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  • Proprietario: Marco
  • LRGB composition of NGC 884 & NGC 869 in Perseo, also known as "The Double Cluster" or H and Chi Persei

    Noticeable facts:
    * The distances from the earth of NGC 884 and NGC 869 are rispectively 7600 and 6800 light-years so they are also close in this arm of the Milky Way
    * Both clusters are realtively young and most of their members are B0 class stars. The few deep-red stars in the field create a spetacular view for both visual observers and astroimagers.
    * Despite their significant overall brightness (they are visible with the naked eyes), they are not included in the Messier catalog.

    Technical data:
    RC-14” F/8,4
    SBIG STX 16803
    LRGB Filters Baader LRGB
    Mount: Gemini Telescope Design - MOFOD Fork Mount
    L-R:G:B 45-15:15:15 (minutes)
    SQM: 21.35
    Seeing: 1.6"-1.8"

    Authors:
    Acquisition: F. Antonucci - M. Angelini - F. Tagliani
    Image Processing: Francesco Antonucci

    Parco Astronomico del Brallo

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NGC 884 & NGC 869: The Double Cluster in Perseo

NGC 884 & NGC 869: The Double Cluster in Perseo More
NGC 884 & NGC 869: The Double Cluster in Perseo LRGB composition of NGC 884 & NGC 869 in Perseo, also known as "The Double Cluster" or H and Chi Persei

Noticeable facts:
* The distances from the earth of NGC 884 and NGC 869 are rispectively 7600 and 6800 light-years so they are also close in this arm of the Milky Way
* Both clusters are realtively young and most of their members are B0 class stars. The few deep-red stars in the field create a spetacular view for both visual observers and astroimagers.
* Despite their significant overall brightness (they are visible with the naked eyes), they are not included in the Messier catalog.

Technical data:
RC-14” F/8,4
SBIG STX 16803
LRGB Filters Baader LRGB
Mount: Gemini Telescope Design - MOFOD Fork Mount
L-R:G:B 45-15:15:15 (minutes)
SQM: 21.35
Seeing: 1.6"-1.8"

Authors:
Acquisition: F. Antonucci - M. Angelini - F. Tagliani
Image Processing: Francesco Antonucci

Parco Astronomico del Brallo

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