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Contains:  M 90, NGC 4569, IC 3583
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M90 NGC 4569 Galaxy, 





    
        

            Jerry Macon
M90 NGC 4569 Galaxy

M90 NGC 4569 Galaxy

Technical card

Resolution: 2967x2384

Dates:June 3, 2019June 19, 2019

Frames:
Astrodon Gen 2 L 36mm: 127x100" (gain: 99.00) -15C bin 1x1
Astrodon Gen 2 RGB 36mm: 95x100" (gain: 99.00) -20C bin 1x1

Integration: 6.2 hours

Avg. Moon age: 8.44 days

Avg. Moon phase: 47.66%

Bortle Dark-Sky Scale: 4.00

Temperature: 10.00

Astrometry.net job: 2767691

RA center: 189.207 degrees

DEC center: 13.175 degrees

Pixel scale: 0.501 arcsec/pixel

Orientation: 177.575 degrees

Field radius: 0.265 degrees

Locations: Dark Star Observatory, Taos, New Mexico, United States

Data source: Own remote observatory

Remote source: Non-commercial independent facility

Description

Images from the following two scopes (piggybacked) contributed to this image:
AG12+ASI1600MM at .70 asec/pix (RGB)
TV127is+ASI183MM at .75 asec/pix. (L)
They were all registered to the best R image taken on the AG12.
Using L from the TV NP127is refractor effectively eliminates the spikes from the AG12.

Messier 90 is a member of the Virgo Cluster, being one of its largest and brightest spiral galaxies, with an absolute magnitude of around -22 (brighter than the Andromeda Galaxy). The galaxy is located approximately 1°.5 away from the subgroup centered on Messier 87. As a consequence of the galaxy's interaction with the intracluster medium in the Virgo Cluster, the galaxy has lost much of its interstellar medium. As a result of this process, which is referred to as ram-pressure stripping, the galaxy's interstellar medium and star formation regions appear severely truncated compared to similar galaxies outside the Virgo Cluster and there are even H II regions outside the galactic plane, as well as long (up to 80 kpcs, 260,000 light-years) tails of ionized gas that has been stripped of M90.

As stated above, the star formation in Messier 90 appears truncated. Consequently, the galaxy's spiral arms appear to be smooth and featureless, rather than knotted like galaxies with extended star formation., which justifies why this galaxy, along with NGC 4921 in the Coma Cluster has been classified as the prototype of an anemic galaxy. Some authors go even further and consider it is a passive spiral galaxy, similar to those found on galaxy clusters with high redshift.

However, the center of Messier 90 appears to be a site of significant star formation activity, where around 50,000 stars of spectral types O and B that formed around 5-6 million years ago are surrounded by a large amount of A-type supergiants that were born in other starburst that took place before the former, between 15 and 30 million years ago.

Multiple supernovae (up to 10,000) in the nucleus have produced 'superwinds' that are blowing the galaxy's interstellar medium outward into the intracluster medium. collimated in two jets, one of which is being disturbed by interaction with Virgo's intracluster medium as the galaxy moves through it.

The spectrum of Messier 90 is blueshifted, which indicates that it is moving towards the Earth. In contrast, the spectra of most other galaxies are redshifted. The blueshift was originally used to argue that Messier 90 was actually an object in the foreground of the Virgo Cluster. However, since the phenomenon was limited mostly to galaxies in the same part of the sky as the Virgo Cluster, it appeared that this inference based on the blueshift was incorrect. Instead, the blueshift is thought to be evidence for the large range in velocities of objects within the Virgo Cluster itself.
(Wikipedia)

Comments

Author

jmacon
Jerry Macon
License: Attribution Creative Commons
3794
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M90 NGC 4569 Galaxy, 





    
        

            Jerry Macon