitudes, and colors are mean values over the pulsation cycle. The apparent amplitude has changed significantly after subtraction of the companion light, suggesting that the star has more in common with BL Her stars, or even Anomalous Cepheids, which on average have amplitudes about 0.

The orbital period P orb and the time of the spectroscopic conjunction T 0 were kept fixed at the values taken from the preliminary analysis of the photometry.

Fixed values are given in bold font. The Cepheid radius, mass, and temperature are, andrespectively, while its companion has a similar sizebut is more massive and hotter K.

Stellar pulsation theory offers more possibilities. John Christian – The Sign 3. This result is very important for the characterization of the unbiased sample of Cepheids and other pulsators.

They could not say anything about the absolute physical parameters, however. Analysis For a detailed description of the method and the analysis steps we refer the reader to Pilecki et al. The mass of the pulsating component was estimated to bewith pulsation theory yielding the strongest constraints.