IC 1101

Image of IC 1101 taken in June 1995 by the Hubble Space Telescope

Observation data (J2000 epoch)
Constellation| Virgo
Right ascension|  15h 10m 56.1s[1]
Declination| +05° 44′ 41″[1]
Redshift| 0.078054±0.000027[1][2]
Helio radial velocity| 22,419 km/s (13,931 mi/s)[1]
Distance| 354.0 ± 24.8 Mpc (1,154.6 ± 80.9 million ly)h−10.67[1]
Group or cluster| Abell 2029
Apparent magnitude (V)| 13.22[1]
Characteristics
Type| cD; S0-[1]
Size| 123.65 to 169.61 kpc (403,300 to 553,200 ly)
(D25 B-band and total K-band isophotes)[3][4][lower-alpha 1]
Apparent size (V)| 1'.2 × 0'.6[1]
Other designations
A2029-BCG[1], UGC 9752[1], PGC 54167[1]

IC 1101 is a class S0 supergiant (cD) lenticular galaxy at the center of the Abell 2029 galaxy cluster. It has an isophotal diameter at about 123.65 to 169.61 kiloparsecs (400,000 to 550,000 light-years). It possesses a diffuse core, which is the largest core of any galaxy known to date,[5] and contains a supermassive black hole, one of the largest discovered.[5]

IC 1101 is located at 354.0 megaparsecs (1.15 billion light-years) from Earth. It was discovered on 19 June 1790, by the German-British astronomer William Herschel.[6]

## Contents

* 1 Observation history
* 2 Characteristics
* 2.1 Morphology
* 2.2 Components and structure
* 2.3 Size
* 2.4 Distance
* 3 Formation
* 4 See also
* 5 Notes
* 6 References
* 7 External links

## Observation history

IC 1101 was catalogued in the Index Catalogue of galaxies in the late 1800s to the early 1900s, which is where the galaxy got its most-used designation.[7] In a 1964 study of galaxies accompanied by radio sources, IC 1101 was listed as being among the diffuse elliptical galaxies chosen for the study. The study noted that IC 1101 had not been considered as a radio source, but radio emissions similar to galaxies with such emissions were detected.[8]

Almost a decade and a half later, in 1978, astronomer Alan Dressler analyzed 12 very rich clusters of galaxies, among them Abell 2029, where IC 1101 is located.[9] The following year, he released a paper dedicated solely to IC 1101 and its related dynamics and properties, revealing a rising velocity dispersion profile.[10] After this, he would publish a paper overviewing his recent studies on the cluster and the galaxy.[11]

During 1985, a team of astronomers obtained the spectra of the gas inside several galaxy clusters known to be luminous at X-ray wavelengths, including Abell 2029.[12] Soon after, an investigation into the dynamics of IC 1101 and the galaxies within a few hundred kiloparsecs of it was conducted.[13]

The centers of galaxy clusters are considered to be among the best laboratories for the study of galaxy and cluster evolution, and so during the late 1980s to early 1990s, numerous papers were released, surveying many brightest cluster galaxies. Among them was IC 1101.[14][15][16] R-band (red light) luminosity profiles were soon obtained for IC 1101, revealing a very vast halo of light that could be traced out for more than several hundred kiloparsecs from the galaxy's center.[17]

In 2002, an analysis of Chandra X-ray surveys of the cluster was performed.[18] In 2011, a survey of over 430 brightest cluster galaxies was conducted, among them IC 1101.[19]

In 2017, a redshift survey of the cluster was conducted, allowing a list of velocity dispersions to be created. This constrains the dynamics of the cluster.[20][21] That same year, an analysis of the galaxy's inner regions using Hubble Space Telescope images found a huge yet diffuse galactic core, accompanied with mass estimates of the central supermassive black hole.[5]

During 2019–2020, 170 local galaxy clusters were surveyed for a study of brightest cluster galaxies, their structures and the intracluster light around them.[22]

## Characteristics

### Morphology

IC 1101 imaged by the Sloan Digital Sky Survey

The galaxy is classified as a supergiant elliptical (E) to lenticular (S0)[23] and is the brightest galaxy in A2029 (hence its other designation A2029-BCG; BCG meaning brightest cluster galaxy).[24][25] The galaxy's morphological type is debated due to it possibly being shaped like a flat disc but only visible from Earth at its broadest dimensions. A morphology of S0- (Hubble stage −2; see Hubble stage for details) has been given by the Third Reference Catalogue of Bright Galaxies (RC3) in 1991.[3]

### Components and structure

Like most large galaxies, IC 1101 is populated by a number of metal-rich stars, some of which are as much as seven billion years older than the Sun, making it appear golden yellow in color. It has a very bright radio source at the center, which is likely associated with an ultramassive black hole in the current estimated mass of 97.7+171.4
−62.2 billion M☉ measured using the break radius of the central core,[26][27] or alternatively at 50–70 billion M☉ using gas accretion rate and growth modelling,[28] or 40–100 billion M☉ using core dynamical models,[5] which would make IC 1101's black hole one of the most massive known to date. The estimates of the mass of IC 1101's black hole are near the upper bound of cosmological limits,[28] and is referred to as an "overmassive" black hole.[5]

IC 1101's mass-to-light ratio has been described as being anomalously high. The galaxy also has a unique velocity dispersion profile, which indicates a massive dark matter halo. The Abell 2029 cluster in which IC 1101 resides accretes roughly 450 solar masses per year. The galaxy lacks nuclear emission in visible light at its center as well as signs of recent star formation.[29] There is also no evidence of dust lanes in the core.[30]

A 2017 paper suggests that IC 1101 has the largest core size of any galaxy, with a core radius of around 4.2 ± 0.1 kpc (13.70 ± 0.33 thousand ly) by fitting a model to a Hubble Space Telescope (HST) image of the galaxy. This makes its core larger than the one observed in A2261-BCG, which is 3.2 kpc (10 thousand ly). The core is also roughly an order of magnitude larger than the cores of other large elliptical galaxies, such as NGC 4889 and NGC 1600. Estimates of the absolute magnitude of IC 1101's spheroid are very faint for such a large core, indicating a large stellar mass deficit estimated at 4.9×1011 M☉ and a large luminosity deficit estimated at 1.1×1011 L☉. A hypothesis for the observed properties and peculiarities of the core is that the merger of the central black holes from the formation of the galaxy flung stars out of the core.[5] However, when examining large and diffuse galactic cores, caution must be taken, as estimates may differ between the computer models used.

IC 1101's major axis is oriented in the northeast to southwest direction. The major axis is even aligned on the axis by which Abell 2029 accretes from Abell 2033.[31] Its components such as the core and main body are well-aligned, but the halo is twisted by 20 degrees from the galaxy's other components. Its isophotes (The shapes connecting areas with the same surface brightness) are predominantly boxy. Closer to the core, IC 1101's isophotes become elongated, suggesting a nuclear disc. This feature might be due to an unresolved double nucleus, produced by a low intensity active galactic nucleus (AGN) or a disrupted satellite galaxy disturbed by the central black hole. Several elliptical galaxies like NGC 4438-B, NGC 5419, and VCC 128 contain two point-sources, producing high ellipticities. The NRAO VLA sky-survey detected a radio source near IC 1101, corroborating a possible AGN. Another, weaker radio source has also been detected nearby, opening up the possibility of a double AGN that cannot be ruled out.[30]

Like most BCGs, IC 1101 has a massive and diffuse stellar halo and has some excessive halo light.[32] The halo is twisted by 20 degrees from the main body and core of IC 1101. This feature, among others, seems to be the reason why IC 1101 is classified as a lenticular galaxy in RC3.[30]

IC 1101 imaged by the 9th data release of the Legacy survey.

### Size

IC 1101 is considered a large galaxy characterized by an extensive, diffuse halo. This is the intracluster light, or ICL, free-flying stars that are not bound to any galaxy. This ubiquitous mass of stars within galaxy clusters are usually more concentrated around the brightest cluster galaxies, such as IC 1101, however.[33] Photometrically, the ICL is indistinguishable from the brightest cluster galaxy, but it can be distinguished kinematically.[22] During the early 2000s, weak-lensing estimates for Abell 2029 were taken, indicating the distribution of the mass throughout the cluster and galaxy.[34]

Defining the size of a galaxy varies according to the method used in the astronomical literature. Photographic plates of blue light from the galaxy (sampling stars excluding the diffuse halo) yield an effective radius (the radius within which half the light is emitted) of 65 ± 12 kpc (212 ± 39 thousand ly)[29] based on an earlier distance measurement. The galaxy has a very large halo of much lower intensity "diffuse light" extending to a radius of 600 kpc (2 million ly).[32] The authors of the study identifying the halo conclude that IC 1101 is "possibly one of the largest and most luminous galaxies in the universe". This view has been stated in several other papers as well, but this figure was based on an earlier assumed distance of 262 megaparsecs (855 million light-years).

More recent measurements, using the 25.0 magnitude/arcsec2 standard (commonly[2][28] known as D25, a method recommended by R.O. Redman in 1936)[35][lower-alpha 2] has been utilized by the RC3 in the B-band, with a measured major axis (log 2a+1) of 1.08 (equivalent to 72.10 arcseconds),[3] translating to a diameter of 123.65 kiloparsecs (403,000 ly).[1] Another calculation by the Two Micron All-Sky Survey using the "total" aperture at the K-band yields a much larger size of 169.61 kiloparsecs (553,000 ly).[4] Both measurements are based on the currently-accepted distance to IC 1101. This would make it one of the largest and most luminous galaxies known, though there are other galaxies with larger isophotal diameter measurements (such as NGC 623, Abell 1413 BCG, and ESO 306-17).

### Distance

The distance to IC 1101 has also been uncertain, with different methods across different wavelengths producing varying results. An earlier distance calculation from 1980 using the galaxy's photometric property yield a distance of 262.0 Mpc (855 million ly) and a redshift of z = 0.077, based on a Hubble constant value H0 of 60 km/s/Mpc.[36] The RC3 catalogue gave a nearly similar value of z = 0.078, based on optical emission lines,[3] a value conformed to as recently as 2017 based on luminosity, stellar mass, and velocity dispersion functions,[2] all yielding distances of 354.0 megaparsecs (1.2 billion light-years) based on the modern value of the Hubble constant H0 = 67.8 km/s/Mpc; the currently accepted values. Lower redshifts have been calculated for other wavelengths such as the photometric redshift measurement by the Two Micron All-Sky Survey (2MASS) in 2014, which gave a value of z = 0.045,[37] translating to a distance of 197.1 megaparsecs (643 million light-years). A measurement made in 2005 by the Arecibo Observatory using the 21-cm hydrogen emission line yields a redshift of z = 0.021,[38] and hence a distance of 97.67 ± 6.84 megaparsecs (318.6 ± 22.3 million light-years). However, the hydrogen emission is likely sourced from the foreground galaxy LEDA 5057632.[39]

## Formation

The lack of other bright and luminous galaxies other than IC 1101 at the center of the Abell 2029 galaxy cluster suggests that they were absorbed and consumed ("chewed-up") by the nascent IC 1101. Since the halo is somewhat flattened, the halo most likely retained the distribution of the bright luminous galaxies as they were consumed.[10]

The depleted core and other characteristics of IC 1101 such as the halo component and its structure at moderate distances from the center suggest that the galaxy underwent numerous galactic mergers and interactions, perhaps as much as 10 or even more.[5] The smoothness of the halo suggests that it formed early in the history of the cluster.[25][10][30]

## See also

* List of galaxies
* ESO 383-76

## Notes

1. ↑ The diameters given at NED were based on a redshift-independent distance measurement. The diameters given here were based on NED's provided scale "Virgo \+ GA \+ Shapley" multiplied with the given angular diameter values of the estimation methods being stated.
2. ↑ Date mistakenly stated as 1963.

## References

1. ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 1.11 "NED results for object IC 1101". NASA/IPAC Extragalactic Database. https://ned.ipac.caltech.edu/byname?objname=IC+1101&hconst=67.8&omegam=0.308&omegav=0.692&wmap=4&corr_z=1.
2. ↑ 2.0 2.1 2.2 "Reference Lookup | NASA/IPAC Extragalactic Database". https://ned.ipac.caltech.edu/reflookup?refcode=2017ApJS..229...20S. Retrieved 9 December 2022.
3. ↑ 3.0 3.1 3.2 3.3 De Vaucouleurs, Gerard; De Vaucouleurs, Antoinette; Corwin, Herold G.; Buta, Ronald J.; Paturel, Georges; Fouque, Pascal (1991). Third Reference Catalogue of Bright Galaxies. Bibcode: 1991rc3..book.....D. https://ui.adsabs.harvard.edu/abs/1991rc3..book.....D/abstract.
4. ↑ 4.0 4.1 "NASA/IPAC Extragalactic Database". https://ned.ipac.caltech.edu/uri/NED::Refcode/20032MASX.C.......:.
5. ↑ 5.0 5.1 5.2 5.3 5.4 5.5 5.6 Dullo, Bililign T.; Graham, Alister W.; Knapen, Johan H. (October 2017). "A remarkably large depleted core in the Abell 2029 BCG IC 1101". Monthly Notices of the Royal Astronomical Society 471 (2): 2321–2333. doi:10.1093/mnras/stx1635. Bibcode: 2017MNRAS.471.2321D.
6. ↑ "William Herschel's astronomical discoveries". University of St Andrews, Scotland. http://mathshistory.st-andrews.ac.uk/Extras/Herschel_William_discoveries.html.
7. ↑ Dreyer, J. L. E. (1895). "Index Catalogue of Nebulae found in the years 1888 to 1894, with Notes and Corrections to the New General Catalogue". Memoirs of the Royal Astronomical Society 51: 185–228. Bibcode: 1895MmRAS..51..185D.
8. ↑ Matthews, Thomas A.; Morgan, William W.; Schmidt, Maarten (July 1964). "A Discussion of Galaxies Identified with Radio Sources". Astrophysical Journal 140: 32,35. doi:10.1086/147890. Bibcode: 1964ApJ...140...35M. https://ui.adsabs.harvard.edu/abs/1964ApJ...140...35M/abstract. Retrieved 21 April 2023.
9. ↑ Dressler, A. (August 1978). "A comprehensive study of 12 very rich clusters of galaxies. I. Photometric technique and analysis of the luminosity function.". Astrophysical Journal 223: 15. doi:10.1086/156310. Bibcode: 1978ApJ...223..765D.
10. ↑ 10.0 10.1 10.2 Dressler, A. (August 1979). "The dynamics and structure of the cD galaxy in Abell 2029.". Astrophysical Journal 231: 659–670. doi:10.1086/157229. Bibcode: 1979ApJ...231..659D. https://ui.adsabs.harvard.edu/abs/1979ApJ...231..659D/abstract. Retrieved January 17, 2023.
11. ↑ Dressler, A. (1981). "The dynamics of the cluster of galaxies A 2029.". Astrophysical Journal 243: 6. doi:10.1086/158562. Bibcode: 1981ApJ...243...26D. https://ui.adsabs.harvard.edu/abs/1981ApJ...243...26D/abstract. Retrieved February 27, 2022.
12. ↑ Hu, E.M.; Cowie, L.L.; Wang, Z. (December 1985). "Long-slit spectroscopy of gas in the cores of X-ray luminous clusters.". Astrophysical Journal Supplement Series 59: 53. doi:10.1086/191081. Bibcode: 1985ApJS...59..447H.
13. ↑ Bower, R.G.; Ellis, R.S.; Efstathiou, G. (October 1988). "A study of satellite galaxies in the rich cluster A 2029.p". Monthly Notices of the Royal Astronomical Society 234 (3): 725. doi:10.1093/mnras/234.3.725. Bibcode: 1988MNRAS.234..725B.
14. ↑ Schombert, James M. (March 1986). "The Structure of Brightest Cluster Members. I. Surface Photometry". Astrophysical Journal 60: 91. doi:10.1086/191100. Bibcode: 1986ApJS...60..603S.
15. ↑ Schombert, James M. (August 1987). "The Structure of Brightest Cluster Members. II. Mergers". Astrophysical Journal Supplement 64: 24. doi:10.1086/191212. Bibcode: 1987ApJS...64..643S. https://articles.adsabs.harvard.edu/pdf/1987ApJS...64..643S. Retrieved March 3, 2023.
16. ↑ Schombert, James M. (1988). "The Structure of Brightest Cluster Members. III. cD Envelopes". Astrophysical Journal 328: 14. doi:10.1086/166306. Bibcode: 1988ApJ...328..475S. https://articles.adsabs.harvard.edu/pdf/1988ApJ...328..475S. Retrieved March 3, 2023.
17. ↑ Boughn, S.P.; Kuhn, J.R.; Uson, Juan M. (1990). "CCD Observation of Diffuse Light in the Rich Cluster A:2029". The Galactic and Extragalactic Background Radiation 139: 7. Bibcode: 1990IAUS..139..357B. https://ui.adsabs.harvard.edu/abs/1990IAUS..139..357B/abstract. Retrieved March 12, 2023.
18. ↑ Lewis, Aaron D.; Stocke, John T.; Buote, David A. (July 2002). "Chandra Observations of Abell 2029: No Cooling Flow and a Steep Abundance Gradient". The Astrophysical Journal 573 (1): 5. doi:10.1086/341990. Bibcode: 2002ApJ...573L..13L. https://ui.adsabs.harvard.edu/abs/2002ApJ...573L..13L/abstract. Retrieved February 27, 2023.
19. ↑ Donzelli, C.G.; Muriel, H.; Madrid, J.P. (August 2011). "The Luminosity Profiles of Brightest Cluster Galaxies". The Astrophysical Journal Supplement 195 (2): 15. doi:10.1088/0067-0049/195/2/15. Bibcode: 2011ApJS..195...15D. https://ui.adsabs.harvard.edu/abs/2011ApJS..195...15D/abstract. Retrieved February 27, 2023.
20. ↑ Sohn, Jubee; Geller, Margaret J.; Zahid, H. Jabran; Fabricant, Daniel G.; Diaferio, Antonaldo; Rines, Kenneth J. (April 2017). "The Velocity Dispersion Function of Very Massive Galaxy Clusters: Abell 2029 and Coma". The Astrophysical Journal 229 (2): 16. doi:10.3847/1538-4365/aa653e. Bibcode: 2017ApJS..229...20S.
21. ↑ Sohn, Jubee; Geller, Margaret J.; Walker, Stephen A.; Dell'Antonio, Ian; Diaferio, Antonaldo; Rines, Kenneth J. (January 2019). "The Massively Accreting Cluster A2029". The Astrophysical Journal 871 (1): 15. doi:10.3847/1538-4357/aaf1cc. Bibcode: 2019ApJ...871..129S.
22. ↑ 22.0 22.1 Kluge, M.; Neureiter, B.; Riffeser, A.; Bender, R.; Gossel, C.; Hopp, U.; Schmidt, M.; Ries, C. et al. (April 2020). "Structure of Brightest Cluster Galaxies and Intracluster Light". The Astrophysical Journal 247 (2): 5194–5199. doi:10.3847/1538-4365/ab733b. PMID 43. Bibcode: 2020ApJS..247...43K.
23. ↑ "IC 1101". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=IC+1101.
24. ↑ Lewis, Aaron D.; Buote, David A.; Stocke, John T. (March 2003). "Chandra Observations of A2029: The Dark Matter Profile Down to below 0.01rvir in an Unusually Relaxed Cluster". The Astrophysical Journal 586 (1): 135–142. doi:10.1086/367556. Bibcode: 2003ApJ...586..135L.
25. ↑ 25.0 25.1 Uson, Juan M.; Boughn, Stephen P.; Kuhn, Jeffrey R. (October 1990). "The central galaxy in Abell 2029 - an old supergiant". Science 250 (4980): 539–540. doi:10.1126/science.250.4980.539. PMID 17751483. Bibcode: 1990Sci...250..539U.
26. ↑ Dullo, B.T. (22 November 2019). "The Most Massive Galaxies with Large Depleted Cores: Structural Parameter Relations and Black Hole Masses". The Astrophysical Journal 886 (2): 80. doi:10.3847/1538-4357/ab4d4f. Bibcode: 2019ApJ...886...80D.
27. ↑ Dullo, B.T.; de Paz, A.G.; Knapen, J.H. (18 February 2021). "Ultramassive black holes in the most massive galaxies: MBH−σ versus MBH−Rb". The Astrophysical Journal 908 (2): 134. doi:10.3847/1538-4357/abceae. Bibcode: 2021ApJ...908..134D.
28. ↑ 28.0 28.1 28.2 Brockamp, M.; Baumgardt, H.; Britzen, S.; Zensus, A. (January 2016). "Unveiling Gargantua: A new search strategy for the most massive central cluster black holes". Astronomy & Astrophysics 585: A153. doi:10.1051/0004-6361/201526873. Bibcode: 2016A&A...585A.153B.
29. ↑ 29.0 29.1 Fisher, David; Illingworth, Garth; Franx, Marijn (January 1995). "Kinematics of 13 brightest cluster galaxies". The Astrophysical Journal 438 (2): 539–562. doi:10.1086/175100. Bibcode: 1995ApJ...438..539F.
30. ↑ 30.0 30.1 30.2 30.3 Dullo, Bililign T. (December 2019). "The Most Massive Galaxies with Large Depleted Cores: Structural Parameter Relations and Black Hole Masses". The Astrophysical Journal 886 (2): 80. doi:10.3847/1538-4357/ab4d4f. Bibcode: 2019ApJ...886...80D.
31. ↑ Gonzalez, Elizabeth Johana; de Los Rios, Martin; Oio, Gabriel A.; Hernández Lang, Daniel; Aguirre Tagliferro, Tania; Domínguez R., Mariano J.; Nilo Castellón, José Luis; Cuevas L., Héctor et al. (March 2018). "Analysis of candidates for interacting galaxy clusters. I. A1204 and A2029/A2033". Astronomy & Astrophysics 611: 12. doi:10.1051/0004-6361/201732003. Bibcode: 2018A&A...611A..78G. https://ui.adsabs.harvard.edu/abs/2018A&A...611A..78G;/abstract. Retrieved February 12, 2023.
32. ↑ 32.0 32.1 Uson, Juan M.; Boughn, Stephen P.; Kuhn, Jeffrey R. (March 1991). "Diffuse light in dense clusters of galaxies. I. R-band observations of Abell 2029". The Astrophysical Journal 369: 46–53. doi:10.1086/169737. Bibcode: 1991ApJ...369...46U. http://scholarship.haverford.edu/cgi/viewcontent.cgi?article=1025&context=astronomy_facpubs.
33. ↑ Montes, Mireia (March 2022). "The faint light in groups and clusters of galaxies". Nature Astronomy 6 (3): 308–316. doi:10.1038/s41550-022-01616-z. Bibcode: 2022NatAs...6..308M. https://ui.adsabs.harvard.edu/abs/2022NatAs...6..308M/abstract. Retrieved February 12, 2023.
34. ↑ Ménard, B.; Erben, T.; Mellier, Y. (2003). "Weak Lensing Study of Abell 2029". Astronomical Society of the Pacific 301: 5. Bibcode: 2003ASPC..301..537M. https://ui.adsabs.harvard.edu/abs/2003ASPC..301..537M/abstract. Retrieved February 12, 2023.
35. ↑ "Dimensions of Galaxies". https://ned.ipac.caltech.edu/level5/PROPERTIES/dog.html. Retrieved 9 December 2022.
36. ↑ Hoessel, J. G.; Gunn, J. E.; Thuan, T. X. (1980). "The photometry properties of brightest cluster galaxies. I. Absolute magnitudes in 116 nearby Abell clusters". The Astrophysical Journal 241: 486. doi:10.1086/158363. Bibcode: 1980ApJ...241..486H. https://ui.adsabs.harvard.edu/abs/1980ApJ...241..486H/abstract.
37. ↑ Bilicki, Maciej; Jarrett, Thomas H.; Peacock, John A.; Cluver, Michelle E.; Steward, Louise (2014). "Two Micron All Sky Survey Photometric Redshift Catalog: A Comprehensive Three-dimensional Census of the Whole Sky". The Astrophysical Journal Supplement Series 210 (1): 9. doi:10.1088/0067-0049/210/1/9. Bibcode: 2014ApJS..210....9B. https://ui.adsabs.harvard.edu/abs/2014ApJS..210....9B/abstract.
38. ↑ Springob, Christopher M.; Haynes, Martha P.; Giovanelli, Riccardo; Kent, Brian R. (2005). "A Digital Archive of H I 21 Centimeter Line Spectra of Optically Targeted Galaxies". The Astrophysical Journal Supplement Series 160 (1): 149. doi:10.1086/431550. Bibcode: 2005ApJS..160..149S. https://ui.adsabs.harvard.edu/abs/2005ApJS..160..149S/abstract.
39. ↑ Clarke, T. E. (February 2004). "Soft X-Ray Absorption Due to a Foreground Edge-on Spiral Galaxy toward the Core of A2029". The Astrophysical Journal 601 (2): 798-804. doi:10.1086/380819. Bibcode: 2004ApJ...601..798C. https://ui.adsabs.harvard.edu/abs/2004ApJ...601..798C/abstract. Retrieved March 26, 2026.

## External links

| Wikimedia Commons has media related to IC 1101.

|

* Wilford, John Noble (26 October 1990). "Sighting of Largest Galaxy Hints Clues on the Clustering of Matter". The New York Times. https://www.nytimes.com/1990/10/26/us/sighting-of-largest-galaxy-hints-clues-on-the-clustering-of-matter.html.
* Nemiroff, R.; Bonnell, J., eds (12 March 2012). "The Scale of the Universe - Interactive". Astronomy Picture of the Day. NASA. https://apod.nasa.gov/apod/ap120312.html.
*   * IC 1101 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images

Coordinates:  15h 10m 56.1s, +05° 44′ 41″

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* 5341
* 5342
* 5344
* 5353
* 5368
* 5384
* 5392
* 5418
* 5424
* 5496
* 5536
* 5584
* 5631

HD|

* 102195
* 102329
* 104078
* 104755
* 106038
* 106252
* 106270
* 106515
* 107148
* 107794
* 109271
* 112495
* 114783
* 116429
* 122577
* 124973
* 125490
* 125612
* 126614
* 128563
* 130322
* 133600

Other|

* EC 14012-1446
* G 64-12
* HAT-P-26
* K2-19
* PG 1159-035
* PG 1323-086
* PG 1325+101
* PSR B1257+12 (Lich)
* Ross 128
* SDSS J121209.31+013627.7
* SDSS J1229+1122
* ULAS J133553.45+113005.2
* WASP-16
* WASP-24
* WASP-37
* WASP-39 (Malmok)
* WASP-40/HAT-P-27
* WD 1145+017
* Wolf 424
* Wolf 485A
* Wolf 489

Star
clusters|

| Open|

* NGC 5634

|

Globular|

* HVGC-1
* Koposov I

Nebulae|

| Planetary|

* Abell 36

|

Galaxies|

| Messier|

* 49
* 58
* 59
* 60
* 61
* 84
* 86
* 87
* 89
* 90
* 104 (Sombrero Galaxy)

|

NGC|

* 3776
* 3817
* 3818
* 3833
* 3843
* 3848
* 3849
* 3852
* 3863
* 3876
* 3907
* 3907B
* 3914
* 3915
* 3952
* 3976
* 3976A
* 3979
* 4006
* 4012
* 4029
* 4030
* 4043
* 4044
* 4045
* 4045A
* 4058
* 4063
* 4067
* 4073
* 4075
* 4077
* 4079
* 4082
* 4083
* 4107
* 4116
* 4119
* 4123
* 4129
* 4139
* 4164
* 4165
* 4168
* 4176
* 4178
* 4179
* 4180
* 4191
* 4193
* 4197
* 4200
* 4201
* 4202
* 4206
* 4207
* 4215
* 4216
* 4223
* 4224
* 4233
* 4234
* 4235
* 4240
* 4241
* 4246
* 4247
* 4249
* 4252
* 4255
* 4257
* 4259
* 4260
* 4261
* 4264
* 4266
* 4267
* 4268
* 4269
* 4270
* 4273
* 4276
* 4277
* 4279
* 4281
* 4282
* 4285
* 4287
* 4289
* 4292
* 4292A
* 4294
* 4296
* 4297
* 4299
* 4300
* 4301
* 4305
* 4306
* 4307
* 4309
* 4309A
* 4313
* 4316
* 4318
* 4320
* 4324
* 4326
* 4330
* 4333
* 4334
* 4339
* 4341
* 4342
* 4343
* 4348
* 4351
* 4352
* 4353
* 4356
* 4360
* 4365
* 4366
* 4368
* 4370
* 4371
* 4376
* 4378
* 4380
* 4385
* 4387
* 4388
* 4390
* 4402
* 4403
* 4404
* 4410
* 4411
* 4412
* 4413
* 4415
* 4416
* 4417
* 4418
* 4420
* 4422
* 4423
* 4424
* 4425
* 4428
* 4429
* 4430
* 4431
* 4432
* 4433
* 4434
* 4436
* 4440
* 4442
* 4445
* 4451
* 4452
* 4453
* 4454
* 4457
* 4458
* 4461
* 4464
* 4465
* 4466
* 4467
* 4469
* 4470
* 4476
* 4478
* 4480
* 4482
* 4483
* 4484
* 4486A
* 4486B
* 4487
* 4488
* 4491
* 4492
* 4493
* 4496
* 4496B
* 4497
* 4503
* 4504
* 4517
* 4517A
* 4518
* 4518B
* 4519
* 4519A
* 4520
* 4522
* 4526
* 4527
* 4528
* 4531
* 4532
* 4533
* 4535
* 4535A
* 4536
* 4538
* 4541
* 4543
* 4544
* 4546
* 4550
* 4551
* 4564
* 4567
* 4568
* 4570
* 4576
* 4577
* 4578
* 4580
* 4581
* 4584
* 4586
* 4587
* 4588
* 4592
* 4593
* 4596
* 4597
* 4598
* 4599
* 4600
* 4602
* 4604
* 4606
* 4607
* 4608
* 4612
* 4620
* 4623
* 4626
* 4628
* 4629
* 4630
* 4632
* 4636
* 4637
* 4638
* 4639
* 4640
* 4640B
* 4641
* 4642
* 4643
* 4747 ([[Arp 116]])
* 4653
* 4654
* 4658
* 4660
* 4663
* 4664
* 4666
* 4668
* 4671
* 4674
* 4678
* 4680
* 4682
* 4684
* 4688
* 4690
* 4691
* 4694
* 4697
* 4698
* 4699
* 4700
* 4701
* 4703
* 4705
* 4708
* 4713
* 4716
* 4717
* 4718
* 4720
* 4731
* 4731A
* 4733
* 4734
* 4739
* 4742
* 4746
* 4753
* 4754
* 4757
* 4759A
* 4760
* 4761
* 4762
* 4764
* 4765
* 4766
* 4770
* 4771
* 4772
* 4773
* 4775
* 4777
* 4778
* 4779
* 4780
* 4780A
* 4781
* 4784
* 4786
* 4790
* 4791
* 4795
* 4796
* 4799
* 4803
* 4808
* 4809
* 4810
* 4813
* 4818
* 4820
* 4822
* 4823
* 4825
* 4829
* 4830
* 4836
* 4838
* 4843
* 4845
* 4847
* 4855
* 4856
* 4862
* 4863
* 4866
* 4877
* 4878
* 4880
* 4885
* 4887
* 4888
* 4890
* 4897
* 4899
* 4900
* 4902
* 4904
* 4915
* 4918
* 4920
* 4924
* 4925
* 4928
* 4933
* 4933C
* 4939
* 4941
* 4942
* 4948
* 4948A
* 4951
* 4958
* 4969
* 4975
* 4981
* 4984
* 4989
* 4990
* 4991
* 4992
* 4995
* 4996
* 4997
* 4999
* 5006
* 5010
* 5013
* 5015
* 5017
* 5018
* 5019
* 5020
* 5022
* 5027
* 5028
* 5030
* 5031
* 5035
* 5036
* 5037
* 5038
* 5039
* 5044
* 5046
* 5047
* 5049
* 5050
* 5054
* 5058
* 5059
* 5060
* 5066
* 5068
* 5071
* 5072
* 5073
* 5075
* 5076
* 5077
* 5079
* 5080
* 5084
* 5087
* 5088
* 5094
* 5095
* 5097
* 5099
* 5104
* 5105
* 5106
* 5111
* 5115
* 5118
* 5119
* 5122
* 5125
* 5129
* 5130
* 5132
* 5133
* 5134
* 5136
* 5137
* 5146
* 5147
* 5148
* 5159
* 5165
* 5167
* 5170
* 5171
* 5174
* 5176
* 5177
* 5178
* 5179
* 5181
* 5183
* 5184
* 5185
* 5186
* 5191
* 5192
* 5196
* 5197
* 5202
* 5203
* 5207
* 5208
* 5209
* 5210
* 5211
* 5212
* 5213
* 5221
* 5222
* 5224
* 5226
* 5227
* 5230
* 5231
* 5232
* 5235
* 5241
* 5245
* 5246
* 5247
* 5252
* 5254
* 5261
* 5270
* 5285
* 5300
* 5306
* 5324
* 5327
* 5329
* 5331
* 5334
* 5335
* 5338
* 5339
* 5343
* 5345
* 5348
* 5356
* 5360
* 5363
* 5364
* 5366
* 5369
* 5373
* 5374
* 5382
* 5384
* 5386
* 5387
* 5392
* 5400
* 5420
* 5442
* 5468
* 5470
* 5472
* 5476
* 5478
* 5491A
* 5491B
* 5493
* 5496
* 5501
* 5506
* 5507
* 5510
* 5521
* 5534
* 5537
* 5549
* 5551
* 5552
* 5554
* 5555
* 5560
* 5563
* 5566
* 5569
* 5573
* 5574
* 5575
* 5576
* 5577
* 5584
* 5599
* 5604
* 5618
* 5619
* 5619C
* 5636
* 5638
* 5645
* 5652
* 5661
* 5668
* 5674
* 5679
* 5679A
* 5679C
* 5679D
* 5680
* 5690
* 5691
* 5692
* 5701
* 5705
* 5713
* 5718
* 5719
* 5725
* 5733
* 5738
* 5740
* 5746
* 5750
* 5765
* 5765B
* 5770
* 5774
* 5775
* 5776
* 5806
* 5811
* 5813
* 5814
* 5831
* 5838
* 5839
* 5845
* 5846
* 5846A
* 5847
* 5848
* 5850
* 5854
* 5855
* 5864
* 5865
* 5869

Other|

* A1689-zD1
* Abell 1835 IR1916
* Arp 240 (NGC 5257 and NGC 5258)
* Arp 271 (NGC 5426 and NGC 5427)
* BR 1202-0725
* 3C 273
* 3C 279
* 3C 298
* 4C 04.42
* Eyes Galaxies
* GR 8
* IC 3258
* IC 3328
* IRAS 12212+0305
* IRAS 13197−1627
* M60-UCD1
* Markarian 50
* Markarian 1318
* PG 1216+069
* PG 1244+026
* PG 1254+047
* PG 1307+085
* PG 1416−129
* PG 1426+015
* PKS 1148-001
* PKS 1167+014
* PKS 1217+023
* PKS 1229−021
* PKS 1302−102
* PKS 1335−127
* PKS 1402+044
* PKS 1405−076
* QSO B1208+1011
* QSO B1243−072
* QSO B1246−057
* QSO B1331+170
* RXJ1242−11
* SMM J14011+0252
* UM 448
* UM 461
* UM 462

Galaxy
clusters|

* Abell 1644
* Abell 1650
* Abell 1651
* Abell 1689
* Abell 1750
* Abell 1835
* Abell 2029
* Abell 2147
* HCG 62
* MKW 4
* NGC 5044 group
* RX J1347.5−1145
* Virgo Cluster

Other|

* GRB 930131
* GRB 030328
* GRB 050408
* GRB 050801
* GRB 080310
* North Polar Spur
* SN 1960F
* SN 1981B
* SN 1990B
* SN 1990N
* SN 1991T
* SN 1991bg
* SN 1994D
* SN 1999br
* SN 2002cx
* SN 2007bi
* U1.11

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Original source: https://en.wikipedia.org/wiki/IC 1101. Read more

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