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: 1.99

Impact Factor Rankings

2015 Impact Factor Available summer 2016
2014 Impact Factor 1.99
2013 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

Additional details

5-year impact 1.52
Cited half-life 3.60
Immediacy index 0.39
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: Polarised light from astronomical targets can yield a wealth of information about their source radiation mechanisms, and about the geometry of the scattered light regions. Optical observations, of both the linear and circular polarisation components, have been impeded due to non-optimised instrumentation. The need for suitable observing conditions and the availability of luminous targets are also limiting factors. GASP uses division of amplitude polarimeter (DOAP) (Compain and Drevillon) to measure the four components of the Stokes vector simultaneously, which eliminates the constraints placed upon the need for moving parts during observation, and offers a real-time complete measurement of polarisation. Results from the GASP calibration are presented in this work for both a 1D detector system, and a pixel-by-pixel analysis on a 2D detector system. Following Compain et al. we use the Eigenvalue Calibration Method (ECM) to measure the polarimetric limitations of the instrument for each of the two systems. Consequently, the ECM is able to compensate for systematic errors introduced by the calibration optics, and it also accounts for all optical elements of the polarimeter in the output. Initial laboratory results of the ECM are presented, using APD detectors, where errors of 0.2% and 0.1{\deg} were measured for the degree of linear polarisation and polarisation angle respectively. Channel-to-channel image registration is an important aspect of 2-D polarimetry. We present our calibration results of the measured Mueller matrix of each sample, used by the ECM. A set of Zenith flat-field images were recorded during an observing campaign at the Palomar 200 inch telescope in November 2012. From these we show the polarimetric errors from the spatial polarimetry indicating both the stability and absolute accuracy of GASP.
    Experimental Astronomy 08/2015; DOI:10.1007/s10686-015-9464-z
  • Experimental Astronomy 08/2015; DOI:10.1007/s10686-015-9473-y
  • J. H. Adams · S. Ahmad · J. -N. Albert · D. Allard · L. Anchordoqui · V. Andreev · A. Anzalone · Y. Arai · K. Asano · M. Ave Pernas · [...] · Y. Yamamoto · J. Yang · H. Yano · I. V. Yashin · D. Yonetoku · K. Yoshida · S. Yoshida · R. Young · M. Yu. Zotov · A. Zuccaro Marchi
    Experimental Astronomy 07/2015; DOI:10.1007/s10686-015-9470-1
  • Source
    [Show abstract] [Hide abstract]
    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
  • Experimental Astronomy 07/2015; DOI:10.1007/s10686-015-9469-7
  • J. H. Adams · S. Ahmad · J. -N. Albert · D. Allard · L. Anchordoqui · V. Andreev · A. Anzalone · Y. Arai · K. Asano · M. Ave Pernas · [...] · Y. Yamamoto · J. Yang · H. Yano · I. V. Yashin · D. Yonetoku · K. Yoshida · S. Yoshida · R. Young · M. Yu. Zotov · A. Zuccaro Marchi
    Experimental Astronomy 07/2015; DOI:10.1007/s10686-014-9420-3
  • [Show abstract] [Hide abstract]
    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
  • [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
  • [Show abstract] [Hide abstract]
    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
  • [Show abstract] [Hide abstract]
    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
  • [Show abstract] [Hide abstract]
    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
  • [Show abstract] [Hide abstract]
    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