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

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    ABSTRACT: This paper describes an alternative approach for generating pointing models for telescopes equipped with serial kinematics, esp. equatorial or alt-az mounts. Our model construction does not exploit any assumption for the underlying physical constraints of the mount, however, one can assign various effects to the respective components of the equations. In order to recover the pointing model parameters, classical linear least squares fitting procedures can be applied. This parameterization also lacks any kind of parametric singularity. We demonstrate the efficiency of this type of model on real measurements with meter-class telescopes where the results provide a root mean square accuracy of 1.5-2 arcseconds.
    Experimental Astronomy 07/2015; DOI:10.1007/s10686-015-9472-z
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    ABSTRACT: The JEM-EUSO telescope will be, after calibration, a very accurate instrument which yields the number of received photons from the number of measured photo-electrons. The project is in phase A (demonstration of the concept) including already operating prototype instruments, i.e. many parts of the instrument have been constructed and tested. Calibration is a crucial part of the instrument and its use. The focal surface (FS) of the JEM-EUSO telescope will consist of about 5000 photo-multiplier tubes (PMTs), which have to be well calibrated to reach the required accuracy in reconstructing the air-shower parameters. The optics system consists of 3 plastic Fresnel (double-sided) lenses of 2.5 m diameter. The aim of the calibration system is to measure the efficiencies (transmittances) of the optics and absolute efficiencies of the entire focal surface detector. The system consists of 3 main components: (i) Pre-flight calibration devices on ground, where the efficiency and gain of the PMTs will be measured absolutely and also the transmittance of the optics will be. (ii) On-board relative calibration system applying two methods: a) operating during the day when the JEM-EUSO lid will be closed with small light sources on board. b) operating during the night, together with data taking: the monitoring of the background rate over identical sites. (iii) Absolute in-flight calibration, again, applying two methods: a) measurement of the moon light, reflected on high altitude, high albedo clouds. b) measurements of calibrated flashes and tracks produced by the Global Light System (GLS). Some details of each calibration method will be described in this paper.
    Experimental Astronomy 07/2015; DOI:10.1007/s10686-015-9453-2
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    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: 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 06/2015; 39(2). 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 06/2015; 39(2). DOI:10.1007/s10686-015-9448-z
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    ABSTRACT: The development of a spectrometer is being carried out in the Near-Infrared (NIR) wavelength range of 1.0-1.7 μm using an Acousto-Optic Tunable Filter (AOTF). The AOTF is based on Tellurium-di-oxide (TeO2) crystal that acts as a dispersing medium and is driven by an external Radio Frequency (RF) signal. The characterization of AOTF is based on the wavelength-tuning frequency relation, spectral bandwidth as a function of wavelength through AOTF Transfer Function (Sinc2), their dependence on the angular aperture and the peak diffraction efficiency of the AOTF. To demonstrate the full scanning capability of the AOTF in the wavelength range of 1.0-1.7 μm, Argon (Ar) and Krypton (Kr) line sources are used. The overall functionality of the spectrometer using the wavelength selection capability of AOTF is demonstrated by scanning the RF in the NIR band to detect water vapour absorption signatures in the Earth's atmosphere. This spectrometer is being designed for future interplanetary missions of ISRO with an aim to study the atmospheres of planets such as Mars or Venus.
    Experimental Astronomy 06/2015; 39(2). DOI:10.1007/s10686-015-9461-2
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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 05/2015; DOI:10.1007/s10686-015-9460-3
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    ABSTRACT: During certain times of the year at middle and low latitudes, winds in the upper stratosphere move in nearly the opposite direction than the wind in the lower stratosphere. Here we present a method for maintaining a high-altitude balloon platform in near station-keeping mode that utilizes this stratospheric wind shear. The proposed method places a balloon-borne science platform high in the stratosphere connected by a lightweight, high-strength tether to a tug vehicle located in the lower or middle stratosphere. Using aerodynamic control surfaces, wind-induced aerodynamic forces on the tug can be manipulated to counter the wind drag acting on the higher altitude science vehicle, thus controlling the upper vehicle’s geographic location. We describe the general framework of this station-keeping method, some important properties required for the upper stratospheric science payload and lower tug platforms, and compare this station-keeping approach with the capabilities of a high altitude airship and conventional tethered aerostat approaches. We conclude by discussing the advantages of such a platform for a variety of missions with emphasis on astrophysical research.
    Experimental Astronomy 05/2015; DOI:10.1007/s10686-015-9459-9
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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: 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