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NGC 1448 (2,629 of 18,816)

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NGC 1448

NGC 1448, NGC 1457, AGC 22916, AM 0342-444, ESO 249-16, LEDA 13727, MCG-07-08-005, SGC 034253-4448.0, h 2585, GC 776

RA: 03h 44m 31.82s
Dec: −44° 38′ 41.3″

Con: Horologium
Ch: MSA:421, U2:391, SA:18

Ref: SIMBAD, Skiff20080430-M, Corwin (2004)

(reference key)

Type: galaxy (in cluster), Sc

Mag: B=11.3, V=?

Size: 7.585′ x 1.698′
PA: 41°

History and Accurate Positions for the NGC/IC Objects (Corwin 2004)

NGC 1448 = NGC 1457, which see.

Historical observations

John Herschel

John Herschel recorded it as "pB, vL, vmE, 3' long, 20 arcseconds broad, position = 221.6 degrees."

Published comments

Reynolds, J.H. (1921)

Reynolds, J.H. (1921) The spiral nebulae in the zone -40° to -90° (from the Franklin-Adams Plates). MNRAS, 81, 598.

Table, p601. 5x1, pa 35; "BN"

Stewart (1908) Ann.Harv.Coll.Obs., 60 (6)

Table IV: not seen; error for 1457 which is identified.

Shapley (1935)

Ann.Harv.Coll.Obs., 88 (5) - Table II, p 110: Size estimate: 2', 45°

Shapley, H. & Paraskevopoulos, J.S. (1940)

Shapley, H. & Paraskevopoulos, J.S. (1940) Southern clusters and galaxies. Harvard Obs. Bull., No.914, 6-8.

de Vaucouleurs, G. (1956)

"Survey of bright galaxies south of -35° declination", Mem. Mount Stromlo, No. 13. (photographic study, plates taken with the 30-inch Reynolds reflector, 20-inch diaphragm). p8: "NGC 1448 = NGC 1457"

de Vaucouleurs, G. (1975)

de Vaucouleurs, G. (1975) Nearby groups of galaxies. In: Kuiper, G. (ed) Stars and Stellar Systems. Volume 9: Galaxies and the Universe. Chapter 14, p557.

NGC 1433 group

Part of the Dorado cloud complex (NGC 1566, NGC 1433, NGC 1672 groups).

Brightest members: 1433 ( B(0) = 10.9), 1512 ( B(0) = 11.58), 1448 ( B(0) = 11.67), 1493 ( B(0) = 12.10), 1411 ( B(0) = 12.16).

("Galaxies and the Universe", Chapter 14 - Nearby Groups of Galaxies) notes that the five brightest members of the NGC 1433 Group, a part of the Dorado Cloud complex, are NGC 1433, NGC 1512, NGC 1448, NGC 1493 & NGC 1411.

Sulentic & Tifft (1973)

(Sulentic and Tifft 1973) notes that this is a 11.5 mag galaxy. Their coded description reads EON,BM,SLDIF,DKLN.

Paturel et al. (1991)

Paturel, G., Petit, C., Kogoshvili, N. et al. (1991) An extragalactic data base. IV. Errors and misprints in catalogues of galaxies. Astrophys.J.Suppl.Ser., 91(3), 371.

NGC 1448 = NGC 1457

Photo index

by Jim Lucyk: Sky&Tel. 1/84 p94, Sky&Tel. 11/88 p491.

Modern observations

Hartung, E.J. (1968) Astron.Obj.South.Tel

Hartung notes: "In a field of scattered stars this long narrow nebula is not bright; it appears about 5' x 0.5' in pa 40 deg and rises in brightness considerably to the central axis but needs close attention to see its length. 15cm will give the shape faintly."

Brian Skiff

15cm - pretty br thin spindle @ 80x. 140x: 4'x0'.8 in pa35. reaches NE 3/4 way to m13.5 * E of maj axis. width approx sep to m13 * SE of cen. wk even concen w/o core or nuc, but brtr region contains *ings. BS, 14Nov1993, LCO.

Contemporary observations

Magda Streicher

(no date)

16-inch f/10 SCT (127x, 290x)

The galaxy is situated unique in a star-field that compliment it. Soft glow, slightly elongated in a NE to SW direction. Two stars 7' to the south, the western 9 Magnitude strong yellow in colour. Long oval 6-7' and 3-4' wide.

Tom Bryant

2010 11 5 3:42:49

Observing site: Fall Star Party

Telescope: C-11

[3h 44m 30s, -44 39' 0"] A faint, elongated (4:1) glow very near the horizon. B: Sc/Sd.

Richard Ford

2013 February 10th, Sunday

Location:Blesfontein Guest Farm,Sutherland.

Time:10:20pm.

Sky Conditions:The most crystal clear sky possible.Dark moon and stars magnitude 6 and fainter are visible with the naked eye.Excellent clean sky,limited star flickering and brilliant objects.

Instrument:12-inch Dobsonian.

This galaxy's faint extensions almost has the shape of a cigar which is obvious at both 57x and 75x.This galaxy has an

elongated structure which is apparent at 75x.The nucleus of this galaxy is slightly bright in the center.This galaxy measures 5'x 1.6'with P.A:NE/SW.Chart No.152,NSOG Vol.3.

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