Andromeda Galaxy (Messier 31)

Messier 31
Messier 31: Andromeda Galaxy; Refractor Takahashi FSQ-106ED f/5.0, SBIG STL-11000M, -20 °C, 10 Micron GM 2000 QCI Ultraportable; 45 x 5 min Baader-RGB-Filter (1x1); Gurnigelpass, 1600 m AMSL; © 10. 9. 2010 Manuel Jung [45]
Messier 31
Messier 31: Andromeda Galaxy; Celestron RASA 11" f/2.22; ZWO ASI6200 Pro; Tentlingen; © 2020 Peter Kocher [33]
M 31
M 31: Andromeda Galaxy; FSQ 106 on AOK Herkules V12 mount, Moravian G3-16200; R 15x5 min, G 15x5 min, B 16x5 min; Lü-Stailas; © 9. 8. 2021 Stefan Berchten, Hansjörg Wälchli [35]

History

Messier 31
Messier 31: Image with and without solarisation; 500/2500 mm Newton + SBIG ST-6; Observatory Bülach; © 1996 Stefan Meister

The Andromeda galaxy was already mentioned in 905 BC. Mentioned BC by the Persian astronomer Al Sufi and was marked on star maps as a "small cloud" long before the invention of the telescope in 1609.

The first observation with a telescope is usually attributed to the German astronomer Simon Marius in 1611 or 1612. He compared the faint glow to that of a candle shining through a horn. Early astronomers suspected that the «Andromeda Nebula» consisted of glowing gas and that a nearby planetary system was being formed. Spectroscopic analyzes nullified this theory and showed that the light must have come from countless stars.

The first indications of the true nature and dimensions of this spiral nebula emerged in late 1923 when several Cepheid variables were found. In a study of these Cepheids using the 100 inch telescope on Mount Wilson, Edwin Hubble finally proved that this must be an extragalactic object and deduced a preliminary distance of 900'000 light years. His publication ended the long controversy about nature this «spiral nebula». Later studies with the newly completed 200 inch telescope showed that the Cepheids in the Andromeda galaxy could be divided into two different populations with different luminosity and that earlier distance measurements were off by a factor of 2-3. [4] Current measurements on Simbad show a distance of 2.5 to 2.6 million light years and that M 31 is moving in our direction at a speed of around 300 km/s. [145]

Physical Properties

M 31 is the largest and closest to us spiral galaxy - apart of course from our own galaxy, the Milky Way with its companions. It owns four small, elliptical companion galaxies, which are located in their gravitational field. Two of them (M 32 and M 110) are in the immediate vicinity. The other two (NGC 147 and NGC 185) lie around 7° to the north in the constellation Cassiopeia. NGC 206 is a bright star cloud within the galaxy M 31. Furthermore, M 31 is home to many globular clusters, of which G 1 is the brightest.

NGC 206
NGC 206: Star cloud NGC 206 in Andromeda Galaxy M 31; 500 mm Cassegrain 3625 mm f/7.2; SBIG STL11K; 90+30+30+30 min LRGB; Bernese Higlands; © 2011 Radek Chromik
Messier 110 (NGC 205)
Messier 110 (NGC 205): Companion of Andromeda Galaxy; 500 mm Cassegrain 3625 mm f/7.2; SBIG STL11K; 150+40+40+40 min LRGB; Bernese Highlands; © 2011 Radek Chromik [32]
NGC 206
NGC 206: Star cloud in M 31; RC 500 on AOK Herkules V48 mount; SBIG STL-11000M/C2; -30 °C chip temperature, R/G/B unbinned, R 12×5 min, G 10×5 min, B 10×5 min; Observatory Son Bi, Mallorca; © 1.–3. 12. 2016 Beat Kohler, Hansjörg Wälchli [35]
NGC 206 + M 32
NGC 206 + M 32: Star cloud NGC 206 and companion galaxy M 32; Takahashi Mewlon 250 CR (2500 mm f/10), SBIG STL 11k; 21L x 600 sec 1×1, 10R, 14G, 15B 2×2 x 600sec, 12HA x 1200 sec; Bernese Highlands; © 3.10. 2016 – 14.10. 2017 Bernhard Blank, Dragan Vogel [32]
Revised+Historic NGC/IC Version 22/9, © 2022 Dr. Wolfgang Steinicke [277]
Name RA Dec Type bMag vMag B-V SB Dim PA z D(z) MD Dreyer Description Identification, Remarks
NGC 147 00 33 11.7 +48 30 26 Gx (E5/P) 10.5 9.5 1.0 14.5 13.2 × 7.8 25 -0.000644 0.730 vF, vL, iR, gsmbM * 11 h 29; GC 72; UGC 326; MCG 8-2-5; DDO 3; CGCG 550-6
NGC 185 00 38 57.6 +48 20 14 Gx (E3) 10.1 9.2 0.9 14.4 8 × 7 35 -0.000674 0.670 pB, vL, iR, vgmbM, r WH II 707; h 35; GC 90; UGC 396; MCG 8-2-10; CGCG 550-9; IRAS 00362+4803
NGC 205 00 40 22.1 +41 41 07 Gx (E5) 8.9 8.1 0.8 14.0 19.5 × 11.5 170 -0.000804 0.800 vB, vL, mE 165°, vgvmbM WH V 18; h 44; GC 105; M 110; UGC 426; MCG 7-2-14; CGCG 535-14; IRAS 00376+4124
NGC 206 00 40 32.3 +40 44 18 GxyP 14.0 4.2 0.790 vF, vL, mE 0° WH V 36; h 45; GC 106; part of M 31
NGC 221 00 42 41.8 +40 51 57 Gx (E2) 9.0 8.1 0.9 12.5 8.5 × 6.5 179 -0.000667 0.770 ! vvB, L, R, psmbMN h 51; GC 117; M 32; UGC 452; MCG 7-2-15; IRAS 00399+4035; ARAK 12; Arp 168; CGCG 535-16
NGC 224 00 42 44.3 +41 16 08 Gx (Sb) 4.4 3.4 1.0 13.5 189.1 × 61.7 35 -0.001001 0.790 !!! eeB, eL, vmE (Andromeda) h 50; GC 116; M 31; UGC 454; MCG 7-2-16; CGCG 535-17; Andromeda nebula

Finder Chart

M 31 is located in the constellation Andromeda, only 1° 20' from the 4.5 mag bright star ν Andromedae. The best observation time is July to February.

Finder Chart Andromeda Galaxy (Messier 31)
Andromeda Galaxy (Messier 31) in constellation Andromeda. Charts created using SkySafari 6 Pro and STScI Digitized Sky Survey. Limiting magnitudes: Constellation chart ~6.5 mag, DSS2 close-ups ~20 mag. [149, 160]

Visual Observation

M 31, M 32, M 110
M 31, M 32, M 110: Pencil drawing; Borg 125/800 f/6.4 ED Apo; © Jozef Cukas

Visible to the eye as a blurred star or nebula. The full extent or size can be seen in the binoculars. The companion galaxies M 32 and M 110 can already be seen in a small amateur telescope. M 32 is almost spherical, while M110 appears elliptical. In addition to the bright core of M 31, the two black dust bands are easily perceptible in medium-sized telescopes. In larger telescopes, nodes or blurred globular clusters that belong to the galaxy become visible. [192]

12.5" Ninja-Dobson, F:4.5 / TV-Nagler 31mm, 46x, 1.78°
Eduard von Bergen

Objects Within a Radius of 15°

References