SearcharxivSearch

arXiv · 0810.2693

The Gas Pixel Detector as an X-ray photoelectric polarimeter with a large field of view

Abstract

The Gas Pixel Detector (GPD) is a new generation device which, thanks to its 50 um pixels, is capable of imaging the photoelectrons tracks produced by photoelectric absorption in a gas. Since the direction of emission of the photoelectrons is strongly correlated with the direction of polarization of the absorbed photons, this device has been proposed as a polarimeter for the study of astrophysical sources, with a sensitivity far higher than the instruments flown to date. The GPD has been always regarded as a focal plane instrument and then it has been proposed to be included on the next generation space-borne missions together with a grazing incidence optics. Instead in this paper we explore the feasibility of a new kind of application of the GPD and of the photoelectric polarimeters in general, i.e. an instrument with a large field of view. By means of an analytical treatment and measurements, we verify if it is possible to preserve the sensitivity to the polarization for inclined beams, opening the way for the measurement of X-ray polarization for transient astrophysical sources. While severe systematic effects arise for inclination greater than about 20 degrees, methods and algorithms to control them are discussed.

Explore related subjects

Keep this discovery

BibTeXRIS

Fabio Muleri, Paolo Soffitta, Ronaldo Bellazzini, Alessandro Brez, Enrico Costa, Sergio Fabiani, Massimo Frutti, Massimo Minuti, Maria Barbara Negri, Michele Pinchera, Alda Rubini, Gloria Spandre. 2008-10-15. The Gas Pixel Detector as an X-ray photoelectric polarimeter with a large field of view. https://doi.org/10.1117/12.789621

Cite the original work for its findings. Save a collection to share your selection of sources.

KEEP EXPLORING

Related papers

Circumstellar water vapour in M-type AGB stars: Radiative transfer models, abundances and predictions for HIFI

Aims: By performing a detailed radiative transfer analysis, we determine fractional abundances of circumstellar H2O in the envelopes around six M-type asymptotic giant branch stars. The models are also used to predict H2O spectral line emission for the upcoming Herschel/HIFI mission. Methods: We use Infrared space observatory long wavelength spectrometer spectra to constrain the circumstellar fractional abundance distribution of ortho-H2O, using a non-local thermal equilibrium, and non-local, radiative transfer code based on the accelerated lambda iteration formalism. The mass-loss rates and kinetic temperature structures for the sample stars are determined through radiative transfer modelling of CO line emission based on the Monte-Carlo method. The density and temperature profiles of the circumstellar dust grains are determined through spectral energy distribution modelling using the publicly available code Dusty. Results: The determined ortho-H2O abundances lie between 1e-4 and 1.5e-3 relative to H2, with the exception of WX Psc, which has a much lower estimated ortho-H2O abundance of only 2e-6, possibly indicating H_2O adsorption onto dust grains or recent mass-loss-rate modulations. The estimated abundances are uncertain by, at best, a factor of a few. Conclusions: The high water abundance found for the majority of the sources suggests that either the `normal' chemical processes are very effective in producing H2O, or else non-local thermal equilibrium atmospheric chemistry, grain surface reactions, or a release of H_2O (e.g. from icy bodies like Kuiper belt objects) play a role. We provide predictions for ortho-H2O lines in the spectral window of Herschel/HIFI.

astro-ph

CMB Anisotropies and Inflation from Non-Standard Spinors

The apparent alignment of the cosmic microwave background multipoles on large scales challenges the standard cosmological model. Scalar field inflation is isotropic and cannot account for the observed alignment. We explore the imprints, a non-standard spinor driven inflation would leave on the cosmic microwave background anisotropies. We show it is natural to expect an anisotropic inflationary expansion of the Universe which has the effect of suppressing the low multipole amplitude of the primordial power spectrum, while at the same time to provide the usual inflationary features.

astro-ph