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

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 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.
  • [Show abstract] [Hide abstract]
    ABSTRACT: Robotic telescopes usually run under the control of a scheduler, which provides high level control by selecting astronomical targets for observation. TUB_ITAK (Scienti�c and Technological Research Council of Turkey) National Observatory (TUG)-T60 Robotic Telescope is controlled by opensource OCAAS software, formally named Talon. This study introduces new software which was designed for Talon to catch GRB, GAIA and transient alerts. The new GRB software module (daemon process) alertd is running with all other modules of Talon such as telescoped; focus, dome; camerad and telrun. Maximum slew velocity and acceleration limits of the T60 telescope are enough fast for the GRB and transient observations
    Experimental Astronomy 02/2015; 1(1):234-240.
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    ABSTRACT: A statistical procedure for the analysis of time-frequency noise maps is presented and applied to LISA Pathfinder mission synthetic data. The procedure is based on the Kolmogorov-Smirnov like test that is applied to the analysis of time-frequency noise maps produced with the spectrogram technique. The influence of the finite size windowing on the statistic of the test is calculated with a Monte Carlo simulation for 4 different windows type. Such calculation demonstrate that the test statistic is modified by the correlations introduced in the spectrum by the finite size of the window and by the correlations between different time bins originated by overlapping between windowed segments. The application of the test procedure to LISA Pathfinder data demonstrates the test capability of detecting non-stationary features in a noise time series that is simulating low frequency non-stationary noise in the system.
    Experimental Astronomy 12/2014; DOI:10.1007/s10686-014-9432-z
  • Experimental Astronomy 12/2014; DOI:10.1007/s10686-014-9411-4
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    ABSTRACT: Stellar activity is the major astrophysical limiting factor for the study of planetary atmospheres. Its variability and spectral characteristics may affect the extraction of the planetary signal even for moderately active stars. A technique based on spectral change in the visible band was developed to estimate the effects in the infrared due to star activity. This method has been purposely developed for the EChO mission which had the crucial characteristics of monitoring simultaneously a broadband from visible to infrared. Thanks to this capability the optical spectrum, whose variations are mainly due to stellar activity, has been used as in an instantaneous calibrator to correct the infrared spectrum. The technique is based on principal component analysis which significantly reduces the dimensionality of the spectra. The method was tested on a set of simulations with realistic photon noise. It can be generalized to any chromatic variability effects provided that optical and infrared variations are correlated.
    Experimental Astronomy 12/2014; DOI:10.1007/s10686-014-9430-1
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    ABSTRACT: Stellar classification is an important topic in astronomical tasks such as the study of stellar populations. However, stellar classification of a region of the sky is a time-consuming process due to the large amount of objects present in an image. Therefore, automatic techniques to speed up the process are required. In this work, we study the application of a sparse representation and a dictionary learning for automatic spectral stellar classification. Our dataset consist of 529 calibrated stellar spectra of classes B to K, belonging to the Pulkovo Spectrophotometric catalog, in the 3400−5500Å range. These stellar spectra are used for both training and testing of the proposed methodology. The sparse technique is applied by using the greedy algorithm OMP (Orthogonal Matching Pursuit) for finding an approximated solution, and the K-SVD (K-Singular Value Decomposition) for the dictionary learning step. Thus, sparse classification is based on the recognition of the common characteristics of a particular stellar type through the construction of a trained basis. In this work, we propose a classification criterion that evaluates the results of the sparse representation techniques and determines the final classification of the spectra. This methodology demonstrates its ability to achieve levels of classification comparable with automatic methodologies previously reported such as the Maximum Correlation Coefficient (MCC) and Artificial Neural Networks (ANN).
    Experimental Astronomy 08/2014; 38(1-2). DOI:10.1007/s10686-014-9413-2