A Method for Optimal Image Subtraction

Example of subtracted image. The two bottom figures of the panel are the original images...

A Method for Optimal Image Subtraction

Noise in the subtracted image. The image on the left is the subtracted image normalized ...

A Method for Optimal Image Subtraction

Examples of bright giant light curves. The x‐axes are days, the y‐axes are percentage va...

A Method for Optimal Image Subtraction

Periodic variables. The x‐axes represent the phase, the y‐axes are percentage variation ...

The Temperature Structure of 30 Nearby ...

Comparison of our temperatures with those from Einstein MPC, EXOSAT, and Ginga (David et...

The Temperature Structure of 30 Nearby ...

Cluster temperature maps. Contours show ROSAT PSPC brightness; gray scale shows ASCA tem...

The Temperature Structure of 30 Nearby ...

Cluster temperature maps. Contours show ROSAT PSPC brightness; gray scale shows ASCA tem...

The Temperature Structure of 30 Nearby ...

Cluster temperature maps. Contours show ROSAT PSPC brightness; gray scale shows ASCA tem...

The Temperature Structure of 30 Nearby ...

Temperature and specific entropy maps of A3395 (see text). Left panels are similar to Fi...

The Temperature Structure of 30 Nearby ...

Radial projected temperature profiles. Crosses are centered on the emission‐weighted rad...

The Temperature Structure of 30 Nearby ...

Radial projected temperature profiles. Crosses are centered on the emission‐weighted rad...

The Temperature Structure of 30 Nearby ...

Radial projected temperature profiles. Crosses are centered on the emission‐weighted rad...

The Temperature Structure of 30 Nearby ...

Normalized temperature profiles of 19 relatively symmetric clusters, plotted against rad...

The Temperature Structure of 30 Nearby ...

Normalized temperature profiles of several cluster subsets. Error bars are omitted for c...

The Temperature Structure of 30 Nearby ...

Normalized profiles of symmetric clusters (those shown in Fig. 5, without AWM 7 and A216...

The Temperature Structure of 30 Nearby ...

Temperature profiles from cluster simulations overlaid on our results. Light‐shaded band...

Neutrinos and Supermassive Stars: Prosp...

Neutrino production distribution inside the homologous core (unnormalized): the distribu...

Neutrinos and Supermassive Stars: Prosp...

Time evolution of the neutrino luminosity according to eq. (17), for ...

Neutrinos and Supermassive Stars: Prosp...

Solid lines: Spectra of ﹩\nu _{e}\,\overline{\nu }_{e}﹩ (upper) and ...

Neutrinos and Supermassive Stars: Prosp...

Event rates from the supermassive star neutrino background in several new‐generation det...

Detection of an Iron K Emission Line fr...

ASCA (a) SIS and (b) GIS spectra of NGC 4579. The best‐fit model consists of an R‐S ther...

Detection of an Iron K Emission Line fr...

ASCA (a) SIS and (b) GIS spectra of NGC 4579. The best‐fit model consists of an R‐S ther...

Detection of an Iron K Emission Line fr...

Data/model ratio for the best‐fit continuum model around an iron K emission line. The cr...

Detection of an Iron K Emission Line fr...

Confidence contours for the line energy and intensity. The energy scale is redshift corr...

Detection of an Iron K Emission Line fr...

Confidence contours for the line width (Gaussian σ) and intensity. The contours correspo...

A New Instability of Accretion Disks ar...

Geometry of the blob–magnetic field interaction. The two panels correspond to different ...

A New Instability of Accretion Disks ar...

Geometry of the reference systems of § 2.1. The K frame is inertial; its z axis is along...

Joule Heating and the Thermal Evolution...

Time dependence of the rate of Joule heating integrated over the star volume and normali...

Joule Heating and the Thermal Evolution...

Thermal evolution of the FP model with and without Joule heating. Curve 1: Be = 1.5 × 10...

Joule Heating and the Thermal Evolution...

Thermal evolution of the PS model with and without Joule heating. Curve 1: Be = 1.5 × 10...