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Physical Information: Based on a recessional velocity of 3885 km/sec, NGC 5150 is about 180 million light-years away. It may be a member of a small group with the interacting pair NGC 5152 and 5153, in which case their common distance would be about 190 to 200 million light-years. Given that and its apparent size of 1.3 by 1.0 arcmin, NGC 5150 is about 75 thousand light-years across..

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Physical Information: Based on a recessional velocity of 8165 km/sec, NGC 5151 is about 380 million light-years away. Given that, the 0.75 by 0.75 arcmin apparent size of its central region corresponds to about 85 thousand light-years, while its 1.8+ by 1.4 arcmin outer regions extend across more than 200 thousand light-years.

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Physical Information: Based on a recessional velocity of 4165 km/sec, NGC 5152 is about 195 million light-years away, in poor agreement with a single redshift-independent distance estimate of 285 million light-years. However, its obvious interaction with NGC 5153 shows that they must be at about the same distance, and the average of their redshift-independent distance measurements (about 215 million light-years) is in good agreement with their recessional velocity distance average of about 200 million light-years. The pair is probably part of a small group with NGC 5150, and if so their common distance of about 190 to 200 million light-years and its apparent size of 1.9 by 0.7 arcmin implies that NGC 5152 is about 110 thousand light-years across.

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Physical Information: Based on a recessional velocity of 4320 km/sec, NGC 5153 is about 200 million light-years away, in poor agreement with redshift-independent distance estimates of 135 to 155 million light-years. However, its obvious interaction with NGC 5152 (which see for images) shows that they must be at about the same distance, and the average of their redshift-independent distance measurements (about 215 million light-years) is in good agreement with their recessional velocity distance average of about 200 million light-years. The pair is probably part of a small group with NGC 5150, and if so their common distance of about 190 to 200 million light-years and its apparent size of 1.5 by 1.3 arcmin implies that NGC 5153 is about 85 thousand light-years across.

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Physical Information: Based on a recessional velocity of 5580 km/sec, NGC 5154 is about 260 million light-years away. Given that and its apparent size of 1.4 by 1.2 arcmin, it is about 105 thousand light-years across. NGC 5154 may be a companion of its nearest apparent neighbor, NGC 5149.

Historical Identification: (refer to Corwin).
Designation Notes: LEDA gives the position as RA 13 29 35.4, Dec -63 25 29, but the poorly defined nature of the "object" makes a determination of its exact position impossible. Also, as in the case of many non-galaxian objects, the PGC designation only reflects a desire to have the object in the catalog and a search for that designation returns no result, so it is shown in quotes above.
Physical Information: About 60 arcmin wide? Corwin lists 55 x 50 arcmin (ESO 096-SC013)

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Physical Information: Magnitudes 14.4 (southwestern star) and 14.6 (northeastern star).

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Use By The de Vaucouleurs Atlas: NGC 5161 is used by the de Vaucouleurs Atlas of Galaxies as an example of type SB(s)cd.

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Historical Identification: JH 1608, GC 3554
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Physical Information: Corwin list notes "offset from N5166 by oEHo"; does this mean a historical discovery?

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 Corwin also lists the 10th magnitude double star at RA 13 31 14.4, Dec -60 56 0d3, presumably as a marker for the cluster?
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Physical Information: Steinicke lists this as a magnitude 12 star at RA 13 29 31.0, Dec +11 02 30

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PGC Designation Note: For purposes of completeness, LEDA assigns a PGC designation to this object, even though it isn't a galaxy; but a search of the database for that designation returns no result, so it is shown in quotes.
Physical Information: Apparent size 3.1 by 2.4 arcmin. The central star is a magnitude 14.5 white dwarf.

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Historical Identification: Per Dreyer, NGC 5191 (Hough (#5), Tempel list VIII, 1860 RA 13 23 50, NPD 78 04.1) is "extremely faint, 9th magnitude star following (to the east) 57 seconds of time." The position precesses to RA 13 30 46.1, Dec +11 12 29, only about 0.5 arcmin northwest of the center of the galaxy listed above, the description fits and there is nothing else nearby, so the identification is certain.
Discovery Note: (Per Gottlieb) Hough found this object while searching for d'Arrest's comete. Tempel's list VIII gives positions and dates of observation for a number of "new" nebulae, none of which are this object; but in his description of his third "nova" he compares it to Hough's nebula (and the star to its east), proving that he also observed what became NGC 5191, and must be why Dreyer included Tempel in the NGC entry.
Physical Information: Based on a recessional velocity relative to the Cosmic Microwave Background radiation of 6810 km/sec (and H₀ = 70 km/sec/Mpc), NGC 5191 is about 315 to 320 million light-years away, in fair agreement with a single redshift-independent distance estimate of about 385 to 390 million light-years. Given that and its apparent size of about 0.85 by 0.45 arcmin for the central galaxy and about 1.8 by 0.9 arcmin for its faint outer region (from the images below), the galaxy is about 75 to 80 thousand light-years across, and its outer region spans about 165 thousand light-years.

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Historical Identification: Per Dreyer, NGC 5194 (= GC 3572 = JH 1622, M51, 1860 RA 13 23 58, NPD 42 04.9) is "a magnificent or otherwise interesting object, Great Spiral nebula". The position precesses to RA 13 29 52.5, Dec +47 11 39, practically dead center on the galaxy listed above and the description fits, so the identification is certain.
Physical Information: NGC 5194's recessional velocity of 465 km/sec is too small to provide a reliable distance indication, but happens to provide a relatively accurate result of 22 million light-years. Redshift-independent distance estimates have ranged from 19 to 30 million light-years, but observations of a 2005 supernova in NGC 5195 slightly lowered the estimated distance to 23 ± 4 million light-years. Given that and its apparent size of 11.2 by 6.9 arcmin, the galaxy is about 70 thousand light-years across. Its spectacular spiral structure is believed to be due to its interaction with NGC 5195, with which it forms Arp 85. (Note: The history of discovery implies that M51 should apply only to NGC 5195, but it is not uncommon for NGC 5194 to be referred to as M51A and for NGC 5195 to be referred to as M51B, as though they had both discovered by Messier.) NGC has a bright central nucleus, making it a Seyfert galaxy (type Sy 2). An extensive bridge of stars, gas and dust connects M51 with its smaller companion. Clusters of hot, bright young stars, and gases heated by their radiation illuminate the spiral arms, and clearly define them. Thick dust lanes straddle the arms, sweep across the "bridge" and partially obscure the companion. The Whirlpool Galaxy was the first nebula observed to have a spiral structure, by the 3rd Lord Rosse, using the 72-inch Leviathan (the largest telescope in the world for many decades) at Birr Castle in 1845. Use By The de Vaucouleurs Atlas: NGC 5194 is used by the de Vaucouleurs Atlas of Galaxies as an example of type SA(s)bc.

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Physical Information: Recessional velocity and redshift-independent distance estimates for NGC 5195 are identical to those of its companion, NGC 5194 (which see for that discussion). In any event their obvious interaction means they share the same distance, in the range of 22 or so million light-years. Given that and the 3.0 by 2.5 arcmin apparent size of the brighter core of NGC 5195, it is about 20 thousand light-years across; but due to its interaction with NGC 5194, its stars are scattered across a region nearly 6 arcmin across, which corresponds to about 40 thousand light-years. (As noted at NGC 5194, NGC 5195 is sometimes referred to as M51B, even though it was not part of Messier's original discovery.) Use By The de Vaucouleurs Atlas: NGC 5195 is used by the de Vaucouleurs Atlas of Galaxies as an example of type I0 / SB(r)0⁺ pec.

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