Hemisphere:  Northern  ·  Constellation: Perseus (Per)  ·  Contains:  38 omi Per  ·  42 n Per  ·  44 zet Per  ·  Atik  ·  B1  ·  B2  ·  B203  ·  B205  ·  B3  ·  B4  ·  B5  ·  IC 348  ·  NGC 1333  ·  NGC 1465  ·  PGC 13025  ·  PGC 13026  ·  PGC 13987  ·  PGC 14033  ·  PGC 14034  ·  PGC 1921731  ·  PGC 1926831  ·  PGC 1930564  ·  PGC 1931819  ·  PGC 1933873  ·  PGC 1963647  ·  PGC 1964449  ·  PGC 1966181  ·  PGC 1966463  ·  PGC 1967364  ·  PGC 1968130  ·  And 63 more.

Image of the day 04/07/2021

Getting plate-solving status, please wait...
    Perseus molecular cloud, 



    
        

            Steed Yu
    Powered byPixInsight

    Perseus molecular cloud

    Image of the day 04/07/2021

    Getting plate-solving status, please wait...
      Perseus molecular cloud, 



    
        

            Steed Yu
      Powered byPixInsight

      Perseus molecular cloud

      Acquisition details

      Dates:
      Oct. 18, 2020 ·  Oct. 19, 2020 ·  Oct. 20, 2020 ·  Oct. 23, 2020 ·  Oct. 24, 2020 ·  Oct. 27, 2020 ·  Oct. 28, 2020 ·  Oct. 30, 2020 ·  Nov. 8, 2020 ·  Nov. 9, 2020 ·  Nov. 10, 2020 ·  Nov. 11, 2020 ·  Nov. 12, 2020 ·  Nov. 13, 2020 ·  Nov. 14, 2020 ·  Nov. 15, 2020 ·  Nov. 16, 2020 ·  Jan. 4, 2021 ·  Jan. 6, 2021 ·  Jan. 8, 2021 ·  Jan. 9, 2021 ·  Jan. 12, 2021 ·  Jan. 15, 2021 ·  Jan. 16, 2021 ·  Jan. 17, 2021 ·  Jan. 30, 2021 ·  Feb. 1, 2021 ·  Feb. 2, 2021 ·  Feb. 3, 2021 ·  Feb. 4, 2021 ·  Feb. 5, 2021 ·  Feb. 7, 2021
      Frames:
      Optolong 2" UV/IR Cut: 137×1000(38h 3′ 20″) (gain: 0.00) -45°C bin 1×1
      Optolong 2" UV/IR Cut: 523×300(43h 35′) (gain: 56.00) -30°C bin 1×1
      Integration:
      81h 38′ 20″
      Darks:
      100
      Flats:
      40
      Flat darks:
      40
      Bias:
      100
      Avg. Moon age:
      16.17 days
      Avg. Moon phase:
      37.90%
      Bortle Dark-Sky Scale:
      2.00

      RA center: 03h39m17s.697

      DEC center: +32°0416.48

      Pixel scale: 0.629 arcsec/pixel

      Orientation: 88.689 degrees

      Field radius: 3.489 degrees

      More info:Open 

      Resolution: 5384x12449

      File size: 19.7 MB

      Locations: Milky Way Observatory, Naobuzi, Zhangjiakou, Hebei, China

      Data source: Own remote observatory

      Remote source: Non-commercial independent facility

      Description

      The Perseus molecular cloud, located at the junction of Taurus, Aries, and Perseus, about 1,000 light-years away from the Earth. It contains over 10,000 solar masses of gas and dust covering an area of 6 by 2 degrees, is the closest giant molecular cloud actively forming large numbers of low to intermediate-mass stars. Unlike the Orion molecular cloud, Perseus molecular cloud is almost invisible apart from two clusters, IC 348 and NGC 1333, where low-mass stars are formed.

      By accumulating a very-long-time of exposure, the dust and gas show up, exhibit a complex and chaotic structure consisting of dense cloud cores surrounded by an interconnected network of filaments and sheets. Many voids surrounded by partial arcs or nearly complete rings are also seen. This complicated structure is one possible signature of supersonic turbulence.

      The eastern (upper) end of the cloud is associated with IC 348 that contains several hundred young stars. Most of the star formation in IC 348 took place within the last 3 Myr, but some stars in this region formed 10 Myr ago. The apparent age spread in IC 348 may be an indication that two episodes of star formation have occurred. IC 348 appears to be an example of a region that is at or near the end of its star-forming phase.

      The western (lower) portion of the Perseus cloud contains the most active region of star formation in the Perseus molecular cloud, including the NGC 1333 cluster. It contains around 150 stars with a median age of a million years, is one of the most active sites of ongoing star formation in the sky within 1500 light-years of the Sun. The molecular ridge extending south (left) from NGC 1333 contains many Herbig–Haro objects, which are bright patches of nebulosity associated with newborn stars.

      Between IC 348 and NGC 1333, right in the middle of this photo, there is an area that appears pinky, which is a low-surface brightness HII region surrounded by a dust ring G159.6-18.5, which appears to lie behind the obscuration of the Perseus molecular cloud. The intense ultraviolet light emitted by the central star HD 278942 ionizes the surrounding hydrogen, giving this region its characteristic pink color. The star appears red in this photo and would have been a blue-white star if it were not obscured by dust. The presence of HD 278942 and its HII region suggests that that massive stars may have formed in the recent past within the Perseus molecular cloud.

      BTW, the cloud of dust, which obscures the central star and the HII region, is called the“Flying Ghost Nebula” because of its shape.

      The area to the west (lower) of the HII region looks relatively empty without too much dense dust, and particularly dark here because the extinction in this region remains high. Perhaps this dead-zone is the youngest portion of the Perseus molecular cloud, formed by the expansion of the dust ring G159.6-18.5.

      There are more areas full of dense dust to the south (left) of NGC 1333, see another photo I took if you are interested: https://www.astrobin.com/ggdhla/C/

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