Groombridge 34: Difference between revisions

Browse history interactively ← Previous edit Next edit →Content deleted Content addedVisual WikitextInline

Revision as of 15:56, 1 November 2020 editLilHelpa (talk \| contribs)Extended confirmed users, Pending changes reviewers413,638 editsm mos← Previous edit		Revision as of 11:45, 11 November 2020 edit undo0blcsp (talk \| contribs)Extended confirmed users1,663 edits Cleanup (punctuation & link corrections)Tag: Visual edit: Switched Next edit →
Line 73:		Line 73:
	}}		}}
	{{Starbox catalog		{{Starbox catalog
	\| names=GX/GQ Andromedae, ]+43° 44, ] 49, ] 15 A/B, ] 171-047/171-048, ] 1326, ] 1475, ] 3/4, LTT 10108/10109, ] 36248.<ref name=SIMBAD/>		\| names=GX/GQ Andromedae, ]+43° 44, ] 49, ] 15 A/B, ] 171-047/171-048, ] 1326, ] 1475, ] 3/4, LTT 10108/10109, ] 36248.<ref name=SIMBAD/>
	}}		}}
	{{Starbox reference		{{Starbox reference
Line 83:		Line 83:
	}}		}}
	{{Starbox end}}		{{Starbox end}}
	'''Groombridge 34''' is a binary star system in the northern ] of ]. It was listed as entry number 34 in ''A Catalogue of Circumpolar Stars'', published posthumously in 1838 by British astronomer ].<ref name=groombridge1838/> Based upon ] measurements taken by the ], the system is located about 11.6 ~~light-years~~ from the ]. This positions the pair among the ] to the Solar System.		'''Groombridge 34''' is a ] system in the northern ] of ]. It was listed as entry number 34 in ''A Catalogue of Circumpolar Stars'', published posthumously in 1838 by British astronomer ].<ref name=groombridge1838/> Based upon ] measurements taken by the ], the system is located about {{Convert\|11.6\|ly\|pc\|abbr=off\|lk=on}} from the ]. This positions the pair among the ] to the Solar System.

	Both components are small, dim ] stars that are too faint to be seen with the naked eye. They orbit around their common ] in a nearly circular orbit with a separation of about 147 ] and a ] of around 2,600 years.<ref name=lippincott1972/> Both stars exhibit random variation in luminosity due to ] and they have been given ]s: the brighter member Groombridge 34 A is designated '''GX And''', while the smaller component is designated '''GQ And'''.<ref name=petit1990/>		Both components are small, dim ] stars that are too faint to be seen with the naked eye. They orbit around their common ] in a nearly circular orbit with a separation of about 147 ] and a ] of around 2,600 years.<ref name=lippincott1972/> Both stars exhibit random variation in luminosity due to ] and they have been given ]s: the brighter member Groombridge 34 A is designated '''GX And''', while the smaller component is designated '''GQ And'''.<ref name=petit1990/>

	The star system has a relatively high proper motion of 2.9 ]s per year,<ref name=aa575_A35/> and is moving away from the Solar System at a velocity of 11.6 km/s.<ref name="Nidever2002"/> It achieved ] some 15,000 years ago when it came within {{~~Convert~~\|3.5\|pc\|ly~~\|abbr=on\|lk=off~~\|order=flip}} of the Sun.<ref name=aa575_A35/>		The star system has a relatively high proper motion of 2.9 ]s per year,<ref name=aa575_A35/> and is moving away from the Solar System at a velocity of 11.6 km/s.<ref name="Nidever2002"/> It achieved ] some 15,000 years ago when it came within {{cvt\|3.5\|pc\|ly\|order=flip}} of the Sun.<ref name=aa575_A35/>

	==GX Andromedae==		==GX Andromedae==
	The most massive and luminous component of the pair has the ] ''GX Andromedae''. It is a ] ] star of ] M1.4<ref name=apj804_1_64/> that varies his brightness due to ]s. ] observations suggest a rotation period of 44 days and a magnetic activity cycle of roughly 9 years.<ref name=Morris2018/>		The most massive and luminous component of the pair has the ] ''GX Andromedae''. It is a ] ] star of ] M1.4<ref name=apj804_1_64/> that varies his brightness due to ]s. ] observations suggest a rotation period of 44 days and a magnetic activity cycle of roughly 9 years.<ref name=Morris2018/>

	==GQ Andromedae==		==GQ Andromedae==
Line 96:		Line 96:

	==Planetary system==		==Planetary system==
	In August 2014, a planet orbiting around Groombridge 34 A was reported.<ref name=apj794_1_51/> The planet's existence was deduced from analysis of the ] of the parent ~~Star~~ by the Eta-Earth Survey using HIRES at ]. At the time of its discovery, it was the sixth-nearest known ].		In August 2014, a planet orbiting around Groombridge 34 A was reported.<ref name=apj794_1_51/> The planet's existence was deduced from analysis of the ] of the parent star by the Eta-Earth Survey using ] at ]. At the time of its discovery, it was the sixth-nearest-known ].

	Using the ] spectrograph combined with the measurements of the HARPS and HIRES spectrographs, researchers failed to detect the purported Groombridge 34 Ab. However, they did propose another that another planet (Groombridge 34 Ac, GJ 15 Ac) could be orbiting the parent star.<ref name=Trifonov>{{cite journal\|doi=10.1051/0004-6361/201731442\|title=The CARMENES search for exoplanets around M dwarfs. First visual-channel radial-velocity measurements and orbital parameter updates of seven M-dwarf planetary systems\|journal=Astronomy & Astrophysics\|volume=609\|pages=A117\|year=2018\|last1=Trifonov\|first1=T\|last2=Kürster\|first2=M\|last3=Zechmeister\|first3=M\|last4=Tal-Or\|first4=L\|last5=Caballero\|first5=J\|last6=Quirrenbach\|first6=A\|last7=Ribas\|first7=I\|last8=Reiners\|first8=A\|arxiv=1710.01595\|bibcode=2018A&A...609A.117T\|s2cid=119340839}}</ref>		Using the ] spectrograph combined with the measurements of the ] and HIRES spectrographs, researchers failed to detect the purported Groombridge 34 Ab. However, they did propose another that another planet (Groombridge 34 Ac, GJ 15 Ac) could be orbiting the parent star.<ref name=Trifonov>{{cite journal\|doi=10.1051/0004-6361/201731442\|title=The CARMENES search for exoplanets around M dwarfs. First visual-channel radial-velocity measurements and orbital parameter updates of seven M-dwarf planetary systems\|journal=Astronomy & Astrophysics\|volume=609\|pages=A117\|year=2018\|last1=Trifonov\|first1=T\|last2=Kürster\|first2=M\|last3=Zechmeister\|first3=M\|last4=Tal-Or\|first4=L\|last5=Caballero\|first5=J\|last6=Quirrenbach\|first6=A\|last7=Ribas\|first7=I\|last8=Reiners\|first8=A\|arxiv=1710.01595\|bibcode=2018A&A...609A.117T\|s2cid=119340839}}</ref>

	This discrepancy was later reconciled with new HIRES observations, covering a longer span of time, where both planets were recovered, constraining their minimum mass to 3.03 {{Earth mass\|link=yes}} for Groombridge 34 Ab and 36 {{Earth mass}} for Groombridge Ac. Their orbital periods are 11.4 and approximately 7,600 days, respectively. To date, this is the fifth-closest multi-planet system to our ], hosting the longest period Neptune-mass exoplanet discovered so far.<ref name=Pinamonti2018/>		This discrepancy was later reconciled with new HIRES observations, covering a longer span of time, where both planets were recovered, constraining their minimum mass to 3.03 {{Earth mass\|link=yes}} for Groombridge 34 Ab and 36 {{Earth mass}} for Groombridge Ac. Their orbital periods are 11.4 and approximately 7,600 days, respectively. To date, this is the fifth-closest multi-planet system to our ], hosting the longest-period Neptune-mass exoplanet discovered so far.<ref name=Pinamonti2018/>

	{{OrbitboxPlanet begin \|name=Groombridge 34 A		{{OrbitboxPlanet begin \|name=Groombridge 34 A
Line 123:		Line 123:
	==See also==		==See also==
	*]		*]
	*]		*]

	==References==		==References==

Revision as of 11:45, 11 November 2020

Groombridge 34
Observation data Epoch J2000 Equinox J2000
Constellation	Andromeda
Groombridge 34 A
Right ascension	00 18 22.8850
Declination	+44° 01′ 22.6373″
Apparent magnitude (V)	8.119
Groombridge 34 B
Right ascension	00 18 25.8244
Declination	+44° 01′ 38.0912″
Apparent magnitude (V)	11.007
Characteristics
Spectral type	M1.4V + M4.1V
U−B color index	+1.24/+1.40
B−V color index	+1.56/+1.80
Variable type	Flare stars
Astrometry
Groombridge 34 A
Radial velocity (R_v)	+11.62±0.08 km/s
Proper motion (μ)	RA: 2891.525±0.061 mas/yr Dec.: 411.903±0.034 mas/yr
Parallax (π)	280.6902 ± 0.0429 mas
Distance	11.620 ± 0.002 ly (3.5626 ± 0.0005 pc)
Groombridge 34 B
Proper motion (μ)	RA: 2863.284±0.069 mas/yr Dec.: 336.529±0.039 mas/yr
Parallax (π)	280.7866 ± 0.0519 mas
Distance	11.616 ± 0.002 ly (3.5614 ± 0.0007 pc)
Orbit
Companion	Groombridge 34 B
Period (P)	2,600 yr
Semi-major axis (a)	41.15″
Eccentricity (e)	0.00
Inclination (i)	61.4°
Longitude of the node (Ω)	45.3°
Periastron epoch (T)	1745
Details
Groombridge 34 A
Mass	0.38±0.05 `M`_☉
Radius	0.38±0.05 `R`_☉
Luminosity	~0.022 `L`_☉
Habitable zone inner limit	0.112 AU
Habitable zone outer limit	0.239 AU
Surface gravity (log g)	4.87±0.04 cgs
Temperature	3607±68 K
Metallicity	−0.34±0.09 dex
Rotation	43.86±0.56 days
Rotational velocity (v sin i)	1.09±0.79 km/s
Age	~3.02 Gyr
Groombridge 34 B
Mass	0.15±0.02 `M`_☉
Radius	0.18±0.03 `R`_☉
Luminosity	~8.5×10 `L`_☉
Habitable zone inner limit	0.048 AU
Habitable zone outer limit	0.103 AU
Surface gravity (log g)	5.08±0.15 cgs
Temperature	3304±70 K
Metallicity	−0.37±0.10 dex
Age	~2.754 Gyr
Other designations
GX/GQ Andromedae, BD+43° 44, GCTP 49, GJ 15 A/B, G 171-047/171-048, HD 1326, HIP 1475, LHS 3/4, LTT 10108/10109, SAO 36248.
Database references
SIMBAD	GJ 15 A
	GJ 15 Ab
	GJ 15 B
ARICNS	GJ 15 A
	GJ 15 B

Groombridge 34 is a binary star system in the northern constellation of Andromeda. It was listed as entry number 34 in A Catalogue of Circumpolar Stars, published posthumously in 1838 by British astronomer Stephen Groombridge. Based upon parallax measurements taken by the Gaia spacecraft, the system is located about 11.6 light-years (3.6 parsecs) from the Sun. This positions the pair among the nearest stars to the Solar System.

Both components are small, dim red dwarf stars that are too faint to be seen with the naked eye. They orbit around their common barycenter in a nearly circular orbit with a separation of about 147 AU and a period of around 2,600 years. Both stars exhibit random variation in luminosity due to flares and they have been given variable star designations: the brighter member Groombridge 34 A is designated GX And, while the smaller component is designated GQ And.

The star system has a relatively high proper motion of 2.9 arc seconds per year, and is moving away from the Solar System at a velocity of 11.6 km/s. It achieved perihelion some 15,000 years ago when it came within 11 ly (3.5 pc) of the Sun.

GX Andromedae

The most massive and luminous component of the pair has the variable star designation GX Andromedae. It is a main-sequence red dwarf star of spectral type M1.4 that varies his brightness due to stellar flares. Gaia observations suggest a rotation period of 44 days and a magnetic activity cycle of roughly 9 years.

GQ Andromedae

The smaller companion bears the variable star name GQ Andromedae. It is a red dwarf main sequence star that undergoes flare events like the primary; it has a spectral type M4.1, so it has also a lower effective temperature.

Planetary system

In August 2014, a planet orbiting around Groombridge 34 A was reported. The planet's existence was deduced from analysis of the radial velocities of the parent star by the Eta-Earth Survey using HIRES at Keck Observatory. At the time of its discovery, it was the sixth-nearest-known exoplanet.

Using the CARMENES spectrograph combined with the measurements of the HARPS and HIRES spectrographs, researchers failed to detect the purported Groombridge 34 Ab. However, they did propose another that another planet (Groombridge 34 Ac, GJ 15 Ac) could be orbiting the parent star.

This discrepancy was later reconciled with new HIRES observations, covering a longer span of time, where both planets were recovered, constraining their minimum mass to 3.03 M_E for Groombridge 34 Ab and 36 M_E for Groombridge Ac. Their orbital periods are 11.4 and approximately 7,600 days, respectively. To date, this is the fifth-closest multi-planet system to our Sun, hosting the longest-period Neptune-mass exoplanet discovered so far.

The Groombridge 34 A planetary system
Companion (in order from star)	Mass	Semimajor axis (AU)	Orbital period (days)	Eccentricity	Inclination	Radius
Ab	≥ 3.03+0.46 −0.44 M_🜨	0.072+0.003 −0.004	11.4407+0.0017 −0.0016	0.094+0.091 −0.065	—	—
Ac	≥ 36+25 −18 M_🜨	5.4+1.0 −0.9	~7,600	0.27+0.28 −0.19	—	—

References

^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
^ Mann, Andrew W.; et al. (May 2015), "How to Constrain Your M Dwarf: Measuring Effective Temperature, Bolometric Luminosity, Mass, and Radius", The Astrophysical Journal, 804 (1): 38, arXiv:1501.01635, Bibcode:2015ApJ...804...64M, doi:10.1088/0004-637X/804/1/64, S2CID 19269312, 64.
^ Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
^ Mermilliod, J.-C. (1986), "Compilation of Eggen's UBV data, transformed to UBV (unpublished)", Catalogue of Eggen's UBV Data. SIMBAD, Bibcode:1986EgUBV........0M.
^ Nidever, David L.; et al. (August 2002), "Radial Velocities for 889 Late-Type Stars", The Astrophysical Journal Supplement Series, 141 (2): 503–522, arXiv:astro-ph/0112477, Bibcode:2002ApJS..141..503N, doi:10.1086/340570, S2CID 51814894.
^ Lippincott, S. L. (March 1972), "Parallax and orbital motion of the two nearby long period visual binaries Groombridge 34 and ADS 9090.", Astronomical Journal, 77: 165–168, Bibcode:1972AJ.....77..165L, doi:10.1086/111261.
^ Pinamonti, M.; Damasso, M.; Marzari, F.; Sozzetti, A.; Desidera, S.; Maldonado, J.; Scandariato, G.; Affer, L.; Lanza, A. F.; Bignamini, A.; Bonomo, A. S.; Borsa, F.; Claudi, R.; Cosentino, R.; Giacobbe, P.; González-Álvarez, E.; González Hernández, J. I.; Gratton, R.; Leto, G.; Malavolta, L.; Martinez Fiorenzano, A.; Micela, G.; Molinari, E.; Pagano, I.; Pedani, M.; Perger, M.; Piotto, G.; Rebolo, R.; Ribas, I.; et al. (2018). "The HADES RV Programme with HARPS-N at TNG. VIII. GJ15A: A multiple wide planetary system sculpted by binary interaction". Astronomy and Astrophysics. 617: A104. arXiv:1804.03476. Bibcode:2018A&A...617A.104P. doi:10.1051/0004-6361/201732535. S2CID 54990041.
^ Cantrell, Justin R.; et al. (October 2013), "The Solar Neighborhood XXIX: The Habitable Real Estate of Our Nearest Stellar Neighbors", The Astronomical Journal, 146 (4): 99, arXiv:1307.7038, Bibcode:2013AJ....146...99C, doi:10.1088/0004-6256/146/4/99, S2CID 44208180.
"V* GX And". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2016-02-09.{{cite web}}: CS1 maint: postscript (link)
Groombridge, Stephen (1838), Airy, George Biddell (ed.), A Catalogue of Circumpolar Stars, J. Murray, p. 2.
Petit, M. (October 1990), "Catalogue des étoiles variables ou suspectes dans le voisinage du Soleil", Astronomy and Astrophysics Supplement (in French), 85 (2): 971, Bibcode:1990A&AS...85..971P.
^ Bailer-Jones, C. A. L. (March 2015). "Close encounters of the stellar kind". Astronomy & Astrophysics. 575: 13. arXiv:1412.3648. Bibcode:2015A&A...575A..35B. doi:10.1051/0004-6361/201425221. S2CID 59039482. A35.
Morris, Brett M.; Agol, Eric; Davenport, James R. A.; Hawley, Suzanne L. (2018). "Spotting stellar activity cycles in Gaia astrometry". Monthly Notices of the Royal Astronomical Society. 476 (4): 5408. arXiv:1802.09943. Bibcode:2018MNRAS.476.5408M. doi:10.1093/mnras/sty568. S2CID 73564680.{{cite journal}}: CS1 maint: unflagged free DOI (link)
Howard, Andrew W.; et al. (October 2014), "The NASA-UC-UH ETA-Earth Program. IV. A Low-mass Planet Orbiting an M Dwarf 3.6 PC from Earth", The Astrophysical Journal, 794 (1): 9, arXiv:1408.5645, Bibcode:2014ApJ...794...51H, doi:10.1088/0004-637X/794/1/51, S2CID 17361592, 51.
Trifonov, T; Kürster, M; Zechmeister, M; Tal-Or, L; Caballero, J; Quirrenbach, A; Ribas, I; Reiners, A (2018). "The CARMENES search for exoplanets around M dwarfs. First visual-channel radial-velocity measurements and orbital parameter updates of seven M-dwarf planetary systems". Astronomy & Astrophysics. 609: A117. arXiv:1710.01595. Bibcode:2018A&A...609A.117T. doi:10.1051/0004-6361/201731442. S2CID 119340839.

External links

← Celestial objects within 15–20 light-years

Primary member type

Celestial objects by systems.

Subgiant stars

G-type	Delta Pavonis (19.893±0.015 ly)

Main-sequence
stars

A-type	Altair (Alpha Aquilae) (16.730±0.049 ly)
G-type	Alsafi (Sigma Draconis) (18.7993±0.0081 ly) Achird (Eta Cassiopeiae) (19.3314±0.0025 ly) K-type main-sequence star B e (82 G.) Eridani (19.7045±0.0093 ly) 3 (6?) planets: b, c?, d (c), e?, f?, g?, d
K-type	Groombridge 1618 (15.8857±0.0017 ly) Omicron (40) Eridani (16.3330±0.0042 ly) white dwarf B red dwarf C 70 Ophiuchi (16.7074±0.0087 ly) K-type main-sequence star B Gliese 570 (19.1987±0.0074 ly) 2 red dwarfs: B, C T-type brown dwarf D 36 Ophiuchi (19.4185±0.0036 ly) 2 K-type main-sequence stars: B, C HR 7703 (19.609±0.013 ly) red dwarf B
M-type (red dwarfs)	GJ 1245 (15.2001±0.0034 ly) 2 red dwarfs: B, C Gliese 876 (15.2382±0.0025 ly) 4 planets: d, c, b, e LHS 288 (15.7586±0.0034 ly) GJ 1002 (15.8060±0.0036 ly) 2 planets: b, c Gliese 412 (15.9969±0.0026 ly) red dwarf B AD Leonis (16.1939±0.0024 ly) Gliese 832 (16.2005±0.0019 ly) planet b Gliese 682 (16.3328±0.0026 ly) 2? planets: b?, c? EV Lacertae (16.4761±0.0018 ly) G 9-38 (16.800±0.011 ly) red dwarf B GJ 3379 (16.9861±0.0027 ly) Gliese 445 (17.1368±0.0017 ly) 2M1540 (17.3738±0.0046 ly) GJ 3323 (17.5309±0.0026 ly) 2 planets: b, c Gliese 526 (17.7263±0.0024 ly) Stein 2051 (17.9925±0.0020 ly) white dwarf B Gliese 251 (18.2146±0.0028 ly) planet b LP 816-60 (18.3305±0.0038 ly) LSR J1835+3259 (18.5534±0.0049 ly) Gliese 205 (18.6042±0.0022 ly) Gliese 229 (18.7906±0.0018 ly) T-type brown dwarf B 2 planets: Ab, Ac Ross 47 (18.8883±0.0031 ly) Gliese 693 (19.2078±0.0053 ly) Gliese 754 (19.2724±0.0067 ly) Gliese 908 (19.2745±0.0032 ly) Gliese 752 (19.2922±0.0027 ly) red dwarf B (vB 10) planet Ab Gliese 588 (19.2996±0.0031 ly) 2? planets: b?, c? YZ Canis Minoris (19.5330±0.0040 ly) GJ 1005 (19.577±0.035 ly) red dwarf B Gliese 268 (19.7414±0.0076 ly) red dwarf B

Degenerate
stars

White dwarfs	Gliese 440 (15.1226±0.0013 ly)

Brown dwarfs

L-type	DENIS 0255−4700 (15.877±0.014 ly)
T-type	WISE 1741+2553 (15.22±0.20 ly) WISE 1506+7027 (16.856±0.052 ly) DENIS 0817-6155 (17.002±0.037 ly) 2MASS 0939-2448 (17.41±0.44 ly) T-type brown dwarf B 2MASS 1114-2618 (18.20±0.14 ly) 2MASS 0415-0935 (18.62±0.18 ly) SIMP0136 (19.955±0.057 ly) 2MASS 0937+2931 (19.96 _−0.21 ly)
Y-type	WISE 1639−6847 (15.450±0.041 ly) WISE 0350−5658 (18.49±0.24 ly)

Sub-brown dwarfs
and rogue planets

Y-type	WISE 1541−2250 (19.54±0.24 ly)

Constellation of Andromeda

Stars

Bayer	α (Alpheratz) β (Mirach) γ (Almach) δ ε ζ η θ ι κ λ μ ν ξ (Adhil) ο π ρ σ τ υ (Titawin) φ χ ψ ω A b c υ Per (Nembus)
Flamsteed	2 3 4 5 6 7 8 9 10 11 12 13 14 (Veritate) 15 18 22 23 26 28 32 36 39 41 44 45 47 55 56 58 59 63 64 65 66 6 Per
Variable	R T U W Z RT RV RX SU SW TU TW WZ XZ AB AC AD AE AF AR BM BX CC CG CN DS DX EG ET EU FF GO GP GQ GX GR GY HH HN IW KK KX KZ LL LN LP LQ OP OS OU PX PY QR QV QX V385 V428 V439 V455 V529 V807
HR	1 40 56 78 104 122 134 178 275 282 283 289 379 410 483 687 746 748 8884 8925 8950 8962 8973 9011 9074 9075 9105
HD	16175 (Buna) 222155
Other	3XMM J004232.1+411314 ADS 48 HAT-P-6 (Sterrennacht) HAT-P-16 HAT-P-19 HAT-P-28 M31-RV KELT-1 NGC 44 NGC 82 NGC 84 NGC 91 NGC 162 NGC 464 Qatar-3 Qatar-4 Qatar-5 PA-99-N2 WASP-1 WISE 0146+4234 WISE J0005+3737 WISE J004945.61+215120.0

Exoplanets	14 Andromedae b κ Andromedae b υ Andromedae b c d Gliese 15 Ab c HD 13931 b HD 16175 b HAT-P-6b HAT-P-32b WASP-1b WASP-33b Qatar-4b Qatar-5b

Star
clusters

NGC	206 272 752 956 7686
Other	Mayall II RBC EXT8

Nebulae

NGC	7662

Galaxies

Messier	32 110
NGC	5 11 13 19 20 21 27 39 43 48 49 51 67 68 69 70 71 72 74 76 79 80 81 83 85 86 90 93 94 96 97 108 109 112 140 149 160 169 181 183 184 214 218 226 228 229 233 243 252 258 260 262 280 304 317 389 393 404 425 431 477 512 513 523 528 529 531 536 542 561 605 620 668 679 687 700 703 704 705 708 709 710 712 714 717 721 732 753 759 801 812 834 891 906 910 911 912 913 920 937 980 995 996 999 1000 7640 7836
Numbered	I II III IV V VIII IX X XI XVIII XIX XXI
Other	3C 66A 3C 66B Andromeda Galaxy Arp 273 Donatiello I UGC 1840

Galaxy clusters	Abell 262 NGC 68 group

Astronomical events	GRB 101225A SN 1885A (S)