NGC 1792

NGC 1792
NGC 1792 with the legacy surveys
Observation data (J2000 epoch)
ConstellationColumba
Right ascension05h 05m 14.454s[1]
Declination−37° 58′ 50.70″[1]
Redshift0.004059[2]
Heliocentric radial velocity1,208[3]
Distance36.4 Mly (11.17 Mpc)[3]
Group or clusterNGC 1808[4]
Apparent magnitude (V)10.18[2]
Apparent magnitude (B)10.68[2]
Characteristics
TypeSA(rs)bc[5]
Mass0.54×1011[6] M☉
Mass/Light ratio3.4[6] M☉/L☉
Other designations
IRAS 05035-3802, NGC 1792, PGC 16709, MCG -6-12-004, ESO 305-6, ESO LV3050060[2]
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NGC 1792 is a spiral galaxy located in the southern Columba constellation. It was discovered by Scottish astronomer James Dunlop on October 4, 1826. This galaxy is located at a distance of about 36.4 million light-years and is receding from the Milky Way with a heliocentric radial velocity of 1,208 km/s.[3] NGC 1792 is a member of the NGC 1808 cluster of galaxies.[4]

The morphological classification of this galaxy in the de Vaucouleurs system is SA(rs)bc,[5] indicating a spiral galaxy with no central bar (SA), moderately wound arms (bc), and an incomplete ring structure.[5] However, the HyperLEDA classification of SBbc suggests it does have a bar. It has a flocculent appearance with no central bulge.[7] In the B-band, the angular extend of the galaxy spans 7′.5 × 3′.1. The plane of the galaxy is inclined at an angle of 66° to the line of sight from the Earth, with the major axis being aligned along a position angle of 317°.[4]

Hubble Space Telescope image of NGC 1792 with the blue regions indicating younger stars

There is a high level of star formation along the spiral arms at distances of more than 3 kpc from the galactic core, which have led to a number of prominent H II regions. A comparable high level of star formation in the nearby NGC 1808 galaxy may indicate a recent, distant tidal interaction between the two.[8] Radio emission from the neutral hydrogen in the NGC 1792 galaxy shows a pronounced asymmetry, most likely as a result of this interaction. As the galaxy appears only slightly disturbed, this interaction mainly impacted the outer parts of the galaxy.[4]

The star formation rate in NGC 1792 is estimated to be 11.0 M☉·yr−1.[6] Soft x-ray emission has been detected, the majority of which may be coming from X-ray binaries.[9]

  1. ^ a b Cite error: The named reference 2MASS was invoked but never defined (see the help page).
  2. ^ a b c d Cite error: The named reference SIMBAD was invoked but never defined (see the help page).
  3. ^ a b c Cite error: The named reference Cosmicflows3 was invoked but never defined (see the help page).
  4. ^ a b c d Cite error: The named reference Dahlem1992 was invoked but never defined (see the help page).
  5. ^ a b c Cite error: The named reference deVaucoulerus_et_al_1991 was invoked but never defined (see the help page).
  6. ^ a b c Cite error: The named reference Dahlem_et_al_2001 was invoked but never defined (see the help page).
  7. ^ Cite error: The named reference Marino_et_al_2010 was invoked but never defined (see the help page).
  8. ^ Cite error: The named reference Dahlem2001 was invoked but never defined (see the help page).
  9. ^ Cite error: The named reference Dahlem_et_al_1994 was invoked but never defined (see the help page).