2012MNRAS.422.1674M

Query : 2012MNRAS.422.1674M

2012MNRAS.422.1674M - Mon. Not. R. Astron. Soc., 422, 1674-1689 (2012/May-2)

A review of source detection approaches in astronomical images.

MASIAS M., FREIXENET J., LLADO X. and PERACAULA M.

Abstract (from CDS):

Astronomical images provide information about the great variety of celestial objects in the Universe, the physical processes taking place in it, and the formation and evolution of the cosmos. Great efforts are made to automatically detect stellar bodies in images due to the large volumes of data and the fact that the intensity of many sources is at the detection level of the instrument. In this paper, we review the main approaches to automated source detection. The main features of the detection algorithms are analysed and the most important techniques are classified into different strategies according to their type of image transformation and their main detection principle; at the same time their strengths and weaknesses are highlighted. A qualitative and quantitative evaluation of the results of the most representative approaches is also presented.

Abstract Copyright: 2012 The Authors Monthly Notices of the Royal Astronomical Society2012 RAS

Journal keyword(s): methods: data analysis - techniques: image processing

Simbad objects: 1

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Number of rows : 1
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NAME Hubble Deep Field reg 12 36 49.5 +62 12 58           ~ 1967 1

Query : 2012MNRAS.422.1674M

Basic data :
NAME Hubble Deep Field -- Region defined in the Sky
Other object types: otypes_help 		reg ()
ICRS coord. (ep=J2000) : 		12 36 49.5 +62 12 58 [ ] D ~
FK4 coord. (ep=B1950 eq=1950) : 		12 34 35.5 +62 29 28 [ ]
Gal coord. (ep=J2000) : 		125.8875 +54.8282 [ ]
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Identifiers (7) :
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NAME HDF NAME HDFN NAME Hubble Deep Field NAME Northern Hubble Deep Field
NAME HDF-N NAME NHDF NAME Hubble Deep Field North

References (1967 between 1850 and 2026) (Total 1967)
Simbad bibliographic survey began in 1850 for stars (at least bright stars) and in 1983 for all other objects (outside the solar system).
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