Experimental Astronomy Journal Impact Factor & Information

Publisher: Springer Verlag

Journal description

Many new instruments for observing astronomical objects at a variety of wavelengths have been and are continually being developed. Furthermore a vast amount of effort is being put into the development of new techniques for data analysis in order to cope with great streams of data collected by these instruments. Experimental Astronomy acts as a medium for the publication of papers on the instrumentation and data handling necessary for the conduct of astronomy at all wavelength fields. Experimental Astronomy publishes full-length articles research letters and reviews on developments in detection techniques instruments and data analysis and image processing techniques. Occasional special issues are published giving an in-depth presentation of the instrumentation and/or analysis connected with specific projects such as satellite experiments or ground-based telescopes or of specialized techniques.

Current impact factor: 2.66

Impact Factor Rankings

2015 Impact Factor Available summer 2015
2013 / 2014 Impact Factor 2.663
2012 Impact Factor 2.969
2011 Impact Factor 1.818
2010 Impact Factor 2.14
2009 Impact Factor 5.444
2008 Impact Factor 2.083
2007 Impact Factor 0.543
2006 Impact Factor 0.184
2005 Impact Factor 0.296
2004 Impact Factor 0.6
2003 Impact Factor 0.556
2002 Impact Factor 0.73
2001 Impact Factor 0.489
2000 Impact Factor 0.8
1999 Impact Factor 0.397

Impact factor over time

Impact factor
Year

Additional details

5-year impact 2.32
Cited half-life 3.50
Immediacy index 0.60
Eigenfactor 0.00
Article influence 0.74
Website Experimental Astronomy website
Other titles Experimental astronomy
ISSN 0922-6435
OCLC 20297628
Material type Periodical, Internet resource
Document type Journal / Magazine / Newspaper, Internet Resource

Publisher details

Springer Verlag

  • Pre-print
    • Author can archive a pre-print version
  • Post-print
    • Author can archive a post-print version
  • Conditions
    • Author's pre-print on pre-print servers such as arXiv.org
    • Author's post-print on author's personal website immediately
    • Author's post-print on any open access repository after 12 months after publication
    • Publisher's version/PDF cannot be used
    • Published source must be acknowledged
    • Must link to publisher version
    • Set phrase to accompany link to published version (see policy)
    • Articles in some journals can be made Open Access on payment of additional charge
  • Classification
    ​ green

Publications in this journal

  • [Show abstract] [Hide abstract]
    ABSTRACT: The Cherenkov Telescope Array (CTA) is the next generation very high energy gamma-ray observatory. Three classes of telescopes, of large, medium and small sizes are designed and developed for the observatory. The single-mirror option for the small-size telescopes (SST-1M), of 4 m diameter, dedicated to the observations of the highest energy gamma-rays above several TeV, consists of 18 hexagonal mirror facets of 78 cm flat-to-flat. The goal of the work described in this paper is the investigation of a surface shape quality of the mirror facets of the SST-1M CTA telescope. The mirrors measured are made of composite materials formed using sheet moulding compound (SMC) technology. This solution is being developed as an alternative to glass mirrors, to minimize the production cost of hundreds of mirrors for the network of telescopes, while retaining the optical quality of the telescope. To evaluate the progress of design, production technology and the mirrors’ functionality in operating conditions, the three-dimensional (3D) Digital Image Correlation (DIC) method was selected and implemented for testing selected mirrors. The method and measurement procedure are described. The novel measurement approach based on 3D DIC has been proven to be well suited to the investigation of the mirrors’ behavior with temperature, producing the necessary accuracy.
    Experimental Astronomy 06/2015; DOI:10.1007/s10686-015-9455-0
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    ABSTRACT: We are conducting tests of optical and electronics components of JEMEUSO at the Telescope Array site in Utah with a ground-based “EUSO-TA” detector. The tests will include an engineering validation of the detector, cross-calibration of EUSO-TA with the TA fluorescence detector and observations of air shower events. Also, the proximity of the TA’s Electron Light Source will allow for convenient use of this calibration device. In this paper, we report initial results obtained with the EUSO-TA telescope.
    Experimental Astronomy 05/2015; DOI:10.1007/s10686-015-9441-6
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    ABSTRACT: The observational facility of 1.5m Russian-Turkish Telescope RTT150 including highly precise positional measurements, photometry and spectroscopy has been broadened with polarimetry. New device was made on the base of Double Wedged Wollaston of well known dual-beam technique. The optic unit was integrated to TFOSC system which is a main telescope detector. Newly designed TFOSC-WP polarimeter capability was investigated by observations of set non-polarized and strongly polarized stars. The recommended working area with linear behavior of instrumental intrinsic polarization is determined as 1 by 5 arcmin in equatorial coordinate system. The instrumental systematic error of polarization degree is 0.2% and position angle is 1.9 degree. The polarimeter integration to the RTT150 has increased its capabilities in ground-based observational support of present and future astrophysical space missions such as GAIA and SRG, which is one of a primary goal of the telescope.
    Experimental Astronomy 04/2015; 1(1):1.
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    ABSTRACT: Searching for sources of electromagnetic emission in spectral-line radio astronomy interferometric data is a computationally intensive process. Parallel programming techniques and High Performance Computing hardware may be used to improve the computational performance of a source finding program. However, it is desirable to further reduce the processing time of source finding in order to decrease the computational resources required for the task. GPU acceleration is a method that may achieve significant increases in performance for some source finding algorithms, particularly for filtering image data. This work considers the application of GPU acceleration to the task of source finding and the techniques used to achieve the best performance, such as memory management. We also examine the changes in performance, where the algorithms that were GPU accelerated achieved a speedup of around 3.2 times the 12 core per node CPU-only performance, while the program as a whole experienced a speedup of 2.0 times.
    Experimental Astronomy 03/2015; 39(1):95-117. DOI:10.1007/s10686-015-9445-2
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    ABSTRACT: Recent lossless still image compression formats are powerful tools for compression of all kind of common images (pictures, text, schemes, etc.). Generally, the performance of a compression algorithm depends on its ability to anticipate the image function of the processed image. In other words, a compression algorithm to be successful, it has to take perfectly the advantage of coded image properties. Astronomical data form a special class of images and they have, among general image properties, also some specific characteristics which are unique. If a new coder is able to correctly use the knowledge of these special properties it should lead to its superior performance on this specific class of images at least in terms of the compression ratio. In this work, the novel lossless astronomical image data compression method will be presented. The achievable compression ratio of this new coder will be compared to theoretical lossless compression limit and also to the recent compression standards of the astronomy and general multimedia.
    Experimental Astronomy 01/2015; DOI:10.1007/s10686-015-9460-3
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    ABSTRACT: Time Projection Chamber (TPC) based X-ray polarimeters using Gas Electron Multiplier (GEM) are currently being developed to make sensitive measurement of polarization in 2-10 keV energy range. The emission direction of the photoelectron ejected via photoelectric effect carries the information of the polarization of the incident X-ray photon. Performance of a gas based polarimeter is affected by the operating drift parameters such as gas pressure, drift field and drift-gap. We present simulation studies carried out in order to understand the effect of these operating parameters on the modulation factor of a TPC polarimeter. Models of Garfield are used to study photoelectron interaction in gas and drift of electron cloud towards GEM. Our study is aimed at achieving higher modulation factors by optimizing drift parameters. Study has shown that Ne/DME (50/50) at lower pressure and drift field can lead to desired performance of a TPC polarimeter.
    Experimental Astronomy 01/2015; DOI:10.1007/s10686-015-9449-y
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    ABSTRACT: We report on the progress in the realization of an electronic / optical simulator for space based, long arm interferometry and its application to the eLISA mission. The goal of this work is to generate realistic optics and electronics signals, especially simulating realistic propagation delays. The first measurements to characterize the simulator are also presented. With the present configuration, noise reduction factors of 5×107 for optical beat notes and 109 for RF beat notes have been achieved using the Time Delay Interferometry algorithm. The principle of the experiment has been validated and further work is ongoing to identify the residual noise sources and optimize the apparatus.
    Experimental Astronomy 01/2015; DOI:10.1007/s10686-015-9448-z